High-precision photometry by telescope defocussing - II. The transiting planetary system WASP-4*

October 2009 • 2009MNRAS.399..287S

Authors • Southworth, John • Hinse, T. C. • Burgdorf, M. J. • Dominik, M. • Hornstrup, A. • Jørgensen, U. G. • Liebig, C. • Ricci, D. • Thöne, C. C. • Anguita, T. • Bozza, V. • Novati, S. Calchi • Harpsøe, K. • Mancini, L. • Masi, G. • Mathiasen, M. • Rahvar, S. • Scarpetta, G. • Snodgrass, C. • Surdej, J. • Zub, M.

Abstract • We present and analyse light curves of four transits of the Southern hemisphere extrasolar planetary system WASP-4, obtained with a telescope defocused so the radius of each point spread function was 17 arcsec (44 pixels). This approach minimizes both random and systematic errors, allowing us to achieve scatters of between 0.60 and 0.88 mmag per observation over complete transit events. The light curves are augmented by published observations and analysed using the jktebop code. The results of this process are combined with theoretical stellar model predictions to derive the physical properties of the WASP-4 system. We find that the mass and radius of the planet are M_b= 1.289^+0.090_-0.090^+0.039_-0.000M_Jup and R_b= 1.371^+0.032_-0.035^+0.021_-0.000R_Jup, respectively (statistical and systematic uncertainties). These quantities give a surface gravity and density of g_b= 17.03^+0.97_-0.54 m s^-2 and ρ_b= 0.500^+0.032_-0.021^+0.000_-0.008ρ_Jup, and fit the trends for short-period extrasolar planets to have relatively high masses and surface gravities. WASP-4 is now one of the best-quantified transiting extrasolar planetary systems, and significant further progress requires improvements to our understanding of the physical properties of low-mass stars.

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Sebastiano Calchi Novati

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