Volume 470, Number 3, August II 2007
|Page(s)||1137 - 1156|
|Section||Planets and planetary systems|
|Published online||24 April 2007|
A new search for planet transits in NGC 6791*
Dipartimento di Astronomia, Università di Padova, Vicolo dell'Osservatorio 2, 35122 Padova, Italy e-mail: firstname.lastname@example.org
2 INAF – Osservatorio Astronomico di Padova, Vicolo dell' Osservatorio 5, 35122 Padova, Italy
3 Department of Physics and Astronomy, University of Aarhus, Denmark
4 University of Sydney, School of Physics, 2006 NSW, Australia
5 Herzberg Institute of Astrophysics, Victoria, Canada
6 Instituto de Astronomía, Universidad Nacional Autónoma de México
7 INAF – Osservatorio Astronomico di Brera, Via E. Bianchi 46, 23807 Merate (LC), Italy
8 Instituto de Astrofisica de Canarias, 38200 La Laguna, Tenerife, Canary Islands, Spain
9 Dipartimento di Fisica, Università di Padova, Italy
Accepted: 12 April 2007
Context.Searching for planets in open clusters allows us to study the effects of dynamical environment on planet formation and evolution.
Aims.Considering the strong dependence of planet frequency on stellar metallicity, we studied the metal rich old open cluster NGC 6791 and searched for close-in planets using the transit technique.
Methods.A ten-night observational campaign was performed using the Canada-France-Hawaii Telescope (3.6 m), the San Pedro Mártir telescope (2.1 m), and the Loiano telescope (1.5 m). To increase the transit detection probability we also made use of the Bruntt et al. (2003, A&A, 410, 323) eight-nights observational campaign. Adequate photometric precision for the detection of planetary transits was achieved.
Results. Should the frequency and properties of close-in planets in NGC 6791 be similar to those orbiting field stars of similar metallicity, then detailed simulations foresee the presence of 2–3 transiting planets. Instead, we do not confirm the transit candidates proposed by Bruntt et al. (2003, A&A, 410, 323). The probability that the null detection is simply due to chance coincidence is estimated to be 3%–10%, depending on the metallicity assumed for the cluster.
Conclusions.Possible explanations of the null-detection of transits include: (i) a lower frequency of close-in planets in star clusters; (ii) a smaller planetary radius for planets orbiting super metal rich stars; or (iii) limitations in the basic assumptions. More extensive photometry with 3–4 m class telescopes is required to allow conclusive inferences about the frequency of planets in NGC 6791.
Key words: Galaxy: open cluster and associations: individual: NGC 6791 / stars: planetary systems / techniques: photometric
Based on observation obtained at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii and on observations obtained at San Pedro Mártir 2.1 m telescope (Mexico), and Loiano 1.5 m telescope (Italy).
© ESO, 2007
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