This process is experimental and the keywords may be updated as the learning algorithm improves.ĭ.M. These keywords were added by machine and not by the authors. The total energies deposited by radio jets exceed the losses from the gas due to radiative cooling, indicating that radio sources are energetically capable of heating the cooling core gas and preventing rapid cooling. The radio bubbles can be used to estimate the total energy output of the radio jets. Low frequency radio observations show that many of the ghost bubbles have radio emission in general, these long wavelength observations show that radio sources are much larger and involve greater energies than had been previously thought. “Ghost bubbles” are often seen at larger radii in clusters and galaxies these bubbles are faint in high radio frequencies, and are believed to be old radio bubbles which have risen buoyantly in the hot gas. Similar radio bubbles are seen in groups and individual early-type galaxies. X-ray observations show many examples of X-ray holes in the central regions of brightest-cluster galaxies in many cases, the X-ray holes are filled with radio lobes. Recent theoretical and observational results on the role of feedback from AGN at the centers of elliptical galaxies on their interstellar gas are reviewed. On the other hand, most bright galaxies in clusters do manage to retain small coronae of X-ray emission. X-ray observations show many examples of nearby galaxies which are undergoing gas stripping. In general, the X-ray halos of early-type galaxies tend to be smaller and fainter in denser environments, with the exception of group-central galaxies. The role of the environment of an elliptical galaxy on its hot interstellar gas is discussed.
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