Abstract

The current generation of Cosmic Microwave Background experiments are measuring fluctuations on a few arcminute scales. To convincingly constrain early universe physics from the Silk damping tail we have to understand the foreground emission from distant dusty star forming galaxies: the Cosmic Infrared Background. In the last few years there has been significant progress in measuring the clustering power of the CIB , both from new microwave data, and from observations in the infrared by BLAST and Herschel. We show how a simple template fits Herschel, Planck, and BLAST CIB power spectra, and can be used to model contamination for CMB experiments. By combining the angular power spectra with galaxy number counts, we also show a new model that more fully describes the physical properties of the dusty CIB galaxies. Finally we discuss how our knowledge of the CIB affects current constraints on the kinetic Sunyaev Zel’dovich effect from patchy reionization.