J/A+A/347/69ivo://CDS.VizieR/J/A+A/347/69doi:10.26093/cds/vizier.33470069CDSRolleston W.R.J.Hambly N.C.Keenan F.P.Dufton P.L.Saffer R.A.1999-06-28T16:22:07Z1999-06-28T16:21:58ZCDS support team

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

cds-question@unistra.frearly-type-starsline-intensitieschemical-abundancesWe present echelle (R~40,000) spectroscopic observations for a sample of apparently normal, high Galactic latitude, early-type stars drawn from the Palomar-Green Survey. The metal-line spectra show evidence for rotational velocity broadening with values of vsini<=300km/s. In conjunction with Kurucz model atmospheres, we derive stellar photospheric abundances that are consistent with a Population I chemical composition; differential abundances with respect to Galactic disk Population I stars indicate no abundance differences outside the estimated errors. From a comparison of the derived atmospheric parameters with recent theoretical evolutionary models, we derive distance and age estimates for individual stars. Using kinematical considerations, we conclude that all these objects are `runaway' stars, formed in the Galactic disk and subsequently ejected, possibly by supernovae explosions or dynamical interactions.1999A&A...347...69Rhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/347/69CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/347/69https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/347/69http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/347/69https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/347/69https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/347/69http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/347/69GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/347/69/table4Equivalent width for the non-diffuse helium and metal lines (PG 0855+294 to PG 2219+094)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintLineWavelength of spectral line0.1nmem.wlfloatSpeciesIonization stage of elementphys.atmol.ionizationcharEW0855? Equivalent width for PG 0855+294pmspect.line.eqWidthfloatnullableA0855? LTE abundances for PG 0855+294 in 12+log(X/H)phys.abundfloatnullableEW0934? Equivalent width for PG 0934+145pmspect.line.eqWidthfloatnullableA0934? LTE abundances for PG 0934+145 in 12+log(X/H)phys.abundfloatnullableEW0955? Equivalent width for PG 0955+291pmspect.line.eqWidthfloatnullableA0955? LTE abundances for PG 0955+291 in 12+log(X/H)phys.abundfloatnullableEW1205? Equivalent width for PG 1205+228pmspect.line.eqWidthfloatnullableA1205? LTE abundances for PG 1205+228 in 12+log(X/H)phys.abundfloatnullableEW2219? Equivalent width for PG 2219+094pmspect.line.eqWidthfloatnullableA2219? LTE abundances for PG 2219+094 in 12+log(X/H)phys.abundfloatnullableJ/A+A/347/69/table5Equivalent width for the non-diffuse helium and metal lines (PG 2229+099 and PG 2345+241)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintLineWavelength of spectral line0.1nmem.wlfloatSpeciesIonization stage of elementphys.atmol.ionizationcharEW2229? Equivalent width for PG 2229+099pmspect.line.eqWidthfloatnullableA2229? LTE abundances for PG 2229+099 in 12+log(X/H)phys.abundfloatnullableEW2345? Equivalent width for PG 2345+241pmspect.line.eqWidthfloatnullableA2345? LTE abundances for PG 2345+241 in 12+log(X/H)phys.abundfloatnullable