J/A+A/660/A7ivo://CDS.VizieR/J/A+A/660/A7doi:10.26093/cds/vizier.36600007CDSFanelli C.Origlia L.Oliva E.Dalessandro E.Mucciarelli A.Sanna N.2022-11-13T16:36:52Z2022-03-30T07:40:37ZCDS support team

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

cds-question@unistra.fratomic-physicsvisible-astronomyinfrared-astronomyThe Perseus complex in the outer disk of the Galaxy hosts a number of clusters and associations of young stars. Gaia is providing a detailed characterisation of their kinematic structure and evolutionary properties. Within the SPA Large Programme at the TNG, we secured HARPS-N and GIANO-B high-resolution optical and near-infrared (NIR) spectra of the young red supergiants (RSG) stars in the Perseus complex, in order to obtain accurate radial velocities, stellar parameters and detailed chemical abundances. We used spectral synthesis to best-fit hundreds of atomic and molecular lines in the spectra of the observed 27 RSGs. We obtained accurate estimates of the stellar temperature, gravity, micro and macro turbulence velocities and chemical abundances for 25 different elements. We also measured the ^12^C/^13^C abundance ratio. Our combined optical and NIR chemical study provides homogeneous half-solar iron with a small dispersion, about solar-scaled abundance ratios for the iron-peak, alpha and other light elements and a small enhancement of Na, K and neutron-capture elements, consistent with the thin disk chemistry traced by older stellar populations at a similar Galactocentric distance of about 10kpc. We inferred enhancement of N, depletion of C and of the ^12^C/^13^C isotopic abundance ratio, consistent with mixing processes in the stellar interiors during the RSG evolution.2022A&A...660A...7Fhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/660/A7CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/660/A7https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/660/A7http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/660/A7https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/660/A7https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/660/A7http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/660/A7GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticalInfrareddefaultJ/A+A/660/A7/tablea1*Optical atomic linesLineLine identificationmeta.id;spect.linefloatEPPotential energyeVphys.energy;phys.atmol.levelfloatlog(gf)Oscillator strengthphys.atmol.oscStrengthfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambdaAirAir wavelength0.1nmem.wldoubleJ/A+A/660/A7/tablea2*NIR atomic linesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambdaAirAir wavelength0.1nmem.wldoubleLineLine identificationmeta.id;spect.linefloatEPPotential energyeVphys.energy;phys.atmol.levelfloatlog(gf)Oscillator strengthphys.atmol.oscStrengthfloatJ/A+A/660/A7/tablea3*NIR molecular linesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambdaAirAir wavelength0.1nmem.wldoubleLineLine identificationmeta.id;spect.linefloatEPPotential energyeVphys.energy;phys.atmol.levelfloatlog(gf)Oscillator strengthphys.atmol.oscStrengthfloat