To convert from DEM to spectral space, we need to fold the DEM through a temperature dependent spectra.
To do this, we will compute an isothermal spectra for a set of temperatures (under the assumption of constant pressure). For now, we can use the CHIANTI IDL tools to do this. At some point, it would be nice to replace this with fiasco.
This isothermal spectra should include line, free-free, free-found, and two-photon continuum and should be done for multiple abundance models (e.g. Feldman, Scott, Schmelz). Tentatively, we can store this in an asdf file (if it gets too big, move it to zarr).
We can do all of this with hissw to integrate it into our Python pipeline.
To convert from DEM to spectral space, we need to fold the DEM through a temperature dependent spectra.
To do this, we will compute an isothermal spectra for a set of temperatures (under the assumption of constant pressure). For now, we can use the CHIANTI IDL tools to do this. At some point, it would be nice to replace this with fiasco.
This isothermal spectra should include line, free-free, free-found, and two-photon continuum and should be done for multiple abundance models (e.g. Feldman, Scott, Schmelz). Tentatively, we can store this in an asdf file (if it gets too big, move it to zarr).
We can do all of this with
hisswto integrate it into our Python pipeline.