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 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:
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RA (2000) DE Designation(s)
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16 37 15.57 +07 11 00.1 WASP-103 = 1SWASP J163715.59+071100.0
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
wasp103.dat 46 2293 Photometry of WASP-103
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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
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Bytes Format Units Label Explanations
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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
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Acknowledgements:
John Southworth, astro.js(at)keele.ac.uk
References:
Southworth et al., Paper I 2009MNRAS.396.1023S 2009MNRAS.396.1023S, Cat. J/MNRAS/396/1023
Southworth et al., Paper II 2009MNRAS.399..287S 2009MNRAS.399..287S, Cat. J/MNRAS/399/287
Southworth et al., Paper III 2010MNRAS.408.1680S 2010MNRAS.408.1680S, Cat. J/MNRAS/408/1680
Southworth et al., Paper IV 2012MNRAS.426.1338S 2012MNRAS.426.1338S, Cat. J/MNRAS/426/1338
Southworth et al., Paper V 2013MNRAS.434.1300S 2013MNRAS.434.1300S, Cat. J/MNRAS/434/1300
Southworth et al., Paper VI 2014MNRAS.444..776S 2014MNRAS.444..776S, Cat. J/MNRAS/444/776
(End) John Southworth [Keele Univ., UK], Patricia Vannier [CDS] 06-Jun-2016