ARES.*
                V. No Evidence For Molecular Absorption in the HST WFC3 Spectrum of GJ 1132 b

Mugnai, Lorenzo V.; Modirrousta-Galian, Darius; Edwards, Billy; Changeat, Quentin; Bouwman, J.; Morello, Giuseppe; Al-Refaie, Ahmed; Baeyens, Robin; Bieger, Michelle Fabienne; Blain, Doriann; Gressier, Amélie; Guilluy, Gloria; Jaziri, Yassin; Kiefer, F.; Morvan, Mario; Pluriel, William; Poveda, Mathilde; Skaf, Nour; Whiteford, Niall; Wright, Sam; Yip, Kai Hou; Zingalès, Tiziano; Charnay, Benjamin; Drossart, P.; Leconte, Jérémy; Venot, Olivia; Waldmann, Ingo; Beaulieu, Jean-Philippe

doi:10.3847/1538-3881/abf3c3

Cited by 60 publications

(53 citation statements)

References 107 publications

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“…Swain et al (2021) analysis produced a sloped spectral feature around 1.3 µm, and a larger negative A H ≈ −0.9. The analysis of Mugnai et al (2021) and Libby-Roberts et al (2021) found instead a visibly flat spectra, and with A H close to zero. Since the last two groups return similar results, we choose to calculate A H using reduced data from Mugnai et al (2021), which is also close to the A H calculated from Libby-Roberts et al (2021).…”

Section: Transmission Data Reductionmentioning

confidence: 91%

“…The analysis of Mugnai et al (2021) and Libby-Roberts et al (2021) found instead a visibly flat spectra, and with A H close to zero. Since the last two groups return similar results, we choose to calculate A H using reduced data from Mugnai et al (2021), which is also close to the A H calculated from Libby-Roberts et al (2021). A trend study using uniform data reduction methods would be preferred, allowing for more rigorous comparison between exoplanets intrinsic properties (e.g., Sing et al 2016;Tsiaras et al 2018;Roudier et al 2021).…”

Section: Transmission Data Reductionmentioning

confidence: 91%

“…In particular, water absorption features were discovered in the transmission spectra taken from the Wide Field Camera Three (WFC3) of the Hubble Space Telescope (HST ) for several sub-Neptunes (e.g, Fraine et al 2014;Wakeford et al 2017;Kreidberg et al 2018;Benneke et al 2019a;Tsiaras et al 2019;Benneke et al 2019b;Kreidberg et al 2020;Guo et al 2020;Edwards et al 2021;Mikal-Evans et al 2021). Meanwhile, many transmission spectra were found to be flat and featureless (e.g, Kreidberg et al 2014;Knutson et al 2014a,b;Libby-Roberts et al 2020;Chachan et al 2020;Mugnai et al 2021). Most notably, GJ 1214 b, with 15 transits, was observed to have an almost completely flat spectrum over the WFC3 range of ∼1.…”

Section: Introductionmentioning

confidence: 99%

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Cleaning our Hazy Lens: Exploring Trends in Transmission Spectra of Warm Exoplanets

Dymont,

Yu,

Ohno

et al. 2021

Preprint

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Relatively little is understood about the atmospheric composition of temperate to warm exoplanets (equilibrium temperature T eq < 1000 K), as many of them are found to have uncharacteristically flat transmission spectra. Their flattened spectra are likely due to atmospheric opacity sources such as planet-wide photochemical hazes and condensation clouds. We compile the transmission spectra of 23 warm exoplanets previously observed by the Hubble Space Telescope and quantify the haziness of each exoplanet using a normalized amplitude of the water absorption feature (A H ). By examining the relationships between A H and various planetary and stellar forcing parameters, we endeavor to find correlations of haziness associated with planetary properties. Our analysis shows that the previously identified linear trends between A H and T eq or hydrogen-helium envelope mass fraction (f HHe ) break down with the addition of new exoplanet data. Among all the parameters we investigated, atmospheric scale height (H), planet gravity (g p ), and planet density (ρ p ) hold the most statistically significant linear or linear logrithmic correlations with A H (p ≤ 0.02). We also tentatively identified positive correlations for eccentricity (e) and stellar age (t age ) with A H . Specifically, lower H, higher g p , ρ p , e, or t age lead to clearer atmospheres. However, none of the parameters show very strong linear correlations with A H , suggesting that haziness in warm exoplanets is not simply controlled by any single planetary/stellar parameter. Additional observations and laboratory experiments are needed to fully understand the complex physical and chemical processes that lead to the hazy/cloudy atmospheres in warm exoplanets.

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Section: Transmission Data Reductionmentioning

confidence: 91%

Section: Transmission Data Reductionmentioning

confidence: 91%

Section: Introductionmentioning

confidence: 99%

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Cleaning our Hazy Lens: Exploring Trends in Transmission Spectra of Warm Exoplanets

Dymont,

Yu,

Ohno

et al. 2021

Preprint

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“…Recent observations have probed the atmospheres of several rocky exoplanets. For example, transmission spectroscopy of GJ 1132 b has suggested an atmosphere with a high-mean-molecular-weight (high-𝜇) and/or high-altitude clouds (Southworth et al 2017;Diamond-Lowe et al 2018;Mugnai et al 2021). Similarly, transmission spectra of Trappist-1 d, e and f have ruled out clear, H 2 -rich atmospheres for these planets (de Wit et al 2018;Moran et al 2018).…”

Section: Introductionmentioning

confidence: 99%

“…Similarly, transmission spectra of Trappist-1 d, e and f have ruled out clear, H 2 -rich atmospheres for these planets (de Wit et al 2018;Moran et al 2018). Furthermore, searches for molecular species such as HCN have now become possible in the atmospheres of rocky exoplanets such as 55 Cnc e and GJ 1132 b (Tsiaras et al 2016;Swain et al 2021;Mugnai et al 2021) and could provide insights into their possible interior and atmospheric conditions (e.g. Madhusudhan et al 2012).…”

Section: Introductionmentioning

confidence: 99%

HyDRo: Atmospheric Retrieval of Rocky Exoplanets in Thermal Emission

Piette,

Madhusudhan,

Mandell

2021

Preprint

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Emission spectroscopy is a promising technique to observe atmospheres of rocky exoplanets, probing both their chemistry and thermal profiles. We present y o, an atmospheric retrieval framework for thermal emission spectra of rocky exoplanets.y o does not make prior assumptions about the background atmospheric composition, and can therefore be used to interpret spectra of secondary atmospheres with unknown compositions. We use y o to assess the chemical constraints which can be placed on rocky exoplanet atmospheres using JWST. Firstly, we identify the best currently-known rocky exoplanet candidates for spectroscopic observations in thermal emission with JWST, finding > 30 known rocky exoplanets whose thermal emission will be detectable by JWST/MIRI in fewer than 10 eclipses at 𝑅 ∼ 10. We then consider the observations required to characterise the atmospheres of three promising rocky exoplanets across the ∼400-800 K equilibrium temperature range: Trappist-1 b, GJ 1132 b, and LHS 3844 b. Considering a range of CO 2 -to H 2 O-rich atmospheric compositions, we find that as few as 8 eclipses of LHS 3844 b or GJ 1132 b with MIRI will be able to place important constraints on the chemical compositions of their atmospheres. This includes confident detections of CO 2 and H 2 O in the case of a cloud-free CO 2 -rich composition, besides ruling out a bare rock scenario. Similarly, 30 eclipses of Trappist-1 b with MIRI/LRS can allow detections of a cloud-free CO 2 -rich or CO 2 -H 2 O atmosphere. y o will allow important atmospheric constraints for rocky exoplanets using JWST observations, providing clues about their geochemical environments.

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Disentangling atmospheric compositions of K2-18 b with next generation facilities

et al. 2021

Self Cite

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Recent analysis of the planet K2-18 b has shown the presence of water vapour in its atmosphere. While the H2O detection is significant, the Hubble Space Telescope (HST) WFC3 spectrum suggests three possible solutions of very different nature which can equally match the data. The three solutions are a primary cloudy atmosphere with traces of water vapour (cloudy sub-Neptune), a secondary atmosphere with a substantial amount (up to 50% Volume Mixing Ratio) of H2O (icy/water world) and/or an undetectable gas such as N2 (super-Earth). Additionally, the atmospheric pressure and the possible presence of a liquid/solid surface cannot be investigated with currently available observations. In this paper we used the best fit parameters from Tsiaras et al. (Nat. Astron. 3, 1086, 2019) to build James Webb Space Telescope (JWST) and Ariel simulations of the three scenarios. We have investigated 18 retrieval cases, which encompass the three scenarios and different observational strategies with the two observatories. Retrieval results show that twenty combined transits should be enough for the Ariel mission to disentangle the three scenarios, while JWST would require only two transits if combining NIRISS and NIRSpec data. This makes K2-18 b an ideal target for atmospheric follow-ups by both facilities and highlights the capabilities of the next generation of space-based infrared observatories to provide a complete picture of low mass planets.

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ARES.* V. No Evidence For Molecular Absorption in the HST WFC3 Spectrum of GJ 1132 b

Cited by 60 publications

References 107 publications

Cleaning our Hazy Lens: Exploring Trends in Transmission Spectra of Warm Exoplanets

Cleaning our Hazy Lens: Exploring Trends in Transmission Spectra of Warm Exoplanets

HyDRo: Atmospheric Retrieval of Rocky Exoplanets in Thermal Emission

Disentangling atmospheric compositions of K2-18 b with next generation facilities

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