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We examine Suzaku, XMM-Newton, and Chandra observations of the Abell2029/2033 system to investigate the nature of a bridge of X-ray emissionjoining the two galaxy clusters. By modelling the contributions from theoutskirts of the two clusters, and excluding the emission from the southerninfalling group and the background group LOS9, we find a significant excess ofX-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 ofthe clusters. This excess component to the surface brightness is consistentwith being emission from a filament with roughly 1.0 Mpc wide. The derivedemission measure for the gas associated with the filament yields an average gasdensity of $3.7^{+1.0}_{-0.7} \times 10^{-5}$ cm$^{-3}$, corresponding roughlyto 160 times the mean baryon density of the Universe. The Suzaku X-ray spectrumof the excess emission indicates that it is significantly colder($1.4_{-0.5}^{+0.7}$ keV) than the cluster outskirts emission from the twoclusters ($\sim$ 5 keV), statistically consistent with the temperature expectedfrom the hottest and densest parts of the warm-hot intergalactic medium (WHIM).The geometry, density, and temperature are similar to those found from X-raystudies of the Abell 222/223 filament.

A detailed study of the bridge of excess X-ray emission between the galaxy clusters Abell 2029 and Abell 2033