any of the two versions of SATLAS.

Instead, extensive grids of ATLAS9 ODF model atmospheres for several metallicities were calculated by @castelli01. These grids are based on solar (or scaled solar) abundances from @grevesse01. Recently, @kirby01 provided a new ATLAS9 grid, but he used abundances from @anders01. The calculations presented in this paper are based on the more recent solar composition from @asplund01. This updated abundance table required new ODFs and Rosseland mean opacity calculations as well. Abundances from @asplund01 were chosen instead of those from newer studies [@asplund02] to match the composition of the MARCS models described below, and those available from the MARCS website.

The MARCS model atmospheres [@gustafsson01; @plez01; @gustafsson02] were developed and have been evolving in close connection with applications primarily to spectroscopic analyses of a wide range of late type stars with different properties. The models are one-dimensional plane-parallel or spherical, and computed in LTE assuming the mixing-length scheme for convective energy transport, as formulated by @henyey01. For luminous stars (giants), where the geometric depth of the photosphere is a non-negligible fraction of the stellar radius, the effects of the radial dilution of the energy transport and the depth-varying gravitational field is taken into account. 