  We analyze the ASCA spectra accumulated within ~100 kpc radii of 12 of the
brightest groups of galaxies. Upon fitting isothermal models (1T) jointly to
the ASCA SIS and GIS spectra we obtain fits for most groups that are of poor or
at best marginal quality and give very sub-solar metallicities similar to
previous studies, <Z> = 0.29 +/- 0.12 Z_sun. Two-temperature models (2T)
provide significantly better fits for 11 out of the 12 groups and in every case
have metallicities that are substantially larger than obtained for the 1T
models, <Z> = 0.75 +/- 0.24 Z_sun. Although not very well constrained, for most
of the groups absorption in excess of the Galactic value is indicated for the
cooler temperature component of the 2T models. A simple multiphase cooling flow
model gives results analogous to the 2T models including large metallicities,
<Z> = 0.65 +/- 0.17 Z_sun. The nearly solar Fe abundances and also solar
alpha/Fe ratios indicated by the 2T and cooling flow models are consistent with
models of the chemical enrichment of ellipticals, groups, and clusters which
assume ratios of Type Ia to Type II supernova and an IMF similar to those of
the Milky Way.
  Thus, we have shown that the very sub-solar Fe abundances and Si/Fe
enhancements obtained from most previous studies within r ~100 kpc of galaxy
groups are an artifact of their fitting isothermal models to the X-ray spectra
which also has been recently demonstrated for the brightest elliptical
galaxies. Owing to the importance of these results for interpreting X-ray
spectra, in an appendix we use simulated ASCA observations to examine in detail
the ``Fe bias'' and ``Si bias'' associated with the spectral fitting of
ellipticals, groups, and clusters of galaxies.
