  Window functions describe, as a function of orbital period, the probability
that an existing planetary transit is detectable in one's data for a given
observing strategy. We show the dependence of this probability upon several
strategy and astrophysical parameters, such as length of observing run,
observing cadence, length of night, and transit duration. The ability to detect
a transit is directly related to the intrinsic noise of the observations. In
our simulations of the window function, we explicitly address non-correlated
(gaussian or white) noise and correlated (red) noise and discuss how these two
different noise components affect window functions in different manners.
