survey'
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Introduction
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The sensitivity and angular resolution of current cosmic microwave background (CMB) experiments make it possible to study interactions between primary CMB photons and cosmic structure—so-called secondary CMB anisotropies—at small angular scales, and the cosmic infrared background (CIB) at the long-wavelength end of its spectrum. With unprecedented precision and multi-frequency data, the current generation of high resolution instruments allow for the separation of individual contributions to the power spectra, and can provide tight constraints on the associated cosmological and astrophysical model parameters. These include the amplitude of local structure, the duration of the reionization epoch, and the correlation between dust and ionized gas in galaxy clusters.

Expected signals {#sec:intro_sig}
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The most prominent secondary CMB anisotropies at few-arcminute scales (multipole number $\ell \sim 3000$) are expected to be the thermal and kinematic Sunyaev-Zel’dovich (SZ) effects [@sunyaev72; @sunyaev80b]. The SZ effects arise from the scattering of primary CMB photons from free electrons, both those distributed throughout the reionized (and reionizing) intergalactic medium and those concentrated in the hot gas in clusters of galaxies. The SZ power spectra depend sensitively on both the growth of structure and the details of cosmic reionization.

When primary CMB photons inverse Compton scatter 