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One of the major sources of X-ray emitting hot gas around galaxies is thefeedback from supernovae (SNe), but most of this metal-enriched feedbackmaterial is often not directly detected in X-ray observations. This missinggalactic feedback problem is extremely prominent in early-type galaxy bulgeswhere there is little cool gas to make the SNe ejecta radiate at lowertemperature beyond the X-ray domain. We herein present a deep Suzakuobservation of an S0 galaxy NGC5866, which is relatively rich in molecular gasas an S0 galaxy and shows significant evidence of cool-hot gas interaction. Byjointly analyzing the Suzaku and an archival Chandra data, we measure the Fe/Oabundance ratio to be $7.63_{-5.52}^{+7.28}$ relative to solar values. Thisabundance ratio is much higher than those of spiral galaxies, and even amongthe highest ones of S0 and elliptical galaxies. NGC5866 also simultaneously hasthe highest Fe/O abundance ratio and molecular gas mass among a small sample ofgas-poor early-type galaxies. An estimation of the Fe budget indicates thatNGC5866 could preserve a larger than usual fraction, but far from the totalamount of Fe injected by Type Ia SNe. We also find that the hot gas temperatureincreases from inner to outer halos, with the inner halo has a temperature of~0.25keV, clearly lower than that expected from Type Ia SNe heating. This lowtemperature could be most naturally explained by additional cooling processesrelated to the cool-hot gas interaction as being indicated by the existence ofmany extraplanar dusty filaments. Our results indicate that the large cool gascontent and the presence of cool-hot gas interaction in the inner region ofNGC5866 have significantly reduced the specific energy of the SN ejecta and sothe velocity of galactic outflow. The galaxy could thus preserve a considerablefraction of metal-enriched feedback material from being blown out.

Do We Detect the Galactic Feedback Material in X-ray Observations of Nearby Galaxies? - A Case Study of NGC 5866