A1 Refereed original research article in a scientific journal
High-precision photometry by telescope defocussing - VIII. WASP-22, WASP-41, WASP-42 and WASP-55
Authors: Southworth J, Tregloan-Reed J, Andersen MI, Novati SC, Ciceri S, Colque JP, D'Ago G, Dominik M, Evans DF, Gu SH, Herrera-Cordova A, Hinse TC, Jorgensen UG, Juncher D, Kuffmeier M, Mancini L, Peixinho N, Popovas A, Rabus M, Skottfelt J, Tronsgaard R, Unda-Sanzana E, Wang XB, Wertz O, Alsubai KA, Andersen JM, Bozza V, Bramich DM, Burgdorf M, Damerdji Y, Diehl C, Elyiv A, Jaimes RF, Haugbolle T, Hundertmark M, Kains N, Kerins E, Korhonen H, Liebig C, Mathiasen M, Penny MT, Rahvar S, Scarpetta G, Schmidt RW, Snodgrass C, Starkey D, Surdej J, Vilela C, von Essen C, Wang Y, Wang Y, von Essen C
Publisher: OXFORD UNIV PRESS
Publication year: 2016
Journal: Monthly Notices of the Royal Astronomical Society
Journal name in source: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Journal acronym: MON NOT R ASTRON SOC
Volume: 457
Issue: 4
First page : 4205
Last page: 4217
Number of pages: 13
ISSN: 0035-8711
DOI: https://doi.org/10.1093/mnras/stw279
Self-archived copy’s web address: https://research.utu.fi/converis/portal/detail/Publication/29391706
We present 13 high-precision and four additional light curves of four bright southern-hemisphere transiting planetary systems: WASP-22, WASP-41, WASP-42 and WASP-55. In the cases of WASP-42 and WASP-55, these are the first follow-up observations since their discovery papers. We present refined measurements of the physical properties and orbital ephemerides of all four systems. No indications of transit timing variations were seen. All four planets have radii inflated above those expected from theoretical models of gas-giant planets; WASP-55 b is the most discrepant with a mass of 0.63M(Jup) and a radius of 1.34 R-Jup. WASP-41 shows brightness anomalies during transit due to the planet occulting spots on the stellar surface. Two anomalies observed 3.1 d apart are very likely due to the same spot. We measure its change in position and determine a rotation period for the host star of 18.6 +/- 1.5 d, in good agreement with a published measurement from spot-induced brightness modulation, and a sky-projected orbital obliquity of lambda = 6 +/- 11 degrees. We conclude with a compilation of obliquity measurements from spot-tracking analyses and a discussion of this technique in the study of the orbital configurations of hot Jupiters.
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