An Achromatic Break in the Afterglow of the Short GRB 140903A: Evidence for a Narrow Jet

We report the results of our observing campaign on GRB 140903A, a nearby (z = 0.351) short-duration (T ∼ 0.3 s) gamma-ray burst discovered by Swift. We monitored the X-ray afterglow with Chandra up to 15 days after the burst and detected a steeper decay of the X-ray flux after t ≈ 1 day. Continued m...

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Autores: Troja, E., Sakamoto, T., Cenko, S. B., Lien, A., Gehrels, N., Castro-Tirado, Alberto J., Ricci, R., Capone, J., Toy, V., Kutyrev, A., Kawai, N., Cucchiara, A., Fruchter, A., Gorosabel, Javier, Jeong, S., Levan, A., Perley, D., Sánchez Ramírez, Rubén, Tanvir, N., Veilleux, S.
Tipo de recurso: artículo
Estado:Versión aceptada para publicación
Fecha de publicación:2016
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/380189
Acceso en línea:http://hdl.handle.net/10261/380189
Access Level:acceso abierto
Palabra clave:Gamma-ray burst: individual (GRB 140903A)
X-rays: bursts
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spelling An Achromatic Break in the Afterglow of the Short GRB 140903A: Evidence for a Narrow JetTroja, E.Sakamoto, T.Cenko, S. B.Lien, A.Gehrels, N.Castro-Tirado, Alberto J.Ricci, R.Capone, J.Toy, V.Kutyrev, A.Kawai, N.Cucchiara, A.Fruchter, A.Gorosabel, JavierJeong, S.Levan, A.Perley, D.Sánchez Ramírez, RubénTanvir, N.Veilleux, S.Gamma-ray burst: individual (GRB 140903A)X-rays: burstsWe report the results of our observing campaign on GRB 140903A, a nearby (z = 0.351) short-duration (T ∼ 0.3 s) gamma-ray burst discovered by Swift. We monitored the X-ray afterglow with Chandra up to 15 days after the burst and detected a steeper decay of the X-ray flux after t ≈ 1 day. Continued monitoring at optical and radio wavelengths showed a similar decay in flux at nearly the same time, and we interpret it as evidence of a narrowly collimated jet. By using the standard fireball model to describe the afterglow evolution, we derive a jet opening angle θ ≈ 5° and a collimation-corrected total energy release E ≈ 2 × 10 erg. We further discuss the nature of the GRB progenitor system. Three main lines disfavor a massive star progenitor: the properties of the prompt gamma-ray emission, the age and low star formation rate of the host galaxy, and the lack of a bright supernova. We conclude that this event likely originated from a compact binary merger. © 2016. The American Astronomical Society. All rights reserved.The scientific results reported in this article are based in part on observations made by the Chandra X-ray Observatory. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Awards GO4-15072A and GO4-15067A issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. These results also made use of Lowell Observatory's Discovery Channel Telescope. Lowell operates the DCT in partnership with Boston University, Northern Arizona University, the University of Maryland, and the University of Toledo. Partial support of the DCT was provided by Discovery Communications. LMI was built by the Lowell Observatory using funds from the National Science Foundation (AST-1005313). This paper is partly based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina), and Ministério da Ciência, Tecnologia e Inovação (Brazil). Observations were also carried out with the 10.4 m Gran Telescopio Canarias installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias in the island of La Palma (GTC59-14B) and with the 3.5 m CAHA telescope at the German-Spanish Calar Alto Observatory operated by the IAA-CSIC. A.J.C.T. acknowledges support from the Spanish Ministry Projects AYA2012-39727-C03-01 and 2015-71718R.Peer reviewedIOP PublishingNASAMinisterio de Economía y Competitividad (España)National Science Foundation (US)Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]2025202520162025info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Postprintinfo:eu-repo/semantics/acceptedVersionhttp://hdl.handle.net/10261/380189reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/MINECO//AYA2012-39727-C03-01http://dx.doi.org/10.3847/0004-637X/827/2/102Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/3801892026-05-22T06:33:51Z
dc.title.none.fl_str_mv An Achromatic Break in the Afterglow of the Short GRB 140903A: Evidence for a Narrow Jet
title An Achromatic Break in the Afterglow of the Short GRB 140903A: Evidence for a Narrow Jet
spellingShingle An Achromatic Break in the Afterglow of the Short GRB 140903A: Evidence for a Narrow Jet
Troja, E.
Gamma-ray burst: individual (GRB 140903A)
X-rays: bursts
title_short An Achromatic Break in the Afterglow of the Short GRB 140903A: Evidence for a Narrow Jet
title_full An Achromatic Break in the Afterglow of the Short GRB 140903A: Evidence for a Narrow Jet
title_fullStr An Achromatic Break in the Afterglow of the Short GRB 140903A: Evidence for a Narrow Jet
title_full_unstemmed An Achromatic Break in the Afterglow of the Short GRB 140903A: Evidence for a Narrow Jet
title_sort An Achromatic Break in the Afterglow of the Short GRB 140903A: Evidence for a Narrow Jet
dc.creator.none.fl_str_mv Troja, E.
Sakamoto, T.
Cenko, S. B.
Lien, A.
Gehrels, N.
Castro-Tirado, Alberto J.
Ricci, R.
Capone, J.
Toy, V.
Kutyrev, A.
Kawai, N.
Cucchiara, A.
Fruchter, A.
Gorosabel, Javier
Jeong, S.
Levan, A.
Perley, D.
Sánchez Ramírez, Rubén
Tanvir, N.
Veilleux, S.
author Troja, E.
author_facet Troja, E.
Sakamoto, T.
Cenko, S. B.
Lien, A.
Gehrels, N.
Castro-Tirado, Alberto J.
Ricci, R.
Capone, J.
Toy, V.
Kutyrev, A.
Kawai, N.
Cucchiara, A.
Fruchter, A.
Gorosabel, Javier
Jeong, S.
Levan, A.
Perley, D.
Sánchez Ramírez, Rubén
Tanvir, N.
Veilleux, S.
author_role author
author2 Sakamoto, T.
Cenko, S. B.
Lien, A.
Gehrels, N.
Castro-Tirado, Alberto J.
Ricci, R.
Capone, J.
Toy, V.
Kutyrev, A.
Kawai, N.
Cucchiara, A.
Fruchter, A.
Gorosabel, Javier
Jeong, S.
Levan, A.
Perley, D.
Sánchez Ramírez, Rubén
Tanvir, N.
Veilleux, S.
author2_role author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
dc.contributor.none.fl_str_mv NASA
Ministerio de Economía y Competitividad (España)
National Science Foundation (US)
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Gamma-ray burst: individual (GRB 140903A)
X-rays: bursts
topic Gamma-ray burst: individual (GRB 140903A)
X-rays: bursts
description We report the results of our observing campaign on GRB 140903A, a nearby (z = 0.351) short-duration (T ∼ 0.3 s) gamma-ray burst discovered by Swift. We monitored the X-ray afterglow with Chandra up to 15 days after the burst and detected a steeper decay of the X-ray flux after t ≈ 1 day. Continued monitoring at optical and radio wavelengths showed a similar decay in flux at nearly the same time, and we interpret it as evidence of a narrowly collimated jet. By using the standard fireball model to describe the afterglow evolution, we derive a jet opening angle θ ≈ 5° and a collimation-corrected total energy release E ≈ 2 × 10 erg. We further discuss the nature of the GRB progenitor system. Three main lines disfavor a massive star progenitor: the properties of the prompt gamma-ray emission, the age and low star formation rate of the host galaxy, and the lack of a bright supernova. We conclude that this event likely originated from a compact binary merger. © 2016. The American Astronomical Society. All rights reserved.
publishDate 2016
dc.date.none.fl_str_mv 2016
2025
2025
2025
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
Postprint
info:eu-repo/semantics/acceptedVersion
format article
status_str acceptedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/380189
url http://hdl.handle.net/10261/380189
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv #PLACEHOLDER_PARENT_METADATA_VALUE#
info:eu-repo/grantAgreement/MINECO//AYA2012-39727-C03-01
http://dx.doi.org/10.3847/0004-637X/827/2/102
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv IOP Publishing
publisher.none.fl_str_mv IOP Publishing
dc.source.none.fl_str_mv reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC
instname:Consejo Superior de Investigaciones Científicas (CSIC)
instname_str Consejo Superior de Investigaciones Científicas (CSIC)
reponame_str DIGITAL.CSIC. Repositorio Institucional del CSIC
collection DIGITAL.CSIC. Repositorio Institucional del CSIC
repository.name.fl_str_mv
repository.mail.fl_str_mv
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