  Numerical simulations predict that some poor groups of galaxies have merged
by the present epoch into giant ellipticals (cf. Barnes 1989). To identify the
possible remnants of such mergers, we have compiled a sample of nearby,
isolated ellipticals (Colbert, Mulchaey, & Zabludoff 1998). ASCA observations
of the first galaxy studied, NGC 1132 reveal an X-ray halo that extends out to
at least 250 kpc. The temperature, metallicity and luminosity of NGC 1132's
X-ray halo are comparable to those of poor group halos. The total mass inferred
from the X-ray emission is also like that of an X-ray detected group. Optical
imaging uncovers a dwarf galaxy population clustered about NGC 1132 that is
consistent in number density and in projected radial distribution with that of
an X-ray group. The similarities of NGC 1132 to poor groups in both the X-ray
band and at the faint end of the galaxy luminosity function, combined with the
deficit of luminous galaxies in the NGC 1132 field, are compatible with the
merged group picture. Another possibility is that the NGC 1132 system is a
`failed' group (i.e., a local overdensity in which other bright galaxies never
formed).
