J/A+A/525/A124ivo://CDS.VizieR/J/A+A/525/A124doi:10.26093/cds/vizier.35250124CDSMonaco L.Saviane I.Correnti M.Bonifacio P.Geisler D.2013-02-13T09:31:13Z2010-12-07T12:55:19ZCDS support team

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

cds-question@unistra.frglobular-star-clustersgiant-starschemical-abundancesline-intensitiesPalomar 1 is a peculiar globular cluster (GC). It is the youngest Galactic GC and it has been tentatively associated to several of the substructures recently discovered in the Milky Way (MW), including the Canis Major (CMa) overdensity and the Galactic Anticenter Stellar Structure (GASS). In order to provide further insights into its origin, we present the first high resolution chemical abundance analysis for one red giant in Pal 1. We obtained high resolution (R=30000) spectra for one red giant star in Pal 1 using the High Dispersion Spectrograph (HDS) mounted at the SUBARU telescope. We used ATLAS-9 model atmospheres coupled with the SYNTHE and WIDTH calculation codes to derive chemical abundances from the measured line equivalent widths of 18 among alpha, Iron-peak, light and heavy elements. The Palomar 1 chemical pattern is broadly compatible to that of the MW open clusters population and similar to disk stars. It is, instead, remarkably different from that of the Sagittarius (Sgr) dwarf spheroidal galaxy. If Pal 1 association with either CMa or GASS will be confirmed, this will imply that these systems had a chemical evolution similar to that of the Galactic disk.2011A&A...525A.124Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/525/A124CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/525/A124https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/525/A124http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/525/A124https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/525/A124https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/525/A124http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/525/A124GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/525/A124/tablea1Adopted line atomic parameters and elemental abundances and equivalent widths measured for Pal1-I and the SunElElementphys.atmol.elementcharn_chi[H] H for HFS (1)meta.notecharepsSun? Abundance (eps=log(X/H)+12) obtained from this line for the Sunphys.abundfloatnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIonIonization degreephys.atmol.ionStagenullablelambdaWavelength of the line ({AA})0.1nmem.wl;spect.linedoubleloggf? Oscillator strength of the linespect.line.intensityfloatnullablen_loggf[H] H for HFS (1)meta.notecharchi? Lower excitation potential of the transitioneVphys.atmol.excitation;stat.minfloatnullableWPal1-ILine equivalent width for Pal1-I0.1pmspect.line.eqWidthfloatepsPal1-IAbundance (eps=log(X/H)+12) obtained from this line for Pal1-Iphys.abundfloatWSun? Line equivalent width for the Sun0.1pmspect.line.eqWidthfloatnullable