J/A+A/691/A350ivo://CDS.VizieR/J/A+A/691/A350doi:10.26093/cds/vizier/bc-nk/ldfaCDSMagnus E.Groenewegen M.A.T.Girardi L.Pastorelli G.Marigo P.,Boyer M.L.2026-07-03T06:36:17Z2025-05-05T14:07:22ZCDS support team

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

cds-question@unistra.frmilky-way-galaxymagellanic-cloudsmultiple-starsgiant-starsvisible-astronomyhe JAGB method is a new way of measuring distances in the Universe with the use of asymptotic giant branch (AGB) that are situated in a selected region in a J versus J-Ks colour-magnitude diagram (CMD), and relying on the fact that the absolute J magnitude is (almost) constant. It is implicitly assumed in the method that the selected stars are carbon-rich AGB stars (carbon stars). However, as the sample selected to determine MJ is purely colour based, there can also be contamination by oxygen-rich AGB stars in principle. As the ratio of carbon-rich to oxygen-rich stars is known to depend on metallicity and initial mass, the star formation history and age-metallicity relation in a galaxy should influence the value of MJ. The aim of this paper is to look at mixed samples of oxygen-rich and carbon-rich stars for the Large Magellanic Cloud (LMC), Small Magellanic Cloud (SMC), and Milky way (MW) using the Gaia catalogue of long-period variables (LPVs) as a basis. The advantage of this catalogue is that it contains a classification of O- and C-stars based on the analysis of Gaia Rp spectra. The LPV catalogue is correlated with data from the Two Micron All Sky Survey (2MASS) and samples in the LMC, SMC, and the MW are retrieved. Following methods proposed in the literature, we report the mean and median magnitudes of the selected sample using different colour and magnitude cuts and the results of fitting Gaussian and Lorentzian profiles to the luminosity function (LF). For the SMC and LMC, we confirm previous results in the literature. The LFs of the SMC and LMC JAGB stars are clearly different, yet it can be argued that the mean magnitude inside a selection box agrees at the 0.021mag level. The results of our analysis of the MW sample are less straightforward. The contamination by O-rich stars is substantial for a classical lower limit of (J-Ks)0=1.3, and becomes less than 10% only for (J-Ks)0=1.5. The sample of AGB stars is smaller than for the MCs for two reasons. Nearby AGB stars (with potentially the best determined parallax) tend to be absent as they saturate in the 2MASS catalogue, and the parallax errors of AGB stars tend to be larger compared to non-AGB stars. Several approaches have been taken to improve the situation but finally the JAGB LF for the MW contains about 130 stars, and the fit of Gaussian and Lorentzian profiles is essentially meaningless. The mean and median magnitudes are fainter than for the MC samples by about 0.4 mag which is not predicted by theory. We do not confirm the claim in the literature that the absolute calibration of the JAGB method is independent of metallicity up to solar metallicity. A reliable calibration of the JAGB method at (near) solar metallicity should await further Gaia data releases, or should be carried out in another environment.2024A&A...691A.350Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/691/A350CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toI/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)I/358 : Gaia DR3 Part 4. Variability (Gaia Collaboration, 2022)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/691/A350https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/691/A350http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/691/A350https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/691/A350https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/691/A350http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/691/A350GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/691/A350/tablee1 (WBS (wide binary systems) candidates)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/691/A350/tablee1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/691/A350/tablee1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/691/A350/tablee1?GETtext/xml+votable180.050000true278.5250528-7.95568440.0055555555555555566/1439 13242 14012 14446 14625 14628 14644 14649 15627 18091 23761 28722 28725 28730 28809 28883 29089 29098 29106 29268 29513 29535 30210 30611 32087 35641 37245 37337 37342 37711 37717 37723 37784 37914 37926 37956 38016 38025 38028 38082 39250 39270 40644 41463 41469-41470 41575 41652 41672 41682 41704 41751 41754 41809 42201 42207 42212 42348 42434 42469 42504 43022-43023 43040 44018https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/691/A350?format=asciiOpticaldefaultJ/A+A/691/A350/tablee1WBS (wide binary systems) candidatesSimbadSimbad column added by the CDSmeta.ref.urlcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSIDGaia DR3 identification number of the AGB starmeta.id.part;meta.mainplxParallax of AGB star (1)maspos.parallax.trigfloate_plxParallax error of AGB star (1)masstat.error;pos.parallaxfloatpmRAProper motion along RA of AGB star (1)mas/yrpos.pm;pos.eq.rafloate_pmRAProper motion along RA error of AGB star (1)mas/yrstat.error;pos.pm;pos.eq.rafloatpmDEProper motion along DE of AGB star (1)mas/yrpos.pm;pos.eq.decfloate_pmDEProper motion along DE error of AGB star (1)mas/yrstat.error;pos.pm;pos.eq.decfloatGoFGoodness-of-fit of AGB star (1)meta.code.qualfloatRUWERUWE of AGB star (1)meta.code.qualfloatNameCommon name of AGB starmeta.idcharSID2Gaia DR3 identification number of the WBS candidate potential companionmeta.id.part;meta.mainthetaDistance of the companion to the target stararcminpos.angDistancefloatplx2Parallax of WBS candidate potential companionmaspos.parallax.trigfloate_plx2Parallax error of WBS candidate potential companionmasstat.errorfloatpmRA2Proper motion along RA of WBS candidate potential companionmas/yrpos.pm;pos.eq.rafloate_pmRA2Proper motion along RA error of WBS candidate potential companionmas/yrstat.error;pos.pm;pos.eq.rafloatpmDE2Proper motion along DE of WBS candidate potential companionmas/yrpos.pm;pos.eq.decfloate_pmDE2Proper motion along DE error of WBS candidate potential companionmas/yrstat.error;pos.pm;pos.eq.decfloatGoF2Goodness-of-fit of WBS candidate potential companionmeta.code.qualfloatRUWE2RUWE of WBS candidate potential companionmeta.code.qualfloat_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.main