The GAPS Programme at TNG

Borsa, F.; Giacobbe, P.; Bonomo, A. S.; Brogi, Matteo; Pino, L.; Fossati, L.; Lanza, A. F.; Nascimbeni, V.; Sozzetti, A.; Amadori, Francesco; Benatti, S.; Biazzo, K.; Bignamini, A.; Boschin, W.; Claudi, R.; Cosentino, R.; Covino, E.; Desidera, S.; Fiorenzano, A. F. Martínez; Guilluy, Gloria; Harutyunyan, A.; Maggio, A.; Maldonado, J.; Mancini, L.; Micela, G.; Molinari, E.; Molinaro, M.; Pagano, I.; Pedani, M.; Piotto, G.; Poretti, E.; Rainer, M.; Scandariato, G.; Stoev, H.

doi:10.1051/0004-6361/202142768

Cited by 14 publications

(30 citation statements)

References 51 publications

(49 reference statements)

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“…Our results show that HRS emission spectroscopy observations of hot gas giants have the potential to reveal much more information when treated as a phase curve rather than a single phase-collapsed emission spectrum, which is the approach that has most often been taken in the literature so far (e.g. Pino et al 2020;Yan et al 2020;Nugroho et al 2020;Borsa et al 2022). Conceptually, an HRS phase curve is similar to a classic lowresolution (LRS) phase curve observed from space (e.g.…”

Section: Hrs Phase Curves As a New Tool For Exoplanet Atmosphere Char...mentioning

confidence: 52%

“…In other words, the westward offset in the peak scaling factor of iron lines found by Herman et al (2022), and confirmed with CO by van Sluijs et al ( 2022) can be interpreted as indirect evidence for an eastward hot-spot offset. Furthermore, based on HARPS-N emission spectroscopy, Borsa et al (2022) report evidence of asymmetry in thermal structure between pre-and post-eclipse spectra of UHJ KELT-20b, albeit not statistically significant. These authors also find that Fe ii and Cr i are only observable post-eclipse, and not pre-eclipse, despite achieving a similar total S/N across both phase ranges.…”

Section: Kelt-9b In the Context Of Ultra-hot Jupitersmentioning

confidence: 83%

“…Indeed, Herman et al (2022) and van Sluijs et al (2022) present the first parameterized studies of phase-dependent Fe i and CO line strengths targeting a UHJ, WASP-33b, for which Cont et al (2021) had already suggested that 3D effects are required to explain the phase-stacked optical HRS emission spectrum of TiO and Fe i. In addition, Borsa et al (2022) found evidence for a different chemistry and thermal profile in pre-and post-eclipse phases of the UHJ In the present paper, we further extend these previous studies to include, for the first time, a simultaneous parameterized analysis of phase-dependent line intensity and Doppler shift of the hottest UHJ: KELT-9b (T eq = 3900 K; Borsa et al 2019).…”

Section: Introductionmentioning

confidence: 96%

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The GAPS Programme at TNG

Pino

Brogi

Désert

et al. 2022

A&A

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Aims. We present a novel method for studying the thermal emission of exoplanets as a function of orbital phase at very high spectral resolution, and use it to investigate the climate of the ultra-hot Jupiter KELT-9b. Methods. We combine three nights of HARPS-N and two nights of CARMENES optical spectra, covering orbital phases between quadratures (0.25 < ϕ < 0.75), when the planet shows its day-side hemisphere with different geometries. We co-add the signal of thousands of Fe i lines through cross-correlation, which we map to a likelihood function. We investigate the phase-dependence of two separate observable quantities, namely (i) the line depths of Fe i and (ii) their Doppler shifts, introducing a new method that exploits the very high spectral resolution of our observations. Results. We confirm a previous detection of Fe i emission, and demonstrate a precision of 0.5 km s −1 on the orbital properties of KELT-9b when combining all nights of observations. By studying the phase-resolved Doppler shift of Fe i lines, we detect an anomaly in the planet's orbital radial velocity well-fitted with a slightly eccentric orbital solution (e = 0.016 ± 0.003, ω = 150 +13 • −11 , 5σ preference). However, we argue that this anomaly is caused by atmospheric circulation patterns, and can be explained if neutral iron gas is advected by day-to-night atmospheric wind flows of the order of a few km s −1 . We additionally show that the Fe i emission line depths are symmetric around the substellar point within 10 • (2σ), possibly indicating the lack of a large hot-spot offset at the altitude probed by neutral iron emission lines. Finally, we do not obtain a significant preference for models with a strong phase-dependence of the Fe i emission line strength. We show that these results are qualitatively compatible with predictions from general circulation models (GCMs) for ultra-hot Jupiter planets. Conclusions. Very high-resolution spectroscopy phase curves are of sufficient sensitivity to reveal a phase dependence in both the line depths and their Doppler shifts throughout the orbit. They constitute an under-exploited treasure trove of information that is highly complementary to space-based phase curves obtained with HST and JWST, and open a new window onto the still poorly understood climate and atmospheric structure of the hottest planets known to date.

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Section: Hrs Phase Curves As a New Tool For Exoplanet Atmosphere Char...mentioning

confidence: 52%

Section: Kelt-9b In the Context Of Ultra-hot Jupitersmentioning

confidence: 83%

Section: Introductionmentioning

confidence: 96%

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The GAPS Programme at TNG

Pino

Brogi

Désert

et al. 2022

A&A

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“…We used the retrieval method developed by Yan et al (2020) to constrain the properties of WASP-33b's atmosphere. This method has already been successfully used to determine the thermal structure in the atmosphere of two other UHJs, WASP-189b and KELT-20b/MASCARA-2b (Yan et al 2020(Yan et al , 2022bBorsa et al 2022). In our implementation, we further developed this method for use with data from multiple instruments with different wavelength coverage.…”

Section: Retrieval Of the Atmospheric Propertiesmentioning

confidence: 99%

“…The atmospheric composition of UHJs has been extensively studied in recent years. For instance, neutral or ionic species of H, Li, O, Na, Mg, Si, K, Ca, Sc, Ti, V, Cr, Mn, Fe, Sr, and Y have been identified in the atmospheres of several UHJs, including KELT-9b (Yan & Henning 2018;Hoeijmakers et al 2018Hoeijmakers et al , 2019Wyttenbach et al 2020;Borsa et al 2021a), WASP-33b (Yan et al 2019(Yan et al , 2021Nugroho et al 2020a;Borsa et al 2021b;Cont et al 2021Cont et al , 2022Herman et al 2022), WASP-189b (Yan et al 2020;Stangret et al 2022;Prinoth et al 2022), WASP-76b (Seidel et al 2019;Ehrenreich et al 2020;Tabernero et al 2021;Deibert et al 2021;Casasayas-Barris et al 2021;Kesseli et al 2022), and KELT-20b/MASCARA-2b (Casasayas-Barris et al 2018, 2019Stangret et al 2020;Nugroho et al 2020b;Hoeijmakers et al 2020a;Rainer et al 2021;Yan et al 2022b;Borsa et al 2022). Also, the spectral signatures of an increasing number of molecular species such as CO, HCN, H 2 O, OH, SiO, or TiO have been identified in UHJ atmospheres (e.g., Nugroho et al 2021;Cont et al 2021;Landman et al 2021;Fu et al 2022;Prinoth et al 2022;Sánchez-López et al 2022;Yan et al 2022a;van Sluijs et al 2022;Lothri...…”

Section: Introductionmentioning

confidence: 99%

Atmospheric characterization of the ultra-hot Jupiter WASP-33b

Cont¹,

Yan²,

Reiners³

et al. 2022

A&A

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Ultra-hot Jupiters are highly irradiated gas giant exoplanets on close-in orbits around their host stars. The dayside atmospheres of these objects strongly emit thermal radiation due to their elevated temperatures, making them prime targets for characterization by emission spectroscopy. We analyzed high-resolution spectra from CARMENES, HARPS-N, and ESPaDOnS taken over eight observation nights to study the emission spectrum of WASP-33b and draw conclusions about its atmosphere. By applying the crosscorrelation technique, we detected the spectral signatures of Ti i, V i, and a tentative signal of Ti ii for the first time via emission spectroscopy. These detections are an important finding because of the fundamental role of Ti-and V-bearing species in the planetary energy balance. Moreover, we assessed and confirm the presence of OH, Fe i, and Si i from previous studies. The spectral lines are all detected in emission, which unambiguously proves the presence of an inverted temperature profile in the planetary atmosphere. By performing retrievals on the emission lines of all the detected species, we determined a relatively weak atmospheric thermal inversion extending from approximately 3400 K to 4000 K. We infer a supersolar metallicity close to 1.5 dex in the planetary atmosphere, and find that its emission signature undergoes significant line broadening with a Gaussian FWHM of about 4.5 km s −1 . Also, we find that the atmospheric temperature profile retrieved at orbital phases far from the secondary eclipse is about 300 K to 700 K cooler than that measured close to the secondary eclipse, which is consistent with different day-and nightside temperatures. Moreover, retrievals performed on the emission lines of the individual chemical species lead to consistent results, which gives additional confidence to our retrieval method. Increasing the number of species included in the retrieval and expanding the set of retrieved atmospheric parameters will further advance our understanding of exoplanet atmospheres.

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The GAPS Programme at TNG

Guilluy

Giacobbe

Carleo

et al. 2022

A&A

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Context. The field of exo-atmospheric characterisation is progressing at an extraordinary pace. Atmospheric observations are now available for tens of exoplanets, mainly hot and warm inflated gas giants, and new molecular species continue to be detected, revealing a richer atmospheric composition than previously expected. Thanks to its warm equilibrium temperature (963±18 K) and low density (0.219±0.031 g cm −3 ), the close-in gas giant WASP-69b represents a golden target for atmospheric characterisation. Aims. With the aim of searching for molecules in the atmosphere of WASP-69b and investigating its properties, we performed high-resolution transmission spectroscopy with the GIANO-B near-infrared spectrograph at the Telescopio Nazionale Galileo. Methods. We observed three transit events of WASP-69b. During a transit, the planetary lines are Doppler-shifted due to the large change in the planet's radial velocity, allowing us to separate the planetary signal from the quasi-stationary telluric and stellar spectrum. Results. Considering the three nights together, we report the detection of CH 4 , NH 3 , CO, C 2 H 2 , and H 2 O, at more than a 3.3σ level. We did not identify the presence of HCN or CO 2 with confidence a level higher than 3σ. This is the first time that five molecules have been simultaneously detected in the atmosphere of a warm giant planet. These results suggest that the atmosphere of WASP-69b is possibly carbon-rich and characterised by the presence of disequilibrium chemistry.

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The GAPS Programme at TNG

Cited by 14 publications

References 51 publications

The GAPS Programme at TNG

The GAPS Programme at TNG

Atmospheric characterization of the ultra-hot Jupiter WASP-33b

The GAPS Programme at TNG

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