We make a quantitative prediction for the detection rate of orphan GRB afterglows as a function of flux sensitivity in X-ray, optical, and radio wavebands, based on a recent model of collimated GRB afterglows. We find that the orphan afterglow rate strongly depends on the opening angle of the jet (roughly ∝θ_jet^-2), as expected from simple geometrical consideration, if the total jet energy is kept constant as suggested by recent studies. The relative beaming factor b_rel, i.e., the ratio of

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... afterglow rate including orphans to those associated with observable prompt GRBs, could be as high as b_rel > 100 for searches deeper than R 24, depending on afterglow parameters. To make the most plausible predictions, we average the model emission for ten sets of afterglow parameters obtained through fits to ten well-observed, collimated GRB jets, weighted by the sky coverage of each jet. Our model expectations are consistent with the results (or constraints) obtained by all past searches. We estimate the number of orphan afterglows in the first 1500deg^2 field of the SDSS to be about 0.2. The relative beaming factor b_rel is rapidly increasing with the search sensitivity: b_rel 3 for the SDSS sensitivity to transient objects in the northern sky (R 19), 14 for the past high-z supernova searches (R 23), and 50 for the sensitivity of the Subaru Suprime-Cam (R 26). Predictions are made for the current facilities and future projects in X-ray, optical, and radio bands. Among them, the southern-sky observation of the SDSS (sensitive to transients down to R 23) could detect 40 orphan afterglows during the five-year operation. Allen Telescope Array would find about 200 afterglows in a radio band at 0.1-1mJy with b_rel 15.