Volume 465, Number 3, April III 2007
|Page(s)||1069 - 1074|
|Section||Planets and planetary systems|
|Published online||05 February 2007|
The “666” collaboration on OGLE transits*
I. Accurate radius of the planets OGLE-TR-10b and OGLE-TR-56b with VLT deconvolution photometry
Observatoire de Genève, 51 chemin des Maillettes, 1290 Sauverny, Switzerland e-mail: firstname.lastname@example.org
2 Laboratoire d'Astrophysique de Marseille, Traverse du Siphon, BP 8, Les Trois Lucs, 13376 Marseille Cedex 12, France
3 Institut d'Astrophysique et de Géophysique, Université de Liège, Allée du 6 Août 17, 4000 Liège, Belgium
4 Warsaw University Observatory, Al. Ujazdowskie 4, 00-478 Warsaw, Poland
5 Observatoire de Haute-Provence, 04870 St-Michel l'Observatoire, France
6 Institut d'Astrophysique de Paris, 98bis Bd. Arago, 75014 Paris, France
7 Grupo de Astrofísica UC, Observatório Astronómico da Universidade de Coimbra, Santa Clara, Coimbra, Portugal
8 Departamento de Fisica, Astronomy Group, Universidad de Concepción, Casilla 160-C, Concepción, Chile
9 School of Physics and Astronomy, Raymond and Beverly Sackler Faculty of Exact Sciences, Tel Aviv University, Tel Aviv, Israel
10 Departmento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Casilla 306, Santiago 22, Chile
11 European Southern Observatory, Casilla 19001, Santiago 19, Chile
12 Department of Astronomy, Universidad de Chile, Santiago, Chile
13 Centro de Astronomia e Astrofísica da Universidade de Lisboa, Observatório Astronómico de Lisboa, Tapada da Ajuda, 1349-018 Lisboa, Portugal
14 Centro de Geofisica de Évora, Rua Romão Ramalho 59, 7002-554 Évora, Portugal
Accepted: 30 January 2007
Transiting planets are essential to study the structure and evolution of extra-solar planets. For that purpose, it is important to measure precisely the radius of these planets. Here we report new high-accuracy photometry of the transits of OGLE-TR-10 and OGLE-TR-56 with VLT/FORS1. One transit of each object was covered in Bessel V and R filters, and treated with the deconvolution-based photometry algorithm DECPHOT, to ensure accurate millimagnitude light curves. Together with earlier spectroscopic measurements, the data imply a radius of RJ for OGLE-TR-10b and 1.30 ± 0.05 RJ for OGLE-TR-56b. A re-analysis of the original OGLE photometry resolves an earlier discrepancy about the radius of OGLE-TR-10. The transit of OGLE-TR-56 is almost grazing, so that small systematics in the photometry can cause large changes in the derived radius. Our study confirms both planets as inflated hot Jupiters, with large radii comparable to that of HD 209458b and at least two other recently discovered transiting gas giants.
Key words: stars: planetary systems / techniques: photometric
© ESO, 2007
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