A library of ATMO forward model transmission spectra for hot Jupiter exoplanets
Goyal, JM; Mayne, N; Sing, DK; et al.Drummond, B; Tremblin, P; Amundsen, DS; Evans, T; Carter, AL; Spake, J; Baraffe, I; Nikolov, N; Manners, J; Chabrier, G; Hebrard, E
Date: 23 November 2017
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Oxford University Press (OUP) / Royal Astronomical Society
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Abstract
We present 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-convectivechemica ...
We present 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-convectivechemical
equilibrium model termed ATMO, with up-to-date high temperature opacities.
We present an interpretation of observations of ten exoplanets, including best fit parameters
and χ
2 maps. In agreement with previous works, we find a continuum from
clear to hazy/cloudy atmospheres for this sample of hot Jupiters. The data for all the
10 planets are consistent with sub-solar to solar C/O ratio, 0.005 to 10 times solar
metallicity and water rather than a methane dominated infrared spectra. We then
explore the range of simulated atmospheric spectra for different exoplanets, based on
characteristics such as temperature, metallicity, C/O-ratio, haziness and cloudiness.
We find a transition value for the metallicity between 10 and 50 times solar, which
leads to substantial changes in the transmission spectra. We also find a transition value
of C/O ratio, from water to carbon species dominated infrared spectra, as found by
previous works, revealing a temperature dependence of this transition point ranging
from ∼0.56 to ∼1-1.3 for equilibrium temperatures from ∼900 to ∼2600 K. We highlight
the potential of the spectral features of HCN and C2H2 to constrain the metallicities
and C/O ratios of planets, using JWST observations. Finally, our entire grid (∼460,000
simulations) is publicly available and can be used directly with the JWST simulator
PandExo for planning observations.
Physics and Astronomy
Faculty of Environment, Science and Economy
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