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S0 galaxies are often thought to be passively evolved from spirals after starformation is quenched. To explore what is occurring in S0s, we present amulti-wavelength study of NGC5866--an isolated nearby edge-on S0. This studyshows strong evidence for dynamic activities in the interstellar medium, whichare most likely driven by supernova explosions in the galactic disk and bulge.We utilize Chandra, HST, and Spitzer data as well as ground-based observationsto characterize the content, structure, and physical state of the medium andits interplay with stars in NGC5866. A cold gas disk is detected with anexponential scale height of 100pc. Numerous off-disk dusty spurs are clearlypresent: prominent ones can extend as far as 300pc from the galactic plane andare probably produced by individual SNe, whereas faint filaments can have ~ kpcscale and are likely produced by SNe collectively in disk/bulge. We also detectsubstantial amounts of diffuse Ha- and Pa-emitting gas with a comparable scaleheight as the cold gas. We find that the heating of the dust and warm ionizedgas cannot be explained by the radiation from evolved stars alone, stronglyindicating the presence of young stars in the disk at a low formation rate of ~0.05Msun/yr. We reveal the presence of diffuse X-ray-emitting hot gas, whichextends as far as 3.5kpc from the disk and can be heated easily by Type Ia SNein the bulge. However, the temperature of this gas is ~ 0.2keV, substantiallylower than what might be expected from the mass-loss of evolved stars and TypeIa SNe heating alone, indicating mass loading from cool gas is important. Thetotal masses of the cold, warm and hot gases are ~ 5*10^8, 10^4 and 3*10^7Msun.The relative richness of the gases, undergoing circulations between disk/halo,is perhaps a result of its relative isolation.

Dynamic S0 Galaxies: a Case Study of NGC 5866