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GRB 160625B :
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Cunningham, VirginiaUniv Maryland, Dept Astron, College Pk, MD 20742 USA.;NASA, Ctr Res & Explorat Space Sci & Technol, GSFC, Greenbelt, MD 20771 USA.
(author)
GRB 160625B : Evidence for a Gaussian-shaped Jet
- Article/chapterEnglish2020
Publisher, publication year, extent ...
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2020-12-01
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American Astronomical Society,2020
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LIBRIS-ID:oai:DiVA.org:kth-288463
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https://urn.kb.se/resolve?urn=urn:nbn:se:kth:diva-288463URI
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https://doi.org/10.3847/1538-4357/abc2cdDOI
Supplementary language notes
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Language:English
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Summary in:English
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Subject category:ref swepub-contenttype
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Subject category:art swepub-publicationtype
Notes
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QC 20210107
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We present multiwavelength modeling of the afterglow from the long gamma-ray burst (GRB) 160625B using Markov Chain Monte Carlo techniques of the afterglowpy Python package. GRB 160625B is an extremely bright burst with a rich set of observations spanning from radio to gamma-ray frequencies. These observations range from similar to 0.1 days to >1000 days, thus making this event extremely well suited to such modeling. In this work we compare top-hat and Gaussian jet structure types in order to find best-fit values for the GRB jet collimation angle, viewing angle, and other physical parameters. We find that a Gaussian-shaped jet is preferred (2.7 sigma-5.3 sigma) over the traditional top-hat model. Our estimate for the opening angle of the burst ranges from 126 to 390, depending on jet-shape model. We also discuss the implications that assumptions on jet shape, viewing angle, and particularly the participation a fraction of electrons have on the final estimation of GRB intrinsic energy release and the resulting energy budget of the relativistic outflow. Most notably, allowing the participation fraction to vary results in an estimated total relativistic energy of similar to 10(53) erg. This is two orders of magnitude higher than when the total fraction is assumed to be unity; thus, this parameter has strong relevance for placing constraints on long GRB central engines, details of the circumburst media, and host environment.
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Cenko, S. BradleyNASA, Astrophys Sci Div, Goddard Space Flight Ctr, MC 661, Greenbelt, MD 20771 USA.;Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
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Ryan, GeoffreyUniv Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
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Vogel, Stuart N.Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
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Corsi, AlessandraTexas Tech Univ, Dept Phys & Astron, Box 1051, Lubbock, TX 79409 USA.
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Cucchiara, AntoninoUniv Virgin Isl, Coll Marin, 120 Kent Ave, Kentfield, CA 94904 USA.
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Fruchter, Andrew S.Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
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Horesh, AssafHebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel.
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Kangas, TuomasKTH,Partikel- och astropartikelfysik,Stockholm University, Oskar Klein Ctr, Dept Phys, SE-10691 Stockholm, Sweden.(Swepub:kth)u1m7rsjb
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Kocevski, DanielNASA, Astrophys Off, ST12, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
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Perley, Daniel A.Liverpool John Moores Univ, Astrophys Res Inst, Liverpool Sci Pk,146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England.
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Racusin, JudithNASA, Astrophys Sci Div, Goddard Space Flight Ctr, MC 661, Greenbelt, MD 20771 USA.
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Univ Maryland, Dept Astron, College Pk, MD 20742 USA.;NASA, Ctr Res & Explorat Space Sci & Technol, GSFC, Greenbelt, MD 20771 USA.NASA, Astrophys Sci Div, Goddard Space Flight Ctr, MC 661, Greenbelt, MD 20771 USA.;Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
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In:Astrophysical Journal: American Astronomical Society904:20004-637X1538-4357
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