X-ray and optical emission-line filaments in the cooling flow cluster 2A 0335 + 096

Details X-ray and optical emission-line filaments in the cooling flow cluster 2A 0335 + 096 X-ray and optical emission-line filaments in the cooling flow cluster 2A 0335 + 096

Sep 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...397l..31s&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 397, no. 1, p. L31-L34.

Astronomy and Astrophysics

Astrophysics

43

Cooling Flows (Astrophysics), Emission Spectra, Galactic Clusters, X Ray Spectra, H Alpha Line, Radio Sources (Astronomy), Rosat Mission, Spaceborne Astronomy, X Ray Imagery

Scientific paper

We present a new high-resolution X-ray image of the 2A 0335 + 096 cluster of galaxies obtained with the High Resolution Imager (HRI) aboard the ROSAT satellite. The presence of dense gas having a very short cooling time in the central regions confirms its earlier identification as a cooling flow. The X-ray emission from the central regions of the cooling flow shows a great deal of filamentary structure. Using the crude spectral resolution of the HRI, we show that these filaments are the result of excess emission, rather than foreground X-ray absorption. Although there are uncertainties in the pointing, many of the X-ray features in the cooling flow region correspond to features in H-alpha optical line emission. This suggests that the optical emission line gas has resulted directly from the cooling of X-ray-emitting gas. The filament material cannot be in hydrostatic equilibrium, and it is likely that other forces such as rotation, turbulence, and magnetic fields influence the dynamical state of the gas.

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