Dynamical, physical, and chemical properties of emission-line nebulae in cooling flows

Details Dynamical, physical, and chemical properties of emission-line nebulae in cooling flows Dynamical, physical, and chemical properties of emission-line nebulae in cooling flows

Mar 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...338...48h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 338, March 1, 1989, p. 48-77. Research supported by the Alfred P. Sloan Fou

Astronomy and Astrophysics

Astrophysics

379

Astronomical Spectroscopy, Cooling Flows (Astrophysics), Emission Spectra, Galactic Clusters, Nebulae, Brightness Distribution, Chemical Properties, Elliptical Galaxies, H Alpha Line, Physical Properties, Very Large Array (Vla)

Scientific paper

The results are reported of a program of long-slit spectroscopy, narrow-band imaging, and VLA mapping of the optical emission-line gas and nonthermal radio continuum emission associated with the dominant galaxy in nine galaxy clusters with cooling flows. All the observed emission-line nebulae are very strongly centrally concentrated with typical characteristic radii of 5 kpc or less. If the mass inflow rate varies linearly with radius in cooling flows out to large radii, then the H-alpha surface brightness does not trace the cooling rate. The velocity field of the emission-line gas provides little evidence for organized rotation or shear. This result can be understood if the emission-line filaments condense out of an intracluster medium in which angular momentum has been transported radially outward. Electron densities are measured over spatially resolved regions and are found to by typically a few hundred per cu cm. Spatial variations in the emission-line ratios in the nebulae agree better with shock models than with photoionization models. The various possible mechanisms for heating and ionizing the emission-line nebulae are discussed.

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