J/A+A/703/A294ivo://CDS.VizieR/J/A+A/703/A294CDSMoltzer C.A.S.Pols O.R.Van Winckel H.Temmink K.D.Wijdeveld M.W.2026-03-02T06:25:50Z2025-12-01T09:55:29ZCDS support team

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

cds-question@unistra.frmultiple-starsstellar-evolutionary-modelsstandard-starsstellar-mass-lossPost-red giant branch (post-RGB) and post-asymptotic giant branch (post-AGB) binaries consist of a primary star that has recently evolved of either the RGB or AGB after losing the majority of its envelope and a main-sequence companion. They are distinguished by having luminosities below and above the tip of the RGB, respectively. These systems are characterised by the presence of a stable, dusty circumbinary disc, identified by a near-IR excess. Observed Galactic post-AGB and post-RGB binaries have orbital periods and eccentricities that are at odds with binary population synthesis models. In this work, we focus on post-RGB binaries. We investigate whether stable mass transfer can explain the orbital periods of such binaries by comparing stable mass transfer models with the known sample of 38 Galactic post-RGB binaries. We systematically determined the luminosities of the Galactic post-RGB and post-AGB binary sample using spectral energy distribution fitting. We computed evolution models for low- and intermediate-mass binaries with RGB donors at two metallicities using the detailed stellar evolution code, MESA. We selected the stable mass transfer models that result in primaries with effective temperatures within the observed range of post-RGB binaries (4000-8500K). From our model grids, we find that low-mass post-RGB binaries are expected to follow strict luminosity-orbital period relations. The Galactic post-RGB binaries appear consistent with these luminosity-orbital period relations if we assume that their orbits remained eccentric during mass transfer and that the donor star filled its Roche lobe at periastron. However, our models are unable to explain the eccentricities themselves. Furthermore, the post-mass-transfer ages of observed post-RGB binaries estimated using our models are significantly longer than the predicted dissipation timescales of their circumbinary discs. The stable mass transfer formation channel appears to explain the orbital periods of Galactic post-RGB binaries. This formation scenario could be tested more extensively by obtaining the orbits of additional Galactic systems, as well as those of the numerous candidates in the Magellanic Clouds, through long-term radial velocity monitoring. Additionally, we expect that Gaia Data Release 4 will improve the luminosities of Galactic post-RGB binaries, which will allow for a more accurate comparison with post-RGB luminosity-orbital period relations.2025A&A...703A.294Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/703/A294CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/703/A294https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/703/A294http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/703/A294https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/703/A294https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/703/A294http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/703/A294GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/703/A294/tablec2 (SED fitting results of the Galactic post-AGB and post-RGB binary sample)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/703/A294/tablec2?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/703/A294/tablec2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/703/A294/tablec2?GETtext/xml+votable180.050000true101.51862513.0840.005555555555555556Cone search capability for table J/A+A/703/A294/tablec3 (SED fitting results of the post-AGB and post-RGB binary candidate samples in the LMC and SMC)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/703/A294/tablec3?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/703/A294/tablec3?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/703/A294/tablec3?GETtext/xml+votable180.050000true74.4394167-68.62336110.005555555555555556Cone search capability for table J/A+A/703/A294/tablec7 (Estimated orbital periods and post-mass-transfer ages of the post-RGB binary candidate subsamples in the LMC and SMC)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/703/A294/tablec7?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/703/A294/tablec7?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/703/A294/tablec7?GETtext/xml+votable180.050000true74.4394167-68.62336110.0055555555555555565/8263 8273-8274 8280 8323 6/1096 2495 3333 7064 8490 12685 12851 12948 12955 13043 13046 13185 13187 13729 14245 14253 14480 14559 14642 14738 14770 14929-14930 18436 20921 21090 21326 21567 21931 22114 22450 23660 23768 23821 24325 24394 24434 25501 28722 28738 29378 29579 29869 29935 30221 30225 30498 30562 31766 32181 32562 32607 33046 33049-33050 33072-33074 33076-33078 33090-33091 33100-33102 33106 33108 33110 33112 33115 33124-33125 33128 33287 33298 33304 33306 33316-33317 33330 36973 37245 37306 37841 37881 37915 37942 37965 38021 38812 39395 39629 39664 39918 40046 40492 41093 41212 41339 41471 41531 41815 42011 42127 42197 42295 42338 42802 43107 43535 43559 43651 47961https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/703/A294?format=asciidefaultJ/A+A/703/A294/tablec2SED fitting results of the Galactic post-AGB and post-RGB binary samplerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSimbadNameSimbad column added by the CDSmeta.idcharnullableIRASIRAS name of objectmeta.idcharNameAlternative identifications of objectmeta.id;meta.maincharTeffEffective temperature (1)Kphys.temperature.effectiveintDist? Distance (2)pcpos.distanceintnullableb_Dist? 16th percentile of distance (2)pcpos.distanceintnullableB_Dist? 84th percentile of distance (2)pcpos.distanceintnullableE(B-V)? Reddeningmagphot.color.excessfloatnullableb_E(B-V)? Lower limit of reddeningmagphys.absorption;stat.minfloatnullableB_E(B-V)? Upper limit of reddeningmagphys.absorption;stat.maxfloatnullableLumLuminosity (3)solLumphys.luminosityintb_LumLower limit of luminosity (3)solLumphys.luminosity;stat.minintB_LumUpper limit of luminosity (3)solLumphys.luminosity;stat.maxintLIRIR-to-stellar luminosity ratio%phys.luminosity;arith.ratioint_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainJ/A+A/703/A294/tablec3SED fitting results of the post-AGB and post-RGB binary candidate samples in the LMC and SMCrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameIdentification (JHHMMSS.ss+DDMMSS.s or OGLE-LMC-T2CEP-NNN or OGLE-SMC-T2CEP-NNN)meta.id;meta.maincharHost[SMC LMC] Host Magellanic Cloudmeta.id.parentcharTeffEffective temperatureKphys.temperature.effectiveintE(B-V)Reddeningmagphot.color.excessfloatb_E(B-V)Lower limit of reddeningmagphys.absorption;stat.minfloatB_E(B-V)Upper limit of reddeningmagphys.absorption;stat.maxfloatLumLuminositysolLumphys.luminosityintb_LumLower limit of luminositysolLumphys.luminosity;stat.minintB_LumUpper limit of luminositysolLumphys.luminosity;stat.maxintLIRIR-to-stellar luminosity ratio%phys.luminosity;arith.ratiointRef[a-d] Reference to the paper from which the object was taken (1)meta.bibchar_RAPositions from Name and Simbad (right ascension part)degpos.eq.ra;meta.main_DEPositions from Name and Simbad (declination part)degpos.eq.dec;meta.mainJ/A+A/703/A294/tablec4Initial parameters of utilised stable mass transfer models with Z = 0.02recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMiInitial masssolMassphys.massfloatMRLOFMass at the onset of RLOFsolMassphys.massfloatlogRRLOFRadius at the onset of RLOFlog(solRad)phys.size.radiusdoubleqminSmallest mass ratio in the model grid for this primary model to result in stable mass transferphys.mass;meta.modelledfloatJ/A+A/703/A294/tablec5Initial parameters of utilised stable mass transfer models with Z = 0.00142recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMiInitial masssolMassphys.massfloatMRLOFMass at the onset of RLOFsolMassphys.massfloatlogRRLOFRadius at the onset of RLOFlog(solRad)phys.size.radiusdoubleqminSmallest mass ratio in the model grid for this primary model to result in stable mass transferphys.mass;meta.modelledfloatJ/A+A/703/A294/tablec7Estimated orbital periods and post-mass-transfer ages of the post-RGB binary candidate subsamples in the LMC and SMCf_Porbmean[0/1] If true (1), the orbital period is a lower limit as the luminosity of the object is larger than the maximum luminosity of the binary modelsmeta.codeintrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintHost[SMC LMC] Host Magellanic Cloudmeta.id.parentcharPorbmean? Estimated orbital period determined from its luminosity (1)dtime.periodintnullablePorbmin? Estimated orbital period determined from the lower limit of its luminosity (1)dtime.periodintnullablePorbmax? Estimated orbital period determined from the upper limit of its luminosity (1)dtime.periodintnullablef_Porbmax[0/1] If true (1), the maximum orbital period is a lower limit as the luminosity upper limit of the object is larger than the maximum luminosity of the binary modelsmeta.codeintAgemeansolEstimated post-mass-transfer age determined from its position in the HRD compared to the solar model gridyrtime.ageintf_Agemeansol[0/1] If true (1), the mean post-mass-transfer age is an upper limit, as the luminosity of the object is larger than the maximum luminosity of the solar model gridmeta.codeintAgeminsolEstimated minimum post-mass-transfer age determined from its position in the HRD compared to the solar model gridyrtime.age;stat.minintf_Ageminsol[0/1] If true (1), the minimum post-mass-transfer age is an upper limit, as the luminosity lower limit of the object is larger than the maximum luminosity of the solar model gridmeta.codeintAgemaxsolEstimated maximum post-mass-transfer age determined from its position in the HRD compared to the solar model gridyrtime.age;stat.maxintf_Agemaxsol[0/1] If true (1), the maximum post-mass-transfer age is an upper limit, as the luminosity upper limit of the object is larger than the maximum luminosity of the solar model gridmeta.codeintAgemeanmpEstimated post-mass-transfer age determined from its position in the HRD compared to the metal-poor model gridyrtime.ageintf_Agemeanmp[0/1] If true (1), the mean post-mass-transfer age is an upper limit, as the luminosity of the object is larger than the maximum luminosity of the metal-poor model gridmeta.codeintAgeminmpEstimated minimum post-mass-transfer age determined from its position in the HRD compared to the metal-poor model gridyrtime.age;stat.minintf_Ageminmp[0/1] If true (1), the minimum post-mass-transfer age is an upper limit, as the luminosity lower limit of the object is larger than the maximum luminosity of the metal-poor model gridmeta.codeintAgemaxmpEstimated maximum post-mass-transfer age determined from its position in the HRD compared to the metal-poor model gridyrtime.age;stat.maxintf_Agemaxmp[0/1] If true (1), the maximum post-mass-transfer age is an upper limit, as the luminosity upper limit of the object is larger than the maximum luminosity of the metal-poor model gridmeta.codeint_RAPositions from Name and Simbad (right ascension part)degpos.eq.ra;meta.main_DEPositions from Name and Simbad (declination part)degpos.eq.dec;meta.mainNameIdentification (JHHMMSS.ss+DDMMSS.s or OGLE-LMC-T2CEP-NNN)meta.id;meta.mainchar