One of the most important techniques used in astronomy is spectroscopy, The receivable photons from the currently most interesting stellar objects are typically quite low. The investigation of such spectra emphasizes consideration of noise, information density, and quantum efficiency. The two major detector techniques are photographic and electronic. The photographic methods are superior for information density and are lacking in quantum efficiency and low noise; whereas, the electronic methods typically have comparatively low information density, but are capable of significantly superior noise and quantum efficiency performance. Considerable improvement in many areas in applying the electronic methods is possible. We will discuss here an electronic device which significantly improves the spectroscopists' capability to detect and measure very faint spectra with comparatively higher inf ormation density and higher accuracy than is usual with similar techniques.