Model Spectra for Morley et al. 2017 (Observing the Atmospheres of Known Temperate Earth-sized Planets with JWST)

<p>README</p> <p>This file contains the model spectra presented in Morley et al. 2017, Observing the Atmospheres of Known Temperate Earth-sized Planets with JWST.&nbsp;</p> <p>The models are organized as follows:&nbsp;</p> <p>##########################<br> ## Transmission spectra ##<br> ##########################</p> <p>transmission_spectra contains 4 folders:<br> alb0.0_massradiusrel includes models with Bond albedo=0.0, and planet masses assuming the Weiss &amp; Marcy 2014 mass-radius relationship<br> alb0.3_massradiusrel includes models with Bond albedo=0.3, and planet masses assuming the Weiss &amp; Marcy 2014 mass-radius relationship<br> alb0.0_measured_masses includes models with Bond albedo=0.0, and observed planet masses, as described in Morley et al. 2017<br> alb0.3_measured_masses includes models with Bond albedo=0.3, and observed planet masses, as described in Morley et al. 2017</p> <p>each file contains the wavelength and model transit depth from 0.3 to 250 microns, calculated at 1 cm-1 wavenumber resolution.&nbsp;</p> <p>The file name indicates the planet name, model surface pressure (in bar), Bond albedo, and the assumed composition (Earth-, Venus-, or<br> Titan-based compositions, calculated in chemical equilibrium at each layer of the model, as described in Morley et al. 2017).&nbsp;</p> <p>(e.g. trans_spect_massradiusrel_gj1132b_psurf0.1_alb0.0_chem_earth.p.txt is a model of GJ 1132b, assuming the Weiss/Marcy mass-radius relationship, with a surface pressure of 0.1 bar, Bond albedo of 0.0, and an Earth-based composition).&nbsp;</p> <p>##########################<br> ## &nbsp; Emission spectra &nbsp; ##<br> ##########################</p> <p>emission_spectra contains 4 folders:<br> alb0.0 includes models with Bond albedo=0.0<br> alb0.3 includes models with Bond albedo=0.3<br> alb0.7 includes models with Bond albedo=0.7<br> emission_spectra_dividestar includes models that have already been divided by a model stellar spectrum, for convenience.&nbsp;</p> <p><br> each file contains the wavelength and model thermal emission flux in W/m2/m from 0.3 to 250 microns, calculated at 1 cm-1 wavenumber resolution.&nbsp;</p> <p>The file name indicates the planet name, model surface pressure (in bar), Bond albedo, and the assumed composition (Earth-, Venus-, or<br> Titan-based compositions, calculated in chemical equilibrium at each layer of the model, as described in Morley et al. 2017).&nbsp;</p> <p>(e.g. gj1132b_psurf0.01_alb0.0_chem_earth.spec is a model of GJ 1132b with a surface pressure of 0.01 bar, Bond albedo of 0.0, and an Earth-based composition).&nbsp;</p> <p>The models in emission_spectra_dividestar instead contain the flux of the planet divided by the flux of the star.&nbsp;</p> <p>&nbsp;</p> <p>##########################<br> ## &nbsp; &nbsp;Eclipse Depths &nbsp; &nbsp;##<br> ##########################</p> <p>eclipse_depths contains a file for each planet with calculated eclipse depths for each of the wide-band JWST MIRI filters (http://ircamera.as.arizona.edu/MIRI/pces.htm).&nbsp;</p> <p>(new version from Jan 29 2018 has fixed a bug in MIRI eclipse depths that affected the&nbsp;longest wavelength filter for GJ 1132b and LHS 1140b only).&nbsp;</p>