MG13 - Talk detail

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In addition to instrument noise, deep cosmological surveys in the far-infrared to millimeter spectral range are limited in depth by confusion from extragalactic sources. As a consequence, the cosmic infrared background (CIB), which records much of the radiant energy released by processes of structure formation that have occurred since the decoupling of matter and radiation following the Big Bang, is barely resolved into its constituents. Thus, in the absence of foreground (Galactic dust) and background (cosmic microwave background, CMB) emissions, and when the instrument noise is subdominant, maps of the diffuse emission at the angular resolution probed by the current surveys reveal a web of structures, characteristic of CIB anisotropies. With the advent of large area far-infrared to millimeter surveys (Planck, but also Herschel, SPT, and ACT), CIB anisotropies constitute a new tool for structure formation and evolution study. The anisotropies detected in the CIB trace the large-scale distribution of star-forming galaxies and, to some extent, the underlying distribution of the dark matter halos in which galaxies reside. The CIB is thus a direct probe of the interplay between baryonic and dark matter throughout cosmic times and its unmatched redshift depth complements current and foreseeable optical or near-infrared measurements. Owing to its frequency coverage from 100 to 857 GHz, the High Frequency Instrument (HFI) on-board Planck is ideally suited to probe the dark matter/star-formation connection. I will review in this talk what we learned from CIB anisotropy measurements with Planck. I will also show the promise of cross-correlating the CIB maps with external tracers of the density field, like the galaxy and quasar distributions in the SDSS, or the CMB lensing map.

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