dc.contributor.author | Goyal, JM | |
dc.contributor.author | Mayne, N | |
dc.contributor.author | Sing, DK | |
dc.contributor.author | Drummond, B | |
dc.contributor.author | Tremblin, P | |
dc.contributor.author | Amundsen, DS | |
dc.contributor.author | Evans, T | |
dc.contributor.author | Carter, AL | |
dc.contributor.author | Spake, J | |
dc.contributor.author | Baraffe, I | |
dc.contributor.author | Nikolov, N | |
dc.contributor.author | Manners, J | |
dc.contributor.author | Chabrier, G | |
dc.contributor.author | Hebrard, E | |
dc.date.accessioned | 2017-11-16T10:19:38Z | |
dc.date.issued | 2017-11-23 | |
dc.description.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-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. | en_GB |
dc.description.sponsorship | J.M.G and N.M are part funded by a Leverhulme
Trust Research Project Grant, and in part by a University
of Exeter College of Engineering, Mathematics and Physical
Sciences PhD studentship. D.K.S, T.E, N.N acknowledges
support from the European Research Council under the European
Unions Seventh Framework Programme (FP7/2007-
2013)/ ERC grant agreement number 336792. B.D. thanks
the University of Exeter for support through a Ph.D. studentship.
D.S.A. acknowledges support from the NASA Astrobiology
Program through the Nexus for Exoplanet System
Science.This work used the DiRAC Complexity system,
operated by the University of Leicester IT Services, which
forms part of the STFC DiRAC HPC Facility. This work also
used the University of Exeter Supercomputer, a DiRAC Facility
jointly funded by STFC, the Large Facilities Capital
Fund of BIS and the University of Exeter. | en_GB |
dc.identifier.citation | Vol. 474 (4), pp. 5158–5185 | en_GB |
dc.identifier.doi | 10.1093/mnras/stx3015 | |
dc.identifier.uri | http://hdl.handle.net/10871/30324 | |
dc.language.iso | en | en_GB |
dc.publisher | Oxford University Press (OUP) / Royal Astronomical Society | en_GB |
dc.relation.url | http://hdl.handle.net/10871/37453 | |
dc.rights | © 2017 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society | en_GB |
dc.subject | planets and satellites: atmospheres | en_GB |
dc.subject | planets and satellites: composition | en_GB |
dc.subject | planets and satellites: gaseous planets | en_GB |
dc.subject | techniques: spectroscopic | en_GB |
dc.title | A library of ATMO forward model transmission spectra for hot Jupiter exoplanets | en_GB |
dc.type | Article | en_GB |
dc.description | This is the final version. Available from OUP via the DOI in this record. | en_GB |
dc.description | The erratum to this article is in ORE at http://hdl.handle.net/10871/37453 | |