In this paper we show that, within the framework of the QSSC, the small scale deviations on angular scales $lesssim 1^{0}$ expected in the MBR are due to inhomogeneities in the distribution of galaxies and clusters. It is shown how these can be estimated on the galaxy-cluster-supercluster scale at the epoch of redshift $sim 5$ when the universe was last passing through the minimum phase of the scale factor. Rich clusters on the scale of 5-10 Mpc generate the kind of peak in the fluctuation power spectrum observed by the Boomrang and Maxima projects. Weaker inhomogeneities on smaller scales with $l~sim 10^3$ are expected to arise from individual galaxies and small groups.
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