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

John Southworth; J. Tregloan-Reed; M. I. Andersen; S. Calchi Novati; S. Ciceri; J. P. Colque; G. D'Ago; Martin Dominik; D. F. Evans; S.-H. Gu; A. Herrera-Cordova; T. C. Hinse; U. G. Jørgensen; D. Juncher; M. Kuffmeier; L. Mancini; N. Peixinho; A. Popovas; M. Rabus; J. Skottfelt; R. Tronsgaard; E. Unda-Sanzana; X.-B. Wang; O. Wertz; K. A. Alsubai; J. M. Andersen; V. Bozza; D. M. Bramich; M. Burgdorf; Y. Damerdji; C. Diehl; A. Elyiv; Roberto Jose Figuera Jaimes; T. Haugbølle; M. Hundertmark; N. Kains; E. Kerins; H. Korhonen; Christine Elisabeth Liebig; M. Mathiasen; M. T. Penny; S. Rahvar; G. Scarpetta; R. W. Schmidt; C. Snodgrass; David Starkey; J. Surdej; C. Vilela; C. von Essen; Y. Wang

doi:10.1093/mnras/stw279

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

John Southworth, J. Tregloan-Reed, M. I. Andersen, S. Calchi Novati, S. Ciceri, J. P. Colque, G. D'Ago, Martin Dominik, D. F. Evans, S.-H. Gu, A. Herrera-Cordova, T. C. Hinse, U. G. Jørgensen, D. Juncher, M. Kuffmeier, L. Mancini, N. Peixinho, A. Popovas, M. Rabus, J. SkottfeltR. Tronsgaard, E. Unda-Sanzana, X.-B. Wang, O. Wertz, K. A. Alsubai, J. M. Andersen, V. Bozza, D. M. Bramich, M. Burgdorf, Y. Damerdji, C. Diehl, A. Elyiv, Roberto Jose Figuera Jaimes, T. Haugbølle, M. Hundertmark, N. Kains, E. Kerins, H. Korhonen, Christine Elisabeth Liebig, M. Mathiasen, M. T. Penny, S. Rahvar, G. Scarpetta, R. W. Schmidt, C. Snodgrass, David Starkey, J. Surdej, C. Vilela, C. von Essen, Y. Wang

School of Physics and Astronomy

Research output: Contribution to journal › Article › peer-review

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.

Original language	English
Pages (from-to)	4205-4217
Journal	Monthly Notices of the Royal Astronomical Society
Volume	457
Issue number	4
Early online date	8 Feb 2016
DOIs	https://doi.org/10.1093/mnras/stw279
Publication status	Published - 21 Apr 2016

Keywords

Stars: fundamental parameters
stars: individual: WASP-22
WASP-41
WASP-42
WASP-55
Planetary systems

Access to Document

10.1093/mnras/stw279

Dominik_2016_HighPrecisionPhotometry_MNRAS_FinalPubVersion
© 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
Final published version, 3.35 MB

Planet population statistics: Planet population statistics from fully-deterministic microlensing campaigns
Dominik, M. (PI)
The Royal Society
1/10/11 → 30/09/15
Project: Fellowship

Cite this

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., ... 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, 457(4), 4205-4217. https://doi.org/10.1093/mnras/stw279

@article{0a551e447d6c47dfbaabf631234c9d43,

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

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.",

keywords = "Stars: fundamental parameters, stars: individual: WASP-22, WASP-41, WASP-42, WASP-55, Planetary systems",

author = "John Southworth and J. Tregloan-Reed and Andersen, {M. I.} and {Calchi Novati}, S. and S. Ciceri and Colque, {J. P.} and G. D'Ago and Martin Dominik and Evans, {D. F.} and S.-H. Gu and A. Herrera-Cordova and Hinse, {T. C.} and J{\o}rgensen, {U. G.} and D. Juncher and M. Kuffmeier and L. Mancini and N. Peixinho and A. Popovas and M. Rabus and J. Skottfelt and R. Tronsgaard and E. Unda-Sanzana and X.-B. Wang and O. Wertz and Alsubai, {K. A.} and Andersen, {J. M.} and V. Bozza and Bramich, {D. M.} and M. Burgdorf and Y. Damerdji and C. Diehl and A. Elyiv and {Figuera Jaimes}, {Roberto Jose} and T. Haugb{\o}lle and M. Hundertmark and N. Kains and E. Kerins and H. Korhonen and Liebig, {Christine Elisabeth} and M. Mathiasen and Penny, {M. T.} and S. Rahvar and G. Scarpetta and Schmidt, {R. W.} and C. Snodgrass and David Starkey and J. Surdej and C. Vilela and Essen, {C. von} and Y. Wang",

note = "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 Communaut{\'e} fran{\c c}aise de Belgique - Actions de recherche concert{\'e}es - Acad{\'e}mie Wallonie-Europe. ",

year = "2016",

month = apr,

day = "21",

doi = "10.1093/mnras/stw279",

language = "English",

volume = "457",

pages = "4205--4217",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

number = "4",

}

Southworth, J, Tregloan-Reed, J, Andersen, MI, Calchi Novati, S, Ciceri, S, Colque, JP, D'Ago, G, Dominik, M, Evans, DF, Gu, S-H, Herrera-Cordova, A, Hinse, TC, Jørgensen, UG, 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, KA, Andersen, JM, Bozza, V, Bramich, DM, Burgdorf, M, Damerdji, Y, Diehl, C, Elyiv, A, Figuera Jaimes, RJ, Haugbølle, T, Hundertmark, M, Kains, N, Kerins, E, Korhonen, H, Liebig, CE, Mathiasen, M, Penny, MT, Rahvar, S, Scarpetta, G, Schmidt, RW, Snodgrass, C, Starkey, D, Surdej, J, Vilela, C, Essen, CV & 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

TY - JOUR

T1 - High-precision photometry by telescope defocussing - VIII. WASP-22, WASP-41, WASP-42 and WASP-55

AU - Southworth, John

AU - Tregloan-Reed, J.

AU - Andersen, M. I.

AU - Calchi Novati, S.

AU - Ciceri, S.

AU - Colque, J. P.

AU - D'Ago, G.

AU - Dominik, Martin

AU - Evans, D. F.

AU - Gu, S.-H.

AU - Herrera-Cordova, A.

AU - Hinse, T. C.

AU - Jørgensen, U. G.

AU - Juncher, D.

AU - Kuffmeier, M.

AU - Mancini, L.

AU - Peixinho, N.

AU - Popovas, A.

AU - Rabus, M.

AU - Skottfelt, J.

AU - Tronsgaard, R.

AU - Unda-Sanzana, E.

AU - Wang, X.-B.

AU - Wertz, O.

AU - Alsubai, K. A.

AU - Andersen, J. M.

AU - Bozza, V.

AU - Bramich, D. M.

AU - Burgdorf, M.

AU - Damerdji, Y.

AU - Diehl, C.

AU - Elyiv, A.

AU - Figuera Jaimes, Roberto Jose

AU - Haugbølle, T.

AU - Hundertmark, M.

AU - Kains, N.

AU - Kerins, E.

AU - Korhonen, H.

AU - Liebig, Christine Elisabeth

AU - Mathiasen, M.

AU - Penny, M. T.

AU - Rahvar, S.

AU - Scarpetta, G.

AU - Schmidt, R. W.

AU - Snodgrass, C.

AU - Starkey, David

AU - Surdej, J.

AU - Vilela, C.

AU - Essen, C. von

AU - Wang, Y.

N1 - 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.

PY - 2016/4/21

Y1 - 2016/4/21

N2 - 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.

AB - 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.

KW - Stars: fundamental parameters

KW - stars: individual: WASP-22

KW - WASP-41

KW - WASP-42

KW - WASP-55

KW - Planetary systems

U2 - 10.1093/mnras/stw279

DO - 10.1093/mnras/stw279

M3 - Article

SN - 0035-8711

VL - 457

SP - 4205

EP - 4217

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 4

ER -

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

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Keywords

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Projects

Planet population statistics: Planet population statistics from fully-deterministic microlensing campaigns

Cite this