HRDs and the LDB for NGC 1960. (a) Same as Fig. 6. Cyan squares are lithium-rich sources without Gaia DR2 parallaxes and purple stars are lithium upper limits or lithium-poor sources without Gaia DR2 parallaxes, both from our LDB sample (see Section 4.2); empty large black circles are confirmed multiple systems and broken lines are suspected multiple systems; over-imposed big black crosses are sources discarded as members after this work. Moreover, grey points are known members from Cantat-Gaudin et al. (2018a). Thin blue lines correspond to isochrones of 1, 10, 100 Ma, and 1 Ga from the BT-Settl models (Allard et al. 2013), while the thick blue one corresponds to 30 Ma. The figure includes: a 20 Ma and a 30 Ma isochrones from D’Antona & Mazzitelli 1994 (black dashed line), a 25 Ma isochrone from Tognelli et al. 2011 (orange dashed dot line), a 30 Ma isochrone from Siess et al. 2000 (red dotted line) and a Zero Age Main Sequence from Stahler & Palla 2005 (green solid line). (b) Zoom on the left plot. A black horizontal line marks the L_{bol LDB}, together with the 16th and 84th percentiles (dotted lines). NGC 1960 is Ma old using the BT-Settl bolometric luminosity-age relationship (Allard et al. 2012). An extensive dashed horizontal green line indicates a possible LDB upper limit (see Section 5.2).