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We report the results of high-resolution subpixel imaging of the hardcontinuum and Fe K{\alpha} line of the Compton Thick (CT) Active GalacticNucleus (AGN) ESO 428-G014, observed with Chandra ACIS. While the 3-4 keVemission is dominated by an extended component, a single nuclear point sourceis prominent in the 4-6 keV range. Instead, two peaks of similar intensity,separated by ~36 pc in projection on the plane of the sky are detected in theFe K{\alpha} emission. The SE knot could be marginally associated with theheavily obscured hard continuum source. We discuss four possibleinterpretations of the nuclear morphology. (1) Given the bolometric luminosityand likely black hole (BH) mass of ESO 428-G014, we may be imaging two clumpsof the CT obscuring torus in the Fe K{\alpha} line. (2) The Fe K{\alpha} knotsmay be connected with the fluorescent emission from the dusty bicone, or (3)with the light echo of a nuclear outburst. (4) We also explore the less likelypossibility that we may be detecting the rare signature of merging nuclei.Considering the large-scale kpc-size extent of the hard continuum and FeK{\alpha} emission (Papers I and II), we conclude that the AGN in ESO 428-G014has been active for at least 104 yrs. Comparison with the models of Czerny etal (2009) suggests high accretion rates during this activity.

Deep Chandra Observations of ESO 428-G014: IV. The Morphology of the Nuclear Region in the Hard Continuum and Fe K{\alpha} Line