J/A+A/658/A148ivo://CDS.VizieR/J/A+A/658/A148doi:10.26093/cds/vizier.36580148CDSAnderson R.I.2022-05-18T12:56:15Z2022-02-12T15:58:26ZCDS support team

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

cds-question@unistra.frastronomical-modelsphotometryRelativistic corrections are estimated for classical Cepheids and the Tip of the Red Giant Branch (TRGB stars), to enable future unbiased 1% measurements of Hubble's constant, H0. We considered four effects: K corrections, time-dilation, the apparent change of host dust extinction due to non-comoving reference frames, and the change of observed color due to redshift. Extinction-dependent K corrections were computed using stellar atmosphere models applicable to giant stars for 0.005<z<0.030 in HST, JWST, and 2MASS filters. The optical-NIR Wesenheit function advantageously combines filters with oppositely signed K-corrections and avoids complications due to host extinction. For TRGB stars, the JWST/NIRCAM F277W filter combines insensitivity to reddening with K corrections <1% at Coma cluster distances. Missing corrections for host extinction due to circumgalactic or circumstellar material are discussed as potential systematics for TRGB distances although their impacts are insufficient to explain differences between H0 based on Cepheid or TRGB supernova calibrations. All stellar standard candles require relativistic corrections to achieve an unbiased 1% H0 measurement in the future. The combined relativistic correction involving K, redshift-Leavitt bias, and the redshift-dependence of the Wesenheit function yield an increase of the Cepheid-based H0 by 0.45+/-0.05km/s/Mpc to 73.65+/-1.30km/s/Mpc and raises the tension with the Planck value from 4.2 to 4.4 sigma. For TRGB stars, we estimate a ~0.5% increase of H0 reported by Freedman et al. (to 70.2+/-1.7km/s/Mpc) and a small decrease by -0.15% for H0 reported by Anand et al. (to 71.4+/-1.8km/s/Mpc). The opposite sign of these corrections is due to different reddening systematics and reduces the difference between the studies by ~0.46km/s/Mpc. The optical-NIR Wesenheit function is particularly attractive for accurate distance measurements because it advantageously combines measurements in filters where K-corrections have opposite signs. The JWST/NIRCAM F277W filter is of particular interest for TRGB stars thanks to its insensitivity to (weak) host reddening and K-corrections below the level of 1% at Coma cluster distances.2022A&A...658A.148Ahttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/658/A148CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/658/A148https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/658/A148http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/658/A148https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/658/A148https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/658/A148http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/658/A148GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/658/A148/tablea1*K-corrections as a function of stellar parameters, redshift, and reddeningTeff[3500/6000] effective temperature TeffKphys.temperature.effectiveintrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlogg[0.0/2.0] surface gravity log(g)log(cm.s**-2)phys.gravityfloat[Fe/H][-2.0/0.5] Iron abundance [Fe/H] relative to Solarlog(Sun)phys.abund.Fefloatz[0.0/0.03] Redshift zsrc.redshiftfloatE(B-V)[0.0/0.5] Host color excess E(B-V)magphot.color.excessfloatF555WK[-0.21/1.61] Extinction-dependent K-correction in HST WFC3/F555Wmagarith.factor;phot.magfloatF555WA[0.0/1.61] Extinction correction based on apparent color excess in HST WFC3/F555Wmagarith.factor;phot.magfloatF814WK[-0.16/0.92] Extinction-dependent K-correction in HST WFC3/F814Wmagarith.factor;phot.magfloatF814WA[0.0/0.911] Extinction correction based on apparent color excess in HST WFC3/F814Wmagarith.factor;phot.magfloatF160WK[-0.11/0.32] Extinction-dependent K-correction in HST WFC3/F160Wmagarith.factor;phot.magfloatF160WA[0.0/0.312] Extinction correction based on apparent color excess in HST WFC3/F160Wmagarith.factor;phot.magfloatJmagK[-0.07/0.45] Extinction-dependent K-correction in 2MASS J-bandmagarith.factor;phot.magfloatJmagA[0.0/0.436] Extinction correction based on apparent color excess in 2MASS J-bandmagarith.factor;phot.magfloatKsmagK[-0.05/0.22] Extinction-dependent K-correction in 2MASS Ks-bandmagarith.factor;phot.magfloatKsmagA[0.0/0.179] Extinction correction based on apparent color excess in 2MASS Ks-bandmagarith.factor;phot.magfloatF115WK[-0.07/0.51] Extinction-dependent K-correction in JWST NIRCAM/F115Wmagarith.factor;phot.magfloatF115WA[0.0/0.497] Extinction correction based on apparent color excess in JWST NIRCAM/F115Wmagarith.factor;phot.magfloatF150WK[-0.09/0.34] Extinction-dependent K-correction in JWST NIRCAM/F150Wmagarith.factor;phot.magfloatF150WA[0.0/0.329] Extinction correction based on apparent color excess in JWST NIRCAM/F150Wmagarith.factor;phot.magfloatF200WK[0.0/0.240] Extinction-dependent K-correction in JWST NIRCAM/F200Wmagarith.factor;phot.magfloatF200WA[0.0/0.214] Extinction correction based on apparent color excess in JWST NIRCAM/F200Wmagarith.factor;phot.magfloatF277WK[-0.01/0.26] Extinction-dependent K-correction in JWST NIRCAM/F277Wmagarith.factor;phot.magfloatF277WA[0.0/0.180] Extinction correction based on apparent color excess in JWST NIRCAM/F277Wmagarith.factor;phot.magfloatJ/A+A/658/A148/tablea2*Relativistic corrections for fiducial 10d Cepheids observed using Wesenheit magnitudesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTeff[5400] Effective TemperatureKphys.temperature.effectiveintlogg[1.5] surface gravitylog(cm.s**-2)phys.gravityfloat[Fe/H]Iron abundance relative to Solarlog(Sun)phys.abund.Fefloatz[0.0/0.03] Redshiftsrc.redshiftfloatE(B-V)Host color excessmagphot.color.excessfloatW(HVI)K[2/10] NIR Wesenheit (W_H,VI_) K-correctionmmagarith.factor;phot.magintDmuRLB[7/42] Redshift-Leavitt bias due to time dilationmmagstat.errorintDmuRW[1/4] Reddening slope-Wesenheit biasmmagstat.errorintJ/A+A/658/A148/tablea3*K-corrections for TRGB starsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTeff[3800/4500] Effective temperatureKphys.temperature.effectiveintloggSurface gravitylog(cm.s**-2)phys.gravityfloat[Fe/H][-2.0/-1.5] Iron abundance relative to Solarphys.abund.Fefloatz[0.0/0.03] Redshiftsrc.redshiftfloatE(B-V)Host color excessmagphot.color.excessfloatW(HVI)K[-33/4] NIR Wesenheit (W_H,VI_) K-correctionmmagarith.factor;phot.magintF555WK[-173/140] Extinction-dependent K-correction in HST WFC3/F555Wmmagarith.factor;phot.magintF814WK[-65/86] Extinction-dependent K-correction in HST WFC3/F814Wmmagarith.factor;phot.magintF160WK[-76/26] Extinction-dependent K-correction in HST WFC3/F160Wmmagarith.factor;phot.magintF606WK[-138/126] Extinction-dependent K-correction in HST ACS/F606Wmmagarith.factor;phot.magintF814W2K[-65/86] Extinction-dependent K-correction in HST ACS/F814Wmmagarith.factor;phot.magintJmagK[-55/39] Extinction-dependent K-correction in 2MASS J-bandmmagarith.factor;phot.magintKsmagK[5/49] Extinction-dependent K-correction in 2MASS Ks-bandmmagarith.factor;phot.magintF115WK[-53/45] Extinction-dependent K-correction in JWST NIRCAM/F115Wmmagarith.factor;phot.magintF150WK[-74/28] Extinction-dependent K-correction in JWST NIRCAM/F150Wmmagarith.factor;phot.magintF200WK[4/47] Extinction-dependent K-correction in JWST NIRCAM/F200Wmmagarith.factor;phot.magintF277WK[2/43] Extinction-dependent K-correction in JWST NIRCAM/F277Wmmagarith.factor;phot.magint