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Department of Astronomy
University of Texas at Austin
RLM, 2515 Speedway
Austin, TX 78712

©2017 BY CAROLINE MORLEY. PROUDLY CREATED WITH WIX.COM

PUBLICLY AVAILABLE MODELS

This is a compilation of exoplanet atmosphere simulations, including synthetic spectra, photometry, and other data from a series of papers on modeling both exoplanets and brown dwarfs. Please cite the references provided.

 

MORLEY ET AL. 2017: TRAPPIST/MEARTH PLANET MODELS

Model transmission and emission spectra, as well as JWST MIRI eclipse depths, for each of the 7 TRAPPIST-1 planets as well as two terrestrial planets found by MEarth, GJ 1132b and LHS 1140b.

MORLEY ET AL. 2015: SUB-NEPTUNE MODELS INCLUDING THE EFFECTS OF CLOUDS AND HAZES

 Models of GJ 1214b “analogs” from Morley et al. 2015, including cloudy, hazy, and cloud-free models. These include thermal emission, transmission, and albedo spectra. Other similar models available upon request. 

MORLEY ET AL. 2012: T/Y DWARF MODELS

Model photometry and spectra currently available. These models include Na2S, KCl, ZnS, MnS, and Cr clouds. Models have effective temperatures from 400 to 1200 K, gravities from log g(cgs) 4.0 to 5.5. These models are especially appropriate for late T dwarfs cooler than ~900 K (spectral type ~T9).  We calculate Vega absolute magnitudes for Y, J, H, K, L’, M’ (all MKO), IRAC bands 1-4, and WISE bands 1-4. Other filters available upon request.

MORLEY ET AL. 2014: Y DWARF MODELS

These models include H2O ice clouds in addition to the Na2S, KCl, ZnS, MnS, and Cr clouds. Models have effective temperatures from 200 to 450 K, gravities from log g(cgs) 3.0 to 5.0. These models are partly cloudy (see Morley et al. 2014): we assume that 50% of the surface is covered in clouds. We calculate Vega absolute magnitudes for Y, J, H, K, L', M' (all MKO), IRAC bands 1-4, and WISE bands 1-4. Other filters available upon request. 

SAUMON ET AL. 2012: CLOUD-FREE MODELS FOR T DWARFS

Model photometry and spectra currently available. These models do not include cloud opacity. Models have effective temperatures from 200 to 1200 K, gravities from log g(cgs) 4.0 to 5.5. These models are appropriate for mid-late T dwarfs cooler than ~1100-1200 K (spectral type ~T3). Note that L dwarfs and early T dwarfs require models that include iron/silicate clouds (photometry not available here). We calculate Vega absolute magnitudes for Y, J, H, K, L’, M’ (all MKO), IRAC bands 1-4, and WISE bands 1-4. Other filters available upon request. 

SAUMON ET AL. 2008: EVOLUTION MODELS

These models include radii, luminosities, temperatures, ages, and masses for brown dwarfs with cloud-free or cloudy atmospheres.

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