Reference : WASP-22 b: A Transiting "Hot Jupiter" Planet in a Hierarchical Triple System
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/76639
WASP-22 b: A Transiting "Hot Jupiter" Planet in a Hierarchical Triple System
English
Maxted, P. F. L. [Astrophysics Group, Keele University, Staffordshire, ST5 5BG, UK]
Anderson, D. R. [Astrophysics Group, Keele University, Staffordshire, ST5 5BG, UK]
Gillon, Michaël mailto [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Astrophysique et traitement de l'image >]
Hellier, C. [Astrophysics Group, Keele University, Staffordshire, ST5 5BG, UK]
Queloz, D. [Observatoire de Genève, Université de Genève, 51 Chemin des Maillettes, 1290 Sauverny, Switzerland]
Smalley, B. [Astrophysics Group, Keele University, Staffordshire, ST5 5BG, UK]
Triaud, A H M J [Observatoire de Genève, Université de Genève, 51 Chemin des Maillettes, 1290 Sauverny, Switzerland]
West, R. G. [Department of Physics and Astronomy, University of Leicester, Leicester, LE1 7RH, UK]
Wilson, D. M. [Astrophysics Group, Keele University, Staffordshire, ST5 5BG, UK]
Bentley, S. J. [Astrophysics Group, Keele University, Staffordshire, ST5 5BG, UK]
Cegla, H. [Astrophysics Group, Keele University, Staffordshire, ST5 5BG, UK ; Physics and Astronomy Department, Vanderbilt University, 6301 Stevenson Center, Nashville, TN 37235, USA ; Astrophysics Research Centre, School of Mathematics and Physics, Queen's University, University Road, Belfast, BT7 1NN, UK]
Collier Cameron, A. [School of Physics and Astronomy, University of St. Andrews, North Haugh, Fife, KY16 9SS, UK]
Enoch, B. [School of Physics and Astronomy, University of St. Andrews, North Haugh, Fife, KY16 9SS, UK]
Hebb, L. [School of Physics and Astronomy, University of St. Andrews, North Haugh, Fife, KY16 9SS, UK]
Horne, K. [School of Physics and Astronomy, University of St. Andrews, North Haugh, Fife, KY16 9SS, UK]
Irwin, J. [Department of Astronomy, Harvard University, 60 Garden Street, MS 10, Cambridge, MA 02138, USA]
Lister, T. A. [Las Cumbres Observatory, 6740 Cortona Drive, Suite 102, Santa Barbara, CA 93117, USA]
Mayor, M. [Observatoire de Genève, Université de Genève, 51 Chemin des Maillettes, 1290 Sauverny, Switzerland]
Parley, N. [School of Physics and Astronomy, University of St. Andrews, North Haugh, Fife, KY16 9SS, UK]
Pepe, F. [Observatoire de Genève, Université de Genève, 51 Chemin des Maillettes, 1290 Sauverny, Switzerland]
Pollacco, D. [Astrophysics Research Centre, School of Mathematics and Physics, Queen's University, University Road, Belfast, BT7 1NN, UK]
Segransan, D. [Observatoire de Genève, Université de Genève, 51 Chemin des Maillettes, 1290 Sauverny, Switzerland]
Udry, S. [Observatoire de Genève, Université de Genève, 51 Chemin des Maillettes, 1290 Sauverny, Switzerland]
Wheatley, P. J. [Department of Physics, University of Warwick, Coventry, CV4 7AL, UK]
1-Dec-2010
Astrophysical Journal
Univ Chicago Press
140
6
2007-2012
Yes (verified by ORBi)
International
0004-637X
1538-4357
Chicago
IL
[en] Astrophysics - Earth and Planetary Astrophysics ; planetary systems
[en] We report the discovery of a transiting planet orbiting the star TYC 6446-326-1. The star, WASP-22, is a moderately bright (V = 12.0) solar-type star (T[SUB]eff[/SUB] = 6000 ± 100 K, [Fe/H] = –0.05 ± 0.08). The light curve of the star obtained with the WASP-South instrument shows periodic transit-like features with a depth of about 1% and a duration of 0.14 days. The presence of a transit-like feature in the light curve is confirmed using z-band photometry obtained with Faulkes Telescope South. High-resolution spectroscopy obtained with the CORALIE and HARPS spectrographs confirms the presence of a planetary mass companion with an orbital period of 3.533 days in a near-circular orbit. From a combined analysis of the spectroscopic and photometric data assuming that the star is a typical main-sequence star we estimate that the planet has a mass M [SUB]p[/SUB] = 0.56 ± 0.02M [SUB]Jup[/SUB] and a radius R [SUB]p[/SUB] = 1.12 ± 0.04R [SUB]Jup[/SUB]. In addition, there is a linear trend of 40 m s[SUP]–1[/SUP] yr[SUP]–1[/SUP] in the radial velocities measured over 16 months, from which we infer the presence of a third body with a long-period orbit in this system. The companion may be a low mass M-dwarf, a white dwarf, or a second planet.
Researchers ; Professionals
http://hdl.handle.net/2268/76639
also: http://hdl.handle.net/2268/60746
10.1088/0004-6256/140/6/2007
http://adsabs.harvard.edu/abs/2010arXiv1004.1514M
http://de.arxiv.org/abs/1004.1514

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