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Catalog Service:
Photmetry and spectroscopy of PMS stars in NGC 2264

Short name: J/ApJ/831/116
IVOA Identifier: ivo://CDS.VizieR/J/ApJ/831/116
DOI (Digital Object Identifier): 10.26093/cds/vizier.18310116
Publisher: CDS[+][Pub. ID]
More Info: https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/831/116
VO Compliance: Level 2: This is a VO-compliant resource.
Status: active
Registered: 2018 Apr 20 06:58:14Z
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Description


The timescale of cluster formation is an essential parameter in order to understand the formation process of star clusters. Pre-main sequence (PMS) stars in nearby young open clusters reveal a large spread in brightness. If the spread were considered to be a result of a real spread in age, the corresponding cluster formation timescale would be about 5-20Myr. Hence it could be interpreted that star formation in an open cluster is prolonged for up to a few tens of Myr. However, difficulties in reddening correction, observational errors, and systematic uncertainties introduced by imperfect evolutionary models for PMS stars can result in an artificial age spread. Alternatively, we can utilize Li abundance as a relative age indicator of PMS star to determine the cluster formation timescale. The optical spectra of 134 PMS stars in NGC 2264 have been obtained with MMT/Hectochelle. The equivalent widths have been measured for 86 PMS stars with a detectable Li line (3500<{T}_eff[K]_<=6500).

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