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WASP-37b: A 1.8 M J exoplanet transiting a metal-poor star

Simpson, E. K.; Faedi, F.; Barros, S. C. C.; Brown, D. J. A.; Cameron, A. Collier; Hebb, L.; Pollacco, D.; Smalley, B.; Todd, I.; Butters, O. W.; Hébrard, G.; McCormac, J.; Miller, G. R. M.; Santerne, A.; Street, R. A.; Skillen, I.; Triaud, A. H. M. J.; Anderson, D. R.; Bento, J.; Boisse, I.; Bouchy, F.; Enoch, B.; Haswell, C. A.; Hellier, C.; Holmes, S.; Horne, K.; Keenan, F. P.; Lister, T. A.; Maxted, P. F. L.; Moulds, V.; Moutou, C.; Norton, A. J.; Parley, N.; Pepe, F.; Queloz, D.; Segransan, D.; Smith, A. M. S.; Stempels, H. C.; Udry, S.; Watson, C. A.; West, R. G. and Wheatley, P. J. (2011). WASP-37b: A 1.8 M J exoplanet transiting a metal-poor star. Astronomical Journal, 141(1), article no. 8.

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DOI (Digital Object Identifier) Link: https://doi.org/10.1088/0004-6256/141/1/8
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Abstract

We report on the discovery of WASP-37b, a transiting hot Jupiter orbiting an m v = 12.7 G2-type dwarf, with a period of 3.577469 ± 0.000011 d, transit epoch T 0 = 2455338.6188 ± 0.0006 (HJD; dates throughout the paper are given in Coordinated Universal Time (UTC)), and a transit duration 0.1304+0.0018,sub>0.0017</sub> d. The planetary companion has a mass M p = 1.80 ± 0.17 M J and radius R p = 1.16+0.070.06 R J, yielding a mean density of 1.15+0.120.15 ρJ. From a spectral analysis, we find that the host star has M* = 0.925 ± 0.120 M ʘ, R * = 1.003 ± 0.053 R ʘ, T eff = 5800 ± 150 K, and [Fe/H] = -0.40 ± 0.12. WASP-37 is therefore one of the lowest metallicity stars to host a transiting planet.

Item Type: Journal Item
Copyright Holders: 2011 The American Astronomical Society. All rights reserved
ISSN: 1538-3881
Keywords: planetary systems; stars; photometric techniques; spectroscopic techniques
Academic Unit/School: Faculty of Science, Technology, Engineering and Mathematics (STEM) > Physical Sciences
Faculty of Science, Technology, Engineering and Mathematics (STEM)
Item ID: 25416
Depositing User: Andrew Norton
Date Deposited: 04 Jan 2011 16:47
Last Modified: 08 Dec 2018 00:58
URI: http://oro.open.ac.uk/id/eprint/25416
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