and mixing information for the CO$^{5}$BOLD code [@steiner07; @freytag10a]. These models are valid for a wide range of T$_{\rm eff}$ (400–8000K), gravities ($\log$(g)=2.5–6.0 dex), and metallicities (from $-$5.0 to solar). The synthetic SEDs span the wavelength range from 10Å up to 1000$\mu$m. The stellar metallicity is defined by the total iron content of a star because iron is the easiest species to measure spectroscopically. The abundance ratio \[Fe/H\] is defined as the logarithm of the ratio of a star’s iron abundance compared to that of the Sun, where $-$1.0 dex means that a star has one-tenth of the solar metallicity. The determination of the metallicity is only valid if the abundance of all elements follow the abundance of iron. However, this statement might not be totally true in the case of halo dwarfs that suffered different nucleosynthesis events.

We downloaded the spectra from the CIFIST2011 grid[^5] and considered the ranges that encompass the spectral types of the three metallicity classes: T$_{\rm eff}$=4000–2500K, gravity ($\log$g=4.5–5.5 dex), and metallicity \[M/H\] (from $-$2.5 dex to solar). These models assumes solar abundance values (Z=0.0153, Z/X=0.0209) from @caffau11a with alpha enhancement taken into account as follows: \[alpha/H\]=$+$0.2 relative to solar for \[M/H\]=$-$0.5 dex and \[alpha/H\]=$+$0.4 