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        A low-mass planet candidate orbiting Proxima Centauri at a distance of 1.5 AU

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        Author
        Damasso, M.
        Del Sordo, Fabio
        Anglada Escude, Guillem
        Giacobbe, P.
        Sozzetti, Alessandro
        Morbidelli, L.
        Pojmański, G.
        Barbato, Domenico
        Butler, R. P.
        Jones, Hugh
        Hambsch, Franz-Josef
        Jenkins, James S.
        Lopez-Gonzalez, Maria J.
        Morales, Nicolas
        Peña Rojas, Pablo A.
        Rodriguez-Lopez, Cristina
        Rodriguez, Eloy
        Amado, Pedro J.
        Anglada, Guillem
        Feng, F.
        Gómez, Jose F.
        Attention
        2299/22125
        Abstract
        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.
        Publication date
        2020-01-15
        Published in
        Science Advances
        Published version
        https://doi.org/10.1126/sciadv.aax7467
        License
        http://creativecommons.org/licenses/by-nc/4.0/
        Other links
        http://hdl.handle.net/2299/22125
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