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Title:
The mass profile and gas content of M87
Authors:
Stewart, G. C.; Canizares, C. R.; Fabian, A. C.; Nulsen, P. E. J.
Affiliation:
AA(Cambridge University, Cambridge, England), AB(Cambridge University, Cambridge, England), AC(Cambridge University, Cambridge, England)
Publication:
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 278, March 15, 1984, p. 536-543. Research supported by the Royal Society. (ApJ Homepage)
Publication Date:
03/1984
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
Elliptical Galaxies, Galactic Structure, Intergalactic Media, Interstellar Gas, Mass Distribution, X Ray Sources, Gas Heating, Gas Temperature, Mass Flow Rate
DOI:
10.1086/161820
Bibliographic Code:
1984ApJ...278..536S

Abstract

The structure of the hot gas and gravitating matter around M87 is constrained using both X-ray images and spectroscopic observations, particularly of the Fe L lines. The data are previously published results from the four focal plane instruments of the Einstein Observatory. Models in which the gravitating mass has a core radius of ≡25 kpc are favored, suggesting that the material is associated with M87 rather than with the Virgo cluster as a whole. The gas structure is consistent with a radiative accretion flow with a mass accretion rate that varies with radius as M≡ 3(R/10 kpc)2/3 M_sun; yr-1 from ≡1 to 70 kpc. About 1 M_sun; yr-1 flows into the central few arcsec of the galaxy.

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