J/PASJ/58/389ivo://CDS.VizieR/J/PASJ/58/389doi:10.26093/cds/vizier/bj-1t-c5CDSTakeda Y.Honda S.Aoki W.Takada-hidai M.Zhao G.Chen Y.-Q.,Shi J.-R.2026-03-17T20:04:44Z2007-01-01T17:26:36ZCDS support team

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

cds-question@unistra.frvariable-starschemically-peculiar-starsstellar-atmospheresIn order to study how the conventional spectroscopic method based on the equivalent widths of the Fe I and Fe II lines effectively applies to determining the atmospheric parameters (Teff, logg, v_t_, [Fe/H]) of RR Lyrae variables and how accurately the abundances can be established from such constructed model atmospheres, we analyzed 15 high-dispersion spectrograms of RR Lyr, DX Del, DH Peg, and VY Ser taken at several different phases by using the HDS spectrograph of the Subaru Telescope, and examined the consistency of the resulting phase-to-phase abundances.2006PASJ...58..389Thttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/PASJ/58/389CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/308/481 : Metallic line doubling phenomenon in RR Lyrae (Chadid+, 1996)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/PASJ/58/389https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/PASJ/58/389http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/PASJ/58/389https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/PASJ/58/389https://vizier.iucaa.in/viz-bin/votable?-source=J/PASJ/58/389http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/PASJ/58/389GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/PASJ/58/389/ewidlistFe line data and the measured equivalent widthsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintLineLine number (7000- for Fe I 8000- for Fe II)meta.id;spect.lineintCodeSpecies code (26.00: Fe I, 26.01: Fe II)meta.codefloatLambdaWavelength0.1nmem.wldoubleEpLower excitation potentialeVphys.atmol.excitation;stat.minfloatloggflog gf valuephys.absorption.coefffloatGammarRadiation damping parameterphys.damping;phys.atmolfloatGammasQuadratic Stark effect damping parameterphys.damping;phys.atmolfloatGammawvan der Waals effect damping parameterphys.damping;phys.atmolfloatEW(rrlyr1)?=0.0 Equivalent width for spectrum rrlyr-10.1pmspect.line.eqWidthfloatnullableEW(rrlyr2)?=0.0 Equivalent width for spectrum rrlyr-20.1pmspect.line.eqWidthfloatnullableEW(rrlyr3)?=0.0 Equivalent width for spectrum rrlyr-30.1pmspect.line.eqWidthfloatnullableEW(rrlyr4)?=0.0 Equivalent width for spectrum rrlyr-40.1pmspect.line.eqWidthfloatnullableEW(rrlyr5)?=0.0 Equivalent width for spectrum rrlyr-50.1pmspect.line.eqWidthfloatnullableEW(dxdel1)?=0.0 Equivalent width for spectrum dxdel-10.1pmspect.line.eqWidthfloatnullableEW(dxdel2)?=0.0 Equivalent width for spectrum dxdel-20.1pmspect.line.eqWidthfloatnullableEW(dxdel3)?=0.0 Equivalent width for spectrum dxdel-30.1pmspect.line.eqWidthfloatnullableEW(dhpeg1)?=0.0 Equivalent width for spectrum dhpeg-10.1pmspect.line.eqWidthfloatnullableEW(dhpeg2)?=0.0 Equivalent width for spectrum dhpeg-20.1pmspect.line.eqWidthfloatnullableEW(dhpeg3)?=0.0 Equivalent width for spectrum dhpeg-30.1pmspect.line.eqWidthfloatnullableEW(vyser1)?=0.0 Equivalent width for spectrum vyser-10.1pmspect.line.eqWidthfloatnullableEW(vyser2)?=0.0 Equivalent width for spectrum vyser-20.1pmspect.line.eqWidthfloatnullableEW(vyser3)?=0.0 Equivalent width for spectrum vyser-30.1pmspect.line.eqWidthfloatnullableEW(vyser4)?=0.0 Equivalent width for spectrum vyser-40.1pmspect.line.eqWidthfloatnullable