Testing circumstellar disk lifetimes in young embedded clusters associated with the Vela Molecular Ridge

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dc.contributor.authorMassi, F.
dc.contributor.authorDi Carlo, E.
dc.contributor.authorCodella, C.
dc.contributor.authorTesti, L.
dc.contributor.authorVanzi, L.
dc.contributor.authorGomes, J. I.
dc.date.accessioned2024-01-10T13:43:43Z
dc.date.available2024-01-10T13:43:43Z
dc.date.issued2010
dc.description.abstractContext. The Vela Molecular Ridge hosts a number of young embedded star clusters at the same evolutionary stage.
dc.description.abstractAims. We test whether the fraction of members with a circumstellar disk in a sample of clusters in the cloud D of the Vela Molecular Ridge, is consistent with relations derived for larger samples of star clusters with an age spread. In addition, we constrain the age of the young embedded star clusters associated with cloud D.
dc.description.abstractMethods. We carried out L (3.78 mu m) photometry using images of six young embedded star clusters associated with cloud D of the Vela Molecular Ridge, taken with ISAAC at the VLT. These data are complemented with the available HKs photometry. The 6 clusters are of roughly the same size and appear to be at the same evolutionary stage. The fraction of stars with a circumstellar disk was measured in each cluster by counting the fraction of sources found to have a NIR excess in colour-colour (HKsL) diagrams.
dc.description.abstractResults. The L photometry allowed us to identify the NIR counterparts of the IRAS sources associated with the clusters. The fraction of stars with a circumstellar disk appears to be constant within the errors for the 6 clusters. There is a hint that this is lower for the most massive stars. The age of the clusters is constrained to be similar to 1-2 Myr.
dc.description.abstractConclusions. The fraction of stars with a circumstellar disk in the observed sample is consistent with the relations derived from larger samples of star clusters and with other age estimates for cloud D. The fraction may be lower for the most massive stars. Our results agree with a scenario where all intermediate and low-mass stars form with a disk, whose lifetime is shorter for higher mass stars.
dc.description.funderEuropean Southern Observatory, Cerro Paranal, Chile
dc.description.funderBasal Center for Astrophysics and Associated Technologies
dc.description.funderFondecyt project
dc.fechaingreso.objetodigital2024-05-02
dc.format.extent12 páginas
dc.fuente.origenWOS
dc.identifier.doi10.1051/0004-6361/200913671
dc.identifier.issn1432-0746
dc.identifier.urihttps://doi.org/10.1051/0004-6361/200913671
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/78737
dc.identifier.wosidWOS:000280275400067
dc.information.autorucIngeniería;Vanzi L;S/I;1006591
dc.language.isoen
dc.nota.accesocontenido parcial
dc.publisherEDP SCIENCES S A
dc.revistaASTRONOMY & ASTROPHYSICS
dc.rightsacceso restringido
dc.subjectstars: formation
dc.subjectstars: pre-main sequence
dc.subjectstars: circumstellar matter
dc.subjectISM: individual objects: Vela Molecular Ridge
dc.subjectopen clusters and associations: general
dc.subjectinfrared: ISM
dc.subjectCLASS-I SOURCES
dc.subjectMAIN-SEQUENCE TRACKS
dc.subjectLOW-MASS STARS
dc.subjectCLOUD-D
dc.subjectINTRINSIC COLORS
dc.subjectPHOTOMETRY
dc.subjectCORES
dc.subjectSPECTROSCOPY
dc.subjectPROTOSTARS
dc.subjectEVOLUTION
dc.titleTesting circumstellar disk lifetimes in young embedded clusters associated with the Vela Molecular Ridge
dc.typeartículo
dc.volumen516
sipa.codpersvinculados1006591
sipa.indexWOS
sipa.indexScopus
sipa.trazabilidadCarga SIPA;09-01-2024
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