J/A+A/644/A176ivo://CDS.VizieR/J/A+A/644/A176doi:10.26093/cds/vizier.36440176CDSRigault M.Brinnel V.Aldering G.Antilogus P.Aragon C.Bailey S.,Baltay C.Barbary K.Bongard S.Boone K.Buton C.Childress M.,Chotard N.Copin Y.Dixon S.Fagrelius P.Feindt U.Fouchez D.,Gangler E.Hayden B.Hillebrandt W.Howell D.A.Kim A.Kowalski M.,Kuesters D.Leget P.-F.Lombardo S.Lin Q.Nordin J.Pain R.,Pecontal E.Pereira R.Perlmutter S.Rabinowitz D.Runge K.Rubin D.,Saunders C.Smadja G.Sofiatti C.Suzuki N.Taubenberger S.Tao C.,Thomas R.C.2021-05-04T13:20:46Z2020-12-17T08:01:06ZCDS support team

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

cds-question@unistra.frsupernovaephotometryvisible-astronomyAs part of an on-going effort to identify, understand and correct for astrophysics biases in the standardization of Type Ia supernovae (SN Ia) for cosmology, we have statistically classified a large sample of nearby SNe Ia into those that are located in predominantly younger or older environments. This classification is based on the specific star formation rate measured within a projected distance of 1kpc from each SN location (LsSFR). This is an important refinement compared to using the local star formation rate directly, as it provides a normalization for relative numbers of available SN progenitors and is more robust against extinction by dust. We find that the SNe Ia in predominantly younger environments are {DELTA}Y=0.163+/-0.029mag (5.7{sigma}) fainter than those in predominantly older environments after conventional light-curve standardization. This is the strongest standardized SN Ia brightness systematic connected to the host-galaxy environment measured to date. The well-established step in standardized brightnesses between SNe Ia in hosts with lower or higher total stellar masses is smaller, at {DELTA}M=0.119+/-0.032mag (4.5{sigma}), for the same set of SNe Ia. When fit simultaneously, the environment-age offset remains very significant, with {DELTA}Y=0.129+/-0.032mag (4.0{sigma}), while the global stellar mass step is reduced to {DELTA}M=0.064+/-0.029mag (2.2{sigma}). Thus, approximately 70% of the variance from the stellar mass step is due to an underlying dependence on environment-based progenitor age. Also, we verify that using the local star formation rate alone is not as powerful as LsSFR at sorting SNe Ia into brighter and fainter subsets. Standardization that only uses the SNe Ia in younger environments reduces the total dispersion from 0.142+/-0.008mag to 0.120+/-0.010mag. We show that as environment-ages evolve with redshift, a strong bias, especially on the measurement of the derivative of the dark energy equation of state, can develop. Fortunately, data that measure and correct for this effect using our local specific star formation rate indicator, are likely to be available for many next-generation SN Ia cosmology experiments.2020A&A...644A.176Rhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/644/A176CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/644/A176https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/644/A176http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/644/A176https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/644/A176https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/644/A176http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/644/A176GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/644/A176/table1 (Magnitudes for the SNe Ia used in this analysis)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/644/A176/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/644/A176/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/644/A176/table1?GETtext/xml+votable180.050000true263.6979-2.35680.0055555555555555566/143 166 719 740 928 1593 2103 4534 5137 5197 5332 5999 6230 8213 8217 8224 8344 8446 8521 8537 8573 8764 8777 8788 8915 9219 9260 9310 9338 9510 9533 9535 9539 9675 10040 10078 10120 10144 10158 10401 10507 10673 10984 11287 11468 11840 12349 12380 13059 13334 13360 15096 16568 16671 17060 17133 17237 17239 17315 17438 17548 17582 17591 17624 17644 17662 17699 17744 17750 17818 17840 17880 18014 18017 18139 18168 18170 18239 18573 18747 18753 18794 18899 19161 19187 19216 19241 19283 19387 19393-19394 19619 19624 19848 19991-19992 20021 20051 20069 20080 20140 20183 20206 20251 20291 20343 21857 22938 23028 23177 23206 25680 26127 26248 26563 27914 28075 28353 28570 28599 30174 31049 31103 31315 31356 31418 31437 31685 32482 32681 32695 36471 36780 44635 44706 48346 48604 48863 48925https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/644/A176?format=asciiOpticaldefaultJ/A+A/644/A176/table1Magnitudes for the SNe Ia used in this analysisSimbadNameSimbad column added by the CDSmeta.idcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameSN Namemeta.id;meta.maincharRAJ2000SN Right ascension (J2000)degpos.eq.ra;meta.mainDEJ2000SN Declination (J2000)degpos.eq.dec;meta.mainRAHdegHost galaxy Right ascension (J2000)degpos.eq.raDEHdegHost galaxy Declination (J2000)degpos.eq.decgmagLocal g magnitudemagphot.mag;em.opt.IfloatE_gmagError on Local g magnitude (upper value)magstat.error;stat.maxfloate_gmagError on Local g magnitude (lower value)magstat.error;phot.magfloatimagLocal i magnitudemagphot.mag;em.opt.IfloatE_imagError on Local i magnitude (upper value)magstat.error;stat.maxfloate_imagError on Local i magnitude (lower value)magstat.error;phot.magfloatgmagGGlobal g magnitudemagphot.mag;em.opt.IfloatE_gmagGError on Global g magnitude (upper value)magstat.error;stat.maxfloate_gmagGError on Global g magnitude (lower value)magstat.error;phot.magfloatimagGGlobal i magnitudemagphot.mag;em.opt.IfloatE_imagGError on Global i magnitude (upper value)magstat.error;stat.maxfloate_imagGError on Global i magnitude (lower value)magstat.error;phot.magfloatNote[a] Note (1)meta.notecharJ/A+A/644/A176/table2Data for the SNe Ia used in this analysisRefs? References (3)meta.ref;pos.frameintnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameSN Namemeta.id;meta.maincharDBmagcorrCorrected decline rate, {DELTA}m_B_^corr^ (1)magphot.mag;arith.difffloate_DBmagcorrrms uncertainty on DBmagcorrmagstat.errorfloatzCMBHeliocentric redshift (2)src.redshiftfloatn_zCMB[*] * for zCMB derived from our local H{alpha} measurements (2)meta.notecharcSALT2 colourstat.fit.paramfloate_crms uncertainty on cstat.errorfloatx1SALT2 light-curve widthstat.fit.paramfloate_x1rms uncertainty on x1stat.errorfloatlogMLLocal masslog(solMass)phys.massfloatE_logMLError on Local mass (upper value)log(solMass)stat.error;stat.maxfloate_logMLError on Local mass (lower value)log(solMass)stat.errorfloatlogSFRLocal SFRlog(solMass.yr**-1.kpc**-2)phys.SFRfloatE_logSFRError on Local SFR (upper value)log(solMass.yr**-1.kpc**-2)stat.error;stat.maxfloate_logSFRError on Local SFR (lower value)log(solMass.yr**-1.kpc**-2)stat.error;phys.SFRfloatlogsSFRLocal sSFRlog(yr**-1.kpc**-2)phys.SFRfloatE_logsSFRError on Local sSFR (upper value)log(yr**-1.kpc**-2)stat.error;stat.maxfloate_logsSFRError on Local sSFR (lower value)log(yr**-1.kpc**-2)stat.errorfloatlogMGGlobal masslog(solMass)phys.massfloatE_logMGError on Global mass (upper value)log(solMass)stat.error;stat.maxfloate_logMGError on Global mass (lower value)log(solMass)stat.errorfloatPY[0/100] Probability for statistical classification for a SN Ia to be young%statintPM[0/100] Probability for the global stellar mass of the SN host galaxy to be higher than log(M*/M_{sun}_)=10.%statint