J/A+A/708/L1ivo://CDS.VizieR/J/A+A/708/L1CDSZallio L.Vioque M.Andrews S.M.Empey A.Rosotti G.P.Miotello A.,Manara C.F.Carpenter J.M.Deng D.Kurtovic N.T.Law C.J.Longarini C.,Paneque-Carreno T.Teague R.Villenave M.Yen H.S.Zagaria F.2026-04-02T06:28:33Z2026-03-25T08:11:38ZCDS support team

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

cds-question@unistra.frpre-main-sequence-starsstellar-massesco-line-emissionastronomical-modelsStellar masses are a fundamental property to understand models of pre-main sequence evolution, but their values derived from Hertzsprung-Russell (HR) diagrams are strongly model dependent. We benchmark pre-main sequence stellar evolutionary tracks using stellar masses dynamically estimated by fitting a parametric model to ALMA observations of the ^12^CO (J=3-2) line transition emitted by the disks orbiting 20 sources in the old (4-14Myr) Upper Scorpius star forming region. We derive stellar masses from HR diagram fitting for ten different stellar evolutionary models, which we then compare with their stellar dynamical masses for comparison in the stellar mass range 0.1-1.3M_{sun}_. Models with a moderate-to-low fraction of cold stellar spots (f=17%) most accurately reproduce the dynamical stellar masses (100% of the targets agree within +/-1{sigma}). While a higher spot coverage (f=34%) provides similar stellar mass predictions similar to magnetic equipartition models, larger fractions (f>=51%) significantly disagree with dynamical masses. Magnetic equipartition models overestimate stellar masses up to a factor ~20%, whereas non-magnetic mod- els underestimate them up to ~12%. For some models, there is evidence that the stellar mass discrepancies are anticorrelated with dynamical stellar masses. When stellar dynamical mass priors are considered in HR diagram fitting, the median age of a single source can change up to ~25%, while the median ages inferred across different tracks become consistent, with the age scatter decreasing by ~77%. These results provide strong empirical constraints for testing and developing evolutionary models of pre-main sequence stars.2026A&A...708L...1Zhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/708/L1CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/705/A49 : 12CO gas structures of protoplanetary disks (Zallio+, 2026)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/708/L1https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/708/L1http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/708/L1https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/708/L1https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/708/L1http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/708/L1GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/708/L1/tabled1 (stellar masses considered in this work)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/708/L1/tabled1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/708/L1/tabled1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/708/L1/tabled1?GETtext/xml+votable180.050000true239.6508-19.770520.0055555555555555566/42954 42958-42959 42972 42976 42980-42982 42990-42991 44317 44359 44364-44365 44370 44372-44373 44377 44379 44389-44390 44401-44402https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/708/L1?format=asciiRadiodefaultJ/A+A/708/L1/tabled1stellar masses considered in this workrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGaiaDR3Gaia DR3 source identifier (Gaia_DR3)meta.idchare_Sf85Mass? Lower uncertainty on Sf85Mass (SPOTS_f85_err_low)solMassstat.errordoublenullableE_Sf85Mass? Upper uncertainty on Sf85Mass (SPOTS_f85_err_up)solMassstat.error;stat.maxdoublenullableSimbadSimbad column added by the CDSmeta.ref.urlchar2MASS2MASS source identifier, JHHMMMSSss+DDMMSSs (Source_2MASS)meta.id;meta.maincharRA_ICRSRight ascension (ICRS) at Ep=2016.0 (Gaia DR3) (RA_GaiaDR3)degpos.eq.ra;meta.mainDE_ICRSDeclination (ICRS) at Ep=2016.0 (Gaia DR3) (DEC_GaiaDR3)degpos.eq.dec;meta.mainMcsaltStellar mass from csalt (M_csalt)solMassphys.massdoublee_McsaltUncertainty on M_csalt (err_csalt)solMassstat.errordoubleB15Mass? Mass from Baraffe et al. (2015A&A...577A..42B) tracks (Baraffe15_mass)solMassphys.massdoublenullablee_B15Mass? Lower uncertainty on B15Mass (16th percentile) (Baraffe15_err_low)solMassstat.errordoublenullableE_B15Mass? Upper uncertainty on B15Mass (84th percentile) (Baraffe15_err_up)solMassstat.error;stat.maxdoublenullableF16noBMass? Mass from Feiden et al. (2016A&A...593A..99F) tracks (no B) (Feiden16_noB_mass)solMassphys.massdoublenullablee_F16noBMass? Lower uncertainty of F16noBMass (Feiden16_noB_err_low)solMassstat.errordoublenullableE_F16noBMass? Upper uncertainty of F16noBMass (Feiden16_noB_err_up)solMassstat.error;stat.maxdoublenullableF16BMass? Mass from Feidenet al. (2016A&A...593A..99F) tracks (with B) (Feiden16_B_mass)solMassphys.massdoublenullablee_F16BMass? Lower uncertainty of F16BMass (Feiden16_B_err_low)solMassstat.errordoublenullableE_F16BMass? Upper uncertainty of F16BMass (Feiden16_B_err_up)solMassstat.error;stat.maxdoublenullablePMass? Mass from PARSEC v2.0 tracks (PARSEC_mass)solMassphys.massdoublenullablee_PMass? Lower uncertainty on PMass (PARSEC_err_low)solMassstat.errordoublenullableE_PMass? Upper uncertainty on PMass (PARSEC_err_up)solMassstat.error;stat.maxdoublenullableS20Mass? Mass from Siess et al. (2000A&A...358..593S) tracks (Siess2000_mass)solMassphys.massdoublenullablee_S20Mass? Lower uncertainty on S20Mass (Siess2000_err_low)solMassstat.errordoublenullableE_S20Mass? Upper uncertainty on S20Mass (Siess2000_err_up)solMassstat.error;stat.maxdoublenullableSf0Mass? Mass from SPOTS models (f=0%) (SPOTS_f0_mass)solMassphys.massdoublenullablee_Sf0Mass? Lower uncertainty on Sf0Mass (SPOTS_f0_err_low)solMassstat.errordoublenullableE_Sf0Mass? Upper uncertainty on Sf0Mass (SPOTS_f0_err_up)solMassstat.error;stat.maxdoublenullableSf17Mass? Mass from SPOTS models (f=17%) (SPOTS_f17_mass)solMassphys.massdoublenullablee_Sf17Mass? Lower uncertainty on Sf17Mass (SPOTS_f17_err_low)solMassstat.errordoublenullableE_Sf17Mass? Upper uncertainty on Sf17Mass (SPOTS_f17_err_up)solMassstat.error;stat.maxdoublenullableSf34Mass? Mass from SPOTS models (f=34%) (SPOTS_f34_mass)solMassphys.massdoublenullablee_Sf34Mass? Lower uncertainty on Sf34Mass (SPOTS_f34_err_low)solMassstat.errordoublenullableE_Sf34Mass? Upper uncertainty on Sf34Mass (SPOTS_f34_err_up)solMassstat.error;stat.maxdoublenullableSf51Mass? Mass from SPOTS models (f=51%) (SPOTS_f51_mass)solMassphys.massdoublenullablee_Sf51Mass? Lower uncertainty on Sf51Mass (SPOTS_f51_err_low)solMassstat.errordoublenullableE_Sf51Mass? Upper uncertainty on Sf51Mass (SPOTS_f51_err_up)solMassstat.error;stat.maxdoublenullableSf85Mass? Mass from SPOTS models (f=85%) (SPOTS_f85_mass)solMassphys.massdoublenullable