J/ApJ/808/103ivo://CDS.VizieR/J/ApJ/808/103doi:10.26093/cds/vizier.18080103CDSNavarrete C.Chaname J.Ramirez I.Meza A.Anglada-Escude G.,Shkolnik E.2017-06-30T05:48:13Z2015-12-18T09:20:55ZCDS support team

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

cds-question@unistra.frchemical-abundancesline-intensitiesglobular-star-clustersradial-velocityThe Kapteyn moving group has been postulated as tidal debris from {omega} Centauri. If true, members of the group should show some of the chemical abundance patterns known for stars in the cluster. We present an optical and near-infrared high-resolution, high-signal-to-noise ratio spectroscopic study of 14 stars of the Kapteyn group, plus 10 additional stars (the {omega} Cen group) that, while not listed as members of the Kapteyn group as originally defined, have nevertheless been associated dynamically with {omega} Centauri. Abundances for Na, O, Mg, Al, Ca, and Ba were derived from the optical spectra, while the strength of the chromospheric HeI10830{AA} line is studied as a possible helium abundance indicator. The resulting Na-O and Mg-Al patterns for stars of the combined Kapteyn and {omega} Cen group samples do not resemble those of {omega} Centauri, and are not different from those of field stars of the Galactic halo. The distribution of equivalent widths of the HeI10830{AA} line is consistent with that found among non-active field stars. Therefore, no evidence is found for second-generation stars within our samples, which most likely rules out a globular-cluster origin. Moreover, no hint of the unique barium overabundance at the metal-rich end, well established for {omega} Centauri stars, is seen among stars of the combined samples. Because this specific Ba pattern is present in {omega} Centauri irrespective of stellar generation, this would rule out the possibility that our entire sample might be composed of only first-generation stars from the cluster. Finally, for the stars of the Kapteyn group, the possibility of an origin in the hypothetical parent galaxy of {omega} Centauri is disfavored by the different run of {alpha}-elements with metallicity between our targets and stars from present-day dwarf galaxies.2015ApJ...808..103Nhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/808/103CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toB/pastel : The PASTEL catalogue (Soubiran+, 2010-)III/260 : General Catalogue of Ap and Am stars (Renson+ 2009)I/311 : Hipparcos, the New Reduction (van Leeuwen, 2007)J/A+A/583/A76 : Ome Cen candidates RAVE-selected (Fernandez-Trincado+, 2015)J/MNRAS/437/1609 : NGC 2808 HB stars abundances (Marino+, 2014)J/ApJ/771/67 : Abundances for 97 metal-poor stars. II. (Ishigaki+, 2013)J/A+A/552/A64 : Gaia-RVS standards (Soubiran+, 2013)J/ApJ/764/78 : Oxygen abundances in nearby FGK stars (Ramirez+, 2013)J/A+A/549/A147 : Microlensed Bulge dwarf stars abundances. V. (Bensby+, 2013)J/ApJ/757/164 : Oxygen abundances of dwarf stars (Ramirez+, 2012)J/A+A/534/A136 : Halo red giants from the SEGUE survey (Martell+, 2011)J/A+A/531/A88 : Optical spectra of 12 Miras (Uttenthaler+, 2011)J/ApJ/731/64 : Spectroscopy of 300 RGBs in {omega} Cen (Marino+, 2011)J/ApJ/722/1373 : {omega} Centauri giants abundances (Johnson+, 2010)J/AJ/140/631 : HST WFC3/UVIS photometry of omega Cen core (Bellini+, 2010)J/ApJ/705/328 : Abundance measurements in Sculptor dSph (Kirby+, 2009)J/A+A/505/139 : Abundances of red giants in 17 GCs (Carretta+, 2009)J/A+A/505/117 : Abundances of red giants in 15 GCs (Carretta+, 2009)J/A+A/497/563 : Chemical abundances of 451 stars (Neves+, 2009)J/AJ/135/1580 : Element abundances in 10 Car dSph red giants (Koch+, 2008)J/ApJ/667/911 : Abundances on the MS of {omega} Cen (Stanford+, 2007)J/A+A/465/815 : Abundances of Sgr dSph stars (Sbordone+, 2007)J/A+A/465/271 : Oxygen abundances in nearby stars (Ramirez+, 2007)J/A+A/464/939 : Abundances of red giants in NGC 6218 (Carretta+, 2007)J/MNRAS/367/1329 : Elemental abundances for 176 stars (Reddy+, 2006)J/ApJ/647/1075 : Age-metallicity relation of {omega} Cen (Stanford+, 2006)J/AJ/128/1177 : Galactic stellar abundances (Venn+, 2004)J/A+A/404/187 : Equivalent widths for metal-poor stars (Gratton+, 2003)J/MNRAS/340/304 : [X/Fe] of Galactic disc F and G dwarfs (Reddy+, 2003)J/ApJS/141/503 : Radial Velocities for 889 late-type stars (Nidever+, 2002)J/A+A/390/235 : OI and FeII EWs in metal-poor stars (Nissen+ 2002)J/AJ/119/2866 : Proper motions of metal-poor stars (Beers+, 2000)J/A+AS/141/491 : Chemical composition of halo and disk stars (Nissen+, 2000)J/PASP/107/1042 : Infrared Arcturus Atlas (Hinkle+ 1995)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/808/103https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/808/103http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/808/103https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/808/103https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/808/103http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/808/103GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/ApJ/808/103/abund (Spectroscopic stellar parameters and chemical abundances for our sample stars)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/ApJ/808/103/abund?https://vizier.iucaa.in/viz-bin/conesearch/J/ApJ/808/103/abund?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/ApJ/808/103/abund?GETtext/xml+votable180.050000true44.2511994-30.41039170.0055555555555555566/4376 12451 16513 17136 17245 25051 29011 29703 31094 31503 32889 33018 33508 34559 35813 35907 35989 36365 38216 40337 41460 42496 42873 43310 43575 43786 43962 44208 44542 44816 45353 45837 46053 46098 46171 46302 46923 47017 47347 47512 47596 48736 48744 48824https://cdsarc.cds.unistra.fr/viz-bin/moc/J/ApJ/808/103?format=asciiOpticaldefaultJ/ApJ/808/103/table4List of atomic transitions and equivalent width measurements for our target starsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambda[4491.4/7836.2] Wavelength in Angstroms0.1nmem.wlfloatSp[8/56.1] Species code (1)phys.atmol.ionStagefloatExPot[0/9.2] Excitation potentialeVphys.atmol.excitationfloatlog(gf)[-5/2.3] Log of the oscillator strengthphys.atmol.oscStrengthfloatEW1[5/94]? The CD-30 1121 equivalent width1e-13mspect.line.eqWidthfloatnullableEW2[4/232]? The CD-62 1346 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW3[4/56]? The HD 110621 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW4[4/111]? The HD 111721 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW5[3/44]? The HD 13979 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW6[3/117]? The HD 181007 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW7[1/33]? The HD 181743 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW8[2/99]? The HD 186478 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW9[3/39]? The HD 188031 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW10[3/95]? The HD 193242 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW11[3/85]? The HD 208069 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW12[4/131]? The HD 21022 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW13[2/154]? The HD 215601 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW14[1/20]? The HD 215801 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW15[2/17]? The BD+02 3375 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW16[3/69]? The CD-61 0282 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW17[2/89]? The HD 113083 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW18[4/99]? The HD 121004 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW19[1/19]? The HD 140283 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW20[2/89]? The HD 148816 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW21[2/82]? The HD 193901 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW22[3/68]? The HD 194598 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW23[1/72]? The HD 3567 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW24[1/21]? The HD 84937 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW25[4/63]? The HD 102200 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW26[2/30]? The HD 116064 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW27[3/49]? The HD 128279 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW28[2/127]? The HD 134439 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW29[4/146]? The HD 134440 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW30[8/142]? The HD 142948 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW31[3/122]? The HD 145417 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW32[5/141]? The HD 151559 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW33[2/156]? The HD 17072 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW34[5/125]? The HD 184266 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW35[3/103]? The HD 190287 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW36[3/74]? The HD 199289 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW37[3/82]? The HD 211998 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW38[2/54]? The HD 219617 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW39[6/137]? The HD 221580 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW40[3/156]? The HD 222434 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW41[5/169]? The HD 222925 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW42[2/145]? The HD 23798 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW43[2/57]? The HD 26169 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW44[2/183]? The HD 83212 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableEW45[5/124]? The HD 9051 equivalent width (2)1e-13mspect.line.eqWidthfloatnullableJ/ApJ/808/103/abundSpectroscopic stellar parameters and chemical abundances for our sample starsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGroupStar group (G1)meta.id.parentcharNameStar namemeta.id;meta.maincharf_Name[a] a: Reference star (see section 3 and table 3)meta.codecharHRV[-398/311] Heliocentric velocitykm/sspect.dopplerVeloc;pos.heliocentricfloate_HRV[0.3/0.5] HRV uncertaintykm/sstat.errorfloatTeff[4396/6288] Effective temperatureKphys.temperature.effectiveinte_Teff[43/195]? Teff uncertaintyKstat.error;phys.temperature.effectiveintnullablelogg[0.6/4.6] Log of surface gravitylog(cm.s**-2)phys.gravityfloate_logg[0.1/0.3]? logg uncertaintylog(cm.s**-2)stat.errorfloatnullable[Fe/H][-2.5/-0.7] Metallicitylog(Sun)phys.abund.Zfloate_[Fe/H][0.04/0.09]? [Fe/H] uncertaintylog(Sun)stat.error;phys.abund.FefloatnullableEWsDisplay the equivalent widths of this star (from table4)meta.ref.urlcharSimbadSimbad column added by the CDSmeta.ref.urlchar[O/Fe]? Abundance of [O/Fe]phys.abundfloatnullablef_[O/Fe][*] Flag on [O/Fe]meta.codechare_[O/Fe][0.04/0.2]? [O/Fe] uncertaintystat.error;phys.abundfloatnullableo_e_[O/Fe][2/3]? Number of lines used for e_[O/Fe]meta.numberintnullable[Na/Fe][-0.4/0.4]? [Na/Fe] abundancephys.abundfloatnullablee_[Na/Fe][0.05/0.2]? [Na/Fe] uncertaintystat.error;phys.abundfloatnullableo_e_[Na/Fe][1/6]? Number of lines used for e_[O/Fe]meta.numberintnullable[Mg/Fe][0.02/0.6] [Mg/Fe] abundancephys.abundfloate_[Mg/Fe][0.04/0.3]? [Mg/Fe] uncertaintystat.error;phys.abundfloatnullableo_e_[Mg/Fe][1/5]? Number of lines used for e_[O/Fe]meta.numberintnullable[Al/Fe][-0.02/0.4]? [Al/Fe] abundancephys.abundfloatnullablee_[Al/Fe][0.04/0.3]? [Al/Fe] uncertaintystat.error;phys.abundfloatnullableo_e_[Al/Fe][1/5]? Number of lines used for e_[O/Fe]meta.numberintnullable[Ca/Fe][0.1/0.6] [Ca/Fe] abundancephys.abundfloate_[Ca/Fe][0.05/0.2]? [Ca/Fe] uncertaintystat.error;phys.abundfloatnullableo_e_[Ca/Fe][6/15]? Number of lines used for e_[O/Fe]meta.numberintnullable[Ba/Fe][-1/1.6] [Ba/Fe] abundancephys.abundfloate_[Ba/Fe][0.04/0.4]? [Ba/Fe] uncertaintystat.error;phys.abundfloatnullableo_e_[Ba/Fe][2/3]? Number of lines used for e_[O/Fe]meta.numberintnullable_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.main