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High-precision photometry by telescope defocussing - VIII. WASP-22, WASP-41, WASP-42 and WASP-55

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Date
21/04/2016
Author
Southworth, John
Tregloan-Reed, J.
Andersen, M. I.
Calchi Novati, S.
Ciceri, S.
Colque, J. P.
D'Ago, G.
Dominik, Martin
Evans, D. F.
Gu, S.-H.
Herrera-Cordova, A.
Hinse, T. C.
Jørgensen, U. G.
Juncher, D.
Kuffmeier, M.
Mancini, L.
Peixinho, N.
Popovas, A.
Rabus, M.
Skottfelt, J.
Tronsgaard, R.
Unda-Sanzana, E.
Wang, X.-B.
Wertz, O.
Alsubai, K. A.
Andersen, J. M.
Bozza, V.
Bramich, D. M.
Burgdorf, M.
Damerdji, Y.
Diehl, C.
Elyiv, A.
Figuera Jaimes, Roberto Jose
Haugbølle, T.
Hundertmark, M.
Kains, N.
Kerins, E.
Korhonen, H.
Liebig, Christine Elisabeth
Mathiasen, M.
Penny, M. T.
Rahvar, S.
Scarpetta, G.
Schmidt, R. W.
Snodgrass, C.
Starkey, David
Surdej, J.
Vilela, C.
Essen, C. von
Wang, Y.
Keywords
Stars: fundamental parameters
stars: individual: WASP-22
WASP-41
WASP-42
WASP-55
Planetary systems
QB Astronomy
QC Physics
NDAS
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Abstract
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 0.63 MJup and a radius of 1.34 RJup. 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 λ = 6 ± 11°. 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.
Citation
Southworth , J , Tregloan-Reed , J , Andersen , M I , Calchi Novati , S , Ciceri , S , Colque , J P , D'Ago , G , Dominik , M , Evans , D F , Gu , S-H , Herrera-Cordova , A , Hinse , T C , Jørgensen , U G , Juncher , D , Kuffmeier , M , Mancini , L , Peixinho , N , Popovas , A , Rabus , M , Skottfelt , J , Tronsgaard , R , Unda-Sanzana , E , Wang , X-B , Wertz , O , Alsubai , K A , Andersen , J M , Bozza , V , Bramich , D M , Burgdorf , M , Damerdji , Y , Diehl , C , Elyiv , A , Figuera Jaimes , R J , Haugbølle , T , Hundertmark , M , Kains , N , Kerins , E , Korhonen , H , Liebig , C E , Mathiasen , M , Penny , M T , Rahvar , S , Scarpetta , G , Schmidt , R W , Snodgrass , C , Starkey , D , Surdej , J , Vilela , C , Essen , C V & Wang , Y 2016 , ' High-precision photometry by telescope defocussing - VIII. WASP-22, WASP-41, WASP-42 and WASP-55 ' , Monthly Notices of the Royal Astronomical Society , vol. 457 , no. 4 , pp. 4205-4217 . https://doi.org/10.1093/mnras/stw279
Publication
Monthly Notices of the Royal Astronomical Society
Status
Peer reviewed
DOI
https://doi.org/10.1093/mnras/stw279
ISSN
0035-8711
Type
Journal article
Rights
© 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at: https://dx.doi.org/10.1093/mnras/stw279
Description
J So acknowledges financial support from the Leverhulme Trust in the form of a Philip Leverhulme Prize. JTR acknowledges financial support from ORAU (Oak Ridge Associated Universities) and NASA in the form of a NASA Post-Doctoral Programme (NPP) Fellowship. DFE is funded by the UK's Science and Technology Facilities Council. EU-S acknowledges the support of CONICYT QUIMAL 130004 project. Funding for the Stellar Astrophysics Centre in Aarhus is provided by The Danish National Research Foundation (grant agreement no. DNRF106). The research is supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (grant agreement no. 267864). TCH acknowledges KASI research grants #2012-1-410-02, #2013-9-400-00, #2014-1-400-06 and #2015-1-850-04. NP acknowledges funding by the Gemini-Conicyt Fund, allocated to project no. 32120036. GD acknowledges Regione Campania for support from POR-FSE Campania 2014–2020. YD, AE, OW and J Su acknowledge support from the Communauté française de Belgique - Actions de recherche concertées - Académie Wallonie-Europe.
Collections
  • University of St Andrews Research
URI
http://hdl.handle.net/10023/8586

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