  Studying the internal dynamics of stellar clusters is conducted primarily
through N-Body simulations. One of the major inputs into N-Body simulations is
the binary star frequency and mass distribution, which is currently constrained
by relations derived from field binary stars. However to truly understand how
clustered environments evolve, binary data from within star clusters is needed
including masses. Detailed information on binaries masses, primary and
secondary, in star clusters has been limited to date. The primary technique
currently available has been radial velocity surveys that are limited in depth.
Using previous two-band photometry-based studies that may cover different mass
ranges produce potentially discrepant interpretations of the observed binary
population. We introduce a new binary detection method, Binary INformation from
Open Clusters Using SEDs (BINOCS) that covers the wide mass range needed to
improve cluster N-body simulation inputs and comparisons. Using newly-observed
multi-wavelength photometric catalogs (0.3 - 8 microns) of the key open
clusters with a range of ages, we can show that the BINOCS method determines
accurate binary component masses for unresolved cluster binaries through
comparison to available RV-based studies. Using this method, we present results
on the dynamical evolution of binaries from 0.4 - 2.5 solar masses within five
prototypical clusters, spaning 30 Myr to 3.5 Gyr, and how the binary
populations evolve as a function of mass.
