Journal Article

A transit timing analysis of seven RISE light curves of the exoplanet system HAT-P-3

N. P. Gibson, D. L. Pollacco, S. Barros, C. Benn, D. Christian, M. Hrudková, Y. C. Joshi, F. P. Keenan, E. K. Simpson, I. Skillen, I. A. Steele and I. Todd

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 401, issue 3, pages 1917-1923
Published in print January 2010 | ISSN: 0035-8711
Published online January 2010 | e-ISSN: 1365-2966 | DOI:
A transit timing analysis of seven RISE light curves of the exoplanet system HAT-P-3

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We present seven light curves of the exoplanet system HAT-P-3, taken as part of a transit timing programme using the rapid imager to search for exoplanets instrument on the Liverpool Telescope. The light curves are analysed using a Markov chain Monte Carlo algorithm to update the parameters of the system. The inclination is found to be i= 86.75+0.22−0.21 °, the planet-star radius ratio to be Rp/R= 0.1098+0.0010−0.0012 and the stellar radius to be R= 0.834+0.018−0.026 R, consistent with previous results but with a significant improvement in the precision. Central transit times and uncertainties for each light curve are also determined, and a residual permutation algorithm is used as an independent check on the errors. The transit times are found to be consistent with a linear ephemeris, and a new ephemeris is calculated as Tc(0) = 245 4856.701 18 ± 0.000 18 HJD and P= 2.899 738 ± 0.000 007 d. Model timing residuals are fitted to the measured timing residuals to place upper mass limits for a hypothetical perturbing planet as a function of the period ratio. These show that we have probed for planets with masses as low as 0.33 and 1.81 M in the interior and exterior 2:1 resonances, respectively, assuming the planets are initially in circular orbits.

Keywords: methods: data analysis; techniques: photometric; stars: individual: HAT-P-3; planetary systems

Journal Article.  4561 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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