J/A+A/704/A322ivo://CDS.VizieR/J/A+A/704/A322CDSMillan-Irigoyen I.Molla M.Cervino M.Garcia-Vargas M.L.2025-12-18T07:41:46Z2025-12-18T08:41:19ZCDS support team

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

cds-question@unistra.frastronomical-modelsstellar-atmospheresgalaxiesstellar-associationsspectral-energy-distributionLow metallicity stellar populations are very abundant in the Universe, either as the remnants of the past history of the Milky Way or similar spiral galaxies, or the young low metallicity stellar populations that are being observed in the local dwarf galaxies or in the high-z objects with low metal content recently found with JWST. Our goal is to develop new high-spectral-resolution models tailored for low-metallicity environments and apply them to analyze stellar population data, particularly in cases where a significant portion of the stellar content exhibits low metallicity. We used the state-of-the-art stellar population synthesis code HR-pyPopStar with available stellar libraries to create a new set of models focused on low metallicity stellar populations. We have compared the new spectral energy distributions with the previous models of HR-pyPopStar for solar metallicity. Once we verified that the spectra, except for the oldest ages that show some differences in the molecular bands of the TiO and G band, are similar, we reanalyzed the high resolution data from the globular cluster M 15 by finding a better estimate of its age and metallicity. Finally, we analyzed a subsample of mostly star-forming dwarf galaxies from the MaNGA survey we found similar stellar mass-mean stellar metallicity weighted by light to other studies that studied star forming dwarf galaxies and slightly higher mean stellar metallicity than the other works that analysed all types of dwarf galaxies at the same time, but are within error bars.2025A&A...704A.322Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/704/A322CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/MNRAS/506/4781 : HR-PYPOPSTAR model (Millan-irigoyen+, 2021)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/704/A322https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/704/A322http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/704/A322https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/704/A322https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/704/A322http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/704/A322GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tap2.367228618189496e-19 6.194049834323928e-19defaultJ/A+A/704/A322/table4Magnitudes in broad-band filters of the SSPs modelsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIMFIMF: CHA, KRO, FER or SAL (G1)meta.id;stat.fitcharZMetallicity: 0.0001,0.0004,0.004,0.008,0.02,0.05phys.abund.ZfloatlogtauLogarithm of the age in yrlog(yr)time.agefloatUmagMagnitude in Johnson-Cousins band Umagphot.mag;em.opt.UdoubleBmagMagnitude in Johnson-Cousins band Bmagphot.mag;em.opt.BdoubleVmagMagnitude in Johnson-Cousins band Vmagphot.mag;em.opt.VdoubleRmagMagnitude in Johnson-Cousins band Rmagphot.mag;em.opt.RdoubleImagMagnitude in Johnson-Cousins band Imagphot.mag;em.opt.IdoubleumagMagnitude in SDSS-SLOAN band umagphot.mag;em.opt.UdoublegmagMagnitude in SDSS-SLOAN band gmagphot.mag;em.opt.BdoublermagMagnitude in SDSS-SLOAN band rmagphot.mag;em.opt.RdoubleimagMagnitude in SDSS-SLOAN band imagphot.mag;em.opt.IdoublezmagMagnitude in SDSS-SLOAN band zmagphot.mag;em.opt.IdoubleJ/A+A/704/A322/table5Properties of the stellar populations of the obtained by FADO using the new SSP modelsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintPlateIdPlate Id from MaNGAmeta.id;instr.platecharlogMstarLog10 of the current stellar mass of the galaxylog(solMass)phys.massdoublemeanlogAgeMMean of the log10 of the age weighted by lightlog(yr)time.agedoublemeanlogAgeLMean of the log10 of the age weighted by masslog(yr)time.agedoublelogmeanZLLog10 of the mean of the metallicity weighted by lightlog(Sun)phys.abund.ZdoublelogmeanZMLog10 of the mean of the metallicity weighted by lightlog(Sun)phys.abund.Zdouble