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.
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- 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!
ExoLyn: a golden mean approach to multi-species cloud modelling in atmospheric retrieval
Huang, Helong; Ormel, Chris W.; Min, Michiel
ExoLyn is a 1D cloud model that balances physical consistency with computational efficiency. ExoLyn solves the transport equation of cloud particles and vapor under cloud condensation rates that are self-consistently calculated from thermodynamics. ExoLyn is a standalone, open source package capable to be combined with optool to calculate solid opacities and with petitRADTRANS to generate transmission or emission spectra. The efficiency of ExoLyn opens the possibility of joint retrieval of exoplanets' gas and cloud components. ExoLyn has been designed to study cloud formation across a variety of planets: hot Jupiters, sub- Neptunes, and self-luminous planets.
GASTLI: GAS gianT modeL for Interiors
Acuña, Lorena; Kreidberg, Laura; Zhai, Meng et al.
GASTLI (GAS gianT modeL for Interiors) calculates the interior structure models for volatile-rich exoplanets with H/He and water envelopes. The code computes mass-radius curves, thermal evolution curves, and interior composition retrievals to fit a interior structure model to your mass, radius, age, and if available, atmospheric metallicity data. GASTLI can also plot the results, including internal and atmospheric profiles, a pressure-temperature diagram, mass-radius relations, and thermal evolution curves.
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.
GEOSCCM: Columbia River Flood Basalt Eruption Output
Guzewich, S.; Oman, L.; Richardson, J.; Whelley, P.; Bastelberger, S.; et al.
Selected output in NetCDF format from baseline and eruption simulations performed with the GEOSCCM global climate model.
Used in the study of volcanic climate warming through radiative and dynamical feedbacks of SO2 Emissions.
The datasets for this resource can be found in the following repositories:
Sonora Diamondback: The Sonora Substellar Atmosphere Models
Morley, Caroline V.; Mukherjee, Sagnick; Marley, Mark S; et al.
This is a new grid of cloudy atmosphere and evolution models for substellar objects. These models include the effect of refractory cloud species, including silicate clouds, on the spectra and evolution. It includes effective temperatures from 900 to 2400 K and surface gravities from log g = 3.5 to 5.5, appropriate for a broad range of objects with masses between 1 and 84 M J.
TriArc: Bayesian Detection Threshold test for Atmospheric Species utilising petitRADTRANS
Claringbold, Alastair B.
TriArc uses Bayesian statistics to determine the minimum abundance of an atmospheric species in a given model atmosphere (excluding the species of interest) and spectral noise profile. The current version is configured for transmission spectroscopy, but can be adjusted to emission spectroscopy on request. It is built using the forward modelling capabilities of petitRADTRANS. Utilised to calculated prebiosignature detection thresholds for various potential JWST targets in Claringbold et al. 2023.
FastChem: Ultra-fast Equilibrium Chemistry
Daniel Kitzmann, Joachim Stock
FastChem 2 is a new version of the established semi-analytical thermochemical equilibrium code FastChem. Whereas the original version of FastChem is limited to atmospheres containing a significant amount of the element hydrogen, FastChem 2 is now also applicable to chemical mixtures dominated by any other species such as CO2, N2, or Si for example. The code is written in object-oriented C++ and also offers an optional Python module.
photochem: A chemical model of planetary atmospheres
Wogan, Nicholas et al.
Photochem is a photochemical and climate model of planet's atmospheres. Given inputs, like the stellar UV flux, the atmospheric temperature structure, etc., this code will find the steady-state chemical composition of an atmosphere, or evolve atmospheres through time. The code also contains 1-D climate models.
ETHANE: Exoplanet Trend Haziness Analysis and Navigation Engine
Xinting Yu; Austin H. Dymont; David Murray; Emran Ismail; Connor Dickinson; Amaan Khwaja; Yash Rajpal
A web application that serves as a tool to understand photochemical hazes in temperate to warm exoplanet atmospheres. The exoplanet targets in this web application include exoplanets with equilibrium temperature < 1000 K, where photochemical hazes may exist to flatten their transmission spectra. The database allows us to examine relationships between exoplanet haziness and various planetary and stellar forcing parameters, so we can better understand the dominant process/property that affects how hazy an exoplanet is. Since the field is actively evolving with more upcoming data, this publicly available website allows us to add any new observations and to keep track of updated trends.
easyCHEM: A Python package for calculating chemical equilibrium abundances in exoplanet atmospheres
Lei, Elise; Mollière, Paul
easyCHEM2 is a Python package for calculating chemical equilibrium abundances (including condensation) and adiabatic gradients by minimization of the so-called Gibbs free energy. Ancillary outputs are the atmospheric adiabatic temperature gradient and mean molar mass. easyCHEM is a clone of the equilibrium chemistry part of NASA’s CEA code, written from scratch and with numerical stability in mind.
pyTPCI
Rosener, Riley; Zhang, Michael; Bean, Jacob L.
pyTPCI is a Python wrapper which couples newer versions of hydrodynamics code PLUTO and gas microphysics code CLOUDY to self-consistently simulate escaping atmospheres in 1D. Following TPCI, we modify CLOUDY to read in depth-dependent wind velocities, and to output useful physical quantities (including mass density, number density, and mean molecular weight as a function of depth).
PHOEBE: PHysics Of Eclipsing BinariEs
Prša, Andrej; Conroy, Kyle; Hambleton, Kelly; Jones, David; DeGroote, Pieter; Fabry, Matthias; Pablo, Herbert; and Giammarco, Joseph
PHOEBE (PHysics Of Eclipsing Binaries) is an eclipsing binary modeling code - reproducing and fitting light curves, radial velocity curves, and spectral line profiles of eclipsing systems, including exoplanetary transits.
MARCS: Model Atmospheres with a Radiative and Convective Scheme
The Uppsala/Montpellier MARCS team
This is a grid of one-dimensional, hydrostatic, plane-parallel and spherical LTE model atmospheres. These may be used together with atomic and molecular spectral line data and software for radiative transfer to generate synthetic stellar spectra.
The MARCS site contains about 52,000 stellar atmospheric models of spectral types F, G, K, and M in 3 different formats and also flux sample files indicating rough surface fluxes.
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.
ExoTR: Bayesian Statistical Analysis for Transmission Spectra Interpretation
Damiano, M. ; Hu, R.
ExoTR (Exoplanetary Transmission Retrieval) is a Bayesian inverse retrieval algorithm to interpret exoplanetary transmission spectra.
The code can be used in two ways:
- Leveraging the physics forward model only to generate synthetic planetary atmospheric transmission spectra (including the addition of errorbars);
- Using a retrieval routine based on nested sampling (i.e. MultiNest) to extract physical and chemical information from the input transmission spectra.
ECCOplanets: Simulation and Analysis of Rocky Planets
Timmermann, Anina
A python code to simulate the formation of rocky planets in chemical equilibrium (based on a Gibbs free energy minimisation) and tools for the analysis of the simulated planet. The code includes a database of thermochemical data and a database of stellar abundance patterns.
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.
The ExoMol database: Molecular line lists for exoplanets and other hot atmospheres
Tennyson, J. et al.
ExoMol is a database of molecular line lists that can be used for spectral characterization and simulation, and as input to atmospheric models of exoplanets, brown dwarfs and cool stars, and other models including those for combustion and sunspots.
sunbather
Linssen, Dion et al.
sunbather performs simulations of escaping planet atmospheres and their transit signatures. The main use of the code is to construct 1D Parker wind profiles using the Python p-winds package, to simulate these with photoionization code Cloudy, and to postprocess the output with a custom radiative transfer module to predict the transmission spectra of exoplanets, for a nearly arbitrary chemical composition.
The Sonora Elf Owl Models: Substellar Atmosphere Models
Mukherjee, Sagnick et al.
The Sonora Elf Owl Models is a successor to the Sonora Bobcat and Sonora Cholla models. The Sonora Elf Owl model grid includes cloud-free radiative-convective equilibrium model atmospheres with vertical mixing induced disequilibrium chemistry with sub-solar to super-solar atmospheric metallicities and Carbon-to-Oxygen ratio. The atmospheric models have been computed using the open-source radiative-convective equilibrium model PICASO. The model grid samples equilibrium temperatures between 275-2400 K and log(g) between 3.25-5.5. The mixing parameter log(Kzz) has been varied from 2-9 in cgs units. The [M/H] and C/O has been varied between [M/H]=-1.0 to [M/H]=+1.0 and C/O=0.22 to C/O=1.14.
SpectralRadex
Holdship, J. ; Vermarien, G. ; Van der Tak, F. F. S. et al.
A python library that serves two purposes: run RADEX directly from python and create model spectra from RADEX outputs.
A number of libraries exist for the first purpose. However, most either launch the RADEX compiled binary as a subprocess or wrap the original code. In the former case, the creating of subprocesses can interfere with many Python multiprocessing methods. In the latter, running multiple models simultanously can be problematic due to the use of F77 common blocks in RADEX.
SpectralRadex uses F2PY to compile a version of RADEX written in modern Fortran, most importantly dropping the use of common blocks. As a result, RADEX models can be run in parallel.
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.
GPS: Genesis Population Synthesis
Chakrabarty, A.; Mulders, G. D.
This is a Python-based population synthesis codebase that uses the Genesis database of planet formation models (Mulders et al. 2020). It consists of independent stages of internal structure and atmopsheric evolution models that can be used to synthesize a population of small exoplanets for comparison with observed domgraphics, e.g., from Kepler. It also offers statistical tools for drawing comparisons with observed distributions and studying occurrence trends. By invoking migration models (e.g., from Genesis), one can explore the occurrence patterns of the speculative water worlds and generate a list of potential targets using GPS.
IsoFATE: Isotopic Fractionation via ATmospheric Escape
Cherubim, Collin et al.
Open source code for the numerical model IsoFATE: Isotopic Fractionation via ATmospheric Escape. IsoFATE models mass fractionation of planetary atmospheres due to molecular diffusion for H, He, and an arbitrary number of trace species (e.g. D, O). The model includes EUV-driven photoevaporation and core-powered mass loss.
mini_chem: Miniature chemical kinetics model for gas giant GCMs
Lee, Elspeth K.H.; Tsai, Shang-Min; Hammond, Mark et al.
Mini-chem is a kinetic chemistry network solver primarily for gas giant atmospheric modelling, pared down from the large chemical networks. This makes use of 'net forward reaction tables', which reduce the number of reactions and species required to be evolved in the ODE solvers significantly. Mini-chem's NCHO network currently consists of only 12 species with 10 reactions, making it a lightweight and easy to couple network to large scale 3D GCM models, or other models of interest (such as 1D or 2D kinetic modelling efforts).
sai: Surface-Atmosphere Interactions on Warm Exoplanets
Byrne, Xander et al.
For warm rocky planets, broadly Venus-like planets, the high temperatures and moderate pressures at the base of their atmospheres may enable thermochemical equilibrium between rock and gas. This links the composition of the surface to that of the observable atmosphere. sai is a repository containing files for the GGchem equilibrium chemistry code, and associated helper functions, which we used to find a boundary in surface pressure-temperature space which simultaneously separates distinct mineralogical regimes and atmospheric regimes, potentially enabling inference of surface mineralogy from spectroscopic observations of the atmosphere (Byrne+23, MNRAS).
VSPEC: Variable Star PhasE Curve
VSPEC (Variable Star PhasE Curve) is an exoplanet modeling suite that combines NASA’s Planetary Spectrum Generator (PSG) with a custom variable star. Originally built to simulate the infrared excess of non-transiting planets, the code supports transit, eclipse, phase curve geometries as well as spots, faculae, flares, granulation, and the transit light source effect. Install it with pip or see the documentation linked below.
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.
photoevolver
Fernández, Jorge
photoevolver is a Python module that evolves the gaseous envelope of planets backwards and forward in time, taking into account internal structure and cooling rate, atmospheric mass loss processes, and the stellar X-ray emission history.
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.
SWAMPE: A Shallow-Water Atmospheric Model in Python for Exoplanets
Landgren, E. and Nadeau, A.
SWAMPE is a Python package for modeling the dynamics of exoplanetary atmospheres. SWAMPE is an intermediate-complexity, two-dimensional shallow-water general circulation model. Benchmarked for synchronously rotating hot Jupiters and sub-Neptunes, the code is modular and could be easily modified to model dissimilar space objects, from Brown Dwarfs to terrestrial, potentially habitable exoplanets. SWAMPE can be easily run on a personal laptop.
PyMieScatt: The Python Mie Scattering package
Sumlin, B., Heinson, W., and Chakrabarty, R.
PyMieScatt is a comprehensive forward and inverse Mie theory solver for Python 3. This package calculates relevant parameters such as absorption, scattering, extinction, asymmetry, backscatter, and more. It also contains single-line functions to calculate optical coefficients (in Mm-1) of ensembles of particles in lognormal (with single or multiple modes) or custom size distributions.
The inverse calculations retrieve the complex refractive index from laboratory measurements of scattering and absorption (or backscatter), useful for studying atmospheric organic aerosol of unknown composition.
Read more in our JQSRT paper!
PHOTOe: An efficient Monte Carlo model for the slowing down of photoelectrons
Monte Carlo model for simulating the slowing down of photoelectrons in gases in the local deposition approximation.
Version v1 works with H and He atoms plus thermal electrons. The model is described in:
García Muñoz, Icarus, Volume 392, 1 March 2023, 115373
The model is available at https://antoniogarciamunoz.wordpress.com/ and upon email request from the author.
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.
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.
Kamodo: a CCMC tool for access, interpolation, and visualization of data in Python
The Community Coordinated Modeling Center at NASA GSFC
Kamodo allows model developers to represent simulation results as mathematical functions which may be manipulated directly by end users. Kamodo handles unit conversion transparently and supports interactive science discovery through jupyter notebooks with minimal coding and is accessible through python.
ECLIPS3D: Public code for linear wave and circulation calculations
Debras, F. et al.
Public Fortran 90 code for linear wave and circulation calculations, developed originally for planetary atmospheres, with python scripts provided for data analysis. 4 setups are provided:
2D_axi: eigenvector setup in spherical coordinates assuming axisymmetry around the axis of rotation. A longitudinal wavenumber, m, must therefore be provided.
2D_shallow: eigenvector setup for shallow water beta-plane. The latitude of the beta plane and characteristic height can be changed.
3D: eigenvector setup in full 3D, spherical coordinates.
3D_steady: linear circulation setup, hence matrix inversion. A forcing and a dissipation have to be implemented for a linear steady state to exist.
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.
VPLanet: The Virtual Planet Simulator
Barnes, Rory et al.
VPLanet simulates planetary system evolution with a single executable: 1) thermal and magnetic evolution of terrestrial planets, 2) magma oceans, 3) radiogenic heating of interiors, 4) tidal effects, 5) rotational axis evolution, 6) stellar evolution, including pre-MS, XUV, and spin-down, 7) stellar flares, 8) climate via a 1-D EBM, 9) atmospheric escape, including water photolysis and H escape, 10) approximate orbital evolution, 11) exact orbital evolution, 12) circumbinary planet orbits, and 13) galactic perturbations on planetary systems. The code is validated by reproducing selected Solar System, exoplanet, and binary star properties. Documentation and numerous examples are provided.
Pytmosph3R: Transmission/emission spectra from 3D atmospheric simulations (GCMs, ...)
Falco, Aurélien; Pluriel, William; Leconte, Jérémy; Caldas, Anthony
Pytmosph3R is a Python-3 library that computes transmission and emission spectra based on 3D atmospheric simulations, for example performed with the LMDZ generic global climate model.
Pytmosph3R can be used in notebooks or on the command line, using a configuration similar to that of TauREx.
The library should include a feature to generate phase/light-curves in the next release.
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.
HOMER: A Bayesian inverse modeling code
Himes, Michael et al.
HOMER (the Helper Of My Eternal Retrievals) is a Bayesian inverse modeling code. Given some data and uncertainties, the posterior distribution is determined for some model. HOMER allows for both nested sampling and Markov chain Monte Carlo (MCMC) frameworks.
HOMER's forward model is a neural network (NN) surrogate model trained by MARGE. For details on MARGE, see the MARGE User Manual at https://exosports.github.io/MARGE/doc/MARGE_User_Manual.html.
HOMER is released under the Reproducible Research Software License and welcomes community contributions via pull requests on Github.
special: SPEctral Characterization of ImAged Low-mass companions
Christiaens, Valentin
special is a package developed for the spectral characterization of directly imaged low-mass companions (MLT dwarfs). Nonetheless, this toolkit can also be used in a more general way for the characterisation of any object with a measured spectrum, provided an input model or template grid. The available tools range from the calculation of spectral covariance matrices (e.g. for IFS datacubes) and empirical spectral indices to the Bayesian inference of atmospheric parameters provided an input grid of models. In the latter case, an MCMC or nested sampler can be used, and additional parameters such as (extra) black body component(s) and extinction can be considered.
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.
Isca: Idealized global circulation modeling: A flexible GCM for modelling planetary atmospheres.
Isca is a framework for the construction of models of the global circulation of planetary atmospheres at varying levels of realism and complexity. Isca itself is not a single model, nor is it intended to provide a fully ‘comprehensive’ model capable of weather forecasts or climate projections for policy use. Rather, our intent is to enable the user to make appropriate models for the planet or problem of interest. Isca can and has been used for Earth, Mars, Jupiter, Titan and various exoplanets.
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.
EVolve: Growth and evolution of volcanically-derived atmospheres
Liggins, Philippa; Kitzmann, Daniel; Stock, Joachim
EVolve calculates the chemical composition and surface pressure of a ID atmosphere on a rocky planet which is being produced by volcanic activity, as it grows over time. Once the initial volatile content of the planet's mantle, and the composition & resultant surface pressure of any pre-existing atmosphere is set, a volcanic degassing model (EVo) will calculate the amount and speciation of any volcanic gases released into the atmosphere over each time step. Thermochemical equilibrium is assumed so the final chemical composition of the atmosphere is calculated according to the pre-set surface temperature. Future versions will include hydrogen escape as a loss mechanism.
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.
UBER: Universal Boltzmann Equation Solver
Zheng, L. et al.
UBER is a Fortran library that solves the general form of Fokker-Planck equation and Boltzmann equation, diffusive or non-diffusive, that appear in modeling planetary radiation belts. Users can freely specify (1) the coordinate system, (2) boundary geometry and boundary conditions, and (3) the equation terms and coefficients. The solver works for problems in one to three spatial dimensions. The solver is based upon the mathematical theory of stochastic differential equations which is of Monte Carlo nature, and the solution stochastic uncertainty may be dictated arbitrarily small at the cost of longer iterations.
PEP: The Planetary Ephemeris Program
Developed by many; original: Michael Ash; most recent and longest- time-involved: John Chandler
This Fortran computer program models orbital motion in the solar system, including almost 100 individual asteroids as well as all of the planets and some moons, along with a detailed model of our moon, and a model of pulsar motions and of distant radio sources. It takes as input diverse astrometric data: radio, radar, laser, timing of signal arrivals, and VLBI. The program can solve for well over 100 parameters, including orbital and (for some bodies) rotational initial conditions, sky coordinates for radio sources, plasma densities, the second harmonic of the Sun's gravitational field, and those related to tests of fundamental physics.
VULCAN: Photochemical kinetics for planetary atmospheres
Tsai, Shang-Min
Photochemical kinetics for (exo-)planetary atmospheres, a fast and easy-to-use python code. The model has hierarchical C-H-N-O-S networks and treats thermochemistry, photochemistry, eddy diffusion, advection transport, condensation, and various boundary conditions.
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.
ATES: ATmospheric EScape
Caldiroli, Andrea; Haardt, Francesco; Gallo, Elena; Spinelli, Riccardo; Malsky, Isaac; Rauscher, Emily
The ATES hydrodynamics code computes the temperature, density, velocity and ionization fraction profiles of highly irradiated planetary atmospheres, along with the current, steady-state mass loss rate. ATES solves the one-dimensional Euler, mass and energy conservation equations in radial coordinates through a finite-volume scheme. The hydrodynamics module is paired with a photoionization equilibrium solver that includes cooling via bremsstrahlung, recombination and collisional excitation/ionization for the case of an atmosphere of primordial composition (i.e., pure atomic hydrogen-helium), while also accounting for advection of the different ion species.
ExoPlaSim: Extending the Planet Simulator for Exoplanets
Paradise, Adiv et al.
A modified version of the PlaSim 3D climate model, designed to simulate planets with Earth-like atmospheric compositions across a wide parameter space, including tidally-locked rotation, 0.1-10 bars surface pressure, and a range of stellar spectra. ExoPlaSim has a Python API for configuring and running models, as well as utilities for interacting with and analyzing the netCDF output files. ExoPlaSim is also pip-installable. As an intermediate-complexity model, ExoPlaSim trades some complexity for speed, and is able to run on a range of hardware including personal laptops and high-performance computing clusters, with typical performance of 1 year of climate at T21 resolution in 1-5 minutes.
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.
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.
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.
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
THOR: Flexible Global Circulation Model to Explore Planetary Atmospheres
Mendonça, J. et al. 2016; Deitrick, R., et al. 2020
THOR is a GCM that solves the three-dimensional non-hydrostatic Euler equations on an icosahedral grid. THOR was designed to run on Graphics Processing Units (GPUs).
Aeolus: Python Library for Object-Oriented Analysis of Atmospheric Model Output
Sergeev, D. E.
Aeolus is a library for analysis and plotting of a climate model output, primarily of the UK Met Office Unified Model when it is used to simulate various planetary atmospheres. Aeolus is built on top of iris and has various functions tailored to exoplanet research, e.g. in the context of tidally-locked exoplanets.
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.
AstroBEAR: An Adaptive Mesh Refinement Code for Computational Astrophysics
Jonathan Carroll-Nellenback, Adam Frank, Baowei Liu, Shule Li, Erica Fogerty, Andrew Cunningham, Sorin Mitran, Zhuo Chen, Kris Yirak, Eddie Hansen, Martin Huarte-Espinosa, Luke Chamandy, Alex Debrecht, Yangyuxin Zou, Atma Anand
AstroBEAR is a parallelized hydrodynamic/MHD simulation code suitable for a variety of astrophysical problems. Derived from the BearCLAW package written by Sorin Mitran, AstroBEAR is designed for 2D and 3D adaptive mesh refinement (AMR), multi-physics simulations. Users write their own project modules by specifying initial conditions and continual processes (such as an inflow condition). In addition, AstroBEAR comes with a number of pre-built physical phenomena such as clumps and winds that can be loaded into a user module.
SVO Theoretical Spectra Server: A Server of Data for over 60 Collections of Theoretical Spectra and Observational Templates
Carlos Rodrigo, Spanish Virtual Observatory, CAB, CSIC-INTA
The SVO Theory Server provides data for more than 60 collections of theoretical spectra and observational templates.
Using this web page you can search for spectra in each collection in terms of the corresponding grid parameter ranges, visualize the spectra and/or download them in ascii or VOTable format. You will be able to compare spectra from different collections too.
Synthetic Photometry is also available for these spectra and all the filters in the SVO Filter Profile Service.
ExoCAM: Exoplanet Extension for the CAM GCM
Wolf, Eric T.
ExoCAM is a model extension to the National Center for Atmospheric Research (NCAR) Community Earth System Model (CESM) 3-D general circulation and climate system model, which facilitates simulations of exoplanetary atmospheres. This software contains system configuration files, source code, initial condition files, namelists, and some basic analysis scripts. Familiarity with CESM is prerequisite. CESM must be downloaded separately. The radiative transfer component of ExoCAM is stored in a separate GitHub link, and can be run independently or coupled with ExoCAM/CESM.
JET: JWST Exoplanet Targeting Program
Fortenbach, Charles; Dressing, Courtney et al.
JWST will devote significant observing time to the study of exoplanets. It will not be serviceable as was the Hubble, and therefore the spacecraft/instruments will have a relatively limited life. It is important to get as much science as possible out of this limited observing time. We provide a computer tool, JET, to optimize lists of exoplanet targets for atmospheric characterization. JET takes catalogs of planet detections; categorizes the targets by radius and equilibrium temp.; estimates planet masses; generates model spectra and simulated instrument spectra; performs a statistical analysis to confirm an atmospheric detection; and finally, ranks the targets by observation time required.
The Opacity Wizard: A Tool for Visualizations of Opacity and Abundance Data for Exoplanet and Brown Dwarf Atmospheres
Morley, Caroline
This tool was developed to allow for easy and fast visualizations of opacity and abundance data for exoplanet and brown dwarf atmospheres. In particular, it was designed to be used by observers studying these substellar objects as an easy way of exploring which molecules are most important for a given planet and predict where the absorption features of those molecules will be. It is simple to use for non-python experts and requires only Python/NumPy/Matplotlib/Jupyter.
REPAST: Rocky ExoPlanet Albedo Spectra Tool
Smith, Adam J. R. W.; Mandell, Avi; Villanueva, Geronimo
Here we present a database of albedo spectra for rocky, Earth-sized and Earth-mass exoplanets, as computed with the NASA Planetary Spectrum Generator tool (psg.gsfc.nasa.gov; Villanueva et al. 2018). The database is presented in two Python .pickle files containing pandas DataFrame objects. The DataFrame index values are wavelength, in micrometers; while the column name values contain the encoded parameters represented in the model object's albedo spectra contained with in that column. Each cell then gives the calculated geometric albedo value for the column-named model planet at the row-indicated wavelength.
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.
Atmos: Packaged Photochemical and Climate Model
Atmos is a package containing two atmospheric models, along with scripts to couple them together. One of the atmospheric models is a 1D photochemical model that calculates the profiles of chemical species, including both gaseous and aerosol phases. The second model is a 1D climate model that calculates the temperature profile. While individually these models may be run for useful information, when coupled they offer a detailed analysis of atmospheric steady-state structures.
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).
CGP: Reflection Spectra Repository for Cool Giant Planets
2
MacDonald, Ryan J.; Marley, Mark S.; Fortney, Jonathan J. et al.
We present an extensive parameter space survey of the prominence of $H_2O$ in reflection spectra of cool giant planets. We explore the influence of a wide range of effective temperatures, gravities, metallicities, and sedimentation efficiencies, providing a grid of >50,000 models for the community. Our models range from $T_{eff}$ = 150 → 400 K, log(g) = 2.0–4.0 (cgs), $f_{sed}$ = 1–10, and log(m) = 0.0–2.0 ́ solar. We discretize this parameter space into intervals of $ΔT_{eff}$ = 10 K, Δlog(g) = 0.1 dex, $Δf_{sed}$= 1, and Δlog(m) = 0.5 dex, generating reflection spectra both with and without $H_2O$ opacity.
PyATMOS NExSci Repository: A Dataset of ~125,000 Simulated 1-D Exoplanet Atmospheres
William Fawcett et al.
The PyATMOS NExSci dataset comprises ~125,000 simulated 1-D exoplanet atmospheres. All of these exoplanets are based around an Earth-like planet that orbits a star similar to the Sun, but with different gas mixtures in their atmospheres. The atmospheres were generated using the PyATMOS code. The parameter space was created by incrementally varying the concentrations of carbon dioxide, oxygen, water vapour, methane, hydrogen, and nitrogen; and for each point in the parameter space an atmosphere was simulated. Other gases with negligible concentrations, such as ozone, were not varied. The planet's composition, orbital parameters and stellar parameters were also not varied.
species: Toolkit for atmospheric characterization of directly imaged exoplanets
Stolker, Tomas
The species toolkit provides a coherent framework for spectral and photometric analysis of directly imaged exoplanets which builds on publicly-available data and models from various resources. There are tools available for both grid retrievals and free retrievals with Bayesian inference, color-magnitude and color-color diagrams, empirical spectral analysis, spectral and photometric calibration, and synthetic photometry.
TROPF: Tidal Response Of Planetary Fluids
Tyler, Robert
The TROPF (Tidal Response Of Planetary Fluids) software package is a MATLAB/Octave package that enables efficient terrestrial fluid tidal studies across a wide range of parameter space. TROPF includes several different solutions to the governing equations in classical tidal theory, and can calculate millions of such solutions on several-minute-long timescales. A comprehensive manual is included in the distribution directory. To help improve the development of TROPF, or become involved in future releases, please send feedback to rtyler@umbc.edu.
ATMO Generic Grid @ ExoCTK: A Generic Model Grid of Planetary Transmission Spectra
Goyal, Jayesh et al.
A generic model grid of planetary transmission spectra, scalable to a wide range of $H_2$/He dominated atmospheres. The grid is computed using the 1D/2D atmosphere model ATMO for two different chemical scenarios, first considering local condensation only, secondly considering global condensation and removal of species from the atmospheric column (rainout). Using the model grid as a framework, we allow you to rescale your models with custom temperature, gravity, and radius values. The web interface is hosted and maintained by the STScI Exoplanet Characterization ToolKit.
ATMO Exoplanet-Specific Grid: A Grid of Forward Model Transmission Spectra
Goyal, Jayesh et al.
A grid of forward model transmission spectra, adopting an isothermal temperature-pressure profile, alongside corresponding equilibrium chemical abundances for 117 observationally significant hot exoplanets (equilibrium temperatures of 547–2710 K). This model grid has been developed using a 1D radiative–convective–chemical equilibrium model termed ATMO, with up-to-date high-temperature opacities.
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.
PyATMOS: Software Package to Configure and Run the Virtual Planetary Laboratories' ATMOS Software
Fawcett, William et al.
PyATMOS is a software package able to configure and run the Virtual Planetary Laboratories' ATMOS software, which is an exoplanetary atmosphere simulator. PyATMOS is written in Python, allowing easy user configuration and running, and is optionally configurable with Docker and therefore can be used on any machine with Docker and Python installed, regardless of the operating system. PyATMOS can be used in "single-use" mode, simulating a single exoplanet atmosphere with a given set of atmospheric parameters, but also in a parallel mode, whereby a grid of possible parameters for many atmospheres is supplied. PyATMOS will explore this parameter space and produce a database of the results.
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.
Exoplanet Boundaries Calculator: An Online Condensations Boundary Calculator
1.1
Kopparapu et al.
The Exoplanet Boundaries Calculator (EBC) is an online calculator that provides condensation boundaries (in stellar fluxes) for ZnS, H2O, CO2 and CH4 for the following planetary radii that represent transition to different planet regimes: 0.5, 1, 1.75, 3.5, 6, and 14.3 RE. The purpose is to classify planets into different categories based on a species condensing in a planet's atmosphere. These boundaries are applicable only for G-dwarf stars.
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:
Aiolos: A multi-purpose 1-D hydrodynamics code for planetary atmospheres
Schulik, M. ; Booth, R. A.
AIOLOS solves differential equations for hydrodynamics, friction, (thermal) radiation transport and (photo)chemistry for simulating accretion onto, and hydrodynamic escape from, planetary atmospheres.
Published in "AIOLOS - A multipurpose 1D hydrodynamics code for planetary atmospheres", 2023, Monthly Notices of the Royal Astronomical Society, Volume 523, Issue 1, pp.286-304.
AlfvenWaver
Rusaitis, L.
AlfvenWaver is a command-line interfaced program package that is aimed at computing shear Alfvén wave resonances along planetary magnetic field lines.
Published in "AlfvenWaver", 2020, Zenodo.
Ariel Big Challenge Database
Changeat, Quentin ; Yip, Kai Hou
The database contains 105,877 realistic Ariel observations in Tier-2 resolutions. All examples are generated with a pre-determined atmospheric assumptions. 26% (26,109) of these observations are complemented with retrieval results produced from Nested Sampling algorithms.
Published in "ESA-Ariel Data Challenge NeurIPS 2022: introduction to exo-atmospheric studies and presentation of the Atmospheric Big Challenge (ABC) Database", 2023, RAS Techniques and Instruments, Volume 2, Issue 1, pp.45-61.
BART: Bayesian Atmospheric Radiative Transfer
Cubillos, Patricio et al.
The BART retrieval package produces estimates and uncertainties for an atmosphere's thermal profile and chemical abundances from observations.
Published in "An Open-source Bayesian Atmospheric Radiative Transfer (BART) Code. I. Design, Tests, and Application to Exoplanet HD 189733b", 2022, The Planetary Science Journal, Volume 3, Issue 4, id.80, 31 pp.
Cloud Transport Model
Ormel, C.
Python module for computing cloud structures.
Published in "ARCiS framework for exoplanet atmospheres. The cloud transport model", 2019, Astronomy & Astrophysics, Volume 622, id.A121, 12 pp.
ExoCTK: The Exoplanet Characterization Toolkit
Bourque, M. et al.
ExoCTK is an open-source, modular, data analysis software package focused primarily on the atmospheric characterization of exoplanets and time-series observation planning.
Published in "The Exoplanet Characterization Toolkit (ExoCTK)", 2021, Zenodo.
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.
Exo_Transmit: Exo-Transmit radiative transfer code for calculating exoplanet transmission spectra
Kempton, E. M. -R. et al.
A software package to calculate exoplanet transmission spectra for planets of varied composition.
Published in "Exo-Transmit: An Open-Source Code for Calculating Transmission Spectra for Exoplanet Atmospheres of Varied Composition", 2017, Publications of the Astronomical Society of the Pacific, Volume 129, Issue 974, pp. 044402 (2017).
gefera
Gordon, Tyler A. ; Agol, Eric
Fast, exact, and differentiable light curves for mutual transits.
Published in "Analytic Light Curve for Mutual Transits of Two Bodies Across a Limb-darkened Star", 2022, The Astronomical Journal, Volume 164, Issue 3, id.111, 23 pp.
GGCHEM: Fast thermo-chemical equilibrium code
Woitke, P. ; Helling, C.
GGchem is a fast thermo-chemical equilibrium code with or without equilibrium condensation down to 100K.
Published in "GGchem: Fast thermo-chemical equilibrium code", 2021, Astrophysics Source Code Library, record ascl:2104.018.
Used in "Equilibrium chemistry down to 100 K. Impact of silicates and phyllosilicates on the carbon to oxygen ratio", 2018, Astronomy & Astrophysics, Volume 614, id.A1, 28 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.
kelp
Morris, B. M. et al.
Photometric phase curves of exoplanets.
Published in "Physically-motivated basis functions for temperature maps of exoplanets", 2022, Astronomy & Astrophysics, Volume 660, id.A123, 17 pp.
LavAtmos: An open-source chemical equilibrium vaporization code for lava worlds
van Buchem, Christiaan P. A. et al.
LavAtmos performs gas-melt equilibrium calculations for a given temperature and melt composition.
Published in "LavAtmos: An open-source chemical equilibrium vaporization code for lava worlds", 2023, Meteoritics & Planetary Science, Volume 58, Issue 8, pp. 1149-1161.
MC-SPAM: Monte-Carlo Synthetic-Photometry/Atmosphere-Model
Espinoza, N.; Jordán, A.
MC-SPAM is an algorithm to generate limb-darkening coefficients from models that are comparable to transit photometry according to the formalism described in Espinoza & Jordan (2015).
Published in "Limb darkening and exoplanets: testing stellar model atmospheres and identifying biases in transit parameters", 2015, Monthly Notices of the Royal Astronomical Society, Volume 450, Issue 2, p.1879-1899.
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.
NLTE TIPS for Planetary Atmospheres: Non-Local Thermodynamic Equilibrium Total Internal Partition Sums for Planetary Atmospheres
Gamache, R. R. et al.
A FORTRAN code (NLTE_TIPS_2021.for) and associated input files to compute partition sums for non-local thermodynamic equilibrium conditions for nine molecules of importance in planetary atmospheres: H2O, CO2, O3, N2O, CO, CH4, NO, NO2, and OH.
Published in "Partition sums for non-local thermodynamic equilibrium conditions for nine molecules of importance in planetary atmospheres", 2022, Icarus, Volume 378, article id. 114947.
OBERON: OBliquity and Energy balance Run on N-body systems
Forgan, Duncan
OBERON models the climate of Earthlike planets under the effects of an arbitrary number and arrangement of other bodies, such as stars, planets and moons.
Published in "Milankovitch cycles of terrestrial planets in binary star systems", 2016, Monthly Notices of the Royal Astronomical Society, Volume 463, Issue 3, p.2768-2780.
PACMAN: Planetary Atmosphere, Crust, and MANtle geochemical evolution model
Krissansen-Totton, Joshua et al.
PACMAN runs a coupled redox-geochemical-climate evolution model.
Published in "Was Venus Ever Habitable? Constraints from a Coupled Interior-Atmosphere-Redox Evolution Model", 2021, The Planetary Science Journal, Volume 2, Issue 5, id.216, 27 pp.
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.
PlaSim: Planet Simulator
Lunkeit, F. et al.
PlaSim is a climate model of intermediate complexity for Earth, Mars and other planets.
Published in "PlaSim: Planet Simulator", 2021, Astrophysics Source Code Library (ASCL).
Used in "Three-dimensional Climate Simulations for the Detectability of Proxima Centauri b", 2021, The Astrophysical Journal, Volume 909, Issue 2, id.191, 15 pp.
PLATYPOS: PLAneTarY PhOtoevaporation Simulator
Ketzer, L.; Poppenhaeger, K.
A python code to perform planetary photoevaporative mass-loss calculations for close-in planets with hydrogen-helium envelopes atop Earth-like rocky cores.
Published in "Estimating photoevaporative mass loss of exoplanets with PLATYPOS", 2022, Astronomische Nachrichten, Volume 343, Issue 4, article id. e10105.
POSEIDON: A Multidimensional Atmospheric Retrieval Code for Exoplanet Spectra
MacDonald, R. J.
POSEIDON is a Python package for the modelling and analysis of exoplanet spectra. POSEIDON supports the modelling and retrieval of exoplanet transmission, emission, and reflection spectra, alongside emission spectra of brown dwarfs. POSEIDON now supports high-resolution cross-correlation retrievals for ground-based high-dispersion instruments.
Published in "POSEIDON: A Multidimensional Atmospheric Retrieval Code for Exoplanet Spectra", 2023, Journal of Open Source Software, Vol. 8(81), id. 4873.
PyLightcurve
Tsiaras, A. et al.
PyLightcurve is a model for light-curves of transiting planets.
Published in "A New Approach to Analyzing HST Spatial Scans: The Transmission Spectrum of HD 209458 b", 2016, The Astrophysical Journal, Volume 832, Issue 2, article id. 202, 17 pp.
Pylightcurve-torch
Morvan, Mario et al.
An exoplanet transit modelling package for deep learning applications in Pytorch.
Published in "PyLightcurve-torch: a transit modeling package for deep learning applications in PyTorch", 2021, Publications of the Astronomical Society of the Pacific, Volume 133, Issue 1021, id.034505, 6 pp.
SimAb
Khorshid, Niloofar et al.
SimAb (Simulating Abundances) simulates planet formation, focusing on the atmosphere accretion of gas giant planets.
Published in "SimAb: A simple, fast, and flexible model to assess the effects of planet formation on the atmospheric composition of gas giants", 2022, Astronomy & Astrophysics, Volume 667, id.A147, 13 pp.
SLOPpy: Spectral Lines Of Planets with python
Sicilia, D. et al.
SLOPpy is a robust, versatile framework for the characterization of atmospheres of planetary systems.
Published in "Characterization of exoplanetary atmospheres with SLOPpy", 2022, Astronomy & Astrophysics, Volume 667, id.A19, 30 pp.
TauREx 3: Tau Retrieval for Exoplanets
Al-Refaie, Ahmed F. et al.
TauREx 3 is a fully bayesian inverse atmospheric retrieval framework.
Published in "TauREx 3: A Fast, Dynamic, and Extendable Framework for Retrievals", 2021, The Astrophysical Journal, Volume 917, Issue 1, id.37, 23 pp.
The Sonora Brown Dwarf Atmosphere and Evolution Models: Model Description and Application to Cloudless Atmospheres in Rainout Chemical Equilibrium
Marley, M. S. et al.
A new generation of substellar atmosphere and evolution models, appropriate for application to studies of L-, T-, and Y-type brown dwarfs and self-luminous extrasolar planets.
Published in "The Sonora Brown Dwarf Atmosphere and Evolution Models. I. Model Description and Application to Cloudless Atmospheres in Rainout Chemical Equilibrium", 2021, The Astrophysical Journal, Volume 920, Issue 2, id.85, 20 pp.
TLC: Tidally Locked Coordinates
Koll, D.
TLC converts global climate model (GCM) output from standard/Earth-like coordinates into a tidally locked coordinate system.
Published in "TLC: Tidally Locked Coordinates", 2020, Astrophysics Source Code Library (ASCL).
Used in "How Does Background Air Pressure Influence the Inner Edge of the Habitable Zone for Tidally Locked Planets in a 3D View?", 2020, The Astrophysical Journal Letters, Volume 901, Issue 2, id.L36, 8 pp.
Transit: Radiative-transfer code for planetary atmospheres
Cubillos, P. et al.
Transit calculates the transmission or emission spectrum of a planetary atmosphere with application to extrasolar-planet transit and eclipse observations, respectively.
Published in "Transit: Radiative-transfer code for planetary atmospheres", 2017, Astrophysics Source Code Library (ASCL).
UTM: Universal Transit Modeller
Deeg, Hans J.
UTM is a light-curve simulator for all kinds of transiting or eclipsing configurations between arbitrary numbers of several types of objects, which may be stars, planets, planetary moons, and planetary rings.
Published in "UTM: Universal Transit Modeller", 2014, Astrophysics Source Code Library (ASCL).
VapoRock
Wolf, A. S. et al.
Thermodynamics of vaporized silicate rocks & melts for modeling magma ocean atmospheres and stellar nebula.
Published in "VapoRock: Thermodynamics of Vaporized Silicate Melts for Modeling Volcanic Outgassing and Magma Ocean Atmospheres", 2023, The Astrophysical Journal, Volume 947, Issue 2, id.64, 20 pp.
Virga: A Cloud Model for Exoplanets and Brown Dwarfs
Batalha, Natasha E.; Rooney, Caoimhe; Mukherjee, Sagnick et al.
The observed atmospheric spectrum of exoplanets and brown dwarfs depends critically on the presence and distribution of atmospheric condensates. The Ackerman and Marley methodology for predicting the vertical distribution of condensate particles is widely used to study cloudy atmospheres and has recently been implemented in an open-source python package, Virga. The model relies upon input parameter, the sedimentation efficiency, which until now has been held constant.
Published in "A New Sedimentation Model for Greater Cloud Diversity in Giant Exoplanets and Brown Dwarfs", Rooney, Caoimhe M., Batalha, Natasha E., Gao, Peter, & Marley, Mark S, 2022, ApJ, 925, 33
water-worlds Grid
Kempton, Eliza. M. -R. et al.
Models of hydrogen-helium-water atmospheres with water abundances ranging from solar to 100% water vapor.
Published in "Where are the Water Worlds?: Self-consistent Models of Water-rich Exoplanet Atmospheres", 2023, The Astrophysical Journal, Volume 953, Issue 1, id.57, 21 pp.
WoMa: World Maker
Ruiz-Bonilla et al.
Create models of rotating and non-rotating planets by solving the differential equations for hydrostatic equilibrium, and create initial conditions for e.g. smoothed particle hydrodynamics (SPH) simulations by placing particles that precisely match the planet's profiles.