DISCOVERY OF AN EXTRA HARD SPECTRAL COMPONENT IN THE HIGH-ENERGY AFTERGLOW EMISSION OF GRB 130427A

被引：44
作者：
Tam, Pak-Hin Thomas [1 ,2 ]
Tang, Qing-Wen [3 ,4 ]
Hou, Shu-Jin [5 ,6 ,7 ]
Liu, Ruo-Yu [3 ,4 ,8 ]
Wang, Xiang-Yu [3 ,4 ]
机构：
[1] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan
[2] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan
[3] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China
[4] Nanjing Univ, Minist Educ, Key Lab Modern Astron & Astrophys, Nanjing 210093, Jiangsu, Peoples R China
[5] Xiamen Univ, Dept Astron, Xiamen 361005, Fujian, Peoples R China
[6] Xiamen Univ, Inst Theoret Phys & Astrophys, Xiamen 361005, Fujian, Peoples R China
[7] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China
[8] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany
来源：
ASTROPHYSICAL JOURNAL LETTERS | 2013年 / 771卷 / 01期
关键词：
gamma-ray burst: individual (GRB 130427A); radiation mechanisms: non-thermal; GAMMA-RAY BURST; ACCELERATION;
D O I：
10.1088/2041-8205/771/1/L13
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
The extended high-energy gamma-ray (> 100 MeV) emission which occurs after prompt gamma-ray bursts (GRBs) is usually characterized by a single power-law spectrum, which has been explained as the afterglow synchrotron radiation. The afterglow inverse Compton emission has long been predicted to be able to produce a high-energy component as well, but previous observations have not clearly revealed such a signature, probably due to the small number of > 10 GeV photons even for the brightest GRBs known so far. In this Letter, we report on the Fermi Large Area Telescope observations of the > 100 MeV emission from the very bright and nearby GRB130427A. We characterize the time-resolved spectra of the GeV emission from the GRB onset to the afterglow phase. By performing time-resolved spectral fits of GRB130427A, we found strong evidence of an extra hard spectral component that exists in the extended high-energy emission of this GRB. We argue that this hard component may arise from the afterglow inverse Compton emission.
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页数：5
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