  The Cosmic Infrared Background (CIB), traced by the emission from dusty
star-forming galaxies, provides a crucial window into the phases of star
formation throughout cosmic history. These galaxies, although challenging to
detect individually at high redshifts due to their faintness, cumulatively
contribute to the CIB which then becomes a powerful probe of galaxy formation,
evolution and clustering. Here, we introduce a physically-motivated model for
the CIB emission spanning a wide range of frequency and angular resolution,
employing a halo model approach and distinguishing, within dark matter halos,
between two main populations of star forming galaxies, i.e. normal late-type
spiral and irregular galaxies and the progenitors of early-type galaxies. The
emission from two galaxy populations maps into different regimes in
frequency/resolution space, allowing us to constrain the clustering parameters
of the model - $M_{\text{min}}$, the mass of a halo with 50% probability of
having a central galaxy and $\alpha$, the power law index regulating the number
of satellite galaxies - through a fit to Planck and Herschel-SPIRE CIB
anisotropy measurements. We find that, while being able to place constraints on
some of the clustering parameters, the Planck frequency and multipole coverage
cannot effectively disentangle the contributions from the two galaxy
populations. On the other side, the Herschel-SPIRE measurements separate out
and constrain the clustering of both populations. Our work, though, highlights
an inconsistency of the results between the two datasets, partially already
reported in other literature and still not understood.
