Evolution of Gas in Elliptical Galaxies

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dc.creatorMathews, William G.
dc.creatorBrighenti, Fabrizio
dc.date2000-10-02
dc.date.accessioned2026-07-07T01:55:46Z
dc.date.available2026-07-07T01:55:46Z
dc.descriptionWe 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.
dc.description4 pages; to appear in "Gas and Galaxy Evolution" ASP Conf. Ser. eds. Hibbard, Rupen & van Gorkom
dc.identifierhttps://arxiv.org/abs/astro-ph/0010040
dc.identifierhttp://arxiv.org/abs/astro-ph/0010040
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/1772
dc.subjectAstrophysics
dc.titleEvolution of Gas in Elliptical Galaxies
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