This repository contains the SEDs for Population III stars and Pop III galaxies used in our paper (http://adsabs.harvard.edu/abs/2016ApJ...833...65M). See the article or seds.ipynb here for detailed descriptions of the parameters used, calculation procedures and references.
The SEDs are computed for zero-metallicity stars (H_He only) in the ZAMS phase. We use the stellar parameters from Schaerer 2002 (2002A&A...382...28S) and Marigo 2001 ( 2001A&A...371..152M) as reported in Kubát 2012 (2012ApJS..203...20K).
Every file contains two columns: First column - frequency [Hz] The SEDs have been computed into a common frequency array of 19 000 points linearly spaced from 5e12 to 5e16 Hz. The values have been computed using linear interpolation. Second column - flux H_\nu [erg s^{-1} cm^{-2} Hz^{-1} sr^{-1}( {M_\odot}^{-1} for the case of galaxy SEDs)]. Note that this is the Eddington flux, so one needs to multiply by 4\pi to obtain the flux F_\nu.
The names of the files denote the stellar mass.
The names of the files denote the parameters of the IMFs; e.g, IMF_m9M50a2 means a population with lower stellar mass limit of 9 solar masses, upper limit 50 solar masses and Salpeter slope, -2.35. Note that, e.g., a top-heavy IMF has a slope of "0" in linear space, not logarithmic.
This is a python notebook to read and plot the galaxy/stellar SEDs in this repository.
It also shows how the galaxy SEDs are calculated for various IMFs, which can be adapted to compute SEDs with different mass ranges and IMF power index.