Volume 620, December 2018
|Number of page(s)||15|
|Section||Planets and planetary systems|
|Published online||10 December 2018|
Departamento de Física, Universidade Federal do Rio Grande do Norte,
2 Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, 1290 Sauverny, Switzerland
3 Universidade Federal do Recôncavo da Bahia, Centro de Ciências Exatas e Tecnológicas, Av. Rui Barbosa, 710, Cruz das Almas, BA, 44380-000, Brazil
4 Departamento de Física, Facultad de Ciencias Básicas, Universidad Metropolitana de la Educación, Av. José Pedro Alessandri 774, 7760197 Nuñoa, Santiago, Chile
5 Millennium Institute of Astrophysics, Santiago, Chile
6 European Southern Observatory, Karl-Schwarzschild-Straße 2, 85748 Garching bei München, Germany
7 ESO, Casilla 19001, Santiago 19, Chile
8 Departamento de Física, Universidade Federal do Ceará, Caixa Postal 6030, Campus do Pici, 60455-900 Fortaleza, Ceará, Brazil
Accepted: 7 July 2018
Context. Detecting exoplanets in clusters of different ages is a powerful tool for understanding a number of open questions, such as how the occurrence rate of planets depends on stellar metallicity, on mass, or on stellar environment.
Aims. We present the first results of our HARPS long-term radial velocity (RV) survey which aims to discover exoplanets around intermediate-mass (between ~2 and 6 M⊙) evolved stars in open clusters.
Methods. We selected 826 bona fide HARPS observations of 114 giants from an initial list of 29 open clusters and computed the half-peak to peak variability of the HARPS RV measurements, namely ΔRV∕2, for each target, to search for the best planet-host candidates. We also performed time series analyses for a few targets for which we have enough observations to search for orbital solutions.
Results. Although we attempted to rule out the presence of binaries on the basis of previous surveys, we detected 14 new binary candidates in our sample, most of them identified from a comparison between HARPS and CORAVEL data. We also suggest 11 new planet-host candidates based on a relation between the stellar surface gravity and ΔRV∕2. Ten of the candidates are less than 3 M⊙, showing evidence of a low planet occurrence rate for massive stars. One of the planet-host candidates and one of the binary candidates show very clear RV periodic variations, allowing us to confirm the discovery of a new planet and to compute the orbital solution for the binary. The planet is IC 4651 9122b, with a minimum mass of m sini = 6.3 MJ and a semimajor axis a = 2.0 AU. The binary companion is NGC 5822 201B, with a very low minimum mass of m sini = 0.11 M⊙ and a semimajor axis a = 6.5 AU, which is comparable to the Jupiter distance to the Sun.
Key words: planetary systems / open clusters and associations: general / stars: late-type / binaries: spectroscopic / techniques: radial velocities
Based on observations collected with the 3.6 m Telescope (La Silla Observatory, ESO, Chile) using the HARPS instrument (programs ID: 091.C-0438, 092.C-0282, and 094.C-0297).
The reduced time series data are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (220.127.116.11) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/620/A139
© ESO 2018
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