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Fig. 3

image

Optical (Gaia) to near-infrared (2MASS) CMD with the same stars (and symbols) as in Fig. 2. Only part of the late-M, early-L dwarfs, and M/L subdwarfs from Dupuy & Liu (2012) could be identified in Gaia (see text). As in Fig. 2, the absolute Gaia magnitudes MG of TGAS stars and UCAC5 CPM candidates are based on TGAS parallaxes, whereas those of the comparison objects are based on the parallaxes from Dupuy & Liu (2012). Objects located below the dashed lines in this figure and in Fig. 2 were considered as WDs.

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