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The discovery of a planetary candidate around the evolved low-mass Kepler giant star HD 175370

par Hrudkova, Marie;Hatzes, Artie;Karjalainen, R.;Lehmann, H.;Hekker, S.;Hartmann, M.;Tkachenko, A.;Prins, S.;Van Winckel, Hans;De Nutte, R.;Dumortier, L.;Frémat, Yves;Hensberge, H.;Jorissen, Alain ;Lampens, Patricia;Laverick, M.;Lombaert, Robert ;Pápics, P.~I.;Raskin, Gert;Sódor, Á.;Thoul, Anne;Van Eck, Sophie ;Waelkens, C.
Référence Monthly notices of the Royal Astronomical Society, 464, page (1018-1028), 1609.05729
Publication Publié, 2017-01

Article révisé par les pairs

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Résumé :

We report on the discovery of a planetary companion candidate with a minimum mass M sin i = 4.6 ± 1.0 MJupiter orbiting the K2 III giant star HD 175370 (KIC 007940959). This star was a target in our programme to search for planets around a sample of 95 giant stars observed with Kepler. This detection was made possible using precise stellar radial velocity measurements of HD 175370 taken over five years and four months using the coudé echelle spectrograph of the 2-m Alfred Jensch Telescope and the fibre-fed echelle spectrograph High Efficiency and Resolution Mercator Echelle Spectrograph of the 1.2-m Mercator Telescope. Our radial velocity measurements reveal a periodic (349.5 ± 4.5 d) variation with a semi-amplitude K = 133 ± 25ms-1, superimposed on a long-term trend. A low-mass stellar companion with an orbital period of ~88 yr in a highly eccentric orbit and a planet in a Keplerian orbit with an eccentricity e = 0.22 are the most plausible explanation of the radial velocity variations. However, we cannot exclude the existence of stellar envelope pulsations as a cause for the low-amplitude radial velocity variations and only future continued monitoring of this system may answer this uncertainty. From Kepler photometry, we find that HD 175370 is most likely a low-mass red giant branch or asymptotic giant branch star.