Статья

THE AFTERGLOW OF GRB 130427A FROM 1 TO 10<sup>16</sup>GHz

D. A. PerleyDepartment of Astronomy, California Institute of Technology, MC 249-17, 1200 East California Blvd, Pasadena, CA 91125, USA; [email protected]S. B. CenkoAstrophysics Science Division, NASA Goddard Space Flight Center, Mail Code 661, Greenbelt, MD 20771, USAA. CorsiPhysics Department, George Washington University, 725 21st St, NW Washington, DC 20052, USAN. R. TanvirDepartment of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UKA. J. LevanDepartment of Physics, University of Warwick, Coventry CV4 7AL, UKД. А. КаннMax-Planck-Institut für extraterrestrische Physik, Giessenbachstraße, D-85748 Garching, GermanyЭ. СонбасDepartment of Physics, University of Adiyaman, 02040 Adiyaman, TurkeyK. WiersemaDepartment of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UKWeiKang ZhengDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAXiaohong ZhaoKey Laboratory for the Structure and Evolution of Celestial Bodies, Chinese Academy of Sciences, P.O. Box 110, 650011 Kunming, ChinaJ. M. BaiKey Laboratory for the Structure and Evolution of Celestial Bodies, Chinese Academy of Sciences, P.O. Box 110, 650011 Kunming, ChinaMichael BremerInstitute de Radioastronomie Millimètrique (IRAM), 300 rue de la Piscine, F-38406 Saint Martin d'Hères, FranceA. J. Castro‐TiradoInstituto de Astrofísica de Andalucía (IAA-CSIC), Glorieta de la Astronomía s/n, E-18008 Granada, SpainLiang ChangKey Laboratory for the Structure and Evolution of Celestial Bodies, Chinese Academy of Sciences, P.O. Box 110, 650011 Kunming, ChinaK. I. ClubbDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAD. A. FrailNational Radio Astronomy Observatory, P.O. Box O, Socorro, NM 87801, USAA. S. FruchterSpace Telescope Science Institute, Baltimore, MD 21218, USAErsin GöğüşSabancı University, Orhanlı- Tuzla, İstanbul 34956, TurkeyJ. GreinerMax-Planck-Institut für extraterrestrische Physik, Giessenbachstraße, D-85748 Garching, GermanyTolga GüverIstanbul University Science Faculty, Department of Astronomy and Space Sciences, 34119, University-Istanbul, TurkeyA. HoreshDepartment of Astronomy, California Institute of Technology, MC 249-17, 1200 East California Blvd, Pasadena, CA 91125, USA; [email protected]A. V. FilippenkoDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAS. KloseThüringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg, GermanyJ. MaoAstrophysical Big Bang Laboratory, RIKEN, Saitama 351-0198, JapanA. N. MorganDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAA. PozanenkoSpace Research Institute, 117997, 84/32 Profsoyuznaya, Moscow, RussiaB. StecklumThüringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg, GermanyM. TangaMax-Planck-Institut für extraterrestrische Physik, Giessenbachstraße, D-85748 Garching, GermanyA. VolnovaSpace Research Institute, 117997, 84/32 Profsoyuznaya, Moscow, RussiaA. E. VolvachRadio Astronomy Laboratory of the Crimean Astrophysical Observatory, Katsiveli, Yalta 98688, UkraineJ.-G. WangKey Laboratory for the Structure and Evolution of Celestial Bodies, Chinese Academy of Sciences, P.O. Box 110, 650011 Kunming, ChinaJ. M. WintersInstitute de Radioastronomie Millimètrique (IRAM), 300 rue de la Piscine, F-38406 Saint Martin d'Hères, FranceYu XinKey Laboratory for the Structure and Evolution of Celestial Bodies, Chinese Academy of Sciences, P.O. Box 110, 650011 Kunming, China

2014en

ABI

Аннотация

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. © 2014. The American Astronomical Society. All rights reserved.

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Идентификаторы

DOI: 10.1088/0004-637x/781/1/37

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Цитирований: 5Использованных источников: 0

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