  We present a Chandra study of the metal distribution in the X-ray bright
compact group of galaxies HCG 62. We find that the diffuse X-ray emission is
peaked at the core of the central galaxy NGC 4778, and is dominated by the
contribution of the hot gas. The diffuse emission is roughly symmetric within
\simeq0.25^{\prime}, which is straddled by double-sided X-ray cavities aligned
in the northeast-southwest direction. By mapping the emission hardness ratio
distributions and by performing the 2-dimensional spectral analysis, we
identify a remarkable high-abundance arc region at about 2^{\prime}
(33.6h_{70}^{-1} kpc) from the X-ray peak that spans over a vast region from
south to northwest, a part of which roughly coinciding with the outer edge of
the southwest X-ray cavity. The measured average abundance in this arc is
higher than that in its neighboring regions by a factor of about 2, and the
abundance ratios therein are nicely consistent with the dominance of the SN Ia
yields. We estimate that the mass of iron contained in the arc is >3\times
10^{6}h_{70}^{-2.5} solar mass, which accounts for >3% of the iron synthesized
in the galaxy. The high-abundance arc could have been formed by the AGN
activities. However, it is also possible that the arc was formed in a recent
merger as is implied by the recent optical kinematic study (Spavone et al.
2006), which implies that mergers may be as important as AGN activities in
metal redistributions in early-type galaxies and their associated groups or
clusters.
