J/A+A/690/A246ivo://CDS.VizieR/J/A+A/690/A246doi:10.26093/cds/vizier.36900246CDSTrentin E.Catanzaro G.Ripepi V.Alonso-Santiago J.Molinaro R.,Storm J.De Somma G.Marconi M.Bhardwaj A.Gatto M.Musella I.,Testa V.2025-02-24T20:02:01Z2024-10-11T08:56:20ZCDS support team

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

cds-question@unistra.frvariable-starsphotometryvisible-astronomychemical-abundancesradial-velocityClassical Cepheids (DCEPs) are crucial for calibrating the extragalactic distance ladder, ultimately enabling the determination of the Hubble constant through the period-luminosity (PL) and period-Wesenheit (PW) relations they exhibit. Hence, it's vital to understand how the PL and PW relations depend on metallicity. This is the purpose of the C-MetaLL survey, within which this work is situated. DCEPs are also very important tracers of the young populations placed along the Galactic disc. We aim to enlarge the sample of DCEPs with accurate abundances from high-resolution spectroscopy. In particular, our goal is to extend the range of measured metallicities towards the metal-poor regime to better cover the parameter space. To this end, we observed objects in a wide range of Galactocentric radii, allowing us to study in detail the abundance gradients present in the Galactic disc. We present the results of the analysis of 331 spectra obtained for 180 individual DCEPs with a variety of high-resolution spectrographs. For each target, we derived accurate atmospheric parameters, radial velocities, and abundances for up to 29 different species. The iron abundances range between 0.5 and ~1dex with a rather homogeneous distribution in metallicity. Results. The sample presented in this paper was complemented with that already published in the context of the C-MetaLL survey, resulting in a total of 292 pulsators whose spectra have been analysed in a homogeneous way. These data were used to study the abundance gradients of the Galactic disc in a range of Galactocentric radii (R_GC_) spanning the range 5-20kpc. For most of the elements we found a clear negative gradient, with a slope of ~0.064+/-0.003dex/kpc for [Fe/H] case. Through a qualitative fit with the Galactic spiral arms we shown how our farthest targets (R_GC_>10kpc) trace both the Outer and Outer Scutum-Centaurus arms. The homogeneity of the sample will be of pivotal importance for the study of the metallicity dependance of the DCEP PL relations.2024A&A...690A.246Thttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/690/A246CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/MNRAS/508/4047 : 47 classical Cepheids HARPSN@TNG spectroscopy (Ripepi+ 2021)J/A+A/681/A65 : Cepheids PL relation metallicity dependence (Trentin+, 2024)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/690/A246https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/690/A246http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/690/A246https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/690/A246https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/690/A246http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/690/A246GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/690/A246/table1 (Main properties of the 180 program DCEPs)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/690/A246/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/690/A246/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/690/A246/table1?GETtext/xml+votable180.050000true91.6456076376326.329219834150.0055555555555555565/9482 6/1445 1467 1653 1752 1858 1894 2684 3020 3045 3310 3316 3342 3361 3600 3616 13288 13963 13990 14205 14262 14271 14303 14337 14340 14359 14388 14409 14431 14600 14618 14625 14678 14718 15360 15379 15424 15432 15618 15638 20805 20818 20822 20849 20854 20861-20862 20945 20953 20978 20980 20983 21514 21525 21546 21551 21600 21634-21635 21648 21664 21666 21672 21675 21677 22046-22047 22073 22078 22090 22112 22120 22165 22167 22213 22218 23617 23620 23622-23623 23627 23630 23640 23650 23660 23749 23756 23769 23797 23852 24088 24138 24145 24159 24327 24347 24372 28717 28808 28893 29042 29081 29095 29126 29216 29897 30210-30211 30222 30260 30646 30659 32067 37245 37325 37331 37361 37716 37735 37739 37783 37833 37904 37906 37918 37925 37936 38017 38403 38408 39225 39314 39364 39392 39708 39737 39743 39748-39749 39755 39766 39771 39786 39790 39799 39824 39831 39837 39862 39871 39875 39880 39883 39885 39889 39892 39894 39898 39905 39908 39919 39930 39933 40576 41626 41651 42356 42819-42820 43020 430641.9867573869263685e-19 3.916500758235022e-19https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/690/A246?format=asciiOpticaldefaultJ/A+A/690/A246/table1Main properties of the 180 program DCEPsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarLiterature name of the DCEPmeta.id;meta.maincharGaiaDR3Gaia DR3 identifiermeta.idRA_ICRSRight ascension (ICRS) at Ep=2016.0degpos.eq.ra;meta.mainDE_ICRSDeclination (ICRS) at Ep=2016.0degpos.eq.dec;meta.mainPeriodPeriod of pulsationdtime.perioddoubleModeMode of pulsationmeta.code;src.varchardDistancekpcpos.distancefloatGmagGaia G magnitudemagphot.mag;em.optfloatBPmagGaia BP magnitudemagphot.mag;em.opt.BfloatRPmagGaia RP magnitudemagphot.mag;em.opt.RfloatPlxGaia parallaxmaspos.parallaxfloate_PlxGaia parallax errormasstat.error;pos.parallaxfloate_dDistance errorkpcstat.errorfloatSourceInstrument used to observe the starmeta.id;instrcharNotesOrigin of the periods and modesmeta.notecharSimbadNameSimbad column added by the CDSmeta.idcharnullableJ/A+A/690/A246/table2Log of the observations for the 331 spectra analysed in this workTexpExposure timestime.duration;obs.exposureintSNRSignal-to-noise ratiostat.snrintTeffEffective temperatureKphys.temperature.effectiveinte_TeffEffective temperature errorKstat.error;phys.temperature.effectiveintloggLogarithm of the gravitylog(cm.s**-2)phys.gravityfloate_logglogg errorlog(cm.s**-2)stat.errorfloatxiMicroturbulent velocitykm/sphys.velocfloate_xixi errorkm/sstat.errorfloatVbrBroadening velocitykm/sphys.velocfloate_VbrVbr errorkm/sstat.errorfloatRVHeliocentric radial velocitykm/sspect.dopplerVeloc;pos.heliocentricfloate_RVRV errorkm/sstat.errorfloatSourceInstrument used to observe the starmeta.id;instrcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarName of the starmeta.id;meta.maincharHJDHeliocentric Julian Daydtime.epoch;pos.heliocentricdoublePhasePhasetime.phasecharJ/A+A/690/A246/table3Estimated chemical abundances for the 180 analysed DCEPs[Ba/H]Barium abundancephys.abundfloate_[Ba/H]Barium abundance errorstat.error;phys.abundfloat[La/H]Lanthanum abundancephys.abundfloate_[La/H]Lanthanum abundance errorstat.error;phys.abundfloat[Ce/H]Cerium abundancephys.abundfloate_[Ce/H]Cerium abundance errorstat.error;phys.abundfloat[Pr/H]Praseodymium abundancephys.abundfloate_[Pr/H]Praseodymium abundance errorstat.error;phys.abundfloat[Nd/H]Neodymium abundancephys.abundfloate_[Nd/H]Neodymium abundance errorstat.error;phys.abundfloat[Sm/H]Samarium abundancephys.abundfloate_[Sm/H]Samarium abundance errorstat.error;phys.abundfloat[Eu/H]Europium abundancephys.abundfloate_[Eu/H]Europium abundance errorstat.error;phys.abundfloat[Gd/H]Gadolinium abundancephys.abundfloate_[Gd/H]Gadolinium abundance errorstat.error;phys.abundfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarName of the starmeta.id;meta.mainchar[C/H]Carbon abundancephys.abundfloate_[C/H]Carbon abundance errorstat.error;phys.abundfloat[Fe/H]Iron abundancephys.abundfloat[O/H]Oxygen abundancephys.abundfloate_[O/H]Oxygen abundance errorstat.error;phys.abundfloat[Na/H]Sodium abundancephys.abundfloate_[Na/H]Sodium abundance errorstat.error;phys.abundfloat[Mg/H]Magnesium abundancephys.abundfloate_[Mg/H]Magnesium abundance errorstat.error;phys.abundfloat[Al/H]Alluminium abundancephys.abundfloate_[Al/H]Alluminium abundance errorstat.error;phys.abundfloat[Si/H]Silicon abundancephys.abundfloate_[Si/H]Silicon abundance errorstat.error;phys.abundfloat[S/H]Solfur abundancephys.abundfloate_[S/H]Solfur abundance errorstat.error;phys.abundfloat[Ca/H]Calcium abundancephys.abundfloate_[Ca/H]Calcium abundance errorstat.error;phys.abundfloat[Sc/H]Scandium abundancephys.abundfloate_[Sc/H]Scandium abundance errorstat.error;phys.abundfloat[Ti/H]Titanium abundancephys.abundfloate_[Ti/H]Titanium abundance errorstat.error;phys.abundfloat[V/H]Vanadium abundancephys.abundfloate_[V/H]Vanadium abundance errorstat.error;phys.abundfloat[Cr/H]Chromium abundancephys.abundfloate_[Cr/H]Chromium abundance errorstat.error;phys.abundfloat[Mn/H]Manganese abundancephys.abundfloate_[Ni/H]Nickel abundance errorstat.error;phys.abundfloat[Cu/H]Copper abundancephys.abundfloate_[Cu/H]Copper abundance errorstat.error;phys.abundfloat[Zn/H]Zinc abundancephys.abundfloate_[Zn/H]Zinc abundance errorstat.error;phys.abundfloat[Sr/H]Strontium abundancephys.abundfloate_[Sr/H]Strontium abundance errorstat.error;phys.abundfloat[Y/H]Yttrium abundancephys.abundfloate_[Y/H]Yttrium abundance errorstat.error;phys.abundfloat[Zr/H]Zirconium abundancephys.abundfloate_[Zr/H]Zirconium abundance errorstat.error;phys.abundfloate_[Mn/H]Manganese abundance errorstat.error;phys.abundfloate_[Fe/H]Iron abundance errorstat.error;phys.abund.Fefloat[Co/H]Cobalt abundancephys.abundfloate_[Co/H]Cobalt abundance errorstat.error;phys.abundfloat[Ni/H]Nickel abundancephys.abundfloat