The GAPS Programme at TNG LVI. Characterisation of the low-density gas giant HAT-P-67 b with GIARPS

被引：5

作者：

Sicilia, D. ^{[1
]}

Scandariato, G. ^{[1
]}

Guilluy, G. ^{[2
]}

Esposito, M. ^{[3
]}

Borsa, F. ^{[4
]}

Stangret, M. ^{[5
]}

Di Maio, C. ^{[6
]}

Lanza, A. F. ^{[1
]}

Bonomo, A. S. ^{[2
]}

Desidera, S. ^{[5
]}

Fossati, L. ^{[7
]}

Nardiello, D. ^{[5
,8
]}

Sozzetti, A. ^{[2
]}

Malavolta, L. ^{[8
]}

Nascimbeni, V. ^{[5
]}

Rainer, M. ^{[4
]}

D'Arpa, M. C. ^{[6
,9
]}

Mancini, L. ^{[2
,10
,11
]}

Singh, V. ^{[1
]}

Zingales, T. ^{[5
,8
]}

Affer, L. ^{[6
]}

Bignamini, A. ^{[12
]}

Claudi, R. ^{[5
]}

Colombo, S. ^{[6
]}

Cosentino, R. ^{[13
]}

Ghedina, A. ^{[13
]}

Micela, G. ^{[6
]}

Molinari, E. ^{[4
]}

Molinaro, M. ^{[12
]}

Pagano, I. ^{[1
]}

Piotto, G. ^{[8
]}

机构：

[1] INAF Osservatorio Astrofis Catania, Via S Sofia 78, I-95123 Catania, Italy

[2] INAF Osservatorio Astrofis Torino, Via Osservatorio 20, I-10025 Pino Torinese, Italy

[3] Thuringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg, Germany

[4] INAF Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, Italy

[5] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy

[6] INAF Osservatorio Astron Palermo, Piazza Parlamento 1, I-90134 Palermo, Italy

[7] Austrian Acad Sci, Space Res Inst, Schmiedl Str 6, A-8042 Graz, Austria

[8] Univ Padua, Dipartimento Fis & Astron Galileo Galilei, Vicolo Osservatorio 3, I-35122 Padua, Italy

[9] Univ Palermo, Dept Phys & Chem Emilio Segre, Via Archirafi 36, I-90123 Palermo, Italy

[10] Univ Roma Tor Vergata, Dept Phys, Via Ric Sci 1, I-00133 Rome, Italy

[11] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany

[12] INAF Osservatorio Astron Trieste, Via Tiepolo 11, I-34143 Trieste, Italy

[13] Fdn Galileo Galilei, INAF, Rambla Jose Ana Fernandez Perez 7, Brena Baja 38712, TF, Spain

来源：

ASTRONOMY & ASTROPHYSICS | 2024年 / 687卷

关键词：

techniques: photometric; techniques: spectroscopic; planets and satellites: atmospheres; planetary systems; planets and satellites: gaseous planets; planets and satellites: individual: HAT-P-67 b; HARPS-N; TRANSMISSION SPECTROSCOPY; ERROR-CORRECTION; SURFACE GRAVITY; HOT JUPITERS; PHASE-CURVE; ATMOSPHERE; PLANET; ABSORPTION; KEPLER;

D O I：

10.1051/0004-6361/202349116

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. HAT-P-67 b is one of the lowest-density gas giants known to date, making it an excellent target for atmospheric characterisation through the transmission spectroscopy technique. Aims. In the framework of the GAPS large programme, we collected four transit events of HAT-P-67 b with the aim of studying the exoplanet atmosphere and deriving the orbital projected obliquity. Methods. We exploited the high-precision GIARPS (GIANO-B + HARPS-N) observing mode of the Telescopio Nazionale Galileo (TNG) along with additional archival TESS photometry to explore the activity level of the host star. We performed transmission spec-troscopy, both in the visible (VIS) and in the near-infrared (NIR) wavelength range, and we analysed the Rossiter-McLaughlin (RML) effect when fitting both the radial velocities and the Doppler shadow. Based on the TESS photometry, we redetermined the transit parameters of HAT-P-67 b. Results. By modelling the RML effect, we derived a sky-projected obliquity of (2.2 +/- 0.4)degrees, indicating an aligned planetary orbit. The chromospheric activity index log R-HK', the CCF profile, and the variability in the transmission spectrum of the H alpha line suggest that the host star shows signatures of stellar activity and/or pulsation. We found no evidence of atomic or molecular species in the optical transmission spectra, with the exception of pseudo-signals corresponding to Cr I, Fe I, H alpha, Na I, and Ti I. In the NIR range, we found an absorption signal of the He I triplet of 5.56(-0.30)(+0.29)% (19.0 sigma), corresponding to an effective planetary radius of similar to 3 R-p (where R-p similar to 2 R-J), which extends beyond the planet's Roche lobe radius. Conclusions. Owing to the stellar variability and the high uncertainty of the model, we could not confirm the planetary origin of the signals found in the optical transmission spectrum. On the other hand, we were able to confirm previous detections of the infrared He I triplet, providing a 19.0 sigma detection. Our finding indicates that the planet's atmosphere is evaporating.

引用

页数：27

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