Closed alexmaragko closed 1 year ago
Merging #224 (b2df3af) into master (920af78) will decrease coverage by
8.64%
. The diff coverage isn/a
.
@@ Coverage Diff @@
## master #224 +/- ##
==========================================
- Coverage 52.56% 43.91% -8.65%
==========================================
Files 9 12 +3
Lines 605 822 +217
==========================================
+ Hits 318 361 +43
- Misses 287 461 +174
Impacted Files | Coverage Δ | |
---|---|---|
pahfit/errors.py | 100.00% <0.00%> (ø) |
|
pahfit/features/features_format.py | 33.33% <0.00%> (ø) |
|
pahfit/features/__init__.py | 100.00% <0.00%> (ø) |
|
pahfit/features/features.py | 15.55% <0.00%> (ø) |
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Here is a brute fit (no redshift correction or proper unit conversion) and comparison between the different packs on the 5-15 micron JWST data of galaxy VV114.
We should be able to fit the emission lines by properly shifting the spectrum back to the rest frame. The redshift of VV114 is 0.02007.
Indeed things are improving with redshift correction.
With the JWST pack the fit is using a larger number of emission lines than required for the galaxy. The ISO pack, which includes ~ 100 less emission lines than the JWST pack, gives a better result.
To give a better description of the above, looking at the large number of emission lines e.g. in the 7 - 7.5 um region when fitting the galaxy with the JWST pack is because these lines are there in the simulations. In the plot below I'm zooming-in in the simulation spectrum at that region.
So these lines are included in the JWST pack file and PAHFIT is using them.
Added new JWST packs based on the PDR dissociation front (DF) simulations.
JWST_PDR_DF_MIRI-MRS_pack_file.ipac
pack file.
JWST_PDR_DF_MIRI-MRS_pack_file.ipac
pack file.
I'm going to close this for now since our pack format has diverged since this was written. Definitely still interested in improvements and the birth of a pdr.yaml
science pack. Probably starting small and building lines in as you go is the right approach.
JWST science pack files in ipac format, based on JWST simulations of the Orion's Bar ionization front (see https://pdrs4all.org/publications/ for details).
Emission lines and dust features were fitted with Gaussian1D and Drude1D models/profiles respectively, at separate smaller wavelength regions (not in one go of the entire NIR/MIR simulated spectra.)
Notes on PAHFIT fitting
Example fitting on the 5 - 15 micron region of the simulations.