TY - JOUR
T1 - A VLA Study of High-redshift GRBs. I. Multiwavelength Observations and Modeling of GRB 140311A
AU - Laskar, Tanmoy
AU - Berger, Edo
AU - Chornock, Ryan
AU - Margutti, Raffaella
AU - Fong, Wen-fai
AU - Zauderer, B. Ashley
N1 - Funding Information:
The Berger Time-Domain Group at Harvard is supported in part by the NSF under grant AST-1411763 and by NASA under grant NNX15AE50G. B.A.Z. acknowledges support from NSF AST-1302954. R.C. acknowledges support from NASA Swift grant NNX16AB04G. VLA observations for this study were obtained via project 14A-344. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research has made use of data supplied by the UK Swift Science Data Centre at the University of Leicester, and of data obtained through the High Energy Astrophysics Science Archive Research Center On-line Service, provided by the NASA/Goddard Space Flight Center.
Funding Information:
We thank the anonymous referee for helpful comments on the manuscript. T.L. is a Jansky Fellow of the National Radio Astronomy Observatory. The Berger Time-Domain Group at Harvard is supported in part by the NSF under grant AST-1411763 and by NASA under grant NNX15AE50G. B.A.Z. acknowledges support from NSF AST-1302954. R.C. acknowledges support from NASA Swift grant NNX16AB04G. VLA observations for this study were obtained via project 14A-344. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research has made use of data supplied by the UK Swift Science Data Centre at the University of Leicester, and of data obtained through the High Energy Astrophysics Science Archive Research Center On-line Service, provided by the NASA/Goddard Space Flight Center.
Publisher Copyright:
© 2018. The American Astronomical Society. All rights reserved.
PY - 2018/5/1
Y1 - 2018/5/1
N2 - We present the first results from a recently concluded study of GRBs at z ≳ 5 with the Karl G. Jansky Very Large Array (VLA). Spanning 1 to 85.5 GHz and 7 epochs from 1.5 to 82.3 days, our observations of GRB 140311A are the most detailed joint radio and millimeter observations of a GRB afterglow at z ≳ 5 to date. In conjunction with optical/near-IR and X-ray data, the observations can be understood in the framework of radiation from a single blast wave shock with energy EK,iso ≈ 8.5 × 1053 erg expanding into a constant density environment with density, density, n0 ≈ 8cm-3. The X-ray and radio observations require a jet break at tjet ≈ 0.6 days, yielding an opening angle of θjet ≈ 4° and a beaming-corrected blast wave kinetic energy of EK ≈ 2.2 × 1050 erg. The results from our radio follow-up and multiwavelength modeling lend credence to the hypothesis that detected high-redshift GRBs may be more tightly beamed than events at lower redshift. We do not find compelling evidence for reverse shock emission, which may be related to fast cooling driven by the moderately high circumburst density.
AB - We present the first results from a recently concluded study of GRBs at z ≳ 5 with the Karl G. Jansky Very Large Array (VLA). Spanning 1 to 85.5 GHz and 7 epochs from 1.5 to 82.3 days, our observations of GRB 140311A are the most detailed joint radio and millimeter observations of a GRB afterglow at z ≳ 5 to date. In conjunction with optical/near-IR and X-ray data, the observations can be understood in the framework of radiation from a single blast wave shock with energy EK,iso ≈ 8.5 × 1053 erg expanding into a constant density environment with density, density, n0 ≈ 8cm-3. The X-ray and radio observations require a jet break at tjet ≈ 0.6 days, yielding an opening angle of θjet ≈ 4° and a beaming-corrected blast wave kinetic energy of EK ≈ 2.2 × 1050 erg. The results from our radio follow-up and multiwavelength modeling lend credence to the hypothesis that detected high-redshift GRBs may be more tightly beamed than events at lower redshift. We do not find compelling evidence for reverse shock emission, which may be related to fast cooling driven by the moderately high circumburst density.
KW - gamma-ray burst: general
KW - gamma-ray burst: individual (140311A)
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U2 - 10.3847/1538-4357/aab8f5
DO - 10.3847/1538-4357/aab8f5
M3 - Article
AN - SCOPUS:85047183301
SN - 0004-637X
VL - 858
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 65
ER -