J/MNRAS/380/1098ivo://CDS.VizieR/J/MNRAS/380/1098doi:10.26093/cds/vizier.73801098CDSHan Z.Podsiadlowski P.Lynas-Gray A.E.2024-07-05T20:15:17Z2007-12-27T13:23:59ZCDS support team

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

cds-question@unistra.frstellar-evolutionary-modelsgalaxiesphotometryultraviolet-astronomyA long-standing problem in the study of elliptical galaxies is the far-ultraviolet (FUV) excess in their spectra (also known as UV-upturn, UV rising-branch, UV rising flux, or UVX). While it is now clear that this UV excess is caused by an old population of hot helium-burning stars without large hydrogen-rich envelopes. We have developed an evolutionary population synthesis (EPS) model for the FUV excess of elliptical galaxies based on the binary model of Han et al. (2002MNRAS.336..449H and 2003MNRAS.341..669H) for the formation of hot subdwarfs in our Galaxy. We give the colour evolution of a simple stellar population (SSP) (including binaries) of 10^10^M_{sun}_ for our standard simulation set. We have also compiled a file for the SED evolution, in which the SEDs without binary interactions are also supplied.2007MNRAS.380.1098Hhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/380/1098CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/380/1098https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/380/1098http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/380/1098https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/380/1098https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/380/1098http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/380/1098GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapUVOpticaldefaultJ/MNRAS/380/1098/table2Colour evolution of a Simple Stellar Population (SSP)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIagePopulation age numbermeta.idintlog(t)Population ageGyrtime.agefloatVMAGAbsolute visual magnitudemagphys.magAbs;em.opt.Vfloat(B-V)B-V colour indexmagphot.color;em.opt.B;em.opt.Vfloat(1550-V)1550-V colour indexmagphot.color;em.UV;em.optfloat(2000-V)2000-V colour indexmagphot.color;em.UV;em.optfloat(2500-V)2500-V colour indexmagphot.color;em.UV;em.optfloat(1500-2500)1500-2500 colour indexmagphot.color;em.UV;em.UVfloat(FUV-r)ABFUV-r colour index in AB systemmagphot.color;em.UV;em.optfloat(NUV-r)ABNUV-r colour index in AB systemmagphot.color;em.UV;em.optfloat(FUV-NUV)ABFUV-NUV colour index in AB systemmagphot.color;em.UV;em.UVfloatbetaFUVFUV spectral indexphot.flux;arith.ratiofloatSEDPlot the spectrum for the agemeta.ref.urlcharJ/MNRAS/380/1098/lambdaThe wavelength corresponding to each wavelength numberrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintJwavWavelength numbermeta.idintlambdaWavelength ({AA})0.1nmem.wldoubleJ/MNRAS/380/1098/sedSED evolution of a Simple Stellar Population (SSP)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIagePopulation age numbermeta.idintJwavWavelength numbermeta.idintFluxbFlux with binary, in erg/s/cm2/{AA} (1)10mW.m**-2.nm**-1phot.fluxdoubleFluxsFlux without binary, in erg/s/cm2/{AA} (2)10mW.m**-2.nm**-1phot.fluxdouble