FERMI GAMMA-RAY SPACE TELESCOPE OBSERVATIONS OF GAMMA-RAY OUTBURSTS FROM 3C 454.3 IN 2009 DECEMBER AND 2010 APRIL

被引：132

作者：

Ackermann, M. ^{[1
,2
]}

Ajello, M. ^{[1
,2
]}

Baldini, L. ^{[3
]}

Ballet, J. ^{[4
]}

Barbiellini, G. ^{[5
,6
]}

Bastieri, D. ^{[7
,8
]}

Bechtol, K. ^{[1
,2
]}

Bellazzini, R. ^{[3
]}

Berenji, B. ^{[1
,2
]}

Blandford, R. D. ^{[1
,2
]}

Bonamente, E. ^{[9
,10
]}

Borgland, A. W. ^{[1
,2
]}

Bregeon, J. ^{[3
]}

Brigida, M. ^{[11
,12
]}

Bruel, P. ^{[13
]}

Buehler, R. ^{[1
,2
]}

Burnett, T. H. ^{[14
]}

Buson, S. ^{[7
,8
]}

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

Cameron, R. A. ^{[1
,2
]}

Caraveo, P. A. ^{[16
]}

Carrigan, S. ^{[8
]}

Casandjian, J. M. ^{[4
]}

Cavazzuti, E. ^{[17
]}

Cecchi, C. ^{[9
,10
]}

Celik, Oe ^{[18
,19
,20
,21
]}

Chekhtman, A. ^{[22
,23
]}

Cheung, C. C. ^{[22
,24
]}

Chiang, J. ^{[1
,2
]}

Ciprini, S. ^{[10
]}

Claus, R. ^{[1
,2
]}

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

Corbel, S. ^{[4
,26
]}

Cutini, S. ^{[17
]}

D'Ammando, F. ^{[27
,28
]}

Dermer, C. D. ^{[22
]}

de Angelis, A. ^{[29
,30
]}

de Palma, F. ^{[11
,12
]}

Digel, S. W. ^{[1
,2
]}

do Couto e Silva, E. ^{[1
,2
]}

Drell, P. S. ^{[1
,2
]}

Dubois, R. ^{[1
,2
]}

Dumora, D. ^{[31
]}

Escande, L. ^{[31
]}

Favuzzi, C. ^{[11
,12
]}

Fegan, S. J. ^{[13
]}

Ferrara, E. C. ^{[18
]}

Fuhrmann, L. ^{[32
]}

Fukazawa, Y. ^{[33
]}

Fusco, P. ^{[11
,12
]}

机构：

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

[19] NASA, CRESST, Greenbelt, MD 20771 USA

[20] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA

[21] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA

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

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

[24] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA

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

[26] Inst Univ France, F-75005 Paris, France

[27] IASF Palermo, I-90146 Palermo, Italy

[28] INAF Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy

[29] Univ Udine, Dipartimento Fis, I-00133 Rome, Italy

[30] Ist Nazl Fis Nucl, Sez Trieste, Grp Coll Udine, I-00133 Rome, Italy

[31] Univ Bordeaux 1, CNRS, Ctr Etud Nucl Bordeaux Gradignan, IN2P3, F-33175 Gradignan, France

[32] Max Planck Inst Radioastron, D-53121 Bonn, Germany

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

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

[35] Univ Alabama, CSPAR, Huntsville, AL 35899 USA

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

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

[38] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden

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

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

[41] Univ Maryland, Dept Phys, College Pk, MD 20742 USA

[42] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

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

[44] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland

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

[46] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan

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

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

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

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

来源：

ASTROPHYSICAL JOURNAL | 2010年 / 721卷 / 02期

关键词：

galaxies: active; gamma rays: galaxies; quasars: individual (3C 454.3); ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; BLAZAR; 3C-454.3; MULTIWAVELENGTH OBSERVATIONS; INFRARED OBSERVATIONS; CRAZY-DIAMOND; FLARE; VARIABILITY; COMPTON; SYNCHROTRON;

D O I：

10.1088/0004-637X/721/2/1383

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The flat spectrum radio quasar 3C 454.3 underwent an extraordinary outburst in 2009 December when it became the brightest gamma-ray source in the sky for over 1 week. Its daily flux measured with the Fermi-Large Area Telescope at photon energiesE > 100 MeV reached F-100 = 22 +/- 1 x 10(6) photon cm(-2) s(-1), representing the highest daily flux of any blazar ever recorded in high-energy. -rays. It again became the brightest source in the sky in 2010 April, triggering a pointed-mode observation by Fermi. The correlated. -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. -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 approximate to 20 GeV and a minimum Doppler factor of approximate to 13 is derived. The gamma-ray spectrum of 3C 454.3 shows a significant spectral break between approximate to 2 and 3 GeV that is very weakly dependent on the flux state, even when the flux changes by an order of magnitude.

引用

页码：1383 / 1396

页数：14

共 56 条

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