J/A+A/658/A80ivo://CDS.VizieR/J/A+A/658/A80doi:10.26093/cds/vizier.36580080CDSTautvaisiene G.Drazdauskas A.Bragaglia A.Martell S.L.Pancino E.,Lardo C.Mikolaitis S.Minkeviciute R.Stonkute E.Ambrosch M.,Bagdonas V.Chorniy Y.Sanna N.Franciosini E.Smiljanic R.Randich S.,Gilmore G.Bensby T.Bergemann M.Gonneau A.Guiglion G.Carraro G.,Heiter U.Korn A.Magrini L.Morbidelli L.Zaggia S.2023-07-20T07:21:02Z2022-02-04T08:13:50ZCDS support team

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

cds-question@unistra.frglobular-star-clusterschemical-abundancesspectroscopyvisible-astronomyNGC 1851 is one of several globular clusters for which multiple stellar populations of the subgiant branch have been clearly identified and a difference in metallicity detected. A crucial piece of information on the formation history of this cluster can be provided by the sum of A(C+N+O) abundances. However, these values have lacked a general consensus thus far. The separation of the subgiant branch can be based on age and/or A(C+N+O) abundance differences. Our main aim was to determine carbon, nitrogen, and oxygen abundances for evolved giants in the globular cluster NGC 1851 in order to check whether or not the double populations of stars are coeval. High-resolution spectra, observed with the FLAMES-UVES spectrograph on the ESO VLT telescope, were analysed using a differential model atmosphere method. Abundances of carbon were derived using spectral synthesis of the C 2 band heads at 5135 and 5635.5{AA}. The wavelength interval 6470-6490{AA}, with CN features, was analysed to determine nitrogen abundances. Oxygen abundances were determined from the [OI] line at 6300{AA}. Abundances of other chemical elements were determined from equivalent widths or spectral syntheses of unblended spectral lines. We provide abundances of up to 29 chemical elements for a sample of 45 giants in NGC 1851. The investigated stars can be separated into two populations with a difference of 0.07dex in the mean metallicity, 0.3dex in the mean C/N, and 0.35 dex in the mean s-process dominated element-to-iron abundance ratios [s/Fe]. No significant difference was determined in the mean values of A(C+N+O) as well as in abundance to iron ratios of carbon, {alpha}- and iron-peak-elements, and of europium. As the averaged A(C+N+O) values between the two populations do not differ, additional evidence is given that NGC 1851 is composed of two clusters, the metal-rich cluster being by about 0.6Gyr older than the metal-poor one. A global overview of NGC 1851 properties and the detailed abundances of chemical elements favour its formation in a dwarf spheroidal galaxy that was accreted by the Milky Way.2022A&A...658A..80Thttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/658/A80CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/MNRAS/442/3044 : Photometry and abundances of NGC1851 stars (Marino+, 2014)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/658/A80https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/658/A80http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/658/A80https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/658/A80https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/658/A80http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/658/A80GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/658/A80/table3 (Main atmospheric parameters and elemental abundances in stars of the globular cluster NGC 1851)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/658/A80/table3?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/658/A80/table3?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/658/A80/table3?GETtext/xml+votable180.050000true78.6033333-40.03963890.0055555555555555566/39517-39518https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/658/A80?format=asciiOpticaldefaultJ/A+A/658/A80/table3Main atmospheric parameters and elemental abundances in stars of the globular cluster NGC 1851SimbadNameSimbad column added by the CDSmeta.idcharnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintCnameCNAME (HHMMSSss+DDMMSSs)meta.id;meta.maincharTeffEffective temperatureKphys.temperature.effectiveinte_TeffError of effective temperatureKstat.error;phys.temperature.effectiveintloggStellar surface gravitylog(cm.s**-2)phys.gravityfloate_loggError of stellar surface gravitylog(cm.s**-2)stat.errorfloat[Fe/H]Metallicityphys.abund.Zfloate_[Fe/H]Error of metallicitystat.error;phys.abund.FefloatvtMicroturbulent velocitykm/sphys.velocfloate_vtError of microturbulent velocitykm/sstat.errorfloat[AlI/H]Abundance [AlI/H]phys.abundfloate_[AlI/H]Error on AlI abundancestat.error;phys.abundfloato_[AlI/H]Number of AlI linesmeta.numberint[BaII/H]Abundance [BaII/H]phys.abundfloate_[BaII/H]Error on BaII abundancestat.error;phys.abundfloato_[BaII/H]Number of BaII linesmeta.numberint[BaII/H]NLTEAbundance [BaII/H]_NLTEphys.abundfloate_[BaII/H]NLTEError on BaII_NLTE abundancestat.error;phys.abundfloato_[BaII/H]NLTENumber of BaII_NLTE linesmeta.numberint[C/H]? Abundance [C/H]phys.abundfloatnullablee_[C/H]? Error on C abundancestat.error;phys.abundfloatnullableo_[C/H]? Number of C linesmeta.numberintnullable[CaI/H]Abundance [CaI/H]phys.abundfloate_[CaI/H]Error on CaI abundancestat.error;phys.abundfloato_[CaI/H]Number of CaI linesmeta.numberint[CaII/H]Abundance [CaII/H]phys.abundfloate_[CaII/H]Error on CaII abundancestat.error;phys.abundfloato_[CaII/H]Number of CaII linesmeta.numberint[CeII/H]Abundance [CeII/H]phys.abundfloate_[CeII/H]Error on CeII abundancestat.error;phys.abundfloato_[CeII/H]Number of CeII linesmeta.numberint[CoI/H]Abundance [CoI/H]phys.abundfloate_[CoI/H]Error on CoI abundancestat.error;phys.abundfloato_[CoI/H]Number of CoI linesmeta.numberint[CrI/H]Abundance [CrI/H]phys.abundfloate_[CrI/H]Error on CrI abundancestat.error;phys.abundfloato_[CrI/H]Number of CrI linesmeta.numberint[CrII/H]Abundance [CrII/H]phys.abundfloate_[CrII/H]Error on CrII abundancestat.error;phys.abundfloato_[CrII/H]Number of CrII linesmeta.numberint[CuI/H]Abundance [CuI/H]phys.abundfloate_[CuI/H]Error on CuI abundancestat.error;phys.abundfloato_[CuI/H]Number of CuI linesmeta.numberint[EuII/H]Abundance [EuII/H]phys.abundfloate_[EuII/H]Error on EuII abundancestat.error;phys.abundfloato_[EuII/H]Number of EuII linesmeta.numberint[LaII/H]? Abundance [LaII/H]phys.abundfloatnullablee_[LaII/H]? Error on LaII abundancestat.error;phys.abundfloatnullableo_[LaII/H]? Number of LaII linesmeta.numberintnullableA(LiI)? A(LiI) abundancephys.abundfloatnullablee_A(LiI)? Error on A(LiI) abundancestat.errorfloatnullableo_A(LiI)? Number of LiI linesmeta.numberintnullableA(LiI)3DNLTE? A(LiI)_3DNLTE abundancephys.abundfloatnullablee_A(LiI)3DNLTE? Error on A(LiI)_3DNLTE abundancestat.errorfloatnullableo_A(LiI)3DNLTE? Number of LiI linesmeta.numberintnullable[MgI/H]Abundance [MgI/H]phys.abundfloate_[MgI/H]Error on MgI abundancestat.error;phys.abundfloato_[MgI/H]Number of MgI linesmeta.numberint[MnI/H]Abundance [MnI/H]phys.abundfloat[N/H]? Abundance [N/H]phys.abundfloatnullablee_[MnI/H]Error on MnI abundancestat.error;phys.abundfloato_[MnI/H]Number of MnI linesmeta.numberint[MoI/H]? Abundance [MoI/H]phys.abundfloatnullablee_[MoI/H]? Error on MoI abundancestat.error;phys.abundfloatnullableo_[MoI/H]? Number of MoI linesmeta.numberintnullablee_[N/H]? Error on N abundancestat.error;phys.abundfloatnullableo_[N/H]? Number of N linesmeta.numberintnullable[NaI/H]Abundance [NaI/H]phys.abundfloate_[NaI/H]Error on NaI abundancestat.error;phys.abundfloato_[NaI/H]Number of NaI linesmeta.numberint[NaI/H]NLTE? Abundance [NaI/H]_NLTEphys.abundfloatnullablee_[NaI/H]NLTE? Error on NaI_NLTE abundancestat.error;phys.abundfloatnullableo_[NaI/H]NLTE? Number of NaI_NLTE linesmeta.numberintnullable[NdII/H]Abundance [NdII/H]phys.abundfloate_[NdII/H]Error on NdII abundancestat.error;phys.abundfloato_[NdII/H]Number of NdII linesmeta.numberint[NiI/H]Abundance [NiI/H]phys.abundfloate_[NiI/H]Error on NiI abundancestat.error;phys.abundfloato_[NiI/H]Number of NiI linesmeta.numberint[OI/H]? Abundance [OI/H]phys.abundfloatnullablee_[OI/H]? Error on OI abundancestat.error;phys.abundfloatnullableo_[OI/H]? Number of OI linesmeta.numberintnullable[PrII/H]? Abundance [PrII/H]phys.abundfloatnullablee_[PrII/H]? Error on PrII abundancestat.error;phys.abundfloatnullableo_[PrII/H]? Number of PrII linesmeta.numberintnullable[ScI/H]Abundance [ScI/H]phys.abundfloate_[ScI/H]Error on ScI abundancestat.error;phys.abundfloato_[ScI/H]Number of ScI linesmeta.numberint[ScII/H]Abundance [ScII/H]phys.abundfloate_[ScII/H]Error on ScII abundancestat.error;phys.abundfloato_[ScII/H]Number of ScII linesmeta.numberint[SiI/H]Abundance [SiI/H]phys.abundfloate_[SiI/H]Error on SiI abundancestat.error;phys.abundfloato_[SiI/H]Number of SiI linesmeta.numberint[SmII/H]? Abundance [SmII/H]phys.abundfloatnullablee_[SmII/H]? Error on SmII abundancestat.error;phys.abundfloatnullableo_[SmII/H]? Number of SmII linesmeta.numberintnullable[TiI/H]Abundance [TiI/H]phys.abundfloate_[TiI/H]Error on TiI abundancestat.error;phys.abundfloato_[TiI/H]Number of TiI linesmeta.numberint[TiII/H]Abundance [TiII/H]phys.abundfloate_[TiII/H]Error on TiII abundancestat.error;phys.abundfloato_[TiII/H]Number of TiII linesmeta.numberint[VI/H]Abundance [VI/H]phys.abundfloate_[VI/H]Error on VI abundancestat.error;phys.abundfloato_[VI/H]Number of VI linesmeta.numberint[YII/H]Abundance [YII/H]phys.abundfloate_[YII/H]Error on YII abundancestat.error;phys.abundfloato_[YII/H]Number of YII linesmeta.numberint[ZnI/H]Abundance [ZnI/H]phys.abundfloate_[ZnI/H]Error on ZnI abundancestat.error;phys.abundfloato_[ZnI/H]Number of ZnI linesmeta.numberint[ZrI/H]? Abundance [ZrI/H]phys.abundfloatnullablee_[ZrI/H]? Error on ZrI abundancestat.error;phys.abundfloatnullableo_[ZrI/H]? Number of ZrI linesmeta.numberintnullableC/N? C/N ratiophys.abundfloatnullable_RAPosition from Cname (right ascension part)degpos.eq.ra;meta.main_DEPosition from Cname (declination part)degpos.eq.dec;meta.main