GRB110721A: AN EXTREME PEAK ENERGY AND SIGNATURES OF THE PHOTOSPHERE

被引：160

作者：

Axelsson, M. ^{[1
,2
,3
]}

Baldini, L. ^{[4
]}

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

Baring, M. G. ^{[7
]}

Bellazzini, R. ^{[4
]}

Bregeon, J. ^{[4
]}

Brigida, M. ^{[8
,9
]}

Bruel, P. ^{[10
]}

Buehler, R. ^{[11
,12
]}

Caliandro, G. A. ^{[13
]}

Cameron, R. A. ^{[11
,12
]}

Caraveo, P. A. ^{[14
]}

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

Chaves, R. C. G. ^{[17
]}

Chekhtman, A. ^{[18
]}

Chiang, J. ^{[11
,12
]}

Claus, R. ^{[11
,12
]}

Conrad, J. ^{[3
,19
]}

Cutini, S. ^{[20
]}

D'Ammando, F. ^{[15
,21
,22
]}

de Palma, F. ^{[8
,9
]}

Dermer, C. D. ^{[23
]}

do Couto e Silva, E. ^{[11
,12
]}

Drell, P. S. ^{[11
,12
]}

Favuzzi, C. ^{[8
,9
]}

Fegan, S. J. ^{[10
]}

Ferrara, E. C. ^{[24
]}

Focke, W. B. ^{[11
,12
]}

Fukazawa, Y. ^{[25
]}

Fusco, P. ^{[8
,9
]}

Gargano, F. ^{[9
]}

Gasparrini, D. ^{[20
]}

Gehrels, N. ^{[24
]}

Germani, S. ^{[15
,16
]}

Giglietto, N. ^{[8
,9
]}

Giroletti, M. ^{[26
]}

Godfrey, G. ^{[11
,12
]}

Guiriec, S. ^{[24
]}

Hadasch, D. ^{[13
]}

Hanabata, Y. ^{[25
]}

Hayashida, M. ^{[11
,12
,27
]}

Hou, X. ^{[28
]}

Iyyani, S. ^{[1
,3
,19
]}

Jackson, M. S. ^{[1
,3
]}

Kocevski, D. ^{[11
,12
]}

Kuss, M. ^{[4
]}

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

Larsson, S. ^{[2
,3
,19
]}

Longo, F. ^{[5
,6
]}

Loparco, F. ^{[8
,9
]}

机构：

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

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

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

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

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

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

[7] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA

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

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

[10] IN2P3, CNRS, Ecole Polytech, Lab Leprince Ringuet, Palaiseau, France

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

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

[13] Inst Ciencies Espai IEEE CSIC, E-08193 Barcelona, Spain

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

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

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

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

[18] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA

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

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

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

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

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

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

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

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

[27] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan

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

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

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

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

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

[33] Univ Montpellier 2, Lab Univers & Particules Montpellier, CNRS, IN2P3, Montpellier, France

[34] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan

[35] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy

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

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

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

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

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

[41] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany

[42] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA

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

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

[45] CIFS, I-10133 Turin, Italy

[46] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy

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

[48] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA

[49] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland

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

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2012年 / 757卷 / 02期

基金：

瑞典研究理事会;

关键词：

gamma-ray burst: general; gamma-ray burst: individual (GRB110721A); radiation mechanisms: thermal; GAMMA-RAY-BURSTS; NONTHERMAL EMISSION; SPECTRAL COMPONENT; PROMPT EMISSION; GRB090902B; MONITOR; PULSES;

D O I：

10.1088/2041-8205/757/2/L31

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

GRB110721A was observed by the Fermi Gamma-ray Space Telescope using its two instruments, the Large Area Telescope (LAT) and the Gamma-ray Burst Monitor (GBM). The burst consisted of one major emission episode which lasted for similar to 24.5 s (in the GBM) and had a peak flux of (5.7 +/- 0.2) x 10(-5) erg s(-1) cm(-2). The time-resolved emission spectrum is best modeled with a combination of a Band function and a blackbody spectrum. The peak energy of the Band component was initially 15 +/- 2 MeV, which is the highest value ever detected in a GRB. This measurement was made possible by combining GBM/BGO data with LAT Low Energy events to achieve continuous 10-100 MeV coverage. The peak energy later decreased as a power law in time with an index of -1.89 +/- 0.10. The temperature of the blackbody component also decreased, starting from similar to 80 keV, and the decay showed a significant break after similar to 2 s. The spectrum provides strong constraints on the standard synchrotron model, indicating that alternative mechanisms may give rise to the emission at these energies.

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