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Title:
Transiting exoplanets from the CoRoT space mission. XXVII. CoRoT-28b, a planet orbiting an evolved star, and CoRoT-29b, a planet showing an asymmetric transit
Authors:
Cabrera, J.; Csizmadia, Sz.; Montagnier, G.; Fridlund, M.; Ammler-von Eiff, M.; Chaintreuil, S.; Damiani, C.; Deleuil, M.; Ferraz-Mello, S.; Ferrigno, A.; Gandolfi, D.; Guillot, T.; Guenther, E. W.; Hatzes, A.; Hébrard, G.; Klagyivik, P.; Parviainen, H.; Pasternacki, Th.; Pätzold, M.; Sebastian, D.; Tadeu dos Santos, M.; Wuchterl, G.; Aigrain, S.; Alonso, R.; Almenara, J.-M.; Armstrong, J. D.; Auvergne, M.; Baglin, A.; Barge, P.; Barros, S. C. C.; Bonomo, A. S.; Bordé, P.; Bouchy, F.; Carpano, S.; Chaffey, C.; Deeg, H. J.; Díaz, R. F.; Dvorak, R.; Erikson, A.; Grziwa, S.; Korth, J.; Lammer, H.; Lindsay, C.; Mazeh, T.; Moutou, C.; Ofir, A.; Ollivier, M.; Pallé, E.; Rauer, H.; Rouan, D.; Samuel, B.; Santerne, A.; Schneider, J.
Affiliation:
AA(Institute of Planetary Research, German Aerospace Center, Rutherfordstrasse 2, 12489, Berlin, Germany ), AB(Institute of Planetary Research, German Aerospace Center, Rutherfordstrasse 2, 12489, Berlin, Germany), AC(Institut d'Astrophysique de Paris, UMR 7095 CNRS, Université Pierre & Marie Curie, 98bis boulevard Arago, 75014, Paris, France), AD(Leiden Observatory, University of Leiden, PO Box 9513, 2300 RA, Leiden, The Netherlands; Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, 439 92, Onsala, Sweden; Max Planck Institute for Astronomy Königstuhl 17, 69117, Heidelberg, Germany), AE(Thüringer Landessternwarte, Sternwarte 5, 07778, Tautenburg, Germany), AF(LESIA, UMR 8109 CNRS, Observatoire de Paris, UPMC, Université Paris-Diderot, 5 place J. Janssen, 92195, Meudon, France), AG(Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France), AH(Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France), AI(IAG-Universidade de Sao Paulo, 05508-090, Sao Paulo, Brasil), AJ(LESIA, UMR 8109 CNRS, Observatoire de Paris, UPMC, Université Paris-Diderot, 5 place J. Janssen, 92195, Meudon, France), AK(Zentrum für Astronomie, Fakultät für Physik und Astronomie, Mönchhofstr. 12-14, 69120, Heidelberg, Germany), AL(Université de Nice-Sophia Antipolis, CNRS UMR 6202, Observatoire de la Côte d'Azur, BP 4229, 06304, Nice Cedex 4, France), AM(Thüringer Landessternwarte, Sternwarte 5, 07778, Tautenburg, Germany; Österreichische Akademie der Wissenschaften, Institut für Weltraumforschung, IWF, Schmiedlstraße 6, 8042, Graz, Austria), AN(Thüringer Landessternwarte, Sternwarte 5, 07778, Tautenburg, Germany), AO(Institut d'Astrophysique de Paris, UMR 7095 CNRS, Université Pierre & Marie Curie, 98bis boulevard Arago, 75014, Paris, France), AP(Instituto de Astrofísica de Canarias, 38205, La Laguna, Tenerife, Spain; Dept. Astrofísica, Universidad de la Laguna, 38206, La Laguna, Tenerife, Spain), AQ(Sub-department of Astrophysics, Department of Physics, University of Oxford, Oxford, OX1 3RH, UK), AR(Institute of Planetary Research, German Aerospace Center, Rutherfordstrasse 2, 12489, Berlin, Germany), AS(Rheinisches Institut fürUmweltforschung an der Universität zu Köln, 50931, Aachener Strasse 209, Germany), AT(Thüringer Landessternwarte, Sternwarte 5, 07778, Tautenburg, Germany), AU(IAG-Universidade de Sao Paulo, 05508-090, Sao Paulo, Brasil), AV(Thüringer Landessternwarte, Sternwarte 5, 07778, Tautenburg, Germany), AW(Sub-department of Astrophysics, Department of Physics, University of Oxford, Oxford, OX1 3RH, UK), AX(Instituto de Astrofísica de Canarias, 38205, La Laguna, Tenerife, Spain; Dept. Astrofísica, Universidad de la Laguna, 38206, La Laguna, Tenerife, Spain), AY(Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France), AZ(University of Hawaii, Institute for Astronomy, 34 Ohia Ku Street, Pukalani, Hawaii, 96768, USA; Las Cumbres Observatory Global Telescope Network, Inc. 6740 Cortona Drive Suite 102, Goleta, CA, 93117, USA), BA(LESIA, UMR 8109 CNRS, Observatoire de Paris, UPMC, Université Paris-Diderot, 5 place J. Janssen, 92195, Meudon, France), BB(LESIA, UMR 8109 CNRS, Observatoire de Paris, UPMC, Université Paris-Diderot, 5 place J. Janssen, 92195, Meudon, France), BC(Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France), BD(Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France), BE(INAF-Osservatorio Astrofisico di Torino, via Osservatorio 20, 10025, Pino Torinese, Italy), BF(LAB, UMR 5804, Univ. Bordeaux & CNRS, 33270, Floirac, France), BG(Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France), BH(Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse 1, 85748, Garching, Germany), BI(Torrance High School, 2200 W Carson St, Torrance, CA, 90501, USA), BJ(Instituto de Astrofísica de Canarias, 38205, La Laguna, Tenerife, Spain; Dept. Astrofísica, Universidad de la Laguna, 38206, La Laguna, Tenerife, Spain), BK(Observatoire de l'Université de Genève, 51 chemin des Maillettes, 1290, Sauverny, Switzerland), BL(University of Vienna, Institute of Astronomy, Türkenschanzstr. 17, 1180, Vienna, Austria), BM(Institute of Planetary Research, German Aerospace Center, Rutherfordstrasse 2, 12489, Berlin, Germany), BN(Rheinisches Institut fürUmweltforschung an der Universität zu Köln, 50931, Aachener Strasse 209, Germany), BO(Rheinisches Institut fürUmweltforschung an der Universität zu Köln, 50931, Aachener Strasse 209, Germany), BP(Österreichische Akademie der Wissenschaften, Institut für Weltraumforschung, IWF, Schmiedlstraße 6, 8042, Graz, Austria), BQ(Iolani School, 563 Kamoku St., Honolulu, HI-96816, USA), BR(School of Physics and Astronomy, Raymond and Beverly Sackler Faculty of Exact Sciences, Tel Aviv University, 6997801, Tel Aviv, Israel), BS(Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France; CFHT Corporation, 65-1238 Mamalahoa Hwy, Kamuela, Hawaii, 96743, USA), BT(Institut für Astrophysik, Friedrich-Hund-Platz 1, 37077, Göttingen, Germany), BU(Institut d'Astrophysique Spatiale, Université Paris-Sud & CNRS, 91405, Orsay, France), BV(Instituto de Astrofísica de Canarias, 38205, La Laguna, Tenerife, Spain; Dept. Astrofísica, Universidad de la Laguna, 38206, La Laguna, Tenerife, Spain), BW(Institute of Planetary Research, German Aerospace Center, Rutherfordstrasse 2, 12489, Berlin, Germany; Center for Astronomy and Astrophysics, TU Berlin, Hardenbergstr. 36, 10623, Berlin, Germany), BX(LESIA, UMR 8109 CNRS, Observatoire de Paris, UPMC, Université Paris-Diderot, 5 place J. Janssen, 92195, Meudon, France), BY(LESIA, UMR 8109 CNRS, Observatoire de Paris, UPMC, Université Paris-Diderot, 5 place J. Janssen, 92195, Meudon, France), BZ(Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762, Porto, Portugal), CA(LUTH, Observatoire de Paris, UMR 8102 CNRS, Université Paris Diderot, 5 place Jules Janssen, 92195, Meudon, France)
Publication:
Astronomy & Astrophysics, Volume 579, id.A36, 19 pp. (A&A Homepage)
Publication Date:
07/2015
Origin:
EDP Sciences
Astronomy Keywords:
planetary systems, techniques: photometric, techniques: radial, velocities, techniques: spectroscopic
DOI:
10.1051/0004-6361/201424501
Bibliographic Code:
2015A&A...579A..36C

Abstract

Context. We present the discovery of two transiting extrasolar planets by the satellite CoRoT.
Aims: We aim at a characterization of the planetary bulk parameters, which allow us to further investigate the formation and evolution of the planetary systems and the main properties of the host stars.
Methods: We used the transit light curve to characterize the planetary parameters relative to the stellar parameters. The analysis of HARPS spectra established the planetary nature of the detections, providing their masses. Further photometric and spectroscopic ground-based observations provided stellar parameters (log g, Teff, v sin i) to characterize the host stars. Our model takes the geometry of the transit to constrain the stellar density into account, which when linked to stellar evolutionary models, determines the bulk parameters of the star. Because of the asymmetric shape of the light curve of one of the planets, we had to include the possibility in our model that the stellar surface was not strictly spherical.
Results: We present the planetary parameters of CoRoT-28b, a Jupiter-sized planet (mass 0.484 ± 0.087 MJup; radius 0.955 ± 0.066 RJup) orbiting an evolved star with an orbital period of 5.208 51 ± 0.000 38 days, and CoRoT-29b, another Jupiter-sized planet (mass 0.85 ± 0.20 MJup; radius 0.90 ± 0.16 RJup) orbiting an oblate star with an orbital period of 2.850 570 ± 0.000 006 days. The reason behind the asymmetry of the transit shape is not understood at this point.
Conclusions: These two new planetary systems have very interesting properties and deserve further study, particularly in the case of the star CoRoT-29.

The CoRoT space mission, launched on December 27th 2006, was developed and is operated by CNES, with the contribution of Austria, Belgium, Brazil, ESA (RSSD and Science Programme), Germany, and Spain. Based on observations obtained with the Nordic Optical Telescope, operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, in time allocated by OPTICON and the Spanish Time Allocation Committee (CAT). The research leading to these results has received funding from the European Community's Seventh Framework Programme (FP7/2007-2013) under grant agreement number RG226604 (OPTICON). This work makes use of observations from the LCOGT network.Appendices are available in electronic form at http://www.aanda.org


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