J/A+A/709/A52ivo://CDS.VizieR/J/A+A/709/A52CDSFeng M.Lei Z.Kou B.Dong Y.Hu K.Xiao H.Zhao J.2026-05-19T14:14:26Z2026-05-01T12:00:36ZCDS support team

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

cds-question@unistra.frsubdwarf-starsstellar-massesstellar-radiiThe formation mechanisms of spectrally diverse hot subdwarfs remain unclear. While existing mass distribution analyses suggest additional channels beyond helium white dwarf (He-WD) mergers contribute to He-rich subdwarf formation, these conclusions are constrained by limited sample sizes of mass-measured He-rich objects. We developed a deep leaning model which combines a convolution neural network (CNN) together with a squeeze-and-excitation (SE) block to calculate synthetic spectral energy distributions (SEDs) for 1012 spectroscopically confirmed hot subdwarfs. Through directly comparison between synthetic SEDs and observed flux density, we derived stellar parameters (mass, radius, luminosity) for unprecedented number size of hot subdwarf stars, enabling more conclusive channel discrimination than prior studies. The mass distribution of sdB/sdOB stars confirmed the results from model predictions of binary populations synthesis (BPS). A primary and secondary peak (i.e., around 0.56 and 0.4 Msun) is obviously presented in the mass distribution of He-rich hot subdwarf stars. By comparing with the results from the predictions of recent BPS model, it proposed that the merger of two He-WDs could produce most of the observed He-rich hot subdwarf stars, but the mass transfer during the stable Roche lobe overflow (RLOF) phase in binary evolution should be partially conserved.2026A&A...709A..52Fhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/709/A52CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/662/A40 : Hot subdwarf stars studied with Gaia (Culpan+, 2022)J/ApJ/953/122 : Masses for hot subdwarf stars in LAMOST & Gaia (Lei+, 2023)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/709/A52https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/709/A52http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/709/A52https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/709/A52https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/709/A52http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/709/A52GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/709/A52/tablea1Main parameters for 1012 selected hot subdwarf starsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameStar designationmeta.id;meta.maincharGaiaDR3Gaia DR3 source identifiermeta.idcharSpClassSpectral classificationspect.indexcharTeffEffective temperatureKphys.temperature.effectiveinte_TeffUncertainty in TeffKstat.error;phys.temperature.effectiveintloggLog of surface gravitylog(cm.s**-2)phys.gravityfloate_loggUncertainty in Logglog(cm.s**-2)stat.errorfloatAVVisual extinctionmagphys.absorptionfloatPlxParallax, Gaia EDR3, after zeropoint correctionmaspos.parallaxfloate_PlxUncertainty in Plxmasstat.error;pos.parallaxfloatAngDiamMedian Angular diameter, log(radians)log(rad)phys.angSize;stat.medianfloatE_AngDiamUpper uncertainty in AngDiam (1)log(rad)stat.error;stat.maxfloate_AngDiamLower uncertainty in AngDiam (1)log(rad)stat.errorfloatRadiusMedian Stellar radiussolRadphys.angSize;srcfloatSimbadSimbad column added by the CDSmeta.ref.urlcharE_RadiusUpper uncertainty in Radius (1)solRadstat.error;stat.maxfloate_RadiusLower uncertainty in Radius (1)solRadstat.error;phys.size.radiusfloatLumMedian Stellar luminositysolLumphys.luminosityfloatE_LumUpper uncertainty in Lum (1)solLumstat.error;stat.maxfloate_LumLower uncertainty in Lum (1)solLumstat.errorfloatMassMedian Stellar masssolMassphys.mass;stat.medianfloatE_MassUpper uncertainty in Mass (1)solMassstat.error;stat.maxfloate_MassLower uncertainty in Mass (1)solMassstat.error;phys.massfloat