J/ApJ/802/103ivo://CDS.VizieR/J/ApJ/802/103doi:10.26093/cds/vizier.18020103CDSTrenti M.Perna R.Jimenez R.2015-09-19T09:54:44Z2015-08-27T13:43:49ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frgamma-ray-astronomyredshiftedstellar-masseschemical-abundancesLong-duration gamma-ray bursts (GRBs) are powerful probes of the star formation history of the universe, but the correlation between the two depends on the highly debated presence and strength of a metallicity bias. To investigate this correlation, we use a phenomenological model that successfully describes star formation rates, luminosities, and stellar masses of star-forming galaxies and apply it to GRB production. We predict the luminosities, stellar masses, and metallicities of host galaxies depending on the presence (or absence) of a metallicity bias. Our best-fitting model includes a moderate metallicity bias, broadly consistent with the large majority of the long-duration GRBs in metal-poor environments originating from a collapsar (probability ~83%, with [0.74;0.91] range at 90% confidence level), but with a secondary contribution (~17%) from a metal-independent production channel, such as binary evolution. Because of the mass-metallicity relation of galaxies, the maximum likelihood model predicts that the metal-independent channel becomes dominant at z~<2, where hosts have higher metallicities and collapsars are suppressed. This possibly explains why some studies find no clear evidence of a metal bias based on low-z samples. However, while metallicity predictions match observations well at high redshift (z>~2), there is tension with low-redshift observations, since a significant fraction of GRB hosts are predicted to have (near) solar metallicity. This is in contrast to observations, unless obscured, metal-rich hosts are preferentially missed in current data sets, and suggests that lower efficiencies of the metal-independent GRB channel might be preferred following a comprehensive fit that includes metallicity of GRB hosts from complete samples. Overall, we are able to clearly establish the presence of a metallicity bias for GRB production, but continued characterization of GRB host galaxies is needed to quantify its strength.2015ApJ...802..103Thttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/802/103CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/ApJ/778/128 : GRB-host galaxies photometry (Perley+, 2013)J/A+A/556/A55 : Multi-color photometry of star-forming galaxies (Ilbert+, 2013)J/ApJ/683/321 : Metallicities of GRB, DLA, and Ly{alpha} galaxies (Fynbo+, 208)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/802/103https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/802/103http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/802/103https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/802/103https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/802/103http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/802/103GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapGamma-rayOpticaldefaultJ/ApJ/802/103/table2Model predictions for GRB host propertiesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintz[0.25/9] Model redshiftsrc.redshiftfloatp[1e-11/10000] Model plateau value (1)stat.paramdoubleMag.d[-25.8/-10.9] GRB host galaxy absolute UV magnitude, including dust extinction (AB scale)magphys.magAbsfloatMag[-28/-11] GRB intrinsic host galaxy absolute UV magnitude M_UV_ (AB scale)magphys.magAbsfloatM*[181894/4.5662e+11] GRB host galaxy stellar masssolMassphys.massdoubleMdmGRB host galaxy dark-matter halo masssolMassphys.massdoublelogZ[-4.8/0.4] Log Metallicity log_10_(Z/Z_{sun}_)log(Sun)phys.abund.ZfloatNCumulative number of GRBs in hosts having magnitude<=M_UV_ (1)meta.numberdouble