SN 2013dx associated with GRB 130702A: A detailed photometric and spectroscopic monitoring and a study of the environment

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dc.contributor.authorD'Elia, V.
dc.contributor.authorPian, E.
dc.contributor.authorMelandri, A.
dc.contributor.authorD'Avanzo, P.
dc.contributor.authorDella Valle, M.
dc.contributor.authorMazzali, P.A.
dc.contributor.authorPiranomonte, S.
dc.contributor.authorTagliaferri, G.
dc.contributor.authorAntonelli, L.A.
dc.contributor.authorBufano, F.
dc.contributor.authorCovino, S.
dc.contributor.authorFugazza, D.
dc.contributor.authorMalesani, D.
dc.contributor.authorMøller, P.
dc.contributor.authorPalazzi, E.
dc.date.accessioned2023-06-15T13:56:32Z
dc.date.available2023-06-15T13:56:32Z
dc.date.issued2015-05
dc.descriptionIndexación: Scopuses
dc.description.abstractAims. Long-duration gamma-ray bursts (GRBs) and broad-line, type Ic supernovae (SNe) are strongly connected. We aim at characterizing SN 2013dx, which is associated with GRB? 130702A, through a sensitive and extensive ground-based observational campaign in the optical-IR band. Methods. We monitored the field of the Swift GRB 130702A (redshift z = 0.145) using the 8.2 m VLT, the 3.6 m TNG and the 0.6 m REM telescopes during the time interval between 4 and 40 days after the burst. Photometric and spectroscopic observations revealed the associated type Ic SN 2013dx. Our multiband photometry allowed constructing a bolometric light curve. Results. The bolometric light curve of SN 2013dx resembles that of 2003dh (associated with GRB? 030329), but is ~10% faster and ~25% dimmer. From this we infer a synthesized 56Ni mass of ∼0.2 Mo. The multi-epoch optical spectroscopy shows that the SN 2013dx behavior is best matched by SN 1998bw, among the other well-known low-redshift SNe associated with GRBs and XRFs, and by SN 2010ah, an energetic type Ic SN not associated with any GRB. The photospheric velocity of the ejected material declines from ∼2.7 × 104 km? s-1 at 8 rest frame days from the explosion, to ∼3.5 × 103 km? s-1 at 40 days. These values are extremely close to those of SN1998bw and 2010ah. We deduce for SN 2013dx a kinetic energy of ∼35 × 1051 erg and an ejected mass of ∼7 M. This suggests that the progenitor of SN2013dx had a mass of ∼25-30 M, which is 15-20% less massive than that of SN 1998bw. Finally, we studied the SN 2013dx environment through spectroscopy of the closeby galaxies: 9 out of the 14 inspected galaxies lie within 0.03 in redshift from z = 0.145, indicating that the host of GRB? 130702A/SN 2013dx belongs to a group of galaxies, an unprecedented finding for a GRB-associated SN and, to our knowledge, for long GRBs in general. © ESO, 2015.es
dc.description.urihttps://www.aanda.org/articles/aa/full_html/2015/05/aa25381-14/aa25381-14.html
dc.identifier.citationAstronomy and Astrophysics Volume 5771 May 2015 Article number A116es
dc.identifier.doi10.1051/0004-6361/201425381
dc.identifier.issn0004-6361
dc.identifier.urihttps://repositorio.unab.cl/xmlui/handle/ria/50719
dc.language.isoenes
dc.publisherEDP Scienceses
dc.rights.licenseAtribución 4.0 Internacional (CC BY 4.0)
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/deed.es
dc.subjectGamma-ray burstes
dc.subjectSupernovae: individual: SN 2013dxes
dc.titleSN 2013dx associated with GRB 130702A: A detailed photometric and spectroscopic monitoring and a study of the environmentes
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