2.4.1. Warm Plasma in Groups
Some surveys are available from low energy X-ray observations with ROSAT (Mulchaey et al. 1996). The X-ray emission from 18 groups with total mass ranging from 1.2 to 8.3 x 1013h M corresponds to plasma mass fractions ranging from 0.004h-3/2 (H97) to 0.09h-3/2 (NGC 4261). The average is
significantly below the number for clusters
(eq. [18]). In fact the baryon fraction shows a trend
increasing with the group mass, approaching to the cluster value
at the high mass end. This could be because groups are
intrinsically poorer in plasma, or because much of the plasma is
cooler and so escapes detection as an X-ray source. The latter is
in line with the shallower gravitational potential wells in
groups. The cool plasma clouds detected by Lyman-
resonance absorption (Section 2.4.2) similarly
are not
detected as X-ray sources. Thus the plasma identifiable from its
discrete X-ray emission might be considered a lower limit to the
net plasma associated with groups of galaxies.
To convert equation (23) into a mean baryon density we
need the mean gravitational mass associated with field galaxies
(which almost always are in groups).
The following measures may be compared.
First, we can extrapolate the
Bahcall-Cen (1993)
mass function
(eq. [15]), which they determined for
M > 1013h M, to systems with the mass
characteristic of
galaxies, M ~ 1012h M. The result of integrating this
mass function from M = 1012h M to M =
1014h M is
The cutoff is the characteristic mass of an L* galaxy, the
minimum for a group.
Second, we have dynamical mass measures from analyses of systems
of galaxies on scales smaller than about 10h-1 Mpc and
outside the rich clusters. The survey of results of these analyses by
Bahcall, Lubin & Dorman
(1995)
indicates Mgrav/L (200+100-50)h. This with
the mean luminosity density in equation (4) gives
Third, we can use the luminosity density,
scaling from M/L calibrated in the great clusters by taking
account of the difference in luminosities from the difference in
morphological mixes (see also
Carlberg et al. 1997).
The small scatter in the
color-magnitude relation for ellipticals and the spheroid
components of spirals suggests these stars formed early,
so it is reasonable to assume that the ratio of spheroid luminosity
to gravitational mass is
the same in clusters and the field. It would follow that the
cosmic mean mass-to-spheroid-light ratio is
(M/LB)cos =
(Mgrav/LB)cl
f (sph, cos) / f (sph, cl) = (270 ± 60)h,
where f (sph, cos)
is the cosmic mean spheroid population luminosity
fraction (eq. [3]), the value in clusters,
f (sph, cl) = 0.64, follows from
equation (21), and (Mgrav/LB)cl
is from equation (20). With
equation (4) we have =
0.19+0.07-0.05.
This however gives the cosmic mean including
clusters; for comparison to
equation (25) we ought to convert to the value outside
rich clusters. The ratio of equation (16) to
equation (20) is the mean luminosity density
provided by the clusters, cl = 0.09.
The spheroid luminosity fraction in the field is
The assumption that the mass-to-spheroid-light ratio is universal
thus indicates the density parameter in gravitational mass
outside the Abell radii of the great clusters is
Despite the substantial uncertainties in each of these arguments
we are encouraged by the
consistency of equations (24), (25), and
(27) to conclude that the density parameter in
gravitational mass that
clusters with galaxies on scales 10h-1 Mpc is likely to be in the range
and that the spheroid-to-dark matter and baryon-to-dark matter
ratios indeed do not vary widely between clusters and the field.
As the evidence has indicated for some time
(Peebles 1986)
and has been widely noted in recent years, this
low density parameter universe offers a natural interpretation of
a variety of observations. Recent examples include the
age/distance scale relation, the abundance of cluster baryons
(White et al. 1993),
the growth rate of correlation functions
(Peacock 1997),
the growth rate of the cluster mass function
(Bahcall, Fan & Cen 1997),
and preliminary indications from the distant supernova Hubble diagram
(Garnavich et al. 1998,
Perlmutter et al. 1998).
The product of equations (23) and (28) is
the estimate of total plasma identified by X-ray
emission in groups,
We remark that this estimate decreases only by 20% when
we incorporate explicitly the trend that the baryon fraction
increases as the group mass,
(MHII/Mgrav)group
~ 0.056h-3/2 (Mgroup / 0.6 x
1014 M) for
Mgroup < 0.6 x 1014 M. As we have noted, an
alternative interpretation is that the trend is only apparent, a
result of less efficient detection of plasma around cooler
groups.