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We use six years (2003 to 2008) of Optical Gravitational Lensing ExperimentIII microlensing observations to derive the survey detection efficiency for arange of planetary masses and projected distances from the host star. Weperform an independent analysis of the microlensing light curves to extract theevent parameters and compute the planet detection probability given the data.2433 light curves satisfy our quality selection criteria and are retained forfurther processing. The aggregate of the detection probabilities over the rangeexplored yields the expected number of microlensing planet detections. Weemploy a Galactic model to convert this distribution from dimensionless tophysical units, \alpha/au and M_E. The survey sensitivity to small planets ishighest in the range 1 to 4 au, shifting to slightly larger separations formore massive ones.

The OGLE-III planet detection efficiency from six years of microlensing observations (2003 to 2008)