Given the observed complexity of Galactic UV extinction, what is the best way to deredden an observed energy distribution? There are three different possibilities, which involve the use of a global mean extinction curve, an R-dependent curve, and a sightline-specific curve. These three alternatives and their inherent uncertainties are discussed below, and a new derivation of the shape of the average IR-through-UV extinction curve is presented. A more thorough discussion of the uncertainties involved in UV extinction corrections is given by Massa (1987).