The distribution and morphology of X-ray-emitting gas in the core of the Perseus cluster

Details The distribution and morphology of X-ray-emitting gas in the core of the Perseus cluster The distribution and morphology of X-ray-emitting gas in the core of the Perseus cluster

Aug 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...248...47f&link_type=abstract

Astrophysical Journal, Part 1, vol. 248, Aug. 15, 1981, p. 47-54. Research supported by the Radcliffe Trust;

Astronomy and Astrophysics

Astrophysics

295

Galactic Clusters, Galactic Structure, Intergalactic Media, Interstellar Gas, Mass Distribution, X Ray Sources, Brightness Distribution, Gas Density, Gas Temperature, Heao 2, Spatial Distribution, Temperature Profiles

Scientific paper

An unresolved source has been found coincident with the nucleus of NGC 1275 in a high-resolution X-ray image of the core of the Perseus cluster. Absorption in the optical features at high velocity with respect to NGC 1275, which are thought to be associated with a foreground galaxy, does not produce any detectable X-ray absorption. The emission tends to become asymmetric in the presence of the lower-velocity filaments, but no obvious, detailed correlation is found between X-ray enhancements and individual filaments. Deprojection of surface brightness to yield temperature and density profiles of the intracluster gas shows results consistent with a quasi-hydrostatic radiative accretion flow onto NGC 1275, and the pressure-driven mass inflow onto the central galaxy is then 200-400 solar masses/yr. The possibility of a problem in the relation of line-of-sight velocity dispersion to cluster gravitational mass is confirmed.

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