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Fig. 4


Near-infrared (2MASS) CMD for our selected UPC 25 pc sample. Absolute magnitudes are based on UPC parallaxes. The start and end values of both axes are the same as in Fig. 2, the dashed line shows our previously chosen limit for the WD region in this CMD (Eq. (3)), the dotted line again indicates the WD/subdwarf dividing line of Subasavage et al. (2017). Stars with photometric quality ‘AAA’ in 2MASS are plotted as plus signs. Overplotted as red filled squares, blue open squares, and black dots are stars without previous parallax measurements (UPC srcflg = 0), with already published data in Finch & Zacharias (2016b) (srcflg = 3), and in the literature (srcflg = 1, 4, 5), respectively. All WD candidates, defined by us as falling below the dashed lines in this figure and in Fig. 5, are shown as open diamonds. The new WD candidates 1 and 2 (already found in our TGAS CPM search in UCAC5), and 4 are indicated. A close binary cool WD is also labelled.

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