A library of ATMO forward model transmission spectra for hot Jupiter exoplanets
| Autor: | Goyal, Jayesh M., Mayne, Nathan, Sing, David K., Drummond, Benjamin, Tremblin, Pascal, Amundsen, David S., Evans, Thomas, Carter, Aarynn L., Spake, Jessica, Baraffe, Isabelle, Nikolov, Nikolay, Manners, James, Chabrier, Gilles, Hebrard, Eric |
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| Rok vydání: | 2017 |
| Předmět: | |
| Zdroj: | Monthly Notices of the Royal Astronomical Society, Volume 474, Issue 4, March 2018, Pages 5158-5185 |
| Druh dokumentu: | Working Paper |
| DOI: | 10.1093/mnras/stx3015 |
| Popis: | 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-convective-chemical 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 $\chi^{2}$ 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 $\sim$0.56 to $\sim$1-1.3 for equilibrium temperatures from $\sim$900 to $\sim$2600 K. We highlight the potential of the spectral features of HCN and C$_2$H$_2$ to constrain the metallicities and C/O ratios of planets, using JWST observations. Finally, our entire grid ($\sim$460,000 simulations) is publicly available and can be used directly with the JWST simulator PandExo for planning observations. Comment: No changes in replacement, main paper now made visible on arXiv as earlier the published Erratum associated with the paper was instead visible. 34 pages, 28 figures. Accepted for Publication in MNRAS. Full grid of model transmission spectra and chemical abundances are available here, https://drive.google.com/drive/folders/1tvlgSWyEAA0cX_yxnA5URD4Zo3Zj4GcH |
| Databáze: | arXiv |
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