We present results from a deep (174 ks) Chandra observation of the FR-II radio galaxy 3C 220.1, the central brightest cluster galaxy (BCG) of a $kT sim$ 4 keV cluster at $z=0.61$. The temperature of the hot cluster medium drops from $sim5.9$ keV to $sim3.9$ keV at $sim$ 35 kpc radius, while the temperature at smaller radii may be substantially lower. The central active galactic nucleus (AGN) outshines the whole cluster in X-rays, with a bolometric luminosity of $2.0times10^{46}$ erg s$^{-1}$ ($sim10$% of the Eddington rate). The system shows a pair of potential X-ray cavities $sim35$ kpc east and west of the nucleus. The cavity power is estimated within the range of $1.0times10^{44}$ erg s$^{-1}$ and $1.7times10^{45}$ erg s$^{-1}$, from different methods. The X-ray enhancements in the radio lobes could be due to inverse Compton emission, with a total 2-10 keV luminosity of $sim8.0times10^{42}$ erg s$^{-1}$. We compare 3C 220.1 with other cluster BCGs, including Cygnus A, as there are few BCGs in rich clusters hosting an FR-II galaxy. We also summarize the jet power of FR-II galaxies from different methods. The comparison suggests that the cavity power of FR-II galaxies likely under-estimates the jet power. The properties of 3C 220.1 suggest that it is at the transition stage from quasar-mode feedback to radio-mode feedback.
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