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Por favor, use este identificador para citar o enlazar a este item: http://hdl.handle.net/10261/140455
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dc.contributor.authorJapelj, J.-
dc.contributor.authorVergani, S. D.-
dc.contributor.authorSalvaterra, Rubén-
dc.contributor.authorD’Avanzo, P.-
dc.contributor.authorFernández-Soto, Alberto-
dc.contributor.authorGallego, Jesús-
dc.contributor.authorTagliaferri, G.-
dc.date.accessioned2016-11-18T13:19:31Z-
dc.date.available2016-11-18T13:19:31Z-
dc.date.issued2016-
dc.identifierdoi: 10.1051/0004-6361/201628314-
dc.identifiere-issn: 1432-0746-
dc.identifierissn: 0004-6361-
dc.identifier.citationAstronomy and Astrophysics 590: A129 (2016)-
dc.identifier.urihttp://hdl.handle.net/10261/140455-
dc.descriptionExtragalactic astronomy.-- et al.-
dc.description.abstract[Aims]: Long gamma-ray bursts (LGRBs) are associated with the deaths of massive stars and might therefore be a potentially powerful tool for tracing cosmic star formation. However, especially at low redshifts (z < 1.5) LGRBs seem to prefer particular types of environment. Our aim is to study the host galaxies of a complete sample of bright LGRBs to investigate the effect of the environment on GRB formation. [Methods]: We studied host galaxy spectra of the Swift/BAT6 complete sample of 14 z < 1 bright LGRBs. We used the detected nebular emission lines to measure the dust extinction, star formation rate (SFR), and nebular metallicity (Z) of the hosts and supplemented the data set with previously measured stellar masses M. The distributions of the obtained properties and their interrelations (e.g. mass-metallicity and SFR-M relations) are compared to samples of field star-forming galaxies. [Results]: We find that LGRB hosts at z < 1 have on average lower SFRs than if they were direct star formation tracers. By directly comparing metallicity distributions of LGRB hosts and star-forming galaxies, we find a good match between the two populations up to 12 + log (O/H) ∼ 8.4-8.5, after which the paucity of metal-rich LGRB hosts becomes apparent. The LGRB host galaxies of our complete sample are consistent with the mass-metallicity relation at similar mean redshift and stellar masses. The cutoff against high metallicities (and high masses) can explain the low SFR values of LGRB hosts. We find a hint of an increased incidence of starburst galaxies in the Swift/BAT6 z < 1 sample with respect to that of a field star-forming population. Given that the SFRs are low on average, the latter is ascribed to low stellar masses. Nevertheless, the limits on the completeness and metallicity availability of current surveys, coupled with the limited number of LGRB host galaxies, prevents us from investigating more quantitatively whether the starburst incidence is such as expected after taking into account the high-metallicity aversion of LGRB host galaxies.-
dc.description.sponsorshipJ.J. and S.C. acknowledge financial contribution from the grant PRIN MIUR 2012 201278X4FL 002 The Intergalactic Medium as a probe of the growth of cosmic structures. S.D.V. and E.L.F. acknowledge the UnivEarthS Labex programme at Sorbonne Paris Cité (ANR-10-LABX-0023 and ANR-11-IDEX-0005-02). A.F.S. acknowledges support from grants AYA2013-48623-C2-2 from the Spanish Ministerio de Economia y Competitividad, and PrometeoII 2014/060 from the Generalitat Valenciana.-
dc.publisherEDP Sciences-
dc.relationinfo:eu-repo/grantAgreement/MINECO/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2013-48623-C2-2-P-
dc.relation.isversionofPublisher's version-
dc.rightsopenAccess-
dc.subjectGalaxies: star formation-
dc.subjectGamma-ray burst: general-
dc.titleAre long gamma-ray bursts biased tracers of star formation? Clues from the host galaxies of the Swift/BAT6 complete sample of bright LGRBs-
dc.title.alternativeII. Star formation rates and metallicities at z < 1-
dc.typeartículo-
dc.identifier.doi10.1051/0004-6361/201628314-
dc.relation.publisherversionhttp://dx.doi.org/10.1051/0004-6361/201628314-
dc.date.updated2016-11-18T13:19:31Z-
dc.description.versionPeer Reviewed-
dc.language.rfc3066eng-
dc.contributor.funderAgence Nationale de la Recherche (France)-
dc.contributor.funderUniversité Paris Diderot-
dc.contributor.funderMinistero dell'Istruzione, dell'Università e della Ricerca-
dc.contributor.funderMinisterio de Economía y Competitividad (España)-
dc.contributor.funderGeneralitat Valenciana-
dc.relation.csicSí-
dc.identifier.funderhttp://dx.doi.org/10.13039/501100001665es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100005736es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100003407es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100003329es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100003359es_ES
dc.type.coarhttp://purl.org/coar/resource_type/c_6501es_ES
item.fulltextWith Fulltext-
item.openairecristypehttp://purl.org/coar/resource_type/c_18cf-
item.openairetypeartículo-
item.cerifentitytypePublications-
item.grantfulltextopen-
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