The Clustering Evolution of Dusty Star-Forming Galaxies
  We present predictions for the clustering of galaxies selected by their
emission at far infra-red (FIR) and sub-millimetre wavelengths. This includes
the first predictions for the effect of clustering biases induced by the coarse
angular resolution of single-dish telescopes at these wavelengths. We combine a
new version of the GALFORM model of galaxy formation with a self-consistent
model for calculating the absorption and re-emission of radiation by
interstellar dust. Model galaxies selected at $850$ $\mu$m reside in dark
matter halos of mass $M_{\rm halo}\sim10^{11.5}-10^{12}$ $h^{-1}$ M$_{\odot}$,
independent of redshift (for $0.2\lesssim z\lesssim4$) or flux (for
$0.25\lesssim S_{850\mu\rm m}\lesssim4$ mJy). At $z\sim2.5$, the brightest
galaxies ($S_{850\mu\rm m}>4$ mJy) exhibit a correlation length of
$r_{0}=5.5_{-0.5}^{+0.3}$ $h^{-1}$ Mpc, consistent with observations. We show
that these galaxies have descendants with stellar masses $M_{\star}\sim10^{11}$
$h^{-1}$ M$_{\odot}$ occupying halos spanning a broad range in mass $M_{\rm
halo}\sim10^{12}-10^{14}$ $h^{-1}$ M$_{\odot}$. The FIR emissivity at shorter
wavelengths ($250$, $350$ and $500$ $\mu$m) is also dominated by galaxies in
the halo mass range $M_{\rm halo}\sim10^{11.5}-10^{12}$ $h^{-1}$ M$_{\odot}$,
again independent of redshift (for $0.5\lesssim z\lesssim5$). We compare our
predictions for the angular power spectrum of cosmic infra-red background
anisotropies at these wavelengths with observations, finding agreement to
within a factor of $\sim2$ over all scales and wavelengths, an improvement over
earlier versions of the model. Simulating images at $850$ $\mu$m, we show that
confusion effects boost the measured angular correlation function on all scales
by a factor of $\sim4$. This has important consequences, potentially leading to
inferred halo masses being overestimated by an order of magnitude.
