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Title:
The distribution and morphology of X-ray-emitting gas in the core of the Perseus cluster
Authors:
Fabian, A. C.; Hu, E. M.; Cowie, L. L.; Grindlay, J.
Affiliation:
AA(Cambridge University, Cambridge, England), AB(Carnegie Institution of Washington, Washington, DC), AC(Princeton University, New Observatory, Princeton, NJ)
Publication:
Astrophysical Journal, Part 1, vol. 248, Aug. 15, 1981, p. 47-54. Research supported by the Radcliffe Trust; (ApJ Homepage)
Publication Date:
08/1981
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
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
DOI:
10.1086/159128
Bibliographic Code:
1981ApJ...248...47F

Abstract

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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