THE PHOENIX MODELS BY FRANCE ALLARD AND COLLABORATORS

These models are for stars/brown dwarfs/planets with a cloud model. These use 
static, spherical symmetric, 1D simulations to completely describe the atmospheric 
emission spectrum. The models account for the formation of molecular bands, such 
as those of water vapor (from Barber & Tennyson BT2 2006), methane, or titanium 
dioxide, with no alpha element enhancement.  The models here are from AGSS2009 
using the Asplund et al. (2009) solar abundances. More information can be found 
at: https://phoenix.ens-lyon.fr/simulator/index.faces

Each directory in this suite includes all the models for a given metallicity. For
example "phoenixm10" includes all the models for [M/H]=-1.0, where "m" is for minus
and "p" is for plus. Each of the files in these directories is for a single Teff.
These fits files have columns for different log_g. For example, the column for 
log_g = 4.0 has column name g40, while that for log_g=3.0 has column g30.
For all metallicities, except for [M/H]= 0.0, each model includes columns for 
all log_gs in the range between 0.0 and 5.5. Those log_gs for which there are no 
phoenix models have FLAM=0 for all wavelengths.

The models for [m/H] = -1.0, -1.5, -2.0, -2.5, -3.0, -3.5, -4.0, 0.3, and 0.5 were 
resampled on November 07,2011 to reduce the number of points from the 
original models. We reduced it to 5K across the 900 to 30 microns wavelength range.
Each model includes columns for all log_gs in the range between 0.0 and 5.5. Those 
log_gs for which there are no phoenix models have FLAM=0 for all wavelengths.

In July 2020, in order to address some issues that were discovered with the resampled 
models, we started the process of replacing the 2011 models with with an updated 
version that includes more data points. The new models have 100K points for each 
log_g and cover an sligtly larger wavelenth range, this time betwee 0.07 and 
30.9 microns. We have done this only for models with [m/H] = 0.0. and -0.5.
For [m/H] =0.0 we used an alpha enhencement [alpha/H] =0.0 relative to solar. For 
[m/H] = -0.5 we used [alpha/H]a= +0.2 (Gebek & Matthee 2022, Hayden et al 2015, 
Recio-Blanco, A. et al 2014). The new files are also slightly different  from
the previous cases in which each file includes columns only for those log_gs for 
which the models exist. Not all the Teffs have the full range of log_gs, which in 
this case goes from 0.0 to 6.0. The list of log_g's included, as well as those 
missing, is provided in the header[0] of each file.

Note also that in order recreate the models, we had to redownload them from the
author's site at https://phoenix.ens-lyon.fr/Grids/BT-Settl/AGSS2009/SPECTRA/. The
models for metallicity = 0.0 and hot stars in this download
(BT-Settl_M-0.0_a+0.0_hot.tar), only included stars with Teff > 2600. We, therefore, 
downloaded the BT-Settl_M-0.0_cool.tar to add stars with Teff between 2000 and 2600, 
which was the case for our original models. Note that in this new set, as well as 
our original models, there were casese where there were four spectra per file 
(the wavelengths were repeated four times within a given file), where each
consisted of about 100K points. For these cases, we took only the first set of
wavelengths and fluxes. However, there are a few cases where the full 400K+ points
contained no repeated wavelengths.

References:

* Allard, F., Guillot, T., Ludwig, H.-G., et al. 2003, IAU Symp., 211, 325
* F. Allard , N. F. Allard , D. Homeier , J. Kielkopf , M. J. McCaughrean , and F. Spiegelman 2007, A&A, 474, L21
* Allard, F., Homeier, D., Freytag, B. 2012, Phil. Trans. R. Soc. A.370, 2765
* Andrea Gebek and Jorryt Matthee 2022, ApJ, 924, 73; 
* Hayden, M. et al 2015, ApJ. 808, 10; 
* Recio-Blanco, A. et al 2014, A&A  567, A5 

Also available here http://phoenix.ens-lyon.fr/Grids/Papers/

* All these models can be found in the ‘Star, Brown Dwarf & Planet
Simulator’:http://phoenix.ens-lyon.fr/simulator/index.faces

Original files have names lte067-1.5-0.0.BT-Settl.7.bz2