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Title

The CARMENES search for exoplanets around M dwarfs: The enigmatic planetary system GJ 4276: One eccentric planet or two planets in a 2:1 resonance

AuthorsNagel, E.; Czesla, S.; Schmitt, J.H.M.M.; Dreizler, S.; Anglada-Escude, G.; Rodríguez Martínez, Eloy ; Ribas, Ignasi ; Reiners, A.; Quirrenbach, A.; Amado, Pedro J. ; Caballero, J.A.; Aceituno, Francisco José ; Bejar, V.J.S.; Cortes-Contreras, M.; Gonzalez-Cuesta, L.; Guenther, E.W.; Henning, T.; Jeffers, S.V.; Kaminski, A.; Kürster, M.; Lafarga, M.; López González, Maria J. ; Montes, D.; Morales, J.C.; Passegger, V.M.; Rodríguez-López, Cristina ; Schweitzer, A.; Zechmeister, M.
KeywordsTechniques: radial velocities
Methods: observational
Methods: data analysis
Stars: low-mass
Planetary systems
Stars: individual: GJ 4276
Issue Date2019
PublisherEDP Sciences
CitationAstronomy and Astrophysics 622:A153 (2019)
AbstractWe report the detection of a Neptune-mass exoplanet around the M4.0 dwarf GJ 4276 (G 232-070) based on radial velocity (RV) observations obtained with the CARMENES spectrograph. The RV variations of GJ 4276 are best explained by the presence of a planetary companion that has a minimum mass of mb sin i 16 M on a Pb = 13.35 day orbit. The analysis of the activity indicators and spectral diagnostics exclude stellar induced RV perturbations and prove the planetary interpretation of the RV signal. We show that a circular single-planet solution can be excluded by means of a likelihood ratio test. Instead, we find that the RV variations can be explained either by an eccentric orbit or interpreted as a pair of planets on circular orbits near a period ratio of 2:1. Although the eccentric single-planet solution is slightly preferred, our statistical analysis indicates that none of these two scenarios can be rejected with high confidence using the RV time series obtained so far. Based on the eccentric interpretation, we find that GJ 4276 b is the most eccentric (eb = 0.37) exoplanet around an M dwarf with such a short orbital period known today.© ESO 2019.
URIhttp://hdl.handle.net/10261/179531
Identifiersdoi: 10.1051/0004-6361/201834569
issn: 1432-0746
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