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High-precision photometry by telescope defocusing - VII. The ultrashort period planet WASP-103

Southworth, John; Mancini, L.; Ciceri, S.; Budaj, J.; Dominik, M.; Figuera Jaimes, R.; Haugbølle, T.; Jørgensen, U.G.; Popovas, A.; Rabus, M.; Rahvar, S.; von Essen, C.; Schmidt, R.W.; Wertz, O.; Alsubai, K.A.; Bozza, V.; Bramich, D.M.; Calchi Novati, S.; D'Ago, G.; Hinse, T.C.; Henning, Th.; Hundertmark, M.; Juncher, D.; Korhonen, H.; Skottfelt, J.; Snodgrass, C.; Starkey, D.; Surdej, J.

High-precision photometry by telescope defocusing - VII. The ultrashort period planet WASP-103 Thumbnail


L. Mancini

S. Ciceri

J. Budaj

M. Dominik

R. Figuera Jaimes

T. Haugbølle

U.G. Jørgensen

A. Popovas

M. Rabus

S. Rahvar

C. von Essen

R.W. Schmidt

O. Wertz

K.A. Alsubai

V. Bozza

D.M. Bramich

S. Calchi Novati

G. D'Ago

T.C. Hinse

Th. Henning

M. Hundertmark

D. Juncher

H. Korhonen

J. Skottfelt

C. Snodgrass

D. Starkey

J. Surdej


We present 17 transit light curves of the ultrashort period planetary system WASP-103, a strong candidate for the detection of tidally-induced orbital decay. We use these to establish a high-precision reference epoch for transit timing studies. The time of the reference transit mid-point is now measured to an accuracy of 4.8 s, versus 67.4 s in the discovery paper, aiding future searches for orbital decay. With the help of published spectroscopic measurements and theoretical stellar models, we determine the physical properties of the system to high precision and present a detailed error budget for these calculations. The planet has a Roche lobe filling factor of 0.58, leading to a significant asphericity; we correct its measured mass and mean density for this phenomenon. A high-resolution Lucky Imaging observation shows no evidence for faint stars close enough to contaminate the point spread function of WASP-103. Our data were obtained in the Bessell RI and the SDSS griz passbands and yield a larger planet radius at bluer optical wavelengths, to a confidence level of 7.3s. Interpreting this as an effect of Rayleigh scattering in the planetary atmosphere leads to a measurement of the planetary mass which is too small by a factor of 5, implying that Rayleigh scattering is not the main cause of the variation of radius with wavelength.

Journal Article Type Article
Acceptance Date Nov 11, 2014
Online Publication Date Dec 17, 2014
Publication Date Feb 11, 2015
Publicly Available Date May 26, 2023
Journal Monthly Notices of the Royal Astronomical Society
Print ISSN 0035-8711
Publisher Oxford University Press
Peer Reviewed Peer Reviewed
Volume 447
Issue 1
Article Number 1365-2966
Pages 711 -721
Keywords stars, fundamental parameters, individual, WASP-103, planetary systems
Publisher URL


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