FERMI DISCOVERY OF GAMMA-RAY EMISSION FROM NGC 1275

被引：164

作者：

Abdo, A. A. ^{[2
]}

Ackermann, M. ^{[3
,4
]}

Ajello, M. ^{[3
,4
]}

Asano, K. ^{[5
]}

Baldini, L. ^{[6
]}

Ballet, J. ^{[7
]}

Barbiellini, G. ^{[8
,9
]}

Bastieri, D. ^{[10
,11
]}

Baughman, B. M. ^{[12
]}

Bechtol, K. ^{[3
,4
]}

Bellazzini, R. ^{[6
]}

Blandford, R. D. ^{[3
,4
]}

Bloom, E. D. ^{[3
,4
]}

Bonamente, E. ^{[13
,14
]}

Borgland, A. W. ^{[3
,4
]}

Bregeon, J. ^{[6
]}

Brez, A. ^{[6
]}

Brigida, M. ^{[15
,16
]}

Bruel, P. ^{[17
]}

Burnett, T. H. ^{[18
]}

Caliandro, G. A. ^{[15
,16
]}

Cameron, R. A. ^{[3
,4
]}

Caraveo, A. ^{[19
]}

Casandjian, J. M. ^{[7
]}

Cavazzuti, E. ^{[20
]}

Cecchi, C. ^{[13
,14
]}

Celotti, A. ^{[21
]}

Chekhtman, A. ^{[2
,22
]}

Cheung, C. C.

Chiang, J. ^{[3
,4
]}

Ciprini, S. ^{[13
,14
]}

Claus, R. ^{[3
,4
]}

Cohen-Tanugi, J. ^{[23
]}

Colafrancesco, S. ^{[20
]}

Cominsky, L. R. ^{[24
]}

Conrad, J. ^{[25
,26
,27
]}

Costamante, L. ^{[3
,4
]}

Dermer, C. D. ^{[2
]}

de Angelis, A. ^{[28
,29
]}

de Palma, F. ^{[15
,16
]}

Digel, S. W. ^{[3
,4
]}

Donato, D.

do Couto e Silva, E. ^{[3
,4
]}

Drell, P. S. ^{[3
,4
]}

Dubois, R. ^{[3
,4
]}

Dumora, D. ^{[30
,31
]}

Farnier, C. ^{[23
]}

Favuzzi, C. ^{[15
,16
]}

Finke, J. ^{[2
]}

Focke, W. B. ^{[3
,4
]}

机构：

[1] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan

[2] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA

[3] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA

[4] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA

[5] Tokyo Inst Technol, Interact Res Ctr Sci, Meguro, Tokyo 1528551, Japan

[6] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy

[7] Univ Paris Diderot, Serv Astrophys, CEA Saclay, Lab AIM,CEA IRFU,CNRS, F-91191 Gif Sur Yvette, France

[8] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy

[9] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy

[10] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy

[11] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy

[12] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA

[13] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy

[14] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy

[15] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy

[16] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy

[17] Ecole Polytech, CNRS, Lab Leprince Ringuet, IN2P3, F-91128 Palaiseau, France

[18] Univ Washington, Dept Phys, Seattle, WA 98195 USA

[19] Ist Astrofis Spaziale & Fis Cosm, INAF, I-20133 Milan, Italy

[20] Sci Data Ctr, ASI, I-00044 Rome, Italy

[21] SISSA, I-34014 Trieste, Italy

[22] George Mason Univ, Fairfax, VA 22030 USA

[23] Univ Montpellier 2, Lab Phys Theor & Astroparticules, CNRS, IN2P3, Montpellier, France

[24] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA

[25] Oskar Klein Ctr Cosmo Particle Phys, SE-10691 Stockholm, Sweden

[26] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden

[27] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden

[28] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy

[29] Ist Nazl Fis Nucl, Sez Trieste, Grp Coll Udine, I-33100 Udine, Italy

[30] CEN Bordeaux Gradignan, CNRS, IN2P3, UMR 5797, F-33175 Gradignan, France

[31] Univ Bordeaux, CEN Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France

[32] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan

[33] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA

[34] Univ Alabama, Huntsville, AL 35899 USA

[35] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA

[36] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA

[37] Dr Remeis Sternwarte Bamberg, D-96049 Bamberg, Germany

[38] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA

[39] Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany

[40] Univ Space Res Assoc, Columbia, MD 21044 USA

[41] Tokyo Inst Technol, Dept Phys, Meguro, Tokyo 1528551, Japan

[42] RIKEN, Inst Phys & Chem Res, Cosm Radiat Lab, Wako, Saitama 3510198, Japan

[43] CNRS UPS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France

[44] Univ Maryland, College Pk, MD 20742 USA

[45] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy

[46] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA

[47] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany

[48] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan

[49] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA

[50] Univ New Mexico, Albuquerque, NM 87131 USA

来源：

ASTROPHYSICAL JOURNAL | 2009年 / 699卷 / 01期

基金：

俄罗斯基础研究基金会;

关键词：

galaxies: active; galaxies: individual (NGC 1275); galaxies: jets; gamma rays: observations; radiation mechanisms: non-thermal; DEEP CHANDRA OBSERVATION; ACTIVE GALACTIC NUCLEI; PERSEUS CLUSTER; X-RAY; GALAXY CLUSTERS; BL-LACERTAE; NONTHERMAL EMISSION; RADIO-GALAXIES; TEV BLAZARS; COSMIC-RAYS;

D O I：

10.1088/0004-637X/699/1/31

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report the discovery of high-energy (E > 100 MeV) gamma-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 gamma-ray source is only approximate to 3' away from the NGC 1275 nucleus, well within the 95% LAT error circle of approximate to 5'. The spatial distribution of gamma-ay 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-gamma = (2.10 +/- 0.23) x 10(-7) ph (>100 MeV) cm(-2) s(-1) and Gamma = 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-gamma < 3.72 x 10(-8) ph (>100 MeV) cm(-2) s(-1) to the gamma-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.

引用

页码：31 / 39

页数：9

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