Supported stellar grids

Here we list each of the available stellar grids.

Phoenix

ld_model = ‘phoenix’

The Phoenix grid used the Husser (2013) stellar models and spans a range of metallicities from -1.5 to 1.0, effective temperatures from 2300 to 15000 k, and logg from 0.0 to 6.0. There are 5079 models in total, each evaluated at 54500 wavelengths and 78 radial positions on the stellar disc.

Kurucz

ld_model = ‘kurucz’ or ‘1D’

The Kurucz (1993) grid (CD-ROM No. 13) span a range of metallicities from -5.0 to 1.0, effective temperatures from 3500 to 6500 k, and logg from 4.0 to 5.0. There are 741 models in total, each evaluated at 1221 wavelengths and 17 radial positions on the stellar disc.

Stagger

ld_model = ‘stagger’ or ‘3D’

The Stagger grid uses the Magic (2015) 3D stellar models and spans a range of metallicities from -3.0 to 0.0, effective temperatures from 4000 to 7000 k, and logg from 1.5 to 5.0. Note that this grid has non-uniform coverage, see figure 1 of Magic (2013). There are 99 models in total, each evaluated at 105767 wavelengths and 10 radial positions on the stellar disc.

MPS-ATLAS-1

ld_model = ‘mps1’

The MPS-ATLAS (set 1) grid uses the Kostogryz (2022) stellar models and spans a range of metallicities from -5.0 to 1.5, effective temperatures from 3500 to 9000 k, and logg from 3.0 to 5.0. This grid has extensive parameter space coverage, showcasing 34160 models in total, each evaluated at 1221 wavelengths and 24 radial positions on the stellar disc. Set 1 uses the Grevesse & Sauval 1998 abundances with a constant chemical mixing length of 1.25.

MPS-ATLAS-2

ld_model = ‘mps2’

The MPS-ATLAS (set 2) grid uses the Kostogryz (2022) stellar models and spans a range of metallicities from -5.0 to 1.5, effective temperatures from 3500 to 9000 k, and logg from 3.0 to 5.0. This grid has extensive parameter space coverage, showcasing 34160 models in total, each evaluated at 1221 wavelengths and 24 radial positions on the stellar disc. Set 2 uses the the Asplund (2009) abundances with a chemical mixing length dependent on stellar parameters from Viani (2018).