The multiplicity fraction in 202 open clusters from Gaia

Autores
Donada, J.; Anders, F.; Jordi, C.; Masana, E.; Gieles, M.; Perren, Gabriel Ignacio; Balaguer Núñez, L.; Castro Ginard, A.; Cantat Gaudin, T.; Casamiquela, L.
Año de publicación
2023
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
In this study, we estimate the fraction of binaries with high mass ratios for 202 open clusters in the extended solar neighbourhood (closer than 1.5 kpc from the Sun). This is one of the largest homogeneous catalogues of multiplicity fractions in open clusters to date, including the unresolved and total (close-binary) multiplicity fractions of main-sequence systems with mass ratio larger than 0.6+0.05−0.15. The unresolved multiplicity fractions are estimated applying a flexible mixture model to the observed Gaia colour-magnitude diagrams of the open clusters. Then we use custom Gaia simulations to account for the resolved systems and derive the total multiplicity fractions. The studied open clusters have ages between 6.6 Myr and 3.0 Gyr and total high-mass-ratio multiplicity fractions between 6% and 80%, with a median of 18%. The multiplicity fractions increase with the mass of the primary star, as expected. The average multiplicity fraction per cluster displays an overall decreasing trend with the open cluster age up to ages about 100 Myr, above which the trend increases. Our simulations show that most of this trend is caused by complex selection effects (introduced by the mass dependence of the multiplicity fraction and the magnitude limit of our sample). Furthermore, the multiplicity fraction is not significantly correlated with the clusters´ position in the Galaxy. The spread in multiplicity fraction decreases significantly with the number of cluster members (used as a proxy for cluster mass). We also find that the multiplicity fraction decreases with metallicity, in line with recent studies using field stars.
Fil: Donada, J.. Universidad de Barcelona; España
Fil: Anders, F.. Universidad de Barcelona; España
Fil: Jordi, C.. Universidad de Barcelona; España
Fil: Masana, E.. Universidad de Barcelona; España
Fil: Gieles, M.. Universidad de Barcelona; España
Fil: Perren, Gabriel Ignacio. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Balaguer Núñez, L.. Universidad de Barcelona; España
Fil: Castro Ginard, A.. Leiden Observatory; Países Bajos
Fil: Cantat Gaudin, T.. Max-planck-institut Für Astronomie; Alemania
Fil: Casamiquela, L.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Materia
GALAXY
EVOLUTION
OPEN
CLUSTER
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/234102
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/234102
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling The multiplicity fraction in 202 open clusters from GaiaDonada, J.Anders, F.Jordi, C.Masana, E.Gieles, M.Perren, Gabriel IgnacioBalaguer Núñez, L.Castro Ginard, A.Cantat Gaudin, T.Casamiquela, L.GALAXYEVOLUTIONOPENCLUSTERhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1In this study, we estimate the fraction of binaries with high mass ratios for 202 open clusters in the extended solar neighbourhood (closer than 1.5 kpc from the Sun). This is one of the largest homogeneous catalogues of multiplicity fractions in open clusters to date, including the unresolved and total (close-binary) multiplicity fractions of main-sequence systems with mass ratio larger than 0.6+0.05−0.15. The unresolved multiplicity fractions are estimated applying a flexible mixture model to the observed Gaia colour-magnitude diagrams of the open clusters. Then we use custom Gaia simulations to account for the resolved systems and derive the total multiplicity fractions. The studied open clusters have ages between 6.6 Myr and 3.0 Gyr and total high-mass-ratio multiplicity fractions between 6% and 80%, with a median of 18%. The multiplicity fractions increase with the mass of the primary star, as expected. The average multiplicity fraction per cluster displays an overall decreasing trend with the open cluster age up to ages about 100 Myr, above which the trend increases. Our simulations show that most of this trend is caused by complex selection effects (introduced by the mass dependence of the multiplicity fraction and the magnitude limit of our sample). Furthermore, the multiplicity fraction is not significantly correlated with the clusters´ position in the Galaxy. The spread in multiplicity fraction decreases significantly with the number of cluster members (used as a proxy for cluster mass). We also find that the multiplicity fraction decreases with metallicity, in line with recent studies using field stars.Fil: Donada, J.. Universidad de Barcelona; EspañaFil: Anders, F.. Universidad de Barcelona; EspañaFil: Jordi, C.. Universidad de Barcelona; EspañaFil: Masana, E.. Universidad de Barcelona; EspañaFil: Gieles, M.. Universidad de Barcelona; EspañaFil: Perren, Gabriel Ignacio. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Balaguer Núñez, L.. Universidad de Barcelona; EspañaFil: Castro Ginard, A.. Leiden Observatory; Países BajosFil: Cantat Gaudin, T.. Max-planck-institut Für Astronomie; AlemaniaFil: Casamiquela, L.. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaEDP Sciences2023-01info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/234102Donada, J.; Anders, F.; Jordi, C.; Masana, E.; Gieles, M.; et al.; The multiplicity fraction in 202 open clusters from Gaia; EDP Sciences; Astronomy and Astrophysics; 675; A89; 1-2023; 1-170004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2023/07/aa45219-22/aa45219-22.htmlinfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202245219info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:53:31Zoai:ri.conicet.gov.ar:11336/234102instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-29 09:53:31.701CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The multiplicity fraction in 202 open clusters from Gaia
title The multiplicity fraction in 202 open clusters from Gaia
spellingShingle The multiplicity fraction in 202 open clusters from Gaia
Donada, J.
GALAXY
EVOLUTION
OPEN
CLUSTER
title_short The multiplicity fraction in 202 open clusters from Gaia
title_full The multiplicity fraction in 202 open clusters from Gaia
title_fullStr The multiplicity fraction in 202 open clusters from Gaia
title_full_unstemmed The multiplicity fraction in 202 open clusters from Gaia
title_sort The multiplicity fraction in 202 open clusters from Gaia
dc.creator.none.fl_str_mv Donada, J.
Anders, F.
Jordi, C.
Masana, E.
Gieles, M.
Perren, Gabriel Ignacio
Balaguer Núñez, L.
Castro Ginard, A.
Cantat Gaudin, T.
Casamiquela, L.
author Donada, J.
author_facet Donada, J.
Anders, F.
Jordi, C.
Masana, E.
Gieles, M.
Perren, Gabriel Ignacio
Balaguer Núñez, L.
Castro Ginard, A.
Cantat Gaudin, T.
Casamiquela, L.
author_role author
author2 Anders, F.
Jordi, C.
Masana, E.
Gieles, M.
Perren, Gabriel Ignacio
Balaguer Núñez, L.
Castro Ginard, A.
Cantat Gaudin, T.
Casamiquela, L.
author2_role author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv GALAXY
EVOLUTION
OPEN
CLUSTER
topic GALAXY
EVOLUTION
OPEN
CLUSTER
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv In this study, we estimate the fraction of binaries with high mass ratios for 202 open clusters in the extended solar neighbourhood (closer than 1.5 kpc from the Sun). This is one of the largest homogeneous catalogues of multiplicity fractions in open clusters to date, including the unresolved and total (close-binary) multiplicity fractions of main-sequence systems with mass ratio larger than 0.6+0.05−0.15. The unresolved multiplicity fractions are estimated applying a flexible mixture model to the observed Gaia colour-magnitude diagrams of the open clusters. Then we use custom Gaia simulations to account for the resolved systems and derive the total multiplicity fractions. The studied open clusters have ages between 6.6 Myr and 3.0 Gyr and total high-mass-ratio multiplicity fractions between 6% and 80%, with a median of 18%. The multiplicity fractions increase with the mass of the primary star, as expected. The average multiplicity fraction per cluster displays an overall decreasing trend with the open cluster age up to ages about 100 Myr, above which the trend increases. Our simulations show that most of this trend is caused by complex selection effects (introduced by the mass dependence of the multiplicity fraction and the magnitude limit of our sample). Furthermore, the multiplicity fraction is not significantly correlated with the clusters´ position in the Galaxy. The spread in multiplicity fraction decreases significantly with the number of cluster members (used as a proxy for cluster mass). We also find that the multiplicity fraction decreases with metallicity, in line with recent studies using field stars.
Fil: Donada, J.. Universidad de Barcelona; España
Fil: Anders, F.. Universidad de Barcelona; España
Fil: Jordi, C.. Universidad de Barcelona; España
Fil: Masana, E.. Universidad de Barcelona; España
Fil: Gieles, M.. Universidad de Barcelona; España
Fil: Perren, Gabriel Ignacio. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Balaguer Núñez, L.. Universidad de Barcelona; España
Fil: Castro Ginard, A.. Leiden Observatory; Países Bajos
Fil: Cantat Gaudin, T.. Max-planck-institut Für Astronomie; Alemania
Fil: Casamiquela, L.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
description In this study, we estimate the fraction of binaries with high mass ratios for 202 open clusters in the extended solar neighbourhood (closer than 1.5 kpc from the Sun). This is one of the largest homogeneous catalogues of multiplicity fractions in open clusters to date, including the unresolved and total (close-binary) multiplicity fractions of main-sequence systems with mass ratio larger than 0.6+0.05−0.15. The unresolved multiplicity fractions are estimated applying a flexible mixture model to the observed Gaia colour-magnitude diagrams of the open clusters. Then we use custom Gaia simulations to account for the resolved systems and derive the total multiplicity fractions. The studied open clusters have ages between 6.6 Myr and 3.0 Gyr and total high-mass-ratio multiplicity fractions between 6% and 80%, with a median of 18%. The multiplicity fractions increase with the mass of the primary star, as expected. The average multiplicity fraction per cluster displays an overall decreasing trend with the open cluster age up to ages about 100 Myr, above which the trend increases. Our simulations show that most of this trend is caused by complex selection effects (introduced by the mass dependence of the multiplicity fraction and the magnitude limit of our sample). Furthermore, the multiplicity fraction is not significantly correlated with the clusters´ position in the Galaxy. The spread in multiplicity fraction decreases significantly with the number of cluster members (used as a proxy for cluster mass). We also find that the multiplicity fraction decreases with metallicity, in line with recent studies using field stars.
publishDate 2023
dc.date.none.fl_str_mv 2023-01
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/234102
Donada, J.; Anders, F.; Jordi, C.; Masana, E.; Gieles, M.; et al.; The multiplicity fraction in 202 open clusters from Gaia; EDP Sciences; Astronomy and Astrophysics; 675; A89; 1-2023; 1-17
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/234102
identifier_str_mv Donada, J.; Anders, F.; Jordi, C.; Masana, E.; Gieles, M.; et al.; The multiplicity fraction in 202 open clusters from Gaia; EDP Sciences; Astronomy and Astrophysics; 675; A89; 1-2023; 1-17
0004-6361
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2023/07/aa45219-22/aa45219-22.html
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202245219
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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score 13.070432

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