High-precision photometry by telescope defocusing – VII. The ultrashort period planet WASP-103
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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.; Jaimes, R. Figuera; Haugbølle, Troels; Jørgensen, Uffe Gråe; Popovas, Andrius; Rabus, M.; Rahvar, S.; Essen, C. von; Schmidt, R. W.; Wertz, O.; Alsubai, K. A.; Bozza, V.; Bramich, D. M.; Novati, S. Calchi; D'Ago, G.; Hinse, T. C.; Henning, T.; Hundertmark, Markus; Juncher, Diana; Korhonen, Heidi Helena; Skottfelt, Jesper Mirsa; Snodgrass, C.; Starkey, D.; Surdej, J.
In: Royal Astronomical Society. Monthly Notices, Vol. 447, No. 1, 2015, p. 711-721.Research output: Contribution to journal › Journal article › Research › peer-review
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TY - JOUR
T1 - High-precision photometry by telescope defocusing – VII. The ultrashort period planet WASP-103
AU - Southworth, John
AU - Mancini, L.
AU - Ciceri, S.
AU - Budaj, J.
AU - Dominik, M.
AU - Jaimes, R. Figuera
AU - Haugbølle, Troels
AU - Jørgensen, Uffe Gråe
AU - Popovas, Andrius
AU - Rabus, M.
AU - Rahvar, S.
AU - Essen, C. von
AU - Schmidt, R. W.
AU - Wertz, O.
AU - Alsubai, K. A.
AU - Bozza, V.
AU - Bramich, D. M.
AU - Novati, S. Calchi
AU - D'Ago, G.
AU - Hinse, T. C.
AU - Henning, T.
AU - Hundertmark, Markus
AU - Juncher, Diana
AU - Korhonen, Heidi Helena
AU - Skottfelt, Jesper Mirsa
AU - Snodgrass, C.
AU - Starkey, D.
AU - Surdej, J.
PY - 2015
Y1 - 2015
N2 - We present 17 transit light curves of the ultra-short 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 midpoint is now measured to an accuracy of 4.8s, versus 67.4s 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 7.3 sigma. 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 five, implying that Rayleigh scattering is not the main cause of the variation of radius with wavelength.
AB - We present 17 transit light curves of the ultra-short 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 midpoint is now measured to an accuracy of 4.8s, versus 67.4s 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 7.3 sigma. 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 five, implying that Rayleigh scattering is not the main cause of the variation of radius with wavelength.
KW - astro-ph.EP
KW - astro-ph.SR
U2 - 10.1093/mnras/stu2394
DO - 10.1093/mnras/stu2394
M3 - Journal article
VL - 447
SP - 711
EP - 721
JO - Royal Astronomical Society. Monthly Notices
JF - Royal Astronomical Society. Monthly Notices
SN - 0035-8711
IS - 1
ER -
ID: 162897883