Exoplanet Modeling and Analysis Center

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    Select the models (one or more) that you would be most likely to use.

    Savransky et al.

    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.

    Reflection Spectra Repository for Cool Giant Planets
    Ryan J. MacDonald; Mark S. Marley; Jonathan J. Fortney; Nikole K. Lewis

    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.

    Exo-CCMC Heliophysics Models
    SWMF team, Glocer, Usmanov, et al.

    In the initial CCMC exoplanet applications adaptation, users are able to view and analyze simulations carried out with three different models: SWMF, PWOM and ALF3D. These simulations are used to demonstrate how heliophysics models hosted at CCMC can be used to explore exoplanetary problems. Please follow the links to individual models for more details and to access the simulation results.

    STARRY: Analytic Occultation Light Curves
    Rodrigo Luger, Eric Agol, Daniel Foreman-Mackey, David P. Fleming, Jacob Lustig-Yaeger, Russell Deitrick

    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.