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In a previous paper, we calculated numerical hydrodynamic models of theinterstellar medium in the Galaxy, which suggested that hot gas (T $\ge$ 3$\times$ 10$^5$ K) has a filling factor near 50\% in the midplane (Rosen \&Bregman 1995, ApJ 440, 634). Here we extend the work to examine the X-rayemission characteristics of the best model and calculate a variety ofobservable measures for comparison with the observed soft X-ray background. Wecalculate the X-ray intensities, spectra, and hardness ratios in two soft X-raybands as Galactic latitude and cool gas column are varied, and make comparisonswith observational data. The observed distribution of N$_{H I}$ is similar tothat seen from one of the simulated bubbles, with the important exception thatthe minimum hydrogen column in the model is too low. Also, there are clearexamples of anticorrelations between H I and X-ray emission as well ascorrelations between H I and X-rays, which is caused by an increased emissionmeasure as a shock enters a cool gas region. Statistically, anticorrelationsare slightly more common than correlations. X-ray spectra are calculated fromthe models and these reveal that for observations to have strong diagnosticpower in probing the hot ISM, a spectral resolution of E/$\Delta$E $>$ 30 isrequired. This analysis demonstrates several shortcomings of our model, whichmay be solved by future simulations that include magnetic fields.

Global Models of the Galactic Interstellar Medium: Comparison to X-Ray and H i Observations