Complete list of the 1892 targets observed during GES in the NGC 2264 field, and of the measured spectroscopic parameters relevant to this study; CFHT optical photometry obtained for the same objects within CSI 2264; disk classification, accretion properties, and derived extinction and stellar parameters for the 655 cluster members identified among GES targets.
|CNAME||CSIMon-#||RA||Dec||Memb||g||r||i||Class||Acc.||γ||T eff||EW(Li)||EW(Hα)||W10%(Hα)||E(u−r)||A V||L bol||M ⋆||Age|
Notes. A full version of the table is available at the CDS. A portion is shown here for guidance regarding its form and content. “CNAME” = GES target identifier. “CSIMon-#” = Object identifier used within CSI 2264 (Cody et al. 2014). “RA, Dec” = Target coordinates. “Memb” = asterisks mark the cluster members selected among all GES targets as described in Sect. 3.1. “g, r, i” = Optical photometry obtained with CFHT/MegaCam and calibrated to the SDSS system (Venuti et al. 2014). “Class” = Object classification according to its disk properties (Lada 1987; II = disk-bearing; III = disk-free). “Acc.” = Object classification according to its accretion properties, following the criteria in Sect. 3.3 (Y = accreting, or CTTS; N = non-accreting, or WTTS). “γ” = GES gravity index (Damiani et al. 2014); typical uncertainties are of order 0.006 for γ ~ 0.85 and 0.002 for γ ~ 0.95. “Teff” = GES released effective temperature; typical uncertainties are of order 3% of the measurement. “EW(Li)” = GES released Li equivalent width; typical uncertainties range between 5 and 20 mÅ. “EW(Hα)” = GES released Hα equivalent width; typical uncertainties range between 0.1 and 0.6 Å. “W10%(Hα)” = GES released Hα width at 10% intensity; typical uncertainties range between 10 and 20 km s-1. “” = difference between the measured r−Hα IPHAS color and the threshold traced in Fig. 3 to separate the accreting and non-accreting stellar loci; values significantly larger than 0 indicate Hα emitters. “E(u−r)” = photometric UV excess measured in Venuti et al. (2014) as the difference between the observed u−r color and the reference u−r color set by the WTTS population of similar brightness; the more negative the value of E(u−r), the stronger the UV excess. “AV” = Individual extinction estimate derived in this study. “Lbol” = Bolometric luminosity derived in this study. “M⋆” = Stellar mass derived in this study. “Age” = Individual age estimated for the target using Baraffe et al.’s (2015) model isochrones.
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