J/A+A/564/A84ivo://CDS.VizieR/J/A+A/564/A84doi:10.26093/cds/vizier.35640084CDSLian J.Zhu Q.Kong X.He J.2014-10-04T08:13:54Z2014-04-10T08:38:43ZCDS support team

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

cds-question@unistra.frastronomical-modelscarbon-starsinfrared-photometrySince asymptotic giant branch (AGB) stars are bright and extended infrared objects, most Galactic AGB stars saturate the Wide-field Infrared Survey Explorer (WISE) detectors and therefore the WISE magnitudes that are restored by applying point-spread-function fitting need to be verified. Statistical properties of circumstellar envelopes around AGB stars are discussed on the basis of a WISE AGB catalog verified in this way. We cross-matched an AGB star sample with the WISE All-Sky Source Catalog and the Two Mircon All Sky Survey catalog. Infrared Space Observatory (ISO) spectra of a subsample of WISE AGB stars were also exploited. The dust radiation transfer code DUSTY was used to help predict the magnitudes in the W1 and W2 bands, the two WISE bands most affected by saturation, for calibration purpose, and to provide physical parameters of the AGB sample stars for analysis.2014A&A...564A..84Lhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/564/A84CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/564/A84https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/564/A84http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/564/A84https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/564/A84https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/564/A84http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/564/A84GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tap8.157980699529898e-21 1.7003137259100215e-19InfrareddefaultJ/A+A/564/A84/grid_cModel grid for C-richrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintJ2MASS J-band photometry of model gridmagphot.mag;em.IR.JdoubleH2MASS H-band photometry of model gridmagphot.mag;em.IR.HdoubleK2MASS K-band photometry of model gridmagphot.mag;em.IR.KdoubleW1WISE W1 band photometry of model gridmagphot.mag;arith.diffdoubleW2WISE W2 band photometry of model gridmagphot.mag;arith.diffdoubleW3WISE W3 band photometry of model gridmagphot.mag;arith.diffdoubleW4WISE W4 band photometry of model gridmagphot.mag;arith.diffdoubleTeff[2100/4500] Stellar effective temperatureKphys.temperature.effectivefloatX[1] Ratio between dust composition (1)stat.paramfloatTin[600/1400] Temperature at inner boundaryKphys.temperaturefloattau[0.01/100] Optical depth {tau}phys.absorption.opticalDepthdoubleJ/A+A/564/A84/grid_oModel grid for O-richrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintJ2MASS J-band photometry of model gridmagphot.mag;em.IR.JdoubleH2MASS H-band photometry of model gridmagphot.mag;em.IR.HdoubleK2MASS K-band photometry of model gridmagphot.mag;em.IR.KdoubleW1WISE W1 band photometry of model gridmagphot.mag;arith.diffdoubleW2WISE W2 band photometry of model gridmagphot.mag;arith.diffdoubleW3WISE W3 band photometry of model gridmagphot.mag;arith.diffdoubleW4WISE W4 band photometry of model gridmagphot.mag;arith.diffdoubleTeff[2100/4500] Stellar effective temperatureKphys.temperature.effectivefloatX[1] Ratio between dust composition (1)stat.paramfloatTin[600/1400] Temperature at inner boundaryKphys.temperaturefloattau[0.01/100] Optical depth {tau}phys.absorption.opticalDepthdouble