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We present a Chandra study of the metal distribution in the X-ray brightcompact group of galaxies HCG 62. We find that the diffuse X-ray emission ispeaked at the core of the central galaxy NGC 4778, and is dominated by thecontribution of the hot gas. The diffuse emission is roughly symmetric within\simeq0.25^{\prime}, which is straddled by double-sided X-ray cavities alignedin the northeast-southwest direction. By mapping the emission hardness ratiodistributions and by performing the 2-dimensional spectral analysis, weidentify 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 fromsouth to northwest, a part of which roughly coinciding with the outer edge ofthe southwest X-ray cavity. The measured average abundance in this arc ishigher than that in its neighboring regions by a factor of about 2, and theabundance ratios therein are nicely consistent with the dominance of the SN Iayields. We estimate that the mass of iron contained in the arc is >3\times10^{6}h_{70}^{-2.5} solar mass, which accounts for >3% of the iron synthesizedin the galaxy. The high-abundance arc could have been formed by the AGNactivities. However, it is also possible that the arc was formed in a recentmerger as is implied by the recent optical kinematic study (Spavone et al.2006), which implies that mergers may be as important as AGN activities inmetal redistributions in early-type galaxies and their associated groups orclusters.Comment: 20 pages, 5 figures, accepted for publication in Ap

A High‐Abundance Arc in the Compact Group of Galaxies HCG 62: An AGN‐ or Merger‐Induced Metal Outflow?