  Modelling the anisotropies in the CIB on all the scales is a challenging task
due to the complex nature of the galaxy evolution and thus often requires too
many parameters in order to fit the observational data. In this paper, we
present a new halo model for the anisotropies of the CIB using only four
parameters. Our model connects the mass accretion on the dark matter halos to
the star formation rate. Using this model, we find that the halo mass with the
maximum efficiency for converting the accreted baryons into stars is
$\log_{10}M_\mathrm{max} = {12.94}^{+0.02}_{-0.02} \: M_\odot$, consistent with
other studies. Accounting for the mass loss through stellar evolution, we find,
for an intermediate age galaxy, that the star formation efficiency defined as
$M_\star(z)/M_b(z)$ is equal to 0.19 and 0.21 at redshift 0.1 and 2
respectively, in good agreement with the values obtained by previous studies.
It is the first time that a CIB model is used to fit Planck and Herschel CIB
power spectra simultaneously. However we find that the large angular scale
Planck and Herschel data are not fully compatible with the small scale Herschel
data (for $\ell>3000$). The CIB is expected to be correlated with the tSZ
signal of the galaxy clusters. Using this halo model for the CIB, and a halo
model for the tSZ with a single parameter, we also provide a consistent
framework to calculate this cross-correlation, which requires no extra
parameter. The CIB$\times$tSZ correlation is found to be higher when inferred
with a combination of two widely spaced frequency channels (e.g. 143x857 GHz).
The CIB, tSZ, and CIB$\times$tSZ act as foregrounds while measuring the kSZ
power spectrum from the CMB power spectrum and need to be removed. Due to its
simplistic nature and low number of parameters, the halo model formalism
presented here is quite useful for such an analysis to measure the kSZ power
spectrum accurately.
