  We examine Suzaku, XMM-Newton, and Chandra observations of the Abell
2029/2033 system to investigate the nature of a bridge of X-ray emission
joining the two galaxy clusters. By modelling the contributions from the
outskirts of the two clusters, and excluding the emission from the southern
infalling group and the background group LOS9, we find a significant excess of
X-ray emission between the two clusters at the level of 6.5-7.0$\sigma$,
depending on the choice of model, that cannot be explained by the overlap of
the clusters. This excess component to the surface brightness is consistent
with being emission from a filament with roughly 1.0 Mpc wide. The derived
emission measure for the gas associated with the filament yields an average gas
density of $3.7^{+1.0}_{-0.7} \times 10^{-5}$ cm$^{-3}$, corresponding roughly
to 160 times the mean baryon density of the Universe. The Suzaku X-ray spectrum
of the excess emission indicates that it is significantly colder
($1.4_{-0.5}^{+0.7}$ keV) than the cluster outskirts emission from the two
clusters ($\sim$ 5 keV), statistically consistent with the temperature expected
from the hottest and densest parts of the warm-hot intergalactic medium (WHIM).
The geometry, density, and temperature are similar to those found from X-ray
studies of the Abell 222/223 filament.
