Characterization of the HD 17156 planetary systemM. Barbieri1, R. Alonso1, S. Desidera2, A. Sozzetti3, A. F. Martinez Fiorenzano4, J. M. Almenara5, M. Cecconi4, R. U. Claudi2, D. Charbonneau6, M. Endl7, V. Granata2, 8, R. Gratton2, G. Laughlin9, B. Loeillet1, 10, and Exoplanet Amateur Consortium
1 Laboratoire d'Astrophysique de Marseille, 38 rue Joliot-Curie, 13388 Marseille Cedex 13, France
2 INAF Osservatorio Astronomico di Padova, Vicolo dell' Osservatorio 5, 35122 Padova, Italy
3 INAF Osservatorio Astronomico di Torino, 10025 Pino Torinese, Italy
4 Fundación Galileo Galilei – INAF, Rambla José Ana Fernández Pérez 7, 38712 Breña Baja (TF), Spain
5 Instituto de Astrofísica de Canarias, C/Vía Láctea s/n, 38200 La Laguna, Spain
6 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
7 McDonald Observatory, The University of Texas at Austin, Austin, TX 78712, USA
8 CISAS, Università di Padova, Italy
9 University of California Observatories, University of California at Santa Cruz Santa Cruz, CA 95064, USA
10 IAP, 98bis Bd Arago, 75014 Paris, France
Received 2 December 2008 / Accepted 12 March 2009
Aims. We present data to improve the known parameters of the HD 17156 system (peculiar due to the eccentricity and long orbital period of its transiting planet) and constrain the presence of stellar companions.
Methods. Photometric data were acquired for 4 transits, and high precision radial velocity measurements were simultaneously acquired with the SARG spectrograph at TNG for one transit. The template spectra of HD 17156 was used to derive effective temperature, gravity, and metallicity. A fit of the photometric and spectroscopic data was performed to measure the stellar and planetary radii, and the spin-orbit alignment. Planet orbital elements and ephemeris were derived from the fit. Near infrared adaptive optic images were acquired with the AdOpt module of TNG.
Results. We found that the star has a radius of RS = 1.440.03 and the planet RP = 1.020.08 RJ. The transit ephemeris is Tc = 2 454 756.73134 0.00020 + N 21.21663 0.00045 BJD. Analysis of the Rossiter-Mclaughlin effect shows that the system is spin orbit aligned with an angle = 4.8°5.3°. The analysis of high resolution images did not reveal any stellar companion with a projected separation between of 150 and 1 000 AU from HD 17156.
Key words: stars: individual: HD 17156 -- stars: binaries: eclipsing -- stars: planetary systems -- techniques: spectroscopic -- techniques: photometric
© ESO 2009