Read me file for M Stars:

The MUSCLES stars are:

GJ 436 - naming convention: spectra436.*
GJ 832 - naming convention: spectra832.*
GJ 1214 - naming convention: spectra121.*
GJ 667C - naming convention: spectra667.*
GJ 876 - naming convention: spectra876.*
GJ 581 - naming convention: spectra581.*

There are three broad categories of M star spectral models described in Rugheimer et al., 2015 809:57. See the paper for full details.

In brief:
Active Stellar Models for M0 to M9 are based off an H-alpha scaling of ADLeo and represent the upper most activity levels expected in M stars. The naming convention is M0A, M2A etc where A means active.

Inactive Stellar Models for M0 to M9 are spectra planet models for a modern Earth-like atmosphere for a planet orbiting an Mstar with the UV - IR flux only taken from the PHOENIX model output. PHOENIX models do not accurately model the UV portion of the spectra which comes from chromospheric activity since they are only photosphere models. Thus these represent the lowest theoretical floor of possible UV flux.

HST MUSCLES Stars:
These stars are M dwarfs which have traditionally been labeled as “quiescent” since they do not have H-alpha in emission. Though these stars have significant chromospheric activity and thus UV fluxes between the active and inactive stellar models. These stellar models have UV observations from HST and then are combined with a PHOENIX model for the VIS-IR. 


The raw output of the spectra code is:

Column 1                   Column 2      Column 3                         Column 4
wavenumber (cm^-1)           Ones     Relative Absorption               1 - column 3
10,000/column 1 = microns  (col 3+4)  This is the column you want

For the rest of this document, column 1 will be in the variable "wave" and column 3 will be "fraction"

You can use a smearing routine to downsample the highresolution spectra

For direct detection spectra:

For IR spectra

Make a variable for the surface temperature of the Planet, Tsurf

Make sure you do proper unit conversions. ie) for W/m^2/um
watts=1.e-7 ;ergs to watts
scale=1.e-4 ; conversion for 1/cm to 1/um
scale2=1.e4 ; conversion for 1/cm^2 to 1/m^2

so you might want to multiply your column 3 by something like:Unit_conversion= watts*scale*scale2*pi for W/m^2/um

For the IR specta, multiply by the blackbody of the surface temperature of your radiating planet

Ultimately what you will plot for the top of the atmosphere emergent IR flux will be something like:

Unit_conversion*Column_3*2*h*c^2*wave_number(column1)^5/(exp(h*c*wave_number/k/Tsurf)-1)

For the VIS spectra

You have to consider the reflected stellar spectrum and the wavelength dependent albedo of the surface.

Rayleigh scattering is not included in the spectra. You have to use an analytical approximation and add that in directly.

So for the flux at the top of the atmopshere you will have something like:

column_3*wavelength_dependent_albedo_surf*Rayleigh_scattering*Unit_conversion*star_flux