![]() | Annu. Rev. Astron. Astrophys. 1994. 32:
531-590 Copyright © 1994 by Annual Reviews. All rights reserved |
The observational evidence for dark matter arises in many different contexts and baryonic dark matter is not necessarily implicated in all of these. We therefore begin by identifying the observational issues most relevant to the baryonic versus nonbaryonic dilemma.
2.1. Local Dark Matter
Measurements of the stellar velocity and density distribution
perpendicular to
the Galactic disk provide an estimate of the total disk density. This
turns out to be about 0.1
M
pc-3 and it has long been suspected
(Oort 1932)
that this
exceeds the density in visible stars. The possibility of disk dark
matter is very
important in the present context because - of all the dark matter
problems - this
is the one most likely to have a baryonic solution. Unfortunately,
the evidence is very controversial. Bahcall
(1984a,
b,
c)
used counts of F dwarfs and K giants
to conclude that the density of unseen material must be at least 50% that of
the visible material. He also concluded that the disk dark matter must
have an
exponential scale height of less than 700 pc, so that it must itself be
confined
to a disk. However, Bahcall assumed a particular model and
Bienayme et al (1987),
using a different model, found a best-fit dark matter density of only
0.01 M
pc-3, and even this could be removed if the halo was slightly
flattened.
Knapp (1988)
came to the same conclusion by studying the velocity dispersion
and scale height of molecular hydrogen. Further doubt was cast in a
series of papers by
Kuijken & Gilmore (1989),
who used the full distribution function for
the velocities and distances of K dwarfs rather than assuming a
particular model. Although
Gould (1990)
used a maximum likelihood analysis to conclude that
Kuijken & Gilmore's data were not inconsistent with the Bahcall et al claim,
Kuijken & Gilmore (1991)
disagreed with this. More recently,
Bahcall et al (1992a)
have concluded from another analysis of K giants that the
no-disk-dark-matter
hypothesis is only consistent with the data at the 14% level and
their best-fit model has a dark density of 0.15
M
pc-3, which corresponds to
53% more dark matter than visible matter. For present purposes the existence
of disk dark matter will be regarded as an open question.