Issue |
A&A
Volume 481, Number 2, April II 2008
|
|
---|---|---|
Page(s) | 529 - 533 | |
Section | Planets and planetary systems | |
DOI | https://doi.org/10.1051/0004-6361:20078167 | |
Published online | 04 February 2008 |
Refined parameters and spectroscopic transit of the super-massive planet HD 147506b*
1
Laboratoire d'Astrophysique de Marseille, BP 8, 13376 Marseille Cedex 12; Université de Provence, CNRS (UMR 6110) and CNES, France e-mail: benoit.loeillet@oamp.fr
2
Institut d'Astrophysique de Paris, UMR 7095 CNRS, Université Pierre et Marie Curie, 98bis Bd Arago, 75014 Paris, France
3
Wise Observatory, Tel Aviv University, 69978, Israel
4
Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, 1290 Sauverny, Switzerland
5
Laboratoire d'Astrophysique de Grenoble, Observatoire de Grenoble, UMR5571, Université J. Fourier et CNRS, BP 53, 38041 Grenoble, France
6
Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal
Received:
26
June
2007
Accepted:
14
January
2008
In this paper, we report a refined determination of the orbital parameters
and the detection of the Rossiter-McLaughlin effect of the recently discovered
transiting exoplanet HD 147506b (HAT-P-2b). The large orbital eccentricity at the short orbital
period of this exoplanet is unexpected and is distinguishing from other known
transiting exoplanets.
We performed high-precision radial velocity spectroscopic observations
of HD 147506 (HAT-P-2) with the new spectrograph SOPHIE, mounted on the 1.93 m telescope at the
Haute-Provence observatory (OHP).
We obtained 63 new measurements, including 35 on May 14 and 20 on June 11,
when the planet was transiting its parent star.
The radial velocity (RV) anomaly observed illustrates that HAT-P-2b orbital motion is set in the
same direction as its parent star spin.
The sky-projected angle between the normal of the orbital plane and the stellar spin
axis, °, is consistent with zero. The planetary and stellar radii were re-determined, yielding
RJup ,
.
The mass (
MJup) and radius of HAT-P-2b
indicate a density of
g cm-3,
suggesting an object in between the known close-in planets with typical density of
the order of 1 g cm-3, and the very low-mass stars, with density greater than
50 g cm-3.
Key words: techniques: radial velocities / stars: individual: HD 147506 / stars: planetary systems
© ESO, 2008
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