distribution of bubble sizes; both features also depend less strongly on the average redshift of reionization [@gruzinov98; @knox98]. Constraints on the kSZ power spectrum can therefore lead to interesting constraints on the epoch of reionization [@mortonson10; @zahn12; @mesinger12].

The sky power at millimeter wavelengths and scales smaller than a few arcminutes ($\ell \gtrsim 3000$) is dominated by the signal from bright extragalactic sources [@vieira10; @marriage11a; @planck11-13], mostly synchrotron-dominated active galactic nuclei (AGN), with additional contributions from nearby infrared galaxies and rare, strongly lensed, dusty, star-forming galaxies (DSFGs, @negrello10 [@vieira13]). With these identifiable sources removed, the remaining power is dominated by fainter DSFGs that contribute the bulk of the CIB [@lagache05; @casey14]. These DSFGs are important both as a foreground for CMB experiments and as a tool to understand the history of star and galaxy formation [e.g., @bond86; @bond91b; @knox01; @madau14]. The power from DSFGs can be separated into a component with no angular clustering (the “Poisson” component) and an angularly clustered component. By definition these two components have distinct angular scale dependencies. Multi-frequency measurements of CIB power can determine the spectral index of both the clustered and Poisson components of the CIB anisotropy, providing constraints on the redshift distributions and 