  The past decade and a half has seen the design and execution of several
ground-based spectroscopic surveys, both Galactic and Extra-galactic.
Additionally, new surveys are being designed that extend the boundaries of
current surveys. In this context, many important considerations must be done
when designing a spectrograph for the future. Among these is the determination
of the optimum wavelength coverage. In this work, we present a new code for
determining the wavelength ranges that provide the optimal amount of
information to achieve the required science goals for a given survey. In its
first mode, it utilizes a user-defined list of spectral features to compute a
figure-of-merit for different spectral configurations. The second mode utilizes
a set of flux-calibrated spectra, determining the spectral regions that show
the largest differences among the spectra. Our algorithm is easily adaptable
for any set of science requirements and any spectrograph design. We apply the
algorithm to several examples, including 4MOST, showing the method yields
important design constraints to the wavelength regions.
