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dc.contributor.authorBravi, L
dc.contributor.authorZari, E
dc.contributor.authorSacco, GG
dc.contributor.authorRandich, S
dc.contributor.authorJeffries, RD
dc.contributor.authorJackson, RJ
dc.contributor.authorFranciosini, E
dc.contributor.authorMoraux, E
dc.contributor.authorLopez-Santiago, J
dc.contributor.authorPancino, E
dc.contributor.authorSpina, L
dc.contributor.authorWright, N
dc.contributor.authorJimenez-Esteban, FM
dc.contributor.authorKlutsch, A
dc.contributor.authorRoccatagliata, V
dc.contributor.authorGilmore, G
dc.contributor.authorBragaglia, A
dc.contributor.authorFlaccomio, E
dc.contributor.authorFrancois, P
dc.contributor.authorKoposov, SE
dc.contributor.authorBayo, A
dc.contributor.authorCarraro, G
dc.contributor.authorCostado, MT
dc.contributor.authorDamiani, F
dc.contributor.authorFrasca, A
dc.contributor.authorHourihane, A
dc.contributor.authorJofre, P
dc.contributor.authorLardo, C
dc.contributor.authorLewis, J
dc.contributor.authorMagrini, L
dc.contributor.authorMorbidelli, L
dc.contributor.authorPrisinzano, L
dc.contributor.authorSousa, SG
dc.contributor.authorWorley, CC
dc.contributor.authorZaggia, S
dc.date.accessioned2018-09-10T09:57:05Z
dc.date.available2018-09-10T09:57:05Z
dc.date.issued2018-07-06
dc.identifier.issn1432-0746
dc.identifier.urihttps://www.repository.cam.ac.uk/handle/1810/279978
dc.description.abstractContext. The origin and dynamical evolution of star clusters is an important topic in stellar astrophysics. Several models have been proposed to understand the formation of bound and unbound clusters and their evolution, and these can be tested by examining the kinematical and dynamical properties of clusters over a wide range of ages and masses. Aims. We use the Gaia -ESO Survey products to study four open clusters (IC 2602, IC 2391, IC 4665, and NGC 2547) that lie in the age range between 20 and 50 Myr. Methods. We employ the gravity index γ and the equivalent width of the lithium line at 6708 Å, together with e ff ective temperature T e ff , and the metallicity of the stars in order to discard observed contaminant stars. Then, we derive the cluster radial velocity disper- sions σ c , the total cluster mass M tot , and the half mass radius r hm . Using the Gaia -DR1 TGAS catalogue, we independently derive the intrinsic velocity dispersion of the clusters from the astrometric parameters of cluster members. Results. The intrinsic radial velocity dispersions derived by the spectroscopic data are larger than those derived from the TGAS data, possibly due to the di ff erent masses of the considered stars. Using M tot and r hm we derive the virial velocity dispersion σ v ir and we find that three out of four clusters are supervirial. This result is in agreement with the hypothesis that these clusters are dispersing, as predicted by the "residual gas expulsion" scenario. However, recent simulations show that the virial ratio of young star clusters may be overestimated if it is determined using the global velocity dispersion, since the clusters are not fully relaxed.
dc.publisherEDP Sciences
dc.subjectstars: pre-main sequence
dc.subjectstars: kinematics and dynamics
dc.subjectopen clusters and associations: general
dc.subjectstars: formation
dc.subjecttechniques: spectroscopic
dc.subjecttechniques: radial velocities
dc.titleThe Gaia-ESO Survey: a kinematical and dynamical study of four young open clusters
dc.typeArticle
prism.numberA37
prism.publicationDate2018
prism.publicationNameAstronomy & Astrophysics
prism.volume615
dc.identifier.doi10.17863/CAM.27344
dcterms.dateAccepted2018-03-03
rioxxterms.versionofrecord10.1051/0004-6361/201832645
rioxxterms.versionVoR
rioxxterms.licenseref.urihttp://www.rioxx.net/licenses/all-rights-reserved
rioxxterms.licenseref.startdate2018-07-06
dc.contributor.orcidGilmore, Gerard [0000-0003-4632-0213]
dc.contributor.orcidWorley, Clare [0000-0001-9310-2898]
dc.identifier.eissn1432-0746
dc.publisher.urlhttp://dx.doi.org/10.1051/0004-6361/201832645
rioxxterms.typeJournal Article/Review
pubs.funder-project-idLeverhulme Trust (RPG-2012-541)
pubs.funder-project-idEuropean Research Council (320360)
pubs.funder-project-idEuropean Commission Horizon 2020 (H2020) Research Infrastructures (RI) (653477)
cam.issuedOnline2018-06-06


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