For given dimensionful stellar dispersion data, the work flow goes as:
- Units are removed in undimensionalize_changeunits.py
- The gfuncs/*.py change the dispersion to be a function of r and v
- Then h_funcs.py and h_values.py compute the dimensionless J-factors as functions of dimensionless radius/angle
- main.py can complete the above steps
- plots.py is written to make plots with the dimensionless data To compute dimensionful J-factors,
- integrated_j_factors.py produces a file with the integrated (dimensionless) J-factor as a function of (dimensionless) angle
- j_tots.py uses this file to calculate J-factors of real dwarfs using the mcmc chain data in /j_factors/dwarfs/
- Then tot_j_factor_plotting.py makes plots of all dwarfs for all annihilation modes it can also make plots to compare this analysis to known results from the data in compare_to_other_values.py To get DM annihilation bounds,
- Using data from PPPC4DMID, integrate_gamma_spectra.py provides the integrated spectra for various channels/
- madhat_formatting.py makes the files with J-factors for MADHAT in models/
- batch_madhat.sh computes bounds for all models/*.txt and channels/*.txt
- madhat_plotting.py produces the cross-section bound plots