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Title:
CoRoT-22 b: a validated 4.9 R⊕ exoplanet in 10-d orbit
Authors:
Moutou, C.; Almenara, J. M.; Díaz, R. F.; Alonso, R.; Deleuil, M.; Guenther, E.; Pasternacki, T.; Aigrain, S.; Baglin, A.; Barge, P.; Bonomo, A. S.; Bordé, P.; Bouchy, F.; Cabrera, J.; Carpano, S.; Cochran, W. D.; Csizmadia, Sz.; Deeg, H. J.; Dvorak, R.; Endl, M.; Erikson, A.; Ferraz-Mello, S.; Fridlund, M.; Gandolfi, D.; Guillot, T.; Hatzes, A.; Hébrard, G.; Lovis, C.; Lammer, H.; MacQueen, P. J.; Mazeh, T.; Ofir, A.; Ollivier, M.; Pätzold, M.; Rauer, H.; Rouan, D.; Santerne, A.; Schneider, J.; Tingley, B.; Wuchterl, G.
Affiliation:
AA(Canada-France-Hawaii Telescope Corporation, 65-1238 Mamalahoa Hwy, Kamuela, HI 96743, USA; Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, Marseille, France ), AB(Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, Marseille, France), AC(Obs. Astronomique de l'Univ. de Genève, Versoix, Switzerland), AD(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain; Universidad de La Laguna, Department Astrofísica, E-38206 La Laguna, Tenerife, Spain), AE(Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, Marseille, France), AF(Thüringer Landessternwarte, Tautenburg, Germany), AG(Inst. of Planetary Research, German Aerospace Center, Berlin, Germany), AH(Department of Physics, Oxford, UK), AI(LESIA, Obs de Paris, Meudon, France), AJ(Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, Marseille, France), AK(INAF - Osservatorio Astronomico di Torino, Pino Torinese, Italy), AL(Institut d'Astrophysique Spatiale, Université Paris XI & CNRS, 91405 Orsay, France), AM(Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, Marseille, France), AN(Inst. of Planetary Research, German Aerospace Center, Berlin, Germany), AO(RSSD, ESTEC/ESA, Noordwijk, the Netherlands), AP(McDonald Observatory, University of Texas, Austin, USA), AQ(Inst. of Planetary Research, German Aerospace Center, Berlin, Germany), AR(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain; Universidad de La Laguna, Department Astrofísica, E-38206 La Laguna, Tenerife, Spain), AS(University of Vienna, Institute of Astronomy, Vienna, Austria), AT(McDonald Observatory, University of Texas, Austin, USA), AU(Inst. of Planetary Research, German Aerospace Center, Berlin, Germany), AV(IAG, Universidade de Sao Paulo, Rua do Matão, 1226-São Paulo-SP, 05508-090 Brazil), AW(Inst. of Planetary Research, German Aerospace Center, Berlin, Germany), AX(Zentrum für Astronomie der Universität Heidelberg, Königstuhl 12, Heidelberg, Germany), AY(Observatoire de la Côte d'Azur, Lab. Cassiopée, Nice, France), AZ(Thüringer Landessternwarte, Tautenburg, Germany), BA(Observatoire de Haute Provence, St Michel l'Obs, France), BB(Obs. Astronomique de l'Univ. de Genève, Versoix, Switzerland), BC(Institut d'Astrophysique de Paris, Paris, France; SRI, Austrian Academy of Science, Graz, Austria), BD(McDonald Observatory, University of Texas, Austin, USA), BE(School of Physics and Astronomy, R.B. Sackler Faculty of Exact Sciences, Tel Aviv, Israel), BF(Institut für Astrophysik, Georg-August-Universität, Göttingen, Germany), BG(Institut d'Astrophysique Spatiale, Université Paris XI & CNRS, 91405 Orsay, France), BH(RIU an der Universität zu Köln, Aachener Strabetae 201-209, D-50931 Köln, Germany), BI(Inst. of Planetary Research, German Aerospace Center, Berlin, Germany; Zentrum für Astronomie und Astrophysik, Technische Universität Berlin, D-10623 Berlin, Germany), BJ(LESIA, Obs de Paris, Meudon, France), BK(Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal), BL(LUTH, Obs de Paris, CNRS, Univ. Paris Diderot, Meudon, France), BM(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain; Universidad de La Laguna, Department Astrofísica, E-38206 La Laguna, Tenerife, Spain; Stellar Astrophysics Center, Institut for Fysik og Astronomi, Aarhus Universitet, Ny Munkegade 120, DK-8000 Aarhus C, Denmark), BN(Thüringer Landessternwarte, Tautenburg, Germany)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 444, Issue 3, p.2783-2792 (MNRAS Homepage)
Publication Date:
11/2014
Origin:
OUP
Astronomy Keywords:
methods: observational, methods: statistical, techniques: photometric, techniques: radial velocities, stars: individual: 2MASS18424010+0613088, planetary systems
Abstract Copyright:
2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
DOI:
10.1093/mnras/stu1645
Bibliographic Code:
2014MNRAS.444.2783M

Abstract

The CoRoT satellite has provided high-precision photometric light curves for more than 163 000 stars and found several hundreds of transiting systems compatible with a planetary scenario. If ground-based velocimetric observations are the best way to identify the actual planets among many possible configurations of eclipsing binary systems, recent transit surveys have shown that it is not always within reach of the radial-velocity detection limits. In this paper, we present a transiting exoplanet candidate discovered by CoRoT whose nature cannot be established from ground-based observations, and where extensive analyses are used to validate the planet scenario. They are based on observing constraints from radial-velocity spectroscopy, adaptive optics imaging and the CoRoT transit shape, as well as from priors on stellar populations, planet and multiple stellar systems frequency. We use the fully Bayesian approach developed in the PASTIS (Planet Analysis and Small Transit Investigation Software) analysis software, and conclude that the planet scenario is at least 1400 times more probable than any other false-positive scenario. The primary star is a metallic solar-like dwarf, with Ms = 1.099 ± 0.049 M&sun; and Rs = 1.136^{+0.038}_{-0.090} R&sun;. The validated planet has a radius of Rp = 4.88^{+0.17}_{-0.39} R⊕ and mass less than 49 M⊕. Its mean density is smaller than 2.56 g cm-3 and orbital period is 9.7566 ± 0.0012 d. This object, called CoRoT-22 b, adds to a large number of validated Kepler planets. These planets do not have a proper measurement of the mass but allow statistical characterization of exoplanets population.
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