Phoenix models:

['MAPKEY'] = ('phoenixBTS11_15', 'Mapping identifier for filetype')
['CONTACT'] = ('J. White/M. McMaster', 'ReDCaT Team Deputy/Lead')
['CREATED'] = (date_string, 'Date of file creation')
['DESCRIP'] = 'Phoenix Models BT-settl Allard et al. 03, 07, 09'
['FILE_TYP'] = ('Atmosphere Grid Model', 'Type of file')
['SYSTEMS'] = ('ETC, CDBS, PYSYNPHOT', 'Systems that will use this filetype')
['REASON'] = 'Delivered to support JWST'
['COMMENT'] = '= Files translated to CDBS format by J. White and R.Diaz'

 
Phoenix Models computed by France Allard
Although the scientific community widely accepts these models,
we found it challenging to locate the relevant documentation
and references o describe the underlying research. In here provide
with the best source of information we could find to describe the 
underlying research. We extracted excerpts from 
the README files of these models and recommendations about papers
that seem to provide relevant information about them.  Readme
file states that information about these models is in Baraffe et
al. 2015, and  Allard et al. 2015. We found a paper that matches
this reference ( https://arxiv.org/abs/1503.04107). In that
paper, the author states that BT-SETL models from Allard et
al. 2012 include some of the changes discussed in the article.
Reference to Allard's paper is Allard, F., Homeier, D., \& 
Freytag, B. 2012a, Royal Society of London Philosophical 
Transactions Series A, 370, 2765. We encourage users to contact 
Dr. Allard and collaborators for any questions about these 
models and the exact references.

 We were also unable to determine how these models are version
controlled;  therefore, we provide with the date when these
models were downloaded and their modification date.  These 
models were obtained from the PHO0ENIX repository 
https://phoenix.ens-lyon.fr/Grids/BT-Settl/CIFIST2011_2015/SPECTRAa/,
but these are also available at 
http://phoenix.ens-lyon.fr/simulator/index.faces . The models were 
downloaded on September 27, 2019.  At that time these models
had been last updated, in the above website, on March 16, 2015.

 The wavelength range differs from the original models in that
it is sampled, using pysynphot, to only 300000 data points 
ranging between 700 A to 35 microns. Resampling is necessary for
the models to work with STScI Tools like Pysynand ETC.  Models
were grouped by metallicity. Each metallicity folder has
several files for different Teff. Each of these files includes
data for different log g. 
Wavelength is provided in Angstroms while fluxes are FLAM.
 

From Dave Soderblom: Teff vs Spectral Type
R. Diaz log G

Rough correspondence of Teff to spectral type for cool objects.  No luminosity class is indicated.  Info from mamajek online.		
		
Teff	Spec.	Log G
1200	T2	5
1300	L9	5
1400	L7	5
1500	L6	5
1600	L5	5
1700	L4	5
1800	L3	5
1900	L2.5	5
2000	L2.5	5
2100	L1	5
2200	L0	5
2300	M9.5	5
2400	M9.5	5
2500	M8	5
2600	M7.5	5
2700	M6.5	5
2800	M6.5	5
2900	M6.5	5
3000	M5.5	5
3100	M4.5	5
3200	M4.5	5
3300	M3.5	5
3400	M3.5	5
3500	M2.5	5