  We present a systematic investigation of X-ray thermal coronae in 157
early-type galaxies and 22 late-type galaxies from a survey of 25 hot (kT>3
keV), nearby (z<0.05) clusters, based on CHANDRA archival data. Cool galactic
coronae (kT=0.5-1.1 keV generally) have been found to be very common, >60% in
NIR selected galaxies that are more luminous than 2L*, and >40% in L* < L_Ks <
2L* galaxies. These embedded coronae in hot clusters are generally smaller
(1.5-4 kpc radii), less luminous (<~ 10^41 erg s^-1), and less massive
(10^6.5-10^8 M_solar}) than coronae in poor environments, demonstrating the
negative effects of hot cluster environments on galactic coronae. Nevertheless,
these coronae still manage to survive ICM stripping, evaporation, rapid
cooling, and powerful AGN outflows, making them a rich source of information
about gas stripping, microscopic transport, and feedback processes in the
cluster environment. Heat conduction across the boundary of the coronae has to
be suppressed by a factor of >100, which implies the X-ray gas in early-type
galaxies is magnetized and the magnetic field plays an important role in energy
transfer. Stripping through transport processes (viscosity or turbulence) also
needs to be suppressed by at least a factor of ten at the coronal boundary...
(abridged) Diffuse thermal coronae have also been detected in at least 8 of 22
late-type (Sb or later) galaxies in our sample. Evidence for enhanced star
formation triggered by the ICM pressure has been found in four late-type
galaxies. The fraction of luminous X-ray AGN (>10^41 ergs s^-1) is not small (~
5%) in our sample.
