J/ApJ/934/110ivo://CDS.VizieR/J/ApJ/934/110doi:10.26093/cds/vizier.19340110CDSShejeelammal J.Goswami A.2024-11-06T20:26:12Z2024-08-16T08:22:08ZCDS support team

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

cds-question@unistra.frchemical-abundancesvisible-astronomyspectroscopycarbon-starsradial-velocitychemically-peculiar-starsline-intensitiesElemental abundances of extrinsic carbon stars provide insight into the poorly understood origin and evolution of elements in the early Galaxy. In this work, we present the results of a detailed spectroscopic analysis of four potential carbon star candidates from the Hamburg/ESO Survey (HES): HE 0457-1805, HE 0920-0506, HE1241-0337, and HE 1327-2116. This analysis is based on the high-resolution spectra obtained with Mercator/HERMES (R~86000) and SUBARU/HDS (R~50000). Although the abundances of a few elements, such as Fe, C, and O, are available from medium-resolution spectra, we present the first ever detailed high-resolution spectroscopic analysis for these objects. The objects HE 0457-1805 and HE 1241-0337 are found to be CEMP-s stars, HE 0920-0506 a CH star, and HE 1327-2116 a CEMP-r/s star. The object HE 0457-1805 is a confirmed binary, whereas the binary status of the other objects is unknown. The locations of program stars on the diagram of absolute carbon abundance A(C) versus [Fe/H] point at their binary nature. We have examined various elemental abundance ratios of the program stars and confirmed the low- mass nature of their former AGB companions. We have shown that the i-process models could successfully reproduce the observed abundance pattern in HE 1327-2116. The analysis performed for HE 0457-1805, HE0920-0506, and HE 1241-0337 based on the FRUITY parametric models confirmed that the surface chemical compositions of these three objects are influenced by pollution from low-mass AGB companions.2022ApJ...934..110Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/934/110CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toIII/272 : RAVE 4th data release (Kordopatis+, 2013)I/345 : Gaia DR2 (Gaia Collaboration, 2018)J/A+AS/141/371 : Low-mass stars evolutionary tracks (Girardi+, 2000)J/A+A/354/169 : Metal-poor field stars abundances (Gratton+, 2000)J/A+A/375/366 : Carbon stars from the Hamburg/ESO survey (Christlieb+ 2001)J/A+A/416/1117 : Abundances in the early Galaxy (Cayrel+, 2004)J/AJ/128/1177 : Galactic stellar abundances (Venn+, 2004)J/A+A/454/895 : Abundances of 26 barium stars. I. (Allen+, 2006)J/ApJ/652/1585 : Bright metal-poor stars from HES survey (Frebel+, 2006)J/MNRAS/367/1329 : Elemental abundances for 176 stars (Reddy+, 2006)J/ApJ/655/492 : Equivalent widths of 26 metal-poor stars (Aoki+, 2007)J/ApJ/658/1203 : Nitrogen-enhanced metal-poor stars (Johnson+, 2007)J/AJ/133/2464 : Parameters and abundances of nearby giants (Luck+, 2007)J/A+A/490/769 : Yields from extremely metal-poor stars (Campbell+, 2008)J/A+A/484/721 : HES survey. IV. Cand. metal-poor stars (Christlieb+, 2008)J/ApJ/696/797 : Evolution & yields of low-mass AGB stars (Cristallo+, 2009)J/MNRAS/404/1529 : s-process in low-metallicity stars (Bisterzo+, 2010)J/ApJ/724/341 : Nucleosynthesis of massive metal-free stars (Heger+, 2010)J/MNRAS/403/1413 : Updated stellar yields from AGB models (Karakas, 2010)J/A+A/509/A93 : Carbon-enhanced metal-poor stars (Masseron+, 2010)J/AJ/142/188 : Metal-poor stars from HES using CH G-band (Placco+, 2011)J/MNRAS/418/284 : s-process in low-metallicity stars. II. (Bisterzo+, 2011)J/A+A/548/A34 : Carbon-enhanced metal-poor star abundances (Allen+, 2012)J/A+A/546/A90 : NLTE analysis of Sr lines (Bergemann+, 2012)J/ApJ/762/25 : The most metal-poor stars in HES & SDSS. I. (Norris+, 2013)J/MNRAS/440/1095 : Chemical analysis of CH stars (Karinkuzhi+, 2014)J/ApJ/781/40 : Metal-poor stars from HES survey. II. Sp. (Placco+, 2014)J/ApJ/797/21 : Carbon-enhanced metal-poor stars (Placco+, 2014)J/A+A/579/A28 : Abundances of 3 CEMP stars (Bonifacio+, 2015)J/MNRAS/446/2348 : Chemical analysis of CH stars. II. (Karinkuzhi+, 2015)J/MNRAS/459/4299 : Barium stars abundances and kinematics (de Castro+, 2016)J/A+A/586/A158 : Binary properties of CH and CEMP stars (Jorissen+, 2016)J/ApJ/833/20 : Carbon-enhanced metal-poor star abundances (Yoon+, 2016)J/ApJ/835/81 : Bright metal-poor stars from HES Survey. II. (Beers+, 2017)J/AJ/153/21 : Abund. in the local region. II. (Luck+, 2017)J/A+A/621/A108 : Rvel compilation for 45 CEMP-no stars (Arentsen+ 2019)J/A+A/623/A128 : Gal. halo CEMP stars abundances & kinematics (Hansen+, 2019)J/MNRAS/486/3266 : Chemical analysis of CH stars (Purandardas+, 2019)J/A+A/649/A49 : Spectroscopic study of CEMP-(s & r/s) stars (Goswami+, 2021)J/A+A/645/A61 : Abundances of 25 metal-poor stars (Karinkuzhi+, 2021)J/ApJ/907/10 : Samples of VMP HK/HES stars (Limberg+, 2021)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/934/110https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/934/110http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/934/110https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/934/110https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/934/110http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/934/110GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/ApJ/934/110/stars (Basic information (Table 1) and derived atmospheric parameters and radial velocity (Table 2) of the program stars)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/ApJ/934/110/stars?https://vizier.iucaa.in/viz-bin/conesearch/J/ApJ/934/110/stars?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/ApJ/934/110/stars?GETtext/xml+votable180.050000true74.9315-18.01999720.0055555555555555560/https://cdsarc.cds.unistra.fr/viz-bin/moc/J/ApJ/934/110?format=asciiOpticaldefaultJ/ApJ/934/110/starsBasic information (Table 1) and derived atmospheric parameters and radial velocity (Table 2) of the program starsSimbadSimbad column added by the CDSmeta.ref.urlcharTeff[4240/5380]? Effective temperatureKphys.temperature.effectiveintnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameStar namemeta.id;meta.maincharRAJ2000Hour of right ascension (J2000)pos.eq.ra;meta.mainnullableDEJ2000Degree of declination (J2000)pos.eq.dec;meta.mainnullableBmag[11.8/15.9] B magnitudemagphot.mag;em.opt.BfloatnullableVmag[10.9/14.3] V magnitudemagphot.mag;em.opt.VfloatnullableJmag[8.9/11.9] J-band magnitudemagphot.mag;em.IR.JfloatnullableHmag[8.4/11.3] H-band magnitudemagphot.mag;em.IR.HfloatnullableKmag[8.1/11.1] K band magnitudemagphot.mag;em.IR.KfloatnullableSN4200A[8/16] S/N at 4200{AA}stat.snrfloatnullableAb1Equivalent widths of Fe lines used for deriving atmospheric parameters (link to Table 9)meta.ref.urlcharAb2Equivalent widths of lines used for deriving elemental abundances (link to Table 10)meta.ref.urlcharRV[49/180]? Radial velocitykm/sphys.veloc;pos.heliocentricfloatnullableAb3Lines used to derive the elemental abundance from spectral synthesis (link to Table 11)meta.ref.urlcharlogg[0.5/3]? Log of surface gravitylog(cm.s**-2)phys.gravityfloatnullableVt[0.69/3.5]? Microturbulent velocitykm/sphys.velocfloatnullable[FeI/H][-3.5/-0.7] Log of FeI/H abundanceSunphys.abundfloate_[FeI/H][0.06/0.2]? [FeI/H] uncertaintySunstat.error;phys.abundfloatnullable[FeII/H][-2.9/-0.7]? Log of FeII/H abundanceSunphys.abundfloatnullablee_[FeII/H][0.01/0.2]? [FeII/H] uncertaintySunstat.error;phys.abundfloatnullablee_RV[0.02/2.2]? RV uncertaintykm/sstat.errorfloatnullableRVGaia[52.4/178]? Gaia DR2 radial velocityphys.veloc;pos.heliocentricfloatnullableSN5500A[29/56] S/N at 5500{AA}stat.snrfloatnullableSN7700A[49/90]? S/N at 7700{AA}stat.snrfloatnullablee_RVGaia[0.3/1.5]? RVGaia uncertaintystat.errorfloatnullableRVrave[72/178]? RAVE DR4 radial velocityphys.veloc;pos.heliocentricfloatnullablee_RVrave[1.5/2.2]? RVrave uncertaintystat.errorfloatnullableRef[1/4] Reference (1)meta.ref;pos.frameintJ/ApJ/934/110/table9Equivalent widths of Fe lines used for deriving atmospheric parametersrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambda[4132.9/6430.9] Wavelength, Angstroms0.1nmem.wldoubleElElementphys.atmol.elementcharElow[0.087/4.6] Energy, lower leveleVphys.energy;phys.atmol.levelfloatloggf[-4.95/-0.02] Log, statistical weight*oscillator strengthstat.weight;phys.atmol.oscStrengthfloatEW-HE0457[55/145.6]? Equivalent width of line, HE0457-18050.1pmspect.line.eqWidthfloatnullableAb-HE0457[5.3/5.7]? Derived absolute abundance for line, HE 0457-1805phys.abundfloatnullableEW-HE0920[27.4/92]? Equivalent width of line, HE0920-05060.1pmspect.line.eqWidthfloatnullableAb-HE0920[6.6/6.9]? Derived absolute abundance for line, HE 0920-0506phys.abundfloatnullableEW-HE1241[20.5/151]? Equivalent width of line, HE1241-03370.1pmspect.line.eqWidthfloatnullableAb-HE1241[4.8/5.3]? Derived absolute abundance for line, HE 1241-0337phys.abundfloatnullableEW-HE1327[20/83.4]? Equivalent width of line, HE1327-21160.1pmspect.line.eqWidthfloatnullableAb-HE1327[4.5/4.8]? Derived absolute abundance for line, HE 1327-2116phys.abundfloatnullableJ/ApJ/934/110/table10Equivalent widths of lines used for deriving elemental abundancesElElementphys.atmol.elementcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambda[4161.5/6643.7] Wavelength, Angstroms0.1nmem.wldoubleElow[0.0/5.8] Energy, lower leveleVphys.energy;phys.atmol.levelfloatloggf[-3.5/0.6] Log, statistical weight*oscillator strengthstat.weight;phys.atmol.oscStrengthfloatEW-HE0457[21.8/150]? Equivalent width of line, HE0457-18050.1pmspect.line.eqWidthfloatnullableAb-HE0457[1.2/7.1]? Derived absolute abundance for line, HE 0457-1805phys.abundfloatnullableEW-HE0920[12.1/173]? Equivalent width of line, HE0920-05060.1pmspect.line.eqWidthfloatnullableAb-HE0920[1.1/7.6]? Derived absolute abundance for line, HE 0920-0506phys.abundfloatnullableEW-HE1241[9.2/166]? Equivalent width of line, HE1241-03370.1pmspect.line.eqWidthfloatnullableAb-HE1241[-0.6/6]? Derived absolute abundance for line, HE 1241-0337phys.abundfloatnullableEW-HE1327[10/98]? Equivalent width of line, HE1327-21160.1pmspect.line.eqWidthfloatnullableAb-HE1327[-0.24/5.5]? Derived absolute abundance for line, HE 1327-2116phys.abundfloatnullableJ/ApJ/934/110/table11Lines used to derive the elemental abundance from spectral synthesisrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambda[4118.7/7800.3] Wavelength, Angstroms0.1nmem.wldoubleElElementphys.atmol.elementcharElow[0/4.1] Energy, lower leveleVphys.energy;phys.atmol.levelfloatloggf[-2.3/0.7] Log, statistical weight*oscillator strengthstat.weight;phys.atmol.oscStrengthfloatAb-HE0457[-0.2/4.5]? Derived absolute abundance for line, HE 0457-1805phys.abundfloatnullableAb-HE0920[-0.5/4.5]? Derived absolute abundance for line, HE 0920-0506phys.abundfloatnullableAb-HE1241[-1.6/3.6]? Derived absolute abundance for line, HE 1241-0337phys.abundfloatnullableAb-HE1327[-1.2/3.7]? Derived absolute abundance for line, HE 1327-2116phys.abundfloatnullable