J/MNRAS/511/1004ivo://CDS.VizieR/J/MNRAS/511/1004doi:10.26093/cds/vizier.75111004CDSLucchesi R.Lardo C.Jablonka P.Sestito F.Mashonkina L.Arentsen A.,Suter W.Venn K.Martin N.Starkenburg E.Aguado D.Hill V.,Kordopatis G.Navarro J.F.Gonzalez Hernandez J.I.Malhan K.Yuan Z.2025-07-03T20:15:03Z2025-02-17T10:07:10ZCDS support team

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

cds-question@unistra.frmilky-way-galaxychemically-peculiar-starsastrometryphotometryspectroscopyvisible-astronomyextinctionradial-velocityeffective-temperaturechemical-abundancesWe present a one-dimensional, local thermodynamic equilibrium homogeneous analysis of 132 stars observed at high resolution with ESPaDOnS. This represents the largest sample observed at high resolution (R ~ 40000) from the Pristine survey. This sample is based on the first version of the Pristine catalogue and covers the full range of metallicities from [Fe/H] ~ -3 to ~ +0.25, with nearly half of our sample (58 stars) composed of very metal-poor (VMP) stars ([Fe/H] <= -2). This wide range of metallicities provides the opportunity of a new detailed study of the Milky Way stellar population. Because it includes both dwarf and giant stars, it also enables the analysis of any potential bias induced by the Pristine selection process. Based on Gaia EDR3, the orbital analysis of this Pristine-ESPaDOnS sample shows that it is composed of 65 halo stars and 67 disc stars. After a general assessment of the sample chemical properties with the {alpha}-elements Mg and Ca, we focus on the abundance of carbon and the neutron capture elements Ba and Sr. While most of our VMP subsample is carbon normal, we also find that 14 stars out of the 38 stars with [Fe/H] <= -2 and measured carbon abundances turn out to be carbon-enhanced metal-poor (CEMP) stars. We show that these CEMP stars are nearly exclusively (i.e. 12 stars out of 14) in the regime of low luminosity, unevolved, dwarf stars, which we interpret as the consequence of bias of the Pristine filter against C-rich giants. Among the VMP stars, we identify two CEMP stars with no enhancement in neutron-capture process elements and another one enriched in s-process element. Finally, one VMP star is found with a very low [Sr/Fe] abundance ratio for its metallicity, as expected if it had been accreted from an ultra-faint dwarf galaxy.2022MNRAS.511.1004Lhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/511/1004CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/MNRAS/492/3241 : The Pristine survey. IX. (Venn+, 2020)J/ApJ/797/21 : Carbon-enhanced metal-poor stars (Placco+, 2014)J/MNRAS/493/4677 : The Pristine survey XI: the FORS2 sample (Caffau+, 2020)J/MNRAS/487/3797 : A bright star sample observed with SOPHIE (Bonifacio+, 2019)J/MNRAS/490/2241 : Spectroscopy of Pristine EMP star candidates (Aguado+, 2019)J/MNRAS/472/2963 : Metallicities of Pristine stars (Youakim+, 2017)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/511/1004https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/511/1004http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/511/1004https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/511/1004https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/511/1004http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/511/1004GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/511/1004/table1 (Photometric and spectroscopic parameters of our selected Pristine stars sample)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/511/1004/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/511/1004/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/511/1004/table1?GETtext/xml+votable180.050000true134.323217.6970.005555555555555556Cone search capability for table J/MNRAS/511/1004/table2 (Elemental abundances of the 128 stars kept for the chemical analysis)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/511/1004/table2?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/511/1004/table2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/511/1004/table2?GETtext/xml+votable180.050000true134.323217.6970.0055555555555555565/8074 6/4350 8259 8274 8276 8278 8289 8292 8295 8329 8359 8364 8392 8448-8449 8468 8475 8481 8517 8724 8727 8731 8733 8736 8744-8745 8749-8750 8752 8770 26034 26036 26047 26102-26103 26111 26284 26356 26366 26448 26455 26460 26462 26470 26478 26510-26511 26513 26516 26518 26530 26543 26548-26549 26551 26553 26573-26574 26579 26589 26595 26599 27649 27652 27661 27666 27670 27703 27724 27730-27731 27754 27844 27859 27864 27906 27912 27918 27925 27934 27938 27953 27969-27970 31397-31399 31406 31454 31470-31471 31487 31543 31546 31582 31585 31592 31604 31607 31610-31611 31614 31621 31628 31635-31636 31653 31655 31658-31659 31679 31689 31703 31707 31716 32385-32386https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/511/1004?format=asciiOpticaldefaultJ/MNRAS/511/1004/table1Photometric and spectroscopic parameters of our selected Pristine stars samplerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarStar name designation Pr_DDD.dddd+DD.dddd (Star)meta.id;meta.maincharRAJ2000Right ascension (J2000) (RA)degpos.eq.ra;meta.mainDEJ2000Declination (J2000) (Dec)degpos.eq.dec;meta.maing0magSDSS g0 apparent magnitude (g0)magphot.mag;em.opt.Bfloati0magSDSS i0 apparent magnitude (i0)magphot.mag;em.opt.IfloatCaHKDe-reddened Pristine calcium H&K lines magnitude centered around ~3933 {AA} and ~3968 {AA} (CaHK0)magphot.mag;em.optfloatE(B-V)Color excess E (B-V)magphot.color.excessfloatRVRadial velocity corrected (RV)km/sphys.veloc;pos.heliocentricfloato_RVThe number of exposures (o_RV)meta.numberinte_RVMean error of RV ({sigma}RV)km/sstat.errorfloatTeffEffective temperature (Teff)Kphys.temperature.effectiveintloggLogarithm of the surface gravity (logg)log(cm.s**-2)phys.gravityfloatVtMicro-turbulence velocity (vt)km/sphys.veloc.microTurbfloat[Fe/H]Iron to hydrogen abundance ratio ([Fe/H])log(Sun)phys.abund.Fe;arith.ratiofloatn_Star? Note for Pristine stars selection (n_Star) (1)meta.noteintnullableSimbadNameSimbad column added by the CDSmeta.idcharnullableJ/MNRAS/511/1004/table2Elemental abundances of the 128 stars kept for the chemical analysis[Sr/Fe]? Strontium to iron abundance ratio ([Sr/Fe])log(Sun)phys.abund;arith.ratiofloatnullablee_[Sr/Fe]? Mean error {sigma} of [Sr/Fe] ({sigma}[Sr/Fe])log(Sun)stat.error;phys.abundfloatnullableo_[Sr/Fe]? Number of lines used to compute [Sr/Fe] (N[Sr/Fe])meta.numberintnullablel_[Ba/Fe]Upper limit flag of [Ba/Fe]meta.code.error;phys.abundchar[Ba/Fe]? Barium to iron abundance ratio ([Ba/Fe])log(Sun)phys.abundfloatnullablee_[Ba/Fe]? Mean error {sigma} of [Ba/Fe] ({sigma}[Ba/Fe])log(Sun)stat.error;phys.abundfloatnullableo_[Ba/Fe]? Number of lines used to compute [Ba/Fe] (N[Ba/Fe])meta.numberintnullable_RAPosition from table1 (right ascension part)degpos.eq.ra;meta.main_DEPosition from table1 (declination part)degpos.eq.dec;meta.mainrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarStar name designation Pr_DDD.dddd+DD.dddd (Star)meta.id;meta.maincharShortNameShort name from RAdeg values in table1.datmeta.iddouble[Fe/H]Iron to hydrogen abundance ratio ([Fe/H])log(Sun)phys.abund.Fe;arith.ratiofloatlog(FeI)Logarithm Fe I abundance relative to log({epsilon}) of H=12 (logFeI)phys.abundfloate_log(FeI)Mean error {sigma} of log (FeI) ({sigma}logFeI)stat.errorfloato_log(FeI)Number of lines used to compute log (FeI) (NFeI)meta.numberintlog(FeII)? Logarithm Fe II abundance relative to log({epsilon}) of H=12 (logFeII)phys.abund.Fefloatnullablee_log(FeII)? Mean error {sigma} of log (FeII) ({sigma}logFeII)stat.errorfloatnullableo_log(FeII)? Number of lines used to compute log (FeII) (NFeII)meta.numberintnullablel_[C/Fe]Upper limit flag of [C/Fe]meta.code.error;phys.abundchar[C/Fe]? Carbon to iron abundance ratio ([C/Fe])log(Sun)phys.abund;arith.ratiofloatnullablee_[C/Fe]? Mean error {sigma} of [C/Fe] ({sigma}[C/Fe])log(Sun)stat.error;phys.abundfloatnullable[Mg/Fe]? Magnesium to iron abundance ratio ([Mg/Fe])log(Sun)phys.abund;arith.ratiofloatnullablee_[Mg/Fe]? Mean error {sigma} of [Mg/Fe] ({sigma}[Mg/Fe])log(Sun)stat.error;phys.abundfloatnullableo_[Mg/Fe]? Number of lines used to compute [Mg/Fe] (N[Mg/Fe])meta.numberintnullablel_[Ca/Fe]Upper limit flag of [Ca/Fe]meta.code.error;phys.abundchar[Ca/Fe]? Calcium to iron abundance ratio ([Ca/Fe])log(Sun)phys.abund;arith.ratiofloatnullablee_[Ca/Fe]? Mean error {sigma} of [Ca/Fe] ({sigma}[Ca/Fe])log(Sun)stat.error;phys.abundfloatnullableo_[Ca/Fe]? Number of lines used to compute [Ca/Fe] (N[Ca/Fe])meta.numberintnullablel_[Sr/Fe]Upper limit flag of [Sr/Fe]meta.code.error;phys.abundchar