Period-Luminosity-Colour distribution and classification of Galactic oxygen-rich LPVs I. Luminosity calibrations

The absolute K magnitudes and kinematic parameters of about 350 oxygen-rich Long-Period Variable stars are calibrated, by means of an up-to-date maximum-likelihood method, using HIPPARCOS parallaxes and proper motions together with radial velocities and, as additional data, periods and V-K colour in...

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Autores: Barthès, D., Luri Carrascoso, Xavier, Alvarez, R., Mennessier, M. O.
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:1999
País:España
Institución:Universidad de Barcelona
Repositorio:Dipòsit Digital de la UB
OAI Identifier:oai:diposit.ub.edu:2445/9225
Acceso en línea:https://hdl.handle.net/2445/9225
Access Level:acceso abierto
Palabra clave:Evolució estel·lar
Cinemàtica galàctica
Stars: variables: long period variables
AGB
Fundamental parameters
Kinematics
Evolution
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spelling Period-Luminosity-Colour distribution and classification of Galactic oxygen-rich LPVs I. Luminosity calibrationsBarthès, D.Luri Carrascoso, XavierAlvarez, R.Mennessier, M. O.Evolució estel·larCinemàtica galàcticaStars: variables: long period variablesAGBFundamental parametersKinematicsEvolutionThe absolute K magnitudes and kinematic parameters of about 350 oxygen-rich Long-Period Variable stars are calibrated, by means of an up-to-date maximum-likelihood method, using HIPPARCOS parallaxes and proper motions together with radial velocities and, as additional data, periods and V-K colour indices. Four groups, differing by their kinematics and mean magnitudes, are found. For each of them, we also obtain the distributions of magnitude, period and de-reddened colour of the base population, as well as de-biased period-luminosity-colour relations and their two-dimensional projections. The SRa semiregulars do not seem to constitute a separate class of LPVs. The SRb appear to belong to two populations of different ages. In a PL diagram, they constitute two evolutionary sequences towards the Mira stage. The Miras of the disk appear to pulsate on a lower-order mode. The slopes of their de-biased PL and PC relations are found to be very different from the ones of the Oxygen Miras of the LMC. This suggests that a significant number of so-called Miras of the LMC are misclassified. This also suggests that the Miras of the LMC do not constitute a homogeneous group, but include a significant proportion of metal-deficient stars, suggesting a relatively smooth star formation history. As a consequence, one may not trivially transpose the LMC period-luminosity relation from one galaxy to the other.EDP Sciences1999info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionapplication/pdfhttps://hdl.handle.net/2445/9225Articles publicats en revistes (Física Quàntica i Astrofísica)reponame:Dipòsit Digital de la UBinstname:Universidad de BarcelonaInglésReproducció del document publicat a http://dx.doi.org/10.1051/aas:1999518Astronomy and Astrophysics Supplement Series, 1999, vol. 140, p. 55-67.http://dx.doi.org/10.1051/aas:1999518(c) The European Southern Observatory, 1999info:eu-repo/semantics/openAccessoai:diposit.ub.edu:2445/92252026-05-27T06:46:51Z
dc.title.none.fl_str_mv Period-Luminosity-Colour distribution and classification of Galactic oxygen-rich LPVs I. Luminosity calibrations
title Period-Luminosity-Colour distribution and classification of Galactic oxygen-rich LPVs I. Luminosity calibrations
spellingShingle Period-Luminosity-Colour distribution and classification of Galactic oxygen-rich LPVs I. Luminosity calibrations
Barthès, D.
Evolució estel·lar
Cinemàtica galàctica
Stars: variables: long period variables
AGB
Fundamental parameters
Kinematics
Evolution
title_short Period-Luminosity-Colour distribution and classification of Galactic oxygen-rich LPVs I. Luminosity calibrations
title_full Period-Luminosity-Colour distribution and classification of Galactic oxygen-rich LPVs I. Luminosity calibrations
title_fullStr Period-Luminosity-Colour distribution and classification of Galactic oxygen-rich LPVs I. Luminosity calibrations
title_full_unstemmed Period-Luminosity-Colour distribution and classification of Galactic oxygen-rich LPVs I. Luminosity calibrations
title_sort Period-Luminosity-Colour distribution and classification of Galactic oxygen-rich LPVs I. Luminosity calibrations
dc.creator.none.fl_str_mv Barthès, D.
Luri Carrascoso, Xavier
Alvarez, R.
Mennessier, M. O.
author Barthès, D.
author_facet Barthès, D.
Luri Carrascoso, Xavier
Alvarez, R.
Mennessier, M. O.
author_role author
author2 Luri Carrascoso, Xavier
Alvarez, R.
Mennessier, M. O.
author2_role author
author
author
dc.subject.none.fl_str_mv Evolució estel·lar
Cinemàtica galàctica
Stars: variables: long period variables
AGB
Fundamental parameters
Kinematics
Evolution
topic Evolució estel·lar
Cinemàtica galàctica
Stars: variables: long period variables
AGB
Fundamental parameters
Kinematics
Evolution
description The absolute K magnitudes and kinematic parameters of about 350 oxygen-rich Long-Period Variable stars are calibrated, by means of an up-to-date maximum-likelihood method, using HIPPARCOS parallaxes and proper motions together with radial velocities and, as additional data, periods and V-K colour indices. Four groups, differing by their kinematics and mean magnitudes, are found. For each of them, we also obtain the distributions of magnitude, period and de-reddened colour of the base population, as well as de-biased period-luminosity-colour relations and their two-dimensional projections. The SRa semiregulars do not seem to constitute a separate class of LPVs. The SRb appear to belong to two populations of different ages. In a PL diagram, they constitute two evolutionary sequences towards the Mira stage. The Miras of the disk appear to pulsate on a lower-order mode. The slopes of their de-biased PL and PC relations are found to be very different from the ones of the Oxygen Miras of the LMC. This suggests that a significant number of so-called Miras of the LMC are misclassified. This also suggests that the Miras of the LMC do not constitute a homogeneous group, but include a significant proportion of metal-deficient stars, suggesting a relatively smooth star formation history. As a consequence, one may not trivially transpose the LMC period-luminosity relation from one galaxy to the other.
publishDate 1999
dc.date.none.fl_str_mv 1999
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv https://hdl.handle.net/2445/9225
url https://hdl.handle.net/2445/9225
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv Reproducció del document publicat a http://dx.doi.org/10.1051/aas:1999518
Astronomy and Astrophysics Supplement Series, 1999, vol. 140, p. 55-67.
http://dx.doi.org/10.1051/aas:1999518
dc.rights.none.fl_str_mv (c) The European Southern Observatory, 1999
info:eu-repo/semantics/openAccess
rights_invalid_str_mv (c) The European Southern Observatory, 1999
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
dc.source.none.fl_str_mv Articles publicats en revistes (Física Quàntica i Astrofísica)
reponame:Dipòsit Digital de la UB
instname:Universidad de Barcelona
instname_str Universidad de Barcelona
reponame_str Dipòsit Digital de la UB
collection Dipòsit Digital de la UB
repository.name.fl_str_mv
repository.mail.fl_str_mv
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score 15.300719

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