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.

I: Royal Astronomical Society. Monthly Notices, Bind 447, Nr. 1, 2015, s. 711-721.

Publikation: Bidrag til tidsskrift › Tidsskriftartikel › Forskning › fagfællebedømt

Harvard

Southworth, J, Mancini, L, Ciceri, S, Budaj, J, Dominik, M, Jaimes, RF, Haugbølle, T, Jørgensen, UG, Popovas, A, Rabus, M, Rahvar, S, Essen, CV, Schmidt, RW, Wertz, O, Alsubai, KA, Bozza, V, Bramich, DM, Novati, SC, D'Ago, G, Hinse, TC, Henning, T, Hundertmark, M, Juncher, D, Korhonen, HH, Skottfelt, JM, Snodgrass, C, Starkey, D & Surdej, J 2015, 'High-precision photometry by telescope defocusing – VII. The ultrashort period planet WASP-103', Royal Astronomical Society. Monthly Notices, bind 447, nr. 1, s. 711-721. https://doi.org/10.1093/mnras/stu2394

APA

Southworth, J., Mancini, L., Ciceri, S., Budaj, J., Dominik, M., Jaimes, R. F., Haugbølle, T., Jørgensen, U. G., Popovas, A., Rabus, M., Rahvar, S., Essen, C. V., Schmidt, R. W., Wertz, O., Alsubai, K. A., Bozza, V., Bramich, D. M., Novati, S. C., D'Ago, G., ... Surdej, J. (2015). High-precision photometry by telescope defocusing – VII. The ultrashort period planet WASP-103. Royal Astronomical Society. Monthly Notices, 447(1), 711-721. https://doi.org/10.1093/mnras/stu2394

Vancouver

Southworth J, Mancini L, Ciceri S, Budaj J, Dominik M, Jaimes RF o.a. High-precision photometry by telescope defocusing – VII. The ultrashort period planet WASP-103. Royal Astronomical Society. Monthly Notices. 2015;447(1):711-721. https://doi.org/10.1093/mnras/stu2394

Author

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. / High-precision photometry by telescope defocusing – VII. The ultrashort period planet WASP-103. I: Royal Astronomical Society. Monthly Notices. 2015 ; Bind 447, Nr. 1. s. 711-721.

Bibtex

@article{0fe60d45b7c04832a081c6e691bdedb3,
title = "High-precision photometry by telescope defocusing – VII. The ultrashort period planet WASP-103",
abstract = "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.",
keywords = "astro-ph.EP, astro-ph.SR",
author = "John Southworth and L. Mancini and S. Ciceri and J. Budaj and M. Dominik and Jaimes, {R. Figuera} and Troels Haugb{\o}lle and J{\o}rgensen, {Uffe Gr{\aa}e} and Andrius Popovas and M. Rabus and S. Rahvar and Essen, {C. von} and Schmidt, {R. W.} and O. Wertz and Alsubai, {K. A.} and V. Bozza and Bramich, {D. M.} and Novati, {S. Calchi} and G. D'Ago and Hinse, {T. C.} and T. Henning and Markus Hundertmark and Diana Juncher and Korhonen, {Heidi Helena} and Skottfelt, {Jesper Mirsa} and C. Snodgrass and D. Starkey and J. Surdej",
year = "2015",
doi = "10.1093/mnras/stu2394",
language = "English",
volume = "447",
pages = "711--721",
journal = "Royal Astronomical Society. Monthly Notices",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "1",

}

RIS

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