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tokens: and also separately on the blue ([3600, 5500] Å) and red ([5500, 7200] Å) regions. The cyan contours overlaid correspond to 1 to 5. The three maps are similar, and the location of the solution is consistent within 1. The elongated shape of the contours, in particular, on the vs. [Fe/H] plane reflects the degeneracy between the parameters. For good data and normal stars, the maps as well as the parameters do not depend on the fitted wavelength range. Figure 6 shows the maps for G 156-031, a star at the edge of the parameter space populated by the MILES stars. The values increase sharply on the low side, resulting in a dissymmetry that is potentially at the origin of a bias. We discuss below the stars labelled in Fig. 1 and listed in Table 6 . Fig. 5 maps for HD 61913 with different fitting wavelength ranges. First with the complete wavelength range used (36007400 Å), second 36005500 Å, and third 55007200 Å. The red crosses indicate the minimum, and the cyan crosses the compiled parameters. The inner contour in cyan correspond to the external errors, and the other contours correspond to the 2, 3, 4 ... levels. Table 6 Remarkable stars labelled in Fig. 1 . (1) V1855 Ori = MS 0515.4-0710 (MILES 175)is a K0 or K2 type star. V1855 Ori and MS0515.4-0710 currently appear as two distinct sources in SIM-BAD, but their cross-identification with a unique sourceleaves no doubt, and allows us to complete our compilation. Favata et al. (1997) and Ce-narro et al. (2007) determined[4570, 3.50, 0.16] using the Strömgren photometry of Moraleet al. (1996) and the calibration re-lation of Alonso et al. (1996) . Xing (2010) gives [en-tity!#x2009!]= 4908 K and = 4.45 dex,computed from the colour and calibrations of Casagrande et al. (2006) . Biazzo et al. (2012) give [5100, 4.2, 0.05], based on high-resolution spectroscopic observations. Martin et al. (1994) adopted = 5150 K from their own relation between the spectral type and the temperature. In our compilation we adopt the average parameters [4860, 4.05, 0.10]. The parameters obtained after fitting the blue range, [], and the red range, [], differ significantly, as is often the case for variable stars. Our adopted measurement is not discrepant with the analysis of Biazzo et al. (2012) and therefore we trust our measurements. (2) HD 113285 (MILES 459) is a M8 III type pulsating variable star. This star belongs to the LICK/IDS library ( Worthey et al. 1994 ). Gorgas et al. (1999) determined = 2924 K by extrapolating the versus spectral type relation of Ridgway et al. (1980) . Gorlova et al. (2003) obtained = K. The parameter was derived from the spectral type and was obtained from , luminosity, and mass. McDonald et al. (2012) derived = 2602 K using spectral energy distribution (SED) fitting, neglecting Galactic extinction and assuming a solar composition. The authors PVK adopted [], and in our compilation we adopt the average of the available measurements [], where = 0.0 dex is a reasonable guess for this type