TY - JOUR
T1 - The PEPSI Exoplanet Transit Survey (PETS)
T2 - III. The detection of Fe I, Cr I, and Ti I in the atmosphere of MASCARA-1 b through high-resolution emission spectroscopy
AU - Scandariato, G.
AU - Borsa, F.
AU - Bonomo, A. S.
AU - Gaudi, B. S.
AU - Henning, Th
AU - Ilyin, I.
AU - Johnson, M. C.
AU - Malavolta, L.
AU - Mallonn, M.
AU - Molaverdikhani, K.
AU - Nascimbeni, V.
AU - Patience, J.
AU - Pino, L.
AU - Poppenhaeger, K.
AU - Schlawin, E.
AU - Shkolnik, E. L.
AU - Sicilia, D.
AU - Sozzetti, A.
AU - Strassmeier, K. G.
AU - Veillet, C.
AU - Wang, J.
AU - Yan, F.
N1 - Publisher Copyright:
© 2021 Lippincott Williams and Wilkins. All rights reserved.
PY - 2023/6/1
Y1 - 2023/6/1
N2 - Context. Hot giant planets such as MASCARA-1 b are expected to have thermally inverted atmospheres, which makes them perfect laboratories for atmospheric characterization through high-resolution spectroscopy. Nonetheless, previous attempts at detecting the atmosphere of MASCARA-1 b in transmission have led to negative results. Aims. We aim to detect the optical emission spectrum of MASCARA-1 b. Methods. We used the high-resolution spectrograph PEPSI to observe MASCARA-1 (spectral type A8) near the secondary eclipse of the planet. We cross-correlated the spectra with synthetic templates computed for several atomic and molecular species. Results. We detect Fe I, Cr I, and Ti I in the atmosphere of MASCARA-1 b with a S/N ≈ 7, 4, and 5, respectively, and confirm the expected systemic velocity of ≈ 13 km s-1 and the radial velocity semi-amplitude of MASCARA-1 b of ≈200 km s-1. The detection of Ti is of particular importance in the context of the recently proposed phenomenon of Ti cold-trapping below a certain planetary equilibrium temperature. Conclusions. We confirm the presence of an atmosphere around MASCARA-1 b through emission spectroscopy. We conclude that the atmospheric non-detection in transmission spectroscopy is due to the strong gravity of the planet and/or to the overlap between the planetary track and its Doppler shadow.
AB - Context. Hot giant planets such as MASCARA-1 b are expected to have thermally inverted atmospheres, which makes them perfect laboratories for atmospheric characterization through high-resolution spectroscopy. Nonetheless, previous attempts at detecting the atmosphere of MASCARA-1 b in transmission have led to negative results. Aims. We aim to detect the optical emission spectrum of MASCARA-1 b. Methods. We used the high-resolution spectrograph PEPSI to observe MASCARA-1 (spectral type A8) near the secondary eclipse of the planet. We cross-correlated the spectra with synthetic templates computed for several atomic and molecular species. Results. We detect Fe I, Cr I, and Ti I in the atmosphere of MASCARA-1 b with a S/N ≈ 7, 4, and 5, respectively, and confirm the expected systemic velocity of ≈ 13 km s-1 and the radial velocity semi-amplitude of MASCARA-1 b of ≈200 km s-1. The detection of Ti is of particular importance in the context of the recently proposed phenomenon of Ti cold-trapping below a certain planetary equilibrium temperature. Conclusions. We confirm the presence of an atmosphere around MASCARA-1 b through emission spectroscopy. We conclude that the atmospheric non-detection in transmission spectroscopy is due to the strong gravity of the planet and/or to the overlap between the planetary track and its Doppler shadow.
KW - Planets and satellites: atmospheres
KW - Planets and satellites: composition
KW - Planets and satellites: individual: MASCARA-1 b
KW - Techniques: spectroscopic
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U2 - 10.1051/0004-6361/202245539
DO - 10.1051/0004-6361/202245539
M3 - Article
AN - SCOPUS:85162186663
SN - 0004-6361
VL - 674
JO - Astronomy and astrophysics
JF - Astronomy and astrophysics
M1 - A58
ER -