TY - JOUR
T1 - A low-mass planet candidate orbiting Proxima Centauri at a distance of 1.5 AU
AU - Damasso, M.
AU - Del Sordo, Fabio
AU - Anglada Escude, Guillem
AU - Giacobbe, P.
AU - Sozzetti, Alessandro
AU - Morbidelli, L.
AU - Pojmański, G.
AU - Barbato, Domenico
AU - Butler, R. P.
AU - Jones, Hugh
AU - Hambsch, Franz-Josef
AU - Jenkins, James S.
AU - Lopez-Gonzalez, Maria J.
AU - Morales, Nicolas
AU - Peña Rojas, Pablo A.
AU - Rodriguez-Lopez, Cristina
AU - Rodriguez, Eloy
AU - Amado, Pedro J.
AU - Anglada, Guillem
AU - Feng, F.
AU - Gómez, Jose F.
N1 - Copyright © 2020 The Authors, some rights reserved; exclusive licensee American Association for the Advancement of Science. No claim to original U.S. Government Works. Distributed under a Creative Commons Attribution NonCommercial License 4.0 (CC BY-NC).
PY - 2020/1/15
Y1 - 2020/1/15
N2 - Our nearest neighbor, Proxima Centauri, hosts a temperate terrestrial planet. We detected in radial velocities evidence of a possible second planet with minimum mass m c sin i c = 5.8 ± 1.9 M ⊕ and orbital period P c = 5.21 - 0.22 + 0.26 years. The analysis of photometric data and spectro-scopic activity diagnostics does not explain the signal in terms of a stellar activity cycle, but follow-up is required in the coming years for confirming its planetary origin. We show that the existence of the planet can be ascertained, and its true mass can be determined with high accuracy, by combining Gaia astrometry and radial velocities. Proxima c could become a prime target for follow-up and characterization with next-generation direct imaging instrumentation due to the large maximum angular separation of ~1 arc second from the parent star. The candidate planet represents a challenge for the models of super-Earth formation and evolution.
AB - Our nearest neighbor, Proxima Centauri, hosts a temperate terrestrial planet. We detected in radial velocities evidence of a possible second planet with minimum mass m c sin i c = 5.8 ± 1.9 M ⊕ and orbital period P c = 5.21 - 0.22 + 0.26 years. The analysis of photometric data and spectro-scopic activity diagnostics does not explain the signal in terms of a stellar activity cycle, but follow-up is required in the coming years for confirming its planetary origin. We show that the existence of the planet can be ascertained, and its true mass can be determined with high accuracy, by combining Gaia astrometry and radial velocities. Proxima c could become a prime target for follow-up and characterization with next-generation direct imaging instrumentation due to the large maximum angular separation of ~1 arc second from the parent star. The candidate planet represents a challenge for the models of super-Earth formation and evolution.
UR - http://www.scopus.com/inward/record.url?scp=85078690983&partnerID=8YFLogxK
U2 - 10.1126/sciadv.aax7467
DO - 10.1126/sciadv.aax7467
M3 - Article
C2 - 31998838
VL - 6
JO - Science Advances
JF - Science Advances
IS - 3
M1 - eaax7467
ER -