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dc.contributor.authorKangas, Tuomases_ES
dc.contributor.authorFruchter, Andrew S.es_ES
dc.contributor.authorCenko, S. Bradleyes_ES
dc.contributor.authorCorsi, Alessandraes_ES
dc.contributor.authorUgarte Postigo, Antonio dees_ES
dc.contributor.authorPe'er, Asafes_ES
dc.contributor.authorVogel, Stuart N.es_ES
dc.contributor.authorCucchiara, Antoninoes_ES
dc.contributor.authorGompertz, Benjamines_ES
dc.contributor.authorGraham, Johnes_ES
dc.contributor.authorLevan, Andrewes_ES
dc.contributor.authorMisra, Kuntales_ES
dc.contributor.authorPerley, Daniel A.es_ES
dc.contributor.authorRacusin, Judith L.es_ES
dc.contributor.authorTanvir, Niales_ES
dc.date.accessioned2020-05-29T07:04:03Z-
dc.date.available2020-05-29T07:04:03Z-
dc.date.issued2020-
dc.identifier.citationAstrophysical Journal 894(1): 43 (2020)es_ES
dc.identifier.issn0004-637X-
dc.identifier.urihttp://hdl.handle.net/10261/212621-
dc.description.abstractWe present post-jet-break Hubble Space Telescope, Very Large Array, and Chandra observations of the afterglow of the long gamma-ray bursts GRB 160625B (between 69 and 209 days) and GRB 160509A (between 35 and 80 days). We calculate the post-jet-break decline rates of the light curves and find the afterglow of GRB 160625B is inconsistent with a simple t(-3/4) steepening over the break, expected from the geometric effect of the jet edge entering our line of sight. However, the favored optical post-break decline is also inconsistent with the f(nu) proportional to t(-p) decline (where p 2.3 from the pre-break light curve), which is expected from exponential lateral expansion of the jet; perhaps suggesting lateral expansion that only affects a fraction of the jet. The post-break decline of GRB 160509A is consistent with both the t(-3/4) steepening and with f(nu) proportional to t(-p). We also use boxfit to fit afterglow models to both light curves and find both to be energetically consistent with a millisecond magnetar central engine, but the magnetar parameters need to be extreme (i.e., E similar to 3 x 10(52) erg). Finally, the late-time radio light curves of both afterglows are not reproduced well by boxfit and are inconsistent with predictions from the standard jet model; instead, both are well represented by a single power-law decline (roughly f(nu) proportional to t(-1)) with no breaks. This requires a highly chromatic jet break and possibly a two-component jet for both bursts.© 2020. The American Astronomical Society. All rights reserved.es_ES
dc.description.sponsorshipA.C. acknowledges support from the National Science Foundation via CAREER award #1455090. A.d.U.P. acknowledges support from a Ramon y Cajal fellowship (RyC-201209975), from the Spanish research project AYA2017-89384-P, and from the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709). A.P. wishes to acknowledge support by the European Research Council via the ERC consolidating grant #773062 (acronym O.M.J.). A.C. acknowledges the support of NASA MIRO grant NNX15AP95A. Based on observations made with the NASA/ESA Hubble Space Telescope (programme GO 14353, PI Fruchter), obtained through the data archive at the Space Telescope Science Institute (STScI). STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. Support for this work was also provided by the National Aeronautics and Space Administration through Chandra Award Number 17500753, PI Fruchter, 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. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester as well as observations made with the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, in the island of La Palma. Development of CIRCE was supported by the University of Florida and the National Science Foundation (grant AST-0352664), in collaboration with IUCAA. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Development of the BOXFIT code was supported in part by NASA through grant NNX10AF62G issued through the Astrophysics Theory Program and by the NSF through grant AST1009863. Simulations for BOXFIT version 2 have been carried out in part on the computing facilities of the Computational Center for Particle and Astrophysics (C2PAP) of the research cooperation "Excellence Cluster Universe" in Garching, Germany.es_ES
dc.language.isoenges_ES
dc.publisherIOP Publishinges_ES
dc.relationMICIU/ICTI2017-2020/AYA2017-89384-Pes_ES
dc.relationMICIU/ICTI2017-2020/SEV-2017-0709es_ES
dc.relationinfo:eu-repo/grantAgreement/EC/H2020/773062es_ES
dc.relation.isversionofPostprintes_ES
dc.rightsopenAccessen_EN
dc.subjectGamma ray burstses_ES
dc.subjectRelativistic jetses_ES
dc.titleThe Late-time Afterglow Evolution of Long Gamma-Ray Bursts GRB 160625B and GRB 160509Aes_ES
dc.typeartículoes_ES
dc.identifier.doi10.3847/1538-4357/ab8799-
dc.description.peerreviewedPeer reviewedes_ES
dc.relation.publisherversionhttp://dx.doi.org/10.3847/1538-4357/ab8799es_ES
dc.embargo.terms2021-05-05es_ES
dc.contributor.funderNational Science Foundation (US)es_ES
dc.contributor.funderMinisterio de Ciencia, Innovación y Universidades (España)es_ES
dc.contributor.funderEuropean Commissiones_ES
dc.contributor.funderEuropean Research Counciles_ES
dc.contributor.funderNational Aeronautics and Space Administration (US)es_ES
dc.contributor.funderUniversity of Floridaes_ES
dc.contributor.funderInter-University Centre for Astronomy and Astrophysics (India)es_ES
dc.relation.csices_ES
oprm.item.hasRevisionno ko 0 false*
dc.identifier.funderhttp://dx.doi.org/10.13039/100000001es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100000780es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100000781es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/100000104es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/100007698es_ES
dc.type.coarhttp://purl.org/coar/resource_type/c_6501es_ES
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item.languageiso639-1en-
item.grantfulltextopen-
item.openairecristypehttp://purl.org/coar/resource_type/c_18cf-
item.fulltextWith Fulltext-
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