J/AN/338/686ivo://CDS.VizieR/J/AN/338/686doi:10.26093/cds/vizier.113380686CDSCaffau E.Bonifacio P.Starkenburg E.Martin N.Youakim K.Henden A.A.,Gonzalez Hernandez J.I.Aguado D.S.Allende Prieto C.Venn K.,Jablonka P.2025-09-29T20:18:06Z2019-05-03T08:56:20ZCDS support team

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

cds-question@unistra.frchemically-peculiar-starsradial-velocitychemical-abundancesExtremely metal-poor (EMP) stars are old objects formed in the first Gyr of the Universe. They are rare and, to select them the most successful strategy has been to build on large and low-resolution spectroscopic surveys. The combination of narrow- and broad-band photometry provides a powerful and cheaper alternative to select metal-poor stars. The ongoing Pristine Survey is adopting this strategy, conducting photometry with the Canada France Hawaii Telescope MegaCam wide-field imager and a narrow-band filter centered at 395.2nm on the Ca II-H and -K lines. In this paper, we present the results of the spectroscopic follow-up conducted on a sample of 26 stars at the bright end of the magnitude range of the Survey (g<=15), using FEROS at the MPG/ESO 2.2-m telescope (manufactured by Zeiss, Oberkochen, Germany). From our chemical investigation on the sample, we conclude that this magnitude range is too bright to use the Sloan Digital Sky Survey (SDSS) gri bands, which are typically saturated. Instead, the Pristine photometry can be usefully combined with the AAVSO Photometric All Sky Survey (APASS) gri photometry to provide reliable metallicity estimates. Data from FEROS.2017AN....338..686Chttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/AN/338/686CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/AN/338/686https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AN/338/686http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AN/338/686https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/AN/338/686https://vizier.iucaa.in/viz-bin/votable?-source=J/AN/338/686http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/AN/338/686GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/AN/338/686/atmpar (Coordinates, atmospheric parameters and radial velocities (table 2))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/AN/338/686/atmpar?https://vizier.iucaa.in/viz-bin/conesearch/J/AN/338/686/atmpar?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/AN/338/686/atmpar?GETtext/xml+votable180.050000true180.666961713.332397460.0055555555555555566/8243 8257 8259 8410 8449 8736 8769 26499 26554 26588 27844 27853 27861 27867 27970 31471 31582 31585 31595 31607 31688 31716 32299https://cdsarc.cds.unistra.fr/viz-bin/moc/J/AN/338/686?format=asciidefaultJ/AN/338/686/atmparCoordinates, atmospheric parameters and radial velocities (table 2)ComComments (1)meta.noterecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintAbundindicates abundances in abund filemeta.ref.urlcharNameName (Pristine DDD.dddd+DD.dddd)meta.id;meta.maincharprimaryRAJ2000Right Ascension (J2000.0)degpos.eq.ra;meta.mainDEJ2000Declination (J2000.0)degpos.eq.dec;meta.maing0magDereddened SDSS g magnitudemagphot.mag;em.opt.BfloatBRVBarycentric radial velocitieskm/sphys.veloc;pos.barycenterfloatTeff? Effective temperatureKphys.temperature.effectiveintnullablelogg? logarithmic surface gravitylog(cm.s**-2)phys.gravityfloatnullableVturb? microturbulent velocitykm/sphys.velocfloatnullable[Fe/H]? logarithmic iron abundance with respect to the Sunlog(Sun)phys.abund.FefloatnullableSimbadSimbad column added by the CDSmeta.ref.urlcharJ/AN/338/686/abundChemical abundances (tables 3-5)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameStar name (Pristine DDD.dddd+DD.dddd)meta.id;meta.maincharA(NaI)? NaI abundance, log[N(X)/N(H)]+12phys.abundfloatnullablee_A(NaI)? Error on A(NaI)stat.errorfloatnullableA(AlI)? AlI abundance, log[N(X)/N(H)]+12phys.abundfloatnullablee_A(AlI)? Error on A(AlI)stat.errorfloatnullableA(MgI)? MgI abundance, log[N(X)/N(H)]+12phys.abundfloatnullablee_A(MgI)? Error on A(MgI)stat.errorfloatnullableA(SiI)? SiI abundance, log[N(X)/N(H)]+12phys.abundfloatnullablee_A(SiI)? Error on A(SiI)stat.errorfloatnullableA(SiII)? SiII abundance, log[N(X)/N(H)]+12phys.abundfloatnullablee_A(SiII)? Error on A(SiII)stat.errorfloatnullableA(SI)? SI abundance, log[N(X)/N(H)]+12phys.abundfloatnullablee_A(SI)? Error on A(SI)stat.errorfloatnullableA(CaI)? CaI abundance, log[N(X)/N(H)]+12phys.abundfloatnullablee_A(CaI)? Error on A(CaI)stat.errorfloatnullableA(ScII)? ScII abundance, log[N(X)/N(H)]+12phys.abundfloatnullablee_A(ScII)? Error on A(ScII)stat.errorfloatnullableA(TiI)? TiI abundance, log[N(X)/N(H)]+12phys.abundfloatnullablee_A(TiI)? Error on A(TiI)stat.errorfloatnullableA(TiII)? TiII abundance, log[N(X)/N(H)]+12phys.abundfloatnullablee_A(TiII)? Error on A(TiII)stat.errorfloatnullableA(VI)? VI abundance, log[N(X)/N(H)]+12phys.abundfloatnullablee_A(VI)? Error on A(VI)stat.errorfloatnullableA(CrI)? CrI abundance, log[N(X)/N(H)]+12phys.abundfloatnullablee_A(CrI)? Error on A(CrI)stat.errorfloatnullableA(MnI)? MnI abundance, log[N(X)/N(H)]+12phys.abundfloatnullablee_A(MnI)? Error on A(MnI)stat.errorfloatnullableA(FeI)? FeI abundance, log[N(X)/N(H)]+12phys.abundfloatnullablee_A(FeI)? Error on A(FeI)stat.errorfloatnullableA(FeII)? FeII abundance, log[N(X)/N(H)]+12phys.abundfloatnullablee_A(FeII)? Error on A(FeII)stat.errorfloatnullableA(CoI)? CoI abundance, log[N(X)/N(H)]+12phys.abundfloatnullablee_A(CoI)? Error on A(CoI)stat.errorfloatnullableA(NiI)? NiI abundance, log[N(X)/N(H)]+12phys.abundfloatnullablee_A(NiI)? Error on A(NiI)stat.errorfloatnullableA(CuI)? CuI abundance, log[N(X)/N(H)]+12phys.abundfloatnullablee_A(CuI)? Error on A(CuI)stat.errorfloatnullableA(ZnI)? ZnI abundance, log[N(X)/N(H)]+12phys.abundfloatnullablee_A(ZnI)? Error on A(ZnI)stat.errorfloatnullableA(YII)? YII abundance, log[N(X)/N(H)]+12phys.abundfloatnullablee_A(YII)? Error on A(YII)stat.errorfloatnullableA(BaII)? BaII abundance, log[N(X)/N(H)]+12phys.abundfloatnullablee_A(BaII)? Error on A(BaII)stat.errorfloatnullable