  At low redshifts, a census of the baryons in all known reservoirs falls a
factor of two to four below the total baryon density predicted from Big Bang
nucleosynthesis arguments and observed light element ratios. Recent
cosmological hydrodynamic simulations suggest that a significant fraction of
these missing baryons could be in the form of warm/hot gas in the filaments and
halos within which most field galaxies are embedded. With the release of source
count results from Chandra and recent detections of this gas in O VI quasar
absorption lines, it becomes interesting to examine the predictions and limits
placed on this component of the X-ray background (XRB). We have used new
hydrodynamical simulations to predict the total X-ray spectrum from the gas in
the 100 eV to 10 keV range. We find that, when uncertainties in the
normalization of the observed XRB and the value of Omega_b are taken into
account, our results are consistent with current observational limits placed on
the contribution of emission from gas to the XRB. In the 0.5-2 keV range, we
expect the contribution from this component to be 0.63 10^{-12} erg s^-1 cm^-2
deg^-2 or between 6% and 18% of the extragalactic surface brightness. The peak
fraction occurs in the 0.5-1 keV range where the predicted line emission
mirrors a spectral bump seen in the latest ASCA/ROSAT XRB data.
