We perform a tomographic cross-correlation analysis of archival FIRAS data and the BOSS galaxy redshift survey to constrain the amplitude of [CII] $^2P_{ 3/2}\rightarrow$ $^2P_{ 1/2}$ fine structure emission. Our analysis employs spherical harmonic tomography (SHT), which is based on the angular cross-power spectrum between FIRAS maps and BOSS galaxy over-densities at each pair of redshift bins, over a redshift range of $0.24<z<0.69$. We develop the SHT approach for intensity mapping, where it has several advantages over existing power spectral estimators. Our analysis constrains the product of the [CII] bias and [CII] specific intensity, $b_{ [CII]}I_{ [CII]i}$, to be $<0.31$ MJy/sr at $z { \approx} 0.35$ and $<0.28$ MJy/sr at $z { \approx} 0.57$ at $95\%$ confidence. These limits are consistent with most current models of the [CII] signal, as well as with higher-redshift [CII] cross-power spectrum measurements from the Planck satellite and BOSS quasars. We also show that our analysis, if applied to data from a more sensitive instrument such as the proposed PIXIE satellite, can detect pessimistic [CII] models at high significance.
Categories: astro-ph.CO astro-ph.GA