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Table B.1

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(ur) A V L bol M Age
(deg) (deg) (K) (mÅ) (Å) (km s-1) (L) (M) (Myr)

06392396+0942016 006120 99.84983 9.70044 17.370 14.993 13.745 1.046 4401 38
06392408+0938088 012537 99.85033 9.63578 19.672 17.960 16.982
06392497+0933151 006507 99.85404 9.55419 18.417 17.020 15.805
06392506+0942515 006066 99.85442 9.71431 * 16.952 15.684 14.842 III N 0.916 4704 492 101 –0.08 1.36 1.047 1.29 6.52
06392535+0943147 006028 99.85562 9.72075 17.210 15.345 14.378 1.003 5126 34
06392550+0931394 006491 99.85625 9.52761 * 18.226 16.746 15.808 II Y 0.881 4272 497 5.8 411 0.03 –1.18 1.03 0.377 0.94 11.0
06392585+0938112 007916 99.85771 9.63644 * 0.900 3607 548
06392623+0947066 012625 99.85929 9.78517 18.213 17.105 16.478 1.009 5998 42
06392625+0941108 001158 99.85937 9.68633 * 15.977 14.903 14.395 III N 0.945 4907 513 1.6 225 –0.08 –0.11 1.15 1.354 1.39 6.90
06392649+0943298 005862 99.86037 9.72494 18.448 16.897 16.016 1.032 5765 76

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(ur)= photometric UV excess measured in Venuti et al. (2014) as the difference between the observed ur color and the reference ur color set by the WTTS population of similar brightness; the more negative the value of E(ur), 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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