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Table 4

Photometry and literature classification for the M-type stars with statistical membership to the NGC 2264 clustered population identified in this study.

RA Dec r-mag i-mag J-mag r-err i-err J-err (r,i)_source J_source AV CSIMon-# Memb
100.39517 9.83891 20.19 18.263 15.606 0.05 0.003 0.008 CSI 2264 UKIDSS 0.205 000002 2
100.32146 9.89437 17.574 16.331 14.192 0.006 0.004 0.005 Pan-STARRS1 UKIDSS 0.933 000005 1
100.32758 9.90211 21.89 19.505 16.084 0.17 0.019 0.008 Pan-STARRS1 UKIDSS 2.301 000013 2
100.30493 9.91909 16.073 15.0328 12.9150 0.003 0.0006 0.0009 CSI 2264 UKIDSS 1.577 000018 1
100.26904 10.01185 17.798 16.2571 13.931 0.008 0.0010 0.007 CSI 2264 UKIDSS 0.527 000022 2
100.30178 9.91670 18.212 16.8474 14.676 0.010 0.0014 0.007 CSI 2264 UKIDSS 0.565 000023 1
100.27161 10.00526 17.180 15.5069 13.052 0.005 0.0007 0.022 CSI 2264 2MASS 0.540 000026 2
100.36946 9.89951 19.95 18.098 15.328 0.03 0.008 0.004 Pan-STARRS1 UKIDSS 1.461 000032 1
100.35084 9.89526 19.26 17.318 14.594 0.04 0.008 0.005 Pan-STARRS1 UKIDSS 0.552 000039 2
100.43947 9.92845 18.314 16.7654 14.410 0.011 0.0013 0.007 CSI 2264 UKIDSS 0.666 000042 1

Notes. A full version of the table is available in electronic form at the CDS. A portion is shown here for guidance regarding its form and content. “r-mag, i-mag” = photometry calibrated to the SDSS system as described in Sect. 2.4. “r-err, i-err, J-err” = photometric uncertainties computed taking into account the instrumental errors and the calibration relationships. “(r, i)_source” = survey from which the original optical photometry for the corresponding object was extracted. Possible values are: CSI 2264, Pan-STARRS1, IPHAS, SDSS (see Sect. 2.1). “J_source” = survey from which the J-band photometry for the corresponding object was extracted. Possible values are: UKIDSS, 2MASS (see Sect. 2.2). “CSIMon-#” = object identifier in the CSI 2264 master catalog, if present. “Memb” = membership flag associated with the corresponding source in the CSI 2264 catalog, if present. Possible values are: 1, 2, 0, −1 (see Sect. 4.2).

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