The Gaia -ESO Survey: N -body modelling of the Gamma Velorum cluster

The Gaia-ESO Survey has recently unveiled the complex kinematic signature of the Gamma Velorum cluster: this cluster is composed of two kinematically distinct populations (hereafter, population A and B), showing two different velocity dispersions and a relative ∼ 2 km? s<sup>-1</sup> rad...

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Autores: Mapelli, M., Vallenari, A., Jeffries, R. D., Gavagnin, E., Cantat-Gaudin, T., Sacco, G. G., Meyer, M. R., Alfaro, Emilio J., Costado, M. T., Damiani, F., Frasca, A., Lanzafame, A. C., Randich, S., Sordo, R., Zaggia, S., Micela, G., Flaccomio, E., Pancino, E., Bergemann, M., Hourihane, A., Lardo, C., Magrini, L., Morbidelli, L., Prisinzano, L., Worley, C. C.
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2015
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/388114
Acceso en línea:http://hdl.handle.net/10261/388114
Access Level:acceso abierto
Palabra clave:Methods: numerical
Open clusters and associations: individual: Gamma Velorum cluster
Stars: formation
Stars: kinematics and dynamics
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network_acronym_str ES
network_name_str España
repository_id_str
dc.title.none.fl_str_mv The Gaia -ESO Survey: N -body modelling of the Gamma Velorum cluster
title The Gaia -ESO Survey: N -body modelling of the Gamma Velorum cluster
spellingShingle The Gaia -ESO Survey: N -body modelling of the Gamma Velorum cluster
Mapelli, M.
Methods: numerical
Open clusters and associations: individual: Gamma Velorum cluster
Stars: formation
Stars: kinematics and dynamics
title_short The Gaia -ESO Survey: N -body modelling of the Gamma Velorum cluster
title_full The Gaia -ESO Survey: N -body modelling of the Gamma Velorum cluster
title_fullStr The Gaia -ESO Survey: N -body modelling of the Gamma Velorum cluster
title_full_unstemmed The Gaia -ESO Survey: N -body modelling of the Gamma Velorum cluster
title_sort The Gaia -ESO Survey: N -body modelling of the Gamma Velorum cluster
dc.creator.none.fl_str_mv Mapelli, M.
Vallenari, A.
Jeffries, R. D.
Gavagnin, E.
Cantat-Gaudin, T.
Sacco, G. G.
Meyer, M. R.
Alfaro, Emilio J.
Costado, M. T.
Damiani, F.
Frasca, A.
Lanzafame, A. C.
Randich, S.
Sordo, R.
Zaggia, S.
Micela, G.
Flaccomio, E.
Pancino, E.
Bergemann, M.
Hourihane, A.
Lardo, C.
Magrini, L.
Morbidelli, L.
Prisinzano, L.
Worley, C. C.
author Mapelli, M.
author_facet Mapelli, M.
Vallenari, A.
Jeffries, R. D.
Gavagnin, E.
Cantat-Gaudin, T.
Sacco, G. G.
Meyer, M. R.
Alfaro, Emilio J.
Costado, M. T.
Damiani, F.
Frasca, A.
Lanzafame, A. C.
Randich, S.
Sordo, R.
Zaggia, S.
Micela, G.
Flaccomio, E.
Pancino, E.
Bergemann, M.
Hourihane, A.
Lardo, C.
Magrini, L.
Morbidelli, L.
Prisinzano, L.
Worley, C. C.
author_role author
author2 Vallenari, A.
Jeffries, R. D.
Gavagnin, E.
Cantat-Gaudin, T.
Sacco, G. G.
Meyer, M. R.
Alfaro, Emilio J.
Costado, M. T.
Damiani, F.
Frasca, A.
Lanzafame, A. C.
Randich, S.
Sordo, R.
Zaggia, S.
Micela, G.
Flaccomio, E.
Pancino, E.
Bergemann, M.
Hourihane, A.
Lardo, C.
Magrini, L.
Morbidelli, L.
Prisinzano, L.
Worley, C. C.
author2_role author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
dc.contributor.none.fl_str_mv Science and Technology Facilities Council (UK)
European Research Council
European Commission
Leverhulme Trust
Istituto Nazionale di Astrofisica
Ministero dell'Istruzione, dell'Università e della Ricerca
European Science Foundation
Consejo Nacional de Ciencia y Tecnología (México)
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Methods: numerical
Open clusters and associations: individual: Gamma Velorum cluster
Stars: formation
Stars: kinematics and dynamics
topic Methods: numerical
Open clusters and associations: individual: Gamma Velorum cluster
Stars: formation
Stars: kinematics and dynamics
description The Gaia-ESO Survey has recently unveiled the complex kinematic signature of the Gamma Velorum cluster: this cluster is composed of two kinematically distinct populations (hereafter, population A and B), showing two different velocity dispersions and a relative ∼ 2 km? s<sup>-1</sup> radial velocity (RV) shift. In this paper, we propose that the two populations of the Gamma Velorum cluster originate from two different sub-clusters, born from the same parent molecular cloud. We investigate this possibility by means of direct-summation N-body simulations. Our scenario is able to reproduce not only the RV shift and the different velocity dispersions, but also the different centroid (∼0.5 pc), the different spatial concentration and the different line-of-sight distance (∼5 pc) of the two populations. The observed 1-2 Myr age difference between the two populations is also naturally explained by our scenario, in which the two sub-clusters formed in two slightly different star formation episodes. Our simulations suggest that population B is strongly supervirial, while population A is close to virial equilibrium. We discuss the implications of our models for the formation of young star clusters and OB associations in the Milky Way. © 2015 ESO.
publishDate 2015
dc.date.none.fl_str_mv 2015
2025
2025
2025
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
Publisher's version
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/388114
url http://hdl.handle.net/10261/388114
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv #PLACEHOLDER_PARENT_METADATA_VALUE#
info:eu-repo/grantAgreement/EC/FP7/320360
http://dx.doi.org/10.1051/0004-6361/201425514
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
dc.source.none.fl_str_mv reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC
instname:Consejo Superior de Investigaciones Científicas (CSIC)
instname_str Consejo Superior de Investigaciones Científicas (CSIC)
reponame_str DIGITAL.CSIC. Repositorio Institucional del CSIC
collection DIGITAL.CSIC. Repositorio Institucional del CSIC
repository.name.fl_str_mv
repository.mail.fl_str_mv
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spelling The Gaia -ESO Survey: N -body modelling of the Gamma Velorum clusterMapelli, M.Vallenari, A.Jeffries, R. D.Gavagnin, E.Cantat-Gaudin, T.Sacco, G. G.Meyer, M. R.Alfaro, Emilio J.Costado, M. T.Damiani, F.Frasca, A.Lanzafame, A. C.Randich, S.Sordo, R.Zaggia, S.Micela, G.Flaccomio, E.Pancino, E.Bergemann, M.Hourihane, A.Lardo, C.Magrini, L.Morbidelli, L.Prisinzano, L.Worley, C. C.Methods: numericalOpen clusters and associations: individual: Gamma Velorum clusterStars: formationStars: kinematics and dynamicsThe Gaia-ESO Survey has recently unveiled the complex kinematic signature of the Gamma Velorum cluster: this cluster is composed of two kinematically distinct populations (hereafter, population A and B), showing two different velocity dispersions and a relative ∼ 2 km? s<sup>-1</sup> radial velocity (RV) shift. In this paper, we propose that the two populations of the Gamma Velorum cluster originate from two different sub-clusters, born from the same parent molecular cloud. We investigate this possibility by means of direct-summation N-body simulations. Our scenario is able to reproduce not only the RV shift and the different velocity dispersions, but also the different centroid (∼0.5 pc), the different spatial concentration and the different line-of-sight distance (∼5 pc) of the two populations. The observed 1-2 Myr age difference between the two populations is also naturally explained by our scenario, in which the two sub-clusters formed in two slightly different star formation episodes. Our simulations suggest that population B is strongly supervirial, while population A is close to virial equilibrium. We discuss the implications of our models for the formation of young star clusters and OB associations in the Milky Way. © 2015 ESO.We thank the anonymous referee for the careful reading of the manuscript and for the helpful comments. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 188.B-3002. These data products have been processed by the Cambridge Astronomy Survey Unit (CASU) at the Institute of Astronomy, University of Cambridge, and by the FLAMES/UVES reduction team at INAF/Osservatorio Astrofisico di Arcetri. These data have been obtained from the Gaia-ESO Survey Data Archive, prepared and hosted by the Wide Field Astronomy Unit, Institute for Astronomy, University of Edinburgh, which is funded by the UK Science and Technology Facilities Council. This work was partly supported by the European Union FP7 programme through ERC grant number 320360 and by the Leverhulme Trust through grant RPG-2012-541. We acknowledge the support from INAF and Ministero dell’ Istruzione, dell’ Università’ e della Ricerca (MIUR) in the form of the grant “Premiale VLT 2012”. The results presented here benefit from discussions held during the Gaia-ESO workshops and conferences supported by the ESF (European Science Foundation) through the GREAT Research Network Programme. M.M. acknowledges financial support from the Italian Ministry of Education, University and Research (MIUR) through grant FIRB 2012 RBFR12PM1F, from INAF through grant PRIN-2011-1 and from CONACyT through grant 169554. The authors acknowledge the CINECA Award N. HP10B3BJEW, HP10CLI3BX, HP10CXB7O8, HP10C894X7, HP10CGUBV0, HP10CP6XSO and HP10C3ANJY for the availability of high performance computing resources and support.EDP SciencesScience and Technology Facilities Council (UK)European Research CouncilEuropean CommissionLeverhulme TrustIstituto Nazionale di AstrofisicaMinistero dell'Istruzione, dell'Università e della RicercaEuropean Science FoundationConsejo Nacional de Ciencia y Tecnología (México)Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]2025202520152025info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/388114reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/EC/FP7/320360http://dx.doi.org/10.1051/0004-6361/201425514Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/3881142026-05-22T06:33:51Z
score 15,811543

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