Tale of Two Molecules PICASO Model Grid 

A grid of models generated with PICASO based on the Elf Owl chemical and temperature profiles 
where we include the abundances of carbon dioxide and phosphine as parameters. There are four 
sub-folders included, one for each of the objects in Beiler et al. 2024, each of which includes
all of the model spectra already smoothed and convolved to the objects' wavelengths. Further 
details about the generation of these models can be found in Section 5 of Beiler et al. 2024a. 
The model fluxes are in units of Janskys, and the model wavelengths are in microns. 

FILE NAME STRUCTURE
Files are named {T}_kz{K}_g{G}_{M}_CO2x{C}_PH3x{P}_CtoO{O}.txt
T is the effecitve temperature value (K) with possible values of '400'-'600' at intervals of 25
K is the log kzz value ([cm^2 s^-1] with possible values of '2','4','7', and '9'
G is the g value (cm s^-2) with possible values of '17', '31', '56', '100', '178', '316', '562', '1000', '1780', and '3160'
M is the [M/H] value with possible values of '+0.0' and '-1.0'
C is the factor that the CO2 abundance is increased by, with possible values of
'1', '50.0', '100.0', '500.0','1000.0','5000.0','10000.0', and '50000.0'
P is the factor that the PH3 abundance is reduced by, with possible values of '1', '2', '5', '10', and '100'
O is the C/O ratio value, with possible values of '0.5', '1.0', '2.5'

CONTENTS OF THE FILES
Column 1: Wavelength of model in microns
Column 2: Flux of model in Janskys

CREDITS
If you use these models in your research, please cite Beiler et al. (2024a)

REFERENCES
Batalha, N., Freedman, R., Gharib-Nezhad, E., & Lupu, R. 2020, 
Resampled Opacity Database for PICASO, Zenodo, doi: 10.5281/zenodo.6928501288

Batalha, N. E., Marley, M. S., Lewis, N. K., & Fortney, J. J. 2019, 
The Astrophysical Journal, 878, 70, doi: 10.3847/1538-4357/ab1b51291

Mukherjee, S., Batalha, N. E., Fortney, J. J., & Marley, M. S. 2023a, 
The Astrophysical Journal, 942, 71, doi: 10.3847/1538-4357/ac9f483

Mukherjee, S., Fortney, J. J., Batalha, N. E., et al. 2022,
The Astrophysical Journal, 938, 107, doi: 10.3847/1538-4357/ac8dfb3