GRB 140606B/iPTF14bfu: detection of shock-breakout emission from a cosmological gamma-ray burst?

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dc.contributor.authorCano, Zach
dc.contributor.authorde Ugarte Postigo, A.
dc.contributor.authorPerley, D.
dc.contributor.authorKruehler, T.
dc.contributor.authorMargutti, R.
dc.contributor.authorFriis, M.
dc.contributor.authorMalesani, D.
dc.contributor.authorJakobsson, P.
dc.contributor.authorFynbo, J. P. U.
dc.contributor.authorGorosabel, J.
dc.contributor.authorHjorth, J.
dc.contributor.authorSanchez Ramirez, R.
dc.contributor.authorSchulze, S.
dc.contributor.authorTanvir, N. R.
dc.contributor.authorThoene, C. C.
dc.contributor.authorXu, D.
dc.date.accessioned2024-01-10T12:39:17Z
dc.date.available2024-01-10T12:39:17Z
dc.date.issued2015
dc.description.abstractWe present optical and near-infrared photometry of GRB 140606B (z = 0.384), and optical photometry and spectroscopy of its associated supernova (SN). The results of our modelling indicate that the bolometric properties of the SN (M-Ni = 0.4 +/- 0.2 M-circle dot, M-ej = 5 +/- 2 M-circle dot, and E-K = 2 +/- 1 x 10(52) erg) are fully consistent with the statistical averages determined for other gamma-ray burst (GRB)-SNe. However, in terms of its gamma-ray emission, GRB 140606B is an outlier of the Amati relation, and occupies the same region as low luminosity (ll) and short GRBs. The gamma-ray emission in llGRBs is thought to arise in some or all events from a shock breakout (SBO), rather than from a jet. The measured peak photon energy (E-p approximate to 800 keV) is close to that expected for. -rays created by an SBO (greater than or similar to 1 MeV). Moreover, based on its position in the M-V,M- (p)- L-iso,L-gamma plane and the E-K-Gamma eta plane, GRB 140606B has properties similar to both SBO-GRBs and jetted-GRBs. Additionally, we searched for correlations between the isotropic gamma-ray emission and the bolometric properties of a sample of GRB-SNe, finding that no statistically significant correlation is present. The average kinetic energy of the sample is (E) over bar (K) = 2.1 x 10(52) erg. All of the GRB-SNe in our sample, with the exception of SN 2006aj, are within this range, which has implications for the total energy budget available to power both the relativistic and non-relativistic components in a GRB-SN event.
dc.description.funderScience and Technology Facilities Council
dc.fechaingreso.objetodigital2024-05-02
dc.format.extent18 páginas
dc.fuente.origenWOS
dc.identifier.doi10.1093/mnras/stv1327
dc.identifier.eissn1365-2966
dc.identifier.issn0035-8711
dc.identifier.urihttps://doi.org/10.1093/mnras/stv1327
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/77171
dc.identifier.wosidWOS:000360851900036
dc.information.autorucFísica;Schulze S;S/I;237742
dc.issue.numero2
dc.language.isoen
dc.nota.accesocontenido parcial
dc.pagina.final1552
dc.pagina.inicio1535
dc.publisherOXFORD UNIV PRESS
dc.revistaMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
dc.rightsacceso restringido
dc.subjectgamma-ray burst: general
dc.subjectgamma-ray burst: individual: GRB 140606B
dc.subjectgamma-ray burst: individual: iPTF14bfu
dc.subjectsupernovae: general
dc.subjectSUPERNOVA 2003DH
dc.subjectLIGHT CURVES
dc.subjectPEAK-ENERGY
dc.subjectLONG
dc.subjectAFTERGLOWS
dc.subjectDISCOVERY
dc.subjectCOLLAPSE
dc.subjectSPECTRA
dc.subjectABSORPTION
dc.subjectPARAMETERS
dc.subject.ods07 Affordable and Clean Energy
dc.subject.odspa07 Energía asequible y no contaminante
dc.titleGRB 140606B/iPTF14bfu: detection of shock-breakout emission from a cosmological gamma-ray burst?
dc.typeartículo
dc.volumen452
sipa.codpersvinculados237742
sipa.indexWOS
sipa.indexScopus
sipa.trazabilidadCarga SIPA;09-01-2024
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