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XXX. Atmospheric Rossiter-McLaughlin effect and atmospheric dynamics of KELT-20b★
M. Rainer1, F. Borsa2, L. Pino1,3, G. Frustagli2,4, M. Brogi5,6,7, K. Biazzo8, A. S. Bonomo6, I. Carleo9,10, R. Claudi10, R. Gratton10, A. F. Lanza11, A. Maggio12, J. Maldonado12, L. Mancini13,14,6, G. Micela12, G. Scandariato11, A. Sozzetti6, N. Buchschacher15, R. Cosentino17, E. Covino16, A. Ghedina17, M. Gonzalez17, G. Leto11, M. Lodi17, A. F. Martinez Fiorenzano17, E. Molinari18, M. Molinaro19, D. Nardiello20,10, E. Oliva1, I. Pagano11, M. Pedani17, G. Piotto21 and E. Poretti17
1 INAF - Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, 50125 Firenze, Italye-mail: monica.rainer@inaf.it2 INAF - Osservatorio Astronomico di Brera, Via E. Bianchi, 46, 23807 Merate (LC), Italy3 Anton Pannekoek Institute for Astronomy, University of Amsterdam Science Park 904 1098 XH Amsterdam, The Netherlands4 Università degli Studi di Milano Bicocca, Piazza dell’Ateneo Nuovo, 1, 20126 Milano, Italy5 Department of Physics, University of Warwick, Coventry CV4 7AL, UK6 INAF - Osservatorio Astrofisico di Torino, Via Osservatorio 20, 10025 Pino Torinese (TO), Italy7 Centre for Exoplanets and Habitability, University of Warwick, Gibbet Hill Road, Coventry CV4 7AL, UK8 INAF - Osservatorio Astronomico di Roma, Via Frascati 33, 00078 Monte Porzio Catone (Roma), Italy9 Astronomy Department and Van Vleck Observatory, Wesleyan University, Middletown, CT 06459, USA10 INAF - Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio, 5, 35122 Padova (PD), Italy11 INAF - Osservatorio Astrofisico di Catania, Via S. Sofia 78, 95123 Catania, Italy12 INAF - Osservatorio Astronomico di Palermo, Piazza del Parlamento, 1, 90134 Palermo, Italythirteen Department of Physics, University of Rome “Tor Vergata”, Via della Ricerca Scientifica 1, 00133 Rome, Italy14 Max Planck Institute for Astronomy, Königstuhl 17, 69117, Heidelberg, Germany15 Department of Astronomy, University of Geneva, Chemin des Maillettes 51, 1290 Versoix, Suisse16 INAF - Osservatorio Astronomico di Capodimonte, Salita Moiariello 16, 80131 Napoli, Italy17 INAF - Fundación Galileo Galilei, Rambla José Ana Fernandez Pérez 7, 38712 Breña Baja (TF), Spain18 INAF - Osservatorio Astronomico di Cagliari, Via della Scienza 5, 09047 Cuccuru Angius, Selargius (CA), Italy19 INAF - Osservatorio Astronomico di Trieste, Via Giambattista Tiepolo, 11, 34131 Trieste, Italy20 Aix-Marseille Université, CNRS, CNES, LAM, Marseille, France21 Dipartimento di Fisica e Astronomia Galileo Galilei - Università di Padova, Vicolo dell’Osservatorio 2, 35122 Padova, Italy
Received: 24 August 2020Accepted: 16 March 2021
Abstract
Context. Transiting extremely-sizzling Jupiters are ultimate candidates for learning the exoplanet atmospheres and their dynamics, particularly by way of high-resolution spectra with high sign-to-noise ratios. One such object is KELT-20b. It orbits the quick-rotating A2-type star KELT-20. Many atomic species have been found in its atmosphere, with blueshifted indicators that point out a day- to night time-facet wind.
Aims. We observe the atmospheric Rossiter-McLaughlin effect within the ultra-hot Jupiter KELT-20b and study any variation of the atmospheric sign in the course of the transit. For this purpose, we analysed 5 nights of HARPS-N spectra overlaying 5 transits of KELT-20b.
Methods. We computed the mean line profiles of the spectra with a least-squares deconvolution utilizing a stellar mask obtained from the Vienna Atomic Line Database (Teff = 10 000 K, log g = 4.3), and then we extracted the stellar radial velocities by fitting them with a rotational broadening profile in order to acquire the radial velocity time-sequence. We used the mean line profile residuals tomography to analyse the planetary atmospheric signal and its variations. We also used the cross-correlation technique to review a previously reported double-peak characteristic within the FeI planetary signal.
Results. We noticed both the classical and the atmospheric Rossiter-McLaughlin impact in the radial velocity time-collection. The latter gave us an estimate of the radius of the planetary environment that correlates with the stellar mask utilized in our work (Rp+atmo∕Rp = 1.13 ± 0.02). We isolated the planetary atmospheric hint within the tomography, and we discovered radial velocity variations of the planetary atmospheric sign during transit with an overall blueshift of ≈10 km s−1, along with small variations within the sign depth, and less significant, in the total width at half maximum (FWHM). We additionally discover a attainable variation in the structure and place of the FeI signal in different transits.
Conclusions. We confirm the beforehand detected blueshift of the atmospheric signal throughout the transit. The FWHM variations of the atmospheric signal, if confirmed, could also be attributable to extra turbulent condition at the beginning of the transit, by a variable contribution of the weather current within the stellar mask to the general planetary atmospheric sign, or by iron condensation. The FeI signal present indications of variability from one transit to the next.
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