The history of star formation from the cosmic infrared background
  anisotropies
  We present a linear clustering model of cosmic infrared background (CIB)
anisotropies at large scales that is used to measure the cosmic star formation
rate density up to redshift 6, the effective bias of the CIB and the mass of
dark-matter halos hosting dusty star-forming galaxies. This is achieved using
the Planck CIB auto- and cross-power spectra (between different frequencies)
and CIBxCMB lensing cross-spectra measurements, as well as external constraints
(e.g. on the CIB mean brightness). We recovered an obscured star formation
history which agrees well with the values derived from infrared deep surveys
and we confirm that the obscured star formation dominates the unobscured one up
to at least z=4. The obscured and unobscured star formation rate densities are
compatible at $1\sigma$ at z=5. We also determined the evolution of the
effective bias of the galaxies emitting the CIB and found a rapid increase from
$\sim$0.8 at z$=$0 to $\sim$8 at z$=$4. At 2$<$z$<$4, this effective bias is
similar to that of galaxies at the knee of the mass functions and submillimeter
galaxies. This effective bias is the weighted average of the true bias with the
corresponding emissivity of the galaxies. The halo mass corresponding to this
bias is thus not exactly the mass contributing the most to the star formation
density. Correcting for this, we obtained a value of
log(M$_h$/M$_{\odot}$)=12.77$_{-0.125}^{+0.128}$ for the mass of the typical
dark matter halo contributing to the CIB at z=2. Finally, we also computed
using a Fisher matrix analysis how the uncertainties on the cosmological
parameters affect the recovered CIB model parameters and find that the effect
is negligible.
