YunMa: Enabling Spectral Retrievals of Exoplanetary Clouds

Ma, Sushuang; Ito, Yuichi; Al-Refaie, Ahmed Faris; Changeat, Quentin; Edwards, Billy; Tinetti, Giovanna

doi:10.3847/1538-4357/acf8ca

Cited by 3 publications

(1 citation statement)

References 104 publications

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“…Additionally, since the model is built using the TAUREX 3.1 framework, EXPLOR is automatically compatible with all the TAUREX 3 plugins. EXPLOR can therefore use GPUaccelerated emission and transmission (Al-Refaie et al 2022a), chemical codes (ACE, GGCHEM, FASTCHEM, and FRECKLL; Agúndez et al 2012;Stock et al 2018;Woitke et al 2018;Al-Refaie et al 2022b), cloud models (YUNMA; Ma et al 2023), stellar activity models (ASTERA; Thompson et al 2024), and optimizers (MULTINEST AND ULTRANEST; Feroz et al 2009;Buchner 2021). EXPLOR uses an implementation of the 1.5D phase-curve model to calculate the spectroscopic thermal emission of the planet and its atmosphere along t, denoted F PC (λ, t), and the spectroscopic contribution to the planetary radius in transit, denoted Δ T (λ).…”

Section: Modelmentioning

confidence: 99%

Toward Atmospheric Retrievals of Panchromatic Light Curves: ExPLOR-ing Generalized Inversion Techniques for Transiting Exoplanets with JWST and Ariel

Changeat,

Ito,

Al-Refaie

et al. 2024

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Conventional atmospheric retrieval codes are designed to extract information, such as chemical abundances, thermal structures, and cloud properties, from fully “reduced” spectra obtained during transit or eclipse. Reduced spectra, however, are assembled by fitting a series of simplified light curves to time-series observations, wavelength by wavelength. Thus, spectra are postprocessed summary statistics of the original data, which by definition do not encode all the available information (i.e., astrophysical signal, model covariance, and instrumental noise). Here, we explore an alternative inversion strategy where the atmospheric retrieval is performed on the light curve directly, i.e., closer to the data. This method is implemented in EXoplanet Panchromatic Light curve Observation and Retrieval (ExPLOR), a novel atmospheric retrieval code inheriting from the TauREx project. By explicitly considering time in the model, ExPLOR naturally handles transits, eclipses, phase curves, and other complex geometries for transiting exoplanets. In this paper, we have validated this new technique by inverting simulated panchromatic light curves. The model was tested on realistic simulations of a WASP-43 b-like exoplanet as observed with the James Webb Space Telescope (JWST) and Ariel telescope. By comparing our panchromatic light-curve approach against conventional spectral retrievals on mock scenarios, we have identified key breaking points in information and noise propagation when employing past literature techniques. Throughout the paper, we discuss the importance of developing “closer-to-data” approaches such as the method presented in this work, and highlight the inevitable increase in model complexity and computing requirements associated with the recent JWST revolution.

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Section: Modelmentioning

confidence: 99%

Toward Atmospheric Retrievals of Panchromatic Light Curves: ExPLOR-ing Generalized Inversion Techniques for Transiting Exoplanets with JWST and Ariel

Changeat,

Ito,

Al-Refaie

et al. 2024

Self Cite

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The 2024 release of the ExoMol database: Molecular line lists for exoplanet and other hot atmospheres

Tennyson,

Yurchenko,

Zhang

et al. 2024

Journal of Quantitative Spectroscopy and Radiative Transfer

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The dark days are overcast: iron-bearing clouds on HD 209458 b and WASP-43 b can explain low-dayside albedos

Chubb,

Samra,

Helling

et al. 2024

Monthly Notices of the Royal Astronomical Society

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We simulate the geometric albedo spectra of hot Jupiter exoplanets HD 209458 b and WASP-43 b, based on global climate model (GCMs) post-processed with kinetic cloud models. We predict WASP-43 b to be cloudy throughout its dayside, while HD 209458 b has a clear upper atmosphere around the hot sub-solar point, largely due to the inclusion of strong optical absorbers TiO and VO in the GCM for the latter causes a temperature inversion. In both cases our models find low geometric albedos - 0.026 for WASP-43b and 0.028 for HD 209458 b when averaged over the CHEOPS bandpass of ∼0.35 - 1.1 μm - indicating dark daysides, similar to the low albedos measured by observations. We demonstrate the strong impact of clouds that contain Fe-bearing species on the modelled geometric albedos; without Fe-bearing species forming in the clouds, the albedos of both planets would be much higher (0.518 for WASP-43 b, 1.37 for HD 209458 b). We conclude that a cloudy upper or mid-to-lower atmosphere that contains strongly absorbing Fe-bearing aerosol species, is an alternative to a cloud-free atmosphere in explaining the low dayside albedos of hot Jupiter atmospheres such as HD 209458 b and WASP-43 b.

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YunMa: Enabling Spectral Retrievals of Exoplanetary Clouds

Cited by 3 publications

References 104 publications

Toward Atmospheric Retrievals of Panchromatic Light Curves: ExPLOR-ing Generalized Inversion Techniques for Transiting Exoplanets with JWST and Ariel

Toward Atmospheric Retrievals of Panchromatic Light Curves: ExPLOR-ing Generalized Inversion Techniques for Transiting Exoplanets with JWST and Ariel

The 2024 release of the ExoMol database: Molecular line lists for exoplanet and other hot atmospheres

The dark days are overcast: iron-bearing clouds on HD 209458 b and WASP-43 b can explain low-dayside albedos

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