The HARPS search for southern extra-solar planets - XXXI. The M-dwarf sample
Xavier Bonfils,X. Delfosse,Stéphane Udry,T. Forveille,Michel Mayor,C. Perrier,François Bouchy,Michaël Gillon,Christophe Lovis,Francesco Pepe,Didier Queloz,Nuno C. Santos,Damien Ségransan,Jean-Loup Bertaux +13 more
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In this paper, the authors used a fraction of the guaranteed time on the ESO/HARPS spectrograph to estimate the radial velocities of 102 southern nearby M dwarfs, and then applied systematic searches for long-term trends, periodic signals, and Keplerian orbits.Abstract:
Searching for planets around stars with different masses helps us to assess the outcome of planetary formation for different initial conditions. The low-mass M dwarfs are also the most frequent stars in our Galaxy and potentially therefore, the most frequent planet hosts. Aims. We present observations of 102 southern nearby M dwarfs, using a fraction of our guaranteed time on the ESO/HARPS spectrograph. We observed for 460 h and gathered 1965 precise (~1-3 m/s) radial velocities (RVs), spanning the period from Feb. 11, 2003 to Apr. 1, 2009. Methods. For each star observed, we derive a time series and its precision as well as its variability. We apply systematic searches for long-term trends, periodic signals, and Keplerian orbits (from one to four planets). We analyze the subset of stars with detected signals and apply several diagnostics to discriminate whether the observed Doppler shifts are caused by either stellar surface inhomogeneities or the radial pull of orbiting planets. To prepare for the statistical view of our survey, we also compute the limits on possible unseen signals, and derive a first estimate of the frequency of planets orbiting M dwarfs. Results. We recover the planetary signals of 9 planets announced by our group (Gl 176 b, Gl 581 b, c, d & e, Gl 674 b, Gl 433 b, Gl 667C b, and Gl 667C c). We present radial velocities confirming that GJ 849 hosts a Jupiter-mass planet, plus a long-term radial-velocity variation. We also present RVs that precise the planetary mass and period of Gl 832b. We detect long-term RV changes for Gl 367, Gl 680, and Gl 880, which are indicative of yet unknown long-period companions. We identify candidate signals in the radial-velocity time series of 11 other M dwarfs. Spectral diagnostics and/or photometric observations demonstrate however that these signals are most probably caused by stellar surface inhomogeneities. Finally, we find that our survey is sensitive to a few Earth-mass planets for periods up to several hundred days. We derive a first estimate of the occurrence of M-dwarf planets as a function of their minimum mass and orbital period. In particular, we find that giant planets (msini = 100 − 1000 M⊕) have a low frequency (e.g. f ≲ 1% for P = 1 − 10 d and f = 0.02+0.03-0.01 for P = 10 − 100 d), whereas super-Earths (msini = 1 − 10 M⊕) are likely very abundant (f = 0.36+0.25-0.10 for P = 1 − 10 d and f = 0.52+0.50-0.16 for P = 10 − 100 d). We also obtained η⊕ = 0.41+0.54-0.13, which is the frequency of habitable planets orbiting M dwarfs (1 ≤ msini ≤ 10 M⊕). For the first time, η⊕ is a direct measure and not a number extrapolated from the statistics of more massive and/or shorter-period planets.read more
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A terrestrial planet candidate in a temperate orbit around Proxima Centauri
Guillem Anglada-Escudé,Pedro J. Amado,John R. Barnes,Z. M. Berdiñas,R. Paul Butler,Gavin A. L. Coleman,Ignacio de la Cueva,Stefan Dreizler,Michael Endl,Benjamin Giesers,Sandra V. Jeffers,James S. Jenkins,Hugh R. A. Jones,Marcin Kiraga,Martin Kürster,Marίa J. López-González,Christopher Marvin,Nicolás Morales,Julien Morin,Richard P. Nelson,Jose Luis Ortiz,Aviv Ofir,Sijme-Jan Paardekooper,Ansgar Reiners,E. Rodriguez,Cristina Rodrίguez-López,L. F. Sarmiento,J. B. P. Strachan,Yiannis Tsapras,Mikko Tuomi,Mathias Zechmeister +30 more
TL;DR: Observations reveal the presence of a small planet with a minimum mass of about 1.3 Earth masses orbiting Proxima with a period of approximately 11.2 days at a semi-major-axis distance of around 0.05 astronomical units.
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The Occurrence of Potentially Habitable Planets Orbiting M Dwarfs Estimated from the Full Kepler Dataset and an Empirical Measurement of the Detection Sensitivity
TL;DR: In this article, the authors presented an improved estimate of the occurrence rate of small planets orbiting small stars by searching the full four-year Kepler data set for transiting planets using their own planet detection pipeline and conducting transit injection and recovery simulations to empirically measure the search completeness of their pipeline.
Journal ArticleDOI
The PLATO 2.0 mission
Heike Rauer,Heike Rauer,C. Catala,Conny Aerts,Thierry Appourchaux,Willy Benz,Alexis Brandeker,Jørgen Christensen-Dalsgaard,Magali Deleuil,Laurent Gizon,Laurent Gizon,M. J. Goupil,Manuel Güdel,Eduardo Janot-Pacheco,M. Mas-Hesse,Isabella Pagano,Giampaolo Piotto,Don Pollacco,Ċ. Santos,Andrew Smith,Juan Carlos Suárez,Róbert Szabó,Stéphane Udry,V. Adibekyan,Yann Alibert,J. M. Almenara,Pau Amaro-Seoane,M. Ammler-von Eiff,Martin Asplund,E. Antonello,Sydney A. Barnes,Frédéric Baudin,K. Belkacem,Maria Bergemann,G. Bihain,Aaron C. Birch,Xavier Bonfils,Isabelle Boisse,Aldo S. Bonomo,Francesco Borsa,I. M. Brandão,Enzo Brocato,S. Brun,Matthew R. Burleigh,R. Burston,Juan Cabrera,Santi Cassisi,William J. Chaplin,Stéphane Charpinet,Cristina Chiappini,Ross P. Church,Sz. Csizmadia,Margarida S. Cunha,Mario Damasso,Mario Damasso,Melvyn B. Davies,Hans J. Deeg,Rodrigo F. Díaz,Stefan Dreizler,C. Dreyer,C. Dreyer,P. Eggenberger,David Ehrenreich,Philipp Eigmüller,Anders Erikson,Robert Farmer,Sofia Feltzing,F. De Oliveira Fialho,Pedro Figueira,T. Forveille,Malcolm Fridlund,Rafael A. García,Paolo Giommi,G. Giuffrida,G. Giuffrida,M. Godolt,J. Gomes da Silva,T. Granzer,John Lee Grenfell,A. Grotsch-Noels,E. Günther,Carole A. Haswell,A. P. Hatzes,Guillaume Hébrard,Saskia Hekker,Saskia Hekker,Ravit Helled,Kevin Heng,Jon M. Jenkins,Anders Johansen,Maxim L. Khodachenko,Kristina G. Kislyakova,Wilhelm Kley,Ulrich Kolb,Natalie A. Krivova,Friedrich Kupka,Helmut Lammer,Antonino F. Lanza,Yveline Lebreton,Demetrio Magrin,P. Marcos-Arenal,P. M. Marrese,P. M. Marrese,J. P. Marques,J. H. C. Martins,S. Mathis,Savita Mathur,S. Messina,Andrea Miglio,Josefina Montalbán,M. Montalto,Mário J. P. F. G. Monteiro,Hamed Moradi,Ehsan Moravveji,Christoph Mordasini,Thierry Morel,Annelies Mortier,Valerio Nascimbeni,Richard P. Nelson,Martin Bo Nielsen,Lena Noack,Andrew Norton,Aviv Ofir,Mahmoudreza Oshagh,R.-M. Ouazzani,Péter Pápics,V. C. Parro,Pascal Petit,Bertrand Plez,Ennio Poretti,Andreas Quirrenbach,Roberto Ragazzoni,Giuliano Raimondo,Monica Rainer,Daniel R. Reese,Ronald Redmer,Sabine Reffert,Bárbara Rojas-Ayala,Ian W. Roxburgh,Stéphanie Salmon,Alexandre Santerne,Jean Schneider,Jesper Schou,Sonja Schuh,Hannah Schunker,A. Silva-Valio,Roberto Silvotti,I. Skillen,Ignas Snellen,Frank Sohl,S. G. Sousa,Alessandro Sozzetti,Dennis Stello,Klaus G. Strassmeier,Michal Švanda,Gy. M. Szabó,Gy. M. Szabó,Andrew Tkachenko,Diana Valencia,Valérie Van Grootel,Sylvie Vauclair,Paolo Ventura,F. W. Wagner,N. A. Walton,Joerg Weingrill,Stephanie C. Werner,Peter J. Wheatley,Konstanze Zwintz +167 more
TL;DR: The PLATO 2.0 mission as discussed by the authors has been selected for ESA's M3 launch opportunity (2022/24) to provide accurate key planet parameters (radius, mass, density and age) in statistical numbers.
Journal ArticleDOI
The Occurrence and Architecture of Exoplanetary Systems
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Prevalence of Earth-size planets orbiting Sun-like stars
TL;DR: In this paper, the authors search for Earth-size planets that cross in front of their host stars by examining the brightness measurements of 42,000 stars from National Aeronautics and Space Administration's Kepler mission.
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