Evolution of Gas in Elliptical Galaxies

William G. Mathews (University of California , Santa Cruz , CA) , Fabrizio Brighenti (University of California , Dipartimento di Astronomia , Universita di Bologna)

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classification 🌌 astro-ph

keywords ellipticalgalaxiesinterstellarcoolingmassstarsx-raybottom-heavy

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We review the origin and structure of hot (cooling flow) gas in elliptical galaxies. X-ray observations can be used to determine the stellar mass to light ratio, the mass profiles of dark matter halos, and the interstellar magnetic field. Interstellar gas cools over a large volume, forming stars with a bottom-heavy IMF. For consistency with the thin fundamental plane, young stars must be optically luminous. Circular X-ray isophotes in rotating elliptical galaxies indicate distributed radiative cooling or strong interstellar turbulence.

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Evolution of Gas in Elliptical Galaxies

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