Figures

 

Figure:   Comparison of the models presented in this paper (full line) to NG-giant models (dotted line) in the optical spectrum. The resolution has been reduced to $5\hbox{\AA}$. The top panel shows models with $\hbox{$\,T_{\rm eff}$}=3000\,{\rm K}$, the bottom panel for $\hbox{$\,T_{\rm eff}$}=4000\,{\rm K}$, both sets have $\log(g)=2.0$ and solar abundances.

 

Figure:   Comparison of the models presented in this paper (full line) to NG-giant models (dotted line) in the near IR spectral range. The resolution has been reduced to $15\hbox{\AA}$. The top panel shows models with $\hbox{$\,T_{\rm eff}$}=2000\,{\rm K}$, the middle panel shows $\hbox{$\,T_{\rm eff}$}=2000\,{\rm K}$, and the bottom panel for $\hbox{$\,T_{\rm eff}$}=4000\,{\rm K}$, all three sets have $\log(g)=2.0$ and solar abundances.

 

Figure 3:  Models with multiple radiative/convective zones. Each point marks a model that has multiple radiative/convective zones. To minimize the number of figures we plotted all metallicities in one graph and used different symbols for different metallicities as indicated in the figure. The log(g) values for sub- and super-solar metallicities have been slightly shifted to keep the figure legible. Note the continuous distribution of models with multiple radiative/convective zones, which is also continuous is metallicity space.

 

Figure:  Absorption coefficients versus optical depth at 1.2. All models have z=-0.3 and log(g)=2.5. The effective temperature of the models are from top to bottom 2800 K, 3000 K, 3200 K and 3400 K. The cross hatched regions are the convective zones. For reference, we indicate the gas pressure and the gas temperature at the respective optical depth at the top of each figure. To the right we labeled the most important opacity sources.

 

Figure:   Comparison of low-resolution (about $50\hbox{\AA}$) synthetic spectra for models with $\hbox{$\,T_{\rm eff}$}=3400\,{\rm K}$, $\log(g)=2.0$ and solar abundances (full line), $[{\rm M/H}]=-0.3$ (dotted line) and $[{\rm M/H}]=+0.3$ (dashed line).

 

Figure:   Comparison of low-resolution (about $50\hbox{\AA}$) synthetic spectra for models with $\hbox{$\,T_{\rm eff}$}=3400\,{\rm K}$, $\log(g)=3.5$ and solar abundances (full line), $[{\rm M/H}]=-0.3$ (dotted line) and $[{\rm M/H}]=+0.3$ (dashed line).

 

Figure:   Comparison of low-resolution (about $50\hbox{\AA}$) synthetic spectra for models with $\hbox{$\,T_{\rm eff}$}=2400\,{\rm K}$, $\log(g)=2.0$ and solar abundances (full line), $[{\rm M/H}]=-0.3$ (dotted line) and $[{\rm M/H}]=+0.3$ (dashed line).

 

Figure:   Comparison of low-resolution (about $50\hbox{\AA}$) synthetic spectra for models with $\hbox{$\,T_{\rm eff}$}=2400\,{\rm K}$, $\log(g)=3.5$ and solar abundances (full line), $[{\rm M/H}]=-0.3$ (dotted line) and $[{\rm M/H}]=+0.3$ (dashed line).