J/A+A/690/A120ivo://CDS.VizieR/J/A+A/690/A120doi:10.26093/cds/vizier.36900120CDSDe Brito Silva D.Jofre P.Worley C.Hawkins K.Das P.2025-02-24T20:01:24Z2024-11-27T12:50:20ZCDS support team

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

cds-question@unistra.frmilky-way-galaxychemically-peculiar-starschemical-abundancesvisible-astronomyThe Milky Way is a mosaic of stars from different origins. In particular, metal-poor accreted star candidates offer a unique opportunity to better understand the accretion history of the Milky Way. In this work, we aim to explore the assembly history of the Milky Way by investigating accreted stars in terms of their ages, dynamical properties, and chemical abundances. We also aim to better characterize the impact of incorporating asteroseismic information on age and chemical abundance calculations of metal-poor accreted stars for which TESS data are available. In this study, we conducted an in-depth examination of 30 metal-poor accreted star candidates using TESS and Gaia data as well as MIKE spectra. We find satisfactory agreement between seismic surface gravity (logg) values and values obtained using spectroscopy, demonstrating the reliability of spectroscopic data produced by our methodology. We find that while age determination is highly dependent on the log g and asteroseismic information used, the overall chemical abundance distributions are similar for different logg. However, we find that calcium (Ca) abundances are more sensitive to the adopted logg. Our study reveals that the majority of our stars have properties that are compatible with those reported for the Gaia-Sausage-Enceladus, with a minority of stars that might be associated with Splash. We find an age distribution with a median of 11.3Gyr when including asteroseismic information. Regarding some key chemical signatures, we note that these stars are metal poor ([Fe/H])<-0.8), {alpha} rich ([{alpha}]/Fe]>0.2), and copper poor ([Cu/Fe]<0 ), with chemical abundances typical of accreted stars. These findings illustrate the importance of multidimensional analyses in unraveling the complex accretion history of the Milky Way.2024A&A...690A.120Dhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/690/A120CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toI/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/690/A120https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/690/A120http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/690/A120https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/690/A120https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/690/A120http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/690/A120GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/690/A120/figure8 (Chemical abundances shown in Figure 8 for the stars analyzed in this study)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/690/A120/figure8?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/690/A120/figure8?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/690/A120/figure8?GETtext/xml+votable180.050000true81.9105933-56.78505390.0055555555555555566/32792 32880 32967 32978 32982 33029 33045 33150 33188 33229 33366 33861 33888 33951 36908 37077 37089 37100 37424 37434 37450 37495 37531 37597 37674 37762 38922 38940 39108https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/690/A120?format=asciiOpticaldefaultJ/A+A/690/A120/figure8Chemical abundances shown in Figure 8 for the stars analyzed in this studye_[Al/Fe]Abundance [Al/Fe] errorstat.error;phys.abundfloat[Sc/Fe]Abundance [Sc/Fe]phys.abunddoublee_[Sc/Fe]Abundance [Sc/Fe] errorstat.error;phys.abundfloat[V/Fe]Abundance [V/Fe]phys.abunddoublee_[V/Fe]Abundance [V/Fe] errorstat.error;phys.abundfloat[Cu/Fe]Abundance [Cu/Fe]phys.abunddoublee_[Cu/Fe]Abundance [Cu/Fe] errorstat.error;phys.abundfloat_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainGaiaDR3Gaia DR3 source_idmeta.id;meta.maine_[Mg/Fe]Abundance [Mg/Fe] errorstat.error;phys.abundfloat[Si/Fe]Abundance [Si/Fe]phys.abunddoublee_[Si/Fe]Abundance [Si/Fe] errorstat.error;phys.abundfloat[Ca/Fe]Abundance [Ca/Fe]phys.abundfloate_[Ca/Fe]Abundance [Ca/Fe] errorstat.error;phys.abundfloat[Ti/Fe]Abundance [Ti/Fe]phys.abundfloate_[Ti/Fe]Abundance [Ti/Fe] errorstat.error;phys.abundfloat[Cr/Fe]Abundance [Cr/Fe]phys.abundfloate_[Cr/Fe]Abundance [Cr/Fe] errorstat.error;phys.abundfloat[Mn/Fe]Abundance [Mn/Fe]phys.abunddoublee_[Mn/Fe]Abundance [Mn/Fe] errorstat.error;phys.abundfloat[Co/Fe]Abundance [Co/Fe]phys.abunddoublee_[Co/Fe]Abundance [Co/Fe] errorstat.error;phys.abundfloat[Ni/Fe]Abundance [Ni/Fe]phys.abundfloate_[Ni/Fe]Abundance [Ni/Fe] errorstat.error;phys.abundfloat[Y/Fe]Abundance [Y/Fe]phys.abunddoublee_[Y/Fe]Abundance [Y/Fe] errorstat.error;phys.abundfloat[Ba/Fe]Abundance [Ba/Fe]phys.abundfloate_[Ba/Fe]Abundance [Ba/Fe] errorstat.error;phys.abundfloat[Na/Fe]Abundance [Na/Fe]phys.abunddoublee_[Na/Fe]Abundance [Na/Fe] errorstat.error;phys.abundfloat[Al/Fe]Abundance [Al/Fe]phys.abunddoubleSimbadSimbad column added by the CDSmeta.ref.urlcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIDIdentification numbermeta.idint[Fe/H]Abundance [Fe/H]phys.abund.Fefloate_[Fe/H]Abundance [Fe/H] errorstat.error;phys.abund.Fefloat[Mg/Fe]Abundance [Mg/Fe]phys.abundfloat