FERMI LARGE AREA TELESCOPE VIEW OF THE CORE OF THE RADIO GALAXY CENTAURUS A
FERMI LARGE AREA TELESCOPE VIEW OF THE CORE OF THE RADIO GALAXY CENTAURUS A
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DOI：
10.1088/0004-637x/719/2/1433
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发表时间：
2010-06
期刊：
影响因子：
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通讯作者：
A. Abdo;A. Abdo;M. Ackermann;M. Ajello;W. Atwood;L. Baldini;J. Ballet;G. Barbiellini;G. Barbiellini;D. Bastieri;D. Bastieri;B. Baughman;K. Bechtol;R. Bellazzini;B. Berenji;R. Blandford;E. Bloom;E. Bonamente;E. Bonamente;A. Borgland;A. Bouvier;T. Brandt;J. Bregeon;A. Brez;M. Brigida;M. Brigida;P. Bruel;R. Buehler;S. Buson;S. Buson;G. Caliandro;R. Cameron;A. Cannon;A. Cannon;P. Caraveo;S. Carrigan;J. Casandjian;E. Cavazzuti;C. Cecchi;C. Cecchi;O. Celik;O. Celik;E. Charles;A. Chekhtman;A. Chekhtman;C. C. Cheung-C.;C. C. Cheung-C.;J. Chiang;S. Ciprini;R. Claus;J. Cohen-Tanugi;S. Colafrancesco;L. Cominsky;J. Conrad;J. Conrad;L. Costamante;D. Davis;D. Davis;C. Dermer;A. Angelis;F. Palma;F. Palma;E. Silva;P. Drell;R. Dubois;D. Dumora;A. Falcone;C. Farnier;C. Favuzzi;C. Favuzzi;S. Fegan;J. Finke;J. Finke;W. Focke;P. Fortin;M. Frailis;Y. Fukazawa;S. Funk;P. Fusco;P. Fusco;F. Gargano;D. Gasparrini;N. Gehrels;M. Georganopoulos;S. Germani;S. Germani;B. Giebels;N. Giglietto;N. Giglietto;P. Giommi;F. Giordano;F. Giordano;M. Giroletti;T. Glanzman;G. Godfrey;P. Grandi;I. Grenier;M. Grondin;J. Grove;L. Guillemot;S. Guiriec;D. Hadasch;A. Harding;H. Hase;M. Hayashida;E. Hays;D. Horan;R. Hughes;R. Itoh;M. Jackson;G. Jóhannesson;A. Johnson;T. Johnson;T. Johnson;W. Johnson;M. Kadler;T. Kamae;H. Katagiri;J. Kataoka;N. Kawai;T. Kishishita;J. Knödlseder;M. Kuss;J. Lande;L. Latronico;Sooheyong Lee;M. Lemoine-Goumard;M. Garde;F. Longo;F. Longo;F. Loparco;F. Loparco;B. Lott;M. Lovellette;P. Lubrano;P. Lubrano;A. Makeev;A. Makeev;M. Mazziotta;W. Mcconville;W. Mcconville;J. Mcenery;J. Mcenery;P. Michelson;W. Mitthumsiri;T. Mizuno;A. Moiseev;A. Moiseev;C. Monte;C. Monte;M. Monzani;A. Morselli;I. Moskalenko;S. Murgia;C. Müller;T. Nakamori;M. Naumann-Godo;P. Nolan;J. Norris;E. Nuss;M. Ohno;T. Ohsugi;R. Ojha;A. Okumura;N. Omodei;E. Orlando;J. Ormes;M. Ozaki;C. Pagani;D. Paneque;J. Panetta;D. Parent;V. Pelassa;M. Pepe;M. Pepe;M. Pesce-Rollins;F. Piron;C. Plötz;T. Porter;S. Rainò;S. Rainò;R. Rando;R. Rando;M. Razzano;S. Razzaque;S. Razzaque;A. Reimer;O. Reimer;T. Reposeur;J. Ripken;S. Ritz;A. Rodríguez;M. Roth;F. Ryde;H. Sadrozinski;D. Sanchez;A. Sander;J. Scargle;C. Sgro’;E. Siskind;P. Smith;G. Spandre;P. Spinelli;P. Spinelli;Jean-Luc Starck;L. Stawarz;M. Strickman;D. Suson;H. Tajima;H. Takahashi;Tadayuki Takahashi;Takaaki Tanaka;J. Thayer;J. Thayer;D. Thompson;L. Tibaldo;D. F. Torres;G. Tosti;G. Tosti;A. Tramacere;Y. Uchiyama;T. Usher;J. Vandenbroucke;V. Vasileiou;V. Vasileiou;N. Vilchez;V. Vitale;A. Waite;Pengfei Wang;B. Winer;K. Wood;Zhirong Yang;T. Ylinen;M. Ziegler
中科院分区：
文献类型：
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作者：
A. Abdo;A. Abdo;M. Ackermann;M. Ajello;W. Atwood;L. Baldini;J. Ballet;G. Barbiellini;G. Barbiellini;D. Bastieri;D. Bastieri;B. Baughman;K. Bechtol;R. Bellazzini;B. Berenji;R. Blandford;E. Bloom;E. Bonamente;E. Bonamente;A. Borgland;A. Bouvier;T. Brandt;J. Bregeon;A. Brez;M. Brigida;M. Brigida;P. Bruel;R. Buehler;S. Buson;S. Buson;G. Caliandro;R. Cameron;A. Cannon;A. Cannon;P. Caraveo;S. Carrigan;J. Casandjian;E. Cavazzuti;C. Cecchi;C. Cecchi;O. Celik;O. Celik;E. Charles;A. Chekhtman;A. Chekhtman;C. C. Cheung-C.;C. C. Cheung-C.;J. Chiang;S. Ciprini;R. Claus;J. Cohen-Tanugi;S. Colafrancesco;L. Cominsky;J. Conrad;J. Conrad;L. Costamante;D. Davis;D. Davis;C. Dermer;A. Angelis;F. Palma;F. Palma;E. Silva;P. Drell;R. Dubois;D. Dumora;A. Falcone;C. Farnier;C. Favuzzi;C. Favuzzi;S. Fegan;J. Finke;J. Finke;W. Focke;P. Fortin;M. Frailis;Y. Fukazawa;S. Funk;P. Fusco;P. Fusco;F. Gargano;D. Gasparrini;N. Gehrels;M. Georganopoulos;S. Germani;S. Germani;B. Giebels;N. Giglietto;N. Giglietto;P. Giommi;F. Giordano;F. Giordano;M. Giroletti;T. Glanzman;G. Godfrey;P. Grandi;I. Grenier;M. Grondin;J. Grove;L. Guillemot;S. Guiriec;D. Hadasch;A. Harding;H. Hase;M. Hayashida;E. Hays;D. Horan;R. Hughes;R. Itoh;M. Jackson;G. Jóhannesson;A. Johnson;T. Johnson;T. Johnson;W. Johnson;M. Kadler;T. Kamae;H. Katagiri;J. Kataoka;N. Kawai;T. Kishishita;J. Knödlseder;M. Kuss;J. Lande;L. Latronico;Sooheyong Lee;M. Lemoine-Goumard;M. Garde;F. Longo;F. Longo;F. Loparco;F. Loparco;B. Lott;M. Lovellette;P. Lubrano;P. Lubrano;A. Makeev;A. Makeev;M. Mazziotta;W. Mcconville;W. Mcconville;J. Mcenery;J. Mcenery;P. Michelson;W. Mitthumsiri;T. Mizuno;A. Moiseev;A. Moiseev;C. Monte;C. Monte;M. Monzani;A. Morselli;I. Moskalenko;S. Murgia;C. Müller;T. Nakamori;M. Naumann-Godo;P. Nolan;J. Norris;E. Nuss;M. Ohno;T. Ohsugi;R. Ojha;A. Okumura;N. Omodei;E. Orlando;J. Ormes;M. Ozaki;C. Pagani;D. Paneque;J. Panetta;D. Parent;V. Pelassa;M. Pepe;M. Pepe;M. Pesce-Rollins;F. Piron;C. Plötz;T. Porter;S. Rainò;S. Rainò;R. Rando;R. Rando;M. Razzano;S. Razzaque;S. Razzaque;A. Reimer;O. Reimer;T. Reposeur;J. Ripken;S. Ritz;A. Rodríguez;M. Roth;F. Ryde;H. Sadrozinski;D. Sanchez;A. Sander;J. Scargle;C. Sgro’;E. Siskind;P. Smith;G. Spandre;P. Spinelli;P. Spinelli;Jean-Luc Starck;L. Stawarz;M. Strickman;D. Suson;H. Tajima;H. Takahashi;Tadayuki Takahashi;Takaaki Tanaka;J. Thayer;J. Thayer;D. Thompson;L. Tibaldo;D. F. Torres;G. Tosti;G. Tosti;A. Tramacere;Y. Uchiyama;T. Usher;J. Vandenbroucke;V. Vasileiou;V. Vasileiou;N. Vilchez;V. Vitale;A. Waite;Pengfei Wang;B. Winer;K. Wood;Zhirong Yang;T. Ylinen;M. Ziegler
我们目前的γ射线观测与大面积望远镜（LAT）上的费米伽马射线太空望远镜附近的射电星系半人马座A（岑A）。证实了先前的EGRET探测，并使用费米科学运行前10个月的数据改进了定位。在以前的工作中，我们提出了通过LAT检测叶，在这项工作中，我们集中在γ射线核心的Cen A。LAT观测到的通量水平与EGRET观测到的通量水平没有显著差异，也没有非常软的LAT光谱（Γ = 2.67 ± 0.10stat ± 0.08sys，其中光子通量为Φ E−Γ）。LAT核心频谱，外推到更高的能量，是勉强一致的非同步HESS频谱的来源。LAT观测得到了来自朱雀的同步观测、Swift Burst Alert望远镜和X射线望远镜的补充，以及利用南方毫角秒干涉仪跟踪活动星系核计划进行的射电观测，沿着来自各种仪器和波长的各种非同步存档数据，以产生光谱能量分布（SED）。我们用单区同步加速器/同步加速器自康普顿模型拟合了这个宽带数据集，该模型很好地描述了GeV辐射的无线电，但未能解释HESS在2004年至2008年期间观察到的非同步高能TeV辐射。该拟合需要低多普勒因子，与BL Lac对象相反，BL Lac对象通常需要较大的值来拟合其宽带SED。这表明γ射线发射来自比BL Lac天体更慢的区域，与之前Cen A的模拟结果一致。这个较慢的区域可能是围绕快速脊柱的较慢移动层，或者是在减速流中远离黑洞的较慢区域。拟合参数也与Cen A能够加速超高能宇宙射线一致，正如Auger天文台的结果所暗示的那样。
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 ± 0.10stat ± 0.08sys where the photon flux is Φ ∝ 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.