Authors

R. F. Díaz, Universidad de Buenos AiresFollow
Xavier Delfosse, Université Grenoble AlpesFollow
Melissa J. Hobson, Aix-Marseille UniversitéFollow
Isabelle Boisse, Aix-Marseille UniversitéFollow
Nicola Astudillo-Defru, Universidad Católica de la Santísima ConcepciónFollow
Xavier Bonfils, Université Grenoble AlpesFollow
Gregory W. Henry, Tennessee State UniversityFollow
Luc Arnold, Observatoire de Haute-ProvenceFollow
François Bouchy, Observatoire astronomique de l’Université de GenèveFollow
Vincent Bourrier, Observatoire Astronomique de l’Université de GenèveFollow
Bastien Brugger, Aix-Marseille Université
Shweta Dalal, Institut d’Astrophysique de ParisFollow
Magali Deleuil, Aix-Marseille UniversitéFollow
Olivier Demangeon, Universidade do PortoFollow
F. Dolon, Aix-Marseille Université
Xavier Dumusque, Observatoire Astronomique de l’Université de Genève
Thierry Forveille, Université Grenoble AlpesFollow
Nathan Hara, Observatoire astronomique de l’Université de GenèveFollow
Guillaume Hébrard, Institut d’Astrophysique de ParisFollow
‪Flavien Kiefer, Institut d’Astrophysique de ParisFollow
Théodore Lopez, Aix-Marseille Université
‪Lucile Mignon, Université Grenoble Alpes
F. Moreau, Aix-Marseille Université
Olivier Mousis, Aix-Marseille Université
C. Moutou, Aix-Marseille UniversitéFollow
Francesco Pepe, Observatoire astronomique de l’Université de GenèveFollow
S. Perruchot, Aix-Marseille Université
Y. Richaud, Aix-Marseille Université
Alexandre Santerne, Aix-Marseille UniversitéFollow
Nuno Santos, Universidade do PortoFollow
R. Sottile, Aix-Marseille Université
Manu Stalport, Observatoire Astronomique de l’Université de Genève
Damien Ségransan, Observatoire Astronomique de l’Université de GenèveFollow
Stéphane Udry, Observatoire Astronomique de l’Université de GenèveFollow
N. Unger, Universidad de Buenos Aires
Paul A. Wilson, University of WarwickFollow

Document Type

Article

Publication Date

5-1-2019

Abstract

Periodic radial velocity variations in the nearby M-dwarf star Gl 411 are reported, based on measurements with the SOPHIE spectrograph. Current data do not allow us to distinguish between a 12.95-day period and its one-day alias at 1.08 days, but favour the former slightly. The velocity variation has an amplitude of 1.6 m s−1, making this the lowest-amplitude signal detected with SOPHIE up to now. We have performed a detailed analysis of the significance of the signal and its origin, including extensive simulations with both uncorrelated and correlated noise, representing the signal induced by stellar activity. The signal is significantly detected, and the results from all tests point to its planetary origin. Additionally, the presence of an additional acceleration in the velocity time series is suggested by the current data. On the other hand, a previously reported signal with a period of 9.9 days, detected in HIRES velocities of this star, is not recovered in the SOPHIE data. An independent analysis of the HIRES dataset also fails to unveil the 9.9-day signal. If the 12.95-day period is the real one, the amplitude of the signal detected with SOPHIE implies the presence of a planet, called Gl 411 b, with a minimum mass of around three Earth masses, orbiting its star at a distance of 0.079 AU. The planet receives about 3.5 times the insolation received by Earth, which implies an equilibrium temperature between 256 and 350 K, and makes it too hot to be in the habitable zone. At a distance of only 2.5 pc, Gl 411 b, is the third closest low-mass planet detected to date. Its proximity to Earth will permit probing its atmosphere with a combination of high-contrast imaging and high-dispersion spectroscopy in the next decade.

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