Mostrar registro simples

dc.contributor.authorQueiroz, Anna Bárbara de Andradept_BR
dc.contributor.authorAnders, Friedrichpt_BR
dc.contributor.authorSantiago, Basilio Xavierpt_BR
dc.contributor.authorChiappini, C.C.M.pt_BR
dc.contributor.authorSteinmetz, M.pt_BR
dc.contributor.authorDal Ponte, Marinapt_BR
dc.contributor.authorStassun, Keivan G.pt_BR
dc.contributor.authorCosta, Luiz N. dapt_BR
dc.contributor.authorMaia, Marcio Antonio Geimbapt_BR
dc.contributor.authorSouza, Juliana Crestani Ribeiro dept_BR
dc.contributor.authorBeers, T.C.pt_BR
dc.contributor.authorFernández-Trincado, José Gregoriopt_BR
dc.contributor.authorGarcía-Hernández, D. A.pt_BR
dc.contributor.authorRoman-Lopes, Alexandrept_BR
dc.contributor.authorZamora, Olgapt_BR
dc.date.accessioned2018-06-21T02:32:01Zpt_BR
dc.date.issued2018pt_BR
dc.identifier.issn0035-8711pt_BR
dc.identifier.urihttp://hdl.handle.net/10183/179599pt_BR
dc.description.abstractUnderstanding the formation and evolution of our Galaxy requires accurate distances, ages, and chemistry for large populations of field stars. Here, we present several updates to our spectrophotometric distance code, which can now also be used to estimate ages, masses, and extinctions for individual stars. Given a set of measured spectrophotometric parameters, we calculate the posterior probability distribution over a given grid of stellar evolutionary models, using flexible Galactic stellar-population priors. The code (called StarHorse) can accommodate different observational data sets, prior options, partially missing data, and the inclusion of parallax information into the estimated probabilities. We validate the code using a variety of simulated stars as well as real stars with parameters determined from asteroseismology, eclipsing binaries, and isochrone fits to star clusters. Our main goal in this validation process is to test the applicability of the code to field stars with known Gaia-like parallaxes. The typical internal precisions (obtained from realistic simulations of an APOGEE+Gaia-like sample) are 8 per cent in distance, 20 per cent in age, 6 per cent in mass, and 0.04 mag in AV. The median external precision (derived from comparisons with earlier work for real stars) varies with the sample used, but lies in the range of [0, 2] per cent for distances, [12, 31] per cent for ages, [4, 12] per cent for masses, and 0.07 mag for AV. We provide StarHorse distances and extinctions for the APOGEE DR14, RAVE DR5, GES DR3, and GALAH DR1 catalogues.en
dc.format.mimetypeapplication/pdfpt_BR
dc.language.isoengpt_BR
dc.relation.ispartofMonthly notices of the royal astronomical society. Oxford. Vol. 476, no. 2 (Apr. 2018), p. 2556–2583pt_BR
dc.rightsOpen Accessen
dc.subjectStars: distancesen
dc.subjectCatalogos astronomicospt_BR
dc.subjectStars: fundamental parametersen
dc.subjectComposicao estelarpt_BR
dc.subjectEvolucao estelarpt_BR
dc.subjectStars: statisticsen
dc.subjectGalaxy: stellar contenten
dc.titleStarHorse : a Bayesian tool for determining stellar masses, ages, distances, and extinctions for field starspt_BR
dc.typeArtigo de periódicopt_BR
dc.identifier.nrb001067865pt_BR
dc.type.originEstrangeiropt_BR


Thumbnail
   

Este item está licenciado na Creative Commons License

Mostrar registro simples