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J/MNRAS/447/711     Transiting planet WASP-103               (Southworth+, 2015)

High-precision photometry by telescope defocusing. VII. The ultrashort period planet WASP-103. Southworth J., Mancini L., Ciceri S., Budaj J., Dominik M., Figuera Jaimes R., Haugbolle T., Jorgensen 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. <Mon. Not. R. Astron. Soc., 447, 711-721 (2015)> =2015MNRAS.447..711S (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Planets ; Photometry Keywords: stars: fundamental parameters - stars: individual: WASP-103 - planetary systems Abstract: 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 4.8s, 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 7.3σ. 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. Description: Light curves of 11 transits of the extrasolar planetary system WASP-103 are presented. The data were obtained using three telescopes and instruments: the Danish 1.54m telescope with DFOSC imager; the MPG 2.2m telescope with GROND imager; and the 2.15m telescope at CASLEO. They were obtained through six different optical broad-band filters. The errorbars for each transit have been scaled so the best-fitting model (obtained using the JKTEBOP code) has a reduced chi-squared value of 1.0. Objects: --------------------------------------------------------------------- RA (2000) DE Designation(s) --------------------------------------------------------------------- 16 37 15.57 +07 11 00.1 WASP-103 = 1SWASP J163715.59+071100.0 --------------------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file wasp103.dat 46 2293 Photometry of WASP-103
See also: J/MNRAS/396/1023 : Transiting planetary system WASP-5 (Southworth+, 2009) J/MNRAS/399/287 : Transiting planetary system WASP-4 (Southworth+, 2009) J/ApJ/707/167 : Transiting planetary system WASP-18 (Southworth+, 2009) J/MNRAS/408/1680 : Transiting planetary system WASP-2 (Southworth+, 2010) J/A+A/527/A8 : Transiting planetary system WASP-7 (Southworth+, 2011) J/MNRAS/420/2580 : Four transits of HAT-P-13 (Southworth+, 2012) J/MNRAS/422/3099 : Transits of HAT-P-5 (Southworth+, 2012) J/MNRAS/426/1338 : Transiting planetary system WASP-17 (Southworth+, 2012) J/MNRAS/434/1300 : Planetary systems WASP-15, WASP-16 (Southworth+, 2013) J/MNRAS/444/776 : WASP-24, WASP-25 and WASP-26 (Southworth+, 2014) Byte-by-byte Description of file: wasp103.dat
Bytes Format Units Label Explanations
1- 6 A6 --- Inst Instrument used for the observation 8 A1 --- Filt [IRgriz] Filter used for the observation 11- 24 F14.6 d BJD Barycentric JD for the midpoint of observation (TDB) 26- 35 F10.7 mag mag Differential magnitude in that filter 38- 46 F9.7 mag e_mag Measurement error of the differential magnitude
Acknowledgements: John Southworth, astro.js(at)keele.ac.uk References: Southworth et al., Paper I 2009MNRAS.396.1023S, Cat. J/MNRAS/396/1023 Southworth et al., Paper II 2009MNRAS.399..287S, Cat. J/MNRAS/399/287 Southworth et al., Paper III 2010MNRAS.408.1680S, Cat. J/MNRAS/408/1680 Southworth et al., Paper IV 2012MNRAS.426.1338S, Cat. J/MNRAS/426/1338 Southworth et al., Paper V 2013MNRAS.434.1300S, Cat. J/MNRAS/434/1300 Southworth et al., Paper VI 2014MNRAS.444..776S, Cat. J/MNRAS/444/776
(End) John Southworth [Keele Univ., UK], Patricia Vannier [CDS] 06-Jun-2016
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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