J/A+A/576/A113ivo://CDS.VizieR/J/A+A/576/A113doi:10.26093/cds/vizier.35760113CDSZenoviene R.Tautvaisiene G.Nordstroem B.Stonkute E.Barisevicius G.2017-06-22T14:29:24Z2015-07-31T08:57:58ZCDS support team

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

cds-question@unistra.frchemical-abundancesA combined study of kinematics and chemical composition of stars is one of the most promising tools of research in Galaxy formation. The main goal in this field of research is to reconstruct the formation history of our Galaxy, to reveal the origin of the thick disc, and to find remnants of ancient mergers. We determine detailed elemental abundances in stars belonging to the so-called Group 1 of the Geneva-Copenhagen survey (GCS) and compare the chemical composition with the Galactic thin- and thick-disc stars, with the GCS Group 2 and Group 3 stars, as well as with several kinematic streams of similar metallicities. The aim is to search for chemical signatures that might give information about the formation history of this kinematic group of stars. High-resolution spectra were obtained with the Fibre-fed Echelle Spectrograph spectrograph at the Nordic Optical Telescope, La Palma, and were analysed with a differential model atmosphere method. Comparison stars were observed and analysed with the same method. The average value of [Fe/H] for the 37 stars of Group 1 is -0.20+/-0.14dex. Investigated Group 1 stars can be separated into three age subgroups. Along with the main 8- and 12-Gyr-old populations, a subgroup of stars younger than 5Gyr can be separated as well. Abundances of oxygen, {alpha}-elements, and r-process dominated elements are higher than in Galactic thin-disc dwarfs. This elemental abundance pattern has similar characteristics to that of the Galactic thick disc and differs slightly from those in Hercules, Arcturus, and AF06 stellar streams. The similar chemical composition of stars in Group 1, as well as in Group 2 and 3, with that in stars of the thick disc might suggest that their formation histories are linked. The chemical composition pattern together with the kinematic properties and ages of stars in the investigated GCS groups provide evidence of their common origin and possible relation to an ancient merging event. A gas-rich satellite merger scenario is proposed as the most likely origin.2015A&A...576A.113Zhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/576/A113CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toV/130 : Geneva-Copenhagen Survey of Solar neighbourhood III (Holmberg+, 2009)J/A+A/530/A138 : Geneva-Copenhagen survey re-analysis (Casagrande+, 2011)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/576/A113https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/576/A113http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/576/A113https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/576/A113https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/576/A113http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/576/A113GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/576/A113/abund (Elemental abundances of programme and comparison stars)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/576/A113/abund?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/576/A113/abund?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/576/A113/abund?GETtext/xml+votable180.050000true10.1367033-23.80487690.0055555555555555566/1786 3200 3386 4423 4920 5062 5160 5929 6231 6308 6436 8275 8450 9323 9476 10019 10598 11691 11773 12056 12337 12621 12899 13140 13620 14380 14459 14559 14726 14882 15000 15049 15590 16679 17578 18688 19424 20149 21748 22263 23794 26521 28129 28148 30576 30943 31037 31220 32064 40722https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/576/A113?format=asciiOpticaldefaultJ/A+A/576/A113/abundElemental abundances of programme and comparison starso_[Ce/Fe]? Number of line for Cemeta.numberintnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGroupGroup (G1)meta.idcharStarStar namemeta.ref;pos.framecharTeffEffective temperatureKphys.temperature.effectiveintloggSurface gravitylog(cm.s**-2)phys.gravityfloatvtMicroturbulent velocitykm/sphys.velocfloat[Fe/H]Metallicitylog(Sun)phys.abund.Zfloats1rms on [FeI/H] {sigma}(FeI)log(Sun)stat.errorfloatn1Number of lines for FeImeta.numberints2rms on [FeII/H] {sigma}(FeII)log(Sun)stat.errorfloatn2Number of lines for FeIImeta.numberint[O/Fe]? [O/Fe] abundancelog(Sun)phys.abundfloatnullable[Na/Fe]? [Na/Fe] abundancelog(Sun)phys.abundfloatnullablee_[Na/Fe]? rms uncertainty on [Na/Fe]log(Sun)stat.error;phys.abundfloatnullableo_[Na/Fe]? Number of lines for Nameta.numberintnullable[Mg/Fe]? [Mg/Fe] abundancelog(Sun)phys.abundfloatnullablee_[Mg/Fe]? rms uncertainty on [Mg/Fe]log(Sun)stat.error;phys.abundfloatnullableo_[Mg/Fe]? Number of lines for Mgmeta.numberintnullable[Al/Fe]? [Al/Fe] abundancelog(Sun)phys.abundfloatnullablee_[Al/Fe]? rms uncertainty on [Al/Fe]log(Sun)stat.error;phys.abundfloatnullableo_[Al/Fe]? Number of line for Almeta.numberintnullable[Si/Fe]? [Si/Fe] abundancelog(Sun)phys.abundfloatnullablee_[Si/Fe]? rms uncertainty on [Si/Fe]log(Sun)stat.error;phys.abundfloatnullableo_[Si/Fe]? Number of line for Simeta.numberintnullable[Ca/Fe]? [Ca/Fe] abundancelog(Sun)phys.abundfloatnullablee_[Ca/Fe]? rms uncertainty on [Ca/Fe]log(Sun)stat.error;phys.abundfloatnullableo_[Ca/Fe]? Number of line for Cameta.numberintnullable[Sc/Fe]? [Sc/Fe] abundancelog(Sun)phys.abundfloatnullablee_[Sc/Fe]? rms uncertainty on [Sc/Fe]log(Sun)stat.error;phys.abundfloatnullableo_[Sc/Fe]? Number of line for Scmeta.numberintnullable[TiI/Fe]? [TiI/Fe] abundancelog(Sun)phys.abundfloatnullablee_[TiI/Fe]? rms uncertainty on [TiI/Fe]log(Sun)stat.error;phys.abundfloatnullableo_[TiI/Fe]? Number of line for TiImeta.numberintnullable[TiII/Fe]? [TiII/Fe] abundancelog(Sun)phys.abundfloatnullablee_[TiII/Fe]? rms uncertainty on [TiII/Fe]log(Sun)stat.error;phys.abundfloatnullableo_[TiII/Fe]? Number of line for TiIImeta.numberintnullable[V/Fe]? [V/Fe] abundancelog(Sun)phys.abundfloatnullablee_[V/Fe]? rms uncertainty on [V/Fe]log(Sun)stat.error;phys.abundfloatnullableo_[V/Fe]? Number of line for Vmeta.numberintnullable[Cr/Fe]? [Cr/Fe] abundancelog(Sun)phys.abundfloatnullablee_[Cr/Fe]? rms uncertainty on [Cr/Fe]log(Sun)stat.error;phys.abundfloatnullableo_[Cr/Fe]? Number of line for Crmeta.numberintnullable[Co/Fe]? [Co/Fe] abundancelog(Sun)phys.abundfloatnullablee_[Co/Fe]? rms uncertainty on [Co/Fe]log(Sun)stat.error;phys.abundfloatnullableo_[Co/Fe]? Number of line for Cometa.numberintnullable[Ni/Fe]? [Ni/Fe] abundancelog(Sun)phys.abundfloatnullablee_[Ni/Fe]? rms uncertainty on [Ni/Fe]log(Sun)stat.error;phys.abundfloatnullableo_[Ni/Fe]? Number of line for Nimeta.numberintnullableSimbadSimbad column added by the CDSmeta.ref.urlchar[Y/Fe]? [Y/Fe] abundancelog(Sun)phys.abundfloatnullablee_[Y/Fe]? rms uncertainty on [Y/Fe]log(Sun)stat.error;phys.abundfloatnullableo_[Y/Fe]? Number of lines for Ymeta.numberintnullable[ZrI/Fe]? [ZrI/Fe] abundancelog(Sun)phys.abundfloatnullablee_[ZrI/Fe]? rms uncertainty on [ZrI/Fe]log(Sun)stat.error;phys.abundfloatnullableo_[ZrI/Fe]? Number of lines for ZrImeta.numberintnullable[ZrII/Fe]? [ZrII/Fe] abundancelog(Sun)phys.abundfloatnullablee_[ZrII/Fe]? rms uncertainty on [ZrII/Fe]log(Sun)stat.error;phys.abundfloatnullableo_[ZrII/Fe]? Number of line for ZrIImeta.numberintnullable[Ba/Fe]? [Ba/Fe] abundancelog(Sun)phys.abundfloatnullable[La/Fe]? [La/Fe] abundancelog(Sun)phys.abundfloatnullablee_[La/Fe]? rms uncertainty on [La/Fe]log(Sun)stat.error;phys.abundfloatnullableo_[La/Fe]? Number of line for Lameta.numberintnullable[Ce/Fe]? [Ce/Fe] abundancelog(Sun)phys.abundfloatnullablee_[Ce/Fe]? rms uncertainty on [Ce/Fe]log(Sun)stat.error;phys.abundfloatnullable[Pr/Fe]? [Pr/Fe] abundancelog(Sun)phys.abundfloatnullablee_[Pr/Fe]? rms uncertainty on [Pr/Fe]log(Sun)stat.error;phys.abundfloatnullableo_[Pr/Fe]? Number of line for Prmeta.numberintnullable[Nd/Fe]? [Nd/Fe] abundancelog(Sun)phys.abundfloatnullablee_[Nd/Fe]? rms uncertainty on [Nd/Fe]log(Sun)stat.error;phys.abundfloatnullableo_[Nd/Fe]? Number of line for Ndmeta.numberintnullable[Sm/Fe]? [Sm/Fe] abundancelog(Sun)phys.abundfloatnullablee_[Sm/Fe]? rms uncertainty on [Sm/Fe]log(Sun)stat.error;phys.abundfloatnullableo_[Sm/Fe]? Number of line for Smmeta.numberintnullable[Eu/Fe]? [Eu/Fe] abundancelog(Sun)phys.abundfloatnullablee_[Eu/Fe]? rms uncertainty on [Eu/Fe]log(Sun)stat.error;phys.abundfloatnullableo_[Eu/Fe]? Number of line for Eumeta.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