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The galactic gaseous halo is a gas reservoir for the interstellar medium inthe galaxy disk, supplying materials for star formation. We developed a gaseoushalo model connecting the galaxy disk and the gaseous halo by assuming the starformation rate on the disk is balanced by the radiative cooling rate of thegaseous halo, including stellar feedback. In addition to a single-temperaturegaseous halo in collisional ionization equilibrium, we also consider thephotoionization effect and a steady-state cooling model. Photoionization isimportant for modifying the ion distribution in low-mass galaxies and outskirtsof massive galaxies due to the low densities. The multi-phase cooling modeldominates the region within the cooling radius, where t_cooling=t_Hubble. Ourmodel reproduces most of the observed high ionization state ions for a widerange of galaxy masses (i.e., OVI, OVII, NeVIII, MgX, and OVIII). We find thatthe OVI column density has a narrow range around ~10^14 cm^-2 for halo massesfrom M_star ~ 3 * 10^10 Msun to 6*10^12 Msun, which is consistent with some butnot all observational studies. For galaxies with halo masses <~ 3 * 10^11 Msun,photoionization produces most of the OVI, while for more massive galaxies, theOVI is from the medium that is cooling from higher temperatures. Fitting theGalactic (Milky-Way) OVII and OVIII suggests a gaseous halo model where themetallicity is ~0.55 Zsun and the gaseous halo has a maximum temperature of ~1.9 * 10^6 K. This gaseous halo model does not close the census of baryonicmaterial within R200.

The Mass and Absorption Columns of Galactic Gaseous Halos