J/MNRAS/479/3563ivo://CDS.VizieR/J/MNRAS/479/3563doi:10.26093/cds/vizier.74793563CDSFriedmann M.Maoz D.2024-08-18T20:20:41Z2022-05-06T08:51:04ZCDS support team

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

cds-question@unistra.frsupernovaegalaxy-clustersredshiftedhst-photometryThe observed delay-time distribution (DTD) of Type-Ia supernovae (SNe Ia) is a valuable probe of SN Ia progenitors and physics, and of the role of SNe Ia in cosmic metal enrichment. The SN Ia rate in galaxy clusters as a function of cluster redshift is an almost-direct measure of the DTD, but current estimates have been limited out to a mean redshift <z>=1.1, corresponding to time delays, after cluster star formation, of >=3.2Gyr. We analyze data from a Hubble Space Telescope monitoring project of 12 galaxy clusters at z=1.13-1.75, where we discover 29 SNe, and present their multiband light curves. Based on the SN photometry and the apparent host galaxies, we assess cluster membership and SN type, finding 11cases that are likely SNe Ia in cluster galaxies and 4 more cases, which are possible but not certain cluster SNe Ia. We conduct simulations to estimate the SN detection efficiency, the experiment's completeness, and the photometric errors, and perform photometry of the cluster galaxies to derive the cluster stellar masses. With this input, we obtain a mean <z>=1.35 cluster rest-frame SN Ia rate per unit formed stellar mass of R_Ia,m*_=2.6^+3.2^_-1.5_x10^-13^yr^-1^M_{sun}_^-1^. Separating the cluster sample into high-z and low-z bins, the rates are 2.2^+2.6^_-1.3_x10^-13^yr^-1^M_{sun}_^-1^ at <z>=1.25, and 3.5^+6.6^_-2.8_x10^-13^yr^-1^M_{sun}_^-1^ at <z>=1.58. Combining our results with previous cluster SN Ia rates, we fit the DTD, now down to delays of 1.5Gyr, with a power-law dependence, t^{alpha}^, with {alpha}=-1.30^+0.23^_-0.16_. We confirm previous indications for a SN Ia production efficiency that is several times higher in galaxy clusters than in the field, perhaps caused by a peculiar stellar initial mass function in clusters, or by a higher incidence of binaries that will evolve into SNe Ia.2018MNRAS.479.3563Fhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/479/3563CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/479/3563https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/479/3563http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/479/3563https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/479/3563https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/479/3563http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/479/3563GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/479/3563/table2 (Supernova candidates)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/479/3563/table2?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/479/3563/table2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/479/3563/table2?GETtext/xml+votable180.050000true216.65958335.1407220.0055555555555555566/9145 9147 10515 16702 17694 27227 27883 33502 35476 35934 45873 47430https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/479/3563?format=asciidefaultJ/MNRAS/479/3563/table2Supernova candidatesSimbadSimbad column added by the CDSmeta.ref.urlcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintClusterCluster Namemeta.id.parentcharzRedshiftsrc.redshiftfloatSNIDSupernova Name (1)meta.id;meta.maincharRAJ2000Right Ascension (J2000)pos.eq.ra;meta.mainDEJ2000Declination (J2000)pos.eq.dec;meta.mainSep? Angular separation between the SN and its host galaxy (if an obvious host exists)arcsecpos.angDistancefloatnullableDistProjected distance between the SN and approximate center of clusterkpcpos.distanceintCl.Ia?Decision on whether transient is a SN Ia at the cluster redshift (2)meta.codecharx1? SALT2 light-curve widthstat.fit.paramfloatnullablee_x1? SALT2 light-curve width error (lower value)stat.errorfloatnullableE_x1? SALT2 light-curve width error (upper value)stat.error;stat.maxfloatnullablec? SALT2 c parameterstat.fit.paramfloatnullableE_c? SALT2 c parameter error (upper value)stat.error;stat.maxfloatnullablee_c? SALT2 c parameter error (lower value)stat.errorfloatnullableMB? Absolute magnitude at maximum light in the rest-frame B obtained through a SN Ia luminosity-width-colour relationmagphys.magAbsfloatnullableE_MB? Magnitude error (upper value)magstat.error;stat.maxfloatnullablee_MB? Magnitude error (lower value)magstat.errorfloatnullablet0? SALT2 Observer-frame time corresponding to the source's phase=0.dtime.epochintnullableE_t0? t0 error (upper value)dstat.error;stat.maxintnullablee_t0? t0 error (lower value)dstat.errorintnullableChi2? Chi-squared of best cluster SN Ia model fitstat.fit.chi2;stat.param;meta.modelledfloatnullabledof? Degree of freedom of best cluster SN Ia model fitstat.fit.dofintnullableJ/MNRAS/479/3563/table3Full photometry table for all SNe candidatesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintClusterCluster Namemeta.id.parentcharSNIDSupernova Namemeta.id;meta.maincharJDJulian Date (JD-2450000)dtime.epochdoubleBandObserved Bandinstr.bandpasscharFluxFlux1e-21W.m**-2phot.flux.densityfloate_FluxFlux Error1e-21W.m**-2stat.error;phot.fluxfloat