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