  Galaxies are often used as tracers of the large scale structure (LSS) to
measure the Integrated Sachs-Wolfe effect (ISW) by cross-correlating the galaxy
survey maps with the Cosmic Microwave Background (CMB) map. We use the Cosmic
Infrared Background (CIB) as a tracer of the LSS to perform a theoretical
CIB-CMB cross-correlation to measure the ISW for different Planck HFI
frequencies. We discuss the detectability of this ISW signal using a
Signal-to-noise ratio analysis and find that the ISW detected this way can
provide us with the highest SNR for a single tracer ranging from 5 to 6.7
(maximum being for 857 GHz) with the CIB and CMB maps extracted over the whole
sky. A Fisher matrix analysis showed that this measurement of the ISW can
improve the constraints on the cosmological parameters; especially the equation
of state of the dark energy $w$ by $\sim 47\%$. Performing a more realistic
analysis including the galactic dust residuals in the CIB maps over realistic
sky fractions shows that the dust power spectra dominate over the CIB power
spectra at $\ell < 100$ and ISW can't be detected with high SNR. We perform the
cross-correlation on the existing CIB-CMB maps over $\sim 11\%$ of the sky in
the southern hemisphere and find that the ISW is not detected with the existing
CIB maps over such small sky fractions.
