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Previously, we have generated six hydrodynamical two-dimensional two-fluid simulations of the interstellar medium that naturally create the filamentary structure of cold gas apparent in neutral hydrogen in the Galaxy. The two fluids in these simulations represent the stars and gas in the interstellar medium, and interact via star formation, mass loss, and heating from stellar winds or supernovae. We have analyzed one image from the simulations for the variation of H I column density with galactic latitude from five positions in the simulation, three of which are within bubbles of hot gas. In addition, we calculate the X-ray intensity in bands near 0.25 kev and 0.75 keV for each of these five positions as well. Our study shows the dominance of the local environment at 0.25 keV, and relatively larger importance of distant material to the 0.75 keV intensity. Our results also show that the 0.75 keV data are more frequently anti-correlated with the H I column density.
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