UV Spectroscopy of Emission Line Gas in the Central Galaxies of X-Ray Luminous Clusters

Details UV Spectroscopy of Emission Line Gas in the Central Galaxies of X-Ray Luminous Clusters UV Spectroscopy of Emission Line Gas in the Central Galaxies of X-Ray Luminous Clusters

Jul 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984iue..prop.1819h&link_type=abstract

IUE Proposal ID #EGGEH

Computer Science

Scientific paper

Optical spectroscopy of the central galaxies in a number of clusters reported to have X-ray cooling flows has revealed low ionization emission line systems similar to those seen in narrow line radio galaxies (NLRG's). Line ratios in [NII] and [SII] indicate temperatures of 10^4 K and densities of 10^2 _ 10^3 cm^3. The Balmer decrements for these systems are unusually high, with characteristic values of 5-6. Comparison of colors and spectra with those of giant ellipticals and central cluster galaxies lacking emission line systems indicate that these lines-of-sight are not affected by global reddening. If dust is responsible for the high H-alpha/H-beta ratios it must be locally distributed within the emitting regions. A test of this hypothesis can be made by measuring the Ly-alpha/H-alpha flux.

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