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Title:
Transiting exoplanets from the CoRoT space mission. XXV. CoRoT-27b: a massive and dense planet on a short-period orbit
Authors:
Parviainen, H.; Gandolfi, D.; Deleuil, M.; Moutou, C.; Deeg, H. J.; Ferraz-Mello, S.; Samuel, B.; Csizmadia, Sz.; Pasternacki, T.; Wuchterl, G.; Havel, M.; Fridlund, M.; Angus, R.; Tingley, B.; Grziwa, S.; Korth, J.; Aigrain, S.; Almenara, J. M.; Alonso, R.; Baglin, A.; Barros, S. C. C.; Bordé, P.; Bouchy, F.; Cabrera, J.; Díaz, R. F.; Dvorak, R.; Erikson, A.; Guillot, T.; Hatzes, A.; Hébrard, G.; Mazeh, T.; Montagnier, G.; Ofir, A.; Ollivier, M.; Pätzold, M.; Rauer, H.; Rouan, D.; Santerne, A.; Schneider, J.
Affiliation:
AA(Instituto de Astrofísica de Canarias (IAC), 38200, La Laguna, Tenerife, Spain ; Dept. Astrofísica, Universidad de La Laguna (ULL), 38206, La Laguna Tenerife, Spain; Department of Physics, Denys Wilkinson Building, Keble Road, Oxford, OX1 3RH, UK), AB(INAF-Catania Astrophysical Observatory, via S. Sofia 78, 95123, Catania, Italy), AC(Aix-Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France), AD(Aix-Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France), AE(Instituto de Astrofísica de Canarias (IAC), 38200, La Laguna, Tenerife, Spain; Dept. Astrofísica, Universidad de La Laguna (ULL), 38206, La Laguna Tenerife, Spain), AF(IAG, Universidade de São Paulo, 05508-090, Säo Paulo, Brazil), AG(LESIA, UMR 8109 CNRS, Observatoire de Paris, UVSQ, Université Paris-Diderot, 5 place J. Janssen, 92195, Meudon Cedex, France), AH(Institute of Planetary Research, German Aerospace Center, Rutherfordstrasse 2, 12489, Berlin, Germany), AI(Institute of Planetary Research, German Aerospace Center, Rutherfordstrasse 2, 12489, Berlin, Germany), AJ(Thüringer Landessternwarte, CoRoT (DLR), Sternwarte 5, Tautenburg, 07778, Tautenburg, Germany), AK(NASA Ames Research Center, MS 244-30, PO Box 1, 94035-0001, Moffett Field, USA), AL(Research and Scientific Support Department, ESTEC/ESA, PO Box 299, 2200 AG, Noordwijk, The Netherlands), AM(Department of Physics, Denys Wilkinson Building, Keble Road, Oxford, OX1 3RH, UK), AN(Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, 8000, Aarhus C, Denmark), AO(Rheinisches Institut für Umweltforschung an der Universität zu Köln, Aachener Strasse 209, 50931, Kölen, Germany), AP(Rheinisches Institut für Umweltforschung an der Universität zu Köln, Aachener Strasse 209, 50931, Kölen, Germany), AQ(Department of Physics, Denys Wilkinson Building, Keble Road, Oxford, OX1 3RH, UK), AR(Aix-Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France), AS(Instituto de Astrofísica de Canarias (IAC), 38200, La Laguna, Tenerife, Spain; Dept. Astrofísica, Universidad de La Laguna (ULL), 38206, La Laguna Tenerife, Spain), AT(LESIA, UMR 8109 CNRS, Observatoire de Paris, UVSQ, Université Paris-Diderot, 5 place J. Janssen, 92195, Meudon Cedex, France), AU(Aix-Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France), AV(Institut d'Astrophysique Spatiale, Université Paris XI, 91405, Orsay, France), AW(Observatoire de Haute-Provence, Saint-Michel-l'Observatoire, 04670, France; Institut d'Astrophysique de Paris, 98bis boulevard Arago, 75014, Paris, France), AX(Institute of Planetary Research, German Aerospace Center, Rutherfordstrasse 2, 12489, Berlin, Germany), AY(Aix-Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France), AZ(University of Vienna, Institute of Astronomy, Türkenschanzstr. 17, 1180, Vienna, Austria), BA(Institute of Planetary Research, German Aerospace Center, Rutherfordstrasse 2, 12489, Berlin, Germany), BB(Observatoire de la Côte d'Azur, Laboratoire Cassiopée, BP 4229, 06304, Nice Cedex 4, France), BC(Thüringer Landessternwarte, CoRoT (DLR), Sternwarte 5, Tautenburg, 07778, Tautenburg, Germany), BD(Institut d'Astrophysique de Paris, 98bis boulevard Arago, 75014, Paris, France; Observatoire de Haute-Provence, Saint-Michel-l'Observatoire, 04670, France), BE(School of Physics and Astronomy, Raymond and Beverly Sackler Faculty of Exact Sciences, Tel Aviv University, 69978, Tel Aviv, Israel), BF(Institut d'Astrophysique de Paris, 98bis boulevard Arago, 75014, Paris, France; Observatoire de Haute-Provence, Saint-Michel-l'Observatoire, 04670, France), BG(Institut für Astrophysik, Georg-August-Universität, Friedrich-Hund-Platz 1, 37077, Göttingen, Germany), BH(Institut d'Astrophysique Spatiale, Université Paris XI, 91405, Orsay, France), BI(Rheinisches Institut für Umweltforschung an der Universität zu Köln, Aachener Strasse 209, 50931, Kölen, Germany), BJ(Institute of Planetary Research, German Aerospace Center, Rutherfordstrasse 2, 12489, Berlin, Germany), BK(LESIA, UMR 8109 CNRS, Observatoire de Paris, UVSQ, Université Paris-Diderot, 5 place J. Janssen, 92195, Meudon Cedex, France), BL(Centro de Astrofísica, Universidade do Porto, rua das Estrelas, 4150-762, Porto, Portugal), BM(LUTH, Observatoire de Paris, CNRS, Université Paris Diderot; 5 place Jules Janssen, 92195, Meudon, France)
Publication:
Astronomy & Astrophysics, Volume 562, id.A140, 12 pp. (A&A Homepage)
Publication Date:
02/2014
Origin:
EDP Sciences
Astronomy Keywords:
planets and satellites: detection, stars: individual: CoRoT-27, techniques: photometric, techniques: radial velocities, techniques: spectroscopic, methods: statistical
DOI:
10.1051/0004-6361/201323049
Bibliographic Code:
2014A&A...562A.140P

Abstract


Aims: We report the discovery of a massive and dense transiting planet CoRoT-27b on a 3.58-day orbit around a 4.2 Gyr-old G2 star. The planet candidate was identified from the CoRoT photometry, and was confirmed as a planet with ground-based spectroscopy.
Methods: The confirmation of the planet candidate is based on radial velocity observations combined with imaging to rule out blends. The characterisation of the planet and its host star was carried out using a Bayesian approach where all the data (CoRoT photometry, radial velocities, and spectroscopic characterisation of the star) are used jointly. The Bayesian analysis included a study whether the assumption of white normally distributed noise holds for the CoRoT photometry and whether the use of a non-normal noise distribution offers advantages in parameter estimation and model selection.
Results: CoRoT-27b has a mass of 10.39 ± 0.55MJup, a radius of 1.01 ± 0.04RJup, a mean density of 12.6-1.67+1.92g cm-3, and an effective temperature of 1500 ± 130 K. The planet orbits around its host star, a 4.2 Gyr-old G2-star with a mass M* = 1.06M&sun; and a radius R* = 1.05R&sun;, on a 0.048 ± 0.007 AU orbit of 3.58 days. The radial velocity observations allow us to exclude highly eccentric orbits, namely, e < 0.065 with 99% confidence. Given its high mass and density, theoretical modelling of CoRoT-27b is demanding. We identify two solutions with heavy element mass fractions of 0.11 ± 0.08M⊕ and 0.07 ± 0.06M⊕, but even solutions void of heavy elements cannot be excluded. We carry out a secondary eclipse search from the CoRoT photometry using a method based on Bayesian model selection, but conclude that the noise level is too high to detect eclipses shallower than 9% of the transit depth. Using a non-normal noise model was shown not to affect the parameter estimation results, but led to significant improvement in the sensitivity of the model selection process.

The CoRoT space mission, launched on December 27, 2006, has been developed and is operated by the CNES, with the contribution of Austria, Belgium, Brazil, ESA (RSSD and Science Programme), Germany, and Spain.

Associated Articles

Part  2     Part  3     Part  4     Part  5     Part  6     Part  7     Part  8     Part  9     Part 10     Part 11     Part 12     Part 13     Part 14     Part 15     Part 16     Part 17     Part 18     Part 19     Part 20     Part 22     Part 21     Part 23     Part 24     Part 25     Part 26     Part  1    

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