  To determine the relative contributions of galactic and intracluster stars to
the enrichment of the intracluster medium (ICM), we present X-ray surface
brightness, temperature, and Fe abundance profiles for a set of twelve galaxy
clusters for which we have extensive optical photometry. Assuming a standard
IMF and simple chemical evolution model scaled to match the present-day cluster
early-type SN Ia rate, the stars in the brightest cluster galaxy (BCG) plus the
intracluster stars (ICS) generate 31^{+11}_{-9}%, on average, of the observed
ICM Fe within r_{500} (~ 0.6 times r_{200}, the virial radius). An alternate,
two-component SN Ia model (including both prompt and delayed detonations)
produces a similar BCG+ICS contribution of 22^{+9}_{-9}%. Because the ICS
typically contribute 80% of the BCG+ICS Fe, we conclude that the ICS are
significant, yet often neglected, contributors to the ICM Fe within r_{500}.
However, the BCG+ICS fall short of producing all the Fe, so metal loss from
stars in other cluster galaxies must also contribute. By combining the
enrichment from intracluster and galactic stars, we can account for all the
observed Fe. These models require a galactic metal loss fraction
(0.84^{+0.11}_{-0.14}) that, while large, is consistent with the metal mass not
retained by galactic stars. The SN Ia rates, especially as a function of galaxy
environment and redshift, remain a significant source of uncertainty in further
constraining the metal loss fraction. For example, increasing the SN Ia rate by
a factor of 1.8 -- to just within the 2 sigma uncertainty for present-day
cluster early-type galaxies -- allows the combined BCG + ICS + cluster galaxy
model to generate all the ICM Fe with a much lower galactic metal loss fraction
(~ 0.35).
