and spectral type is given in Table 3. The T$_{\rm eff}$ $-$ log $g$ distribution is plotted in Figure 2. Extreme metal-poor and metal-rich compositions were also included.

![The gravity (log $g$) as a function of effective temperature (T$_{\rm eff}$) of ATLAS9 and MARCS models calculated for each composition. Acceptable models are denoted by filled circles, while models not acceptable (and missing) are denoted by open circles for the solar composition. Models with C/O $>$ 1.7 and T$_{\rm eff} < 4000$K are not published (see Section 4.2). ](figure02.eps){width="2.5in"}

All the ATLAS codes use atomic and molecular linelists made available by Kurucz on a series of CDROM [@kurucz02]. They can now be found at the Kurucz website[^5]. The molecular line lists for TiO and H$_{2}$O were provided by @schwenke01 and @partridge01, respectively, and reformatted by Kurucz in ATLAS format. These are also available for download at the Kurucz website. For these models, we used the same linelists as @castelli01, except for H$_{2}$O, for which a new Kurucz release of the @partridge01 data was adopted[^6].

The solar reference abundance table was adopted from @asplund01. Convection was turned on with the mixing length parameter set to $l/H_{p} = 1.25$, but the convective overshooting 