FERMI OBSERVATIONS OF GRB 090510: A SHORT-HARD GAMMA-RAY BURST WITH AN ADDITIONAL, HARD POWER-LAW COMPONENT FROM 10 keV TO GeV ENERGIES

被引：305

作者：

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

Asano, K. ^{[3
]}

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

Axelsson, M. ^{[6
,7
,8
]}

Baldini, L. ^{[9
]}

Ballet, J. ^{[10
]}

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

Baring, M. G. ^{[13
]}

Bastieri, D. ^{[14
,15
]}

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

Bellazzini, R. ^{[9
]}

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

Bhat, P. N. ^{[16
]}

Bissaldi, E. ^{[17
]}

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

Bloom, E. D. ^{[1
,2
]}

Bonamente, E. ^{[18
,19
]}

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

Bouvier, A. ^{[1
,2
]}

Bregeon, J. ^{[9
]}

Brez, A. ^{[9
]}

Briggs, M. S. ^{[16
]}

Brigida, M. ^{[20
,21
]}

Bruel, P. ^{[22
]}

Buson, S. ^{[14
]}

Caliandro, G. A. ^{[23
]}

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

Caraveo, P. A. ^{[24
]}

Carrigan, S. ^{[15
]}

Casandjian, J. M. ^{[10
]}

Cecchi, C. ^{[18
,19
]}

Celik, Oe. ^{[25
,26
,27
,28
]}

Charles, E. ^{[1
,2
]}

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

Ciprini, S. ^{[19
]}

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

Cohen-Tanugi, J. ^{[29
]}

Connaughton, V. ^{[16
]}

Conrad, J. ^{[30
]}

Dermer, C. D. ^{[31
]}

de Palma, F. ^{[20
,21
]}

Dingus, B. L. ^{[32
]}

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

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

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

Dumora, D. ^{[33
,34
]}

Farnier, C. ^{[29
]}

Favuzzi, C. ^{[20
,21
]}

Fegan, S. J. ^{[22
]}

Finke, J. ^{[31
,35
]}

机构：

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

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

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

[4] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept 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] Lund Observ, SE-22100 Lund, Sweden

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

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

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

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

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

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

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

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

[16] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA

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

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

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

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

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

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

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

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

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

[26] CRESST, Greenbelt, MD 20771 USA

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

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

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

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

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

[32] Los Alamos Natl Lab, Los Alamos, NM 87545 USA

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

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

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

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

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

[38] Ist Nazl Astrofis, Osservatorio Astron Trieste, I-34143 Trieste, Italy

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

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

[41] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England

[42] ICREA, Barcelona, Spain

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

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

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

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

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

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

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

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

来源：

ASTROPHYSICAL JOURNAL | 2010年 / 716卷 / 02期

关键词：

gamma-ray burst: individual (GRB 090510); radiation mechanisms: non-thermal; RELATIVISTIC COLLISIONLESS SHOCKS; SPECTRAL COMPONENT; PROMPT EMISSION; AFTERGLOW; DURATION; ACCELERATION; RADIATION; FIREBALLS; PHOTONS; PROTONS;

D O I：

10.1088/0004-637X/716/2/1178

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present detailed observations of the bright short-hard gamma-ray burst GRB 090510 made with the Gammaray Burst Monitor (GBM) and Large Area Telescope (LAT) on board the Fermi observatory. GRB 090510 is the first burst detected by the LAT that shows strong evidence for a deviation from a Band spectral fitting function during the prompt emission phase. The time-integrated spectrum is fit by the sum of a Band function with E-peak = 3.9 +/- 0.3 MeV, which is the highest yet measured, and a hard power-law component with photon index -1.62 +/- 0.03 that dominates the emission below approximate to 20 keV and above approximate to 100 MeV. The onset of the high-energy spectral component appears to be delayed by similar to 0.1 s with respect to the onset of a component well fit with a single Band function. A faint GBM pulse and a LAT photon are detected 0.5 s before the main pulse. During the prompt phase, the LAT detected a photon with energy 30.5(-2.6)(+5.8) GeV, the highest ever measured from a short GRB. Observation of this photon sets a minimum bulk outflow Lorentz factor, Gamma greater than or similar to 1200, using simple.. opacity arguments for this GRB at redshift z = 0.903 and a variability timescale on the order of tens of ms for the approximate to 100 keV-few MeV flux. Stricter high confidence estimates imply Gamma greater than or similar to 1000 and still require that the outflows powering short GRBs are at least as highly relativistic as those of long-duration GRBs. Implications of the temporal behavior and power-law shape of the additional component on synchrotron/synchrotron self-Compton, external-shock synchrotron, and hadronic models are considered.

引用

页码：1178 / 1190

页数：13

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