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The Warm Ionized Medium in Spiral Galaxies: A View from Above

The Warm Ionized Medium (WIM), also referred to as Diffuse Ionized Gas, contains most of the mass of interstellar medium in ionized form, contributing as much as 30% of the total atomic gas mass in the solar neighborhood. The advent of CCDs has enabled unprecedented study of this medium in external galaxies, probing a variety of environments. In particular, we can derive the morphology of the WIM, its distribution across disks, and the correlation with other Population I material. Spectroscopy of the WIM makes it possible to test various ionization models. I will review here our current understanding of the properties of the WIM in spiral galaxies. A perhaps unexpected result is that the H-alpha emission from the WIM contributes about 40% of the total observed H-alpha luminosity from spirals. This places severe constraints on possible sources of ionization, since only photo ionization by OB stars meets this requirement. Spectroscopic measurements of forbidden line strengths appear in reasonable agreement with photo ionization models. It is not yet clear if the Lyman continuum photons that ionize the WIM are mostly from OB stars located inside traditional HII regions, or from field OB stars.