Model calculations

We have calculated the models presented in this paper using our multipurpose model atmosphere code PHOENIX, version 10.7. Details of the code and the general input physics setup are discussed in and and references therein. The model atmospheres presented here were calculated with the same general input physics as in NG-giant. However, the change of the line lists has some impact on the model structure and synthetic spectra (see below). Our combined molecular line list includes about 550 million molecular lines. These lines are treated with a direct opacity sampling technique where each line has its individual Voigt (for strong lines) or Gauss (weak lines) line profile . The number of lines selected by this procedure depends on the the model parameters. Typically, the smallest amounts of molecular lines are selected at the cool and hot ends of the grid, e.g., about 75 million for $\hbox{$\,T_{\rm eff}$}=2000\,{\rm K}$,$\log(g)=3.5$ and 80 million for $\hbox{$\,T_{\rm eff}$}=4000\,{\rm K}$, $\log(g)=2.0$. The maximum number of selected molecular lines is about 215 million at $\hbox{$\,T_{\rm eff}$}=3000\,{\rm K}$, $\log(g)=2.0$ (all data are for solar abundances).

. The number of lines selected by this procedure depends on the the model parameters. Typically, the smallest amounts of molecular lines are selected at the cool and hot ends of the grid, e.g., about 75 million for $\hbox{$\,T_{\rm eff}$}=2000\,{\rm K}$,$\log(g)=3.5$ and 80 million for $\hbox{$\,T_{\rm eff}$}=4000\,{\rm K}$, $\log(g)=2.0$. The maximum number of selected molecular lines is about 215 million at $\hbox{$\,T_{\rm eff}$}=3000\,{\rm K}$, $\log(g)=2.0$ (all data are for solar abundances).