Hot Exoplanet Atmospheres Resolved with Transit Spectroscopy (HEARTS) IV. A spectral inventory of atoms and molecules in the high-resolution transmission spectrum of WASP-121 b

Hoeijmakers, H. J.; Seidel, J. V.; Pino, L.; Kitzmann, D.; Sindel, J. P.; Ehrenreich, D.; Oza, A. V.; Bourrier, V.; Allart, R.; Gebek, A.; Lovis, C.; Yurchenko, S. N.; Astudillo-Defru, N.; Bayliss, D.; Cegla, H.; Lavie, B.; Lendl, M.; Melo, C.; Murgas, F.; Nascimbeni, V.; Pepe, F.; Ségransan, D.; Udry, S.; Wyttenbach, A.; Heng, Kevin

doi:10.48550/arxiv.2006.11308

Cited by 8 publications

(26 citation statements)

References 71 publications

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“…We confirm the detection of Cr by Ben-Yami et al (2020), Hoeĳmakers et al (2020b and Borsa et al (2021), recovering the signal at 5.0 𝜎 at a position consistent with these works (𝐾 p = 198 + 76 km s −1 , 𝑣 sys = −5.5 ± 4.6 km s −1 ) and fulfilling all five of our detection criteria. As can be seen in Fig 1, the signals are found in slightly different velocity locations in the blue and red arms.…”

Section: Cr and Vsupporting

confidence: 91%

“…We also confirm the detections of V (Ben-Yami et al 2020;Hoeĳmakers et al 2020b;Borsa et al 2021), recovering the signal at 4.4 𝜎 within range of the expected location (𝐾 p = 226 ± 44.2 km s −1 , 𝑣 sys = −5.5 ± 7.0 km s −1 ) and fulfilling all five of our detection criteria.…”

Section: Cr and Vsupporting

confidence: 84%

“…3). The negative 𝑣 sys offset is also consistent with those observed by Hoeĳmakers et al (2020b), Ben-Yami et al (2020, Bourrier et al (2020a) and Cabot et al (2020) and is thus thought to be reliable. We thus judge any signal that lies within 3 km s −1 in 𝑣 sys and 20 km s −1 of 𝐾 p of the Fe signal presented in Gibson et al (2020) to lie at the 'expected' position.…”

Section: Detection Criteriasupporting

confidence: 84%

“…As expected from previous work, we detect the Fe signal strongly at 8.8𝜎, within range of the expected location (𝐾 p = 200 ± 41.1 km s −1 , 𝑣 sys = −7.3 ± 5.8 km s −1 ), in the combined blue + red map. This independent confirmation of our previous detection using both arms of the data fulfils all five of our detection criteria and serves as a benchmark test for our analysis, as the detection was previously well-characterised by Gibson et al (2020) using the blue arm of this dataset and confirmed by Cabot et al (2020), Bourrier et al (2020a), Ben-Yami et al (2020 and Hoeĳmakers et al (2020b) in the HARPS dataset. Our detection is consistent with these works.…”

Section: Fesupporting

confidence: 82%

“…(v) Whether the species has been detected before, whether in other analyses of WASP-121b (e.g. Hoeĳmakers et al 2020b;Cabot et al 2020;Ben-Yami et al 2020), or in other ultra-hot Jupiters such as KELT-9b (Hoeĳmakers et al 2018(Hoeĳmakers et al , 2019 or KELT-20b (e.g. Casasayas-Barris et al 2019;Nugroho et al 2020a).…”

Section: Detection Criteriamentioning

confidence: 99%

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Non-detection of TiO and VO in the atmosphere of WASP-121b using high-resolution spectroscopy

Merritt

Gibson

Nugroho

et al. 2020

A&A

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Thermal inversions have long been predicted to exist in the atmospheres of ultra-hot Jupiters. However, detection of two species thought to be responsible -TiO and VO -remain elusive. We present a search for TiO and VO in the atmosphere of the ultra-hot Jupiter WASP-121b (T eq 2400 K), an exoplanet already known to show water features in its dayside spectrum characteristic of a temperature inversion as well as tentative evidence for VO at low-resolution. We observed its transmission spectrum with UVES/VLT and used the cross-correlation method -a powerful tool for the unambiguous identification of the presence of atomic and molecular species -in an effort to detect whether TiO or VO were responsible for the observed temperature inversion. No evidence for the presence of TiO or VO was found at the terminator of WASP-121b. By injecting signals into our data at varying abundance levels, we set rough detection limits of [VO] −7.9 and [TiO] −9.3. However, these detection limits are largely degenerate with scattering properties and the position of the cloud deck. Our results may suggest that neither TiO or VO are the main drivers of the thermal inversion in WASP-121b, but until a more accurate line list is developed for VO, we cannot conclusively rule out its presence. Future work will search for finding other strong optically-absorbing species that may be responsible for the excess absorption in the redoptical.

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Section: Cr and Vsupporting

confidence: 91%

Section: Cr and Vsupporting

confidence: 84%

Section: Detection Criteriasupporting

confidence: 84%

Section: Fesupporting

confidence: 82%

Section: Detection Criteriamentioning

confidence: 99%

See 3 more Smart Citations

Non-detection of TiO and VO in the atmosphere of WASP-121b using high-resolution spectroscopy

Merritt

Gibson

Nugroho

et al. 2020

A&A

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Tracing bulk elemental ratios in exoplanetary atmospheres with TiO chemistry

Ramírez

Cridland

Mollière

2020

A&A

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Deciphering the bulk elemental abundances of exoplanetary atmospheres is not an easy task, yet it is crucial to understanding the formation history of planets. The purpose of this work is to show that the observability of TiO features at optical wavelengths in the transmission spectra of hot Jupiter atmospheres is sensitive to the bulk chemical properties of the atmosphere. To this end, we ran a grid of chemical models, which include TiO formation and destruction, for the ultra-hot Jupiter WASP-19b and an ultra-hot version of HD 209458b. We take into account non-equilibrium chemistry and changes in the temperature and pressure structure of these atmospheres caused by different C/O ratios. We calculated synthetic transmission spectra for these models, and studied the relative strengths of TiO and H2O features quantitatively. To compare with observations, we used a model-independent metric for molecular abundances, ΔZTiO−H2O/Heq, which has previously been used in observational studies of exoplanetary atmospheres. We find that with this metric we can differentiate between different chemical models and place constraints on the bulk carbon and oxygen abundances of the atmosphere. From chemical considerations, we expected the TiO abundance to depend on the bulk nitrogen. However, we find that changes in N/H do not result in changes in the resulting TiO. We applied our method to a set of known exoplanets that have been observed in the relevant optical wavelengths and find good agreement between low-resolution observations and our model for WASP-121b, marginally good agreement with WASP-79b, WASP-76b, and WASP-19b, and poorer agreement with HD 209458b. Our method will be particularly helpful for indirect studies of the bulk abundances of carbon and oxygen.

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A temperature inversion with atomic iron in the ultra-hot dayside atmosphere of WASP-189b

Yan

Πάλλη

Reiners

et al. 2020

A&A

117

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Temperature inversion layers are predicted to be present in ultra-hot giant planet atmospheres. Although such inversion layers have recently been observed in several ultra-hot Jupiters, the chemical species responsible for creating the inversion remain unidentified. Here, we present observations of the thermal emission spectrum of an ultra-hot Jupiter, WASP-189b, at high spectral resolution using the HARPS-N spectrograph. Using the cross-correlation technique, we detect a strong Fe I signal. The detected Fe I spectral lines are found in emission, which is direct evidence of a temperature inversion in the planetary atmosphere. We further performed a retrieval on the observed spectrum using a forward model with an MCMC approach. When assuming a solar metallicity, the best-fit result returns a temperature of 4320−100+120 K at the top of the inversion, which is significantly hotter than the planetary equilibrium temperature (2641 K). The temperature at the bottom of the inversion is determined as 2200−800+1000 K. Such a strong temperature inversion is probably created by the absorption of atomic species like Fe I.

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Hot Exoplanet Atmospheres Resolved with Transit Spectroscopy (HEARTS) IV. A spectral inventory of atoms and molecules in the high-resolution transmission spectrum of WASP-121 b

Cited by 8 publications

References 71 publications

Non-detection of TiO and VO in the atmosphere of WASP-121b using high-resolution spectroscopy

Non-detection of TiO and VO in the atmosphere of WASP-121b using high-resolution spectroscopy

Tracing bulk elemental ratios in exoplanetary atmospheres with TiO chemistry

A temperature inversion with atomic iron in the ultra-hot dayside atmosphere of WASP-189b

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