J/A+A/632/A74ivo://CDS.VizieR/J/A+A/632/A74doi:10.26093/cds/vizier.36320074CDSJohnston C.Aerts C.Pedersen M.G.Bastian N.2020-04-08T12:54:22Z2019-12-03T08:46:29ZCDS support team

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

cds-question@unistra.frgalaxy-clustersgalaxiesphotometryccd-photometryastronomical-modelsExtended main-sequence turn-offs (eMSTO) are a commonly observed property of young clusters. A global theoretical interpretation for the eMSTOs is still lacking, but stellar rotation is considered a necessary ingredient to explain the eMSTO. We aim to assess the importance of core-boundary and envelope mixing in stellar interiors for the interpretation of eMSTOs in terms of one coeval population. We construct isochrone-clouds based on interior mixing profiles of stars with a convective core calibrated from asteroseismology of isolated galactic field stars. We fit these isochrone-clouds to the measured eMSTO to estimate the age and core mass of the stars in the two young clusters NGC 1850 and NGC 884, assuming one coeval population and fixing the metallicity to the one measured from spectroscopy. We assess the correlations between the interior mixing properties of the cluster members and their rotational and pulsational properties. We find that stellar models based on asteroseismically-calibrated interior mixing profiles lead to enhanced core masses of eMSTO stars and can explain a good fraction of the observed eMSTOs of the two considered clusters in terms of one coeval population of stars, with similar ages to those in the literature, given the large uncertainties. The rotational and pulsational properties of the stars in NGC 884 are not sufficiently well known to perform asteroseismic modelling, as it is achieved for field stars from space photometry. The stars in NGC 884 for which we have vsini and a few pulsation frequencies show no correlation between these properties and the core masses of the stars that set the cluster age. Future cluster space asteroseismology may allow to interpret the values of the core masses in terms of the physical processes that cause them, based on the modelling of the interior mixing profiles for the individual member stars with suitable identified modes.2019A&A...632A..74Jhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/632/A74CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/632/A74https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/632/A74http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/632/A74https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/632/A74https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/632/A74http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/632/A74GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/632/A74/z00060icIsochrone-clouds for Z=0.0060recnoRecord number assigned by the VizieR team. 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Correction in the Johnson U filter (bc_U)magphot.mag.bcdoubleBCVBolometric Correction in the Johnson V filter (bc_V)magphot.mag.bcdoublecenterH1Mass fraction of hydrogen left in the core burning region (center_h1)phys.abund.X;obs.fielddoublecenterHe4Mass fraction of helium left in the core burning region (center_he4)phys.abund.Y;obs.fielddoubledeltanuAsymptotic large frequency spacing for p-modes (delta_nu)uHzem.freq;src.vardoublefovOvershooting parameter (fov)stat.paramdoubleHecoreMassHelium core mass (he_core_mass)solMassphys.mass;arith.ratiodoubleHecoreRadsHelium core radius (he_core_radius)solRadphysdoublelogDextlogarithm of the D_ext mixing parameter (logDext)stat.paramdoublelogLlogarithm of the luminosity (log_L)log(solLum)phys.luminositydoublelogRlogarithm of the radius (log_R)log(solRad)phys.size.radiusdoublelogTefflogarithm of the effective temperature (log_Teff)log(K)phys.temperature.effectivedoublelogglogarithm of the surface gravity (log_g)log(cm.s**-2)phys.gravitydoubleLumBLuminosity in the Johnson B filter (lum_band_B)Wphys.luminosity;em.opt.BdoubleLumF170WLuminosity in the Hubble F170W filter (lum_band_F170W)Wphys.luminosity;em.UV.100-200nmdoubleLumF218WLuminosity in the Hubble F218W filter (lum_band_F218W)Wphys.luminosity;em.UV.200-300nmdoubleLumF255WLuminosity in the Hubble F255W filter (lum_band_F255W)Wphys.luminosity;em.UV.200-300nmdoubleLumF300WLuminosity in the Hubble F300W filter (lum_band_F300W)Wphys.luminosity;em.UV.200-300nmdoubleLumF336WLuminosity in the Hubble F336W filter (lum_band_F336W)Wphys.luminosity;em.opt.UdoubleLumF439WLuminosity in the Hubble F439W filter (lum_band_F439W)Wphys.luminosity;em.opt.BdoubleLumF450WLuminosity in the Hubble F450W filter (lum_band_F450W)Wphys.luminosity;em.opt.BdoubleLumF555WLuminosity in the Hubble F555W filter (lum_band_F555W)Wphys.luminosity;em.opt.VdoubleLumF606WLuminosity in the Hubble F606W filter (lum_band_F606W)Wphys.luminosity;em.opt.RdoubleLumF702WLuminosity in the Hubble F702W filter (lum_band_F702W)Wphys.luminosity;em.opt.RdoubleLumF814WLuminosity in the Hubble F814W filter (lum_band_F814W)Wphys.luminosity;em.opt.IdoubleLumF850LPLuminosity in the Hubble F850LP filter (lum_band_F850LP)Wphys.luminosity;em.opt.IdoubleLumHLuminosity in the Johnson H filter (lum_band_H)Wphys.luminosity;em.IR.HdoubleLumILuminosity in the Johnson I filter (lum_band_I)Wphys.luminosity;em.opt.IdoubleLumJLuminosity in the Johnson J filter (lum_band_J)Wphys.luminosity;em.IR.JdoubleLumKLuminosity in the Johnson K filter (lum_band_K)Wphys.luminosity;em.IR.KdoubleLumLLuminosity in the Johnson L filter (lum_band_L)Wphys.luminosity;em.IR.3-4umdoubleLumLpLuminosity in the Johnson L' filter (lum_band_Lprime)Wphys.luminosity;em.IR.3-4umdoubleLumMLuminosity in the Johnson M filter (lum_band_M)Wphys.luminosity;em.IR.4-8umdoubleLumRLuminosity in the Johnson R filter (lum_band_R)Wphys.luminositydoubleLumULuminosity in the Johnson U filter (lum_band_U)Wphys.luminosity;em.opt.UdoubleLumVLuminosity in the Johnson V filter (lum_band_V)Wphys.luminosity;em.opt.VdoubleMassConvCoreMass of the convective core (mass_conv_core)solMassphys.mass;arith.ratiodoublenuMaxFrequency of highest amplitude (nu_max)uHzsrc.var.amplitude;stat.maxdoubleMstarStellar mass (star_mass)solMassphys.massdouble