J/A+A/658/A29ivo://CDS.VizieR/J/A+A/658/A29doi:10.26093/cds/vizier.36580029CDSRomaniello M.Riess A.S. Mancino S.Anderson R.I.Freudling W.,Kudritzki R.-P.Macri L.Mucciarelli A.Yuan W.2022-11-13T17:04:22Z2022-01-27T07:57:06ZCDS support team

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

cds-question@unistra.frmagellanic-cloudsvariable-starschemical-abundancesvisible-astronomyClassical Cepheids are primary distance indicators and a crucial stepping stone to determining the present-day value of the Hubble constant Ho to the precision and accuracy required to constrain apparent deviations from the LCDM Concordance Cosmological Model. We have measured the iron and oxygen abundances of a statistically significant sample of 89 Cepheids in the LMC, one of the anchors of the local Distance Scale, quadrupling the prior sample and including 68 of the 70 Cepheids used to constrain Ho by the SH0ES program. The goal is to constrain the extent to which the Cepheid luminosity is influenced by their chemical composition, which is an important contributor to the uncertainty on the determination of the Hubble Constant itself and a critical factor in the internal consistency of the distance ladder. We have derived stellar parameters and chemical abundances from a self-consistent spectroscopic analysis based on Equivalent Width of absorption lines. The iron distribution of Cepheids in the LMC can be very accurately described by a single Gaussian with a mean [Fe/H]=-0.409+/-0.003dex and sigma=0.076+/-0.003dex. We estimate a systematic uncertainty on the absolute mean values of 0.1dex. The width of the distribution is fully compatible with the measurement error and supports the low dispersion of 0.069 mag seen in the NIR HST LMC period-luminosity relation. The uniformity of the abundance has the important consequence that the LMC Cepheids alone cannot provide any meaningful constraint on the dependence of the Cepheid Period-Luminosity relation on chemical composition at any wavelength. This revises a prior claim based on a small sample of 22 LMC Cepheids that there was little dependence (or uncertainty) between composition and NIR luminosity, a conclusion which would produce an apparent conflict between anchors of the distance ladder with different mean abundance. The chemical homogeneity of the LMC Cepheid population makes it an ideal environment to calibrate the metallicity dependence between the more metal poor SMC and metal rich Milky Way and NGC 4258.2022A&A...658A..29Rhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/658/A29CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/AcA/65/297 : OGLE4 LMC and SMC Cepheids (Soszynski+, 2015)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/658/A29https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/658/A29http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/658/A29https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/658/A29https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/658/A29http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/658/A29GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/658/A29/table3 (Stellar parameters as derived in the abundance analysis for the SH0ES sample)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/658/A29/table3?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/658/A29/table3?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/658/A29/table3?GETtext/xml+votable180.050000true74.1146533-69.37965890.005555555555555556Cone search capability for table J/A+A/658/A29/table4 (Stellar parameters as re-derived here in the abundance analysis for the archival sample)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/658/A29/table4?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/658/A29/table4?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/658/A29/table4?GETtext/xml+votable180.050000true72.213925-69.35632250.0055555555555555565/8274 6/33054 33076-33078 33095 33101 33103-33104 33106-33108 33110 33112-33113 33120-33122 33124 33126https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/658/A29?format=asciiOpticaldefaultJ/A+A/658/A29/table1Log of the spectroscopic observations of the 68 SH0ES Cepheids (updated version, 24-May-2022, from erratum 2022A&A...662C...1R)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameStar name, OGLENNNN for OGLE-LMC-CEP-XXXXmeta.id;meta.maincharFileNameTimestamp ESO archive file name: UVES.timestampmeta.id;time.epoch;meta.filecharMJD[51828.19/59170.33] Modified Julian date (JD-2400000.5)dtime.epochdoubleJ/A+A/658/A29/table2List of the 189 FeI, 28 FeII and 2 OI lines used as input in the analysisrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambda[4892.85/6400.32] Line wavelength0.1nmem.wl;spect.linedoubleIonIonphys.atmol.ionStagecharlog(gf)[-10.26/0.78] Oscillator strength (1)phys.atmol.oscStrengthfloatEPExcitation Potential (1)eVphys.atmol.excitationfloatJ/A+A/658/A29/table3Stellar parameters as derived in the abundance analysis for the SH0ES samplerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameStar name, OGLENNNN for OGLE-LMC-CEP-XXXX (1)meta.id;meta.maincharSimbadSimbad column added by the CDSmeta.ref.urlcharTeff[4830/6420] effective temperatureKphys.temperature.effectiveinte_Teff[36/322] Uncertainty on effective temperatureKstat.error;phys.temperature.effectiveintloggLog surface gravitylog(cm.s**-2)phys.gravityfloate_logg[0.04/0.26] Uncertainty on log surface gravitylog(cm.s**-2)stat.errorfloatvturb[2.6/4.0] Microturbulent velocitykm/sphys.velocfloate_vturb[0.06/1.04] Uncertainty on microturbulent velocitykm/sstat.errorfloatPhase[0.0/0.99] Pulsational phase at observationtime.phasefloatappenbDisplay the GALA input file for this starmeta.ref.urlchar_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainJ/A+A/658/A29/table4Stellar parameters as re-derived here in the abundance analysis for the archival sampleSimbadSimbad column added by the CDSmeta.ref.urlcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameStar name, OGLENNNN for OGLE-LMC-CEP-XXXX (1)meta.id;meta.maincharTeff[4830/6420] effective temperatureKphys.temperature.effectiveinte_Teff[36/322] Uncertainty on effective temperatureKstat.error;phys.temperature.effectiveintloggLog surface gravitylog(cm.s**-2)phys.gravityfloate_logg[0.04/0.26] Uncertainty on log surface gravitylog(cm.s**-2)stat.errorfloatvturb[2.6/4.0] Microturbulent velocitykm/sphys.velocfloate_vturb[0.06/1.04] Uncertainty on microturbulent velocitykm/sstat.errorfloatPhase[0.0/0.99] Pulsational phase at observationtime.phasefloatappenbDisplay the GALA input file for this starmeta.ref.urlchar_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainJ/A+A/658/A29/table5Stellar iron abundances for the SH0ES sampleo_FeI[52/108] Number of FeI lines usedmeta.numberint[FeII/H][-0.82/-0.13] [FeII/H]=A(FeII)-7.50 (1)phys.abundfloats_[FeII/H][0.02/0.21] Standard deviation [FeII/H]stat.stdev;phys.abundfloate_[FeII/H][-0.02/0.17] Uncertainty [FeII/H] (2)stat.error;phys.abundfloato_FeII[6/18] Number of FeII lines usedmeta.numberintrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameStar name, OGLENNNN for OGLE-LMC-CEP-XXXXmeta.id;meta.mainchar[FeI/H][-0.79/-0.13] [FeI/H]=A(FeI)-7.50 (1)phys.abundfloats_[FeI/H][0.07/0.16] Standard deviation [FeI/H]stat.stdev;phys.abundfloate_[FeI/H][0.03/0.23] Uncertainty [FeI/H] (2)stat.error;phys.abundfloatJ/A+A/658/A29/table6Stellar iron abundances from the re-analysis of the archival samplerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameStar name, OGLENNNN for OGLE-LMC-CEP-XXXXmeta.id;meta.mainchar[FeI/H][-0.79/-0.13] [FeI/H]=A(FeI)-7.50 (1)phys.abundfloats_[FeI/H][0.07/0.16] Standard deviation [FeI/H]stat.stdev;phys.abundfloate_[FeI/H][0.03/0.23] Uncertainty [FeI/H] (2)stat.error;phys.abundfloato_FeI[52/108] Number of FeI lines usedmeta.numberint[FeII/H][-0.82/-0.13] [FeII/H]=A(FeII)-7.50 (1)phys.abundfloats_[FeII/H][0.02/0.21] Standard deviation [FeII/H]stat.stdev;phys.abundfloate_[FeII/H][-0.02/0.17] Uncertainty [FeII/H] (2)stat.error;phys.abundfloato_FeII[6/18] Number of FeII lines usedmeta.numberintJ/A+A/658/A29/table7Stellar oxygen abundances for the SH0ES samplerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameStar name, OGLENNNN for OGLE-LMC-CEP-XXXXmeta.id;meta.mainchar[OI/H][-0.61/0.43]? [OI/H]=A(OI)-8.69 (1)phys.abundfloatnullablee_[OI/H][0.02/0.27]? Uncertainty [OI/H] (2)stat.error;phys.abundfloatnullableo_OI[1/2]? Number of OI lines usedmeta.numberintnullableJ/A+A/658/A29/table8Stellar oxygen abundances from the re-analysis of the archival samplerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameStar name, OGLENNNN for OGLE-LMC-CEP-XXXXmeta.id;meta.mainchar[OI/H][-0.61/0.43]? [OI/H]=A(OI)-8.69 (1)phys.abundfloatnullablee_[OI/H][0.02/0.27]? Uncertainty [OI/H] (2)stat.error;phys.abundfloatnullableo_OI[1/2]? Number of OI lines usedmeta.numberintnullableJ/A+A/658/A29/tablea1Content of the GALA configuration file autofl.paramrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintParamParameter namemeta.id;stat.paramcharValueValue as used in the analysisstat.fit.paramcharDescriptionParameter descriptionmeta.notechar