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We perform a systematic search for rings around 168 Kepler planet candidateswith sufficient signal-to-noise ratios that are selected from all theshort-cadence data. We fit ringed and ringless models to their lightcurves, andcompare the fitting results to search for the signatures of planetary rings.First, we identify 29 tentative systems, for which the ringed models exhibitstatistically significant improvement over the ringless models. The lightcurvesof those systems are individually examined, but we are not able to identify anycandidate that indicates evidence for rings. In turn, we find out severalmechanisms of false-positives that would produce ring-like signals, and thenull detection enables us to place upper limits on the size of rings.Furthermore, assuming the tidal alignment between axes of the planetary ringsand orbits, we conclude that the occurrence rate of rings larger than twice theplanetary radius is less than 15 percent. Even though the majority of ourtargets are short-period planets, our null detection provides statistical andquantitative constraints on largely uncertain theoretical models of origin,formation, and evolution of planetary rings.

Systematic Search for Rings around Kepler Planet Candidates: Constraints on Ring Size and Occurrence Rate