Spectro-photometric distances to stars : a general purpose Bayesian approach

Detalhes bibliográficos
Autor(a) principal: Santiago, Basilio Xavier
Data de Publicação: 2016
Outros Autores: Brauer, Dorothée, Anders, Friedrich, Chiappini, C.C.M., Queiroz, Anna Bárbara de Andrade, Girardi, Leo Alberto, Rocha-Pinto, H.J., Balbinot, Eduardo, Costa, Luiz N. da, Maia, Marcio Antonio Geimba, Schultheis, Mathias, Steinmetz, M., Miglio, Andrea, Montalbán, Josefina, Schneider, D.P., Beers, T.C., Frinchaboy, P.M., Lee, Y.S., Zasowski, G.
Tipo de documento: Artigo
Idioma: eng
Título da fonte: Repositório Institucional da UFRGS
Texto Completo: http://hdl.handle.net/10183/150006
Resumo: Context. Determining distances to individual field stars is a necessary step towards mapping Galactic structure and determining spatial variations in the chemo-dynamical properties of stellar populations in the Milky Way. Aims. In order to provide stellar distance estimates for various spectroscopic surveys, we have developed a code that estimates distances to stars using measured spectroscopic and photometric quantities. We employ a Bayesian approach to build the probability distribution function over stellar evolutionary models given these data, delivering estimates of model parameters (including distances) for each star individually. Our method provides several alternative distance estimates for each star in the output, along with their associated uncertainties. This facilitates the use of our method even in the absence of some measurements. Methods. The code was first tested on simulations, successfully recovering input distances to mock stars with .1% bias. We found the uncertainties scale with the uncertainties in the adopted spectro-photometric parameters. The method-intrinsic random distance uncertainties for typical spectroscopic survey measurements amount to around 10% for dwarf stars and 20% for giants, and are most sensitive to the quality of log g measurements. Results. The code was then validated by comparing our distance estimates to parallax measurements from the Hipparcos mission for nearby stars (<300 pc), to asteroseismic distances of CoRoT red giant stars, and to known distances of well-studied open and globular clusters. The photometric data of these reference samples cover both optical and infrared wavelengths. The spectroscopic parameters are also based on spectra taken at various wavelengths, with varying spectral coverage and resolution: the Sloan Digital Sky Survey programs SEGUE and APOGEE, as well as various ESO instruments Conclusions. External comparisons confirm that our distances are subject to very small systematic biases with respect to the fundamental Hipparcos scale (+0:4% for dwarfs, and +1:6% for giants). The typical random distance scatter is 18% for dwarfs, and 26% for giants. For the CoRoT-APOGEE sample, which spans Galactocentric distances of 414 kpc, the typical random distance scatter is '15% both for the nearby and farther data. Our distances are systematically larger than the CoRoT distances by about +9%, which can mostly be attributed to the di erent choice of priors. The comparison to known distances of star clusters from SEGUE and APOGEE has led to significant systematic di erences for many cluster stars, but with opposite signs and substantial scatter. Finally, we tested our distances against those previously determined for a high-quality sample of giant stars from the RAVE survey, again finding a small systematic trend of +5% and an rms scatter of 30%. E orts are underway to provide our code to the community by running it on a public server.
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spelling Santiago, Basilio XavierBrauer, DorothéeAnders, FriedrichChiappini, C.C.M.Queiroz, Anna Bárbara de AndradeGirardi, Leo AlbertoRocha-Pinto, H.J.Balbinot, EduardoCosta, Luiz N. daMaia, Marcio Antonio GeimbaSchultheis, MathiasSteinmetz, M.Miglio, AndreaMontalbán, JosefinaSchneider, D.P.Beers, T.C.Frinchaboy, P.M.Lee, Y.S.Zasowski, G.2016-12-07T02:26:26Z20160004-6361http://hdl.handle.net/10183/150006001004677Context. Determining distances to individual field stars is a necessary step towards mapping Galactic structure and determining spatial variations in the chemo-dynamical properties of stellar populations in the Milky Way. Aims. In order to provide stellar distance estimates for various spectroscopic surveys, we have developed a code that estimates distances to stars using measured spectroscopic and photometric quantities. We employ a Bayesian approach to build the probability distribution function over stellar evolutionary models given these data, delivering estimates of model parameters (including distances) for each star individually. Our method provides several alternative distance estimates for each star in the output, along with their associated uncertainties. This facilitates the use of our method even in the absence of some measurements. Methods. The code was first tested on simulations, successfully recovering input distances to mock stars with .1% bias. We found the uncertainties scale with the uncertainties in the adopted spectro-photometric parameters. The method-intrinsic random distance uncertainties for typical spectroscopic survey measurements amount to around 10% for dwarf stars and 20% for giants, and are most sensitive to the quality of log g measurements. Results. The code was then validated by comparing our distance estimates to parallax measurements from the Hipparcos mission for nearby stars (<300 pc), to asteroseismic distances of CoRoT red giant stars, and to known distances of well-studied open and globular clusters. The photometric data of these reference samples cover both optical and infrared wavelengths. The spectroscopic parameters are also based on spectra taken at various wavelengths, with varying spectral coverage and resolution: the Sloan Digital Sky Survey programs SEGUE and APOGEE, as well as various ESO instruments Conclusions. External comparisons confirm that our distances are subject to very small systematic biases with respect to the fundamental Hipparcos scale (+0:4% for dwarfs, and +1:6% for giants). The typical random distance scatter is 18% for dwarfs, and 26% for giants. For the CoRoT-APOGEE sample, which spans Galactocentric distances of 414 kpc, the typical random distance scatter is '15% both for the nearby and farther data. Our distances are systematically larger than the CoRoT distances by about +9%, which can mostly be attributed to the di erent choice of priors. The comparison to known distances of star clusters from SEGUE and APOGEE has led to significant systematic di erences for many cluster stars, but with opposite signs and substantial scatter. Finally, we tested our distances against those previously determined for a high-quality sample of giant stars from the RAVE survey, again finding a small systematic trend of +5% and an rms scatter of 30%. E orts are underway to provide our code to the community by running it on a public server.application/pdfengAstronomy and astrophysics. Les Ulis. Vol. 585 (Jan. 2016), A42, 15 p.EspectrofotometriaModelos estatísticosMapeamentos astronômicosStars: distancesGalaxy: structureStars: statisticsMethods: statisticalSurveysSpectro-photometric distances to stars : a general purpose Bayesian approachEstrangeiroinfo:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/openAccessreponame:Repositório Institucional da UFRGSinstname:Universidade Federal do Rio Grande do Sul (UFRGS)instacron:UFRGSORIGINAL001004677.pdf001004677.pdfTexto completo (inglês)application/pdf2430386http://www.lume.ufrgs.br/bitstream/10183/150006/1/001004677.pdf5adc78c776ebbf09dd6708ddb0445fbcMD51TEXT001004677.pdf.txt001004677.pdf.txtExtracted Texttext/plain87871http://www.lume.ufrgs.br/bitstream/10183/150006/2/001004677.pdf.txt37cc47e866c15927897f96e9295399f9MD52THUMBNAIL001004677.pdf.jpg001004677.pdf.jpgGenerated Thumbnailimage/jpeg2102http://www.lume.ufrgs.br/bitstream/10183/150006/3/001004677.pdf.jpg02629006e0d93acb3d4123a59f5e39d3MD5310183/1500062023-07-02 03:41:34.583713oai:www.lume.ufrgs.br:10183/150006Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2023-07-02T06:41:34Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false
dc.title.pt_BR.fl_str_mv Spectro-photometric distances to stars : a general purpose Bayesian approach
title Spectro-photometric distances to stars : a general purpose Bayesian approach
spellingShingle Spectro-photometric distances to stars : a general purpose Bayesian approach
Santiago, Basilio Xavier
Espectrofotometria
Modelos estatísticos
Mapeamentos astronômicos
Stars: distances
Galaxy: structure
Stars: statistics
Methods: statistical
Surveys
title_short Spectro-photometric distances to stars : a general purpose Bayesian approach
title_full Spectro-photometric distances to stars : a general purpose Bayesian approach
title_fullStr Spectro-photometric distances to stars : a general purpose Bayesian approach
title_full_unstemmed Spectro-photometric distances to stars : a general purpose Bayesian approach
title_sort Spectro-photometric distances to stars : a general purpose Bayesian approach
author Santiago, Basilio Xavier
author_facet Santiago, Basilio Xavier
Brauer, Dorothée
Anders, Friedrich
Chiappini, C.C.M.
Queiroz, Anna Bárbara de Andrade
Girardi, Leo Alberto
Rocha-Pinto, H.J.
Balbinot, Eduardo
Costa, Luiz N. da
Maia, Marcio Antonio Geimba
Schultheis, Mathias
Steinmetz, M.
Miglio, Andrea
Montalbán, Josefina
Schneider, D.P.
Beers, T.C.
Frinchaboy, P.M.
Lee, Y.S.
Zasowski, G.
author_role author
author2 Brauer, Dorothée
Anders, Friedrich
Chiappini, C.C.M.
Queiroz, Anna Bárbara de Andrade
Girardi, Leo Alberto
Rocha-Pinto, H.J.
Balbinot, Eduardo
Costa, Luiz N. da
Maia, Marcio Antonio Geimba
Schultheis, Mathias
Steinmetz, M.
Miglio, Andrea
Montalbán, Josefina
Schneider, D.P.
Beers, T.C.
Frinchaboy, P.M.
Lee, Y.S.
Zasowski, G.
author2_role author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
dc.contributor.author.fl_str_mv Santiago, Basilio Xavier
Brauer, Dorothée
Anders, Friedrich
Chiappini, C.C.M.
Queiroz, Anna Bárbara de Andrade
Girardi, Leo Alberto
Rocha-Pinto, H.J.
Balbinot, Eduardo
Costa, Luiz N. da
Maia, Marcio Antonio Geimba
Schultheis, Mathias
Steinmetz, M.
Miglio, Andrea
Montalbán, Josefina
Schneider, D.P.
Beers, T.C.
Frinchaboy, P.M.
Lee, Y.S.
Zasowski, G.
dc.subject.por.fl_str_mv Espectrofotometria
Modelos estatísticos
Mapeamentos astronômicos
topic Espectrofotometria
Modelos estatísticos
Mapeamentos astronômicos
Stars: distances
Galaxy: structure
Stars: statistics
Methods: statistical
Surveys
dc.subject.eng.fl_str_mv Stars: distances
Galaxy: structure
Stars: statistics
Methods: statistical
Surveys
description Context. Determining distances to individual field stars is a necessary step towards mapping Galactic structure and determining spatial variations in the chemo-dynamical properties of stellar populations in the Milky Way. Aims. In order to provide stellar distance estimates for various spectroscopic surveys, we have developed a code that estimates distances to stars using measured spectroscopic and photometric quantities. We employ a Bayesian approach to build the probability distribution function over stellar evolutionary models given these data, delivering estimates of model parameters (including distances) for each star individually. Our method provides several alternative distance estimates for each star in the output, along with their associated uncertainties. This facilitates the use of our method even in the absence of some measurements. Methods. The code was first tested on simulations, successfully recovering input distances to mock stars with .1% bias. We found the uncertainties scale with the uncertainties in the adopted spectro-photometric parameters. The method-intrinsic random distance uncertainties for typical spectroscopic survey measurements amount to around 10% for dwarf stars and 20% for giants, and are most sensitive to the quality of log g measurements. Results. The code was then validated by comparing our distance estimates to parallax measurements from the Hipparcos mission for nearby stars (<300 pc), to asteroseismic distances of CoRoT red giant stars, and to known distances of well-studied open and globular clusters. The photometric data of these reference samples cover both optical and infrared wavelengths. The spectroscopic parameters are also based on spectra taken at various wavelengths, with varying spectral coverage and resolution: the Sloan Digital Sky Survey programs SEGUE and APOGEE, as well as various ESO instruments Conclusions. External comparisons confirm that our distances are subject to very small systematic biases with respect to the fundamental Hipparcos scale (+0:4% for dwarfs, and +1:6% for giants). The typical random distance scatter is 18% for dwarfs, and 26% for giants. For the CoRoT-APOGEE sample, which spans Galactocentric distances of 414 kpc, the typical random distance scatter is '15% both for the nearby and farther data. Our distances are systematically larger than the CoRoT distances by about +9%, which can mostly be attributed to the di erent choice of priors. The comparison to known distances of star clusters from SEGUE and APOGEE has led to significant systematic di erences for many cluster stars, but with opposite signs and substantial scatter. Finally, we tested our distances against those previously determined for a high-quality sample of giant stars from the RAVE survey, again finding a small systematic trend of +5% and an rms scatter of 30%. E orts are underway to provide our code to the community by running it on a public server.
publishDate 2016
dc.date.accessioned.fl_str_mv 2016-12-07T02:26:26Z
dc.date.issued.fl_str_mv 2016
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dc.relation.ispartof.pt_BR.fl_str_mv Astronomy and astrophysics. Les Ulis. Vol. 585 (Jan. 2016), A42, 15 p.
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