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 \simeq 0.25 ^ { \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 } ( 33.6 h _ { 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 } M _ { \odot } , 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 .