HRDs and the LDB for NGC 2547. (a) the same as in Fig. 6 and A.2 but for NGC 2547. 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 lines to 40 and 50 Ma. The figure includes: a 30 Ma and a 50 Ma isochrones from D’Antona & Mazzitelli 1994 (black dashed lines), a 35 Ma isochrone from Tognelli et al. 2011 (orange dashed dot line), a 40 Ma isochrone from Siess et al. 2000 (red dotted line). (b) Zoom on the (a) plot around the 52 radial velocity members from Jeffries et al. (2004) sample. (c) Zoom around the LDB. NGC 2547 is Ma old using the BT-Settl bolometric luminosity-age relationship (Allard et al. 2012). We show the names of all the objects but not the uncertainties (for the purposes of clarity).