Astronomy and Astrophysics – Astronomy
Scientific paper
Nov 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987mnras.229..119s&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 229, Nov. 1, 1987, p. 119-128. Research supported by th
Astronomy and Astrophysics
Astronomy
3
Elliptical Galaxies, Stellar Motions, Velocity Distribution, Astronomical Models, Black Holes (Astronomy), Brightness, Galactic Nuclei, Stellar Mass Accretion, Virgo Galactic Cluster
Scientific paper
The distribution of stars formed from the cooling flow in M87 has been calculated assuming that the system is spherically symmetric, that the stars follow radial orbits, and that the gas inflow rate has not varied over a Hubble time. The authors find that, while such "cooling flow" stars cannot significantly affect the dynamics of M87, they can affect the observed kinematics: a relatively small population of stars on nearly radial orbits can cause a dramatic increase in the line-of-sight velocity dispersion in the central regions. The cooling flow population in M87 can explain in detail the observed radial dependence of stellar velocity dispersion in this galaxy if this population has roughly the same mass function as in the initial galaxy. Thus, the existence of a super-massive black hole in the centre of M87 is not demanded by the observed high central velocity dispersions.
Sanders Robert H.
Soares Domingos S. L.
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