Detection and Doppler monitoring of K2-285 (EPIC 246471491), a system of four transiting planets smaller than Neptune

Research output: Contribution to journal/Conference contribution in journal/Contribution to newspaperJournal articleResearchpeer-review

  • E. Palle, Instituto de Astrofísica de Canarias, La Laguna University
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  • G. Nowak, Instituto de Astrofísica de Canarias, La Laguna University
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  • R. Luque, Instituto de Astrofísica de Canarias, La Laguna University
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  • D. Hidalgo, Instituto de Astrofísica de Canarias, La Laguna University
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  • O. Barragán, Università degli Studi di Torino
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  • J. Prieto-Arranz, Instituto de Astrofísica de Canarias, La Laguna University
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  • T. Hirano, Tokyo Institute of Technology
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  • M. Fridlund, Leiden Observatory Research Institute, Chalmers University of Technology, Onsala Space Observatory
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  • D. Gandolfi, Università degli Studi di Torino
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  • J. Livingston, University Tokyo
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  • F. Dai, Princeton University, Princeton, NJ, Massachusetts Institute of Technology
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  • J. C. Morales, Instituto de Ciencias del Espacio (ICE-CSIC/IEEC), Institut d'Estudis Espacials de Catalunya
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  • M. Lafarga, Instituto de Ciencias del Espacio (ICE-CSIC/IEEC), Institut d'Estudis Espacials de Catalunya
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  • S. Albrecht
  • R. Alonso, Instituto de Astrofísica de Canarias, La Laguna University
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  • P. J. Amado, Instituto de Astrofysica de Andalucia - CSIC
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  • J. A. Caballero, Centro de Astrobiología (CSIC-INTA)
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  • J. Cabrera, Deutsches Zentrum für Luft- und Raumfahrt, Institut für Physik der Atmosphäre
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  • W. D. Cochran, School of Business and Economics
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  • Sz Csizmadia, Deutsches Zentrum für Luft- und Raumfahrt, Institut für Physik der Atmosphäre
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  • H. Deeg, Instituto de Astrofísica de Canarias, La Laguna University
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  • Ph Eigmüller, Deutsches Zentrum für Luft- und Raumfahrt, Institut für Physik der Atmosphäre, Technical University of Berlin
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  • M. Endl, University of Texas, Austin, Texas
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  • A. Erikson, Deutsches Zentrum für Luft- und Raumfahrt, Institut für Physik der Atmosphäre
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  • A. Fukui, Instituto de Astrofísica de Canarias, National Astronomical Observatory of Japan
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  • E. W. Guenther, Thüringer Landessternwarte Tautenburg (TLS)
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  • S. Grziwa, Universitat zu Koln
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  • A. P. Hatzes, Thüringer Landessternwarte Tautenburg (TLS)
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  • J. Korth, Universitat zu Koln
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  • M. Kürster, Max-Planck-Institut für Astronomie, Königstuhl 17, 69117, Heidelberg, Germany
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  • M. Kuzuhara, NINS, National Astronomical Observatory of Japan
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  • P. Montañes Rodríguez, Instituto de Astrofísica de Canarias, La Laguna University
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  • F. Murgas, Instituto de Astrofísica de Canarias, La Laguna University
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  • N. Narita, Instituto de Astrofísica de Canarias, NINS, National Astronomical Observatory of Japan
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  • D. Nespral, Instituto de Astrofísica de Canarias, La Laguna University
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  • M. Pätzold, Universitat zu Koln
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  • C. M. Persson, Chalmers University of Technology, Onsala Space Observatory
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  • A. Quirrenbach, Landessternwarte Heidelberg
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  • H. Rauer, Deutsches Zentrum für Luft- und Raumfahrt, Institut für Physik der Atmosphäre, School of Business and Economics, Technical University of Berlin
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  • S. Redfield, Wesleyan University Middletown
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  • A. Reiners, University of Göttingen
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  • I. Ribas, Instituto de Ciencias del Espacio (ICE-CSIC/IEEC), Institut d'Estudis Espacials de Catalunya
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  • A. M.S. Smith, Institute for Planetary Research, DLR, Deutsches Zentrum für Luft- und Raumfahrt, Institut für Physik der Atmosphäre
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  • V. Van Eylen, Leiden Observatory Research Institute
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  • J. N. Winn, Princeton University, Princeton, NJ
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  • M. Zechmeister, University of Göttingen

Context. The Kepler extended mission, also known as K2, has provided the community with a wealth of planetary candidates that orbit stars typically much brighter than the targets of the original mission. These planet candidates are suitable for further spectroscopic follow-up and precise mass determinations, leading ultimately to the construction of empirical mass-radius diagrams. Particularly interesting is to constrain the properties of planets that are between Earth and Neptune in size, the most abundant type of planet orbiting Sun-like stars with periods of less than a few years. Aims. Among many other K2 candidates, we discovered a multi-planetary system around EPIC 246471491, referred to henceforth as K2-285, which contains four planets, ranging in size from twice the size of Earth to nearly the size of Neptune. We aim here at confirming their planetary nature and characterizing the properties of this system. Methods. We measure the mass of the planets of the K2-285 system by means of precise radial-velocity measurements using the CARMENES spectrograph and the HARPS-N spectrograph. Results. With our data we are able to determine the mass of the two inner planets of the system with a precision better than 15%, and place upper limits on the masses of the two outer planets. Conclusions. We find that K2-285b has a mass of Mb = 9.68-1.37+1.21 M· and a radius of Rb = 2.59-0.06+0.06 R·, yielding a mean density of ρb = 3.07-0.45+0.45 g cm-3, while K2-285c has a mass of Mc = 15.68-2.13+2.28 M·, radius of Rc = 3.53-0.08+0.08 R·, and a mean density of ρc = 1.95-0.28+0.32 g cm-3. For K2-285d (Rd = 2.48-0.06+0.06 R·) and K2-285e (Re = 1.95-0.05+0.05 R·), the upper limits for the masses are 6.5 M· and 10.7 M·, respectively. The system is thus composed of an (almost) Neptune-twin planet (in mass and radius), two sub-Neptunes with very different densities and presumably bulk composition, and a fourth planet in the outermost orbit that resides right in the middle of the super-Earth/sub-Neptune radius gap. Future comparative planetology studies of this system would provide useful insights into planetary formation, and also a good test of atmospheric escape and evolution theories.

Original languageEnglish
Article numberA41
JournalAstronomy and Astrophysics
Volume623
Number of pages10
ISSN0004-6361
DOIs
Publication statusPublished - 2019

    Research areas

  • Planetary systems, Planets and satellites: atmospheres, Planets and satellites: detection, Planets and satellites: dynamical evolution and stability, Planets and satellites: fundamental parameters

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