Upper limits on the hot Jupiter fraction in the field of NGC 7789

Abstract

We describe a method of estimating the abundance of short-period extrasolar planets based on the results of a photometric survey for planetary transits. We apply the method to a 21-night survey with the 2.5m Isaac Newton Telescope of \~32000 stars in a ~0.5 deg by 0.5 deg square field including the open cluster NGC 7789. From the colour-magnitude diagram we estimate the mass and radius of each star by comparison with the cluster main sequence. We search for injected synthetic transits throughout the lightcurve of each star in order to determine their recovery rate, and thus calculate the expected number of transit detections and false alarms in the survey. We take proper account of the photometric accuracy, time sampling of the observations and criteria (signal-to-noise and number of transits) adopted for transit detection. Assuming that none of the transit candidates found in the survey will be confirmed as real planets, we place conservative upper limits on the abundance of planets as a function of planet radius, orbital period and spectral type.

arXiv commentSubmitted to MNRAS (04/11/2005)

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• The dynamical fate of planetary systems in young star clusters
• Effects of Collisions with Rocky Planets on the Properties of Hot Jupiters
• The Monitor project: the search for transits in the open cluster NGC 2362
• Planets in Open Clusters Detectable by Kepler
• Did a stellar fly-by shape the planetary system around Pr 0211 in the cluster M 44?