Aug. 2021, 2021次世代放射線シンポジウム（応用物理学会放射線分科会主催）優秀研究賞（放射線分科会）, 核医学施設における回転機能付き高感度全方向コンプトンカメラを用いた測定
石川咲貴、村石 浩、榎本良治、片桐秀明、加賀谷美佳、渡辺 宝、加納大輔、中村哲志、渡邉祐介、石山博條
Japan society

Apr. 2016, 第111回日本医学物理学会学術大会 大会長賞, Development of an all-sky RI imaging monitor capable of measuring high-dose-rate gamma-ray sources, 日本医学物理学会
渡辺 宝;内田 智久;榎本 良治;加賀谷 美佳;片桐 秀明;加納 大輔;佐藤 一弘;佐藤 亘;武田 徹;田中 真伸;西尾 禎治;村石 浩;吉田 龍生;若松 諒;和田 清人
Japan society

Apr. 2016, 第111回日本医学物理学会学術大会 大会長賞, Development of an all-sky RI imaging monitor capable of measuring high-dose-rate gamma-ray sources, 日本医学物理学会
13.渡辺 宝;内田 智久;榎本 良治、加賀谷 美佳;片桐 秀明;加納 大輔;佐藤 一弘;佐藤 亘;武田 徹;田中 真伸;西尾 禎治;村石 浩;吉田 龍生;若松 諒;和田 清人
Japan society

Sep. 2015, 第110 回日本医学物理学会学術大会 優秀研究賞, ガンマ線の到来方向がわかるコンプトン型サーベイメータの開発, 日本医学物理学会
加賀谷 美佳;若松 諒;榎本 良治;片桐 秀明;加納 大輔;西尾 禎治;伊東 良和;内田 智久;佐藤 一弘;佐藤 亘;武田 徹;田中 真伸;花房 龍治;細川 正男;村石 浩;吉田 龍生;渡辺 宝;和田 清人
Japan society

Sep. 2015, 第110 回日本医学物理学会学術大会 優秀研究賞, ガンマ線の到来方向がわかるコンプトン型サーベイメータの開発, 日本医学物理学会
加賀谷 美佳、若松 諒、榎本 良治、片桐 秀明、加納 大輔、西尾 禎治、伊東 良和、内田 智久、佐藤 一弘、佐藤 亘、武田 徹、田中 真伸、花房 龍治、細川 正男、村石 浩、吉田 龍生、渡辺 宝、和田 清人
Japan society

2014, 第107回日本医学物理学会学術大会大会長賞, Development of a novel γ-ray imaging system (γI:gamma-eye) using Compton camera technique
村石 浩、内田 智久、榎本 良治、加賀谷 美佳、片桐 秀明、佐藤 一弘、武田 徹、田中 真伸、中山 浩平、花房 龍治、柳田 昭平、吉田 龍生、渡辺 宝

2013, 第33回日本医用画像工学会大会 奨励賞, コンプトカメラ法による360°パノラマRI イメージングモニターの開発, 日本医用画像工学会
渡辺 宝;井上優介;内田智久;榎本良治;加賀谷美佳;片桐秀明;菊池 敬;武田徹;田中真伸;徳重 尊宣;中山浩平;村石 浩;柳田昭平;吉田龍生
Japan society

2013, 第106 回日本医学物理学会学術大会優秀研究賞, Application of a filtered back projection algorithm to Compton camera technique
村石 浩、榎本 良治、加賀谷 美佳、片桐 秀明、武田 徹、中山 浩平、柳田 昭平、吉田 龍生

2013, 第33回日本医用画像工学会大会 奨励賞, コンプトカメラ法による360°パノラマRI イメージングモニターの開発, 日本医用画像工学会
3.渡辺 宝、井上優介、内田智久、榎本良治、加賀谷美佳、片桐秀明、菊池 敬、武田徹、田中真伸、徳重 尊宣、中山浩平、村石 浩、柳田昭平、吉田龍生
Japan society

〔Major achievements〕Evaluating the capability of detecting recoil-electron tracks using an electron-tracking Compton camera with a silicon-on-insulator pixel sensor
Mika Kagaya; Hideaki Katagiri; Ryo Kato; Naomi Tojo; Takeshi Go Tsuru; Ayaki Takeda; Yasuo Arai; Kenji Shimazoe, Sub-MeV gamma-ray line observations are crucial for the understanding of high-energy astrophysical processes. In this energy range, the presence of a significant amount of background poses a serious problem. Therefore, it is essential to reduce this background to achieve high-sensitivity observations. An electron-tracking Compton camera can efficiently mitigate the impact of background on scientific results thanks to its ability to fully resolve the Compton process. In addition if we utilize a semiconductor detector as the sensor, the electron-tracking Compton camera can achieve high-energy resolution for the detection of gamma-ray lines. To operate the electron-tracking Compton camera effectively, the sensor needs to coincidence events for each detection signal and resolve the complex structure of recoiled-electron tracks of a few hundred ,. We focused on the silicon-on-insulator pixel sensor XRPIX2b developed for X-ray observations, which satisfies requirements. We developed a prototype electron-tracking Compton camera using XRPIX2b and carried out a quantitative evaluation of its detection capability for estimating the recoil directions of electrons at various angles. As a result, we successfully detected short recoil-electron tracks with a length of , corresponded to scattering angles of 30°-40° for 511 keV gamma rays entering the sensor. In term of angular resolution measure and scatter plane deviation of a reconstructed image, the evaluations showed results of 15° and 40° (full width at half maximum), respectively, in cases where 511 keV gamma rays were scattered at 90° and recoil electrons tracked the surface of the sensor detection plane. We confirmed that these results were consistent with simulation results, within approximately a 15% margin.
Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, May 2024, [Reviewed]

Performance of the joint LST-1 and MAGIC observations evaluated with Crab Nebula data
H. Abe; K. Abe; S. Abe; V. A. Acciari; A. Aguasca-Cabot; I. Agudo; N. Alvarez Crespo; T. Aniello; S. Ansoldi; L. A. Antonelli; C. Aramo; A. Arbet-Engels; C. Arcaro; M. Artero; K. Asano; P. Aubert; D. Baack; A. Babić; A. Baktash; A. Bamba; A. Baquero Larriva; L. Baroncelli; U. Barres De Almeida; J. A. Barrio; I. Batković; J. Baxter; J. Becerra González; W. Bednarek; E. Bernardini; M. I. Bernardos; J. Bernete Medrano; A. Berti; J. Besenrieder; P. Bhattacharjee; N. Biederbeck; C. Bigongiari; A. Biland; E. Bissaldi; O. Blanch; G. Bonnoli; P. Bordas; Bošnjak; A. Bulgarelli; I. Burelli; L. Burmistrov; M. Buscemi; G. Busetto; A. Campoy Ordaz; M. Cardillo; S. Caroff; A. Carosi; R. Carosi; M. S. Carrasco; M. Carretero-Castrillo; F. Cassol; A. J. Castro-Tirado; D. Cauz; D. Cerasole; G. Ceribella; Y. Chai; K. Cheng; A. Chiavassa; M. Chikawa; L. Chytka; A. Cifuentes; S. Cikota; E. Colombo; J. L. Contreras; A. Cornelia; J. Cortina; H. Costantini; S. Covino; G. D'Amico; V. D'Elia; P. Da Vela; M. Dalchenko; F. Dazzi; A. De Angelis; M. De Bony De Lavergne; B. De Lotto; M. De Lucia; R. De Menezes; L. Del Peral; A. Del Popolo; G. Deleglise; M. Delfino; C. Delgado Mendez; J. Delgado Mengual; D. Della Volpe; M. Dellaiera; D. Depaoli; A. De Angelis; A. Di Piano; F. Di Pierro; A. Di Pilato; R. Di Tria; L. Di Venere; R. M. Dominik; D. Dominis Prester; A. Donini, Aims. Large-Sized Telescope 1 (LST-1), the prototype for the Large-Sized Telescope at the upcoming Cherenkov Telescope Array Observatory, is concluding its commissioning phase at the Observatorio del Roque de los Muchachos on the island of La Palma. The proximity of LST-1 to the two MAGIC (Major Atmospheric Gamma Imaging Cherenkov) telescopes makes it possible to carry out observations of the same gamma-ray events with both systems.,,Methods. We describe the joint LST-1+MAGIC analysis pipeline and used simultaneous Crab Nebula observations and Monte Carlo simulations to assess the performance of the three-telescope system. The addition of the LST-1 telescope allows for the recovery of events in which one of the MAGIC images is too dim to survive analysis quality cuts.,,Results. Thanks to the resulting increase in the collection area and stronger background rejection, we found a significant improvement in sensitivity, allowing for the detection of 30% weaker fluxes in the energy range between 200 GeV and 3 TeV. The spectrum of the Crab Nebula, reconstructed in the energy range between ~60 GeV and ~10 TeV, is in agreement with previous measurements.
Astronomy and Astrophysics, 01 Dec. 2023, [Reviewed]

Observations of the Crab Nebula and Pulsar with the Large-sized Telescope Prototype of the Cherenkov Telescope Array
H. Abe; K. Abe; S. Abe; A. Aguasca-Cabot; I. Agudo; N. Alvarez Crespo; L. A. Antonelli; C. Aramo; A. Arbet-Engels; C. Arcaro; M. Artero; K. Asano; P. Aubert; A. Baktash; A. Bamba; A. Baquero Larriva; L. Baroncelli; U. Barres de Almeida; J. A. Barrio; I. Batkovic; J. Baxter; J. Becerra González; E. Bernardini; M. I. Bernardos; J. Bernete Medrano; A. Berti; P. Bhattacharjee; N. Biederbeck; C. Bigongiari; E. Bissaldi; O. Blanch; G. Bonnoli; P. Bordas; A. Borghese; A. Bulgarelli; I. Burelli; M. Buscemi; M. Cardillo; S. Caroff; A. Carosi; F. Cassol; D. Cauz; G. Ceribella; Y. Chai; K. Cheng; A. Chiavassa; M. Chikawa; L. Chytka; A. Cifuentes; J. L. Contreras; J. Cortina; H. Costantini; G. D’Amico; M. Dalchenko; A. De Angelis; M. de Bony de Lavergne; B. De Lotto; R. de Menezes; G. Deleglise; C. Delgado; J. Delgado Mengual; D. della Volpe; M. Dellaiera; D. Depaoli; A. Di Piano; F. Di Pierro; R. Di Tria; L. Di Venere; C. Díaz; R. M. Dominik; D. Dominis Prester; A. Donini; D. Dorner; M. Doro; D. Elsässer; G. Emery; J. Escudero; V. Fallah Ramazani; G. Ferrara; F. Ferrarotto; A. Fiasson; L. Freixas Coromina; S. Fröse; S. Fukami; Y. Fukazawa; E. Garcia; R. Garcia López; C. Gasbarra; D. Gasparrini; F. Geyer; J. Giesbrecht Paiva; N. Giglietto; F. Giordano; E. Giro; P. Gliwny; N. Godinovic; R. Grau; D. Green; J. Green; S. Gunji, The Cherenkov Telescope Array (CTA) is a next-generation ground-based observatory for gamma-ray astronomy at very high energies. The Large-Sized Telescope prototype (LST-1) is located at the CTA-North site, on the Canary Island of La Palma. LSTs are designed to provide optimal performance in the lowest part of the energy range covered by CTA, down to ≃20 GeV. LST-1 started performing astronomical observations in 2019 November, during its commissioning phase, and it has been taking data ever since. We present the first LST-1 observations of the Crab Nebula, the standard candle of very-high-energy gamma-ray astronomy, and use them, together with simulations, to assess the performance of the telescope. LST-1 has reached the expected performance during its commissioning period—only a minor adjustment of the preexisting simulations was needed to match the telescope's behavior. The energy threshold at trigger level is around 20 GeV, rising to ≃30 GeV after data analysis. Performance parameters depend strongly on energy, and on the strength of the gamma-ray selection cuts in the analysis: angular resolution ranges from 0fdg12–0fdg40, and energy resolution from 15%–50%. Flux sensitivity is around 1.1% of the Crab Nebula flux above 250 GeV for a 50 hr observation (12% for 30 minutes). The spectral energy distribution (in the 0.03–30 TeV range) and the light curve obtained for the Crab Nebula agree with previous measurements, considering statistical and systematic uncertainties. A clear periodic signal is also detected from the pulsar at the center of the Nebula.
Astrophysical Journal, 01 Oct. 2023, [Reviewed]

Multiwavelength study of the galactic PeVatron candidate LHAASO J2108+515
Abe; S.; Aguasca-Cabot; A.; Agudo; I.; et al., Context. Several new ultrahigh-energy (UHE) γ-ray sources have recently been discovered by the Large High Altitude Air Shower Observatory (LHAASO) collaboration. These represent a step forward in the search for the so-called Galactic PeVatrons, the enigmatic sources of the Galactic cosmic rays up to PeV energies. However, it has been shown that multi-TeV γ-ray emission does not necessarily prove the existence of a hadronic accelerator in the source; indeed this emission could also be explained as inverse Compton scattering from electrons in a radiation-dominated environment. A clear distinction between the two major emission mechanisms would only be made possible by taking into account multi-wavelength data and detailed morphology of the source.

Aims. We aim to understand the nature of the unidentified source LHAASO J2108+5157, which is one of the few known UHE sources with no very high-energy (VHE) counterpart.

Methods. We observed LHAASO J2108+5157 in the X-ray band with XMM-Newton in 2021 for a total of 3.8 hours and at TeV energies with the Large-Sized Telescope prototype (LST-1), yielding 49 hours of good-quality data. In addition, we analyzed 12 years of Fermi-LAT data, to better constrain emission of its high-energy (HE) counterpart 4FGL J2108.0+5155. We used naima and jetset software packages to examine the leptonic and hadronic scenario of the multi-wavelength emission of the source.

Results. We found an excess (3.7σ) in the LST-1 data at energies E > 3 TeV. Further analysis of the whole LST-1 energy range, assuming a point-like source, resulted in a hint (2.2σ) of hard emission, which can be described with a single power law with a photon index of Γ = 1.6 ± 0.2 the range of 0.3 − 100 TeV. We did not find any significant extended emission that could be related to a supernova remnant (SNR) or pulsar wind nebula (PWN) in the XMM-Newton data, which puts strong constraints on possible synchrotron emission of relativistic electrons. We revealed a new potential hard source in Fermi-LAT data with a significance of 4σ and a photon index of Γ = 1.9 ± 0.2, which is not spatially correlated with LHAASO J2108+5157, but including it in the source model we were able to improve spectral representation of the HE counterpart 4FGL J2108.0+5155.

Conclusions. The LST-1 and LHAASO observations can be explained as inverse Compton-dominated leptonic emission of relativistic electrons with a cutoff energy of 100₋₃₀⁺⁷⁰ TeV. The low magnetic field in the source imposed by the X-ray upper limits on synchrotron emission is compatible with a hypothesis of a PWN or a TeV halo. Furthermore, the spectral properties of the HE counterpart are consistent with a Geminga-like pulsar, which would be able to power the VHE-UHE emission. Nevertheless, the lack of a pulsar in the neighborhood of the UHE source is a challenge to the PWN/TeV-halo scenario. The UHE γ rays can also be explained as π⁰ decay-dominated hadronic emission due to interaction of relativistic protons with one of the two known molecular clouds in the direction of the source. Indeed, the hard spectrum in the LST-1 band is compatible with protons escaping a shock around a middle-aged SNR because of their high low-energy cut-off, but the origin of the HE γ-ray emission remains an open question., EDP Sciences
Astronomy & Astrophysics, May 2023, [Reviewed]

Gamma-ray imaging in a nuclear medicine facility using a compact and portable high-sensitivity omnidirectional Compton camera with detector rotation function
石川咲貴; 村石浩; 榎本良治; 片桐秀明; 加賀谷美佳; 渡辺宝; 加納大輔; 中村哲志; 渡邉祐介; 石山博條
放射線(Web), Oct. 2022, [Reviewed]

Reconstruction of extensive air shower images of the first Large Size Telescope prototype of CTA using a novel likelihood technique
Gabriel Emery; Cyril Alispach; Mykhailo Dalchenko; Luca Foffano; Matthieu Heller; Teresa Montaruli; H. Abe; A. Aguasca; I. Agudo; L. A. Antonelli; C. Aramo; T. Armstrong; M. Artero; K. Asano; H. Ashkar; P. Aubert; A. Baktash; A. Bamba; A. Baquero Larriva; L. Baroncelli; U. Barres de Almeida; J. A. Barrio; I. Batkovic; J. Becerra González; M. I. Bernardos; A. Berti; N. Biederbeck; C. Bigongiari; O. Blanch; G. Bonnoli; P. Bordas; D. Bose; A. Bulgarelli; I. Burelli; M. Buscemi; M. Cardillo; S. Caroff; A. Carosi; F. Cassol; M. Cerruti; Y. Chai; K. Cheng; M. Chikawa; L. Chytka; J. L. Contreras; J. Cortina; H. Costantini; A. De Angelis; M. de Bony de Lavergne; G. Deleglise; C. Delgado; J. Delgado Mengual; D. della Volpe; D. Depaoli; F. Di Pierro; L. Di Venere; C. Díaz; R. M. Dominik; D. Dominis Prester; A. Donini; D. Dorner; M. Doro; D. Elsässer; J. Escudero; A. Fiasson; M. V. Fonseca; L. Freixas Coromina; S. Fukami; Y. Fukazawa; E. Garcia; R. Garcia López; N. Giglietto; F. Giordano; P. Gliwny; N. Godinovic; D. Green; P. Grespan; S. Gunji; J. Hackfeld; D. Hadasch; A. Hahn; T. Hassan; K. Hayashi; L. Heckmann; J. Herrera Llorente; K. Hirotani; D. Hoffmann; D. Horns; J. Houles; M. Hrabovsky; D. Hrupec; D. Hui; M. Hütten; T. Inada; Y. Inome; M. Iori; K. Ishio; Y. Iwamura; M. Jacquemont; I. Jimenez Martinez, Ground-based gamma-ray astronomy aims at reconstructing the energy and direction of gamma rays from the extensive air showers they initiate in the atmosphere. Imaging Atmospheric Cherenkov Telescopes (IACT) collect the Cherenkov light induced by secondary charged particles in extensive air showers (EAS), creating an image of the shower in a camera positioned in the focal plane of optical systems. This image is used to evaluate the type, energy and arrival direction of the primary particle that initiated the shower. This contribution shows the results of a novel reconstruction method based on likelihood maximization. The novelty with respect to previous likelihood reconstruction methods lies in the definition of a likelihood per single camera pixel, accounting not only for the total measured charge, but also for its development over time. This leads to more precise reconstruction of shower images. The method is applied to observations of the Crab Nebula acquired with the Large Size Telescope prototype (LST-1) deployed at the northern site of the Cherenkov Telescope Array.
Proceedings of Science, 18 Mar. 2022

Cross-calibration and combined analysis of the CTA-LST prototype and the MAGIC telescopes
Y. Ohtani; A. Berti; D. Depaoli; F. Di Pierro; D. Green; L. Heckmann; M. Hütten; T. Inada; R. López-Coto; E. Medina; A. Moralejo; D. Morcuende; G. Pirola; M. Strzys; Y. Suda; I. Vovk; H. Abe; A. Aguasca; I. Agudo; L. A. Antonelli; C. Aramo; T. Armstrong; M. Artero; K. Asano; H. Ashkar; P. Aubert; A. Baktash; A. Bamba; A. Baquero Larriva; L. Baroncelli; U. Barres de Almeida; J. A. Barrio; I. Batkovic; J. Becerra González; M. I. Bernardos; N. Biederbeck; C. Bigongiari; O. Blanch; G. Bonnoli; P. Bordas; D. Bose; A. Bulgarelli; I. Burelli; M. Buscemi; M. Cardillo; S. Caroff; A. Carosi; F. Cassol; M. Cerruti; Y. Chai; K. Cheng; M. Chikawa; L. Chytka; J. L. Contreras; J. Cortina; H. Costantini; M. Dalchenko; A. De Angelis; M. de Bony de Lavergne; G. Deleglise; C. Delgado; J. Delgado Mengual; D. della Volpe; L. Di Venere; C. Díaz; R. M. Dominik; D. Dominis Prester; A. Donini; D. Dorner; M. Doro; D. Elsässer; G. Emery; J. Escudero; A. Fiasson; L. Foffano; M. V. Fonseca; L. Freixas Coromina; S. Fukami; Y. Fukazawa; E. Garcia; R. Garcia López; N. Giglietto; F. Giordano; P. Gliwny; N. Godinovic; P. Grespan; S. Gunji; J. Hackfeld; D. Hadasch; A. Hahn; T. Hassan; K. Hayashi; M. Heller; J. Herrera Llorente; K. Hirotani; D. Hoffmann; D. Horns; J. Houles; M. Hrabovsky; D. Hrupec, The Cherenkov Telescope Array (CTA) will be the next generation gamma-ray observatory, which will consist of three kinds of telescopes of different sizes. Among those, the Large Size Telescope (LST) will be the most sensitive in the low energy range starting from 20 GeV. The prototype LST (LST-1) proposed for CTA was inaugurated in October 2018 in the northern hemisphere site, La Palma (Spain), and is currently in its commissioning phase. MAGIC is a system of two gamma-ray Cherenkov telescopes of the current generation, located approximately 100 m away from LST-1, that have been operating in stereoscopic mode since 2009. Since LST-1 and MAGIC can observe the same air shower events, we can compare the brightness of showers, estimated energies of gamma rays, and other parameters event by event, which can be used to cross-calibrate the telescopes. Ultimately, by performing combined analyses of the events triggering the three telescopes, we can reconstruct the shower geometry more accurately, leading to better energy and angular resolutions, and a better discrimination of the background showers initiated by cosmic rays. For that purpose, as part of the commissioning of LST-1, we performed joint observations of established gamma-ray sources with LST-1 and MAGIC. Also, we have developed Monte Carlo simulations for such joint observations and an analysis pipeline which finds event coincidence in the offline analysis based on their timestamps. In this work, we present the first detection of an astronomical source, the Crab Nebula, with combined observation of LST-1 and MAGIC. Moreover, we show results of the inter-telescope cross-calibration obtained using Crab Nebula data taken during joint observations with LST-1 and MAGIC.
Proceedings of Science, 18 Mar. 2022

Deep-learning-driven event reconstruction applied to simulated data from a single Large-Sized Telescope of CTA
H. Abe; A. Aguasca; I. Agudo; L. A. Antonelli; C. Aramo; T. Armstrong; M. Artero; K. Asano; H. Ashkar; P. Aubert; A. Baktash; A. Bamba; A. Baquero Larriva; L. Baroncelli; U. Barres de Almeida; J. A. Barrio; I. Batkovic; J. Becerra González; M. I. Bernardos; A. Berti; N. Biederbeck; C. Bigongiari; O. Blanch; G. Bonnoli; P. Bordas; D. Bose; A. Bulgarelli; I. Burelli; M. Buscemi; M. Cardillo; S. Caroff; A. Carosi; F. Cassol; M. Cerruti; Y. Chai; K. Cheng; M. Chikawa; L. Chytka; J. L. Contreras; J. Cortina; H. Costantini; M. Dalchenko; A. De Angelis; M. de Bony de Lavergne; G. Deleglise; C. Delgado; J. Delgado Mengual; D. della Volpe; D. Depaoli; F. Di Pierro; L. Di Venere; C. Díaz; R. M. Dominik; D. Dominis Prester; A. Donini; D. Dorner; M. Doro; D. Elsässer; G. Emery; J. Escudero; A. Fiasson; L. Foffano; M. V. Fonseca; L. Freixas Coromina; S. Fukami; Y. Fukazawa; E. Garcia; R. Garcia López; N. Giglietto; F. Giordano; P. Gliwny; N. Godinovic; D. Green; P. Grespan; S. Gunji; J. Hackfeld; D. Hadasch; A. Hahn; T. Hassan; K. Hayashi; L. Heckmann; M. Heller; J. Herrera Llorente; K. Hirotani; D. Hoffmann; D. Horns; J. Houles; M. Hrabovsky; D. Hrupec; D. Hui; M. Hütten; T. Inada; Y. Inome; M. Iori; K. Ishio; Y. Iwamura; M. Jacquemont; I. Jimenez Martinez; L. Jouvin; J. Jurysek, When very-high-energy gamma rays interact high in the Earth's atmosphere, they produce cascades of particles that induce flashes of Cherenkov light. Imaging Atmospheric Cherenkov Telescopes (IACTs) detect these flashes and convert them into shower images that can be analyzed to extract the properties of the primary gamma ray. The dominant background for IACTs is comprised of air shower images produced by cosmic hadrons, with typical noise-to-signal ratios of several orders of magnitude. The standard technique adopted to differentiate between images initiated by gamma rays and those initiated by hadrons is based on classical machine learning algorithms, such as Random Forests, that operate on a set of handcrafted parameters extracted from the images. Likewise, the inference of the energy and the arrival direction of the primary gamma ray is performed using those parameters. State-of-the-art deep learning techniques based on convolutional neural networks (CNNs) have the potential to enhance the event reconstruction performance, since they are able to autonomously extract features from raw images, exploiting the pixel-wise information washed out during the parametrization process. Here we present the results obtained by applying deep learning techniques to the reconstruction of Monte Carlo simulated events from a single, next-generation IACT, the Large-Sized Telescope (LST) of the Cherenkov Telescope Array (CTA). We use CNNs to separate the gamma-ray-induced events from hadronic events and to reconstruct the properties of the former, comparing their performance to the standard reconstruction technique. Three independent implementations of CNN-based event reconstruction models have been utilized in this work, producing consistent results.
Proceedings of Science, 18 Mar. 2022

CTA – the World's largest ground-based gamma-ray observatory
Zanin; R.; Abdalla; H.; Abe; H.; et al.
37th International Cosmic Ray Conference. 12-23 July 2021. Berlin, 5, Mar. 2022

Analysis of the Cherenkov Telescope Array first Large Size Telescope real data using convolutional neural networks
CTA-LST Project; T.; Abe; H.; Aguasca; A.; et al.
37th International Cosmic Ray Conference. 12-23 July 2021. Berlin, 703, Mar. 2022

Monitoring the pointing of the Large Size Telescope prototype using star reconstruction in the Cherenkov camera
Foffano; L.; Carosi; A.; Della Volpe; D.; et al.
37th International Cosmic Ray Conference. 12-23 July 2021. Berlin, 712, Mar. 2022

Commissioning of the camera of the first Large Size Telescope of the Cherenkov Telescope Array
Blanch; O.; Delgado; C.; Saito; T.; et al.
37th International Cosmic Ray Conference. 12-23 July 2021. Berlin, 718, Mar. 2022

Physics Performance of the Large Size Telescope prototype of the Cherenkov Telescope Array
CTA-LST Project; T.; Abe; H.; Aguasca; A.; et al., 37th International Cosmic Ray Conference. 12-23 July 2021. Berlin, 806
37th International Cosmic Ray Conference. 12-23 July 2021. Berlin, 806, Mar. 2022

First follow-up of transient events with the CTA Large Size Telescope prototype
CTA-LST Project; T.; Abe; H.; Aguasca; A.; et al.
37th International Cosmic Ray Conference. 12-23 July 2021. Berlin, 838, Mar. 2022

Status and results of the prototype LST of CTA
CTA-LST Project; T.; Abe; H.; Aguasca; A.; et al.
37th International Cosmic Ray Conference. 12-23 July 2021. Berlin, 872, Mar. 2022

Development of an advanced SiPM camera for the Large Size Telescope of the Cherenkov TelescopeArray Observatory
CTA-LST Project; T.; Abe; H.; Aguasca; A.; et al.
37th International Cosmic Ray Conference. 12-23 July 2021. Berlin, 889, Mar. 2022

Camera Calibration of the CTA-LST prototype
Y. Kobayashi; A. Okumura; F. Cassol; H. Katagiri; J. Sitarek; P. Gliwny and S. Nozaki et al., The Cherenkov Telescope Array (CTA) is the next-generation gamma-ray observatory that is expected to reach one order of magnitude better sensitivity than that of current telescope arrays. The Large-Sized Telescopes (LSTs) have an essential role in extending the energy range down to 20 GeV. The prototype LST (LST-1) proposed for CTA was built in La Palma, the northern site of CTA, in 2018. LST-1 is currently in its commissioning phase and moving towards scientific observations. The LST-1 camera consists of 1855 photomultiplier tubes (PMTs) which are sensitive to Cherenkov light. PMT signals are recorded as waveforms sampled at 1 GHz rate with Domino Ring Sampler version 4 (DRS4) chips. Fast sampling is essential to achieve a low energy threshold by minimizing the integration of background light from the night sky. Absolute charge calibration can be performed by the so-called F-factor method, which allows calibration constants to be monitored even during observations. A calibration pipeline of the camera readout has been developed as part of the LST analysis chain. The pipeline performs DRS4 pedestal and timing corrections, as well as the extraction and calibration of charge and time of pulses for subsequent higher-level analysis. The performance of each calibration step is examined, and especially charge and time resolution of the camera readout are evaluated and compared to CTA requirements. We report on the current status of the calibration pipeline, including the performance of each step through to signal reconstruction, and the consistency with Monte Carlo simulations.
37th International Cosmic Ray Conference. 12-23 July 2021. Berlin, 720, Mar. 2022

Development of an omnidirectional Compton camera using CaF2(Eu) scintillators to visualize gamma rays with energy below 250 keV for radioactive environmental monitoring in nuclear medicine facilities
H. Katagiri; N. Narita; R. Enomoto; H. Muraishi; D. Kano; T. Watanabe; R. Wakamatsu; M. Kagaya; M.M. Tanaka, Lead, We developed an omnidirectional Compton camera for radioactive environmental monitoring which can visualize gamma rays with energy below 250 keV emitted from various radiopharmaceuticals used in nuclear medicine facilities to prevent occupational radiation exposure. An omnidirectional Compton camera based on high light yield scintillators CsI(Tl) or NaI(Tl) developed in our previous studies is a promising system for environmental radiation monitoring because it has a wide field of view and high sensitivity for sub-MeV gamma rays. However, its sensitivity rapidly decreases below 250 keV because photoelectric effect becomes more dominant than the Compton scattering process due to their large effective atomic numbers (approximately 50). Thus, CaF(Eu) was adopted, which has both low effective atomic number (approximately 15) and high light yield. Four CaF(Eu) crystals were arranged symmetrically to achieve a relatively uniform acceptance in all directions. Similarly, the detector rotation technique was adopted to suppress artificial patterns in a reconstructed gamma-ray image because of the small number of crystals. Through experiments in a laboratory and at, Elsevier B.V.
Nuclear Instruments and Methods in Physics Research Section A, 21 Apr. 2021, [Reviewed]

Calibration and performance of the readout system based on switched capacitor arrays for the Large-Sized Telescope of the Cherenkov Telescope Array
Seiya Nozaki; et al., The Cherenkov Telescope Array1 (CTA) is the next-generation ground-based observatory for very-high-energy gamma rays. The CTA consists of three types of telescopes with different mirror areas to cover a wide energy range (20 GeV–300 TeV) with an order of magnitude higher sensitivity than the predecessors. Among those telescopes, the Large-Sized Telescope (LST) is designed to detect low-energy gamma rays between 20 GeV and a few TeV with a 23 m diameter mirror. To make the most of such a large light collection area (about 400 m2), the focal plane camera must detect as much reflected Cherenkov light as possible. We have developed each camera component to meet the CTA performance requirements for more than ten years and performed quality-control tests before installing the camera to the telescope.2, 3 The first LST (LST-1) was inaugurated in October 2018 in La Palma, Spain (Figure 1).4 After the inauguration, various calibration tests were performed to adjust hardware parameters and verify the camera performance. In parallel,, SPIE
Proc. SPIE 11447, Ground-based and Airborne Instrumentation for Astronomy VIII, 13 Dec. 2020, [Reviewed]

Design and production of segment mirrors for the Large-Sized Telescopes of the Cherenkov Telescope Array
Tomohiro Inada; et al., CTA (Cherenkov Telescope Array) is a project for the next generation of the ground-based gamma-ray observatory. CTA will cover a wide energy range, 20 GeV and 300 TeV, by 3 types of the telescopes whose diameters are different. The Large-Sized Telescopes (LSTs) of the CTA are designed to cover the lowest energy range. We are working on mirrors for 4 LSTs which will be built at La Palma, Spain. The parabolic primary mirror of CTA-LST is 23 m diameter and its focal length is 28 m. The primary mirror consists of 198 segmented mirrors. Total effective reflective area is about 370 m2. Each mirror has a hexagonal shape of 1.51 m side-by-side size. It has a sandwich structure which consists of aluminum honeycomb (60 mm thickness) and two glass surfaces (2.7 mm) and the total weight is about 47 kg. We used a sputtering deposition technique to coat in the surface with 5 layer. The coated layers protect the surface for long operation such as 10 years at outside with a reflectance degradation of less than 1 % a year. The reflectance of the mirror reaches about 92 % at 400 nm and its resolution is 0.5 mrad in diameter that contains the 80 % light reflected by, SPIE
Proc. SPIE 11451, Advances in Optical and Mechanical Technologies for Telescopes and Instrumentation IV, 13 Dec. 2020, [Reviewed]

Shift-invariant gamma-ray imaging by adding a detector rotation function to a high-sensitivity omnidirectional Compton camera
Hiroshi Muraishi; Ryoji Enomoto; Hideaki Katagiri; Mika Kagaya; Takara Watanabe; Naofumi Narita; Daisuke Kano; Saki Ishikawa and Hiromichi Ishiyama, The Compton camera technique is a well-known method of visualizing the distribution of radiation sources that emit gamma rays with energies of approximately 1 MeV. One major disadvantage of this technique is that the reconstructed image is degraded owing to the appearance of artificial uneven structures caused by accumulating rings estimated from each event. In this study, we demonstrated that we can easily achieve shift-invariant gamma-ray imaging with a drastic reduction in these artificial uneven structures by rotating the Compton camera during the measurement while also applying image sharpening techniques based on the filtered back-projection algorithm used in computed tomography., IOP Publishing
The Japanese Journal of Applied Physics, 04 Sep. 2020, [Reviewed]

¹⁸F-FDG PET受診者の尿中放射能を測定可能な高感度コンプトンカメラの開発
渡辺 宝; 加納 大輔; 村石 浩; 榎本 良治; 片桐 秀明; 加賀谷 美佳; 石川 咲貴; 中神 佳宏, 公益社団法人 応用物理学会
応用物理学会学術講演会講演予稿集, 26 Aug. 2020

シイタケ栽培に用いる立木の微量放射能を伐採前に測定可能な可搬型非破壊検査装置の開発
加賀谷 美佳; 片桐 秀明; 榎本 良治; 金田一 美有; 村石 浩; 石川 咲貴; 渡辺 宝, 公益社団法人 応用物理学会
応用物理学会学術講演会講演予稿集, 26 Aug. 2020

On the Origin of the Gamma-Ray Emission toward SNR CTB 37A with Fermi-LAT
Abdollahi, Soheila; Ballet, Jean; Fukazawa, Yasushi; Katagiri, Hideaki; Condon, Benjamin, The middle-aged supernova remnant (SNR) CTB 37A is known to interact with several dense molecular clouds through the detection of shocked H2 and OH 1720 MHz maser emission. In the present work, we use eight years of Fermi-LAT Pass 8 data, with an improved point-spread function and an increased acceptance, to perform detailed morphological and spectral studies of the γ-ray emission toward CTB 37A from 200 MeV to 200 GeV. The best fit of the source extension is obtained for a very compact Gaussian model with a significance of 5.75σ and a 68% containment radius of 0°116 ± 0°014stat ± 0°017sys above 1 GeV, which is larger than the TeV emission size. The energy spectrum is modeled as a LogParabola, resulting in a spectral index α = 1.92 ± 0.19 at 1 GeV and a curvature β = 0.18 ± 0.05, which becomes softer than the TeV spectrum above 10 GeV. The SNR properties, including a dynamical age of 6000 yr, are derived assuming the Sedov phase. From the multiwavelength modeling of emission toward the remnant, we conclude that the nonthermal radio and GeV emission is mostly due to the reacceleration of
The Astrophysical Journal, Jun. 2020, [Reviewed]

Measurements of radiation from the Fukushima Dai-ichi Nuclear Power,Plant by the Compton Camera: Estimation of Plant-derived Radioactivity
Ryoji Enomoto1; †; Hideaki Katagiri2; Wataru Sato2; Ryo Wakamatsu2; Hiroshi Muraishi3; Mika Kagaya4 and Takara Watanabe5, The dominant interaction of γ-rays (662 keV) from 137Cs in the air is the Compton scattering. The meanfree-,path is approximately 10 g/cm2 (～100 m at NTP). The γ-rays lose their energies and change directions in,this distance. Moreover, there are many obstacles around the ground level in nuclear power plants. The effects,of the scattered γ-rays from the upper air, therefore, become dominant at the long distance (skyshine) from,the radiation source. We observed the two-dimensional images of those scattered γ-rays (the scattering angle,between 18 and 34 degrees) in the site of the Fukushima Dai-ichi Nuclear Power Plant using the Compton,camera. The detail study of those images enables us to estimate radioactivity derived from the Unit-2., Japan Radioisotope Association
RADIOISOTOPES, Jun. 2020, [Reviewed]

回転型高感度コンプトンカメラによる全方向γ線イメージング
村石 浩; 榎本 良治; 片桐 秀明; 加賀谷 美佳; 成田 尚史; 渡辺 宝; 加納 大輔, 公益社団法人 応用物理学会
応用物理学会学術講演会講演予稿集, 28 Feb. 2020

SOIピクセルセンサーを用いた電子飛跡検出型コンプトンカメラの電子反跳角依存性の評価
加藤 凌; 片桐 秀明; 加賀谷 美佳; 東城 直美; 新井 康夫; 武田 彩希; 鶴 剛, 一般社団法人 日本物理学会
日本物理学会講演概要集, 2020

CTA report 161: Cross-calibration of the CTA-LST1 and the MAGIC telescopes
Ohtani Y.; Orito R.; Kajiwara Y.; Katagiri H.; Kushida J.; Kubo H.; Gunji S.; Kobayashi Y.; Saito T.; Sakaki N.; Sakurai S.; Abe H.; Zenin A.; Takahashi Mari; Takahashi Mitsunari; Tateishi D.; Chikawa M.; Choshi Y.; Teshima M.; Nakamori T.; Nabatame Y.; Nishijima K.; Inada T.; Nogami Y.; Nozaki S.; Nomura R.; Harada Y.; Fukami S.; Fujihara C.; Furuta T.; Yamamoto T.; Yoshikoshi T.; Yoshida T.; Imagawa K.; for the CTA-Japan; Iwamura Y.; Ohishi M.; Oka T.; Ogata T.; Okumura A., The Physical Society of Japan
Meeting Abstracts of the Physical Society of Japan, 2020

CTA Report 160: Status of the mono analysis for the LST proposed for CTA
Nozaki S.; Okumura A.; Orito R.; Kajiwara Y.; Katagiri H.; Kushida J.; Kubo H.; Gunji S.; Kobayashi S.; Saito T.; Sakaki N.; Abe H.; Sakurai S.; Zenin A.; Takahashi Mari; Takahashi Mitsunari; Tateishi D.; Chikawa M.; Choshi Y.; Teshima M.; Nakamori T.; Nabatame Y.; Inada T.; Nishijima K.; Nogami Y.; Nomura R.; Harada Y.; Fukami S.; Fujihara C.; Furuta T.; Yamamoto T.; Yoshikoshi T.; Yoshida T.; Imagawa K.; the CTA-Japan Consortium; Iwamura Y.; Ohishi M.; Ohtani Y.; Oka T.; Ogata T., The Physical Society of Japan
Meeting Abstracts of the Physical Society of Japan, 2020

CTA Report 163: Assembly and quality control of focal-plane-camera modules for the 2nd to 4th Large-Sized Telescopes of CTA
������������������ ������������������; ���������������� ��������; ���������������� ��������������; Kawashima Shotaro; Kawamura Kiomei; �������������� ����������; �������� ������������������; ���������� ��������������; ������������������ ������������; ���������� ����������������; �������������� ����������������; ���������� ������������; ������������ ������������; ������������ ��������; ������������ ������������; ������������ ����������; �������������� ����������; Tsukamoto Yusuke; �������������� ����������������; ������������ ������������������; �������������� ������������; ���������������� ��������������; Imagawa Kaname; ������������������ ��������������; Nabatame Yasuyuki; ������������������ ������������; ������������ ��������; ������������ ����������; �������� ��������; �������������� ��������������; ������������ ������������; ���������� ������������; ������������ ������; �������������� ��������; ���������������� ������������������; �������������� ������������; ������ ������-���������� ��������������������; ���������� Masahiro; Sasaki Nobuaki; Dettlaff Antonios; ���������� ����������������; ������ ����������������; �������������� ������; �������������� ����������; ���������� ����������, The Physical Society of Japan
Meeting Abstracts of the Physical Society of Japan, 2020

CTA Report 159: General Report
Kubo Hidetoshi; Inada Tomohiro; Hara Satoshi; Harada Yoshiki; Bamba Aya; Hiroshima Nagisa; Hirotani Kouichi; Hui David C. Y.; Ferrand Gilles; Fukazawa Yasushi; Fukami Satoshi; Fukui Yasuo; Inoue Susumu; Fujikawa Yui; Fujita Yutaka; Fujihara Chikako; Furuta Tomoya; He Haoning; Vovk Ievgen; Majumdar Pratik; Mazin Daniel; Matsumoto Hironori; Mizuno Tsunefumi; Inoue Tsuyoshi; Muraishi Hiroshi; Murase Kohta; Mori Koji; Yanagita Shohei; Yamazaki Ryo; Yamane Yumiko; Yamamoto Tokonatsu; Yamamoto Hiroaki; Yoshikoshi Takanori; Yoshida Atsumasa; Inoue Yoshiyuki; Yoshida Tatsuo; Lee Shiu-Hang (Herman); Inome Yusuke; Imagawa Kaname; Iwamura Yuki; Warren Donald; Uchiyama Yasunobu; Ohishi Michiko; Teshima Masahiro; Ohoka Hideyuki; Ohtani Yoshiki; Ohira Yutaka; Oka Tomohiko; Okazaki Nao; Ogata Tomoyuki; Okumura Akira; Obara Kotaro; Orito Reiko; Kagaya Mika; Totani Tomonori; Kajiwara Yuki; Kataoka Jun; Katagiri Hideaki; Katsukura Daisuke; Katsuda Satoru; Khalikov Emil; Kawashima Shotaro; Kawanaka Norita; Kawamura Kiomei; Kisaka Shota; Asano Katsuaki; Cui Xiaohong; Kushida Junko; Kuroda Yusuke; Gunji Shuichi; Kohri Kazunori; Kobayashi Yukiho; Kong Albert K. H.; Saito Takayuki; Sakaki Naoto; Sakurai Shunsuke; Abe Hyuga; Sano Hidetoshi; Sawada Makoto; Shibata Toru; Dzhatdoev Timur; Suzuki Megumi; Suzuki Hiromasa; Suda Yusuke; Strzys Marcel; Sunada Yuji; Zenin Anatolii; Awai Kyosuke; Takata Jumpei; Takahashi Mari; Takahashi Keitaro; Takahashi Hiromitsu; Takahashi Mitsunari; Tajima Hiroyasu; Tachihara Kengo; Tateishi Dai; Tanaka Shuta; Tanaka Takaaki; Ioka Kunihito; Tanaka Manobu; Tam Thomas P. H.; Tamura Kenji; Cheng K. S.; Chikawa Michiyuki; Choushi Yuuki; Tsukamoto Yusuke; Tsujimoto Shimpei; Tsuru Takeshi; Tian Wenwu; Ishio Kazuma; Terada Yukikatsu; Toma Kenji; Tokanai Fuyuki; Naito Tsuguya; Nagataki Shigehiro; Nakamura Yuki; Nakamori Takeshi; Nakayama Kazunori; Nabatame Yasuyuki; Nishijima Kyoshi; Ishizaki Wataru; Nogami Yuto; Nozaki Seiya; Noda Koji; Nomura Ryosuke; Barkov Maxim; Hadasch Daniela; Hayakawa Takahiro; Hayashi Kohei; Hayashi Katsuhiro; Hayashida Masaaki, The Physical Society of Japan
Meeting Abstracts of the Physical Society of Japan, 2020

CTA Report 162: CTA-LST1 camera calibration
Kobayashi Y.; Oka T.; Okazaki N.; Ogata T.; Okumura A.; Orito R.; Kajiwara Y.; Katagiri H.; Kushida J.; Kubo H.; Gunji S.; Abe H.; Saito T.; Sakaki N.; Sakurai S.; Suzuki M.; Sunada Y.; Zenin A.; Takahashi Mari; Takahashi Mitsunari; Tateishi D.; Tanaka M.; Inada T.; Tamura K.; Chikawa M.; Choshi Y.; Teshima M.; Terada Y.; Tokanai F.; Nakamori T.; Nabatame Y.; Nishijima K.; Nogami Y.; Inome Y.; Nozaki S.; Noda K.; Nomura R.; Hadasch D.; Harada Y.; Fukami S.; Fujihara C.; Furuta T.; Mazin D.; Yamamoto T.; Imagawa K.; Yoshikoshi T.; Yoshida T.; for the CTA-Japan Consortium; Iwamura Y.; Ohishi M.; Ohoka H.; Ohtani Y., The Physical Society of Japan
Meeting Abstracts of the Physical Society of Japan, 2020

Visualization of Low-Level Gamma Radiation Sources Using a Low-Cost, High-Sensitivity, Omnidirectional Compton Camera
Muraishi; H.; Enomoto; R.; Katagiri; H.; Kagaya; M.; Watanabe; T.; Narita; N.; Kano; D., We present experimental protocols for visualizing various low-level gamma radiation sources in the ambient environment. Experiments were conducted by using a low-cost, high-sensitivity, omnidirectional, gamma-ray imaging Compton camera. In the laboratory, the position of a sub-MeV gamma radiation source such as 137Cs can easily be monitored via omnidirectional gamma-ray imaging obtained by the Compton camera. In contrast, a stationary, wall-mounted dose rate monitor cannot always successfully monitor such a source. Furthermore, we successfully demonstrated the possibility of visualizing the radioactivity movement in the environment, for example, the movement of a patient injected with 18F-fluorodeoxyglucose (18F-FDG) in a nuclear medicine facility. In the Fukushima field, we easily obtained omnidirectional gamma-ray images concerned with the distribution on the ground of low-level radioactive contamination by radioactive cesium released by the Fukushima Daiichi nuclear power plant accident in 2011. We demonstrate clear advantages of using our procedure with this camera to visualize gamma-ray sources..., MyJove Corporation
Journal of Visualized Experiments, Jan. 2020, [Reviewed]

高感度コンプトンカメラを用いたPET受診者の尿中放射能遠隔測定　　　　　　　　　　　　　　　
渡辺 宝; 加納 大輔; 村石 浩; 榎本 良治; 片桐 秀明; 加賀谷 美佳; 成田 尚史; 細川 翔太, (一社)日本核医学会
核医学, Oct. 2019, [Reviewed]

低線量環境下での原木シイタケ栽培用ホダ木の放射能濃度の屋外検査用スクリーニング装置
加賀谷 美佳; 片桐 秀明; 榎本 良治; 山口 晶子; 石川 洋一; 平出 政和; 村石 浩; 渡辺 宝; 内田 智久; 田中 真伸; 吉田 龍生, 福島県およびその周辺地域の原木シイタケ栽培は東京電力福島第一原子力発電所事故によって衰退している。林野庁は安全な原木シイタケ（<100 Bq/kg）を栽培するために，ホダ木の放射能濃度の最大値を50 Bq/kgに設定した。安全なホダ木を選定するために，屋外の汚染地域で測定可能な可搬型の放射能検査装置の開発が必要とされている。本研究では，遮蔽体を用いない安価な可搬型放射能検査装置を開発した。可搬型検査装置を用いたスクリーニング検査によって安全なホダ木の選定を実現した。, Japan Radioisotope Association
RADIOISOTOPES, 15 May 2019, [Reviewed]

CTA Report 149: Development of analysis software for CTA LST-1
Iwamura Yuki; Kubo Hidetoshi; Gunji Shuichi; Kobayashi Yukiho; Saito Takayuki; Sakaki Naoto; Sakurai Shunsuke; Sasai Yoshinori; Sunada Yuji; Takahashi Tomoya; Taneda Yuki; Inada Tomohiro; Chikawa Michiyuki; Choushi Yuuki; Teshima Masahiro; Terada Yukikatsu; Nakamori Takeshi; Nishijima Kyoshi; Nozaki Seiya; Noda Koji; Hayashida Masaaki; Hiroshima Nagisa; Ohishi Michiko; Fukami Satoshi; Fujihara Chikako; Miura Chika; Yamamoto Tokonatsu; Yoshikoshi Takanori; Yoshida Tatsuo; Ri Ken; Zenin Anatolii; the CTA-Japan Consortium; Ohtani Yoshiki; Okumura Akira; Orito Reiko; Katagiri Hideaki; Kamimoto Takumi; Kushida Junko, The Physical Society of Japan
Meeting Abstracts of the Physical Society of Japan, 2019

Science with the Cherenkov Telescope Array
Cherenkov Telescope Array Consortium; Acharya, B. S.; Agudo, I.; Al Samarai, I.; Alfaro, R.; Alfaro, J.; Alispach, C.; Alves Batista, R.; Amans, J. -P.; Amato, E.; Ambrosi, G.; Antolini, E.; Antonelli, L. A.; Aramo, C.; Araya, M.; Armstrong, T.; Arqueros, F.; Arrabito, L.; Asano, K.; Ashley, M.; Backes, M.; Balazs, C.; Balbo, M.; Ballester, O.; Ballet, J.; Bamba, A.; Barkov, M.; Barres de Almeida, U.; Barrio, J. A.; Bastieri, D.; Becherini, Y.; Belfiore, A.; Benbow, W.; Berge, D.; Bernardini, E.; Bernardini, M. G.; Bernardos, M.; Bernlöhr, K.; Bertucci, B.; Biasuzzi, B.; Bigongiari, C.; Biland, A.; Bissaldi, E.; Biteau, J.; Blanch, O.; Blazek, J.; Boisson, C.; Bolmont, J.; Bonanno, G.; Bonardi, A.; Bonavolontà, C.; Bonnoli, G.; Bosnjak, Z.; Böttcher, M.; Braiding, C.; Bregeon, J.; Brill, A.; Brown, A. M.; Brun, P.; Brunetti, G.; Buanes, T.; Buckley, J.; Bugaev, V.; Bühler, R.; Bulgarelli, A.; Bulik, T.; Burton, M.; Burtovoi, A.; Busetto, G.; Canestrari, R.; Capalbi, M.; Capitanio, F.; Caproni, A.; Caraveo, P.; Cárdenas, V.; Carlile, C.; Carosi, R.; Carquín, E.; Carr, J.; Casanova, S.; Cascone, E.; Catalani, F.; Catalano, O.; Cauz, D.; Cerruti, M.; Chadwick, P.; Chaty, S.; Chaves, R. C. G.; Chen, A.; Chen, X.; Chernyakova, M.; Chikawa, M.; Christov, A.; Chudoba, J.; Cieślar, M.; Coco, V.; Colafrancesco, S.; Colin, P.; Conforti, V.; Connaughton, V.; Conrad, J.; Contreras, J. L.; Cortina, J.; Costa, A.; Costantini, H.; Cotter, G.; Covino, S.; Crocker, R.; Cuadra, J.; Cuevas, O.; Cumani, P.; D'Aì, A.; D'Ammando, F.; D'Avanzo, P.; D'Urso, D.; Daniel, M.; Davids, I.; Dawson, B.; Dazzi, F.; De Angelis, A.; de Cássia dos Anjos, R.; De Cesare, G.; De Franco, A.; de Gouveia Dal Pino, E. M.; de la Calle, I.; de los Reyes Lopez, R.; De Lotto, B.; De Luca, A.; De Lucia, M.; de Naurois, M.; de Oña Wilhelmi, E.; De Palma, F.; De Persio, F.; de Souza, V.; Deil, C.; Del Santo, M.; Delgado, C.; della Volpe, D.; Di Girolamo, T.; Di Pierro, F.; Di Venere, L.; Díaz, C.; Dib, C.; Diebold, S.; Djannati-Ataï, A.; Domínguez, A.; Dominis Prester, D.; Dorner, D.; Doro, M.; Drass, H.; Dravins, D.; Dubus, G.; Dwarkadas, V. V.; Ebr, J.; Eckner, C.; Egberts, K.; Einecke, S.; Ekoume, T. R. N.; Elsässer, D.; Ernenwein, J. -P.; Espinoza, C.; Evoli, C.; Fairbairn, M.; Falceta-Goncalves, D.; Falcone, A.; Farnier, C.; Fasola, G.; Fedorova, E.; Fegan, S.; Fernandez-Alonso, M.; Fernández-Barral, A.; Ferrand, G.; Fesquet, M.; Filipovic, M.; Fioretti, V.; Fontaine, G.; Fornasa, M.; Fortson, L.; Freixas Coromina, L.; Fruck, C.; Fujita, Y.; Fukazawa, Y.; Funk, S.; Füßling, M.; Gabici, S.; Gadola, A.; Gallant, Y.; Garcia, B.; Garcia López, R.; Garczarczyk, M.; Gaskins, J.; Gasparetto, T.; Gaug, M.; Gerard, L.; Giavitto, G.; Giglietto, N.; Giommi, P.; Giordano, F.; Giro, E.; Giroletti, M.; Giuliani, A.; Glicenstein, J. -F.; Gnatyk, R.; Godinovic, N.; Goldoni, P.; Gómez-Vargas, G.; González, M. M.; González, J. M.; Götz, D.; Graham, J.; Grandi, P.; Granot, J.; Green, A. J.; Greenshaw, T.; Griffiths, S.; Gunji, S.; Hadasch, D.; Hara, S.; Hardcastle, M. J.; Hassan, T.; Hayashi, K.; Hayashida, M.; Heller, M.; Helo, J. C.; Hermann, G.; Hinton, J.; Hnatyk, B.; Hofmann, W.; Holder, J.; Horan, D.; Hörandel, J.; Horns, D.; Horvath, P.; Hovatta, T.; Hrabovsky, M.; Hrupec, D.; Humensky, T. B.; Hütten, M.; Iarlori, M.; Inada, T.; Inome, Y.; Inoue, S.; Inoue, T.; Inoue, Y.; Iocco, F.; Ioka, K.; Iori, M.; Ishio, K.; Iwamura, Y.; Jamrozy, M.; Janecek, P.; Jankowsky, D.; Jean, P.; Jung-Richardt, I.; Jurysek, J.; Kaaret, P.; Karkar, S.; Katagiri, H.; Katz, U.; Kawanaka, N.; Kazanas, D.; Khélifi, B.; Kieda, D. B.; Kimeswenger, S.; Kimura, S.; Kisaka, S.; Knapp, J.; Knödlseder, J.; Koch, B.; Kohri, K.; Komin, N.; Kosack, K.; Kraus, M.; Krause, M.; Krauß, F.; Kubo, H.; Kukec Mezek, G.; Kuroda, H.; Kushida, J.; La Palombara, N.; Lamanna, G.; Lang, R. G.; Lapington, J.; Le Blanc, O.; Leach, S.; Lees, J. -P.; Lefaucheur, J.; Leigui de Oliveira, M. A.; Lenain, J. -P.; Lico, R.; Limon, M.; Lindfors, E.; Lohse, T.; Lombardi, S.; Longo, F.; López, M.; López-Coto, R.; Lu, C. -C.; Lucarelli, F.; Luque-Escamilla, P. L.; Lyard, E.; Maccarone, M. C.; Maier, G.; Majumdar, P.; Malaguti, G.; Mandat, D.; Maneva, G.; Manganaro, M.; Mangano, S.; Marcowith, A.; Marín, J.; Markoff, S.; Martí, J.; Martin, P.; Martínez, M.; Martínez, G.; Masetti, N.; Masuda, S.; Maurin, G.; Maxted, N.; Mazin, D.; Medina, C.; Melandri, A.; Mereghetti, S.; Meyer, M.; Minaya, I. A.; Mirabal, N.; Mirzoyan, R.; Mitchell, A.; Mizuno, T.; Moderski, R.; Mohammed, M.; Mohrmann, L.; Montaruli, T.; Moralejo, A.; Morcuende-Parrilla, D.; Mori, K.; Morlino, G.; Morris, P.; Morselli, A.; Moulin, E.; Mukherjee, R.; Mundell, C.; Murach, T.; Muraishi, H.; Murase, K.; Nagai, A.; Nagataki, S.; Nagayoshi, T.; Naito, T.; Nakamori, T.; Nakamura, Y.; Niemiec, J.; Nieto, D.; Nikołajuk, M.; Nishijima, K.; Noda, K.; Nosek, D.; Novosyadlyj, B.; Nozaki, S.; O'Brien, P.; Oakes, L.; Ohira, Y.; Ohishi, M.; Ohm, S.; Okazaki, N.; Okumura, A.; Ong, R. A.; Orienti, M.; Orito, R.; Osborne, J. P.; Ostrowski, M.; Otte, N.; Oya, I.; Padovani, M.; Paizis, A.; Palatiello, M.; Palatka, M.; Paoletti, R.; Paredes, J. M.; Pareschi, G.; Parsons, R. D.; Pe'er, A.; Pech, M.; Pedaletti, G.; Perri, M.; Persic, M.; Petrashyk, A.; Petrucci, P.; Petruk, O.; Peyaud, B.; Pfeifer, M.; Piano, G.; Pisarski, A.; Pita, S.; Pohl, M.; Polo, M.; Pozo, D.; Prandini, E.; Prast, J.; Principe, G.; Prokhorov, D.; Prokoph, H.; Prouza, M.; Pühlhofer, G.; Punch, M.; Pürckhauer, S.; Queiroz, F.; Quirrenbach, A.; Rainò, S.; Razzaque, S.; Reimer, O.; Reimer, A.; Reisenegger, A.; Renaud, M.; Rezaeian, A. H.; Rhode, W.; Ribeiro, D.; Ribó, M.; Richtler, T.; Rico, J.; Rieger, F.; Riquelme, M.; Rivoire, S.; Rizi, V.; Rodriguez, J.; Rodriguez Fernandez, G.; Rodríguez Vázquez, J. J.; Rojas, G.; Romano, P.; Romeo, G.; Rosado, J.; Rovero, A. C.; Rowell, G.; Rudak, B.; Rugliancich, A.; Rulten, C.; Sadeh, I.; Safi-Harb, S.; Saito, T.; Sakaki, N.; Sakurai, S.; Salina, G.; Sánchez-Conde, M.; Sandaker, H.; Sandoval, A.; Sangiorgi, P.; Sanguillon, M.; Sano, H.; Santander, M.; Sarkar, S.; Satalecka, K.; Saturni, F. G.; Schioppa, E. J.; Schlenstedt, S.; Schneider, M.; Schoorlemmer, H.; Schovanek, P.; Schulz, A.; Schussler, F.; Schwanke, U.; Sciacca, E.; Scuderi, S.; Seitenzahl, I.; Semikoz, D.; Sergijenko, O.; Servillat, M.; Shalchi, A.; Shellard, R. C.; Sidoli, L.; Siejkowski, H.; Sillanpää, A.; Sironi, G.; Sitarek, J.; Sliusar, V.; Slowikowska, A.; Sol, H.; Stamerra, A.; Stanič, S.; Starling, R.; Stawarz, Ł.; Stefanik, S.; Stephan, M.; Stolarczyk, T.; Stratta, G.; Straumann, U.; Suomijarvi, T.; Supanitsky, A. D.; Tagliaferri, G.; Tajima, H.; Tavani, M.; Tavecchio, F.; Tavernet, J. -P.; Tayabaly, K.; Tejedor, L. A.; Temnikov, P.; Terada, Y.; Terrier, R.; Terzic, T.; Teshima, M.; Testa, V.; Thoudam, S.; Tian, W.; Tibaldo, L.; Tluczykont, M.; Todero Peixoto, C. J.; Tokanai, F.; Tomastik, J.; Tonev, D.; Tornikoski, M.; Torres, D. F.; Torresi, E.; Tosti, G.; Tothill, N.; Tovmassian, G.; Travnicek, P.; Trichard, C.; Trifoglio, M.; Troyano Pujadas, I.; Tsujimoto, S.; Umana, G.; Vagelli, V.; Vagnetti, F.; Valentino, M.; Vallania, P.; Valore, L.; van Eldik, C.; Vandenbroucke, J.; Varner, G. S.; Vasileiadis, G.; Vassiliev, V.; Vázquez Acosta, M.; Vecchi, M.; Vega, A.; Vercellone, S.; Veres, P.; Vergani, S.; Verzi, V.; Vettolani, G. P.; Viana, A.; Vigorito, C.; Villanueva, J.; Voelk, H.; Vollhardt, A.; Vorobiov, S.; Vrastil, M.; Vuillaume, T.; Wagner, S. J.; Wagner, R.; Walter, R.; Ward, J. E.; Warren, D.; Watson, J. J.; Werner, F.; White, M.; White, R.; Wierzcholska, A.; Wilcox, P.; Will, M.; Williams, D. A.; Wischnewski, R.; Wood, M.; Yamamoto, T.; Yamazaki, R.; Yanagita, S.; Yang, L.; Yoshida, T.; Yoshiike, S.; Yoshikoshi, T.; Zacharias, M.; Zaharijas, G.; Zampieri, L.; Zandanel, F.; Zanin, R.; Zavrtanik, M.; Zavrtanik, D.; Zdziarski, A. A.; Zech, A.; Zechlin, H.; Zhdanov, V. I.; Ziegler, A.; Zorn, J., The Cherenkov Telescope Array, CTA, will be the major global observatory for very high energy gamma-ray astronomy over the next decade and beyond. The scientific potential of CTA is extremely broad: from understanding the role of relativistic cosmic particles to the search for dark matter. CTA is an explorer of the extreme universe, probing environments from the immediate neighbourhood of black holes to cosmic voids on the largest scales. Covering a huge range in photon energy from 20 GeV to 300 TeV, CTA will improve on all aspects of performance with respect to current instruments. The observatory will operate arrays on sites in both hemispheres to provide full sky coverage and will hence maximize the potential for the rarest phenomena such as very nearby supernovae, gamma-ray bursts or gravitational wave transients. With 99 telescopes on the southern site and 19 telescopes on the northern site, flexible operation will be possible, with sub-arrays available for specific tasks. CTA will have important synergies with many of the new generation of major astronomical and astroparticle observatories. Multi-wavelength and multi-messenger approaches combining CTA data with those from other instruments will lead to a deeper understanding of the broad-band non-thermal properties of target sources. The CTA Observatory will be operated as an open, proposal-driven observatory, with all data available on a public archive after a pre-defined proprietary period. Scientists from institutions worldwide have combined together to form the CTA Consortium. This Consortium has prepared a proposal for a Core Programme of highly motivated observations. The programme, encompassing approximately 40% of the available observing time over the first ten years of CTA operation, is made up of individual Key Science Projects (KSPs), which are presented in this document...., Science with the Cherenkov Telescope Array
2019

漏洩線量測定によるFDG-PET受診者の尿中放射線量の推定
加納 大輔; 望月 伸夫; 山口 正和; 村石 浩; 渡辺 宝; 榎本 良治; 片桐 秀明; 細川 翔太, (一社)日本核医学会
核医学, Dec. 2018, [Reviewed]

Visualization of Radium-223 chloride using an omnidirectional gamma-ray imaging Compton camera for radioactive environmental monitoring
H. Muraishi; R. Kondo; T. Watanabe; R. Enomoto; H. Katagiri; M. Kagaya; D. Kano; T. Takeda; S. Noda; K. Kikuchi; H. Hara; T. Maegaki; T. Uchida; M. Tanaka, We investigated the possibility of visualizing low-level radioactive contamination by 223Ra chloride injection in medical facilities using a highly sensitive gamma-ray omnidirectional imaging Compton camera. The detector consisted of CsI(Tl) scintillator cubes of 3.5 cm in size, which acted as scatterers or absorbers. The measurements were carried out using the detector in the nuclear medicine facility, where the 223Ra sources (such as used vial, syringe, etc.) with the radioactivities of less than 1 MBq were placed inside the preparation room. We confirmed four groups of gamma-ray full-absorption peaks between 270 keV and 810 keV as expected in the energy spectrum made by the sum of energy deposits in two counter coincidence events. Furthermore, we successfully detected the direction of the 223Ra source in the reconstructed gamma-ray image. Our proposed technique would be used as a low-level imaging dose monitor to visualize radioactive contamination by 223Ra in medical facilities., Institute of Electrical and Electronics Engineers Inc.
2018 IEEE Nuclear Science Symposium and Medical Imaging Conference, NSS/MIC 2018 - Proceedings, 01 Nov. 2018

Evaluation of the detection capability of the recoil electron tracks of 511 keV gamma rays with an advanced Compton camera using an SOI pixel sensor
Mika Kagaya; Hideaki Katagiri; Naomi Tojo; Ryo Kato; Takeshi Go Tsuru; Ayaki Takeda; Yasuo Arai, In the fields of astrophysics and nuclear medicine diagnostics, the use of a 511-keV line gamma rays probe is indispensable. Compton-imaging techniques are suitable for measuring 511-keV line gamma rays because of the high probability of Compton scattering at this energy level. However, a reconstructed image obtained by a traditional Compton camera has false spots because this camera reconstructs an image with smeared rings. On the other hand, an advanced Compton camera can enhance the angular resolution and reduce the background by detecting recoil electron tracks. We focus on a silicon-on-insulator (SOI) pixel sensor with 30 m cells because of its small pixel pitch and high-energy resolution. In this study, we developed a prototype of an advanced Compton camera using an SOI sensor and evaluated its performance for detecting the recoil electron tracks of 511-keV gamma rays., Institute of Electrical and Electronics Engineers Inc.
2018 IEEE Nuclear Science Symposium and Medical Imaging Conference, NSS/MIC 2018 - Proceedings, 01 Nov. 2018

Remote measurement of urinary radioactivity in F-18-FDG PET patients using Compton camera for accuracy evaluation of standardized uptake value
Takara Watanabe; Daisuke Kano; Ryoji Enomoto; Hiroshi Muraishi; Ryo Wakamatsu; Hideaki Katagiri; Mika Kagaya; Ryotaro Kondo; Masahiro Fukushi; Syota Hosokawa; Tohoru Takeda; Manobu M. Tanaka; Tomohisa Uchida; Yoshihiro Nakagami, Currently, the most commonly used estimate of metabolic activity during clinical positron emission tomography (PET) is standardized uptake value (SUV) obtained from F-18-fluorodeoxyglucose (F-18-FDG) captured in cancer cells. Although SUV is evaluated after corrections for the injected dose, weight, and other such parameters, the entire injected dose is inappropriate for this calculation because some FDG is excreted in urine. Therefore, the injected dose warrants correction by assessment of urinary radioactivity in patients before PET to enhance the accuracy of FDG calculation. However, this is not typically performed in clinical practice owing to secondary effects of radioactive contamination in hospitals and radiation exposure risk to the attending staff. Therefore, we aimed to develop a remote method for the measurement of urinary radioactivity in FDG-PET patients. Urinary radioactivity was estimated in a toilet bowl using gamma-ray distribution obtained with a Compton camera. The gamma-ray events from the toilet bowl per unit time (5 s) facilitated radioactivity calculation. Between 0 and 40 MBq, deviation of our detector from the linearity for radioactivity was <8.3%. The accuracy of radioactive assessment was 11% for a 5-s measurement of 19.7 MBq F-18-FDG. Overall, we obtained 75 samples (45 males and 30 females). Our results revealed that excretion of FDG in the urine per person varied between 1.9% and 15.6% of the injected dose (range, 225-305 MBq). Urinary radioactivity can be evaluated before PET using a Compton camera. SUV determination in clinical context could be enhanced by considering urinary radioactivity for corrections caused by individual differences in radioactivity., IOP PUBLISHING LTD
BIOMEDICAL PHYSICS & ENGINEERING EXPRESS, Nov. 2018, [Reviewed]

A technique for estimating the absolute gain of a photomultiplier tube
A Takahashi; M.; Inome; Y.; Yoshii; S.; Bamba; A.; Gunji; S.; Hadasch; D.; Hayashida; M.; Katagiri; H.; Konno; Y.; Kubo; H.; Kushida; J.;; Nakajima; D.; Nakamori; T.; Nagayoshi; T.; Nishijima; K.; Nozaki; S.;; Mazin; D.; Mashuda; S.; Mirzoyan; R.; Ohoka; H.; Orito; R.; Saito; T.;; Sakurai; S.; Takeda; J.; Teshima; M.; Terada; Y.; Tokanai; F.; Yamamoto; T.; Yoshida; T., Detection of low-intensity light relies on the conversion of photons to photoelectrons, which are then multiplied and detected as an electrical signal. To measure the actual intensity of the light, one must know the factor by which the photoelectrons have been multiplied. To obtain this amplification factor, we have developed a procedure for estimating precisely the signal caused by a single photoelectron. The method utilizes the fact that the photoelectrons conform to a Poisson distribution. The average signal produced by a single photoelectron can then be estimated from the number of noise events, without requiring analysis of the distribution of the signal produced by a single photoelectron. The signal produced by one or more photoelectrons can be estimated experimentally without any assumptions. This technique, and an example of the analysis of a signal from a photomultiplier tube, are described in this study., ELSEVIER SCIENCE BV
Nuclear Instruments and Methods in Physics Research A, 21 Jun. 2018, [Reviewed]

Development of an all-sky gamma-ray Compton camera based on scintillators for high-dose environments
Hideaki Katagiri; Wataru Satoh; Ryoji Enomoto; Ryo Wakamatsu; Takara Watanabe; Hiroshi Muraishi; Mika Kagaya; Souichi Tanaka; Kiyoto Wada; Manobu Tanaka & Tomohisa Uchida, Lead, We developed an all-sky Compton camera for the detection of sub-MeV gamma rays emitted by radioactive cesium in high-dose environments. The camera consisted of six NaI (Tl) scintillators with a diameter of 1/2 in (1.3 cm) placed symmetrically at the vertexes of an octahedron. Irradiation tests with a point-like source at a high-dose irradiation facility confirmed that the camera can measure the arrival directions of sub-MeV gamma rays and visualize a gamma-ray source distribution in environments of up to ∼1 mSv/h. Due to the symmetrical geometry of the camera, the directional variance of its acceptance fell within ±23% (full width) of the average value. The camera capability to detect gamma rays in high-dose environments, in which multiple and/or extended sources exist, was verified in environments of up to ∼0.2 mSv/h by tests at the Fukushima Daiichi nuclear power plant. The imaging capability was confirmed also in lower dose environments such as 1 μSv/h for a reasonable observation time of 2 h, indicating that the developed camera is adequate for practical use in environments with a wide dynamic range of dose rate (∼200 times), i.e. from 1 μSv/h to 0.2 mSv/h., Informa UK Limited
Journal of Nuclear Science and Technology, 19 Jun. 2018, [Reviewed]

CTA Project 130: General Report
Teshima Masahiro; Kubo Hidetoshi; Totani Tomonori; Consortium for the CTA-Japan, The Physical Society of Japan
Meeting Abstracts of the Physical Society of Japan, 2018

CTA Report 134：Study of the aging effect of the photomultiplier tube for the CTA Large Size Telescope
Sakurai S.; Kataoka J.; Katagiri H.; Kimura S.; Kushida J.; Kubo H.; Gunji S.; Koyama S.; Konno Y.; Saito T.; Sawada M.; Nagayoshi T.; Sunada Y.; Takahashi M.; Tsujimoto S.; Teshima M.; Terada Y.; Tokanai F.; Nakajima D.; Nakamori T.; Nishijima K.; Nishiyama G.; Inada T.; Nozaki S.; Hayashida M.; Bamba A.; Hirako J.; Fukami S.; Masuda S.; Yamamoto T.; Yoshida T.; Hadasch D.; Mazin D.; Inome Y.; the CTA-Japan consortium; Iwamura Y.; Ohoka H.; Okumura A.; Okazaki N.; Orito R., The Physical Society of Japan
Meeting Abstracts of the Physical Society of Japan, 2018

CTA Report 133: Integration test of the focal plane camera for the first CTA Large Sized Telescope
Nozaki S.; Katagiri H.; Kato S.; Kimura S.; Kushida J.; Kubo H.; Gunji S.; Koyama S.; Konno Y.; Saito T.; Sakurai S.; Inada T.; Sawada M.; Sunada Y.; Takahashi M.; Takahara H.; Tanaka M.; Tsujimoto S.; Teshima M.; Terada Y.; Okanai F.; NakajimaT D.; Inome Y.; Nakamori T.; Nagayoshi T.; Nishijima K.; Nishiyama G.; Hayashida M.; Bamba A.; Hirako J.; Fukami S.; Masuda S.; Yamamoto T.; Iwamura Y.; Yoshida T.; Hadasch D.; Mazin D.; the CTA-Japan consortium; Ikeno M.; Uchida T.; Ohoka H.; Okumura A.; Okazaki N.; Orito R.; Kataoka J., The Physical Society of Japan
Meeting Abstracts of the Physical Society of Japan, 2018

CTA Report 142: Integration test of the focal plane camera for the first CTA Large Sized Telescope(II)
Sunada Y.; Katagiri H.; Kushida J.; Kimura S.; Kubo H.; Gunji S.; Koyama S.; Saito T.; Sakurai S.; Sawada M.; Suzuki M.; Inada T.; Takahashi M.; Takahara H.; Tanaka M.; Tujimoto S.; Teshima M.; Terada Y.; Tokanai F.; Nakajima D.; Nakamori K.; Nagayoshi T.; Inome Y.; Nishijima K.; Nishiyama G.; Nozaki S.; Hayashida M.; Bamba A.; Hirako J.; Fukami S.; Masuda S.; Yamamoto T.; Yoshida T.; Iwamura Y.; Hadasch Daniela; Mazin Daniel; the CTA-Japan consortium; Ohoka H.; Okazaki N.; Okumura A.; Orito R.; Kataoka J., The Physical Society of Japan
Meeting Abstracts of the Physical Society of Japan, 2018

Development of an omnidirectional gamma-ray imaging Compton camera for low-radiation-level environmental monitoring
Watanabe Takara; Enomoto Ryoji; Muraishi Hiroshi; Katagiri Hideaki; Kagaya Mika; Fukushi Masahiro; Kano Daisuke; Satoh Wataru; Takeda Tohoru; Tanaka Manobu; Tanaka Souichi; Uchida Tomohisa; Wada Kiyoto; Wakamatsu Ryo, We have developed an omnidirectional gamma-ray imaging Compton camera for environmental monitoring at low levels of radiation. The camera consisted of only six CsI(Tl) scintillator cubes of 3.5 cm, each of which was readout by super-bialkali photo-multiplier tubes (PMTs). Our camera enables the visualization of the position of gamma-ray sources in all directions (∼4π sr) over a wide energy range between 300 and 1400 keV. The angular resolution (σ) was found to be ∼11°, which was realized using an image-sharpening technique. A high detection efficiency of 18 cps/(µSv/h) for 511 keV (1.6 cps/MBq at 1 m) was achieved, indicating the capability of this camera to visualize hotspots in areas with low-radiation-level contamination from the order of µSv/h to natural background levels. Our proposed technique can be easily used as a low-radiation-level imaging monitor in radiation control areas, such as medical and accelerator facilities., Institute of Physics
Jpn. J. Appl. Phys., 27 Dec. 2017, [Reviewed]

Detection of Two TeV Shell-type Remnants at GeV Energies with FERMI LAT: HESS J1731-347 and SN 1006
Condon, B.; Lemoine-Goumard, M.; Acero, F.; Katagiri, H., We report the first high-significance GeV γ-ray detections of supernova remnants HESS J1731-347 and SN 1006, both of which have been previously detected by imaging atmospheric Cherenkov Telescopes above 1 TeV. Using 8 years of Fermi-LAT Pass 8 data at energies between 1 GeV and 2 TeV, we detect emission at the position of HESS J1731-347 with a significance of ∼ 5σ and a spectral index of { { Γ } }=1.66+/- {0.16},{stat}+/- {0.12},{syst}. The hardness of the index and the good connection with the TeV spectrum of HESS J1731-347 support an association between the two sources. We also confirm the detection of SN 1006 at ∼ 6σ with a spectral index of { { Γ } }=1.79+/- {0.17},{stat}+/- {0.27},{syst}. The northeast (NE) and southwest (SW) limbs of SN 1006 were also fit separately, resulting in the detection of the NE region ({ { Γ } }=1.47+/- {0.26},{stat}) and the non-detection of the SW region. The significance of different spectral components for the two limbs is 3.6σ , providing first indications of an asymmetry in the GeV γ-ray emission., IOP Publishing
The Astrophysical Journal, 18 Dec. 2017, [Reviewed]

Prototyping hexagonal light concentrators using high-reflectance specular films for the Large-Sized Telescopes of the Cherenkov Telescope Array
Okumura, A.; Dang, T. V.; Ono, S.; Tanaka, S.; Hayashida, M.; Hinton, J.; Katagiri, H.; Noda, K.; Teshima, M.; Yamamoto, T.; Yoshida, T., We have developed a prototype hexagonal light concentrator for the Large-Sized Telescopes of the Cherenkov Telescope Array. To maximize the photodetection efficiency of the focal-plane camera pixels for atmospheric Cherenkov photons and to lower the energy threshold, a specular film with a very high reflectance of 92-99% has been developed to cover the inner surfaces of the light concentrators. The prototype has a relative anode sensitivity (which can be roughly regarded as collection efficiency) of about 95 to 105% at the most important angles of incidence. The design, simulation, production procedure, and performance measurements of the light-concentrator prototype are reported., IOP Publishing
Journal of Instrumentation, 06 Dec. 2017, [Reviewed]

Constraints on Physical Conditions for the Acceleration on Ultra-high-energy Cosmic Rays in Nearby Active Galactic Nuclei Observed with the Fermi Large Area Telescope
Kagaya; M.; Katagiri; H.; Yoshida; T.; and Fukuda; A., We investigated the possibility of acceleration of ultra-high-energy cosmic rays (UHECRs) in nearby active galactic nuclei (AGNs) using archival multi-wavelength observational data, and then we constrained their physical conditions, i.e., the luminosity of the synchrotron radiation and the size of the acceleration site. First, we investigated the spatial correlation between the arrival directions of UHECRs and the positions of nearby AGNs in the Fermi third gamma-ray source catalog. We selected 27 AGNs as candidates of accelerators of UHECRs. Then, we evaluated the physical conditions in the acceleration regions of these AGNs via the Pe'er and Loeb method, which uses the peak luminosity of synchrotron radiation and the peak flux ratio of inverse Compton scattering to synchrotron radiation. From the evaluation, we found that six AGNs have the ability to accelerate ultra-high-energy (UHE) protons in the AGN cores. Furthermore, we found that the minimum acceleration size must be more than a few kpc for acceleration of UHE protons in the AGN lobes., IOP PUBLISHING LTD
The Astrophysical Journal, Nov. 2017, [Reviewed]

Cherenkov Telescope Array Contributions to the 35th International Cosmic Ray Conference (ICRC2017)
Acero, F.; Acharya, B. S.; Acín Portella, V.; Adams, C.; Agudo, I.; Aharonian, F.; Samarai, I. Al; Alberdi, A.; Alcubierre, M.; Alfaro, R.; Alfaro, J.; Alispach, C.; Aloisio, R.; Alves Batista, R.; Amans, J. -P.; Amato, E.; Ambrogi, L.; Ambrosi, G.; Ambrosio, M.; Anderson, J.; Anduze, M.; Angüner, E. O.; Antolini, E.; Antonelli, L. A.; Antonuccio, V.; Antoranz, P.; Aramo, C.; Araya, M.; Arcaro, C.; Armstrong, T.; Arqueros, F.; Arrabito, L.; Arrieta, M.; Asano, K.; Asano, A.; Ashley, M.; Aubert, P.; Singh, C. B.; Babic, A.; Backes, M.; Bajtlik, S.; Balazs, C.; Balbo, M.; Ballester, O.; Ballet, J.; Ballo, L.; Balzer, A.; Bamba, A.; Bandiera, R.; Barai, P.; Barbier, C.; Barcelo, M.; Barkov, M.; Barres de Almeida, U.; Barrio, J. A.; Bastieri, D.; Bauer, C.; Becciani, U.; Becherini, Y.; Becker Tjus, J.; Bednarek, W.; Belfiore, A.; Benbow, W.; Benito, M.; Berge, D.; Bernardini, E.; Bernardini, M. G.; Bernardos, M.; Bernhard, S.; Bernlöhr, K.; Bertinelli Salucci, C.; Bertucci, B.; Besel, M. -A.; Beshley, V.; Bettane, J.; Bhatt, N.; Bhattacharyya, W.; Bhattachryya, S.; Biasuzzi, B.; Bicknell, G.; Bigongiari, C.; Biland, A.; Bilinsky, A.; Bird, R.; Bissaldi, E.; Biteau, J.; Bitossi, M.; Blanch, O.; Blasi, P.; Blazek, J.; Boccato, C.; Bockermann, C.; Boehm, C.; Bohacova, M.; Boisson, C.; Bolmont, J.; Bonanno, G.; Bonardi, A.; Bonavolontà, C.; Bonnoli, G.; Borkowski, J.; Bose, R.; Bosnjak, Z.; Böttcher, M.; Boutonnet, C.; Bouyjou, F.; Bowman, L.; Bozhilov, V.; Braiding, C.; Brau-Nogué, S.; Bregeon, J.; Briggs, M.; Brill, A.; Brisken, W.; Bristow, D.; Britto, R.; Brocato, E.; Brown, A. M.; Brown, S.; Brügge, K.; Brun, P.; Brun, P.; Brun, F.; Brunetti, L.; Brunetti, G.; Bruno, P.; Bryan, M.; Buckley, J.; Bugaev, V.; Bühler, R.; Bulgarelli, A.; Bulik, T.; Burton, M.; Burtovoi, A.; Busetto, G.; Buson, S.; Buss, J.; Byrum, K.; Caccianiga, A.; Cameron, R.; Canelli, F.; Canestrari, R.; Capalbi, M.; Capasso, M.; Capitanio, F.; Caproni, A.; Capuzzo-Dolcetta, R.; Caraveo, P.; Cárdenas, V.; Cardenzana, J.; Cardillo, M.; Carlile, C.; Caroff, S.; Carosi, R.; Carosi, A.; Carquín, E.; Carr, J.; Casandjian, J. -M.; Casanova, S.; Cascone, E.; Castro-Tirado, A. J.; Castroviejo Mora, J.; Catalani, F.; Catalano, O.; Cauz, D.; Celestino Silva, C.; Celli, S.; Cerruti, M.; Chabanne, E.; Chadwick, P.; Chakraborty, N.; Champion, C.; Chatterjee, A.; Chaty, S.; Chaves, R.; Chen, A.; Chen, X.; Cheng, K.; Chernyakova, M.; Chikawa, M.; Chitnis, V. R.; Christov, A.; Chudoba, J.; Cieślar, M.; Clark, P.; Coco, V.; Colafrancesco, S.; Colin, P.; Colombo, E.; Colome, J.; Colonges, S.; Conforti, V.; Connaughton, V.; Conrad, J.; Contreras, J. L.; Cornat, R.; Cortina, J.; Costa, A.; Costantini, H.; Cotter, G.; Courty, B.; Covino, S.; Covone, G.; Cristofari, P.; Criswell, S. J.; Crocker, R.; Croston, J.; Crovari, C.; Cuadra, J.; Cuevas, O.; Cui, X.; Cumani, P.; Cusumano, G.; D'Aì, A.; D'Ammando, F.; D'Avanzo, P.; D'Urso, D.; Da Vela, P.; Dale, Ø.; Dang, V. T.; Dangeon, L.; Daniel, M.; Davids, I.; Dawson, B.; Dazzi, F.; De Angelis, A.; De Caprio, V.; de Cássia dos Anjos, R.; De Cesare, G.; De Franco, A.; De Frondat, F.; de Gouveia Dal Pino, E. M.; de la Calle, I.; De Lisio, C.; de los Reyes Lopez, R.; De Lotto, B.; De Luca, A.; De Lucia, M.; de Mello Neto, J. R. T.; de Naurois, M.; de Oña Wilhelmi, E.; De Palma, F.; De Persio, F.; de Souza, V.; Decock, J.; Deil, C.; Deiml, P.; Del Santo, M.; Delagnes, E.; Deleglise, G.; Delfino Reznicek, M.; Delgado, C.; Delgado Mengual, J.; Della Ceca, R.; della Volpe, D.; Detournay, M.; Devin, J.; Di Girolamo, T.; Di Giulio, C.; Di Pierro, F.; Di Venere, L.; Diaz, L.; Díaz, C.; Dib, C.; Dickinson, H.; Diebold, S.; Digel, S.; Djannati-Ataï, A.; Doert, M.; Domínguez, A.; Dominis Prester, D.; Donnarumma, I.; Dorner, D.; Doro, M.; Dournaux, J. -L.; Downes, T.; Drake, G.; Drappeau, S.; Drass, H.; Dravins, D.; Drury, L.; Dubus, G.; Dundas Morå, K.; Durkalec, A.; Dwarkadas, V.; Ebr, J.; Eckner, C.; Edy, E.; Egberts, K.; Einecke, S.; Eisch, J.; Eisenkolb, F.; Ekoume, T. R. N.; Eleftheriadis, C.; Elsässer, D.; Emmanoulopoulos, D.; Ernenwein, J. -P.; Escarate, P.; Eschbach, S.; Espinoza, C.; Evans, P.; Evoli, C.; Fairbairn, M.; Falceta-Goncalves, D.; Falcone, A.; Fallah Ramazani, V.; Farakos, K.; Farrell, E.; Fasola, G.; Favre, Y.; Fede, E.; Fedora, R.; Fedorova, E.; Fegan, S.; Fernandez-Alonso, M.; Fernández-Barral, A.; Ferrand, G.; Ferreira, O.; Fesquet, M.; Fiandrini, E.; Fiasson, A.; Filipovic, M.; Fink, D.; Finley, J. P.; Finley, C.; Finoguenov, A.; Fioretti, V.; Fiorini, M.; Flores, H.; Foffano, L.; Föhr, C.; Fonseca, M. V.; Font, L.; Fontaine, G.; Fornasa, M.; Fortin, P.; Fortson, L.; Fouque, N.; Fraga, B.; Franco, F. J.; Freixas Coromina, L.; Fruck, C.; Fugazza, D.; Fujita, Y.; Fukami, S.; Fukazawa, Y.; Fukui, Y.; Funk, S.; Furniss, A.; Füßling, M.; Gabici, S.; Gadola, A.; Gallant, Y.; Galloway, D.; Gallozzi, S.; Garcia, B.; Garcia, A.; García Gil, R.; Garcia López, R.; Garczarczyk, M.; Gardiol, D.; Gargano, F.; Gargano, C.; Garozzo, S.; Garrido-Ruiz, M.; Gascon, D.; Gasparetto, T.; Gaté, F.; Gaug, M.; Gebhardt, B.; Gebyehu, M.; Geffroy, N.; Genolini, B.; Ghalumyan, A.; Ghedina, A.; Ghirlanda, G.; Giammaria, P.; Gianotti, F.; Giebels, B.; Giglietto, N.; Gika, V.; Gimenes, R.; Giommi, P.; Giordano, F.; Giovannini, G.; Giro, E.; Giroletti, M.; Gironnet, J.; Giuliani, A.; Glicenstein, J. -F.; Gnatyk, R.; Godinovic, N.; Goldoni, P.; Gómez, J. L.; Gómez-Vargas, G.; González, M. M.; González, J. M.; Gothe, K. S.; Gotz, D.; Goullon, J.; Grabarczyk, T.; Graciani, R.; Graham, J.; Grandi, P.; Granot, J.; Grasseau, G.; Gredig, R.; Green, A. J.; Greenshaw, T.; Grenier, I.; Griffiths, S.; Grillo, A.; Grondin, M. -H.; Grube, J.; Guarino, V.; Guest, B.; Gueta, O.; Gunji, S.; Gyuk, G.; Hadasch, D.; Hagge, L.; Hahn, J.; Hahn, A.; Hakobyan, H.; Hara, S.; Hardcastle, M. J.; Hassan, T.; Haubold, T.; Haupt, A.; Hayashi, K.; Hayashida, M.; He, H.; Heller, M.; Helo, J. C.; Henault, F.; Henri, G.; Hermann, G.; Hermel, R.; Herrera Llorente, J.; Herrero, A.; Hervet, O.; Hidaka, N.; Hinton, J.; Hiroshima, N.; Hirotani, K.; Hnatyk, B.; Hoang, J. K.; Hoffmann, D.; Hofmann, W.; Holder, J.; Horan, D.; Hörandel, J.; Hörbe, M.; Horns, D.; Horvath, P.; Houles, J.; Hovatta, T.; Hrabovsky, M.; Hrupec, D.; Huet, J. -M.; Hughes, G.; Hui, D.; Hull, G.; Humensky, T. B.; Hussein, M.; Hütten, M.; Iarlori, M.; Ikeno, Y.; Illa, J. M.; Impiombato, D.; Inada, T.; Ingallinera, A.; Inome, Y.; Inoue, S.; Inoue, T.; Inoue, Y.; Iocco, F.; Ioka, K.; Ionica, M.; Iori, M.; Iriarte, A.; Ishio, K.; Israel, G. L.; Iwamura, Y.; Jablonski, C.; Jacholkowska, A.; Jacquemier, J.; Jamrozy, M.; Janecek, P.; Jankowsky, F.; Jankowsky, D.; Jansweijer, P.; Jarnot, C.; Jean, P.; Johnson, C. A.; Josselin, M.; Jung-Richardt, I.; Jurysek, J.; Kaaret, P.; Kachru, P.; Kagaya, M.; Kakuwa, J.; Kalekin, O.; Kankanyan, R.; Karastergiou, A.; Karczewski, M.; Karkar, S.; Katagiri, H.; Kataoka, J.; Katarzyński, K.; Katz, U.; Kawanaka, N.; Kaye, L.; Kazanas, D.; Kelley-Hoskins, N.; Khélifi, B.; Kieda, D. B.; Kihm, T.; Kimeswenger, S.; Kimura, S.; Kisaka, S.; Kishida, S.; Kissmann, R.; Kluźniak, W.; Knapen, J.; Knapp, J.; Knödlseder, J.; Koch, B.; Kocot, J.; Kohri, K.; Komin, N.; Kong, A.; Konno, Y.; Kosack, K.; Kowal, G.; Koyama, S.; Kraus, M.; Krause, M.; Krauß, F.; Krennrich, F.; Kruger, P.; Kubo, H.; Kudryavtsev, V.; Kukec Mezek, G.; Kumar, S.; Kuroda, H.; Kushida, J.; Kushwaha, P.; La Palombara, N.; La Parola, V.; La Rosa, G.; Lahmann, R.; Lalik, K.; Lamanna, G.; Landoni, M.; Landriu, D.; Landt, H.; Lang, R. G.; Lapington, J.; Laporte, P.; Le Blanc, O.; Le Flour, T.; Le Sidaner, P.; Leach, S.; Leckngam, A.; Lee, S. -H.; Lee, W. H.; Lees, J. -P.; Lefaucheur, J.; Leigui de Oliveira, M. A.; Lemoine-Goumard, M.; Lenain, J. -P.; Leto, G.; Lico, R.; Limon, M.; Lindemann, R.; Lindfors, E.; Linhoff, L.; Lipniacka, A.; Lloyd, S.; Lohse, T.; Lombardi, S.; Longo, F.; Lopez, M.; Lopez-Coto, R.; Louge, T.; Louis, F.; Louys, M.; Lucarelli, F.; Lucchesi, D.; Luque-Escamilla, P. L.; Lyard, E.; Maccarone, M. C.; Maccarone, T.; Mach, E.; Madejski, G. M.; Maier, G.; Majczyna, A.; Majumdar, P.; Makariev, M.; Malaguti, G.; Malouf, A.; Maltezos, S.; Malyshev, D.; Malyshev, D.; Mandat, D.; Maneva, G.; Manganaro, M.; Mangano, S.; Manigot, P.; Mannheim, K.; Maragos, N.; Marano, D.; Marcowith, A.; Marín, J.; Mariotti, M.; Marisaldi, M.; Markoff, S.; Martí, J.; Martin, J. -M.; Martin, P.; Martin, L.; Martínez, M.; Martínez, G.; Martínez, O.; Marx, R.; Masetti, N.; Massimino, P.; Mastichiadis, A.; Mastropietro, M.; Masuda, S.; Matsumoto, H.; Matthews, N.; Mattiazzo, S.; Maurin, G.; Maxted, N.; Mayer, M.; Mazin, D.; Mazziotta, M. N.; Mc Comb, L.; McHardy, I.; Medina, C.; Melandri, A.; Melioli, C.; Melkumyan, D.; Mereghetti, S.; Meunier, J. -L.; Meures, T.; Meyer, M.; Micanovic, S.; Michael, T.; Michałowski, J.; Mievre, I.; Miller, J.; Minaya, I. A.; Mineo, T.; Mirabel, F.; Miranda, J. M.; Mirzoyan, R.; Mitchell, A.; Mizuno, T.; Moderski, R.; Mohammed, M.; Mohrmann, L.; Molijn, C.; Molinari, E.; Moncada, R.; Montaruli, T.; Monteiro, I.; Mooney, D.; Moore, P.; Moralejo, A.; Morcuende-Parrilla, D.; Moretti, E.; Mori, K.; Morlino, G.; Morris, P.; Morselli, A.; Moscato, F.; Motohashi, D.; Moulin, E.; Mueller, S.; Mukherjee, R.; Munar, P.; Mundell, C.; Mundet, J.; Murach, T.; Muraishi, H.; Murase, K.; Murphy, A.; Nagai, A.; Nagar, N.; Nagataki, S.; Nagayoshi, T.; Nagesh, B. K.; Naito, T.; Nakajima, D.; Nakamori, T.; Nakamura, Y.; Nakayama, K.; Naumann, D.; Nayman, P.; Neise, D.; Nellen, L.; Nemmen, R.; Neronov, A.; Neyroud, N.; Nguyen, T.; Nguyen, T. T.; Nguyen Trung, T.; Nicastro, L.; Nicolau-Kukliński, J.; Niemiec, J.; Nieto, D.; Nievas-Rosillo, M.; Nikołajuk, M.; Nishijima, K.; Nishikawa, K. -I.; Nishiyama, G.; Noda, K.; Nogues, L.; Nolan, S.; Nosek, D.; Nöthe, M.; Novosyadlyj, B.; Nozaki, S.; Nunio, F.; O'Brien, P.; Oakes, L.; Ocampo, C.; Ochoa, J. P.; Oger, R.; Ohira, Y.; Ohishi, M.; Ohm, S.; Okazaki, N.; Okumura, A.; Olive, J. -F.; Ong, R. A.; Orienti, M.; Orito, R.; Orlati, A.; Osborne, J. P.; Ostrowski, M.; Otte, N.; Ou, Z.; Ovcharov, E.; Oya, I.; Ozieblo, A.; Padovani, M.; Paiano, S.; Paizis, A.; Palacio, J.; Palatiello, M.; Palatka, M.; Pallotta, J.; Panazol, J. -L.; Paneque, D.; Panter, M.; Paoletti, R.; Paolillo, M.; Papitto, A.; Paravac, A.; Paredes, J. M.; Pareschi, G.; Parsons, R. D.; Paśko, P.; Pavy, S.; Pe'er, A.; Pech, M.; Pedaletti, G.; Peñil Del Campo, P.; Perez, A.; Pérez-Torres, M. A.; Perri, L.; Perri, M.; Persic, M.; Petrashyk, A.; Petrera, S.; Petrucci, P. -O.; Petruk, O.; Peyaud, B.; Pfeifer, M.; Piano, G.; Piel, Q.; Pieloth, D.; Pintore, F.; García, C. Pio; Pisarski, A.; Pita, S.; Pizarro, L.; Platos, Ł.; Pohl, M.; Poireau, V.; Pollo, A.; Porthault, J.; Poutanen, J.; Pozo, D.; Prandini, E.; Prasit, P.; Prast, J.; Pressard, K.; Principe, G.; Prokhorov, D.; Prokoph, H.; Prouza, M.; Pruteanu, G.; Pueschel, E.; Pühlhofer, G.; Puljak, I.; Punch, M.; Pürckhauer, S.; Queiroz, F.; Quinn, J.; Quirrenbach, A.; Rafighi, I.; Rainò, S.; Rajda, P. J.; Rando, R.; Rannot, R. C.; Razzaque, S.; Reichardt, I.; Reimer, O.; Reimer, A.; Reisenegger, A.; Renaud, M.; Reposeur, T.; Reville, B.; Rezaeian, A. H.; Rhode, W.; Ribeiro, D.; Ribó, M.; Richer, M. G.; Richtler, T.; Rico, J.; Rieger, F.; Riquelme, M.; Ristori, P. R.; Rivoire, S.; Rizi, V.; Rodriguez, J.; Rodriguez Fernandez, G.; Rodríguez Vázquez, J. J.; Rojas, G.; Romano, P.; Romeo, G.; Roncadelli, M.; Rosado, J.; Rosen, S.; Rosier Lees, S.; Rousselle, J.; Rovero, A. C.; Rowell, G.; Rudak, B.; Rugliancich, A.; Ruíz del Mazo, J. E.; Rujopakarn, W.; Rulten, C.; Russo, F.; Saavedra, O.; Sabatini, S.; Sacco, B.; Sadeh, I.; Sæther Hatlen, E.; Safi-Harb, S.; Sahakian, V.; Sailer, S.; Saito, T.; Sakaki, N.; Sakurai, S.; Salek, D.; Salesa Greus, F.; Salina, G.; Sanchez, D.; Sánchez-Conde, M.; Sandaker, H.; Sandoval, A.; Sangiorgi, P.; Sanguillon, M.; Sano, H.; Santander, M.; Santangelo, A.; Santos, E. M.; Sanuy, A.; Sapozhnikov, L.; Sarkar, S.; Satalecka, K.; Sato, Y.; Saturni, F. G.; Savalle, R.; Sawada, M.; Schanne, S.; Schioppa, E. J.; Schlenstedt, S.; Schmidt, T.; Schmoll, J.; Schneider, M.; Schoorlemmer, H.; Schovanek, P.; Schulz, A.; Schussler, F.; Schwanke, U.; Schwarz, J.; Schweizer, T.; Schwemmer, S.; Sciacca, E.; Scuderi, S.; Seglar-Arroyo, M.; Segreto, A.; Seitenzahl, I.; Semikoz, D.; Sergijenko, O.; Serre, N.; Servillat, M.; Seweryn, K.; Shah, K.; Shalchi, A.; Sharma, M.; Shellard, R. C.; Shilon, I.; Sidoli, L.; Sidz, M.; Siejkowski, H.; Silk, J.; Sillanpää, A.; Simone, D.; Singh, B. B.; Sironi, G.; Sitarek, J.; Sizun, P.; Sliusar, V.; Slowikowska, A.; Smith, A.; Sobczyńska, D.; Sokolenko, A.; Sol, H.; Sottile, G.; Springer, W.; Stahl, O.; Stamerra, A.; Stanič, S.; Starling, R.; Staszak, D.; Stawarz, Ł.; Steenkamp, R.; Stefanik, S.; Stegmann, C.; Steiner, S.; Stella, C.; Stephan, M.; Sternberger, R.; Sterzel, M.; Stevenson, B.; Stodulska, M.; Stodulski, M.; Stolarczyk, T.; Stratta, G.; Straumann, U.; Stuik, R.; Suchenek, M.; Suomijarvi, T.; Supanitsky, A. D.; Suric, T.; Sushch, I.; Sutcliffe, P.; Sykes, J.; Szanecki, M.; Szepieniec, T.; Tagliaferri, G.; Tajima, H.; Takahashi, K.; Takahashi, H.; Takahashi, M.; Takalo, L.; Takami, S.; Takata, J.; Takeda, J.; Tam, T.; Tanaka, M.; Tanaka, T.; Tanaka, Y.; Tanaka, S.; Tanci, C.; Tavani, M.; Tavecchio, F.; Tavernet, J. -P.; Tayabaly, K.; Tejedor, L. A.; Temme, F.; Temnikov, P.; Terada, Y.; Terrazas, J. C.; Terrier, R.; Terront, D.; Terzic, T.; Tescaro, D.; Teshima, M.; Testa, V.; Thoudam, S.; Tian, W.; Tibaldo, L.; Tiengo, A.; Tiziani, D.; Tluczykont, M.; Todero Peixoto, C. J.; Tokanai, F.; Tokarz, M.; Toma, K.; Tomastik, J.; Tonachini, A.; Tonev, D.; Tornikoski, M.; Torres, D. F.; Torresi, E.; Tosti, G.; Totani, T.; Tothill, N.; Toussenel, F.; Tovmassian, G.; Trakarnsirinont, N.; Travnicek, P.; Trichard, C.; Trifoglio, M.; Troyano Pujadas, I.; Tsirou, M.; Tsujimoto, S.; Tsuru, T.; Uchiyama, Y.; Umana, G.; Uslenghi, M.; Vagelli, V.; Vagnetti, F.; Valentino, M.; Vallania, P.; Valore, L.; Van den Berg, A. M.; van Driel, W.; van Eldik, C.; van Soelen, B.; Vandenbroucke, J.; Vanderwalt, J.; Varner, G. S.; Vasileiadis, G.; Vassiliev, V.; Vázquez, J. R.; Vázquez Acosta, M.; Vecchi, M.; Vega, A.; Veitch, P.; Venault, P.; Venter, C.; Vercellone, S.; Veres, P.; Vergani, S.; Verzi, V.; Vettolani, G. P.; Veyssiere, C.; Viana, A.; Vicha, J.; Vigorito, C.; Villanueva, J.; Vincent, P.; Vink, J.; Visconti, F.; Vittorini, V.; Voelk, H.; Voisin, V.; Vollhardt, A.; Vorobiov, S.; Vovk, I.; Vrastil, M.; Vuillaume, T.; Wagner, S. J.; Wagner, R.; Wagner, P.; Wakely, S. P.; Walstra, T.; Walter, R.; Ward, M.; Ward, J. E.; Warren, D.; Watson, J. J.; Webb, N.; Wegner, P.; Weiner, O.; Weinstein, A.; Weniger, C.; Werner, F.; Wetteskind, H.; White, M.; White, R.; Wierzcholska, A.; Wiesand, S.; Wijers, R.; Wilcox, P.; Wilhelm, A.; Wilkinson, M.; Will, M.; Williams, D. A.; Winter, M.; Wojcik, P.; Wolf, D.; Wood, M.; Wörnlein, A.; Wu, T.; Yadav, K. K.; Yaguna, C.; Yamamoto, T.; Yamamoto, H.; Yamane, N.; Yamazaki, R.; Yanagita, S.; Yang, L.; Yelos, D.; Yoshida, T.; Yoshida, M.; Yoshiike, S.; Yoshikoshi, T.; Yu, P.; Zaborov, D.; Zacharias, M.; Zaharijas, G.; Zajczyk, A.; Zampieri, L.; Zandanel, F.; Zanin, R.; Zanmar Sanchez, R.; Zaric, D.; Zavrtanik, M.; Zavrtanik, D.; Zdziarski, A. A.; Zech, A.; Zechlin, H.; Zhdanov, V. I.; Ziegler, A.; Ziemann, J.; Ziętara, K.; Zink, A.; Ziółkowski, J.; Zitelli, V.; Zoli, A.; Zorn, J., List of contributions from the Cherenkov Telescope Array Consortium presented at the 35th International Cosmic Ray Conference, July 12-20 2017, Busan, Korea...., arXiv e-prints
Sep. 2017

TARGET 5: A new multi-channel digitizer with triggering capabilities for gamma-ray atmospheric Cherenkov telescopes
Albert, A.; Funk, S.; Katagiri, H.; Kawashima, T.; Murphy, M.; Okumura, A.; Quagliani, R.; Sapozhnikov, L.; Shigenaka, A.; Tajima, H.; Tibaldo, L.; Vandenbroucke, J.; Varner, G.; Wu, T., TARGET 5 is a new application-specific integrated circuit (ASIC) of the TARGET family, designed for the readout of signals from photosensors in the cameras of imaging atmospheric Cherenkov telescopes (IACTs) for ground-based gamma-ray astronomy. TARGET 5 combines sampling and digitization on 16 signal channels with the formation of trigger signals based on the analog sum of groups of four channels. We describe the ASIC architecture and performance. TARGET 5 improves over the performance of the first-generation TARGET ASIC, achieving: tunable sampling frequency from <0.4 GSa/s to >1 GSa/s; a dynamic range on the data path of 1.2 V with effective dynamic range of 11 bits and DC noise of ∼0.6 mV; 3-dB bandwidth of 500 MHz; crosstalk between adjacent channels <1.3%; charge resolution improving from 40% to <4% between 3 photoelectrons (p.e.) and >100 p.e. (assuming 4 mV per p.e.); and minimum stable trigger threshold of 20 mV (5 p.e.) with trigger noise of 5 mV (1.2 p.e.), which is mostly limited by, Elsevier B.V.
Astroparticle Physics, Jun. 2017, [Reviewed]

Prospects for Cherenkov Telescope Array Observations of the Young Supernova Remnant RX J1713.7-3946
Acero; F.; Aloisio; R.; Amans; J.; et al., Corresponding, We perform simulations for future Cherenkov Telescope Array (CTA) observations of RX J1713.7-3946, a young supernova remnant (SNR) and one of the brightest sources ever discovered in very high energy (VHE) gamma rays. Special attention is paid to exploring possible spatial (anti)correlations of gamma rays with emission at other wavelengths, in particular X-rays and CO/H I emission. We present a series of simulated images of RX J1713.7-3946 for CTA based on a set of observationally motivated models for the gamma-ray emission. In these models, VHE gamma rays produced by high-energy electrons are assumed to trace the nonthermal X-ray emission observed by XMM-Newton, whereas those originating from relativistic protons delineate the local gas distributions. The local atomic and molecular gas distributions are deduced by the NANTEN team from CO and H I observations. Our primary goal is to show how one can distinguish the emission mechanism(s) of the gamma rays (I.e., hadronic versus leptonic, or a mixture of the two) through information provided by their spatial distribution, spectra, and time variation. This work is the first attempt to quantitatively evaluate the capabilities of CTA to, IOP Publishing
The Astrophysical Journal, 09 May 2017, [Reviewed]

TARGET: A Digitizing And Trigger ASIC For The Cherenkov Telescope Array
S. Funk; D. Jankowsky; H. Katagiri; M. Kraus; A. Okumura; H. Schoorlemmer; A. Shigenaka; H. Tajima; L. Tibaldo; G. Varner; A. Zink; J. Zorn, The future ground-based gamma-ray observatory Cherenkov Telescope Array (CTA) will feature multiple types of imaging atmospheric Cherenkov telescopes, each with thousands of pixels. To be affordable, camera concepts for these telescopes have to feature low cost per channel and at the same time meet the requirements for CTA in order to achieve the desired scientific goals. We present the concept of the TeV Array Readout Electronics with GSa/s sampling and Event Trigger (TARGET) Application Specific Circuit (ASIC), envisaged to be used in the cameras of various CTA telescopes, e. g. the Gamma-ray Cherenkov Telescope (GCT), a proposed 2-Mirror Small-Sized Telescope, and the Schwarzschild-Couder Telescope (SCT), a proposed Medium-Sized Telescope. In the latest version of this readout concept the sampling and trigger parts are split into dedicated ASICs, TARGET C and T5TEA, both providing 16 parallel input channels. TARGET C features a tunable sampling rate (usually 1 GSa/s), a 16k sample deep buffer for each channel and on-demand digitization and transmission of waveforms with typical spans of similar to 100 ns. The trigger ASIC, T5TEA, provides 4 low voltage differential signal (LVDS) trigger outputs and can generate a pedestal voltage independently for each channel. Trigger signals are generated by T5TEA based on the analog sum of the input in four independent groups of four adjacent channels and compared to a threshold set by the user. Thus, T5TEA generates four LVDS trigger outputs, as well as 16 pedestal voltages fed to TARGET C independently for each channel. We show preliminary results of the characterization and testing of TARGET C and T5TEA., AMER INST PHYSICS
HIGH ENERGY GAMMA-RAY ASTRONOMY, 2017

CTA Report 120: Development of readout boards for the second Large Sized Telescope and timing calibration of the DRS chips.
Saito T.; Ohoka H.; Okazaki N.; Orito R.; Katagiri H.; Kubo H.; Gunji S.; Konno Y.; Sakurai S.; Takeda J.; Tanaka M.; Tanigawa S.; Teshima M.; Nakajima D.; Nakamori T.; Nozaki S.; Masuda S.; Yamamoto T.; Hadasch D.; Mazin D.; CTA-Japan consortium; Ikeno M.; Uchida T., Cherenkov Telescope Array(CTA)計画は、口径の異なる複数の望遠鏡を用いて20GeVから100TeV 以上のガンマ線を従来よりも10倍高い感度で全天観測する望遠鏡建設計画である。我々は大口径望遠鏡搭載用カメラの試験・開発を行っている。カメラには1855本のPMTを用いるが、その信号波形の保存にアナログメモリ”DRS4”を用いる。本講演では、初号期用読み出し回路におけるDRS4チップのサンプリング時間間隔の較正方法と、2号機以降の読み出し回路の開発について報告する。, The Physical Society of Japan
Meeting Abstracts of the Physical Society of Japan, 2017

CTA Report 125：Status report for the construction of Focal Plane Instrument of LST-1
Sakurai S.; Orito R.; Kataoka J.; Katagiri H.; Kimura S.; Kushida J.; Kubo H.; Gunji S.; Koyama S.; Konno Y.; Saito T.; Ikeno M.; Sawada M.; Sunada Y.; Takahashi M.; Tanaka M.; Tsujimoto S.; Teshima M.; Terada Y.; Tokanai F.; Nakajima D.; Nakamori T.; Inada T.; Nagayoshi T.; Nishijima K.; Nishiyama G.; Nozaki S.; Hayashida M.; Bamba A.; Hirako J.; Fukami S.; Masuda S.; Yamamoto T.; Inome Y.; Yoshida T.; Hadasch D.; Mazin D.; the CTA-Japan consortium; Iwamura Y.; Uchida T.; Ohoka H.; Okumura A.; Okazaki N., The Physical Society of Japan
Meeting Abstracts of the Physical Society of Japan, 2017

CTA Report 126 : Improvement and calibration of the focal plane detector for LST
Sunada Y.; Orito R.; Kataoka J.; Katagiri H.; Kimura S.; Kushida J.; Kubo H.; Gunji S.; Koyama S.; Konno Y.; Saito T.; Ikeno M.; Sawada M.; Sakurai S.; Takahashi M.; Tanaka M.; Tsujimoto S.; Teshima M.; Terada Y.; Tokanai F.; Nakajima D.; Nakamori T.; Inada T.; Nagayoshi T.; Nishijima K.; Nishiyama G.; Nozaki S.; Hayashida M.; Bamba A.; Hirako J.; Fukami S.; Masuda S.; Yamamoto T.; Inome Y.; Yoshida T.; Hadasch D.; Mazin D.; the CTA-Japan consortium; Iwamura Y.; Uchida T.; Ohoka H.; Okumura A.; Okazaki N., The Physical Society of Japan
Meeting Abstracts of the Physical Society of Japan, 2017

FERMI/LAT STUDY OF GAMMA-RAY EMISSION IN THE DIRECTION OF THE MONOCEROS LOOP SUPERNOVA REMNANT
H. Katagiri; S. Sugiyama; M. Ackermann; J. Ballet; J. M. Casandjian; Y. Hanabata; J. W. Hewitt; M. Kerr; H. Kubo; M. Lemoine-Goumard; P. S. Ray, We present an analysis of the gamma-ray measurements by the Large Area Telescope on. board the Fermi Gammaray Space Telescope in the region of the supernova remnant. (SNR) Monoceros Loop. (G205.5+0.5). The brightest gamma-ray peak is spatially correlated with the Rosette Nebula, which is a molecular cloud complex adjacent to the southeast edge of the SNR. After subtraction of this emission by spatial modeling, the gamma-ray emission from the SNR emerges, which is extended and fit by a Gaussian spatial template. The gamma-ray spectra are significantly better reproduced by a curved shape than a simple power law. The luminosities between 0.2 and 300 GeV are similar to 4 x 10(34) erg s(-1) for the SNR and similar to 3 x 10(34) erg s(-1) for the Rosette Nebula, respectively. We argue that the gamma-rays likely originate from the interactions of particles accelerated in the SNR. The decay of neutral pions produced in nucleon-nucleon interactions of accelerated hadrons with interstellar gas provides a reasonable explanation for the gamma-ray emission of both the Rosette Nebula and the Monoceros SNR., IOP PUBLISHING LTD
ASTROPHYSICAL JOURNAL, Nov. 2016, [Reviewed]

Contributions of the Cherenkov Telescope Array (CTA) to the 6th International Symposium on High-Energy Gamma-Ray Astronomy (Gamma 2016)
CTA Consortium, The; :; Abchiche, A.; Abeysekara, U.; Abril, Ó.; Acero, F.; Acharya, B. S.; Adams, C.; Agnetta, G.; Aharonian, F.; Akhperjanian, A.; Albert, A.; Alcubierre, M.; Alfaro, J.; Alfaro, R.; Allafort, A. J.; Aloisio, R.; Amans, J. -P.; Amato, E.; Ambrogi, L.; Ambrosi, G.; Ambrosio, M.; Anderson, J.; Anduze, M.; Angüner, E. O.; Antolini, E.; Antonelli, L. A.; Antonucci, M.; Antonuccio, V.; Antoranz, P.; Aramo, C.; Aravantinos, A.; Araya, M.; Arcaro, C.; Arezki, B.; Argan, A.; Armstrong, T.; Arqueros, F.; Arrabito, L.; Arrieta, M.; Asano, K.; Ashley, M.; Aubert, P.; Singh, C. B.; Babic, A.; Backes, M.; Bais, A.; Bajtlik, S.; Balazs, C.; Balbo, M.; Balis, D.; Balkowski, C.; Ballester, O.; Ballet, J.; Balzer, A.; Bamba, A.; Bandiera, R.; Barber, A.; Barbier, C.; Barcelo, M.; Barkov, M.; Barnacka, A.; Barres de Almeida, U.; Barrio, J. A.; Basso, S.; Bastieri, D.; Bauer, C.; Becciani, U.; Becherini, Y.; Becker Tjus, J.; Beckmann, V.; Bednarek, W.; Benbow, W.; Benedico Ventura, D.; Berdugo, J.; Berge, D.; Bernardini, E.; Bernardini, M. G.; Bernhard, S.; Bernlöhr, K.; Bertucci, B.; Besel, M. -A.; Beshley, V.; Bhatt, N.; Bhattacharjee, P.; Bhattacharyya, W.; Bhattachryya, S.; Biasuzzi, B.; Bicknell, G.; Bigongiari, C.; Biland, A.; Bilinsky, A.; Bilnik, W.; Biondo, B.; Bird, R.; Bird, T.; Bissaldi, E.; Bitossi, M.; Blanch, O.; Blasi, P.; Blazek, J.; Bockermann, C.; Boehm, C.; Bogacz, L.; Bogdan, M.; Bohacova, M.; Boisson, C.; Boix, J.; Bolmont, J.; Bonanno, G.; Bonardi, A.; Bonavolontà, C.; Bonifacio, P.; Bonnarel, F.; Bonnoli, G.; Borkowski, J.; Bose, R.; Bosnjak, Z.; Böttcher, M.; Bousquet, J. -J.; Boutonnet, C.; Bouyjou, F.; Bowman, L.; Braiding, C.; Brantseg, T.; Brau-Nogué, S.; Bregeon, J.; Briggs, M.; Brigida, M.; Bringmann, T.; Brisken, W.; Bristow, D.; Britto, R.; Brocato, E.; Bron, S.; Brook, P.; Brooks, W.; Brown, A. M.; Brügge, K.; Brun, F.; Brun, P.; Brun, P.; Brunetti, G.; Brunetti, L.; Bruno, P.; Buanes, T.; Bucciantini, N.; Buchholtz, G.; Buckley, J.; Bugaev, V.; Bühler, R.; Bulgarelli, A.; Bulik, T.; Burton, M.; Burtovoi, A.; Busetto, G.; Buson, S.; Buss, J.; Byrum, K.; Cadoux, F.; Calvo Tovar, J.; Cameron, R.; Canelli, F.; Canestrari, R.; Capalbi, M.; Capasso, M.; Capobianco, G.; Caproni, A.; Caraveo, P.; Cardenzana, J.; Cardillo, M.; Carius, S.; Carlile, C.; Carosi, A.; Carosi, R.; Carquín, E.; Carr, J.; Carroll, M.; Carter, J.; Carton, P. -H.; Casandjian, J. -M.; Casanova, S.; Casanova, S.; Cascone, E.; Casiraghi, M.; Castellina, A.; Castroviejo Mora, J.; Catalani, F.; Catalano, O.; Catalanotti, S.; Cauz, D.; Cavazzani, S.; Cerchiara, P.; Chabanne, E.; Chadwick, P.; Chaleil, T.; Champion, C.; Chatterjee, A.; Chaty, S.; Chaves, R.; Chen, A.; Chen, X.; Chen, X.; Cheng, K.; Chernyakova, M.; Chiappetti, L.; Chikawa, M.; Chinn, D.; Chitnis, V. R.; Cho, N.; Christov, A.; Chudoba, J.; Cieślar, M.; Ciocci, M. A.; Clay, R.; Colafrancesco, S.; Colin, P.; Colley, J. -M.; Colombo, E.; Colome, J.; Colonges, S.; Conforti, V.; Connaughton, V.; Connell, S.; Conrad, J.; Contreras, J. L.; Coppi, P.; Corbel, S.; Coridian, J.; Cornat, R.; Corona, P.; Corti, D.; Cortina, J.; Cossio, L.; Costa, A.; Costantini, H.; Cotter, G.; Courty, B.; Covino, S.; Covone, G.; Crimi, G.; Criswell, S. J.; Crocker, R.; Croston, J.; Cuadra, J.; Cumani, P.; Cusumano, G.; Da Vela, P.; Dale, Ø.; D'Ammando, F.; Dang, D.; Dang, V. T.; Dangeon, L.; Daniel, M.; Davids, I.; Davids, I.; Dawson, B.; Dazzi, F.; de Aguiar Costa, B.; De Angelis, A.; de Araujo Cardoso, R. F.; De Caprio, V.; de Cássia dos Anjos, R.; De Cesare, G.; De Franco, A.; De Frondat, F.; de Gouveia Dal Pino, E. M.; de la Calle, I.; De Lisio, C.; de los Reyes Lopez, R.; De Lotto, B.; De Luca, A.; de Mello Neto, J. R. T.; de Naurois, M.; de Oña Wilhelmi, E.; De Palma, F.; De Persio, F.; de Souza, V.; Decock, G.; Decock, J.; Deil, C.; Del Santo, M.; Delagnes, E.; Deleglise, G.; Delgado, C.; Delgado, J.; della Volpe, D.; Deloye, P.; Detournay, M.; Dettlaff, A.; Devin, J.; Di Girolamo, T.; Di Giulio, C.; Di Paola, A.; Di Pierro, F.; Diaz, M. A.; Díaz, C.; Dib, C.; Dick, J.; Dickinson, H.; Diebold, S.; Digel, S.; Dipold, J.; Disset, G.; Distefano, A.; Djannati-Ataï, A.; Doert, M.; Dohmke, M.; Domínguez, A.; Dominik, N.; Dominique, J. -L.; Dominis Prester, D.; Donat, A.; Donnarumma, I.; Dorner, D.; Doro, M.; Dournaux, J. -L.; Downes, T.; Doyle, K.; Drake, G.; Drappeau, S.; Drass, H.; Dravins, D.; Drury, L.; Dubus, G.; Ducci, L.; Dumas, D.; Dundas Morå, K.; Durand, D.; D'Urso, D.; Dwarkadas, V.; Dyks, J.; Dyrda, M.; Ebr, J.; Edy, E.; Egberts, K.; Eger, P.; Egorov, A.; Einecke, S.; Eisch, J.; Eisenkolb, F.; Eleftheriadis, C.; Elsaesser, D.; Elsässer, D.; Emmanoulopoulos, D.; Engelbrecht, C.; Engelhaupt, D.; Ernenwein, J. -P.; Escarate, P.; Eschbach, S.; Espinoza, C.; Evans, P.; Fairbairn, M.; Falceta-Goncalves, D.; Falcone, A.; Fallah Ramazani, V.; Fantinel, D.; Farakos, K.; Farnier, C.; Farrell, E.; Fasola, G.; Favre, Y.; Fede, E.; Fedora, R.; Fedorova, E.; Fegan, S.; Ferenc, D.; Fernandez-Alonso, M.; Fernández-Barral, A.; Ferrand, G.; Ferreira, O.; Fesquet, M.; Fetfatzis, P.; Fiandrini, E.; Fiasson, A.; Filipčič, A.; Filipovic, M.; Fink, D.; Finley, C.; Finley, J. P.; Finoguenov, A.; Fioretti, V.; Fiorini, M.; Fleischhack, H.; Flores, H.; Florin, D.; Föhr, C.; Fokitis, E.; Fonseca, M. V.; Font, L.; Fontaine, G.; Fontes, B.; Fornasa, M.; Fornasa, M.; Förster, A.; Fortin, P.; Fortson, L.; Fouque, N.; Franckowiak, A.; Franckowiak, A.; Franco, F. J.; Freire Mota Albuquerque, I.; Freixas Coromina, L.; Fresnillo, L.; Fruck, C.; Fuessling, M.; Fugazza, D.; Fujita, Y.; Fukami, S.; Fukazawa, Y.; Fukuda, T.; Fukui, Y.; Funk, S.; Furniss, A.; Gäbele, W.; Gabici, S.; Gadola, A.; Galindo, D.; Gall, D. D.; Gallant, Y.; Galloway, D.; Gallozzi, S.; Galvez, J. A.; Gao, S.; Garcia, A.; Garcia, B.; García Gil, R.; Garcia López, R.; Garczarczyk, M.; Gardiol, D.; Gargano, C.; Gargano, F.; Garozzo, S.; Garrecht, F.; Garrido, L.; Garrido-Ruiz, M.; Gascon, D.; Gaskins, J.; Gaudemard, J.; Gaug, M.; Gaweda, J.; Gebhardt, B.; Gebyehu, M.; Geffroy, N.; Genolini, B.; Gerard, L.; Ghalumyan, A.; Ghedina, A.; Ghislain, P.; Giammaria, P.; Giannakaki, E.; Gianotti, F.; Giarrusso, S.; Giavitto, G.; Giebels, B.; Gieras, T.; Giglietto, N.; Gika, V.; Gimenes, R.; Giomi, M.; Giommi, P.; Giordano, F.; Giovannini, G.; Girardot, P.; Giro, E.; Giroletti, M.; Gironnet, J.; Giuliani, A.; Glicenstein, J. -F.; Gnatyk, R.; Godinovic, N.; Goldoni, P.; Gomez, G.; Gonzalez, M. M.; González, A.; Gora, D.; Gothe, K. S.; Gotz, D.; Goullon, J.; Grabarczyk, T.; Graciani, R.; Graham, J.; Grandi, P.; Granot, J.; Grasseau, G.; Gredig, R.; Green, A. J.; Green, A. M.; Greenshaw, T.; Grenier, I.; Griffiths, S.; Grillo, A.; Grondin, M. -H.; Grube, J.; Grudzinska, M.; Grygorczuk, J.; Guarino, V.; Guberman, D.; Gunji, S.; Gyuk, G.; Hadasch, D.; Hagedorn, A.; Hagge, L.; Hahn, J.; Hakobyan, H.; Hara, S.; Hardcastle, M. J.; Hassan, T.; Hatanaka, K.; Haubold, T.; Haupt, A.; Hayakawa, T.; Hayashida, M.; Heller, M.; Heller, R.; Helo, J. C.; Henault, F.; Henri, G.; Hermann, G.; Hermel, R.; Herrera Llorente, J.; Herrera Llorente, J.; Herrero, A.; Hervet, O.; Hidaka, N.; Hinton, J.; Hirai, W.; Hirotani, K.; Hnatyk, B.; Hoang, J.; Hoffmann, D.; Hofmann, W.; Holch, T.; Holder, J.; Hooper, S.; Horan, D.; Hörandel, J.; Hörbe, M.; Horns, D.; Horvath, P.; Hose, J.; Houles, J.; Hovatta, T.; Hrabovsky, M.; Hrupec, D.; Huet, J. -M.; Huetten, M.; Hughes, G.; Hui, D.; Humensky, T. B.; Hussein, M.; Iacovacci, M.; Ibarra, A.; Ikeno, Y.; Illa, J. M.; Impiombato, D.; Inada, T.; Incorvaia, S.; Infante, L.; Inome, Y.; Inoue, S.; Inoue, T.; Inoue, Y.; Iocco, F.; Ioka, K.; Iori, M.; Ishio, K.; Ishio, K.; Israel, G. L.; Iwamura, Y.; Jablonski, C.; Jacholkowska, A.; Jacquemier, J.; Jamrozy, M.; Janecek, P.; Janiak, M.; Jankowsky, D.; Jankowsky, F.; Jean, P.; Jegouzo, I.; Jenke, P.; Jimenez, J. J.; Jingo, M.; Jingo, M.; Jocou, L.; Jogler, T.; Johnson, C. A.; Jones, M.; Josselin, M.; Journet, L.; Jung, I.; Kaaret, P.; Kagaya, M.; Kakuwa, J.; Kalekin, O.; Kalkuhl, C.; Kamon, H.; Kankanyan, R.; Karastergiou, A.; Kärcher, K.; Karczewski, M.; Karkar, S.; Karn, P.; Kasperek, J.; Katagiri, H.; Kataoka, J.; Katarzyński, K.; Kato, S.; Katz, U.; Kawanaka, N.; Kaye, L.; Kazanas, D.; Kelley-Hoskins, N.; Kersten, J.; Khélifi, B.; Kieda, D. B.; Kihm, T.; Kimeswenger, S.; Kisaka, S.; Kishida, S.; Kissmann, R.; Klepser, S.; Kluźniak, W.; Knapen, J.; Knapp, J.; Knödlseder, J.; Koch, B.; Köck, F.; Kocot, J.; Kohri, K.; Kokkotas, K.; Kokkotas, K.; Kolitzus, D.; Komin, N.; Kominis, I.; Kong, A.; Konno, Y.; Kosack, K.; Koss, G.; Kossatz, M.; Kowal, G.; Koyama, S.; Kozioł, J.; Kraus, M.; Krause, J.; Krause, M.; Krawzcynski, H.; Krennrich, F.; Kretzschmann, A.; Kruger, P.; Kubo, H.; Kudryavtsev, V.; Kukec Mezek, G.; Kuklis, M.; Kuroda, H.; Kushida, J.; La Barbera, A.; La Palombara, N.; La Parola, V.; La Rosa, G.; Laffon, H.; Lahmann, R.; Lakicevic, M.; Lalik, K.; Lamanna, G.; Landriu, D.; Landt, H.; Lang, R. G.; Lapington, J.; Laporte, P.; Le Fèvre, J. -P.; Le Flour, T.; Le Sidaner, P.; Lee, S. -H.; Lee, W. H.; Lees, J. -P.; Lefaucheur, J.; Leffhalm, K.; Leich, H.; Leigui de Oliveira, M. A.; Lelas, D.; Lemière, A.; Lemoine-Goumard, M.; Lenain, J. -P.; Leonard, R.; Leoni, R.; Lessio, L.; Leto, G.; Leveque, A.; Lieunard, B.; Limon, M.; Lindemann, R.; Lindfors, E.; Linhoff, L.; Liolios, A.; Lipniacka, A.; Lockart, H.; Lohse, T.; Łokas, E.; Lombardi, S.; Longo, F.; Lopatin, A.; Lopez, M.; Loreggia, D.; Louge, T.; Louis, F.; Louys, M.; Lucarelli, F.; Lucchesi, D.; Lüdecke, H.; Luigi, T.; Luque-Escamilla, P. L.; Lyard, E.; Maccarone, M. C.; Maccarone, T.; Maccarone, T. J.; Mach, E.; Madejski, G. M.; Madonna, A.; Magniette, F.; Magniez, A.; Mahabir, M.; Maier, G.; Majumdar, P.; Majumdar, P.; Makariev, M.; Malaguti, G.; Malaspina, G.; Mallot, A. K.; Malouf, A.; Maltezos, S.; Malyshev, D.; Mancilla, A.; Mandat, D.; Maneva, G.; Manganaro, M.; Mangano, S.; Manigot, P.; Mankushiyil, N.; Mannheim, K.; Maragos, N.; Marano, D.; Marchegiani, P.; Marcomini, J. A.; Marcowith, A.; Mariotti, M.; Marisaldi, M.; Markoff, S.; Martens, C.; Martí, J.; Martin, J. -M.; Martin, L.; Martin, P.; Martínez, G.; Martínez, M.; Martínez, O.; Martynyuk-Lototskyy, K.; Marx, R.; Masetti, N.; Massimino, P.; Mastichiadis, A.; Mastroianni, S.; Mastropietro, M.; Masuda, S.; Matsumoto, H.; Matsuoka, S.; Matthews, N.; Mattiazzo, S.; Maurin, G.; Maxted, N.; Maxted, N.; Maya, J.; Mayer, M.; Mazin, D.; Mazziotta, M. N.; Mc Comb, L.; McCubbin, N.; McHardy, I.; Medina, C.; Mehrez, F.; Melioli, C.; Melkumyan, D.; Melse, T.; Mereghetti, S.; Merk, M.; Mertsch, P.; Meunier, J. -L.; Meures, T.; Meyer, M.; Meyrelles, J. L., jr; Miccichè, A.; Michael, T.; Michałowski, J.; Mientjes, P.; Mievre, I.; Mihailidis, A.; Miller, J.; Mineo, T.; Minuti, M.; Mirabal, N.; Mirabel, F.; Miranda, J. M.; Mirzoyan, R.; Mitchell, A.; Mizuno, T.; Moderski, R.; Mognet, I.; Mohammed, M.; Moharana, R.; Mohrmann, L.; Molinari, E.; Molyneux, P.; Monmarthe, E.; Monnier, G.; Montaruli, T.; Monte, C.; Monteiro, I.; Mooney, D.; Moore, P.; Moralejo, A.; Morello, C.; Moretti, E.; Mori, K.; Morris, P.; Morselli, A.; Moscato, F.; Motohashi, D.; Mottez, F.; Moudden, Y.; Moulin, E.; Mueller, S.; Mukherjee, R.; Munar, P.; Munari, M.; Mundell, C.; Mundet, J.; Muraishi, H.; Murase, K.; Muronga, A.; Murphy, A.; Nagar, N.; Nagataki, S.; Nagayoshi, T.; Nagesh, B. K.; Naito, T.; Nakajima, D.; Nakajima, D.; Nakamori, T.; Nakayama, K.; Nanni, J.; Naumann, D.; Nayman, P.; Nellen, L.; Nemmen, R.; Neronov, A.; Neyroud, N.; Nguyen, T.; Nguyen, T. T.; Nguyen Trung, T.; Nicastro, L.; Nicolau-Kukliński, J.; Niederwanger, F.; Niedźwiecki, A.; Niemiec, J.; Nieto, D.; Nievas-Rosillo, M.; Nikolaidis, A.; Nikołajuk, M.; Nishijima, K.; Nishikawa, K. -I.; Nishiyama, G.; Noda, K.; Noda, K.; Nogues, L.; Nolan, S.; Northrop, R.; Nosek, D.; Nöthe, M.; Novosyadlyj, B.; Nozka, L.; Nunio, F.; Oakes, L.; O'Brien, P.; Ocampo, C.; Occhipinti, G.; Ochoa, J. P.; OFaolain de Bhroithe, A.; Oger, R.; Ohira, Y.; Ohishi, M.; Ohm, S.; Ohoka, H.; Okazaki, N.; Okumura, A.; Olive, J. -F.; Olszowski, D.; Ong, R. A.; Ono, S.; Orienti, M.; Orito, R.; Orlati, A.; Osborne, J.; Ostrowski, M.; Ottaway, D.; Otte, N.; Öttl, S.; Ovcharov, E.; Oya, I.; Ozieblo, A.; Padovani, M.; Pagano, I.; Paiano, S.; Paizis, A.; Palacio, J.; Palatka, M.; Pallotta, J.; Panagiotidis, K.; Panazol, J. -L.; Paneque, D.; Panter, M.; Panzera, M. R.; Paoletti, R.; Paolillo, M.; Papayannis, A.; Papyan, G.; Paravac, A.; Paredes, J. M.; Pareschi, G.; Park, N.; Parsons, D.; Paśko, P.; Pavy, S.; Pech, M.; Peck, A.; Pedaletti, G.; Pe'er, A.; Peet, S.; Pelat, D.; Pepato, A.; Perez, M. d. C.; Perri, L.; Perri, M.; Persic, M.; Persic, M.; Petrashyk, A.; Petrucci, P. -O.; Petruk, O.; Peyaud, B.; Pfeifer, M.; Pfeiffer, G.; Piano, G.; Pieloth, D.; Pierre, E.; Pinto de Pinho, F.; García, C. Pio; Piret, Y.; Pisarski, A.; Pita, S.; Platos, Ł.; Platzer, R.; Podkladkin, S.; Pogosyan, L.; Pohl, M.; Poinsignon, P.; Pollo, A.; Porcelli, A.; Porthault, J.; Potter, W.; Poulios, S.; Poutanen, J.; Prandini, E.; Prandini, E.; Prast, J.; Pressard, K.; Principe, G.; Profeti, F.; Prokhorov, D.; Prokoph, H.; Prouza, M.; Pruchniewicz, R.; Pruteanu, G.; Pueschel, E.; Pühlhofer, G.; Puljak, I.; Punch, M.; Pürckhauer, S.; Pyzioł, R.; Queiroz, F.; Quel, E. J.; Quinn, J.; Quirrenbach, A.; Rafighi, I.; Rainò, S.; Rajda, P. J.; Rameez, M.; Rando, R.; Rannot, R. C.; Rataj, M.; Ravel, T.; Razzaque, S.; Reardon, P.; Reichardt, I.; Reimann, O.; Reimer, A.; Reimer, O.; Reisenegger, A.; Renaud, M.; Renner, S.; Reposeur, T.; Reville, B.; Rezaeian, A.; Rhode, W.; Ribeiro, D.; Ribeiro Prado, R.; Ribó, M.; Richards, G.; Richer, M. G.; Richtler, T.; Rico, J.; Ridky, J.; Rieger, F.; Riquelme, M.; Ristori, P. R.; Rivoire, S.; Rizi, V.; Roache, E.; Rodriguez, J.; Rodriguez Fernandez, G.; Rodríguez Vázquez, J. J.; Rojas, G.; Romano, P.; Romeo, G.; Roncadelli, M.; Rosado, J.; Rose, J.; Rosen, S.; Rosier Lees, S.; Ross, D.; Rouaix, G.; Rousselle, J.; Rovero, A. C.; Rowell, G.; Roy, F.; Royer, S.; Rubini, A.; Rudak, B.; Rugliancich, A.; Rujopakarn, W.; Rulten, C.; Rupiński, M.; Russo, F.; Russo, F.; Rutkowski, K.; Saavedra, O.; Sabatini, S.; Sacco, B.; Sadeh, I.; Saemann, E. O.; Safi-Harb, S.; Saggion, A.; Sahakian, V.; Saito, T.; Sakaki, N.; Sakurai, S.; Salamon, A.; Salega, M.; Salek, D.; Salesa Greus, F.; Salgado, J.; Salina, G.; Salinas, L.; Salini, A.; Sanchez, D.; Sanchez-Conde, M.; Sandaker, H.; Sandoval, A.; Sangiorgi, P.; Sanguillon, M.; Sano, H.; Santander, M.; Santangelo, A.; Santos, E. M.; Santos-Lima, R.; Sanuy, A.; Sapozhnikov, L.; Sarkar, S.; Satalecka, K.; Satalecka, K.; Sato, Y.; Savalle, R.; Sawada, M.; Sayède, F.; Schanne, S.; Schanz, T.; Schioppa, E. J.; Schlenstedt, S.; Schmid, J.; Schmidt, T.; Schmoll, J.; Schneider, M.; Schoorlemmer, H.; Schovanek, P.; Schubert, A.; Schullian, E. -M.; Schultze, J.; Schulz, A.; Schulz, S.; Schure, K.; Schussler, F.; Schwab, T.; Schwanke, U.; Schwarz, J.; Schweizer, T.; Schwemmer, S.; Schwendicke, U.; Schwerdt, C.; Sciacca, E.; Scuderi, S.; Segreto, A.; Seiradakis, J. -H.; Sembroski, G. H.; Semikoz, D.; Sergijenko, O.; Serre, N.; Servillat, M.; Seweryn, K.; Shafi, N.; Shalchi, A.; Sharma, M.; Shayduk, M.; Shellard, R. C.; Shibata, T.; Shigenaka, A.; Shilon, I.; Shum, E.; Sidoli, L.; Sidz, M.; Sieiro, J.; Siejkowski, H.; Silk, J.; Sillanpää, A.; Simone, D.; Simpson, H.; Singh, B. B.; Sinha, A.; Sironi, G.; Sitarek, J.; Sizun, P.; Sliusar, V.; Sliusar, V.; Smith, A.; Sobczyńska, D.; Sol, H.; Sottile, G.; Sowiński, M.; Spanier, F.; Spengler, G.; Spiga, R.; Stadler, R.; Stahl, O.; Stamerra, A.; Stanič, S.; Starling, R.; Staszak, D.; Stawarz, Ł.; Steenkamp, R.; Stefanik, S.; Stegmann, C.; Steiner, S.; Stella, C.; Stephan, M.; Stergioulas, N.; Sternberger, R.; Sterzel, M.; Stevenson, B.; Stinzing, F.; Stodulska, M.; Stodulski, M.; Stolarczyk, T.; Stratta, G.; Straumann, U.; Stringhetti, L.; Strzys, M.; Stuik, R.; Sulanke, K. -H.; Suomijärvi, T.; Supanitsky, A. D.; Suric, T.; Sushch, I.; Sutcliffe, P.; Sykes, J.; Szanecki, M.; Szepieniec, T.; Szwarnog, P.; Tacchini, A.; Tachihara, K.; Tagliaferri, G.; Tajima, H.; Takahashi, H.; Takahashi, K.; Takahashi, M.; Takalo, L.; Takami, S.; Takata, J.; Takeda, J.; Talbot, G.; Tam, T.; Tanaka, M.; Tanaka, S.; Tanaka, T.; Tanaka, Y.; Tanci, C.; Tanigawa, S.; Tavani, M.; Tavecchio, F.; Tavernet, J. -P.; Tayabaly, K.; Taylor, A.; Tejedor, L. A.; Telezhinsky, I.; Temme, F.; Temnikov, P.; Tenzer, C.; Terada, Y.; Terrazas, J. C.; Terrier, R.; Terront, D.; Terzic, T.; Tescaro, D.; Teshima, M.; Teshima, M.; Testa, V.; Tezier, D.; Thayer, J.; Thornhill, J.; Thoudam, S.; Thuermann, D.; Tibaldo, L.; Tiengo, A.; Timpanaro, M. C.; Tiziani, D.; Tluczykont, M.; Todero Peixoto, C. J.; Tokanai, F.; Tokarz, M.; Toma, K.; Tomastik, J.; Tomono, Y.; Tonachini, A.; Tonev, D.; Torii, K.; Tornikoski, M.; Torres, D. F.; Torres, M.; Torresi, E.; Toso, G.; Tosti, G.; Totani, T.; Tothill, N.; Toussenel, F.; Tovmassian, G.; Toyama, T.; Travnicek, P.; Trichard, C.; Trifoglio, M.; Troyano Pujadas, I.; Trzeciak, M.; Tsinganos, K.; Tsujimoto, S.; Tsuru, T.; Uchiyama, Y.; Umana, G.; Umetsu, Y.; Upadhya, S. S.; Uslenghi, M.; Vagelli, V.; Vagnetti, F.; Valdes-Galicia, J.; Valentino, M.; Vallania, P.; Valore, L.; van Driel, W.; van Eldik, C.; van Soelen, B.; Vandenbroucke, J.; Vanderwalt, J.; Vasileiadis, G.; Vassiliev, V.; Vázquez, J. R.; Vázquez Acosta, M. L.; Vecchi, M.; Vega, A.; Vegas, I.; Veitch, P.; Venault, P.; Venema, L.; Venter, C.; Vercellone, S.; Vergani, S.; Verma, K.; Verzi, V.; Vettolani, G. P.; Veyssiere, C.; Viana, A.; Viaux, N.; Vicha, J.; Vigorito, C.; Vincent, P.; Vincent, S.; Vink, J.; Vittorini, V.; Vlahakis, N.; Vlahos, L.; Voelk, H.; Voisin, V.; Vollhardt, A.; Volpicelli, A.; von Brand, H.; Vorobiov, S.; Vovk, I.; Vrastil, M.; Vu, L. V.; Vuillaume, T.; Wagner, R.; Wagner, R.; Wagner, S. J.; Wakely, S. P.; Walstra, T.; Walter, R.; Walther, T.; Ward, J. E.; Ward, M.; Warda, K.; Warren, D.; Wassberg, S.; Watson, J. J.; Wawer, P.; Wawrzaszek, R.; Webb, N.; Wegner, P.; Weiner, O.; Weinstein, A.; Wells, R.; Werner, F.; Wetteskind, H.; White, M.; White, R.; Więcek, M.; Wierzcholska, A.; Wiesand, S.; Wijers, R.; Wilcox, P.; Wild, N.; Wilhelm, A.; Wilkinson, M.; Will, M.; Will, M.; Williams, D. A.; Williams, J. T.; Willingale, R.; Wilson, N.; Winde, M.; Winiarski, K.; Winkler, H.; Winter, M.; Wischnewski, R.; Witt, E.; Wojcik, P.; Wolf, D.; Wood, M.; Wörnlein, A.; Wu, E.; Wu, T.; Yadav, K. K.; Yamamoto, H.; Yamamoto, T.; Yamane, N.; Yamazaki, R.; Yanagita, S.; Yang, L.; Yelos, D.; Yoshida, A.; Yoshida, M.; Yoshida, T.; Yoshiike, S.; Yoshikoshi, T.; Yu, P.; Zabalza, V.; Zaborov, D.; Zacharias, M.; Zaharijas, G.; Zajczyk, A.; Zampieri, L.; Zandanel, F.; Zanmar Sanchez, R.; Zaric, D.; Zavrtanik, D.; Zavrtanik, M.; Zdziarski, A.; Zech, A.; Zechlin, H.; Zhao, A.; Zhdanov, V.; Ziegler, A.; Ziemann, J.; Ziętara, K.; Zink, A.; Ziółkowski, J.; Zitelli, V.; Zoli, A.; Zorn, J.; Żychowski, P., List of contributions from the Cherenkov Telescope Array (CTA) Consortium presented at the 6th International Symposium on High-Energy Gamma-Ray Astronomy (Gamma 2016), July 11-15, 2016, in Heidelberg, Germany...., arXiv e-prints
Oct. 2016

The First Fermi LAT Supernova Remnant Catalog
Acero, F.; Ackermann, M.; Ajello, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bellazzini, R.; Bissaldi, E.; Blandford, R. D.; Bloom, E. D.; Bonino, R.; Bottacini, E.; Brandt, T. J.; Bregeon, J.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caputo, R.; Caragiulo, M.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Chekhtman, A.; Chiang, J.; Chiaro, G.; Ciprini, S.; Claus, R.; Cohen, J. M.; Cohen-Tanugi, J.; Cominsky, L. R.; Condon, B.; Conrad, J.; Cutini, S.; D'Ammando, F.; de Angelis, A.; de Palma, F.; Desiante, R.; Digel, S. W.; Di Venere, L.; Drell, P. S.; Drlica-Wagner, A.; Favuzzi, C.; Ferrara, E. C.; Franckowiak, A.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Gomez-Vargas, G. A.; Grenier, I. A.; Grondin, M. -H.; Guillemot, L.; Guiriec, S.; Gustafsson, M.; Hadasch, D.; Harding, A. K.; Hayashida, M.; Hays, E.; Hewitt, J. W.; Hill, A. B.; Horan, D.; Hou, X.; Iafrate, G.; Jogler, T.; Jóhannesson, G.; Johnson, A. S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Katsuta, J.; Kerr, M.; Knödlseder, J.; Kocevski, D.; Kuss, M.; Laffon, H.; Lande, J.; Larsson, S.; Latronico, L.; Lemoine-Goumard, M.; Li, J.; Li, L.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Magill, J.; Maldera, S.; Marelli, M.; Mayer, M.; Mazziotta, M. N.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nemmen, R.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orienti, M.; Orlando, E.; Ormes, J. F.; Paneque, D.; Perkins, J. S.; Pesce-Rollins, M.; Petrosian, V.; Piron, F.; Pivato, G.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Razzaque, S.; Reimer, A.; Reimer, O.; Renaud, M.; Reposeur, T.; Rousseau, R.; Saz Parkinson, P. M.; Schmid, J.; Schulz, A.; Sgrò, C.; Siskind, E. J.; Spada, F.; Spandre, G.; Spinelli, P.; Strong, A. W.; Suson, D. J.; Tajima, H.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Tibolla, O.; Torres, D. F.; Tosti, G.; Troja, E.; Uchiyama, Y.; Vianello, G.; Wells, B.; Wood, K. S.; Wood, M.; Yassine, M.; den Hartog, P. R.; Zimmer, S., To uniformly determine the properties of supernova remnants (SNRs) at high energies, we have developed the first systematic survey at energies from 1 to 100 GeV using data from the Fermi Large Area Telescope (LAT). Based on the spatial overlap of sources detected at GeV energies with SNRs known from radio surveys, we classify 30 sources as likely GeV SNRs. We also report 14 marginal associations and 245 flux upper limits. A mock catalog in which the positions of known remnants are scrambled in Galactic longitude allows us to determine an upper limit of 22% on the number of GeV candidates falsely identified as SNRs. We have also developed a method to estimate spectral and spatial systematic errors arising from the diffuse interstellar emission model, a key component of all Galactic Fermi LAT analyses. By studying remnants uniformly in aggregate, we measure the GeV properties common to these objects and provide a crucial context for the detailed modeling of individual SNRs. Combining our GeV results with multiwavelength (MW) data, including radio, X-ray, and TeV, we demonstrate the need for improvements to previously sufficient, simple models describing the GeV and radio emission from these objects. We model the GeV and MW emission from SNRs in aggregate to constrain their maximal contribution to observed Galactic cosmic rays....
The Astrophysical Journal Supplement Series, May 2016

FERMI LAT DISCOVERY OF EXTENDED GAMMA-RAY EMISSIONS IN THE VICINITY OF THE HB 3 SUPERNOVA REMNANT
H. Katagiri; K. Yoshida; J. Ballet; M. -H. Grondin; Y. Hanabata; J. W. Hewitt; H. Kubo; M. Lemoine-Goumard, We report the discovery of extended gamma-ray emission measured by the Large Area Telescope. (LAT) onboard the Fermi Gamma-ray Space Telescope in the region of the supernova remnant. (SNR) HB 3 (G132.7+1.3) and the W3 II complex adjacent to the southeast of the remnant. W3 is spatially associated with bright (CO)-C-12 (J = 1-0) emission. The gamma-ray emission is spatially correlated with this gas and the SNR. We discuss the possibility that gamma rays originate in interactions between particles accelerated in the SNR and interstellar gas or radiation fields. The decay of neutral pions produced in nucleon-nucleon interactions between accelerated hadrons and interstellar gas provides a reasonable explanation for the gamma-ray emission. The emission from W3 is consistent with irradiation of the CO clouds by the cosmic rays accelerated in HB 3., IOP PUBLISHING LTD
ASTROPHYSICAL JOURNAL, Feb. 2016, [Reviewed]

22pAM-2 Evaluation of the timing response of a waveform sampling circuit TARGET for the next generation gamma-ray observatory CTA
Shigenaka Akane; Katagiri Hideaki; Tajima Hiroyasu; Okumura Akira; the CTA Consortium, The Physical Society of Japan (JPS)
Meeting Abstracts of the Physical Society of Japan, 2016

CTA Report 109: Monte Carlo simulation study for cosmic-ray chemical composition measurement using direct Cherenkov photons (V)
Ohishi Michiko; Ikeno Yuhei; Inada Tomohiro; Okumura Akira; Katagiri Hideaki; Kushida Junko; Gunji Shuichi; Saito Takayuki; Sakaki Naoto; Sato Yuta; Tan Dang Viet; Nagayoshi Tsutomu; Nishijima Kyoshi; Masuda Shu; Yoshikoshi Takanori; Yoshida Tatsuo; the CTA-Japan Consortium,

近年、宇宙線原子核が上空で放出するDirect Cherenkov光を地上のチェレンコフ望遠鏡で測定する手法がsub-PeV領域の化学組成測定に有効であることが分かってきた。一方で、宇宙線が非弾性散乱後に形成する空気シャワーの発展の様態にも核種の情報は残されている。本講演では、CTAアレイのシミュレーションデータに対して上記2種類の観測情報を取り入れた解析を適用した場合に、得られる電荷分解能・事象数を予測した結果について報告する。

, The Physical Society of Japan
Meeting Abstracts of the Physical Society of Japan, 2016

CTA Report 110: Development of light concentrators to improve the photodetection efficiency of focal-plane photodetectors
Okumura A.; Ono S.; Tan Dang Viet; Asano A.; Katagiri H.; Tajima H.; Teshima M.; Nakamura Y.; Hayashida M.; Yamamoto T.; Yoshida T.; the CTA Consortium,

大気チェレンコフ光望遠鏡による超高エネルギーガンマ線の観測では、焦点面検出器の光検出効率がガンマ線検出感度を決める要因のひとつである。高い光検出効率は夜光に対するチェレンコフ光の信号比を高め低エネルギーガンマ線の観測を可能にする。また同時に、鏡の面積やシリコン半導体の使用面積を減らすことで望遠鏡建設費の低減も可能にする。本講演ではCTA大口径望遠鏡用の集光装置の開発状況、また中・小口径望遠鏡用の集光装置の開発可能性について報告する。

, The Physical Society of Japan
Meeting Abstracts of the Physical Society of Japan, 2016

A simulation study of the performance of the CTA Small-Sized Telescopes equipped with silicon photomultipliers
Sato Yuta; Ikeno Yuhei; Inada Tomohiro; Ohishi Michiko; Katagiri Hideaki; Kushida Junko; Gunji Shuichi; Saito Takayuki; Sakaki Naoto; Tajima Hiroyasu; Tan Dang Viet; Nagayoshi Tsutomu; Nishijima Kyoshi; Hidaka Naoya; Masuda Shu; Yamane Nobuhito; Yoshikoshi Takanori; Yoshida Tatsuo; The CTA Consortium,

国際ガンマ線天文台CTAの小口径望遠鏡には、光検出器として半導体光電子増倍素子を採用する予定である。この素子は高い光検出効率をもっているが、オプティカルクロストークが生じるという特徴をもつ。また、この特性に加え夜光や月光の影響は、光検出効率の波長特性や時間応答特性に大きく左右される。本講演では複数の採用候補の素子特性を組み込んだモンテカルロシミュレーションを行い、小口径望遠鏡の総合性能について報告する。

, The Physical Society of Japan
Meeting Abstracts of the Physical Society of Japan, 2016

CTA Report 113: Development of Small-Sized and Medium-Sized Telescopes with Schwarzschild-Couder optics
Okumura A.; Asano A.; Katagiri H.; Sato Y.; Shigenaka A.; Tajima H.; Nakamura Y.; Yamane N.; the CTA Consortium,

結像性能を維持したまま大気チェレンコフ光望遠鏡の視野を広げるため、我々は従来の Davies-Cotton 光学系に代わり Schwarzschild-Couder 光学系を用いた CTA 小口径・中口径望遠鏡の開発を行っている。視野 8–10° を約 0.1° の画素で観測には焦点面カメラに数千画素が必要となるため、小型の多チャンネル半導体光検出器と専用集積回路を用いたカメラの開発を進めている。本講演ではこれらカメラの開発状況について報告する。

, The Physical Society of Japan
Meeting Abstracts of the Physical Society of Japan, 2016

22aAT-5 CTA Report 106 : Camera test for the first unit of the CTA Large-Sized Telescope
Inome Y.; Ishio K.; Umetsu Y.; Ohoka H.; Okumura A.; Ono S.; Orito R.; Katagiri H.; Kamon H.; Kushida J.; Kubo H.; Gunji S.; Koyama S.; Konno Y.; Saito T.; Takahashi M.; Takeda J.; Tanaka M.; Tanigawa S.; Tsujimoto S.; Teshima M.; Tomono Y.; Nakajima D.; Nakamori T.; Nagayoshi T.; Nishijima K.; Hatanaka K.; Hayashida M.; Masuda S.; Matsuoka S.; Yamamoto T.; Yoshida T.; TAN DANG VIET; Hadasch Daniela; Mazin Daniel; CTA-Japan consortium, The Physical Society of Japan (JPS)
Meeting Abstracts of the Physical Society of Japan, 2016

21pCA-12 Development of a scintillator-based Compton camera for gamma-ray imaging under high dose-rate environments
Satoh W.; Katagiri H.; Itoh Y.; Uchida T.; Enomoto R.; Kagaya M.; Satoh K.; Takeda T.; Tanaka M.; Hanafusa R.; Hosokawa M.; Muraishi H.; Yoshida T.; Wakamatsu R.; Watanabe T.; Wada K.; Open-it consortium, The Physical Society of Japan (JPS)
Meeting Abstracts of the Physical Society of Japan, 2016

22aAT-6 CTA Report 107 : Performance Tests of segmented mirrors for the CTA Large-Sized Telescope
Cho Norihito; Hayashida Masaaki; Inada Tomohiro; Iwamura Yuki; Okumura Akira; Ono Sakiya; Kagaya Mika; Katagiri Hideaki; Kato Sho; Kishida Shu; Saito Takayuki; Shigenaka Akane; Chikawa Michiyuki; Teshima Masahiro; Nakajima Daisuke; Noda Koji; Hanabata Yoshitaka; Fukami Satoshi; Motohashi Daisuke; Yamamoto Tokonatsu; Yoshida Tatsuo; the CTA-Japan consortium, The Physical Society of Japan (JPS)
Meeting Abstracts of the Physical Society of Japan, 2016

CTA Report 115 : Software Development for Active Mirror Control system of CTA Large-Sized Telescope
Fukami Satoshi; Noda Koji; Hayashida Masaaki; Inada Tomohiro; Okumura Akira; Kagaya Mika; Katagiri Hideaki; Kuroda Hayato; Saito Takayuki; Shigenaka Akane; Chikawa Michiyuki; Teshima Masahiro; Nakajima Daisuke; Motohashi Daisuke; Yamamoto Tokonatsu; Yoshida Tatsuo; the CTA-Japan consortium,

CTA大口径望遠鏡には約47kgの球面分割鏡がおよそ200枚取り付けられる。主に自重により望遠鏡全体の向きに依存して構造体に歪みが発生し、分割鏡の方向が変化して信号光は正しく集光されない。そのため、各分割鏡に設置したカメラで光軸レーザーのスポットを常にモニターしてずれを検知し、分割鏡を支えるアクチュエータの長さを制御し方向を微調整する、Active Mirror Control (AMC) と呼ばれる手法が採用された。望遠鏡サイトに近い環境での試験を通じて、すでにこの手法による分割鏡の高精度補正の成功を確認している。本講演ではAMCシステムを外部PCからの動作を可能にするためにソフトウェアを改善し、実際の望遠鏡の運用時に向けて開発したシステムの現状を報告する。

, The Physical Society of Japan
Meeting Abstracts of the Physical Society of Japan, 2016

CTA Report 111: Evaluation results of 7-dynode PMTs for improvement of CTA Large-Sized Telescope
Takahashi M.; Nagayoshi T.; Ishio K.; Inome Y.; Ohoka H.; Okumura A.; Orito R.; Katagiri H.; Kishida S.; Kubo H.; Kushida J.; Gunji S.; Koyama S.; Konno Y.; Saito T.; Takeda J.; Tanaka M.; Tanigawa S.; Tsujimoto S.; Teshima M.; Terada Y.; Tomono Y.; Nakajima D.; Nakamori T.; Nishijima K.; Nozaki S.; Hayashida M.; Bamba A.; Masuda S.; Yamamoto T.; Yoshida T.; Tan Dang Viet; Hadasch Daniela; Mazin Daniel; CTA-Japan consortium,

CTA大口径望遠鏡はチェレンコフ光密度が低くなる数十GeVのガンマ線を観測するため、高感度かつ低バックグラウンドの光電子増倍管が求められる。2基目以降に向け浜松ホトニクス(株)と共同開発した R12992は、S/N比に影響するパルス幅がダイノードの段数を8段から7段とすることにより初号機用に比べ大きく改善された。また量子効率もピーク値で平均43%にまで上昇した。このR12992の諸特性を測定、評価した結果を報告する。

, The Physical Society of Japan
Meeting Abstracts of the Physical Society of Japan, 2016

CTA Report 112: Camera test for the first unit of CTA Large-Sized Telescope
Nozaki S.; Ishio K.; Inome Y.; Ohoka H.; Okumura A.; Orito R.; Katagiri H.; Kishida S.; Kubo H.; Kushida J.; Gunji S.; Koyama S.; Konno Y.; Saito T.; Takahashi M.; Takeda J.; Tanaka M.; Tanigawa S.; Tsujimoto S.; Teshima M.; Terada Y.; Tomono Y.; Nakajima D.; Nakamori T.; Nagayoshi T.; Nishijima K.; Hayashida M.; Bamba A.; Masuda S.; Yamamoto T.; Yoshida T.; Tan Dang Viet; Hadasch Daniela; Mazin Daniel; CTA-Japan Consortium; Ikeno M.; Uchida T.,

Cherenkov Telescope Array(CTA)計画は、口径の異なる複数の望遠鏡を用いて 20GeVから100TeV 以上のガンマ線を従来よりも10倍高い感度で全天観測する望遠鏡 建設計画である。我々は大口径望遠鏡搭載用カメラの試験・ 開発を行っている。本講演では、初号機で用いるPMT、 波形読出し回路それぞれ133本、19個のモジュールから成る試 験用ミニカメラの構成、動作試験の結果、 及び次号機での搭載に向けた、 新版の波形読出し回路基板の設計の概要、 開発状況について報告する。

, The Physical Society of Japan
Meeting Abstracts of the Physical Society of Japan, 2016

21pCA-13 Development of four channels high sensitivity survey meter capable of detecting arrival direction of gamma rays
Wakamatsu R.; Kagaya M.; Enomoto R.; Katagiri H.; Kanoh D.; Hosokawa S.; Itoh Y.; Uchida T.; Satoh K.; Satoh W.; Takeda T.; Tanaka M.; Muraishi H.; Hosokawa M.; Yoshida T.; Watanabe T.; Wada K.; Open-it consortium, The Physical Society of Japan (JPS)
Meeting Abstracts of the Physical Society of Japan, 2016

Optical Spectroscopic Observations of Gamma-Ray Blazar Candidates. VI. Further Observations from TNG, WHT, OAN, SOAR, and Magellan Telescopes
N. Alvarez Crespo; F. Massaro; D. Milisavljevic; M. Landoni; V. Chavushyan; V. Patino-Alvarez; N. Masetti; E. Jimenez-Bailon; J. Strader; L. Chomiuk; H. Katagiri; M. Kagaya; C. C. Cheung; A. Paggi; R. D'Abrusco; F. Ricci; F. La Franca; Howard A. Smith; G. Tosti, Blazars, one of the most extreme classes of active galaxies, constitute so far the largest known population of γ-ray sources, and their number is continuously growing in the Fermi catalogs. However, in the latest release of the Fermi catalog there is still a large fraction of sources that are classified as blazar candidates of uncertain type (BCUs) for which optical spectroscopic observations are necessary to confirm their nature and their associations. In addition, IOP PUBLISHING LTD
The Astronomical Journal, 2016, [Reviewed]

Development of a low-cost-high-sensitivity Compton camera using CsI (Tl) scintillators (gamma I)
M. Kagaya; H. Katagiri; R. Enomoto; R. Hanafusa; M. Hosokawa; Y. Itoh; H. Muraishi; K. Nakayama; K. Satoh; T. Takeda; M. M. Tanaka; T. Uchida; T. Watanabe; S. Yanagita; T. Yoshida; K. Umehara, We have developed a novel low-cost gamma-ray imaging Compton camera gamma I that has a high detection efficiency. Our motivation for the development of this detector was to measure the arrival directions of gamma rays produced by radioactive nuclides that were released by the Fukushima Daiichi nuclear power plant accident in 2011. The detector comprises two arrays of inorganic scintillation detectors, which act as a scatterer and an absorber. Each array has eight scintillation detectors, each comprising a large CsI (TI) scintillator cube of side 3.5 cm, which is inexpensive and has a good energy resolution. Energies deposited by the Compton scattered electrons and subsequent photoelectric absorption, measured by each scintillation counter, are used for image reconstruction. The angular resolution was found to be 3.5 after using an image-sharpening technique. With this angular resolution, we can resolve a 1 m(2) radiation hot spot that is located at a distance of 10 m from the detector with a wide field of view of 1 sr. Moreover, the detection efficiency 0.68 cps/MBq at 1 m for 662 keV (7.6 cps/mu Sv/h) is sufficient for measuring low-level contamination (i.e., less than 1 mu Sv/h) corresponding to typical values in large areas of eastern Japan. In addition to the laboratory tests, the imaging capability of our detector was verified in various regions with dose rates less than 1 mu Sv/h (e.g., Fukushima city). (C) 2015 Elsevier B.V. All rights reserved., ELSEVIER SCIENCE BV
NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT, Dec. 2015, [Reviewed]

CTA Contributions to the 34th International Cosmic Ray Conference (ICRC2015)
CTA Consortium, The; :; Abchiche, A.; Abeysekara, U.; Abril, Ó.; Acero, F.; Acharya, B. S.; Actis, M.; Agnetta, G.; Aguilar, J. A.; Aharonian, F.; Akhperjanian, A.; Albert, A.; Alcubierre, M.; Alfaro, R.; Aliu, E.; Allafort, A. J.; Allan, D.; Allekotte, I.; Aloisio, R.; Amans, J. -P.; Amato, E.; Ambrogi, L.; Ambrosi, G.; Ambrosio, M.; Anderson, J.; Anduze, M.; Angüner, E. O.; Antolini, E.; Antonelli, L. A.; Antonucci, M.; Antonuccio, V.; Antoranz, P.; Aramo, C.; Aravantinos, A.; Argan, A.; Armstrong, T.; Arnaldi, H.; Arnold, L.; Arrabito, L.; Arrieta, M.; Arrieta, M.; Asano, K.; Asorey, H. G.; Aune, T.; Singh, C. B.; Babic, A.; Backes, M.; Bais, A.; Bajtlik, S.; Balazs, C.; Balbo, M.; Balis, D.; Balkowski, C.; Ballester, O.; Ballet, J.; Balzer, A.; Bamba, A.; Bandiera, R.; Barber, A.; Barbier, C.; Barceló, M.; Barnacka, A.; Barres de Almeida, U.; Barrio, J. A.; Basso, S.; Bastieri, D.; Bauer, C.; Baushev, A.; Becciani, U.; Becherini, Y.; Becker Tjus, J.; Beckmann, V.; Bednarek, W.; Benbow, W.; Benedico Ventura, D.; Berdugo, J.; Berge, D.; Bernardini, E.; Bernhard, S.; Bernlöhr, K.; Bertucci, B.; Besel, M. -A.; Bhatt, N.; Bhattacharjee, P.; Bhattachryya, S.; Biasuzzi, B.; Bicknell, G.; Bigongiari, C.; Biland, A.; Billotta, S.; Bilnik, W.; Biondo, B.; Bird, T.; Birsin, E.; Bissaldi, E.; Biteau, J.; Bitossi, M.; Blanch Bigas, O.; Blasi, P.; Boehm, C.; Bogacz, L.; Bogdan, M.; Bohacova, M.; Boisson, C.; Boix Gargallo, J.; Bolmont, J.; Bonanno, G.; Bonardi, A.; Bonifacio, P.; Bonnoli, G.; Borkowski, J.; Bose, R.; Bosnjak, Z.; Bottani, A.; Böttcher, M.; Bousquet, J. -J.; Boutonnet, C.; Bouyjou, F.; Braiding, C.; Brandt, L.; Brau-Nogué, S.; Bregeon, J.; Bretz, T.; Briggs, M.; Brigida, M.; Bringmann, T.; Brisken, W.; Brocato, E.; Brook, P.; Brown, A. M.; Brun, P.; Brunetti, G.; Brunetti, L.; Bruno, P.; Bryan, M.; Buanes, T.; Bucciantini, N.; Buchholtz, G.; Buckley, J.; Bugaev, V.; Bühler, R.; Bulgarelli, A.; Bulik, T.; Burton, M.; Burtovoi, A.; Busetto, G.; Buson, S.; Buss, J.; Byrum, K.; Cameron, R.; Camprecios, J.; Canelli, F.; Canestrari, R.; Cantu, S.; Capalbi, M.; Capasso, M.; Capobianco, G.; Caraveo, P.; Cardenzana, J.; Carius, S.; Carlile, C.; Carmona, E.; Carosi, A.; Carosi, R.; Carr, J.; Carroll, M.; Carter, J.; Carton, P. -H.; Caruso, R.; Casandjian, J. -M.; Casanova, S.; Cascone, E.; Casiraghi, M.; Castellina, A.; Catalano, O.; Catalanotti, S.; Cavazzani, S.; Cazaux, S.; Cefalà, M.; Cerchiara, P.; Cereda, M.; Cerruti, M.; Chabanne, E.; Chadwick, P.; Champion, C.; Chaty, S.; Chaves, R.; Cheimets, P.; Chen, A.; Chen, X.; Chernyakova, M.; Chiappetti, L.; Chikawa, M.; Chinn, D.; Chitnis, V. R.; Cho, N.; Christov, A.; Chudoba, J.; Cieślar, M.; Cillis, A.; Ciocci, M. A.; Clay, R.; Cohen-Tanugi, J.; Colafrancesco, S.; Colin, P.; Colombo, E.; Colome, J.; Colonges, S.; Compin, M.; Conforti, V.; Connaughton, V.; Connell, S.; Conrad, J.; Contreras, J. L.; Coppi, P.; Corbel, S.; Coridian, J.; Corona, P.; Corti, D.; Cortina, J.; Cossio, L.; Costa, A.; Costantini, H.; Cotter, G.; Courty, B.; Covino, S.; Covone, G.; Crimi, G.; Criswell, S. J.; Crocker, R.; Croston, J.; Cusumano, G.; Da Vela, P.; Dale, Ø.; D'Ammando, F.; Dang, D.; Daniel, M.; Davids, I.; Dawson, B.; Dazzi, F.; de Aguiar Costa, B.; De Angelis, A.; de Araujo Cardoso, R. F.; De Caprio, V.; De Cesare, G.; De Franco, A.; De Frondat, F.; de Gouveia Dal Pino, E. M.; de la Calle, I.; De La Vega, G. A.; de los Reyes Lopez, R.; De Lotto, B.; De Luca, A.; de Mello Neto, J. R. T.; de Naurois, M.; de Oña Wilhelmi, E.; De Palma, F.; de Souza, V.; Decock, G.; Deil, C.; Del Santo, M.; Delagnes, E.; Deleglise, G.; Delgado, C.; della Volpe, D.; Deloye, P.; Depaola, G.; Detournay, M.; Dettlaff, A.; Di Girolamo, T.; Di Giulio, C.; Di Paola, A.; Di Pierro, F.; Di Sciascio, G.; Díaz, C.; Dick, J.; Dickinson, H.; Diebold, S.; Diez, V.; Digel, S.; Dipold, J.; Disset, G.; Distefano, A.; Djannati-Ataï, A.; Doert, M.; Dohmke, M.; Domainko, W.; Dominik, N.; Dominis Prester, D.; Donat, A.; Donnarumma, I.; Dorner, D.; Doro, M.; Dournaux, J. -L.; Doyle, K.; Drake, G.; Dravins, D.; Drury, L.; Dubus, G.; Dumas, D.; Dumm, J.; Durand, D.; D'Urso, D.; Dwarkadas, V.; Dyks, J.; Dyrda, M.; Ebr, J.; Echaniz, J. C.; Edy, E.; Egberts, K.; Egberts, K.; Eger, P.; Einecke, S.; Eisch, J.; Eisenkolb, F.; Eleftheriadis, C.; Elsässer, D.; Emmanoulopoulos, D.; Engelbrecht, C.; Engelhaupt, D.; Ernenwein, J. -P.; Errando, M.; Eschbach, S.; Etchegoyen, A.; Evans, P.; Fairbairn, M.; Falcone, A.; Fantinel, D.; Farakos, K.; Farnier, C.; Farrell, E.; Farrell, S.; Fasola, G.; Fegan, S.; Feinstein, F.; Ferenc, D.; Fernandez, A.; Fernandez-Alonso, M.; Ferreira, O.; Fesquet, M.; Fetfatzis, P.; Fiasson, A.; Filipčič, A.; Filipovic, M.; Fink, D.; Finley, C.; Finley, J. P.; Finoguenov, A.; Fioretti, V.; Fiorini, M.; Firpo Curcoll, R.; Fleischhack, H.; Flores, H.; Florin, D.; Föhr, C.; Fokitis, E.; Font, L.; Fontaine, G.; Fontes, B.; Forest, F.; Fornasa, M.; Förster, A.; Fortin, P.; Fortson, L.; Fouque, N.; Franckowiak, A.; Franco, F. J.; Frankowski, A.; Frega, N.; Freire Mota Albuquerque, I.; Freixas Coromina, L.; Fresnillo, L.; Fruck, C.; Fuessling, M.; Fugazza, D.; Fujita, Y.; Fukami, S.; Fukazawa, Y.; Fukuda, T.; Fukui, Y.; Funk, S.; Gäbele, W.; Gabici, S.; Gadola, A.; Galante, N.; Gall, D. D.; Gallant, Y.; Galloway, D.; Gallozzi, S.; Gao, S.; Garcia, B.; García Gil, R.; Garcia López, R.; Garczarczyk, M.; Gardiol, D.; Gargano, C.; Gargano, F.; Garozzo, S.; Garrecht, F.; Garrido, D.; Garrido, L.; Gascon, D.; Gaskins, J.; Gaudemard, J.; Gaug, M.; Gaweda, J.; Geffroy, N.; Gérard, L.; Ghalumyan, A.; Ghedina, A.; Ghigo, M.; Ghislain, P.; Giannakaki, E.; Gianotti, F.; Giarrusso, S.; Giavitto, G.; Giebels, B.; Giglietto, N.; Gika, V.; Gimenes, R.; Giomi, M.; Giommi, P.; Giordano, F.; Giovannini, G.; Giro, E.; Giroletti, M.; Giuliani, A.; Glicenstein, J. -F.; Godinovic, N.; Goldoni, P.; Gomez Berisso, M.; Gomez Vargas, G. A.; Gonzalez, M. M.; González, A.; González, F.; González Muñoz, A.; Gothe, K. S.; Gotz, D.; Grabarczyk, T.; Graciani, R.; Grandi, P.; Grañena, F.; Granot, J.; Grasseau, G.; Gredig, R.; Green, A. J.; Green, A. M.; Greenshaw, T.; Grenier, I.; Grillo, A.; Grondin, M. -H.; Grube, J.; Grudzinska, M.; Grygorczuk, J.; Guarino, V.; Guberman, D.; Gunji, S.; Gyuk, G.; Hadasch, D.; Hagedorn, A.; Hahn, J.; Hakansson, N.; Hamer Heras, N.; Hanabata, Y.; Hara, S.; Hardcastle, M. J.; Harris, J.; Hassan, T.; Hatanaka, K.; Haubold, T.; Haupt, A.; Hayakawa, T.; Hayashida, M.; Heller, M.; Heller, R.; Henault, F.; Henri, G.; Hermann, G.; Hermel, R.; Herrera Llorente, J.; Herrero, A.; Hervet, O.; Hidaka, N.; Hinton, J.; Hirai, W.; Hirotani, K.; Hoard, D.; Hoffmann, D.; Hofmann, W.; Hofverberg, P.; Holch, T.; Holder, J.; Hooper, S.; Horan, D.; Hörandel, J. R.; Hormigos, S.; Horns, D.; Hose, J.; Houles, J.; Hovatta, T.; Hrabovsky, M.; Hrupec, D.; Huet, J. -M.; Hütten, M.; Humensky, T. B.; Huovelin, J.; Huppert, J. -F.; Iacovacci, M.; Ibarra, A.; Idźkowski, B.; Ikawa, D.; Illa, J. M.; Impiombato, D.; Incorvaia, S.; Inome, Y.; Inoue, S.; Inoue, T.; Inoue, Y.; Iocco, F.; Ioka, K.; Iori, M.; Ishio, K.; Israel, G. L.; Jablonski, C.; Jacholkowska, A.; Jacquemier, J.; Jamrozy, M.; Janecek, P.; Janiak, M.; Jankowsky, F.; Jean, P.; Jeanney, C.; Jegouzo, I.; Jenke, P.; Jimenez, J. J.; Jingo, M.; Jingo, M.; Jocou, L.; Jogler, T.; Johnson, C. A.; Journet, L.; Juffroy, C.; Jung, I.; Kaaret, P. E.; Kagaya, M.; Kakuwa, J.; Kalekin, O.; Kalkuhl, C.; Kankanyan, R.; Karastergiou, A.; Kärcher, K.; Karczewski, M.; Karkar, S.; Karn, P.; Kasperek, J.; Katagiri, H.; Kataoka, J.; Katarzyński, K.; Katz, U.; Kaufmann, S.; Kawanaka, N.; Kawashima, T.; Kazanas, D.; Kelley-Hoskins, N.; Kellner-Leidel, B.; Kendziorra, E.; Kersten, J.; Khélifi, B.; Kieda, D. B.; Kihm, T.; Kisaka, S.; Kissmann, R.; Klepser, S.; Kluźniak, W.; Knapen, J.; Knapp, J.; Knödlseder, J.; Köck, F.; Kocot, J.; Kodakkadan, A.; Kodani, K.; Kohri, K.; Kojima, T.; Kokkotas, K.; Kolitzus, D.; Komin, N.; Kominis, I.; Konno, Y.; Kosack, K.; Koss, G.; Koul, R.; Kowal, G.; Koyama, S.; Kozioł, J.; Kraus, M.; Krause, J.; Krause, M.; Krawzcynski, H.; Krennrich, F.; Kretzschmann, A.; Kruger, P.; Kubo, H.; Kudryavtsev, V.; Kukec Mezek, G.; Kushida, J.; Kuznetsov, A.; La Barbera, A.; La Palombara, N.; La Parola, V.; La Rosa, G.; Laffon, H.; Lagadec, T.; Lahmann, R.; Lalik, K.; Lamanna, G.; Landriu, D.; Landt, H.; Lang, R. G.; Languignon, D.; Lapington, J.; Laporte, P.; Latovski, N.; Law-Green, D.; Le Fèvre, J. -P.; Le Flour, T.; Le Sidaner, P.; Lee, S. -H.; Lee, W. H.; Leffhalm, K.; Leich, H.; Leigui de Oliveira, M. A.; Lelas, D.; Lemière, A.; Lemoine-Goumard, M.; Lenain, J. -P.; Leonard, R.; Leoni, R.; Lessio, L.; Leto, G.; Leveque, A.; Lieunard, B.; Limon, M.; Lindemann, R.; Lindfors, E.; Liolios, A.; Lipniacka, A.; Lockart, H.; Lohse, T.; Loiseau, D.; Łokas, E.; Lombardi, S.; Longo, F.; Longo, G.; Lopatin, A.; Lopez, M.; López-Coto, R.; López-Oramas, A.; Loreggia, D.; Louge, T.; Louis, F.; Lu, C. -C.; Lucarelli, F.; Lucchesi, D.; Lüdecke, H.; Luque-Escamilla, P. L.; Luz, O.; Lyard, E.; Maccarone, M. C.; Maccarone, T. J.; Mach, E.; Madejski, G. M.; Madonna, A.; Mahabir, M.; Maier, G.; Majumdar, P.; Makariev, M.; Malaguti, G.; Malaspina, G.; Mallot, A. K.; Maltezos, S.; Mancilla, A.; Mandat, D.; Maneva, G.; Manigot, P.; Mankushiyil, N.; Mannheim, K.; Maragos, N.; Marano, D.; Marchegiani, P.; Marcomini, J. A.; Marcowith, A.; Mariotti, M.; Marisaldi, M.; Markoff, S.; Marszałek, A.; Martens, C.; Martí, J.; Martin, J. -M.; Martin, P.; Martínez, G.; Martínez, M.; Martínez, O.; Marx, R.; Massimino, P.; Mastichiadis, A.; Mastroianni, S.; Mastropietro, M.; Masuda, S.; Matsumoto, H.; Matsuoka, S.; Mattiazzo, S.; Maurin, G.; Maxted, N.; Maya, J.; Mayer, M.; Mazin, D.; Mazureau, E.; Mazziotta, M. N.; Mc Comb, L.; McCann, A.; McCubbin, N.; McHardy, I.; McKay, R.; McKinney, K.; Meagher, K.; Medina, C.; Mehrez, F.; Melioli, C.; Melkumyan, D.; Melo, D.; Melse, T.; Mereghetti, S.; Mertsch, P.; Meyer, M.; Meyrelles, J. L., jr; Miccichè, A.; Michałowski, J.; Micolon, P.; Mientjes, P.; Mignot, S.; Mihailidis, A.; Mineo, T.; Minuti, M.; Mirabal, N.; Mirabel, F.; Miranda, J. M.; Mirzoyan, R.; Mistò, A.; Mitchell, A.; Mizuno, T.; Moderski, R.; Mognet, I.; Mohammed, M.; Moharana, R.; Molinari, E.; Monmarthe, E.; Monnier, G.; Montaruli, T.; Monte, C.; Monteiro, I.; Moore, P.; Moralejo Olaizola, A.; Morello, C.; Moretti, E.; Mori, K.; Morlino, G.; Morselli, A.; Mottez, F.; Moudden, Y.; Moulin, E.; Mrusek, I.; Mueller, S.; Mukherjee, R.; Munar-Adrover, P.; Mundell, C.; Muraishi, H.; Murase, K.; Muronga, A.; Murphy, A.; Nagataki, S.; Nagayoshi, T.; Nagesh, B. K.; Naito, T.; Nakajima, D.; Nakamori, T.; Nakayama, K.; Naumann, D.; Nayman, P.; Nellen, L.; Nemmen, R.; Neronov, A.; Neustroev, V.; Neyroud, N.; Nguyen, T.; Nicastro, L.; Nicolau-Kukliński, J.; Niederwanger, F.; Niedźwiecki, A.; Niemiec, J.; Nieto, D.; Nievas, M.; Nikolaidis, A.; Nishijima, K.; Nishikawa, K. -I.; Noda, K.; Nogues, L.; Nolan, S.; Northrop, R.; Nosek, D.; Nozka, L.; Nunio, F.; Oakes, L.; O'Brien, P.; Occhipinti, G.; O'Faolain de Bhroithe, A.; Ogino, M.; Ohira, Y.; Ohishi, M.; Ohm, S.; Ohoka, H.; Okumura, A.; Olive, J. -F.; Olszowski, D.; Ong, R. A.; Ono, S.; Orienti, M.; Orito, R.; Orlati, A.; Orlati, A.; Osborne, J.; Ostrowski, M.; Otero, L. A.; Ottaway, D.; Otte, N.; Oya, I.; Ozieblo, A.; Padovani, M.; Pagano, I.; Paiano, S.; Paizis, A.; Palacio, J.; Palatka, M.; Pallotta, J.; Panagiotidis, K.; Panazol, J. -L.; Paneque, D.; Panter, M.; Panzera, M. R.; Paoletti, R.; Paolillo, M.; Papayannis, A.; Papyan, G.; Paravac, A.; Paredes, J. M.; Pareschi, G.; Park, N.; Parsons, D.; Paśko, P.; Pavy, S.; Arribas, M. Paz; Pech, M.; Peck, A.; Pedaletti, G.; Peet, S.; Pelassa, V.; Pelat, D.; Peres, C.; Perez, M. d. C.; Perri, L.; Persic, M.; Petrashyk, A.; Petrucci, P. -O.; Peyaud, B.; Pfeifer, M.; Pfeiffer, G.; Piano, G.; Pichel, A.; Pieloth, D.; Pierbattista, M.; Pierre, E.; Pinto de Pinho, F.; García, C. Pio; Piret, Y.; Pita, S.; Planes, A.; Platino, M.; Platos, Ł.; Platzer, R.; Podkladkin, S.; Pogosyan, L.; Pohl, M.; Poinsignon, P.; Ponz, J. D.; Porcelli, A.; Potter, W.; Poulios, S.; Poutanen, J.; Prandini, E.; Prast, J.; Preece, R.; Profeti, F.; Prokhorov, D.; Prokoph, H.; Prouza, M.; Proyetti, M.; Pruchniewicz, R.; Pueschel, E.; Pühlhofer, G.; Puljak, I.; Punch, M.; Pyzioł, R.; Queiroz, F.; Quel, E. J.; Quinn, J.; Quirrenbach, A.; Racero, E.; Räck, T.; Rafalski, J.; Rafighi, I.; Rainò, S.; Rajda, P. J.; Rameez, M.; Rando, R.; Rannot, R. C.; Rataj, M.; Rateau, S.; Ravel, T.; Ravignani, D.; Razzaque, S.; Reardon, P.; Reimann, O.; Reimer, A.; Reimer, O.; Reitberger, K.; Renaud, M.; Renner, S.; Reposeur, T.; Rettig, R.; Reville, B.; Rhode, W.; Ribeiro, D.; Ribó, M.; Richards, G.; Richer, M. G.; Rico, J.; Ridky, J.; Rieger, F.; Ringegni, P.; Ristori, P. R.; Rivière, A.; Rivoire, S.; Roache, E.; Rodeghiero, G.; Rodriguez, J.; Rodriguez Fernandez, G.; Rodríguez Vázquez, J. J.; Rogers, T.; Rojas, G.; Romano, P.; Romay Rodriguez, M. P.; Romeo, G.; Romero, G. E.; Roncadelli, M.; Rose, J.; Rosen, S.; Rosier Lees, S.; Ross, D.; Rossiter, P.; Rouaix, G.; Rousselle, J.; Rovero, A. C.; Rowell, G.; Roy, F.; Royer, S.; Różańska, A.; Rudak, B.; Rugliancich, A.; Rulten, C.; Rupiński, M.; Russo, F.; Rutkowski, K.; Saavedra, O.; Sabatini, S.; Sacco, B.; Saemann, E. O.; Saggion, A.; Saha, L.; Sahakian, V.; Saito, K.; Saito, T.; Sakaki, N.; Salega, M.; Salek, D.; Salgado, J.; Salini, A.; Sanchez, D.; Sanchez, F.; Sanchez-Conde, M.; Sandaker, H.; Sandoval, A.; Sangiorgi, P.; Sanguillon, M.; Sano, H.; Santander, M.; Santangelo, A.; Santos, E. M.; Santos-Lima, R.; Sanuy, A.; Sapozhnikov, L.; Sarkar, S.; Satalecka, K.; Savalle, R.; Sawada, M.; Sayède, F.; Schafer, J.; Schanne, S.; Schanz, T.; Schioppa, E. J.; Schlenstedt, S.; Schlickeiser, R.; Schmidt, T.; Schmoll, J.; Schneider, M.; Schovanek, P.; Schubert, A.; Schultz, C.; Schultze, J.; Schulz, A.; Schulz, S.; Schure, K.; Schussler, F.; Schwab, T.; Schwanke, U.; Schwarz, J.; Schweizer, T.; Schwemmer, S.; Schwendicke, U.; Schwerdt, C.; Segreto, A.; Seiradakis, J. -H.; Sembroski, G. H.; Semikoz, D.; Serre, N.; Servillat, M.; Seweryn, K.; Shafi, N.; Sharma, M.; Shayduk, M.; Shellard, R. C.; Shibata, T.; Shiningayamwe Pandeni, K.; Shukla, A.; Shum, E.; Sidoli, L.; Sidz, M.; Sieiro, J.; Siejkowski, H.; Silk, J.; Sillanpää, A.; Simone, D.; Singh, B. B.; Sinha, A.; Sironi, G.; Sitarek, J.; Sizun, P.; Slyusar, V.; Smith, A.; Smith, J.; Sobczyńska, D.; Sol, H.; Sottile, G.; Sowiński, M.; Spanier, F.; Spengler, G.; Spiga, D.; Stadler, R.; Stahl, O.; Stamatescu, V.; Stamerra, A.; Stanič, S.; Starling, R.; Stawarz, Ł.; Steenkamp, R.; Stefanik, S.; Stegmann, C.; Steiner, S.; Stella, C.; Stergioulas, N.; Sternberger, R.; Sterzel, M.; Stevenson, B.; Stinzing, F.; Stodulska, M.; Stodulski, M.; Stolarczyk, T.; Straumann, U.; Strazzeri, E.; Stringhetti, L.; Strzys, M.; Stuik, R.; Sulanke, K. -H.; Supanitsky, A. D.; Suric, T.; Sushch, I.; Sutcliffe, P.; Sykes, J.; Szanecki, M.; Szepieniec, T.; Szwarnog, P.; Tacchini, A.; Tachihara, K.; Tagliaferri, G.; Tajima, H.; Takahashi, H.; Takahashi, K.; Takahashi, M.; Takalo, L.; Takami, H.; Talbot, G.; Tammi, J.; Tanaka, M.; Tanaka, S.; Tanaka, T.; Tanaka, Y.; Tanci, C.; Tarantino, E.; Tavani, M.; Tavecchio, F.; Tavernet, J. -P.; Tayabaly, K.; Tejedor, L. A.; Telezhinsky, I.; Temme, F.; Temnikov, P.; Tenzer, C.; Terada, Y.; Terrier, R.; Tescaro, D.; Teshima, M.; Testa, V.; Tezier, D.; Thayer, J.; Thomas, V.; Thornhill, J.; Thuermann, D.; Tibaldo, L.; Tibolla, O.; Tiengo, A.; Tijsseling, G.; Timpanaro, M. C.; Tluczykont, M.; Todero Peixoto, C. J.; Tokanai, F.; Tokarz, M.; Toma, K.; Toma, K.; Tomastik, J.; Tomono, Y.; Tonachini, A.; Tonev, D.; Torii, K.; Tornikoski, M.; Torres, D. F.; Torres, M.; Torresi, E.; Toscano, S.; Toso, G.; Tosti, G.; Totani, T.; Tothill, N.; Toussenel, F.; Tovmassian, G.; Townsley, C.; Toyama, T.; Travnicek, P.; Trifoglio, M.; Troyano Pujadas, I.; Troyano Pujadas, I.; Trzeciak, M.; Tsinganos, K.; Tsubone, Y.; Tsuchiya, Y.; Tsujimoto, S.; Tsuru, T.; Uchiyama, Y.; Umana, G.; Umetsu, Y.; Underwood, C.; Upadhya, S. S.; Uslenghi, M.; Vagnetti, F.; Valdes-Galicia, J.; Vallania, P.; Vallejo, G.; Valore, L.; van Driel, W.; van Eldik, C.; van Soelen, B.; Vandenbroucke, J.; Vanderwalt, J.; Vasileiadis, G.; Vassiliev, V.; Vázquez Acosta, M. L.; Vecchi, M.; Vegas, I.; Veitch, P.; Venema, L.; Venter, C.; Vercellone, S.; Vergani, S.; Verma, K.; Verzi, V.; Vettolani, G. P.; Viana, A.; Vicha, J.; Videla, M.; Vigorito, C.; Vincent, P.; Vincent, S.; Vink, J.; Vittorini, V.; Vlahakis, N.; Vlahos, L.; Voelk, H.; Vogler, P.; Voisin, V.; Vollhardt, A.; Volpicelli, A.; Vorobiov, S.; Vovk, I.; Vu, L. V.; Wagner, R.; Wagner, R. M.; Wagner, R. G.; Wagner, S. J.; Wakely, S. P.; Walter, R.; Walther, T.; Ward, J. E.; Ward, M.; Warda, K.; Warwick, R.; Wassberg, S.; Watson, J.; Wawer, P.; Wawrzaszek, R.; Webb, N.; Wegner, P.; Weinstein, A.; Weitzel, Q.; Wells, R.; Werner, F.; Werner, M.; Wetteskind, H.; White, M.; White, R.; Więcek, M.; Wierzcholska, A.; Wiesand, S.; Wijers, R.; Wild, N.; Wilhelm, A.; Wilkinson, M.; Will, M.; Williams, D. A.; Williams, J. T.; Willingale, R.; Winde, M.; Winiarski, K.; Winkler, H.; Wischnewski, R.; Wojcik, P.; Wolf, D.; Wood, M.; Wörnlein, A.; Wu, E.; Wu, T.; Yadav, K. K.; Yamamoto, H.; Yamamoto, T.; Yamazaki, R.; Yanagita, S.; Yang, L.; Yebras, J. M.; Yelos, D.; Yeung, W.; Yoshida, A.; Yoshida, T.; Yoshiike, S.; Yoshikoshi, T.; Yu, P.; Zabalza, V.; Zabalza, V.; Zacharias, M.; Zaharijas, G.; Zajczyk, A.; Zampieri, L.; Zandanel, F.; Zanin, R.; Zanmar Sanchez, R.; Zavrtanik, D.; Zavrtanik, M.; Zdziarski, A.; Zech, A.; Zechlin, H.; Zhao, A.; Ziegler, A.; Ziemann, J.; Ziętara, K.; Ziółkowski, J.; Zitelli, V.; Zoli, A.; Zurbach, C.; Żychowski, P., List of contributions from the CTA Consortium presented at the 34th International Cosmic Ray Conference, 30 July - 6 August 2015, The Hague, The Netherlands...., arXiv e-prints
Aug. 2015

Erratum: "The Second Catalog of Active Galactic Nuclei Detected by the Fermi Large Area Telescope'' (2011, ApJ, 743, 171)
Ackermann, M.; Ajello, M.; Allafort, A.; Antolini, E.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bottacini, E.; Bouvier, A.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Charles, E.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Costamante, L.; Cutini, S.; de Angelis, A.; de Palma, F.; Dermer, C. D.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Escande, L.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Finke, J.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grove, J. E.; Guiriec, S.; Gustafsson, M.; Hadasch, D.; Hayashida, M.; Hays, E.; Healey, S. E.; Horan, D.; Hou, X.; Hughes, R. E.; Iafrate, G.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Larsson, S.; Latronico, L.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Naumann-Godo, M.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orienti, M.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Parent, D.; Pesce-Rollins, M.; Pierbattista, M.; Piranomonte, S.; Piron, F.; Pivato, G.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Razzaque, S.; Reimer, A.; Reimer, O.; Ritz, S.; Rochester, L. S.; Romani, R. W.; Roth, M.; Sanchez, D. A.; Sbarra, C.; Scargle, J. D.; Schalk, T. L.; SGRO, C.; Shaw, M. S.; Siskind, E. J.; Spandre, G.; Spinelli, P.; Strong, A. W.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Tinivella, M.; Torres, D. F.; Tosti, G.; Troja, E.; Uchiyama, Y.; Vandenbroucke, J.; Vasileiou, V.; Vianello, G.; Vitale, V.; Waite, A. P.; Wallace, E.; Wang, P.; Winer, B. L.; Wood, D. L.; Wood, K. S.; Zimmer, S., ...
The Astrophysical Journal, Jun. 2015

Constraints on acceleration of ultra-high-energy cosmic rays in fermi gamma-ray sources　　　　　　　　　　　　　　　
Mika Kagaya; Hideaki Katagiri; Tatsuo Yoshida, We investigate the candidates of accelerator of ultra-high-energy cosmic rays (UHECRs) using the multi-wavelength spectral energy distributions, and discuss about the ability to accelerate UHECRs and constrain their physical conditions (acceleration site and size). The current experimental statistics of UHECRs is not sufficient for identification of the sources, although a spatial correlation between the arrival directions of UHECRs and nearby active galactic nuclei (AGNs) has been discussed using the data of the Pierre Auger Observatory and the Telescope Array. Some authors have discussed about the acceleration of UHECRs using various methods. Among them, Pe'er and Loeb (2012) derived constraints on the ability of AGNs to produce UHECRs by using observational quantities which are synchrotron peak luminosity and the peak flux ratio of inverse Compton scattering to synchrotron emission. For adopting this method, we need data of gammaray observation to determine the peak flux for high-energy region due to inverse Compton scattering. Thus, we focused on the Fermi Large Area Telescope gamma-ray sources. We investigated a spatial correlation between AGNs and the arrival directions of UHECRs, and we selected six AGNs as candidates of accelerator of UHECRs. We analyzed their spectral energy distributions by using multi-wavelength archival observational data. By introducing the constraints of Pe'er and Loeb (2012), we evaluate the physical conditions in the acceleration regions of these six AGNs and discuss whether they can accelerate to UHECRs. From the analysis, we found that three AGNs have ability to accelerate UHE protons to UHECRs in the AGN cores. Furthermore, we constrained the minimum size of the acceleration region for each source when UHE particles are accelerated in the AGN lobes. If UHE protons are accelerated, a few kpc-100 kpc are required as the minimum acceleration size. In the case of acceleration of heavy nucleus, the heavy particles can be accelerated in the AGN lobes if the size is larger than a few kpc. In this paper, we show that we achieved to establish a test method for individual candidate sources of acceleration of UHECRs., Proceedings of Science (PoS)
Proceedings of Science, 2015

Development of the photomultiplier tube readout system for the first large-sized telescope of the cherenkov telescope array　　　　　　　　　　　　　　　
Shu Masuda; Yusuke Konno; Juan Abel Barrio; Oscar Blanch Bigas; Carlos Delgado; Lluís Freixas Coromina; Shuichi Gunji; Daniela Hadasch; Kenichiro Hatanaka; Masahiro Ikeno; Jose Maria Illa Laguna; Yusuke Inome; Kazuma Ishio; Hideaki Katagiri; Hidetoshi Kubo; Gustavo Martínez; Daniel Mazin; Daisuke Nakajima; Takeshi Nakamori; Hideyuki Ohoka; Riccardo Paoletti; Stefan Ritt; Andrea Rugliancich; Takayuki Saito; Karl-Heinz Sulanke; Junki Takeda; Manobu Tanaka; Shunsuke Tanigawa; Luis Angel Tejedor; Masahiro Teshima; Yugo Tsuchiya; Tomohisa Uchida; Tokonatsu Yamamoto, The Cherenkov Telescope Array (CTA) is the next generation ground-based very high energy gamma-ray observatory. The Large-Sized Telescope (LST) of CTA targets 20 GeV - 1 TeV gamma rays and has 1855 photomultiplier tubes (PMTs) installed in the focal plane camera. With the 23 m mirror dish, the night sky background (NSB) rate amounts to several hundreds MHz per pixel. In order to record clean images of gamma-ray showers with minimal NSB contamination, a fast sampling of the signal waveform is required so that the signal integration time can be as short as the Cherenkov light flash duration (a few ns). We have developed a readout board which samples waveforms of seven PMTs per board at a GHz rate. Since a GHz FADC has a high power consumption, leading to large heat dissipation, we adopted the analog memory ASIC 'DRS4'. The sampler has 1024 capacitors per channel and can sample the waveform at a GHz rate. Four channels of a chip are cascaded to obtain deeper sampling depth with 4096 capacitors. After a trigger is generated in a mezzanine on the board, the waveform stored in the capacitor array is subsequently digitized with a low speed (33 MHz) ADC and transferred via the FPGAbased Gigabit Ethernet to a data acquisition system. Both a low power consumption (2.64 W per channel) and high speed sampling with a bandwidth of >
300 MHz have been achieved. In addition, in order to increase the dynamic range of the readout we adopted a two gain system achieving from 0.2 up to 2000 photoelectrons in total. We finalized the board design for the first LST and proceeded to mass production. Performance of produced boards are being checked with a series of quality control (QC) tests. We report the readout board specifications and QC results., Proceedings of Science (PoS)
Proceedings of Science, 2015

Simulating cherenkov telescope array observation of RX J1713.7-3946
Nakamori T; Katagiri H; Sano H; Yamazaki R; Ohira Y; Bamba A; Fukui Y; Mori K; Lee S.-H; Fujita Y; Tajima H; Inoue T; Gunji S; Hanabata Y; Hayashida M; Kubo H; Kushida J; Inoue S; Ioka K; Kohri K; Murase K; Nagataki S; Naito T; Okumura A; Saito T; Sawada M; Tanaka T; Terada Y; Uchiyama Y; Yanagita S; Yoshida T; Yoshikoshi T
Proceedings of Science, 2015, [Reviewed]

27pSJ-1 CTA Report 96 : General Report on the CTA Project
Teshima M.; Tan Dang Viet; Hadasch Daniela; Mazin Daniel; CTA Japan Collaboration, The Physical Society of Japan (JPS)
Meeting Abstracts of the Physical Society of Japan, 2015

27pSJ-3 CTA Report 98 : Result of characterization of PMTs for the first Large-Sized Telescope of CTA
Takahashi Mitsunari; Inome Yusuke; Umetsu Yohei; Ohoka Hideyuki; Orito Reiko; Katagiri Hideaki; Kushida Junko; Kubo Hidetoshi; Gunji Shuichi; Koyama Shu; Sawada Makoto; Tsujimoto Shimpei; Teshima Masahiro; Terada Yukikatsu; Tomono Yayoi; Nakajima Daisuke; Nagayoshi Tsutomu; Nishijima Kyoshi; Hayashida Masaaki; Bamba Aya; Matsuoka Shunsuke; Yamamoto Tokonatsu; CTA-Japan Consortium, The Physical Society of Japan (JPS)
Meeting Abstracts of the Physical Society of Japan, 2015

27pSJ-4 CTA Report 99 : Development of the readout system to be installed on the first Large Sized Telescope of CTA
Tanigawa S.; Kubo H.; Saito T.; Konno Y.; Hatanaka K.; Masuda S.; Gunji S.; Takeda J.; Nakamori T.; Ishio K.; Ohka H.; Teshima M.; Nakajima D.; Hadasch Daniela; Hayashida M.; Mazin Daniel; Orito R.; Katagiri H.; Tanaka M.; Yamamoto T.; CTA-Japan Consortium, The Physical Society of Japan
Meeting Abstracts of the Physical Society of Japan, 2015

28pSN-3 Evaluation of the angular resolution of a Compton camera by the energy resolutions of inorganic scintillators
Satoh W.; Katagiri H.; Itoh Y.; Uchida T.; Enomoto R.; Kagaya M.; Satoh K.; Takeda T.; Tanaka M.; Hanafusa R.; Hosokawa M.; Muraishi H.; Yoshida T.; Wakamatsu R.; Watanabe T.; Wada K., The Physical Society of Japan (JPS)
Meeting Abstracts of the Physical Society of Japan, 2015

27pSJ-6 CTA Report 101 : Operation Tests with wireless connection for Active Mirror Control software of CTA Large-Sized Telescope
Fukami Satoshi; Hayashida Masaaki; Noda Koji; Inada Tomohiro; Iwamura Yuki; Okumura Akira; Ono Sakiya; Kagaya Mika; Katagiri Hideaki; Kato Sho; Kishida Shu; Saito Takayuki; Shigenaka Akane; Chikawa Michiyuki; Cho Norihito; Teshima Masahiro; Nakajima Daisuke; Hanabata Yoshitaka; Motohashi Daisuke; Yamamoto Tokonatsu; Yoshida Tatsuo; CTA-Japan consortium, The Physical Society of Japan (JPS)
Meeting Abstracts of the Physical Society of Japan, 2015

27pSJ-5 CTA Report 100 : Mass production and performance evaluation of lightguides for the first model of the CTA Large-Sized Telescope
Ono Sakiya; Okumura Akira; Hayashida Masaaki; Katagiri Hideaki; Inada Tomohiro; Iwamura Yuki; Kagaya Mika; Kishida Shu; Saito Takayuki; Shigenaka Akane; Chikawa Michiyuki; Cho Norihito; Teshima Masahiro; Nakajima Daisuke; Noda Koji; Hanabata Yoshitaka; Fukami Satoshi; Motohashi Daisuke; Yamamoto Tokonatsu; Yoshida Tatsuo; CTA-Japan Consortium, The Physical Society of Japan (JPS)
Meeting Abstracts of the Physical Society of Japan, 2015

21pDD-8 CTA Report 93 : Development of AMC system for CTA Large-Sized Telescope and optical tests with Test Structure
Fukami Satoshi; Kojima Takumi; Noda Koji; Teshima Masahiro; Ogino Momoko; Okumura Akira; Ono Sakiya; Kagaya Mika; Katagiri Hideaki; Saito Koji; Saito Takayuki; Chikawa Michiyuki; Cho Norihito; Nakajima Daisuke; Hanabata Yoshitaka; Hayashida Masaaki; Yanagita Shohei; Yamamoto Tokonatsu; Yoshida Tatsuo; CTA-Japan consortium, The Physical Society of Japan (JPS)
Meeting Abstracts of the Physical Society of Japan, 2015

21pDD-9 CTA Report 94 : Development of the central CCD pixel for the CTA Large-sized telescopes
Saito T.; Ogino M.; Okumura A.; Ono S.; Kagaya M.; Katagiri H.; Kojima T.; Saito K.; Chikawa M.; Cho N.; Teshima M.; Nakajima D.; Noda K.; Hayashida M.; Hanabata Y.; Fukami S.; Yanagita S.; Yamamoto T.; Yoshida R., The Physical Society of Japan (JPS)
Meeting Abstracts of the Physical Society of Japan, 2015

21pDD-7 CTA Report 92 : Development of Lightguides for the first model of the CTA Large-Sized Telescope
Ono Sakiya; Okumura Akira; Hayashida Masaaki; Katagiri Hideaki; Ogino Momoko; Kagaya Mika; Kojima Takumi; Saito Koji; Saito Takayuki; Chikawa Michiyuki; Cho Norihito; Teshima Masahiro; Nakajima Daisuke; Noda Koji; Hanabata Yoshitaka; Fukami Satoshi; Yanagita Shohei; Yamamoto Tokonatsu; Yoshida Tatsuo; CTA Consortium, The Physical Society of Japan (JPS)
Meeting Abstracts of the Physical Society of Japan, 2015

27pSJ-2 CTA Report 97 : Monte Carlo simulation study for comic-ray chemical composition measurement using direct Cherenkov photons (III)
Ohishi Michiko; Ikeno Yuhei; Ishio Kazuma; Inada Tomohiro; Okumura Akira; Katagiri Hideaki; Kushida Junko; Gunji Shuichi; Saito Takayuki; Sakaki Naoto; Tan Dang Viet; Nagayoshi Tsutomu; Nishijima Kyoshi; Hirai Wataru; Masuda Shu; Yoshikoshi Takanori; Yoshida Tatsuo; CTA-Japan Consortium, The Physical Society of Japan (JPS)
Meeting Abstracts of the Physical Society of Japan, 2015

21pDD-2 CTA Report 87 : Evaluation of CTA Large-Sized telescope optics by an air-shower simulation
Ogino M.; Ishio K.; Ohishi M.; Okumura A.; Ono S.; Kagaya M.; Katagiri H.; Kushida J.; Gunji S.; Kojima T.; Saito K.; Saito T.; Sakai N.; Chilawa M.; Cho N.; Teshima M.; Nakajima D.; Nishijima K.; Noda K.; Hanabata Y.; Hayashida M.; Hirai W.; Fukami S.; Masuda S.; Yanagita S.; Yamamoto T.; Yoshikoshi T.; Yoshida T.; CTA-Japan consortium, The Physical Society of Japan (JPS)
Meeting Abstracts of the Physical Society of Japan, 2015

21pDD-5 CTA Report 90 : High precision measurement of PMTs for the first Large-Sized Telescope of CTA
Takahashi Mitsunari; Inome Yusuke; Umetsu Yohei; Ohoka Hideyuki; Ogino Momoko; Orito Reiko; Katagiri Hideaki; Kushida Junko; Kubo Hidetoshi; Gunji Shuichi; Koyama Shu; Sawada Makoto; Tsujimoto Shimpei; Tsubone Yoshio; Teshima Masahiro; Terada Yukikatsu; Tomono Yayoi; Nakajima Daisuke; Nagayoshi Tsutomu; Nishijima Kyoshi; Hanabata Yoshitaka; Hayashida Masaaki; Bamba Aya; Matsuoka Shunsuke; Yamamoto Tokonatsu; CTA-Japan consortium, The Physical Society of Japan (JPS)
Meeting Abstracts of the Physical Society of Japan, 2015

21pDD-6 CTA Report 91 : Development of the readout system to be installed on the first Large-Sized Telescope of CTA
Masuda S.; Kubo H.; Saito T.; Konno Y.; Tsuchiya Y.; Hatanaka K.; Teshima M.; Ishio K.; Ohoka H.; Hanabata Y.; Hayashida M.; Nakajima D.; Katagiri H.; Orito R.; Gunji S.; Nakamori T.; Yamamoto T.; Tanaka M.; CTA-Japan Consortium; Ikeno M.; Uchida T., The Physical Society of Japan (JPS)
Meeting Abstracts of the Physical Society of Japan, 2015

21pDD-4 CTA Report 89 : Calibration system and results of Photomultiplier Tubes for CTA first Large-Sized Telescope
Nagayoshi Tsutomu; Inome Yusuke; Umetsu Yohei; Ohoka Hideyuki; Orito Reiko; Katagiri Hideaki; Kushida Junko; Kubo Hidetoshi; Gunji Shuichi; Koyama Shu; Sawada Makoto; Takahashi Mitsunari; Tsujimoto Shimpei; Tsubone Yoshio; Teshima Masahiro; Terada Yukikatsu; Tomono Yayoi; Nakajima Daisuke; Nishijima Kyoshi; Hanabata Yoshitaka; Hayashida Masaaki; Bamba Aya; Matsuoka Shunsuke; Yamamoto Tokonatsu; CTA consortium, The Physical Society of Japan (JPS)
Meeting Abstracts of the Physical Society of Japan, 2015

24pDL-2 Development of Compton camera γI with high angular resolution
Nakayama K.; Itoh Y.; Uchida T.; Enomoto R.; Kagaya M.; Katagiri H.; Sato K.; Satoh W.; Takayanagi Y.; Takeda T.; Tanaka M.; Hanafusa R.; Matsushita A.; Muraishi H.; Yanagita S.; Yoshida T.; Wada K.; Wakamatsu R.; Watanabe T., The Physical Society of Japan (JPS)
Meeting Abstracts of the Physical Society of Japan, 2015

24pDL-1 Development of a survey meter which measures the directions of gamma rays for radioactive cesium.
Kagaya M.; Wakamatsu R.; Katagiri H.; Itoh Y.; Uchida T.; Enomoto R.; Sato K.; Sato W.; Takayanagi Y.; Takeda T.; Tanaka M.; Nakayama K.; Hanafusa R.; Hosokawa T.; Matsushita A.; Muraishi H.; Yanagita S.; Yoshida T.; Wada K.; Watanabe T., The Physical Society of Japan (JPS)
Meeting Abstracts of the Physical Society of Japan, 2015

28pSN-2 Development of high sensitivity survey meter capable of detecting arrival direction of gamma rays
Wakamatsu R.; Kagaya M.; Enomoto R.; Katagiri H.; Itoh Y.; Uchida T.; Satoh K.; Satoh W.; Takeda T.; Tanaka M.; Muraishi H.; Hanahusa R.; Hosokawa M.; Yoshida T.; Watanabe T.; Wada K.; Open-It consortium, The Physical Society of Japan (JPS)
Meeting Abstracts of the Physical Society of Japan, 2015

DETAILED INVESTIGATION OF THE GAMMA-RAY EMISSION IN THE VICINITY OF SNR W28 WITH FERMI-LAT
Y. Hanabata; H. Katagiri; J. W. Hewitt; J. Ballet; Y. Fukazawa; Y. Fukui; T. Hayakawa; M. Lemoine-Goumard; G. Pedaletti; A. W. Strong; D. F. Torres; R. Yamazaki, We present a detailed investigation of the gamma-ray emission in the vicinity of the supernova remnant (SNR) W28 (G6.4-0.1) observed by the Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope. We detected significant gamma-ray emission spatially coincident with TeV sources HESS J1800-240A, B, and C, located outside the radio boundary of the SNR. Their spectra in the 2-100 GeV band are consistent with the extrapolation of the power-law spectra of the TeV sources. We also identified a new source of GeV emission, dubbed Source W, which lies outside the boundary of TeV sources and coincides with radio emission from the western part of W28. All of the GeV gamma-ray sources overlap with molecular clouds in the velocity range from 0 to 20 km s(-1). Under the assumption that the gamma-ray emission toward HESS J1800-240A, B, and C comes from pi(0) decay due to the interaction between the molecular clouds and cosmic rays (CRs) escaping from W28, they can be naturally explained by a single model in which the CR diffusion coefficient is smaller than the theoretical expectation in the interstellar space. The total energy of the CRs escaping from W28 is constrained through the same modeling to be larger than similar to 2 x 10(49) erg. The emission from Source W can also be explained with the same CR escape scenario., IOP PUBLISHING LTD
ASTROPHYSICAL JOURNAL, May 2014, [Reviewed]

Development of a high detection efficiency and low-cost imaging gamma-ray camera γI　　　　　　　　　　　　　　　
M. Kagaya; R. Enomoto; R. Hanafusa; Y. Itoh; H. Katagiri; H. Muraishi; K. Nakayama; K. Satoh; T. Takeda; M. M. Tanaka; T. Uchida; T. Watanabe; S. Yanagita; T. Yoshida, We developed a novel Compton camera γI using CsI (Tl) scintillators which has high detection efficiency and is low-cost. Our motivation for the development of this detector is measuring gamma rays produced by radioactive nuclides from Fukushima Daiichi Nuclear Power Plant accident. Our detector consists of two arrays of detectors which act as a Compton scatterer and absorber. Energies deposited by Compton scattered electrons and subsequent photoelectric absorption measured by photomultipliers are used for image reconstruction. Each array consists of 8 large CsI (Tl) scintillator cubes, 3.5 cm on a side, which are inexpensive and have good energy resolution. The angular resolution is around 3.5° by using an image sharpening technique, and the detection efficiency is typically more than 10 times better than other detectors for the same purpose. We did measurement tests for contaminated area around 1 μSv/h. The imaging capability was verified by test measurements in Fukushima Prefecture together with the laboratory tests. In this paper, we reported the development of γI and the results of the measurement tests., Proceedings of Science (PoS)
Proceedings of Science, 2014

The Large Size Telescope of the Cherenkov Telescope Array
G. Ambrosi; Y. Awane; H. Baba; A. Bamba; M. Barcelo; U. Barres de Almeida; J. A. Barrio; O. Blanch Bigas; J. Boix; L. Brunetti; E. Carmona; E. Chabanne; M. Chikawa; P. Colin; J. Cortina; J. L. Contreras; F. Dazzi; A. de Angelis; G. Deleglise; C. Delgado; C. Diaz; A. Fiasson; D. Fink; N. Fouque; L. Freixas; C. Fruck; A. Gadola; R. Garcia; D. Gascon; N. Geffroy; N. Giglietto; F. Giordano; F. Granena; S. Gunji; R. Hagiwara; N. Hamer; Y. Hanabata; T. Hassan; K. Hatanaka; T. Haubold; M. Hayashida; R. Hermel; D. Herranz; K. Hirotani; S. Inoue; Y. Inoue; K. Ioka; C. Jablonski; M. Kagaya; H. Katagiri; T. Kishimoto; K. Kodani; K. Kohri; Y. Konno; S. Koyama; H. Kubo; J. Kushida; G. Lamanna; T. Le Flour; E. Lorenz; R. Lopez; M. Lopez-Moya; P. Majumdar; A. Manalaysay; M. Mariotti; G. Martinez; M. Martinez; D. Mazin; J. M. Miranda; R. Mirzoyan; I. Monteiro; A. Moralejo; K. Murase; S. Nagataki; D. Nakajima; T. Nakamori; K. Nishijima; K. Noda; A. Nozato; Y. Ohira; M. Ohishi; H. Ohoka; A. Okumura; R. Orito; J. L. Panazol; D. Paneque; R. Paoletti; J. M. Paredes; G. Pauletta; S. Podkladkin; J. Prast; R. Rando; O. Reimann; M. Ribo; S. Rosier-Lees; K. Saito; T. Saito; Y. Saito; N. Sakaki; R. Sakonaka; A. Sanuy; H. Sasaki; M. Sawada; V. Scalzotto; S. Schultz; T. Schweizer; T. Shibata; S. Shu; J. Sieiro; V. Stamatescu; S. Steiner; U. Straumann; R. Sugawara; H. Tajima; H. Takami; S. Tanaka; M. Tanaka; L. A. Tejedor; Y. Terada; M. Teshima; T. Totani; H. Ueno; K. Umehara; A. Vollhardt; R. Wagner; H. Wetteskind; T. Yamamoto; R. Yamazaki; A. Yoshida; T. Yoshida; T. Yoshikoshi, The Cherenkov Telescope Array (CTA) project aims to implement the world's largest next generation of Very High Energy gamma-ray Imaging Atmospheric Cherenkov Telescopes devoted to the observation from a few tens of GeV to more than 100 TeV. To view the whole sky, two CTA sites are foreseen, one for each hemisphere. The sensitivity at the lowest energy range will be dominated by four Large Size Telescopes, LSTs, located at the center of each array and designed to achieve observations of high red-shift objects with the threshold energy of 20 GeV. The LST is optimized also for transient low energy sources, such as Gamma Ray Bursts (GRB), which require fast repositioning of the telescope. The overall design and the development status of the first LST telescope will be discussed., SPIE-INT SOC OPTICAL ENGINEERING
GROUND-BASED AND AIRBORNE TELESCOPES V, 2014

コンプトンカメラ法における新しい画像再構成法の提案
村石 浩; 加賀谷 美佳; 片桐 秀明; 武田 徹; 渡辺 宝, The Compton camera technique is a novel method that enables us to estimate the direction of incident sub-MeV photons for each event without the collimator usually used in SPECT, and then to realize photon imaging. Some studies have constructed Compton camera systems using components such as a Si/CdTe semiconductor, or a CsI(T1) scintillator. In this technique, the photon source is reproduced by a superposition of back-projected rings in the 2D plane with the estimated scattering angle θ, but this degrades the spatial resolution in the reconstructed image. In this paper, we propose a novel reconstruction method for the Compton camera technique that is based on the filtered back projection algorithm used in computed tomography. We conducted reconstruction simulations assuming computed tomography and the Compton camera. We demonstrated that our proposed method drastically improves the spatial resolution of the Compton camera technique., Japan Academy of Health Sciences
日本保健科学学会誌, 2014, [Reviewed]

Erratum: "Fermi Large Area Telescope Study of Cosmic-Rays and the Interstellar Medium in Nearby Molecular Clouds" (2012, ApJ, 755, 22)
Ackermann, M.; Ajello, M.; Allafort, A.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bottacini, E.; Brandt, T. J.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Busetto, G.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Charles, E.; Chekhtman, A.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; D'Ammando, F.; de Angelis, A.; de Palma, F.; Dermer, C. D.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Drlica-Wagner, A.; Falletti, L.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Focke, W. B.; Fukazawa, Y.; Fukui, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Germani, S.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guiriec, S.; Hadasch, D.; Hanabata, Y.; Harding, A. K.; Hayashi, K.; Horan, D.; Hou, X.; Hughes, R. E.; Itoh, R.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Larsson, S.; Lee, S. -H.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Martin, P.; Mazziotta, M. N.; McEnery, J. E.; Mehault, J.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Naumann-Godo, M.; Nemmen, R.; Nishino, S.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Pivato, G.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Romoli, C.; Roth, M.; Sada, T.; Sadrozinski, H. F. -W.; Sanchez, D. A.; Sbarra, C.; Sgrò, C.; Siskind, E. J.; Spandre, G.; Spinelli, P.; Strong, A. W.; Suson, D. J.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Tibolla, O.; Tinivella, M.; Torres, D. F.; Tosti, G.; Tramacere, A.; Troja, E.; Uchiyama, Y.; Uehara, T.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vianello, G.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yamamoto, H.; Yang, Z.; Zimmer, S., ...
The Astrophysical Journal, Nov. 2013

Erratum: "Constraints on the Cosmic-Ray Density Gradient beyond the Solar Circle from Fermi γ-Ray Observations of the Third Galactic Quadrant" (2011, ApJ, 726, 81)
Ackermann, M.; Ajello, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Brandt, T. J.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Charles, E.; Chekhtman, A.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Dermer, C. D.; de Palma, F.; Digel, S. W.; Drell, P. S.; Dubois, R.; Favuzzi, C.; Ferrara, E. C.; Focke, W. B.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Germani, S.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Guiriec, S.; Hadasch, D.; Hanabata, Y.; Harding, A. K.; Hayashi, K.; Hayashida, M.; Hughes, R. E.; Itoh, R.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Llena-Garde, M.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Martin, P.; Mazziotta, M. N.; McEnery, J. E.; Mehault, J.; Michelson, P. F.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Naumann-Godo, M.; Nishino, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Ripken, J.; Sada, T.; Sadrozinski, H. F. -W.; Sgrò, C.; Siskind, E. J.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Strong, A. W.; Suson, D. J.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tramacere, A.; Uchiyama, Y.; Uehara, T.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Vladimirov, A. E.; Waite, A. P.; Wang, P.; Wood, K. S.; Yang, Z.; Ziegler, M., ...
The Astrophysical Journal, Aug. 2013

CTA contributions to the 33rd International Cosmic Ray Conference (ICRC2013)
CTA Consortium, The; :; Abril, O.; Acharya, B. S.; Actis, M.; Agnetta, G.; Aguilar, J. A.; Aharonian, F.; Ajello, M.; Akhperjanian, A.; Alcubierre, M.; Aleksic, J.; Alfaro, R.; Aliu, E.; Allafort, A. J.; Allan, D.; Allekotte, I.; Aloisio, R.; Amato, E.; Ambrosi, G.; Ambrosio, M.; Anderson, J.; Angüner, E. O.; Antonelli, L. A.; Antonuccio, V.; Antonucci, M.; Antoranz, P.; Aravantinos, A.; Argan, A.; Arlen, T.; Aramo, C.; Armstrong, T.; Arnaldi, H.; Arrabito, L.; Asano, K.; Ashton, T.; Asorey, H. G.; Aune, T.; Awane, Y.; Baba, H.; Babic, A.; Baby, N.; Bähr, J.; Bais, A.; Baixeras, C.; Bajtlik, S.; Balbo, M.; Balis, D.; Balkowski, C.; Ballet, J.; Bamba, A.; Bandiera, R.; Barber, A.; Barbier, C.; Barceló, M.; Barnacka, A.; Barnstedt, J.; Barres de Almeida, U.; Barrio, J. A.; Basili, A.; Basso, S.; Bastieri, D.; Bauer, C.; Baushev, A.; Becciani, U.; Becerra, J.; Becerra, J.; Becherini, Y.; Bechtol, K. C.; Becker Tjus, J.; Beckmann, V.; Bednarek, W.; Behera, B.; Belluso, M.; Benbow, W.; Berdugo, J.; Berge, D.; Berger, K.; Bernard, F.; Bernardino, T.; Bernlöhr, K.; Bertucci, B.; Bhat, N.; Bhattacharyya, S.; Biasuzzi, B.; Bigongiari, C.; Biland, A.; Billotta, S.; Bird, T.; Birsin, E.; Bissaldi, E.; Biteau, J.; Bitossi, M.; Blake, S.; Blanch Bigas, O.; Blasi, P.; Bobkov, A.; Boccone, V.; Böttcher, M.; Bogacz, L.; Bogart, J.; Bogdan, M.; Boisson, C.; Boix Gargallo, J.; Bolmont, J.; Bonanno, G.; Bonardi, A.; Bonev, T.; Bonifacio, P.; Bonnoli, G.; Bordas, P.; Borgland, A.; Borkowski, J.; Bose, R.; Botner, O.; Bottani, A.; Bouchet, L.; Bourgeat, M.; Boutonnet, C.; Bouvier, A.; Brau-Nogué, S.; Braun, I.; Bretz, T.; Briggs, M.; Brigida, M.; Bringmann, T.; Britto, R.; Brook, P.; Brun, P.; Brunetti, L.; Bruno, P.; Bucciantini, N.; Buanes, T.; Buckley, J.; Bühler, R.; Bugaev, V.; Bulgarelli, A.; Bulik, T.; Busetto, G.; Buson, S.; Byrum, K.; Cailles, M.; Cameron, R.; Camprecios, J.; Canestrari, R.; Cantu, S.; Capalbi, M.; Caraveo, P.; Carmona, E.; Carosi, A.; Carosi, R.; Carr, J.; Carter, J.; Carton, P. -H.; Caruso, R.; Casanova, S.; Cascone, E.; Casiraghi, M.; Castellina, A.; Catalano, O.; Cavazzani, S.; Cazaux, S.; Cerchiara, P.; Cerruti, M.; Chabanne, E.; Chadwick, P.; Champion, C.; Chaves, R.; Cheimets, P.; Chen, A.; Chiang, J.; Chiappetti, L.; Chikawa, M.; Chitnis, V. R.; Chollet, F.; Christof, A.; Chudoba, J.; Cieślar, M.; Cillis, A.; Cilmo, M.; Codino, A.; Cohen-Tanugi, J.; Colafrancesco, S.; Colin, P.; Colome, J.; Colonges, S.; Compin, M.; Conconi, P.; Conforti, V.; Connaughton, V.; Conrad, J.; Contreras, J. L.; Coppi, P.; Coridian, J.; Corona, P.; Corti, D.; Cortina, J.; Cossio, L.; Costa, A.; Costantini, H.; Cotter, G.; Courty, B.; Couturier, S.; Covino, S.; Crimi, G.; Criswell, S. J.; Croston, J.; Cusumano, G.; Dafonseca, M.; Dale, O.; Daniel, M.; Darling, J.; Davids, I.; Dazzi, F.; de Angelis, A.; De Caprio, V.; De Frondat, F.; de Gouveia Dal Pino, E. M.; de la Calle, I.; De La Vega, G. A.; de los Reyes Lopez, R.; de Lotto, B.; De Luca, A.; de Naurois, M.; de Oliveira, Y.; de Oña Wilhelmi, E.; de Palma, F.; de Souza, V.; Decerprit, G.; Decock, G.; Deil, C.; Delagnes, E.; Deleglise, G.; Delgado, C.; della Volpe, D.; Demange, P.; Depaola, G.; Dettlaff, A.; Di Girolamo, T.; Di Giulio, C.; Di Paola, A.; Di Pierro, F.; di Sciascio, G.; Díaz, C.; Dick, J.; Dickherber, R.; Dickinson, H.; Diez-Blanco, V.; Digel, S.; Dimitrov, D.; Disset, G.; Djannati-Ataï, A.; Doert, M.; Dohmke, M.; Domainko, W.; Dominis Prester, D.; Donat, A.; Dorner, D.; Doro, M.; Dournaux, J. -L.; Drake, G.; Dravins, D.; Drury, L.; Dubois, F.; Dubois, R.; Dubus, G.; Dufour, C.; Dumas, D.; Dumm, J.; Durand, D.; Dwarkadas, V.; Dyks, J.; Dyrda, M.; Ebr, J.; Edy, E.; Egberts, K.; Eger, P.; Einecke, S.; Eleftheriadis, C.; Elles, S.; Emmanoulopoulos, D.; Engelhaupt, D.; Enomoto, R.; Ernenwein, J. -P.; Errando, M.; Etchegoyen, A.; Evans, P. A.; Falcone, A.; Faltenbacher, A.; Fantinel, D.; Farakos, K.; Farnier, C.; Farrell, E.; Fasola, G.; Favill, B. W.; Fede, E.; Federici, S.; Fegan, S.; Feinstein, F.; Ferenc, D.; Ferrando, P.; Fesquet, M.; Fetfatzis, P.; Fiasson, A.; Fillin-Martino, E.; Fink, D.; Finley, C.; Finley, J. P.; Fiorini, M.; Firpo Curcoll, R.; Flandrini, E.; Fleischhack, H.; Flores, H.; Florin, D.; Focke, W.; Föhr, C.; Fokitis, E.; Font, L.; Fontaine, G.; Fornasa, M.; Förster, A.; Fortson, L.; Fouque, N.; Franckowiak, A.; Franco, F. J.; Frankowski, A.; Fransson, C.; Fraser, G. W.; Frei, R.; Fresnillo, L.; Fruck, C.; Fugazza, D.; Fujita, Y.; Fukazawa, Y.; Fukui, Y.; Funk, S.; Gäbele, W.; Gabici, S.; Gabriele, R.; Gadola, A.; Galante, N.; Gall, D.; Gallant, Y.; Gámez-García, J.; Garczarczyk, M.; García, B.; Garcia López, R.; Gardiol, D.; Gargano, F.; Garrido, D.; Garrido, L.; Gascon, D.; Gaug, M.; Gaweda, J.; Gebremedhin, L.; Geffroy, N.; Gerard, L.; Ghedina, A.; Ghigo, M.; Ghislain, P.; Giannakaki, E.; Gianotti, F.; Giarrusso, S.; Giavitto, G.; Giebels, B.; Giglietto, N.; Gika, V.; Giomi, M.; Giommi, P.; Giordano, F.; Girard, N.; Giro, E.; Giuliani, A.; Glanzman, T.; Glicenstein, J. -F.; Godinovic, N.; Golev, V.; Gomez Berisso, M.; Gómez-Ortega, J.; Gonzalez, M. M.; González, A.; González, F.; González Muñoz, A.; Gothe, K. S.; Grabarczyk, T.; Gougerot, M.; Graciani, R.; Grandi, P.; Grañena, F.; Granot, J.; Grasseau, G.; Gredig, R.; Green, A.; Greenshaw, T.; Grégoire, T.; Grillo, A.; Grimm, O.; Grondin, M. -H.; Grube, J.; Grudzinska, M.; Gruev, V.; Grünewald, S.; Grygorczuk, J.; Guarino, V.; Gunji, S.; Gyuk, G.; Hadasch, D.; Hagedorn, A.; Hagiwara, R.; Hahn, J.; Hakansson, N.; Hallgren, A.; Hamer Heras, N.; Hara, S.; Hardcastle, M. J.; Harezlak, D.; Harris, J.; Hassan, T.; Hatanaka, K.; Haubold, T.; Haupt, A.; Hayakawa, T.; Hayashida, M.; Heller, R.; Henault, F.; Henri, G.; Hermann, G.; Hermel, R.; Herrero, A.; Hervet, O.; Hidaka, N.; Hinton, J. A.; Hirotani, K.; Hoffmann, D.; Hofmann, W.; Hofverberg, P.; Holder, J.; Hörandel, J. R.; Horns, D.; Horville, D.; Houles, J.; Hrabovsky, M.; Hrupec, D.; Huan, H.; Huber, B.; Huet, J. -M.; Hughes, G.; Humensky, T. B.; Huovelin, J.; Huppert, J. -F.; Ibarra, A.; Ikawa, D.; Illa, J. M.; Impiombato, D.; Incorvaia, S.; Inoue, S.; Inoue, Y.; Iocco, F.; Ioka, K.; Israel, G. L.; Jablonski, C.; Jacholkowska, A.; Jacquemier, J.; Jamrozy, M.; Janiak, M.; Jean, P.; Jeanney, C.; Jimenez, J. J.; Jogler, T.; Johnson, C.; Johnson, T.; Journet, L.; Juffroy, C.; Jung, I.; Kaaret, P.; Kabuki, S.; Kagaya, M.; Kakuwa, J.; Kalkuhl, C.; Kankanyan, R.; Karastergiou, A.; Kärcher, K.; Karczewski, M.; Karkar, S.; Kasperek, J.; Kastana, D.; Katagiri, H.; Kataoka, J.; Katarzyński, K.; Katz, U.; Kawanaka, N.; Kazanas, D.; Kelley-Hoskins, N.; Kellner-Leidel, B.; Kelly, H.; Kendziorra, E.; Khélifi, B.; Kieda, D. B.; Kifune, T.; Kihm, T.; Kishimoto, T.; Kitamoto, K.; Kluźniak, W.; Knapic, C.; Knapp, J.; Knödlseder, J.; Köck, F.; Kocot, J.; Kodani, K.; Köhne, J. -H.; Kohri, K.; Kokkotas, K.; Kolitzus, D.; Komin, N.; Kominis, I.; Konno, Y.; Köppel, H.; Korohoda, P.; Kosack, K.; Koss, G.; Kossakowski, R.; Koul, R.; Kowal, G.; Koyama, S.; Kozioł, J.; Krähenbühl, T.; Krause, J.; Krawzcynski, H.; Krennrich, F.; Krepps, A.; Kretzschmann, A.; Krobot, R.; Krueger, P.; Kubo, H.; Kudryavtsev, V. A.; Kushida, J.; Kuznetsov, A.; La Barbera, A.; La Palombara, N.; La Parola, V.; La Rosa, G.; Lacombe, K.; Lamanna, G.; Lande, J.; Languignon, D.; Lapington, J. S.; Laporte, P.; Laurent, B.; Lavalley, C.; Le Flour, T.; Le Padellec, A.; Lee, S. -H.; Lee, W. H.; Lefèvre, J. -P.; Leich, H.; Leigui de Oliveira, M. A.; Lelas, D.; Lenain, J. -P.; Leoni, R.; Leopold, D. J.; Lerch, T.; Lessio, L.; Leto, G.; Lieunard, B.; Lieunard, S.; Lindemann, R.; Lindfors, E.; Liolios, A.; Lipniacka, A.; Lockart, H.; Lohse, T.; Lombardi, S.; Longo, F.; Lopatin, A.; Lopez, M.; López-Coto, R.; López-Oramas, A.; Lorca, A.; Lorenz, E.; Louis, F.; Lubinski, P.; Lucarelli, F.; Lüdecke, H.; Ludwin, J.; Luque-Escamilla, P. L.; Lustermann, W.; Luz, O.; Lyard, E.; Maccarone, M. C.; Maccarone, T. J.; Madejski, G. M.; Madhavan, A.; Mahabir, M.; Maier, G.; Majumdar, P.; Malaguti, G.; Malaspina, G.; Maltezos, S.; Manalaysay, A.; Mancilla, A.; Mandat, D.; Maneva, G.; Mangano, A.; Manigot, P.; Mannheim, K.; Manthos, I.; Maragos, N.; Marcowith, A.; Mariotti, M.; Marisaldi, M.; Markoff, S.; Marszałek, A.; Martens, C.; Martí, J.; Martin, J. -M.; Martin, P.; Martínez, G.; Martínez, F.; Martínez, M.; Massaro, F.; Masserot, A.; Mastichiadis, A.; Mathieu, A.; Matsumoto, H.; Mattana, F.; Mattiazzo, S.; Maurer, A.; Maurin, G.; Maxfield, S.; Maya, J.; Mazin, D.; Mc Comb, L.; McCann, A.; McCubbin, N.; McHardy, I.; McKay, R.; Meagher, K.; Medina, C.; Melioli, C.; Melkumyan, D.; Melo, D.; Mereghetti, S.; Mertsch, P.; Meucci, M.; Meyer, M.; Michałowski, J.; Micolon, P.; Mihailidis, A.; Mineo, T.; Minuti, M.; Mirabal, N.; Mirabel, F.; Miranda, J. M.; Mirzoyan, R.; Mistò, A.; Mizuno, T.; Moal, B.; Moderski, R.; Mognet, I.; Molinari, E.; Molinaro, M.; Montaruli, T.; Monte, C.; Monteiro, I.; Moore, P.; Moralejo Olaizola, A.; Mordalska, M.; Morello, C.; Mori, K.; Morlino, G.; Morselli, A.; Mottez, F.; Moudden, Y.; Moulin, E.; Mrusek, I.; Mukherjee, R.; Munar-Adrover, P.; Muraishi, H.; Murase, K.; StJ. Murphy, A.; Nagataki, S.; Naito, T.; Nakajima, D.; Nakamori, T.; Nakayama, K.; Naumann, C.; Naumann, D.; Naumann-Godo, M.; Nayman, P.; Nedbal, D.; Neise, D.; Nellen, L.; Neronov, A.; Neustroev, V.; Neyroud, N.; Nicastro, L.; Nicolau-Kukliński, J.; Niedźwiecki, A.; Niemiec, J.; Nieto, D.; Nikolaidis, A.; Nishijima, K.; Nishikawa, K. -I.; Noda, K.; Nolan, S.; Northrop, R.; Nosek, D.; Nowak, N.; Nozato, A.; Oakes, L.; O'Brien, P. T.; Ohira, Y.; Ohishi, M.; Ohm, S.; Ohoka, H.; Okuda, T.; Okumura, A.; Olive, J. -F.; Ong, R. A.; Orito, R.; Orr, M.; Osborne, J. P.; Ostrowski, M.; Otero, L. A.; Otte, N.; Ovcharov, E.; Oya, I.; Ozieblo, A.; Padilla, L.; Pagano, I.; Paiano, S.; Paillot, D.; Paizis, A.; Palanque, S.; Palatka, M.; Pallota, J.; Palatiello, M.; Panagiotidis, K.; Panazol, J. -L.; Paneque, D.; Panter, M.; Panzera, M. R.; Paoletti, R.; Papayannis, A.; Papyan, G.; Paredes, J. M.; Pareschi, G.; Parraud, J. -M.; Parsons, D.; Pauletta, G.; Paz Arribas, M.; Pech, M.; Pedaletti, G.; Pelassa, V.; Pelat, D.; Perez, M. d. C.; Persic, M.; Petrucci, P. -O.; Peyaud, B.; Pichel, A.; Pieloth, D.; Pierre, E.; Pita, S.; Pivato, G.; Pizzolato, F.; Platino, M.; Platos, Ł.; Platzer, R.; Podkladkin, S.; Pogosyan, L.; Pohl, M.; Pojmanski, G.; Ponz, J. D.; Potter, W.; Poutanen, J.; Prandini, E.; Prast, J.; Preece, R.; Profeti, F.; Prokoph, H.; Prouza, M.; Proyetti, M.; Puerto-Giménez, I.; Pühlhofer, G.; Puljak, I.; Punch, M.; Pyzioł, R.; Quel, E. J.; Quesada, J.; Quinn, J.; Quirrenbach, A.; Racero, E.; Rainò, S.; Rajda, P. J.; Rameez, M.; Ramon, P.; Rando, R.; Rannot, R. C.; Rataj, M.; Raue, M.; Ravignani, D.; Reardon, P.; Reimann, O.; Reimer, A.; Reimer, O.; Reitberger, K.; Renaud, M.; Renner, S.; Reville, B.; Rhode, W.; Ribó, M.; Ribordy, M.; Richards, G.; Richer, M. G.; Rico, J.; Ridky, J.; Rieger, F.; Ringegni, P.; Ripken, J.; Ristori, P. R.; Rivière, A.; Rivoire, S.; Rob, L.; Rodeghiero, G.; Roeser, U.; Rohlfs, R.; Rojas, G.; Romano, P.; Romaszkan, W.; Romero, G. E.; Rosen, S. R.; Rosier Lees, S.; Ross, D.; Rouaix, G.; Rousselle, J.; Rousselle, S.; Rovero, A. C.; Roy, F.; Royer, S.; Rudak, B.; Rulten, C.; Rupiński, M.; Russo, F.; Ryde, F.; Saavedra, O.; Sacco, B.; Saemann, E. O.; Saggion, A.; Sahakian, V.; Saito, K.; Saito, T.; Saito, Y.; Sakaki, N.; Sakonaka, R.; Salini, A.; Sanchez, F.; Sanchez-Conde, M.; Sandoval, A.; Sandaker, H.; Sant'Ambrogio, E.; Santangelo, A.; Santos, E. M.; Sanuy, A.; Sapozhnikov, L.; Sarkar, S.; Sartore, N.; Sasaki, H.; Satalecka, K.; Sawada, M.; Scalzotto, V.; Scapin, V.; Scarcioffolo, M.; Schafer, J.; Schanz, T.; Schlenstedt, S.; Schlickeiser, R.; Schmidt, T.; Schmoll, J.; Schovanek, P.; Schroedter, M.; Schubert, A.; Schultz, C.; Schultze, J.; Schulz, A.; Schure, K.; Schussler, F.; Schwab, T.; Schwanke, U.; Schwarz, J.; Schwarzburg, S.; Schweizer, T.; Schwemmer, S.; Schwendicke, U.; Schwerdt, C.; Segreto, A.; Seiradakis, J. -H.; Sembroski, G. H.; Servillat, M.; Seweryn, K.; Sharma, M.; Shayduk, M.; Shellard, R. C.; Shi, J.; Shibata, T.; Shibuya, A.; Shore, S.; Shum, E.; Sideras-Haddad, E.; Sidoli, L.; Sidz, M.; Sieiro, J.; Sikora, M.; Silk, J.; Sillanpää, A.; Singh, B. B.; Sironi, G.; Sitarek, J.; Skole, C.; Smareglia, R.; Smith, A.; Smith, D.; Smith, J.; Smith, N.; Sobczyńska, D.; Sol, H.; Sottile, G.; Sowiński, M.; Spanier, F.; Spiga, D.; Spyrou, S.; Stamatescu, V.; Stamerra, A.; Starling, R. L. C.; Stawarz, Ł.; Steenkamp, R.; Stegmann, C.; Steiner, S.; Stella, C.; Stergioulas, N.; Sternberger, R.; Sterzel, M.; Stinzing, F.; Stodulski, M.; Stolarczyk, Th.; Straumann, U.; Strazzeri, E.; Stringhetti, L.; Suarez, A.; Suchenek, M.; Sugawara, R.; Sulanke, K. -H.; Sun, S.; Supanitsky, A. D.; Suric, T.; Sutcliffe, P.; Sykes, J. M.; Szanecki, M.; Szepieniec, T.; Szostek, A.; Tagliaferri, G.; Tajima, H.; Takahashi, H.; Takahashi, K.; Takalo, L.; Takami, H.; Talbot, G.; Tammi, J.; Tanaka, M.; Tanaka, S.; Tasan, J.; Tavani, M.; Tavernet, J. -P.; Tejedor, L. A.; Telezhinsky, I.; Temnikov, P.; Tenzer, C.; Terada, Y.; Terrier, R.; Teshima, M.; Testa, V.; Tezier, D.; Thayer, J.; Thuermann, D.; Tibaldo, L.; Tibaldo, L.; Tibolla, O.; Tiengo, A.; Timpanaro, M. C.; Tluczykont, M.; Todero Peixoto, C. J.; Tokanai, F.; Tokarz, M.; Toma, K.; Tonachini, A.; Torii, K.; Tornikoski, M.; Torres, D. F.; Torres, M.; Toscano, S.; Toso, G.; Tosti, G.; Totani, T.; Toussenel, F.; Tovmassian, G.; Travnicek, P.; Treves, A.; Trifoglio, M.; Troyano, I.; Tsinganos, K.; Ueno, H.; Umana, G.; Umehara, K.; Upadhya, S. S.; Usher, T.; Uslenghi, M.; Vagnetti, F.; Valdes-Galicia, J. F.; Vallania, P.; Vallejo, G.; van Driel, W.; van Eldik, C.; Vandenbrouke, J.; Vanderwalt, J.; Vankov, H.; Vasileiadis, G.; Vassiliev, V.; Veberic, D.; Vegas, I.; Vercellone, S.; Vergani, S.; Verzi, V.; Vettolani, G. P.; Veyssière, C.; Vialle, J. P.; Viana, A.; Videla, M.; Vigorito, C.; Vincent, P.; Vincent, S.; Vink, J.; Vlahakis, N.; Vlahos, L.; Vogler, P.; Voisin, V.; Vollhardt, A.; von Gunten, H. -P.; Vorobiov, S.; Vuerli, C.; Waegebaert, V.; Wagner, R.; Wagner, R. G.; Wagner, S.; Wakely, S. P.; Walter, R.; Walther, T.; Warda, K.; Warwick, R. S.; Wawer, P.; Wawrzaszek, R.; Webb, N.; Wegner, P.; Weinstein, A.; Weitzel, Q.; Welsing, R.; Werner, M.; Wetteskind, H.; White, R. J.; Wierzcholska, A.; Wiesand, S.; Wilhelm, A.; Wilkinson, M. I.; Williams, D. A.; Willingale, R.; Winde, M.; Winiarski, K.; Wischnewski, R.; Wiśniewski, Ł.; Wojcik, P.; Wood, M.; Wörnlein, A.; Xiong, Q.; Yadav, K. K.; Yamamoto, H.; Yamamoto, T.; Yamazaki, R.; Yanagita, S.; Yebras, J. M.; Yelos, D.; Yoshida, A.; Yoshida, T.; Yoshikoshi, T.; Yu, P.; Zabalza, V.; Zacharias, M.; Zajczyk, A.; Zampieri, L.; Zanin, R.; Zdziarski, A.; Zech, A.; Zhao, A.; Zhou, X.; Zietara, K.; Ziolkowski, J.; Ziółkowski, P.; Zitelli, V.; Zurbach, C.; Zychowski, P., Compilation of CTA contributions to the proceedings of the 33rd International Cosmic Ray Conference (ICRC2013), which took place in 2-9 July, 2013, in Rio de Janeiro, Brazil..., arXiv e-prints
Jul. 2013

X-Ray Observations of the W 51 Complex with Suzaku
Yoshitaka Hanabata; Makoto Sawada; Hideaki Katagiri; Aya Bamba; Yasushi Fukazawa, We present a detailed analysis of X-ray emission from the middle-aged supernova remnant W 51 C and star-forming region W 51 B with Suzaku. The soft X-ray emission from W 51 C is well-represented by an optically thin thermal plasma in a non-equilibrium ionization state with a temperature of similar to 0.7 keV. The elemental abundance of Mg is significantly higher than the solar value. We find no significant feature of an over-ionized plasma in W 51 C. The hard X-ray emission is spatially coincident with the molecular clouds associated with W 51 B, overlapping with W 51 C. The spectrum is represented by an optically thin thermal plasma with a temperature of similar to 5 keV, or a powerlaw model with a photon index of similar to 2.2. The emission probably has a diffuse nature, since its luminosity of 1 x 10(34) erg s(-1) in the 0.5-10 keV band cannot be explained by any emission from point sources in this region. We discuss the possibility that the hard X-ray emission comes from stellar winds of OB stars in W 51 B, or accelerated particles in W 51 C., OXFORD UNIV PRESS
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Apr. 2013, [Reviewed]

Detailed X-ray study of the supernova remnant W51C with Suzaku .　　　　　　　　　　　　　　　
Hanabata, Y.; Sawada, M.; Katagiri, H.; Bamba, A.; Fukazawa, Y., We present a detailed analysis of the X-ray emission from the W51 complex, focusing on the middle-aged supernova remnant and star-forming region W51B with Suzaku. The soft X-ray emission from W51C is well represented by a thermal plasma in non-equilibrium ionization state with the enhanced Mg abundance. The hard X-ray emission is spatially coincident with the molecular clouds associated with W51B, overlapping with W51C. The spectrum is represented by a thermal plasma or a power-law model. We discuss the possibility that the hard X-ray emission comes from stellar winds of OB stars in W51B or particles accelerated in W51C. You can see more details in Hanabata et al. 2013, \pasj, 65, 42....
Memorie della Societa Astronomica Italiana, 2013

The cherenkov telescope array large size telescope
G. Ambrosi; Y. Awane; H. Baba; A. Bamba; M. Barceló; U. Barres; de Almeida; J. A. Barrio; O. Blanch Bigas; J. Boix; L. Brunetti; E. Carmona; E. Chabanne; M. Chikawa; P. Colin; J. L. Conteras; J. Cortina; F. Dazzi; A. Deangelis; G. Deleglise; C. Delgado; C. Díaz; F. Dubois; A. Fiasson; D. Fink; N. Fouque; L. Freixas; C. Fruck; A. Gadola; R. García; D. Gascon; N. Geffroy; N. Giglietto; F. Giordano; F. Grañena; S. Gunji; R. Hagiwara; N. Hamer; Y. Hanabata; T. Hassan; K. Hatanaka; T. Haubold; M. Hayashida; R. Hermel; D. Herranz; K. Hirotani; S. Inoue; Y. Inoue; K. Ioka; C. Jablonski; M. Kagaya; H. Katagiri; T. Kishimoto; K. Kodani; K. Kohri; Y. Konno; S. Koyama; H. Kubo; J. Kushida; G. Lamanna; T. L.E. Flour; M. López-Moya; R. López; E. Lorenz; P. Majumdar; A. Manalaysay; M. Mariotti; G. Martínez; M. Martínez; D. Mazin; J. M. Miranda; R. Mirzoyan; I. Monteiro; A. Moralejo; K. Murase; S. Nagataki; D. Nakajima; T. Nakamori; K. Nishijima; K. Noda; A. Nozato; Y. Ohira; M. Ohishi; H. Ohoka; A. Okumura; R. Orito; J. L. Panazol; D. Paneque; R. Paoletti; J. M. Paredes; G. Pauletta; S. Podkladkin; J. Prast; R. Rando; O. Reimann; M. Ribó; S. Rosier-Lees; K. Saito; T. Saito; Y. Saito; N. Sakaki, © 2013 Sociedade Brasileira de Fisica. All Rights Reserved. The two arrays of the Very High Energy gamma-ray observatory Cherenkov Telescope Array (CTA) will include four Large Size Telescopes (LSTs) each with a 23 m diameter dish and 28 m focal distance. These telescopes will enable CTA to achieve a low-energy threshold of 20 GeV, which is critical for important studies in astrophysics, astroparticle physics and cosmology. This work presents the key specifications and performance of the current LST design in the light of the CTA scientific objectives.
Proceedings of the 33rd International Cosmic Rays Conference, ICRC 2013, 01 Jan. 2013

Development of the photomultiplier-tube readout system for the CTA large size telescope
H. Kubo; R. Paoletti; Y. Awane; A. Bamba; M. Barcelo; J. A. Barrio; O. Blanch; J. Boix; C. Delgado; D. Fink; D. Gascon; S. Gunji; R. Hagiwara; Y. Hanabata; K. Hatanaka; M. Hayashida; M. Ikeno; S. Kabuki; H. Katagiri; J. Kataoka; Y. Konno; S. Koyama; T. Kishimoto; J. Kushida; G. Martínez; S. Masuda; J. M. Miranda; R. Mirzoyan; T. Mizuno; T. Nagayoshi; D. Nakajima; T. Nakamori; H. Ohoka; A. Okumura; R. Orito; T. Saito; A. Sanuy; H. Sasaki; M. Sawada; T. Schweizer; R. Sugawara; K. H. Sulanke; H. Tajima; M. Tanaka; S. Tanaka; L. A. Tejedor; Y. Terada; M. Teshima; F. Tokanai; Y. Tsuchiya; T. Uchida; H. Ueno; K. Umehara; T. Yamamoto, We have developed a prototype of the photomultiplier tube (PMT) readout system for the Cherenkov Telescope Array (CTA) Large Size Telescope (LST). Two thousand PMTs along with their readout systems are arranged on the focal plane of each telescope, with one readout system per 7-PMT cluster. The Cherenkov light pulses generated by the air showers are detected by the PMTs and amplified in a compact, low noise and wide dynamic range gain block. The output of this block is then digitized at a sampling rate of the order of GHz using the Domino Ring Sampler DRS4, an analog memory ASIC developed at Paul Scherrer Institute. The sampler has 1,024 capacitors per channel and four channels are cascaded for increased depth. After a trigger is generated in the system, the charges stored in the capacitors are digitized by an external slow sampling ADC and then transmitted via Gigabit Ethernet. An onboard FPGA controls the DRS4, trigger threshold, and Ethernet transfer. In addition, the control and monitoring of the Cockcroft-Walton circuit that provides high voltage for the 7-PMT cluster are performed by the same FPGA. A prototype named Dragon has been developed that has successfully sampled PMT signals at a rate of 2 GHz, and generated single photoelectron spectra.
Proceedings of the 33rd International Cosmic Rays Conference, ICRC 2013, 2013

Introducing the CTA concept
B. S. Acharya; M. Actis; T. Aghajani; G. Agnetta; J. Aguilar; F. Aharonian; M. Ajello; A. Akhperjanian; M. Alcubierre; J. Aleksić; R. Alfaro; E. Aliu; A. J. Allafort; D. Allan; I. Allekotte; E. Amato; J. Anderson; E. O. Anguner; L. A. Antonelli; P. Antoranz; A. Aravantinos; T. Arlen; T. Armstrong; H. Arnaldi; L. Arrabito; K. Asano; T. Ashton; H. G. Asorey; Y. Awane; H. Baba; A. Babic; N. Baby; J. Bahr; A. Bais; C. Baixeras; S. Bajtlik; M. Balbo; D. Balis; C. Balkowski; A. Bamba; R. Bandiera; A. Barber; C. Barbier; M. Barcelo; A. Barnacka; J. Barnstedt; U. De AlmeidaBarres; J. A. Barrio; A. Basili; S. Basso; D. Bastieri; C. Bauer; A. Baushev; J. Becerra; Y. Becherini; K. C. Bechtol; J. Becker Tjus; V. Beckmann; W. Bednarek; B. Behera; M. Belluso; W. Benbow; J. Berdugo; K. Berger; F. Bernard; T. Bernardino; K. Bernlohr; N. Bhat; S. Bhattacharyya; C. Bigongiari; A. Biland; S. Billotta; T. Bird; E. Birsin; E. Bissaldi; J. Biteau; M. Bitossi; S. Blake; O. Blanch Bigas; P. Blasi; A. Bobkov; V. Boccone; M. Boettcher; L. Bogacz; J. Bogart; M. Bogdan; C. Boisson; J. Boix Gargallo; J. Bolmont; G. Bonanno; A. Bonardi; T. Bonev; P. Bonifacio; G. Bonnoli; P. Bordas; A. Borgland; J. Borkowski; R. Bose; O. Botner; A. Bottani, The Cherenkov Telescope Array (CTA) is a new observatory for very high-energy (VHE) gamma rays. CTA has ambitions science goals, for which it is necessary to achieve full-sky coverage, to improve the sensitivity by about an order of magnitude, to span about four decades of energy, from a few tens of GeV to above 100 TeV with enhanced angular and energy resolutions over existing VHE gamma-ray observatories. An international collaboration has formed with more than 1000 members from 27 countries in Europe, Asia, Africa and North and South America. In 2010 the CTA Consortium completed a Design Study and started a three-year Preparatory Phase which leads to production readiness of CTA in 2014. In this paper we introduce the science goals and the concept of CTA, and provide an overview of the project. © 2013 Elsevier B.V. All rights reserved.
Astroparticle Physics, 2013, [Reviewed]

The Fermi Large Area Telescope on Orbit: Event Classification, Instrument Response Functions, and Calibration
Ackermann, M.; Ajello, M.; Albert, A.; Allafort, A.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Bissaldi, E.; Blandford, R. D.; Bloom, E. D.; Bogart, J. R.; Bonamente, E.; Borgland, A. W.; Bottacini, E.; Bouvier, A.; Brandt, T. J.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chaves, R. C. G.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Corbet, R.; Cutini, S.; D'Ammando, F.; Davis, D. S.; de Angelis, A.; DeKlotz, M.; de Palma, F.; Dermer, C. D.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Focke, W. B.; Fortin, P.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Giebels, B.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grove, J. E.; Guiriec, S.; Hadasch, D.; Hayashida, M.; Hays, E.; Horan, D.; Hou, X.; Hughes, R. E.; Jackson, M. S.; Jogler, T.; Jóhannesson, G.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kerr, M.; Knödlseder, J.; Kuss, M.; Lande, J.; Larsson, S.; Latronico, L.; Lavalley, C.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Mehault, J.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Naumann-Godo, M.; Nemmen, R.; Nishino, S.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orienti, M.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J. H.; Perkins, J. S.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Pivato, G.; Porter, T. A.; Racusin, J. L.; Rainò, S.; Rando, R.; Razzano, M.; Razzaque, S.; Reimer, A.; Reimer, O.; Reposeur, T.; Reyes, L. C.; Ritz, S.; Rochester, L. S.; Romoli, C.; Roth, M.; Sadrozinski, H. F. -W.; Sanchez, D. A.; Saz Parkinson, P. M.; Sbarra, C.; Scargle, J. D.; Sgrò, C.; Siegal-Gaskins, J.; Siskind, E. J.; Spandre, G.; Spinelli, P.; Stephens, T. E.; Suson, D. J.; Tajima, H.; Takahashi, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Tinivella, M.; Tosti, G.; Troja, E.; Usher, T. L.; Vandenbroucke, J.; Van Klaveren, B.; Vasileiou, V.; Vianello, G.; Vitale, V.; Waite, A. P.; Wallace, E.; Winer, B. L.; Wood, D. L.; Wood, K. S.; Wood, M.; Yang, Z.; Zimmer, S., The Fermi Large Area Telescope (Fermi-LAT, hereafter LAT), the primary instrument on the Fermi Gamma-ray Space Telescope (Fermi) mission, is an imaging, wide field-of-view, high-energy γ-ray telescope, covering the energy range from 20 MeV to more than 300 GeV. During the first years of the mission, the LAT team has gained considerable insight into the in-flight performance of the instrument. Accordingly, we have updated the analysis used to reduce LAT data for public release as well as the instrument response functions (IRFs), the description of the instrument performance provided for data analysis. In this paper, we describe the effects that motivated these updates. Furthermore, we discuss how we originally derived IRFs from Monte Carlo simulations and later corrected those IRFs for discrepancies observed between flight and simulated data. We also give details of the validations performed using flight data and quantify the residual uncertainties in the IRFs. Finally, we describe techniques the LAT team has developed to propagate those uncertainties into estimates of the systematic errors on common measurements such as fluxes and spectra of astrophysical sources....
The Astrophysical Journal Supplement Series, Nov. 2012

Fermi Observations of γ-Ray Emission from the Moon
Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwoo, W. B.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bonamente, E.; Borgland, A. W.; Bottacini, E.; Bouvier, A.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Charles, E.; Chekhtman, A.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Cutini, S.; D'Ammando, F.; de Angelis, A.; de Palma, F.; Dermer, C. D.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fortin, P.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gehrels, N.; Germani, S.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Gomez-Vargas, G. A.; Grenier, I. A.; Grove, J. E.; Guiriec, S.; Hadasch, D.; Hays, E.; Hill, A. B.; Horan, D.; Hou, X.; Hughes, R. E.; Iafrate, G.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Larsson, S.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Mazziotta, M. N.; McEnery, J. E.; Mehault, J.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Naumann-Godo, M.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orienti, M.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Pivato, G.; Poon, H.; Porter, T. A.; Prokhorov, D.; Rainò, S.; Rando, R.; Razzano, M.; Razzaque, S.; Reimer, A.; Reimer, O.; Reposeur, T.; Rochester, L. S.; Roth, M.; Sadrozinski, H. F. -W.; Sanchez, D. A.; Sbarra, C.; Schalk, T. L.; Sgrò, C.; Share, G. H.; Siskind, E. J.; Spandre, G.; Spinelli, P.; Stawarz, Ł.; Takahashi, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Tinivella, M.; Torres, D. F.; Tosti, G.; Troja, E.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vianello, G.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, D. L.; Wood, K. S.; Yang, Z.; Zimmer, S., We report on the detection of high-energy γ-ray emission from the Moon during the first 24 months of observations by the Fermi Large Area Telescope (LAT). This emission comes from particle cascades produced by cosmic-ray (CR) nuclei and electrons interacting with the lunar surface. The differential spectrum of the Moon is soft and can be described as a log-parabolic function with an effective cutoff at 2-3 GeV, while the average integral flux measured with the LAT from the beginning of observations in 2008 August to the end of 2010 August is F(>100\ MeV) =(1.04+/- 0.01\,{[statistical\ error]}+/- 0.1\,{[systematic\ error]})\times 10^{-6} cm^-2 s^-1. This flux is about a factor 2-3 higher than that observed between 1991 and 1994 by the EGRET experiment on board the Compton Gamma Ray Observatory, F(>100 MeV) ≈ 5 × 10^-7 cm^-2 s^-1, when solar activity was relatively high. The higher γ-ray flux measured by Fermi is consistent with the deep solar minimum conditions during the first 24 months of the mission, which reduced effects of heliospheric modulation, and thus increased the heliospheric flux of Galactic CRs. A detailed comparison of the light curve with McMurdo Neutron Monitor rates suggests a correlation of the trends. The Moon and the Sun are so far the only known bright emitters of γ-rays with fast celestial motion. Their paths across the sky are projected onto the Galactic center and high Galactic latitudes as well as onto other areas crowded with high-energy γ-ray sources. Analysis of the lunar and solar emission may thus be important for studies of weak and transient sources near the ecliptic....
The Astrophysical Journal, Oct. 2012

Gamma-Ray Observations of the Orion Molecular Clouds with the Fermi Large Area Telescope
Ackermann, M.; Ajello, M.; Allafort, A.; Antolini, E.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bottacini, E.; Brandt, T. J.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Cecchi, C.; Chekhtman, A.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; D'Ammando, F.; de Angelis, A.; de Palma, F.; Dermer, C. D.; Silva, E. do Couto e.; Drell, P. S.; Drlica-Wagner, A.; Enoto, T.; Falletti, L.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Focke, W. B.; Fukazawa, Y.; Fukui, Y.; Fusco, P.; Gargano, F.; Gasparrini, D.; Germani, S.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Guiriec, S.; Hadasch, D.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hayashi, K.; Horan, D.; Hou, X.; Hughes, R. E.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kerr, M.; Knödlseder, J.; Kuss, M.; Lande, J.; Larsson, S.; Lee, S. -H.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Makishima, K.; Mazziotta, M. N.; Mehault, J.; Mitthumsiri, W.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Naumann-Godo, M.; Nishino, S.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Okumura, A.; Orienti, M.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Pivato, G.; Porter, T. A.; Rainò, S.; Razzano, M.; Reimer, A.; Reimer, O.; Roth, M.; Sadrozinski, H. F. -W.; Sgrò, C.; Siskind, E. J.; Spandre, G.; Spinelli, P.; Strong, A. W.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Tibolla, O.; Tinivella, M.; Torres, D. F.; Tramacere, A.; Troja, E.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vianello, G.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Zimmer, S., We report on the gamma-ray observations of giant molecular clouds Orion A and B with the Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope. The gamma-ray emission in the energy band between ~100 MeV and ~100 GeV is predicted to trace the gas mass distribution in the clouds through nuclear interactions between the Galactic cosmic rays (CRs) and interstellar gas. The gamma-ray production cross-section for the nuclear interaction is known to ~10% precision which makes the LAT a powerful tool to measure the gas mass column density distribution of molecular clouds for a known CR intensity. We present here such distributions for Orion A and B, and correlate them with those of the velocity-integrated CO intensity (W _CO) at a 1° × 1° pixel level. The correlation is found to be linear over a W _CO range of ~10-fold when divided in three regions, suggesting penetration of nuclear CRs to most of the cloud volumes. The W _CO-to-mass conversion factor, X _CO, is found to be ~2.3 × 10²⁰ cm^-2(K km s^-1)^-1 for the high-longitude part of Orion A (l > 212°), ~1.7 times higher than ~1.3 × 10²⁰ found for the rest of Orion A and B. We interpret the apparent high X _CO in the high-longitude region of Orion A in the light of recent works proposing a nonlinear relation between H₂ and CO densities in the diffuse molecular gas. W _CO decreases faster than the H₂ column density in the region making the gas "darker" to W _CO....
The Astrophysical Journal, Sep. 2012

Fermi Large Area Telescope Study of Cosmic Rays and the Interstellar Medium in nearby Molecular Clouds
Ackermann, M.; Ajello, M.; Allafort, A.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bottacini, E.; Brandt, T. J.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Busetto, G.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Charles, E.; Chekhtman, A.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; D'Ammando, F.; de Angelis, A.; de Palma, F.; Dermer, C. D.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Drlica-Wagner, A.; Falletti, L.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Focke, W. B.; Fukazawa, Y.; Fukui, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Germani, S.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guiriec, S.; Hadasch, D.; Hanabata, Y.; Harding, A. K.; Hayashi, K.; Horan, D.; Hou, X.; Hughes, R. E.; Itoh, R.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Larsson, S.; Lee, S. -H.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Martin, P.; Mazziotta, M. N.; McEnery, J. E.; Mehault, J.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Naumann-Godo, M.; Nemmen, R.; Nishino, S.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Pivato, G.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Romoli, C.; Roth, M.; Sada, T.; Sadrozinski, H. F. -W.; Sanchez, D. A.; Sbarra, C.; Sgrò, C.; Siskind, E. J.; Spandre, G.; Spinelli, P.; Strong, A. W.; Suson, D. J.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Tibolla, O.; Tinivella, M.; Torres, D. F.; Tosti, G.; Tramacere, A.; Troja, E.; Uchiyama, Y.; Uehara, T.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vianello, G.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yamamoto, H.; Yang, Z.; Zimmer, S., We report an analysis of the interstellar γ-ray emission from the Chamaeleon, R Coronae Australis (R CrA), and Cepheus and Polaris flare regions with the Fermi Large Area Telescope. They are among the nearest molecular cloud complexes, within ~300 pc from the solar system. The γ-ray emission produced by interactions of cosmic rays (CRs) and interstellar gas in those molecular clouds is useful to study the CR densities and distributions of molecular gas close to the solar system. The obtained γ-ray emissivities above 250 MeV are (5.9 ± 0.1_stat ^+0.9 _-1.0sys) × 10^-27 photons s^-1 sr^-1 H-atom^-1, (10.2 ± 0.4_stat ^+1.2 _-1.7sys) × 10^-27 photons s^-1 sr^-1 H-atom^-1, and (9.1 ± 0.3_stat ^+1.5 _-0.6sys) × 10^-27 photons s^-1 sr^-1 H-atom^-1 for the Chamaeleon, R CrA, and Cepheus and Polaris flare regions, respectively. Whereas the energy dependences of the emissivities agree well with that predicted from direct CR observations at the Earth, the measured emissivities from 250 MeV to 10 GeV indicate a variation of the CR density by ~20% in the neighborhood of the solar system, even if we consider systematic uncertainties. The molecular mass calibrating ratio, X _CO = N(H₂)/W _CO, is found to be (0.96 ± 0.06_stat ^+0.15 _-0.12sys) × 10²⁰ H₂-molecule cm^-2 (K km s^-1)^-1, (0.99 ± 0.08_stat ^+0.18 _-0.10sys) × 10²⁰ H₂-molecule cm^-2 (K km s^-1)^-1, and (0.63 ± 0.02_stat ^+0.09 _-0.07sys) × 10²⁰ H₂-molecule cm^-2 (K km s^-1)^-1 for the Chamaeleon, R CrA, and Cepheus and Polaris flare regions, respectively, suggesting a variation of X _CO in the vicinity of the solar system. From the obtained values of X _CO, the masses of molecular gas traced by W _CO in the Chamaeleon, R CrA, and Cepheus and Polaris flare regions are estimated to be ~5 × 10³ M _☉, ~10³ M _☉, and ~3.3 × 10⁴ M _☉, respectively. A comparable amount of gas not traced well by standard H I and CO surveys is found in the regions investigated....
The Astrophysical Journal, Aug. 2012

GeV Observations of Star-forming Galaxies with the Fermi Large Area Telescope
Ackermann, M.; Ajello, M.; Allafort, A.; Baldini, L.; Ballet, J.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Cillis, A. N.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Cutini, S.; de Palma, F.; Dermer, C. D.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Drlica-Wagner, A.; Favuzzi, C.; Fegan, S. J.; Fortin, P.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Germani, S.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Guiriec, S.; Gustafsson, M.; Hadasch, D.; Hayashida, M.; Hays, E.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Martin, P.; Mazziotta, M. N.; McEnery, J. E.; Michelson, P. F.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nishino, S.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ozaki, M.; Parent, D.; Persic, M.; Pesce-Rollins, M.; Petrosian, V.; Pierbattista, M.; Piron, F.; Pivato, G.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Ritz, S.; Roth, M.; Sbarra, C.; Sgrò, C.; Siskind, E. J.; Spandre, G.; Spinelli, P.; Stawarz, Łukasz; Strong, A. W.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Tibaldo, L.; Tinivella, M.; Torres, D. F.; Tosti, G.; Troja, E.; Uchiyama, Y.; Vandenbroucke, J.; Vianello, G.; Vitale, V.; Waite, A. P.; Wood, M.; Yang, Z., Recent detections of the starburst galaxies M82 and NGC 253 by gamma-ray telescopes suggest that galaxies rapidly forming massive stars are more luminous at gamma-ray energies compared to their quiescent relatives. Building upon those results, we examine a sample of 69 dwarf, spiral, and luminous and ultraluminous infrared galaxies at photon energies 0.1-100 GeV using 3 years of data collected by the Large Area Telescope (LAT) on the Fermi Gamma-ray Space Telescope (Fermi). Measured fluxes from significantly detected sources and flux upper limits for the remaining galaxies are used to explore the physics of cosmic rays in galaxies. We find further evidence for quasi-linear scaling relations between gamma-ray luminosity and both radio continuum luminosity and total infrared luminosity which apply both to quiescent galaxies of the Local Group and low-redshift starburst galaxies (conservative P-values <~ 0.05 accounting for statistical and systematic uncertainties). The normalizations of these scaling relations correspond to luminosity ratios of log (L _{0.1-100 GeV}/L _{1.4 GHz}) = 1.7 ± 0.1_{(statistical)} ± 0.2_(dispersion) and log (L _{0.1-100 GeV}/L _{8-1000 μm}) = -4.3 ± 0.1_{(statistical)} ± 0.2_(dispersion) for a galaxy with a star formation rate of 1 M _☉ yr^-1, assuming a Chabrier initial mass function. Using the relationship between infrared luminosity and gamma-ray luminosity, the collective intensity of unresolved star-forming galaxies at redshifts 0 < z < 2.5 above 0.1 GeV is estimated to be 0.4-2.4 × 10^-6 ph cm^-2 s^-1 sr^-1 (4%-23% of the intensity of the isotropic diffuse component measured with the LAT). We anticipate that ~10 galaxies could be detected by their cosmic-ray-induced gamma-ray emission during a 10 year Fermi mission....
The Astrophysical Journal, Aug. 2012

A Statistical Approach to Recognizing Source Classes for Unassociated Sources in the First Fermi-LAT Catalog
Ackermann, M.; Ajello, M.; Allafort, A.; Antolini, E.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Brandt, T. J.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Chen, A. W.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Cutini, S.; de Angelis, A.; DeCesar, M. E.; De Luca, A.; de Palma, F.; Dermer, C. D.; Silva, E. do Couto e.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Enoto, T.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Focke, W. B.; Fortin, P.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Gustafsson, M.; Hadasch, D.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Healey, S. E.; Hill, A. B.; Horan, D.; Hou, X.; Jóhannesson, G.; Johnson, A. S.; Johnson, T. J.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kerr, M.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Mazziotta, M. N.; McEnery, J. E.; Mehault, J.; Michelson, P. F.; Mignani, R. P.; Mitthumsiri, W.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Naumann-Godo, M.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Pivato, G.; Porter, T. A.; Rainò, S.; Rando, R.; Ray, P. S.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Romani, R. W.; Sadrozinski, H. F. -W.; Salvetti, D.; Saz Parkinson, P. M.; Schalk, T. L.; Sgrò, C.; Shaw, M. S.; Siskind, E. J.; Smith, P. D.; Spandre, G.; Spinelli, P.; Suson, D. J.; Takahashi, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Tibolla, O.; Torres, D. F.; Tosti, G.; Tramacere, A.; Troja, E.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vianello, G.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wallace, E.; Wang, P.; Winer, B. L.; Wolff, M. T.; Wood, D. L.; Wood, K. S.; Yang, Z.; Zimmer, S., The Fermi Large Area Telescope (LAT) First Source Catalog (1FGL) provided spatial, spectral, and temporal properties for a large number of γ-ray sources using a uniform analysis method. After correlating with the most-complete catalogs of source types known to emit γ rays, 630 of these sources are "unassociated" (i.e., have no obvious counterparts at other wavelengths). Here, we employ two statistical analyses of the primary γ-ray characteristics for these unassociated sources in an effort to correlate their γ-ray properties with the active galactic nucleus (AGN) and pulsar populations in 1FGL. Based on the correlation results, we classify 221 AGN-like and 134 pulsar-like sources in the 1FGL unassociated sources. The results of these source "classifications" appear to match the expected source distributions, especially at high Galactic latitudes. While useful for planning future multiwavelength follow-up observations, these analyses use limited inputs, and their predictions should not be considered equivalent to "probable source classes" for these sources. We discuss multiwavelength results and catalog cross-correlations to date, and provide new source associations for 229 Fermi-LAT sources that had no association listed in the 1FGL catalog. By validating the source classifications against these new associations, we find that the new association matches the predicted source class in ~80% of the sources....
The Astrophysical Journal, Jul. 2012

Multi-wavelength Observations of Blazar AO 0235+164 in the 2008-2009 Flaring State
Ackermann, M.; Ajello, M.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bellazzini, R.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bottacini, E.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Charles, E.; Chekhtman, A.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cutini, S.; D'Ammando, F.; de Palma, F.; Dermer, C. D.; Silva, E. do Couto e.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Focke, W. B.; Fortin, P.; Fuhrmann, L.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Guiriec, S.; Hadasch, D.; Hayashida, M.; Hughes, R. E.; Itoh, R.; Jóhannesson, G.; Johnson, A. S.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Larsson, S.; Lee, S. -H.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Mazziotta, M. N.; McEnery, J. E.; Mehault, J.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Naumann-Godo, M.; Nishino, S.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Pelassa, V.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Pivato, G.; Porter, T. A.; Rainò, S.; Rando, R.; Rastawicki, D.; Razzano, M.; Readhead, A.; Reimer, A.; Reimer, O.; Reyes, L. C.; Richards, J. L.; Sbarra, C.; Sgrò, C.; Siskind, E. J.; Spandre, G.; Spinelli, P.; Szostek, A.; Takahashi, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Thompson, D. J.; Tinivella, M.; Torres, D. F.; Tosti, G.; Troja, E.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vianello, G.; Vitale, V.; Waite, A. P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Zimmer, S.; Fermi-LAT Collaboration; Moderski, R.; Nalewajko, K.; Sikora, M.; Villata, M.; Raiteri, C. M.; Aller, H. D.; Aller, M. F.; Arkharov, A. A.; Benítez, E.; Berdyugin, A.; Blinov, D. A.; Boettcher, M.; Bravo Calle, O. J. A.; Buemi, C. S.; Carosati, D.; Chen, W. P.; Diltz, C.; Di Paola, A.; Dolci, M.; Efimova, N. V.; Forné, E.; Gurwell, M. A.; Heidt, J.; Hiriart, D.; Jordan, B.; Kimeridze, G.; Konstantinova, T. S.; Kopatskaya, E. N.; Koptelova, E.; Kurtanidze, O. M.; Lähteenmäki, A.; Larionova, E. G.; Larionova, L. V.; Larionov, V. M.; Leto, P.; Lindfors, E.; Lin, H. C.; Morozova, D. A.; Nikolashvili, M. G.; Nilsson, K.; Oksman, M.; Roustazadeh, P.; Sievers, A.; Sigua, L. A.; Sillanpää, A.; Takahashi, T.; Takalo, L. O.; Tornikoski, M.; Trigilio, C.; Troitsky, I. S.; Umana, G.; GASP-WEBT Consortium; Angelakis, E.; Krichbaum, T. P.; Nestoras, I.; Riquelme, D.; F-GAMMA; Krips, M.; Trippe, S.; Iram-PdBI; Arai, A.; Kawabata, K. S.; Sakimoto, K.; Sasada, M.; Sato, S.; Uemura, M.; Yamanaka, M.; Yoshida, M.; Kanata; Belloni, T.; Tagliaferri, G.; RXTE; Bonning, E. W.; Isler, J.; Urry, C. M.; SMARTS; Hoversten, E.; Falcone, A.; Pagani, C.; Stroh, M.; (Swift-XRT, The blazar AO 0235+164 (z = 0.94) has been one of the most active objects observed by Fermi Large Area Telescope (LAT) since its launch in Summer 2008. In addition to the continuous coverage by Fermi, contemporaneous observations were carried out from the radio to γ-ray bands between 2008 September and 2009 February. In this paper, we summarize the rich multi-wavelength data collected during the campaign (including F-GAMMA, GASP-WEBT, Kanata, OVRO, RXTE, SMARTS, Swift, and other instruments), examine the cross-correlation between the light curves measured in the different energy bands, and interpret the resulting spectral energy distributions in the context of well-known blazar emission models. We find that the γ-ray activity is well correlated with a series of near-IR/optical flares, accompanied by an increase in the optical polarization degree. On the other hand, the X-ray light curve shows a distinct 20 day high state of unusually soft spectrum, which does not match the extrapolation of the optical/UV synchrotron spectrum. We tentatively interpret this feature as the bulk Compton emission by cold electrons contained in the jet, which requires an accretion disk corona with an effective covering factor of 19% at a distance of 100 R _g. We model the broadband spectra with a leptonic model with external radiation dominated by the infrared emission from the dusty torus....
The Astrophysical Journal, Jun. 2012

超新星残骸の折れ曲がったガンマ線スペクトルについての研究
花畑 義隆; 片桐 秀明, 日本天文学会
天文月報, 20 May 2012, [Reviewed]

Fermi-LAT Observations of the Diffuse γ-Ray Emission: Implications for Cosmic Rays and the Interstellar Medium
Ackermann, M.; Ajello, M.; Atwood, W. B.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Brandt, T. J.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Cavazzuti, E.; Cecchi, C.; Charles, E.; Chekhtman, A.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Cutini, S.; de Angelis, A.; de Palma, F.; Dermer, C. D.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Drlica-Wagner, A.; Falletti, L.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Focke, W. B.; Fortin, P.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gaggero, D.; Gargano, F.; Germani, S.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grove, J. E.; Guiriec, S.; Gustafsson, M.; Hadasch, D.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Horan, D.; Hou, X.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Mazziotta, M. N.; McEnery, J. E.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Naumann-Godo, M.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J. H.; Parent, D.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Pivato, G.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Razzaque, S.; Reimer, A.; Reimer, O.; Sadrozinski, H. F. -W.; Sgrò, C.; Siskind, E. J.; Spandre, G.; Spinelli, P.; Strong, A. W.; Suson, D. J.; Takahashi, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Tinivella, M.; Torres, D. F.; Tosti, G.; Troja, E.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vianello, G.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Wood, M.; Yang, Z.; Ziegler, M.; Zimmer, S., The γ-ray sky >100 MeV is dominated by the diffuse emissions from interactions of cosmic rays with the interstellar gas and radiation fields of the Milky Way. Observations of these diffuse emissions provide a tool to study cosmic-ray origin and propagation, and the interstellar medium. We present measurements from the first 21 months of the Fermi Large Area Telescope (Fermi-LAT) mission and compare with models of the diffuse γ-ray emission generated using the GALPROP code. The models are fitted to cosmic-ray data and incorporate astrophysical input for the distribution of cosmic-ray sources, interstellar gas, and radiation fields. To assess uncertainties associated with the astrophysical input, a grid of models is created by varying within observational limits the distribution of cosmic-ray sources, the size of the cosmic-ray confinement volume (halo), and the distribution of interstellar gas. An all-sky maximum-likelihood fit is used to determine the X _CO factor, the ratio between integrated CO-line intensity and H₂ column density, the fluxes and spectra of the γ-ray point sources from the first Fermi-LAT catalog, and the intensity and spectrum of the isotropic background including residual cosmic rays that were misclassified as γ-rays, all of which have some dependency on the assumed diffuse emission model. The models are compared on the basis of their maximum-likelihood ratios as well as spectra, longitude, and latitude profiles. We also provide residual maps for the data following subtraction of the diffuse emission models. The models are consistent with the data at high and intermediate latitudes but underpredict the data in the inner Galaxy for energies above a few GeV. Possible explanations for this discrepancy are discussed, including the contribution by undetected point-source populations and spectral variations of cosmic rays throughout the Galaxy. In the outer Galaxy, we find that the data prefer models with a flatter distribution of cosmic-ray sources, a larger cosmic-ray halo, or greater gas density than is usually assumed. Our results in the outer Galaxy are consistent with other Fermi-LAT studies of this region that used different analysis methods than employed in this paper....
The Astrophysical Journal, May 2012

Fermi Large Area Telescope Second Source Catalog
Nolan, P. L.; Abdo, A. A.; Ackermann, M.; Ajello, M.; Allafort, A.; Antolini, E.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Belfiore, A.; Bellazzini, R.; Berenji, B.; Bignami, G. F.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Bonnell, J.; Borgland, A. W.; Bottacini, E.; Bouvier, A.; Brandt, T. J.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Campana, R.; Cañadas, B.; Cannon, A.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Ceccanti, M.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Chipaux, R.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cominsky, L. R.; Conrad, J.; Corbet, R.; Cutini, S.; D'Ammando, F.; Davis, D. S.; de Angelis, A.; DeCesar, M. E.; DeKlotz, M.; De Luca, A.; den Hartog, P. R.; de Palma, F.; Dermer, C. D.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Dumora, D.; Enoto, T.; Escande, L.; Fabiani, D.; Falletti, L.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Gustafsson, M.; Hadasch, D.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Hill, A. B.; Horan, D.; Hou, X.; Hughes, R. E.; Iafrate, G.; Itoh, R.; Jóhannesson, G.; Johnson, R. P.; Johnson, T. E.; Johnson, A. S.; Johnson, T. J.; Kamae, T.; Katagiri, H.; Kataoka, J.; Katsuta, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocevski, D.; Kuss, M.; Lande, J.; Landriu, D.; Latronico, L.; Lemoine-Goumard, M.; Lionetto, A. M.; Llena Garde, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Marelli, M.; Massaro, E.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Mehault, J.; Michelson, P. F.; Minuti, M.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Mongelli, M.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Naumann-Godo, M.; Norris, J. P.; Nuss, E.; Nymark, T.; Ohno, M.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Perkins, J. S.; Pesce-Rollins, M.; Pierbattista, M.; Pinchera, M.; Piron, F.; Pivato, G.; Porter, T. A.; Racusin, J. L.; Rainò, S.; Rando, R.; Razzano, M.; Razzaque, S.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rochester, L. S.; Romani, R. W.; Roth, M.; Rousseau, R.; Ryde, F.; Sadrozinski, H. F. -W.; Salvetti, D.; Sanchez, D. A.; Saz Parkinson, P. M.; Sbarra, C.; Scargle, J. D.; Schalk, T. L.; Sgrò, C.; Shaw, M. S.; Shrader, C.; Siskind, E. J.; Smith, D. A.; Spandre, G.; Spinelli, P.; Stephens, T. E.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Tibolla, O.; Tinebra, F.; Tinivella, M.; Torres, D. F.; Tosti, G.; Troja, E.; Uchiyama, Y.; Vandenbroucke, J.; Van Etten, A.; Van Klaveren, B.; Vasileiou, V.; Vianello, G.; Vitale, V.; Waite, A. P.; Wallace, E.; Wang, P.; Werner, M.; Winer, B. L.; Wood, D. L.; Wood, K. S.; Wood, M.; Yang, Z.; Zimmer, S., We present the second catalog of high-energy γ-ray sources detected by the Large Area Telescope (LAT), the primary science instrument on the Fermi Gamma-ray Space Telescope (Fermi), derived from data taken during the first 24 months of the science phase of the mission, which began on 2008 August 4. Source detection is based on the average flux over the 24 month period. The second Fermi-LAT catalog (2FGL) includes source location regions, defined in terms of elliptical fits to the 95% confidence regions and spectral fits in terms of power-law, exponentially cutoff power-law, or log-normal forms. Also included are flux measurements in five energy bands and light curves on monthly intervals for each source. Twelve sources in the catalog are modeled as spatially extended. We provide a detailed comparison of the results from this catalog with those from the first Fermi-LAT catalog (1FGL). Although the diffuse Galactic and isotropic models used in the 2FGL analysis are improved compared to the 1FGL catalog, we attach caution flags to 162 of the sources to indicate possible confusion with residual imperfections in the diffuse model. The 2FGL catalog contains 1873 sources detected and characterized in the 100 MeV to 100 GeV range of which we consider 127 as being firmly identified and 1171 as being reliably associated with counterparts of known or likely γ-ray-producing source classes. We dedicate this paper to the memory of our colleague Patrick Nolan, who died on 2011 November 6. His career spanned much of the history of high-energy astronomy from space and his work on the Large Area Telescope (LAT) began nearly 20 years ago when it was just a concept. Pat was a central member in the operation of the LAT collaboration and he is greatly missed....
The Astrophysical Journal Supplement Series, Apr. 2012

Search for Gamma-ray Emission from X-Ray-selected Seyfert Galaxies with Fermi-LAT
Ackermann, M.; Ajello, M.; Allafort, A.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Cutini, S.; D'Ammando, F.; de Angelis, A.; de Palma, F.; Dermer, C. D.; Silva, E. do Couto e.; Drell, P. S.; Drlica-Wagner, A.; Enoto, T.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Fortin, P.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Godfrey, G.; Grove, J. E.; Guiriec, S.; Hadasch, D.; Hayashida, M.; Hays, E.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Llena Garde, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Mazziotta, M. N.; Michelson, P. F.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nishino, S.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Okumura, A.; Orlando, E.; Ozaki, M.; Paneque, D.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Pivato, G.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Ritz, S.; Roth, M.; Sanchez, D. A.; Sbarra, C.; Sgrò, C.; Siskind, E. J.; Spandre, G.; Spinelli, P.; Stawarz, Ł.; Strong, A. W.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Tinivella, M.; Torres, D. F.; Tosti, G.; Troja, E.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vianello, G.; Vitale, V.; Waite, A. P.; Winer, B. L.; Wood, K. S.; Wood, M.; Yang, Z.; Zimmer, S., We report on a systematic investigation of the γ-ray properties of 120 hard X-ray-selected Seyfert galaxies classified as "radio-quiet" objects, utilizing the three-year accumulation of Fermi Large Area Telescope (LAT) data. Our sample of Seyfert galaxies is selected using the Swift Burst Alert Telescope 58 month catalog, restricting the analysis to the bright sources with average hard X-ray fluxes F _{14 - 195 keV} >= 2.5 × 10^-11 erg cm^-2 s^-1 at high Galactic latitudes (|b| > 10°). In order to remove "radio-loud" objects from the sample, we use the "hard X-ray radio loudness parameter," R _rX, defined as the ratio of the total 1.4 GHz radio to 14-195 keV hard X-ray energy fluxes. Among 120 X-ray bright Seyfert galaxies with R _rX <10^-4, we did not find a statistically significant γ-ray excess (TS > 25) positionally coincident with any target Seyferts, with possible exceptions of ESO 323-G077 and NGC 6814. The mean value of the 95% confidence level γ-ray upper limit for the integrated photon flux above 100 MeV from the analyzed Seyferts is ~= 4 × 10^-9 photons cm^-2 s^-1 , and the upper limits derived for several objects reach ~= 1 × 10^-9 photons cm^-2 s^-1 . Our results indicate that no prominent γ-ray emission component related to active galactic nucleus activity is present in the spectra of Seyferts around GeV energies. The Fermi-LAT upper limits derived for our sample probe the ratio of γ-ray to X-ray luminosities L _γ/L _X < 0.1, and even <0.01 in some cases. The obtained results impose novel constraints on the models for high-energy radiation of "radio-quiet" Seyfert galaxies....
The Astrophysical Journal, Mar. 2012

Search for Dark Matter Satellites Using Fermi-LAT
Ackermann, M.; Albert, A.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bottacini, E.; Brandt, T. J.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Charles, E.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Cutini, S.; de Palma, F.; Dermer, C. D.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Drlica-Wagner, A.; Essig, R.; Falletti, L.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Germani, S.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Guiriec, S.; Gustafsson, M.; Hadasch, D.; Hayashida, M.; Hou, X.; Hughes, R. E.; Johnson, R. P.; Johnson, A. S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Lionetto, A. M.; Llena Garde, M.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Mazziotta, M. N.; McEnery, J. E.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Naumann-Godo, M.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Pelassa, V.; Pierbattista, M.; Piron, F.; Pivato, G.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Ritz, S.; Sadrozinski, H. F. -W.; Sehgal, N.; Sgrò, C.; Siskind, E. J.; Spinelli, P.; Strigari, L.; Suson, D. J.; Tajima, H.; Takahashi, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Tinivella, M.; Torres, D. F.; Troja, E.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vianello, G.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Zalewski, S.; Zimmer, S., Numerical simulations based on the ΛCDM model of cosmology predict a large number of as yet unobserved Galactic dark matter satellites. We report the results of a Large Area Telescope (LAT) search for these satellites via the γ-ray emission expected from the annihilation of weakly interacting massive particle (WIMP) dark matter. Some dark matter satellites are expected to have hard γ-ray spectra, finite angular extents, and a lack of counterparts at other wavelengths. We sought to identify LAT sources with these characteristics, focusing on γ-ray spectra consistent with WIMP annihilation through the b \bar{b} channel. We found no viable dark matter satellite candidates using one year of data, and we present a framework for interpreting this result in the context of numerical simulations to constrain the velocity-averaged annihilation cross section for a conventional 100 GeV WIMP annihilating through the b \bar{b} channel....
The Astrophysical Journal, Mar. 2012

The cosmic-ray and gas content of the Cygnus region as measured in γ-rays by the Fermi Large Area Telescope
Ackermann, M.; Ajello, M.; Allafort, A.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Belfiore, A.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bottacini, E.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Chekhtman, A.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; de Angelis, A.; de Palma, F.; Dermer, C. D.; Silva, E. Do Couto E.; Drell, P. S.; Dumora, D.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fortin, P.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Germani, S.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Guillemot, L.; Guiriec, S.; Hadasch, D.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hayashi, K.; Hays, E.; Jóhannesson, G.; Johnson, A. S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kerr, M.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Martin, P.; Mazziotta, M. N.; McEnery, J. E.; Mehault, J.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Naumann-Godo, M.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Parent, D.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, O.; Reposeur, T.; Ritz, S.; Saz Parkinson, P. M.; Sgrò, C.; Siskind, E. J.; Smith, P. D.; Spinelli, P.; Strong, A. W.; Takahashi, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Troja, E.; Uchiyama, Y.; Vandenbroucke, J.; Vasileiou, V.; Vianello, G.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Zimmer, S.; Bontemps, S., Context. The Cygnus region hosts a giant molecular-cloud complex that actively forms massive stars. Interactions of cosmic rays with interstellar gas and radiation fields make it shine at γ-ray energies. Several γ-ray pulsars and other energetic sources are seen in this direction.
Aims: In this paper we analyze the γ-ray emission measured by the Fermi Large Area Telescope (LAT) in the energy range from 100 MeV to 100 GeV in order to probe the gas and cosmic-ray content on the scale of the whole Cygnus complex. The γ-ray emission on the scale of the central massive stellar clusters and from individual sources is addressed elsewhere.
Methods: The signal from bright pulsars is greatly reduced by selecting photons in their off-pulse phase intervals. We compare the diffuse γ-ray emission with interstellar gas maps derived from radio/mm-wave lines and visual extinction data. A general model of the region, including other pulsars and γ-ray sources, is sought.
Results: The integral H i emissivity above 100 MeV averaged over the whole Cygnus complex amounts to [2.06 ± 0.11 (stat.) _-0.84^+0.15(syst.)] × 10^-26 photons s^-1 sr^-1 H-atom^-1, where the systematic error is dominated by the uncertainty on the H i opacity to calculate its column densities. The integral emissivity and its spectral energy distribution are both consistent within the systematics with LAT measurements in the interstellar space near the solar system. The average X_CO = N(H₂)/W_CO ratio is found to be [1.68 ± 0.05 (stat.) _-0.10^+0.87(HI opacity)] × 10²⁰ molecules cm^-2 (K km s^-1)^-1, consistent with other LAT measurements in the Local Arm. We detect significant γ-ray emission from dark neutral gas for a mass corresponding to ~40% of what is traced by CO. The total interstellar mass in the Cygnus complex inferred from its γ-ray emission amounts to 8_-1⁺⁵ × 10⁶ M_☉ at a distance of 1.4 kpc.
Conclusions: Despite the conspicuous star formation activity and high masses of the interstellar clouds, the cosmic-ray population in the Cygnus complex averaged over a few hundred parsecs is similar to that of the local interstellar space....
Astronomy and Astrophysics, Feb. 2012

Limits on large extra dimensions based on observations of neutron stars with the Fermi-LAT
Fermi-LAT Collaboration; Ajello, M.; Baldini, L.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Charles, E.; Chekhtman, A.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Cutini, S.; de Angelis, A.; de Palma, F.; Dermer, C. D.; Silva, E. do Couto e.; Drell, P. S.; Drlica-Wagner, A.; Enoto, T.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Gasparrini, D.; Germani, S.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Graham, P.; Grenier, I. A.; Guiriec, S.; Gustafsson, M.; Hadasch, D.; Hayashida, M.; Hughes, R. E.; Johnson, A. S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lionetto, A. M.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Mazziotta, M. N.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Pivato, G.; Rainò, S.; Razzano, M.; Ritz, S.; Roth, M.; Saz Parkinson, P. M.; Scargle, J. D.; Schalk, T. L.; Sgrò, C.; Siskind, E. J.; Spandre, G.; Spinelli, P.; Suson, D. J.; Tajima, H.; Takahashi, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Tinivella, M.; Torres, D. F.; Troja, E.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vianello, G.; Vitale, V.; Waite, A. P.; Winer, B. L.; Wood, K. S.; Wood, M.; Yang, Z.; Zimmer, S., We present limits for the compactification scale in the theory of Large Extra Dimensions (LED) proposed by Arkani-Hamed, Dimopoulos, and Dvali. We use 11 months of data from the Fermi Large Area Telescope (Fermi-LAT) to set gamma ray flux limits for 6 gamma-ray faint neutron stars (NS). To set limits on LED we use the model of Hannestad and Raffelt (HR) that calculates the Kaluza-Klein (KK) graviton production in supernova cores and the large fraction subsequently gravitationally bound around the resulting NS. The predicted decay of the bound KK gravitons to γγ should contribute to the flux from NSs. Considering 2 to 7 extra dimensions of the same size in the context of the HR model, we use Monte Carlo techniques to calculate the expected differential flux of gamma-rays arising from these KK gravitons, including the effects of the age of the NS, graviton orbit, and absorption of gamma-rays in the magnetosphere of the NS. We compare our Monte Carlo-based differential flux to the experimental differential flux using maximum likelihood techniques to obtain our limits on LED. Our limits are more restrictive than past EGRET-based optimistic limits that do not include these important corrections. Additionally, our limits are more stringent than LHC based limits for 3 or fewer LED, and comparable for 4 LED. We conclude that if the effective Planck scale is around a TeV, then for 2 or 3 LED the compactification topology must be more complicated than a torus....
Journal of Cosmology and Astroparticle Physics, Feb. 2012

FERMI LARGE AREA TELESCOPE OBSERVATIONS OF THE SUPERNOVA REMNANT G8.7-0.1
M. Ajello; A. Allafort; L. Baldini; J. Ballet; G. Barbiellini; D. Bastieri; K. Bechtol; R. Bellazzini; B. Berenji; R. D. Blandford; E. D. Bloom; E. Bonamente; A. W. Borgland; J. Bregeon; M. Brigida; P. Bruel; R. Buehler; S. Buson; G. A. Caliandro; R. A. Cameron; P. A. Caraveo; J. M. Casandjian; C. Cecchi; E. Charles; A. Chekhtman; S. Ciprini; R. Claus; J. Cohen-Tanugi; S. Cutini; A. de Angelis; F. de Palma; C. D. Dermer; E. do Couto e Silva; P. S. Drell; A. Drlica-Wagner; R. Dubois; C. Favuzzi; S. J. Fegan; E. C. Ferrara; W. B. Focke; M. Frailis; Y. Fukazawa; Y. Fukui; P. Fusco; F. Gargano; D. Gasparrini; S. Germani; N. Giglietto; P. Giommi; F. Giordano; M. Giroletti; T. Glanzman; G. Godfrey; J. E. Grove; S. Guiriec; D. Hadasch; Y. Hanabata; A. K. Harding; K. Hayashi; E. Hays; R. Itoh; G. Johannesson; A. S. Johnson; T. Kamae; H. Katagiri; J. Kataoka; J. Knoedlseder; H. Kubo; M. Kuss; J. Lande; L. Latronico; S. -H. Lee; A. M. Lionetto; F. Longo; F. Loparco; M. N. Lovellette; P. Lubrano; M. N. Mazziotta; J. Mehault; P. F. Michelson; T. Mizuno; A. A. Moiseev; C. Monte; M. E. Monzani; A. Morselli; I. V. Moskalenko; S. Murgia; T. Nakamori; M. Naumann-Godo; S. Nishino; P. L. Nolan; J. P. Norris; E. Nuss; M. Ohno; T. Ohsugi; A. Okumura; N. Omodei; E. Orlando; J. F. Ormes; D. Paneque; D. Parent; V. Pelassa; M. Pesce-Rollins; M. Pierbattista; F. Piron; T. A. Porter; S. Raino; R. Rando; A. Reimer; O. Reimer; T. Reposeur; M. Roth; H. F. -W. Sadrozinski; C. Sgro; E. J. Siskind; P. D. Smith; G. Spandre; P. Spinelli; D. J. Suson; H. Tajima; H. Takahashi; T. Tanaka; J. G. Thayer; J. B. Thayer; L. Tibaldo; O. Tibolla; D. F. Torres; G. Tosti; A. Tramacere; E. Troja; Y. Uchiyama; T. Uehara; T. L. Usher; J. Vandenbroucke; A. Van Etten; V. Vasileiou; G. Vianello; N. Vilchez; V. Vitale; A. P. Waite; P. Wang; B. L. Winer; K. S. Wood; H. Yamamoto; R. Yamazaki; Z. Yang; H. Yasuda; M. Ziegler; S. Zimmer, We present a detailed analysis of the GeV gamma-ray emission toward the supernova remnant (SNR) G8.7-0.1 with the Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope. An investigation of the relationship between G8.7-0.1 and the TeV unidentified source HESS J1804-216 provides us with an important clue on diffusion process of cosmic rays if particle acceleration operates in the SNR. The GeV gamma-ray emission is extended with most of the emission in positional coincidence with the SNR G8.7-0.1 and a lesser part located outside the western boundary of G8.7-0.1. The region of the gamma-ray emission overlaps spatially connected molecular clouds, implying a physical connection for the gamma-ray structure. The total gamma-ray spectrum measured with LAT from 200 MeV-100 GeV can be described by a broken power-law function with a break of 2.4 +/- 0.6 (stat) +/- 1.2 (sys) GeV, and photon indices of 2.10 +/- 0.06 (stat) +/- 0.10 (sys) below the break and 2.70 +/- 0.12 (stat) +/- 0.14 (sys) above the break. Given the spatial association among the gamma rays, the radio emission of G8.7-0.1, and the molecular clouds, the decay of pi(0)s produced by particles accelerated in the SNR and hitting the molecular clouds naturally explains the GeV gamma-ray spectrum. We also find that the GeV morphology is not well represented by the TeV emission from HESS J1804-216 and that the spectrum in the GeV band is not consistent with the extrapolation of the TeV gamma-ray spectrum. The spectral index of the TeV emission is consistent with the particle spectral index predicted by a theory that assumes energy-dependent diffusion of particles accelerated in an SNR. We discuss the possibility that the TeV spectrum originates from the interaction of particles accelerated in G8.7-0.1 with molecular clouds, and we constrain the diffusion coefficient of the particles., IOP PUBLISHING LTD
ASTROPHYSICAL JOURNAL, Jan. 2012, [Reviewed]

Measurement of Separate Cosmic-Ray Electron and Positron Spectra with the Fermi Large Area Telescope
Ackermann, M.; Ajello, M.; Allafort, A.; Atwood, W. B.; Baldini, L.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Cutini, S.; de Angelis, A.; de Palma, F.; Dermer, C. D.; Digel, S. W.; Do Couto E Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Focke, W. B.; Fortin, P.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Germani, S.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grove, J. E.; Guiriec, S.; Gustafsson, M.; Hadasch, D.; Harding, A. K.; Hayashida, M.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Llena Garde, M.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Mazziotta, M. N.; McEnery, J. E.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Parent, D.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Pivato, G.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Razzaque, S.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Romani, R. W.; Roth, M.; Sadrozinski, H. F. -W.; Sbarra, C.; Schalk, T. L.; Sgrò, C.; Siskind, E. J.; Spandre, G.; Spinelli, P.; Strong, A. W.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Tinivella, M.; Torres, D. F.; Tosti, G.; Troja, E.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vianello, G.; Vitale, V.; Waite, A. P.; Winer, B. L.; Wood, K. S.; Wood, M.; Yang, Z.; Zimmer, S., We measured separate cosmic-ray electron and positron spectra with the Fermi Large Area Telescope. Because the instrument does not have an onboard magnet, we distinguish the two species by exploiting Earth’s shadow, which is offset in opposite directions for opposite charges due to Earth’s magnetic field. We estimate and subtract the cosmic-ray proton background using two different methods that produce consistent results. We report the electron-only spectrum, the positron-only spectrum, and the positron fraction between 20 and 200 GeV. We confirm that the fraction rises with energy in the 20-100 GeV range. The three new spectral points between 100 and 200 GeV are consistent with a fraction that is continuing to rise with energy....
Physical Review Letters, Jan. 2012

Periodic Emission from the Gamma-Ray Binary 1FGL J1018.6-5856
Fermi LAT Collaboration; Ackermann, M.; Ajello, M.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Belfiore, A.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chaty, S.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini; , S.; Claus, R.; Cohen-Tanugi, J.; Corbel, S.; Corbet, R. H. D.; Cutini, S.; de Luca, A.; den Hartog, P. R.; de Palma, F.; Dermer, C. D.; Digel, S. W.; do Couto e Silva, E.; Donato, D.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Dubus, G.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Focke, W. B.; Fortin, P.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grove, J. E.; Guiriec, S.; Hadasch, D.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Hill, A. B.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, T. J.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kerr, M.; Knödlseder, J.; Kuss, M.; Lande, J.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Mazziotta, M. N.; McEnery, J. E.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Naumann-Godo, M.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ozaki, M.; Paneque, D.; Parent, D.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Pivato, G.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Ritz, S.; Romani, R. W.; Roth, M.; Saz Parkinson, P. M.; Sgrò, C.; Siskind, E. J.; Spandre, G.; Spinelli, P.; Suson, D. J.; Takahashi, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Tinivella, M.; Torres, D. F.; Tosti, G.; Troja, E.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Vitale, V.; Waite, A. P.; Winer, B. L.; Wood, K. S.; Wood, M.; Yang, Z.; Zimmer, S.; Coe, M. J.; Di Mille, F.; Edwards, P. G.; Filipović, M. D.; Payne, J. L.; Stevens, J.; Torres, M. A. P., Gamma-ray binaries are stellar systems containing a neutron star or black hole, with gamma-ray emission produced by an interaction between the components. These systems are rare, even though binary evolution models predict dozens in our Galaxy. A search for gamma-ray binaries with the Fermi Large Area Telescope (LAT) shows that 1FGL J1018.6-5856 exhibits intensity and spectral modulation with a 16.6-day period. We identified a variable x-ray counterpart, which shows a sharp maximum coinciding with maximum gamma-ray emission, as well as an O6V((f)) star optical counterpart and a radio counterpart that is also apparently modulated on the orbital period. 1FGL J1018.6-5856 is thus a gamma-ray binary, and its detection suggests the presence of other fainter binaries in the Galaxy....
Science, Jan. 2012

25pFB-1 Development of the PMP-waveform sampling circuit using an analog memory for the CTA project
Konno Yusuke; CTA-Japan consortium; Open-It, The Physical Society of Japan
Meeting Abstracts of the Physical Society of Japan, 2012

24pGK-8 CTA35 : Development of readout circuits for LST
Hagiwara Ryouta, The Physical Society of Japan
Meeting Abstracts of the Physical Society of Japan, 2012

13pSP-7 CTA44 : Development of readout circuits for LST
Hagiwara Ryouta, The Physical Society of Japan
Meeting Abstracts of the Physical Society of Japan, 2012

In-flight measurement of the absolute energy scale of the Fermi Large Area Telescope
M. Ackermann; M. Ajello; A. Allafort; W.B. Atwood; M. Axelsson; L. Baldini; G. Barbiellini; D. Bastieri; K. Bechtol; R. Bellazzini; B. Berenji; E.D. Bloom; E. Bonamente; A.W. Borgland; A. Bouvier; J. Bregeon; A. Brez; M. Brigida; P. Bruel; R. Buehler; S. Buson; G.A. Caliandro; R.A. Cameron; P.A. Caraveo; J.M. Casandjian; C. Cecchi; E. Charles; A. Chekhtman; J. Chiang; S. Ciprini; R. Claus; J. Cohen-Tanugi; S. Cutini; F. De Palma; C.D. Dermer; S.W. Digel; E. Do Couto E Silva; P.S. Drell; A. Drlica-Wagner; R. Dubois; T. Enoto; L. Falletti; C. Favuzzi; S.J. Fegan; W.B. Focke; P. Fortin; Y. Fukazawa; S. Funk; P. Fusco; F. Gargano; N. Gehrels; S. Germani; N. Giglietto; F. Giordano; M. Giroletti; T. Glanzman; G. Godfrey; I.A. Grenier; J.E. Grove; S. Guiriec; D. Hadasch; M. Hayashida; E. Hays; R.E. Hughes; G. Jóhannesson; A.S. Johnson; T.J. Johnson; T. Kamae; H. Katagiri; J. Kataoka; J. Knödlseder; M. Kuss; J. Lande; L. Latronico; S.-H. Lee; F. Longo; F. Loparco; M.N. Lovellette; P. Lubrano; G.M. Madejski; M.N. Mazziotta; J.E. McEnery; P.F. Michelson; T. Mizuno; A.A. Moiseev; C. Monte; M.E. Monzani; A. Morselli; I.V. Moskalenko; S. Murgia; T. Nakamori; M. Naumann-Godo; P.L. Nolan; J.P. Norris; E. Nuss; T. Ohsugi; A. Okumura; N. Omodei; E. Orlando; J.F. Ormes; M. Ozaki; D. Paneque; J.H. Panetta; D. Parent; M. Pesce-Rollins; M. Pierbattista; F. Piron; S. Rain; R. Rando; M. Razzano; A. Reimer; O. Reimer; T. Reposeur; S. Ritz; L.S. Rochester; C. Sgr; E.J. Siskind; P.D. Smith; G. Spandre; P. Spinelli; D.J. Suson; H. Takahashi; T. Tanaka; J.G. Thayer; J.B. Thayer; D.J. Thompson; L. Tibaldo; G. Tosti; E. Troja; T.L. Usher; J. Vandenbroucke; V. Vasileiou; G. Vianello; N. Vilchez; V. Vitale; A.P. Waite; P. Wang; B.L. Winer; K.S. Wood; Z. Yang; S. Zimmer, The Large Area Telescope (LAT) on-board the Fermi Gamma-ray Space Telescope is a pair-conversion telescope designed to survey the gamma-ray sky from 20 MeV to several hundreds of GeV. In this energy band there are no astronomical sources with sufficiently well known and sharp spectral features to allow an absolute calibration of the LAT energy scale. However, the geomagnetic cutoff in the cosmic ray electron-plus-positron (CRE) spectrum in low Earth orbit does provide such a spectral feature. The energy and spectral shape of this cutoff can be calculated with the aid of a numerical code tracing charged particles in the Earth's magnetic field. By comparing the cutoff value with that measured by the LAT in different geomagnetic positions, we have obtained several calibration points between ∼6 and ∼13 GeV with an estimated uncertainty of ∼2%. An energy calibration with such high accuracy reduces the systematic uncertainty in LAT measurements of, for example, the spectral cutoff in the emission from gamma ray pulsars. © 2011 Elsevier B.V. All rights reserved.
Astroparticle Physics, Jan. 2012, [Reviewed]

Fermi Large Area Telescope Discovery of GeV Gamma-Ray Emission from the Vicinity of SNR W44
Yasunobu Uchiyama; Stefan Funk; Hideaki Katagiri; Junichiro Katsuta; Marianne Lemoine-Goumard; Hiroyasu Tajima; Takaaki Tanaka; Diego F. Torres, We report the detection of GeV gamma-ray emission from the molecular cloud complex that surrounds the supernova remnant (SNR) W44 using the Large Area Telescope on board Fermi. While the previously reported gamma-ray emission from SNR W44 is likely to arise from the dense radio-emitting filaments within the remnant, the gamma-ray emission that appears to come from the surrounding molecular cloud complex can be ascribed to the cosmic rays (CRs) that have escaped from W44. The non-detection of synchrotron radio emission associated with the molecular cloud complex suggests the decay of pi(0) mesons produced in hadronic collisions as the gamma-ray emission mechanism. The total kinetic energy channeled into the escaping CRs is estimated to be W-esc similar to (0.3-3) x 10(50) erg, in broad agreement with the conjecture that SNRs are the main sources of Galactic CRs., IOP PUBLISHING LTD
The Astrophysical Journal Letters, 2012

The Second Catalog of Active Galactic Nuclei Detected by the Fermi Large Area Telescope
Ackermann, M.; Ajello, M.; Allafort, A.; Antolini, E.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bottacini, E.; Bouvier, A.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Charles, E.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Costamante, L.; Cutini, S.; de Angelis, A.; de Palma, F.; Dermer, C. D.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Escande, L.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Finke, J.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grove, J. E.; Guiriec, S.; Gustafsson, M.; Hadasch, D.; Hayashida, M.; Hays, E.; Healey, S. E.; Horan, D.; Hou, X.; Hughes, R. E.; Iafrate, G.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Larsson, S.; Latronico, L.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Naumann-Godo, M.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orienti, M.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Parent, D.; Pesce-Rollins, M.; Pierbattista, M.; Piranomonte, S.; Piron, F.; Pivato, G.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Razzaque, S.; Reimer, A.; Reimer, O.; Ritz, S.; Rochester, L. S.; Romani, R. W.; Roth, M.; Sanchez, D. A.; Sbarra, C.; Scargle, J. D.; Schalk, T. L.; Sgrò, C.; Shaw, M. S.; Siskind, E. J.; Spandre, G.; Spinelli, P.; Strong, A. W.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Tinivella, M.; Torres, D. F.; Tosti, G.; Troja, E.; Uchiyama, Y.; Vandenbroucke, J.; Vasileiou, V.; Vianello, G.; Vitale, V.; Waite, A. P.; Wallace, E.; Wang, P.; Winer, B. L.; Wood, D. L.; Wood, K. S.; Zimmer, S., The second catalog of active galactic nuclei (AGNs) detected by the Fermi Large Area Telescope (LAT) in two years of scientific operation is presented. The second LAT AGN catalog (2LAC) includes 1017 γ-ray sources located at high Galactic latitudes (|b| > 10°) that are detected with a test statistic (TS) greater than 25 and associated statistically with AGNs. However, some of these are affected by analysis issues and some are associated with multiple AGNs. Consequently, we define a Clean Sample which includes 886 AGNs, comprising 395 BL Lacertae objects (BL Lac objects), 310 flat-spectrum radio quasars (FSRQs), 157 candidate blazars of unknown type (i.e., with broadband blazar characteristics but with no optical spectral measurement yet), 8 misaligned AGNs, 4 narrow-line Seyfert 1 (NLS1s), 10 AGNs of other types, and 2 starburst galaxies. Where possible, the blazars have been further classified based on their spectral energy distributions (SEDs) as archival radio, optical, and X-ray data permit. While almost all FSRQs have a synchrotron-peak frequency <10¹⁴ Hz, about half of the BL Lac objects have a synchrotron-peak frequency >10¹⁵ Hz. The 2LAC represents a significant improvement relative to the first LAT AGN catalog (1LAC), with 52% more associated sources. The full characterization of the newly detected sources will require more broadband data. Various properties, such as γ-ray fluxes and photon power-law spectral indices, redshifts, γ-ray luminosities, variability, and archival radio luminosities and their correlations are presented and discussed for the different blazar classes. The general trends observed in 1LAC are confirmed....
The Astrophysical Journal, Dec. 2011

Design concepts for the Cherenkov Telescope Array CTA: an advanced facility for ground-based high-energy gamma-ray astronomy
Actis, M.; Agnetta, G.; Aharonian, F.; Akhperjanian, A.; Aleksić, J.; Aliu, E.; Allan, D.; Allekotte, I.; Antico, F.; Antonelli, L. A.; Antoranz, P.; Aravantinos, A.; Arlen, T.; Arnaldi, H.; Artmann, S.; Asano, K.; Asorey, H.; Bähr, J.; Bais, A.; Baixeras, C.; Bajtlik, S.; Balis, D.; Bamba, A.; Barbier, C.; Barceló, M.; Barnacka, A.; Barnstedt, J.; Barres de Almeida, U.; Barrio, J. A.; Basso, S.; Bastieri, D.; Bauer, C.; Becerra, J.; Becherini, Y.; Bechtol, K.; Becker, J.; Beckmann, V.; Bednarek, W.; Behera, B.; Beilicke, M.; Belluso, M.; Benallou, M.; Benbow, W.; Berdugo, J.; Berger, K.; Bernardino, T.; Bernlöhr, K.; Biland, A.; Billotta, S.; Bird, T.; Birsin, E.; Bissaldi, E.; Blake, S.; Blanch, O.; Bobkov, A. A.; Bogacz, L.; Bogdan, M.; Boisson, C.; Boix, J.; Bolmont, J.; Bonanno, G.; Bonardi, A.; Bonev, T.; Borkowski, J.; Botner, O.; Bottani, A.; Bourgeat, M.; Boutonnet, C.; Bouvier, A.; Brau-Nogué, S.; Braun, I.; Bretz, T.; Briggs, M. S.; Brun, P.; Brunetti, L.; Buckley, J. H.; Bugaev, V.; Bühler, R.; Bulik, T.; Busetto, G.; Buson, S.; Byrum, K.; Cailles, M.; Cameron, R.; Canestrari, R.; Cantu, S.; Carmona, E.; Carosi, A.; Carr, J.; Carton, P. H.; Casiraghi, M.; Castarede, H.; Catalano, O.; Cavazzani, S.; Cazaux, S.; Cerruti, B.; Cerruti, M.; Chadwick, P. M.; Chiang, J.; Chikawa, M.; Cieślar, M.; Ciesielska, M.; Cillis, A.; Clerc, C.; Colin, P.; Colomé, J.; Compin, M.; Conconi, P.; Connaughton, V.; Conrad, J.; Contreras, J. L.; Coppi, P.; Corlier, M.; Corona, P.; Corpace, O.; Corti, D.; Cortina, J.; Costantini, H.; Cotter, G.; Courty, B.; Couturier, S.; Covino, S.; Croston, J.; Cusumano, G.; Daniel, M. K.; Dazzi, F.; de Angelis, A.; de Cea Del Pozo, E.; de Gouveia Dal Pino, E. M.; de Jager, O.; de La Calle Pérez, I.; de La Vega, G.; de Lotto, B.; de Naurois, M.; de Oña Wilhelmi, E.; de Souza, V.; Decerprit, B.; Deil, C.; Delagnes, E.; Deleglise, G.; Delgado, C.; Dettlaff, T.; di Paolo, A.; di Pierro, F.; Díaz, C.; Dick, J.; Dickinson, H.; Digel, S. W.; Dimitrov, D.; Disset, G.; Djannati-Ataï, A.; Doert, M.; Domainko, W.; Dorner, D.; Doro, M.; Dournaux, J. -L.; Dravins, D.; Drury, L.; Dubois, F.; Dubois, R.; Dubus, G.; Dufour, C.; Durand, D.; Dyks, J.; Dyrda, M.; Edy, E.; Egberts, K.; Eleftheriadis, C.; Elles, S.; Emmanoulopoulos, D.; Enomoto, R.; Ernenwein, J. -P.; Errando, M.; Etchegoyen, A.; Falcone, A. D.; Farakos, K.; Farnier, C.; Federici, S.; Feinstein, F.; Ferenc, D.; Fillin-Martino, E.; Fink, D.; Finley, C.; Finley, J. P.; Firpo, R.; Florin, D.; Föhr, C.; Fokitis, E.; Font, Ll.; Fontaine, G.; Fontana, A.; Förster, A.; Fortson, L.; Fouque, N.; Fransson, C.; Fraser, G. W.; Fresnillo, L.; Fruck, C.; Fujita, Y.; Fukazawa, Y.; Funk, S.; Gäbele, W.; Gabici, S.; Gadola, A.; Galante, N.; Gallant, Y.; García, B.; García López, R. J.; Garrido, D.; Garrido, L.; Gascón, D.; Gasq, C.; Gaug, M.; Gaweda, J.; Geffroy, N.; Ghag, C.; Ghedina, A.; Ghigo, M.; Gianakaki, E.; Giarrusso, S.; Giavitto, G.; Giebels, B.; Giro, E.; Giubilato, P.; Glanzman, T.; Glicenstein, J. -F.; Gochna, M.; Golev, V.; Gómez Berisso, M.; González, A.; González, F.; Grañena, F.; Graciani, R.; Granot, J.; Gredig, R.; Green, A.; Greenshaw, T.; Grimm, O.; Grube, J.; Grudzińska, M.; Grygorczuk, J.; Guarino, V.; Guglielmi, L.; Guilloux, F.; Gunji, S.; Gyuk, G.; Hadasch, D.; Haefner, D.; Hagiwara, R.; Hahn, J.; Hallgren, A.; Hara, S.; Hardcastle, M. J.; Hassan, T.; Haubold, T.; Hauser, M.; Hayashida, M.; Heller, R.; Henri, G.; Hermann, G.; Herrero, A.; Hinton, J. A.; Hoffmann, D.; Hofmann, W.; Hofverberg, P.; Horns, D.; Hrupec, D.; Huan, H.; Huber, B.; Huet, J. -M.; Hughes, G.; Hultquist, K.; Humensky, T. B.; Huppert, J. -F.; Ibarra, A.; Illa, J. M.; Ingjald, J.; Inoue, Y.; Inoue, S.; Ioka, K.; Jablonski, C.; Jacholkowska, A.; Janiak, M.; Jean, P.; Jensen, H.; Jogler, T.; Jung, I.; Kaaret, P.; Kabuki, S.; Kakuwa, J.; Kalkuhl, C.; Kankanyan, R.; Kapala, M.; Karastergiou, A.; Karczewski, M.; Karkar, S.; Karlsson, N.; Kasperek, J.; Katagiri, H.; Katarzyński, K.; Kawanaka, N.; Kȩdziora, B.; Kendziorra, E.; Khélifi, B.; Kieda, D.; Kifune, T.; Kihm, T.; Klepser, S.; Kluźniak, W.; Knapp, J.; Knappy, A. R.; Kneiske, T.; Knödlseder, J.; Köck, F.; Kodani, K.; Kohri, K.; Kokkotas, K.; Komin, N.; Konopelko, A.; Kosack, K.; Kossakowski, R.; Kostka, P.; Kotuła, J.; Kowal, G.; Kozioł, J.; Krähenbühl, T.; Krause, J.; Krawczynski, H.; Krennrich, F.; Kretzschmann, A.; Kubo, H.; Kudryavtsev, V. A.; Kushida, J.; La Barbera, N.; La Parola, V.; La Rosa, G.; López, A.; Lamanna, G.; Laporte, P.; Lavalley, C.; Le Flour, T.; Le Padellec, A.; Lenain, J. -P.; Lessio, L.; Lieunard, B.; Lindfors, E.; Liolios, A.; Lohse, T.; Lombardi, S.; Lopatin, A.; Lorenz, E.; Lubiński, P.; Luz, O.; Lyard, E.; Maccarone, M. C.; Maccarone, T.; Maier, G.; Majumdar, P.; Maltezos, S.; Małkiewicz, P.; Mañá, C.; Manalaysay, A.; Maneva, G.; Mangano, A.; Manigot, P.; Marín, J.; Mariotti, M.; Markoff, S.; Martínez, G.; Martínez, M.; Mastichiadis, A.; Matsumoto, H.; Mattiazzo, S.; Mazin, D.; McComb, T. J. L.; McCubbin, N.; McHardy, I.; Medina, C.; Melkumyan, D.; Mendes, A.; Mertsch, P.; Meucci, M.; Michałowski, J.; Micolon, P.; Mineo, T.; Mirabal, N.; Mirabel, F.; Miranda, J. M.; Mirzoyan, R.; Mizuno, T.; Moal, B.; Moderski, R.; Molinari, E.; Monteiro, I.; Moralejo, A.; Morello, C.; Mori, K.; Motta, G.; Mottez, F.; Moulin, E.; Mukherjee, R.; Munar, P.; Muraishi, H.; Murase, K.; Murphy, A. Stj.; Nagataki, S.; Naito, T.; Nakamori, T.; Nakayama, K.; Naumann, C.; Naumann, D.; Nayman, P.; Nedbal, D.; Niedźwiecki, A.; Niemiec, J.; Nikolaidis, A.; Nishijima, K.; Nolan, S. J.; Nowak, N.; O'Brien, P. T.; Ochoa, I.; Ohira, Y.; Ohishi, M.; Ohka, H.; Okumura, A.; Olivetto, C.; Ong, R. A.; Orito, R.; Orr, M.; Osborne, J. P.; Ostrowski, M.; Otero, L.; Otte, A. N.; Ovcharov, E.; Oya, I.; Oziȩbło, A.; Paiano, S.; Pallota, J.; Panazol, J. L.; Paneque, D.; Panter, M.; Paoletti, R.; Papyan, G.; Paredes, J. M.; Pareschi, G.; Parsons, R. D.; Paz Arribas, M.; Pedaletti, G.; Pepato, A.; Persic, M.; Petrucci, P. O.; Peyaud, B.; Piechocki, W.; Pita, S.; Pivato, G.; Płatos, Ł.; Platzer, R.; Pogosyan, L.; Pohl, M.; Pojmański, G.; Ponz, J. D.; Potter, W.; Prandini, E.; Preece, R.; Prokoph, H.; Pühlhofer, G.; Punch, M.; Quel, E.; Quirrenbach, A.; Rajda, P.; Rando, R.; Rataj, M.; Raue, M.; Reimann, C.; Reimann, O.; Reimer, A.; Reimer, O.; Renaud, M.; Renner, S.; Reymond, J. -M.; Rhode, W.; Ribó, M.; Ribordy, M.; Rico, J.; Rieger, F.; Ringegni, P.; Ripken, J.; Ristori, P.; Rivoire, S.; Rob, L.; Rodriguez, S.; Roeser, U.; Romano, P.; Romero, G. E.; Rosier-Lees, S.; Rovero, A. C.; Roy, F.; Royer, S.; Rudak, B.; Rulten, C. B.; Ruppel, J.; Russo, F.; Ryde, F.; Sacco, B.; Saggion, A.; Sahakian, V.; Saito, K.; Saito, T.; Sakaki, N.; Salazar, E.; Salini, A.; Sánchez, F.; Sánchez Conde, M. Á.; Santangelo, A.; Santos, E. M.; Sanuy, A.; Sapozhnikov, L.; Sarkar, S.; Scalzotto, V.; Scapin, V.; Scarcioffolo, M.; Schanz, T.; Schlenstedt, S.; Schlickeiser, R.; Schmidt, T.; Schmoll, J.; Schroedter, M.; Schultz, C.; Schultze, J.; Schulz, A.; Schwanke, U.; Schwarzburg, S.; Schweizer, T.; Seiradakis, J.; Selmane, S.; Seweryn, K.; Shayduk, M.; Shellard, R. C.; Shibata, T.; Sikora, M.; Silk, J.; Sillanpää, A.; Sitarek, J.; Skole, C.; Smith, N.; Sobczyńska, D.; Sofo Haro, M.; Sol, H.; Spanier, F.; Spiga, D.; Spyrou, S.; Stamatescu, V.; Stamerra, A.; Starling, R. L. C.; Stawarz, Ł.; Steenkamp, R.; Stegmann, C.; Steiner, S.; Stergioulas, N.; Sternberger, R.; Stinzing, F.; Stodulski, M.; Straumann, U.; Suárez, A.; Suchenek, M.; Sugawara, R.; Sulanke, K. H.; Sun, S.; Supanitsky, A. D.; Sutcliffe, P.; Szanecki, M.; Szepieniec, T.; Szostek, A.; Szymkowiak, A.; Tagliaferri, G.; Tajima, H.; Takahashi, H.; Takahashi, K.; Takalo, L.; Takami, H.; Talbot, R. G.; Tam, P. H.; Tanaka, M.; Tanimori, T.; Tavani, M.; Tavernet, J. -P.; Tchernin, C.; Tejedor, L. A.; Telezhinsky, I.; Temnikov, P.; Tenzer, C.; Terada, Y.; Terrier, R.; Teshima, M.; Testa, V.; Tibaldo, L.; Tibolla, O.; Tluczykont, M.; Todero Peixoto, C. J.; Tokanai, F.; Tokarz, M.; Toma, K.; Torres, D. F.; Tosti, G.; Totani, T.; Toussenel, F.; Vallania, P.; Vallejo, G.; van der Walt, J.; van Eldik, C.; Vandenbroucke, J.; Vankov, H.; Vasileiadis, G.; Vassiliev, V. V.; Vegas, I.; Venter, L.; Vercellone, S.; Veyssiere, C.; Vialle, J. P.; Videla, M.; Vincent, P.; Vink, J.; Vlahakis, N.; Vlahos, L.; Vogler, P.; Vollhardt, A.; Volpe, F.; von Gunten, H. P.; Vorobiov, S.; Wagner, S.; Wagner, R. M.; Wagner, B.; Wakely, S. P.; Walter, P.; Walter, R.; Warwick, R.; Wawer, P.; Wawrzaszek, R.; Webb, N.; Wegner, P.; Weinstein, A.; Weitzel, Q.; Welsing, R.; Wetteskind, H.; White, R.; Wierzcholska, A.; Wilkinson, M. I.; Williams, D. A.; Winde, M.; Wischnewski, R.; Wiśniewski, Ł.; Wolczko, A.; Wood, M.; Xiong, Q.; Yamamoto, T.; Yamaoka, K.; Yamazaki, R.; Yanagita, S.; Yoffo, B.; Yonetani, M.; Yoshida, A.; Yoshida, T.; Yoshikoshi, T.; Zabalza, V.; Zagdański, A.; Zajczyk, A.; Zdziarski, A.; Zech, A.; Ziȩtara, K.; Ziółkowski, P.; Zitelli, V.; Zychowski, P., Ground-based gamma-ray astronomy has had a major breakthrough with the impressive results obtained using systems of imaging atmospheric Cherenkov telescopes. Ground-based gamma-ray astronomy has a huge potential in astrophysics, particle physics and cosmology. CTA is an international initiative to build the next generation instrument, with a factor of 5-10 improvement in sensitivity in the 100 GeV-10 TeV range and the extension to energies well below 100 GeV and above 100 TeV. CTA will consist of two arrays (one in the north, one in the south) for full sky coverage and will be operated as open observatory. The design of CTA is based on currently available technology. This document reports on the status and presents the major design concepts of CTA....
Experimental Astronomy, Dec. 2011

Constraining Dark Matter Models from a Combined Analysis of Milky Way Satellites with the Fermi Large Area Telescope
Ackermann, M.; Ajello, M.; Albert, A.; Atwood, W. B.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Cañadas, B.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Charles, E.; Chekhtman, A.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Cutini, S.; de Angelis, A.; de Palma, F.; Dermer, C. D.; Digel, S. W.; Do Couto E Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Falletti, L.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Guiriec, S.; Gustafsson, M.; Hadasch, D.; Hayashida, M.; Hays, E.; Hughes, R. E.; Jeltema, T. E.; Jóhannesson, G.; Johnson, R. P.; Johnson, A. S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lionetto, A. M.; Llena Garde, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Mazziotta, M. N.; McEnery, J. E.; Mehault, J.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Naumann-Godo, M.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Parent, D.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Pivato, G.; Porter, T. A.; Profumo, S.; Rainò, S.; Razzano, M.; Reimer, A.; Reimer, O.; Ritz, S.; Roth, M.; Sadrozinski, H. F. -W.; Sbarra, C.; Scargle, J. D.; Schalk, T. L.; Sgrò, C.; Siskind, E. J.; Spandre, G.; Spinelli, P.; Strigari, L.; Suson, D. J.; Tajima, H.; Takahashi, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Tinivella, M.; Torres, D. F.; Troja, E.; Uchiyama, Y.; Vandenbroucke, J.; Vasileiou, V.; Vianello, G.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Wood, M.; Yang, Z.; Zimmer, S.; Kaplinghat, M.; Martinez, G. D., Satellite galaxies of the Milky Way are among the most promising targets for dark matter searches in gamma rays. We present a search for dark matter consisting of weakly interacting massive particles, applying a joint likelihood analysis to 10 satellite galaxies with 24 months of data of the Fermi Large Area Telescope. No dark matter signal is detected. Including the uncertainty in the dark matter distribution, robust upper limits are placed on dark matter annihilation cross sections. The 95% confidence level upper limits range from about 10^-26cm³s^-1 at 5 GeV to about 5×10^-23cm³s^-1 at 1 TeV, depending on the dark matter annihilation final state. For the first time, using gamma rays, we are able to rule out models with the most generic cross section (̃3×10^-26cm³s^-1 for a purely s-wave cross section), without assuming additional boost factors....
Physical Review Letters, Dec. 2011

The Radio/Gamma-Ray Connection in Active Galactic Nuclei in the Era of the Fermi Large Area Telescope
Ackermann, M.; Ajello, M.; Allafort, A.; Angelakis, E.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Cannon, A.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cutini, S.; de Palma, F.; Dermer, C. D.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Escande, L.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fortin, P.; Frailis, M.; Fuhrmann, L.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grandi, P.; Grenier, I. A.; Guiriec, S.; Hadasch, D.; Hayashida, M.; Hays, E.; Healey, S. E.; Jóhannesson, G.; Johnson, A. S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Lee, S. -H.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Max-Moerbeck, W.; Mazziotta, M. N.; McEnery, J. E.; Mehault, J.; Michelson, P. F.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Naumann-Godo, M.; Nishino, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Pavlidou, V.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Porter, T. A.; Rainò, S.; Razzano, M.; Readhead, A.; Reimer, A.; Reimer, O.; Richards, J. L.; Romani, R. W.; Sadrozinski, H. F. -W.; Scargle, J. D.; Sgrò, C.; Siskind, E. J.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Tanaka, T.; Taylor, G. B.; Thayer, J. G.; Thayer, J. B.; Thompson, D. J.; Torres, D. F.; Tosti, G.; Tramacere, A.; Troja, E.; Vandenbroucke, J.; Vianello, G.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ziegler, M., We present a detailed statistical analysis of the correlation between radio and gamma-ray emission of the active galactic nuclei (AGNs) detected by Fermi during its first year of operation, with the largest data sets ever used for this purpose. We use both archival interferometric 8.4 GHz data (from the Very Large Array and ATCA, for the full sample of 599 sources) and concurrent single-dish 15 GHz measurements from the Owens Valley Radio Observatory (OVRO, for a sub sample of 199 objects). Our unprecedentedly large sample permits us to assess with high accuracy the statistical significance of the correlation, using a surrogate data method designed to simultaneously account for common-distance bias and the effect of a limited dynamical range in the observed quantities. We find that the statistical significance of a positive correlation between the centimeter radio and the broadband (E > 100 MeV) gamma-ray energy flux is very high for the whole AGN sample, with a probability of <10^-7 for the correlation appearing by chance. Using the OVRO data, we find that concurrent data improve the significance of the correlation from 1.6 × 10^-6 to 9.0 × 10^-8. Our large sample size allows us to study the dependence of correlation strength and significance on specific source types and gamma-ray energy band. We find that the correlation is very significant (chance probability < 10^-7) for both flat spectrum radio quasars and BL Lac objects separately; a dependence of the correlation strength on the considered gamma-ray energy band is also present, but additional data will be necessary to constrain its significance....
The Astrophysical Journal, Nov. 2011

γ-Ray and Parsec-scale Jet Properties of a Complete Sample of Blazars From the MOJAVE Program
Lister, M. L.; Aller, M.; Aller, H.; Hovatta, T.; Kellermann, K. I.; Kovalev, Y. Y.; Meyer, E. T.; Pushkarev, A. B.; Ros, E.; MOJAVE Collaboration; Ackermann, M.; Antolini, E.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Boeck, M.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Chang, C. S.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Cutini, S.; de Palma, F.; Dermer, C. D.; Silva, E. do Couto e.; Drell, P. S.; Drlica-Wagner, A.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Finke, J.; Focke, W. B.; Fortin, P.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Guiriec, S.; Hadasch, D.; Hayashida, M.; Hays, E.; Horan, D.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Kadler, M.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Mehault, J.; Michelson, P. F.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Naumann-Godo, M.; Nishino, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ozaki, M.; Paneque, D.; Parent, D.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Pivato, G.; Rainò, S.; Readhead, A.; Reimer, A.; Reimer, O.; Richards, J. L.; Ritz, S.; Sadrozinski, H. F. -W.; Sgrò, C.; Shaw, M. S.; Siskind, E. J.; Spandre, G.; Spinelli, P.; Takahashi, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Thompson, D. J.; Tosti, G.; Tramacere, A.; Troja, E.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vianello, G.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Zimmer, S.; Fermi LAT Collaboration, We investigate the Fermi Large Area Telescope γ-ray and 15 GHz Very Long Baseline Array radio properties of a joint γ-ray and radio-selected sample of active galactic nuclei (AGNs) obtained during the first 11 months of the Fermi mission (2008 August 4-2009 July 5). Our sample contains the brightest 173 AGNs in these bands above declination -30° during this period, and thus probes the full range of γ-ray loudness (γ-ray to radio band luminosity ratio) in the bright blazar population. The latter quantity spans at least 4 orders of magnitude, reflecting a wide range of spectral energy distribution (SED) parameters in the bright blazar population. The BL Lac objects, however, display a linear correlation of increasing γ-ray loudness with synchrotron SED peak frequency, suggesting a universal SED shape for objects of this class. The synchrotron self-Compton model is favored for the γ-ray emission in these BL Lac objects over external seed photon models, since the latter predict a dependence of Compton dominance on Doppler factor that would destroy any observed synchrotron SED-peak-γ-ray-loudness correlation. The high-synchrotron peaked (HSP) BL Lac objects are distinguished by lower than average radio core brightness temperatures, and none display large radio modulation indices or high linear core polarization levels. No equivalent trends are seen for the flat-spectrum radio quasars (FSRQs) in our sample. Given the association of such properties with relativistic beaming, we suggest that the HSP BL Lac objects have generally lower Doppler factors than the lower-synchrotron peaked BL Lac objects or FSRQs in our sample....
The Astrophysical Journal, Nov. 2011

A Cocoon of Freshly Accelerated Cosmic Rays Detected by Fermi in the Cygnus Superbubble
Ackermann, M.; Ajello, M.; Allafort, A.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Belfiore, A.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bottacini, E.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; de Angelis, A.; de Palma, F.; Dermer, C. D.; do Couto e Silva, E.; Drell, P. S.; Dumora, D.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fortin, P.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Germani, S.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Guillemot, L.; Guiriec, S.; Hadasch, D.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hayashi, K.; Hays, E.; Jóhannesson, G.; Johnson, A. S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kerr, M.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Martin, P.; Mazziotta, M. N.; McEnery, J. E.; Mehault, J.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Naumann-Godo, M.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Parent, D.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Pohl, M.; Prokhorov, D.; Rainò, S.; Rando, R.; Razzano, M.; Reposeur, T.; Ritz, S.; Parkinson, P. M. Saz; Sgrò, C.; Siskind, E. J.; Smith, P. D.; Spinelli, P.; Strong, A. W.; Takahashi, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Troja, E.; Uchiyama, Y.; Vandenbroucke, J.; Vasileiou, V.; Vianello, G.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Zimmer, S.; Bontemps, S., The origin of Galactic cosmic rays is a century-long puzzle. Indirect evidence points to their acceleration by supernova shockwaves, but we know little of their escape from the shock and their evolution through the turbulent medium surrounding massive stars. Gamma rays can probe their spreading through the ambient gas and radiation fields. The Fermi Large Area Telescope (LAT) has observed the star-forming region of Cygnus X. The 1- to 100-gigaelectronvolt images reveal a 50-parsec-wide cocoon of freshly accelerated cosmic rays that flood the cavities carved by the stellar winds and ionization fronts from young stellar clusters. It provides an example to study the youth of cosmic rays in a superbubble environment before they merge into the older Galactic population....
Science, Nov. 2011

Fermi Detection of a Luminous γ-Ray Pulsar in a Globular Cluster
Freire, P. C. C.; Abdo, A. A.; Ajello, M.; Allafort, A.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G.; Cameron, R.; Camilo, F.; Caraveo, P. A.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cognard, I.; Cohen-Tanugi, J.; Cominsky, L. R.; de Palma, F.; Dermer, C. D.; do Couto e Silva, E.; Dormody, M.; Drell, P. S.; Dubois, R.; Dumora, D.; Espinoza, C. M.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Focke, W. B.; Fortin, P.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hadasch, D.; Harding, A. K.; Jóhannesson, G.; Johnson, A. S.; Johnson, T. J.; Johnston, S.; Katagiri, H.; Kataoka, J.; Keith, M.; Kerr, M.; Knödlseder, J.; Kramer, M.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Lyne, A. G.; Manchester, R. N.; Marelli, M.; Mazziotta, M. N.; McEnery, J. E.; Michelson, P. F.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ozaki, M.; Paneque, D.; Parent, D.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Porter, T. A.; Rainò, S.; Ransom, S. M.; Ray, P. S.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Romani, R. W.; Roth, M.; Sadrozinski, H. F. -W.; Saz Parkinson, P. M. Sgrò, C.; Shannon, R.; Siskind, E. J. Smith, D. A.; Smith, P. D.; Spinelli, P.; Stappers, B. W.; Suson, D. J.; Takahashi, H.; Tanaka, T.; Tauris, T. M.; Thayer, J. B.; Theureau, G.; Thompson, D. J.; Thorsett, S. E.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Troja, E.; Vandenbroucke, J.; Van Etten, A.; Vasileiou, V.; Venter, C.; Vianello, G.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Wood, K. S.; Yang, Z.; Ziegler, M.; Zimmer, S., We report on the Fermi Large Area Telescope’s detection of γ-ray (>100 mega-electron volts) pulsations from pulsar J1823-3021A in the globular cluster NGC 6624 with high significance (̃7 σ). Its γ-ray luminosity, L_γ = (8.4 ± 1.6) × 10³⁴ ergs per second, is the highest observed for any millisecond pulsar (MSP) to date, and it accounts for most of the cluster emission. The nondetection of the cluster in the off-pulse phase implies that it contains <32 γ-ray MSPs, not ̃100 as previously estimated. The γ-ray luminosity indicates that the unusually large rate of change of its period is caused by its intrinsic spin-down. This implies that J1823-3021A has the largest magnetic field and is the youngest MSP ever detected and that such anomalous objects might be forming at rates comparable to those of the more normal MSPs....
Science, Nov. 2011

CANGAROO-III Observation of TeV Gamma Rays from the Unidentified Gamma-Ray Source HESS J1614-518
Mizukami, T.; Kubo, H.; Yoshida, T.; Nakamori, T.; Enomoto, R.; Tanimori, T.; Akimoto, M.; Bicknell, G. V.; Clay, R. W.; Edwards, P. G.; Gunji, S.; Hara, S.; Hara, T.; Hayashi, S.; Ishioka, H.; Kabuki, S.; Kajino, F.; Katagiri, H.; Kawachi, A.; Kifune, T.; Kiuchi, R.; Kunisawa, T.; Kushida, J.; Matoba, T.; Matsubara, Y.; Matsuzawa, I.; Mizumura, Y.; Mizumoto, Y.; Mori, M.; Muraishi, H.; Naito, T.; Nakayama, K.; Nishijima, K.; Ohishi, M.; Otake, Y.; Ryoki, S.; Saito, K.; Sakamoto, Y.; Stamatescu, V.; Suzuki, T.; Swaby, D. L.; Thornton, G.; Tokanai, F.; Toyota, Y.; Tsuchiya, K.; Yanagita, S.; Yokoe, Y.; Yoshikoshi, T.; Yukawa, Y., We report the detection, with the CANGAROO-III imaging atmospheric Cherenkov telescope array, of a very high energy gamma-ray signal from the unidentified gamma-ray source HESS J1614-518, which was discovered in the H.E.S.S. Galactic plane survey. Diffuse gamma-ray emission was detected above 760 GeV at the 8.9σ level during an effective exposure of 54 hr from 2008 May to August. The spectrum can be represented by a power law: (8.2 ± 2.2_stat ± 2.5_sys) × 10^-12 × (E/1 TeV)^-γ cm^-2 s^-1 TeV^-1 with a photon index γ of 2.4 ± 0.3_stat ± 0.2_sys, which is compatible with that of the H.E.S.S. observations. By combining our result with multiwavelength data, we discuss the possible counterparts for HESS J1614-518 and consider radiation mechanisms based on hadronic and leptonic processes for a supernova remnant (SNR), stellar winds from massive stars, and a pulsar wind nebula (PWN). Although a leptonic origin from a PWN driven by an unknown pulsar remains possible, hadronic-origin emission from an unknown SNR is preferred....
The Astrophysical Journal, Oct. 2011, [Reviewed]

Simultaneous multi-wavelength campaign on PKS 2005-489 in a high state
H. E. S. S. Collaboration; Abramowski, A.; Acero, F.; Aharonian, F.; Akhperjanian, A. G.; Anton, G.; Barnacka, A.; Barres de Almeida, U.; Bazer-Bachi, A. R.; Becherini, Y.; Becker, J.; Behera, B.; Bernlöhr, K.; Bochow, A.; Boisson, C.; Bolmont, J.; Bordas, P.; Brucker, J.; Brucker, J.; Brun, F.; Brun, P.; Bulik, T.; Büsching, I.; Casanova, S.; Cerruti, M.; Chadwick, P. M.; Charbonnier, A.; Chaves, R. C. G.; Cheesebrough, A.; Chounet, L. -M.; Clapson, A. C.; Coignet, G.; Conrad, J.; Dalton, M.; Daniel, M. K.; Davids, I. D.; Degrange, B.; Deil, C.; Dickinson, H. J.; Djannati-Ataï, A.; Domainko, W.; O'C. Drury, L.; Dubois, F.; Dubus, G.; Dyks, J.; Dyrda, M.; Egberts, K.; Eger, P.; Espigat, P.; Fallon, L.; Farnier, C.; Fegan, S.; Feinstein, F.; Fernandes, M. V.; Fiasson, A.; Fontaine, G.; Förster, A.; Füßling, M.; Gabici, S.; Gallant, Y. A.; Gast, H.; Gérard, L.; Gerbig, D.; Giebels, B.; Glicenstein, J. F.; Glück, B.; Goret, P.; Göring, D.; Hague, J. D.; Hampf, D.; Hauser, M.; Heinz, S.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hinton, J. A.; Hoffmann, A.; Hofmann, W.; Hofverberg, P.; Horns, D.; Jacholkowska, A.; de Jager, O. C.; Jahn, C.; Jamrozy, M.; Jung, I.; Kastendieck, M. A.; Katarzynski, K.; Katz, U.; Kaufmann, S.; Keogh, D.; Kerschhaggl, M.; Khangulyan, D.; Khélifi, B.; Klochkov, D.; Kluzniak, W.; Kneiske, T.; Komin, Nu.; Kosack, K.; Kossakowski, R.; Laffon, H.; Lamanna, G.; Lenain, J. -P.; Lennarz, D.; Lohse, T.; Lopatin, A.; Lu, C. -C.; Marandon, V.; Marcowith, A.; Masbou, J.; Maurin, D.; Maxted, N.; McComb, T. J. L.; Medina, M. C.; Méhault, J.; Nguyen, N.; Moderski, R.; Moulin, E.; Naumann-Godo, M.; de Naurois, M.; Nedbal, D.; Nekrassov, D.; Nicholas, B.; Niemiec, J.; Nolan, S. J.; Ohm, S.; Olive, J. -F.; de Oña Wilhelmi, E.; Opitz, B.; Ostrowski, M.; Oya, I.; Panter, M.; Paz Arribas, M.; Pedaletti, G.; Pelletier, G.; Petrucci, P. -O.; Pita, S.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raue, M.; Rayner, S. M.; Reimer, A.; Reimer, O.; Renaud, M.; de Los Reyes, R.; Rieger, F.; Ripken, J.; Rob, L.; Rosier-Lees, S.; Rowell, G.; Rudak, B.; Rulten, C. B.; Ruppel, J.; Ryde, F.; Sahakian, V.; Santangelo, A.; Schlickeiser, R.; Schöck, F. M.; Schulz, A.; Schwanke, U.; Schwarzburg, S.; Schwemmer, S.; Shalchi, A.; Sikora, M.; Skilton, J. L.; Sol, H.; Spengler, G.; Stawarz, L.; Steenkamp, R.; Stegmann, C.; Stinzing, F.; Sushch, I.; Szostek, A.; Tam, P. H.; Tavernet, J. -P.; Terrier, R.; Tibolla, O.; Tluczykont, M.; Valerius, K.; van Eldik, C.; Vasileiadis, G.; Venter, C.; Vialle, J. P.; Viana, A.; Vincent, P.; Vivier, M.; Völk, H. J.; Volpe, F.; Vorobiov, S.; Vorster, M.; Wagner, S. J.; Ward, M.; White, R.; Wierzcholska, A.; Zajczyk, A.; Zdziarski, A. A.; Zech, A.; Zechlin, H. -S.; Fermi LAT Collboration; Abdo, A. A.; Ackermann, M.; Ajello, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Cannon, A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cutini, S.; Dermer, C. D.; de Palma, F.; Do Couto E Silva, E.; Drell, P. S.; Dubois, R.; Dumora, D.; Escande, L.; Favuzzi, C.; Ferrara, E. C.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grove, J. E.; Guiriec, S.; Hadasch, D.; Hays, E.; Horan, D.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Michelson, P. F.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Nishino, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Sgrò, C.; Siskind, E. J.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Troja, E.; Uehara, T.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ylinen, T.; Ziegler, M., The high-frequency peaked BL Lac object PKS 2005-489 was the target of a multi-wavelength campaign with simultaneous observations in the TeV γ-ray (H.E.S.S.), GeV γ-ray (Fermi/LAT), X-ray (RXTE, Swift), UV (Swift) and optical (ATOM, Swift) bands. This campaign was carried out during a high flux state in the synchrotron regime. The flux in the optical and X-ray bands reached the level of the historical maxima. The hard GeV spectrum observed with Fermi/LAT connects well to the very high energy (VHE, E > 100 GeV) spectrum measured with H.E.S.S....
Astronomy and Astrophysics, Sep. 2011

Fermi Large Area Telescope Observations of Markarian 421: The Missing Piece of its Spectral Energy Distribution
Abdo, A. A.; Ackermann, M.; Ajello, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Cannon, A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Cutini, S.; de Angelis, A.; de Palma, F.; Dermer, C. D.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Escande, L.; Favuzzi, C.; Fegan, S. J.; Finke, J.; Focke, W. B.; Fortin, P.; Frailis, M.; Fuhrmann, L.; Fukazawa, Y.; Fukuyama, T.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Georganopoulos, M.; Germani, S.; Giebels, B.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Guiriec, S.; Hadasch, D.; Hayashida, M.; Hays, E.; Horan, D.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kadler, M.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Max-Moerbeck, W.; Mazziotta, M. N.; McEnery, J. E.; Mehault, J.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Naumann-Godo, M.; Nishino, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pavlidou, V.; Pearson, T. J.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Readhead, A.; Reimer, A.; Reimer, O.; Reyes, L. C.; Richards, J. L.; Ritz, S.; Roth, M.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Sgrò, C.; Siskind, E. J.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stawarz, Ł.; Stevenson, M.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Troja, E.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vianello, G.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Wehrle, A. E.; Winer, B. L.; Wood, K. S.; Yang, Z.; Yatsu, Y.; Ylinen, T.; Zensus, J. A.; Ziegler, M.; Fermi LAT Collaboration; Aleksić, J.; Antonelli, L. A.; Antoranz, P.; Backes, M.; Barrio, J. A.; Becerra González, J.; Bednarek, W.; Berdyugin, A.; Berger, K.; Bernardini, E.; Biland, A.; Blanch, O.; Bock, R. K.; Boller, A.; Bonnoli, G.; Bordas, P.; Borla Tridon, D.; Bosch-Ramon, V.; Bose, D.; Braun, I.; Bretz, T.; Camara, M.; Carmona, E.; Carosi, A.; Colin, P.; Colombo, E.; Contreras, J. L.; Cortina, J.; Covino, S.; Dazzi, F.; de Angelis, A.; De Cea del Pozo, E.; Delgado Mendez, C.; De Lotto, B.; De Maria, M.; De Sabata, F.; Diago Ortega, A.; Doert, M.; Domínguez, A.; Dominis Prester, D.; Dorner, D.; Doro, M.; Elsaesser, D.; Ferenc, D.; Fonseca, M. V.; Font, L.; García López, R. J.; Garczarczyk, M.; Gaug, M.; Giavitto, G.; Godinovi, N.; Hadasch, D.; Herrero, A.; Hildebrand, D.; Höhne-Mönch, D.; Hose, J.; Hrupec, D.; Jogler, T.; Klepser, S.; Krähenbühl, T.; Kranich, D.; Krause, J.; La Barbera, A.; Leonardo, E.; Lindfors, E.; Lombardi, S.; López, M.; Lorenz, E.; Majumdar, P.; Makariev, E.; Maneva, G.; Mankuzhiyil, N.; Mannheim, K.; Maraschi, L.; Mariotti, M.; Martínez, M.; Mazin, D.; Meucci, M.; Miranda, J. M.; Mirzoyan, R.; Miyamoto, H.; Moldón, J.; Moralejo, A.; Nieto, D.; Nilsson, K.; Orito, R.; Oya, I.; Paoletti, R.; Paredes, J. M.; Partini, S.; Pasanen, M.; Pauss, F.; Pegna, R. G.; Perez-Torres, M. A.; Persic, M.; Peruzzo, J.; Pochon, J.; Prada, F.; Prada Moroni, P. G.; Prandini, E.; Puchades, N.; Puljak, I.; Reichardt, T.; Rhode, W.; Ribó, M.; Rico, J.; Rissi, M.; Rügamer, S.; Saggion, A.; Saito, K.; Saito, T. Y.; Salvati, M.; Sánchez-Conde, M.; Satalecka, K.; Scalzotto, V.; Scapin, V.; Schultz, C.; Schweizer, T.; Shayduk, M.; Shore, S. N.; Sierpowska-Bartosik, A.; Sillanpää, A.; Sitarek, J.; Sobczynska, D.; Spanier, F.; Spiro, S.; Stamerra, A.; Steinke, B.; Storz, J.; Strah, N.; Struebig, J. C.; Suric, T.; Takalo, L. O.; Tavecchio, F.; Temnikov, P.; Terzić, T.; Tescaro, D.; Teshima, M.; Vankov, H.; Wagner, R. M.; Weitzel, Q.; Zabalza, V.; Zandanel, F.; Zanin, R.; MAGIC Collaboration; Villata, M.; Raiteri, C.; Aller, H. D.; Aller, M. F.; Chen, W. P.; Jordan, B.; Koptelova, E.; Kurtanidze, O. M.; Lähteenmäki, A.; McBreen, B.; Larionov, V. M.; Lin, C. S.; Nikolashvili, M. G.; Reinthal, R.; Angelakis, E.; Capalbi, M.; Carramiñana, A.; Carrasco, L.; Cassaro, P.; Cesarini, A.; Falcone, A.; Gurwell, M. A.; Hovatta, T.; Kovalev, Yu. A.; Kovalev, Y. Y.; Krichbaum, T. P.; Krimm, H. A.; Lister, M. L.; Moody, J. W.; Maccaferri, G.; Mori, Y.; Nestoras, I.; Orlati, A.; Pace, C.; Pagani, C.; Pearson, R.; Perri, M.; Piner, B. G.; Ros, E.; Sadun, A. C.; Sakamoto, T.; Tammi, J.; Zook, A., We report on the γ-ray activity of the high-synchrotron-peaked BL Lacertae object Markarian 421 (Mrk 421) during the first 1.5 years of Fermi operation, from 2008 August 5 to 2010 March 12. We find that the Large Area Telescope (LAT) γ-ray spectrum above 0.3 GeV can be well described by a power-law function with photon index Γ = 1.78 ± 0.02 and average photon flux F(> 0.3 GeV) = (7.23 ± 0.16) × 10^-8 ph cm^-2 s^-1. Over this time period, the Fermi-LAT spectrum above 0.3 GeV was evaluated on seven-day-long time intervals, showing significant variations in the photon flux (up to a factor ~3 from the minimum to the maximum flux) but mild spectral variations. The variability amplitude at X-ray frequencies measured by RXTE/ASM and Swift/BAT is substantially larger than that in γ-rays measured by Fermi-LAT, and these two energy ranges are not significantly correlated. We also present the first results from the 4.5 month long multifrequency campaign on Mrk 421, which included the VLBA, Swift, RXTE, MAGIC, the F-GAMMA, GASP-WEBT, and other collaborations and instruments that provided excellent temporal and energy coverage of the source throughout the entire campaign (2009 January 19 to 2009 June 1). During this campaign, Mrk 421 showed a low activity at all wavebands. The extensive multi-instrument (radio to TeV) data set provides an unprecedented, complete look at the quiescent spectral energy distribution (SED) for this source. The broadband SED was reproduced with a leptonic (one-zone synchrotron self-Compton) and a hadronic model (synchrotron proton blazar). Both frameworks are able to describe the average SED reasonably well, implying comparable jet powers but very different characteristics for the blazar emission site....
The Astrophysical Journal, Aug. 2011

Constraints on dark matter models from a Fermi LAT search for high-energy cosmic-ray electrons from the Sun
Ajello, M.; Atwood, W. B.; Baldini, L.; Barbiellini, G.; Bastieri, D.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bottacini, E.; Bouvier, A.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Cecchi, C.; Charles, E.; Chekhtman, A.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cutini, S.; de Angelis, A.; de Palma, F.; Dermer, C. D.; Digel, S. W.; Do Couto E Silva, E.; Drell, P. S.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Gehrels, N.; Germani, S.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Guiriec, S.; Gustafsson, M.; Hadasch, D.; Iafrate, G.; Jóhannesson, G.; Johnson, A. S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kuss, M.; Latronico, L.; Lionetto, A. M.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Mazziotta, M. N.; McEnery, J. E.; Michelson, P. F.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Naumann-Godo, M.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Ritz, S.; Schalk, T. L.; Sgrò, C.; Siegal-Gaskins, J.; Siskind, E. J.; Smith, P. D.; Spandre, G.; Spinelli, P.; Suson, D. J.; Takahashi, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Tosti, G.; Troja, E.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vianello, G.; Vilchez, N.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Zimmer, S., During its first year of data taking, the Large Area Telescope (LAT) onboard the Fermi Gamma-Ray Space Telescope has collected a large sample of high-energy cosmic-ray electrons and positrons (CREs). We present the results of a directional analysis of the CRE events, in which we searched for a flux excess correlated with the direction of the Sun. Two different and complementary analysis approaches were implemented, and neither yielded evidence of a significant CRE flux excess from the Sun. We derive upper limits on the CRE flux from the Sun’s direction, and use these bounds to constrain two classes of dark matter models which predict a solar CRE flux: (1) models in which dark matter annihilates to CREs via a light intermediate state, and (2) inelastic dark matter models in which dark matter annihilates to CREs....
Physical Review D, Aug. 2011

Discovery of High-energy Gamma-ray Emission from the Binary System PSR B1259-63/LS 2883 around Periastron with Fermi
Abdo, A. A.; Ackermann, M.; Ajello, M.; Allafort, A.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Camilo, F.; Caraveo, P. A.; Cecchi, C.; Charles, E.; Chaty, S.; Chekhtman, A.; Chernyakova, M.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cominsky, L. R.; Corbel, S.; Cutini, S.; D'Ammando, F.; de Angelis, A.; den Hartog, P. R.; de Palma, F.; Dermer, C. D.; Digel, S. W.; Silva, E. do Couto e.; Dormody, M.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Dubus, G.; Dumora, D.; Enoto, T.; Espinoza, C. M.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Focke, W. B.; Fortin, P.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Grundstrom, E.; Guiriec, S.; Gwon, C.; Hadasch, D.; Harding, A. K.; Hayashida, M.; Hays, E.; Jóhannesson, G.; Johnson, A. S.; Johnson, T. J.; Johnston, S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Keith, M.; Kerr, M.; Knödlseder, J.; Kramer, M.; Kuss, M.; Lande, J.; Lee, S. -H.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Manchester, R. N.; Marelli, M.; Mazziotta, M. N.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Naumann-Godo, M.; Neronov, A.; Nolan, P. L.; Norris, J. P.; Noutsos, A.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Parent, D.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Porter, T. A.; Possenti, A.; Rainò, S.; Rando, R.; Ray, P. S.; Razzano, M.; Razzaque, S.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Sadrozinski, H. F. -W.; Scargle, J. D.; Sgrò, C.; Shannon, R.; Siskind, E. J.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Thompson, D. J.; Thorsett, S. E.; Tibaldo, L.; Tibolla, O.; Torres, D. F.; Tosti, G.; Troja, E.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vianello, G.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wolff, M. T.; Wood, D. L.; Wood, K. S.; Yang, Z.; Ziegler, M.; Zimmer, S., We report on the discovery of >=100 MeV γ-rays from the binary system PSR B1259-63/LS 2883 using the Large Area Telescope (LAT) on board Fermi. The system comprises a radio pulsar in orbit around a Be star. We report on LAT observations from near apastron to ~128 days after the time of periastron, t_p , on 2010 December 15. No γ-ray emission was detected from this source when it was far from periastron. Faint γ-ray emission appeared as the pulsar approached periastron. At ~t_p + 30 days, the >=100 MeV γ-ray flux increased over a period of a few days to a peak flux 20-30 times that seen during the pre-periastron period, but with a softer spectrum. For the following month, it was seen to be variable on daily timescales, but remained at ~(1-4) × 10^-6 cm^-2 s^-1 before starting to fade at ~t_p + 57 days. The total γ-ray luminosity observed during this period is comparable to the spin-down power of the pulsar. Simultaneous radio and X-ray observations of the source showed no corresponding dramatic changes in radio and X-ray flux between the pre-periastron and post-periastron flares. We discuss possible explanations for the observed γ-ray-only flaring of the source....
The Astrophysical Journal, Jul. 2011

Detection of high-energy gamma-ray emission during the X-ray flaring activity in GRB 100728A
A.A. Abdo; M. Ackermann; M. Ajello; L. Baldini; J. Ballet; G. Barbiellini; M.G. Baring; D. Bastieri; K. Bechtol; R. Bellazzini; B. Berenji; P.N. Bhat; E. Bissaldi; R.D. Blandford; E. Bonamente; J. Bonnell; A.W. Borgland; A. Bouvier; J. Bregeon; M. Brigida; P. Bruel; R. Buehler; S. Buson; G.A. Caliandro; R.A. Cameron; P.A. Caraveo; J.M. Casandjian; C. Cecchi; E. Charles; A. Chekhtman; J. Chiang; S. Ciprini; R. Claus; V. Connaughton; J. Conrad; S. Cutini; A. De Angelis; F. De Palma; C.D. Dermer; E. Do Couto E Silva; P.S. Drell; R. Dubois; C. Favuzzi; Y. Fukazawa; P. Fusco; F. Gargano; N. Gehrels; S. Germani; N. Giglietto; P. Giommi; F. Giordano; M. Giroletti; T. Glanzman; G. Godfrey; J. Granot; I.A. Grenier; S. Guiriec; D. Hadasch; Y. Hanabata; R.E. Hughes; G. Jóhannesson; A.S. Johnson; T. Kamae; H. Katagiri; J. Kataoka; M. Kerr; J. Knödlseder; M. Kuss; J. Lande; L. Latronico; S.-H. Lee; F. Longo; F. Loparco; B. Lott; P. Lubrano; M.N. Mazziotta; J.E. McEnery; P. Mészros; P.F. Michelson; T. Mizuno; A.A. Moiseev; M.E. Monzani; A. Morselli; I.V. Moskalenko; S. Murgia; T. Nakamori; M. Naumann-Godo; P.L. Nolan; J.P. Norris; E. Nuss; T. Ohsugi; A. Okumura; N. Omodei; E. Orlando; W.S. Paciesas; V. Pelassa; M. Pesce-Rollins; M. Pierbattista; F. Piron; T.A. Porter; J.L. Racusin; S. Rainò; M. Razzano; S. Razzaque; A. Reimer; O. Reimer; L.C. Reyes; M. Roth; H.F.-W. Sadrozinski; C. Sgrò; E.J. Siskind; P.D. Smith; E. Sonbas; G. Spandre; P. Spinelli; M. Stamatikos; M.S. Strickman; H. Takahashi; T. Tanaka; Y. Tanaka; J.G. Thayer; J.B. Thayer; D.F. Torres; G. Tosti; E. Troja; T. Uehara; T.L. Usher; J. Vandenbroucke; V. Vasileiou; G. Vianello; N. Vilchez; V. Vitale; A. Von Kienlin; A.P. Waite; P. Wang; B.L. Winer; K.S. Wood; R. Yamazaki; Z. Yang; M. Ziegler; L. Piro, We present the simultaneous Swift and Fermi observations of the bright GRB 100728A and its afterglow. The early X-ray emission is dominated by a vigorous flaring activity continuing until 1ks after the burst. In the same time interval, high-energy emission is significantly detected by the Fermi/Large Area Telescope. Marginal evidence ofGeV emission is observed up to later times. We discuss the broadband properties of this burst within both the internal and external shock scenarios, with a particular emphasis on the relation between X-ray flares, theGeV emission, and a continued long-duration central engine activity as their power source. © 2011. The American Astronomical Society. All rights reserved.
Astrophysical Journal Letters, 20 Jun. 2011, [Reviewed]

Fermi large area telescope observations of two gamma-ray emission components from the quiescent sun
A.A. Abdo; M. Ackermann; M. Ajello; L. Baldini; J. Ballet; G. Barbiellini; D. Bastieri; K. Bechtol; R. Bellazzini; B. Berenji; E. Bonamente; A.W. Borgland; A. Bouvier; J. Bregeon; A. Brez; M. Brigida; P. Bruel; R. Buehler; S. Buson; G.A. Caliandro; R.A. Cameron; P.A. Caraveo; J.M. Casandjian; C. Cecchi; E. Charles; A. Chekhtman; J. Chiang; S. Ciprini; R. Claus; J. Cohen-Tanugi; J. Conrad; S. Cutini; A. De Angelis; F. De Palma; C.D. Dermer; S.W. Digel; E. Do Couto E Silva; P.S. Drell; R. Dubois; C. Favuzzi; S.J. Fegan; W.B. Focke; P. Fortin; M. Frailis; S. Funk; P. Fusco; F. Gargano; D. Gasparrini; N. Gehrels; S. Germani; N. Giglietto; F. Giordano; M. Giroletti; T. Glanzman; G. Godfrey; I.A. Grenier; L. Grillo; S. Guiriec; D. Hadasch; E. Hays; R.E. Hughes; G. Iafrate; G. Jóhannesson; A.S. Johnson; T.J. Johnson; T. Kamae; H. Katagiri; J. Kataoka; J. Knödlseder; M. Kuss; J. Lande; L. Latronico; S.-H. Lee; A.M. Lionetto; F. Longo; F. Loparco; B. Lott; M.N. Lovellette; P. Lubrano; A. Makeev; M.N. Mazziotta; J.E. McEnery; J. Mehault; P.F. Michelson; W. Mitthumsiri; T. Mizuno; A.A. Moiseev; C. Monte; M.E. Monzani; A. Morselli; I.V. Moskalenko; S. Murgia; T. Nakamori; M. Naumann-Godo; P.L. Nolan; J.P. Norris; E. Nuss; T. Ohsugi; A. Okumura; N. Omodei; E. Orlando; J.F. Ormes; M. Ozaki; D. Paneque; V. Pelassa; M. Pesce-Rollins; M. Pierbattista; F. Piron; T.A. Porter; S. Rainò; R. Rando; M. Razzano; A. Reimer; O. Reimer; T. Reposeur; S. Ritz; H.F.-W. Sadrozinski; T.L. Schalk; C. Sgrò; G.H. Share; E.J. Siskind; P.D. Smith; G. Spandre; P. Spinelli; M.S. Strickman; A.W. Strong; H. Takahashi; T. Tanaka; J.G. Thayer; J.B. Thayer; D.J. Thompson; L. Tibaldo; D.F. Torres; G. Tosti; A. Tramacere; E. Troja; Y. Uchiyama; T.L. Usher; J. Vandenbroucke; V. Vasileiou; G. Vianello; N. Vilchez; V. Vitale; A.E. Vladimirov; A.P. Waite; P. Wang; B.L. Winer; K.S. Wood; Z. Yang; M. Ziegler, We report the detection of high-energy γ-rays from the quiescent Sun with the Large Area Telescope on board the Fermi Gamma-Ray Space Telescope (Fermi) during the first 18 months of the mission. These observations correspond to the recent period of low solar activity when the emission induced by cosmic rays (CRs) is brightest. For the first time, the high statistical significance of the observations allows clear separation of the two components: the point-like emission from the solar disk due to CR cascades in the solar atmosphere and extended emission from the inverse Compton (IC) scattering of CR electrons on solar photons in the heliosphere. The observed integral flux (≥100MeV) from the solar disk is (4.6 ± 0.2[statistical error] +1.0- 0.8[systematic error]) × 10 -7cm-2s-1, which is 7 times higher than predicted by the "nominal" model of Seckel etal. In contrast, the observed integral flux (≥100MeV) of the extended emission from a region of 20° radius centered on the Sun, but excluding the disk itself, (6.8 ± 0.7[stat.]+0.5- 0.4[syst.]) × 10 -7cm-2s-1, along with the observed spectrum and the angular profile, is in good agreement with the theoretical predictions for the IC emission. © 2011. The American Astronomical Society. All rights reserved.
Astrophysical Journal, 20 Jun. 2011, [Reviewed]

Fermi Gamma-ray Space Telescope Observations of the Gamma-ray Outburst from 3C454.3 in November 2010
Abdo, A. A.; Ackermann, M.; Ajello, M.; Allafort, A.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Conrad, J.; Cutini, S.; D'Ammando, F.; de Angelis, A.; de Palma, F.; Dermer, C. D.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Escande, L.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Fortin, P.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grove, J. E.; Guiriec, S.; Hadasch, D.; Hayashida, M.; Hays, E.; Horan, D.; Itoh, R.; Jóhannesson, G.; Johnson, A. S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Larsson, S.; Latronico, L.; Lee, S. -H.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Naumann-Godo, M.; Nishino, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Orlando, E.; Ormes, J. F.; Paneque, D.; Pelassa, V.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzaque, S.; Reimer, A.; Reimer, O.; Ritz, S.; Roth, M.; Sadrozinski, H. F. -W.; Sanchez, D.; Scargle, J. D.; Schalk, T. L.; Sgrò, C.; Siskind, E. J.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Tanaka, Y.; Thayer, J. G.; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Troja, E.; Vandenbroucke, J.; Vasileiou, V.; Vianello, G.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ziegler, M., The flat-spectrum radio quasar 3C454.3 underwent an extraordinary 5 day γ-ray outburst in 2010 November when the daily flux measured with the Fermi Large Area Telescope (LAT) at photon energies E > 100 MeV reached (66 ± 2) × 10^-6 photons cm^-2 s^-1. This is a factor of three higher than its previous maximum flux recorded in 2009 December and >~ 5 times brighter than the Vela pulsar, which is normally the brightest source in the γ-ray sky. The 3 hr peak flux was (85 ± 5)×10^-6 photons cm^-2 s^-1, corresponding to an apparent isotropic luminosity of (2.1 ± 0.2)×10⁵⁰ erg s^-1, the highest ever recorded for a blazar. In this Letter, we investigate the features of this exceptional event in the γ-ray band of the Fermi-LAT. In contrast to previous flares of the same source observed with the Fermi-LAT, clear spectral changes are observed during the flare....
The Astrophysical Journal, Jun. 2011

Observations of the Young Supernova Remnant RX J1713.7-3946 with the Fermi Large Area Telescope
Abdo, A. A.; Ackermann, M.; Ajello, M.; Allafort, A.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Brandt, T. J.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Chaty, S.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Cillis, A. N.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Corbel, S.; Cutini, S.; de Angelis, A.; de Palma, F.; Dermer, C. D.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Dumora, D.; Favuzzi, C.; Ferrara, E. C.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Fukui, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Guiriec, S.; Hadasch, D.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hayashi, K.; Hays, E.; Horan, D.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kerr, M.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Mazziotta, M. N.; McEnery, J. E.; Michelson, P. F.; Mignani, R. P.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Naumann-Godo, M.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Orlando, E.; Ormes, J. F.; Paneque, D.; Parent, D.; Pelassa, V.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Pohl, M.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, O.; Reposeur, T.; Ritz, S.; Romani, R. W.; Roth, M.; Sadrozinski, H. F. -W.; Saz Parkinson, P. M.; Sgrò, C.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Tibolla, O.; Torres, D. F.; Tosti, G.; Tramacere, A.; Troja, E.; Uchiyama, Y.; Vandenbroucke, J.; Vasileiou, V.; Vianello, G.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yamamoto, H.; Yamazaki, R.; Yang, Z.; Ziegler, M., We present observations of the young supernova remnant (SNR) RX J1713.7-3946 with the Fermi Large Area Telescope (LAT). We clearly detect a source positionally coincident with the SNR. The source is extended with a best-fit extension of 0fdg55 ± 0fdg04 matching the size of the non-thermal X-ray and TeV gamma-ray emission from the remnant. The positional coincidence and the matching extended emission allow us to identify the LAT source with SNR RX J1713.7-3946. The spectrum of the source can be described by a very hard power law with a photon index of Γ = 1.5 ± 0.1 that coincides in normalization with the steeper H.E.S.S.-detected gamma-ray spectrum at higher energies. The broadband gamma-ray emission is consistent with a leptonic origin as the dominant mechanism for the gamma-ray emission....
The Astrophysical Journal, Jun. 2011

The First Fermi Multifrequency Campaign on BL Lacertae: Characterizing the Low-activity State of the Eponymous Blazar
Abdo, A. A.; Ackermann, M.; Ajello, M.; Antolini, E.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Cannon, A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Costamante, L.; Cutini, S.; Dermer, C. D.; de Palma, F.; Donato, D.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Escande, L.; Favuzzi, C.; Fegan, S. J.; Finke, J.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Guiriec, S.; Hadasch, D.; Hayashida, M.; Hays, E.; Hughes, R. E.; Itoh, R.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Larsson, S.; Latronico, L.; Lee, S. -H.; Llena Garde, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Mazziotta, M. N.; McEnery, J. E.; Mehault, J.; Michelson, P. F.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Naumann-Godo, M.; Nishino, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Ritz, S.; Roth, M.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Schinzel, F. K.; Sgrò, C.; Siskind, E. J.; Smith, P. D.; Sokolovsky, K. V.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uehara, T.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wallace, E.; Wang, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ylinen, T.; Ziegler, M.; Berdyugin, A.; Boettcher, M.; Carramiñana, A.; Carrasco, L.; de la Fuente, E.; Diltz, C.; Hovatta, T.; Kadenius, V.; Kovalev, Y. Y.; Lähteenmäki, A.; Lindfors, E.; Marscher, A. P.; Nilsson, K.; Pereira, D.; Reinthal, R.; Roustazadeh, P.; Savolainen, T.; Sillanpää, A.; Takalo, L. O.; Tornikoski, M., We report on observations of BL Lacertae during the first 18 months of Fermi LAT science operations and present results from a 48 day multifrequency coordinated campaign from 2008 August 19 to 2008 October 7. The radio to gamma-ray behavior of BL Lac is unveiled during a low-activity state thanks to the coordinated observations of radio-band (Metsähovi and VLBA), near-IR/optical (Tuorla, Steward, OAGH, and MDM), and X-ray (RXTE and Swift) observatories. No variability was resolved in gamma rays during the campaign, and the brightness level was 15 times lower than the level of the 1997 EGRET outburst. Moderate and uncorrelated variability has been detected in UV and X-rays. The X-ray spectrum is found to be concave, indicating the transition region between the low- and high-energy components of the spectral energy distribution (SED). VLBA observation detected a synchrotron spectrum self-absorption turnover in the innermost part of the radio jet appearing to be elongated and inhomogeneous, and constrained the average magnetic field there to be less than 3 G. Over the following months, BL Lac appeared variable in gamma rays, showing flares (in 2009 April and 2010 January). There is no evidence for the correlation of gamma rays with the optical flux monitored from the ground in 18 months. The SED may be described by a single-zone or a two-zone synchrotron self-Compton (SSC) model, but a hybrid SSC plus external radiation Compton model seems to be preferred based on the observed variability and the fact that it provides a fit closest to equipartition....
The Astrophysical Journal, Apr. 2011

Erratum: "Multi-wavelength Observations of the Flaring Gamma-ray Blazar 3C 66A in 2008 October" (2011, ApJ, 726, 43)
Abdo, A. A.; Ackermann, M.; Ajello, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Costamante, L.; Cutini, S.; Davis, D. S.; Dermer, C. D.; de Palma, F.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Favuzzi, C.; Fegan, S. J.; Fortin, P.; Frailis, M.; Fuhrmann, L.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hadasch, D.; Hayashida, M.; Hays, E.; Horan, D.; Hughes, R. E.; Itoh, R.; Jóhannesson, G.; Johnson, A. S.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Mazziotta, M. N.; McEnery, J. E.; Mehault, J.; Michelson, P. F.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Naumann-Godo, M.; Nestoras, I.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reyes, L. C.; Ripken, J.; Ritz, S.; Romani, R. W.; Roth, M.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Scargle, J. D.; Sgrò, C.; Shaw, M. S.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ylinen, T.; Ziegler, M.; Fermi LAT Collaboration; Acciari, V. A.; Aliu, E.; Arlen, T.; Aune, T.; Beilicke, M.; Benbow, W.; Böttcher, M.; Boltuch, D.; Bradbury, S. M.; Buckley, J. H.; Bugaev, V.; Byrum, K.; Cannon, A.; Cesarini, A.; Christiansen, J. L.; Ciupik, L.; Cui, W.; de la Calle Perez, I.; Dickherber, R.; Errando, M.; Falcone, A.; Finley, J. P.; Finnegan, G.; Fortson, L.; Furniss, A.; Galante, N.; Gall, D.; Gillanders, G. H.; Godambe, S.; Grube, J.; Guenette, R.; Gyuk, G.; Hanna, D.; Holder, J.; Hui, C. M.; Humensky, T. B.; Imran, A.; Kaaret, P.; Karlsson, N.; Kertzman, M.; Kieda, D.; Konopelko, A.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Maier, G.; McArthur, S.; McCann, A.; McCutcheon, M.; Moriarty, P.; Mukherjee, R.; Ong, R. A.; Otte, A. N.; Pandel, D.; Perkins, J. S.; Pichel, A.; Pohl, M.; Quinn, J.; Ragan, K.; Reynolds, P. T.; Roache, E.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Senturk, G. Demet; Smith, A. W.; Steele, D.; Swordy, S. P.; Tešić, G.; Theiling, M.; Thibadeau, S.; Varlotta, A.; Vassiliev, V. V.; Vincent, S.; Wakely, S. P.; Ward, J. E.; Weekes, T. C.; Weinstein, A.; Weisgarber, T.; Williams, D. A.; Wissel, S.; Wood, M.; VERITAS Collaboration; Villata, M.; Raiteri, C. M.; Gurwell, M. A.; Larionov, V. M.; Kurtanidze, O. M.; Aller, M. F.; Lähteenmäki, A.; Chen, W. P.; Berduygin, A.; Agudo, I.; Aller, H. D.; Arkharov, A. A.; Bach, U.; Bachev, R.; Beltrame, P.; Benítez, E.; Buemi, C. S.; Dashti, J.; Calcidese, P.; Capezzali, D.; Carosati, D.; Da Rio, D.; Di Paola, A.; Diltz, C.; Dolci, M.; Dultzin, D.; Forné, E.; Gómez, J. L.; Hagen-Thorn, V. A.; Halkola, A.; Heidt, J.; Hiriart, D.; Hovatta, T.; Hsiao, H. -Y.; Jorstad, S. G.; Kimeridze, G. N.; Konstantinova, T. S.; Kopatskaya, E. N.; Koptelova, E.; Leto, P.; Ligustri, R.; Lindfors, E.; Lopez, J. M.; Marscher, A. P.; Mommert, M.; Mujica, R.; Nikolashvili, M. G.; Nilsson, K.; Palma, N.; Pasanen, M.; Roca-Sogorb, M.; Ros, J. A.; Roustazadeh, P.; Sadun, A. C.; Saino, J.; Sigua, L. A.; Sillanää, A.; Sorcia, M.; Takalo, L. O.; Tornikoski, M.; Trigilio, C.; Turchetti, R.; Umana, G.; GASP-WEBT Consortium; Belloni, T.; Blake, C. H.; Bloom, J. S.; Angelakis, E.; Fumagalli, M.; Hauser, M.; Prochaska, J. X.; Riquelme, D.; Sievers, A.; Starr, D. L.; Tagliaferri, G.; Ungerechts, H.; Wagner, S.; Zensus, J. A., ...
The Astrophysical Journal, Apr. 2011

Detection of a Spectral Break in the Extra Hard Component of GRB 090926A
Ackermann, M.; Ajello, M.; Asano, K.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bhat, P. N.; Bissaldi, E.; Blandford, R. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Briggs, M. S.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Chaplin, V.; Charles, E.; Chekhtman, A.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Connaughton, V.; Conrad, J.; Cutini, S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Dingus, B. L.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Focke, W. B.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Goldstein, A.; Granot, J.; Greiner, J.; Grenier, I. A.; Grove, J. E.; Guiriec, S.; Hadasch, D.; Hanabata, Y.; Harding, A. K.; Hayashi, K.; Hayashida, M.; Hays, E.; Horan, D.; Hughes, R. E.; Itoh, R.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kippen, R. M.; Knödlseder, J.; Kocevski, D.; Kouveliotou, C.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Llena Garde, M.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Mazziotta, M. N.; McBreen, S.; McEnery, J. E.; McGlynn, S.; Meegan, C.; Mehault, J.; Mészáros, P.; Michelson, P. F.; Mizuno, T.; Monte, C.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakajima, H.; Nakamori, T.; Naumann-Godo, M.; Nishino, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paciesas, W. S.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Petrosian, V.; Piron, F.; Porter, T. A.; Preece, R.; Racusin, J. L.; Rainò, S.; Rando, R.; Rau, A.; Razzano, M.; Razzaque, S.; Reimer, A.; Reimer, O.; Reposeur, T.; Reyes, L. C.; Ripken, J.; Ritz, S.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sander, A.; Scargle, J. D.; Schalk, T. L.; Sgrò, C.; Siskind, E. J.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stamatikos, M.; Stecker, F. W.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Tanaka, T.; Tanaka, Y.; Thayer, J. B.; Thayer, J. G.; Tibaldo, L.; Tierney, D.; Toma, K.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Uehara, T.; Usher, T. L.; Vandenbroucke, J.; van der Horst, A. J.; Vasileiou, V.; Vilchez, N.; Vitale, V.; von Kienlin, A.; Waite, A. P.; Wang, P.; Wilson-Hodge, C.; Winer, B. L.; Wood, K. S.; Wu, X. F.; Yamazaki, R.; Yang, Z.; Ylinen, T.; Ziegler, M., We report on the observation of the bright, long gamma-ray burst, GRB 090926A, by the Gamma-ray Burst Monitor and Large Area Telescope (LAT) instruments on board the Fermi Gamma-ray Space Telescope. GRB 090926A shares several features with other bright LAT bursts. In particular, it clearly shows a short spike in the light curve that is present in all detectors that see the burst, and this in turn suggests that there is a common region of emission across the entire Fermi energy range. In addition, while a separate high-energy power-law component has already been observed in other gamma-ray bursts, here we report for the first time the detection with good significance of a high-energy spectral break (or cutoff) in this power-law component around 1.4 GeV in the time-integrated spectrum. If the spectral break is caused by opacity to electron-positron pair production within the source, then this observation allows us to compute the bulk Lorentz factor for the outflow, rather than a lower limit....
The Astrophysical Journal, Mar. 2011

Erratum: "The First Fermi Large Area Telescope Catalog of Gamma-Ray Pulsars" (2010, ApJS, 187, 460)
Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Camilo, F.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cognard, I.; Cohen-Tanugi, J.; Cominsky, L. R.; Conrad, J.; Corbet, R.; Cutini, S.; den Hartog, P. R.; Dermer, C. D.; de Angelis, A.; de Luca, A.; de Palma, F.; Digel, S. W.; Dormody, M.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Espinoza, C.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Focke, W. B.; Fortin, P.; Frailis, M.; Freire, P. C. C.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giavitto, G.; Giebels, B.; Giglietto, N.; Giommi, P.; Giordano, F.; Glanzman, T.; Godfrey, G.; Gotthelf, E. V.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Gwon, C.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Hughes, R. E.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Johnston, S.; Kamae, T.; Kanbach, G.; Kaspi, V. M.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocian, M. L.; Kramer, M.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Livingstone, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Lyne, A. G.; Madejski, G. M.; Makeev, A.; Manchester, R. N.; Marelli, M.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; McGlynn, S.; Meurer, C.; Michelson, P. F.; Mineo, T.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Nolan, P. L.; Norris, J. P.; Noutsos, A.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Ransom, S. M.; Ray, P. S.; Razzano, M.; Rea, N.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Schalk, T. L.; Sellerholm, A.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stappers, B. W.; Starck, J. -L.; Striani, E.; Strickman, M. S.; Strong, A. W.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Theureau, G.; Thompson, D. J.; Thorsett, S. E.; Tibaldo, L.; Tibolla, O.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Van Etten, A.; Vasileiou, V.; Venter, C.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Wang, N.; Watters, K.; Weltevrede, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M., ...
The Astrophysical Journal Supplement Series, Mar. 2011

Radio and γ-ray Constraints on the Emission Geometry and Birthplace of PSR J2043+2740
Noutsos, A.; Abdo, A. A.; Ackermann, M.; Ajello, M.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Buehler, R.; Busetto, G.; Caliandro, G. A.; Cameron, R. A.; Camilo, F.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Chaty, S.; Chekhtman, A.; Chiang, J.; Ciprini, S.; Claus, R.; Cognard, I.; Cohen-Tanugi, J.; Colafrancesco, S.; Cutini, S.; Dermer, C. D.; de Palma, F.; Drell, P. S.; Dumora, D.; Ea, C. M.; Favuzzi, C.; Ferrara, E. C.; Focke, W. B.; Frailis, M.; Freire, P. C. C.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Germani, S.; Giglietto, N.; Giordano, F.; Giroletti, M.; Godfrey, G.; Grandi, P.; Grenier, I. A.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Harding, A. K.; Hughes, R. E.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, T. J.; Johnson, W. N.; Johnston, S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kramer, M.; Kuss, M.; Lande, J.; Lee, S. -H.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Lyne, A. G.; Makeev, A.; Marelli, M.; Mazziotta, M. N.; McEnery, J. E.; Mehault, J.; Michelson, P. F.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Naumann-Godo, M.; Nolan, P. L.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Persic, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Ray, P. S.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Romani, R. W.; Sadrozinski, H. F. -W.; Sander, A.; Saz Parkinson, P. M.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stappers, B. W.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Tanaka, T.; Theureau, G.; Thompson, D. J.; Thorsett, S. E.; Tibolla, O.; Torres, D. F.; Tramacere, A.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Vilchez, N.; Villata, M.; Vitale, V.; von Kienlin, A.; Waite, A. P.; Wang, P.; Watters, K.; Weltevrede, P.; Winer, B. L.; Wood, K. S.; Ziegler, M., We report on the first year of Fermi γ-ray observations of pulsed high-energy emission from the old PSR J2043 + 2740. The study of the γ-ray efficiency of such old pulsars gives us an insight into the evolution of pulsars' ability to emit in γ rays as they age. The γ-ray light curve of this pulsar above 0.1 GeV is clearly defined by two sharp peaks, 0.353 ± 0.035 periods apart. We have combined the γ-ray profile characteristics of PSR J2043 + 2740 with the geometrical properties of the pulsar's radio emission, derived from radio-polarization data, and constrained the pulsar-beam geometry in the framework of a two-pole caustic (TPC) and an outer gap (OG) model. The ranges of magnetic inclination and viewing angle were determined to be {α, ζ} ~ {52°-57°, 61°-68°} for the TPC model, and {α, ζ} ~ {62°-73°, 74°-81°} and {α, ζ} ~ {72°-83°, 60°-75°} for the OG model. Based on this geometry, we assess possible birth locations for this pulsar and derive a likely proper motion, sufficiently high to be measurable with VLBI. At a characteristic age of 1.2 Myr, PSR J2043 + 2740 is the third oldest of all discovered, non-recycled, γ-ray pulsars: it is twice as old as the next oldest, PSR J0357 + 32, and younger only than the recently discovered PSR J1836 + 5925 and PSR J2055 + 25, both of which are at least five and ten times less energetic, respectively....
The Astrophysical Journal, Feb. 2011

Insights into the High-energy γ-ray Emission of Markarian 501 from Extensive Multifrequency Observations in the Fermi Era
Abdo, A. A.; Ackermann, M.; Ajello, M.; Allafort, A.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Brandt, T. J.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Cannon, A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Cutini, S.; Dermer, C. D.; de Palma, F.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Focke, W. B.; Fortin, P.; Frailis, M.; Fuhrmann, L.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Guillemot, L.; Guiriec, S.; Hayashida, M.; Hays, E.; Horan, D.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kadler, M.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Max-Moerbeck, W.; Mazziotta, M. N.; McEnery, J. E.; Mehault, J.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Naumann-Godo, M.; Nishino, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J. H.; Parent, D.; Pavlidou, V.; Pearson, T. J.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Readhead, A.; Reimer, A.; Reimer, O.; Richards, J. L.; Ripken, J.; Ritz, S.; Roth, M.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Scargle, J. D.; Sgrò, C.; Siskind, E. J.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stawarz, Ł.; Stevenson, M.; Strickman, M. S.; Sokolovsky, K. V.; Suson, D. J.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Wehrle, A. E.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ylinen, T.; Zensus, J. A.; Ziegler, M.; Fermi LAT Collaboration; Aleksić, J.; Antonelli, L. A.; Antoranz, P.; Backes, M.; Barrio, J. A.; Becerra González, J.; Bednarek, W.; Berdyugin, A.; Berger, K.; Bernardini, E.; Biland, A.; Blanch, O.; Bock, R. K.; Boller, A.; Bonnoli, G.; Bordas, P.; Borla Tridon, D.; Bosch-Ramon, V.; Bose, D.; Braun, I.; Bretz, T.; Camara, M.; Carmona, E.; Carosi, A.; Colin, P.; Colombo, E.; Contreras, J. L.; Cortina, J.; Covino, S.; Dazzi, F.; de Angelis, A.; De Cea del Pozo, E.; De Lotto, B.; De Maria, M.; De Sabata, F.; Delgado Mendez, C.; Diago Ortega, A.; Doert, M.; Domínguez, A.; Dominis Prester, D.; Dorner, D.; Doro, M.; Elsaesser, D.; Ferenc, D.; Fonseca, M. V.; Font, L.; García López, R. J.; Garczarczyk, M.; Gaug, M.; Giavitto, G.; Godinovi, N.; Hadasch, D.; Herrero, A.; Hildebrand, D.; Höhne-Mönch, D.; Hose, J.; Hrupec, D.; Jogler, T.; Klepser, S.; Krähenbühl, T.; Kranich, D.; Krause, J.; La Barbera, A.; Leonardo, E.; Lindfors, E.; Lombardi, S.; López, M.; Lorenz, E.; Majumdar, P.; Makariev, E.; Maneva, G.; Mankuzhiyil, N.; Mannheim, K.; Maraschi, L.; Mariotti, M.; Martínez, M.; Mazin, D.; Meucci, M.; Miranda, J. M.; Mirzoyan, R.; Miyamoto, H.; Moldón, J.; Moralejo, A.; Nieto, D.; Nilsson, K.; Orito, R.; Oya, I.; Paoletti, R.; Paredes, J. M.; Partini, S.; Pasanen, M.; Pauss, F.; Pegna, R. G.; Perez-Torres, M. A.; Persic, M.; Peruzzo, J.; Pochon, J.; Prada Moroni, P. G.; Prada, F.; Prandini, E.; Puchades, N.; Puljak, I.; Reichardt, T.; Reinthal, R.; Rhode, W.; Ribó, M.; Rico, J.; Rissi, M.; Rügamer, S.; Saggion, A.; Saito, K.; Saito, T. Y.; Salvati, M.; Sánchez-Conde, M.; Satalecka, K.; Scalzotto, V.; Scapin, V.; Schultz, C.; Schweizer, T.; Shayduk, M.; Shore, S. N.; Sierpowska-Bartosik, A.; Sillanpää, A.; Sitarek, J.; Sobczynska, D.; Spanier, F.; Spiro, S.; Stamerra, A.; Steinke, B.; Storz, J.; Strah, N.; Struebig, J. C.; Suric, T.; Takalo, L. O.; Tavecchio, F.; Temnikov, P.; Terzić, T.; Tescaro, D.; Teshima, M.; Vankov, H.; Wagner, R. M.; Weitzel, Q.; Zabalza, V.; Zandanel, F.; Zanin, R.; MAGIC Collaboration; Acciari, V. A.; Arlen, T.; Aune, T.; Benbow, W.; Boltuch, D.; Bradbury, S. M.; Buckley, J. H.; Bugaev, V.; Cannon, A.; Cesarini, A.; Ciupik, L.; Cui, W.; Dickherber, R.; Errando, M.; Falcone, A.; Finley, J. P.; Finnegan, G.; Fortson, L.; Furniss, A.; Galante, N.; Gall, D.; Gillanders, G. H.; Godambe, S.; Grube, J.; Guenette, R.; Gyuk, G.; Hanna, D.; Holder, J.; Huang, D.; Hui, C. M.; Humensky, T. B.; Kaaret, P.; Karlsson, N.; Kertzman, M.; Kieda, D.; Konopelko, A.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; Maier, G.; McArthur, S.; McCann, A.; McCutcheon, M.; Moriarty, P.; Mukherjee, R.; Ong, R.; Otte, A. N.; Pandel, D.; Perkins, J. S.; Pichel, A.; Pohl, M.; Quinn, J.; Ragan, K.; Reyes, L. C.; Reynolds, P. T.; Roache, E.; Rose, H. J.; Rovero, A. C.; Schroedter, M.; Sembroski, G. H.; Senturk, G. D.; Steele, D.; Swordy, S. P.; Tešić, G.; Theiling, M.; Thibadeau, S.; Varlotta, A.; Vincent, S.; Wakely, S. P.; Ward, J. E.; Weekes, T. C.; Weinstein, A.; Weisgarber, T.; Williams, D. A.; Wood, M.; Zitzer, B.; VERITAS Collaboration; Villata, M.; Raiteri, C. M.; Aller, H. D.; Aller, M. F.; Arkharov, A. A.; Blinov, D. A.; Calcidese, P.; Chen, W. P.; Efimova, N. V.; Kimeridze, G.; Konstantinova, T. S.; Kopatskaya, E. N.; Koptelova, E.; Kurtanidze, O. M.; Kurtanidze, S. O.; Lähteenmäki, A.; Larionov, V. M.; Larionova, E. G.; Larionova, L. V.; Ligustri, R.; Morozova, D. A.; Nikolashvili, M. G.; Sigua, L. A.; Troitsky, I. S.; Angelakis, E.; Capalbi, M.; Carramiñana, A.; Carrasco, L.; Cassaro, P.; de la Fuente, E.; Gurwell, M. A.; Kovalev, Y. Y.; Kovalev, Yu. A.; Krichbaum, T. P.; Krimm, H. A.; Leto, P.; Lister, M. L.; Maccaferri, G.; Moody, J. W.; Mori, Y.; Nestoras, I.; Orlati, A.; Pagani, C.; Pace, C.; Pearson, R., III; Perri, M.; Piner, B. G.; Pushkarev, A. B.; Ros, E.; Sadun, A. C.; Sakamoto, T.; Tornikoski, M.; Yatsu, Y.; Zook, A., We report on the γ-ray activity of the blazar Mrk 501 during the first 480 days of Fermi operation. We find that the average Large Area Telescope (LAT) γ-ray spectrum of Mrk 501 can be well described by a single power-law function with a photon index of 1.78 ± 0.03. While we observe relatively mild flux variations with the Fermi-LAT (within less than a factor of two), we detect remarkable spectral variability where the hardest observed spectral index within the LAT energy range is 1.52 ± 0.14, and the softest one is 2.51 ± 0.20. These unexpected spectral changes do not correlate with the measured flux variations above 0.3 GeV. In this paper, we also present the first results from the 4.5 month long multifrequency campaign (2009 March 15—August 1) on Mrk 501, which included the Very Long Baseline Array (VLBA), Swift, RXTE, MAGIC, and VERITAS, the F-GAMMA, GASP-WEBT, and other collaborations and instruments which provided excellent temporal and energy coverage of the source throughout the entire campaign. The extensive radio to TeV data set from this campaign provides us with the most detailed spectral energy distribution yet collected for this source during its relatively low activity. The average spectral energy distribution of Mrk 501 is well described by the standard one-zone synchrotron self-Compton (SSC) model. In the framework of this model, we find that the dominant emission region is characterized by a size lsim0.1 pc (comparable within a factor of few to the size of the partially resolved VLBA core at 15-43 GHz), and that the total jet power (sime10⁴⁴ erg s^-1) constitutes only a small fraction (~10^-3) of the Eddington luminosity. The energy distribution of the freshly accelerated radiating electrons required to fit the time-averaged data has a broken power-law form in the energy range 0.3 GeV-10 TeV, with spectral indices 2.2 and 2.7 below and above the break energy of 20 GeV. We argue that such a form is consistent with a scenario in which the bulk of the energy dissipation within the dominant emission zone of Mrk 501 is due to relativistic, proton-mediated shocks. We find that the ultrarelativistic electrons and mildly relativistic protons within the blazar zone, if comparable in number, are in approximate energy equipartition, with their energy dominating the jet magnetic field energy by about two orders of magnitude....
The Astrophysical Journal, Feb. 2011

Gamma-Ray Flares from the Crab Nebula
Abdo, A. A.; Ackermann, M.; Ajello, M.; Allafort, A.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Brandt, T. J.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Cannon, A.; Caraveo, P. A.; Casandjian, J. M.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Costamante, L.; Cutini, S.; D'Ammando, F.; Dermer, C. D.; de Angelis, A.; de Luca, A.; de Palma, F.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Dumora, D.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guiriec, S.; Hadasch, D.; Hanabata, Y.; Harding, A. K.; Hayashi, K.; Hayashida, M.; Hays, E.; Horan, D.; Itoh, R.; Jóhannesson, G.; Johnson, A. S.; Johnson, T. J.; Khangulyan, D.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kerr, M.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Marelli, M.; Mazziotta, M. N.; McEnery, J. E.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Naumann-Godo, M.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Ray, P. S.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Romani, R. W.; Sadrozinski, H. F. -W.; Sanchez, D.; Parkinson, P. M. Saz; Scargle, J. D.; Schalk, T. L.; Sgrò, C.; Siskind, E. J.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Troja, E.; Uchiyama, Y.; Vandenbroucke, J.; Vasileiou, V.; Vianello, G.; Vitale, V.; Wang, P.; Wood, K. S.; Yang, Z.; Ziegler, M., A young and energetic pulsar powers the well-known Crab Nebula. Here, we describe two separate gamma-ray (photon energy greater than 100 mega-electron volts) flares from this source detected by the Large Area Telescope on board the Fermi Gamma-ray Space Telescope. The first flare occurred in February 2009 and lasted approximately 16 days. The second flare was detected in September 2010 and lasted approximately 4 days. During these outbursts, the gamma-ray flux from the nebula increased by factors of four and six, respectively. The brevity of the flares implies that the gamma rays were emitted via synchrotron radiation from peta-electron-volt (10¹⁵ electron volts) electrons in a region smaller than 1.4 × 10^-2 parsecs. These are the highest-energy particles that can be associated with a discrete astronomical source, and they pose challenges to particle acceleration theory....
Science, Feb. 2011

Fermi-LAT Search for Pulsar Wind Nebulae Around Gamma-ray Pulsars
Ackermann, M.; Ajello, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Camilo, F.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cognard, I.; Cohen-Tanugi, J.; Conrad, J.; Dermer, C. D.; de Angelis, A.; de Luca, A.; de Palma, F.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Favuzzi, C.; Focke, W. B.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Germani, S.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hadasch, D.; Hanabata, Y.; Harding, A. K.; Hayashi, K.; Hays, E.; Hobbs, G.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Johnston, S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Keith, M.; Kerr, M.; Knödlseder, J.; Kramer, M.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Lyne, A. G.; Makeev, A.; Marelli, M.; Mazziotta, M. N.; McEnery, J. E.; Mehault, J.; Michelson, P. F.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Naumann-Godo, M.; Nolan, P. L.; Noutsos, A.; Nuss, E.; Ohsugi, T.; Okumura, A.; Ormes, J. F.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Ransom, S. M.; Ray, P. S.; Razzano, M.; Rea, N.; Reimer, A.; Reimer, O.; Reposeur, T.; Ripken, J.; Ritz, S.; Romani, R. W.; Sadrozinski, H. F. -W.; Sander, A.; Saz Parkinson, P. M.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Theureau, G.; Thompson, D. J.; Thorsett, S. E.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Uehara, T.; Usher, T. L.; Vandenbroucke, J.; Van Etten, A.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Weltevrede, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ylinen, T.; Ziegler, M., The high sensitivity of the Fermi-LAT (Large Area Telescope) offers the first opportunity to study faint and extended GeV sources such as pulsar wind nebulae (PWNe). After one year of observation the LAT detected and identified three PWNe: the Crab Nebula, Vela-X, and the PWN inside MSH 15-52. In the meantime, the list of LAT detected pulsars increased steadily. These pulsars are characterized by high energy loss rates (\dot{E}) from ~3 × 10³³ erg s^-1 to 5 × 10³⁸ erg s^-1 and are therefore likely to power a PWN. This paper summarizes the search for PWNe in the off-pulse windows of 54 LAT-detected pulsars using 16 months of survey observations. Ten sources show significant emission, seven of these likely being of magnetospheric origin. The detection of significant emission in the off-pulse interval offers new constraints on the γ-ray emitting regions in pulsar magnetospheres. The three other sources with significant emission are the Crab Nebula, Vela-X, and a new PWN candidate associated with the LAT pulsar PSR J1023-5746, coincident with the TeV source HESS J1023-575. We further explore the association between the HESS and the Fermi source by modeling its spectral energy distribution. Flux upper limits derived for the 44 remaining sources are used to provide new constraints on famous PWNe that have been detected at keV and/or TeV energies....
The Astrophysical Journal, Jan. 2011

Multi-wavelength Observations of the Flaring Gamma-ray Blazar 3C 66A in 2008 October
Abdo, A. A.; Ackermann, M.; Ajello, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Costamante, L.; Cutini, S.; Davis, D. S.; Dermer, C. D.; de Palma, F.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Dumora, D.; Favuzzi, C.; Fegan, S. J.; Fortin, P.; Frailis, M.; Fuhrmann, L.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hadasch, D.; Hayashida, M.; Hays, E.; Horan, D.; Hughes, R. E.; Itoh, R.; Jóhannesson, G.; Johnson, A. S.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Mazziotta, M. N.; McEnery, J. E.; Mehault, J.; Michelson, P. F.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Naumann-Godo, M.; Nestoras, I.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reyes, L. C.; Ripken, J.; Ritz, S.; Romani, R. W.; Roth, M.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Scargle, J. D.; Sgrò, C.; Shaw, M. S.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ylinen, T.; Ziegler, M.; Acciari, V. A.; Aliu, E.; Arlen, T.; Aune, T.; Beilicke, M.; Benbow, W.; Böttcher, M.; Boltuch, D.; Bradbury, S. M.; Buckley, J. H.; Bugaev, V.; Byrum, K.; Cannon, A.; Cesarini, A.; Christiansen, J. L.; Ciupik, L.; Cui, W.; de la Calle Perez, I.; Dickherber, R.; Errando, M.; Falcone, A.; Finley, J. P.; Finnegan, G.; Fortson, L.; Furniss, A.; Galante, N.; Gall, D.; Gillanders, G. H.; Godambe, S.; Grube, J.; Guenette, R.; Gyuk, G.; Hanna, D.; Holder, J.; Hui, C. M.; Humensky, T. B.; Imran, A.; Kaaret, P.; Karlsson, N.; Kertzman, M.; Kieda, D.; Konopelko, A.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Maier, G.; McArthur, S.; McCann, A.; McCutcheon, M.; Moriarty, P.; Mukherjee, R.; Ong, R. A.; Otte, A. N.; Pandel, D.; Perkins, J. S.; Pichel, A.; Pohl, M.; Quinn, J.; Ragan, K.; Reynolds, P. T.; Roache, E.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Senturk, G. Demet; Smith, A. W.; Steele, D.; Swordy, S. P.; Tešić, G.; Theiling, M.; Thibadeau, S.; Varlotta, A.; Vassiliev, V. V.; Vincent, S.; Wakely, S. P.; Ward, J. E.; Weekes, T. C.; Weinstein, A.; Weisgarber, T.; Williams, D. A.; Wissel, S.; Wood, M.; Villata, M.; Raiteri, C. M.; Gurwell, M. A.; Larionov, V. M.; Kurtanidze, O. M.; Aller, M. F.; Lähteenmäki, A.; Chen, W. P.; Berduygin, A.; Agudo, I.; Aller, H. D.; Arkharov, A. A.; Bach, U.; Bachev, R.; Beltrame, P.; Benítez, E.; Buemi, C. S.; Dashti, J.; Calcidese, P.; Capezzali, D.; Carosati, D.; Da Rio, D.; Di Paola, A.; Diltz, C.; Dolci, M.; Dultzin, D.; Forné, E.; Gómez, J. L.; Hagen-Thorn, V. A.; Halkola, A.; Heidt, J.; Hiriart, D.; Hovatta, T.; Hsiao, H. -Y.; Jorstad, S. G.; Kimeridze, G. N.; Konstantinova, T. S.; Kopatskaya, E. N.; Koptelova, E.; Leto, P.; Ligustri, R.; Lindfors, E.; Lopez, J. M.; Marscher, A. P.; Mommert, M.; Mujica, R.; Nikolashvili, M. G.; Nilsson, K.; Palma, N.; Pasanen, M.; Roca-Sogorb, M.; Ros, J. A.; Roustazadeh, P.; Sadun, A. C.; Saino, J.; Sigua, L. A.; Sillanää, A.; Sorcia, M.; Takalo, L. O.; Tornikoski, M.; Trigilio, C.; Turchetti, R.; Umana, G.; Belloni, T.; Blake, C. H.; Bloom, J. S.; Angelakis, E.; Fumagalli, M.; Hauser, M.; Prochaska, J. X.; Riquelme, D.; Sievers, A.; Starr, D. L.; Tagliaferri, G.; Ungerechts, H.; Wagner, S.; Zensus, J. A.; Fermi LAT Collaboration; VERITAS Collaboration; GASP-WEBT Consortium, The BL Lacertae object 3C 66A was detected in a flaring state by the Fermi Large Area Telescope (LAT) and VERITAS in 2008 October. In addition to these gamma-ray observations, F-GAMMA, GASP-WEBT, PAIRITEL, MDM, ATOM, Swift, and Chandra provided radio to X-ray coverage. The available light curves show variability and, in particular, correlated flares are observed in the optical and Fermi-LAT gamma-ray band. The resulting spectral energy distribution can be well fitted using standard leptonic models with and without an external radiation field for inverse Compton scattering. It is found, however, that only the model with an external radiation field can accommodate the intra-night variability observed at optical wavelengths....
The Astrophysical Journal, Jan. 2011

Constraints on the Cosmic-ray Density Gradient Beyond the Solar Circle from Fermi γ-ray Observations of the Third Galactic Quadrant
Ackermann, M.; Ajello, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Brandt, T. J.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Charles, E.; Chekhtman, A.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Dermer, C. D.; de Palma, F.; Digel, S. W.; Drell, P. S.; Dubois, R.; Favuzzi, C.; Ferrara, E. C.; Focke, W. B.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Germani, S.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Guiriec, S.; Hadasch, D.; Hanabata, Y.; Harding, A. K.; Hayashi, K.; Hayashida, M.; Hughes, R. E.; Itoh, R.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Llena Garde, M.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Martin, P.; Mazziotta, M. N.; McEnery, J. E.; Mehault, J.; Michelson, P. F.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Naumann-Godo, M.; Nishino, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Ripken, J.; Sada, T.; Sadrozinski, H. F. -W.; Sgrò, C.; Siskind, E. J.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Strong, A. W.; Suson, D. J.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tramacere, A.; Uchiyama, Y.; Uehara, T.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Vladimirov, A. E.; Waite, A. P.; Wang, P.; Wood, K. S.; Yang, Z.; Ziegler, M., We report an analysis of the interstellar γ-ray emission in the third Galactic quadrant measured by the Fermi Large Area Telescope. The window encompassing the Galactic plane from longitude 210° to 250° has kinematically well-defined segments of the Local and the Perseus arms, suitable to study the cosmic-ray (CR) densities across the outer Galaxy. We measure no large gradient with Galactocentric distance of the γ-ray emissivities per interstellar H atom over the regions sampled in this study. The gradient depends, however, on the optical depth correction applied to derive the H I column densities. No significant variations are found in the interstellar spectra in the outer Galaxy, indicating similar shapes of the CR spectrum up to the Perseus arm for particles with GeV to tens of GeV energies. The emissivity as a function of Galactocentric radius does not show a large enhancement in the spiral arms with respect to the interarm region. The measured emissivity gradient is flatter than expectations based on a CR propagation model using the radial distribution of supernova remnants and uniform diffusion properties. In this context, observations require a larger halo size and/or a flatter CR source distribution than usually assumed. The molecular mass calibrating ratio, X _CO = N(H₂)/W _CO, is found to be (2.08 ± 0.11) × 10²⁰ cm^-2(K km s^-1)^-1 in the Local arm clouds and is not significantly sensitive to the choice of H I spin temperature. No significant variations are found for clouds in the interarm region....
The Astrophysical Journal, Jan. 2011

17aSE-6 Development of the PMT- waveform sampling circuit using an analog memory for the CTA project
Awane Yusuke; CTA-Japan Consortium, The Physical Society of Japan
Meeting Abstracts of the Physical Society of Japan, 2011

19aSY-9 CTA25 : Development of readout circuits for LSI
Hagiwara Ryouta; CTA-Japan Consortium, The Physical Society of Japan
Meeting Abstracts of the Physical Society of Japan, 2011

26pGR-8 CTA 15 : Development of readout circuits for LST
Nakamori Takeshi, The Physical Society of Japan
Meeting Abstracts of the Physical Society of Japan, 2011

25aGF-1 Development of the PMT-waveform sampling circuit using an analog memory for the CTA project
Aono Masahiro; CTA-Japan Consortium; Open-It, The Physical Society of Japan
Meeting Abstracts of the Physical Society of Japan, 2011

Development of Non-sequential Ray-tracing Software for Cosmic-ray Telescopes　　　　　　　　　　　　　　　
Akira Okumura; Masaaki Hayashida; Hideaki Katagiri; Takayuki Saito; Vladimir Vassiliev
Proceedings of the 32nd International Cosmic Ray Conference, 2011

Fermi Large Area Telescope Observations of the Cygnus Loop Supernova Remnant
Katagiri; H.; et al., Lead, We present an analysis of the gamma-raymeasurements by the Large Area Telescope onboard the Fermi Gamma-ray Space Telescope in the region of the supernova remnant (SNR) Cygnus Loop (G74.0-8.5). We detect significant gamma-ray emission associated with the SNR in the energy band 0.2-100 GeV. The gamma-ray spectrum shows a break in the range 2-3 GeV. The gamma-ray luminosity is similar to 1 x 10(33) erg s(-1) between 1 and 100 GeV, much lower than those of other GeV-emitting SNRs. The morphology is best represented by a ring shape, with inner/outer radii 0.degrees 7 +/- 0.degrees 1 and 1.degrees 6 +/- 0.degrees 1. Given the association among X-ray rims, H alpha filaments, and gamma-ray emission, we argue that gamma rays originate in interactions between particles accelerated in the SNR and interstellar gas or radiation fields adjacent to the shock regions. The decay of neutral pions produced in nucleon-nucleon interactions between accelerated hadrons and interstellar gas provides a reasonable explanation for the gamma-ray spectrum., IOP PUBLISHING LTD
The Astrophysical Journal, 2011, [Reviewed]

Fermi Large Area Telescope Observations of the Supernova Remnant G8.7-0.1
Ajello; M. and the Fermi LAT collaboration (corresponding author: H. Katagiri et al.), Corresponding, We present an analysis of the gamma-raymeasurements by the Large Area Telescope onboard the Fermi Gamma-ray Space Telescope in the region of the supernova remnant (SNR) Cygnus Loop (G74.0-8.5). We detect significant gamma-ray emission associated with the SNR in the energy band 0.2-100 GeV. The gamma-ray spectrum shows a break in the range 2-3 GeV. The gamma-ray luminosity is similar to 1 x 10(33) erg s(-1) between 1 and 100 GeV, much lower than those of other GeV-emitting SNRs. The morphology is best represented by a ring shape, with inner/outer radii 0.degrees 7 +/- 0.degrees 1 and 1.degrees 6 +/- 0.degrees 1. Given the association among X-ray rims, H alpha filaments, and gamma-ray emission, we argue that gamma rays originate in interactions between particles accelerated in the SNR and interstellar gas or radiation fields adjacent to the shock regions. The decay of neutral pions produced in nucleon-nucleon interactions between accelerated hadrons and interstellar gas provides a reasonable explanation for the gamma-ray spectrum., IOP PUBLISHING LTD
The Astrophysical Journal, 2011, [Reviewed]

A population of gamma-ray emitting globular clusters seen with the Fermi Large Area Telescope
Abdo, A. A.; Ackermann, M.; Ajello, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bellazzini, R.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Brandt, T. J.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Charles, E.; Chaty, S.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Decesar, M. E.; Dermer, C. D.; de Palma, F.; Digel, S. W.; Silva, E. Do Couto E.; Drell, P. S.; Dubois, R.; Dumora, D.; Favuzzi, C.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hadasch, D.; Harding, A. K.; Hays, E.; Jean, P.; Jóhannesson, G.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kerr, M.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Lemoine-Goumard, M.; Llena Garde, M.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Mazziotta, M. N.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Naumann-Godo, M.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Pancrazi, B.; Parent, D.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Reimer, A.; Reimer, O.; Reposeur, T.; Ripken, J.; Romani, R. W.; Roth, M.; Sadrozinski, H. F. -W.; Saz Parkinson, P. M.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Venter, C.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Webb, N.; Winer, B. L.; Yang, Z.; Ylinen, T.; Ziegler, M.; Fermi LAT Collaboration, Context. Globular clusters with their large populations of millisecond pulsars (MSPs) are believed to be potential emitters of high-energy gamma-ray emission. The observation of this emission provides a powerful tool to assess the millisecond pulsar population of a cluster, is essential for understanding the importance of binary systems for the evolution of globular clusters, and provides complementary insights into magnetospheric emission processes.
Aims: Our goal is to constrain the millisecond pulsar populations in globular clusters from analysis of gamma-ray observations.
Methods: We use 546 days of continuous sky-survey observations obtained with the Large Area Telescope aboard the Fermi Gamma-ray Space Telescope to study the gamma-ray emission towards 13 globular clusters.
Results: Steady point-like high-energy gamma-ray emission has been significantly detected towards 8 globular clusters. Five of them (47 Tucanae, Omega Cen, NGC 6388, Terzan 5, and M 28) show hard spectral power indices (0.7 < Γ <1.4) and clear evidence for an exponential cut-off in the range 1.0-2.6 GeV, which is the characteristic signature of magnetospheric emission from MSPs. Three of them (M 62, NGC 6440 and NGC 6652) also show hard spectral indices (1.0 < Γ < 1.7), however the presence of an exponential cut-off can not be unambiguously established. Three of them (Omega Cen, NGC 6388, NGC 6652) have no known radio or X-ray MSPs yet still exhibit MSP spectral properties. From the observed gamma-ray luminosities, we estimate the total number of MSPs that is expected to be present in these globular clusters. We show that our estimates of the MSP population correlate with the stellar encounter rate and we estimate 2600-4700 MSPs in Galactic globular clusters, commensurate with previous estimates.
Conclusions: The observation of high-energy gamma-ray emission from globular clusters thus provides a reliable independent method to assess their millisecond pulsar populations....
Astronomy and Astrophysics, Dec. 2010

Search for Gamma-ray Emission from Magnetars with the Fermi Large Area Telescope
Abdo, A. A.; Ackermann, M.; Ajello, M.; Allafort, A.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Bellazzini, R.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Cecchi, C.; Çelik, Ö.; Chaty, S.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Conrad, J.; den Hartog, P. R.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Dib, R.; Dormody, M.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Enoto, T.; Favuzzi, C.; Frailis, M.; Fusco, P.; Gargano, F.; Gehrels, N.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Guiriec, S.; Hadasch, D.; Hanabata, Y.; Harding, A. K.; Hays, E.; Israel, G. L.; Jóhannesson, G.; Johnson, A. S.; Kaspi, V. M.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Lee, S. -H.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Marelli, M.; Mazziotta, M. N.; McEnery, J. E.; Mehault, J.; Michelson, P. F.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Naumann-Godo, M.; Nolan, P. L.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Parent, D.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Rea, N.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Sadrozinski, H. F. -W.; Saz Parkinson, P. M.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Troja, E.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vianello, G.; Vitale, V.; Waite, A. P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ziegler, M., We report on the search for 0.1-10 GeV emission from magnetars in 17 months of Fermi Large Area Telescope (LAT) observations. No significant evidence for gamma-ray emission from any of the currently known magnetars is found. The most stringent upper limits to date on their persistent emission in the Fermi energy range are estimated between ~10^-12and10^-10 erg s^-1 cm^-2, depending on the source. We also searched for gamma-ray pulsations and possible outbursts, also with no significant detection. The upper limits derived support the presence of a cutoff at an energy below a few MeV in the persistent emission of magnetars. They also show the likely need for a revision of current models of outer-gap emission from strongly magnetized pulsars, which, in some realizations, predict detectable GeV emission from magnetars at flux levels exceeding the upper limits identified here using the Fermi-LAT observations....
The Astrophysical Journal, Dec. 2010

Fermi Large Area Telescope observations of Local Group galaxies: detection of M 31 and search for M 33
Abdo, A. A.; Ackermann, M.; Ajello, M.; Allafort, A.; Atwood, W. B.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Brandt, T. J.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Cannon, A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Silva, E. Do Couto E.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Favuzzi, C.; Fegan, S. J.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Germani, S.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Guiriec, S.; Gustafsson, M.; Hadasch, D.; Harding, A. K.; Hayashi, K.; Hayashida, M.; Hays, E.; Healey, S. E.; Jean, P.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, T. J.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kerr, M.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Martin, P.; Mazziotta, M. N.; Mehault, J.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Naumann-Godo, M.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pepe, M.; Persic, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Ritz, S.; Romani, R. W.; Sadrozinski, H. F. -W.; Saz Parkinson, P. M.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Strigari, L.; Strong, A. W.; Suson, D. J.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ziegler, M., Context. Cosmic rays (CRs) can be studied through the galaxy-wide gamma-ray emission that they generate when propagating in the interstellar medium. The comparison of the diffuse signals from different systems may inform us about the key parameters in CR acceleration and transport.
Aims: We aim to determine and compare the properties of the cosmic-ray-induced gamma-ray emission of several Local Group galaxies.
Methods: We use 2 years of nearly continuous sky-survey observations obtained with the Large Area Telescope aboard the Fermi Gamma-ray Space Telescope to search for gamma-ray emission from M 31 and M 33. We compare the results with those for the Large Magellanic Cloud, the Small Magellanic Cloud, the Milky Way, and the starburst galaxies M 82 and NGC 253.
Results: We detect a gamma-ray signal at 5σ significance in the energy range 200 MeV-20 GeV that is consistent with originating from M 31. The integral photon flux above 100 MeV amounts to (9.1 ± 1.9_stat ± 1.0_sys) × 10^-9 ph cm^-2 s^-1. We find no evidence for emission from M 33 and derive an upper limit on the photon flux >100 MeV of 5.1 × 10^-9 ph cm^-2 s^-1 (2σ). Comparing these results to the properties of other Local Group galaxies, we find indications of a correlation between star formation rate and gamma-ray luminosity that also holds for the starburst galaxies.
Conclusions: The gamma-ray luminosity of M 31 is about half that of the Milky Way, which implies that the ratio between the average CR densities in M 31 and the Milky Way amounts to ξ = 0.35 ± 0.25. The observed correlation between gamma-ray luminosity and star formation rate suggests that the flux of M 33 is not far below the current upper limit from the LAT observations. Appendix A is only available in electronic form at http://www.aanda.org...
Astronomy and Astrophysics, Nov. 2010

Hard X-ray and gamma-ray detector for ASTRO-H based on Si and CdTe imaging sensors
Kokubun, M.; Watanabe, S.; Nakazawa, K.; Tajima, H.; Fukazawa, Y.; Takahashi, T.; Kataoka, J.; Kamae, T.; Katagiri, H.; Madejski, G. M.; Makishima, K.; Mizuno, T.; Ohno, M.; Sato, R.; Takahashi, H.; Tanaka, T.; Tashiro, M.; Terada, Y.; Yamaoka, K.; HXI/SGD Team, We have been developing a hard X-ray imager and soft gamma-ray detector as on board instruments of the ASTRO-H mission. The Hard X-ray Imager (HXI) is one of the three focal plane detectors of ASTRO-H, which is aimed to realize the focusing imaging of hard X-ray photons in combination with hard X-ray telescopes. By use of the hybrid structure composed of double-sided silicon strip detectors and a cadmium telluride strip detector, it fully covers the energy range up to 80 keV with a high quantum efficiency. High spatial resolutions of 250μm pitch and energy resolutions of 1-2 keV (FWMH) are at the same time achieved with low noise front-end ASICs. The Soft Gamma-ray Detector (SGD) is a novel and unique detector which is characterized by semiconductor Compton cameras surrounded by narrow field-of-view active shields, and covers a higher energy range (30-600 keV) than that of HXI. It consists of four Compton Cameras constructed with many layers of Silicon and CdTe pad detectors. With its multi-layer structure and Compton reconstruction capability, in addition to the BGO active shields read by Avalanche photo-diodes, this detector will achieve an extremely high background rejection efficiency in the orbit. We report the current status of hardware development including the design requirement, expected performance, and technical readinesses of key technologies....
Nuclear Instruments and Methods in Physics Research A, Nov. 2010

Searches for cosmic-ray electron anisotropies with the Fermi Large Area Telescope
Ackermann, M.; Ajello, M.; Atwood, W. B.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Buehler, R.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Cuoco, A.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; di Bernardo, G.; Do Couto E Silva, E.; Drell, P. S.; Dubois, R.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gaggero, D.; Gargano, F.; Germani, S.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grasso, D.; Grenier, I. A.; Grove, J. E.; Guiriec, S.; Gustafsson, M.; Hadasch, D.; Harding, A. K.; Hayashi, K.; Hays, E.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kerr, M.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Lemoine-Goumard, M.; Llena Garde, M.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Mazziotta, M. N.; McEnery, J. E.; Mehault, J.; Michelson, P. F.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Naumann-Godo, M.; Nolan, P. L.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Profumo, S.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ripken, J.; Ritz, S.; Roth, M.; Sadrozinski, H. F. -W.; Sander, A.; Schalk, T. L.; Sgrò, C.; Siegal-Gaskins, J.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Strong, A. W.; Suson, D. J.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ylinen, T.; Zaharijas, G.; Ziegler, M., The Large Area Telescope on board the Fermi satellite (Fermi LAT) detected more than 1.6×10⁶ cosmic-ray electrons/positrons with energies above 60 GeV during its first year of operation. The arrival directions of these events were searched for anisotropies of angular scale extending from ̃10° up to 90°, and of minimum energy extending from 60 GeV up to 480 GeV. Two independent techniques were used to search for anisotropies, both resulting in null results. Upper limits on the degree of the anisotropy were set that depended on the analyzed energy range and on the anisotropy’s angular scale. The upper limits for a dipole anisotropy ranged from ̃0.5% to ̃10%....
Physical Review D, Nov. 2010

Detection of the Small Magellanic Cloud in gamma-rays with Fermi/LAT
Abdo, A. A.; Ackermann, M.; Ajello, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Brandt, T. J.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Dermer, C. D.; de Palma, F.; Digel, S. W.; Silva, E. Do Couto E.; Drell, P. S.; Dubois, R.; Dumora, D.; Favuzzi, C.; Fegan, S. J.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guiriec, S.; Hadasch, D.; Harding, A. K.; Hayashida, M.; Hays, E.; Horan, D.; Hughes, R. E.; Jean, P.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kerr, M.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Lemoine-Goumard, M.; Llena Garde, M.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Martin, P.; Mazziotta, M. N.; McEnery, J. E.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Naumann-Godo, M.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ripken, J.; Ritz, S.; Romani, R. W.; Sadrozinski, H. F. -W.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Strong, A. W.; Suson, D. J.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ylinen, T.; Ziegler, M., Context. The flux of gamma rays with energies greater than 100 MeV is dominated by diffuse emission coming from cosmic-rays (CRs) illuminating the interstellar medium (ISM) of our Galaxy through the processes of Bremsstrahlung, pion production and decay, and inverse-Compton scattering. The study of this diffuse emission provides insight into the origin and transport of cosmic rays.
Aims: We searched for gamma-ray emission from the Small Magellanic Cloud (SMC) in order to derive constraints on the cosmic-ray population and transport in an external system with properties different from the Milky Way.
Methods: We analysed the first 17 months of continuous all-sky observations by the Large Area Telescope (LAT) of the Fermi mission to determine the spatial distribution, flux and spectrum of the gamma-ray emission from the SMC. We also used past radio synchrotron observations of the SMC to study the population of CR electrons specifically.
Results: We obtained the first detection of the SMC in high-energy gamma rays, with an integrated >100 MeV flux of (3.7±0.7) × 10^-8 ph cm^-2 s^-1, with additional systematic uncertainty of ≤16%. The emission is steady and from an extended source ~3° in size. It is not clearly correlated with the distribution of massive stars or neutral gas, nor with known pulsars or supernova remnants, but a certain correlation with supergiant shells is observed.
Conclusions: The observed flux implies an upper limit on the average CR nuclei density in the SMC of ~15% of the value measured locally in the Milky Way. The population of high-energy pulsars of the SMC may account for a substantial fraction of the gamma-ray flux, which would make the inferred CR nuclei density even lower. The average density of CR electrons derived from radio synchrotron observations is consistent with the same reduction factor but the uncertainties are large. From our current knowledge of the SMC, such a low CR density does not seem to be due to a lower rate of CR injection and rather indicates a smaller CR confinement volume characteristic size....
Astronomy and Astrophysics, Nov. 2010

Fermi Large Area Telescope Observation of a Gamma-ray Source at the Position of Eta Carinae
Abdo, A. A.; Ackermann, M.; Ajello, M.; Allafort, A.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Brandt, T. J.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Buehler, R.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Chaty, S.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cominsky, L. R.; Conrad, J.; Dermer, C. D.; de Palma, F.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Frailis, M.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Gehrels, N.; Germani, S.; Giglietto, N.; Giordano, F.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hadasch, D.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Hill, A. B.; Horan, D.; Hughes, R. E.; Itoh, R.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kerr, M.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Lemoine-Goumard, M.; Livingstone, M.; Llena Garde, M.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Mazziotta, M. N.; McEnery, J. E.; Mehault, J.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Naumann-Godo, M.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Sadrozinski, H. F. -W.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Tibolla, O.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wallace, E.; Wang, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ylinen, T.; Ziegler, M., The Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope detected a γ-ray source that is spatially consistent with the location of Eta Carinae. This source has been persistently bright since the beginning of the LAT survey observations (from 2008 August to 2009 July, the time interval considered here). The γ-ray signal is detected significantly throughout the LAT energy band (i.e., up to ~100 GeV). The 0.1-100 GeV energy spectrum is well represented by a combination of a cutoff power-law model (<10 GeV) and a hard power-law component (>10 GeV). The total flux (>100 MeV) is 3.7^+0.3 _-0.1 × 10^-7 photons s^-1 cm^-2, with additional systematic uncertainties of 10%, and consistent with the average flux measured by AGILE. The light curve obtained by Fermi is consistent with steady emission. Our observations do not confirm the presence of a γ-ray flare in 2008 October, as reported by Tavani et al., although we cannot exclude that a flare lasting only a few hours escaped detection by the Fermi LAT. We also do not find any evidence for γ-ray variability that correlates with the large X-ray variability of Eta Carinae observed during 2008 December and 2009 January. We are thus not able to establish an unambiguous identification of the LAT source with Eta Carinae....
The Astrophysical Journal, Nov. 2010

Fermi Large Area Telescope Constraints on the Gamma-ray Opacity of the Universe
Abdo, A. A.; Ackermann, M.; Ajello, M.; Allafort, A.; Atwood, W. B.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bhat, P. N.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Brandt, T. J.; Bregeon, J.; Brez, A.; Briggs, M. S.; Brigida, M.; Bruel, P.; Buehler, R.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Chen, A. W.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Connaughton, V.; Conrad, J.; Costamante, L.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Dingus, B. L.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Favuzzi, C.; Fegan, S. J.; Finke, J.; Fortin, P.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Gilmore, R. C.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Granot, J.; Greiner, J.; Grenier, I. A.; Grove, J. E.; Guiriec, S.; Gustafsson, M.; Hadasch, D.; Hayashida, M.; Hays, E.; Horan, D.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kocevski, D.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Llena Garde, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; McGlynn, S.; Mehault, J.; Mészáros, P.; Michelson, P. F.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Naumann-Godo, M.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Primack, J. R.; Rainò, S.; Rando, R.; Razzano, M.; Razzaque, S.; Reimer, A.; Reimer, O.; Reyes, L. C.; Ripken, J.; Ritz, S.; Romani, R. W.; Roth, M.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Scargle, J. D.; Schalk, T. L.; Sgrò, C.; Shaw, M. S.; Siskind, E. J.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stecker, F. W.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vilchez, N.; Vitale, V.; von Kienlin, A.; Waite, A. P.; Wang, P.; Wilson-Hodge, C.; Winer, B. L.; Wood, K. S.; Yamazaki, R.; Yang, Z.; Ylinen, T.; Ziegler, M., The extragalactic background light (EBL) includes photons with wavelengths from ultraviolet to infrared, which are effective at attenuating gamma rays with energy above ~10 GeV during propagation from sources at cosmological distances. This results in a redshift- and energy-dependent attenuation of the γ-ray flux of extragalactic sources such as blazars and gamma-ray bursts (GRBs). The Large Area Telescope on board Fermi detects a sample of γ-ray blazars with redshift up to z ~ 3, and GRBs with redshift up to z ~ 4.3. Using photons above 10 GeV collected by Fermi over more than one year of observations for these sources, we investigate the effect of γ-ray flux attenuation by the EBL. We place upper limits on the γ-ray opacity of the universe at various energies and redshifts and compare this with predictions from well-known EBL models. We find that an EBL intensity in the optical-ultraviolet wavelengths as great as predicted by the "baseline" model of Stecker et al. can be ruled out with high confidence....
The Astrophysical Journal, Nov. 2010

Fermi LAT observations of cosmic-ray electrons from 7 GeV to 1 TeV
Ackermann, M.; Ajello, M.; Atwood, W. B.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellardi, F.; Bellazzini, R.; Belli, F.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bogart, J. R.; Bonamente, E.; Borgland, A. W.; Brandt, T. J.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Buehler, R.; Burnett, T. H.; Busetto, G.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carlson, P.; Carrigan, S.; Casandjian, J. M.; Ceccanti, M.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Cillis, A. N.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Corbet, R.; Deklotz, M.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; di Bernardo, G.; Do Couto E Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Fabiani, D.; Favuzzi, C.; Fegan, S. J.; Fortin, P.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gaggero, D.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grasso, D.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guiriec, S.; Gustafsson, M.; Hadasch, D.; Harding, A. K.; Hayashida, M.; Hays, E.; Horan, D.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kerr, M.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Llena Garde, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Mazziotta, M. N.; McEnery, J. E.; Mehault, J.; Michelson, P. F.; Minuti, M.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Naumann-Godo, M.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Petrosian, V.; Pinchera, M.; Piron, F.; Porter, T. A.; Profumo, S.; Rainò, S.; Rando, R.; Rapposelli, E.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ripken, J.; Ritz, S.; Rochester, L. S.; Romani, R. W.; Roth, M.; Sadrozinski, H. F. -W.; Saggini, N.; Sanchez, D.; Sander, A.; Sgrò, C.; Siskind, E. J.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stawarz, Ł.; Stephens, T. E.; Strickman, M. S.; Strong, A. W.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Tibolla, O.; Torres, D. F.; Tosti, G.; Tramacere, A.; Turri, M.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wallace, E.; Wang, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ylinen, T.; Ziegler, M., We present the results of our analysis of cosmic-ray electrons using about 8×10⁶ electron candidates detected in the first 12 months on-orbit by the Fermi Large Area Telescope. This work extends our previously published cosmic-ray electron spectrum down to 7 GeV, giving a spectral range of approximately 2.5 decades up to 1 TeV. We describe in detail the analysis and its validation using beam-test and on-orbit data. In addition, we describe the spectrum measured via a subset of events selected for the best energy resolution as a cross-check on the measurement using the full event sample. Our electron spectrum can be described with a power law ∝E^-3.08±0.05 with no prominent spectral features within systematic uncertainties. Within the limits of our uncertainties, we can accommodate a slight spectral hardening at around 100 GeV and a slight softening above 500 GeV....
Physical Review D, Nov. 2010

Fermi Gamma-ray Space Telescope Observations of Gamma-ray Outbursts from 3C 454.3 in 2009 December and 2010 April
Ackermann, M.; Ajello, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Corbel, S.; Cutini, S.; D'Ammando, F.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Escande, L.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Fuhrmann, L.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grove, J. E.; Guiriec, S.; Hadasch, D.; Hayashida, M.; Hays, E.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Larsson, S.; Latronico, L.; Lee, S. -H.; Llena Garde, M.; Longo, F.; Loparco, F.; Lott, B.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Marchili, N.; Mazziotta, M. N.; McEnery, J. E.; Mehault, J.; Michelson, P. F.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Nalewajko, K.; Naumann-Godo, M.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reyes, L. C.; Ripken, J.; Ritz, S.; Roth, M.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Scargle, J. D.; Sgrò, C.; Sikora, M.; Siskind, E. J.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Tanaka, Y.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Usher, T. L.; Vandenbroucke, J.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Wehrle, A. E.; Winer, B. L.; Yang, Z.; Ylinen, T.; Ziegler, M., The flat spectrum radio quasar 3C 454.3 underwent an extraordinary outburst in 2009 December when it became the brightest γ-ray source in the sky for over 1 week. Its daily flux measured with the Fermi-Large Area Telescope at photon energies E>100 MeV reached F ₁₀₀ = 22 ± 1 × 10^-6 photon cm^-2 s^-1, representing the highest daily flux of any blazar ever recorded in high-energy γ-rays. It again became the brightest source in the sky in 2010 April, triggering a pointed-mode observation by Fermi. The correlated γ-ray temporal and spectral properties during these exceptional events are presented and discussed. The main results show flux variability over time scales less than 3 hr and very mild spectral variability with an indication of gradual hardening preceding major flares. The light curves during periods of enhanced activity in 2008 July-August and 2010 December show strong resemblance, with a flux plateau of a few days preceding the major flare. No consistent loop pattern emerged in the γ-ray spectral index versus the flux plane as would be expected in acceleration and cooling scenarios. The maximum energy of a photon from 3C 454.3 is ≈20 GeV and a minimum Doppler factor of ≈13 is derived. The γ-ray spectrum of 3C 454.3 shows a significant spectral break between ≈2 and 3 GeV that is very weakly dependent on the flux state, even when the flux changes by an order of magnitude....
The Astrophysical Journal, Oct. 2010

Fermi Large Area Telescope and Multi-wavelength Observations of the Flaring Activity of PKS 1510-089 between 2008 September and 2009 June
Abdo, A. A.; Ackermann, M.; Agudo, I.; Ajello, M.; Allafort, A.; Aller, H. D.; Aller, M. F.; Antolini, E.; Arkharov, A. A.; Axelsson, M.; Bach, U.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berdyugin, A.; Berenji, B.; Blandford, R. D.; Blinov, D. A.; Bloom, E. D.; Boettcher, M.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Buehler, R.; Buemi, C. S.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carosati, D.; Carrigan, S.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Chen, W. P.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Corbel, S.; Costamante, L.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Donato, D.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Focke, W. B.; Forné, E.; Fortin, P.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grove, J. E.; Guiriec, S.; Gurwell, M. A.; Gusbar, C.; Gómez, J. L.; Hadasch, D.; Hagen-Thorn, V. A.; Hayashida, M.; Hays, E.; Horan, D.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kimeridze, G.; Knödlseder, J.; Konstantinova, T. S.; Kopatskaya, E. N.; Koptelova, E.; Kovalev, Y. Y.; Kurtanidze, O. M.; Kuss, M.; Lahteenmaki, A.; Lande, J.; Larionov, V. M.; Larionova, E. G.; Larionova, L. V.; Larsson, S.; Latronico, L.; Lee, S. -H.; Leto, P.; Lister, M. L.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Massaro, E.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; McHardy, I. M.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morozova, D. A.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Naumann-Godo, M.; Nikolashvili, M. G.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pasanen, M.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Pushkarev, A. B.; Rainò, S.; Raiteri, C. M.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reinthal, R.; Ripken, J.; Ritz, S.; Roca-Sogorb, M.; Rodriguez, A. Y.; Roth, M.; Roustazadeh, P.; Ryde, F.; Sadrozinski, H. F. -W.; Sander, A.; Scargle, J. D.; Sgrò, C.; Sigua, L. A.; Smith, P. D.; Sokolovsky, K.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Takahashi, T.; Takalo, L. O.; Tanaka, T.; Taylor, B.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Tornikoski, M.; Torres, D. F.; Tosti, G.; Tramacere, A.; Trigilio, C.; Troitsky, I. S.; Umana, G.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vilchez, N.; Villata, M.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ylinen, T.; Ziegler, M., We report on the multi-wavelength observations of PKS 1510-089 (a flat spectrum radio quasar (FSRQ) at z = 0.361) during its high activity period between 2008 September and 2009 June. During this 11 month period, the source was characterized by a complex variability at optical, UV, and γ-ray bands, on timescales down to 6-12 hr. The brightest γ-ray isotropic luminosity, recorded on 2009 March 26, was sime2 × 10⁴⁸ erg s^-1. The spectrum in the Fermi Large Area Telescope energy range shows a mild curvature described well by a log-parabolic law, and can be understood as due to the Klein-Nishina effect. The γ-ray flux has a complex correlation with the other wavelengths. There is no correlation at all with the X-ray band, a weak correlation with the UV, and a significant correlation with the optical flux. The γ-ray flux seems to lead the optical one by about 13 days. From the UV photometry, we estimated a black hole mass of sime5.4 × 10⁸ M _sun and an accretion rate of sime0.5 M _sun yr^-1. Although the power in the thermal and non-thermal outputs is smaller compared to the very luminous and distant FSRQs, PKS 1510-089 exhibits a quite large Compton dominance and a prominent big blue bump (BBB) as observed in the most powerful γ-ray quasars. The BBB was still prominent during the historical maximum optical state in 2009 May, but the optical/UV spectral index was softer than in the quiescent state. This seems to indicate that the BBB was not completely dominated by the synchrotron emission during the highest optical state. We model the broadband spectrum assuming a leptonic scenario in which the inverse Compton emission is dominated by the scattering of soft photons produced externally to the jet. The resulting model-dependent jet energetic content is compatible with a scenario in which the jet is powered by the accretion disk, with a total efficiency within the Kerr black hole limit....
The Astrophysical Journal, Oct. 2010

Gamma-ray Light Curves and Variability of Bright Fermi-detected Blazars
Abdo, A. A.; Ackermann, M.; Ajello, M.; Antolini, E.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Buehler, R.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cominsky, L. R.; Conrad, J.; Costamante, L.; Cutini, S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giommi, P.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guiriec, S.; Hadasch, D.; Hayashida, M.; Hays, E.; Healey, S. E.; Horan, D.; Hughes, R. E.; Itoh, R.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Knödlseder, J.; Kuss, M.; Lande, J.; Larsson, S.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Massaro, E.; Mazziotta, M. N.; McEnery, J. E.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Mueller, M.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Ritz, S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sander, A.; Scargle, J. D.; Sgrò, C.; Shaw, M. S.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wallace, E.; Wang, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ylinen, T.; Ziegler, M., This paper presents light curves as well as the first systematic characterization of variability of the 106 objects in the high-confidence Fermi Large Area Telescope Bright AGN Sample (LBAS). Weekly light curves of this sample, obtained during the first 11 months of the Fermi survey (2008 August 4-2009 July 4), are tested for variability and their properties are quantified through autocorrelation function and structure function analysis. For the brightest sources, 3 or 4 day binned light curves are extracted in order to determine power density spectra (PDSs) and to fit the temporal structure of major flares. More than 50% of the sources are found to be variable with high significance, where high states do not exceed 1/4 of the total observation range. Variation amplitudes are larger for flat spectrum radio quasars and low/intermediate synchrotron frequency peaked BL Lac objects. Autocorrelation timescales derived from weekly light curves vary from four to a dozen of weeks. Variable sources of the sample have weekly and 3-4 day bin light curves that can be described by 1/f ^α PDS, and show two kinds of gamma-ray variability: (1) rather constant baseline with sporadic flaring activity characterized by flatter PDS slopes resembling flickering and red noise with occasional intermittence and (2)—measured for a few blazars showing strong activity—complex and structured temporal profiles characterized by long-term memory and steeper PDS slopes, reflecting a random walk underlying mechanism. The average slope of the PDS of the brightest 22 FSRQs and of the 6 brightest BL Lacs is 1.5 and 1.7, respectively. The study of temporal profiles of well-resolved flares observed in the 10 brightest LBAS sources shows that they generally have symmetric profiles and that their total duration vary between 10 and 100 days. Results presented here can assist in source class recognition for unidentified sources and can serve as reference for more detailed analysis of the brightest gamma-ray blazars....
The Astrophysical Journal, Oct. 2010

Fermi-LAT Study of Gamma-ray Emission in the Direction of Supernova Remnant W49B
Abdo, A. A.; Ackermann, M.; Ajello, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Dermer, C. D.; de Palma, F.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Dumora, D.; Favuzzi, C.; Funk, S.; Fusco, P.; Gargano, F.; Gehrels, N.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hadasch, D.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Horan, D.; Hughes, R. E.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Katsuta, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Mazziotta, M. N.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Naumann-Godo, M.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ripken, J.; Roth, M.; Sadrozinski, H. F. -W.; Sander, A.; Saz Parkinson, P. M.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Tibaldo, L.; Tibolla, O.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M., We present an analysis of the gamma-ray data obtained with the Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope in the direction of SNR W49B (G43.3-0.2). A bright unresolved gamma-ray source detected at a significance of 38σ is found to coincide with SNR W49B. The energy spectrum in the 0.2-200 GeV range gradually steepens toward high energies. The luminosity is estimated to be 1.5 × 10³⁶ (D/8 kpc)² erg s^-1 in this energy range. There is no indication that the gamma-ray emission comes from a pulsar. Assuming that the supernova remnant (SNR) shell is the site of gamma-ray production, the observed spectrum can be explained either by the decay of neutral π mesons produced through the proton-proton collisions or by electron bremsstrahlung. The calculated energy density of relativistic particles responsible for the LAT flux is estimated to be remarkably large, U _e,p >10⁴ eV cm^-3, for either gamma-ray production mechanism....
The Astrophysical Journal, Oct. 2010

The Fermi-LAT High-Latitude Survey: Source Count Distributions and the Origin of the Extragalactic Diffuse Background
Abdo, A. A.; Ackermann, M.; Ajello, M.; Antolini, E.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Costamante, L.; Cutini, S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giommi, P.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grove, J. E.; Guiriec, S.; Hadasch, D.; Hayashida, M.; Hays, E.; Healey, S. E.; Horan, D.; Hughes, R. E.; Itoh, R.; Jóhannesson, G.; Johnson, A. S.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Lemoine-Goumard, M.; Llena Garde, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Sadrozinski, H. F. -W.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Sgrò, C.; Shaw, M. S.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Strickman, M. S.; Strong, A. W.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ylinen, T.; Ziegler, M.; Fermi LAT Collaboration, This is the first of a series of papers aimed at characterizing the populations detected in the high-latitude sky of the Fermi-LAT survey. In this work, we focus on the intrinsic spectral and flux properties of the source sample. We show that when selection effects are properly taken into account, Fermi sources are on average steeper than previously found (e.g., in the bright source list) with an average photon index of 2.40 ± 0.02 over the entire 0.1-100 GeV energy band. We confirm that flat spectrum radio quasars have steeper spectra than BL Lacertae objects with an average index of 2.48 ± 0.02 versus 2.18 ± 0.02. Using several methods, we build the deepest source count distribution at GeV energies, deriving that the intrinsic source (i.e., blazar) surface density at F ₁₀₀ >= 10^-9 ph cm^-2 s^-1 is 0.12^+0.03 _-0.02 deg^-2. The integration of the source count distribution yields that point sources contribute 16(±1.8)% (±7% systematic uncertainty) of the GeV isotropic diffuse background. At the fluxes currently reached by LAT, we can rule out the hypothesis that pointlike sources (i.e., blazars) produce a larger fraction of the diffuse emission....
The Astrophysical Journal, Sep. 2010

Fermi Large Area Telescope Observations of Gamma-ray Pulsars PSR J1057-5226, J1709-4429, and J1952+3252
Abdo, A. A.; Ajello, M.; Antolini, E.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Buehler, R.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Camilo, F.; Caraveo, P. A.; Çelik, Ö.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cognard, I.; Cohen-Tanugi, J.; Dermer, C. D.; de Palma, F.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Favuzzi, C.; Ferrara, E. C.; Fortin, P.; Frailis, M.; Freire, P. C. C.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gehrels, N.; Germani, S.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hadasch, D.; Hanabata, Y.; Harding, A. K.; Hays, E.; Jóhannesson, G.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Johnston, S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Keith, M.; Kerr, M.; Knödlseder, J.; Kramer, M.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lubrano, P.; Makeev, A.; Manchester, R. N.; Marelli, M.; Mazziotta, M. N.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Nolan, P. L.; Norris, J. P.; Noutsos, A.; Nuss, E.; Ohsugi, T.; Okumura, A.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Rainò, S.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ripken, J.; Romani, R. W.; Sadrozinski, H. F. -W.; Sander, A.; Saz Parkinson, P. M.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Theureau, G.; Thompson, D. J.; Thorsett, S. E.; Tibaldo, L.; Tibolla, O.; Torres, D. F.; Tosti, G.; Tramacere, A.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vitale, V.; Waite, A. P.; Wang, P.; Weltevrede, P.; Winer, B. L.; Yang, Z.; Ylinen, T.; Ziegler, M., The Fermi Large Area Telescope (LAT) data have confirmed the pulsed emission from all six high-confidence gamma-ray pulsars previously known from the EGRET observations. We report results obtained from the analysis of 13 months of LAT data for three of these pulsars (PSR J1057-5226, PSR J1709-4429, and PSR J1952+3252) each of which had some unique feature among the EGRET pulsars. The excellent sensitivity of LAT allows more detailed analysis of the evolution of the pulse profile with energy and also of the variation of the spectral shape with phase. We measure the cutoff energy of the pulsed emission from these pulsars for the first time and provide a more complete picture of the emission mechanism. The results confirm some, but not all, of the features seen in the EGRET data....
The Astrophysical Journal, Sep. 2010

Fermi-LAT Observations of the Geminga Pulsar
Abdo, A. A.; Ackermann, M.; Ajello, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bignami, G. F.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Dermer, C. D.; de Palma, F.; Dormody, M.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Edmonds, Y.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giavitto, G.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hadasch, D.; Harding, A. K.; Hays, E.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Marelli, M.; Mazziotta, M. N.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Ray, P. S.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Usher, T. L.; Van Etten, A.; Vasileiou, V.; Venter, C.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Watters, K.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M., We report on the Fermi-LAT observations of the Geminga pulsar, the second brightest non-variable GeV source in the γ-ray sky and the first example of a radio-quiet γ-ray pulsar. The observations cover one year, from the launch of the Fermi satellite through 2009 June 15. A data sample of over 60,000 photons enabled us to build a timing solution based solely on γ-rays. Timing analysis shows two prominent peaks, separated by ∆phi = 0.497 ± 0.004 in phase, which narrow with increasing energy. Pulsed γ-rays are observed beyond 18 GeV, precluding emission below 2.7 stellar radii because of magnetic absorption. The phase-averaged spectrum was fitted with a power law with exponential cutoff of spectral index Γ = (1.30 ± 0.01 ± 0.04), cutoff energy E ₀ = (2.46 ± 0.04 ± 0.17) GeV, and an integral photon flux above 0.1 GeV of (4.14 ± 0.02 ± 0.32) × 10^-6 cm^-2 s^-1. The first uncertainties are statistical and the second ones are systematic. The phase-resolved spectroscopy shows a clear evolution of the spectral parameters, with the spectral index reaching a minimum value just before the leading peak and the cutoff energy having maxima around the peaks. The phase-resolved spectroscopy reveals that pulsar emission is present at all rotational phases. The spectral shape, broad pulse profile, and maximum photon energy favor the outer magnetospheric emission scenarios....
The Astrophysical Journal, Sep. 2010

Fermi Large Area Telescope Observations of Misaligned Active Galactic Nuclei
Abdo, A. A.; Ackermann, M.; Ajello, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Brandt, T. J.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Buehler, R.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Cannon, A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Celotti, A.; Charles, E.; Chekhtman, A.; Chen, A. W.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Colafrancesco, S.; Conrad, J.; Davis, D. S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grandi, P.; Grenier, I. A.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hadasch, D.; Hayashida, M.; Hays, E.; Horan, D.; Hughes, R. E.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Lemoine-Goumard, M.; Llena Garde, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Malaguti, G.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Michelson, P. F.; Migliori, G.; Mitthumsiri, W.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Naumann-Godo, M.; Nestoras, I.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Persic, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Razzaque, S.; Reimer, A.; Reimer, O.; Reyes, L. C.; Roth, M.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Scargle, J. D.; Sgrò, C.; Siskind, E. J.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stawarz, Ł.; Stecker, F. W.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Torresi, E.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vilchez, N.; Villata, M.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ylinen, T.; Ziegler, M., Analysis is presented for 15 months of data taken with the Large Area Telescope (LAT) on the Fermi Gamma-ray Space Telescope for 11 non-blazar active galactic nuclei (AGNs), including seven FRI radio galaxies and four FRII radio sources consisting of two FRII radio galaxies and two steep spectrum radio quasars. The broad line FRI radio galaxy 3C 120 is reported here as a γ-ray source for the first time. The analysis is based on directional associations of LAT sources with radio sources in the 3CR, 3CRR, and MS4 (collectively referred to as 3C-MS) catalogs. Seven of the eleven LAT sources associated with 3C-MS radio sources have spectral indices larger than 2.3 and, except for the FRI radio galaxy NGC 1275 that shows possible spectral curvature, are well described by a power law. No evidence for time variability is found for any sources other than NGC 1275. The γ-ray luminosities of FRI radio galaxies are significantly smaller than those of the BL Lac objects detected by the LAT, whereas the γ-ray luminosities of the FRII sources are quite similar to those of FSRQs, which could reflect different beaming factors for the γ-ray emission. A core dominance (CD) study of the 3CRR sample indicates that sources closer to the jet axis are preferentially detected with the Fermi LAT, insofar as the γ-ray-detected misaligned AGNs have larger CD at a given average radio flux. The results are discussed in view of the AGN unification scenario....
The Astrophysical Journal, Sep. 2010

Infrared/optical-X-ray simultaneous observations of X-ray flares in GRB 071112C and GRB 080506
T. Uehara; M. Uemura; K. S. Kawabata; Y. Fukazawa; R. Yamazaki; A. Arai; M. Sasada; T. Ohsugi; T. Mizuno; H. Takahashi; H. Katagiri; T. Yamashita; M. Ohno; G. Sato; S. Sato; M. Kino, Aims. We investigate the origin of short X-ray flares which are occasionally observed in early stages of afterglows of gamma-ray bursts (GRBs).
Methods. We observed two Swift events, GRB 071112C and GRB 080506, before the start of X-ray flares in the optical and near-infrared (NIR) bands with the 1.5-m Kanata telescope. In conjunction with published X-ray and optical data, we analyzed densely sampled light curves of the early afterglows and spectral energy distributions (SEDs) in the NIR-X-ray ranges.
Results. We found that the SEDs had a break between the optical and X-ray bands in the normal decay phases of both GRBs regardless of the model for the correction of the interstellar extinction in host galaxies of GRBs. In the X-ray flares, X-ray flux increased by 3 and 15 times in the case of GRB 071112C and 080506, respectively, and the X-ray spectra became harder than those in the normal decay phases. No significant variation in the optical-NIR range was detected together with the X-ray flares.
Conclusions. These results suggest that the X-ray flares were associated with either late internal shocks or external shocks from two-component jets., EDP SCIENCES S A
ASTRONOMY & ASTROPHYSICS, Sep. 2010

Infrared/optical-X-ray simultaneous observations of X-ray flares in GRB 071112C and GRB 080506
Uehara Takeshi; Uemura Makoto; Kawabata Koji S; Fukazawa Yasushi; Yamazaki Ryo; Arai Akira; Sasada Mahito; Ohsugi Takashi; Mizuno Tsunefumi; Takahashi Hiromitsu; Katagiri Hideaki; Yamashita Takuya; Ohno Masanori; Sato Goro; Sato Shuji; Kino Masaru, Aims. We investigate the origin of short X-ray flares which are occasionally observed in early stages of afterglows of gamma-ray bursts (GRBs).Methods. We observed two Swift events, GRB 071112C and GRB 080506, before the start of X-ray flares in the optical and near-infrared (NIR) bands with the 1.5-m Kanata telescope. In conjunction with published X-ray and optical data, we analyzed densely sampled light curves of the early afterglows and spectral energy distributions (SEDs) in the NIR-X-ray ranges.Results. We found that the SEDs had a break between the optical and X-ray bands in the normal decay phases of both GRBs regardless of the model for the correction of the interstellar extinction in host galaxies of GRBs. In the X-ray flares, X-ray flux increased by 3 and 15 times in the case of GRB 071112C and 080506, respectively, and the X-ray spectra became harder than those in the normal decay phases. No significant variation in the optical-NIR range was detected together with the X-ray flares.Conclusions. These results suggest that the X-ray flares were associated with either late internal shocks or external shocks from two-component jets., EDP Sciences S A
Astronomy & Astrophysics, Sep. 2010, [Reviewed]

Fermi Large Area Telescope View of the Core of the Radio Galaxy Centaurus A
Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Brandt, T. J.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Cannon, A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Colafrancesco, S.; Cominsky, L. R.; Conrad, J.; Costamante, L.; Davis, D. S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Falcone, A.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Finke, J.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Georganopoulos, M.; Germani, S.; Giebels, B.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grandi, P.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hadasch, D.; Harding, A. K.; Hase, Hayo; Hayashida, M.; Hays, E.; Horan, D.; Hughes, R. E.; Itoh, R.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, T. J.; Johnson, W. N.; Kadler, M.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kishishita, T.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Lemoine-Goumard, M.; Llena Garde, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Müller, C.; Nakamori, T.; Naumann-Godo, M.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Ojha, R.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Pagani, C.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Plötz, C.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Razzaque, S.; Reimer, A.; Reimer, O.; Reposeur, T.; Ripken, J.; Ritz, S.; Rodriguez, A. Y.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Scargle, J. D.; Sgrò, C.; Siskind, E. J.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Stawarz, L.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ylinen, T.; Ziegler, M., We present γ-ray observations with the Large Area Telescope (LAT) on board the Fermi Gamma-Ray Space Telescope of the nearby radio galaxy Centaurus A (Cen A). The previous EGRET detection is confirmed, and the localization is improved using data from the first 10 months of Fermi science operation. In previous work, we presented the detection of the lobes by the LAT; in this work, we concentrate on the γ-ray core of Cen A. Flux levels as seen by the LAT are not significantly different from that found by EGRET, nor is the extremely soft LAT spectrum (Γ = 2.67 ± 0.10_stat ± 0.08_sys where the photon flux is Φ vprop E ^-Γ). The LAT core spectrum, extrapolated to higher energies, is marginally consistent with the non-simultaneous HESS spectrum of the source. The LAT observations are complemented by simultaneous observations from Suzaku, the Swift Burst Alert Telescope and X-ray Telescope, and radio observations with the Tracking Active Galactic Nuclei with Austral Milliarcsecond Interferometry program, along with a variety of non-simultaneous archival data from a variety of instruments and wavelengths to produce a spectral energy distribution (SED). We fit this broadband data set with a single-zone synchrotron/synchrotron self-Compton model, which describes the radio through GeV emission well, but fails to account for the non-simultaneous higher energy TeV emission observed by HESS from 2004 to 2008. The fit requires a low Doppler factor, in contrast to BL Lac objects which generally require larger values to fit their broadband SEDs. This indicates that the γ-ray emission originates from a slower region than that from BL Lac objects, consistent with previous modeling results from Cen A. This slower region could be a slower moving layer around a fast spine, or a slower region farther out from the black hole in a decelerating flow. The fit parameters are also consistent with Cen A being able to accelerate ultra-high energy cosmic-rays, as hinted at by results from the Auger observatory....
The Astrophysical Journal, Aug. 2010

Gamma-Ray Emission Concurrent with the Nova in the Symbiotic Binary V407 Cygni
Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Brandt, T. J.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Buehler, R.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cecchi, C.; Celik, O.; Charles, E.; Chaty, S.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Corbel, S.; Corbet, R.; DeCesar, M. E.; den Hartog, P. R.; Dermer, C. D.; de Palma, F.; Digel, S. W.; Donato, D.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Dubus, G.; Dumora, D.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Fortin, P.; Frailis, M.; Fuhrmann, L.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. H.; Grove, J. E.; Guiriec, S.; Hadasch, D.; Harding, A. K.; Hayashida, M.; Hays, E.; Healey, S. E.; Hill, A. B.; Horan, D.; Hughes, R. E.; Itoh, R.; Jean, P.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kerr, M.; Knödlseder, J.; Koerding, E.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. H.; Lemoine-Goumard, M.; Garde, M. L.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Mehault, J.; Michelson, P. F.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Naumann-Godo, M.; Nestoras, I.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainó, S.; Rando, R.; Ray, P. S.; Razzano, M.; Razzaque, S.; Rea, N.; Reimer, A.; Reimer, O.; Reposeur, T.; Ripken, J.; Ritz, S.; Romani, R. W.; Roth, M.; Sadrozinski, H. F.; Sander, A.; Parkinson, P. M.; Scargle, J. D.; Schinzel, F. K.; Sgrò, C.; Shaw, M. S.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Sokolovsky, K. V.; Spandre, G.; Spinelli, P.; Stawarz, Ł.; Strickman, M. S.; Suson, D. J.; Takahashi,, H.; Takahashi, T.; Tanaka, T.; Tanaka, Y.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J, Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wallace, E.; Wang, P.; Winer, B. L.; Wolff, M. T.; Wood, K. S.; Yang, Z.; Ylinen, T.; Ziegler, M.; Maehara, H.; Nishiyama, K.; Kabashima, F.; Bach, U.; Bower, G. C.; Falcone, A.; Forster, J. R.; Henden, A.; Kawabata, K. S.; Koubsky, P.; Mukai, K.; Nelson, T.; Oates, S. R.; Sakimoto, K.; Sasada, M.; Shenavrin, V. I.; Shore, S. N.; Skinner, G. K.; Sokoloski, J.; Stroh, M.; Tatarnikov, A. M.; Uemura, M.; Wahlgren, G. M.; Yamanaka, M.; Fermi LAT Collaboration, Novae are thermonuclear explosions on a white dwarf surface fueled by mass accreted from a companion star. Current physical models posit that shocked expanding gas from the nova shell can produce x-ray emission, but emission at higher energies has not been widely expected. Here, we report the Fermi Large Area Telescope detection of variable γ-ray emission (0.1 to 10 billion electron volts) from the recently detected optical nova of the symbiotic star V407 Cygni. We propose that the material of the nova shell interacts with the dense ambient medium of the red giant primary and that particles can be accelerated effectively to produce π⁰ decay γ-rays from proton-proton interactions. Emission involving inverse Compton scattering of the red giant radiation is also considered and is not ruled out....
Science, Aug. 2010

Optical and Near-Infrared Photometry of Nova V2362 Cyg: Rebrightening Event and Dust Formation
Akira Arai; Makoto Uemura; Koji S. Kawabata; Hiroyuki Maehara; Kazuhiro Nakajima; Seiichiro Kiyota; Taichi Kato; Takashi Ohsugi; Takuya Yamashita; Mizuki Isogai; Osamu Nagae; Shingo Chiynobu; Yasushi Fukazawa; Tsunefumi Mizuno; Hideaki Katagiri; Hiromitsu Takahashi; Kiichi Okita; Michitoshi Yoshida; Kenshi Yanagisawa; Shuji Sato; Masaru Kino; Masahiro Kitagawa; Kozo Sadakane, We present optical and near-infrared (NIR) photometry of a classical nova, V2362 Cyg (= Nova Cygni 2006). V2362 Cyg experienced a peculiar rebrightening during the period between 100 and 240d after the maximum of the nova. Our multicolor observation indicates the emergence of a pseudophotosphere with an effective temperature of similar to 9000 K at the rebrightening maximum. After the rebrightening maximum, the object showed a slow fading homogeneously in all of the used bands for one week. This implies that the fading soon after the rebrightening maximum (less than or similar to 1 week) was caused by a slowly shrinking pseudophotosphere. Then, the NIR flux drastically increased, while the optical flux steeply declined. The optical and NIR fluxes were consistent with blackbody radiation with a temperature of similar to 1500 K during this NIR rising phase. These facts are likely to be explained by dust formation in the nova ejecta. Assuming an optically thin case, we estimated the dust mass to be 10(-10)-10(-8) M-circle dot, which is less than those in typical dust-forming novae. These results support the senario that a second, long-lasting outflow which caused the rebrightening interacted with a fraction of the initial outflow and formed dust grains., OXFORD UNIV PRESS
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Aug. 2010, [Reviewed]

GeV Gamma-ray Flux Upper Limits from Clusters of Galaxies
Ackermann, M.; Ajello, M.; Allafort, A.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Blandford, R. D.; Blasi, P.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Brandt, T. J.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Colafrancesco, S.; Cominsky, L. R.; Conrad, J.; Dermer, C. D.; de Palma, F.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Edmonds, Y.; Farnier, C.; Favuzzi, C.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Guiriec, S.; Hadasch, D.; Harding, A. K.; Hayashida, M.; Hays, E.; Horan, D.; Hughes, R. E.; Jeltema, T. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kerr, M.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Mazziotta, M. N.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Naumann-Godo, M.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Pepe, M.; Pesce-Rollins, M.; Petrosian, V.; Pfrommer, C.; Piron, F.; Porter, T. A.; Profumo, S.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ripken, J.; Ritz, S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Sadrozinski, H. F. -W.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Sgrò, C.; Siskind, E. J.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Stawarz, Ł.; Strickman, M. S.; Strong, A. W.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tibaldo, L.; Tibolla, O.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ylinen, T.; Ziegler, M., The detection of diffuse radio emission associated with clusters of galaxies indicates populations of relativistic leptons infusing the intracluster medium (ICM). Those electrons and positrons are either injected into and accelerated directly in the ICM, or produced as secondary pairs by cosmic-ray ions scattering on ambient protons. Radiation mechanisms involving the energetic leptons together with the decay of neutral pions produced by hadronic interactions have the potential to produce abundant GeV photons. Here, we report on the search for GeV emission from clusters of galaxies using data collected by the Large Area Telescope on the Fermi Gamma-ray Space Telescope from 2008 August to 2010 February. Thirty-three galaxy clusters have been selected according to their proximity and high mass, X-ray flux and temperature, and indications of non-thermal activity for this study. We report upper limits on the photon flux in the range 0.2-100 GeV toward a sample of observed clusters (typical values (1-5) ×10^-9 photon cm^-2 s^-1) considering both point-like and spatially resolved models for the high-energy emission and discuss how these results constrain the characteristics of energetic leptons and hadrons, and magnetic fields in the ICM. The volume-averaged relativistic-hadron-to-thermal energy density ratio is found to be <5%-10% in several clusters....
The Astrophysical Journal, Jul. 2010

Fermi Observations of High-energy Gamma-ray Emission from GRB 090217A
Ackermann, M.; Ajello, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bhat, P. N.; Bissaldi, E.; Blandford, R. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Briggs, M. S.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Connaughton, V.; Conrad, J.; Cutini, S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Frailis, M.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Granot, J.; Grenier, I. A.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hadasch, D.; Hays, E.; Horan, D.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kippen, R. M.; Knödlseder, J.; Kocevski, D.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Llena Garde, M.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Mazziotta, M. N.; McBreen, S.; McEnery, J. E.; McGlynn, S.; Meegan, C.; Mehault, J.; Mészáros, P.; Michelson, P. F.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakajima, H.; Nakamori, T.; Naumann-Godo, M.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paciesas, W. S.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Petrosian, V.; Piron, F.; Porter, T. A.; Preece, R.; Racusin, J. L.; Rainò, S.; Rando, R.; Rau, A.; Razzano, M.; Razzaque, S.; Reimer, A.; Reimer, O.; Ripken, J.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sander, A.; Scargle, J. D.; Schalk, T. L.; Sgrò, C.; Siskind, E. J.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stamatikos, M.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uehara, T.; Usher, T. L.; Vandenbroucke, J.; van der Horst, A. J.; Vasileiou, V.; Vilchez, N.; Vitale, V.; von Kienlin, A.; Waite, A. P.; Wang, P.; Wilson-Hodge, C.; Winer, B. L.; Wood, K. S.; Wu, X. F.; Yamazaki, R.; Yang, Z.; Ylinen, T.; Ziegler, M.; Fermi LAT Collaboration; Fermi GBM Collaboration, The Fermi observatory is advancing our knowledge of gamma-ray bursts (GRBs) through pioneering observations at high energies, covering more than seven decades in energy with the two on-board detectors, the Large Area Telescope (LAT) and the Gamma-ray Burst Monitor (GBM). Here, we report on the observation of the long GRB 090217A which triggered the GBM and has been detected by the LAT with a significance greater than 9σ. We present the GBM and LAT observations and on-ground analyses, including the time-resolved spectra and the study of the temporal profile from 8 keV up to ~1 GeV. All spectra are well reproduced by a Band model. We compare these observations to the first two LAT-detected, long bursts GRB 080825C and GRB 080916C. These bursts were found to have time-dependent spectra and exhibited a delayed onset of the high-energy emission, which are not observed in the case of GRB 090217A. We discuss some theoretical implications for the high-energy emission of GRBs....
The Astrophysical Journal, Jul. 2010

The Spectral Energy Distribution of Fermi Bright Blazars
Abdo, A. A.; Ackermann, M.; Agudo, I.; Ajello, M.; Aller, H. D.; Aller, M. F.; Angelakis, E.; Arkharov, A. A.; Axelsson, M.; Bach, U.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Benitez, E.; Berdyugin, A.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Boettcher, M.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Burrows, D.; Buson, S.; Caliandro, G. A.; Calzoletti, L.; Cameron, R. A.; Capalbi, M.; Caraveo, P. A.; Carosati, D.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chaty, S.; Chekhtman, A.; Chen, W. P.; Chiang, J.; Chincarini, G.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Colafrancesco, S.; Cominsky, L. R.; Conrad, J.; Costamante, L.; Cutini, S.; D'ammando, F.; Deitrick, R.; D'Elia, V.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Donnarumma, I.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dultzin, D.; Dumora, D.; Falcone, A.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Forné, E.; Fortin, P.; Frailis, M.; Fuhrmann, L.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gómez, J. L.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giommi, P.; Giordano, F.; Giuliani, A.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Gronwall, C.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Gurwell, M. A.; Hadasch, D.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Healey, S. E.; Heidt, J.; Hiriart, D.; Horan, D.; Hoversten, E. A.; Hughes, R. E.; Itoh, R.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Jorstad, S. G.; Kadler, M.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kennea, J.; Kerr, M.; Kimeridze, G.; Knödlseder, J.; Kocian, M. L.; Kopatskaya, E. N.; Koptelova, E.; Konstantinova, T. S.; Kovalev, Y. Y.; Kovalev, Yu. A.; Kurtanidze, O. M.; Kuss, M.; Lande, J.; Larionov, V. M.; Latronico, L.; Leto, P.; Lindfors, E.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Marchegiani, P.; Marscher, A. P.; Marshall, F.; Max-Moerbeck, W.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nestoras, I.; Nilsson, K.; Nizhelsky, N. A.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Ojha, R.; Omodei, N.; Orlando, E.; Ormes, J. F.; Osborne, J.; Ozaki, M.; Pacciani, L.; Padovani, P.; Pagani, C.; Page, K.; Paneque, D.; Panetta, J. H.; Parent, D.; Pasanen, M.; Pavlidou, V.; Pelassa, V.; Pepe, M.; Perri, M.; Pesce-Rollins, M.; Piranomonte, S.; Piron, F.; Pittori, C.; Porter, T. A.; Puccetti, S.; Rahoui, F.; Rainò, S.; Raiteri, C.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Richards, J. L.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Ros, J. A.; Roth, M.; Roustazadeh, P.; Ryde, F.; Sadrozinski, H. F. -W.; Sadun, A.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Sellerholm, A.; Sgrò, C.; Shaw, M. S.; Sigua, L. A.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Stevenson, M.; Stratta, G.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Takalo, L. O.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Verrecchia, F.; Vilchez, N.; Villata, M.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Zensus, J. A.; Zhekanis, G. V.; Ziegler, M., We have conducted a detailed investigation of the broadband spectral properties of the γ-ray selected blazars of the Fermi LAT Bright AGN Sample (LBAS). By combining our accurately estimated Fermi γ-ray spectra with Swift, radio, infra-red, optical, and other hard X-ray/γ-ray data, collected within 3 months of the LBAS data taking period, we were able to assemble high-quality and quasi-simultaneous spectral energy distributions (SED) for 48 LBAS blazars. The SED of these γ-ray sources is similar to that of blazars discovered at other wavelengths, clearly showing, in the usual log ν-log ν F _ν representation, the typical broadband spectral signatures normally attributed to a combination of low-energy synchrotron radiation followed by inverse Compton emission of one or more components. We have used these SED to characterize the peak intensity of both the low- and the high-energy components. The results have been used to derive empirical relationships that estimate the position of the two peaks from the broadband colors (i.e., the radio to optical, α_ro, and optical to X-ray, α_ox, spectral slopes) and from the γ-ray spectral index. Our data show that the synchrotron peak frequency (ν ^S _peak) is positioned between 10^12.5 and 10^14.5 Hz in broad-lined flat spectrum radio quasars (FSRQs) and between 10¹³ and 10¹⁷ Hz in featureless BL Lacertae objects. We find that the γ-ray spectral slope is strongly correlated with the synchrotron peak energy and with the X-ray spectral index, as expected at first order in synchrotron-inverse Compton scenarios. However, simple homogeneous, one-zone, synchrotron self-Compton (SSC) models cannot explain most of our SED, especially in the case of FSRQs and low energy peaked (LBL) BL Lacs. More complex models involving external Compton radiation or multiple SSC components are required to reproduce the overall SED and the observed spectral variability. While more than 50% of known radio bright high energy peaked (HBL) BL Lacs are detected in the LBAS sample, only less than 13% of known bright FSRQs and LBL BL Lacs are included. This suggests that the latter sources, as a class, may be much fainter γ-ray emitters than LBAS blazars, and could in fact radiate close to the expectations of simple SSC models. We categorized all our sources according to a new physical classification scheme based on the generally accepted paradigm for Active Galactic Nuclei and on the results of this SED study. Since the LAT detector is more sensitive to flat spectrum γ-ray sources, the correlation between ν ^S _peak and γ-ray spectral index strongly favors the detection of high energy peaked blazars, thus explaining the Fermi overabundance of this type of sources compared to radio and EGRET samples. This selection effect is similar to that experienced in the soft X-ray band where HBL BL Lacs are the dominant type of blazars....
The Astrophysical Journal, Jun. 2010

Suzaku Observations of Luminous Quasars: Revealing the Nature of High-energy Blazar Emission in Low-level Activity States
Abdo, A. A.; Ackermann, M.; Ajello, M.; Antolini, E.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Carrigan, S.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Chen, A. W.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Colafrancesco, S.; Conrad, J.; Cutini, S.; Dermer, C. D.; de Palma, F.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Focke, W. B.; Frailis, M.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Giebels, B.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grandi, P.; Grenier, I. A.; Guillemot, L.; Guiriec, S.; Hadasch, D.; Harding, A. K.; Hayashida, M.; Horan, D.; Hughes, R. E.; Itoh, R.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Mazziotta, M. N.; McEnery, J. E.; McGlynn, S.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nestoras, I.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reyes, L. C.; Rodriguez, A. Y.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sambruna, R.; Sander, A.; Sato, R.; Sgrò, C.; Shaw, M. S.; Siskind, E. J.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stawarz, Ł.; Stecker, F. W.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibolla, O.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Vilchez, N.; Villata, M.; Vitale, V.; von Kienlin, A.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ylinen, T.; Ziegler, M.; Tavecchio, F.; Sikora, M.; Schady, P.; Roming, P.; Chester, M. M.; Maraschi, L., We present the results from the Suzaku X-ray observations of five flat-spectrum radio quasars (FSRQs), namely PKS 0208-512, Q 0827+243, PKS 1127-145, PKS 1510-089, and 3C 454.3. All these sources were additionally monitored simultaneously or quasi-simultaneously by the Fermi satellite in gamma rays and the Swift UVOT in the UV and optical bands, respectively. We constructed their broadband spectra covering the frequency range from 10¹⁴ Hz up to 10²⁵ Hz, and those reveal the nature of high-energy emission of luminous blazars in their low-activity states. The analyzed X-ray spectra are well fitted by a power-law model with photoelectric absorption. In the case of PKS 0208-512, PKS 1127-145, and 3C 454.3, the X-ray continuum showed indication of hardening at low energies. Moreover, when compared with the previous X-ray observations, we see a significantly increasing contribution of low-energy photons to the total X-ray fluxes when the sources are getting fainter. The same behavior can be noted in the Suzaku data alone. A likely explanation involves a variable, flat-spectrum component produced via inverse-Compton emission, plus an additional, possibly steady soft X-ray component prominent when the source gets fainter. This soft X-ray excess is represented either by a steep power-law (photon indices Γ ~ 3-5) or a blackbody-type emission with temperatures kT ~ 0.1-0.2 keV. We model the broadband spectra of the five observed FSRQs using synchrotron self-Compton and/or external-Compton radiation models. Our modeling suggests that the difference between the low- and high-activity states in luminous blazars is due to the different total kinetic power of the jet, most likely related to varying bulk Lorentz factor of the outflow within the blazar emission zone....
The Astrophysical Journal, Jun. 2010

Fermi Observations of GRB 090510: A Short-Hard Gamma-ray Burst with an Additional, Hard Power-law Component from 10 keV TO GeV Energies
Ackermann, M.; Asano, K.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bhat, P. N.; Bissaldi, E.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Briggs, M. S.; Brigida, M.; Bruel, P.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Connaughton, V.; Conrad, J.; Dermer, C. D.; de Palma, F.; Dingus, B. L.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Finke, J.; Focke, W. B.; Frailis, M.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Granot, J.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guiriec, S.; Hadasch, D.; Harding, A. K.; Hays, E.; Horan, D.; Hughes, R. E.; Jóhannesson, G.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kippen, R. M.; Knödlseder, J.; Kocevski, D.; Kouveliotou, C.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Llena Garde, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Mazziotta, M. N.; McEnery, J. E.; McGlynn, S.; Meegan, C.; Mészáros, P.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakajima, H.; Nakamori, T.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paciesas, W. S.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Preece, R.; Rainò, S.; Rando, R.; Razzano, M.; Razzaque, S.; Reimer, A.; Ritz, S.; Rodriguez, A. Y.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sander, A.; Scargle, J. D.; Schalk, T. L.; Sgrò, C.; Siskind, E. J.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stamatikos, M.; Stecker, F. W.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Toma, K.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Uehara, T.; Usher, T. L.; van der Horst, A. J.; Vasileiou, V.; Vilchez, N.; Vitale, V.; von Kienlin, A.; Waite, A. P.; Wang, P.; Wilson-Hodge, C.; Winer, B. L.; Wu, X. F.; Yamazaki, R.; Yang, Z.; Ylinen, T.; Ziegler, M., We present detailed observations of the bright short-hard gamma-ray burst GRB 090510 made with the Gamma-ray Burst Monitor (GBM) and Large Area Telescope (LAT) on board the Fermi observatory. GRB 090510 is the first burst detected by the LAT that shows strong evidence for a deviation from a Band spectral fitting function during the prompt emission phase. The time-integrated spectrum is fit by the sum of a Band function with E _peak = 3.9 ± 0.3 MeV, which is the highest yet measured, and a hard power-law component with photon index -1.62 ± 0.03 that dominates the emission below ≈20 keV and above ≈100 MeV. The onset of the high-energy spectral component appears to be delayed by ~0.1 s with respect to the onset of a component well fit with a single Band function. A faint GBM pulse and a LAT photon are detected 0.5 s before the main pulse. During the prompt phase, the LAT detected a photon with energy 30.5^+5.8 _-2.6 GeV, the highest ever measured from a short GRB. Observation of this photon sets a minimum bulk outflow Lorentz factor, Γgsim 1200, using simple γγ opacity arguments for this GRB at redshift z = 0.903 and a variability timescale on the order of tens of ms for the ≈100 keV-few MeV flux. Stricter high confidence estimates imply Γ >~ 1000 and still require that the outflows powering short GRBs are at least as highly relativistic as those of long-duration GRBs. Implications of the temporal behavior and power-law shape of the additional component on synchrotron/synchrotron self-Compton, external-shock synchrotron, and hadronic models are considered....
The Astrophysical Journal, Jun. 2010

Fermi Large Area Telescope First Source Catalog
Abdo, A. A.; Ackermann, M.; Ajello, M.; Allafort, A.; Antolini, E.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Belli, F.; Berenji, B.; Bisello, D.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Bonnell, J.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Busetto, G.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Campana, R.; Canadas, B.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cavazzuti, E.; Ceccanti, M.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Cillis, A. N.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Corbet, R.; Davis, D. S.; DeKlotz, M.; den Hartog, P. R.; Dermer, C. D.; de Angelis, A.; de Luca, A.; de Palma, F.; Digel, S. W.; Dormody, M.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Fabiani, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giavitto, G.; Giebels, B.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Gustafsson, M.; Hadasch, D.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Healey, S. E.; Hill, A. B.; Horan, D.; Hughes, R. E.; Iafrate, G.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocevski, D.; Kuss, M.; Lande, J.; Landriu, D.; Latronico, L.; Lee, S. -H.; Lemoine-Goumard, M.; Lionetto, A. M.; Llena Garde, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Marangelli, B.; Marelli, M.; Massaro, E.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Michelson, P. F.; Minuti, M.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Mongelli, M.; Monte, C.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakajima, H.; Nakamori, T.; Naumann-Godo, M.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paccagnella, A.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Pinchera, M.; Piron, F.; Porter, T. A.; Poupard, L.; Rainò, S.; Rando, R.; Ray, P. S.; Razzano, M.; Razzaque, S.; Rea, N.; Reimer, A.; Reimer, O.; Reposeur, T.; Ripken, J.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Sadrozinski, H. F. -W.; Salvetti, D.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Schalk, T. L.; Scolieri, G.; Sgrò, C.; Shaw, M. S.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Stephens, T. E.; Striani, E.; Strickman, M. S.; Strong, A. W.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Tibolla, O.; Tinebra, F.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Van Etten, A.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wallace, E.; Wang, P.; Watters, K.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ylinen, T.; Ziegler, M.; Fermi LAT Collaboration, We present a catalog of high-energy gamma-ray sources detected by the Large Area Telescope (LAT), the primary science instrument on the Fermi Gamma-ray Space Telescope (Fermi), during the first 11 months of the science phase of the mission, which began on 2008 August 4. The First Fermi-LAT catalog (1FGL) contains 1451 sources detected and characterized in the 100 MeV to 100 GeV range. Source detection was based on the average flux over the 11 month period, and the threshold likelihood Test Statistic is 25, corresponding to a significance of just over 4σ. The 1FGL catalog includes source location regions, defined in terms of elliptical fits to the 95% confidence regions and power-law spectral fits as well as flux measurements in five energy bands for each source. In addition, monthly light curves are provided. Using a protocol defined before launch we have tested for several populations of gamma-ray sources among the sources in the catalog. For individual LAT-detected sources we provide firm identifications or plausible associations with sources in other astronomical catalogs. Identifications are based on correlated variability with counterparts at other wavelengths, or on spin or orbital periodicity. For the catalogs and association criteria that we have selected, 630 of the sources are unassociated. Care was taken to characterize the sensitivity of the results to the model of interstellar diffuse gamma-ray emission used to model the bright foreground, with the result that 161 sources at low Galactic latitudes and toward bright local interstellar clouds are flagged as having properties that are strongly dependent on the model or as potentially being due to incorrectly modeled structure in the Galactic diffuse emission....
The Astrophysical Journal Supplement Series, Jun. 2010

Multiband Photopolarimetric Monitoring of an Outburst of the Blazar 3C 454.3 in 2007
Mahito Sasada; Makoto Uemura; Akira Arai; Yasushi Fukazawa; Koji S. Kawabata; Takashi Ohsugi; Takuya Yamashita; Mizuki Isogai; Osamu Nagae; Takeshi Uehara; Tsunefumi Mizuno; Hideaki Katagiri; Hiromitsu Takahashi; Shuji Sato; Masaru Kino, We report on optical-near-infrared photopolarimetric observations of a blazar 3C 454.3 over 200 d. The object experienced an optical outburst in 2007 July. This outburst was followed by a short state fainter than V = 15.2 mag. lasting similar to 25 d. The object then entered an active state during which we observed short flares having a timescale of 3-10 d. The object showed two types of features in the color-magnitude relationship. One was a "bluer-when-brighter" trend in the outburst state, and the other was a "redder-when-brighter" trend in the faint state. These two types of features suggest a contribution of thermal emission to the observed flux, as suspected in previous studies. Our polarimetric observation detected two episodes of rotation of the polarization vector. The first one was a counterclockwise rotation in the Q U plane during the outburst state. After this rotation event of the polarization vector, the object entered a rapidly fading stage. The second one was seen in a series of flares during the active state. Each flare had a specific position angle of polarization, which apparently rotated clockwise from the first to the last flares. Thus, the object exhibited rotations of the polarization vector in opposite directions. We estimated a decay timescale of the short flares during the active state, and then calculated an upper limit of the strength of the magnetic B = 0.2G. assuming a typical beaming factor of blazars, delta = 20. This upper limit of B is smaller than those previously estimated from spectral analysis., OXFORD UNIV PRESS
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Jun. 2010, [Reviewed]

Detection of the Energetic Pulsar PSR B1509-58 and its Pulsar Wind Nebula in MSH 15-52 Using the Fermi-Large Area Telescope
Abdo, A. A.; Ackermann, M.; Ajello, M.; Allafort, A.; Asano, K.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Camilo, F.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; den Hartog, P. R.; Dermer, C. D.; de Luca, A.; de Palma, F.; Dormody, M.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Focke, W. B.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gehrels, N.; Germani, S.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Gotthelf, E. V.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hays, E.; Hobbs, G.; Horan, D.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, T. J.; Johnson, W. N.; Johnston, S.; Kamae, T.; Kanai, Y.; Kanbach, G.; Katagiri, H.; Kataoka, J.; Kawai, N.; Keith, M.; Kerr, M.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Llena Garde, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Manchester, R. N.; Marelli, M.; Mazziotta, M. N.; McEnery, J. E.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Rea, N.; Reimer, A.; Reimer, O.; Reposeur, T.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sander, A.; Saz Parkinson, P. M.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Thorsett, S. E.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Venter, C.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Weltevrede, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ylinen, T.; Ziegler, M.; Fermi LAT Collaboration; Pulsar Timing Consortium, We report the detection of high-energy γ-ray emission from the young and energetic pulsar PSR B1509 - 58 and its pulsar wind nebula (PWN) in the composite supernova remnant G320.4 - 1.2 (aka MSH 15 - 52). Using 1 yr of survey data with the Fermi-Large Area Telescope (LAT), we detected pulsations from PSR B1509 - 58 up to 1 GeV and extended γ-ray emission above 1 GeV spatially coincident with the PWN. The pulsar light curve presents two peaks offset from the radio peak by phases 0.96 ± 0.01 and 0.33 ± 0.02. New constraining upper limits on the pulsar emission are derived below 1 GeV and confirm a severe spectral break at a few tens of MeV. The nebular spectrum in the 1-100 GeV energy range is well described by a power law with a spectral index of (1.57 ± 0.17 ± 0.13) and a flux above 1 GeV of (2.91 ± 0.79 ± 1.35) × 10^-9 cm^-2 s^-1. The first errors represent the statistical errors on the fit parameters, while the second ones are the systematic uncertainties. The LAT spectrum of the nebula connects nicely with Cherenkov observations, and indicates a spectral break between GeV and TeV energies....
The Astrophysical Journal, May 2010

Fermi-Large Area Telescope Observations of the Exceptional Gamma-ray Outbursts of 3C 273 in 2009 September
Abdo, A. A.; Ackermann, M.; Ajello, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Cannon, A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Costamante, L.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giommi, P.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Guiriec, S.; Hayashida, M.; Hays, E.; Hill, A. B.; Horan, D.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Knödlseder, J.; Kuss, M.; Lande, J.; Larsson, S.; Latronico, L.; Lemoine-Goumard, M.; Llena Garde, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Mansutti, O.; Massaro, E.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J. H.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Ritz, S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sander, A.; Scargle, J. D.; Schalk, T. L.; Sgrò, C.; Siskind, E. J.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Wehrle, A. E.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ylinen, T.; Ziegler, M., We present the light curves and spectral data of two exceptionally luminous gamma-ray outbursts observed by the Large Area Telescope experiment on board the Fermi Gamma-ray Space Telescope from 3C 273 in 2009 September. During these flares, having a duration of a few days, the source reached its highest γ-ray flux ever measured. This allowed us to study, in some details, their spectral and temporal structures. The rise and the decay are asymmetric on timescales of 6 hr, and the spectral index was significantly harder during the flares than during the preceding 11 months. We also found that short, very intense flares put out the same time-integrated energy as long, less intense flares like that observed in 2009 August....
The Astrophysical Journal, May 2010

The First Catalog of Active Galactic Nuclei Detected by the Fermi Large Area Telescope
Abdo, A. A.; Ackermann, M.; Ajello, M.; Allafort, A.; Antolini, E.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bogart, J. R.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Buehler, R.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Cannon, A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Celotti, A.; Charles, E.; Chekhtman, A.; Chen, A. W.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Costamante, L.; Cotter, G.; Cutini, S.; D'Elia, V.; Dermer, C. D.; de Angelis, A.; de Palma, F.; De Rosa, A.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Escande, L.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grandi, P.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guiriec, S.; Hadasch, D.; Harding, A. K.; Hayashida, M.; Hays, E.; Healey, S. E.; Hill, A. B.; Horan, D.; Hughes, R. E.; Iafrate, G.; Itoh, R.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lavalley, C.; Lemoine-Goumard, M.; Llena Garde, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Malaguti, G.; Massaro, E.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; McGlynn, S.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piranomonte, S.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ripken, J.; Ritz, S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Sgrò, C.; Shaw, M. S.; Siskind, E. J.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Stawarz, Ł.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Taylor, G. B.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Ubertini, P.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Vilchez, N.; Villata, M.; Vitale, V.; Waite, A. P.; Wallace, E.; Wang, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ylinen, T.; Ziegler, M., We present the first catalog of active galactic nuclei (AGNs) detected by the Large Area Telescope (LAT), corresponding to 11 months of data collected in scientific operation mode. The First LAT AGN Catalog (1LAC) includes 671 γ-ray sources located at high Galactic latitudes (|b|>10°) that are detected with a test statistic greater than 25 and associated statistically with AGNs. Some LAT sources are associated with multiple AGNs, and consequently, the catalog includes 709 AGNs, comprising 300 BL Lacertae objects, 296 flat-spectrum radio quasars, 41 AGNs of other types, and 72 AGNs of unknown type. We also classify the blazars based on their spectral energy distributions as archival radio, optical, and X-ray data permit. In addition to the formal 1LAC sample, we provide AGN associations for 51 low-latitude LAT sources and AGN "affiliations" (unquantified counterpart candidates) for 104 high-latitude LAT sources without AGN associations. The overlap of the 1LAC with existing γ-ray AGN catalogs (LBAS, EGRET, AGILE, Swift, INTEGRAL, TeVCat) is briefly discussed. Various properties—such as γ-ray fluxes and photon power-law spectral indices, redshifts, γ-ray luminosities, variability, and archival radio luminosities—and their correlations are presented and discussed for the different blazar classes. We compare the 1LAC results with predictions regarding the γ-ray AGN populations, and we comment on the power of the sample to address the question of the blazar sequence....
The Astrophysical Journal, May 2010

The Discovery of γ-Ray Emission from the Blazar RGB J0710+591
Acciari, V. A.; Aliu, E.; Arlen, T.; Aune, T.; Bautista, M.; Beilicke, M.; Benbow, W.; Böttcher, M.; Boltuch, D.; Bradbury, S. M.; Buckley, J. H.; Bugaev, V.; Byrum, K.; Cannon, A.; Cesarini, A.; Ciupik, L.; Cui, W.; Dickherber, R.; Duke, C.; Falcone, A.; Finley, J. P.; Finnegan, G.; Fortson, L.; Furniss, A.; Galante, N.; Gall, D.; Gibbs, K.; Gillanders, G. H.; Godambe, S.; Grube, J.; Guenette, R.; Gyuk, G.; Hanna, D.; Holder, J.; Hui, C. M.; Humensky, T. B.; Imran, A.; Kaaret, P.; Karlsson, N.; Kertzman, M.; Kieda, D.; Konopelko, A.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; Lamerato, A.; LeBohec, S.; Maier, G.; McArthur, S.; McCann, A.; McCutcheon, M.; Moriarty, P.; Mukherjee, R.; Ong, R. A.; Otte, A. N.; Pandel, D.; Perkins, J. S.; Petry, D.; Pichel, A.; Pohl, M.; Quinn, J.; Ragan, K.; Reyes, L. C.; Reynolds, P. T.; Roache, E.; Rose, H. J.; Roustazadeh, P.; Schroedter, M.; Sembroski, G. H.; Senturk, G. Demet; Smith, A. W.; Steele, D.; Swordy, S. P.; Tešić, G.; Theiling, M.; Thibadeau, S.; Varlotta, A.; Vassiliev, V. V.; Vincent, S.; Wagner, R. G.; Wakely, S. P.; Ward, J. E.; Weekes, T. C.; Weinstein, A.; Weisgarber, T.; Williams, D. A.; Wissel, S.; Wood, M.; Zitzer, B.; Ackermann, M.; Ajello, M.; Antolini, E.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Dermer, C. D.; de Palma, F.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grove, J. E.; Guiriec, S.; Hays, E.; Horan, D.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Llena Garde, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Mazziotta, M. N.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J. H.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Ripken, J.; Rodriguez, A. Y.; Roth, M.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Scargle, J. D.; Sgrò, C.; Siskind, E. J.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Usher, T. L.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ylinen, T.; Ziegler, M., The high-frequency-peaked BL Lacertae object RGB J0710+591 was observed in the very high-energy (VHE; E > 100 GeV) wave band by the VERITAS array of atmospheric Cherenkov telescopes. The observations, taken between 2008 December and 2009 March and totaling 22.1 hr, yield the discovery of VHE gamma rays from the source. RGB J0710+591 is detected at a statistical significance of 5.5 standard deviations (5.5σ) above the background, corresponding to an integral flux of (3.9 ± 0.8) × 10^-12 cm^-2 s^-1 (3% of the Crab Nebula's flux) above 300 GeV. The observed spectrum can be fit by a power law from 0.31 to 4.6 TeV with a photon spectral index of 2.69 ± 0.26_stat ± 0.20_sys. These data are complemented by contemporaneous multiwavelength data from the Fermi Large Area Telescope, the Swift X-ray Telescope, the Swift Ultra-Violet and Optical Telescope, and the Michigan-Dartmouth-MIT observatory. Modeling the broadband spectral energy distribution (SED) with an equilibrium synchrotron self-Compton model yields a good statistical fit to the data. The addition of an external-Compton component to the model does not improve the fit nor brings the system closer to equipartition. The combined Fermi and VERITAS data constrain the properties of the high-energy emission component of the source over 4 orders of magnitude and give measurements of the rising and falling sections of the SED....
The Astrophysical Journal, May 2010

Constraints on dark matter annihilation in clusters of galaxies with the Fermi large area telescope
Ackermann, M.; Ajello, M.; Allafort, A.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Brandt, T. J.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cecchi, C.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cominsky, L. R.; Conrad, J.; de Angelis, A.; de Palma, F.; Silva, E. do Couto e.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Dumora, D.; Edmonds, Y.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Frailis, M.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Guiriec, S.; Gustafsson, M.; Harding, A. K.; Hayashida, M.; Horan, D.; Hughes, R. E.; Jeltema, T. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Llena Garde, M.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Mazziotta, M. N.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Panetta, J. H.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Profumo, S.; Rainò, S.; Razzano, M.; Reposeur, T.; Ritz, S.; Rodriguez, A. Y.; Roth, M.; Sadrozinski, H. F. -W.; Sander, A.; Scargle, J. D.; Sgrò, C.; Siskind, E. J.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Usher, T. L.; Vasileiou, V.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ylinen, T.; Ziegler, M.; Fermi LAT Collaboration, Nearby clusters and groups of galaxies are potentially bright sources of high-energy gamma-ray emission resulting from the pair-annihilation of dark matter particles. However, no significant gamma-ray emission has been detected so far from clusters in the first 11 months of observations with the Fermi Large Area Telescope. We interpret this non-detection in terms of constraints on dark matter particle properties. In particular for leptonic annihilation final states and particle masses greater than ~ 200 GeV, gamma-ray emission from inverse Compton scattering of CMB photons is expected to dominate the dark matter annihilation signal from clusters, and our gamma-ray limits exclude large regions of the parameter space that would give a good fit to the recent anomalous Pamela and Fermi-LAT electron-positron measurements. We also present constraints on the annihilation of more standard dark matter candidates, such as the lightest neutralino of supersymmetric models. The constraints are particularly strong when including the fact that clusters are known to contain substructure at least on galaxy scales, increasing the expected gamma-ray flux by a factor of ~ 5 over a smooth-halo assumption. We also explore the effect of uncertainties in cluster dark matter density profiles, finding a systematic uncertainty in the constraints of roughly a factor of two, but similar overall conclusions. In this work, we focus on deriving limits on dark matter models; a more general consideration of the Fermi-LAT data on clusters and clusters as gamma-ray sources is forthcoming....
Journal of Cosmology and Astro-Particle Physics, May 2010

Fermi Gamma-Ray Imaging of a Radio Galaxy
Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Colafrancesco, S.; Cominsky, L. R.; Conrad, J.; Costamante, L.; Cutini, S.; Davis, D. S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Finke, J.; Focke, W. B.; Fortin, P.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Georganopoulos, M.; Germani, S.; Giebels, B.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Hughes, R. E.; Jackson, M. S.; Jóhannesson G.; Johnson, S.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocian, M. L.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Razzaque, S.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sambruna, R.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Sgrò, C.; Siskind, J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Stawarz, L.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y. Usher, T. L.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wallace, E.; Wang, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M.; Hardcastle, M. J.; Kazanas, D.; Fermi LAT Collaboration, The Fermi Gamma-ray Space Telescope has detected the γ-ray glow emanating from the giant radio lobes of the radio galaxy Centaurus A. The resolved γ-ray image shows the lobes clearly separated from the central active source. In contrast to all other active galaxies detected so far in high-energy γ-rays, the lobe flux constitutes a considerable portion (greater than one-half) of the total source emission. The γ-ray emission from the lobes is interpreted as inverse Compton-scattered relic radiation from the cosmic microwave background, with additional contribution at higher energies from the infrared-to-optical extragalactic background light. These measurements provide γ-ray constraints on the magnetic field and particle energy content in radio galaxy lobes, as well as a promising method to probe the cosmic relic photon fields....
Science, May 2010

Discovery of Pulsed γ-Rays from PSR J0034-0534 with the Fermi Large Area Telescope: A Case for Co-Located Radio and γ-Ray Emission Regions
Abdo, A. A.; Ackermann, M.; Ajello, M.; Allafort, A.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Camilo, F.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cognard, I.; Cohen-Tanugi, J.; Conrad, J.; Corbet, R.; DeCesar, M. E.; Dermer, C. D.; Desvignes, G.; de Angelis, A.; de Palma, F.; Digel, S. W.; Dormody, M.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Espinoza, C.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Frailis, M.; Freire, P. C. C.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giavitto, G.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hadasch, D.; Harding, A. K.; Hays, E.; Hobbs, G.; Horan, D.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, T. J.; Johnson, W. N.; Johnston, S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kramer, M.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Llena Garde, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Lyne, A. G.; Makeev, A.; Manchester, R. N.; Marelli, M.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; McGlynn, S.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Noutsos, A.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Ransom, S. M.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ripken, J.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stappers, B. W.; Starck, J. -L.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Theureau, G.; Thompson, D. J.; Thorsett, S. E.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Usher, T. L.; Van Etten, A.; Vasileiou, V.; Venter, C.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wallace, E.; Wang, P.; Weltevrede, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M., Millisecond pulsars (MSPs) have been firmly established as a class of γ-ray emitters via the detection of pulsations above 0.1 GeV from eight MSPs by the Fermi Large Area Telescope (LAT). Using 13 months of LAT data, significant γ-ray pulsations at the radio period have been detected from the MSP PSR J0034-0534, making it the ninth clear MSP detection by the LAT. The γ-ray light curve shows two peaks separated by 0.274 ± 0.015 in phase which are very nearly aligned with the radio peaks, a phenomenon seen only in the Crab pulsar until now. The >=0.1 GeV spectrum of this pulsar is well fit by an exponentially cutoff power law with a cutoff energy of 1.8 ± 0.6 ± 0.1 GeV and a photon index of 1.5 ± 0.2 ± 0.1, first errors are statistical and second are systematic. The near-alignment of the radio and γ-ray peaks strongly suggests that the radio and γ-ray emission regions are co-located and both are the result of caustic formation....
The Astrophysical Journal, Apr. 2010

Fermi Large Area Telescope Observations of PSR J1836+5925
Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Bechtol, K.; Belfiore, A.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Camilo, F.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; de Angelis, A.; de Luca, A.; de Palma, F.; Digel, S. W.; Dormody, M.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Edmonds, Y.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giavitto, G.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Gwon, C.; Hadasch, D.; Harding, A. K.; Hays, E.; Horan, D.; Hughes, R. E.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Kanai, Y.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Marelli, M.; Mazziotta, M. N.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Ransom, S. M.; Ray, P. S.; Razzano, M.; Rea, N.; Reimer, A.; Reimer, O.; Reposeur, T.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Thorsett, S. E.; Tibaldo, L.; Tibolla, O.; Torres, D. F.; Tosti, G.; Tramacere, A.; Usher, T. L.; Van Etten, A.; Vasileiou, V.; Venter, C.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Watters, K.; Winer, B. L.; Wolff, M. T.; Wood, K. S.; Ylinen, T.; Ziegler, M., The discovery of the γ-ray pulsar PSR J1836+5925, powering the formerly unidentified EGRET source 3EG J1835+5918, was one of the early accomplishments of the Fermi Large Area Telescope (LAT). Sitting 25° off the Galactic plane, PSR J1836+5925 is a 173 ms pulsar with a characteristic age of 1.8 million years, a spindown luminosity of 1.1 × 10³⁴ erg s^-1, and a large off-peak (OP) emission component, making it quite unusual among the known γ-ray pulsar population. We present an analysis of one year of LAT data, including an updated timing solution, detailed spectral results, and a long-term light curve showing no indication of variability. No evidence for a surrounding pulsar wind nebula is seen and the spectral characteristics of the OP emission indicate it is likely magnetospheric. Analysis of recent XMM-Newton observations of the X-ray counterpart yields a detailed characterization of its spectrum, which, like Geminga, is consistent with that of a neutron star showing evidence for both magnetospheric and thermal emission....
The Astrophysical Journal, Apr. 2010

Fermi Large Area Telescope Observations of the Vela-X Pulsar Wind Nebula
Abdo, A. A.; Ackermann, M.; Ajello, M.; Allafort, A.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Chung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; de Angelis, A.; de Palma, F.; Dormody, M.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gehrels, N.; Germani, S.; Giavitto, G.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Harding, A. K.; Hayashida, M.; Hays, E.; Horan, D.; Hughes, R. E.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, T. J.; Johnson, W. N.; Johnston, S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Lemoine-Goumard, M.; Llena Garde, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Marelli, M.; Mazziotta, M. N.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Nolan, P. L.; Norris, J. P.; Noutsos, A.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Ray, P. S.; Rea, N.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Van Etten, A.; Vasileiou, V.; Venter, C.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Weltevrede, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M., We report on gamma-ray observations in the off-pulse window of the Vela pulsar PSR B0833-45 using 11 months of survey data from the Fermi Large Area Telescope (LAT). This pulsar is located in the 8° diameter Vela supernova remnant, which contains several regions of non-thermal emission detected in the radio, X-ray, and gamma-ray bands. The gamma-ray emission detected by the LAT lies within one of these regions, the 2° × 3° area south of the pulsar known as Vela-X. The LAT flux is significantly spatially extended with a best-fit radius of 0fdg88 ± 0fdg12 for an assumed radially symmetric uniform disk. The 200 MeV to 20 GeV LAT spectrum of this source is well described by a power law with a spectral index of 2.41 ± 0.09 ± 0.15 and integral flux above 100 MeV of (4.73 ± 0.63 ± 1.32) × 10^-7 cm^-2 s^-1. The first errors represent the statistical error on the fit parameters, while the second ones are the systematic uncertainties. Detailed morphological and spectral analyses give strong constraints on the energetics and magnetic field of the pulsar wind nebula system and favor a scenario with two distinct electron populations....
The Astrophysical Journal, Apr. 2010

The Vela Pulsar: Results from the First Year of Fermi LAT Observations
Abdo, A. A.; Ackermann, M.; Ajello, M.; Allafort, A.; Atwood, W. B.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Dermer, C. D.; de Luca, A.; de Palma, F.; Dormody, M.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giavitto, G.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hadasch, D.; Harding, A. K.; Hays, E.; Hobbs, G.; Horan, D.; Hughes, R. E.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Lemoine-Goumard, M.; Llena Garde, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Manchester, R. N.; Marelli, M.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; McGlynn, S.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Nolan, P. L.; Norris, J. P.; Noutsos, A.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Ray, P. S.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sander, A.; Saz Parkinson, P. M.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Usher, T. L.; Van Etten, A.; Vasileiou, V.; Venter, C.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Watters, K.; Weltevrede, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M., We report on analysis of timing and spectroscopy of the Vela pulsar using 11 months of observations with the Large Area Telescope (LAT) on the Fermi Gamma-ray Space Telescope. The intrinsic brightness of Vela at GeV energies combined with the angular resolution and sensitivity of the LAT allows us to make the most detailed study to date of the energy-dependent light curves and phase-resolved spectra, using a LAT-derived timing model. The light curve consists of two peaks (P1 and P2) connected by bridge emission containing a third peak (P3). We have confirmed the strong decrease of the P1/P2 ratio with increasing energy seen with EGRET and previous Fermi LAT data, and observe that P1 disappears above 20 GeV. The increase with energy of the mean phase of the P3 component can be followed with much greater detail, showing that P3 and P2 are present up to the highest energies of pulsation. We find significant pulsed emission at phases outside the main profile, indicating that magnetospheric emission exists over 80% of the pulsar period. With increased high-energy counts the phase-averaged spectrum is seen to depart from a power law with simple exponential cutoff, and is better fit with a more gradual cutoff. The spectra in fixed-count phase bins are well fit with power laws with exponential cutoffs, revealing a strong and complex phase dependence of the cutoff energy, especially in the peaks. By combining these results with predictions of the outer magnetosphere models that map emission characteristics to phase, it will be possible to probe the particle acceleration and the structure of the pulsar magnetosphere with unprecedented detail....
The Astrophysical Journal, Apr. 2010

The First Fermi Large Area Telescope Catalog of Gamma-ray Pulsars
Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Camilo, F.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cognard, I.; Cohen-Tanugi, J.; Cominsky, L. R.; Conrad, J.; Corbet, R.; Cutini, S.; den Hartog, P. R.; Dermer, C. D.; de Angelis, A.; de Luca, A.; de Palma, F.; Digel, S. W.; Dormody, M.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Espinoza, C.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Focke, W. B.; Fortin, P.; Frailis, M.; Freire, P. C. C.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giavitto, G.; Giebels, B.; Giglietto, N.; Giommi, P.; Giordano, F.; Glanzman, T.; Godfrey, G.; Gotthelf, E. V.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Gwon, C.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Hughes, R. E.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Johnston, S.; Kamae, T.; Kanbach, G.; Kaspi, V. M.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocian, M. L.; Kramer, M.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Livingstone, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Lyne, A. G.; Madejski, G. M.; Makeev, A.; Manchester, R. N.; Marelli, M.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; McGlynn, S.; Meurer, C.; Michelson, P. F.; Mineo, T.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Nolan, P. L.; Norris, J. P.; Noutsos, A.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Ransom, S. M.; Ray, P. S.; Razzano, M.; Rea, N.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Schalk, T. L.; Sellerholm, A.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stappers, B. W.; Starck, J. -L.; Striani, E.; Strickman, M. S.; Strong, A. W.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Theureau, G.; Thompson, D. J.; Thorsett, S. E.; Tibaldo, L.; Tibolla, O.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Van Etten, A.; Vasileiou, V.; Venter, C.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Wang, N.; Watters, K.; Weltevrede, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M., The dramatic increase in the number of known gamma-ray pulsars since the launch of the Fermi Gamma-ray Space Telescope (formerly GLAST) offers the first opportunity to study a sizable population of these high-energy objects. This catalog summarizes 46 high-confidence pulsed detections using the first six months of data taken by the Large Area Telescope (LAT), Fermi's main instrument. Sixteen previously unknown pulsars were discovered by searching for pulsed signals at the positions of bright gamma-ray sources seen with the LAT, or at the positions of objects suspected to be neutron stars based on observations at other wavelengths. The dimmest observed flux among these gamma-ray-selected pulsars is 6.0 × 10^-8 ph cm^-2 s^-1 (for E>100 MeV). Pulsed gamma-ray emission was discovered from 24 known pulsars by using ephemerides (timing solutions) derived from monitoring radio pulsars. Eight of these new gamma-ray pulsars are millisecond pulsars. The dimmest observed flux among the radio-selected pulsars is 1.4 × 10^-8 ph cm^-2 s^-1 (for E>100 MeV). The remaining six gamma-ray pulsars were known since the Compton Gamma Ray Observatory mission, or before. The limiting flux for pulse detection is non-uniform over the sky owing to different background levels, especially near the Galactic plane. The pulsed energy spectra can be described by a power law with an exponential cutoff, with cutoff energies in the range ~1-5 GeV. The rotational energy-loss rate (Ė) of these neutron stars spans five decades, from ~3 × 10³³ erg s^-1 to 5 × 10³⁸ erg s^-1, and the apparent efficiencies for conversion to gamma-ray emission range from ~0.1% to ~ unity, although distance uncertainties complicate efficiency estimates. The pulse shapes show substantial diversity, but roughly 75% of the gamma-ray pulse profiles have two peaks, separated by gsim0.2 of rotational phase. For most of the pulsars, gamma-ray emission appears to come mainly from the outer magnetosphere, while polar-cap emission remains plausible for a remaining few. Spatial associations imply that many of these pulsars power pulsar wind nebulae. Finally, these discoveries suggest that gamma-ray-selected young pulsars are born at a rate comparable to that of their radio-selected cousins and that the birthrate of all young gamma-ray-detected pulsars is a substantial fraction of the expected Galactic supernova rate....
The Astrophysical Journal Supplement Series, Apr. 2010

Constraints on cosmological dark matter annihilation from the Fermi-LAT isotropic diffuse gamma-ray measurement
Abdo, A. A.; Ackermann, M.; Ajello, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Cutini, S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Edmonds, Y.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Gustafsson, M.; Hadasch, D.; Harding, A. K.; Horan, D.; Hughes, R. E.; Johnson, A. S.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Llena Garde, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Mazziotta, M. N.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Rainò, S.; Rando, R.; Reimer, A.; Reimer, O.; Reposeur, T.; Rodriguez, A. Y.; Roth, M.; Sadrozinski, H. F. -W.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Sellerholm, A.; Sgrò, C.; Siskind, E. J.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Torres, D. F.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Zaharijas, G.; Ziegler, M., The first published Fermi large area telescope (Fermi-LAT) measurement of the isotropic diffuse gamma-ray emission is in good agreement with a single power law, and is not showing any signature of a dominant contribution from dark matter sources in the energy range from 20 to 100 GeV. We use the absolute size and spectral shape of this measured flux to derive cross section limits on three types of generic dark matter candidates: annihilating into quarks, charged leptons and monochromatic photons. Predicted gamma-ray fluxes from annihilating dark matter are strongly affected by the underlying distribution of dark matter, and by using different available results of matter structure formation we assess these uncertainties. We also quantify how the dark matter constraints depend on the assumed conventional backgrounds and on the Universe's transparency to high-energy gamma-rays. In reasonable background and dark matter structure scenarios (but not in all scenarios we consider) it is possible to exclude models proposed to explain the excess of electrons and positrons measured by the Fermi-LAT and PAMELA experiments. Derived limits also start to probe cross sections expected from thermally produced relics (e.g. in minimal supersymmetry models) annihilating predominantly into quarks. For the monochromatic gamma-ray signature, the current measurement constrains only dark matter scenarios with very strong signals....
Journal of Cosmology and Astro-Particle Physics, Apr. 2010

PSR J1907+0602: A Radio-Faint Gamma-Ray Pulsar Powering a Bright TeV Pulsar Wind Nebula
Abdo, A. A.; Ackermann, M.; Ajello, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Camilo, F.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cognard, I.; Cohen-Tanugi, J.; Cominsky, L. R.; Conrad, J.; Cutini, S.; de Angelis, A.; de Palma, F.; Digel, S. W.; Dingus, B. L.; Dormody, M.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fortin, P.; Frailis, M.; Freire, P. C. C.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giavitto, G.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hays, E.; Hughes, R. E.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, T. J.; Johnson, W. N.; Johnston, S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocian, M. L.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Marelli, M.; Mazziotta, M. N.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Ray, P. S.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Roberts, M. S. E.; Rochester, L. S.; Rodriguez, A. Y.; Ro'mani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Theureau, G.; Thompson, D. J.; Tibaldo, L.; Tibolla, O.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Van Etten, A.; Vasileiou, V.; Venter, C.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Watters, K.; Winer, B. L.; Wolff, M. T.; Wood, K. S.; Ylinen, T.; Ziegler, M., We present multiwavelength studies of the 106.6 ms γ-ray pulsar PSR J1907+06 near the TeV source MGRO J1908+06. Timing observations with Fermi result in a precise position determination for the pulsar of R.A. = 19^h07^m54.^s7(2), decl. = +06°02'16(2)'' placing the pulsar firmly within the TeV source extent, suggesting the TeV source is the pulsar wind nebula of PSR J1907+0602. Pulsed γ-ray emission is clearly visible at energies from 100 MeV to above 10 GeV. The phase-averaged power-law index in the energy range E > 0.1 GeV is Γ = 1.76 ± 0.05 with an exponential cutoff energy E_c = 3.6 ± 0.5 GeV. We present the energy-dependent γ-ray pulsed light curve as well as limits on off-pulse emission associated with the TeV source. We also report the detection of very faint (flux density of ~= 3.4 μJy) radio pulsations with the Arecibo telescope at 1.5 GHz having a dispersion measure DM = 82.1 ± 1.1 cm^-3 pc. This indicates a distance of 3.2 ± 0.6 kpc and a pseudo-luminosity of L ₁₄₀₀ ~= 0.035 mJy kpc². A Chandra ACIS observation revealed an absorbed, possibly extended, compact (lsim4'') X-ray source with significant nonthermal emission at R.A. = 19^h07^m54.^s76, decl. = +06°02'14farcs6 with a flux of 2.3^+0.6 _-1.4 × 10^-14 erg cm^-2 s^-1. From archival ASCA observations, we place upper limits on any arcminute scale 2-10 keV X-ray emission of ~1 × 10^-13 erg cm^-2 s^-1. The implied distance to the pulsar is compatible with that of the supernova remnant G40.5 - 0.5, located on the far side of the TeV nebula from PSR J1907+0602, and the S74 molecular cloud on the nearer side which we discuss as potential birth sites....
The Astrophysical Journal, Mar. 2010

Spectrum of the Isotropic Diffuse Gamma-Ray Emission Derived from First-Year Fermi Large Area Telescope Data
Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cominsky, L. R.; Conrad, J.; Cutini, S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; di Bernardo, G.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gaggero, D.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giommi, P.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Gustafsson, M.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hughes, R. E.; Itoh, R.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocian, M. L.; Kuehn, F.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Parkinson, P. M. Saz; Scargle, J. D.; Sellerholm, A.; Sgrò, C.; Shaw, M. S.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Strickman, M. S.; Strong, A. W.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M.; Fermi LAT Collaboration, We report on the first Fermi Large Area Telescope (LAT) measurements of the so-called “extragalactic” diffuse γ-ray emission (EGB). This component of the diffuse γ-ray emission is generally considered to have an isotropic or nearly isotropic distribution on the sky with diverse contributions discussed in the literature. The derivation of the EGB is based on detailed modeling of the bright foreground diffuse Galactic γ-ray emission, the detected LAT sources, and the solar γ-ray emission. We find the spectrum of the EGB is consistent with a power law with a differential spectral index γ=2.41±0.05 and intensity I(>100MeV)=(1.03±0.17)×10^-5cm^-2s^-1sr^-1, where the error is systematics dominated. Our EGB spectrum is featureless, less intense, and softer than that derived from EGRET data....
Physical Review Letters, Mar. 2010

Observations of Milky Way Dwarf Spheroidal Galaxies with the Fermi-Large Area Telescope Detector and Constraints on Dark Matter Models
Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; de Angelis, A.; de Palma, F.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Gustafsson, M.; Harding, A. K.; Hays, E.; Horan, D.; Hughes, R. E.; Jackson, M. S.; Jeltema, T. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kerr, M.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Mazziotta, M. N.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Profumo, S.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rodriguez, A. Y.; Roth, M.; Sadrozinski, H. F. -W.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Schalk, T. L.; Sellerholm, A.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M.; Bullock, James S.; Kaplinghat, Manoj; Martinez, Gregory D.; Fermi LAT Collaboration, We report on the observations of 14 dwarf spheroidal galaxies (dSphs) with the Fermi Gamma-Ray Space Telescope taken during the first 11 months of survey mode operations. The Fermi telescope, which is conducting an all-sky γ-ray survey in the 20 MeV to >300 GeV energy range, provides a new opportunity to test particle dark matter models through the expected γ-ray emission produced by pair annihilation of weakly interacting massive particles (WIMPs). Local Group dSphs, the largest galactic substructures predicted by the cold dark matter scenario, are attractive targets for such indirect searches for dark matter because they are nearby and among the most extreme dark matter dominated environments. No significant γ-ray emission was detected above 100 MeV from the candidate dwarf galaxies. We determine upper limits to the γ-ray flux assuming both power-law spectra and representative spectra from WIMP annihilation. The resulting integral flux above 100 MeV is constrained to be at a level below around 10^-9 photons cm^-2 s^-1. Using recent stellar kinematic data, the γ-ray flux limits are combined with improved determinations of the dark matter density profile in eight of the 14 candidate dwarfs to place limits on the pair-annihilation cross section of WIMPs in several widely studied extensions of the standard model, including its supersymmetric extension and other models that received recent attention. With the present data, we are able to rule out large parts of the parameter space where the thermal relic density is below the observed cosmological dark matter density and WIMPs (neutralinos here) are dominantly produced non-thermally, e.g., in models where supersymmetry breaking occurs via anomaly mediation. The γ-ray limits presented here also constrain some WIMP models proposed to explain the Fermi and PAMELA e ⁺ e ^- data, including low-mass wino-like neutralinos and models with TeV masses pair annihilating into muon-antimuon pairs....
The Astrophysical Journal, Mar. 2010

Observation of Supernova Remnant IC 443 with the Fermi Large Area Telescope
Abdo, A. A.; Ackermann, M.; Ajello, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Cillis, A. N.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cominsky, L. R.; Conrad, J.; Cutini, S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Silva, E. do Couto e.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giavitto, G.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hughes, R. E.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocian, M. L.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Mazziotta, M. N.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Strong, A. W.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Van Etten, A.; Vasileiou, V.; Venter, C.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M., We report observation of the supernova remnant (SNR) IC 443 (G189.1+3.0) with the Fermi Gamma-ray Space Telescope Large Area Telescope (LAT) in the energy band between 200 MeV and 50 GeV. IC 443 is a shell-type SNR with mixed morphology located off the outer Galactic plane where high-energy emission has been detected in the X-ray, GeV and TeV gamma-ray bands. Past observations suggest IC 443 has been interacting with surrounding interstellar matter. Proximity between dense shocked molecular clouds and GeV-TeV gamma-ray emission regions detected by EGRET, MAGIC, and VERITAS suggests an interpretation that cosmic-ray (CR) particles are accelerated by the SNR. With the high gamma-ray statistics and broad energy coverage provided by the LAT, we accurately characterize the gamma-ray emission produced by the CRs accelerated at IC 443. The emission region is extended in the energy band with θ₆₈ = 0fdg27 ± 0fdg01(stat) ± 0fdg03(sys) for an assumed two-dimensional Gaussian profile and overlaps almost completely with the extended source region of VERITAS. Its centroid is displaced significantly from the known pulsar wind nebula (PWN) which suggests the PWN is not the major contributor in the present energy band. The observed spectrum changes its power-law slope continuously and continues smoothly to the MAGIC and VERITAS data points. The combined gamma-ray spectrum (200 MeV <E< 2 TeV) is reproduced well by decays of neutral pions produced by a broken power-law proton spectrum with a break around 70 GeV....
The Astrophysical Journal, Mar. 2010

Fermi Detection of Delayed GeV Emission from the Short Gamma-Ray Burst 081024B
Abdo, A. A.; Ackermann, M.; Ajello, M.; Asano, K.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bhat, P. N.; Bissaldi, E.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Briggs, M. S.; Brigida, M.; Bruel, P.; Burgess, J. M.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Chaplin, V.; Charles, E.; Chekhtman, A.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cominsky, L. R.; Connaughton, V.; Conrad, J.; Cutini, S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Fishman, G.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giommi, P.; Giordano, F.; Glanzman, T.; Godfrey, G.; Granot, J.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Haynes, R. H.; Hays, E.; Horan, D.; Hughes, R. E.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Kippen, R. M.; Knödlseder, J.; Kocevski, D.; Kocian, M. L.; Komin, N.; Kouveliotou, C.; Kuehn, F.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Mazziotta, M. N.; McBreen, S.; McEnery, J. E.; McGlynn, S.; Meegan, C.; Mészáros, P.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paciesas, W. S.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Preece, R.; Rainò, S.; Rando, R.; Razzano, M.; Razzaque, S.; Reimer, A.; Reimer, O.; Reposeur, T.; Ripken, J.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Schalk, T. L.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stamatikos, M.; Strickman, M. S.; Suson, D. J.; Tagliaferri, G.; Tajima, H.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Toma, K.; Torres, D. F.; Tosti, G.; Tramacere, A.; Troja, E.; Uchiyama, Y.; Usher, T. L.; van der Horst, A. J.; Vasileiou, V.; Vilchez, N.; Vitale, V.; von Kienlin, A.; Waite, A. P.; Wang, P.; Wilson-Hodge, C.; Winer, B. L.; Wood, K. S.; Wu, X. F.; Yamazaki, R.; Ylinen, T.; Ziegler, M., We report on the detailed analysis of the high-energy extended emission from the short gamma-ray burst (GRB) 081024B detected by the Fermi Gamma-ray Space Telescope. Historically, this represents the first clear detection of temporal extended emission from a short GRB. The light curve observed by the Fermi Gamma-ray Burst Monitor lasts approximately 0.8 s whereas the emission in the Fermi Large Area Telescope lasts for about 3 s. Evidence of longer lasting high-energy emission associated with long bursts has been already reported by previous experiments. Our observations, together with the earlier reported study of the bright short GRB 090510, indicate similarities in the high-energy emission of short and long GRBs and open the path to new interpretations....
The Astrophysical Journal, Mar. 2010

Fermi Large Area Telescope Search for Photon Lines from 30 to 200 GeV and Dark Matter Implications
Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Do Couto E Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Dumora, D.; Edmonds, Y.; Essig, R.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Gustafsson, M.; Hadasch, D.; Harding, A. K.; Horan, D.; Hughes, R. E.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Llena Garde, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Mazziotta, M. N.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ripken, J.; Ritz, S.; Rodriguez, A. Y.; Roth, M.; Sadrozinski, H. F. -W.; Sander, A.; Parkinson, P. M. Saz; Scargle, J. D.; Schalk, T. L.; Sellerholm, A.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tibaldo, L.; Torres, D. F.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M.; Fermi LAT Collaboration, Dark matter (DM) particle annihilation or decay can produce monochromatic γ rays readily distinguishable from astrophysical sources. γ-ray line limits from 30 to 200 GeV obtained from 11 months of Fermi Large Area Space Telescope data from 20-300 GeV are presented using a selection based on requirements for a γ-ray line analysis, and integrated over most of the sky. We obtain γ-ray line flux upper limits in the range 0.6-4.5×10^-9cm^-2s^-1, and give corresponding DM annihilation cross-section and decay lifetime limits. Theoretical implications are briefly discussed....
Physical Review Letters, Mar. 2010

Swift and Fermi Observations of the Early Afterglow of the Short Gamma-Ray Burst 090510
De Pasquale, M.; Schady, P.; Kuin, N. P. M.; Page, M. J.; Curran, P. A.; Zane, S.; Oates, S. R.; Holland, S. T.; Breeveld, A. A.; Hoversten, E. A.; Chincarini, G.; Grupe, D.; Abdo, A. A.; Ackermann, M.; Ajello, M.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bissaldi, E.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Briggs, M. S.; Brigida, M.; Bruel, P.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Connaughton, V.; Conrad, J.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Dingus, B. L.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Fishman, G.; Focke, W. B.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Granot, J.; Greiner, J.; Grenier, I. A.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Harding, A. K.; Hayashida, M.; Hays, E.; Horan, D.; Hughes, R. E.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Kippen, R. M.; Knödlseder, J.; Kocevski, D.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Mazziotta, M. N.; McEnery, J. E.; McGlynn, S.; Meegan, C.; Mészáros, P.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Monte, C.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paciesas, W. S.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Preece, R.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Schalk, T. L.; Sgrò, C.; Siskind, E. J.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stamatikos, M.; Starck, J. -L.; Stecker, F. W.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Toma, K.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Uehara, T.; Usher, T. L.; van der Horst, A. J.; Vasileiou, V.; Vilchez, N.; Vitale, V.; von Kienlin, A.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Wu, X. F.; Yamazaki, R.; Ylinen, T.; Ziegler, M., We present the observations of GRB090510 performed by the Fermi Gamma-Ray Space Telescope and the Swift observatory. This is a bright, short burst that shows an extended emission detected in the GeV range. Furthermore, its optical emission initially rises, a feature so far observed only in long bursts, while the X-ray flux shows an initial shallow decrease, followed by a steeper decay. This exceptional behavior enables us to investigate the physical properties of the gamma-ray burst outflow, poorly known in short bursts. We discuss internal and external shock models for the broadband energy emission of this object....
The Astrophysical Journal, Feb. 2010

Fermi Observations of Cassiopeia and Cepheus: Diffuse Gamma-ray Emission in the Outer Galaxy
Abdo, A. A.; Ackermann, M.; Ajello, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cominsky, L. R.; Conrad, J.; Dermer, C. D.; de Palma, F.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gehrels, N.; Germani, S.; Giavitto, G.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Harding, A. K.; Hayashida, M.; Horan, D.; Hughes, R. E.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Mazziotta, M. N.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Rodriguez, A. Y.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Sgrò, C.; Siskind, E. J.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Strickman, M. S.; Strong, A. W.; Suson, D. J.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M.; Fermi/LAT Collaboration, We present the analysis of the interstellar γ-ray emission measured by the Fermi Large Area Telescope toward a region in the second Galactic quadrant at 100° <= l <= 145° and -15° <= b <= +30°. This region encompasses the prominent Gould Belt clouds of Cassiopeia, Cepheus, and the Polaris flare, as well as atomic and molecular complexes at larger distances, like that associated with NGC 7538 in the Perseus arm. The good kinematic separation in velocity between the local, Perseus, and outer arms, and the presence of massive complexes in each of them, make this region well suited to probe cosmic rays (CRs) and the interstellar medium beyond the solar circle. The γ-ray emissivity spectrum of the gas in the Gould Belt is consistent with expectations based on the locally measured CR spectra. The γ-ray emissivity decreases from the Gould Belt to the Perseus arm, but the measured gradient is flatter than expectations for CR sources peaking in the inner Galaxy as suggested by pulsars. The X _CO = N(H₂)/W _CO conversion factor is found to increase from (0.87 ± 0.05) × 10²⁰ cm^-2 (K km s^-1)^-1 in the Gould Belt to (1.9 ± 0.2) × 10²⁰ cm^-2 (K km s^-1)^-1 in the Perseus arm. We derive masses for the molecular clouds under study. Dark gas, not properly traced by radio and microwave surveys, is detected in the Gould Belt through a correlated excess of dust and γ-ray emission: its mass amounts to ~50% of the CO-traced mass....
The Astrophysical Journal, Feb. 2010

PKS 1502+106: A New and Distant Gamma-ray Blazar in Outburst Discovered by the Fermi Large Area Telescope
Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bloom, E. D.; Bogaert, G.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Cutini, S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Focke, W. B.; Frailis, M.; Fuhrmann, L.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, W. N.; Kadler, M.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kerr, M.; Knödlseder, J.; Kocian, M. L.; Kuehn, F.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Marelli, M.; Massaro, E.; Max-Moerbeck, W.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pavlidou, V.; Pearson, T. J.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Razzaque, S.; Readhead, A.; Reimer, A.; Reimer, O.; Reposeur, T.; Richards, J. L.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Sgrò, C.; Shaw, M. S.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stevenson, M.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Tibolla, O.; Torres, D. F.; Tosti, G.; Tramacere, A.; Ubertini, P.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yasuda, H.; Ylinen, T.; Zensus, J. A.; Ziegler, M.; Fermi LAT Collaboration; Angelakis, E.; Hovatta, T.; Hoversten, E.; Ikejiri, Y.; Kawabata, K. S.; Kovalev, Y. Y.; Kovalev, Yu. A.; Krichbaum, T. P.; Lister, M. L.; Lähteenmäki, A.; Marchili, N.; Ogle, P.; Pagani, C.; Pushkarev, A. B.; Sakimoto, K.; Sasada, M.; Tornikoski, M.; Uemura, M.; Yamanaka, M.; Yamashita, T.; Fermi LAT Collaboration; Multifrequency Campaign Collaboration, The Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope discovered a rapid (~5 days duration), high-energy (E > 100 MeV) gamma-ray outburst from a source identified with the blazar PKS 1502+106 (OR 103, S3 1502+10, z = 1.839) starting on 2008 August 5 (~23 UTC, MJD 54683.95), and followed by bright and variable flux over the next few months. Results on the gamma-ray localization and identification, as well as spectral and temporal behavior during the first months of the Fermi all-sky survey, are reported here in conjunction with a multiwaveband characterization as a result of one of the first Fermi multifrequency campaigns. The campaign included a Swift ToO (followed up by a 16 day observation on August 7-22, MJD 54685-54700), VLBA (within the MOJAVE program), Owens Valley Radio Observatory (OVRO) 40 m, Effelsberg-100 m, Metsähovi-14 m, RATAN-600, and Kanata-Hiroshima radio/optical observations. Results from the analysis of archival observations by INTEGRAL, XMM-Newton, and Spitzer space telescopes are reported for a more complete picture of this new gamma-ray blazar. PKS 1502+106 is a sub-GeV peaked, powerful flat spectrum radio quasar (luminosity at E > 100 MeV, L _γ, is about 1.1 × 10⁴⁹ erg s^-1, and black hole mass likely close to 10⁹ M _sun), exhibiting marked gamma-ray bolometric dominance, in particular during the asymmetric outburst (L _γ/L _opt ~ 100, and 5 day averaged flux F _{E > 100 MeV} = 2.91 ± 1.4 × 10^-6 ph cm^-2 s^-1), which was characterized by a factor greater than 3 of flux increase in less than 12 hr. The outburst was observed simultaneously from optical to X-ray bands (F _{0.3 - 10 keV} = 2.18^+0.15 _-0.12 × 10^-12 erg cm^-2 s^-1, and hard photon index ~1.5, similar to past values) with a flux increase of less than 1 order of magnitude with respect to past observations, and was likely controlled by Comptonization of external-jet photons produced in the broad-line region (BLR) in the gamma-ray band. No evidence of a possible blue bump signature was observed in the optical-UV continuum spectrum, while some hints for a possible 4 day time lag with respect to the gamma-ray flare were found. Nonetheless, the properties of PKS 1502+106 and the strict optical/UV, X-, and gamma-ray cross-correlations suggest the contribution of the synchrotron self-Compton (SSC), in-jet, process should dominate from radio to X-rays. This mechanism may also be responsible for the consistent gamma-ray variability observed by the LAT on longer timescales, after the ignition of activity at these energies provided by the BLR-dissipated outburst. Modulations and subsequent minor, rapid flare events were detected, with a general fluctuation mode between pink-noise and a random-walk. The averaged gamma-ray spectrum showed a deviation from a simple power law, and can be described by a log-parabola curved model peaking around 0.4-0.5 GeV. The maximum energy of photons detected from the source in the first four months of LAT observations was 15.8 GeV, with no significant consequences on extragalactic background light predictions. A possible radio counterpart of the gamma-ray outburst can be assumed only if a delay of more than three months is considered on the basis of opacity effects at cm and longer wavelengths. The rotation of the electric vector position angle observed by VLBA from 2007 to 2008 could represent a slow field ordering and alignment with respect to the jet axis, likely a precursor feature of the ejection of a superluminal radio knot and the high-energy outburst. This observing campaign provides more insight into the connection between MeV-GeV flares and the moving, polarized structures observed by the VLBI....
The Astrophysical Journal, Feb. 2010

Spectral Properties of Bright Fermi-Detected Blazars in the Gamma-Ray Band
Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Cutini, S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giommi, P.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Harding, A. K.; Hartman, R. C.; Hayashida, M.; Hays, E.; Healey, S. E.; Horan, D.; Hughes, R. E.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Persic, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Vilchez, N.; Villata, M.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M., The gamma-ray energy spectra of bright blazars of the LAT Bright AGN Sample (LBAS) are investigated using Fermi-LAT data. Spectral properties (hardness, curvature, and variability) established using a data set accumulated over 6 months of operation are presented and discussed for different blazar classes and subclasses: flat spectrum radio quasars (FSRQs), low-synchrotron peaked BLLacs (LSP-BLLacs), intermediate-synchrotron peaked BLLacs (ISP-BLLacs), and high-synchrotron peaked BLLacs (HSP-BLLacs). The distribution of photon index (Γ, obtained from a power-law fit above 100 MeV) is found to correlate strongly with blazar subclass. The change in spectral index from that averaged over the 6 months observing period is < 0.2-0.3 when the flux varies by about an order of magnitude, with a tendency toward harder spectra when the flux is brighter for FSRQs and LSP-BLLacs. A strong departure from a single power-law spectrum appears to be a common feature for FSRQs. This feature is also present for some high-luminosity LSP-BLLacs, and a small number of ISP-BLLacs. It is absent in all LBAS HSP-BLLacs. For 3C 454.3 and AO 0235+164, the two brightest FSRQ source and LSP-BLLac source, respectively, a broken power law (BPL) gives the most acceptable of power law, BPL, and curved forms. The consequences of these findings are discussed....
The Astrophysical Journal, Feb. 2010

Fermi-Lat Discovery of GeV Gamma-Ray Emission from the Young Supernova Remnant Cassiopeia A
Abdo, A. A.; Ackermann, M.; Ajello, M.; Allafort, A.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Buehler, R.; Burnett, T. H.; Busetto, G.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chaty, S.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Cillis, A. N.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Corbel, S.; de Palma, F.; Digel, S. W.; Dormody, M.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Edmonds, Y.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giavitto, G.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Hays, E.; Harding, A. K.; Hayashida, M.; Horan, D.; Hughes, R. E.; Jackson, M. S.; Johnson, A. S.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Mazziotta, M. N.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J. H.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Pohl, M.; Porter, T. A.; Rainò, S.; Rando, R.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Sadrozinski, H. F. -W.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Thorsett, S. E.; Tibaldo, L.; Tibolla, O.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Van Etten, A.; Vasileiou, V.; Venter, C.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yamazaki, R.; Ylinen, T.; Ziegler, M., We report on the first detection of GeV high-energy gamma-ray emission from a young supernova remnant (SNR) with the Large Area Telescope aboard the Fermi Gamma-ray Space Telescope. These observations reveal a source with no discernible spatial extension detected at a significance level of 12.2σ above 500 MeV at a location that is consistent with the position of the remnant of the supernova explosion that occurred around 1680 in the Cassiopeia constellation—Cassiopeia A (Cas A). The gamma-ray flux and spectral shape of the source are consistent with a scenario in which the gamma-ray emission originates from relativistic particles accelerated in the shell of this remnant. The total content of cosmic rays (electrons and protons) accelerated in Cas A can be estimated as W _CR ~= (1-4) × 10⁴⁹ erg thanks to the well-known density in the remnant assuming that the observed gamma ray originates in the SNR shell(s). The magnetic field in the radio-emitting plasma can be robustly constrained as B >= 0.1 mG, providing new evidence of the magnetic field amplification at the forward shock and the strong field in the shocked ejecta....
The Astrophysical Journal, Feb. 2010

A change in the optical polarization associated with a γ-ray flare in the blazar 3C279
Abdo, A. A.; Ackermann, M.; Ajello, M.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bock, D. C. -J.; Bogart, J. R.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Collmar, W.; Cominsky, L. R.; Conrad, J.; Corbel, S.; Corbet, R.; Costamante, L.; Cutini, S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Do Couto E Silva, E.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Focke, W. B.; Fortin, P.; Frailis, M.; Fuhrmann, L.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Horan, D.; Hughes, R. E.; Iafrate, G.; Itoh, R.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kadler, M.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocian, M. L.; Kuss, M.; Lande, J.; Larsson, S.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Macquart, J.; Madejski, G. M.; Makeev, A.; Max-Moerbeck, W.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; McGlynn, S.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nestoras, I.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J. H.; Parent, D.; Pavlidou, V.; Pearson, T. J.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Readhead, A.; Reimer, A.; Reimer, O.; Reposeur, T.; Reyes, L. C.; Richards, J. L.; Rochester, L. S.; Rodriguez, A. Y.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Sgrò, C.; Shaw, M. S.; Shrader, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stawarz, L.; Stevenson, M.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Taylor, G. B.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Wehrle, A. E.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Zensus, J. A.; Uemura, M.; Ikejiri, Y.; Kawabata, K. S.; Kino, M.; Sakimoto, K.; Sasada, M.; Sato, S.; Yamanaka, M.; Villata, M.; Raiteri, C. M.; Agudo, I.; Aller, H. D.; Aller, M. F.; Angelakis, E.; Arkharov, A. A.; Bach, U.; Benítez, E.; Berdyugin, A.; Blinov, D. A.; Boettcher, M.; Buemi, C. S.; Chen, W. P.; Dolci, M.; Dultzin, D.; Efimova, N. V.; Gurwell, M. A.; Gusbar, C.; Gómez, J. L.; Heidt, J.; Hiriart, D.; Hovatta, T.; Jorstad, S. G.; Konstantinova, T. S.; Kopatskaya, E. N.; Koptelova, E.; Kurtanidze, O. M.; Lahteenmaki, A.; Larionov, V. M.; Larionova, E. G.; Leto, P.; Lin, H. C.; Lindfors, E.; Marscher, A. P.; McHardy, I. M.; Melnichuk, D. A.; Mommert, M.; Nilsson, K.; di Paola, A.; Reinthal, R.; Richter, G. M.; Roca-Sogorb, M.; Roustazadeh, P.; Sigua, L. A.; Takalo, L. O.; Tornikoski, M.; Trigilio, C.; Troitsky, I. S.; Umana, G.; Villforth, C.; Grainge, K.; Moderski, R.; Nalewajko, K.; Sikora, M.; Fermi LAT Collaboration; Members of the 3C Multi-Band Campaign, It is widely accepted that strong and variable radiation detected over all accessible energy bands in a number of active galaxies arises from a relativistic, Doppler-boosted jet pointing close to our line of sight. The size of the emitting zone and the location of this region relative to the central supermassive black hole are, however, poorly known, with estimates ranging from light-hours to a light-year or more. Here we report the coincidence of a gamma (γ)-ray flare with a dramatic change of optical polarization angle. This provides evidence for co-spatiality of optical and γ-ray emission regions and indicates a highly ordered jet magnetic field. The results also require a non-axisymmetric structure of the emission zone, implying a curved trajectory for the emitting material within the jet, with the dissipation region located at a considerable distance from the black hole, at about 10⁵ gravitational radii....
Nature, Feb. 2010

Gamma-Ray Emission from the Shell of Supernova Remnant W44 Revealed by the Fermi LAT
Abdo, A. A.; Ackermann, M.; Ajello, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cognard, I.; Cohen-Tanugi, J.; Cominsky, L. R.; Conrad, J.; Cutini, S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Dumora, D.; Espinoza, C.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giavitto, G.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Hughes, R. E.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Katsuta, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocian, M. L.; Kramer, M.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Lyne, A. G.; Madejski, G. M.; Makeev, A.; Mazziotta, M. N.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Nolan, P. L.; Norris, J. P.; Noutsos, A.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Parkinson, P. M. Saz; Scargle, J. D.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stappers, B. W.; Stecker, F. W.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Theureau, G.; Thompson, D. J.; Tibaldo, L.; Tibolla, O.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Venter, C.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yamazaki, R.; Ylinen, T.; Ziegler, M., Recent observations of supernova remnants (SNRs) hint that they accelerate cosmic rays to energies close to ~10¹⁵ electron volts. However, the nature of the particles that produce the emission remains ambiguous. We report observations of SNR W44 with the Fermi Large Area Telescope at energies between 2 × 10⁸ electron volts and 3 ×10¹¹ electron volts. The detection of a source with a morphology corresponding to the SNR shell implies that the emission is produced by particles accelerated there. The gamma-ray spectrum is well modeled with emission from protons and nuclei. Its steepening above ~10⁹ electron volts provides a probe with which to study how particle acceleration responds to environmental effects such as shock propagation in dense clouds and how accelerated particles are released into interstellar space....
Science, Feb. 2010

DETECTION OF GAMMA-RAY EMISSION FROM THE STARBURST GALAXIES M82 AND NGC 253 WITH THE LARGE AREA TELESCOPE ON FERMI
A. A. Abdo; M. Ackermann; M. Ajello; W. B. Atwood; M. Axelsson; L. Baldini; J. Ballet; G. Barbiellini; D. Bastieri; K. Bechtol; R. Bellazzini; B. Berenji; E. D. Bloom; E. Bonamente; A. W. Borgland; J. Bregeon; A. Brez; M. Brigida; P. Bruel; T. H. Burnett; G. A. Caliandro; R. A. Cameron; P. A. Caraveo; J. M. Casandjian; E. Cavazzuti; C. Cecchi; Oe Celik; E. Charles; A. Chekhtman; C. C. Cheung; J. Chiang; S. Ciprini; R. Claus; J. Cohen-Tanugi; J. Conrad; C. D. Dermer; A. de Angelis; F. de Palma; S. W. Digel; E. do Couto e Silva; P. S. Drell; A. Drlica-Wagner; R. Dubois; D. Dumora; C. Farnier; C. Favuzzi; S. J. Fegan; W. B. Focke; L. Foschini; M. Frailis; Y. Fukazawa; S. Funk; P. Fusco; F. Gargano; D. Gasparrini; N. Gehrels; S. Germani; B. Giebels; N. Giglietto; F. Giordano; T. Glanzman; G. Godfrey; I. A. Grenier; M. -H. Grondin; J. E. Grove; L. Guillemot; S. Guiriec; Y. Hanabata; A. K. Harding; M. Hayashida; E. Hays; R. E. Hughes; G. Johannesson; A. S. Johnson; R. P. Johnson; W. N. Johnson; T. Kamae; H. Katagiri; J. Kataoka; N. Kawai; M. Kerr; J. Knoedlseder; M. L. Kocian; M. Kuss; J. Lande; L. Latronico; M. Lemoine-Goumard; F. Longo; F. Loparco; B. Lott; M. N. Lovellette; P. Lubrano; G. M. Madejski; A. Makeev; M. N. Mazziotta; W. McConville; J. E. McEnery; C. Meurer; P. F. Michelson; W. Mitthumsiri; T. Mizuno; A. A. Moiseev; C. Monte; M. E. Monzani; A. Morselli; I. V. Moskalenko; S. Murgia; T. Nakamori; P. L. Nolan; J. P. Norris; E. Nuss; T. Ohsugi; N. Omodei; E. Orlando; J. F. Ormes; M. Ozaki; D. Paneque; J. H. Panetta; D. Parent; V. Pelassa; M. Pepe; M. Pesce-Rollins; F. Piron; T. A. Porter; S. Raino; R. Rando; M. Razzano; A. Reimer; O. Reimer; T. Reposeur; S. Ritz; A. Y. Rodriguez; R. W. Romani; M. Roth; F. Ryde; H. F. -W. Sadrozinski; A. Sander; P. M. Saz Parkinson; J. D. Scargle; A. Sellerholm; C. Sgro; M. S. Shaw; D. A. Smith; P. D. Smith; G. Spandre; P. Spinelli; M. S. Strickman; A. W. Strong; D. J. Suson; H. Takahashi; T. Tanaka; J. B. Thayer; J. G. Thayer; D. J. Thompson; L. Tibaldo; O. Tibolla; D. F. Torres; G. Tosti; A. Tramacere; Y. Uchiyama; T. L. Usher; V. Vasileiou; N. Vilchez; V. Vitale; A. P. Waite; P. Wang; B. L. Winer; K. S. Wood; T. Ylinen; M. Ziegler, We report the detection of high-energy gamma-ray emission from two starburst galaxies using data obtained with the Large Area Telescope on board the Fermi Gamma-ray Space Telescope. Steady point-like emission above 200 MeV has been detected at significance levels of 6.8 sigma and 4.8 sigma, respectively, from sources positionally coincident with locations of the starburst galaxies M82 and NGC 253. The total fluxes of the sources are consistent with gamma-ray emission originating from the interaction of cosmic rays with local interstellar gas and radiation fields and constitute evidence for a link between massive star formation and gamma-ray emission in star-forming galaxies., IOP PUBLISHING LTD
ASTROPHYSICAL JOURNAL LETTERS, Feb. 2010

Fermi Large Area Telescope Observations of the Crab Pulsar And Nebula
Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Camilo, F.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cognard, I.; Cohen-Tanugi, J.; Cominsky, L. R.; Conrad, J.; Dermer, C. D.; de Angelis, A.; de Luca, A.; de Palma, F.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Espinoza, C.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Focke, W. B.; Frailis, M.; Freire, P. C. C.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giavitto, G.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Johnston, S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocian, M. L.; Kramer, M.; Kuehn, F.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Lyne, A. G.; Makeev, A.; Marelli, M.; Mazziotta, M. N.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Nolan, P. L.; Norris, J. P.; Noutsos, A.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Ray, P. S.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stappers, B. W.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Theureau, G.; Thompson, D. J.; Thorsett, S. E.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Van Etten, A.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wallace, E.; Wang, P.; Watters, K.; Weltevrede, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M., We report on γ-ray observations of the Crab Pulsar and Nebula using 8 months of survey data with the Fermi Large Area Telescope (LAT). The high quality light curve obtained using the ephemeris provided by the Nançay and Jodrell Bank radio telescopes shows two main peaks stable in phase with energy. The first γ-ray peak leads the radio main pulse by (281 ± 12 ± 21) μs, giving new constraints on the production site of non-thermal emission in pulsar magnetospheres. The first uncertainty is due to γ-ray statistics, and the second arises from the rotation parameters. The improved sensitivity and the unprecedented statistics afforded by the LAT enable precise measurement of the Crab Pulsar spectral parameters: cut-off energy at E_c = (5.8 ± 0.5 ± 1.2) GeV, spectral index of Γ = (1.97 ± 0.02 ± 0.06) and integral photon flux above 100 MeV of (2.09 ± 0.03 ± 0.18) × 10^-6 cm^-2 s^-1. The first errors represent the statistical error on the fit parameters, while the second ones are the systematic uncertainties. Pulsed γ-ray photons are observed up to ~ 20 GeV which precludes emission near the stellar surface, below altitudes of around 4-5 stellar radii in phase intervals encompassing the two main peaks. A detailed phase-resolved spectral analysis is also performed: the hardest emission from the Crab Pulsar comes from the bridge region between the two γ-ray peaks while the softest comes from the falling edge of the second peak. The spectrum of the nebula in the energy range 100 MeV-300 GeV is well described by the sum of two power laws of indices Γ_sync = (3.99 ± 0.12 ± 0.08) and Γ_IC = (1.64 ± 0.05 ± 0.07), corresponding to the falling edge of the synchrotron and the rising edge of the inverse Compton (IC) components, respectively. This latter, which links up naturally with the spectral data points of Cherenkov experiments, is well reproduced via IC scattering from standard magnetohydrodynamic nebula models, and does not require any additional radiation mechanism....
The Astrophysical Journal, Jan. 2010

Fermi Observations of the Very Hard Gamma-ray Blazar PG 1553+113
Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Cutini, S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Horan, D.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocian, M. L.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Sgrò, C.; Shaw, M. S.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M.; Fermi LAT Collaboration, We report the observations of PG 1553+113 during the first ~ 200 days of Fermi Gamma-ray Space Telescope science operations, from 2008 August 4 to 2009 February 22 (MJD 54682.7-54884.2). This is the first detailed study of PG 1553+113 in the GeV gamma-ray regime and it allows us to fill a gap of three decades in energy in its spectral energy distribution (SED). We find PG 1553+113 to be a steady source with a hard spectrum that is best fit by a simple power law in the Fermi energy band. We combine the Fermi data with archival radio, optical, X-ray, and very high energy (VHE) gamma-ray data to model its broadband SED and find that a simple, one-zone synchrotron self-Compton model provides a reasonable fit. PG 1553+113 has the softest VHE spectrum of all sources detected in that regime and, out of those with significant detections across the Fermi energy bandpass so far, the hardest spectrum in that energy regime. Thus, it has the largest spectral break of any gamma-ray source studied to date, which could be due to the absorption of the intrinsic gamma-ray spectrum by the extragalactic background light (EBL). Assuming this to be the case, we selected a model with a low level of EBL and used it to absorb the power-law spectrum from PG 1553+113 measured with Fermi (200 MeV-157 GeV) to find the redshift, which gave the best fit to the measured VHE data (90 GeV-1.1 TeV) for this parameterization of the EBL. We show that this redshift can be considered an upper limit on the distance to PG 1553+113....
The Astrophysical Journal, Jan. 2010

Gamma-ray and Radio Properties of Six Pulsars Detected by the Fermi Large Area Telescope
Weltevrede, P.; Abdo, A. A.; Ackermann, M.; Ajello, M.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Camilo, F.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cognard, I.; Cohen-Tanugi, J.; Cominsky, L. R.; Conrad, J.; Cutini, S.; Dermer, C. D.; Desvignes, G.; de Angelis, A.; de Luca, A.; de Palma, F.; Digel, S. W.; Dormody, M.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fortin, P.; Frailis, M.; Freire, P. C. C.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giavitto, G.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hays, E.; Hobbs, G.; Hughes, R. E.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, T. J.; Johnson, W. N.; Johnston, S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Keith, M.; Kerr, M.; Knödlseder, J.; Kocian, M. L.; Kramer, M.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Lyne, A. G.; Makeev, A.; Manchester, R. N.; Mazziotta, M. N.; McEnery, J. E.; McGlynn, S.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Ransom, S. M.; Razzano, M.; Rea, N.; Reimer, A.; Reimer, O.; Reposeur, T.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stappers, B. W.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Theureau, G.; Thompson, D. J.; Thorsett, S. E.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Van Etten, A.; Vasileiou, V.; Venter, C.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Wang, N.; Watters, K.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M., We report the detection of pulsed γ-rays for PSRs J0631+1036, J0659+1414, J0742-2822, J1420-6048, J1509-5850, and J1718-3825 using the Large Area Telescope on board the Fermi Gamma-ray Space Telescope (formerly known as GLAST). Although these six pulsars are diverse in terms of their spin parameters, they share an important feature: their γ-ray light curves are (at least given the current count statistics) single peaked. For two pulsars, there are hints for a double-peaked structure in the light curves. The shapes of the observed light curves of this group of pulsars are discussed in the light of models for which the emission originates from high up in the magnetosphere. The observed phases of the γ-ray light curves are, in general, consistent with those predicted by high-altitude models, although we speculate that the γ-ray emission of PSR J0659+1414, possibly featuring the softest spectrum of all Fermi pulsars coupled with a very low efficiency, arises from relatively low down in the magnetosphere. High-quality radio polarization data are available showing that all but one have a high degree of linear polarization. This allows us to place some constraints on the viewing geometry and aids the comparison of the γ-ray light curves with high-energy beam models....
The Astrophysical Journal, Jan. 2010

Discovery of Very High Energy Gamma Rays from PKS 1424+240 and Multiwavelength Constraints on Its Redshift
Acciari, V. A.; Aliu, E.; Arlen, T.; Aune, T.; Bautista, M.; Beilicke, M.; Benbow, W.; Böttcher, M.; Boltuch, D.; Bradbury, S. M.; Buckley, J. H.; Bugaev, V.; Byrum, K.; Cannon, A.; Cesarini, A.; Chow, Y. C.; Ciupik, L.; Cogan, P.; Cui, W.; Duke, C.; Falcone, A.; Finley, J. P.; Finnegan, G.; Fortson, L.; Furniss, A.; Galante, N.; Gall, D.; Gillanders, G. H.; Godambe, S.; Grube, J.; Guenette, R.; Gyuk, G.; Hanna, D.; Holder, J.; Hui, C. M.; Humensky, T. B.; Kaaret, P.; Karlsson, N.; Kertzman, M.; Kieda, D.; Konopelko, A.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Maier, G.; McArthur, S.; McCann, A.; McCutcheon, M.; Millis, J.; Moriarty, P.; Nagai, T.; Ong, R. A.; Otte, A. N.; Pandel, D.; Perkins, J. S.; Pichel, A.; Pohl, M.; Quinn, J.; Ragan, K.; Reyes, L. C.; Reynolds, P. T.; Roache, E.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Senturk, G. Demet; Smith, A. W.; Steele, D.; Swordy, S. P.; Theiling, M.; Thibadeau, S.; Varlotta, A.; Vassiliev, V. V.; Vincent, S.; Wagner, R. G.; Wakely, S. P.; Ward, J. E.; Weekes, T. C.; Weinstein, A.; Weisgarber, T.; Williams, D. A.; Wissel, S.; Wood, M.; Zitzer, B.; VERITAS Collaboration; Abdo, A. A.; Ackermann, M.; Ajello, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Cutini, S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giommi, P.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Hays, E.; Hughes, R. E.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocian, M. L.; Kuss, M.; Lande, J.; Latronico, L.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Mazziotta, M. N.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Rodriguez, A. Y.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Sgrò, C.; Shaw, M. S.; Siskind, E. J.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M.; Fermi LAT Collaboration; Barber, S. D.; Terndrup, D. M., We report the first detection of very high energy⁸³Gamma-ray emission above 100 GeV. (VHE) gamma-ray emission above 140 GeV from PKS 1424+240, a BL Lac object with an unknown redshift. The photon spectrum above 140 GeV measured by VERITAS is well described by a power law with a photon index of 3.8 ± 0.5_stat ± 0.3_syst and a flux normalization at 200 GeV of (5.1 ± 0.9_stat ± 0.5_syst) × 10^-11 TeV^-1 cm^-2 s^-1, where stat and syst denote the statistical and systematical uncertainties, respectively. The VHE flux is steady over the observation period between MJD 54881 and 55003 (from 2009 February 19 to June 21). Flux variability is also not observed in contemporaneous high-energy observations with the Fermi Large Area Telescope. Contemporaneous X-ray and optical data were also obtained from the Swift XRT and MDM observatory, respectively. The broadband spectral energy distribution is well described by a one-zone synchrotron self-Compton model favoring a redshift of less than 0.1. Using the photon index measured with Fermi in combination with recent extragalactic background light absorption models it can be concluded from the VERITAS data that the redshift of PKS 1424+240 is less than 0.66....
The Astrophysical Journal, Jan. 2010

Fermi Large Area Telescope Observations of the Supernova Remnant W28 (G6.4-0.1)
Abdo; A. and the Fermi LAT collaboration (corresponding author: H. Katagiri et al.), Corresponding, We present detailed analysis of two gamma-ray sources, 1FGL J1801.3-2322c and 1FGL J1800.5-2359c, that have been found toward the supernova remnant (SNR) W28 with the Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope. 1FGL J1801.3-2322c is found to be an extended source within the boundary of SNR W28, and to extensively overlap with the TeV gamma-ray source HESS J1801-233, which is associated with a dense molecular cloud interacting with the SNR. The gamma-ray spectrum measured with the LAT from 0.2 to 100 GeV can be described by a broken power-law function with a break at similar to 1 GeV and photon indices of 2.09 +/- 0.08 (stat) +/- 0.28 (sys) below the break and 2.74 +/- 0.06 (stat) +/- 0.09 (sys) above the break. Given the clear association between HESS J1801-233 and the shocked molecular cloud and a smoothly connected spectrum in the GeV-TeV band, we consider the origin of the gamma-ray emission in both GeV and TeV ranges to be the interaction between particles accelerated in the SNR and the molecular cloud. The decay of neutral pions produced in interactions between accelerated hadrons and dense molecular gas provides a reasonable explanation for the broadband gamma-ray spectrum. 1FGL J1800.5-2359c, located outside the southern boundary of SNR W28, cannot be resolved. An upper limit on the size of the gamma-ray emission was estimated to be similar to 16' using events above similar to 2 GeV under the assumption of a circular shape with uniform surface brightness. It appears to coincide with the TeV source HESS J1800-240B, which is considered to be associated with a dense molecular cloud that contains the ultra compact H II region W28A2 (G5.89-0.39). We found no significant gamma-ray emission in the LAT energy band at the positions of TeV sources HESS J1800-230A and HESS J1800-230C. The LAT data for HESS J1800-230A combined with the TeV data points indicate a spectral break between 10 GeV and 100 GeV., IOP PUBLISHING LTD
The Astrophysical Journal, 2010, [Reviewed]

Observations of the Large Magellanic Cloud with Fermi
Fukazawa Yasushi; Hanabata Yoshitaka; Katagiri Hideaki; Mizuno Tsunefumi; Ohsugi Takashi; Takahashi Hiromitsu, Context. The Large Magellanic Cloud (LMC) is to date the only normal external galaxy that has been detected in high-energy gamma rays. High-energy gamma rays trace particle acceleration processes and gamma-ray observations allow the nature and sites of acceleration to be studied.Aims. We characterise the distribution and sources of cosmic rays in the LMC from analysis of gamma-ray observations.Methods. We analyse 11 months of continuous sky-survey observations obtained with the Large Area Telescope aboard the Fermi Gamma-Ray Space Telescope and compare it to tracers of the interstellar medium and models of the gamma-ray sources in the LMC.Results. The LMC is detected at 33σ significance. The integrated >100 MeV photon flux of the LMC amounts to (2.6 ± 0.2) × 10-7 ph cm-2 s-1 which corresponds to an energy flux of (1.6 ± 0.1) × 10-10 erg cm-2 s-1, with additional, EDP Sciences S A
Astronomy & Astrophysics, 2010

Radio-Loud Narrow-Line Seyfert 1 as a New Class of Gamma-Ray Active Galactic Nuclei
Abdo, A. A.; Ackermann, M.; Ajello, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Cutini, S.; Dermer, C. D.; de Palma, F.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Foschini, L.; Frailis, M.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hayashida, M.; Hays, E.; Horan, D.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kadler, M.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kerr, M.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Pelassa, V.; Pepe, M.; Persic, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Rochester, L. S.; Rodriguez, A. Y.; Ryde, F.; Sadrozinski, H. F. -W.; Sambruna, R.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Sgrò, C.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Tagliaferri, G.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Tibolla, O.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M.; Fermi/LAT Collaboration; Ghisellini, G.; Maraschi, L.; Tavecchio, F., We report the discovery with Fermi/LAT of γ-ray emission from three radio-loud narrow-line Seyfert 1 galaxies: PKS 1502+036 (z = 0.409), 1H 0323+342 (z = 0.061), and PKS 2004 - 447 (z = 0.24). In addition to PMN J0948+0022 (z = 0.585), the first source of this type to be detected in γ rays, they may form an emerging new class of γ-ray active galactic nuclei (AGNs). These findings can have strong implications on our knowledge about relativistic jets and the unified model of the AGN....
The Astrophysical Journal, 20 Dec. 2009, [Reviewed]

Multiwavelength Monitoring of the Enigmatic Narrow-Line Seyfert 1 PMN J0948+0022 in 2009 March-July
Abdo, A. A.; Ackermann, M.; Ajello, M.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Celotti, A.; Chekhtman, A.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Collmar, W.; Conrad, J.; Costamante, L.; Cutini, S.; de Angelis, A.; de Palma, F.; Silva, E. Do Couto e.; Drell, P. S.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fortin, P.; Foschini, L.; Frailis, M.; Fuhrmann, L.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gehrels, N.; Germani, S.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Hays, E.; Hughes, R. E.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kadler, M.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocian, M. L.; Kuss, M.; Lande, J.; Latronico, L.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Max-Moerbeck, W.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; McGlynn, S.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Nestoras, I.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Parent, D.; Pavlidou, V.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Readhead, A.; Reimer, O.; Reposeur, T.; Richards, J. L.; Rodriguez, A. Y.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Sgrò, C.; Shaw, M. S.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Tagliaferri, G.; Tajima, H.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Tibolla, O.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Wehrle, A. E.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Zensus, J. A.; Ziegler, M.; Fermi/LAT Collaboration; Angelakis, E.; Bailyn, C.; Bignall, H.; Blanchard, J.; Bonning, E. W.; Buxton, M.; Canterna, R.; Carramiñana, A.; Carrasco, L.; Colomer, F.; Doi, A.; Ghisellini, G.; Hauser, M.; Hong, X.; Isler, J.; Kino, M.; Kovalev, Y. Y.; Kovalev, Yu. A.; Krichbaum, T. P.; Kutyrev, A.; Lahteenmaki, A.; van Langevelde, H. J.; Lister, M. L.; Macomb, D.; Maraschi, L.; Marchili, N.; Nagai, H.; Paragi, Z.; Phillips, C.; Pushkarev, A. B.; Recillas, E.; Roming, P.; Sekido, M.; Stark, M. A.; Szomoru, A.; Tammi, J.; Tavecchio, F.; Tornikoski, M.; Tzioumis, A. K.; Urry, C. M.; Wagner, S., Following the recent discovery of γ rays from the radio-loud narrow-line Seyfert 1 galaxy PMN J0948+0022 (z = 0.5846), we started a multiwavelength campaign from radio to γ rays, which was carried out between the end of 2009 March and the beginning of July. The source displayed activity at all the observed wavelengths: a general decreasing trend from optical to γ-ray frequencies was followed by an increase of radio emission after less than two months from the peak of the γ-ray emission. The largest flux change, about a factor of about 4, occurred in the X-ray band. The smallest was at ultraviolet and near-infrared frequencies, where the rate of the detected photons dropped by a factor 1.6-1.9. At optical wavelengths, where the sampling rate was the highest, it was possible to observe day scale variability, with flux variations up to a factor of about 3. The behavior of PMN J0948+0022 observed in this campaign and the calculated power carried out by its jet in the form of protons, electrons, radiation, and magnetic field are quite similar to that of blazars, specifically of flat-spectrum radio quasars. These results confirm the idea that radio-loud narrow-line Seyfert 1 galaxies host relativistic jets with power similar to that of average blazars....
The Astrophysical Journal, Dec. 2009

Modulated High-Energy Gamma-Ray Emission from the Microquasar Cygnus X-3
Fermi LAT Collaboration; Abdo, A. A.; Ackermann, M.; Ajello, M.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Chaty, S.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cominsky, L. R.; Conrad, J.; Corbel, S.; Corbet, R.; Dermer, C. D.; de Palma, F.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Dubus, G.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fortin, P.; Frailis, M.; Fusco, P.; Gargano, F.; Gehrels, N.; Germani, S.; Giavitto, G.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Hill, A. B.; Hjalmarsdotter, L.; Horan, D.; Hughes, R. E.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocian, M. L.; Koerding, E.; Kuss, M.; Lande, J.; Latronico, J.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Marchand, L.; Marelli, M.; Max-Moerbeck, W.; Mazziotta, M. N.; McColl, N.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Migliari, S.; Mitthumsiri, W.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Ong, R. A.; Ormes, J. F.; Paneque, D.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Pooley, G.; Porter, T. A.; Pottschmidt, K.; Rainò, S.; Rando, R.; Ray, P. S.; Razzano, M.; Rea, N.; Readhead, A.; Reimer, A.; Reimer, O.; Richards, J. L.; Rochester, L. S.; Rodriguez, J.; Rodriguez, A. Y.; Romani, R. W.; Ryde, F.; Sadrozinski, H. F. -W.; Sander, A.; Saz Parkinson, P. M.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spinelli, P.; Starck, J. -L.; Stevenson, M.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Tomsick, J. A.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Wilms, J.; Winer, B. L.; Wood, K. W.; Ylinen, T.; Ziegler, M., Microquasars are accreting black holes or neutron stars in binary systems with associated relativistic jets. Despite their frequent outburst activity, they have never been unambiguously detected emitting high-energy gamma rays. The Fermi Large Area Telescope (LAT) has detected a variable high-energy source coinciding with the position of the x-ray binary and microquasar Cygnus X-3. Its identification with Cygnus X-3 is secured by the detection of its orbital period in gamma rays, as well as the correlation of the LAT flux with radio emission from the relativistic jets of Cygnus X-3. The gamma-ray emission probably originates from within the binary system, opening new areas in which to study the formation of relativistic jets....
Science, Dec. 2009

Fermi Large Area Telescope Detection of Pulsed γ-rays from the Vela-like Pulsars PSR J1048-5832 and PSR J2229+6114
Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Caliandro, G. A.; Cameron, R. A.; Camilo, F.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cognard, I.; Cohen-Tanugi, J.; Conrad, J.; de Angelis, A.; de Palma, F.; Dormody, M.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Frailis, M.; Freire, P. C. C.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Halpern, J.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Hobbs, G.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Johnston, S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocian, M. L.; Kramer, M.; Kuehn, F.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Lyne, A. G.; Makeev, A.; Manchester, R. N.; Marelli, M.; Mazziotta, M. N.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Noutsos, A.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Ransom, S. M.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stappers, B. W.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Theureau, G.; Thompson, D. J.; Thorsett, S. E.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Uchiyama, Y.; Usher, T. L.; Van Etten, A.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Wang, N.; Watters, K.; Weltevrede, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M., We report the detection of γ-ray pulsations (>=0.1 GeV) from PSR J2229+6114 and PSR J1048-5832, the latter having been detected as a low-significance pulsar by EGRET. Data in the γ-ray band were acquired by the Large Area Telescope (LAT) aboard the Fermi Gamma-ray Space Telescope, while the radio rotational ephemerides used to fold the γ-ray light curves were obtained using the Green Bank Telescope, the Lovell telescope at Jodrell Bank, and the Parkes Telescope. The two young radio pulsars, located within the error circles of the previously unidentified EGRET sources 3EG J1048-5840 and 3EG J2227+6122, present spin-down characteristics similar to the Vela pulsar. PSR J1048-5832 shows two sharp peaks at phases 0.15 ± 0.01 and 0.57 ± 0.01 relative to the radio pulse confirming the EGRET light curve, while PSR J2229+6114 presents a very broad peak at phase 0.49 ± 0.01. The γ-ray spectra above 0.1 GeV of both pulsars are fit with power laws having exponential cutoffs near 3 GeV, leading to integral photon fluxes of (2.19 ± 0.22 ± 0.32) × 10^-7 cm^-2 s^-1 for PSR J1048-5832 and (3.77 ± 0.22 ± 0.44) × 10^-7 cm^-2 s^-1 for PSR J2229+6114. The first uncertainty is statistical and the second is systematic. PSR J1048-5832 is one of the two LAT sources which were entangled together as 3EG J1048-5840. These detections add to the growing number of young γ-ray pulsars that make up the dominant population of GeV γ-ray sources in the Galactic plane....
The Astrophysical Journal, Dec. 2009

Fermi Large Area Telescope Gamma-Ray Detection of the Radio Galaxy M87
Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Cannon, A.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Charles, E.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Colafrancesco, S.; Conrad, J.; Costamante, L.; Cutini, S.; Davis, D. S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Donato, D.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Edmonds, Y.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Finke, J.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Georganopoulos, M.; Germani, S.; Giebels, B.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Horan, D.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocian, M. L.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sambruna, R.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Sgrò, C.; Shaw, M. S.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Tanaka, T.; Taylor, G. B.; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Vilchez, N.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M.; Harris, D. E.; Massaro, F.; Stawarz, Ł., We report the Fermi Large Area Telescope (LAT) discovery of high-energy (MeV/GeV) γ-ray emission positionally consistent with the center of the radio galaxy M87, at a source significance of over 10σ in 10 months of all-sky survey data. Following the detections of Cen A and Per A, this makes M87 the third radio galaxy seen with the LAT. The faint point-like γ-ray source has a >100 MeV flux of 2.45 (±0.63) × 10^-8 photons cm^-2 s^-1 (photon index = 2.26 ± 0.13) with no significant variability detected within the LAT observation. This flux is comparable with the previous EGRET upper limit (<2.18 × 10^-8 photons cm^-2 s^-1, 2σ), thus there is no evidence for a significant MeV/GeV flare on decade timescales. Contemporaneous Chandra and Very Long Baseline Array data indicate low activity in the unresolved X-ray and radio core relative to previous observations, suggesting M87 is in a quiescent overall level over the first year of Fermi-LAT observations. The LAT γ-ray spectrum is modeled as synchrotron self-Compton (SSC) emission from the electron population producing the radio-to-X-ray emission in the core. The resultant SSC spectrum extrapolates smoothly from the LAT band to the historical-minimum TeV emission. Alternative models for the core and possible contributions from the kiloparsec-scale jet in M87 are considered, and cannot be excluded....
The Astrophysical Journal, Dec. 2009

Fermi Observations of TeV-Selected Active Galactic Nuclei
Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cominsky, L. R.; Conrad, J.; Cutini, S.; de Angelis, A.; de Palma, F.; Di Bernardo, G.; Silva, E. do Couto e.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Finke, J.; Focke, W. B.; Fortin, P.; Foschini, L.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giavitto, G.; Giebels, B.; Giglietto, N.; Giommi, P.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Hayashida, M.; Hays, E.; Horan, D.; Hughes, R. E.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocian, M. L.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Reyes, L. C.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Schalk, T. L.; Sellerholm, A.; Sgrò, C.; Shaw, M. S.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Tanaka, Y.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M., We report on observations of TeV-selected active galactic nuclei (AGNs) made during the first 5.5 months of observations with the Large Area Telescope (LAT) on-board the Fermi Gamma-ray Space Telescope (Fermi). In total, 96 AGNs were selected for study, each being either (1) a source detected at TeV energies (28 sources) or (2) an object that has been studied with TeV instruments and for which an upper limit has been reported (68 objects). The Fermi observations show clear detections of 38 of these TeV-selected objects, of which 21 are joint GeV-TeV sources, and 29 were not in the third EGRET catalog. For each of the 38 Fermi-detected sources, spectra and light curves are presented. Most can be described with a power law of spectral index harder than 2.0, with a spectral break generally required to accommodate the TeV measurements. Based on an extrapolation of the Fermi spectrum, we identify sources, not previously detected at TeV energies, which are promising targets for TeV instruments. Evidence for systematic evolution of the γ-ray spectrum with redshift is presented and discussed in the context of interaction with the extragalactic background light....
The Astrophysical Journal, Dec. 2009

Fermi large area telescope observations of the cosmic-ray induced γ-ray emission of the Earth's atmosphere
Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Buehler, R.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; de Palma, F.; Digel, S. W.; Do Couto E Silva, E.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hays, E.; Horan, D.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Mazziotta, M. N.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Rochester, L. S.; Rodriguez, A. Y.; Roth, M.; Sadrozinski, H. F. -W.; Sander, A.; Saz Parkinson, P. M.; Sgrò, C.; Share, G. H.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M., We report on measurements of the cosmic-ray induced γ-ray emission of Earth’s atmosphere by the Large Area Telescope on board the Fermi Gamma-ray Space Telescope. The Large Area Telescope has observed the Earth during its commissioning phase and with a dedicated Earth limb following observation in September 2008. These measurements yielded ̃6.4×10⁶ photons with energies >100MeV and ̃250 hours total live time for the highest quality data selection. This allows the study of the spatial and spectral distributions of these photons with unprecedented detail. The spectrum of the emission—often referred to as Earth albedo gamma-ray emission—has a power-law shape up to 500 GeV with spectral index Γ=2.79±0.06....
Physical Review D, Dec. 2009

Fermi Large Area Telescope Measurements of the Diffuse Gamma-Ray Emission at Intermediate Galactic Latitudes
Abdo, A. A.; Ackermann, M.; Ajello, M.; Anderson, B.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Dereli, H.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; di Bernardo, G.; Dormody, M.; Do Couto E Silva, E.; Drell, P. S.; Dubois, R.; Dumora, D.; Edmonds, Y.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gaggero, D.; Gargano, F.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocian, M. L.; Kuehn, F.; Kuss, M.; Lande, J.; Latronico, L.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rodriguez, A. Y.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Sellerholm, A.; Sgrò, C.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Stecker, F. W.; Striani, E.; Strickman, M. S.; Strong, A. W.; Suson, D. J.; Tajima, H.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M., The diffuse galactic γ-ray emission is produced by cosmic rays (CRs) interacting with the interstellar gas and radiation field. Measurements by the Energetic Gamma-Ray Experiment Telescope (EGRET) instrument on the Compton Gamma-Ray Observatory indicated excess γ-ray emission ≳1GeV relative to diffuse galactic γ-ray emission models consistent with directly measured CR spectra (the so-called “EGRET GeV excess”). The Large Area Telescope (LAT) instrument on the Fermi Gamma-Ray Space Telescope has measured the diffuse γ-ray emission with improved sensitivity and resolution compared to EGRET. We report on LAT measurements for energies 100 MeV to 10 GeV and galactic latitudes 10°≤|b|≤20°. The LAT spectrum for this region of the sky is well reproduced by a diffuse galactic γ-ray emission model that is consistent with local CR spectra and inconsistent with the EGRET GeV excess....
Physical Review Letters, Dec. 2009

FERMI OBSERVATIONS OF HIGH-ENERGY GAMMA-RAY EMISSION FROM GRB 080825C
A. A. Abdo; M. Ackermann; K. Asano; W. B. Atwood; M. Axelsson; L. Baldini; J. Ballet; D. L. Band; G. Barbiellini; D. Bastieri; K. Bechtol; R. Bellazzini; B. Berenji; P. N. Bhat; E. Bissaldi; E. D. Bloom; E. Bonamente; A. W. Borgland; A. Bouvier; J. Bregeon; A. Brez; M. S. Briggs; M. Brigida; P. Bruel; T. H. Burnett; G. A. Caliandro; R. A. Cameron; P. A. Caraveo; J. M. Casandjian; C. Cecchi; V. Chaplin; A. Chekhtman; C. C. Cheung; J. Chiang; S. Ciprini; R. Claus; J. Cohen-Tanugi; L. R. Cominsky; V. Connaughton; J. Conrad; S. Cutini; C. D. Dermer; A. de Angelis; F. de Palma; S. W. Digel; E. do Couto e Silva; P. S. Drell; R. Dubois; D. Dumora; C. Farnier; C. Favuzzi; W. B. Focke; M. Frailis; Y. Fukazawa; P. Fusco; F. Gargano; D. Gasparrini; N. Gehrels; S. Germani; L. Gibby; B. Giebels; N. Giglietto; F. Giordano; T. Glanzman; G. Godfrey; A. Goldstein; J. Granot; I. A. Grenier; M. -H. Grondin; J. E. Grove; L. Guillemot; S. Guiriec; Y. Hanabata; A. K. Harding; M. Hayashida; E. Hays; R. E. Hughes; G. Johannesson; A. S. Johnson; W. N. Johnson; T. Kamae; H. Katagiri; J. Kataoka; N. Kawai; M. Kerr; J. Knoedlseder; D. Kocevski; N. Komin; C. Kouveliotou; F. Kuehn; M. Kuss; L. Latronico; F. Longo; F. Loparco; B. Lott; M. N. Lovellette; P. Lubrano; A. Makeev; M. N. Mazziotta; S. McBreen; J. E. McEnery; S. McGlynn; C. Meegan; C. Meurer; P. F. Michelson; W. Mitthumsiri; T. Mizuno; C. Monte; M. E. Monzani; E. Moretti; A. Morselli; I. V. Moskalenko; S. Murgia; T. Nakamori; P. L. Nolan; J. P. Norris; E. Nuss; M. Ohno; T. Ohsugi; N. Omodei; E. Orlando; J. F. Ormes; M. Ozaki; W. S. Paciesas; D. Paneque; J. H. Panetta; D. Parent; V. Pelassa; M. Pepe; M. Pesce-Rollins; F. Piron; T. A. Porter; R. Preece; S. Raino; R. Rando; M. Razzano; S. Razzaque; O. Reimer; T. Reposeur; S. Ritz; L. S. Rochester; A. Y. Rodriguez; M. Roth; F. Ryde; H. F. -W. Sadrozinski; D. Sanchez; A. Sander; P. M. Saz Parkinson; J. D. Scargle; C. Sgro; E. J. Siskind; D. A. Smith; P. D. Smith; G. Spandre; P. Spinelli; M. Stamatikos; M. S. Strickman; D. J. Suson; H. Tajima; H. Takahashi; T. Tanaka; J. B. Thayer; J. G. Thayer; L. Tibaldo; D. F. Torres; G. Tosti; A. Tramacere; Y. Uchiyama; T. L. Usher; A. J. van der Horst; V. Vasileiou; N. Vilchez; V. Vitale; A. von Kienlin; A. P. Waite; P. Wang; C. Wilson-Hodge; B. L. Winer; K. S. Wood; T. Ylinen; M. Ziegler, The Fermi Gamma-ray Space Telescope has opened a new high-energy window in the study of gamma-ray bursts (GRBs). Here we present a thorough analysis of GRB 080825C, which triggered the Fermi Gamma-ray Burst Monitor (GBM), and was the first firm detection of a GRB by the Fermi Large Area Telescope (LAT). We discuss the LAT event selections, background estimation, significance calculations, and localization for Fermi GRBs in general and GRB 080825C in particular. We show the results of temporal and time-resolved spectral analysis of the GBM and LAT data. We also present some theoretical interpretation of GRB 080825C observations as well as some common features observed in other LAT GRBs., IOP PUBLISHING LTD
ASTROPHYSICAL JOURNAL, Dec. 2009

Fermi LAT Discovery of Extended Gamma-Ray Emission in the Direction of Supernova Remnant W51C
Abdo, A. A.; Ackermann, M.; Ajello, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cominsky, L. R.; Conrad, J.; Cutini, S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Dormody, M.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giavitto, G.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Hughes, R. E.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Katsuta, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocian, M. L.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Mazziotta, M. N.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Schalk, T. L.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Tibolla, O.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Venter, C.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yamazaki, R.; Ylinen, T.; Ziegler, M., The discovery of bright gamma-ray emission coincident with supernova remnant (SNR) W51C is reported using the Large Area Telescope (LAT) onboard the Fermi Gamma-ray Space Telescope. W51C is a middle-aged remnant (~10⁴ yr) with intense radio synchrotron emission in its shell and known to be interacting with a molecular cloud. The gamma-ray emission is spatially extended, broadly consistent with the radio and X-ray extent of SNR W51C. The energy spectrum in the 0.2-50 GeV band exhibits steepening toward high energies. The luminosity is greater than 1 × 10³⁶ erg s^-1 given the distance constraint of D > 5.5 kpc, which makes this object one of the most luminous gamma-ray sources in our Galaxy. The observed gamma-rays can be explained reasonably by a combination of efficient acceleration of nuclear cosmic rays at supernova shocks and shock-cloud interactions. The decay of neutral π mesons produced in hadronic collisions provides a plausible explanation for the gamma-ray emission. The product of the average gas density and the total energy content of the accelerated protons amounts to \bar{n}_HW_p ≃ 5× 10^{51} (D/6 kpc)^2 erg cm^{-3}. Electron density constraints from the radio and X-ray bands render it difficult to explain the LAT signal as due to inverse Compton scattering. The Fermi LAT source coincident with SNR W51C sheds new light on the origin of Galactic cosmic rays....
The Astrophysical Journal, Nov. 2009

Fermi/LAT observations of LS 5039
Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Chaty, S.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cominsky, L. R.; Conrad, J.; Corbel, S.; Corbet, R.; Cutini, S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dubus, G.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Hill, A. B.; Horan, D.; Hughes, R. E.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocian, M. L.; Kuehn, F.; Kuss, M.; Lande, J.; Larsson, S.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Marelli, M.; Mazziotta, M. N.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Ray, P. S.; Razzano, M.; Rea, N.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Sgrò, C.; Sierpowska-Bartosik, A.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Tanaka, Y.; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Venter, C.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wallace, E.; Wang, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M., The first results from observations of the high-mass X-ray binary LS 5039 using the Fermi Gamma-ray Space Telescope data between 2008 August and 2009 June are presented. Our results indicate variability that is consistent with the binary period, with the emission being modulated with a period of 3.903 ± 0.005 days; the first detection of this modulation at GeV energies. The light curve is characterized by a broad peak around superior conjunction in agreement with inverse Compton scattering models. The spectrum is represented by a power law with an exponential cutoff, yielding an overall flux (100 MeV-300 GeV) of 4.9 ± 0.5(stat) ± 1.8(syst) ×10^-7 photon cm^-2 s^-1, with a cutoff at 2.1 ± 0.3(stat) ± 1.1(syst) GeV and photon index Γ = 1.9 ± 0.1(stat) ± 0.3(syst). The spectrum is observed to vary with orbital phase, specifically between inferior and superior conjunction. We suggest that the presence of a cutoff in the spectrum may be indicative of magnetospheric emission similar to the emission seen in many pulsars by Fermi....
The Astrophysical Journal, Nov. 2009

Fermi Observations of GRB 090902B: A Distinct Spectral Component in the Prompt and Delayed Emission
Abdo, A. A.; Ackermann, M.; Ajello, M.; Asano, K.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bhat, P. N.; Bissaldi, E.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Briggs, M. S.; Brigida, M.; Bruel, P.; Burgess, J. M.; Burrows, D. N.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cominsky, L. R.; Connaughton, V.; Conrad, J.; Cutini, S.; d'Elia, V.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Dingus, B. L.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Finke, J.; Fishman, G.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gehrels, N.; Germani, S.; Giavitto, G.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Goldstein, A.; Granot, J.; Greiner, J.; Grenier, I. A.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Horan, D.; Hughes, R. E.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Kippen, R. M.; Knödlseder, J.; Kocevski, D.; Komin, N.; Kouveliotou, C.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Mazziotta, M. N.; McBreen, S.; McEnery, J. E.; McGlynn, S.; Meegan, C.; Mészáros, P.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paciesas, W. S.; Paneque, D.; Panetta, J. H.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Petrosian, V.; Piron, F.; Porter, T. A.; Preece, R.; Rainò, S.; Rando, R.; Rau, A.; Razzano, M.; Razzaque, S.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Roming, P. W. A.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Schalk, T. L.; Sgrò, C.; Siskind, E. J.; Smith, P. D.; Spinelli, P.; Stamatikos, M.; Stecker, F. W.; Stratta, G.; Strickman, M. S.; Suson, D. J.; Swenson, C. A.; Tajima, H.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Uehara, T.; Usher, T. L.; van der Horst, A. J.; Vasileiou, V.; Vilchez, N.; Vitale, V.; von Kienlin, A.; Waite, A. P.; Wang, P.; Wilson-Hodge, C.; Winer, B. L.; Wood, K. S.; Yamazaki, R.; Ylinen, T.; Ziegler, M., We report on the observation of the bright, long gamma-ray burst (GRB), GRB 090902B, by the Gamma-ray Burst Monitor (GBM) and Large Area Telescope (LAT) instruments on-board the Fermi observatory. This was one of the brightest GRBs to have been observed by the LAT, which detected several hundred photons during the prompt phase. With a redshift of z = 1.822, this burst is among the most luminous detected by Fermi. Time-resolved spectral analysis reveals a significant power-law component in the LAT data that is distinct from the usual Band model emission that is seen in the sub-MeV energy range. This power-law component appears to extrapolate from the GeV range to the lowest energies and is more intense than the Band component, both below ~50 keV and above 100 MeV. The Band component undergoes substantial spectral evolution over the entire course of the burst, while the photon index of the power-law component remains constant for most of the prompt phase, then hardens significantly toward the end. After the prompt phase, power-law emission persists in the LAT data as late as 1 ks post-trigger, with its flux declining as t ^-1.5. The LAT detected a photon with the highest energy so far measured from a GRB, 33.4^+2.7 _-3.5 GeV. This event arrived 82 s after the GBM trigger and ~50 s after the prompt phase emission had ended in the GBM band. We discuss the implications of these results for models of GRB emission and for constraints on models of the extragalactic background light....
The Astrophysical Journal, Nov. 2009

A limit on the variation of the speed of light arising from quantum gravity effects
Abdo, A. A.; Ackermann, M.; Ajello, M.; Asano, K.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bhat, P. N.; Bissaldi, E.; Bloom, E. D.; Bonamente, E.; Bonnell, J.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Briggs, M. S.; Brigida, M.; Bruel, P.; Burgess, J. M.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Chaplin, V.; Charles, E.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cominsky, L. R.; Connaughton, V.; Conrad, J.; Cutini, S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Dingus, B. L.; Do Couto E Silva, E.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Finke, J.; Fishman, G.; Focke, W. B.; Foschini, L.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Gibby, L.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Granot, J.; Greiner, J.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Grupe, D.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Hoversten, E. A.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Kippen, R. M.; Knödlseder, J.; Kocevski, D.; Kouveliotou, C.; Kuehn, F.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Mazziotta, M. N.; McBreen, S.; McEnery, J. E.; McGlynn, S.; Mészáros, P.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paciesas, W. S.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Petrosian, V.; Piron, F.; Porter, T. A.; Preece, R.; Rainò, S.; Ramirez-Ruiz, E.; Rando, R.; Razzano, M.; Razzaque, S.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Schalk, T. L.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stamatikos, M.; Stecker, F. W.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Toma, K.; Torres, D. F.; Tosti, G.; Troja, E.; Uchiyama, Y.; Uehara, T.; Usher, T. L.; van der Horst, A. J.; Vasileiou, V.; Vilchez, N.; Vitale, V.; von Kienlin, A.; Waite, A. P.; Wang, P.; Wilson-Hodge, C.; Winer, B. L.; Wood, K. S.; Wu, X. F.; Yamazaki, R.; Ylinen, T.; Ziegler, M.; Fermi LAT Collaboration, A cornerstone of Einstein’s special relativity is Lorentz invariance—the postulate that all observers measure exactly the same speed of light in vacuum, independent of photon-energy. While special relativity assumes that there is no fundamental length-scale associated with such invariance, there is a fundamental scale (the Planck scale, l_Planck~1.62×10^-33cm or E_Planck = M_Planckc²~1.22×10¹⁹GeV), at which quantum effects are expected to strongly affect the nature of space-time. There is great interest in the (not yet validated) idea that Lorentz invariance might break near the Planck scale. A key test of such violation of Lorentz invariance is a possible variation of photon speed with energy. Even a tiny variation in photon speed, when accumulated over cosmological light-travel times, may be revealed by observing sharp features in γ-ray burst (GRB) light-curves. Here we report the detection of emission up to ~31GeV from the distant and short GRB090510. We find no evidence for the violation of Lorentz invariance, and place a lower limit of 1.2E_Planck on the scale of a linear energy dependence (or an inverse wavelength dependence), subject to reasonable assumptions about the emission (equivalently we have an upper limit of l_Planck/1.2 on the length scale of the effect). Our results disfavour quantum-gravity theories in which the quantum nature of space-time on a very small scale linearly alters the speed of light....
Nature, Nov. 2009

The on-orbit calibration of the Fermi Large Area Telescope
Abdo, A. A.; Ackermann, M.; Ajello, M.; Ampe, J.; Anderson, B.; Atwood, W. B.; Axelsson, M.; Bagagli, R.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bartelt, J.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bédérède, D.; Bellardi, F.; Bellazzini, R.; Belli, F.; Berenji, B.; Bisello, D.; Bissaldi, E.; Bloom, E. D.; Bogaert, G.; Bogart, J. R.; Bonamente, E.; Borgland, A. W.; Bourgeois, P.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Busetto, G.; Caliandro, G. A.; Cameron, R. A.; Campell, M.; Caraveo, P. A.; Carius, S.; Carlson, P.; Casandjian, J. M.; Cavazzuti, E.; Ceccanti, M.; Cecchi, C.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Chipaux, R.; Cillis, A. N.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Condamoor, S.; Conrad, J.; Corbet, R.; Cutini, S.; Davis, D. S.; DeKlotz, M.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Dizon, P.; Dormody, M.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Dumora, D.; Edmonds, Y.; Fabiani, D.; Farnier, C.; Favuzzi, C.; Ferrara, E. C.; Ferreira, O.; Fewtrell, Z.; Flath, D. L.; Fleury, P.; Focke, W. B.; Fouts, K.; Frailis, M.; Freytag, D.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Goodman, J.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hakimi, M.; Haller, G.; Hanabata, Y.; Hart, P. A.; Hascall, P.; Hays, E.; Huffer, M.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kavelaars, A.; Kelly, H.; Kerr, M.; Klamra, W.; Knödlseder, J.; Kocian, M. L.; Kuehn, F.; Kuss, M.; Latronico, L.; Lavalley, C.; Leas, B.; Lee, B.; Lee, S. -H.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Lung, D. K.; Madejski, G. M.; Makeev, A.; Marangelli, B.; Marchetti, M.; Massai, M. M.; May, D.; Mazzenga, G.; Mazziotta, M. N.; McEnery, J. E.; McGlynn, S.; Meurer, C.; Michelson, P. F.; Minuti, M.; Mirizzi, N.; Mitra, P.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Mongelli, M.; Monte, C.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nelson, D.; Nilsson, L.; Nishino, S.; Nolan, P. L.; Nuss, E.; Ohno, M.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paccagnella, A.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Picozza, P.; Pinchera, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Rapposelli, E.; Raynor, W.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Reyes, L. C.; Ritz, S.; Robinson, S.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sacchetti, A.; Sadrozinski, H. F. -W.; Saggini, N.; Sanchez, D.; Sander, A.; Sapozhnikov, L.; Saxton, O. H.; Saz Parkinson, P. M.; Sellerholm, A.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Stephens, T. E.; Strickman, M. S.; Strong, A. W.; Sugizaki, M.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Tenze, A.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Tibolla, O.; Torres, D. F.; Tosti, G.; Tramacere, A.; Turri, M.; Usher, T. L.; Vilchez, N.; Virmani, N.; Vitale, V.; Wai, L. L.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, D. L.; Wood, K. S.; Yasuda, H.; Ylinen, T.; Ziegler, M., The Large Area Telescope (LAT) on-board the Fermi Gamma-ray Space Telescope began its on-orbit operations on June 23, 2008. Calibrations, defined in a generic sense, correspond to synchronization of trigger signals, optimization of delays for latching data, determination of detector thresholds, gains and responses, evaluation of the perimeter of the South Atlantic Anomaly (SAA), measurements of live time, of absolute time, and internal and spacecraft boresight alignments. Here we describe on-orbit calibration results obtained using known astrophysical sources, galactic cosmic rays, and charge injection into the front-end electronics of each detector. Instrument response functions will be described in a separate publication. This paper demonstrates the stability of calibrations and describes minor changes observed since launch. These results have been used to calibrate the LAT datasets to be publicly released in August 2009....
Astroparticle Physics, Oct. 2009

Fermi LAT Observation of Diffuse Gamma Rays Produced Through Interactions Between Local Interstellar Matter and High-energy Cosmic Rays
Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carlson, P.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Cheung, C. C.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Cutini, S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocian, M. L.; Kuehn, F.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Mazziotta, M. N.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Pohl, M.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Schalk, T. L.; Sellerholm, A.; Sgrò, C.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Stecker, F. W.; Strickman, M. S.; Strong, A. W.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M., Observations by the Large Area Telescope (LAT) on the Fermi mission of diffuse γ-rays in a mid-latitude region in the third quadrant (Galactic longitude l from 200° to 260° and latitude |b| from 22° to 60°) are reported. The region contains no known large molecular cloud and most of the atomic hydrogen is within 1 kpc of the solar system. The contributions of γ-ray point sources and inverse Compton scattering are estimated and subtracted. The residual γ-ray intensity exhibits a linear correlation with the atomic gas column density in energy from 100 MeV to 10 GeV. The measured integrated γ-ray emissivity is (1.63 ± 0.05) × 10^-26 photons s^-1sr^-1 H-atom^-1 and (0.66 ± 0.02) × 10^-26 photons s^-1sr^-1 H-atom^-1 above 100 MeV and above 300 MeV, respectively, with an additional systematic error of ~10%. The differential emissivity from 100 MeV to 10 GeV agrees with calculations based on cosmic ray spectra consistent with those directly measured, at the 10% level. The results obtained indicate that cosmic ray nuclei spectra within 1 kpc from the solar system in regions studied are close to the local interstellar spectra inferred from direct measurements at the Earth within ~10%....
The Astrophysical Journal, Oct. 2009

CANGAROO-III Observation of TeV Gamma Rays from the Vicinity of PSR B1706-44
Enomoto, R.; Kushida, J.; Nakamori, T.; Kifune, T.; Bicknell, G. V.; Clay, R. W.; Edwards, P. G.; Gunji, S.; Hara, S.; Hara, T.; Hattori, T.; Hayashi, S.; Higashi, Y.; Hirai, Y.; Inoue, K.; Ishioka, H.; Kabuki, S.; Kajino, F.; Katagiri, H.; Kawachi, A.; Kiuchi, R.; Kubo, H.; Kunisawa, T.; Matoba, T.; Matsubara, Y.; Matsuzawa, I.; Mizukami, T.; Mizumura, Y.; Mizumoto, Y.; Mori, M.; Muraishi, H.; Naito, T.; Nakano, S.; Nishijima, K.; Ohishi, M.; Otake, Y.; Ryoki, S.; Saito, K.; Sakamoto, Y.; Seki, A.; Stamatescu, V.; Suzuki, T.; Swaby, D. L.; Tanimori, T.; Thornton, G.; Tokanai, F.; Tsuchiya, K.; Watanabe, S.; Yamazaki, E.; Yanagita, S.; Yoshida, T.; Yoshikoshi, T.; Yukawa, Y., Observation by the CANGAROO-III stereoscopic system of the Imaging Cherenkov Telescope has detected extended emission of TeV gamma rays in the vicinity of the pulsar PSR B1706-44. The strength of the signal observed as gamma-ray-like events varies when we apply different ways of emulating background events. The reason for such uncertainties is argued in relevance to gamma rays embedded in the "OFF-source data," that is, unknown sources and diffuse emission in the Galactic plane, namely, the existence of a complex structure of TeV gamma-ray emission around PSR B1706-44....
The Astrophysical Journal, Oct. 2009

CANGAROO-III Search for TeV Gamma Rays from Two Clusters of Galaxies
Kiuchi, R.; Mori, M.; Bicknell, G. V.; Clay, R. W.; Edwards, P. G.; Enomoto, R.; Gunji, S.; Hara, S.; Hara, T.; Hattori, T.; Hayashi, S.; Higashi, Y.; Hirai, Y.; Inoue, K.; Itoh, C.; Kabuki, S.; Kajino, F.; Katagiri, H.; Kawachi, A.; Kifune, T.; Kubo, H.; Kushida, J.; Matsubara, Y.; Mizukami, T.; Mizumoto, Y.; Mizuniwa, R.; Muraishi, H.; Muraki, Y.; Naito, T.; Nakamori, T.; Nakano, S.; Nishida, D.; Nishijima, K.; Ohishi, M.; Sakamoto, Y.; Seki, A.; Stamatescu, V.; Suzuki, T.; Swaby, D. L.; Tanimori, T.; Thornton, G.; Tokanai, F.; Tsuchiya, K.; Watanabe, S.; Yamada, Y.; Yamazaki, E.; Yanagita, S.; Yoshida, T.; Yoshikoshi, T.; Yukawa, Y., Because accretion and merger shocks in clusters of galaxies may accelerate particles to high energies, clusters are candidate sites for the origin of ultra-high-energy (UHE) cosmic rays. A prediction was presented for gamma-ray emission from a cluster of galaxies at a detectable level with the current generation of imaging atmospheric Cherenkov telescopes. The gamma-ray emission was produced via inverse Compton upscattering of cosmic microwave background photons by electron-positron pairs generated by collisions of UHE cosmic rays in the cluster. We observed two clusters of galaxies, Abell 3667 and Abell 4038, searching for very high energy gamma-ray emission with the CANGAROO-III atmospheric Cherenkov telescope system in 2006. The analysis showed no significant excess around these clusters, yielding upper limits on the gamma-ray emission. From a comparison of the upper limit for the northwest radio relic region of Abell 3667 with a model prediction, we derive a lower limit for the magnetic field of the region of ~0.1 μG. This shows the potential of gamma-ray observations in studies of the cluster environment. We also discuss the flux upper limit from cluster center regions using a model of gamma-ray emission from neutral pions produced in hadronic collisions of cosmic-ray protons with the intracluster medium. The derived upper limit of the cosmic-ray energy density within this framework is an order of magnitude higher than that of our Galaxy....
The Astrophysical Journal, Oct. 2009

Optical and Near-Infrared Photometric Observation during the Superoutburst of the WZ Sge-Type Dwarf Nova, V455 Andromedae
Risako Matsui; Makoto Uemura; Akira Arai; Mahito Sasada; Takashi Ohsugi; Takuya Yamashita; Koji Kawabata; Yasushi Fukazawa; Tsumefumi Mizuno; Hideaki Katagiri; Hiromitsu Takahashi; Shuji Sato; Masaru Kino; Michitoshi Yoshida; Yasuhiro Shimizu; Shogo Nagayama; Kenshi Yanagisawa; Hiroyuki Toda; Kiichi Okita; Nobuyuki Kawai, We report on optical and infrared photometric observations of a WZ Sge-type dwarf nova, V455 And during a superoutburst in 2007. These observations were performed with the KANATA (V, J, and K-s bands) and MITSuME (g', R-C, and I-C bands) telescopes. Our 6-band simultaneous observations allowed us to investigate the temporal variation of the temperature and the size of the emitting region associated with the superoutburst and short-term modulations, Such as early and ordinary superhumps. A hot (> 11000 K) accretion disk suddenly disappeared when the superoutburst finished, while blackbody emission, probably from the disk, still remained dominant in the optical region with a moderately high temperature (similar to 8000 K). This indicates that a substantial amount of gas was stored in the disk even after the outburst. This remnant matter may be a sign of an expected mass-reservoir, which can trigger echo outbursts observed in several WZ Sge stars. The color variation associated with superhumps indicates that viscous heating in a superhump source stopped on the way to the superhump maximum, and a subsequent expansion of a low-temperature region made the maximum. The color variation of early superhumps was totally different from that of superhumps: the object was bluest at the early superhump minimum. The temperature of the early superhump light source was lower than that of an underlying component, indicating that the early superhump light source was a vertically expanded low-temperature region at the outermost part of the disk., OXFORD UNIV PRESS
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Oct. 2009, [Reviewed]

Search for VHE gamma rays from SS433/W50 with the CANGAROO-II telescope
Hayashi, Sei.; Kajino, F.; Naito, T.; Asahara, A.; Bicknell, G. V.; Clay, R. W.; Doi, Y.; Edwards, P. G.; Enomoto, R.; Gunji, S.; Hara, S.; Hara, T.; Hattori, T.; Itoh, C.; Kabuki, S.; Katagiri, H.; Kawachi, A.; Kifune, T.; Ksenofontov, L. T.; Kubo, H.; Kurihara, T.; Kurosaka, R.; Kushida, J.; Matsubara, Y.; Miyashita, Y.; Mizumoto, Y.; Mori, M.; Mori, H.; Muraishi, H.; Muraki, Y.; Nakase, T.; Nishida, D.; Nishijima, K.; Ohishi, M.; Okumura, K.; Patterson, J. R.; Protheroe, R. J.; Sakamoto, N.; Sakurazawa, K.; Swaby, D. L.; Tanimori, T.; Tanimura, H.; Thornton, G.; Tokanai, F.; Tsuchiya, K.; Uchida, T.; Watanabe, S.; Yamaoka, T.; Yanagita, S.; Yoshida, T.; Yoshikoshi, T., SS433, located at the center of the supernova remnant W50, is a close proximity binary system consisting of a compact star and a normal star. Jets of material are directed outwards from the vicinity of the compact star symmetrically to the east and west. Non-thermal hard X-ray emission is detected from lobes lying on both sides. Shock accelerated electrons are expected to generate VHE gamma rays through the inverse-Compton process in the lobes. Observations of the western X-ray lobe region of SS433/W50 system have been performed to detect VHE gamma rays using the 10 m CANGAROO-II telescope in August and September, 2001, and July and September, 2002. The total observation times are 85.2 h for ON source, and 80.8 h for OFF source data. No significant excess of VHE gamma rays has been found at three regions of the western X-ray lobe of SS433/W50 system. We have derived 99% confidence level upper limits to the fluxes of gamma rays and have set constraints on the strengths of the magnetic fields assuming the synchrotron/inverse-Compton model for the wide energy range of photon spectrum from radio to TeV. The derived lower limits are 4.3μG for the center of the brightest X-ray emission region and 6.3μG for the far end from SS433 in the western X-ray lobe. In addition, we suggest that the spot-like X-ray emission may provide a major contribution to the hardest X-ray spectrum in the lobe....
Astroparticle Physics, Sep. 2009

Pulsed Gamma-rays from PSR J2021+3651 with the Fermi Large Area Telescope
Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Battelino, M.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bloom, E. D.; Bogaert, G.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Camilo, F.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Charles, E.; Chekhtman, A.; Chen, A. W.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Cognard, I.; Cohen-Tanugi, J.; Cominsky, L. R.; Conrad, J.; Cutini, S.; Demorest, P.; Dermer, C. D.; de Angelis, A.; de Luca, A.; de Palma, F.; Digel, S. W.; Dormody, M.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Dumora, D.; Espinoza, C.; Farnier, C.; Favuzzi, C.; Focke, W. B.; Frailis, M.; Freire, P. C. C.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Johnston, S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Kiziltan, B.; Knödlseder, J.; Komin, N.; Kramer, M.; Kuehn, F.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Lyne, A. G.; Makeev, A.; Manchester, R. N.; Marelli, M.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; McLaughlin, M. A.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Noutsos, A.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Ransom, S. M.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Parkinson, P. M. Saz; Sgrò, C.; Sierpowska-Bartosik, A.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stappers, B. W.; Starck, J. -L.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Theureau, G.; Thompson, D. J.; Thorsett, S. E.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Van Etten, A.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wallace, E.; Watters, K.; Weltevrede, P.; Wood, K. S.; Ylinen, T.; Ziegler, M., We report the detection of pulsed gamma-rays from the young, spin-powered radio pulsar PSR J2021+3651 using data acquired with the Large Area Telescope (LAT) on the Fermi Gamma-ray Space Telescope (formerly GLAST). The light curve consists of two narrow peaks of similar amplitude separated by 0.468 ± 0.002 in phase. The first peak lags the maximum of the 2 GHz radio pulse by 0.162 ± 0.004 ± 0.01 in phase. The integral gamma-ray photon flux above 100 MeV is (56 ± 3 ± 11) × 10^-8 cm^-2 s^-1. The photon spectrum is well described by an exponentially cut-off power law of the form {dF \over dE} = kE^{-Γ} e^{(-E/E_c)}, where the energy E is expressed in GeV. The photon index is Γ = 1.5 ± 0.1 ± 0.1 and the exponential cut-off is E_c = 2.4 ± 0.3 ± 0.5 GeV. The first uncertainty is statistical and the second is systematic. The integral photon flux of the bridge is approximately 10% of the pulsed emission, and the upper limit on off-pulse gamma-ray emission from a putative pulsar wind nebula is < 10% of the pulsed emission at the 95% confidence level. Radio polarization measurements yield a rotation measure of RM = 524 ± 4 rad m^-2 but a poorly constrained magnetic geometry. Re-analysis of Chandra X-ray Observatory data enhanced the significance of the weak X-ray pulsations, and the first peak is roughly phase aligned with the first gamma-ray peak. We discuss the emission region and beaming geometry based on the shape and spectrum of the gamma-ray light curve combined with radio and X-ray measurements, and the implications for the pulsar distance. Gamma-ray emission from the polar cap region seems unlikely for this pulsar....
The Astrophysical Journal, Aug. 2009

Fermi LAT Observations of LS I +61°303: First Detection of an Orbital Modulation in GeV Gamma Rays
Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chaty, S.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cominsky, L. R.; Conrad, J.; Corbel, S.; Corbet, R.; Cutini, S.; Dermer, C. D.; de Angelis, A.; de Luca, A.; de Palma, F.; Digel, S. W.; Dormody, M.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Dubus, G.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Hill, A. B.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocian, M. L.; Kuehn, F.; Kuss, M.; Lande, J.; Larsson, S.; Latronico, L.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Marelli, M.; Mazziotta, M. N.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Ray, P. S.; Razzano, M.; Rea, N.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Sgrò, C.; Shaw, M. S.; Sierpowska-Bartosik, A.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Striani, E.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M., This Letter presents the first results from the observations of LS I +61°303 using Large Area Telescope data from the Fermi Gamma-Ray Space Telescope between 2008 August and 2009 March. Our results indicate variability that is consistent with the binary period, with the emission being modulated at 26.6 ± 0.5 days. This constitutes the first detection of orbital periodicity in high-energy gamma rays (20 MeV-100 GeV, HE). The light curve is characterized by a broad peak after periastron, as well as a smaller peak just before apastron. The spectrum is best represented by a power law with an exponential cutoff, yielding an overall flux above 100 MeV of 0.82 ± 0.03(stat) ± 0.07(syst) 10^-6 ph cm^-2 s^-1, with a cutoff at 6.3 ± 1.1(stat) ± 0.4(syst) GeV and photon index Γ = 2.21 ± 0.04(stat) ± 0.06(syst). There is no significant spectral change with orbital phase. The phase of maximum emission, close to periastron, hints at inverse Compton scattering as the main radiation mechanism. However, previous very high-energy gamma ray (>100 GeV, VHE) observations by MAGIC and VERITAS show peak emission close to apastron. This and the energy cutoff seen with Fermi suggest that the link between HE and VHE gamma rays is nontrivial....
The Astrophysical Journal, Aug. 2009

Detection of 16 Gamma-Ray Pulsars Through Blind Frequency Searches Using the Fermi LAT
Abdo, A. A.; Ackermann, M.; Ajello, M.; Anderson, B.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bignami, G. F.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Cutini, S.; Dermer, C. D.; de Angelis, A.; de Luca, A.; de Palma, F.; Digel, S. W.; Dormody, M.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giommi, P.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Gwon, C.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Hughes, R. E.; Jóhannesson, G.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocian, M. L.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Marelli, M.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Porter, T. A.; Primack, J. R.; Rainò, S.; Rando, R.; Ray, P. S.; Razzano, M.; Rea, N.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Parkinson, P. M. Saz; Scargle, J. D.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Tibolla, O.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Van Etten, A.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Watters, K.; Winer, B. L.; Wolff, M. T.; Wood, K. S.; Ylinen, T.; Ziegler, M.; Fermi LAT Collaboration, Pulsars are rapidly rotating, highly magnetized neutron stars emitting radiation across the electromagnetic spectrum. Although there are more than 1800 known radio pulsars, until recently only seven were observed to pulse in gamma rays, and these were all discovered at other wavelengths. The Fermi Large Area Telescope (LAT) makes it possible to pinpoint neutron stars through their gamma-ray pulsations. We report the detection of 16 gamma-ray pulsars in blind frequency searches using the LAT. Most of these pulsars are coincident with previously unidentified gamma-ray sources, and many are associated with supernova remnants. Direct detection of gamma-ray pulsars enables studies of emission mechanisms, population statistics, and the energetics of pulsar wind nebulae and supernova remnants....
Science, Aug. 2009

Detection of High-Energy Gamma-Ray Emission from the Globular Cluster 47 Tucanae with Fermi
Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chaty, S.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Cutini, S.; Dermer, C. D.; de Palma, F.; Digel, S. W.; Dormody, M.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Frailis, M.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Horan, D.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kuehn, F.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pierbattista, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Rea, N.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Sgrò, C.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Wang, P.; Webb, N.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M., We report the detection of gamma-ray emissions above 200 megaelectron volts at a significance level of 17σ from the globular cluster 47 Tucanae, using data obtained with the Large Area Telescope onboard the Fermi Gamma-ray Space Telescope. Globular clusters are expected to emit gamma rays because of the large populations of millisecond pulsars that they contain. The spectral shape of 47 Tucanae is consistent with gamma-ray emission from a population of millisecond pulsars. The observed gamma-ray luminosity implies an upper limit of 60 millisecond pulsars present in 47 Tucanae....
Science, Aug. 2009

A Population of Gamma-Ray Millisecond Pulsars Seen with the Fermi Large Area Telescope
Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bignami, G. F.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Camilo, F.; Caraveo, P. A.; Carlson, P.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cognard, I.; Cohen-Tanugi, J.; Cominsky, L. R.; Conrad, J.; Corbet, R.; Cutini, S.; Dermer, C. D.; Desvignes, G.; de Angelis, A.; de Luca, A.; de Palma, F.; Digel, S. W.; Dormody, M.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Dumora, D.; Edmonds, Y.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Frailis, M.; Freire, P. C. C.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Hobbs, G.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Johnston, S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocian, M. L.; Kramer, M.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Manchester, R. N.; Marelli, M.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; McLaughlin, M. A.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Ransom, S. M.; Ray, P. S.; Razzano, M.; Rea, N.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Schalk, T. L.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stappers, B. W.; Starck, J. L.; Striani, E.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Theureau, G.; Thompson, D. J.; Thorsett, S. E.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Van Etten, A.; Vasileiou, V.; Venter, C.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wallace, E.; Wang, P.; Watters, K.; Webb, N.; Weltevrede, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M., Pulsars are born with subsecond spin periods and slow by electromagnetic braking for several tens of millions of years, when detectable radiation ceases. A second life can occur for neutron stars in binary systems. They can acquire mass and angular momentum from their companions, to be spun up to millisecond periods and begin radiating again. We searched Fermi Large Area Telescope data for pulsations from all known millisecond pulsars (MSPs) outside of globular clusters, using rotation parameters from radio telescopes. Strong gamma-ray pulsations were detected for eight MSPs. The gamma-ray pulse profiles and spectral properties resemble those of young gamma-ray pulsars. The basic emission mechanism seems to be the same for MSPs and young pulsars, with the emission originating in regions far from the neutron star surface....
Science, Aug. 2009

Fermi Discovery of Gamma-ray Emission from NGC 1275
Abdo, A. A.; Ackermann, M.; Ajello, M.; Asano, K.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Celotti, A.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Colafrancesco, S.; Cominsky, L. R.; Conrad, J.; Costamante, L.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Donato, D.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Finke, J.; Focke, W. B.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Georganopoulos, M.; Germani, S.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hartman, R. C.; Hayashida, M.; Hays, E.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, W. N.; Kadler, M.; Kamae, T.; Kanai, Y.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kuehn, F.; Kuss, M.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Mazziotta, M. N.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J. H.; Parent, D.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rodriguez, A. Y.; Romani, R. W.; Ryde, F.; Sadrozinski, H. F. -W.; Sambruna, R.; Sanchez, D.; Sander, A.; Sato, R.; Parkinson, P. M. Saz; Sgrò, C.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Strickman, M. S.; Strong, A. W.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Taylor, G. B.; Thayer, J. G.; Thompson, D. J.; Torres, D. F.; Tosti, G.; Uchiyama, Y.; Usher, T. L.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wood, K. S.; Ylinen, T.; Ziegler, M.; Aller, H. D.; Aller, M. F.; Kellermann, K. I.; Kovalev, Y. Y.; Kovalev, Yu. A.; Lister, M. L.; Pushkarev, A. B., We report the discovery of high-energy (E > 100 MeV) γ-ray emission from NGC 1275, a giant elliptical galaxy lying at the center of the Perseus cluster of galaxies, based on observations made with the Large Area Telescope (LAT) of the Fermi Gamma-ray Space Telescope. The positional center of the γ-ray source is only ≈3' away from the NGC 1275 nucleus, well within the 95% LAT error circle of ≈5'. The spatial distribution of γ-ray photons is consistent with a point source. The average flux and power-law photon index measured with the LAT from 2008 August 4 to 2008 December 5 are F _γ = (2.10 ± 0.23) × 10^-7 ph (>100 MeV) cm^-2 s^-1 and Γ = 2.17 ± 0.05, respectively. The measurements are statistically consistent with constant flux during the four-month LAT observing period. Previous EGRET observations gave an upper limit of F _γ < 3.72 × 10^-8 ph (>100 MeV) cm^-2 s^-1 to the γ-ray flux from NGC 1275. This indicates that the source is variable on timescales of years to decades, and therefore restricts the fraction of emission that can be produced in extended regions of the galaxy cluster. Contemporaneous and historical radio observations are also reported. The broadband spectrum of NGC 1275 is modeled with a simple one-zone synchrotron/synchrotron self-Compton model and a model with a decelerating jet flow....
The Astrophysical Journal, Jul. 2009

Early Fermi Gamma-ray Space Telescope Observations of the Quasar 3C 454.3
Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Battelino, M.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Charles, E.; Chaty, S.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cominsky, L. R.; Conrad, J.; Costamante, L.; Cutini, S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Silva, E. do Couto e.; Donato, D.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Focke, W. B.; Foschini, L.; Frailis, M.; Fuhrmann, L.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giommi, P.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hartman, R. C.; Hayashida, M.; Hays, E.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocian, M. L.; Kuehn, F.; Kuss, M.; Latronico, L.; Lee, S. -H.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Massaro, E.; Mazziotta, M. N.; McEnery, J. E.; McGlynn, S.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Reyes, L. C.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Rahoui, F.; Ryde, F.; Sadrozinski, H. F. -W.; Sambruna, R.; Sanchez, D.; Sander, A.; Parkinson, P. M. Saz; Sgrò, C.; Shaw, M. S.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vilchez, N.; Villata, M.; Vitale, V.; Waite, A. P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Zensus, J. A.; Ziegler, M., This is the first report of Fermi Gamma-Ray Space Telescope observations of the quasar 3C 454.3, which has been undergoing pronounced long-term outbursts since 2000. The data from the Large Area Telescope, covering 2008 July 7-October 6, indicate strong, highly variable γ-ray emission with an average flux of ~3 × 10^-6 photons cm^-2 s^-1, for energies >100 MeV. The γ-ray flux is variable, with strong, distinct, symmetrically shaped flares for which the flux increases by a factor of several on a timescale of about 3 days. This variability indicates a compact emission region, and the requirement that the source is optically thin to pair production implies relativistic beaming with Doppler factor δ>8, consistent with the values inferred from Very Long Baseline Interferometry observations of superluminal expansion (δ ~ 25). The observed γ-ray spectrum is not consistent with a simple power law, but instead steepens strongly above ~2 GeV, and is well described by a broken power law with photon indices of ~2.3 and ~3.5 below and above the break, respectively. This is the first direct observation of a break in the spectrum of a high-luminosity blazar above 100 MeV, and it is likely direct evidence for an intrinsic break in the energy distribution of the radiating particles. Alternatively, the spectral softening above 2 GeV could be due to γ-ray absorption via photon-photon pair production on the soft X-ray photon field of the host active galactic nucleus, but such an interpretation would require the dissipation region to be located very close (lsim100 gravitational radii) to the black hole, which would be inconsistent with the X-ray spectrum of the source....
The Astrophysical Journal, Jul. 2009

Fermi/Large Area Telescope Discovery of Gamma-Ray Emission from a Relativistic Jet in the Narrow-Line Quasar PMN J0948+0022
Abdo, A. A.; Ackermann, M.; Ajello, M.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Battelino, M.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Collmar, W.; Conrad, J.; Costamante, L.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Focke, W. B.; Foschini, L.; Frailis, M.; Fuhrmann, L.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hartman, R. C.; Hayashida, M.; Hays, E.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kerr, M.; Knödlseder, J.; Kuehn, F.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Max-Moerbeck, W.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J. H.; Parent, D.; Pavlidou, V.; Pearson, T. J.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Readhead, A.; Reimer, A.; Reimer, O.; Reposeur, T.; Richards, J. L.; Ritz, S.; Rodriguez, A. Y.; Romani, R. W.; Ryde, F.; Sadrozinski, H. F. -W.; Sambruna, R.; Sanchez, D.; Sander, A.; Parkinson, P. M. Saz; Scargle, J. D.; Schalk, T. L.; Sgrò, C.; Smith, D. A.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Stevenson, M.; Strickman, M. S.; Suson, D. J.; Tagliaferri, G.; Takahashi, H.; Tanaka, T.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Tibolla, O.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vilchez, N.; Vitale, V.; Waite, A. P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Zensus, J. A.; Ziegler, M.; Fermi/LAT Collaboration; Ghisellini, G.; Maraschi, L.; Tavecchio, F.; Angelakis, E., We report the discovery by the Large Area Telescope (LAT) onboard the Fermi Gamma-Ray Space Telescope of high-energy γ-ray emission from the peculiar quasar PMN J0948+0022 (z = 0.5846). The optical spectrum of this object exhibits rather narrow Hβ (FWHM(Hβ) ~1500 km s^-1), weak forbidden lines, and is therefore classified as a narrow-line type I quasar. This class of objects is thought to have relatively small black hole mass and to accrete at a high Eddington ratio. The radio loudness and variability of the compact radio core indicate the presence of a relativistic jet. Quasi-simultaneous radio/optical/X-ray and γ-ray observations are presented. Both radio and γ-ray emissions (observed over five months) are strongly variable. The simultaneous optical and X-ray data from Swift show a blue continuum attributed to the accretion disk and a hard X-ray spectrum attributed to the jet. The resulting broadband spectral energy distribution (SED) and, in particular, the γ-ray spectrum measured by Fermi are similar to those of more powerful Flat-Spectrum Radio Quasars (FSRQs). A comparison of the radio and γ-ray characteristics of PMN J0948+0022 with the other blazars detected by LAT shows that this source has a relatively low radio and γ-ray power with respect to other FSRQs. The physical parameters obtained from modeling the SED also fall at the low power end of the FSRQ parameter region discussed in Celotti & Ghisellini. We suggest that the similarity of the SED of PMN J0948+0022 to that of more massive and more powerful quasars can be understood in a scenario in which the SED properties depend on the Eddington ratio rather than on the absolute power....
The Astrophysical Journal, Jul. 2009

Pulsed Gamma Rays from the Millisecond Pulsar J0030+0451 with the Fermi Large Area Telescope
Abdo, A. A.; Ackermann, M.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Battelino, M.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cognard, I.; Cohen-Tanugi, J.; Cominsky, L. R.; Conrad, J.; Cutini, S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Dormody, M.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Focke, W. B.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocian, M. L.; Komin, N.; Kuehn, F.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Marelli, M.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Pancrazi, B.; Paneque, D.; Panetta, J. H.; Parent, D.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Parkinson, P. M. Saz; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Theureau, G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Van Etten, A.; Vilchez, N.; Vitale, V.; Waite, A. P.; Watters, K.; Webb, N.; Wood, K. S.; Ylinen, T.; Ziegler, M., We report the discovery of gamma-ray pulsations from the nearby isolated millisecond pulsar (MSP) PSR J0030+0451 with the Large Area Telescope on the Fermi Gamma-ray Space Telescope (formerly GLAST). This discovery makes PSR J0030+0451 the second MSP to be detected in gamma rays after PSR J0218+4232, observed by the EGRET instrument on the Compton Gamma-Ray Observatory. The spin-down power \dot{E} = 3.5 × 10^{33} erg s^-1 is an order of magnitude lower than the empirical lower bound of previously known gamma-ray pulsars. The emission profile is characterized by two narrow peaks, 0.07 ± 0.01 and 0.08 ± 0.02 wide, respectively, separated by 0.44 ± 0.02 in phase. The first gamma-ray peak falls 0.15 ± 0.01 after the main radio peak. The pulse shape is similar to that of the "normal" gamma-ray pulsars. An exponentially cutoff power-law fit of the emission spectrum leads to an integral photon flux above 100 MeV of (6.76 ± 1.05 ± 1.35) × 10^-8 cm^-2 s^-1 with cutoff energy (1.7 ± 0.4 ± 0.5) GeV. Based on its parallax distance of (300 ± 90) pc, we obtain a gamma-ray efficiency L_γ/ \dot{E} ≃ 15% for the conversion of spin-down energy rate into gamma-ray radiation, assuming isotropic emission....
The Astrophysical Journal, Jul. 2009

Fermi/Large Area Telescope Bright Gamma-Ray Source List
Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Band, D. L.; Barbiellini, G.; Bastieri, D.; Battelino, M.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bignami, G. F.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cominsky, L. R.; Conrad, J.; Corbet, R.; Costamante, L.; Cutini, S.; Davis, D. S.; Dermer, C. D.; de Angelis, A.; de Luca, A.; de Palma, F.; Digel, S. W.; Dormody, M.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Focke, W. B.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giommi, P.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hartman, R. C.; Hayashida, M.; Hays, E.; Healey, S. E.; Horan, D.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocevski, D.; Kocian, M. L.; Komin, N.; Kuehn, F.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Marelli, M.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; McGlynn, S.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Poupard, L.; Rainò, S.; Rando, R.; Ray, P. S.; Razzano, M.; Rea, N.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Schalk, T. L.; Sellerholm, A.; Sgrò, C.; Shaw, M. S.; Shrader, C.; Sierpowska-Bartosik, A.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Stephens, T. E.; Strickman, M. S.; Strong, A. W.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Tibolla, O.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Van Etten, A.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wallace, E.; Wang, P.; Watters, K.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M.; Fermi/LAT Collaboration, Following its launch in 2008 June, the Fermi Gamma-ray Space Telescope (Fermi) began a sky survey in August. The Large Area Telescope (LAT) on Fermi in three months produced a deeper and better resolved map of the γ-ray sky than any previous space mission. We present here initial results for energies above 100 MeV for the 205 most significant (statistical significance greater than ~10σ) γ-ray sources in these data. These are the best characterized and best localized point-like (i.e., spatially unresolved) γ-ray sources in the early mission data....
The Astrophysical Journal Supplement Series, Jul. 2009

Discovery of Pulsations from the Pulsar J0205+6449 in SNR 3C 58 with the Fermi Gamma-Ray Space Telescope
Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Camilo, F.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cognard, I.; Cohen-Tanugi, J.; Conrad, J.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Dormody, M.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Dumora, D.; Edmonds, Y.; Espinoza, C.; Farnier, C.; Favuzzi, C.; Focke, W. B.; Frailis, M.; Freire, P. C. C.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Hobbs, G.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Johnston, S.; Kamae, T.; Kaspi, V. M.; Katagiri, H.; Kataoka, J.; Kawai, N.; Keith, M.; Kerr, M.; Knödlseder, J.; Kramer, M.; Kuehn, F.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Livingstone, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Lyne, A. G.; Makeev, A.; Manchester, R. N.; Marelli, M.; Mazziotta, M. N.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Ransom, S. M.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stappers, B. W.; Striani, E.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Theureau, G.; Thompson, D. J.; Thorsett, S. E.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Van Etten, A.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Watters, K.; Weltevrede, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M., We report the discovery of γ-ray pulsations (>=0.1 GeV) from the young radio and X-ray pulsar PSR J0205 + 6449 located in the Galactic supernova remnant 3C 58. Data in the γ-ray band were acquired by the Large Area Telescope aboard the Fermi Gamma-ray Space Telescope (formerly GLAST), while the radio rotational ephemeris used to fold γ-rays was obtained using both the Green Bank Telescope and the Lovell telescope at Jodrell Bank. The light curve consists of two peaks separated by 0.49 ± 0.01 ± 0.01 cycles which are aligned with the X-ray peaks. The first γ-ray peak trails the radio pulse by 0.08 ± 0.01 ± 0.01, while its amplitude decreases with increasing energy as for the other γ-ray pulsars. Spectral analysis of the pulsed γ-ray emission suggests a simple power law of index -2.1 ± 0.1 ± 0.2 with an exponential cutoff at 3.0^+1.1 _-0.7 ± 0.4 GeV. The first uncertainty is statistical and the second is systematic. The integral γ-ray photon flux above 0.1 GeV is (13.7 ± 1.4 ± 3.0) × 10^-8 cm^-2 s^-1, which implies for a distance of 3.2 kpc and assuming a broad fan-like beam a luminosity of 8.3 × 10³⁴ erg s^-1 and an efficiency η of 0.3%. Finally, we report a 95% upper limit on the flux of 1.7 × 10^-8 cm^-2 s^-1 for off-pulse emission from the object....
The Astrophysical Journal, Jul. 2009

Bright Active Galactic Nuclei Source List from the First Three Months of the Fermi Large Area Telescope All-Sky Survey
Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Charles, E.; Chekhtman, A.; Chen, A. W.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Colafrancesco, S.; Collmar, W.; Cominsky, L. R.; Conrad, J.; Costamante, L.; Cutini, S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Finke, J.; Focke, W. B.; Foschini, L.; Frailis, M.; Fuhrmann, L.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hartman, R. C.; Hayashida, M.; Hays, E.; Healey, S. E.; Horan, D.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Kadler, M.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kerr, M.; Knödlseder, J.; Kocian, M. L.; Kuehn, F.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Massaro, E.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; McGlynn, S.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Razzaque, S.; Reimer, A.; Reimer, O.; Reposeur, T.; Reyes, L. C.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Schalk, T. L.; Sellerholm, A.; Sgrò, C.; Shaw, M. S.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Taylor, G. B.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vilchez, N.; Villata, M.; Vitale, V.; Waite, A. P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M., The first three months of sky-survey operation with the Large Area Telescope (LAT) onboard the Fermi Gamma-Ray Space Telescope reveal 132 bright sources at |b|>10° with test statistic greater than 100 (corresponding to about 10σ). Two methods, based on the CGRaBS, CRATES, and BZCat catalogs, indicate high-confidence associations of 106 of these sources with known active galactic nuclei (AGNs). This sample is referred to as the LAT Bright AGN Sample (LBAS). It contains two radio galaxies, namely, Centaurus A and NGC 1275, and 104 blazars consisting of 58 flat spectrum radio quasars (FSRQs), 42 BL Lac objects, and 4 blazars with unknown classification. Four new blazars were discovered on the basis of the LAT detections. Remarkably, the LBAS includes 10 high-energy-peaked BL Lacs (HBLs), sources which were previously difficult to detect in the GeV range. Another 10 lower-confidence associations are found. Only 33 of the sources, plus two at |b| < 10°, were previously detected with Energetic Gamma-Ray Experiment Telescope(EGRET), probably due to variability. The analysis of the γ-ray properties of the LBAS sources reveals that the average GeV spectra of BL Lac objects are significantly harder than the spectra of FSRQs. No significant correlation between radio and peak γ-ray fluxes is observed. Blazar log N-log S distributions and luminosity functions are constructed to investigate the evolution of the different blazar classes, with positive evolution indicated for FSRQs but none for BL Lacs. The contribution of LAT blazars to the total extragalactic γ-ray intensity is estimated....
The Astrophysical Journal, Jul. 2009

Anti-Correlation of Near-Infrared and X-Ray Variations of the Microquasar GRS 1915+105 in the Soft State
Arai Akira; Uemura Makoto; Sasada Mahito; TRUSHKIN Sergei A.; UEDA Yoshihiro; TAKAHASHI Hiromitsu; KAWABATA Koji S.; YAMANAKA Masayuki; NAGAE Osamu; IKEJIRI Yuki; SAKIMOTO Kiyoshi; MATSUI Risako; OHSUGI Takashi; YAMASHITA Takuya; ISOGAI Mizuki; FUKAZAWA Yasushi; MIZUNO Tsunefumi; KATAGIRI Hideaki; OKITA Kiichi; YOSHIDA Michitoshi; YANAGISAWA Kenshi; SATO Shuji; KINO Masaru; SADAKANE Kozo, We present detailed, long term near-infrared (NIR) light curves of GRS 1915+105 obtained in 2007-2008, covering its long "soft state" for the first time. From our NIR monitoring and X-ray data of the All Sky Monitor onboard Rossi X-ray Timing Explorer, we discovered that the NIR flux dropped by > 1 mag during short X-ray flares with a time-scale of days. Upon termination of the soft state, the H - K-s color reddened and the anti-correlation pattern was broken. The observed H - K-s color variation suggests that the dominant NIR source was an accretion disk during the soft state. The short X-ray flares during the soft state were associated with spectral hardening in X-rays and increasing radio emission, indicating jet ejection. The temporal NIR fading during the X-ray flares thus implies a sudden decrease in the contribution of the accretion disk when a jet is ejected., Astronomical Society of Japan
PASJ : publications of the Astronomical Society of Japan, 25 Jun. 2009, [Reviewed]

The large area telescope on the fermi gamma-ray space telescope mission
W.B. Atwood; A.A. Abdo; M. Ackermann; W. Althouse; B. Anderson; M. Axelsson; L. Baldini; J. Ballet; D.L. Band; G. Barbiellini; J. Bartelt; D. Bastieri; B.M. Baughman; K. Bechtol; D. Bédérède; F. Bellardi; R. Bellazzini; B. Berenji; G.F. Bignami; D. Bisello; E. Bissaldi; R.D. Blandford; E.D. Bloom; J.R. Bogart; E. Bonamente; J. Bonnell; A.W. Borgland; A. Bouvier; J. Bregeon; A. Brez; M. Brigida; P. Bruel; T.H. Burnett; G. Busetto; G.A. Caliandro; R.A. Cameron; P.A. Caraveo; S. Carius; P. Carlson; J.M. Casandjian; E. Cavazzuti; M. Ceccanti; C. Cecchi; E. Charles; A. Chekhtman; C.C. Cheung; J. Chiang; R. Chipaux; A.N. Cillis; S. Ciprini; R. Claus; J. Cohen-Tanugi; S. Condamoor; J. Conrad; R. Corbet; L. Corucci; L. Costamante; S. Cutini; D.S. Davis; D. Decotigny; M. Deklotz; C.D. Dermer; A. De Angelis; S.W. Digel; E. Do Couto E Silva; P.S. Drell; R. Dubois; D. Dumora; Y. Edmonds; D. Fabiani; C. Farnier; C. Favuzzi; D.L. Flath; P. Fleury; W.B. Focke; S. Funk; P. Fusco; F. Gargano; D. Gasparrini; N. Gehrels; F.-X. Gentit; S. Germani; B. Giebels; N. Giglietto; P. Giommi; F. Giordano; T. Glanzman; G. Godfrey; I.A. Grenier; M.-H. Grondin; J.E. Grove; L. Guillemot; S. Guiriec; G. Haller; A.K. Harding; P.A. Hart; E. Hays; S.E. Healey; M. Hirayama; L. Hjalmarsdotter; R. Horn; R.E. Hughes; G. Jóhannesson; G. Johansson; A.S. Johnson; R.P. Johnson; T.J. Johnson; W.N. Johnson; T. Kamae; H. Katagiri; J. Kataoka; A. Kavelaars; N. Kawai; H. Kelly; M. Kerr; W. Klamra; J. Knödlseder; M.L. Kocian; N. Komin; F. Kuehn; M. Kuss; D. Landriu; L. Latronico; B. Lee; S.-H. Lee; M. Lemoine-Goumard; A.M. Lionetto; F. Longo; F. Loparco; B. Lott; M.N. Lovellette; P. Lubrano; G.M. Madejski; A. Makeev; B. Marangelli; M.M. Massai; M.N. Mazziotta; J.E. McEnery; N. Menon; C. Meurer; P.F. Michelson; M. Minuti; N. Mirizzi; W. Mitthumsiri; T. Mizuno; A.A. Moiseev; C. Monte; M.E. Monzani; E. Moretti; A. Morselli; I.V. Moskalenko; S. Murgia; T. Nakamori; S. Nishino; P.L. Nolan; J.P. Norris; E. Nuss; M. Ohno; T. Ohsugi; N. Omodei; E. Orlando; J.F. Ormes; A. Paccagnella; D. Paneque; J.H. Panetta; D. Parent; M. Pearce; M. Pepe; A. Perazzo; M. Pesce-Rollins; P. Picozza; L. Pieri; M. Pinchera; F. Piron; T.A. Porter; L. Poupard; S. Rainò; R. Rando; E. Rapposelli; M. Razzano; A. Reimer; O. Reimer; T. Reposeur; L.C. Reyes; S. Ritz; L.S. Rochester; A.Y. Rodriguez; R.W. Romani; M. Roth; J.J. Russell; F. Ryde; S. Sabatini; H.F.-W. Sadrozinski; D. Sanchez; A. Sander; L. Sapozhnikov; P.M.S. Parkinson; J.D. Scargle; T.L. Schalk; G. Scolieri; C. Sgrò; G.H. Share; M. Shaw; T. Shimokawabe; C. Shrader; A. Sierpowska-Bartosik; E.J. Siskind; D.A. Smith; P.D. Smith; G. Spandre; P. Spinelli; J.-L. Starck; T.E. Stephens; M.S. Strickman; A.W. Strong; D.J. Suson; H. Tajima; H. Takahashi; T. Takahashi; T. Tanaka; A. Tenze; S. Tether; J.B. Thayer; J.G. Thayer; D.J. Thompson; L. Tibaldo; O. Tibolla; D.F. Torres; G. Tosti; A. Tramacere; M. Turri; T.L. Usher; N. Vilchez; V. Vitale; P. Wang; K. Watters; B.L. Wine, The Large Area Telescope (Fermi/LAT, hereafter LAT), the primary instrument on the Fermi Gamma-ray Space Telescope (Fermi) mission, is an imaging, wide field-of-view (FoV), high-energy γ-ray telescope, covering the energy range from below 20 MeV to more than 300 GeV. The LAT was built by an international collaboration with contributions from space agencies, high-energy particle physics institutes, and universities in France, Italy, Japan, Sweden, and the United States. This paper describes the LAT, its preflight expected performance, and summarizes the key science objectives that will be addressed. On-orbit performance will be presented in detail in a subsequent paper. The LAT is a pair-conversion telescope with a precision tracker and calorimeter, each consisting of a 4 × 4 array of 16 modules, a segmented anticoincidence detector that covers the tracker array, and a programmable trigger and data acquisition system. Each tracker module has a vertical stack of 18 (x, y) tracking planes, including two layers (x and y) of single-sided silicon strip detectors and high-Z converter material (tungsten) per tray. Every calorimeter module has 96 CsI(Tl) crystals, arranged in an eight-layer hodoscopic configuration with a total depth of 8.6 radiation lengths, giving both longitudinal and transverse information about the energy deposition pattern. The calorimeter's depth and segmentation enable the high-energy reach of the LAT and contribute significantly to background rejection. The aspect ratio of the tracker (height/width) is 0.4, allowing a large FoV (2.4 sr) and ensuring that most pair-conversion showers initiated in the tracker will pass into the calorimeter for energy measurement. Data obtained with the LAT are intended to (1) permit rapid notification of high-energy γ-ray bursts and transients and facilitate monitoring of variable sources, (2) yield an extensive catalog of several thousand high-energy sources obtained from an all-sky survey, (3) measure spectra from 20 MeV to more than 50 GeV for several hundred sources, (4) localize point sources to 0.3-2 arcmin, (5) map and obtain spectra of extended sources such as SNRs, molecular clouds, and nearby galaxies, (6) measure the diffuse isotropic γ-ray background up to TeV energies, and (7) explore the discovery space for dark matter. © 2009. The American Astronomical Society. All rights reserved.
Astrophysical Journal Letters, 01 Jun. 2009, [Reviewed]

Simultaneous Observations of PKS 2155-304 with HESS, Fermi, RXTE, and Atom: Spectral Energy Distributions and Variability in a Low State
Aharonian, F.; Akhperjanian, A. G.; Anton, G.; Barres de Almeida, U.; Bazer-Bachi, A. R.; Becherini, Y.; Behera, B.; Bernlöhr, K.; Boisson, C.; Bochow, A.; Borrel, V.; Brion, E.; Brucker, J.; Brun, P.; Bühler, R.; Bulik, T.; Büsching, I.; Boutelier, T.; Chadwick, P. M.; Charbonnier, A.; Chaves, R. C. G.; Cheesebrough, A.; Chounet, L. -M.; Clapson, A. C.; Coignet, G.; Dalton, M.; Daniel, M. K.; Davids, I. D.; Degrange, B.; Deil, C.; Dickinson, H. J.; Djannati-Ataï, A.; Domainko, W.; O'C. Drury, L.; Dubois, F.; Dubus, G.; Dyks, J.; Dyrda, M.; Egberts, K.; Emmanoulopoulos, D.; Espigat, P.; Farnier, C.; Feinstein, F.; Fiasson, A.; Förster, A.; Fontaine, G.; Füßling, M.; Gabici, S.; Gallant, Y. A.; Gérard, L.; Giebels, B.; Glicenstein, J. F.; Glück, B.; Goret, P.; Göhring, D.; Hauser, D.; Hauser, M.; Heinz, S.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hinton, J. A.; Hoffmann, A.; Hofmann, W.; Holleran, M.; Hoppe, S.; Horns, D.; Jacholkowska, A.; de Jager, O. C.; Jahn, C.; Jung, I.; Katarzyński, K.; Katz, U.; Kaufmann, S.; Kendziorra, E.; Kerschhaggl, M.; Khangulyan, D.; Khélifi, B.; Keogh, D.; Kluźniak, W.; Komin, Nu.; Kosack, K.; Lamanna, G.; Lenain, J. -P.; Lohse, T.; Marandon, V.; Martin, J. M.; Martineau-Huynh, O.; Marcowith, A.; Maurin, D.; McComb, T. J. L.; Medina, M. C.; Moderski, R.; Moulin, E.; Naumann-Godo, M.; de Naurois, M.; Nedbal, D.; Nekrassov, D.; Niemiec, J.; Nolan, S. J.; Ohm, S.; Olive, J. -F.; de Oña Wilhelmi, E.; Orford, K. J.; Ostrowski, M.; Panter, M.; Arribas, M. Paz; Pedaletti, G.; Pelletier, G.; Petrucci, P. -O.; Pita, S.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raubenheimer, B. C.; Raue, M.; Rayner, S. M.; Renaud, M.; Rieger, F.; Ripken, J.; Rob, L.; Rosier-Lees, S.; Rowell, G.; Rudak, B.; Rulten, C. B.; Ruppel, J.; Sahakian, V.; Santangelo, A.; Schlickeiser, R.; Schöck, F. M.; Schröder, R.; Schwanke, U.; Schwarzburg, S.; Schwemmer, S.; Shalchi, A.; Sikora, M.; Skilton, J. L.; Sol, H.; Spangler, D.; Stawarz, Ł.; Steenkamp, R.; Stegmann, C.; Superina, G.; Szostek, A.; Tam, P. H.; Tavernet, J. -P.; Terrier, R.; Tibolla, O.; van Eldik, C.; Vasileiadis, G.; Venter, C.; Venter, L.; Vialle, J. P.; Vincent, P.; Vivier, M.; Völk, H. J.; Volpe, F.; Wagner, S. J.; Ward, M.; Zdziarski, A. A.; Zech, A.; H. E. S. S. Collaboration; Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Battelino, M.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Charles, E.; Chekhtman, A.; Chen, A. W.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Colafrancesco, S.; Conrad, J.; Costamante, L.; Cutini, S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Dubus, G.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Fleury, P.; Focke, W. B.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giordano, F.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Horan, D.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, W. N.; Kadler, M.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kerr, M.; Knödlseder, J.; Kuehn, F.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S. -H.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Madejski, G. M.; Makeev, A.; Mazziotta, M. N.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rodriguez, A. Y.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Scargle, J. D.; Schalk, T. L.; Sellerholm, A.; Sgrò, C.; Shaw, M.; Smith, D. A.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Strickman, M. S.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vilchez, N.; Villata, M.; Vitale, V.; Waite, A. P.; Wood, K. S.; Ylinen, T.; Ziegler, M.; Fermi LAT Collaboration, We report on the first simultaneous observations that cover the optical, X-ray, and high-energy gamma-ray bands of the BL Lac object PKS 2155-304. The gamma-ray bands were observed for 11 days, between 2008 August 25 and 2008 September 6 (MJD 54704-54715), jointly with the Fermi Gamma-ray Space Telescope and the HESS atmospheric Cherenkov array, providing the first simultaneous MeV-TeV spectral energy distribution (SED) with the new generation of γ-ray telescopes. The ATOM telescope and the RXTE and Swift observatories provided optical and X-ray coverage of the low-energy component over the same time period. The object was close to the lowest archival X-ray and very high energy (VHE; >100 GeV) state, whereas the optical flux was much higher. The light curves show relatively little (~30%) variability overall when compared to past flaring episodes, but we find a clear optical/VHE correlation and evidence for a correlation of the X-rays with the high-energy spectral index. Contrary to previous observations in the flaring state, we do not find any correlation between the X-ray and VHE components. Although synchrotron self-Compton models are often invoked to explain the SEDs of BL Lac objects, the most common versions of these models are at odds with the correlated variability we find in the various bands for PKS 2155-304....
The Astrophysical Journal, May 2009

Fermi Large Area Telescope Observations of the Vela Pulsar
Abdo, A. A.; Ackermann, M.; Atwood, W. B.; Bagagli, R.; Baldini, L.; Ballet, J.; Band, D. L.; Barbiellini, G.; Baring, M. G.; Bartelt, J.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellardi, F.; Bellazzini, R.; Berenji, B.; Bisello, D.; Blandford, R. D.; Bloom, E. D.; Bogart, J. R.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Camilo, F.; Caraveo, P. A.; Casandjian, J. M.; Ceccanti, M.; Cecchi, C.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cognard, I.; Cohen-Tanugi, J.; Cominsky, L. R.; Conrad, J.; Corbet, R.; Corucci, L.; Cutini, S.; Davis, D. S.; DeKlotz, M.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Dormody, M.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Espinoza, C.; Farnier, C.; Favuzzi, C.; Flath, D. L.; Fleury, P.; Focke, W. B.; Frailis, M.; Freire, P. C. C.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giannitrapani, R.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Gotthelf, E. V.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Haller, G.; Harding, A. K.; Hart, P. A.; Hartman, R. C.; Hays, E.; Hobbs, G.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Johnston, S.; Kamae, T.; Kanbach, G.; Kaspi, V. M.; Katagiri, H.; Kataoka, J.; Kavelaars, A.; Kawai, N.; Kelly, H.; Kerr, M.; Kiziltan, B.; Klamra, W.; Knödlseder, J.; Kramer, M.; Kuehn, F.; Kuss, M.; Lande, J.; Landriu, D.; Latronico, L.; Lee, B.; Lee, S. -H.; Lemoine-Goumard, M.; Livingstone, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Lyne, A. G.; Madejski, G. M.; Makeev, A.; Manchester, R. N.; Marangelli, B.; Marelli, M.; Mazziotta, M. N.; McEnery, J. E.; McGlynn, S.; McLaughlin, M. A.; Menon, N.; Meurer, C.; Michelson, P. F.; Mineo, T.; Mirizzi, N.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Mongelli, M.; Monte, C.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Nolan, P. L.; Noutsos, A.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paccagnella, A.; Paneque, D.; Panetta, J. H.; Parent, D.; Pearce, M.; Pepe, M.; Perchiazzi, M.; Pesce-Rollins, M.; Pieri, L.; Pinchera, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Ransom, S. M.; Rapposelli, E.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Reyes, L. C.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sacchetti, A.; Sadrozinski, H. F. -W.; Saggini, N.; Sanchez, D.; Sander, A.; Parkinson, P. M. Saz; Segal, K. N.; Sellerholm, A.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stamatikos, M.; Starck, J. -L.; Stecker, F. W.; Stephens, T. E.; Strickman, M. S.; Strong, A. W.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Tenze, A.; Thayer, J. B.; Thayer, J. G.; Theureau, G.; Thompson, D. J.; Thorsett, S. E.; Tibaldo, L.; Tibolla, O.; Torres, D. F.; Tramacere, A.; Turri, M.; Usher, T. L.; Vigiani, L.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Watters, K.; Weltevrede, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M., The Vela pulsar is the brightest persistent source in the GeV sky and thus is the traditional first target for new γ-ray observatories. We report here on initial Fermi Large Area Telescope observations during verification phase pointed exposure and early sky survey scanning. We have used the Vela signal to verify Fermi timing and angular resolution. The high-quality pulse profile, with some 32,400 pulsed photons at E >= 0.03 GeV, shows new features, including pulse structure as fine as 0.3 ms and a distinct third peak, which shifts in phase with energy. We examine the high-energy behavior of the pulsed emission; initial spectra suggest a phase-averaged power-law index of Γ = 1.51^+0.05 _-0.04 with an exponential cutoff at E_c = 2.9 ± 0.1 GeV. Spectral fits with generalized cutoffs of the form e^{-(E/E_c)^b} require b <= 1, which is inconsistent with magnetic pair attenuation, and thus favor outer-magnetosphere emission models. Finally, we report on upper limits to any unpulsed component, as might be associated with a surrounding pulsar wind nebula....
The Astrophysical Journal, May 2009

Fermi/Large Area Telescope Discovery of Gamma-Ray Emission from the Flat-Spectrum Radio Quasar PKS 1454-354
Abdo, A. A.; Ackermann, M.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bogaert, G.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Colafrancesco, S.; Conrad, J.; Costamante, L.; Cutini, S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Dumora, D.; Edmonds, Y.; Farnier, C.; Favuzzi, C.; Ferrara, E. C.; Fleury, P.; Focke, W. B.; Foschini, L.; Frailis, M.; Fuhrmann, L.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Harding, A. K.; Hartman, R. C.; Hayashida, M.; Hays, E.; Healey, S. E.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, W. N.; Kadler, M.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocian, M. L.; Kuehn, F.; Kuss, M.; Latronico, L.; Lee, S. -H.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Marelli, M.; Mazziotta, M. N.; McEnery, J. E.; McGlynn, S.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Nuss, E.; Ohno, M.; Ohsugi, T.; Ojha, R.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J. H.; Parent, D.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Reyes, L. C.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sambruna, R.; Sanchez, D.; Sander, A.; Parkinson, P. M. Saz; Sgrò, C.; Shaw, M. S.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Tibolla, O.; Torres, D. F.; Tosti, G.; Tramacere, A.; Usher, T. L.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M.; Fermi/LAT Collaboration; Edwards, P. G.; Chester, M. M.; Burrows, D. N.; Hauser, M.; Wagner, S., We report the discovery by the Large Area Telescope (LAT) onboard the Fermi Gamma-Ray Space Telescope of high-energy γ-ray (GeV) emission from the flat-spectrum radio quasar PKS 1454-354 (z = 1.424). On 2008 September 4, the source rose to a peak flux of (3.5 ± 0.7) × 10^-6 ph cm^-2 s^-1 (E > 100 MeV) on a timescale of hours and then slowly dropped over the following 2 days. No significant spectral changes occurred during the flare. Fermi/LAT observations also showed that PKS 1454-354 is the most probable counterpart of the unidentified EGRET source 3EG J1500-3509. Multiwavelength measurements performed during the following days (7 September with Swift; 6-7 September with the ground-based optical telescope Automated Telescope for Optical Monitoring; 13 September with the Australia Telescope Compact Array) resulted in radio, optical, UV, and X-ray fluxes greater than archival data, confirming the activity of PKS 1454-354....
The Astrophysical Journal, May 2009

Measurement of the Cosmic Ray e⁺+e^- Spectrum from 20GeV to 1TeV with the Fermi Large Area Telescope
Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Battelino, M.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bogaert, G.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carlson, P.; Casandjian, J. M.; Cecchi, C.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cominsky, L. R.; Conrad, J.; Cutini, S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; di Bernardo, G.; Do Couto E Silva, E.; Drell, P. S.; Dubois, R.; Dumora, D.; Edmonds, Y.; Farnier, C.; Favuzzi, C.; Focke, W. B.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gaggero, D.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grasso, D.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hartman, R. C.; Hayashida, M.; Hays, E.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocevski, D.; Kuehn, F.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Massai, M. M.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Pohl, M.; Porter, T. A.; Profumo, S.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Schalk, T. L.; Sellerholm, A.; Sgrò, C.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Stephens, T. E.; Strickman, M. S.; Strong, A. W.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Tibolla, O.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; van Etten, A.; Vasileiou, V.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wallace, E.; Wang, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M., Designed as a high-sensitivity gamma-ray observatory, the Fermi Large Area Telescope is also an electron detector with a large acceptance exceeding 2m²sr at 300 GeV. Building on the gamma-ray analysis, we have developed an efficient electron detection strategy which provides sufficient background rejection for measurement of the steeply falling electron spectrum up to 1 TeV. Our high precision data show that the electron spectrum falls with energy as E^-3.0 and does not exhibit prominent spectral features. Interpretations in terms of a conventional diffusive model as well as a potential local extra component are briefly discussed....
Physical Review Letters, May 2009

Discovery of Pulsed γ-Rays from the Young Radio Pulsar PSR J1028-5819 with the Fermi Large Area Telescope
Abdo, A. A.; Ackermann, M.; Atwood, W. B.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cominsky, L. R.; Conrad, J.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Donato, D.; Dormody, M.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Dumora, D.; Edmonds, Y.; Farnier, C.; Favuzzi, C.; Fleury, P.; Focke, W. B.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Harding, A. K.; Hayashida, M.; Hays, E.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Johnston, S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Komin, N.; Kramer, M.; Kuehn, F.; Kuss, M.; Latronico, L.; Lee, S. -H.; Lemoine-Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Marelli, M.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J. H.; Parent, D.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Parkinson, P. M. Saz; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Thorsett, S. E.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Van Etten, A.; Vilchez, N.; Vitale, V.; Waite, A. P.; Watters, K.; Wood, K. S.; Ylinen, T.; Ziegler, M.; Hobbs, G.; Keith, M.; Manchester, R. N.; Weltevrede, P., Radio pulsar PSR J1028-5819 was recently discovered in a high-frequency search (at 3.1 GHz) in the error circle of the Energetic Gamma-Ray Experiment Telescope (EGRET) source 3EG J1027-5817. The spin-down power of this young pulsar is great enough to make it very likely the counterpart for the EGRET source. We report here the discovery of γ-ray pulsations from PSR J1028-5819 in early observations by the Large Area Telescope (LAT) on the Fermi Gamma-Ray Space Telescope. The γ-ray light curve shows two sharp peaks having phase separation of 0.460 ± 0.004, trailing the very narrow radio pulse by 0.200 ± 0.003 in phase, very similar to that of other known γ-ray pulsars. The measured γ-ray flux gives an efficiency for the pulsar of ~10-20% (for outer magnetosphere beam models). No evidence of a surrounding pulsar wind nebula is seen in the current Fermi data but limits on associated emission are weak because the source lies in a crowded region with high background emission. However, the improved angular resolution afforded by the LAT enables the disentanglement of the previous COS-B and EGRET source detections into at least two distinct sources, one of which is now identified as PSR J1028-5819....
The Astrophysical Journal, Apr. 2009

Search for Sc-K Line Emission from RX J0852.0-4622 Supernova Remnant with Suzaku
Junko S. Hiraga; Yusuke Kobayashi; Toru Tamagawa; Asami Hayato; Aya Bamba; Yukikatsu Terada; Robert Petre; Hideaki Katagiri; Hiroshi Tsunemi, We searched for evidence of line emission around 4 keV from the northwestern rim of the supernova remnant RX J0852.0-4622 using Suzaku XIS data. Several papers have reported on the detection of an emission line around 4.1 keV from this region of the sky. This line Would arise from K-band fluorescence by Sc-44, the immediate decay product of Ti-44. We performed spectral analysis for the entire portion of the NW rim of the remnant within the XIS field of view, as well as various regions corresponding to regions of published claims of line emission. We found no line emission around 4.1 keV anywhere, and are able to set a restrictive Upper limit to the X-ray flux: 1.1 x 10(-6) s(-1) cm(-2) for the entire field. For every region, our flux upper limit falls below that of the previously claimed detection. Therefore, we conclude that, to date, no definite X-ray line feature from Sc-K emission has been detected in the NW rim of RX J0852.0-4622. Our negative-detection supports the recent claim that RX J0852-4622 is neither young (1700-4000 yr) nor nearby (similar to 750 pc)., OXFORD UNIV PRESS
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Apr. 2009, [Reviewed]

Fermi Observations of High-Energy Gamma-Ray Emission from GRB 080916C
Abdo, A. A.; Ackermann, M.; Arimoto, M.; Asano, K.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Band, D. L.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Battelino, M.; Baughman, B. M.; Bechtol, K.; Bellardi, F.; Bellazzini, R.; Berenji, B.; Bhat, P. N.; Bissaldi, E.; Blandford, R. D.; Bloom, E. D.; Bogaert, G.; Bogart, J. R.; Bonamente, E.; Bonnell, J.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Briggs, M. S.; Brigida, M.; Bruel, P.; Burnett, T. H.; Burrows, D.; Busetto, G.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Ceccanti, M.; Cecchi, C.; Celotti, A.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cominsky, L. R.; Connaughton, V.; Conrad, J.; Costamante, L.; Cutini, S.; DeKlotz, M.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Dingus, B. L.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Dumora, D.; Edmonds, Y.; Evans, P. A.; Fabiani, D.; Farnier, C.; Favuzzi, C.; Finke, J.; Fishman, G.; Focke, W. B.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giommi, P.; Giordano, F.; Glanzman, T.; Godfrey, G.; Goldstein, A.; Granot, J.; Greiner, J.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Haller, G.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Morata, J. A. Hernando; Hoover, A.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kavelaars, A.; Kawai, N.; Kelly, H.; Kennea, J.; Kerr, M.; Kippen, R. M.; Knödlseder, J.; Kocevski, D.; Kocian, M. L.; Komin, N.; Kouveliotou, C.; Kuehn, F.; Kuss, M.; Lande, J.; Landriu, D.; Larsson, S.; Latronico, L.; Lavalley, C.; Lee, B.; Lee, S. -H.; Lemoine-Goumard, M.; Lichti, G. G.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Marangelli, B.; Mazziotta, M. N.; McBreen, S.; McEnery, J. E.; McGlynn, S.; Meegan, C.; Mészáros, P.; Meurer, C.; Michelson, P. F.; Minuti, M.; Mirizzi, N.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Nelson, D.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paciesas, W. S.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Perri, M.; Pesce-Rollins, M.; Petrosian, V.; Pinchera, M.; Piron, F.; Porter, T. A.; Preece, R.; Rainò, S.; Ramirez-Ruiz, E.; Rando, R.; Rapposelli, E.; Razzano, M.; Razzaque, S.; Rea, N.; Reimer, A.; Reimer, O.; Reposeur, T.; Reyes, L. C.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Parkinson, P. M. Saz; Scargle, J. D.; Schalk, T. L.; Segal, K. N.; Sgrò, C.; Shimokawabe, T.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stamatikos, M.; Starck, J. -L.; Stecker, F. W.; Steinle, H.; Stephens, T. E.; Strickman, M. S.; Suson, D. J.; Tagliaferri, G.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Tenze, A.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Turri, M.; Tuvi, S.; Usher, T. L.; van der Horst, A. J.; Vigiani, L.; Vilchez, N.; Vitale, V.; von Kienlin, A.; Waite, A. P.; Williams, D. A.; Wilson-Hodge, C.; Winer, B. L.; Wood, K. S.; Wu, X. F.; Yamazaki, R.; Ylinen, T.; Ziegler, M.; Fermi LAT Collaboration; Fermi GBM Collaboration, Gamma-ray bursts (GRBs) are highly energetic explosions signaling the death of massive stars in distant galaxies. The Gamma-ray Burst Monitor and Large Area Telescope onboard the Fermi Observatory together record GRBs over a broad energy range spanning about 7 decades of gamma-ray energy. In September 2008, Fermi observed the exceptionally luminous GRB 080916C, with the largest apparent energy release yet measured. The high-energy gamma rays are observed to start later and persist longer than the lower energy photons. A simple spectral form fits the entire GRB spectrum, providing strong constraints on emission models. The known distance of the burst enables placing lower limits on the bulk Lorentz factor of the outflow and on the quantum gravity mass....
Science, Mar. 2009

Gamma-ray spectrum of RX J1713.7-3946 in the Fermi era and future detection of neutrinos
R. Yamazaki; K. Kohri; H. Katagiri, The recently launched satellite, Fermi Gamma-ray Space Telescope, is expected to find out if cosmic-ray (CR) protons are generated from supernova remnants (SNRs), especially RX J1713.7-3946, by observing the GeV-to-TeV gamma-rays. The GeV emission is thought to be bright if the TeV emission is hadronic, i.e., of proton origin, while dim if leptonic. We reexamine the above view using a simple theoretical model of nonlinear acceleration of particles to calculate the gamma-ray spectrum of Galactic young SNRs. If the nonlinear effects of CR acceleration are considered, it may be impossible to distinguish the evidence of proton acceleration from leptonic in the gamma-ray spectrum of Galactic young SNRs like RX J1713.7-3946. On the other hand, future km(3)-class neutrino observations will likely find a clear evidence of the proton acceleration there., EDP SCIENCES S A
ASTRONOMY & ASTROPHYSICS, Feb. 2009, [Reviewed]

The Fermi Gamma-Ray Space Telescope Discovers the Pulsar in the Young Galactic Supernova Remnant CTA 1
Abdo, A. A.; Ackermann, M.; Atwood, W. B.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bogaert, G.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carlson, P.; Casandjian, J. M.; Cecchi, C.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cominsky, L. R.; Conrad, J.; Cutini, S.; Davis, D. S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Dormody, M.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Dumora, D.; Edmonds, Y.; Farnier, C.; Focke, W. B.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M. -H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Harding, A. K.; Hartman, R. C.; Hays, E.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Kanai, Y.; Kanbach, G.; Katagiri, H.; Kawai, N.; Kerr, M.; Kishishita, T.; Kiziltan, B.; Knödlseder, J.; Kocian, M. L.; Komin, N.; Kuehn, F.; Kuss, M.; Latronico, L.; Lemoine-Goumard, M.; Longo, F.; Lonjou, V.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Marelli, M.; Mazziotta, M. N.; McEnery, J. E.; McGlynn, S.; Meurer, C.; Michelson, P. F.; Mineo, T.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Nolan, P. L.; Nuss, E.; Ohno, M.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piano, G.; Pieri, L.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Ray, P. S.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sadrozinski, H. F. -W.; Sanchez, D.; Sander, A.; Parkinson, P. M. Saz; Schalk, T. L.; Sellerholm, A.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, J. -L.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Thorsett, S. E.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Usher, T. L.; Van Etten, A.; Vilchez, N.; Vitale, V.; Wang, P.; Watters, K.; Winer, B. L.; Wood, K. S.; Yasuda, H.; Ylinen, T.; Ziegler, M., Energetic young pulsars and expanding blast waves [supernova remnants (SNRs)] are the most visible remains after massive stars, ending their lives, explode in core-collapse supernovae. The Fermi Gamma-Ray Space Telescope has unveiled a radio quiet pulsar located near the center of the compact synchrotron nebula inside the supernova remnant CTA 1. The pulsar, discovered through its gamma-ray pulsations, has a period of 316.86 milliseconds and a period derivative of 3.614 × 10^-13 seconds per second. Its characteristic age of 10⁴ years is comparable to that estimated for the SNR. We speculate that most unidentified Galactic gamma-ray sources associated with star-forming regions and SNRs are such young pulsars....
Science, Nov. 2008

The 2006 November Outburst of EG Aquarii: the SU UMa Nature Revealed
Akira Imada; Rod Stubbings; Taichi Kato; Makoto Uemura; Thomas Krajci; Kei'ichi Torii; Kei Sugiyasu; Kaori Kubota; Yuuki Moritani; Ryoko Ishioka; Gianluca Masi; Seiichiro Kiyota; L. A. G. Monard; Hiroyuki Maehara; Kazuhiro Nakajima; Akira Arai; Takashi Ohsugi; Takuya Yamashita; Koji S. Kawabata; Osamu Nagae; Shingo Chiyonobu; Yasushi Fukazawa; Tsunefumi Mizuno; Hideaki Katagiri; Hiromitsu Takahashi; Atsushi Ueda; Takehiro Hayashi; Kiichi Okita; Michitoshi Yoshida; Kenshi Yanagisawa; Shuji Sato; Masaru Kino; Masahiro Kitagawa; Kozo Sadakane; Daisaku Nogami, We report on time-resolved CCD photometry of the cataclysmic variable EG Aquarii during a 2006 November outburst. During the outburst, superhumps were unambiguously detected with a mean period of 0.078828(6) d, allowing for the first time to classify the object as an SU UMa-type dwarf nova. It also turned out that the outburst contained a precursor. At the end of the precursor, immature profiles of humps were observed. By a phase analysis of these humps, we interpreted the features as being superhumps. This is the second example that the superhumps were shown during a precursor. Near the maximum stage of the outburst, we discovered an abrupt shift of the superhump period by similar to 0.002d. After the supermaximum, the superhump period decreased at a rate of (P) over dot/P -8.2 x 10(-5), which is typical for SU UMa-type dwarf novae. Although the outburst light curve was characteristic of SU UMa-type dwarf novae, long-term monitoring of the variable shows no outbursts over the past decade. We also comment on the basic properties of long period and inactive SU UMa-type dwarf novae., OXFORD UNIV PRESS
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Oct. 2008, [Reviewed]

Very high energy gamma-ray observations of the Galactic Plane with the CANGAROO-III telescopes
Ohishi, M.; Mori, M.; Adachi, Y.; Asahara, A.; Bicknell, G. V.; Clay, R. W.; Doi, Y.; Edwards, P. G.; Enomoto, R.; Gunji, S.; Hara, S.; Hara, T.; Hattori, T.; Hayashi, Sei.; Higashi, Y.; Hirai, Y.; Inoue, K.; Itoh, C.; Kabuki, S.; Kajino, F.; Katagiri, H.; Kawachi, A.; Kifune, T.; Kiuchi, R.; Kubo, H.; Kurihara, T.; Kurosaka, R.; Kushida, J.; Matsubara, Y.; Miyashita, Y.; Mizukami, T.; Mizuniwa, R.; Muraishi, H.; Muraki, Y.; Naito, T.; Nakamori, T.; Nakano, S.; Nakase, T.; Nishida, D.; Nishijima, K.; Sakamoto, N.; Sakamoto, Y.; Sato, M.; Seki, A.; Stamatescu, V.; Suzuki, T.; Swaby, D. L.; Tanimori, T.; Tanimura, H.; Thornton, G. J.; Tokanai, F.; Tsuchiya, K.; Watanabe, S.; Yamada, Y.; Yamaoka, T.; Yamazaki, E.; Yanagita, S.; Yoshida, T.; Yoshikoshi, T.; Yukawa, Y., In 2004, we searched for very high energy (VHE) gamma-ray emission from the Galactic Plane using the CANGAROO-III stereoscopic observation system. Two different longitude regions (ℓ = -19°.5 and ℓ = +13°.0) on the Galactic Plane were observed during July and August 2004. We analyzed events that triggered three telescopes aiming to measure the diffuse emission component. No significant signal associated with the Galactic Plane was found from either of the regions. Assuming that the gamma-ray spectrum is described by a single power-law for energies ranging between a few GeV and TeV, lower limits of the power-law spectral indices were found to be 2.2 for both of the regions with a 99.9% confidence level. This result is consistent with the other VHE measurements and constrains a hypothesis in which a very hard (̃2.0) cosmic ray electron spectrum was introduced to explain the EGRET GeV anomaly....
Astroparticle Physics, Sep. 2008

CANGAROO-III Search for Gamma Rays from Kepler's Supernova Remnant
Enomoto, R.; Higashi, Y.; Yoshida, T.; Tanimori, T.; Bicknell, G. V.; Clay, R. W.; Edwards, P. G.; Gunji, S.; Hara, S.; Hara, T.; Hattori, T.; Hayashi, S.; Hirai, Y.; Inoue, K.; Kabuki, S.; Kajino, F.; Katagiri, H.; Kawachi, A.; Kifune, T.; Kiuchi, R.; Kubo, H.; Kushida, J.; Matsubara, Y.; Mizukami, T.; Mizumoto, Y.; Mizuniwa, R.; Mori, M.; Muraishi, H.; Muraki, Y.; Naito, T.; Nakamori, T.; Nakano, S.; Nishida, D.; Nishijima, K.; Ohishi, M.; Sakamoto, Y.; Seki, A.; Stamatescu, V.; Suzuki, T.; Swaby, D. L.; Thornton, G.; Tokanai, F.; Tsuchiya, K.; Watanabe, S.; Yamada, Y.; Yamazaki, E.; Yanagita, S.; Yoshikoshi, T.; Yukawa, Y., Kepler's supernova, discovered in 1604 October, produced a remnant that has been well studied observationally in the radio, infrared, optical, and X-ray bands, and theoretically. Some models have predicted a TeV gamma-ray flux that is detectable with current Imaging Cerenkov Atmospheric Telescopes. We report on observations carried out in 2005 April with the CANGAROO-III Telescope. No statistically significant excess was observed, and limitations on the allowed parameter range in the model are discussed....
The Astrophysical Journal, Aug. 2008, [Reviewed]

Observation of Very High Energy Gamma Rays from HESS J1804-216 with CANGAROO-III Telescopes
Higashi, Y.; Kubo, H.; Yoshida, T.; Enomoto, R.; Tanimori, T.; Edwards, P. G.; Naito, T.; Bicknell, G. V.; Clay, R. W.; Gunji, S.; Hara, S.; Hara, T.; Hattori, T.; Hayashi, S.; Hirai, Y.; Inoue, K.; Kabuki, S.; Kajino, F.; Katagiri, H.; Kawachi, A.; Kifune, T.; Kiuchi, R.; Kushida, J.; Matsubara, Y.; Mizukami, T.; Mizumoto, Y.; Mizuniwa, R.; Mori, M.; Muraishi, H.; Muraki, Y.; Nakamori, T.; Nakano, S.; Nishida, D.; Nishijima, K.; Ohishi, M.; Sakamoto, Y.; Seki, A.; Stamatescu, V.; Suzuki, T.; Swaby, D. L.; Thornton, G.; Tokanai, F.; Tsuchiya, K.; Watanabe, S.; Yamada, Y.; Yamazaki, E.; Yanagita, S.; Yoshikoshi, T.; Yukawa, Y., We observed the unidentified TeV gamma-ray source HESS J1804-216 with the CANGAROO-III atmospheric Cerenkov telescopes from 2006 May to July. We detected very high energy gamma rays above 600 GeV at the 10 σ level in an effective exposure of 76 hr. We obtained a differential flux of (5.0 +/- 1.5_stat+/- 1.6_sys) × 10^-12(E/1 TeV)^-α cm^-2 s^-1 TeV^-1 with a photon index α of 2.69 +/- 0.30_stat+/- 0.34_sys, which is consistent with that of the H.E.S.S. observation in 2004. We also confirm the extended morphology of the source. By combining our result with multiwavelength observations, we discuss the possible counterparts of HESS J1804-216 and the radiation mechanism based on leptonic and hadronic processes for a supernova remnant and a pulsar wind nebula....
The Astrophysical Journal, Aug. 2008, [Reviewed]

Observation of an Extended Very High Energy Gamma-Ray Emission from MSH 15-52 with CANGAROO-III
Nakamori, T.; Kubo, H.; Yoshida, T.; Tanimori, T.; Enomoto, R.; Bicknell, G. V.; Clay, R. W.; Edwards, P. G.; Gunji, S.; Hara, S.; Hara, T.; Hattori, T.; Hayashi, S.; Higashi, Y.; Hirai, Y.; Inoue, K.; Kabuki, S.; Kajino, F.; Katagiri, H.; Kawachi, A.; Kifune, T.; Kiuchi, R.; Kushida, J.; Matsubara, Y.; Mizukami, T.; Mizumoto, Y.; Mizuniwa, R.; Mori, M.; Muraishi, H.; Muraki, Y.; Naito, T.; Nakano, S.; Nishida, D.; Nishijima, K.; Ohishi, M.; Sakamoto, Y.; Seki, A.; Stamatescu, V.; Suzuki, T.; Swaby, D. L.; Thornton, G.; Tokanai, F.; Tsuchiya, K.; Watanabe, S.; Yamada, Y.; Yamazaki, E.; Yanagita, S.; Yoshikoshi, T.; Yukawa, Y., We have observed the supernova remnant MSH 15-52 (G320.4-1.2), which contains the gamma-ray pulsar PSR B1509-58, using the CANGAROO-III imaging atmospheric Cerenkov telescope array from 2006 April to June. We detected gamma rays above 810 GeV at the 7 σ level during a total effective exposure of 48.4 hr. We obtained a differential gamma-ray flux at 2.35 TeV of (7.9 +/- 1.5_stat+/- 1.7_sys) × 10^-13 cm^-2 s^-1 TeV^-1, with a photon index of 2.21 +/- 0.39_stat+/- 0.40_sys, which is compatible with that of the H.E.S.S. observation in 2004. The morphology shows extended emission compared to our point spread function. We consider the plausible origin of the high-energy emission based on a multiwavelength spectral analysis and energetics arguments....
The Astrophysical Journal, Apr. 2008

Discovery of a WZ sge-type dwarf nova, SDSS j102146.44+234926.3: Unprecedented infrared activity during a rebrightening phase
Makoto Uemura; Akira Arai; Tom Krajci; Elena Pavlenko; Sergei Yu. Shugarov; Nataly A. Katysheva; Vitalij P. Goranskij; Hiroyuki Maehara; Akira Imada; Taichi Kato; Daisaku Nogami; Kazuhiro Nakajima; Takashi Ohsugi; Takuya Yamashita; Koji S. Kawabata; Osamu Nagae; Shingo Chiyonobu; Yasushi Fukazawa; Tsunefumi Mizuno; Hideaki Katagiri; Hiromitsu Takahashi; Atsushi Ueda; Takehiro Hayashi; Kiichi Okita; Michitoshi Yoshida; Kenshi Yanagisawa; Shuji Sato; Masaru Kino; Kozo Sadakane, Several SU UMa-type dwarf novae and WZ Sge-type stars tend to exhibit rebrightenings after superoutbursts. The rebrightening phenomenon is problematic for the disk instability theory of dwarf novae, since it requires a large amount of remnant matter in the disk, even after superoutbursts. Here, we report on our optical and infrared observations during the first-ever outburst of a new dwarf nova, SDSS J 102146.44 + 234926.3. During the outburst, we detected superhumps with a period of 0.056281 +/- 0.000015 d, which is typical for superhump periods in WZ Sge stars. In conjunction with the appearance of a long-lived rebrightening, we concluded that the object is a new member of WZ Sge stars. Our observations, furthermore, revealed infrared behaviors for the first time in the rebrightening phase of WZ Sge stars. We discovered prominent infrared superhumps. We calculated the color temperature of the infrared superhump source to be 4600-6400 K. These temperatures are too low to be explained by a fully ionized disk appearing during dwarf-nova outbursts. We also found a K-s-band excess over the hot disk component. These unprecedented infrared activities provide evidence for the presence of mass reservoir at the outermost part of the accretion disk. We propose that a moderately high mass-accretion rate at this infrared active region leads to the long-lived rebrightening observed in SDSS J102146.44 + 234926.3., OXFORD UNIV PRESS
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Apr. 2008, [Reviewed]

CANGAROO-III Observations of the 2006 Outburst of PKS 2155-304
Sakamoto, Y.; Nishijima, K.; Mizukami, T.; Yamazaki, E.; Kushida, J.; Enomoto, R.; Ohishi, M.; Bicknell, G. V.; Clay, R. W.; Edwards, P. G.; Gunji, S.; Hara, S.; Hattori, T.; Hayashi, S.; Higashi, Y.; Hirai, Y.; Inoue, K.; Itoh, C.; Kabuki, S.; Kajino, F.; Katagiri, H.; Kawachi, A.; Kifune, T.; Kiuchi, R.; Kubo, H.; Mizuniwa, R.; Mori, M.; Muraishi, H.; Naito, T.; Nakamori, T.; Nakano, S.; Nishida, D.; Seki, A.; Stamatescu, V.; Suzuki, T.; Swaby, D. L.; Tanimori, T.; Thornton, G.; Tokanai, F.; Tsuchiya, K.; Watanabe, S.; Yamada, Y.; Yanagita, S.; Yoshida, T.; Yoshikoshi, T.; Yukawa, Y., We have used the CANGAROO-III imaging atmospheric Cerenkov telescopes to observe the high-frequency-peaked BL Lacertae (HBL) object PKS 2155-304 between 2006 July 28 (MJD 53,944) and August 2, triggered by the H.E.S.S. report that the source was in a high state of TeV gamma-ray emission. A signal was detected at the 4.8 σ level in an effective live time of 25.1 hr during the outburst period. The flux of very high energy gamma rays from the CANGAROO-III observations shows variability on the timescale of less than a few hours. The averaged integral flux above 660 GeV is (1.6 +/- 0.3_stat+/- 0.5_syst) × 10^-11 cm^-2 s^-1, which corresponds to ~45% of the flux observed from the Crab Nebula. Follow-up observations between August 17 (MJD 53,964) and 25 indicate that the source activity had decreased....
The Astrophysical Journal, Mar. 2008

Discovery of Extended X-Ray Emission from an Unidentified TeV Source, HESS J1614-518, Using the Suzaku Satellite
Matsumoto Hironori; Uchiyama Hideki; Sawada Makoto; TSURU Takeshi G.; KOYAMA Katsuji; KATAGIRI Hideaki; YAMAZAKI Ryo; BAMBA Aya; KOHRI Kazunori; MORI Koji; UCHIYAMA Yasunobu, We report Suzaku results concerning HESS J1614-518, which is the brightest extended TeV gamma-ray source discovered in the Galactic plane survey conducted using the H.E.S.S. telescope. We discovered three X-ray objects in the field of view of the X-ray Imaging Spectrometer, which were designated as Suzaku J1614-5141 (src A), Suzaku J1614-5152 (src B), and Suzaku J1614-5148 (src C). Src A is an extended source located at the peak position of HESS J1614-518, and is therefore a plausible counterpart to HESS J1614-518. The X-ray flux in the 2-10 keV band is 5 x 10(-13) erg s(-1) cm(-2), which is an order of magnitude smaller than the TeV flux. The photon index is 1.7, which is smaller than the canonical value of synchrotron emissions from high-energy electrons found in some supernova remnants. These findings present a challenge to models in which the origin of TeV emission is inverse Compton scattering of the cosmic microwave background by accelerated electrons that emit X-rays via synchrotron emission. Src B is located at a relatively dim region in the TeV band image; however, its hydrogen column density is the same as that of src A. Therefore, src B may also be physically related to HESS J1614-518. Src C is a foreground late-type B star. We also discovered soft extended X-ray emission near HESS J1614-518., Astronomical Society of Japan
PASJ : publications of the Astronomical Society of Japan, 20 Feb. 2008, [Reviewed]

Suzaku Wide-Band Observations of SN 1006
Bamba Aya; Fukazawa Yasushi; Hiraga Junko S.; HUGHES John P.; KATAGIRI Hideaki; KOKUBUN Motohide; KOYAMA Katsuji; MIYATA Emi; MIZUNO Tsunefumi; MORI Koji; NAKAJIMA Hiroshi; OZAKI Masanobu; PETRE Rob; TAKAHASHI Hiromitsu; TAKAHASHI Tadayuki; TANAKA Takaaki; TERADA Yukikatsu; UCHIYAMA Yasunobu; WATANABE Shin; YAMAGUCHI Hiroya, We report on the wide-band spectra of SN 1006, as observed by Suzaku. Thermal and nonthermal emissions were successfully resolved thanks to the excellent spectral response of Suzaku's X-ray CCD XIS. The nonthermal emission could not be reproduced by a simple power-law model, but needed a roll-off at 5.7 x 10(16) Hz = 0.23 keV. The roll-off frequency is significantly higher in the northeastern rim than in the southwestern rim. We also placed the most stringent upper limit of the flux above 10 keV using the Hard X-ray Detector., Astronomical Society of Japan
PASJ : publications of the Astronomical Society of Japan, 20 Feb. 2008, [Reviewed]

Measuring the broad-band X-ray spectrum from 400 eV to 40 keV in the southwest part of the supernova remnant RX J1713.7-3946
Tadayuki Takahashi; Takaaki Tanaka; Yasunobu Uchiyama; Junko S. Hiraga; Kazuhiro Nakazawa; Shin Watanabe; Aya Bamba; John P. Hughes; Hideaki Katagiri; Jun Kataoka; Motohide Kokubun; Katsuji Koyama; Koji Mori; Robert Petre; Hiromitsu Takahashi; Yoko Tsuboi, We report on results from Suzaku broadband X-ray observations of the southwest part of the galactic supernova remnant (SNR) RX J1713.7-3946 with an energy coverage of 0.4-40keV. The X-ray spectrum, presumably of synchrotron origin, is known to be completely lineless, making this SNR ideally suited for a detailed study of the X-ray spectral shape formed through efficient particle acceleration at high-speed shocks. With a sensitive hard X-ray measurement from the HXD PIN aboard Suzaku, we determined the hard X-ray spectrum in the 12-40 keV range to be described by a power law with photon index of Gamma = 3.2 +/- 0.2, significantly steeper than the soft X-ray index of Gamma = 2.4 +/- 0.05 measured previously with ASCA and other missions. We find that a simple power law fails to describe the full spectral range of 0.4-40 keV, and instead a power-law with an exponential cutoff with a hard index of Gamma = 1.50 +/- 0.09 and a high-energy cutoff of epsilon(c) = 1.2 +/- 0.3 keV formally provides an excellent fit over the full bandpass. If we use the so-called SRCUT model, as an alternative model, it gives a best-fit rolloff energy of epsilon(roll) = 0.95 +/- 0.04 keV. Together with the TeV gamma-ray spectrum, ranging from 0.3 to 100 TeV, recently obtained by HESS observations, our Suzaku observations of RX J1713.7-3946 provide stringent constraints on the highest-energy particles accelerated in a supernova shock., OXFORD UNIV PRESS
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Feb. 2008, [Reviewed]

Environmental tests of the flight GLAST LAT tracker towers
Bagagli, R.; Baldini, L.; Bellazzini, R.; Barbiellini, G.; Belli, F.; Borden, T.; Brez, A.; Brigida, M.; Caliandro, G. A.; Cecchi, C.; Cohen-Tanugi, J.; de Angelis, A.; Drell, P.; Favuzzi, C.; Fusco, P.; Gargano, F.; Germani, S.; Giglietto, N.; Giordano, F.; Goodman, J.; Himel, T.; Hirayama, M.; Johnson, R. P.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kroeger, W.; Ku, J.; Kuss, M.; Latronico, L.; Longo, F.; Loparco, F.; Lubrano, P.; Marangelli, B.; Marcucci, F.; Marchetti, M.; Massai, M. M.; Mazziotta, M. N.; Minori, M.; Minuti, M.; Mirizzi, N.; Mongelli, M.; Monte, C.; Morselli, A.; Nelson, D.; Nordby, M.; Omodei, N.; Pepe, M.; Pesce-Rollins, M.; Rainò, S.; Rando, R.; Razzano, M.; Rich, D.; Scolieri, G.; Sgrò, C.; Spandre, G.; Spinelli, P.; Sugizaki, M.; Takahashi, H.; Tenze, A.; Young, C., The Gamma-ray Large Area Space telescope (GLAST) is a gamma-ray satellite scheduled for launch in 2008. Before the assembly of the Tracker subsystem of the Large Area Telescope (LAT) science instrument of GLAST, every component (tray) and module (tower) has been subjected to extensive ground testing required to ensure successful launch and on-orbit operation. This paper describes the sequence and results of the environmental tests performed on an engineering model and all the flight hardware of the GLAST LAT Tracker. Environmental tests include vibration testing, thermal cycles and thermal-vacuum cycles of every tray and tower as well as the verification of their electrical performance....
Nuclear Instruments and Methods in Physics Research A, Jan. 2008

Oxygen line mapping of SN 1006 with Suzaku
Bamba, Aya; Yamaguchi, Hiroya; Koyama, Katsuji; Hiraga, Junko S.; Holt, Steve; Hughes, John P.; Katagiri, Hideaki; Kataoka, Jun; Katsuda, Satoru; Kitamoto, Shunji; Kokubun, Motohide; Matsumoto, Hironori; Miyata, Emi; Mori, Koji; Nakajima, Hiroshi; Ozaki, Masanobu; Petre, Rob; Sekiguchi, Akiko; Takahashi, Tadayuki; Tanaka, Takaaki; Terada, Yukikatsu; Tomida, Hiroshi; Tsuboi, Yohko; Tsujimoto, Masahiro; Tsunemi, Hiroshi; Uchiyama, Yasunobu; Ueno, Masaru; Watanabe, Shin, SN 1006 is one of the supernova remnants (SNRs) with relatively low-temperature electrons, considering the young age of just 1000 years. We carried out SN 1006 mapping observations with the X-ray Imaging Spectrometers (XIS) and the Hard X-ray Detector (HXD) onboard Suzaku, the fifth Japanese X-ray satellite. Thanks to the excellent spectral resolution of XIS in the soft X-ray band, H-like and He-like oxygen emission lines were clearly detected, and we could make a map of the line intensity, and as well as a flux and the photon index of nonthermal component. We found that these parameters have spatial dependences from region to region in the SNR; the north region is bright in nonthermal, while dim in thermal; the east region is bright in both nonthermal and thermal; the inner region shows dim nonthermal and bright thermal emission. The photon index is the smallest in the north region....
Advances in Space Research, 2008, [Reviewed]

Hard X-ray Imager (HXI) for the NeXT mission
Motohide Kokubun; Kazuhiro Nakazawa; Shin Watanabe; Yasushi Fukazawa; Jun Kataoka; Hideaki Katagiri; Tsunefumi Mizuno; Kazuo Makishima; Masanori Ohno; Goro Sato; Rie Sato; Hiroyasu Tajima; Tadayuki Takahashi; Toru Tamagawa; Takaaki Ta Na Ka; Makoto Tashiro; Hiromitsu Takahashi; Yukikatsu Terada; Yasunobu Uchiyama; Yuji Urata; Kazutaka Yamaoka; Shin'ichiro Takeda; Tetsuichi Kishishita; Masayoshi Ushio; Jun'ichiro Katsuta; Shin'nosuke Ishikawa; Hirokazu Odaka; Hiroyuki Aono; Souichiro Sugimoto; Yuu Koseki; Takao Kitaguchi; Teruaki Enoto; Shin'ya Yamada; Takayuki Yuasa; Tsuyoshi Ueda; Yuichi Uehara; Sho Okuyama; Hajimu Yasuda; Sho Nishino; Yudai Umeki; Katsuhiro Hayashi; Masayuki Matsuoka; Yuki Ikejiri; Akira Endo; Yuichi Yaji; Natsuki Kodaka; Wataru Iwakiri; Tomomi Kouzu; Takako Sugasawara; Atsushi Harayama; Satoshi Nakahira, The Hard X-ray Imager (HXI) is one of three focal plane detectors on board the NeXT (New exploration X-ray Telescope) mission, which is scheduled to be launched in 2013. By use of the hybrid structure composed of double-sided silicon strip detectors and a cadmium telluride strip detector, it fully covers the energy range of photons collected with the hard X-ray telescope up to 80 keV with a high quantum efficiency. High spatial resolutions of 400 micron pitch and energy resolutions of 1-2 keV (FWMH) are at the same time achieved with low noise front-end ASICs. In addition, thick BGO active shields compactly surrounding the main detection part, as a heritage of the successful performance of the Hard X-ray Detector (HXD) on board Suzaku satellite, enable to achive an extremely high background reduction for the cosmic-ray particle background and in-orbit activation. The current status of hardware development including the design requirement, expected performance, and technical readinesses of key technologies are summarized.
Proceedings of SPIE - The International Society for Optical Engineering, 2008, [Reviewed]

Design and initial tests of the Tracker-converter of the Gamma-ray Large Area Space Telescope
Atwood, W. B.; Bagagli, R.; Baldini, L.; Bellazzini, R.; Barbiellini, G.; Belli, F.; Borden, T.; Brez, A.; Brigida, M.; Caliandro, G. A.; Cecchi, C.; Cohen-Tanugi, J.; De Angelis, A.; Drell, P.; Favuzzi, C.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Germani, S.; Giannitrapani, R.; Giglietto, N.; Giordano, F.; Himel, T.; Hirayama, M.; Johnson, R. P.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kroeger, W.; Kuss, M.; Latronico, L.; Longo, F.; Loparco, F.; Lubrano, P.; Massai, M. M.; Mazziotta, M. N.; Minuti, M.; Mizuno, T.; Morselli, A.; Nelson, D.; Nordby, M.; Ohsugi, T.; Omodei, N.; Ozaki, M.; Pepe, M.; Rainò, S.; Rando, R.; Razzano, M.; Rich, D.; Sadrozinski, H. F. -W.; Scolieri, G.; Sgrò, C.; Spandre, G.; Spinelli, P.; Sugizaki, M.; Tajima, H.; Takahashi, H.; Takahashi, T.; Yoshida, S.; Young, C.; Ziegler, M., The Tracker subsystem of the Large Area Telescope (LAT) science instrument of the Gamma-ray Large Area Space Telescope (GLAST) mission has been completed and tested. It is the central detector subsystem of the LAT and serves both to convert an incident gamma-ray into an electron-positron pair and to track the pair in order to measure the gamma-ray direction. It also provides the principal trigger for the LAT. The Tracker uses silicon strip detectors, read out by custom electronics, to detect charged particles. The detectors and electronics are packaged, along with tungsten converter foils, in 16 modular, high-precision carbon-composite structures. It is the largest silicon-strip detector system ever built for launch into space, and its aggressive design emphasizes very low power consumption, passive cooling, low noise, high efficiency, minimal dead area, and a structure that is highly transparent to charged particles. The test program has demonstrated that the system meets or surpasses all of its performance specifications as well as environmental requirements. It is now installed in the completed LAT, which is being prepared for launch in early 2008....
Astroparticle Physics, Dec. 2007

Construction, test and calibration of the GLAST silicon tracker
Sgrò, C.; Atwood, W. B.; Baldini, L.; Barbiellini, G.; Bellazzini, R.; Belli, F.; Bonamente, E.; Borden, T.; Bregeon, J.; Brez, A.; Brigida, M.; Caliandro, G. A.; Cecchi, C.; Cohen-Tanugi, J.; de Angelis, A.; Drell, P.; Favuzzi, C.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Germani, S.; Giglietto, N.; Giordano, F.; Himel, T.; Hirayama, M.; Johnson, R. P.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kroeger, W.; Kuss, M.; Latronico, L.; Longo, F.; Loparco, F.; Lubrano, P.; Massai, M. M.; Mazziotta, M. N.; Minuti, M.; Mizuno, T.; Morselli, A.; Nelson, D.; Nordby, M.; Ohsugi, T.; Omodei, N.; Ozaki, M.; Pepe, M.; Rainò, S.; Rando, R.; Razzano, M.; Rich, D.; Sadrozinski, H. F. -W.; Scolieri, G.; Spandre, G.; Spinelli, P.; Sugizaki, M.; Tajima, H.; Takahashi, H.; Takahashi, T.; Yoshida, S.; Young, C.; Ziegler, M., The Gamma-ray Large Area Space Telescope represents a great advance in space application of silicon detectors. With a surface of 80m and about 1 M readout channels it is the largest silicon tracker ever built for a space experiment. GLAST is an astro-particle mission that will study the mostly unexplored, high energy (20 MeV 300 GeV) spectrum coming from active sources or diffused in the Universe. The detector integration and test phase is complete. The full instrument underwent environmental testing and the spacecraft integration phase has just started: the launch is foreseen in late 2007. In the meanwhile the spare modules are being used for instrument calibration and performance verification employing the CERN accelerator complex. A Calibration Unit has been exposed to photon, electron and hadron beams from a few GeV up to 300 GeV. We report on the status of the instrument and on the calibration campaign....
Nuclear Instruments and Methods in Physics Research A, Dec. 2007

CANGAROO-III Search for Gamma Rays from SN 1987A and the Surrounding Field
Enomoto, R.; Bicknell, G. V.; Clay, R. W.; Edwards, P. G.; Gunji, S.; Hara, S.; Hattori, T.; Hayashi, S.; Higashi, Y.; Hirai, Y.; Inoue, K.; Kabuki, S.; Kajino, F.; Katagiri, H.; Kawachi, A.; Kifune, T.; Kiuchi, R.; Kubo, H.; Kushida, J.; Mizukami, T.; Mizuniwa, R.; Mori, M.; Muraishi, H.; Naito, T.; Nakamori, T.; Nakano, S.; Nishida, D.; Nishijima, K.; Ohishi, M.; Sakamoto, Y.; Seki, A.; Stamatescu, V.; Suzuki, T.; Swaby, D. L.; Tanimori, T.; Thornton, G.; Tokanai, F.; Tsuchiya, K.; Watanabe, S.; Yamada, Y.; Yamazaki, E.; Yanagita, S.; Yoshida, T.; Yoshikoshi, T.; Yukawa, Y., Optical images of SN 1987A show a triple-ring structure. The inner (dust) ring has recently increased in brightness and in the number of hot spots, suggesting that the supernova shock wave has collided with the dense preexisting circumstellar medium, a scenario supported by radio and X-ray observations. Such a shocked environment is widely expected to result in the acceleration of charged particles and the accompanying emission of very high energy gamma-rays. Here we report the results of observations made in 2004 and 2006, yielding upper limits on the TeV gamma-ray flux, which are compared with a theoretical prediction. In addition, we set upper limits on the TeV flux for four high-energy objects which are located within the same field of view of the observation: the superbubble 30 Dor C, the Crab-like pulsar PSR B0540-69, the X-ray binary LMC X-1, and the supernova remnant N157B....
The Astrophysical Journal, Dec. 2007, [Reviewed]

CANGAROO III Search for Gamma Rays from Centaurus A and the ω Centauri Region
Kabuki, S.; Enomoto, R.; Bicknell, G. V.; Clay, R. W.; Edwards, P. G.; Gunji, S.; Hara, S.; Hattori, T.; Hayashi, S.; Higashi, Y.; Inoue, R.; Itoh, C.; Kajino, F.; Katagiri, H.; Kawachi, A.; Kawasaki, S.; Kifune, T.; Kiuchi, R.; Konno, K.; Kubo, H.; Kushida, J.; Matsubara, Y.; Mizukami, T.; Mizuniwa, R.; Mori, M.; Muraishi, H.; Naito, T.; Nakamori, T.; Nishida, D.; Nishijima, K.; Ohishi, M.; Sakamoto, Y.; Stamatescu, V.; Suzuki, S.; Suzuki, T.; Swaby, D. L.; Tanimori, T.; Thornton, G.; Tokanai, F.; Tsuchiya, K.; Watanabe, S.; Yamada, Y.; Yamazaki, M.; Yanagita, S.; Yoshida, T.; Yoshikoshi, T.; Yuasa, M.; Yukawa, Y., We have observed the giant radio galaxy Centaurus A and the globular cluster ω Centauri in the TeV energy region using the CANGAROO III stereoscopic system. The system has been in operation since 2004 with an array of four Imaging Atmospheric Cerenkov Telescopes (IACT) with ~100 m spacings. The observations were carried out in 2004 March and April. In total, approximately 10 hr of data were obtained for each target. No statistically significant gamma-ray signal has been found above 420 GeV over a wide angular region (a 1° radius from the pointing center), and we derive flux upper limits using the wholefield of view. Implications for the total energy of cosmic rays and the density of the cold dark matter are considered....
The Astrophysical Journal, Oct. 2007, [Reviewed]

Suzaku Observations of HESS J1616-508 : Evidence for a Dark Particle Accelerator
Matsumoto Hironori; Ueno Masaru; Bamba Aya; HYODO Yoshiaki; MORI Hideyuki; UCHIYAMA Hideki; TSURU Takeshi Go; KOYAMA Katsuji; KATAOKA Jun; KATAGIRI Hideaki; TAKAHASHI Tadayuki; HIRAGA Junko; YAMAUCHI Shigeo; HUGHES John P.; SENDA Atsushi; KOKUBUN Motohide; KOHMURA Takayoshi; PORTER Frederick S., We observed the bright unidentified TeV γ -ray source HESS J1616-508 with the X-ray Imaging Spectrometers onboard the Suzaku satellite. No X-ray counterpart was found to a limiting flux of 3.1 × 10-13 erg s-1 cm-2 in the 2–10 keV band, which is some 60-times below the γ -ray flux in the 1–10 TeV band. This object is bright in TeV γ -rays, but very dim in the X-ray band, and thus is one of the best examples in the Galaxy of a "dark particle accelerator." We also detected soft thermal emission with kT ∼ 0.3–0.6keV near the location of HESS J1616-508. This may be due to a dust-grain scattering halo from the nearby bright supernova remnant RCW 103., 日本天文学会
PASJ : publications of the Astronomical Society of Japan, 31 Jan. 2007, [Reviewed]

The X-Ray Observatory Suzaku
Mitsuda Kazuhisa; Bautz Mark; Inoue Hajime; KELLEY Richard. L.; KOYAMA Katsuji; KUNIEDA Hideyo; MAKISHIMA Kazuo; OGAWARA Yoshiaki; PETRE Robert; TAKAHASHI Tadayuki; TSUNEMI Hiroshi; WHITE Nicholas E.; ANABUKI Naohisa; ANGELINI Lorella; ARNAUD Keith; AWAKI Hisamitsu; BAMBA Aya; BOYCE Kevin; BROWN Gregory V.; CHAN Kai-Wing; COTTAM Jean; DOTANI Tadayasu; DOTY John; EBISAWA Ken; EZOE Yuichiro; FABIAN Andrew C.; FIGUEROA Enectali; FUJIMOTO Ryuichi; FUKAZAWA Yasushi; FURUSHO Tae; FURUZAWA Akihiro; GENDREAU Keith; GRIFFITHS Richard E.; HABA Yoshito; HAMAGUCHI Kenji; HARRUS Ilana; HASINGER Gunther; HATSUKADE Isamu; HAYASHIDA Kiyoshi; HENRY Patrick J.; HIRAGA Junko S.; HOLT Stephen S.; HORNSCHEMEIER Ann; HUGHES John P.; HWANG Una; ISHIDA Manabu; ISHISAKI Yoshitaka; ISOBE Naoki; ITOH Masayuki; IYOMOTO Naoko; KAHN Steven M.; KAMAE Tuneyoshi; KATAGIRI Hideaki; KATAOKA Jun; KATAYAMA Haruyoshi; KAWAI Nobuyuki; KILBOURNE Caroline; KINUGASA Kenzo; KISSEL Steve; KITAMOTO Shunji; KOHAMA Mitsuhiro; KOHMURA Takayoshi; KOKUBUN Motohide; KOTANI Taro; KOTOKU Jun'ichi; KUBOTA Aya; MADEJSKI Greg M.; MAEDA Yoshitomo; MAKINO Fumiyoshi; MARKOWITZ Alex; MATSUMOTO Chiho; MATSUMOTO Hironori; MATSUOKA Masaru; MATSUSHTIA Kyoko; MCCAMMON Dan; MIHARA Tatehiko; MISAKI Kazutami; MIYATA Emi; MIZUNO Tsunefumi; MORI Koji; MORI Hideyuki; MORII Mikio; MOSELEY Harvey; MUKAI Koji; MURAKAMI Hiroshi; MURAKAMI Toshio; MUSHOTZKY Richard; NAGASE Fumiaki; NAMIKI Masaaki; NEGORO Hitoshi; NAKAZAWA Kazuhiro; NOUSEK John A.; OKAJIMA Takashi; OGASAKA Yasushi; OHASHI Takaya; OSHIMA Tai; OTA Naomi; OZAKI Masanobu; OZAWA Hideki; PARMAR Arvind N.; PENCE William D.; PORTER F. Scott; REEVES James N.; RICKER George R.; SAKURAI Ikuya; SANDERS Wilton T.; SENDA Atsushi; SERLEMITSOS Peter; SHIBATA Ryo; SOONG Yang; SMITH Randall; SUZUKI Motoko; SZYMKOWIAK Andrew E.; TAKAHASHI Hiromitsu; TAMAGAWA Toru; TAMURA Keisuke; TAMURA Takayuki; TANAKA Yasuo; TASHIRO Makoto; TAWARA Yuzuru; TERADA Yukikatsu; TERASHIMA Yuichi; TOMIDA Hiroshi; TORII Ken'ichi; TSUBOI Yohko; TSUJIMOTO Masahiro; TSURU Takeshi Go; TURNER Martin J. L.; UEDA Yoshihiro; UENO Shiro; UENO Masaru; UNO Shin'ichiro; URATA Yuji; WATANABE Shin; YAMAMOTO Norimasa; YAMAOKA Kazutaka; YAMASAKI Noriko Y.; YAMASHITA Koujun; YAMAUCHI Makoto; YAMAUCHI Shigeo; YAQOOB Tahir; YONETOKU Daisuke; YOSHIDA Atsumasa, High-sensitivity wide-band X-ray spectroscopy is the key feature of the Suzaku X-ray observatory, launched on 2005 July 10. This paper summarizes the spacecraft, in-orbit performance, operations, and data processing that are related to observations. The scientific instruments, the high-throughput X-ray telescopes, X-ray CCD cameras, non-imaging hard X-ray detector are also described., Astronomical Society of Japan
PASJ : publications of the Astronomical Society of Japan, 31 Jan. 2007, [Reviewed]

GLAST simulation study of an extended TeV-emitting supernova remnant for the origin of cosmic-ray nuclei
H. Katagiri; H. Yoshida; T. Mizuno; H. Takahashi; Y. Fukazawa; T. Ohsugi, We extracted the gamma-ray emission of the π°-decay, which will be a decisive evidence of cosmic-ray proton acceleration, from the one-year data of an extended TeV-emitting supernova remnant, generated by the GLAST full detector simulation, although many assumptions were oversimplified. © 2007 American Institute of Physics.
AIP Conference Proceedings, 2007, [Reviewed]

Evidence of TeV gamma-ray emission from the nearby starburst galaxy NGC 253
Itoh, C.; Enomoto, R.; Yanagita, S.; Yoshida, T.; Asahara, A.; Bicknell, G. V.; Clay, R. W.; Edwards, P. G.; Gunji, S.; Hara, S.; Hara, T.; Hattori, T.; Hayashi, Shin.; Hayashi, Sei.; Kabuki, S.; Kajino, F.; Katagiri, H.; Kawachi, A.; Kifune, T.; Kubo, H.; Kushida, J.; Matsubara, Y.; Mizumoto, Y.; Mori, M.; Moro, H.; Muraishi, H.; Muraki, Y.; Naito, T.; Nakase, T.; Nishida, D.; Nishijima, K.; Okumura, K.; Ohishi, M.; Patterson, J. R.; Protheroe, R. J.; Sakurazawa, K.; Swaby, D. L.; Tanimori, T.; Tokanai, F.; Tsuchiya, K.; Tsunoo, H.; Uchida, T.; Watanabe, A.; Watanabe, S.; Yoshikoshi, T., Aims:The CANGAROO-II telescope observed sub-TeV gamma-ray emission from the nearby starburst galaxy NGC 253. The emission region was extended with a radial size of 0.3-0.6 degree. On the contrary, HESS could not confirm this emission and gave upper limits at the level of the CANGAROO-II flux. In order to resolve this discrepancy, we analyzed new observational results for NGC 253 by CANGAROO-III and also assessed the results by CANGAROO-II.
Methods: Observation was made with three telescopes of the CANGAROO-III in October 2004. We analyzed three-fold coincidence data by the robust Fisher Discriminant method to discriminate gamma ray events from hadron events.
Results: The result by the CANGAROO-III was negative. The upper limit of gamma ray flux was 5.8% Crab at 0.58 TeV for point-source assumption. In addition, the significance of the excess flux of gamma-rays by the CANGAROO-II was lowered to less than 4 sigma after assessing treatment of malfunction of photomultiplier tubes....
Astronomy and Astrophysics, Jan. 2007

Simultaneous observation of the gamma-ray binary LS I+61 303 with GLAST and Suzaku
Takuya Tanaka; Yasushi Fukazawa; Tsunefumi Mizuno; Hideaki Katagiri; Hiromitsu Takahashi; Koji S. Kawabata; Osamu Nagae; Takashi Ohsugi, The gamma-ray binary LS I+61 303 is a bright gamma-ray source, and thus an attracting object for GLAST. We proposed to observe this object with the X-ray satellite Suzaku (AO-2), simultaneously with GLAST, radio wave, and optical spectro-polarimetry, in order to probe the geometrical state of the binary system emitting the gamma-ray radiation, as a function of the binary orbital phase for the first time. This is essential to understand the mechanism of jet production and gamma-ray emission. The idea is not only to measure the multi-band overall continuum shape, but also to make use of continuous monitoring capability of GLAST, wide X-ray band of Suzaku, and good accessibility of the Kanata optical/NIR telescope (Hiroshima University) with the sensitive optical spectro-polarimetry. Further collaboration with TeV gamma-ray telescopes is also hoped to constrain the jet constitution. © 2007 American Institute of Physics.
AIP Conference Proceedings, 2007, [Reviewed]

Multi-wavelength observations of galactic microquasars
Hiromitsu Takahashi; Hiroaki Yoshida; Hideaki Katagiri; Tsunefumi Mizuno; Yasushi Fukazawa; Takashi Ohsugi; Makoto Uemura, Recent observations reveal ∼ 20 microquasars with astrophysical jets in our Galaxy. However, the generation mechanism or the composition (i.e. hadronic/leptonic) of the jet is still unclear, as well as those of active galactic nuclei. Multi-wavelength observations are the key to detect the synchrotron and inverse-Compton (as well as π0-decay) emission from the jets. The Gamma-ray Large Area Space Telescope (GLAST) has unprecedented sensitivity, and will provide us the opportunities to study the gamma-rays from the microquasars. Through the survey observation of GLAST, there are also possibilities to reveal unidentified EGRET sources as new microquasars in our Galaxy. As an example of X-ray observations, arecent Suzaku observation of a microquasar GRO J1655-40 is exemplified. © 2007 American Institute of Physics.
AIP Conference Proceedings, 2007, [Reviewed]

Suzaku observation of TeV SNR RX J1713.7-3946
Tadayuki Takahashi; Takaaki Tanaka; Yasunobu Uchiyama; Junko S. Hiraga; Kazuhiro Nakazawa; Shin Watanabe; Aya Bamba; John P. Hughes; Hideaki Katagiri; Jun Kataoka; Motohide Kokubun; Katsuji Koyama; Koji Mopa; Robert Petre; Hiromitsu Takahashi; Yoko Tsub, We report on results from Suzaku broadband X-ray observations of the Galactic supernova, remnant (SNR) RX J1713.7-3946 with an energy coverage of 0.4-40 keV. With a sensitive hard X-ray measurement from the HXD PIN on board Suzaku, we determine the hard X-ray spectrum in the 12-40 keV range to be described by a power law with photon index Gamma = 3.2 +/- 0.2, significantly steeper than the soft X-ray index of Gamma = 2.4 +/- 0.05 measured previously with ASCA and other missions. We find that a simple power law fails to describe the full spectral range of 0.4-40 keV and instead a cutoff power law with bard index Gamma = 1.96 +/- 0.05 and high energy cutoff epsilon(c) = 9 +/- 1 keV provides an excellerit fit over the full bandpass., PROGRESS THEORETICAL PHYSICS PUBLICATION OFFICE
PROGRESS OF THEORETICAL PHYSICS SUPPLEMENT, 2007

Millenium study of SN 1006 with suzaku
Aya Bamba; Hiroya Yamaguchi; Katsuji Koyama; Junko S. Hiraga; Steve Holt; John P. Hughes; Hideaki Katagiri; Jun Kataoka; Shunji Kitamoto; Motohide Kokubun; Hironori Matumoto; Emi Miyata; Koji Mori; Hiroshi Nakajima; Masanobu Ozaki; Robert Petre; Akiko Sekiguchi; Tadayuki Takahashi; Takaaki Tanaka; Yukikatsu Terada; Hiroshi Tomida; Hiroshi Tsunemi; Yohko Tsub; Masahiro Tsujimoto; Yasunobu Uchiyama; Masaru Ueno; Shin Watanabe, SN 1006 is the milestone of understanding the acceleration mechanism of cosmic rays, and this year is the millennium year for the remnant. We carried out SN 1006 mapping observations with the X-ray Imaging Spectrometers (XIS) onboard Suzaku satellite. Thanks to the excellent spectral response of XIS, K emission lines from highly ionized oxygen were clearly resolved. The intensity maps of these lines have been made additional to the intensity and photon index maps of the nonthermal component. We discovered that regions with strong and hard nonthermal component has weak thermal emission. The north rim of the SNR has the hardest nonthermal component. These facts might have information of efficient cosmic ray acceleration and background plasma., PROGRESS THEORETICAL PHYSICS PUBLICATION OFFICE
PROGRESS OF THEORETICAL PHYSICS SUPPLEMENT, 2007

Development of a Pixel-Readout μ-PIC (Micro Pixel Chamber) for X-ray Polarimetry
Katagiri; H. et al., Lead, We developed a pixel-readout micro-pixel chamber (mu-PIC) as an astronomical X-ray polarimeter and demonstrated its ability to achieve a higher sensitivity than a strip-readout one by a beam test. The mu-PIC is one of the micropattern gas detectors that have been developed so far. However, its readout was of the strip type. This limits the sensitivity to polarization because it cannot determine the polarization angle uniquely without rotating the detector. Thus, we started developing the pixel-readout type of mu-PIC. A beam test at a synchrotron-radiation facility was carried out to examine the performance for polarimetry. Without rotating the detector, we successfully detected the polarization angle. The modulation factor for 8 keV X-rays in a neon-based mixture was 0.12 +/- 0.03, which is at the same level as that of the strip-type mu-PIC, and 0.07 +/- 0.01 at 15 keV in an argon-based mixture. These results indicate the ability of the new mu-PIC to achieve a higher sensitivity to X-ray polarization than that obtainable with the strip-type mu-PIC., INST PURE APPLIED PHYSICS
Jpn. J. Appl. Phys., 2007, [Reviewed]

Performance of Pixel-Readout Micro-Pixel Chamber with Analog-Readout System Used as X-ray Polarimeter
Katagiri; H. et al., Lead, We developed an analog-readout system for a pixel-readout micro-pixel chamber (mu-PIC) to be used as an astronomical X-ray polarimeter, and demonstrated that the sensitivity of the new system reached up to that predicted by a simulation. A pixel-readout mu-PIC is a micro-pattern gaseous detector with a fine position resolution and good stability at sufficient gain operation, and is suited for astronomical X-ray polarimetry. However, as shown by Katagiri et al. (2007), the sensitivity to X-ray polarization was found to be statistically lower by a significant amount than that expected from the simulation of Ueno et al. [Nucl. Instrum. Methods Phys. Res., Sect. A 525 (2004) 28] because of the readout system and background produced by the scattering of the X-ray beam in air. We therefore developed a new readout system and carried out a beam test with aluminum tubes that reduced the background. As a result, we demonstrated that for collimated beams, the modulation factors, which are indicators of the sensitivity to X-ray polarization, were 0.24 +/- 0.08 at 8 keV and 0.18 +/- 0.07 at 15 keV in a neon-based gas mixture, and 0.18 +/- 0.04 at 15 keV in an argon-based mixture. These values are consistent with those predicted by the simulation within errors., INST PURE APPLIED PHYSICS
Jpn. J. Appl. Phys., 2007, [Reviewed]

CANGAROO III observations of the supernova remnant rx j0852.0-4622
R. Enomoto; S. Watanabe; T. Tanimori; A. Asahara; G. V. Bicknell; R. W. Clay; P. G. Edwards; S. Gunji; S. Hara; T. Hattori; S. Hayashi; Y. Higashi; R. Inoue; C. Itoh; S. Kabuki; F. Kajino; H. Katagiri; A. Kawachi; S. Kawasaki; T. Kifune; R. Kiuchi; K. Konno; L. Ksenofontov; H. Kubo; J. Kushida; Y. Matsubara; T. Mizukami; R. Mizuniwa; M. Mori; H. Muraishi; T. Naito; T. Nakamori; D. Nishida; K. Nishijima; M. Ohishi; Y. Sakamoto; V. Stamatescu; S. Suzuki; T. Suzuki; D. L. Swaby; H. Tanimura; G. Thornton; F. Tokanai; K. Tsuchiya; Y. Yamada; M. Yamazaki; S. Yanagita; T. Yoshida; T. Yoshikoshi; M. Yuasa; Y. Yukawa, Sub-TeV gamma-ray emission from the northwest rim of the supernova remnant RX J0852.0-4622 was detected with the CANGAROO II telescope and recently confirmed by the HESS group. In addition, the HESS data revealed a very wide (up to 2 degrees in diameter), shell-like profile of the gamma-ray emission. We carried out CANGAROO III observations in 2005 January and February with three telescopes and show here the results of threefold coincidence data. We confirm the HESS results about the morphology and the energy spectrum and find that the energy spectrum in the NW rim is consistent with that of the whole remnant., UNIV CHICAGO PRESS
ASTROPHYSICAL JOURNAL, Dec. 2006, [Reviewed]

Development of the x-ray polarimeter by using pixel-readout mu-PICs (micro pixel chambers)
Katagiri, Hideaki; Ono, Kenichi; Uchiyama, Hideki; Tsuru, Takeshi; Matsumoto, Hironori; Ueno, Masaru; Nagayoshi, Tsutomu; Hyodo, Yosiaki; Tanimori, Toru; Miuchi, Kentaro; Kubo, Hidetoshi
Proceedings of the SPIE, Jun. 2006

A Search for Sub-TeV Gamma Rays from the Vela Pulsar Region with CANGAROO-III
Enomoto, R.; Tsuchiya, K.; Adachi, Y.; Kabuki, S.; Edwards, P. G.; Asahara, A.; Bicknell, G. V.; Clay, R. W.; Doi, Y.; Gunji, S.; Hara, S.; Hara, T.; Hattori, T.; Hayashi, Sei.; Higashi, Y.; Inoue, R.; Itoh, C.; Kajino, F.; Katagiri, H.; Kawachi, A.; Kawasaki, S.; Kifune, T.; Kiuchi, R.; Konno, K.; Ksenofontov, L. T.; Kubo, H.; Kushida, J.; Matsubara, Y.; Mizumoto, Y.; Mori, M.; Muraishi, H.; Muraki, Y.; Naito, T.; Nakamori, T.; Nishida, D.; Nishijima, K.; Ohishi, M.; Patterson, J. R.; Protheroe, R. J.; Sakamoto, Y.; Sato, M.; Suzuki, S.; Suzuki, T.; Swaby, D. L.; Tanimori, T.; Tanimura, H.; Thornton, G. J.; Watanabe, S.; Yamaoka, T.; Yamazaki, M.; Yanagita, S.; Yoshida, T.; Yoshikoshi, T.; Yuasa, M.; Yukawa, Y., We made stereoscopic observations of the Vela pulsar region with two of the 10 m diameter CANGAROO-III imaging atmospheric Cerenkov telescopes in 2004 January and February in a search for sub-TeV gamma rays from the pulsar and surrounding regions. We describe the observations, provide a detailed account of the calibration methods, and introduce the improved and bias-free analysis techniques employed for CANGAROO-III data. No evidence of gamma-ray emission is found from either the pulsar position or the previously reported position offset by 0.13d, and the resulting upper limits are a factor of 5 less than the previously reported flux from observations with the CANGAROO-I 3.8 m telescope. Following the recent report by the H.E.S.S. group of TeV gamma-ray emission from the pulsar wind nebula, which is ~0.5d south of the pulsar position, we examined this region and found supporting evidence for emission extended over ~0.6d....
The Astrophysical Journal, Feb. 2006

27aTF-1 Report on the maintenance work and observation of the CANGAROO-III telescopes
Ohishi Michiko; Edwards P.G., The Physical Society of Japan
Meeting Abstracts of the Physical Society of Japan, 2006

Detection of Gamma Rays around 1 TeV from RX J0852.0－4622 by CANGAROO-II
Katagiri; H. et al., Lead, We have detected gamma-ray emission at the 6 sigma level at energies greater than 500 GeV from the supernova remnant RX J0852.0 - 4622 (G266.2 - 1.2) using the CANGAROO-II imaging atmospheric Cerenkov telescope. The flux was 0.12 times that of Crab at 1 TeV. The signal centroid is consistent with the peak of the X-ray emission in the northwest rim of the remnant., UNIV CHICAGO PRESS
The Astrophysical Journal, 2005, [Reviewed]

A Search for TeV Gamma-Ray Emission from the PSR B1259-63/SS 2883 Binary System with the CANGAROO-II 10 Meter Telescope
Kawachi, A.; Naito, T.; Patterson, J. R.; Edwards, P. G.; Asahara, A.; Bicknell, G. V.; Clay, R. W.; Enomoto, R.; Gunji, S.; Hara, S.; Hara, T.; Hattori, T.; Hayashi, Seuchi; Hayashi, Shin'ichiro; Itoh, C.; Kabuki, S.; Kajino, F.; Katagiri, H.; Kifune, T.; Ksenofontov, L.; Kubo, H.; Kushida, J.; Matsubara, Y.; Mizumoto, Y.; Mori, M.; Moro, H.; Muraishi, H.; Muraki, Y.; Nakase, T.; Nishida, D.; Nishijima, K.; Ohishi, M.; Okumura, K.; Protheroe, R. J.; Sakurazawa, K.; Swaby, D. L.; Tanimori, T.; Tokanai, F.; Tsuchiya, K.; Tsunoo, H.; Uchida, T.; Watanabe, A.; Watanabe, S.; Yanagita, S.; Yoshida, T.; Yoshikoshi, T., Observations of the PSR B1259-63/SS 2883 binary system using the CANGAROO-II Cerenkov telescope are reported. This nearby binary consists of a 48 ms radio pulsar in a highly eccentric orbit around a Be star and offers a unique laboratory to investigate the interactions between the outflows of the pulsar and Be star at various distances. It has been pointed out that the relativistic pulsar wind and the dense mass outflow of the Be star may result in the emission of gamma rays up to TeV energies. We have observed the binary in 2000 and 2001, ~47 and ~157 days after the 2000 October periastron. Upper limits at the 0.13-0.54 crab level are obtained. A new model calculation for high-energy gamma-ray emission from the Be star outflow is introduced, and the estimated gamma-ray flux, considering bremsstrahlung, inverse Compton scattering, and the decay of neutral pions produced in proton-proton interactions, is found to be comparable to the upper limits of these observations. Comparing our results with these model calculations, we constrain the mass-outflow parameters of the Be star....
The Astrophysical Journal, Jun. 2004, [Reviewed]

Detection of Sub-TeV Gamma Rays from the Galactic Center Direction by CANGAROO-II
Tsuchiya, K.; Enomoto, R.; Ksenofontov, L. T.; Mori, M.; Naito, T.; Asahara, A.; Bicknell, G. V.; Clay, R. W.; Doi, Y.; Edwards, P. G.; Gunji, S.; Hara, S.; Hara, T.; Hattori, T.; Hayashi, Sei.; Itoh, C.; Kabuki, S.; Kajino, F.; Katagiri, H.; Kawachi, A.; Kifune, T.; Kubo, H.; Kurihara, T.; Kurosaka, R.; Kushida, J.; Matsubara, Y.; Miyashita, Y.; Mizumoto, Y.; Moro, H.; Muraishi, H.; Muraki, Y.; Nakase, T.; Nishida, D.; Nishijima, K.; Ohishi, M.; Okumura, K.; Patterson, J. R.; Protheroe, R. J.; Sakamoto, N.; Sakurazawa, K.; Swaby, D. L.; Tanimori, T.; Tanimura, H.; Thornton, G.; Tokanai, F.; Uchida, T.; Watanabe, S.; Yamaoka, T.; Yanagita, S.; Yoshida, T.; Yoshikoshi, T., We have detected sub-TeV gamma-ray emission from the direction of the Galactic center (GC) using the CANGAROO-II Imaging Atmospheric Cerenkov Telescope. We detected a statistically significant excess at energies greater than 250 GeV. The flux was 1 order of magnitude lower than that of the Crab Nebula at 1 TeV with a soft spectrum proportional to E^-4.6+/-0.5. The signal centroid is consistent with the GC direction, and the observed profile is consistent with a pointlike source. Our data suggest that the GeV source 3EG J1746-2851 is identical to this TeV source, and we study the combined spectra to determine the possible origin of the gamma-ray emission. We also obtain an upper limit on the cold dark matter density in the Galactic halo....
The Astrophysical Journal, May 2004

Status of the CANGAROO-III project
Kubo, H.; Asahara, A.; Bicknell, G. V.; Clay, R. W.; Doi, Y.; Edwards, P. G.; Enomoto, R.; Gunji, S.; Hara, S.; Hara, T.; Hattori, T.; Hayashi, Sei.; Itoh, C.; Kabuki, S.; Kajino, F.; Katagiri, H.; Kawachi, A.; Kifune, T.; Ksenofontov, L. T.; Kurihara, T.; Kurosaka, R.; Kushida, J.; Matsubara, Y.; Miyashita, Y.; Mizumoto, Y.; Mori, M.; Moro, H.; Muraishi, H.; Muraki, Y.; Naito, T.; Nakase, T.; Nishida, D.; Nishijima, K.; Ohishi, M.; Okumura, K.; Patterson, J. R.; Protheroe, R. J.; Sakamoto, N.; Sakurazawa, K.; Swaby, D. L.; Tanimori, T.; Tanimura, H.; Thornton, G.; Tokanai, F.; Tsuchiya, K.; Uchida, T.; Watanabe, S.; Yamaoka, T.; Yanagita, S.; Yoshida, T.; Yoshikoshi, T., The CANGAROO-III project, which consists of an array of four 10-m atmospheric Cherenkov telescopes for gamma-ray astrophysics, started in 1999 in Woomera, South Australia. The first 10-m telescope has been in operation since 2000, and stereoscopic observations with the first and second telescopes started in 2002. The full array will be operational in 2003. Here we report on the status of the CANGAROO-III project including the results of observations with the first telescope....
New Astronomy Reviews, Apr. 2004

Search for TeV γ-rays from the remnant of SN 1987A
Ksenofontov, L. T.; Enomoto, R.; Katagiri, H.; Tsuchiya, K.; The Cangaroo Collaboration, We searched for TeV γ-rays from the remnant of SN 1987A around 5400 days after the supernova. The observations were carried out in 2001, from November 16 to December 11, using the CANGAROO-II Imaging Atmospheric Cherenkov Telescope. The detection threshold was estimated to be 1 TeV, due to the mean zenith angle of 39°. The upper limits (ULs) for the γ-ray flux were obtained and compared with the previous observations and theoretical models. The observations indicate that the γ-ray luminosity is lower than 10 ³⁷ erg s ^-1 at ̃10 TeV....
New Astronomy Reviews, Apr. 2004, [Reviewed]

A Search for TeV Gamma Rays from SN 1987A in 2001
Enomoto, R.; Ksenofontov, L. T.; Katagiri, H.; Tsuchiya, K.; Asahara, A.; Bicknell, G. V.; Clay, R. W.; Edwards, P. G.; Gunji, S.; Hara, S.; Hara, T.; Hattori, H.; Hayashi, Sei.; Hayashi, Shin.; Itoh, C.; Kabuki, S.; Kajino, F.; Kawachi, A.; Kifune, T.; Kubo, H.; Kushida, J.; Matsubara, Y.; Mizumoto, Y.; Mori, M.; Moro, H.; Muraishi, H.; Muraki, Y.; Naito, T.; Nakase, T.; Nishida, D.; Nishijima, K.; Ohishi, M.; Okumura, K.; Patterson, J. R.; Protheroe, R. J.; Sakurazawa, K.; Swaby, D. L.; Tanimori, T.; Tokanai, F.; Tsunoo, H.; Uchida, T.; Watanabe, A.; Watanabe, S.; Yanagita, S.; Yoshida, T.; Yoshikoshi, T., We searched for TeV gamma rays from the remnant of SN 1987A around 5400 days after the supernova. The observations were carried out in 2001, from November 16 to December 11, using the CANGAROO-II imaging atmospheric Cerenkov telescope. In total, 708 minutes of ON- and 1019 minutes of OFF-source data were obtained under good conditions. The detection threshold was estimated to be 1 TeV, owing to the mean zenith angle of 39°. The upper limits for the gamma-ray flux were obtained and compared with the previous observations and theoretical models. The observations indicate that the gamma-ray luminosity is lower than 1×10³⁷ ergs s^-1 at ~10 TeV....
The Astrophysical Journal, Jul. 2003, [Reviewed]

Evidence of TeV gamma-ray emission from the nearby starburst galaxy NGC 253
Itoh, C.; Enomoto, R.; Yanagita, S.; Yoshida, T.; Tanimori, T.; Okumura, K.; Asahara, A.; Bicknell, G. V.; Clay, R. W.; Edwards, P. G.; Gunji, S.; Hara, S.; Hara, T.; Hattori, T.; Hayashi, Shin.; Hayashi, Sei.; Kabuki, S.; Kajino, F.; Katagiri, H.; Kawachi, A.; Kifune, T.; Kubo, H.; Kushida, J.; Matsubara, Y.; Mizumoto, Y.; Mori, M.; Moro, H.; Muraishi, H.; Muraki, Y.; Naito, T.; Nakase, T.; Nishida, D.; Nishijima, K.; Ohishi, M.; Patterson, J. R.; Protheroe, R. J.; Sakurazawa, K.; Swaby, D. L.; Tokanai, F.; Tsuchiya, K.; Tsunoo, H.; Uchida, T.; Watanabe, A.; Watanabe, S.; Yoshikoshi, T., TeV gamma-rays were recently detected from the nearby normal spiral galaxy NGC 253 (Itoh et al. \cite{Itoh2002}). Observations to detect the Cherenkov light images initiated by gamma-rays from the direction of NGC 253 were carried out in 2000 and 2001 over a total period of ~ 150 hours. The orientation of images in gamma-ray-like events is not consistent with emission from a point source, and the emission region corresponds to a size greater than 10 kpc in radius. Here, detailed descriptions of the analysis procedures and techniques are given....
Astronomy and Astrophysics, May 2003, [Reviewed]

Observation of Gamma Rays Greater than 10 TeV from Markarian 421
Okumura, K.; Asahara, A.; Bicknell, G. V.; Edwards, P. G.; Enomoto, R.; Gunji, S.; Hara, S.; Hara, T.; Hayashi, S.; Itoh, C.; Kabuki, S.; Kajino, F.; Katagiri, H.; Kataoka, J.; Kawachi, A.; Kifune, T.; Kubo, H.; Kushida, J.; Maeda, S.; Maeshiro, A.; Matsubara, Y.; Mizumoto, Y.; Mori, M.; Moriya, M.; Muraishi, H.; Muraki, Y.; Naito, T.; Nakase, T.; Nishijima, K.; Ohishi, M.; Patterson, J. R.; Sakurazawa, K.; Suzuki, R.; Swaby, D. L.; Takano, K.; Takano, T.; Tanimori, T.; Tokanai, F.; Tsuchiya, K.; Tsunoo, H.; Uruma, K.; Watanabe, A.; Yanagita, S.; Yoshida, T.; Yoshikoshi, T., We have observed Markarian 421 in 2001 January and March with the CANGAROO-II imaging Cerenkov telescope during an extraordinarily high state at TeV energies. From 14 hr of observations at very large zenith angles, ∼70°, a signal of 298 ± 52 gamma-ray-like events (5.7 σ) was detected at E > 10 TeV, where a higher sensitivity is achieved than those of usual observations near the zenith, owing to a greatly increased collecting area. Under the assumption of an intrinsic power-law spectrum, we derived a differential energy spectrum dN/dE = (3.3 ± 0.9stat ± 0.3syst) × 10-13(E/10 TeV) -(4.0-0.6+0.9, stat±0.3syst) photons cm-2 s -1 TeV-1, which is steeper than those previously measured around 1 TeV and supports the evidence for a cutoff in the spectrum of Mrk 421. However, the 4 σ excess at energies greater than 20 TeV in our data favors a cutoff energy of ∼8 TeV, at the upper end of the range previously reported from measurements at TeV energies.
The Astrophysical Journal, 01 Nov. 2002

The acceleration of cosmic-ray protons in the supernova remnant RX J1713.7-3946
Enomoto, R.; Tanimori, T.; Naito, T.; Yoshida, T.; Yanagita, S.; Mori, M.; Edwards, P. G.; Asahara, A.; Bicknell, G. V.; Gunji, S.; Hara, S.; Hara, T.; Hayashi, S.; Itoh, C.; Kabuki, S.; Kajino, F.; Katagiri, H.; Kataoka, J.; Kawachi, A.; Kifune, T.; Kubo, H.; Kushida, J.; Maeda, S.; Maeshiro, A.; Matsubara, Y.; Mizumoto, Y.; Moriya, M.; Muraishi, H.; Muraki, Y.; Nakase, T.; Nishijima, K.; Ohishi, M.; Okumura, K.; Patterson, J. R.; Sakurazawa, K.; Suzuki, R.; Swaby, D. L.; Takano, K.; Takano, T.; Tokanai, F.; Tsuchiya, K.; Tsunoo, H.; Uruma, K.; Watanabe, A.; Yoshikoshi, T., Protons with energies up to ~10¹⁵eV are the main component of cosmic rays, but evidence for the specific locations where they could have been accelerated to these energies has been lacking. Electrons are known to be accelerated to cosmic-ray energies in supernova remnants, and the shock waves associated with such remnants, when they hit the surrounding interstellar medium, could also provide the energy to accelerate protons. The signature of such a process would be the decay of pions (π⁰), which are generated when the protons collide with atoms and molecules in an interstellar cloud: pion decay results in γ-rays with a particular spectral-energy distribution. Here we report the observation of cascade showers of optical photons resulting from γ-rays at energies of ~10¹²eV hitting Earth's upper atmosphere, in the direction of the supernova remnant RX J1713.7-3946. The spectrum is a good match to that predicted by pion decay, and cannot be explained by other mechanisms....
Nature, Apr. 2002, [Reviewed]

13aRA-12 CANGAROO-II望遠鏡の観測報告IV(高エネルギーガンマ線,宇宙線)
梶野 文義; 林 清一; 伊藤 千枝; 株木 重人; 片桐 秀明; 河内 明子; 木舟 正; Ksenofontov L.; 窪 秀利; 粟原 工; 黒坂 亮治; 浅原 明広; 櫛田 淳子; 松原 豊; 宮下 靖史; 水本 好彦; 森 正樹; 茂呂 寿子; 村石 浩; 村木 綏; 内藤 統也; 中瀬 友和; 土井 康博; 西田 大輔; 西嶋 恭司; 荻尾 彰一; 大石 理子; 奥村 公宏; 坂本 直樹; さこ 隆志; 桜澤 幸司; 薄田 竜太郎; 田村 忠久; Edwards P.G.; 谷森 達; 谷村 英樹; 門叶 冬樹; 土屋 兼一; 内田 直志; 渡部 至緒; 山岡 知隆; 柳田 昭平; 吉田 龍生; 吉越 貴紀; 榎本 良治; CANGAROOチーム; 郡司 修一; 服部 敬裕; 原 敏; 原 忠生, 一般社団法人 日本物理学会
日本物理学会講演概要集, 2002, [Reviewed]

Design study of CANGAROO-III, stereoscopic imaging atmospheric Cherenkov telescopes for sub-TeV gamma-ray detection
R Enomoto; S Hara; A Asahara; GV Bicknell; PG Edwards; S Gunji; T Hara; J Jimbo; F Kajino; H Katagiri; J Kataoka; A Kawachi; T Kifune; H Kubo; J Kushida; Y Matsubara; Y Mizumoto; M Mori; M Moriya; H Muraishi; Y Muraki; T Naito; T Nakase; K Nishijima; K Okumura; Patterson, JR; K Sakurazawa; DL Swaby; K Takano; T Tanimori; T Tamura; K Tsuchiya; K Uruma; S Yanagita; T Yoshida; T Yoshikoshi; A Yuki, CANGAROO-III is an imaging atmospheric Cherenkov telescope array of four 10-m telescopes for very high energy (sub-TeV) gamma-ray astronomy. A design study of the CANGAROO-III telescope system was carried out using the Monte Carlo technique in order to optimize the pixel size and the telescope spacing. Studies were also made of observations at low elevation angles. (C) 2002 Elsevier Science B.V. All rights reserved., ELSEVIER SCIENCE BV
ASTROPARTICLE PHYSICS, Jan. 2002, [Reviewed]

Measurement of environmental radioactivity in medical facilities using a rotating Compton camera
石川咲貴; 村石浩; 榎本良治; 片桐秀明; 加賀谷美佳; 渡辺宝; 加納大輔; 中村哲志; 渡邉祐介; 石山博條
応用物理学会秋季学術講演会講演予稿集(CD-ROM), 2021

CTA報告151:CTA大口径望遠鏡初号機におけるカメラ集光器の量産と性能評価
鈴木萌; 山本常夏; 吉田龍生; 稲田知大; 猪目祐介; 岩村由樹; 大岡秀行; 岡崎奈緒; 岡知彦; 奥村曉; 折戸玲子; 梶原侑貴; 片桐秀明; 櫛田淳子; 木村颯一朗; 窪秀利; 郡司修一; 小山志勇; 齋藤隆之; 櫻井駿介; 澤田真理; 砂田裕志; 高橋光成; 田中真伸; 田村謙治; 町支勇貴; 辻本晋平; 手嶋政廣; 手嶋政廣; 寺田幸功; 門叶冬樹; 中森健之; 永吉勤; 西嶋恭司; 西山楽; 野崎誠也; 林田将明; 馬場彩; 平子丈; 深見哲志; 古田智也; 増田周; HADASCH Daniela; MAZIN Daniel
日本物理学会講演概要集(CD-ROM), 22 Mar. 2019

CTA Report 147: General Report
Kubo Hidetoshi; Teshima Masahiro; Totani Tomonori; Asano Katsuaki; Asano Akira; Ioka Kunihito; Ishio Kazuma; Inada Tomohiro; Inoue Susumu; Inoue Tsuyoshi; Inoue Yoshiyuki; Inome Yusuke; Iwamura Yuki; Warren Donald; Uchiyama Yasunobu; Ohishi Michiko; Ohoka Hideyuki; Ohtani Yoshiki; Ohira Yutaka; Oka Tomohiko; Okazaki Nao; Ogata Tomoyuki; Okumura Akira; Orito Reiko; Kagaya Mika; Kajiwara Yuki; Kataoka Jun; Katagiri Hideaki; Katsukura Daisuke; Katsuda Satoru; Kamimoto Takumi; Khalikov Emil; Kawanaka Norita; Kisaka Shota; Cui Xiaohong; Kushida Junko; Kumon Taku; Gunji Shuichi; Kohri Kazunori; Kobayashi Yukiho; Kong Albert K. H.; Saito Takayuki; Sakaki Naoto; Sakurai Shunsuke; Sasai Yoshinori; Sano Hidetoshi; Sawada Makoto; Shibata Toru; Dzhatdoev Timur; Suzuki Megumi; Suda Yusuke; Sunada Yuji; Sekizaki Haruhito; Zenin Anatolii; Takata Jumpei; Takahashi Keitaro; Takahashi Tomoya; Takahashi Hiromitsu; Takahashi Mitsunari; Tajima Norio; Tajima Hiroyasu; Tachihara Kengo; Tanaka Shuta; Tanaka Takaaki; Tanaka Manobu; Taneda Yuuki; Tam Thomas P. H.; Tamura Kenji; Cheng K. S.; Chikawa Michiyuki; Choushi Yuuki; Tsujimoto Shimpei; Tsuru Takeshi; Tian Wenwu; Terada Yukikatsu; Toma Kenji; Tokanai Fuyuki; Naito Tsuguya; Nagataki Shigehiro; Nakamura Yuki; Nakamori Takeshi; Nakayama Kazunori; Nagayoshi Tsutomu; Nishijima Kyoshi; Nozaki Seiya; Noda Koji; Barkov Maxim; Hadasch Daniela; Hayakawa Takahiro; Hayashi Katsuhiro; Hayashida Masaaki; Hara Satoshi; Bamba Aya; Hidaka Naoya; Hirako Joe; Hiroshima Nagisa; Hirotani Kouichi; Hui David C. Y.; Ferrand Gilles; Fukazawa Yasushi; Fukami Satoshi; Fukui Yasuo; Fujita Yutaka; Fujihara Chikako; Furuta Tomoya; He Haoning; Majumdar Pratik; Mazin Daniel; Masuda Shu; Matsumoto Hironori; Miura Chika; Mizuno Tsunefumi; Muraishi Hiroshi; Murase Kohta; Mori Koji; Yanagita Shohei; Yamazaki Ryo; Yamane Yumiko; Yamamoto Tokonatsu; Yamamoto Hiroaki; Yoshiike Satoshi; Yoshikoshi Takanori; Yoshid Atsumasa; Yoshida Tatsuo; Ri Ken; Lee Shiu-Hang (Herman)
Meeting Abstracts of the Physical Society of Japan, 2019

CTA Project 155: Status Report
Teshima Masahiro; Kubo Hidetoshi; Totani Tomonori; Asano Katsuaki; Ioka Kunihito; Ishio Kazuma; Inada Tomohiro; Inoue Susumu; Inoue Tsuyoshi; Inoue Yoshiyuki; Inome Yusuke; Iwamura Yuki; Warren Donald; Uchiyama Yasunobu; Ohishi Michiko; Ohoka Hideyuki; Ohtani Yoshiki; Ohira Yutaka; Oka Tomohiko; Okazaki Nao; Ogata Tomoyuki; Okumura Akira; Orito Reiko; Kagaya Mika; Kajiwara Yuki; Kataoka Jun; Katagiri Hideaki; Katsukura Daisuke; Katsuda Satoru; Khalikov Emil; Kawanaka Norita; Kisaka Shota; Cui Xiaohong; Kushida Junko; Gunji Shuichi; Kohri Kazunori; Kobayashi Yukiho; Kong Albert K. H.; Saito Takayuki; Sakaki Naoto; Sakurai Shunsuke; Sano Hidetoshi; Sawada Makoto; Shibata Toru; Dzhatdoev Timur; Suzuki Megumi; Suzuki Hiromasa; Suda Yusuke; Sunada Yuji; Zenin Anatolii; Takata Jumpei; Takahashi Keitaro; Takahashi Hiromitsu; Takahashi Mitsunari; Tajima Hiroyasu; Tachihara Kengo; Tanaka Shuta; Tanaka Takaaki; Tanaka Manobu; Tam Thomas P. H.; Tamura Kenji; Cheng K. S.; Chikawa Michiyuki; Choushi Yuuki; Tsujimoto Shimpei; Tsuru Takeshi; Tian Wenwu; Terada Yukikatsu; Toma Kenji; Tokanai Fuyuki; Naito Tsuguya; Nagataki Shigehiro; Nakamura Yuki; Nakamori Takeshi; Nakayama Kazunori; Nishijima Kyoshi; Nozaki Seiya; Noda Koji; Barkov Maxim; Hadasch Daniela; Hayakawa Takahiro; Hayashi Katsuhiro; Hayashida Masaaki; Hara Satoshi; Bamba Aya; Hidaka Naoya; Hiroshima Nagisa; Hirotani Kouichi; Hui David C. Y.; Ferrand Gilles; Fukazawa Yasushi; Fukami Satoshi; Fukui Yasuo; Fujita Yutaka; Fujihara Chikako; Furuta Tomoya; He Haoning; Majumdar Pratik; Mazin Daniel; Matsumoto Hironori; Mizuno Tsunefumi; Muraish Hiroshi; Murase Kohta; Mori Koji; Yanagita Shohei; Yamazaki Ryo; Yamane Yumiko; Yamamoto Tokonatsu; Yamamoto Hiroaki; Yoshikoshi Takanori; Yoshida Atsumasa; Yoshida Tatsuo; Lee Shiu-Hang (Herman)
Meeting Abstracts of the Physical Society of Japan, 2019

CTA Report 156: Evaluation of effect of uncertainty in hadronic interaction models on the estimation of CTA sensitivity
Ohishi Michiko; Iwamura Yuki; Ohtani Yoshiki; Ogata Tomoyuki; Okumura Akira; Orito Reiko; Katagiri Hideaki; Kushida Junko; Gunji Shuichi; Kobayashi Yukiho; Saito Takayuki; Arbeletche Luan; Sakaki Naoto; Sakurai Shunsuke; Zenin Anatolii; Chikawa Michiyuki; Nakamori Takeshi; Nishijima Kyoshi; Miura Chika; Nozaki Seiya; Fukami Satoshi; Fujihara Chikako; Souza Vitor de; Furuta Tomoya; Yoshida Tatsuo; the CTA-Japan Consortium; Maier Gernot; Bernloehr Konrad; Moralejo Abelardo; Bregeon Johan; Arrabito Luisa; Yoshikoshi Takanori
Meeting Abstracts of the Physical Society of Japan, 2019

CTA Report 150: Commissioning test of the focal plane camera of the first CTA Large-Sized Telescope.
Nozaki S.; Kajiwara Y.; Katagiri H.; Kushida J.; Kimura S.; Kubo H.; Gunji S.; Koyama S.; Saito T.; Sakurai S.; Sawada M.; Inada T.; Suzuki M.; Sunada Y.; Takahashi M.; Takahara H.; Tanaka M.; Tamura K.; Choushi Y.; Tujimoto S.; Teshima M.; Terada Y.; Inome Y.; Tokanai F.; Nakamori T.; Nagayoshi T.; Nishijima K.; Nishiyama G.; Noda K.; Hayashida M.; Bamba A.; Hirako J.; Fukami S.; Iwamura Y.; Furuta T.; Masuda S.; Yamamoto T.; Yoshida T.; Hadasch Daniela; Mazin Daniel; the CTA-Japan consortium; Ikeno M.; Uchida T.; Ohoka H.; Okazaki N.; Oka T.; Okumura A.; Orito R.
Meeting Abstracts of the Physical Society of Japan, 2019

CTA Report 157: Measurement of timing response performance of photomultiplier tube used for CTA large sized telescope
Sunada Yuji; Katagiri Hideaki; Kushida Junko; Kubo Hidetoshi; Gunji Shuichi; Kobayashi Yukiho; Saito Takayuki; Sakurai Shunsuke; Suzuki Megumi; Takahashi Mitsunari; Tanaka Manobu; Inome Yusuke; Tamura Kenji; Choushi Yuuki; Teshima Masahiro; Terada Yukikatsu; Tokanai Fuyuki; Nakamori Takeshi; Nagayoshi Tsutomu; Nishijima Kyoshi; Nogami Yuto; Nozaki Seiya; Iwamura Yuki; Noda Koji; Hadasch Daniela; Hayashida Masaaki; Bamba Aya; Hirako Joe; Furuta Tomoya; Mazin Daniel; Masuda Shu; Yamamoto Tokonatsu; Yoshida Tatsuo; Ohoka Hideyuki; Ikeno Masahiro; Uchida Tomohisa; Oka Tomohiko; Okazaki Nao; Okumura Akira; Orito Reiko; Kajiwara Yuki
Meeting Abstracts of the Physical Society of Japan, 2019

CTA Report 148: A Monte Carlo simulation study using muon events of Large Size Telescope
Ri Ken; Gunji Shuichi; Saito Takayuki; Sakaki Naoto; Sasai Yoshinori; Takahashi Tomoya; Taneda Yuki; Nakamori Takeshi; Nishijima Kyoshi; Miura Chika; Yoshikoshi Takanori; Fujihara Chikako; Yoshida Tatsuo; Zenin Anatolii; the CTA-Japan Consortium; Chikawa Michiyuki; Ohishi Michiko; Okumura Akira; Orito Reiko; Katagiri Hideaki; Kamimoto Takumi; Kushida Junko
Meeting Abstracts of the Physical Society of Japan, 2019

CTA Report 139: General Report
Kubo Hidetoshi; Teshima Masahiro; Totani Tomonori; Asano Akira; Asano Katsuaki; Ioka Kunihito; Ishio Kazuma; Inada Tomohiro; Inoue Susumu; Inoue Tsuyoshi; Inoue Yoshiyuki; Inome Yusuke; Iwamura Yuki; Warren Donald; Uchiyama Yasunobu; Ohishi Michiko; Ohoka Hideyuki; Ohira Yutaka; Okazaki Nao; Okumura Akira; Orito Reiko; Kagaya Mika; Kakuwa Jun; Kataoka Jun; Katagiri Hideaki; Katsukura Daisuke; Katsuda Satoru; Kato Sho; Kamimoto Takumi; Kawanaka Norita; Kisaka Shota; Kimura Souichiro; Cui Xiaohong; Kushida Junko; Kumon Taku; Kuroda Hayato; Gunji Shuichi; Kohri Kazunori; Koyama Shu; Kong Albert K. H.; Saito Takayuki; Sakaki Naoto; Sakurai Shunsuke; Sasai Yoshinori; Sano Hidetoshi; Sawada Makoto; Shibata Toru; Dzhatdoev Timur; Suzuki Megumi; Sunada Yuji; Sekizaki Haruhito; Zenin Anatolii; Takata Jumpei; Takahashi Keitaro; Takahashi Tomoya; Takahashi Hiromitsu; Takahashi Mitsunari; Takahara Hiro; Tajima Hiroyasu; Tachihara Kengo; Tanaka Shuta; Tanaka Takaaki; Tanaka Manobu; Tanaka Yasuyuki; Taneda Yuuki; Tam Thomas P. H.; Cheng K. S.; Chikawa Michiyuki; Tsujimoto Shimpei; Tsuru Takeshi; Tian Wenwu; Terada Yukikatsu; Toma Kenji; Tokanai Fuyuki; Naito Tsuguya; Nakajima Daisuke; Nagataki Shigehiro; Nakamura Yuki; Nakamori Takeshi; Nakayama Kazunori; Nagayoshi Tsutomu; Nishijima Kyoshi; Nishiyama Gaku; Nozaki Seiya; Noda Koji; Barkov Maxim; Hadasch Daniela; Hayakawa Takahiro; Hayashi Katsuhiro; Hayashida Masaaki; Hara Satoshi; Bamba Aya; Hidaka Naoya; Hirako Joe; Hiroshima Nagisa; Hirotani Kouichi; Hui David C. Y.; Ferrand Gilles; Fukazawa Yasushi; Fukami Satoshi; Fukui Yasuo; Fujita Yutaka; Fujihara Chikako; He Haoning; Majumdar Pratik; Mazin Daniel; Masuda Shu; Matsumoto Hironori; Miura Chika; Mizuno Tsunefumi; Muraishi Hiroshi; Murase Kohta; Mori Koji; Yanagita Shohei; Yamazaki Ryo; Yamamoto Tokonatsu; Yamamoto Hiroaki; Yoshiike Satoshi; Yoshikoshi Takanori; Yoshida Atsumasa; Yoshida Tatsuo; Ri Ken; Lee Shiu-Hang (Herman)
Meeting Abstracts of the Physical Society of Japan, 2018

CTA report 135: Optimization of the trigger performance for the Small-Sized Telescope
Sasai Yoshinori; Sakaki Naoto; Takahashi Tomoya; Taneda Yuki; Chikawa Michiyuki; Nakamori Takeshi; Nishijina Kyoshi; Miura Chika; Yoshikoshi Takanori; Yoshida Tatsuo; Ri Ken; Ohishi Michiko; the CTA-Japan Consortium; Okumura Akira; Orito Reiko; Katagiri Hideaki; Kamimoto Takumi; Kushida Junko; Gunji Shuichi; Saito Takayuki
Meeting Abstracts of the Physical Society of Japan, 2018

CTA report 132: A simulation study on CTA performance for the measurement of electron/positron spectrum in TeV region(III)
Ohishi Michiko; Sasai Yoshinori; Takahashi Tomoya; Taneda Yuki; Chikawa Michiyuki; Nakamori Takeshi; Nishijina Kyoshi; Miura Chika; Yoshikoshi Takanori; Yoshida Tatsuo; Ri Ken; Okumura Akira; the CTA-Japan Consortium; Orito Reiko; Katagiri Hideaki; Kamimoto Takumi; Kushida Junko; Gunji Shuichi; Saito Takayuki; Sakaki Naoto
Meeting Abstracts of the Physical Society of Japan, 2018

CTA report 143: Evaluation of the sensitivity of the Small-Sized Telescopes under moonlight
Sasai Yoshinori; Sakaki Naoto; Takahashi Tomoya; Tajima Hiroyasu; Taneda Yuki; Chikawa Michiyuki; Nakamura Yuki; Nakamori Takeshi; Nishijina Kyoshi; Fujihara Chikako; Miura Chika; Ohishi Michiko; Yoshikoshi Takanori; Yoshida Tatsuo; Ri Ken; Zenin Anatolii; the CTA-Japan Consortium; Okumura Akira; Orito Reiko; Katagiri Hideaki; Kamimoto Takumi; Kushida Junko; Gunji Shuichi; Saito Takayuki
Meeting Abstracts of the Physical Society of Japan, 2018

CTA report 140: A Monte Carlo simulation study on gamma-ray like proton events in CTA and dependence on hadronic interaction models
Ohishi Michiko; Sasai Yoshinori; Takahashi Tomoya; Taneda Yuki; Chikawa Michiyuki; Nakamori Takeshi; Nishijima Kyoshi; Fujiwara Chikako; Miura Chika; Yoshikoshi Takanori; Yoshida Tatsuo; Okumura Akira; Ri Ken; Zenin Anatolii; the CTA-Japan Consortium; Orito Reiko; Katagiri Hideaki; Kamimoto Takumi; Kushida Junko; Gunji Shuichi; Saito Takayuki; Sakaki Naoto
Meeting Abstracts of the Physical Society of Japan, 2018

CTA Report 141: Monte Carlo performance studies of the Cherenkov Telescope Array under moonlight (II)
Miura Chika; Sakaki Naoto; Sasai Yoshinori; Takahashi Tomoya; Taneda Yuki; Chikawa Michiyuki; Nakamori Takeshi; Nishijima Kyoshi; Fujihara Chikako; Yoshikoshi Takanori; Yoshida Tatsuo; Ohishi Michiko; Ri Ken; Zenin Anatolii; the CTA-Japan Consortium; Okumura Akira; Orito Reiko; Katagiri Hideaki; Kamimoto Takumi; Kushida Junko; Gunji Shuichi; Saito Takayuki
Meeting Abstracts of the Physical Society of Japan, 2018

CTA報告123:全体報告
窪秀利; 手嶋政廣; 手嶋政廣; 戸谷友則; 浅野勝晃; 朝野彰; 井岡邦仁; 石尾一馬; 石尾一馬; 稲田知大; 井上進; 井上剛志; 井上芳幸; 猪目祐介; 岩村由樹; WARREN Donald; 内山泰伸; 大石理子; 大岡秀行; 大平豊; 岡崎奈緒; 奥村曉; 折戸玲子; 加賀谷美佳; 格和純; 片岡淳; 片桐秀明; 勝倉大輔; 勝田哲; 加藤翔; 神本匠; 川中宣太; 木坂将大; 木村颯一朗; CUI Xiaohong; 櫛田淳子; 久門拓; 黒田隼人; 郡司修一; 郡和範; 小山志勇; KONG Albert K. H; 齋藤隆之; 榊直人; 櫻井駿介; 佐々井義矩; 佐野栄俊; 澤田真理; 柴田徹; DZHATDOEV Timur; 砂田裕志; 関崎晴仁; 高田順平; 高橋慶太郎; 高橋知也; 高橋弘充; 高橋光成; 田島宏康; 立原研悟; 田中周太; 田中孝明; 田中真伸; 田中康之; 種田裕貴; TAM Thomas P. H; CHENG K. S; 千川道幸; 辻本晋平; 鶴剛; TIAN Wenwu; 寺田幸功; 當真賢二; 門叶冬樹; 内藤統也; 中嶋大輔; 長瀧重博; 中村裕樹; 中森健之; 中山和則; 永吉勤; 西嶋恭司; 西山楽; 野崎誠也; 野田浩司; BARKOV Maxim; HADASCH Daniela; 早川貴敬; 林克洋; 林田将明; 原敏; 馬場彩; 日高直哉; 平子丈; 廣島渚; 廣島渚; 広谷幸一; HUI David C. Y; FERRAND Gilles; 深沢泰司; 深見哲志; 福井康雄; 藤田裕; HE Haoning; MAJUMDAR Pratik; MAZIN Daniel; 増田周; 松本浩典; 三浦知佳; 水野恒史; 村石浩; 村瀬孔大; 森浩二; 柳田昭平; 山崎了; 山本常夏; 山本宏昭; 吉池智史; 吉越貴紀; 吉田篤正; 吉田龍生
日本物理学会講演概要集(CD-ROM), 25 Sep. 2017

高角度分解能コンプトンカメラ(γI)開発のためのカウンターコンポーネントの評価
近藤亮太郎; 村石浩; 村石浩; 榎本良治; 榎本良治; 渡辺宝; 渡辺宝; 加賀谷美佳; 加賀谷美佳; 片桐秀明; 片桐秀明; 内田智久; 内田智久; 加納大輔; 武田徹; 田中聡一; 田中真伸; 田中真伸; 福士政広; 吉田龍生; 和田清人
日本物理学会講演概要集(CD-ROM), 25 Sep. 2017

結晶配置の対称性を考慮した高感度オールスカイガンマ線コンプトンカメラの開発
渡辺宝; 渡辺宝; 渡辺宝; 村石浩; 村石浩; 榎本良治; 榎本良治; 加賀谷美佳; 加賀谷美佳; 片桐秀明; 片桐秀明; 内田智久; 内田智久; 加納大輔; 近藤亮太郎; 武田徹; 田中聡一; 田中真伸; 田中真伸; 福士政広; 吉田龍生; 吉田龍生; 和田清人
日本物理学会講演概要集(CD-ROM), 25 Sep. 2017

CTA報告117:全体報告
手嶋政廣; 手嶋政廣; 窪秀利; 戸谷友則; 朝野彰; 浅野勝晃; 井岡邦仁; 池野祐平; 石尾一馬; 石尾一馬; 稲田知大; 井上進; 井上剛志; 井上芳幸; 猪目祐介; 岩村由樹; WARREN Donald; 内山泰伸; 梅津陽平; 大石理子; 大岡秀行; 大平豊; 岡崎奈緒; 奥村曉; 折戸玲子; 加賀谷美佳; 格和純; 片岡淳; 片桐秀明; 加藤翔; 川中宣太; 木坂将大; 岸田柊; 木村颯一朗; CUI Xiaohong; 櫛田淳子; 黒田隼人; 郡司修一; 郡和範; 小山志勇; KONG Albert K. H; 今野裕介; 齋藤隆之; 榊直人; 櫻井駿介; 佐藤雄太; 佐野栄俊; 澤田真理; 重中茜; 柴田徹; 高田順平; 高橋慶太郎; 高橋弘充; 高橋光成; 高見将太; 武田淳希; 田島宏康; 立原研悟; 田中周太; 田中孝明; 田中真伸; 田中康之; 谷川俊介; TAM Thomas P. H; TAN Dang Viet; CHENG K. S; 千川道幸; 辻本晋平; 鶴剛; TIAN Wenwu; 寺田幸功; 當真賢二; 門叶冬樹; 友野弥生; 内藤統也; 中嶋大輔; 長瀧重博; 中村裕樹; 中森健之; 中山和則; 永吉勤; 西嶋恭司; 西山楽; 野崎誠也; 野田浩司; BARKOV Maxim; HADASCH Daniela; 早川貴敬; 林克洋; 林田将明; 原敏; 馬場彩; 日高直哉; 平井亘; 廣島渚; 廣島渚; 広谷幸一; HUI DavidC. Y; FERRAND Gilles; 深沢泰司; 深見哲志; 福井康雄; 藤田裕; HE Haoning; MAJUMDAR Pratik; MAZIN Daniel; 増田周; 松本浩典; 水野恒史; 村石浩; 村瀬孔大; 本橋大輔; 森浩二; 柳田昭平; 山崎了; 山根暢仁; 山本常夏; 山本宏昭; 吉池智史; 吉越貴紀
日本物理学会講演概要集(CD-ROM), 21 Mar. 2017

A Technique for Estimating the Absolute Gain of a Photomultiplier Tube
Yamamoto T.; Nakamori T.; Nagayoshi T.; Nishijima K.; Nozaki S.; Mazin D.; Mashuda S.; Mirzoyan R.; Ohoka H.; Orito R.; Saito T.; Inome Y.; Sakurai S.; Takahashi M.; Teshima M.; Terada Y.; Tokanai F.; Yoshida T.; Yoshii S.; Gunji S.; Hadasch D.; Hayashida M.; Katagiri H.; Konno Y.; Kubo H.; Kushida J.
Meeting Abstracts of the Physical Society of Japan, 2017

超高エネルギーガンマ線による超新星残骸の観測の現状と展望
中森健之; 片桐秀明; 佐野栄俊; 福井康雄; 山崎了; 大平豊
日本天文学会年会講演予稿集, 2017

CTA Report 124: A simulation study of CTA performance for measurement of electron/positron spectrum in TeV region(II)
Ohishi Michiko; Nishijima Kyoshi; Miura Chika; Yoshikoshi Takanori; Yoshida Tatsuo; Ri Ken; the CTA-Japan; Inada Tomohiro; Okumura Akira; Katagiri Hideaki; Kushida Junko; Gunji Shuichi; Saito Takayuki; Sakaki Naoto; Chikawa Michiyuki
Meeting Abstracts of the Physical Society of Japan, 2017

CTA Report 119: Integration test of the focal plane camera of the first CTA Large Size Telescope
Nakajima D.; Kushida J.; Gunji S.; Konno Y.; Saito T.; Sakurai S.; Takahashi M.; Takeda J.; Tanigawa S.; Tan D.V.; Tsujimoto S.; Inome Y.; Teshima M.; Terada Y.; Tokanai F.; Nakamori T.; Nagayoshi T.; Nishijima K.; Nishiyama G.; Nozaki S.; Hayashida M.; Bamba A.; Ohoka H.; Masuda S.; Yamamoto T.; Yoshida T.; Yoshida M.; Mazine D.; Hadasch D.; CTA-Japan consortium; Okumura Akira; Orito R.; Katagiri H.; Kishida S.; Kimura S.; Kubo H.
Meeting Abstracts of the Physical Society of Japan, 2017

22aAT-4 CTA Report 105 : A simulation study of the performance of a focal plane camera with silicon photomultipliers for the CTA Small-Sized Telescopes
Sato Yuta; Tan Dang Viet; The CTA Consortium
Meeting Abstracts of the Physical Society of Japan, 2016

21pCA-11 Development of an all-sky gamma-ray Compton camera using CsI(Tl) scintillators
Muraishi H.; Tanaka M.; Nishio T.; Yoshida T.; Wakamatsu R.; Watanabe T.; Wada K.; Open-it consortium; Uchida T.; Enomoto R.; Kagaya M.; Katagiri H.; Kanoh D.; Satoh K.; Satoh W.; Takeda T.
Meeting Abstracts of the Physical Society of Japan, 2016

CTAで探る宇宙線の起源:RX J1713.7‐3946のガンマ線シミュレーション
佐野栄俊; 福井康雄; 田島宏康; 奥村暁; 中森健之; 郡司修一; 片桐秀明; 柳田昭平; 吉田龍生; 山崎了; 大平豊; 馬場彩; 澤田真理; 森浩二; 李兆衡; 藤田裕; 井上剛志; 花畑義隆; 林田将明; 吉越貴紀; 窪秀利; 斎藤隆之; 田中孝明; 櫛田淳子; 井上進; 井岡邦仁; 郡和範; 村瀬孔大; 長瀧重博; 内藤統也; 寺田幸功; 内山泰伸; GABICI Stefano
日本天文学会年会講演予稿集, 20 Aug. 2015

コンプトンカメラ法による高感度360°パノラマRIイメージングモニターの開発　　　　　　　　　　　　　　　
渡辺 宝; 伊東 良和; 内田 智久; 榎本 良治; 加賀谷 美佳; 片桐 秀明; 加納 大輔; 佐藤 一弘; 佐藤 亘; 武田 徹; 田中 真伸; 中山 浩平; 西尾 禎治; 花房 龍治; 石村 浩; 細川 正男; 吉田 龍生; 若松 諒; 和田 清人; オープンソースコンソーシアム(Open-It)
MEDICAL IMAGING TECHNOLOGY, Jul. 2015

宇宙線の起源に迫る
中森健之; 片桐秀明; 佐野栄俊; 山崎了; 大平豊; 馬場彩; 福井康雄; 森浩二; 李兆衡; 藤田裕; 田島宏康; 井上剛志; 郡司修一; 花畑義隆; 林田将明; 窪秀利; 櫛田淳子; 井上進; 井岡邦仁; 郡和範; 村瀬孔大; 長瀧重博; 内藤統也; 奥村曉; 奥村曉; 斎藤隆之; 澤田真理; 田中孝明; 寺田幸功; 内山泰伸; 柳田昭平; 吉田龍生; 吉越貴紀; GABICI Stefano
日本物理学会講演概要集(CD-ROM), 24 Mar. 2015

18pSB-4 CTA Report 76 : CTA Key Science Projects
Inoue Susumu; Inoue Yoshiyuki; Hayashida Masaaki; Tanaka Yasuyuki; Takami Hajime; Murase Kohta; Okumura Akira; Mizuno Tsunefumi; Yamazaki Ryo; Nakamori Takeshi; Sano Hidetoshi; Bamba Aya; Katagiri Hideaki; Ohira Yutaka; Lee Shiu-Hang Herman; Ioka Kunihito; Uchiyama Yasunobu; Mori Koji; Saito Takayuki; Kohri Kazunori; Mazin Daniel; Zech Andreas, Wilhelmi; Emma de Ona; Doro Michele; Pedaletti Giovanna; Torres Diego; Hinton Jim; CTA consortium
Meeting abstracts of the Physical Society of Japan, 22 Aug. 2014

18pSB-11 CTA report 83 : Evaluation of segmented mirrors for Large-Sized telescope and study of optical parameters
Ogino M; Hayashida M; Noda K; Okumura A; Ono S; Kagaya M; Katagiri H; Kojima T; Saito K; Saito T; Chikawa M; Cho N; Teshima M; Nakajima D; Hanabata Y; Fukami S; Yanagita S; Yamamoto T; Yoshida T; CTA-Japan Consortium
Meeting abstracts of the Physical Society of Japan, 22 Aug. 2014

18pSB-12 CTA Report 84 : Test of optical system using test structure for Large size telescope
Fukami Satoshi; Ogino Momoko; Okumura Akira; Ono Sakiya; Kagaya Mika; Katagiri Hideaki; Kojima Takumi; Saito Koji; Saito Takayuki; Chikawa Michiyuki; Cho Norihito; Teshima Masahiro; Nakajima Daisuke; Noda Koji; Hanabata Yoshitaka; Hayashida Masaaki; Yanagita Shohei; Yamamoto Tokonatsu; Yoshida Tatsuo
Meeting abstracts of the Physical Society of Japan, 22 Aug. 2014

Development of the camera for the large size telescopes of the Cherenkov Telescope Array
Y. Inome; G. Ambrosi; Y. Awane; H. Baba; A. Bamba; M. Barceló; U. Barres de Almeida; J. A. Barrio; O. Blanch Bigas; J. Boix; L. Brunetti; E. Carmona; E. Chabanne; M. Chikawa; N. Cho; P. Colin; J. L. Contreras; J. Cortina; F. Dazzi; A. Deangelis; G. Deleglise; C. Delgado; C. Díaz; F. Dubois; A. Fiasson; D. Fink; N. Fouque; L. Freixas; C. Fruck; A. Gadola; R. García; D. Gascón; N. Geffroy; N. Giglietto; F. Giordano; F. Grañena; S. Gunji; R. Hagiwara; N. Hamer; Y. Hanabata; T. Hassan; K. Hatanaka; T. Haubold; M. Hayashida; R. Hermel; D. Herranz; K. Hirotani; J. Hose; D. Hugh; S. Inoue; Y. Inoue; K. Ioka; C. Jablonski; M. Kagaya; H. Katagiri; J. Kataoka; H. Kellermann; T. Kishimoto; M. Knoetig; K. Kodani; K. Kohri; T. Kojima; Y. Konno; S. Koyama; H. Kubo; J. Kushida; G. Lamanna; T. Le Flour; M. López-Moya; R. López; E. Lorenz; P. Majumdar; A. Manalaysay; M. Mariotti; G. Martínez; M. Martinez; S. Masuda; S. Matsuoka; D. Mazin; U. Menzel; J. M. Miranda; R. Mirzoyan; I. Monteiro; A. Moralejo; K. Murase; S. Nagataki; T. Nagayoshi; D. Nakajima; T. Nakamori; K. Nishijima; K. Noda; A. Nozato; M. Ogino; Y. Ohira; M. Ohishi; H. Ohoka; A. Okumura; S. Ono; R. Orito; J. L. Panazol; D. Paneque; R. Paoletti; J. M. Paredes; G. Pauletta; S. Podkladkin; J. Prast; R. Rando; O. Reimann; M. Ribó; S. Rosier-Lees; K. Saito; T. Saito; Y. Saito; N. Sakaki; R. Sakonaka; A. Sanuy; M. Sawada; V. Scalzotto; S. Schultz; T. Schweizer; T. Shibata; S. Shu; J. Sieiro; V. Stamatescu; S. Steiner; U. Straumann; R. Sugawara; H. Tajima; H. Takami; M. Takahashi; S. Tanaka; M. Tanaka; L. A. Tejedor; Y. Terada; M. Teshima; Y. Tomono; T. Totani; T. Toyama; Y. Tsubone; Y. Tsuchiya; S. Tsujimoto; H. Ueno; K. Umehara; Y. Umetsu; A. Vollhardt; R. Wagner; H. Wetteskind; T. Yamamoto; R. Yamazaki; A. Yoshida; T. Yoshida; T. Yoshikoshi
SPIE, 07 Aug. 2014, [Reviewed]

30aTJ-2 Development of Compton Camera γI (gamma eye) 16 channel prototype detector
Kagaya M.; Uchida T.; Enomoto R.; Katagiri H.; Sato K.; Takeda T.; Tanaka M.; Nakayama K.; Hanafusa R.; Muraishi H.; Yanagita S.; Yoshida T.; Open-It consortium
Meeting abstracts of the Physical Society of Japan, 05 Mar. 2014

CTA報告 58:全体報告
手嶋政廣; 手嶋政廣; 窪秀利; 戸谷友則; 浅野勝晃; 井岡邦仁; 井川大地; 石尾一馬; 井上進; 井上芳幸; 猪目祐介; 上野遥; 大石理子; 大岡秀行; 大竹峻平; 大平豊; 荻野桃子; 奥村曉; 奥村曉; 折戸玲子; 加賀谷美佳; 格和純; 片岡淳; 片桐秀明; 株木重人; 河島孝則; 川中宣太; 岸本哲朗; 櫛田淳子; 郡司修一; 郡和範; 小島拓実; 小谷一仁; 小山志勇; 今野裕介; 齋藤浩二; 榊直人; 佐々木浩人; 澤田真理; 柴田徹
日本物理学会講演概要集, 2013

13aSK-5 Development of the PMT-waveform sampling circuit using an analog memory for the CTAproject
Konno Yusuke
Meeting abstracts of the Physical Society of Japan, 24 Aug. 2012

13aSP-10 MAGIC 33 : MAGIC telescopes observation of the HBL object 1ES 1727+502
Kodani K; Inoue S; Orito R; Katagiri H; Kushida J; Kubo H; Konno Y; Saito K; Saito T; Takami H; Teshima M; Toyama T; Nakajima D; Nishijima K; Hayashida M; Miyamoto H; MAGIC Collaboration
Meeting abstracts of the Physical Society of Japan, 24 Aug. 2012

13pSP-8 CTA-45 : Development of Segment Mirror for CTA
Zhou Xiaoxi; Sakonaka Ryosuke; Nozato Asuka; Kitamoto Kanetsuku; Chikawa Michiyuki; Teshima Masahiro; Kagaya Mika; Baba Hironori; Yanagita Shouhei; Tanaka Shunya; Katagiri Hideaki; Yoshida Tatsuo; Yamamoto Tokonatsu; Okumura Akira; Hayashida Masaaki; CTA-Japan consortium
Meeting abstracts of the Physical Society of Japan, 24 Aug. 2012

CTA報告34:CTA大口径望遠鏡のための焦点面検出器の開発
梅原克典; 片桐秀明; 黒田和典; 佐々木美佳; 粟根悠介; 榎本良治; 大岡秀行; 奥村暁; 折戸玲子; 株木重人; 櫛田淳子; 窪秀利; 郡司修一; 小谷一仁; 小山志勇; 今野裕介; 渋谷明伸; 菅原隆希; 高橋弘充; 田島宏康; 谷森達; 千川道幸; 千葉順成; 手嶋政廣; 寺田幸功; 門叶冬樹; 中森健之; 西嶋恭司; 林田将明; 馬場彩; 日高直哉; 深沢泰司; 水野恒史; 山岡和貴; 山本常夏; 吉田篤正; 米谷光生; MIRZOYAN Razmik; REIMANN Olaf
日本物理学会講演概要集, 05 Mar. 2012

CTA大口径望遠鏡のための焦点面検出器の開発(2)
小山志勇; 上野遥; 寺田幸功; 粟根悠介; 窪秀利; 今野裕介; 谷森達; 林田将明; 梅原克典; 片桐秀明; 黒田和典; 佐々木美佳; 榎本良治; 大岡秀行; 手嶋政廣; 奥村曉; 折戸玲子; 菅原隆希; 櫛田淳子; 株木重人; 小谷一仁; 西嶋恭司; 郡司修一; 門叶冬樹; 渋谷明伸; 田島宏康; 日高直哉; 高橋弘充; 深沢泰司; 水野恒史; 米谷光生; 千川道幸; 千葉順成; 中森健之; 馬場彩; 山岡和貴; 吉田篤正; 山本常夏; MIRZOYAN Razmik
日本天文学会年会講演予稿集, 20 Feb. 2012

13pSP-1 CTA Project 38 : General Report
Teshima Masahiro
Meeting Abstracts of the Physical Society of Japan, 2012

CTA大口径望遠鏡の焦点面検出器の開発
櫛田淳子; 株木重人; 小谷一仁; 西嶋恭司; 粟根悠介; 窪秀利; 今野裕介; 谷森達; 林田将明; 梅原克典; 片桐秀明; 黒田和典; 佐々木美佳; 榎本良治; 大岡秀行; 手嶋政廣; 奥村曉; 小山志勇; 寺田幸功; 折戸玲子; 菅原隆希; 郡司修一; 門叶冬樹; 渋谷明伸; 田島宏康; 日高直哉; 高橋弘充; 深沢泰司; 水野恒史; 米谷光生; 千川道幸; 千葉順成; 中森健之; 馬場彩; 山岡和貴; 吉田篤正; 山本常夏; MIRZOYAN Razmik; REIMANN Olaf
日本天文学会年会講演予稿集, 20 Aug. 2011

CTA報告19:CTA時代におけるSNR研究
吉田龍生; 井岡邦仁; 大平豊; 片桐秀明; 馬場彩; 藤田裕; 山崎了
日本物理学会講演概要集, 2011

Development of the readout system for CTA using the DRS4 waveform digitizing chip
H. Kubo; R. Paoletti; M. Aono; Y. Awane; M. Bitossi; R. Enomoto; S. Gunji; R. Hagiwara; N. Hidaka; M. Ikeno; S. Kabuki; H. Katagiri; Y. Konno; T. Nakamori; H. Ohoka; A. Okumura; R. Orito; M. Sasaki; A. Shibuya; H. Tajima; M. Tanaka; M. Teshima; T. Uchida; K. Umehara; M. Yonetani
Proceedings of the 32nd International Cosmic Ray Conference, ICRC 2011, 01 Jan. 2011

次期X線衛星ASTRO‐H搭載軟γ線検出器に向けたSi‐Pad検出器の開発
道津匡平; 西野翔; 林克洋; 松岡正之; 朴寅春; 深沢泰司; 片桐秀明; 渡辺伸; 国分紀秀; 高橋忠幸; 田中孝明; 田島宏康; 中澤知洋
日本天文学会年会講演予稿集, 20 Feb. 2010

フェルミ衛星による超新星残骸からのガンマ線放射の研究
片桐秀明; 内山泰伸; 釜江常好; 田島宏康; 田中孝明; 山崎了
天文月報, 2010
Lead

CTA計画
井上進; 榎本良治; 大石理子; 片桐秀明; 株木重人; 河内明子; 木舟正; 櫛田順子; 窪秀利; 郡司修一; 高橋弘充; 森谷達; 門叶冬樹; 戸谷友則; 内藤統也; 中森健之; 西嶋恭司; 原敏; 深沢泰司; 水野恒司; 村石浩; 柳田昭平; 山崎了; 吉越貴紀; 吉田龍生
ICRRニュース, 01 Oct. 2009

TeV gamma-ray observations of some extragalactic objects with CANGAROO-III
Kyoshi Nishijima; Michiyo Akimoto; Yoshitaka Mizumura; Junko Kushida; Hidetoshi Kubo; Geoffry V. Bicknell; Roger W. Clay; Philip G. Edwards; Ryoji Enomoto; Shuichi Gunji; Satoshi Hara; Tadao Hara; Takahiro Hattori; Sei'Ichi Hayashi; Yusuke Higashi; Yasufumi Hirai; Kenji Inoue; Hisanori Ishioka; Shigeto Kabuki; Fumiyoshi Kajino; Hideaki Katagiri; Akiko Kawachi; Tadashi Kifune; Ryuta Kiuchi; Toshiki Kunisawa; Takashi Matoba; Yutaka Matsubara; Ikuma Matsuzawa; Taku Mizukami; Yoshihiko Mizumoto; Masaki Mori; Hiroshi Muraishi; Tsuguya Naito; Takeshi Nakamori; Shintaro Nakano; Michiko Ohishi; Yuhki Ohtake; Shin'ichi Ryoki; Koji Saito; Yukiko Sakamoto; Atsushi Seki; Victor Stamatescu; Toshitaka Suzuki; David L. Swaby; Toru Tanimori; Greg Thornton; Fuyuki Tokanai; Ken'ichi Tsuchiya; Shio Watanabe; Eiichi Yamazaki; Shohei Yanagita; Tatsuo Yoshida; Takanori Yoshikoshi; Yohei Yukawa
31st International Cosmic Ray Conference, ICRC 2009, 01 Jan. 2009

23aSH-1 Initial Status of the Gamma-ray Large Area Telescope (GLAST)
Fukazawa Y; Kawai N; Kataoka J; Nakamori T; Kanai Y; Shimokawabe T; Takahashi T; Ozaki M; Ohno M; Sato R; Kamae T; Ohsugi T; Tajima H; Tanaka T; Okumura A; Makishima K; CLAST team; Mizuno T; Katagiri H; Takahashi H; Yasuda H; Nishino S; Yoshida H; Hanabata Y
Meeting Abstracts of the Physical Society of Japan, 2008

24aZJ-1 X-ray & γ-ray Polarimetry Satellite Polaris
Hayashida Kiyoshi
Meeting abstracts of the Physical Society of Japan, 21 Aug. 2007

完全ピクセル読みだし型μ‐PICを用いたX線偏光検出器の開発(3)
鶴剛; 片桐秀明; 小野健一; 内山秀樹; 兵藤義明; 松本浩典; 小山勝二; 谷森達; 窪秀利; 身内賢太朗; 植野優; 永吉勉
日本天文学会年会講演予稿集, 20 Feb. 2006

すざく衛星によるTeV γ線天体HESS J1616‐508の観測
松本浩典; 片桐秀明; 鶴剛; 小山勝二; 馬場彩; 千田篤史; 平賀純子; 高橋忠幸; 植野優; 片岡淳
日本天文学会年会講演予稿集, 20 Feb. 2006

ピクセル読み出し型μ‐PICによるX線偏光検出器の開発(III)
小野健一; 片桐秀明; 内山秀樹; 鶴剛; 松本浩典; 兵藤義明; 永吉勉; 植野優
日本天文学会年会講演予稿集, 20 Aug. 2005

ピクセル読み出し型μ‐PICによるX線偏光検出器の開発(IV)
内山秀樹; 片桐秀明; 小野健一; 鶴剛; 松本浩典; 兵藤義明; 永吉勉; 植野優
日本天文学会年会講演予稿集, 20 Aug. 2005

ピクセル読み出し型μ‐PICによるX線偏光検出器の開発(II)
片桐秀明; 小野健一; 鶴剛; 松本浩典; 植野優; 兵藤義明; 永吉勉
日本天文学会年会講演予稿集, 20 Feb. 2005

ピクセル読み出し型μ‐PICによるX線偏光検出器の開発
小野健一; 森谷達; 鶴剛; 松本浩典; 片桐秀明; 永吉勉; 植野優
日本天文学会年会講演予稿集, 2004

Development of an atmospheric Cherenkov imaging camera for the CANGAROO-III experiment
S Kabuki; K Tsuchiya; K Okumura; R Enomoto; T Uchida; H Tsunoo; S Hayashi; S Hayashi; F Kajino; A Maeshiro; Tada, I; C Itoh; A Asahara; GV Bicknell; RW Clay; PG Edwards; S Gunji; S Hara; T Hara; T Hattori; H Katagiri; A Kawachi; T Kifune; H Kubo; J Kushida; Y Matsubara; Y Mizumoto; M Mori; H Moro; H Muraishi; Y Muraki; T Naito; T Nakase; D Nishida; K Nishijima; M Ohishi; Patterson, JR; RJ Protheroe; K Sakurazawa; DL Swaby; T Tanimori; F Tokanai; A Watanabe; S Watanabe; S Yanagita; T Yoshida; T Yoshikoshi
NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT, Mar. 2003

Detection of diffuse TeV gamma-ray emission from the neaby starburst galaxy NGC 253
Itoh, C.; Enomoto, R.; Yanagita, S.; Yoshida, T.; Asahara, A.; Bicknell, G. V.; Clay, R. W.; Edwards, P. G.; Gunji, S.; Hara, S.; Hara, T.; Hattori, T.; Hayashi, Shin.; Hayashi, Sei.; Kabuki, S.; Kajino, F.; Katagiri, H.; Kawachi, A.; Kifune, T.; Kubo, H.; Kushida, J.; Matsubara, Y.; Mizumoto, Y.; Mori, M.; Moro, H.; Muraishi, H.; Muraki, Y.; Naito, T.; Nakase, T.; Nishida, D.; Nishijima, K.; Okumura, K.; Ohishi, M.; Patterson, J. R.; Protheroe, R. J.; Sakurazawa, K.; Swaby, D. L.; Tanimori, T.; Tokanai, F.; Tsuchiya, K.; Tsunoo, H.; Uchida, T.; Watanabe, A.; Watanabe, S.; Yoshikoshi, T.
Astronomy and Astrophysics, Dec. 2002

25pXD-6 CANGAROO-II望遠鏡の観測報告V
土屋 兼一; 浅原 明広; 榎本 良治; 郡司 修一; 服部 敬裕; 原 敏; 原 忠生; 林 清一; 林 慎一郎; 伊藤 千枝; 株木 重人; 梶野 文義; 片桐 秀明; 河内 明子; 木舟 正; 窪 秀利; 櫛田 淳子; 松原 豊; 水本 好彦; 森 正樹; 茂呂 寿子; 村石 浩; 村木 綬; 内藤 統也; 中瀬 友和; 西田 大輔; 西嶋 恭司; 荻尾 彰一; 大石 理子; 奥村 公宏; 折戸 玲子; さこ 隆志; 桜澤 幸司; 薄田 竜太郎; 鈴木 理映子; 田村 忠久; 谷森 達; 津野尾 肇; 門叶 冬樹; 内田 直志; 渡部 晃; 渡部 至緒; 柳田 昭平; 吉田 龍生; 吉越 貴紀
日本物理学会講演概要集, 2002

Science with the Cherenkov Telescope Array
Cherenkov Telescope Array Consortium; Acharya; B. S.; Agudo; I.; et al., Joint work
World Scientific Publishing Co. Pte. Ltd., Mar. 2019
9789813270084

Investigation of a high-sensitivity Compton camera for 177Lu radioactive contamination imaging: A Geant4 simulation　　　　　　　　　　　　　　　
[E1] Hikari Tsukamoto; Hiroshi Muraishi; Ryoji Enomoto; Hideaki Katagiri; Mika Kagaya; Takara Watanabe; Daisuke Kano; Yusuke Watanabe
第125回日本医学物理学会学術大会, 14 Apr. 2023, 日本医学物理学会
20230413, 20230416

177Lu放射能汚染イメージング用高感度コンプトンカメラの開発　　　　　　　　　　　　　　　
塚本 ひかり、村石 浩、榎本 良治、片桐 秀明、加賀谷 美佳、渡辺 宝、加納 大輔、渡邉 祐介
第70回応用物理学会春季学術講演会, 15 Mar. 2023, 応用物理学会
20230315, 20230318

CTA 大口径望遠鏡 2-4 号機における波形記録チップ DRS4 のサンプリング時間幅較正　　　　　　　　　　　　　　　
服部勇大; 片桐秀明; 他 CTA-Japan consortium
日本天文学会2023年春季年会, Mar. 2023
202303, 202303

CTA-LST 初号基と MAGIC による TeV ガンマ線同時観測のための解析手法の開発　　　　　　　　　　　　　　　
須田祐介; 他 CTA LST project; MAGIC Collaboration
日本天文学会2023年春季年会, Mar. 2023
202303, 202303

Cherenkov Telescope Array (CTA) 計画：全体報告（23）　　　　　　　　　　　　　　　
窪秀利; 他 CTA Consortium
日本天文学会2023年春季年会, Mar. 2023
202303, 202303

伐採前の立木に含まれる微量放射能を測定可能な可搬型非破壊検査装置の開発および実地試験による実証　　　　　　　　　　　　　　　
加賀谷美佳; 片桐秀明; 榎本良治; 小林久泰; 金田一美有; 関根直樹; 村石浩; 渡辺宝
日本きのこ学会第25回大会, Sep. 2022, 日本きのこ学会
20220926, 20220928

ルテチウムオキソドトレオチド(177Lu)注射液を用いる核医学治療における放射能汚染の可視化　　　　　　　　　　　　　　　
渡辺 宝、加納 大輔、村石 浩、榎本 良治、片桐 秀明、加賀谷 美佳、中神 佳宏
第83回応用物理学会秋季学術講演会, 22 Sep. 2022, 応用物理学会
20220920, 20220923

Cherenkov Telescope Array (CTA) 計画：全体報告 (22)　　　　　　　　　　　　　　　
野田浩司; 他 CTA Consortium
日本天文学会2022年秋季年会, Sep. 2022
202209, 202209

CTA 大口径望遠鏡のための SiPM モジュールの開発　　　　　　　　　　　　　　　
橋山和明; 他 CTA-Japan Consortium
日本天文学会2022年秋季年会, Sep. 2022
202209, 202209

CTA報告199：全体報告　　　　　　　　　　　　　　　
窪秀利; 他CTA LST プロジェクト
日本物理学会2022年秋季大会, Sep. 2022
202209, 202209

CTA報告201：大天頂角観測時におけるCTA大口径望遠鏡初号機の性能評価 (2)　　　　　　　　　　　　　　　
阿部正太郎; 他CTA LST プロジェクト
日本物理学会2022年秋季大会, Sep. 2022
202209, 202209

シイタケ栽培用立木に含まれる微量放射能を伐採前に測定可能な可搬型非破壊検査装置の開発　　　　　　　　　　　　　　　
加賀谷美佳,片桐秀明,榎本良治,小林久泰,金田一美有,関根直樹,村石浩,石川咲貴,渡辺宝
日本きのこ学会第24回大会（オンライン）, 01 Mar. 2022
202203, 202203

CTA報告188：全体報告　　　　　　　　　　　　　　　
野田浩司; 他CTA LST プロジェクト
日本物理学会第77回年次大会, Mar. 2022
202203, 202203

CTA報告 189：CTA大口径望遠鏡初号機による20 GeVガンマ線の検出　　　　　　　　　　　　　　　
野崎誠也; 他CTA LST プロジェクト
日本物理学会第77回年次大会, Mar. 2022
202203, 202203

CTA報告 190：CTA大口径望遠鏡初号機による新星へびつかい座RS星の観測データの解析　　　　　　　　　　　　　　　
小林志鳳; 他CTA LST プロジェクト
日本物理学会第77回年次大会, Mar. 2022
202203, 202203

CTA報告191：大天頂角観測時におけるCTA大口径望遠鏡初号機の性能評価　　　　　　　　　　　　　　　
阿部正太郎; 他CTA LST プロジェクト
日本物理学会第77回年次大会, Mar. 2022
202203, 202203

CTA報告192：CTA大口径望遠鏡初号機とMAGIC望遠鏡の同時イベント解析手法の研究 (2)　　　　　　　　　　　　　　　
大谷恵生; 他CTA LST プロジェクト
日本物理学会第77回年次大会, Mar. 2022
202203, 202203

CTA報告193：大口径望遠鏡初号機とMAGIC望遠鏡間におけるハードウェアトリガーの実装及び観測時の性能推定の研究　　　　　　　　　　　　　　　
バクスタージョシュア稜; 他CTA LST プロジェクト
日本物理学会第77回年次大会, Mar. 2022
202203, 202203

CTA報告 194：CTA大口径望遠鏡2-4号機のカメラ開発の現状　　　　　　　　　　　　　　　
阿部日向; 他CTA LST プロジェクト
日本物理学会第77回年次大会, Mar. 2022
202203, 202203

CTA報告195：CTA大口径望遠鏡のPMTにおける出力応答の磁場依存性の測定　　　　　　　　　　　　　　　
立石大; 他CTA LST プロジェクト
日本物理学会第77回年次大会, Mar. 2022
202203, 202203

CTA報告196：CTA大口径望遠鏡のためのSiPMモジュールの開発　　　　　　　　　　　　　　　
橋山和明; 他CTA LST プロジェクト
日本物理学会第77回年次大会, Mar. 2022
202203, 202203

CTA報告197：CTA大・中口径望遠鏡のカメラのSiPM化に向けた，集光器を用いた夜光低減の検討（２）　　　　　　　　　　　　　　　
芳賀純也; 他CTA LST プロジェクト
日本物理学会第77回年次大会, Mar. 2022
202203, 202203

SOIPIX を用いたsub-MeVガンマ線観測用の電子飛跡検出型コンプトンカメラの開発　　　　　　　　　　　　　　　
加賀谷美佳; 片桐秀明; 加藤凌; 東城直美; 武田彩希; 島添健次; 鶴剛; 田中孝明; 上ノ町水紀; Lan Zhang
日本物理学会第77回年次大会, Mar. 2022
202203, 202203

CTA大口径望遠鏡用波形サンプリング回路に用いるアナログメモリDRS4のスパイク特性　　　　　　　　　　　　　　　
岡知彦; 他CTA-Japan Consortium
日本物理学会第77回年次大会, Mar. 2022
202203, 202203

CTA 大口径望遠鏡の高画素化に向けた SiPM モジュールの開発　　　　　　　　　　　　　　　
齋藤隆之; 他 CTA-Japan consortium
日本天文学会2022年春季年会, Mar. 2022
202203, 202203

CTA 大口径望遠鏡 2-4 号機カメラ製作の現状　　　　　　　　　　　　　　　
岩崎啓; 他 CTA-Japan consortium; 池野正弘,Antonios Dettlaff
日本天文学会2022年春季年会, Mar. 2022
202203, 202203

Development of a compact and portable high-sensitivity omnidirectional Compton camera with detector rotation function　　　　　　　　　　　　　　　
Saki Ishikawa; Hiroshi Muraishi; Ryoji Enomoto; Hideaki Katagiri; Mika Kagaya; Takara Watanabe; Daisuke Kano; Satoshi Nakamura; Yusuke Watanabe; Hiromichi Ishiyama
2021 VIRTUAL IEEE NUCLEAR SCIENCE SYMPOSIUM AND MEDICAL IMAGING CONFERENCE, 20 Oct. 2021
202110, 202110

回転コンプトンカメラを用いた医療施設における環境放射能測定　　　　　　　　　　　　　　　
石川咲貴; 村石 浩; 榎本良治; 片桐秀明; 加賀谷美佳; 渡辺宝; 加納大輔; 中村哲志; 渡邉祐介; 石山博條
第82回応用物理学会秋季学術講演会, 13 Sep. 2021
202109, 202109

CTA 報告 182：全体報告　　　　　　　　　　　　　　　
齋藤隆之; 他CTA LST プロジェクト
日本物理学会2021年秋季大会, Sep. 2021
202109, 202109

CTA報告 183：CTA大口径望遠鏡初号機の観測データ解析の現状　　　　　　　　　　　　　　　
武石隆治; 他CTA LST プロジェクト
日本物理学会2021年秋季大会, Sep. 2021
202109, 202109

CTA報告184：CTA大口径望遠鏡初号機とMAGIC望遠鏡の同時イベント解析手法の研究　　　　　　　　　　　　　　　
大谷恵生; 他CTA LST プロジェクト
日本物理学会2021年秋季大会, Sep. 2021
202109, 202109

CTA報告185：CTA大口径望遠鏡用PMTの増幅応答に対する磁場と入射光波長の効果の調査　　　　　　　　　　　　　　　
小林志鳳; 他 CTA-Japan consourtium
日本物理学会2021年秋季大会, Sep. 2021
202109, 202109

CTA報告186：CTA大口径望遠鏡のためのSiPMカメラの開発　　　　　　　　　　　　　　　
橋山和明; 他 CTA-Japan consourtium
日本物理学会2021年秋季大会, Sep. 2021
202109, 202109

Cherenkov Telescope Array (CTA) 計画：全体報告 (20)　　　　　　　　　　　　　　　
野田浩司; 他 CTA Consortium
日本天文学会2021年秋季年会, Sep. 2021
202109, 202109

核医学施設における回転機能付き高感度全方向コンプトンカメラを用いた測定　　　　　　　　　　　　　　　
石川咲貴、村石 浩、榎本良治、片桐秀明、加賀谷美佳、渡辺 宝、加納大輔、中村哲志、渡邉祐介、石山博條
2021次世代放射線シンポジウム, Aug. 2021, 応用物理学会放射線分科会
20210819, 20210820

CTA 大口径望遠鏡におけるDRS4波形記録チップのサンプリング時間幅較正　　　　　　　　　　　　　　　
野上優人; 片桐秀明; 他 CTA-Japan Consortium
日本天文学会2021年春季年会, 17 Mar. 2021
202103, 202103

シイタケ栽培用ホダ木に用いる立木の微量放射能を伐採前に測定可能な非破壊検査装置の開発　　　　　　　　　　　　　　　
加賀谷美佳,片桐秀明,榎本良治,金田一美有,村石浩,石川咲貴,渡辺宝
第68回応用物理学会春季学術講演会（オンライン）, 16 Mar. 2021
202103, 202103

回転機能を備えた高感度全方向コンプトンカメラの小型化　　　　　　　　　　　　　　　
石川咲貴; 村石 浩; 榎本良治; 片桐秀明; 加賀谷美佳; 渡辺宝
第68回応用物理学会春季学術講演会, Mar. 2021
202103, 202103

コンプトンカメラを用いた18F-FDG PET受診者の尿中放射能測における放射能の算出方法の検討　　　　　　　　　　　　　　　
渡辺宝; 加納大輔; 村石 浩; 榎本良治; 片桐秀明; 加賀谷美佳; 石川咲貴; 中神佳宏
第68回応用物理学会春季学術講演会, Mar. 2021
202103, 202103

CTA報告 170：CTA大口径望遠鏡2-4号基における分割鏡配置の決定と光学性能の検証　　　　　　　　　　　　　　　
1.小原光太郎; 稲田知大; 野田浩司; 深見哲志; Ievgen Vovk; 奥村曉; 加賀谷美佳; 片桐秀明; 齋藤隆之; 手嶋政廣; 千川道幸; 山本常夏; 吉田龍生; 他 CTA-Japanコンソーシアム
日本物理学会2020年秋季大会, 15 Sep. 2020
202009, 202009

シイタケ栽培用ホダ木に用いる立木の微量放射能を伐採前に測定可能な非破壊検査装置の開発　　　　　　　　　　　　　　　
加賀谷美佳,片桐秀明,榎本良治,金田一美有,村石浩,石川咲貴,渡辺宝
第81回応用物理学会秋季学術講演会（オンライン）, 10 Sep. 2020
202009, 202009

18F-FDG PET受診者の尿中放射能を測定可能な高感度コンプトンカメラの開発　　　　　　　　　　　　　　　
渡辺宝; 加納大輔; 村石 浩; 榎本良治; 片桐秀明; 加賀谷美佳; 石川咲貴; 中神佳宏
第81回応用物理学会秋季学術講演会, Sep. 2020
202009, 202009

回転機能を備えた高感度全方向コンプトンカメラの小型化　　　　　　　　　　　　　　　
石川咲貴、村石 浩、榎本良治、片桐秀明、加賀谷美佳、渡辺 宝
次世代放射線シンポジウム2020, Aug. 2020
20200820, 20200821

回転型高感度コンプトンカメラによる全方向γ線イメージング　　　　　　　　　　　　　　　
村石 浩; 榎本良治; 片桐秀明; 加賀谷美佳; 成田尚史; 渡辺宝; 加納大輔
第67回応用物理学会春季学術講演会, Mar. 2020
202003, 202003

SOIピクセルセンサーを用いた電子飛跡検出型コンプトンカメラの電子反跳角依存性の評価　　　　　　　　　　　　　　　
加藤凌; 片桐秀明; 加賀谷美佳; 東城直美; 新井康夫; 武田彩希; 鶴剛
日本物理学会第75回年次大会, Mar. 2020
202003, 202003

CTA大口径望遠鏡初号機における波形サンプリング時間幅較正および2-4号機用カメラの組立・品質管理　　　　　　　　　　　　　　　
野上優人
日本天文学会2020年春季年会, Mar. 2020
202003, 202003

Cherenkov Telescope Array(CTA) 計画: 全体報告(17)　　　　　　　　　　　　　　　
野田浩司
日本天文学会2020年春季年会, Mar. 2020
202003, 202003

高感度コンプトンカメラを用いたPET受診者の尿中放射能遠隔測定　　　　　　　　　　　　　　　
渡辺宝、加納大輔 、村石 浩、 榎本良治、片桐秀明、加賀谷美佳、成田尚史 、細川翔太
第59回日本核医学学会学術総会, Nov. 2019
20191101, 20191103

Development of a high-sensitivity omnidirectional Compton camera with rotation function for radioactive environmental monitoring　　　　　　　　　　　　　　　
Hiroshi Muraishi; Ryoji; Enomoto; Hideaki Katagiri; Mika Kagaya; Takara Watanabe; Naofumi Narita; Daisuke Kano; Hidetake Hara; Yusuke Watanabe; Hiromichi Ishiyama
19th Asia-Oceania Congress of Medical Physics (AOCMP) in conjunction with the 2019 Engineering & Physical Sciences in Medicine Conference (EPSM), Oct. 2019
20191028, 20191030

全方向コンプトンカメラを用いた環境中におけるさまざまな低線量γ線源の可視化　　　　　　　　　　　　　　　
村石 浩,榎本良治,片桐秀明,加賀谷美佳,渡辺 宝,成田尚史,加納大輔
2019年 第80回応用物理学会秋季学術大会, Sep. 2019
20190918, 20190921

Development of omnidirectional Compton camera for visualizing low energy gamma rays from radiopharmaceuticals with high sensitivity　　　　　　　　　　　　　　　
Naofumi Narita; Hideaki Katagiri; Ryoji Enomoto; Hiroshi Muraishi; Takara Watanabe; Mika Kagaya; Ryotaro Kondo; Daisuke Kano
19th International Conference on Solid State Dosimetry, Sep. 2019
20190911, 20190914

Development of a portable and sensitive radioactive detection system for outdoor nondestructive measurement of radioactive cesium in standing trees　　　　　　　　　　　　　　　
Mika Kagaya; Hideaki Katagiri; Ryoji Enomoto; Akiko Yamaguchi; Hiroshi Muraishi; Nofumi Narita; Takara Watanabe
19th International Conference on Solid State Dosimetry, Sep. 2019
20190911, 20190914

テクネチウム９９ｍからの軟ガンマ線を高感度に可視化する全方位コンプトンカメラの開発　　　　　　　　　　　　　　　
Naofumi Narita; Hideaki Katagiri; Ryoji Enomoto; Hiroshi Muraishi; Takara Watanabe; Mika Kagaya; Ryotaro Kondo; Daisuke Kano
第117回医学物理学会学術大会, Apr. 2019
201904, 201904

回転機能付き全方向γ線コンプトンカメラの開発　　　　　　　　　　　　　　　
近藤亮太郎、村石 浩、榎本良治、片桐秀明、加賀谷美佳、成田尚史、渡辺 宝、加納大輔、武田 徹、内田智久、田中真伸
2019年 第66回応用物理学会春季学術大会, Mar. 2019
20190309, 20190312

SOIピクセルセンサーを用いた電子飛跡検出型コンプトンカメラの反跳電子飛跡検出の性能評価
加藤凌; 片桐秀明; 加賀谷美佳; 東城直美; 新井康夫; 内田智久; 武田彩希; 鶴剛
日本物理学会第74回年次大会, Mar. 2020
201903, 201903

SOIピクセルセンサーを用いた電子飛跡検出型コンプトンカメラの反跳電子飛跡検出の性能評価
加藤凌; 片桐秀明; 加賀谷美佳; 東城直美; 新井康夫; 内田智久; 武田彩希; 鶴剛
日本物理学会第74回年次大会, Mar. 2019
201903, 201903

ガンマ線カメラ ガンマアイ　　　　　　　　　　　　　　　
片桐秀明
オートラジオグラフィ技術の研究会, 17 Jan. 2019, [Invited]
201901, 201901

無機シンチレーターを用いた高線量場用コンプトン型全方向ガンマ線カメラの実証試験　　　　　　　　　　　　　　　
片桐 秀明
日本原子力学会2018年春の年会, 26 Mar. 2018

CTA報告131：CTA 大口径望遠鏡のモンテカルロシミュレーションによる月光下での性能評価　　　　　　　　　　　　　　　
三浦智佳; 大石理子; 奥村曉; 折戸玲子; 片桐秀明; 他CTA-Japan consortium
日本物理学会第73回年次大会, Mar. 2018
201803, 201803

CTA報告136：ガンマ線望遠鏡CTAにおけるSiPMの多チャンネル同時較正手法の実機検証　　　　　　　　　　　　　　　
中村裕樹; 奥村曉; 片桐秀明; 他CTA Consortium
日本物理学会第73回年次大会, Mar. 2018
201803, 201803

地上ガンマ線望遠鏡 CTA のための高効率な集光装置の試作　　　　　　　　　　　　　　　
奥村曉; Dang Viet Tan; 林田将明; Hinton Jim; 片桐秀明; 他CTA Consortium
日本物理学会第73回年次大会, Mar. 2018
201803, 201803

CTA報告138：CTA大口径望遠鏡の分割鏡制御システム
野田 浩司; 千川 道幸; 中嶋 大輔; 林田 将明; 山本 常夏; 吉田 龍生; 李 健; 他CTA-Japan consortium; 深見 哲志; 手嶋 政廣; 稲田 知大; 奥村 曉; 加賀谷 美佳; 片桐 秀明; 黒田 隼人; 齋藤 隆之
日本物理学会講演概要集, 2018, 一般社団法人 日本物理学会

CTA報告137：CTA大口径望遠鏡分割鏡性能評価と開発状況について
稲田 知大; 中嶋 大輔; 林田 将明; 深見 哲志; 山本 常夏; 吉田 龍生; 李 健; 他CTA-Japan Consortium; 手嶋 政廣; 野田 浩司; 奥村 曉; 加賀谷 美佳; 片桐 秀明; 黒田 隼人; 齋藤 隆之; 千川 道幸
日本物理学会講演概要集, 2018, 一般社団法人 日本物理学会

Visualization of Radium-223 chloride using an omnidirectional gamma-ray imaging Compton camera for radioactive environmental monitoring　　　　　　　　　　　　　　　
H. Muraishi; R. Kondo; T. Watanabe; R. Enomoto; H. Katagiri; M. Kagaya; D. Kano; T. Takeda; S. Noda; K. Kikuchi; H. Hara; T. Maegaki; T. Uchida; M. Tanaka
2018 IEEE Nuclear Science Symposium and Medical Imaging Conference, 2018

CsI (Tl) 結晶シンチレータを用いた可搬型キュリーメータの開発　　　　　　　　　　　　　　　
加賀谷美佳; 榎本良治; 片桐秀明; 他ガンマアイチーム
日本物理学会第72回年次大会, Mar. 2017
201703, 201703

最小カウンター数で高感度に全方向ガンマ線イメージングできるコンプトン型カメラの開発　　　　　　　　　　　　　　　
若松諒; 加納大輔; 榎本良治; 加賀谷美佳; 片桐秀明; 他ガンマアイチーム
日本物理学会第72回年次大会, Mar. 2017
201703, 201703

高線量場用全方向ガンマ線イメージングカメラの開発と実証試験結果　　　　　　　　　　　　　　　
佐藤亘; 片桐秀明; 他ガンマアイチーム
日本物理学会第72回年次大会, Mar. 2017
201703, 201703

次世代ガンマ線望遠鏡CTAにおける波形記録回路TARGETの時間応答較正手法の開発　　　　　　　　　　　　　　　
重中茜; 片桐秀明; 奥村曉; 田島宏康; 中村裕樹; 他 CTA Consortium
日本物理学会第72回年次大会, Mar. 2017
201703, 201703

CTA報告123：全体報告
窪 秀利; 井上 剛志; He Haoning; Majumdar Pratik; Mazin Daniel; 増田 周; 松本 浩典; 三浦 知佳; 水野 恒史; 村石 浩; 村瀬 孔大; 森 浩二; 井上 芳幸; 柳田 昭平; 山崎 了; 山本 常夏; 山本 宏昭; 吉池 智史; 吉越 貴紀; 吉田 篤正; 吉田 龍生; 李 健; 李 兆衡; 猪目 祐介; 岩村 由樹; Warren Donald; 内山 泰伸; 大石 理子; 大岡 秀行; 大平 豊; 岡崎 奈緒; 手嶋 政廣; 奥村 曉; 折戸 玲子; 加賀谷 美佳; 格和 純; 片岡 淳; 片桐 秀明; 勝倉 大輔; 勝田 哲; 加藤 翔; 神本 匠; 戸谷 友則; 川中 宣太; 木坂 将大; 木村 颯一朗; Cui Xiaohong; 櫛田 淳子; 久門 拓; 黒田 隼人; 郡司 修一; 郡 和範; 小山 志勇; 浅野 勝晃; Kong Albert K. H; 齋藤 隆之; 榊 直人; 櫻井 駿介; 佐々井 義矩; 佐野 栄俊; 澤田 真理; 柴田 徹; Dzhatdoev Timur; 砂田 裕志; 朝野 彰; 関崎
日本物理学会講演概要集, 2017, 一般社団法人 日本物理学会

CTA報告122：CTA大口径望遠鏡の光学性能最適化に向けた分割鏡測定とその配置の検討
稲田 知大; 千川 道幸; 手嶋 政廣; 中嶋 大輔; 深見 哲志; 本橋 大輔; 山本 常夏; 吉越 貴紀; 吉田 龍生; 他CTA-Japan consortium; 林田 将明; 野田 浩司; 奥村 曉; 加賀谷 美佳; 片桐 秀明; 黒田 隼人; 齋藤 隆之; 重中 茜
日本物理学会講演概要集, 2017, 一般社団法人 日本物理学会

CTA報告117：全体報告
手嶋 政廣; 井上 進; 藤田 裕; He Haoning; Majumdar Pratik; Mazin Daniel; 増田 周; 松本 浩典; 水野 恒史; 村石 浩; 村瀬 孔大; 本橋 大輔; 井上 剛志; 森 浩二; 柳田 昭平; 山崎 了; 山根 暢仁; 山本 常夏; 山本 宏昭; 吉池 智史; 吉越 貴紀; 吉田 篤正; 吉田 龍生; 井上 芳幸; 吉田 麻佑; 李 兆衡; 猪目 祐介; 岩村 由樹; Warren Donald; 内山 泰伸; 梅津 陽平; 大石 理子; 大岡 秀行; 窪 秀利; 大平 豊; 岡崎 奈緒; 奥村 曉; 折戸 玲子; 加賀谷 美佳; 格和 純; 片岡 淳; 片桐 秀明; 加藤 翔; 川中 宣太; 戸谷 友則; 木坂 将大; 岸田 柊; 木村 颯一朗; Cui Xiaohong; 櫛田 淳子; 黒田 隼人; 郡司 修一; 郡 和範; 小山 志勇; Kong Albert K. H; 朝野 彰; 今野 裕介; 齋藤 隆之; 榊 直人; 櫻井 駿介; 佐藤 雄太; 佐野 栄俊; 澤田 真理; 重中 茜; 柴田 徹; 高田 順平; 浅野 勝晃
日本物理学会講演概要集, 2017, 一般社団法人 日本物理学会

コンプトンカメラを用いた尿中FDG放射能濃度の測定　　　　　　　　　　　　　　　
若松 諒,細川 翔太; 榎本 良治,加納 大輔,加賀谷 美佳,片桐 秀明; 他ガンマアイチーム
第112回日本医学物理学会学術大会, Sep. 2016
201609, 201609

Development of an all-sky RI imaging monitor capable of measuring high-dose-rate gamma-ray sources　　　　　　　　　　　　　　　
T. Watanabe; R. Enomoto; M. Kagaya; H. Katagiri; D. Kano; H. Muraishi; T. Nishio; K. Satoh; W. Satoh; T. Takeda; M. Tanaka; T. Uchida; K. Wada; R. Wakamatsu; T. Yoshida; Open-it consortium
日本医学物理学会, Apr. 2016
201604, 201604

Performance of radiation spectrometer for education of radiation physics　　　　　　　　　　　　　　　
T. Maegaki; H. Muraishi; R. Enomoto; M. Doi; H. Inagaki; M. Kagaya; H. Katagiri; M. Satoh; W. Satoh; H. Sanada; T. Takeda; M. Tanaka; T. Uchida; R. Wakamatsu; T. Watanabe; T. Yoshida
第111回日本医学物理学会学術大会, Apr. 2016
201604, 201604

Performance of radiation spectrometer for education of radiation physics　　　　　　　　　　　　　　　
16.T. Maegaki; H. Muraishi; R. Enomoto; M. Doi; H. Inagaki; M. Kagaya; H. Katagiri; M. Satoh; W. Satoh; H. Sanada; T. Takeda; M. Tanaka; T. Uchida; R. Wakamatsu; T. Watanabe; T. Yoshida
第111回日本医学物理学会学術大会, Apr. 2016

22pAM-2 次世代ガンマ線望遠鏡CTAで用いる波形記録回路TARGETの時間応答特性の評価
重中 茜; 片桐 秀明; 田島 宏康; 奥村 曉; the CTA Consortium
日本物理学会講演概要集, 19 Mar. 2016, 一般社団法人日本物理学会

CTA大口径望遠鏡による2FHL ソースの観測シミュレーション　　　　　　　　　　　　　　　
Dang Viet Tan
日本天文学会, Mar. 2016

ガンマ線の到来方向が判断できる4チャンネル型高感度サーベイメータの開発　　　　　　　　　　　　　　　
若松 諒
日本物理学会, Mar. 2016

シンチレータを用いた高線量場測定用コンプトンカメラの開発　　　　　　　　　　　　　　　
佐藤 亘
日本物理学会, Mar. 2016

CsI(Tl)シンチレータによるオールスカイガンマ線コンプトンカメラの開発　　　　　　　　　　　　　　　
村石 浩
日本物理学会, Mar. 2016

CTA 報告115：CTA大口径望遠鏡用Active Mirror Controlシステムのソフトウェア開発
深見 哲志; 重中 茜; 千川 道幸; 手嶋 政廣; 中嶋 大輔; 本橋 大輔; 山本 常夏; 吉田 龍生; 他CTA-Japan consortium; 野田 浩司; 林田 将明; 稲田 知大; 奥村 曉; 加賀谷 美佳; 片桐 秀明; 黒田 隼人; 齋藤 隆之
日本物理学会講演概要集, 2016, 一般社団法人 日本物理学会

22aAT-6 CTA報告107 : CTA大口径望遠鏡用分割鏡の性能評価
長 紀仁; 岸田 柊; 齋藤 隆之; 重中 茜; 千川 道幸; 手嶋 政廣; 中嶋 大輔; 野田 浩司; 花畑 義隆; 深見 哲志; 本橋 大輔; 林田 将明; 山本 常夏; 吉田 龍生; CTA-Japan consortium; 稲田 知大; 岩村 由樹; 奥村 曉; 小野 祥弥; 加賀谷 美佳; 片桐 秀明; 加藤 翔
日本物理学会講演概要集, 2016, 一般社団法人 日本物理学会

Gamma-ray Observations of SNRs by Fermi and CTA　　　　　　　　　　　　　　　
SNSNR2015 Symposium on Supernovae and Supernova Remnants, 09 Nov. 2015, [Invited]

γ I（ガンマアイ）による電子陽電子対消滅ラインガンマ線の探査　　　　　　　　　　　　　　　
片桐 秀明
2015年大気球シンポジウム, 06 Nov. 2015

コンプトンカメラ法による All Sky RI イメージングモニターの開発　　　　　　　　　　　　　　　
日本医学物理学会, Sep. 2015

高感度で到来方向がわかるサーベイメータの開発　　　　　　　　　　　　　　　
若松 諒
日本物理学会, Sep. 2015

無機シンチレータのエネルギー分解能の測定によるコンプトンカメラの角度分解能の評価　　　　　　　　　　　　　　　
佐藤 亘
日本物理学会, Sep. 2015

ガンマ線の到来方向がわかるコンプトン型サーベイメータの開発　　　　　　　　　　　　　　　
加賀谷 美佳
日本医学物理学会, Sep. 2015

コンプトンカメラ法による高感度360°パノラマRIイメージングモニタの開発　　　　　　　　　　　　　　　
渡辺 宝
日本医用画像工学会大会, Jul. 2015

CsI (Tl) 結晶を用いたコンプトンカメラ "ガンマアイ" の開発　　　　　　　　　　　　　　　
加賀谷 美佳
日本医学物理学会, Apr. 2015

CsI(Tl)結晶を用いた360度パノラマコンプトンカメラの開発　　　　　　　　　　　　　　　
渡辺 宝
日本医学物理学会, Apr. 2015

ガンマ線の到来方向がわかる放射性セシウム用サーベイメータの開発　　　　　　　　　　　　　　　
加賀谷 美佳
日本物理学会, 24 Mar. 2015

コンプトンカメラγI（ガンマアイ）の高角度分解能化に向けた32chプロトタイプの開発　　　　　　　　　　　　　　　
中山 浩平
日本物理学会, 24 Mar. 2015

CsI(Tl)結晶シンチレータを用いたガンマ線カメラγI（ガンマアイ）の開発　　　　　　　　　　　　　　　
中山 浩平
日本原子力学会, Mar. 2015

ガンマアイ360度パノラマモニターの開発　　　　　　　　　　　　　　　
加賀谷 美佳
日本物理学会, 21 Sep. 2014

コンプトンカメラγI（ガンマアイ）の高角度分解能化に向けた開発　　　　　　　　　　　　　　　
中山 浩平
日本物理学会, 21 Sep. 2014

フェルミ・ガンマ線宇宙望遠鏡による超新星残骸HB3(G132.7+1.3)の観測　　　　　　　　　　　　　　　
吉田和人
日本物理学会, 19 Sep. 2014

フェルミ・ガンマ線宇宙望遠鏡による超新星残骸Monoceros Loopの観測　　　　　　　　　　　　　　　
片桐 秀明
日本物理学会, 19 Sep. 2014

コンプトンカメラγI（ガンマアイ）の16チャンネルプロトタイプの開発　　　　　　　　　　　　　　　
加賀谷美佳; 内田智久; 榎本良治; 佐藤一弘; 片桐秀明; 武田徹; 田中真伸; 中山浩平; 花房龍治; 村石浩; 柳田昭平; 吉田龍生; オープンソースコンソーシアム(Open-I
日本物理学会, 30 Mar. 2014

フィールドワークによるコンプトンカメラγI（ガンマアイ）の実証試験　　　　　　　　　　　　　　　
片桐秀明; 内田智久; 榎本良治; 加賀谷美佳; 佐藤一弘; 武田徹; 田中真伸; 中山浩平; 花房龍治; 村石浩; 柳田昭平; 吉田龍生; オープンソースコンソーシアム(Open-I
日本物理学会, 30 Mar. 2014

CTA 報告71：CTA大口径望遠鏡用ライトガイドの試作機性能評価及び形状最適化に向けた研究　　　　　　　　　　　　　　　
田中駿也; 林田将明; 奥村曉; 片桐秀明; 手嶋政廣; 大岡秀行; 荻野桃子; 加賀谷美佳; 小島拓実; 齋藤浩二; 千川道幸; 中嶋大輔; 野里明香; 野田浩司; 花畑義隆; 馬場浩則; 柳田昭平; 山本常夏; 吉田龍生; 他CTA-Japan consortium
日本物理学会, 27 Mar. 2014

CTA 大口径望遠鏡の分割鏡の開発(6)　　　　　　　　　　　　　　　
馬場浩則; 加賀谷美佳; 片桐秀明; 田中駿也; 吉田龍生; 手嶋政廣; 研; Max-Planck-Inst. fuer Phys; 荻野桃子; 小島拓実; 斎藤浩二; 中嶋大輔; 花畑義隆; 林田将明; 奥村曉(名大; STE 研; レスター大; 千川道幸; 野里明香; 野田浩司(Max-Planck-Inst. fuer Phy; 山本常夏; 他CTA-Japan Consortium
日本天文学会, 22 Mar. 2014

コンプトンカメラ法による新しいγ 線イメージング装置(γI：ガンマアイ)の開発　　　　　　　　　　　　　　　
村石 浩
第107 回日本医学物理学会学術大会, 2014

コンプトンカメラγI（ガンマアイ）12チャンネルプロトタイプ検出器の開発　　　　　　　　　　　　　　　
加賀谷美佳; 内田智久; 榎本良治; 佐藤一弘; 片桐秀明; 武田徹; 田中真伸; 中山浩平; 花房龍治; 村石浩; 柳田昭平; 吉田龍生; オープンソースコンソーシアム(Open-I
日本物理学会, 22 Sep. 2013

コンプトンカメラγI（ガンマアイ）実用化に向けたγI16の開発　　　　　　　　　　　　　　　
中山浩平; 内田智久; 榎本良治; 加賀谷美佳; 佐藤一弘; 片桐秀明; 武田徹; 田中真伸; 花房龍治; 村石浩; 柳田昭平; 吉田龍生; オープンソースコンソーシアム(Open-I
日本物理学会, 22 Sep. 2013

CTA 報告62：CTA 大口径望遠鏡用ライトガイドの試作機性能評価及び大量生産に向けた開発　　　　　　　　　　　　　　　
田中駿也; 林田将明; 奥村曉; 手嶋政廣; 大岡秀行; 加賀谷美佳; 片桐秀明; 齋藤浩二; 千川道幸; 中嶋大輔; 野里明香; 野田浩司; 花畑義隆; 馬場浩則; 柳田昭平; 山本常夏; 吉田龍生; 他CTA-Japan consortium
日本物理学会, 22 Sep. 2013

CTA 報告63：CTA 大口径望遠鏡用分割鏡の形状測定システムであるPhase Measuring Deflectometry法の開発　　　　　　　　　　　　　　　
馬場浩則; 手嶋政廣; 中嶋大輔; 林田将明; 齋藤浩二; 花畑義隆; 佐々木浩人; 吉田龍生; 奥村曉; 加賀谷美佳; 片桐秀明; 田中駿也; 千川道幸; 野里明香; 野田浩司; 柳田昭平; 山本常夏; 他 CTA-Japan consortium; R.Krobot
日本物理学会, 22 Sep. 2013

ガンマ線の方向のわかる検出器ガンマアイ　　　　　　　　　　　　　　　
榎本 良治; 加賀谷 美佳; 片桐 秀明; 中山 浩平; 村石 浩; 吉田 龍生; 柳田 昭平
「次期電子デバイス・太陽電池の展開、および清浄環境の必要性と未来」, 19 Jul. 2013, [Invited]

ガンマ線の方向のわかる検出器ガンマアイ　　　　　　　　　　　　　　　
榎本 良治; 加賀谷 美佳; 片桐 秀明; 中山 浩平; 村石 浩; 吉田 龍生; 柳田 昭平
第50回アイソトープ・放射線研究発表会, 05 Jul. 2013, [Invited]

フェルミ⋅ガンマ線宇宙望遠鏡による超新星残骸W28周辺領域の観測　　　　　　　　　　　　　　　
花畑義隆; 深沢泰司; 水野恒史; 高橋弘充; 大野雅功; 田中康之; 大杉節; 片桐秀明; 福井康雄; 早川貴敬
日本天文学会, Mar. 2013

コンプトンカメラγI（ガンマアイ）のプロトタイプ製作　　　　　　　　　　　　　　　
片桐秀明; 内田智久; 梅原克典; 榎本良治; 加賀谷美佳; 田中真伸; 中山浩平; 花房龍治; 村石浩; 柳田昭平; 吉田龍生; 他 オープンソースコンソーシアム(Open-It
日本物理学会, Mar. 2013

CsI結晶シンチレータを用いたコンプトンカメラγI（ガンマアイ）の開発（2）　　　　　　　　　　　　　　　
加賀谷美佳; 内田智久; 梅原克典; 榎本良治; 片桐秀明; 田中真伸; 中山浩平; 花房龍治; 村石浩; 柳田昭平; 吉田龍生; 他 オープンソースコンソーシアム(Open-It
日本物理学会, Mar. 2013

Application of a filtered back projection algorithm to Compton camera technique　　　　　　　　　　　　　　　
村石 浩; 榎本 良治; 加賀谷 美佳; 片桐 秀明; 武田 徹; 中山 浩平; 柳田 昭平; 吉田 龍生
日本医学物理学会, 2013

CTA 大口径望遠鏡の分割鏡の開発(3)　　　　　　　　　　　　　　　
加賀谷; 美佳; 奥村 曉; 名大ST; 片桐 秀明; 北本 兼続; 峪中 良介; 周 小溪; 田中 駿也; 千川 道幸; 手嶋 政廣; 宇宙線研; Max-Planck-Inst.fuer Phys; 中嶋 大輔(Max; Planck-Inst; 野里 明香; 林田 将明; 柳田 昭平; 山本 常夏; 吉田 龍生; R.Krobot(University Erlangen; ほかCTA-Japan consortium
日本天文学会, 20 Sep. 2012

CsI結晶シンチレータを用いたコンプトンカメラγI（ガンマアイ）の開発　　　　　　　　　　　　　　　
加賀谷美佳A; 梅原克典A; 榎本良治B; 片桐秀明A; 村石浩C; 柳田昭平A; 吉田龍生A; 城大理A; 東大宇宙線研B; 北里大医衛
日本物理学会, 14 Sep. 2012

CsI(Tl)による方向のわかるガンマ線検出器（γI：ガンマアイ）の概要　　　　　　　　　　　　　　　
榎本良治; 梅原克典A; 加賀谷美佳A; 片桐秀明A; 村石浩B; 柳田昭平A; 吉田龍生A; 宙線研; 茨城理A; 北里医衛
日本物理学会, 14 Sep. 2012

CTA報告42：CTA 大口径望遠鏡用焦点面検出器の開発　　　　　　　　　　　　　　　
梅原克典; 粟根悠介A; 上野遥B; 大岡秀行C; 奥村曉D; 折戸玲子E; 片桐秀明; 株木重人F; 櫛田淳子G; 窪秀利A; 郡司修一H; 小谷一仁G; 小山志勇B; 今野裕介A; 齋藤浩二C; 佐々木浩人I; 渋谷明伸D; 菅原隆希E; 高橋弘充J; 田島宏康D; 田中駿也; 千川道幸K; 手嶋政廣C; 寺田幸功B; 門叶冬樹G; 中嶋大輔C; 中森健之L; 西嶋恭司G; 萩原亮太H; 馬場彩M; 林田将明A; 日高直哉D; 深沢泰司J; 水野恒史J; 山本常夏I; 吉田篤正M; Razmik MirzoyanN; Olaf ReimannN; David FinkN; Thomas SchweizerN; 他 CTA-Japan Consortium
日本物理学会, 13 Sep. 2012

CTA 報告46:CTA 大口径望遠鏡用分割鏡の開発:形状測定システム　　　　　　　　　　　　　　　
馬場浩則A; 奥村曉F; 加賀谷美佳A; 片桐秀明A; 北本兼続E; 峪中良介E; 周小溪E; 田中駿也A; 千川道幸E; 手嶋政廣B; 中嶋大輔C; 野里明香E; 林田将明G; 柳田昭平A; 山本常夏D; 吉田龍生A; R.KrobotH; 他 CTA-Japan consortium
日本物理学会, 13 Sep. 2012

14aSH-3 CsI結晶シンチレータを用いたコンプトンカメラγI(ガンマアイ)の開発(14aSH 光検出器・カウンター,素粒子実験領域)
加賀谷 美佳; 梅原 克典; 榎本 良治; 片桐 秀明; 村石 浩; 柳田 昭平; 吉田 龍生
日本物理学会講演概要集, 24 Aug. 2012, 一般社団法人日本物理学会

フェルミ・ガンマ線宇宙望遠鏡による超新星残骸「白鳥座ループ」の観測と放射機構の考察　　　　　　　　　　　　　　　
片桐秀明; Luigi Tibaldo; Jean Ballet; Francesco Giordano; Isabelle A. Grenier; Troy A. Porter; Marshall Roth; Omar Tibolla; 内山泰伸; 山崎了
日本天文学会, 22 Sep. 2011

フェルミ・ガンマ線宇宙望遠鏡による超新星残骸「白鳥座ループ」の観測と放射機構の考察　　　　　　　　　　　　　　　
片桐秀明; Luigi Tibaldo; Jean Ballet; Francesco Giordano; Isabelle A. Grenier; Troy A. Porter; Marshall Roth; Omar Tibolla; 内山泰伸; 山崎了
日本物理学会, 18 Sep. 2011

CTA報告34：CTA大口径望遠鏡のための焦点面検出器の開発　　　　　　　　　　　　　　　
梅原克典; 粟根悠介A; 榎本良治B; 大岡秀行B; 奥村曉C; 折戸玲子D; 片桐秀明; 株木重人E; 櫛田淳子F; 窪秀利A; 黒田和典; 郡司修一G; 小谷一仁F; 小山志勇H; 今野裕介A; 佐々木美佳; 渋谷明伸C; 菅原隆希D; 高橋弘充I; 田島宏康C; 谷森達A; 千川道幸J; 千葉順成K; 手嶋政廣B; 寺田幸功H; 門叶冬樹G; 中森健之L; 西嶋恭司F; 林田将明A; 馬場彩M; 日高直哉C; 深沢泰司I; 水野恒史I; 山岡和貴M; 山本常夏N; 吉田篤正M; 米谷光生I; Razmik MirzoyanO; Olaf ReimannO; David FinkO; Thomas SchweizerO; 他 CTA-Japan Consortium
日本物理学会, 24 Mar. 2011

CTA報告34：CTA大口径望遠鏡のための焦点面検出器の開発　　　　　　　　　　　　　　　
梅原克典; 粟根悠介A; 榎本良治B; 大岡秀行B; 奥村曉C; 折戸玲子D; 片桐秀明; 株木重人E; 櫛田淳子F; 窪秀利A; 黒田和典; 郡司修一G; 小谷一仁F; 小山志勇H; 今野裕介A; 佐々木美佳; 渋谷明伸C; 菅原隆希D; 高橋弘充I; 田島宏康C; 谷森達A; 千川道幸J; 千葉順成K; 手嶋政廣B; 寺田幸功H; 門叶冬樹G; 中森健之L; 西嶋恭司F; 林田将明A; 馬場彩M; 日高直哉C; 深沢泰司I; 水野恒史I; 山岡和貴M; 山本常夏N; 吉田篤正M; 米谷光生I; Razmik MirzoyanO; Olaf ReimannO; David FinkO; Thomas SchweizerO; 他 CTA-Japan Consortium
日本物理学会, 24 Mar. 2011

CTA報告36：CTA大口径望遠鏡用分割鏡の開発　　　　　　　　　　　　　　　
加賀谷美佳; 榎本良治B; 奥村曉F; 片桐秀明A; 黒田和典A; 周小溪E; 千川道幸E; 手嶋政廣B; 林田将明G; 柳田昭平A; 山本常夏D; 吉田龍生A; 他 CTA-Japan consortium
日本物理学会, 24 Mar. 2011

CTA報告37：CTA大口径望遠鏡用ライトガイドの開発　　　　　　　　　　　　　　　
黒田和典; 片桐秀明A; 吉田龍生A; 柳田昭平A; 加賀谷美佳A; 手嶋政廣B; 榎本良治B; 奥村曉C; 林田将明D; 山本常夏E; 千川道幸F; ほかCTA-Japan一同
日本物理学会, 24 Mar. 2011

The Astronomical Society of Japan

The Physical Society of Japan

Investigation of a gamma-ray Compton camera for visualizing dose distribution during proton therapy
Grant-in-Aid for Scientific Research (B)
Kitasato University
Apr. 2023 - Mar. 2027

暗黒物質探査に特化した半導体を用いた電子飛跡検出型コンプトンカメラの開発
基盤研究(B)
仙台高等専門学校
Apr. 2022 - Mar. 2027

脱励起ラインガンマ線で探る銀河系内宇宙線の起源
基盤研究(C)
茨城大学
Apr. 2022 - Mar. 2025

放射線治療に用いる陽子線・重粒子線ビームで生じるガンマ線の計測に特化した革新的ガンマ線カメラの開発　　　　　　　　　　　　　　　
Apr. 2021 - Mar. 2023

高感度γ線コンプトンカメラ技術の医療現場への実践的展開
Grant-in-Aid for Scientific Research (B)
北里大学
Apr. 2019 - Mar. 2023

脱励起ラインガンマ線観測で解明する銀河系内宇宙線の起源　　　　　　　　　　　　　　　
基盤研究(B)
Apr. 2019 - Mar. 2022

大口径大気チェレンコフγ線望遠鏡の稼働で迫る高エネルギー天体現象の発展的理解
基盤研究(A)
京都大学
Apr. 2017 - Mar. 2021

原木シイタケ栽培のための立木・原木測定用の可搬型放射能検査装置の開発　　　　　　　　　　　　　　　
機能検証フェーズ A-STEP機能検証フェーズ 試験研究タイプ
仙台高等専門学校
2019 - Nov. 2020

Study of dark matter using a advanced Compton camera with 3D-semiconductor detector
Grant-in-Aid for Young Scientists (B)
Sendai National College of Technology
01 Apr. 2017 - 31 Mar. 2019

核融合、放射線治療、宇宙観測分野で応用可能な革新的ガンマ線カメラの原理実証　　　　　　　　　　　　　　　
平成30年度研究推進経費（Research Booster）
Jul. 2018 - Mar. 2019

結晶シンチレータによる医療用高感度γ線コンプトンカメラの開発　　　　　　　　　　　　　　　
Apr. 2015 - Mar. 2019

ガンマ線可視化カメラの開発　　　　　　　　　　　　　　　
Jan. 2017 - Mar. 2018

放射能汚染地域におけるシイタケ原木林の利用再開・再生技術の開発　　　　　　　　　　　　　　　
農林水産業・食品産業科学技術研究推進事業 【実用技術開発ステージ】 （現場ニーズ対応型）
2016 - 2018

究極感度GeV・TeV広帯域宇宙ガンマ線観測による高エネルギー天体の研究　　　　　　　　　　　　　　　
Grant-in-Aid for Scientific Research(A)
Apr. 2012 - Mar. 2017

放射線の到来方向が分かる低コストかつ好感度な検出器「ガンマアイ」の分野横断的な応用可能性の開拓　　　　　　　　　　　　　　　
2015 - 2017

ガンマ線可視化カメラの開発　　　　　　　　　　　　　　　
Nov. 2015 - Sep. 2016

Development and verification of a large-area semiconductor Cherenkov camera
Grant-in-Aid for Scientific Research (A)
Nagoya University
01 Apr. 2011 - 31 Mar. 2016

ガンマ線可視化カメラの開発　　　　　　　　　　　　　　　
May 2014 - Mar. 2015

新手法を用いたラインガンマ線用コンプトンカメラによる宇宙暗黒物質の探索　　　　　　　　　　　　　　　
Grant-in-Aid for Exploratory Research
Apr. 2014 - Mar. 2015

方向の分かる放射線セシウム用サーベイメーターの開発　　　　　　　　　　　　　　　
茨城大学イノベーション研究推進プログラム
2014 - 2015

セシウム137からのガンマ線の到来方向が分かる安価な高感度放射線検出器「ガンマアイ」の改良　　　　　　　　　　　　　　　
茨城大学復興支援プロジェクト
2014 - 2015

セシウム137からのガンマ線の到来方向が分かる安価な高感度放射線検出器の開発　　　　　　　　　　　　　　　
茨城大学復興支援プロジェクト
Apr. 2013 - 2015

ガンマアイ（γＩ）コンプトンカメラの研究開発　　　　　　　　　　　　　　　
2013 - 2014

セシウム137からのガンマ線の到来方向が分かる安価な高感度放射線検出器の開発　　　　　　　　　　　　　　　
茨城大学復興支援プロジェクト
2013 - 2014

GeVガンマ線全天サーベイによる超新星残骸における宇宙線加速の系統的研究
Grant-in-Aid for Young Scientists(B)
Ibaraki University
Apr. 2010 - Mar. 2012

大規模チェレンコフ望遠鏡アレイ計画における分割鏡等の準備研究
Grant-in-Aid for Scientific Research(A)
The University of Tokyo
Apr. 2010 - Mar. 2012

宇宙ガンマ線観測用大規模チェレンコフ望遠鏡計画（CTA）の焦点面検出器用較正システムの立ち上げ　　　　　　　　　　　　　　　
Apr. 2010 - Mar. 2011

Study of cosmic-ray energy and spatial distribution by observing Galactic diffuse gamma-ray emission
Grant-in-Aid for Scientific Research (B)
Hiroshima University
2009 - 2011

GeVガンマ線観測による超新星残骸における宇宙線加速機構の研究
Grant-in-Aid for Young Scientists(B)
Hiroshima University
Apr. 2007 - Mar. 2009

高感度GeVγ線観測で探る巨大ブラックホールの進化とジェットの放出機構
特定領域研究
広島大学
2002 - 2006

特許第7207646, 特開2020-41930, 特願2018-170201, 放射能測定装置、放射能測定方法、放射能情報処理サーバおよび放射能情報処理システム
加賀谷 美佳, 片桐 秀明, 榎本 良治

特開2021-60320, 2019-185442, ガンマ線測定システム、ガンマ線測定方法、及びガンマ線測定プログラム
片桐 秀明

特許第6846800号(P6846800), 2018-151225, 2017-046902, 放射能測定システム及び放射能測定方法
片桐 秀明, 加賀谷 美佳

茨城大学ホームページの記事「研究に恋して」に寄稿
contribution
18 Apr. 2022 - 18 Apr. 2022

茨城大学重点研究「宇宙科学教育研究センターを核とした宇宙惑星科学教育研究の新展開」サマリー研究会　　　　　　　　　　　　　　　
Planning etc
18 Dec. 2021 - 18 Dec. 2021

茨城大学重点研究 研究会：「突発・変動現象の電波フォローアップ」　　　　　　　　　　　　　　　
Planning etc
27 Feb. 2019 - 28 Feb. 2019

茨城大学重点研究 研究会：「高萩・日立32m電波望遠鏡によるサイエンス」　　　　　　　　　　　　　　　
Planning etc
20 Feb. 2018 - 21 Feb. 2018

茨城大学重点研究 研究会：「突発・変動天体の多波長連携観測」　　　　　　　　　　　　　　　
Planning etc
06 Mar. 2017 - 06 Mar. 2017

茨城大学推進研究プロジェクト研究会：中性子を用いた研究の現場におけるガンマ線可視化技術の応用　　　　　　　　　　　　　　　
Planning etc
14 Sep. 2016 - 14 Sep. 2016

茨城大学重点研究 研究会「偏波・偏光観測によるサイエンス」　　　　　　　　　　　　　　　
Planning etc
Jan. 2016 - Jan. 2016

茨城大学推進研究プロジェクト研究会 「様々な変光現象とその観測的アプローチ」　　　　　　　　　　　　　　　
Planning etc
Mar. 2013 - Mar. 2013

茨城大学推進研究プロジェクト・ミニワークショップ 「マイクロ波帯観測が切り開く宇宙科学・地球科学の未来」　　　　　　　　　　　　　　　
Planning etc
Jan. 2012 - Jan. 2012