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Anders Bo Justesen

TESS's first planet. A super-Earth transiting the naked-eye star π Mensae

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  • D. Gandolfi, Dipartimento di Fisica, Università degli Studi di Torino, Via Pietro Giuria 1, 10125, Torino, Italy davide.gandolfi@unito.it
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  • O. Barragán, Dipartimento di Fisica, Università degli Studi di Torino, Via Pietro Giuria 1, 10125, Torino, Italy
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  • J. H. Livingston, Department of Astronomy, Graduate School of Science, The University of Tokyo, Hongo 7-3-1, Bunkyo-ku, Tokyo, 113-0033, Japan
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  • M. Fridlund, Leiden Observatory, Leiden University, P.O. Box 9513, NL-2300 RA Leiden, The Netherlands
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  • A. B. Justesen
  • S. Redfield, Astronomy Department and Van Vleck Observatory, Wesleyan University, Middletown, CT 06459, USA pniraula@wesleyan.edu 0000-0002-8052-3893
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  • L. Fossati, Space Research Institute, Austrian Academy of Sciences, Schmiedlstrasse 6, 8041, Graz, Austria
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  • S. Mathur, Instituto de Astrofísica de Canarias
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  • S. Grziwa, Rheinisches Institut für Umweltforschung, Abteilung Planetenforschung an der Universität zu Köln, Aachener Strasse 209, 50931, Köln, Germany
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  • J. Cabrera, Institute of Planetary Research, German Aerospace Center, Rutherfordstrasse 2, 12489, Berlin, Germany
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  • R. A. García, Université Paris Diderot, AIM, Sorbonne Paris Cité, CEA, CNRS, F-91191 Gif-sur-Yvette, France
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  • C. M. Persson, Department of Space, Earth and Environment, Chalmers University of Technology, Onsala Space Observatory, SE-439 92 Onsala, Sweden 0000-0003-2180-9936
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  • V. Van Eylen, Department of Astrophysical Sciences, Princeton University, 4 Ivy Lane, Princeton, NJ 08544, USA
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  • A. P. Hatzes, Thüringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenberg, Germany
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  • D. Hidalgo, Instituto de Astrofísica de Canarias
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  • S. Albrecht
  • L. Bugnet, Université Paris Diderot, AIM, Sorbonne Paris Cité, CEA, CNRS, F-91191 Gif-sur-Yvette, France
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  • W. D. Cochran, Department of Astronomy and McDonald Observatory, University of Texas at Austin, 2515 Speedway, Stop C1400, Austin, TX 78712, USA
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  • Sz. Csizmadia, Institute of Planetary Research, German Aerospace Center, Rutherfordstrasse 2, 12489, Berlin, Germany
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  • H. Deeg, Instituto de Astrofísica de Canarias
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  • Ph. Eigmüller, Institute of Planetary Research, German Aerospace Center, Rutherfordstrasse 2, 12489, Berlin, Germany
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  • M. Endl, Department of Astronomy and McDonald Observatory, University of Texas at Austin, 2515 Speedway, Stop C1400, Austin, TX 78712, USA
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  • A. Erikson, Institute of Planetary Research, German Aerospace Center, Rutherfordstrasse 2, 12489, Berlin, Germany
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  • M. Esposito, Thüringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenberg, Germany
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  • E. Guenther, Thüringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenberg, Germany
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  • J. Korth, Rheinisches Institut für Umweltforschung, Abteilung Planetenforschung an der Universität zu Köln, Aachener Strasse 209, 50931, Köln, Germany
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  • R. Luque, Instituto de Astrofísica de Canarias
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  • P. Montañes Rodríguez, Instituto de Astrofísica de Canarias
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  • D. Nespral, Instituto de Astrofísica de Canarias
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  • G. Nowak, Instituto de Astrofísica de Canarias
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  • M. Pätzold, Rheinisches Institut für Umweltforschung, Abteilung Planetenforschung an der Universität zu Köln, Aachener Strasse 209, 50931, Köln, Germany
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  • J. Prieto-Arranz, Instituto de Astrofísica de Canarias
We report on the confirmation and mass determination of π Men c, the first transiting planet discovered by NASA's TESS space mission. π Men is a naked-eye (V = 5.65 mag), quiet G0 V star that was previously known to host a sub-stellar companion (π Men b) on a longperiod (Porb = 2091 days), eccentric (e = 0.64) orbit. Using TESS time-series photometry, combined with Gaia data, published UCLES at AAT Doppler measurements, and archival HARPS at ESO-3.6m radial velocities, we found that π Men c is a close-in planet with an orbital period of Porb = 6.27 days, a mass of Mc = 4.52 ± 0.81 M⊕, and a radius of Rc = 2.06 ± 0.03 R⊕. Based on the planet's orbital period and size, π Men c is a super-Earth located at, or close to, the radius gap, while its mass and bulk density suggest it may have held on to a significant atmosphere. Because of the brightness of the host star, this system is highly suitable for a wide range of further studies to characterize the planetary atmosphere and dynamical properties. We also performed an asteroseismic analysis of the TESS data and detected a hint of power excess consistent with the seismic values expected for this star, although this result depends on the photometric aperture used to extract the light curve. This marginal detection is expected from pre-launch simulations hinting at the asteroseismic potential of the TESS mission for longer, multi-sector observations and/or for more evolved bright stars. The entire RV data (Tables A.1, A.3 and full Table A.2) are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/619/L10
OriginalsprogEngelsk
ArtikelnummerL10
TidsskriftAstronomy & Astrophysics
Vol/bind619
Antal sider10
ISSN0004-6361
DOI
StatusUdgivet - 1 nov. 2018

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