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Infrared fine-structure emission lines from trace metals are powerfuldiagnostics of the interstellar medium in galaxies. We explore the possibilityof studying the redshifted far-IR fine-structure line emission using thethree-dimensional (3-D) power spectra obtained with an imaging spectrometer.The intensity mapping approach measures the spatio-spectral fluctuations due toline emission from all galaxies, including those below the individual detectionthreshold. The technique provides 3-D measurements of galaxy clustering andmoments of the galaxy luminosity function. Furthermore, the linear portion ofthe power spectrum can be used to measure the total line emission intensityincluding all sources through cosmic time with redshift information naturallyencoded. Total line emission, when compared to the total star formationactivity and/or other line intensities reveals evolution of the interstellarconditions of galaxies in aggregate. As a case study, we consider measurementof [CII] autocorrelation in the 0.5 < z < 1.5 epoch, where interloper lines areminimized, using far-IR/submm balloon-borne and future space-borne instrumentswith moderate and high sensitivity, respectively. In this context, we comparethe intensity mapping approach to blind galaxy surveys based on individualdetections. We find that intensity mapping is nearly always the best way toobtain the total line emission because blind, wide-field galaxy surveys lacksufficient depth and deep pencil beams do not observe enough galaxies in therequisite luminosity and redshift bins. Also, intensity mapping is often themost efficient way to measure the power spectrum shape, depending on thedetails of the luminosity function and the telescope aperture.

Measuring Galaxy Clustering and the Evolution of [CII] Mean Intensity with far-IR Line Intensity Mapping During 0.5 < z < 1.5