petitRADTRANS documentation¶
Welcome to the petitRADTRANS (pRT) documentation. pRT is a Python package for calculating transmission and emission spectra of exoplanets, at low (\(\lambda/\Delta\lambda=1000\)) and high (\(\lambda/\Delta\lambda=10^6\)) resolution, for clear and cloudy atmospheres.
Important
In addition to transmission spectra, pRT now includes scattering also for emission spectra, if specifically turned on (note that scattering increases the runtime), see Scattering for Emission Spectra. Currently the self-scattering by the planetary atmosphere is included, which is appropriate for, for example, brown dwarf and directly imaged atmospheres. The scattering of stellar light, following the implementation of petitCODE, is currently being tested in pRT and will be published soon.
petitRADTRANS is available under the MIT License, and documented in Mollière et al. (2019), for the general code, and Mollière et al. (2020), for the scattering implementation. Please cite these papers if you make use of petitRADTRANS in your work.
This documentation webpage currently contains an installation guide, a tutorial, a first code documentation, and an implemented retrieval example for mock JWST emission and transmission spectra. Also, we give a tutorial on how to include opacities that may be missing from our database.
News¶
- September 2020: self-scattering for emission spectra and chemical equilibrium interpolation now available
pRT now includes scattering also for emission spectra, if specifically turned on (note that scattering increases the runtime), see Scattering for Emission Spectra. Currently the self-scattering by the planetary atmosphere is included, which is appropriate for, for example, brown dwarf and directly imaged atmospheres. In addition, you can now download our chemical equilibrium interpolation package, which is documented in Interpolating chemical equilibrium abundances
- September 2020: petitRADTRANS opacities available on the Exomol website
Opacity tables created specifically in the petitRADTRANS format are now available on the Exomol website, also see Chubb et al. (2020) for the accompanying paper. The opacities can be installed in petitRADTRANS in an easy plug-and-play fashion. Please see Section Adding opacities for more information.
- September 2020: More high-temperature atom and ion opacities available
We have added more atom and ion opacities, bringing the total list to Al, AlII, AlIII, AlIV, AlV, AlVI, B, BII, BIII, Be, BeII, C, CII, CIII, CIV, Ca, CaII, Cr, Fe, FeII, K, KII, KIII, KIV, KV, KVI, Li, Mg, MgII, MgIII, MgIV, MgV, MgVI, N, NII, NIII, NIV, NV, Na, NaII, NaIII, NaIV, NaV, NaVI, Si, SiII, Ti, TiII, V, VII, Y
- May 2019: high-temperature atom and ion opacities now available
We have added the opacities of Fe, Fe+, Mg, Mg+, Li, Ca, Ca+, Si, Si+, O, O+, Al, Al+, Ti, Ti+, V and V+, up to temperatures of 4000 K. As usual, if the atmospheric temperatures increase above 4000 K, petitRADTRANS will use the absorbers respective opacities at 4000 K. Please make sure to install the latest petitRADTRANS version to make use of the high-temperature points of the new opacity tables!
Developers¶
Paul Mollière
Eleonora Alei
Evert Nasedkin
Contributors¶
Karan Molaverdikhani
Mantas Zilinskas
Code documentation: