J/ApJ/972/151ivo://CDS.VizieR/J/ApJ/972/151doi:10.26093/cds/vizier.19720151CDSZheng C.Huang Y.Liu J.Lu Y.Han H.Tan Y.Beers T.C.2025-12-15T20:06:11Z2024-12-23T10:58:17ZCDS support team

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

cds-question@unistra.frastronomical-modelsstellar-atmospheresvisible-astronomysloan-photometryinfrared-photometrybroad-band-photometryultraviolet-photometrymultiple-starsThe Doppler beaming effect, induced by the reflex motion of stars, introduces flux modulations and serves as an efficient method to photometrically determine mass functions for a large number of close binary systems, particularly those involving compact objects. In order to convert observed beaming-flux variations into a radial-velocity curve, precise determination of the beaming factor is essential. Previously, this factor was calculated as a constant, assuming a power-law profile for stellar spectra. In this study, we present a novel approach to directly compute this factor. Our new method not only simplifies the computation, especially for blue bands and cool stars, but also enables us to evaluate whether the relationship between beaming flux and radial velocity can be accurately described as linear. We develop a Python code and compute a comprehensive beaming-factor table for commonly used filter systems covering main-sequence, subgiant, and giant stars, as well as hot subdwarf and white dwarf stars. Both the code and our table are archived and publicly available on Zenodo: doi:10.5281/zenodo.13049419.2024ApJ...972..151Zhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/972/151CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/972/151https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/972/151http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/972/151https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/972/151https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/972/151http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/972/151GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapUVOpticalInfrareddefaultJ/ApJ/972/151/atlas9Beaming factors computed with ATLAS 9 (Castelli & Kurucz, 2003IAUS..210P.A20C) synthetic spectrarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTeff[3500/50000] Effective temperatureKphys.temperature.effectiveintloggSurface gravity in [0/5] intervallog(cm.s**-2)phys.gravityfloat[M/H]Metallicity in [-4/0.5] intervalphys.abund.Zfloatalpha[False/True ] False for solar abundance, True for alpha +0.4meta.codecharDYHelium abundance (0 for solar value)spect.indexfloatvturbMicro-turbulence velocitykm/sphys.veloc.microTurbintE(B-V)Stellar extinction E(B-V)magphot.color.excessfloatBFFIT[0.82/36.03] Beaming factors from linear fittingphys.angSizedoublee_BFFITBeaming factor uncertainties from linear fittingstat.errordoubleBFC[0.82/36.04] A reference index (Do not use BFFIT when it deviate from this value too much)meta.codedoubleD1D1 indexspect.indexdoubleD2D2 indexspect.indexfloatD5D5 indexspect.indexfloatBandFilter name (G1)meta.code;instr.filtercharJ/ApJ/972/151/tmapBeaming factors computed with TMAP (Huegelmeyer et al., 2007ASPC..372...87H) synthetic spectrarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTeff[50000/190000] Effective temperatureKphys.temperature.effectiveintlogg[5.0/9.0] Surface gravitylog(cm.s**-2)phys.gravityfloatH[0/1] Hydrogen abundance in percentage by massphys.abund.XfloatHe[0/1] Helium abundance in percentage by massphys.abund.YfloatE(B-V)Stellar extinction E(B-V)magphot.color.excessfloatBFFIT[0.87/1.55] Beaming factors from linear fittingphys.angSizedoublee_BFFITBeaming factor uncertainties from linear fittingstat.errordoubleBFC[0.88/1.55] A reference index (Do not use BFFIT when it deviate from this value too much)meta.codedoubleD1D1 indexspect.indexdoubleD2D2 indexspect.indexdoubleD5D5 indexspect.indexdoubleBandFilter name (G1)meta.code;instr.filtercharJ/ApJ/972/151/phoenixBeaming factors computed with PHOENIX (Husser et al., 2013A&A...553A...6H) synthetic spectrarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTeff[2300/12000] Effective temperatureKphys.temperature.effectiveintlogg[0/6] Surface gravitylog(cm.s**-2)phys.gravityfloatZ[-4.0/1.0] Metallicityphys.abund.ZfloatE(B-V)Stellar extinction E(B-V)magphot.color.excessfloatBFFIT[-4.32/67.84] Beaming factors from linear fitphys.angSizedoublee_BFFITBeaming factor uncertainties from linear fitstat.errordoubleBFC[-4.32/68.64] A reference index (Do not use BFFIT when it deviate from this value too much)meta.codedoubleD1D1 indexspect.indexdoubleD2D2 indexspect.indexdoubleD5D5 indexspect.indexdoublealpha[-0.2/1.2] Alpha elements abundances (0 for sun)phys.abundfloatBandFilter name (G1)meta.code;instr.filtercharJ/ApJ/972/151/tlustyBeaming factors computed with TLUSTY (Lanz & Hubeny, 2003ApJS..146..417L, 2007ApJS..169...83L) synthetic spectrae_BFFITBeaming factor uncertainties from linear fittingstat.errordoubleBFC[1.05/6.98] A reference index (Do not use BFFIT when it deviate from this value too much)meta.codedoubleD1D1 indexspect.indexdoubleD2D2 indexspect.indexdoubleD5D5 indexspect.indexfloatBandFilter name (G1)meta.code;instr.filtercharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTeff[15000/55000] Effective temperatureKphys.temperature.effectiveintlogg[1.75/4.75] Surface gravitylog(cm.s**-2)phys.gravityfloatZ[0/2] Ratio of Z/Zsun (A value 0 refers to metal free)Sunsrc.redshift;arith.ratiofloatE(B-V)Stellar extinction E(B-V)magphot.color.excessfloatBFFIT[1.06/6.98] Beaming factors from linear fittingphys.angSizedouble