J/A+A/503/945ivo://CDS.VizieR/J/A+A/503/945doi:10.26093/cds/vizier.35030945CDSFossati L.Ryabchikova T.Bagnulo S.Alecian E.Grunhut J.,Kochukhov O.Wade G.2009-10-28T19:46:55Z2009-10-28T20:39:19ZCDS support team

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

cds-question@unistra.frearly-type-starsspectroscopyatomic-physicsModern spectroscopy of early-type stars often aims at studying complex physical phenomena such as stellar pulsation, the peculiarity of the composition of the photosphere, chemical stratification, the presence of a magnetic field, and its interplay with the stellar atmosphere and the circumstellar environment. Comparatively less attention is paid to identifying and studying the "normal" A- and B-type stars and testing how the basic atomic parameters and standard spectral analysis allow one to fit the observations. By contrast, this kind of study is paramount for eventually allowing one to correctly quantify the impact of the various physical processes that occur inside the atmospheres of A- and B-type stars. We wish to establish whether the chemical composition of the solar photosphere can be regarded as a reference for early A- and late B-type stars.2009A&A...503..945Fhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/503/945CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/503/945https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/503/945http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/503/945https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/503/945https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/503/945http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/503/945GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/503/945/table9Linelist of the lines used for the abundance analysis of HD 145788, 21 Peg and {pi} CetAbund3? {pi} Cet line abundancephys.abundfloatnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIonElement/Ionphys.atmol.ionStagecharlambdaWavelength0.1nmem.wldoubleEPExcitation potentialeVphys.atmol.excitationfloatlog(gf)log(gf) valuestat.value;arith.zpfloate_log(gf)? Error on the log(gf) valuestat.errorfloatnullableEW1? HD 145788 Line equivalent width0.1pmspect.line.eqWidthfloatnullableAbund1? HD 145788 Line abundancephys.abundfloatnullableu_Abund1Uncertainty flag on Abund1meta.code.errorcharEW2? 21 Peg line equivalent width0.1pmspect.line.eqWidthfloatnullableAbund2? 21 Peg line abundancephys.abundfloatnullableu_Abund2Uncertainty flag on Abund1meta.code.errorcharEW3? {pi} Cet line equivalent width0.1pmspect.line.eqWidthfloatnullableu_Abund3Uncertainty flag on Abund3meta.code.errorcharr_log(gf)Reference for the log(gf) valuemeta.ref;pos.framecharN1[S: ] Note for HD 145788 (1)meta.notecharN2[S] Note for 21 Peg (1)meta.notecharN3[S: ] Note for {pi} Cet (1)meta.notecharJ/A+A/503/945/refsReferencesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRefReference codemeta.notecharBibCodeBibCodemeta.bib.bibcodecharAutAuthor's namemeta.bib.authorcharComCommentsmeta.notechar