Welcome to the GSFC Exoplanet Modeling and Analysis Center (EMAC)
EMAC serves as a repository and integration platform for modeling and analysis resources focused on the study of exoplanet characteristics and environments. EMAC provides community access to hosted models and tools, along with user-friendly web interfaces and a searchable database of exoplanet resources - both those hosted locally by EMAC as well as existing external tools and repositories hosted elsewhere.
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 as a contribution for others to use. If you would like to submit a new tool/model to EMAC, please visit the Submit a Resource page. If you have suggestions for improvements, please email us at
EMAC is a key project of the GSFC Sellers Exoplanet Environments Collaboration (SEEC). The P.I. is Avi Mandell, and the Deputy P.I. is Eric Lopez; more information on EMAC staffing and organization will be posted shortly.
Claire et al. Atm
IN PROGRESS — Atmos is a packaged photochemical model and climate model used to understand the vertical structure of various terrestrial atmospheres. Its photochemical model calculates the profiles of various chemicals in the atmosphere, including both gaseous and aerosol phases. Its climate model calculates the temperature profile of the atmosphere. While individually these models may be run for useful information, when coupled they offer a detailed analysis of atmospheric steady-state structures.
Coronagraphic Mission Simulator
Arney et al. Obs
This simplified coronagraph simulator tool is based on the coronagraph noise model in Robinson et al. 2016, adapted by J. Lustig-Yaeger, G. Arney and J. Tumlinson. The tool was developed for the LUVOIR mission concept, but can be used to simulated observations for any exoplanet coronagraphy mission.
Exoplanet Boundaries Calculator v1.0
Kopparapu et al. Atm
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.
Exoplanet Composition Interpolator
Eric Lopez, NASA GSFC Int
IN PROGRESS — This tool allows the user to load pre-computed planet evolution models and interpolate between those models to explore the possible structures of transiting exoplanets. Select a planet mass, radius, age, and irradiation and this tool will estimate it’s possible present-day gaseous envelope mass, rocky core mass, and thermal brightness.
Savransky et al. Obs
EXOSIMS is a modular, open source, Python-based framework for the simulation and analysis of exoplanet imaging space missions. The base code is highly extensible and allows for the end-to-end simulation of imaging missions, taking into account details about the spacecraft, its orbit, the instrumentation, the assumed population of exoplanets, and the mission operating rules.
Gabrielle Suissa, David Kipping Int
IN PROGRESS — HARDCORE exploits boundary conditions on exoplanet internal composition to solve for the minimum and maximum core radius fraction based on mass and radius limits.
Vinícius, Barentsen, Hedges, et al. Fit
IN PROGRESS — The lightkurve Python package offers a beautiful and user-friendly way to analyze astronomical flux time series data, in particular the pixels and lightcurves obtained by NASA’s Kepler, K2, and TESS missions.
PandExo JWST/HST Simulator v1.2.2
Batalha et al. Obs
PandExo is both an online tool and a Python package for generating instrument simulations of JWST's NIRSpec, NIRCam, NIRISS and NIRCam and HST WFC3. It uses throughput calculations from STScI's Exposure Time Calculator, Pandeia.
Planetary Spectrum Generator
Villanueva et al. Atm RT Obs
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).
Reflection Spectra Repository for Cool Giant Planets
Ryan J. MacDonald; Mark S. Marley; Jonathan J. Fortney; Nikole K. Lewis Atm
We present an extensive parameter space survey of the prominence of H2O 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 Teff = 150 → 400 K, log(g) = 2.0 - 4.0 (cgs), fsed = 1 - 10, and log(m) = 0.0 - 2.0 ́ solar. We discretize this parameter space into intervals of ΔTeff = 10 K, Δlog (g) = 0.1 dex, Δfsed = 1, and Δlog (m) = 0.5 dex, generating reflection spectra both with and without H2O opacity.
STARRY: Analytic Occultation Light Curves
Rodrigo Luger, Eric Agol, Daniel Foreman-Mackey, David P. Fleming, Jacob Lustig-Yaeger, Russell Deitrick Obs Fit
The STARRY code package enables the computation of light curves for various applications in astronomy: transits and secondary eclipses of exoplanets, light curves of eclipsing binaries, rotational phase curves of exoplanets, light curves of planet-planet and planet-moon occultations, and more. By modeling celestial body surface maps as sums of spherical harmonics, STARRY does all this analytically and is therefore fast, stable, and differentiable. Coded in C++ but wrapped in Python, STARRY is easy to install and use.
The LAPS (The Live Atmosphere-of-Planets Simulator)
Martin Turbet (LMD), Cédric Schott (ESEP) and the LMD team Atm RT
LAPS is a new tool that 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.