![]() | Annu. Rev. Astron. Astrophys. 2000. 38: 289-335
Copyright © 2000 by Annual Reviews. All rights reserved |
5.2. Mass Estimates
One of the most important applications of X-ray observations of groups has been mass estimates. Prior to ROSAT, mass determinations for groups were largely based on application of the virial theorem to the group galaxies. For a typical cataloged group with only four or five velocity measurements, the virial method can be unreliable (e.g. Barnes 1985, Diaferio et al 1993).
The method used to estimate group masses from X-ray data is analogous to the technique developed for rich clusters (e.g. Fabricant et al 1980, 1984; Fabricant & Gorenstein 1983; Cowie et al 1987). The fundamental assumption is that the hot gas is trapped in the potential well of the group and is in rough hydrostatic equilibrium. This assumption is probably a reasonable one for most groups, given the short sound-crossing times in these systems. A further assumption is that the only source of heating for the gas is gravitational, i.e. that the gas temperature is a direct measure of the potential depth and therefore of the total mass. This assumption may not be strictly true for some groups. In particular, the fact that the heavy metal abundance of the intragroup medium is non-zero suggests that some of the gas has been reprocessed in the stars in galaxies and ejected by supernovae-driven winds. In addition to polluting the intragroup gas with metals, such winds also provide additional energy to the gas. It has generally been assumed in the literature that the energy contribution of such winds is negligible. Semi-analytic models suggest that this assumption is fair as long as the temperature of the system is greater than about 0.8 keV (Balogh et al 1999, Cavaliere et al 1999). Thus, for many groups, the hydrostatic mass estimator should be valid.
With the further assumption of spherical symmetry, the mass interior to radius R is given by (Fabricant et al 1984):
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where k is Boltzmann's constant, Tgas(R) is the gas
temperature at radius R, G is the gravitational constant, µ
is the mean molecular weight, mp is the mass of the proton,
and
is the gas
density. In principle, all of the unknowns in this equation can be
calculated from the X-ray data. Typically, the gas temperature is
measured directly from the X-ray spectrum and the gas density profile is
determined by fitting the standard beta model to the surface brightness
profile. Unfortunately, it is often necessary to make a further
assumption that the gas is isothermal (i.e. d log T /
d log r = 0). For a few groups, the temperature profile
can be directly measured. The resulting mass estimates suggest that the
isothermal assumption generally results in an error in the mass of no
more than about 10% (e.g.
David et al 1994,
Davis et al 1996).
With the isothermal assumption, Mtotal (< R)
Tgas
R (as long as
R is much larger than the core radius in the beta model. Therefore, if
is
underestimated from the surface brightness profile fits by a factor of ~
2 (see Sections 3.3.3 and
3.4.3), then the mass estimates are
also too small by a factor of ~ 2.)
ROSAT measurements indicated a small range of total group masses with
nearly all of the systems clustered around 1013 h-1
M (see
Figure 8;
Mulchaey et al
1993,
Ponman & Bertram
1993,
David et al 1994,
Pildis et al 1995,
Henry et al 1995,
Mulchaey et al
1996a).
The narrow range of group masses is not too surprising, given that
nearly all the groups in these surveys have temperatures of ~ 1 keV.
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Figure 8. Distribution of X-ray-determined total group masses. In each case, the masses are determined out to the radius to which the X-ray emission is detected. The sample is based on the compilation given in Mulchaey et al 1996a, with the addition of a few groups with more recent X-ray mass estimates in the literature. |
The X-ray mass estimates can generally be applied only to a radius of
several hundred kiloparsecs. Beyond that, the gas density profile is not
well-constrained. Because the virial radius for a 1 keV group is
approximately ~ 0.5 h-1100 Mpc, the X-ray method
measures only a fraction of the total mass
(Ponman & Bertram
1993;
David et al 1995;
Henry et al 1995).
Simply extrapolating out to the virial radius, the total group masses
are a factor of approximately two to three times larger than those
implied from the X-ray studies (Mass
R). However, if
non-gravitational heat is important in groups, the extrapolation out to
the virial radius is more uncertain
(Loewenstein 2000).
Because of their relatively large masses, X-ray groups make a
substantial contribution to the mass density of the universe
(Mulchaey et al
1993,
Henry et al 1995,
Mulchaey et al
1996a).
Based on their X-ray-selected group sample,
Henry et al (1995)
estimate that X-ray luminous groups contribute
~ 0.05. However,
their sample contained only the most luminous, elliptical-rich
groups. When one corrects for the groups missing from
Henry et al's (1995)
sample (assuming a similar mass density), groups might contribute as
much as
~ 0.25. These
estimates are comparable to the numbers found for richer clusters, which
verifies the cosmological significance of poor groups.