J/A+A/575/A51ivo://CDS.VizieR/J/A+A/575/A51doi:10.26093/cds/vizier.35750051CDSLiu C.Ruchti G.Feltzing S.Martinez-Barbosa A.C.Bensby T.,Brown G.A.A.Portegies Zwart F.S.2015-07-19T10:39:37Z2015-02-20T08:36:19ZCDS support team

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

cds-question@unistra.fropen-star-clusterschemical-abundancesspectroscopystellar-agesThe aim of this paper is to find lost siblings of the Sun by analyzing high resolution spectra. Finding solar siblings will enable us to constrain the parameters of the parental cluster and the birth place of the Sun in the Galaxy. The solar siblings can be identified by accurate measurements of metallicity, stellar age and elemental abundances for solar neighbourhood stars. The solar siblings candidates were kinematically selected based on their proper motions, parallaxes and colours. Stellar parameters were determined through a purely spectroscopic approach and partly physical method, respectively. Comparing synthetic with observed spectra, elemental abundances were computed based on the stellar parameters obtained using a partly physical method. A chemical tagging technique was used to identify the solar siblings. We present stellar parameters, stellar ages, and detailed elemental abundances for Na, Mg, Al, Si, Ca, Ti, Cr, Fe, and Ni for 32 solar sibling candidates. Our abundances analysis shows that four stars are chemically homogeneous together with the Sun. Technique of chemical tagging gives us a high probability that they might be from the same open cluster. Only one candidate, HIP 40317, which has solar metallicity and age could be a solar sibling. We performed simulations of the Sun's birth cluster in analytical Galactic model and found that most of the radial velocities of the solar siblings lie in the range -10<=Vr<=10km/s, which is smaller than the radial velocity of HIP 40317 (Vr=34.2km/s), under different Galactic parameters and different initial conditions of the Sun's birth cluster. The sibling status for HIP 40317 is not directly supported by our dynamical analysis.2015A&A...575A..51Lhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/575/A51CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/410/527 : Abundances in the Galactic disk (Bensby+, 2003)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/575/A51https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/575/A51http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/575/A51https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/575/A51https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/575/A51http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/575/A51GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/575/A51/table2Atomic line datarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIonElement and ionization stage (I=neutral)phys.atmol.ionStagecharlambda[4508/8774] Line wavelength {lambda} ({AA})0.1nmem.wl;spect.linedoubleLEP[0/6] Lower excitation potential {chi}eVphys.atmol.excitation;stat.minfloatloggfOscillator strengthphys.atmol.oscStrengthfloatr_loggfReference for loggf (see refs.dat)meta.ref;pos.frameintJ/A+A/575/A51/refsReferences for loggf valuesAutAuthor's namemeta.bib.authorcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRefReference codemeta.noteintBibCodeBibcodemeta.bib.bibcodechar