Abstract
Abstract Accurate estimations of atmospheric properties of exoplanets from transmission spectra require the understanding of degeneracies between model parameters and observations that can resolve them. We conduct a systematic investigation of such degeneracies using a combination of detailed atmospheric retrievals and a range of model assumptions, focusing on H2-rich atmospheres. As a case study, we consider the well-studied hot Jupiter HD 209458 b. We perform extensive retrievals with models ranging from simple isothermal and isobaric atmospheres to those with full pressure–temperature profiles, inhomogeneous cloud/haze coverage, multiple-molecular species, and data in the optical–infrared wavelengths. Our study reveals four key insights. First, we find that a combination of models with minimal assumptions and broadband transmission spectra with current facilities allows precise estimates of chemical abundances. In particular, high-precision optical and infrared spectra, along with models including variable cloud coverage and prominent opacity sources, with Na and K being important in the optical, provide joint constraints on cloud/haze properties and chemical abundances. Second, we show that the degeneracy between planetary radius and its reference pressure is well characterized and has little effect on abundance estimates, contrary to previous claims using semi-analytic models. Third, collision-induced absorption due to H2–H2 and H2–He interactions plays a critical role in correctly estimating atmospheric abundances. Finally, our results highlight the inadequacy of simplified semi-analytic models with isobaric assumptions for reliable retrievals of transmission spectra. Transmission spectra obtained with current facilities such as the Hubble Space Telescope and Very Large Telescope can provide strong constraints on atmospheric abundances of exoplanets.
Highlights
Transmission spectroscopy of transiting exoplanets offers a powerful probe to study their atmospheres
Recent observational advancements have enabled high-precision transmission spectra of exoplanets over a broad spectral range. Such observations have been obtained in low resolution from space using Hubble Space Telescope (HST) spectrographs—the Space Telescope Imaging Spectrograph (STIS) in the NUV/ Optical and the Wide Field Camera 3 (WFC3) in the nearinfrared (e.g., Deming et al 2013; Kreidberg et al 2015; Sing et al 2016)
We investigate the validity of the assumptions of the semi-analytic model above by including collision-induced absorption (CIA) absorption as an additional source of opacity
Summary
Transmission spectroscopy of transiting exoplanets offers a powerful probe to study their atmospheres. Recent observational advancements have enabled high-precision transmission spectra of exoplanets over a broad spectral range. Such observations have been obtained in low resolution from space using Hubble Space Telescope (HST) spectrographs—the Space Telescope Imaging Spectrograph (STIS) in the NUV/ Optical and the Wide Field Camera 3 (WFC3) in the nearinfrared (e.g., Deming et al 2013; Kreidberg et al 2015; Sing et al 2016). Optical spectra can provide important constraints on the possibility and properties of clouds and hazes (e.g., Brown 2001; Line & Parmentier 2016; Barstow et al 2017; MacDonald & Madhusudhan 2017a) Statistical constraints on these various properties have been reported from such data sets using rigorous atmospheric retrieval methods for various planets
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