The Spitzer observations at 24 microns resolves 80% of the CIB at this wavelength. We estimate the total CIB brighteness from our legacy counts (Bethermin et al., 2010a, AandA). We extrapolate the faint-end slope of the counts to estimate the contribution of non-detected populations. At 70 and 160, the confusion limits the depth of Spitzer observations. 
We use a stacking analysis with 24 microns as a prior to produce deep counts. We then obtain an estimation of the CIB brighteness from these counts. The CIB Resolved Contribution of sources brighter than Scut to the CIB at 24, 70 and 160 microns (from Bethermin, Dole, Beelen and Aussel, 2010, AandA). A new SED of the EBL has been derived (see below). Download the CIB contributions as a function of flux density Scut on Spitzer source counts web page