Synthetic observables with PLATON #343
Conversation
…bservables -> plot_bolometry. Add plot for transit/eclipse depths
|
Example |
| WRITE_FMT="%.7e" | ||
| PLATON_DOWNSAMPLE=8 | ||
| PLATON_METHOD="xsec" | ||
| PLATON_GASES=["H2", "H", "He", "H2O", "CH4", "CO", "CO2", "O", "C", "N", "NH3", "N2", |
There was a problem hiding this comment.
How are these gasses processed if not in an AGNI simulation?
There was a problem hiding this comment.
The spectra only include the intersection of gases supported by PROTEUS and PLATON. Others are ignored, in the sense that their opacities are set to zero, but they still contribute to the height, pressure, temperature, etc.
There was a problem hiding this comment.
Ok, and how are the abundances of these (that do not contribute to opacity) then set?
There was a problem hiding this comment.
In PLATON they are set to zero. However, it's worth noting that the species supported by PROTEUS are a subset of those supported by PLATON (until we start including rock vapours). This means that the radiative transfer in PLATON is consistent with that done by SOCRATES.
There was a problem hiding this comment.
When the legend refers to "removed gases" it just means that they are removed from the transmission/emission spectra calculations. Not from the full time-evolution. This is to associate the particular features with different species.
There was a problem hiding this comment.
I see, thanks for the clarification! Good forward-planning. :)
Simulations can now be post-processed with PLATON to generate synthetic transmission and emission spectra. These are calculated only at the end of the simulation. Using PLATON requires downloading about 10 GB of data, which is done automatically when you run the script
tools/get_platon.sh. Closes #339.Future work could include: putting these through telescope simulators, or binning them down to instruments bandpasses.