Andrea Bignamini, Riccardo Smareglia, Marco Pedani, Luca Malavolta, Isabella Pagano, Ivan Bruni, Jesus Maldonado, John Southworth, Antonio Maggio, Alexis M. S. Smith, Matteo Brogi, Giampaolo Piotto, Aldo S. Bonomo, S. Masiero, R. Cosentino, Laura Affer, E. Gonzalez-Alvarez, Emilio Molinari, Riccardo Claudi, E. Covino, Raffaele Gratton, Serena Benatti, Alessandro Sozzetti, Gloria Andreuzzi, Th. Henning, Giuseppe Leto, Gaetano Scandariato, A. Martinez-Fiorenzano, Giuseppina Micela, C. Boccato, I. Carleo, Daniel F. Evans, A. F. Lanza, Monica Rainer, Avet Harutyunyan, P. Giacobbe, M. Esposito, Paula Sarkis, F. Borsa, Silvano Desidera, K. Biazzo, Luigi Mancini, Valerio Nascimbeni, E. Poretti, Simona Ciceri, Mario Damasso, and ITA
We characterised five transiting planetary systems (HAT-P-3, HAT-P-12, HAT-P-22, WASP-39 and WASP-60) and determined their sky-projected planet orbital obliquity through the measurement of the RM effect. We used HARPS-N high-precision radial velocity measurements, gathered during transit events, to measure the RM effect in the target systems and determine the sky-projected angle between the planetary orbital plane and the stellar equator. The characterisation of stellar atmospheric parameters was performed exploiting the HARPS-N spectra, using line equivalent width ratios, and spectral synthesis methods. Photometric parameters of the five transiting exoplanets were re-analysed through 17 new light curves, obtained with an array of medium-class telescopes, and other light curves from the literature. Survey-time-series photometric data were analysed for determining the rotation periods of the five stars and their spin inclination. From the analysis of the RM effect we derived a sky-projected obliquity of 21.2 degree, -54 degree, -2.1 degree, 0 degree and -129 degree for HAT-P-3b, HAT-P-12b, HAT-P-22b, WASP-39b and WASP-60b, respectively. The latter value indicates that WASP-60b is moving on a retrograde orbit. These values represent the first measurements of \lambda for the five exoplanetary systems under study. The stellar activity of HAT-P-22 indicates a rotation period of 28.7 days, which allowed us to estimate the true misalignment angle of HAT-P-22b, \psi=24 degree. The revision of the physical parameters of the five exoplanetary systems returned values that are fully compatible with those existing in the literature. The exception to this is the WASP-60 system, for which, based on higher quality spectroscopic and photometric data, we found a more massive and younger star and a larger and hotter planet., Comment: 21 pages, 10 figure, accepted for publication in Astronomy & Astrophysics