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Using a sample of nearly half a million galaxies, intersected by over 8million lines of sight from the Sloan Digital Sky Survey Data Release 12, weextend our previous study of the recombination radiation emitted by the gaseoushalos of nearby galaxies. We identify an inflection in the radial profile ofthe H$\alpha$+N[{\small II}] radial emission profile at a projected radius of$\sim 50$ kpc and suggest that beyond this radius the emission from ionized gasin spatially correlated halos dominates the profile. We confirm that this is aviable hypothesis using results from a highly simplified theoretical treatmentin which the dark matter halo distribution from cosmological simulations isstraightforwardly populated with gas. Whether we fit the fraction of halo gasin a cooler (T $= 12,000$ K), smooth ($c = 1$) component (0.26 for galaxieswith M$_* = 10^{10.88}$ M$_\odot$ and 0.34 for those with M$_* = 10^{10.18}$M$_\odot$) or take independent values of this fraction from publishedhydrodynamical simulations (0.19 and 0.38, respectively), this modelsuccessfully reproduces the radial location and amplitude of the observedinflection. We also observe that the physical nature of the gaseous haloconnects to primary galaxy morphology beyond any relationship to the galaxy'sstellar mass and star formation rate. We explore whether the model reproducesbehavior related to the central galaxy's stellar mass, star formation rate, andmorphology. We find that it is unsuccessful in reproducing the observations atthis level of detail and discuss various shortcomings of our simple model thatmay be responsible.

Emission from the Ionized Gaseous Halos of Low Redshift Galaxies and Their Neighbors