dust temperatures for each component. [@addison12a]

Both the tSZ and CIB are tracers of the underlying dark matter distribution, and thus we expect the two signals to be correlated [@addison12b]. This correlation is itself an interesting probe of cluster physics and evolution, but it complicates the separation of individual components in multi-frequency measurements [@reichardt12b; @dunkley13].

Previous measurements {#sec:intro_prevmeas}
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The first robust measurement of the amplitude of the SZ power spectrum was presented by @lueker10 [hereafter L10] using 100 [deg$^2$]{} of data from the South Pole Telescope (SPT) in the angular multipole range $(2000 < \ell < 9500)$. Improved SPT measurements of the power spectrum have since been reported by @shirokoff11 and @reichardt12b (hereafter S11 and R12) using 200 [deg$^2$]{} and 800 [deg$^2$]{} of data respectively. R12 measured the tSZ and kSZ power at $\ell = 3000$ to $D^{\rm tSZ}_{3000} = 3.26\pm1.06\,\mu{\rm K}^2$ and $D^{\rm kSZ}_{3000} < 6.7\,\mu{\rm K}^2$ (95% CL) at 153GHz. The Atacama Cosmology Telescope (ACT) collaboration has also measured the high-$\ell$ power spectrum [@das11b; @das14] with multi-frequency band powers covering the multipole range from $(1540<\ell<9440)$. @dunkley13 use the power spectra presented in @das14 to measure $D^{\rm tSZ}_{3000} = 3.3\pm1.4\,\mu{\rm K}^2$ and $D^{\rm kSZ}_{3000} < 8.6\,\mu{\rm K}^2$ (95% 