The Transit Light Curve Project. I. Four Consecutive Transits of the Exoplanet XO-1b

By M. Holman, J. Winn, D. Latham, Francis T. O'Donovan, D. Charbonneau, Gáspár Á. Bakos, G. Esquerdo, C. Hergenrother, Mark E. Everett, A. Pál. 2006

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We present RIz photometry of four consecutive transits of the newly discovered exoplanet XO-1b. We improve on the estimates of the transit parameters, finding the planetary radius to be RP = 1.184RJ, and the stellar radius to be R⋆ = 0.928 R☉, assuming a stellar mass of M⋆ = (1.00 ± 0.03) M☉. The uncertainties in the planetary and stellar radii are dominated by the uncertainty in the stellar mass. These uncertainties increase by a factor of 2-3 if a more conservative uncertainty of 0.10 M☉ is assumed for the stellar mass. Our estimate of the planetary radius is smaller than that reported by McCullough and coworkers, and the resulting estimate for the mean density of XO-1b is intermediate between that of the low-density planet HD 209458b and the higher density planets TrES-1 and HD 189733b. The timings of the transits have an accuracy ranging from 0.2 to 2.5 minutes and are marginally consistent with a uniform period.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Instrumentation

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Citations in the corpus

The Transit Light Curve Project. V. System Parameters and Stellar Rotation Period of HD 189733 (2006, result): “Previous papers in this series have reported results for the exoplanets XO-1b (Holman et al. 2006), OGLE-TR-111b (Winn et al. 2007b), TrES-1 (Winn et al. 2007a), and OGLE-TR-10b (Holman et al. 2007).”
Analytic Approximations for Transit Light-Curve Observables, Uncertainties, and Covariances (2008, methodology): “More recently it has become common to use Markov Chain Monte Carlo methods (e.g., Holman et al. 2006, Winn et al. 2007, Burke et al. 2007).”
A Gaussian process framework for modelling instrumental systematics: application to transmission spectroscopy (2011, methodology): “In practice this can be done using Monte-Carlo MarkovChains (MCMC) methods, which are widely used in the exoplanet community to explore the joint posterior probability distribution of multivariate models (see e.g. Collier Cameron et al. 2007; Holman et al. 2006; Winn et al. 2008).”
Tidal Heating of Extrasolar Planets (2008, methodology): “For XO-1b, tides are unlikely to have played a significant role unless the current e is larger than 0.03.”
Homogeneous studies of transiting extrasolar planets – I. Light-curve analyses (2008, background): “Parameters of the jktebop best fits of the XO-1 light curve from the FLWO 1.2m telescope (Holman et al. 2006) (z band, Nobs = 821) for different treatment of LD.”
THE FLAT TRANSMISSION SPECTRUM OF THE SUPER-EARTH GJ1214b FROM WIDE FIELD CAMERA 3 ON THE HUBBLE SPACE TELESCOPE (2011, background): “For quadratic limb-darkening, the commonly quoted 2u1 + u2 combination (Holman et al. 2006) has the same physical meaning.”
FRIENDS OF HOT JUPITERS. I. A RADIAL VELOCITY SEARCH FOR MASSIVE, LONG-PERIOD COMPANIONS TO CLOSE-IN GAS GIANT PLANETS (2013, methodology): “We considered the chains wellmixed and halted the DE-MCMC run when the number of independent draws (Tz, as defined in Ford 2006) was greater than 1000 and the Gelman-Rubin statistic (Gelman et al. 2003; Ford 2006; Holman et al. 2006) was within 1% of unity for all parameters.”
Efficient identification of exoplanetary transit candidates from SuperWASP light curves (2007, background): “The parameters Rp/R∗, R∗/a and b are strongly covariant, leading to correlation lengths of several hundred to 1000 steps in the Markov chain (Holman et al. 2006; Winn, Holman, & Roussanova 2007) if they are used directly as proposal parameters.”
Transits and Occultations (2010, unknown): “Although a complete MCMC briefing is beyond the scope of this chapter, the interested reader should consult the textbook by Gregory (2005) as well as case studies such as Holman et al. (2006), Collier Cameron et al. (2007), and Burke et al. (2007).”
A STUDY OF THE SHORTEST-PERIOD PLANETS FOUND WITH KEPLER (2014, methodology): “…were found, the allowed region in parameter space was defined with a Markov Chain Monte Carlo (MCMC) routine , which used the Gibbs sampler and the Metropolis-Hastings algorithm, and a likelihood proportional to exp(−χ2/2) (see, e.g., Appendix A of Tegmark et al. 2004, or Holman et al. 2006).”
Prospects for the Characterization and Confirmation of Transiting Exoplanets via the Rossiter-McLaughlin Effect (2006, unknown): “For XO-1, we adopt V ¼ 1:11 km s$1, b ¼ 0:12, and # ¼ 0:131 (McCullough et al. 2006; Holman et al. 2006), and find 'k ¼ 95" and 'V ¼ 0:39 km s$1 for k ¼ 0, and 'k ¼ 20" and 'V ¼ 1:8 km s$1 for k ¼ 90".”
WASP-121 b: a hot Jupiter close to tidal disruption transiting an active F star (2015, methodology): “However, we did not use these coefficients themselves as jump parameters but their combinations, c1 = 2 × u1 + u2 and c2 = u1−2×u2, to minimize the correlation of the obtained uncertainties as introduced by Holman et al. (2006).”
Improving Stellar and Planetary Parameters of Transiting Planet Systems: The Case of TrES-2 (2007, background): “…the quality of the light curves of several of the known transiting planets (Charbonneau et al. 2006, 2007b; Bakos et al. 2006; Gillon et al. 2006; Holman et al. 2006, 2007a, 2007b; Winn et al. 2007a, 2007b, 2007c; Knutson et al. 2007; Pont et al. 2007; Minniti et al. 2007; Diaz et al. 2007), the…”