The SOPHIE search for northern extrasolar planets XV. A Warm Neptune around the M-dwarf Gl378. (arXiv:1902.05998v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Hobson_M/0/1/0/all/0/1">M. J. Hobson</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Delfosse_X/0/1/0/all/0/1">X. Delfosse</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Astudillo_Defru_N/0/1/0/all/0/1">N. Astudillo-Defru</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Boisse_I/0/1/0/all/0/1">I. Boisse</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Diaz_R/0/1/0/all/0/1">R. F. Díaz</a> (4 and 5), <a href="http://arxiv.org/find/astro-ph/1/au:+Bouchy_F/0/1/0/all/0/1">F. Bouchy</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Bonfils_X/0/1/0/all/0/1">X.Bonfils</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Forveille_T/0/1/0/all/0/1">T. Forveille</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Arnold_L/0/1/0/all/0/1">L.Arnold</a> (7), <a href="http://arxiv.org/find/astro-ph/1/au:+Borgniet_S/0/1/0/all/0/1">S. Borgniet</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Bourrier_V/0/1/0/all/0/1">V. Bourrier</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Brugger_B/0/1/0/all/0/1">B. Brugger</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Salazar_N/0/1/0/all/0/1">N. Cabrera Salazar</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Courcol_B/0/1/0/all/0/1">B. Courcol</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Dalal_S/0/1/0/all/0/1">S. Dalal</a> (8), <a href="http://arxiv.org/find/astro-ph/1/au:+Deleuil_M/0/1/0/all/0/1">M. Deleuil</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Demangeon_O/0/1/0/all/0/1">O.Demangeon</a> (9), <a href="http://arxiv.org/find/astro-ph/1/au:+Dumusque_X/0/1/0/all/0/1">X. Dumusque</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Hara_N/0/1/0/all/0/1">N. Hara</a> (6 and 11), <a href="http://arxiv.org/find/astro-ph/1/au:+Hebrard_G/0/1/0/all/0/1">G. Hébrard</a> (8 and 7), <a href="http://arxiv.org/find/astro-ph/1/au:+Kiefer_F/0/1/0/all/0/1">F. Kiefer</a> (8), <a href="http://arxiv.org/find/astro-ph/1/au:+Lopez_T/0/1/0/all/0/1">T. Lopez</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Mignon_L/0/1/0/all/0/1">L. Mignon</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Montagnier_G/0/1/0/all/0/1">G. Montagnier</a> (8 and 7), <a href="http://arxiv.org/find/astro-ph/1/au:+Mousis_O/0/1/0/all/0/1">O. Mousis</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Moutou_C/0/1/0/all/0/1">C. Moutou</a> (1 and 12), <a href="http://arxiv.org/find/astro-ph/1/au:+Pepe_F/0/1/0/all/0/1">F. Pepe</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Rey_J/0/1/0/all/0/1">J. Rey</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Santerne_A/0/1/0/all/0/1">A. Santerne</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Santos_N/0/1/0/all/0/1">N. C. Santos</a> (9 and 10), <a href="http://arxiv.org/find/astro-ph/1/au:+Stalport_M/0/1/0/all/0/1">M. Stalport</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Segransan_D/0/1/0/all/0/1">D. Ségransan</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Udry_S/0/1/0/all/0/1">S. Udry</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Wilson_P/0/1/0/all/0/1">P. A. Wilson</a> (13,14, and 8) ((1) Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France, (2) Univ. Grenoble Alpes, CNRS, IPAG, Grenoble, France, (3) Universidad de Concepción, Departamento de Astronomía, Concepción, Chile, (4) Universidad de Buenos Aires, Facultad de Ciencias Exactas y Naturales. Buenos Aires, Argentina, (5) CONICET – Universidad de Buenos Aires. Instituto de Astronomía y Física del Espacio (IAFE). Buenos Aires, Argentina, (6) Observatoire Astronomique de l'Université de Genève, Versoix, Switzerland, (7) Observatoire de Haute-Provence, CNRS, Aix Marseille Université, Institut Pythéas UMS 3470, Saint-Michel-l'Observatoire, France, (8) Institut d'Astrophysique de Paris, UMR7095 CNRS, Université Pierre & Marie Curie, Paris, France, (9) Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Porto, Portugal, (10) Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, Porto, Portugal, (11) ASD/IMCCE, CNRS-UMR8028, Observatoire de Paris, PSL, UPMC, Paris, France, (12) Canada-France-Hawaii Telescope Corporation, Kamuela, HI, USA, (13) Department of Physics, University of Warwick, Coventry, UK, (14) Centre for Exoplanets and Habitability, University of Warwick, Coventry CV4 7AL, UK)
We present the detection of a Warm Neptune orbiting the M-dwarf Gl378, using
radial velocity measurements obtained with the SOPHIE spectrograph at the
Observatoire de Haute-Provence. The star was observed in the context of the
SOPHIE exoplanets consortium’s subprogramme dedicated to finding planets around
M-dwarfs. Gl378 is an M1 star, of solar metallicity, at a distance of 14.96 pc.
The single planet detected, Gl378 b, has a minimum mass of 13.02 $rm
M_{Earth}$ and an orbital period of 3.82 days, which place it at the lower
boundary of the Hot Neptune desert. As one of only a few such planets around
M-dwarfs, Gl378 b provides important clues to the evolutionary history of these
close-in planets. In particular, the eccentricity of 0.1 may point to a
high-eccentricity migration. The planet may also have lost part of its envelope
due to irradiation.
We present the detection of a Warm Neptune orbiting the M-dwarf Gl378, using
radial velocity measurements obtained with the SOPHIE spectrograph at the
Observatoire de Haute-Provence. The star was observed in the context of the
SOPHIE exoplanets consortium’s subprogramme dedicated to finding planets around
M-dwarfs. Gl378 is an M1 star, of solar metallicity, at a distance of 14.96 pc.
The single planet detected, Gl378 b, has a minimum mass of 13.02 $rm
M_{Earth}$ and an orbital period of 3.82 days, which place it at the lower
boundary of the Hot Neptune desert. As one of only a few such planets around
M-dwarfs, Gl378 b provides important clues to the evolutionary history of these
close-in planets. In particular, the eccentricity of 0.1 may point to a
high-eccentricity migration. The planet may also have lost part of its envelope
due to irradiation.
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