J/A+A/686/A142ivo://CDS.VizieR/J/A+A/686/A142doi:10.26093/cds/vizier.36860142CDSLi G.Aerts C.Bedding T.R.Fritzewski D.J.Murphy S.J.Van Reeth T.,Montet B.T.Jian M.Mombarg J.S.G.Gossage S.Sreenivas K.R.2025-07-03T20:01:03Z2024-09-03T13:04:07ZCDS support team

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

cds-question@unistra.fropen-star-clustersearly-type-starsasteroseismologyvisible-astronomyAsteroseismic modelling of isolated stars presents significant challenges due to the difficulty in accurately determining stellar parameters, particularly the stellar age. These challenges can be overcome by observing stars in open clusters whose coeval members share an initial chemical composition. The light curves from the all-sky survey by the Transiting Exoplanet Survey Satellite (TESS) allow us to investigate and analyse stellar variations in clusters with an unprecedented level of detail for the first time. We aim to detect gravity-mode oscillations in the early-type main-sequence members of the young open cluster NGC 2516 to deduce their internal rotation rates. We selected the 301 member stars with no more than mild contamination as our sample. We analysed the full-frame image light curves, which provide nearly continuous observations in the first and third years of TESS monitoring. We also collected high-resolution spectra using the Fiber-fed Extended Range Optical Spectrograph for the g-mode pulsators, with the aim of assessing the Gaia effective temperatures and gravities and preparing for future seismic modelling. By fitting the theoretical isochrones to the colour-magnitude diagram of a cluster, we determined an age of 102+/-15Myr and inferred that the extinction at 550nm (A0) is 0.53+/-0.0mag. We identified 147 stars with surface-brightness modulations: 24 with gravity (g-)mode pulsations ({gamma} Doradus or slowly pulsating B-type stars) and 35 with pressure (p-)mode pulsations ({delta} Sct stars). When sorted by colour index, the amplitude spectra of the {delta} Sct stars show a distinct ordering and reveal a discernible frequency-temperature relationship. The near-core rotation rates, measured from period spacing patterns in two slowly pulsating B-type (SPB) stars and nine {gamma} Dor stars, reach up to 3d^-1^. This is at the high end of the values found from Kepler data of field stars of similar variability type. The {gamma} Dor stars of NGC 2516 have internal rotation rates as high as 50% of their critical value, whereas the SPB stars exhibit rotation rates close to their critical rate. Although the B-type stars are rotating rapidly, we did not find long-term brightness and colour variations in the mid-infrared, which suggests that there are no disc or shell formation events in our sample. We also discussed the results of our spectroscopic observations for the g-mode pulsators.2024A&A...686A.142Lhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/686/A142CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toI/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)IV/38 : TESS Input Catalog - v8.0 (TIC-8) (Stassun+, 2019)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/686/A142https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/686/A142http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/686/A142https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/686/A142https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/686/A142http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/686/A142GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/686/A142/tablea1 (Surface modulation periods for NGC 2516 cluster member stars in this study)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/686/A142/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/686/A142/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/686/A142/tablea1?GETtext/xml+votable180.050000true119.5121342-60.61478560.005555555555555556Cone search capability for table J/A+A/686/A142/param (Stellar parameters of the NGC 2516 cluster member stars)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/686/A142/param?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/686/A142/param?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/686/A142/param?GETtext/xml+votable180.050000true101.5511703125-71.03125665760.0055555555555555565/9374 9396 9398 9404 6/32837 36866 36907 36992 37001 37007-37008 37019 37022 37026 37044 37052 37096 37396 37406 37421 37450-37452 37464 37475-37476 37478-37479 37485-37488 37490 37573-37575 37580-37581 37583 37588 37590 37596 37599 37605 37607 37620-37622 37624-37625 37628 38992 38997-389991.9867573869263685e-19 3.916500758235022e-19https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/686/A142?format=asciiOpticaldefaultJ/A+A/686/A142/tablea1Surface modulation periods for NGC 2516 cluster member stars in this studyrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTICTIC number of stars with surface modulationsmeta.id;meta.mainlongSimbadSimbad column added by the CDSmeta.ref.urlcharBP-RPGaia colour index, BP-RPphot.color;em.opt.B;em.opt.RfloatFreqMeasured surface rotation frequencyd**-1em.freq;src.varfloate_FreqMeasured surface rotation frequency errord**-1stat.errorfloatPerPerioddtime.perioddoublee_PerPeriod errordstat.errordouble_RAPositions from TIC (right ascension part)degpos.eq.ra;meta.main_DEPositions from TIC (declination part)degpos.eq.dec;meta.mainJ/A+A/686/A142/paramStellar parameters of the NGC 2516 cluster member starsS/N? Signal-to-noise ratio of the FEROS spectrad**-1stat.snrfloatnullablePi0? Asymptotic spacing of g modes, measured by g modes, only available for 11 starstime.periodfloatnullablee_Pi0? Asymptotic spacing of g modes uncertaintystat.errorfloatnullabledP/dt? Near-core rotation rate, measured by g modes, only available for 11 starsd**-1time.perioddoublenullablee_dP/dt? Near-core rotation rate uncertaintyd**-1stat.errordoublenullablePer? Surface rotation period measured by surface modulationsmeta.notedoublenullableSimbadSimbad column added by the CDSmeta.ref.urlcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGaiaDR3Gaia DR3 source IDmeta.idTICTIC numbermeta.id;meta.mainlongRA_ICRSGaia right ascension (ICRS) at Ep=2016.0degpos.eq.ra;meta.mainDE_ICRSGaia declination (ICRS) at Ep=2016.0degpos.eq.dec;meta.mainGmagGaia G band magnitudemagphot.mag;em.optdoublee_GmagGaia G band magnitude uncertaintymagstat.error;phot.magdoubleGMAGGaia G band absolute magnitude, without the correction of extinctionmagphys.magAbsdoublee_GMAGGaia G band absolute magnitude uncertaintymagstat.errordoublelogLlog of luminosity, calculated by Gaia effective temperature, with the bolometric correction and extinction correction. Use with cautionlog(solLum)phys.luminositydoublee_logLlog of luminosity uncertaintylog(solLum)stat.errordoubleTeffEffective temperature provided by Gaia. Use with cautionKphys.temperature.effectivefloate_TeffEffective temperature uncertainty (1)Kstat.error;phys.temperature.effectivefloatBP-RPGaia colour indexmagphot.color;em.opt.B;em.opt.Rdoublee_BP-RPGaia colour index uncertaintymagstat.errordoubleTeffspEffective temperature by FEROS spectra, better than Tegg, only available for nine starsKphys.temperature.effectivefloate_Teffsp? Effective temperature by FEROS spectra uncertaintyKstat.errorfloatnullablelogLsp? log of luminosity calculated by Teffsp, with the bolometric correction and extinction correction, better than logLlog(solLum)phys.luminositydoublenullablee_logLsp? log of luminosity calculated by Teffsp uncertaintylog(solLum)stat.errordoublenullablelogg? Surface gravity by FEROS spectra, only available for nine starslog(cm.s**-2)phys.gravitydoublenullablee_logg? Surface gravity uncertaintylog(cm.s**-2)stat.errordoublenullablevsini? Projected equatorial velocity by FEROS spectra, only available for nine starskm/sphys.velocfloatnullablee_vsini? Projected equatorial velocity uncertaintykm/sstat.error;phys.veloc.rotatfloatnullable[M/H]? Metallicity by FEROS spectra, only available for nine starsphys.abund.Zdoublenullablee_[M/H]? Metallicity by FEROS spectra uncertaintystat.error;phys.abunddoublenullableRVsp? Radial velocity by FEROS spectra, only available for nine starskm/sphys.veloc;pos.heliocentricfloatnullablee_RVsp? Radial velocity by FEROS spectra uncertaintykm/sstat.errorfloatnullableVmic? Microturbulent velocity by FEROS spectra, only available for nine starskm/sphys.velocfloatnullablee_Vmic? Microturbulent velocity by FEROS spectra uncertaintykm/sstat.errordoublenullablee_Per? Surface rotation period uncertaintystat.errordoublenullable