J/ApJ/720/872ivo://CDS.VizieR/J/ApJ/720/872doi:10.26093/cds/vizier.17200872CDSFossati L.Bagnulo S.Elmasli A.Haswell C.A.Holmes S.Kochukhov O.,Shkolnik E.L.Shulyak D.V.Bohlender D.Albayrak B.Froning C.Hebb L.2012-08-23T07:31:13Z2012-08-23T07:31:05ZCDS support team

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

cds-question@unistra.frchemical-abundancesline-intensitiesmultiple-starssolar-system-planetsThe knowledge of accurate stellar parameters is paramount in several fields of stellar astrophysics, particularly in the study of extrasolar planets, where often the star is the only visible component and therefore used to infer the planet's fundamental parameters. Another important aspect of the analysis of planetary systems is the stellar activity and the possible star-planet interaction. Here, we present a self-consistent abundance analysis of the planet-hosting star WASP-12 and a high-precision search for a structured stellar magnetic field on the basis of spectropolarimetric observations obtained with the ESPaDOnS spectropolarimeter. Our results show that the star does not have a structured magnetic field, and that the obtained fundamental parameters are in good agreement with what was previously published. In addition, we derive improved constraints on the stellar age (1.0-2.65Gyr), mass (1.23-1.49M/M_{sun}_), and distance (295-465pc). WASP-12 is an ideal object in which to look for pollution signatures in the stellar atmosphere. We analyze the WASP-12 abundances as a function of the condensation temperature and compare them with those published by several other authors on planet-hosting and non-planet-hosting stars.2010ApJ...720..872Fhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/720/872CatalogResearchIsServedByTAP VizieR generic servicerelated-toV/136 : Teff and metallicities for Tycho-2 stars (Ammons+, 2006)J/A+A/528/A65 : WASP-12b transits (Maciejewski+, 2011)J/MNRAS/411/L46 : Exoplanet magnetic fields (Vidotto+, 2011)J/MNRAS/414/108 : Calibrator of exoplanet-host stars (Beust+, 2011)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/720/872https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/720/872http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/720/872https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/720/872https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/720/872http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/720/872GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/ApJ/720/872/table1Lines used for the abundance analysisIonIon identificationphys.atmol.ionStagecharf_EW[S] S: abundance was measured with synthetic spectrameta.codecharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambdaWavelength in Angstroms0.1nmem.wldoublef_lambda[#*] multiplet or hyoerfine structure (1)meta.codecharExPotExcitation potentialeVphys.atmol.excitationfloatlog(gf)Log of the oscillator strengthphys.abundfloatr_log(gf)Reference code for log(gf) (see refs.dat file)meta.ref;pos.framecharEW? Equivalent width in milli-Angstroms1e-13mspect.line.eqWidthfloatnullablel_log(A)Limit flag on log(Abd)meta.code.errorcharlog(A)Log of the number abundancephys.abundfloatJ/ApJ/720/872/refsReferencesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRefReference codemeta.notecharBibCodeBibcodemeta.bib.bibcodecharAutAuthor's name(s)meta.bib.authorcharCommCommentmeta.notechar