Classifying the spectral types of individual components of composite spectrum stars can be a difficult task. Markowitz (1969) discussed the problems of blended and veiled lines associated with the visual assessment of blue spectrograms. Although synthetic spectra (i.e. formed by the intentional superposition of two different spectra) can be used as a means of calibration, the classification of composites with slit spectrograms is a subjective process. Classifications based upon broad- and intermediate-band photometry (Young 1971) can be highly objective, but the lack of spectral resolution introduces other complications. For example, colors in the UBVR system measure the gross behavior of a star's energy distribution. Results based upon this information are not only affected by interstellar reddening but also are incapable of identifying common spectral peculiarities. The use of spectrophotometric indices (Beavers and Cook 1980) avoids the major difficulties of other techniques. The results are not influenced by the veiling or blending of lines, nor are the results influenced by interstellar reddening. If a sufficient number of features are observed, common types of spectral peculiarities can be identified.