Karl Gordon
Karl Gordon
Thinking from the physics model standpoint, it would be based on the evolutionary phase or log(g)/Teff or something like that. Mapping the stellar atmosphere models to the tracks/isochrones is done...
Not sure the isochrones we download from the website have the evolutionary phase. This needs to be checked via the file (there are lots of columns!).
Would it be possible to do this? I thought that they way this was setup, all had to be imported otherwise the python won't run.
But there are is more info (I think) in the downloaded isochrone file.
How do the points (say in log(T) and log(g)) compare to the Kurucz stellar models? Do they overlap? Do they extend the log(g)-T(eff) coverage?
The dust_extinction package has been updated to include various dust grain models including the Weingartner & Draine (2001) models. See https://dust-extinction.readthedocs.io/en/latest/dust_extinction/model_flavors.html#grain-models
Plot?
Great. I think then there is an "easy" way forward. I think we can just add the models to the stellar atmosphere grid. The ordering does matter. The standard is...
There were multiple figures that I found useful in her presentation. Some of them were your work - and those should be included as well!
If you plot the spectra for the same log(g)/Teff/metallicity from Kurucz and Aringer, do they overlap/look the same?