Hot Exoplanet Atmospheres Resolved with Transit Spectroscopy (HEARTS)

Seidel, J. V.; Lendl, M.; Bourrier, V.; Ehrenreich, D.; Allart, R.; Sousa, S. G.; Cegla, H. M.; Bonfils, X.; Conod, U.; Grandjean, A.; Wyttenbach, A.; Astudillo-Defru, N.; Bayliss, Daniel; Heng, Kevin; Lavie, B.; Melo, C.; Pepe, F.; Ségransan, D.; Udry, S.

doi:10.1051/0004-6361/202039058

Cited by 25 publications

(18 citation statements)

References 77 publications

(41 reference statements)

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“…In particular, as several groups of gasses are associated with clouds that condense at similar temperatures on hot Jupiters (e.g., TiO/VO, aluminum, and calcium at the highest temperatures, iron, magnesium, silicon, chromium, and manganese at moderate temperatures, and potassium and sodium at lower temperatures, see Figure 1), measuring the absolute abundances of these gases and their ratios as a function of planetary temperature and gravity could help constrain the condensation sequence in exoplanet atmospheres (Lothringer et al, 2020). However, while many species have been detected for ultra-hot Jupiters (e.g., Ben-Yami et al, 2020;Cabot et al, 2020;Fossati et al, 2010;Haswell et al, 2012;Hoeijmakers et al, 2018;Nugroho et al, 2020;Sing et al, 2019;von Essen et al, 2019;Yan et al, 2019), suggesting largely cloud-free atmospheres, efforts at lower temperatures have yielded mixed results due to controversial detections that are difficult to replicate (e.g., Chen et al, 2018;Cubillos et al, 2020;Espinoza et al, 2019;Gibson et al, 2019Gibson et al, , 2017McGruder et al, 2020;Sedaghati et al, 2017;Seidel et al, 2020;Sing et al, 2015;Vidal-Madjar et al, 2013) and aerosol opacity at optical wavelengths that reduce the amplitudes of atomic and molecular absorption features (Charbonneau et al, 2002;Heng, 2016;Pont et al, 2008;Sing et al, 2016).…”

Section: Future Observationsmentioning

confidence: 99%

Aerosols in Exoplanet Atmospheres

2021

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Section: Future Observationsmentioning

confidence: 99%

Aerosols in Exoplanet Atmospheres

2021

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“…E-mail: jseidel@eso.org † ESO Fellow ‡ UKRI Future Leaders Fellow Recently, various groups have started to characterize the tenuous atmospheres within or at the edge of the Neptune desert with detections of atmospheric sodium, hydrogen, helium, and water vapour (e.g. Armstrong et al 2020 ;Allart et al 2020 ;Crossfield et al 2020 ;Dragomir et al 2020 ;Seidel et al 2020c ;Murgas et al 2021 ;Brande et al 2022 ). In this sample of desert inhabitants, WASP-166 b remains a rare gem, a planet that has apparently retained its atmosphere which exhibits extreme bloating with a density of ρ = 0 .…”

Section: Introductionmentioning

confidence: 99%

The hot Neptune WASP-166 b with ESPRESSO II: confirmation of atmospheric sodium

Seidel

Cegla

Doyle

et al. 2022

Monthly Notices of the Royal Astronomical Society: Letters

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The hot Neptune desert, a distinct lack of highly irradiated planets in the size range of Neptune, remains one of the most intriguing results of exoplanet population studies. A deeper understanding of the atmosphere of exoplanets sitting at the edge or even within the Neptune desert will allow us to better understand if planetary formation or evolution processes are at the origin of the desert. A detection of sodium in WASP-166 b was presented previously with tentative line broadening at the 3.4 σ with the HARPS spectrograph. We update this result with two transits observed with the ESPRESSO spectrograph, confirming the detection in each night and the broadened character of the line. This result marks the first confirmed resolved sodium detection within the Neptune desert. In this work, we additionally highlight the importance of treating low-SNR spectral regions particularly where absorption lines of stellar sodium and planetary sodium overlap at mid-transit - an important caveat for future observations of the system.

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“…For WASP-127b, one of the only exoplanets with a scale height of the same order of magnitude as KELT-11 b (see Fig. 6), a curiously large sodium feature was originally found in Žák et al (2019) in HARPS data which was later attributed to stellar contamination in Seidel et al (2020c). The upper limit on a possible sodium signal provided in Seidel et al (2020c) for the HARPS HEARTS dataset is consistent with the subsequent sodium detection with ESPRESSO presented in Allart et al (2020).…”

Section: Comparison With Previous Kelt-11 B Resultsmentioning

confidence: 76%

Hot Exoplanet Atmospheres Resolved with Transit Spectroscopy (HEARTS)

Mounzer

Seidel

Attia

et al. 2022

A&A

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Context. High-resolution transmission spectroscopy has allowed for in-depth information on the composition and structure of exoplanetary atmospheres to be garnered in the last few years, especially in the visible and in the near-infrared. Many atomic and molecular species have been detected thanks to data gathered from state-of-the-art spectrographs installed on large ground-based telescopes. Nevertheless, the Earth daily cycle has been limiting observations to exoplanets with the shortest transits. Aims. The inflated sub-Saturn KELT-11 b has a hot atmosphere and orbits a bright evolved subgiant star, making it a prime choice for atmospheric characterization. The challenge lies in its transit duration -of more than seven hours -which can only be covered partially or without enough out-of-transit baselines when observed from the ground. Methods. To overcome this constraint, we observed KELT-11 b with the HARPS spectrograph in series of three consecutive nights, each focusing on a different phase of the planetary orbit: before, during, and after the transit. This allowed us to gather plenty of outof-transit baseline spectra, which was critical to build a spectrum of the unocculted star with sufficient precision. Telluric absorption lines were corrected using the atmospheric transmission code Molecfit. Individual high-resolution transmission spectra were merged to obtain a high signal-to-noise transmission spectrum to search for sodium in KELT-11 b's atmosphere through the ∼ 5900 Å doublet. Results. Our results highlight the potential for independent observations of a long-transiting planet over consecutive nights. Our study reveals a sodium excess absorption of 0.28 ± 0.05 % and 0.50 ± 0.06 % in the Na D1 and D2 lines, respectively. This corresponds to 1.44 and 1.69 times the white-light planet radius in the line cores. Wind pattern modeling tends to prefer day-to-night side winds with no vertical winds, which is surprising considering the planet bloatedness. The modeling of the Rossiter-Mclaughlin effect yields a significantly misaligned orbit, with a projected spin-orbit angle of λ = -77.86 +2.36 −2.26• . Conclusions. Belonging to the under-studied group of inflated sub-Saturns, the characteristics of KELT-11 b -notably its extreme scale height and long transit -make it an ideal and unique target for next-generation telescopes. Our results as well as recent findings from HST, TESS, and CHEOPS observations could make KELT-11 b a benchmark exoplanet in atmospheric characterization.

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Hot Exoplanet Atmospheres Resolved with Transit Spectroscopy (HEARTS)

Cited by 25 publications

References 77 publications

Aerosols in Exoplanet Atmospheres

Aerosols in Exoplanet Atmospheres

The hot Neptune WASP-166 b with ESPRESSO II: confirmation of atmospheric sodium

Hot Exoplanet Atmospheres Resolved with Transit Spectroscopy (HEARTS)

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