CoRoT-22 b: a validated 4.9 R⊕ exoplanet in 10-d orbit

Autor(en)

C. Moutou, J. M. Almenara, R. F. Diaz, R. Alonso, M. Deleuil, E. Guenther, T. Pasternacki, S. Aigrain, A. Baglin, P. Barge, A. S. Bonomo, P. Borde, F. Bouchy, J. Cabrera, S. Carpano, W. D. Cochran, Sz Csizmadia, H. J. Deeg, R. Dvorak, M. Endl, A. Erikson, S. Ferraz-Mello, M. Fridlund, D. Gandolfi, T. Guillot, A. Hatzes, G. Hebrard, C. Lovis, H. Lammer, P. J. MacQueen, T. Mazeh, A. Ofir, M. Ollivier, M. Paetzold, H. Rauer, D. Rouan, A. Santerne, J. Schneider, B. Tingley, G. Wuchterl

Abstrakt

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 M

_s = 1.099 ± 0.049 M{N-ary circled dot operator} and R

_s = 1.136

^+0.038

_-0.090 R{N-ary circled dot operator}. The validated planet has a radius of R

_p = 4.88

^+0.17

_-0.39 R{N-ary circled plus operator} and mass less than 49 M{N-ary circled plus operator}. 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.

Organisation(en)

Institut für Astrophysik

Externe Organisation(en)

Canada-France-Hawaii Telescope, Centre National De La Recherche Scientifique (CNRS), Universität Zürich (UZH), Hôpitaux Universitaires de Genève, Instituto de Astrofísica de Canarias (IAC), Universidad de La Laguna, Thüringer Landessternwarte Tautenburg, Helmholtz-Zentrum Berlin für Materialien und Energie, Deutsches Zentrum für Luft- und Raumfahrt e.V. (DLR), League of European Research Universities - LERU, Oxford University Museum of Natural History, Instituto Nazionale die Astrofisica (INAF), Université Paris1 Panthéon-Sorbonne, HE Space Operations BV, University of Texas at El Paso, University of Texas, Austin, Universidade de São Paulo, Ludwig-Maximilians-Universität München, Universität Leipzig, Université Côte d'Azur, Observ Haute Provence, Junge Akademie der Österreichischen Akademie der Wissenschaften, Tel Aviv University, Georg-August-Universität Göttingen, Fachhochschule Köln, Technische Universität Berlin, Universidade do Porto, Aarhus University Hospital, Université Paris VII - Paris-Diderot, Université Paris VI - Pierre-et-Marie-Curie, Aix-Marseille Université, Université de Paris

Journal

Monthly Notices of the Royal Astronomical Society

Band

444

Seiten

2783-2792

Anzahl der Seiten

10

ISSN

0035-8711

DOI

https://doi.org/10.1093/mnras/stu1645

Publikationsdatum

11-2014

Peer-reviewed

Ja

ÖFOS 2012

103003 Astronomie, 103004 Astrophysik

Schlagwörter

ASJC Scopus Sachgebiete

Astronomy and Astrophysics, Space and Planetary Science

Link zum Portal

https://ucrisportal.univie.ac.at/de/publications/26688cec-2ccb-4b90-887e-a6a2e1c3c4e7