We present measurements of the auto- and cross-frequency power spectra of the cosmic infrared background ( CIB ) at 250 , 350 , and 500 \mathrm { \upmu } m ( 1200 , 860 , and 600 GHz ) from observations totaling \sim 70 deg ^ { 2 } made with the SPIRE instrument aboard the Herschel Space Observatory .
We measure a fractional anisotropy \delta I / I = 14 \pm 4 % , detecting signatures arising from the clustering of dusty star-forming galaxies in both the linear ( 2-halo ) and non-linear ( 1-halo ) regimes ; and that the transition from the 2- to 1-halo terms , below which power originates predominantly from multiple galaxies within dark matter halos , occurs at k _ { \theta } \sim 0.10 – 0.12 arcmin ^ { -1 } ( \ell \sim 2160 –2380 ) , from 250 to 500 \mathrm { \upmu } m. New to this paper is clear evidence of a dependence of the Poisson and 1-halo power on the flux-cut level of masked sources — suggesting that some fraction of the more luminous sources occupy more massive halos as satellites , or are possibly close pairs .
We measure the cross-correlation power spectra between bands , finding that bands which are farthest apart are the least correlated , as well as hints of a reduction in the correlation between bands when resolved sources are more aggressively masked .
In the second part of the paper we attempt to interpret the measurements in the framework of the halo model .
With the aim of fitting simultaneously with one model the power spectra , number counts , and absolute CIB level in all bands , we find that this is achievable by invoking a luminosity-mass relationship , such that the luminosity-to-mass ratio peaks at a particular halo mass scale and declines towards lower and higher mass halos .
Our best-fit model finds that the halo mass which is most efficient at hosting star formation in the redshift range of peak star-forming activity , z \sim 1 - 3 , is { log } ( M _ { peak } / M _ { \odot } ) \sim 12.1 \pm 0.5 , and that the minimum halo mass to host infrared galaxies is { log } ( M _ { min } / M _ { \odot } ) \sim 10.1 \pm 0.6 .