MULTIWAVELENGTH OBSERVATIONS OF GRB 110731A: GeV EMISSION FROM ONSET TO AFTERGLOW

被引：80

作者：

Ackermann, M. ^{[1
]}

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

Asano, K. ^{[4
]}

Baldini, L. ^{[5
]}

Barbiellini, G. ^{[6
,7
]}

Baring, M. G. ^{[8
]}

Bastieri, D. ^{[9
,10
]}

Bellazzini, R. ^{[5
]}

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

Bonamente, E. ^{[11
,12
]}

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

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

Bregeon, J. ^{[5
]}

Brigida, M. ^{[13
,14
,15
]}

Bruel, P. ^{[16
]}

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

Buson, S. ^{[9
,10
]}

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

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

Caraveo, P. A. ^{[18
]}

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

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

Chaves, R. C. G. ^{[19
]}

Chekhtman, A. ^{[20
]}

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

Ciprini, S. ^{[12
,21
]}

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

Cohen-Tanugi, J. ^{[22
]}

Conrad, J. ^{[23
,24
]}

Cutini, S. ^{[25
]}

D'Ammando, F. ^{[11
,26
,27
]}

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

de Palma, F. ^{[13
,14
,15
]}

Dermer, C. D. ^{[30
]}

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

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

Drlica-Wagner, A. ^{[2
,3
]}

Favuzzi, C. ^{[13
,14
,15
]}

Fegan, S. J. ^{[16
]}

Focke, W. B. ^{[2
,3
]}

Franckowiak, A. ^{[2
,3
]}

Fukazawa, Y. ^{[31
]}

Fusco, P. ^{[13
,14
,15
]}

Gargano, F. ^{[15
]}

Gasparrini, D. ^{[25
]}

Gehrels, N. ^{[32
]}

Giglietto, N. ^{[13
,14
,15
]}

Giordano, F. ^{[13
,14
,15
]}

Giroletti, M. ^{[33
]}

Glanzman, T. ^{[2
,3
]}

机构：

[1] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

[34] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England

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

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

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

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

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

[40] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland

[41] IRAP, CNRS, F-31028 Toulouse 4, France

[42] Univ Toulouse, UPS OMP, IRAP, GAHEC, Toulouse, France

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

[44] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy

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

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

[47] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA

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

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

[50] Boise State Univ, Dept Phys, Boise, ID 83725 USA

来源：

ASTROPHYSICAL JOURNAL | 2013年 / 763卷 / 02期

关键词：

gamma-ray burst: individual (GRB110731A); GAMMA-RAY BURST; HIGH-ENERGY EMISSION; LARGE-AREA TELESCOPE; LIGHT CURVES; FERMI OBSERVATIONS; SPECTRAL CATALOG; PEAK LUMINOSITY; PRE-SWIFT; DUST; CALIBRATION;

D O I：

10.1088/0004-637X/763/2/71

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report on the multiwavelength observations of the bright, long gamma-ray burst GRB 110731A, by the Fermi and Swift observatories, and by the MOA and GROND optical telescopes. The analysis of the prompt phase reveals that GRB 110731A shares many features with bright Large Area Telescope bursts observed by Fermi during the first three years on-orbit: a light curve with short time variability across the whole energy range during the prompt phase, delayed onset of the emission above 100 MeV, extra power-law component and temporally extended high-energy emission. In addition, this is the first GRB for which simultaneous GeV, X-ray, and optical data are available over multiple epochs beginning just after the trigger time and extending for more than 800 s, allowing temporal and spectral analysis in different epochs that favor emission from the forward shock in a wind-type medium. The observed temporally extended GeV emission is most likely part of the high-energy end of the afterglow emission. Both the single-zone pair transparency constraint for the prompt signal and the spectral and temporal analysis of the forward-shock afterglow emission independently lead to an estimate of the bulk Lorentz factor of the jet Gamma similar to 500-550.

引用

页数：19

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