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The planet detection efficiency is computed by using measured noise and the observed timespans of the light curves for $\\sim 120,000$ Kepler target stars. We focus on deriving the shape of planet period and radius distribution functions. We find that for orbital period $P>10$ days, the planet frequency d$N_p$/d$\\log$P for \"Neptune-size\" planets ($R_p = 4-8 R_{\\rm Earth}$) increases with period as $\\propto P^{0.7\\pm0.1}$. 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The planet detection efficiency is computed by using measured noise and the observed timespans of the light curves for $\\sim 120,000$ Kepler target stars. We focus on deriving the shape of planet period and radius distribution functions. We find that for orbital period $P>10$ days, the planet frequency d$N_p$/d$\\log$P for \"Neptune-size\" planets ($R_p = 4-8 R_{\\rm Earth}$) increases with period as $\\propto P^{0.7\\pm0.1}$. 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