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Title:
A candidate super-Earth planet orbiting near the snow line of Barnard's star
Authors:
Ribas, I.; Tuomi, M.; Reiners, A.; Butler, R. P.; Morales, J. C.; Perger, M.; Dreizler, S.; Rodríguez-López, C.; González Hernández, J. I.; Rosich, A.; Feng, F.; Trifonov, T.; Vogt, S. S.; Caballero, J. A.; Hatzes, A.; Herrero, E.; Jeffers, S. V.; Lafarga, M.; Murgas, F.; Nelson, R. P.; Rodríguez, E.; Strachan, J. B. P.; Tal-Or, L.; Teske, J.; Toledo-Padrón, B.; Zechmeister, M.; Quirrenbach, A.; Amado, P. J.; Azzaro, M.; Béjar, V. J. S.; Barnes, J. R.; Berdiñas, Z. M.; Burt, J.; Coleman, G.; Cortés-Contreras, M.; Crane, J.; Engle, S. G.; Guinan, E. F.; Haswell, C. A.; Henning, Th.; Holden, B.; Jenkins, J.; Jones, H. R. A.; Kaminski, A.; Kiraga, M.; Kürster, M.; Lee, M. H.; López-González, M. J.; Montes, D.; Morin, J.; Ofir, A.; Pallé, E.; Rebolo, R.; Reffert, S.; Schweitzer, A.; Seifert, W.; Shectman, S. A.; Staab, D.; Street, R. A.; Suárez Mascareño, A.; Tsapras, Y.; Wang, S. X.; Anglada-Escudé, G.
Affiliation:
AA(Institut de Ciències de l'Espai (ICE, CSIC), Campus UAB, Bellaterra, Spain; Institut d'Estudis Espacials de Catalunya (IEEC), Barcelona, Spain), AB(Centre for Astrophysics Research, University of Hertfordshire, Hatfield, UK), AC(Institut für Astrophysik Göttingen, Georg-August-Universität Göttingen, Göttingen, Germany), AD(Department of Terrestrial Magnetism, Carnegie Institution for Science, Washington, DC, USA), AE(Institut de Ciències de l'Espai (ICE, CSIC), Campus UAB, Bellaterra, Spain; Institut d'Estudis Espacials de Catalunya (IEEC), Barcelona, Spain), AF(Institut de Ciències de l'Espai (ICE, CSIC), Campus UAB, Bellaterra, Spain; Institut d'Estudis Espacials de Catalunya (IEEC), Barcelona, Spain), AG(Institut für Astrophysik Göttingen, Georg-August-Universität Göttingen, Göttingen, Germany), AH(Instituto de Astrofísica de Andalucía (IAA, CSIC), Granada, Spain), AI(Instituto de Astrofísica de Canarias (IAC), La Laguna, Spain; Universidad de La Laguna (ULL), Departamento de Astrofísica, La Laguna, Spain), AJ(Institut de Ciències de l'Espai (ICE, CSIC), Campus UAB, Bellaterra, Spain; Institut d'Estudis Espacials de Catalunya (IEEC), Barcelona, Spain), AK(Centre for Astrophysics Research, University of Hertfordshire, Hatfield, UK), AL(Max-Planck-Institut für Astronomie, Heidelberg, Germany), AM(UCO/Lick Observatory, University of California at Santa Cruz, Santa Cruz, CA, USA), AN(Centro de Astrobiología, CSIC-INTA, ESAC, Villanueva de la Cañada, Spain), AO(Thüringer Landessternwarte, Tautenburg, Germany), AP(Institut de Ciències de l'Espai (ICE, CSIC), Campus UAB, Bellaterra, Spain; Institut d'Estudis Espacials de Catalunya (IEEC), Barcelona, Spain), AQ(Institut für Astrophysik Göttingen, Georg-August-Universität Göttingen, Göttingen, Germany), AR(Institut de Ciències de l'Espai (ICE, CSIC), Campus UAB, Bellaterra, Spain; Institut d'Estudis Espacials de Catalunya (IEEC), Barcelona, Spain), AS(Instituto de Astrofísica de Canarias (IAC), La Laguna, Spain; Universidad de La Laguna (ULL), Departamento de Astrofísica, La Laguna, Spain), AT(School of Physics and Astronomy, Queen Mary University of London, London, UK), AU(Instituto de Astrofísica de Andalucía (IAA, CSIC), Granada, Spain), AV(School of Physics and Astronomy, Queen Mary University of London, London, UK), AW(Institut für Astrophysik Göttingen, Georg-August-Universität Göttingen, Göttingen, Germany; School of Geosciences, Raymond and Beverly Sackler Faculty of Exact Sciences, Tel-Aviv University, Tel Aviv, Israel), AX(Department of Terrestrial Magnetism, Carnegie Institution for Science, Washington, DC, USA), AY(Instituto de Astrofísica de Canarias (IAC), La Laguna, Spain; Universidad de La Laguna (ULL), Departamento de Astrofísica, La Laguna, Spain), AZ(Institut für Astrophysik Göttingen, Georg-August-Universität Göttingen, Göttingen, Germany), BA(Landessternwarte, Zentrum für Astronomie der Universität Heidelberg, Heidelberg, Germany), BB(Instituto de Astrofísica de Andalucía (IAA, CSIC), Granada, Spain), BC(Centro Astronómico Hispano-Alemán (CSIC-MPG), Observatorio Astronómico de Calar Alto, Gérgal, Spain), BD(Instituto de Astrofísica de Canarias (IAC), La Laguna, Spain; Universidad de La Laguna (ULL), Departamento de Astrofísica, La Laguna, Spain), BE(School of Physical Sciences, The Open University, Milton Keynes, UK), BF(Departamento de Astronomía, Universidad de Chile, Santiago, Chile), BG(Kavli Institute, Massachusetts Institute of Technology, Cambridge, MA, USA), BH(Physikalisches Institut, Universität Bern, Bern, Switzerland), BI(Centro de Astrobiología, CSIC-INTA, ESAC, Villanueva de la Cañada, Spain), BJ(The Observatories, Carnegie Institution for Science, Pasadena, CA, USA), BK(Department of Astrophysics and Planetary Science, Villanova University, Villanova, PA, USA), BL(Department of Astrophysics and Planetary Science, Villanova University, Villanova, PA, USA), BM(School of Physical Sciences, The Open University, Milton Keynes, UK), BN(Max-Planck-Institut für Astronomie, Heidelberg, Germany), BO(UCO/Lick Observatory, University of California at Santa Cruz, Santa Cruz, CA, USA), BP(Departamento de Astronomía, Universidad de Chile, Santiago, Chile), BQ(Centre for Astrophysics Research, University of Hertfordshire, Hatfield, UK), BR(Landessternwarte, Zentrum für Astronomie der Universität Heidelberg, Heidelberg, Germany), BS(Warsaw University Observatory, Warsaw, Poland), BT(Max-Planck-Institut für Astronomie, Heidelberg, Germany), BU(Department of Earth Sciences and Department of Physics, The University of Hong Kong, Pok Fu Lam, Hong Kong), BV(Instituto de Astrofísica de Andalucía (IAA, CSIC), Granada, Spain), BW(Departamento de Física de la Tierra Astronomía y Astrofísica and UPARCOS-UCM (Unidad de Física de Partículas y del Cosmos de la UCM), Facultad de Ciencias Físicas, Universidad Complutense de Madrid, Madrid, Spain), BX(Laboratoire Univers et Particules de Montpellier, Université de Montpellier, CNRS, Montpellier, France), BY(Department of Earth and Planetary Sciences, Weizmann Institute of Science, Rehovot, Israel), BZ(Instituto de Astrofísica de Canarias (IAC), La Laguna, Spain; Universidad de La Laguna (ULL), Departamento de Astrofísica, La Laguna, Spain), CA(Instituto de Astrofísica de Canarias (IAC), La Laguna, Spain; Universidad de La Laguna (ULL), Departamento de Astrofísica, La Laguna, Spain; Consejo Superior de Investigaciones Científicas (CSIC), Madrid, Spain), CB(Landessternwarte, Zentrum für Astronomie der Universität Heidelberg, Heidelberg, Germany), CC(Hamburger Sternwarte, Universität Hamburg, Hamburg, Germany), CD(Landessternwarte, Zentrum für Astronomie der Universität Heidelberg, Heidelberg, Germany), CE(The Observatories, Carnegie Institution for Science, Pasadena, CA, USA), CF(School of Physical Sciences, The Open University, Milton Keynes, UK), CG(Las Cumbres Observatory Global Telescope Network, Goleta, CA, USA), CH(Instituto de Astrofísica de Canarias (IAC), La Laguna, Spain; Observatoire Astronomique de l'Université de Genève, Versoix, Switzerland), CI(Zentrum für Astronomie der Universität Heidelberg, Astronomisches Rechen-Institut, Heidelberg, Germany), CJ(Department of Terrestrial Magnetism, Carnegie Institution for Science, Washington, DC, USA), CK(Instituto de Astrofísica de Andalucía (IAA, CSIC), Granada, Spain; School of Physics and Astronomy, Queen Mary University of London, London, UK)
Publication:
Nature, Volume 563, Issue 7731, p.365-368 (Nature Homepage)
Publication Date:
11/2018
Origin:
NATURE
DOI:
10.1038/s41586-018-0677-y
Bibliographic Code:
2018Natur.563..365R

Abstract

Barnard's star is a red dwarf, and has the largest proper motion (apparent motion across the sky) of all known stars. At a distance of 1.8 parsecs1, it is the closest single star to the Sun; only the three stars in the alpha Centauri system are closer. Barnard's star is also among the least magnetically active red dwarfs known2,3 and has an estimated age older than the Solar System. Its properties make it a prime target for planetary searches; various techniques with different sensitivity limits have been used previously, including radial-velocity imaging4-6, astrometry7,8 and direct imaging9, but all ultimately led to negative or null results. Here we combine numerous measurements from high-precision radial-velocity instruments, revealing the presence of a low-amplitude periodic signal with a period of 233 days. Independent photometric and spectroscopic monitoring, as well as an analysis of instrumental systematic effects, suggest that this signal is best explained as arising from a planetary companion. The candidate planet around Barnard's star is a cold super-Earth, with a minimum mass of 3.2 times that of Earth, orbiting near its snow line (the minimum distance from the star at which volatile compounds could condense). The combination of all radial-velocity datasets spanning 20 years of measurements additionally reveals a long-term modulation that could arise from a stellar magnetic-activity cycle or from a more distant planetary object. Because of its proximity to the Sun, the candidate planet has a maximum angular separation of 220 milliarcseconds from Barnard's star, making it an excellent target for direct imaging and astrometric observations in the future.

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