Abstract
Context. Young nearby stars are good candidates in the search for planets with both radial velocity (RV) and direct imaging techniques. This, in turn, allows for the computation of the giant planet occurrence rates at all separations. The RV search around young stars is a challenge as they are generally faster rotators than older stars of similar spectral types and they exhibit signatures of magnetic activity (spots) or pulsation in their RV time series. Specific analyses are necessary to characterize, and possibly correct for, this activity. Aims. Our aim is to search for planets around young nearby stars and to estimate the giant planet (GP) occurrence rates for periods up to 1000 days. Methods. We used the HARPS spectrograph on the 3.6 m telescope at La Silla Observatory to observe 89 A−M young (<600 Myr) stars. We used our SAFIR (Spectroscopic data via Analysis of the Fourier Interspectrum Radial velocities) software to compute the RV and other spectroscopic observables. Then, we computed the companion occurrence rates on this sample. Results. We confirm the binary nature of HD 177171, HD 181321 and HD 186704. We report the detection of a close low mass stellar companion for HIP 36985. No planetary companion was detected. We obtain upper limits on the GP (<13 MJup) and BD (∈ [13;80] MJup) occurrence rates based on 83 young stars for periods less than 1000 days, which are set, 2−2+3 and 1−1+3%.
Highlights
More than four thousand exoplanets have been confirmed and most of them have been found by transit or radial velocity (RV) techniques1
We have carried out an RV survey to search for planets around such young stars with the High Accuracy Radial velocity Planet Searcher (HARPS; Mayor et al 2003) and SOPHIE (Bouchy & Sophie Team 2006) spectrographs with the final aim of coupling RV data with direct imaging (DI) data, which will allow for the computation of detection limits, for each targets at
We observed 89 young A- to M-type stars over 3 yr or more with HARPS to search for giant planet (GP) and brown dwarf (BD) with periods less than 1000 days
Summary
More than four thousand exoplanets have been confirmed and most of them have been found by transit or radial velocity (RV) techniques. Young stars are generally faster rotators than their older counterparts (Stauffer et al 2016; Rebull et al 2016; Gallet & Bouvier 2015) They can exhibit activity-induced RV jitter with amplitudes up to 1 km s−1 (Lagrange et al 2013), larger than the planet’s induced signal. We have carried out an RV survey to search for planets around such young stars with the High Accuracy Radial velocity Planet Searcher (HARPS; Mayor et al 2003) and SOPHIE (Bouchy & Sophie Team 2006) spectrographs with the final aim of coupling RV data with direct imaging (DI) data, which will allow for the computation of detection limits, for each targets at.
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