We have analyzed ASCA and ROSAT PSPC spectra and images of the galaxy
cluster Abell 2029. The ASCA spectra of the cluster indicate that the
gas temperature declines with radius. The PSPC image shows that the cl
uster is very regular and smooth. Also, there is no significant eviden
ce for any irregularities in the temperature distribution in the clust
er, as would be produced by a subcluster merger. These results suggest
that A2029 is a relaxed cluster and that the gas is in hydrostatic eq
uilibrium. We use the assumption of equilibrium to determine the gravi
tational mass of the cluster as a function of radius. At a radius of 1
6' (1.92 h(50)(-1) Mpc; H-0 = 50 h(50) km s(-1) Mpc(-1)), the gravitat
ional mass is M-tot = (9.42 +/- 4.22) x 10(14) h(50)(-1) M., while the
mass of gas is M-gas = (2.52 +/- 0.77) x 10(14) h(50)(-5/2) M.. The g
as fraction is found to increase with radius; within a spherical radiu
s of 16', the fraction is M-gas/M-tot = (0.26 +/- 0.14) h(50)(-3/2). T
he iron abundance in the gas is found to be 0.40 +/- 0.04 solar. There
is no significant evidence for any variation in the abundance with po
sition in the cluster. The global X-ray spectra, central X-ray spectra
, and ROSAT surface brightness all require a cooling flow at the clust
er center. The global X-ray spectrum implies that the total cooling ra
te is 363(-96)(+79) h(50)(-2) M. yr(-1). The global X-ray spectra are
consistent with the Galactic value for the soft X-ray absorption towar
d the cluster. White et al. and Alien & Fabian have suggested that the
re is significant excess absorption associated with the cooling flow i
n the cluster. The ROSAT PSPC spectra of the central regions of the cl
uster are inconsistent with a large value of foreground excess absorpt
ion. The upper limit on excess foreground absorption is 7.3 x 10(19) c
m(-2). However, the spectra do not rule out a significant amount of in
trinsic absorbing gas located within the cooling flow region.