Spin-orbit angle measurements for six southern transiting planets
A. H. M. J. Triaud1, A. Collier Cameron2, D. Queloz1, D. R. Anderson3, M. Gillon4, L. Hebb5, C. Hellier3, B. Loeillet6, P. F. L. Maxted3, M. Mayor1, F. Pepe1, D. Pollacco7, D. Ségransan1, B. Smalley3, S. Udry1, R. G. West8 and P. J. Wheatley9
Observatoire Astronomique de l’Université de Genève,
Chemin des Maillettes 51,
2 School of Physics & Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS, Fife, Scotland, UK
3 Astrophysics Group, Keele University, Staffordshire ST55 BG, UK
4 Institut d’Astrophysique et de Géophysique, Université de Liège, Allée du 6 Août, 17, Bât. B5C, Liège 1, Belgium
5 Department of Physics and Astronomy, Vanderbilt University, Nashville, TN37235, USA
6 Laboratoire d’Astrophysique de Marseille, BP 8, 13376 Marseille Cedex 12, France
7 Astrophysics Research Centre, School of Mathematics & Physics, Queens University, University Road, Belfast BT71 NN, UK
8 Department of Physics and Astronomy, University of Leicester, Leicester LE17 RH, UK
9 Department of Physics, University of Warwick, Coventry CV4 7AL, UK
Received: 28 March 2010
Accepted: 11 August 2010
Context. Several competing scenarios for planetary-system formation and evolution seek to explain how hot Jupiters came to be so close to their parent stars. Most planetary parameters evolve with time, making it hard to distinguish between models. The obliquity of an orbit with respect to the stellar rotation axis is thought to be more stable than other parameters such as eccentricity. Most planets, to date, appear aligned with the stellar rotation axis; the few misaligned planets so far detected are massive (> 2MJ).
Aims. Our goal is to measure the degree of alignment between planetary orbits and stellar spin axes, to search for potential correlations with eccentricity or other planetary parameters and to measure long term radial velocity variability indicating the presence of other bodies in the system.
Methods. For transiting planets, the Rossiter-McLaughlin effect allows the measurement of the sky-projected angle β between the stellar rotation axis and a planet’s orbital axis. Using the HARPS spectrograph, we observed the Rossiter-McLaughlin effect for six transiting hot Jupiters found by the WASP consortium. We combine these with long term radial velocity measurements obtained with CORALIE. We used a combined analysis of photometry and radial velocities, fitting model parameters with the Markov Chain Monte Carlo method. After obtaining β we attempt to statistically determine the distribution of the real spin-orbit angle ψ.
Results. We found that three of our targets have β above 90°: WASP-2b: , WASP-15b: and WASP-17b: ; the other three (WASP-4b, WASP-5b and WASP-18b) have angles compatible with 0°. We find no dependence between the misaligned angle and planet mass nor with any other planetary parameter. All six orbits are close to circular, with only one firm detection of eccentricity in WASP-18b. No long-term radial acceleration was detected for any of the targets. Combining all previous 20 measurements of β and our six and transforming them into a distribution of ψ we find that between about 45 and 85% of hot Jupiters have ψ > 30°.
Conclusions. Most hot Jupiters are misaligned, with a large variety of spin-orbit angles. We find observations and predictions using the Kozai mechanism match well. If these observational facts are confirmed in the future, we may then conclude that most hot Jupiters are formed from a dynamical and tidal origin without the necessity to use type I or II migration. At present, standard disc migration cannot explain the observations without invoking at least another additional process.
Key words: binaries: eclipsing / stars: general / techniques: spectroscopic
Using observations with the high resolution échelle spectrograph HARPS mounted on the ESO 3.6 m (under proposals 072.C-0488, 082.C-0040 & 283.C-5017), and with the high resolution échelle spectrograph CORALIE on the 1.2 m Euler Swiss Telescope, both installed at the ESO La Silla Observatory in Chile.
RV data is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (126.96.36.199) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/524/A25
© ESO, 2010