FERMI LARGE AREA TELESCOPE GAMMA-RAY DETECTION OF THE RADIO GALAXY M87

被引：150

作者：

Abdo, A. A. ^{[1
]}

Ackermann, M. ^{[2
,3
]}

Ajello, M. ^{[2
,3
]}

Atwood, W. B. ^{[4
,5
]}

Axelsson, M. ^{[6
,7
]}

Baldini, L. ^{[8
]}

Ballet, J. ^{[9
]}

Barbiellini, G. ^{[10
,11
]}

Bastieri, D. ^{[12
,13
]}

Bechtol, K. ^{[2
,3
]}

Bellazzini, R. ^{[8
]}

Berenji, B. ^{[2
,3
]}

Blandford, R. D. ^{[2
,3
]}

Bloom, E. D. ^{[2
,3
]}

Bonamente, E. ^{[14
,15
]}

Borgland, A. W. ^{[2
,3
]}

Bregeon, J. ^{[8
]}

Brez, A. ^{[8
]}

Brigida, M. ^{[16
,17
]}

Bruel, P. ^{[18
]}

Burnett, T. H. ^{[19
]}

Caliandro, G. A. ^{[16
,17
]}

Cameron, R. A. ^{[2
,3
]}

Cannon, A. ^{[21
]}

Caraveo, P. A. ^{[22
]}

Casandjian, J. M. ^{[9
]}

Cavazzuti, E. ^{[23
]}

Cecchi, C. ^{[14
,15
]}

Celik, Oe ^{[20
,24
]}

Charles, E. ^{[2
,3
]}

Cheung, C. C. ^{[1
]}

Chiang, J. ^{[2
,3
]}

Ciprini, S. ^{[14
,15
]}

Claus, R. ^{[2
,3
]}

Cohen-Tanugi, J. ^{[25
]}

Colafrancesco, S. ^{[23
]}

Conrad, J. ^{[7
,26
]}

Costamante, L. ^{[2
,3
]}

Cutini, S. ^{[23
]}

Davis, D. S. ^{[24
]}

Dermer, C. D. ^{[1
]}

de Angelis, A. ^{[27
,28
]}

de Palma, F. ^{[16
,17
]}

Digel, S. W. ^{[2
,3
]}

Donato, D.

do Couto e Silva, E. ^{[2
,3
]}

Drell, P. S. ^{[2
,3
]}

Dubois, R. ^{[2
,3
]}

Dumora, D. ^{[29
,30
]}

Edmonds, Y. ^{[2
,3
]}

机构：

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

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

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

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

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

[6] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden

[7] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden

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

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

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

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

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

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

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

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

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

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

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

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

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

[21] Univ Coll Dublin, Dublin 4, Ireland

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

[23] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Frascati, Roma, Italy

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

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

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

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

[28] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy

[29] Univ Bordeaux, Ctr Etud Nucl Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France

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

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

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

[33] INAF Ist Radioastron, I-40129 Bologna, Italy

[34] Univ Alabama, Huntsville, AL 35899 USA

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

[36] Waseda Univ, Shinjuku Ku, Tokyo 1698050, Japan

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

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

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

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

[41] Univ Denver, Dept Phys & Astrophys, Denver, CO 80208 USA

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

[43] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan

[44] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria

[45] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria

[46] CSIC, IEEC, Inst Ciencies Espai, Barcelona 08193, Spain

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

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

[49] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA

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

来源：

ASTROPHYSICAL JOURNAL | 2009年 / 707卷 / 01期

基金：

美国国家科学基金会;

关键词：

galaxies: active; galaxies: individual (M87); galaxies: jets; gamma rays: observations; radiation mechanisms: non-thermal; ACTIVE GALACTIC NUCLEI; SYNCHROTRON-PROTON BLAZAR; SUPERMASSIVE BLACK-HOLE; TEV EMISSION; UNIFIED SCHEMES; LAC OBJECTS; SOURCE LIST; EGRET DATA; JET; VARIABILITY;

D O I：

10.1088/0004-637X/707/1/55

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report the Fermi Large Area Telescope (LAT) discovery of high-energy (MeV/GeV) gamma-ray emission positionally consistent with the center of the radio galaxy M87, at a source significance of over 10 sigma 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 gamma-ray source has a >100 MeV flux of 2.45 (+/-0.63) x 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 x 10-8 photons cm(-2) s(-1), 2 sigma), 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 gamma-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.

引用

页码：55 / 60

页数：6

共 61 条

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