HerMES: COSMIC INFRARED BACKGROUND ANISOTROPIES AND THE CLUSTERING OF DUSTY STAR-FORMING GALAXIES

Abstract

Star formation is well traced by dust, which absorbs the
\nUV/optical light produced by young stars in actively starforming
\nregions and re-emits the energy in the far-infrared/
\nsubmillimeter (FIR/submm; e.g., Savage & Mathis 1979).
\nRoughly half of all starlight ever produced has been reprocessed
\nby dusty star-forming galaxies (DSFGs; e.g., Hauser & Dwek
\n2001; Dole et al. 2006), and this emission is responsible
\nfor the ubiquitous cosmic infrared background (CIB; Puget
\net al. 1996; Fixsen et al. 1998). The mechanisms responsible
\nfor the presence or absence of star formation are partially
\ndependent on the local environment (e.g., major mergers:
\nNarayanan et al. 2010; condensation or cold accretion: Dekel
\net al. 2009, photoionization heating, supernovae, active galactic
\nnuclei, and virial shocks: Birnboim & Dekel 2003; Granato
\net al. 2004; Bower et al. 2006). Thus, the specifics of the
\ngalaxy distribution—which can be determined statistically to
\nhigh precision by measuring their clustering properties—inform
\nthe relationship of star formation and dark matter density, and
\nare valuable inputs for models of galaxy formation. However,
\nmeasuring the clustering of DSFGs has historically proven
\ndifficult to do.