Annu. Rev. Astron. Astrophys. 1991. 29:
239-274 Copyright © 1991 by Annual Reviews. All rights reserved |
3.5.1
High spatial resolution observations of nearby galaxies have indicated
M / L
values that increase sharply in the nuclear regions. These are usually
interpreted with supermassive black holes, but a cluster of dark remnants
cannot be excluded for most cases
(291). Nearby
well-studied systems are M31
(98,
191,
291)
and M32
(98,
291,
330).
The inferred black hole masses are
106 - 107 M and 107 -
108 M, respectively. A similar
increase in M / L was found for NGC 4594
(176,
192), and
corresponds to a black hole mass of around 109
M. Surprisingly, the
case is weakest for M87, a known active galaxy. The early claims of a
detection of a central black hole
(301,
377)
were based mostly on surface photometry and velocity dispersions. It was soon
realized that anisotropies in the velocity dispersion, and a non-stellar
contribution to the light, can explain the observations with a constant
M / L model
(45,
101,
261).
More recent data
can be modeled with only a modest anisotropy in the velocity distribution
(73,
99).
The requirement that these models are
stable provides an extra constraint
(238),
but the stability of the most recent models has not been studied.
The evidence for nuclear black holes in M31, M32 and NGC 4594 rests on curves
of velocity dispersions and rotation. Modeling this type of data is not
straightforward, as it involves the coupled deconvolution of the surface
brightness, radial velocity and velocity dispersion profiles. This makes it
difficult to search the complete solution space. The models employed are
usually assumed to be spherical or axisymmetric
(46), but to date
no axisymmetric models based on explicit distribution functions f
0 have
been constructed. Additional information is contained in the line profiles
(71,
233,
290),
which can now be derived from
digital spectra. Application of this powerful technique may well put much
tighter constraints on the behavior of M / L.
Gerhard has argued that the rapid central rotation in M31, M32 and NGC 4594
can be produced by a small bar which is viewed down its major axis
(138).
This hypothesis can be tested by observing a larger sample of
galaxies, for which one would expect random viewing angles.