  We review estimates of the metallicities in elliptical galaxies, with an
emphasis on recent results from the ASCA satellite. X-ray spectra of elliptical
galaxies are adequately fit by models consisting of hot gas with subsolar Fe
abundance and roughly solar Si-to-Fe ratio, plus a hard component from an
ensemble of X-ray binaries. Although complications in the form of an extra soft
continuum or multiple phases can be considered, we show that the consistency of
the Si line diagnostic and continuum temperatures demonstrates that the data --
at the present level of sensitivity and spectral resolution -- do not require
these. Optical and X-ray Fe abundance estimates are converging, although there
are some cases with anomalously low X-ray values. Subsolar elliptical galaxy
abundances require serious reconsideration of our preconceptions about
elliptical galaxy chemical evolution, intracluster enrichment, and Type Ia
supernova rates.
