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When an AGN is obscured, the warm reflecting gas nearby can be seen by acombination of bremsstrahlung, intrinsic line emission, and reflection of thenuclear continuum, both by electron scattering and by resonance linescattering. Resonance lines, due both to intrinsic emission and scattering, areparticularly prominent in the soft X-ray band.  When our line of sight to the nucleus is not obscured, the dominant effect isabsorption. In the soft X-ray band, ionization edges of highly ionized speciesand resonance lines contribute comparably to the opacity; in the ultraviolet,the gas is almost transparent except for a small number of resonance lines. Weidentify the "warm absorbers" seen in many AGN X-ray spectra with this gas, butargue that most of the UV absorption lines seen must be due to a small amountof more weakly ionized gas which is embedded in the main body of the warm,reflecting gas. Because the ionization equilibration timescales of some ionsmay be as long as the variability timescales in AGN, the ionic abundancesindicated by the transmission spectra may not be well-described by ionizationequilibrium.Comment: 24 pages, AASLaTeX, to appear in July 10 1995 Ap.J.; figures  obtainable in uuencoded form at  ftp://jhufos.pha.jhu.edu/pub/put/jhk/warmabsfigs.u

Observable Properties of X-Ray--heated Winds in Active Galactic Nuclei: Warm Reflectors and Warm Absorbers