J/A+A/470/317ivo://CDS.VizieR/J/A+A/470/317doi:10.26093/cds/vizier.34700317CDSRauch T.Ziegler M.Werner K.Kruk J.W.Oliveira C.M.Vande Putte D.,Migniani R.P.Kerber F.2007-10-28T12:15:37Z2007-10-28T13:11:58ZCDS support team

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

cds-question@unistra.frplanetary-nebulaespectroscopyultraviolet-astronomyWe perform a comprehensive spectral analysis of LS V +46 21 in order to compare its photospheric properties to theoretical predictions from stellar evolution theory as well as from diffusion calculations. LS V +46 21 is the DAO-type central star of the planetary nebula Sh 2-216. High-resolution, high-S/N ultraviolet observations obtained with FUSE and STIS aboard the HST as well as the optical spectrum have been analyzed in order to determine the photospheric parameters and the spectroscopic distance. We performed a detailed spectral analysis of the ultraviolet and optical spectrum by means of state-of-the-art NLTE model-atmosphere techniques. From the NIV-NV, OIV-OVI, SiIV-SiV, and FeV-FeVII ionization equilibria, we determined an effective temperature of 95+/-2kK with high precision. The surface gravity is logg=6.9+/-0.2. An unexplained discrepancy appears between the spectroscopic distance d=224^+46^_-58_pc and the parallax distance d=129^+6^_-5_pc of LS V +46 21. For the first time, we have identified Mg IV and Ar VI absorption lines in the spectrum of a hydrogen-rich central star and determined the Mg and Ar abundances as well as the individual abundances of iron-group elements (Cr, Mn, Fe, Co, and Ni). With the realistic treatment of metal opacities up to the iron group in the model-atmosphere calculations, the so-called Balmer-line problem (found in models that neglect metal-line blanketing) vanishes. Spectral analysis by means of NLTE model atmospheres has presently arrived at a high level of sophistication, which is now hampered largely by the lack of reliable atomic data and accurate line-broadening tables. Strong efforts should be made to improve upon this situation.2007A&A...470..317Rhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/470/317CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/470/317https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/470/317http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/470/317https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/470/317https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/470/317http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/470/317GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapUVdefaultJ/A+A/470/317/tablea1Positions of identified lines in the FUSE (Fig. A1) and STIS (Fig. A2) spectra of LS V +46 21, the white dwarf central star of Sh 2-216recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintLineLine identification (ion)meta.id;spect.linecharn_LinePhotospheric (ph) or interstellar (is) originmeta.notecharlambdaObsObserved spectrum is shifted to the stellar rest wavelength, the given wavelength is the NIST wavelength0.1nmem.wl.effectivedoublelambdaLab? Rest wavelength of interstellar lines0.1nmem.wldoublenullable