Volume 594, October 2016
|Number of page(s)||7|
|Section||Planets and planetary systems|
|Published online||10 October 2016|
K2-30 b and K2-34 b: Two inflated hot Jupiters around solar-type stars ⋆
1 European Southern Observatory (ESO), Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago de Chile, Chile
2 Depto. de Astrofísica, Centro de Astrobiología (CSIC-INTA), ESAC campus, 28692 Villanueva de la Cañada, Madrid, Spain
3 Aix Marseille Université, CNRS, Laboratoire d’Astrophysique de Marseille UMR 7326, 13388 Marseille, France
4 Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal
5 Institut d’Astrophysique de Paris, UMR7095 CNRS, Université Pierre & Marie Curie, 98bis boulevard Arago, 75014 Paris, France
6 Observatoire de Haute-Provence, Université d’Aix-Marseille & CNRS, 04870 Saint-Michel l’ Observatoire, France
7 Department of Physics, University of Warwick, Gibbet Hill Road, Coventry, CV4 7AL, UK
8 Université Grenoble Alpes, IPAG, 38000 Grenoble, France
9 CNRS, IPAG, 38000 Grenoble, France
10 Observatoire Astronomique de l’Université de Genève, 51 chemin des Maillettes, 1290 Versoix, Switzerland
11 Astronomy and Astrophysics Division, Physical Research Laboratory, 380009 Ahmedabad, India
12 ARC, School of Mathematics & Physics, Queen’s University Belfast, University Road, Belfast BT7 1NN, UK
13 Depto. de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, Rua Campo Alegre, 4169-007 Porto, Portugal
Received: 28 January 2016
Accepted: 20 May 2016
We report the discovery of the two hot Jupiters K2-30 b and K2-34 b. The two planets were detected during campaigns 4 and 5 of the extension of the Kepler mission, K2; they transit their main-sequence stars with periods of ~4.099 and ~2.996 days. Subsequent ground-based radial velocity follow-up with SOPHIE, HARPS-N, and CAFE established the planetary nature of the transiting objects. We analyzed the transit signal, radial velocity, and spectral energy distributions of the two systems to characterize their properties. Both planets (K2-30 b and K2-34 b) are bloated hot Jupiters (1.20 RJup and 1.22 RJup) around relatively bright (V = 13.5 and V = 11.5) slow rotating main-sequence (G8 and F9) stars. Thus, these systems are good candidates for detecting the Rossiter-MacLaughlin effect in order to measure their obliquity and for atmospheric studies.
Key words: planets and satellites: detection / planets and satellites: gaseous planets / techniques: radial velocities / techniques: photometric / techniques: high angular resolution
Full Tables 1 and 2 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (22.214.171.124) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/594/A50
© ESO, 2016
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