The GAPS Programme at TNG

被引:8
作者
Basilicata, M. [1 ,2 ]
Giacobbe, P. [2 ]
Bonomo, A. S. [2 ]
Scandariato, G. [3 ]
Brogi, M. [2 ,4 ]
Singh, V. [3 ]
Di Paola, A. [4 ]
Mancini, L. [1 ,2 ,5 ]
Sozzetti, A. [2 ]
Lanza, A. F. [3 ]
Cubillos, P. E. [2 ,14 ]
Damasso, M. [2 ]
Desidera, S. [13 ]
Biazzo, K. [3 ]
Bignamini, A. [10 ]
Borsa, F. [6 ]
Cabona, L. [13 ]
Carleo, I. [2 ,11 ]
Ghedina, A. [7 ]
Guilluy, G. [2 ]
Maggio, A. [8 ]
Mainella, G. [7 ]
Micela, G. [8 ]
Molinari, E. [6 ]
Molinaro, M. [10 ]
Nardiello, D. [13 ]
Pedani, M. [7 ]
Pino, L. [12 ]
Poretti, E. [6 ,7 ]
Southworth, J. [9 ]
Stangret, M. [13 ]
Turrini, D. [2 ]
机构
[1] Univ Roma Tor Vergata, Dept Phys, Via Ric Sci 1, I-00133 Rome, Italy
[2] INAF Osservatorio Astrofis Torino, Via Osservatorio 20, I-10025 Pino Torinese, Italy
[3] INAF Osservatorio Astrofis Catania, Via S Sofia 78, I-95123 Catania, Italy
[4] Univ Turin, Dept Phys, Via Pietro Giuria 1, I-10125 Turin, Italy
[5] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany
[6] INAF Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, LC, Italy
[7] Fdn Galileo Galilei INAF, Rambla Jose Ana Fernandez Perez 7, Brena Baja 38712, Spain
[8] INAF Osservatorio Astron Palermo, Piazza Parlamento 1, I-90134 Palermo, Italy
[9] Keele Univ, Astrophys Grp, Keele ST5 5BG, England
[10] INAF Osservatorio Astron Trieste, Via Tiepolo 11, I-34143 Trieste, Italy
[11] Inst Astrofis Canarias IAC, San Cristobal la Laguna 38205, Tenerife, Spain
[12] INAF Osservatorio Astrofis Arcetri, Largo Enrico Fermi 5, I-50125 Florence, Italy
[13] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy
[14] Austrian Acad Sci, Space Res Inst, Schmiedlsstr 6, A-8042 Graz, Austria
基金
奥地利科学基金会;
关键词
techniques: spectroscopic; planets and satellites: atmospheres; planets and satellites: individual: HAT-P-11 b; COLLISION-INDUCED ABSORPTION; INDUCED INFRARED-SPECTRA; HIPPARCOS-GAIA CATALOG; CHAIN MONTE-CARLO; RADIATIVE-TRANSFER; HIGH-RESOLUTION; WATER-VAPOR; HOT JUPITER; GIANT PLANETS; H-2-HE PAIRS;
D O I
10.1051/0004-6361/202347659
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Context. The atmospheric characterisation of hot and warm Neptune-size exoplanets is challenging mainly due to their relatively small radius and atmospheric scale height, which reduce the amplitude of atmospheric spectral features. The warm-Neptune HAT-P-11 b is a remarkable target for atmospheric characterisation because of the large brightness of its host star (V = 9.46 mag; H = 7.13 mag). Aims. The aims of this work are to review the main physical and architectural properties of the HAT-P-11 planetary system, and to probe the presence of eight molecular species in the atmosphere of HAT-P-11 b through near-infrared (NIR) high-resolution transmission spectroscopy. Methods. We reviewed the physical and architectural properties of the HAT-P-11 planetary system by analysing transits and occultations of HAT-P-11 b from the Kepler data set as well as HIRES at Keck archival radial-velocity data. We modelled the latter with Gaussian-process regression and a combined quasi-periodic and squared-exponential kernel to account for stellar variations on both (short-term) rotation and (long-term) activity-cycle timescales. In order to probe the atmospheric composition of HAT-P-11 b, we observed four transits of this target with the NIR GIANO-B at TNG spectrograph and cross-correlated the data with template atmospheric transmission spectra. Results. We find that the long-period radial-velocity signal previously attributed to the HAT-P-11 c planet (P similar to 9.3 yr; M-p sin i similar to 1.6 M-J; e similar to 0.6) is more likely due to the stellar magnetic activity cycle. Nonetheless, the HIPPARCOS-Gaia difference in the proper-motion anomaly suggests that an outer-bound companion might still exist. For HAT-P-11 b, we measure a radius of R-p = 0.4466 +/- 0.0059 R-J, a mass of M-p = 0.0787 +/- 0.0048 M-J, a bulk density of rho p = 1.172 +/- 0.085 g cm(-3), and an orbital eccentricity of e = 0.2577(-0.0025)(+0.0033). These values are compatible with those from the literature. Probing its atmosphere, we detect the presence of two molecular species, H2O and NH3, with a S/N of 5.1 and 5.3, and a significance of 3.4 sigma and 5.0 sigma, respectively. We also tentatively detect the presence of CO2 and CH4, with a S/N of 3.0 and 4.8, and a significance of 3.2 sigma and 2.6 sigma, respectively. Conclusions. We revisit the HAT-P-11 planetary system, confirm the presence of H2O, and report the detection of NH3 in the atmosphere of HAT-P-11 b, also finding hints for the presence of CO2 and CH4 that need to be confirmed by further observations.
引用
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页数:26
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