THE AFTERGLOW OF GRB 130427A FROM 1 TO 1016 GHz

被引：171

作者：

Perley, D. A. ^{[1
]}

Cenko, S. B. ^{[2
,3
,4
]}

Corsi, A. ^{[5
]}

Tanvir, N. R. ^{[6
]}

Levan, A. J. ^{[7
]}

Kann, D. A. ^{[8
,9
]}

Sonbas, E. ^{[10
]}

Wiersema, K. ^{[6
]}

Zheng, W. ^{[3
]}

Zhao, X. -H. ^{[11
,12
]}

Bai, J. -M. ^{[11
,12
]}

Bremer, M. ^{[13
]}

Castro-Tirado, A. J. ^{[14
,15
]}

Chang, L. ^{[11
,12
]}

Clubb, K. I. ^{[3
]}

Frail, D. ^{[16
]}

Fruchter, A. ^{[17
]}

Gogus, E. ^{[18
]}

Greiner, J. ^{[8
]}

Guver, T. ^{[19
]}

Horesh, A. ^{[1
]}

Filippenko, A. V. ^{[3
]}

Klose, S. ^{[9
]}

Mao, J. ^{[11
,20
]}

Morgan, A. N. ^{[3
]}

Pozanenko, A. S. ^{[21
]}

Schmidl, S. ^{[9
]}

Stecklum, B. ^{[9
]}

Tanga, M. ^{[8
]}

Volnova, A. A. ^{[21
]}

Volvach, A. E. ^{[22
]}

Wang, J. -G. ^{[11
,12
]}

Winters, J. -M. ^{[13
]}

Xin, Y. -X. ^{[11
,12
]}

机构：

[1] CALTECH, Dept Astron, Pasadena, CA 91125 USA

[2] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA

[3] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA

[4] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA

[5] George Washington Univ, Dept Phys, Washington, DC 20052 USA

[6] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England

[7] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England

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

[9] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany

[10] Adiyaman Univ, Dept Phys, TR-02040 Adiyaman, Turkey

[11] Chinese Acad Sci, Yunnan Observ, Kunming 650011, Peoples R China

[12] Chinese Acad Sci, Key Lab Struct & Evolut Celestial Bodies, Kunming 650011, Peoples R China

[13] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France

[14] CSIC, IAA, E-18008 Granada, Spain

[15] Univ Malaga, Unidad Asociada Dept Ingn Sistemas & Automat, ETS Ingn Ind, E-29071 Malaga, Spain

[16] Natl Radio Astron Observ, Socorro, NM 87801 USA

[17] Space Telescope Sci Inst, Baltimore, MD 21218 USA

[18] Sabanci Univ, TR-34956 Istanbul, Turkey

[19] Istanbul Univ, Istanbul Univ Sci Fac, Dept Astron & Space Sci, TR-34119 Istanbul, Turkey

[20] RIKEN, Astrophys Big Bang Lab, Wako, Saitama 3510198, Japan

[21] Space Res Inst, Moscow 117997, Russia

[22] Crimean Astrophys Observ, Radio Astron Lab, UA-98688 Katsiveli, Yalta, Ukraine

来源：

ASTROPHYSICAL JOURNAL | 2014年 / 781卷 / 01期

基金：

美国国家科学基金会;

关键词：

gamma-ray burst: individual (GRB 130427A); radiation mechanisms: non-thermal; GAMMA-RAY BURST; HIGH-ENERGY EMISSION; DIGITAL SKY SURVEY; WIND-INTERACTION-MODELS; STAR-FORMATION HISTORY; LARGE-AREA TELESCOPE; REVERSE-SHOCK; OPTICAL AFTERGLOW; LIGHT-CURVE; LONG-DURATION;

D O I：

10.1088/0004-637X/781/1/37

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present multiwavelength observations of the afterglow of GRB 130427A, the brightest (in total fluence) gamma-ray burst (GRB) of the past 29 yr. Optical spectroscopy from Gemini-North reveals the redshift of the GRB to be z = 0.340, indicating that its unprecedented brightness is primarily the result of its relatively close proximity to Earth; the intrinsic luminosities of both the GRB and its afterglow are not extreme in comparison to other bright GRBs. We present a large suite of multiwavelength observations spanning from 300 s to 130 days after the burst and demonstrate that the afterglow shows relatively simple, smooth evolution at all frequencies, with no significant late-time flaring or rebrightening activity. The entire data set from 1 GHz to 10 GeV can be modeled as synchrotron emission from a combination of reverse and forward shocks in good agreement with the standard afterglow model, providing strong support to the applicability of the underlying theory and clarifying the nature of the GeV emission observed to last for minutes to hours following other very bright GRBs. A tenuous, wind-stratified circumburst density profile is required by the observations, suggesting a massive-star progenitor with a low mass-loss rate, perhaps due to low metallicity. GRBs similar in nature to GRB 130427A, inhabiting low-density media and exhibiting strong reverse shocks, are probably not uncommon but may have been difficult to recognize in the past owing to their relatively faint late-time radio emission; more such events should be found in abundance by the new generation of sensitive radio and millimeter instruments.

引用

页数：21

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