Motivated by the integral field units on large aperture telescopes and proposals for ultravioletsensitive space telescopes to probe circumgalactic medium (CGM) emission, we survey the most promising CGM emission lines and how such observations can inform our understanding of the CGM and its relation to galaxy formation. We tie our emission estimates to HST/COS absorption measurements of ions around z ≈ 0.2 Milky Way mass halos and motivated models for the density and temperature of gas, and we provide formulas that simplify extending our estimates to other samples and physical scenarios. We find that O iii 5007 Å and N ii 6583 Å, which at fixed ionic column density are primarily sensitive to the thermal pressure of the gas they inhabit, may be detectable with KCWI and especially IFUs on 30 m telescopes out to half a virial radius. We comment on the implications of existing O iii and N ii stacking measurements by Zhang and coworkers (2018). O v 630 Å and O vi 1032, 1038 Å are perhaps the most promising ultraviolet lines, with motivated models predicting intensities > 100 γ cm −2 s −1 sr −1 in the inner 100 kpc of Milky-Way like systems. A detection would confirm the collisionally ionized picture and constrain the density profile of the CGM. Other ultraviolet metal lines constrain the amount of gas that is actively cooling and mixing. We find that C iii 978 Å and C iv 1548 Å may be detectable if an appreciable fraction of the observed O vi column is associated with mixing or cooling gas. Hydrogen n > 2 Lyman-series lines are too weak to be detectable, and Hα emission within 100 kpc of Milky Way-like galaxies is within the reach of current integral field units even for the minimum signal from ionizing background-fluorescence.