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Por favor, use este identificador para citar o enlazar a este item: http://hdl.handle.net/10261/139946
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dc.contributor.authorKohn, S. A.-
dc.contributor.authorMichalowski, M. J.-
dc.contributor.authorBaes, M.-
dc.contributor.authorZotti, G. de-
dc.contributor.authorDye, S.-
dc.contributor.authorEales, S.-
dc.contributor.authorGonzález-Nuevo, J.-
dc.contributor.authorIvison, R. J.-
dc.contributor.authorMaddox, S. J.-
dc.contributor.authorScott, Douglas-
dc.contributor.authorSmith, D. J. B.-
dc.date.accessioned2016-11-08T12:21:18Z-
dc.date.available2016-11-08T12:21:18Z-
dc.date.issued2015-
dc.identifierdoi: 10.1093/mnras/stv088-
dc.identifiere-issn: 1365-2966-
dc.identifierissn: 0035-8711-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society 448(2): 1494-1503 (2015)-
dc.identifier.urihttp://hdl.handle.net/10261/139946-
dc.descriptionet al.-
dc.description.abstractGamma-ray bursts (GRBs) are themost energetic phenomena in theUniverse; believed to result from the collapse and subsequent explosion of massive stars. Even though it has profound consequences for our understanding of their nature and selection biases, little is known about the dust properties of the galaxies hosting GRBs. We present analysis of the far-infrared properties of an unbiased sample of 20 BeppoSAX and Swift GRB host galaxies (at an average redshift of z = 3.1) located in the Herschel Astrophysical Terahertz Large Area Survey, the Herschel Virgo Cluster Survey, the Herschel Fornax Cluster Survey, the Herschel Stripe 82 Survey and the Herschel Multi-tiered Extragalactic Survey, totalling 880 deg2, or ~3 per cent of the sky in total. Our sample selection is serendipitous, based only on whether the Xray position of a GRB lies within a large-scale Herschel survey - therefore our sample can be considered completely unbiased. Using deep data at wavelengths of 100-500 μm, we tentatively detected 1 out of 20GRBhosts located in these fields.We constrain their dustmasses and star formation rates (SFRs), and discuss these in the context of recent measurements of submillimetre galaxies and ultraluminous infrared galaxies. The average far-infrared flux of our sample gives an upper limit on SFR of <114 M⊙ yr-1. The detection rate of GRB hosts is consistent with that predicted assuming that GRBs trace the cosmic SFR density in an unbiased way, i.e. that the fraction of GRB hosts with SFR > 500M⊙ yr-1 is consistent with the contribution of such luminous galaxies to the cosmic star formation density.-
dc.description.sponsorshipMJM acknowledges the support of the UK Science and Technology Facilities Council. NB is supported by the EC FP7 SPACE project ASTRODEEP (Ref. No. 312725). EI acknowledges funding from CONICYT/FONDECYT postdoctoral project no. 3130504. LD, RJI and SJM acknowledge support from ERC Advanced Grant COSMICISM. JGN acknowledges financial support from the Spanish CSIC for a JAE-DOC fellowship, co-funded by the European Social Fund, by the Spanish Ministerio de Ciencia e Innovacion, AYA2012-39475-C02-01, and Consolider-Ingenio 2010, CSD2010-00064, projects.-
dc.publisherOxford University Press-
dc.relationinfo:eu-repo/grantAgreement/EC/FP7/312725-
dc.relationinfo:eu-repo/grantAgreement/EC/FP7/321302-
dc.relation.isversionofPublisher's version-
dc.rightsopenAccess-
dc.subjectGalaxies: star formation-
dc.subjectGamma-ray burst: general-
dc.subjectDust, extinction-
dc.subjectGalaxies: high-redshift-
dc.subjectInfrared: galaxies-
dc.titleFar-infrared observations of an unbiased sample of gamma-ray burst host galaxies-
dc.typeartículo-
dc.identifier.doi10.1093/mnras/stv088-
dc.relation.publisherversionhttps://doi.org/10.1093/mnras/stv088-
dc.date.updated2016-11-08T12:21:18Z-
dc.description.versionPeer Reviewed-
dc.language.rfc3066eng-
dc.contributor.funderFondo Nacional de Desarrollo Científico y Tecnológico (Chile)-
dc.contributor.funderMinisterio de Ciencia e Innovación (España)-
dc.contributor.funderConsejo Superior de Investigaciones Científicas (España)-
dc.contributor.funderScience and Technology Facilities Council (UK)-
dc.contributor.funderEuropean Commission-
dc.contributor.funderEuropean Research Council-
dc.contributor.funderComisión Nacional de Investigación Científica y Tecnológica (Chile)-
dc.relation.csicSí-
dc.identifier.funderhttp://dx.doi.org/10.13039/501100002850es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100004837es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100003339es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100000271es_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/10.13039/501100002848es_ES
dc.type.coarhttp://purl.org/coar/resource_type/c_6501es_ES
item.grantfulltextopen-
item.openairetypeartículo-
item.cerifentitytypePublications-
item.fulltextWith Fulltext-
item.openairecristypehttp://purl.org/coar/resource_type/c_18cf-
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