Welcome to the GSFC Exoplanet Modeling and Analysis Center (EMAC)
EMAC serves as a catalog, repository and integration platform for modeling and analysis resources focused on the study of exoplanet characteristics and environments. EMAC is a key project of the GSFC Sellers Exoplanet Environments Collaboration (SEEC).
If you've used EMAC in any part of your research, please cite our RNAAS paper either in your methods section or in the "Software used" portion of any manuscripts; see the FAQ for more information.
More Information on EMAC for first-time visitors...If you make use of tools linked or hosted on EMAC: please use the following statement in your publication acknowledgements: “This research made use of the NASA Exoplanet Modeling and Analysis Center (EMAC), which is funded by the NASA Planetary Science Division's Internal Scientist Funding Model.”
Stay up to date with EMAC!- Subscribe to our monthly RSS messages on new updates and tools.
- Check out the Bluesky account @exoplanetmodels.bsky.social (not an official NASA account), where new tools and features are highlighted.
- Email us with general feedback at and tell us what you'd change or improve.
- Click the
icon in a resource box to provide suggestions for an individual tool or tools.
- EMAC is intended as a clearinghouse for the whole research community interested in exoplanets, where any software or model developer can submit their tool/model or their model output as a contribution for others to use.
- EMAC provides a searchable and sortable database for available source code and data output files - both resources hosted locally by EMAC as well as existing external tools and repositories hosted elsewhere.
- The EMAC team also helps develop new web interfaces for tools that can be run “on-demand” or model grids that can be interpolated for more individualized results.
- If you would like to submit a new tool/model to EMAC, please visit our Submit a Resource page.
- For help with tutorials for select resources/tools use the “Demo” buttons below and subscribe to our YouTube channel.
- Watch this video for a walk-through of the whole EMAC site, including how to submit a new tool and how to access information for each resource.
EMAC co-leads are Joe P. Renaud and Eric Lopez; more information on EMAC staffing and organization can be found on Our Team page.
EMAC has launched a new community-supported curator program, and we need your help! Check out our curator page to learn how exoplanet experts like yourself can support EMAC's mission, and help us spread the word about this new initiative!
eclipsoid: Open-source JAX-based Python package
Dholakia, Shashank; Dholakia, Shishir; Pope, Benjamin J. S.
Eclipsoid provides a general framework allowing rotational deformation to be modeled in transits, occultations, phase curves, transmission spectra and more of bodies in orbit around each other, such as an exoplanet orbiting a host star.
ExoJAX: Differentiable Spectrum Modeling of Exoplanets/Brown Dwarfs using JAX
Kawahara, Hajime; Kawashima, Yui; The ExoJAX team et al.
ExoJAX is designed to directly calculate cross-sections as functions of temperature and pressure, rather than interpolating tabulated data, to minimize errors in high-dispersion spectra modeling. Has developed differentiable radiative transfer schemes, including emission, transmission, and reflection spectroscopy. These enhancements significantly expand the range of applications.
RADIS: Fast Line-by-line code for infrared emission & absorption spectra at equilibrium & non-LTE
RADIS uses a new algorithm that can resolve spectra with millions of lines within seconds on a single-CPU, and can be GPU-accelerated for almost-instant-computation (up to 5e14 lines*spectral points/s).
It supports HITRAN, HITEMP and ExoMol out-of-the-box (auto-download), and therefore is particularly suitable to compute cross-sections or transmission spectra at high-temperature.
It includes equilibrium calculations for all species, and non-LTE for CO2 and CO.
The code is an open-source Python library (https://github.com/radis/radis) and can also be executed in an online environment with pre-configured HITEMP databases (https://radis.github.io/radis-lab/).
NEMESISPY: A Python package for simulating and retrieving exoplanetary spectra
Yang, Jingxuan ; Alday, Juan ; Irwin, Patrick
NEMESISPY is a Python package developed for atmospheric retrievals, which is the inference of atmospheric properties such as chemical composition using spectroscopic data. The package contains code for radiative transfer calculation using the correlated-k approximation and for parametric atmospheric modelling. NEMESISPY is a recent and active development of the well-established Fortran NEMESIS library (Irwin et al., 2008), which has been applied to the atmospheric retrievals of both solar system planets and exoplanets employing numerous different observing geometries.
radioBEAR: radio - BErkeley Atmospheric Radiative transfer
DeBoer, David
Radio BErkeley Atmospheric Radiative-transfer (RadioBEAR) is a planetary atmosphere code to calculate the brightness temperature of planetary atmospheres in the meter-to-millimeter wavelength range.
PyExoCross: A Python program for generating spectra and cross-sections from molecular line lists
Zhang, Jingxin
PyExoCross is designed for postprocessing the huge molecular line lists generated by the ExoMol project and other similar initiatives such as the HITRAN and HITEMP. It generates LTE and non-LTE absorption and emission stick spectra, cross sections, and other properties (partition functions, specific heats, cooling functions, lifetimes, and oscillator strengths) based on molecular line lists. PyExoCross calculates cross sections with four line profiles: Doppler, Gaussian, Lorentzian, and Voigt; a number of options are available for computing Voigt profiles. PyExoCross can convert data format between ExoMol and HITRAN. PyExoCross supports line lists in the ExoMol and HITRAN/HITEMP formats.
MOLPOP-CEP: An exact, fast line transfer code for multi-level line emission
Asensio Ramos, Andrés ; Elitzur, Moshe
MOLPOP-CEP is a universal line transfer code that allows the exact calculation of multi-level line emission from a slab with variable physical conditions for any arbitrary atom or molecule for which atomic data exist.
OoT: Out-of-Transit Light Curve Generator
Penoyre, Z. ; Sandford, E.
OoT (Out-of-Transit) calculates the light curves and radial velocity signals due to a planet orbiting a star. It explicitly models the effects of tides, orbital motion, relativistic beaming, and reflection of the stars light by the planet. The code can also be used to model secondary eclipses.
PyRADS: Python RADiation model for planetary atmosphereS
Koll, D. et al.
The Python line-by-line RADiation model for planetary atmosphereS (PyRADS) is a 1D line-by-line radiation code. The default version is for longwave radiation (no scattering), a version for shortwave radiation (with scattering) is also available on github.
Citation: Koll & Cronin (2018), Proceedings of the National Academy of Sciences, vol. 115, issue 41, pp.10293-10298.
Atmospheric Athena: 3D Atmospheric escape model with ionizing radiative transfer
Tripathi, Anjali ; Krumholz, Mark R.
Atmospheric Athena is a code intended to simulate hydrodynamic escape from close-in giant planets in 3D. It uses the Athena hydrodynamics code (v4.1) with a new ionizing radiative transfer implementation based on Krumholz et al, 2007, to self-consistently model photoionization driven winds from the planet. The code is fully compatible with static mesh refinement and MPI parallelization.
optool: Command-line driven tool to create dust opacities.
Dominik, C.; Min, M.; Tazaki, R.
Optool computes dust opacities and scattering matrices, for specific grain sizes or averaged over size distributions. It is derived from OpacityTool (ascl:2104.009) and implements the Distribution of Hollow Spheres (DHS) statistical method to approximate irregular and low porosity grains. Mie theory is available as a limiting case of DHS. It also implements the Tazaki Modified Mean Field Theory (MMF) to treat fractal and highly porous aggregates. The refractive index data for many astronomically relevant materials are compiled into the code, and external refractive index data can be used as well.
cortecs: Compressed representations of opacity for radiative transfer
Savel, A.; Bedell, M.; Kempton, E. M.-R.
cortecs is a Python package for compressing opacity files used in radiative transfer. We offer a few different types of compression methods with a range of flexibility, from polynomial to neural networks. We also provide utility functions for working with opacity files, such as chunking and interpolating them onto different grids.
Exo_Transmit with Tholin Opacities
Corrales, Lia; Gavilan, Lisseth; Teal, D. J.; Kempton, E. M. R.
A static, refactored version of Exo_Transmit (Kempton et al. 2017, Teal et al. 2022, Corrales et al. 2023) for computing exoplanet transmission spectra with the new tholin species. This code uses optical constants from tholins grown in the laboratory and computed cross-sections (Mie) for a wide range of particle sizes, for wavelengths of 0.13-10 micron.
PCM_LBL: Planetary Climate Model (Line-By-Line)
Wordsworth, Robin et al.
PCM_LBL is a 1D radiative-convective code designed to simulate the climates of diverse planetary atmospheres, from present-day Earth to early Mars and exoplanets. The code is written in modular modern Fortran and uses a 'brute-force' spectral approach where absorption coefficients are computed on a fixed spectral grid directly from line data. This allows climate calculations to be performed more simply and at higher accuracy than in a correlated-k approach.
CROCODILE: CROss-COrrelation retrievals of Directly-Imaged self-Luminous Exoplanets
Hayoz, J. et al. 2023
CROCODILE provides the statistical framework to interpret the three main observables of directly-imaged exoplanetary atmospheres, namely photometry, low-resolution spectroscopy, and medium (and higher) resolution cross-correlation spectroscopy. These will be measured by the next generation of instruments such as ERIS at the Very Large Telescope, MIRI aboard the James Webb Space Telescope, and METIS at the future Extremely Large Telescope.
rfast: A fast tool for planetary spectral forward and inverse modeling.
Robinson, T.
The rfast tool is an ultra-quick planetary spectrum simulator and remote sensing tool, originally designed for rapid retrieval explorations for mission concept studies. Through a convenient runscript, users can generate a noise-free spectrum of a planetary environment, add instrumental noise, and perform inverse modeling. The rfast tool is capable of applications to simulated and real observations spanning reflected-light, thermal emission, and transit transmission.
Pyshellspec: Binary systems with circumstellar matter (β Lyrae)
Brož, Miroslav, Nemravová, Jana
PYSHELLSPEC is an astrophysical tool for modeling of binary systems with circumstellar matter (e.g. accretion disk, jet, shell), computation of interferometric observables |V2|, arg T3, |T3|, |dV|, arg dV, comparison of light curves, spectro-interferometry, spectra, and SED with observations, and both global and local optimisation of system parameters. It is based on Shellspec, a long-characteristic LTE radiation transfer code by Budaj & Richards (2004).
RAPOC: Rosseland And Planck Opacity Converter
Lorenzo V. Mugnai and Darius Modirrousta-Galian
RAPOC (Rosseland and Planck Opacity Converter) is a Python 3 code that calculates Rosseland and Planck mean opacities from wavelength-dependent opacities for a given temperature, pressure, and wavelength range. In addition to being user-friendly and rapid, RAPOC can interpolate between discrete data points, making it flexible and widely applicable to the astrophysical and Earth-sciences fields, as well as in engineering. For the input data, RAPOC can use ExoMol and DACE data, or any user-defined data, provided that it is in a readable format.
THAI: TRAPPIST Habitable Atmosphere Intercomparison GCM Data Repository
THAI Team (Fauchez, Thomas et al.)
The TRAPPIST Habitable Atmosphere Intercomparison (THAI) project is a model inter-comparison effort between four GCMs: ExoCAM, LMD-G, ROCKE3D and the UM – examining a single interesting test case (TRAPPIST-1e) under several different atmosphere scenarios. The CKAN data repository provides NetCDF files for each case, allowing for examination and intercomparison of results from the different models. Scripts to process the data and plot them are available on our Github repository.
HELIOS-K: A GPU opacity calculator for exoplanetary atmospheres
Simon Grimm, Kevin Heng
HELIOS-K calculates opacity functions for planetary atmopheres by using opacity line lists from different databases. Before the opacity functions can be calculated, the line lists need to be downloaded and preprocessed into binary files that can be read from HELIOS-K.
HELIOS-K provides tools to automatically download and preprocess files from the ExoMol, HITRAN, HITEMP, NIST, Kurucz and VALD3 databases.
HELIOS-K is running on GPUs and require a Nvidia GPU with compute capability of 3.0 or higher.
MARGE: A Python package to train and evaluate neural networks
Himes et al.
MARGE (Machine learning Algorithm for Radiative transfer of Generated Exoplanets) is an all-in-one package to generate exoplanet spectra across a defined parameter space, process the output, and train machine learning (ML) models as a fast approximation to radiative transfer (RT). Despite its backronym name, MARGE is a general package that can train neural networks on a provided data set of inputs and outputs.
MARGE is an open-source project under the Reproducible Research Software License and welcomes improvements from the community to be submitted via pull requests on Github.
spectools_ir: A suite of tools designed for analysis of medium/high-resolution IR molecular spectra
Colette Salyk
Spectools_ir is a small suite of tools designed for analysis of medium/high-resolution IR molecular astronomical spectra. It consists of three main sub-modules (flux_calculator, slabspec, and slab_fitter) as well as a 'utils' sub-module, with a few additional functions.
Spectools_ir was written with infrared medium/high-resolution molecular spectroscopy in mind. It often assumes spectra are in units of Jy and microns, and it uses information from the HITRAN molecular database. Some routines are more general, but users interested in other applications should proceed with caution.
ROCKE-3D: A fully coupled ocean atmosphere 3-D General Circulation Model
Resolving Orbital and Climate Keys of Earth and Extraterrestrial Environments with Dynamics (ROCKE-3D) is a three-dimensional General Circulation Model (GCM) developed at the NASA Goddard Institute for Space Studies for the modeling of atmospheres and oceans of solar system and exoplanetary terrestrial planets.
P-winds: An open-source Python code to model planetary outflows and upper atmospheres
Leonardo A. Dos Santos, Aline A. Vidotto, Shreyas Vissapragada, et al.
Python implementation of Parker wind models for planetary atmospheres. The main goal of this code is to produce simplified, 1-D models of the upper atmosphere of a planet, and perform radiative transfer to calculate observable spectral signatures. The scalable implementation of 1D models allows for atmospheric retrievals to calculate atmospheric escape rates and temperatures. In addition, the modular implementation allows for a smooth plugging-in of more complex descriptions to forward model their corresponding spectral signatures (e.g., self-consistent or 3D models).
PyMieDAP: Radiative Transfer of Polarized Light in Planetary Atmospheres
Rossi, L. et al.
PyMieDAP (Python Mie Doubling Adding Program) is a Fortran-Python package to make light scattering computations with Mie scattering and radiative transfer computations
with full orders of scattering, using the Doubling-Adding method. PyMieDAP takes into account the polarization of the light scattered.
Full planet modeling at any phase angle is possible. Inhomogeneous planets can be modeled.
With the subpackage exopy, it is also possible to simulate systems with a star, a planet and a possible moon.
gCMCRT: A GPU accelerated MCRT code for (exo)planetary atmospheres
Lee, Elspeth K. H.
gCMCRT (gpu Cloudy Monte Carlo Radiative Transfer) is a 3D Monte Carlo Radiative-Transfer (MCRT) and ray-tracing hybrid code suitable for a wide variety of synthetic spectra modeling for (exo)planetary atmospheres, using GPU hardware to accelerate the RT calculation.
Primarily aimed at post-processing 1D global averaged or 3D GCM model output, gCMCRT can calculate albedo, emission and transmission spectra as well as phase curves from model outputs. gCMCRT has functionality to model high-resolution spectra including doppler shifting effects.
gCMCRT also contains an opacity mixer/interpolator (optools) as well as a Mie theory solver to help produce the opacity structures of the atmosphere.
ThERESA: Three-Dimensional Eclipse Mapping with Spectroscopic Lightcurves
Challener, Ryan C.; Rauscher, Emily
ThERESA is a 3D exoplanet atmospheric retrieval package. ThERESA individually fits 2D temperature maps for each lightcurve in a spectroscopic eclipse (or phase curve) observation using maximally-informative "eigencurves." It then places these 2D maps in 3D space, using a variety of models, to retrieve the planet's 3D temperature structure. ThERESA then calculates thermochemical equilibrium abundances and emission across the planet, which is then integrated spectrally and spatially to compare with all lightcurves simultaneously. This is repeated behind MCMC to obtain accurate parameter uncertainty estimates. Analyses can take a few days to a few weeks, depending on model complexity.
Exo-REM: 1D self-consistent radiative-equilibrium model for exoplanetary atmospheres
Baudino, J.-L.; Bézard, B.; Charnay, B. and Blain, D.
Exo-REM is a 1D radiative-equilibrium model developed for the simulation of the atmosphere of H2-dominated exoplanetary atmospheres. Fluxes are calculated using the two-stream approximation. The radiative-convective equilibrium is solved assuming that the net flux (radiative + convective) is conservative. The conservation of flux over the pressure grid is solved iteratively using a constrained linear inversion method. Rayleigh scattering as well as absorption and scattering by clouds (calculated from extinction coefficient, single scattering albedo, and asymmetry factor interpolated from precomputed tables for a set of wavelengths and particle radii) are also taken into account.
APOLLO: MCMC Exoplanet Atmosphere Retrieval Code
Howe, Alex; Adams, Arthur
APOLLO is an exoplanet atmosphere retrieval code designed for flexibility and comparison of models. The code computes 1-D forward models of exoplanet spectrum in transit or emission and fits them to observations using an MCMC method. APOLLO includes options for multiple radiative transfer algorithms, temperature-pressure profiles, and cloud parameterizations, allowing for comparison of models using different physics prescriptions. APOLLO can also generate synthetic spectra in the JWST spectroscopic modes, as well as compute photometric fluxes.
Pyratbay: A Forward-modeling and retrieval code to model exoplanet atmospheres and spectra
Cubillos, P. E. and Blecic, J.
The Pyrat Bay framework is an open-source pack for exoplanet atmospheric modeling, spectral synthesis, and Bayesian retrieval. The modular design of the code allows the users to generate atmospheric 1D parametric models of the temperature, abundances (equilibrium or constant profiles), and altitude profiles in hydrostatic equilibrium; sample ExoMol and HITRAN line-by-line cross sections with custom resolving power and line-wing cutoff values; compute emission or transmission spectra considering cross sections from molecular line transitions, collision-induced absorption, Rayleigh scattering, gray clouds, and alkali resonance lines; and perform Markov chain Monte Carlo atmospheric retrievals.
ESO SkyCalc: Web and API interface to The Cerro Paranal Advanced Sky Model
SkyCalc is a web application based on the Cerro Paranal Advanced Sky Model, which was developed in particular to be used in the ESO Exposure Time Calculators, by a team of astronomers at the Institute for Astro- and Particle Physics at the University of Innsbruck, as part of an Austrian in-kind contribution to ESO.
A command-line tool, skycalc_cli, is available to execute the SkyCalc backend engine through an API. The C source code is available to download.
ARTES: Radiative transfer of polarized light in 3D exoplanet atmospheres
Tomas Stolker
ARTES is a 3D Monte Carlo radiative transfer code for polarized scattered light simulations of exoplanet atmospheres. The code can be used for post-processing of a pre-calculated or parametrized atmosphere structure. Multiple scattering, absorption, and polarization are fully treated and the output includes an image, spectrum, or phase curve of reflected stellar light or thermal photons. Several tools are included for calculating opacities and scattering matrices of molecules and clouds but the user can also adopt their own opacities.
ShellSpec: Lightcurves, spectra and images of binaries and exoplanets with moving circum-object material
Jan Budaj
Program SHELLSPEC is designed to calculate lightcurves, spectra and images of interacting binaries and extrasolar planets immersed in a moving circumstellar matter (CM). It solves a simple radiative transfer along the line of sight in 3D moving CM. Roche model with a reflection effect and synthetic spectra from the stellar atmosphere models can be used as a boundary condition for the radiative transfer. Dust, including non-isotropic Mie scattering, can also be taken into account. The assumptions include LTE and optional known state quantities and velocity fields in 3D.
EXOCROSS: A general program for generating spectra from molecular line lists
Yurchenko, Sergei N.; Al-Refaie, Ahmed F.; Tennyson, Jonathan
ExoCross is a Fortran code for generating spectra (emission, absorption) and thermodynamic properties (partition function, specific heat etc.) from molecular line lists including ExoMol and HITRAN. Input is taken in several formats, including ExoMol and HITRAN formats. ExoCross can work with several line profiles such as Doppler, Lorentzian and Voigt and support several broadening schemes. ExoCross supports calculations of lifetimes, cooling functions, specific heats and other properties. It is capable of simulating non-LTE spectra using a two-temperature approach as well as custom-built models.
ChromaStarPy: Transit light-curve modelling integrated with stellar atmosphere and surface intensity modeling
Short, Ian C.; Bennett, Philip D.
An approximate stellar atmosphere and spectrum modelling code in Python that includes in situ modelling of the transit light-curve due to a "small" exo-planet occulting the computed stellar surface intensity distribution.
ATMO: 1D-2D radiative/convective atmospheric code
Tremblin P. et al. (see description)
ATMO is a 1D-2D atmospheric code for the study of the atmosphere of brown dwarfs and exoplanets. The code has originally been developed at the University of Exeter (here) and is currently a collaboration between different groups across the globe. The main developers are:
1D and 2D newton solver: P. Tremblin
Radiative transfer: D. Amundsen, P. Tremblin
Opacities: D. Amundsen, M. Phillips, R. Ridgway, J. Goyal
Equilibrium chemistry: P. Tremblin, B. Drummond, J. Goyal
Condensation and rainouts: P. Tremblin, J. Goyal
Out-of-equilibrium chemistry: O. Venot, E. Hebrard, B. Drummond
Convection: P. Tremblin, M. Phillips
Retrieval: D. Sing
CHIMERA: Exoplanet Emission/Transmission Atmospheric Retrieval Tool
M. Line et al. (J. Lustig-Yaeger, N. Batalha, M. Marley, X. Zhang, A. Wolf)
Flexible atmospheric retrieval tool for exoplanet atmospheres. Can be used for both transmission and emission geometries with options for both the "free" and "chemically consistent" abundance retrievals. Uses correlated-K opacities (R=100) with the random-overlap resort-rebin procedure (Amundsen et al. 2017). Includes full multiple scattering in emission (both planetary and stellar reflected light) using a two stream approximation variant (Toon et al. 1989). Various cloud parameterizations ranging from "grey+power-law" to the "Ackerman & Marley 2001" eddy-sed routine in both emission and transmission. Includes multiple Bayesian samplers, including PyMultiNest (recommended) and Dynesty.
HELIOS: 1D radiative-convective model for exoplanetary atmospheres
Malik et al.
HELIOS is an open-source radiative transfer code designed to study exoplanetary atmospheres, from rocky terrestrial planets to ultra-hot Jupiters. For given opacities and planetary parameters, HELIOS finds the atmospheric temperature profile in radiative-convective equilibrium and the synthetic planetary emission spectrum. HELIOS is written in Python, with the core computations parallelized to run on a GPU. HELIOS is part of the Exoclimes Simulation Platform.
PLATON: PLanetary Atmospheric Tool for Observer Noobs
Zhang, Michael; Chachan, Yayaati; Kempton, Eliza; Knutson, Heather
PLATON is a Python package that can calculate transmission and emission spectra for exoplanets, as well as retrieve atmospheric characteristics based on observed spectra. PLATON is easy to install and use, with common use cases taking no more than a few lines of code. It is also fast, with the forward model taking less than 100 ms and a typical retrieval finishing in ~10 min on an ordinary desktop. PLATON supports the most common atmospheric parameters, such as temperature, metallicity, C/O ratio, cloud-top pressure, and scattering slope. It also has less commonly included features, such as a Mie scattering cloud model and unocculted starspot corrections.
Planetary Spectrum Generator: An Online Tool for Synthesizing Planetary Spectra
Villanueva, Geronimo et al.
The Planetary Spectrum Generator (PSG) is an online tool for synthesizing planetary spectra (atmospheres and surfaces) for a broad range of wavelengths (100 nm to 100 mm, UV/Vis/near-IR/IR/far-IR/THz/sub-mm/Radio) from any observatory (e.g., JWST, ALMA, Keck, SOFIA).
PICASO: Open-Source RT Model for Computing Reflected Exoplanet Light at any Phase Geometry
Batalha, Natasha; Marley, Mark; Lewis, Nikole; Fortney, Jonathon
The Planetary Intensity Code for Atmospheric Scattering Observations (PICASO) is an open-source radiative transfer model for computing the reflected light of exoplanets at any phase geometry. This code, written in Python, has heritage from a decades old, well-known Fortran model used for several studies of planetary objects within the Solar System and beyond. We have adopted it to include several methodologies for computing both direct and diffuse scattering phase functions, and have added several updates including the ability to compute Raman scattering spectral features.
petitRADTRANS: Tool for Calculating Transmission and Emission Spectra of Exoplanets with Clear and Cloudy Atm.
Mollière, Paul
PetitRADTRANS (pRT) is a Python package for calculating transmission and emission spectra of exoplanets, at low (𝜆/Δ𝜆=1000) and high (𝜆/Δ𝜆= $10^6$) resolution, for clear and cloudy atmospheres. pRT offers a large variety of atomic and molecular gas opacities, cloud cross-sections from optical constants, or parametrized cloud models using either opacity power laws or grey cloud decks. The code also calculation of emission and transmission contribution functions, and contains a PHOENIX/ATLAS9 spectral library for host stars to calculate planet-to-star contrasts. Implemented examples for MCMC retrievals with pRT can be found on the code website.
LAPS: The Live Atmosphere-of-Planets Simulator
Martin Turbet (LMD), Cédric Schott (ESEP) and the LMD team
LAPS was developed to easily simulate the climate of planets similar to Earth (i.e., terrestrial but not giant planets). This model is based on the LMD (Laboratoire de Météorologie Dynamique) Global Climate Model (GCM), a complex 3-D numerical model of climate solving equations of thermodynamics, radiative transfer and hydrodynamics. This complex 3-D model has been simplified to a 1-D code (Turbet et al. 2016, 2017), which is therefore much faster to run and can now be used online in an interactive fashion.
Other resources in the literature:
DIAPHANE: A portable radiation transport library for astrophysical applications
Reed, Darren S. et al.
DIAPHANE is a portable, scalable, and extensible library for modelling the transport of energy by radiation or relativistic particles (in particular neutrinos).
Published in "DIAPHANE: A portable radiation transport library for astrophysical applications", 2020, Computer Physics Communications, Volume 252, article id. 107230.
DISORT: DIScrete Ordinate Radiative Transfer
LLLab (Stamnes, Knut et al.)
DISORT (DIScrete Ordinate Radiative Transfer) solves the problem of 1D scalar radiative transfer in a single optical medium, such as a planetary atmosphere. The code correctly accounts for multiple scattering by an isotropic or plane-parallel beam source, internal Planck sources, and reflection from a lower boundary. Provided that polarization effects can be neglected, DISORT efficiently calculates accurate fluxes and intensities at any user-specified angle and location within the user-specified medium.
Exo_k
Leconte, Jérémy
Exo_k is a Python 3 based library to handle radiative opacities from various sources for atmospheric applications. It now comes with a full-fledged 1D atmospheric evolution model.
Published in "Spectral binning of precomputed correlated-k coefficients", 2021, Astronomy & Astrophysics, Volume 645, id.A20, 7 pp.
HARP: High-performance Atmospheric Radiation Package
Li, C. et al.
HARP is an open-source program written in C++ that utilizes high-level data structure and parallel-computing algorithms for studying multiple-scattering planetary atmospheres.
Published in "A high-performance atmospheric radiation package: With applications to the radiative energy budgets of giant planets", 2018, Journal of Quantitative Spectroscopy and Radiative Transfer, Volume 217, p. 353-362.
NEMESIS: Non-linear Optimal Estimator for MultivariatE Spectral AnalySIS
Irwin, Patrick G. J. et al.
NEMESIS is a general purpose radiative transfer and retrieval tool designed for analyzing visible/infrared observations of any planetary atmosphere.
Published in "Radiative transfer models for Galileo NIMS studies of the atmosphere of Jupiter", 1997, Advances in Space Research, Volume 19, Issue 8, p. 1149-1158.
PHOENIX
Baron, E.; Chen, Bin; Hauschildt, P. H.
PHOENIX is a general-purpose state-of-the-art stellar and planetary atmosphere code. It can calculate atmospheres and spectra of stars all across the HR-diagram including main sequence stars, giants, white dwarfs, stars with winds, TTauri stars, novae, supernovae, brown dwarfs and extrasolar giant planets.
planetplanet
Luger, R.; Lustig-Yaeger, J.; Agol, E.
planetplanet models exoplanet transits, secondary eclipses, phase curves, and exomoons, as well as eclipsing binaries, circumbinary planets, and more. planetplanet is coded in C and wrapped in a user-friendly Python interface.
Published in "Planet-Planet Occultations in TRAPPIST-1 and Other Exoplanet Systems", 2017, The Astrophysical Journal, Volume 851, Issue 2, article id. 94, 30 pp.
POLARIS: POLArized RadIation Simulator
Reissl, S. et al.
POLARIS (POLArized RadIation Simulator) simulates the intensity and polarization of light emerging from analytical astrophysical models as well as complex magneto-hydrodynamic simulations on various grids.
Published in "Radiative transfer with POLARIS. I. Analysis of magnetic fields through synthetic dust continuum polarization measurements", 2016, Astronomy & Astrophysics, Volume 593, id.A87, 17 pp.
PyMieDap: Python Mie Doubling Adding Program
Rossi, Loïc ; Berzosa-Molina, Javier ; Stam, Daphne M.
PyMieDAP makes light scattering computations with Mie scattering and radiative transfer computations with full orders of scattering and taking into account the polarization of the light scattered.
Published in "PYMIEDAP: a Python-Fortran tool for computing fluxes and polarization signals of (exo)planets", 3028, Astronomy & Astrophysics, Volume 616, id.A147, 15 pp.
STaRS: Sejong Radiative Transfer through Raman and Rayleigh Scattering with atomic hydrogen
Chang, S.-J.; Lee, H.-W.
The 3D grid-based Monte Carlo code STaRS traces radiative transfer through Raman and Rayleigh scattering.
Published in "STaRS: A 3D Grid-based Monte Carlo Code for Radiative Transfer through Raman and Rayleigh Scattering with Atomic Hydrogen", 2020, Journal of the Korean Astronomical Society, vol. 53, pp. 169-179.