  The Sachs-Wolfe effect is known to produce large angular scale fluctuations
in the Cosmic Microwave Background Radiation (CMBR) due to gravitational
potential fluctuations. We show how the angular correlation function of the
CMBR can be expressed explicitly in terms of the mass autocorrelation function
$\xi (r)$ in the Universe. We derive analytic expressions for the angular
correlation function and its multipole moments in terms of integrals over $\xi
(r)$ or its second moment, $J_3 (r)$, which does not need to satisfy the sort
of integral constraint that $\xi (r)$ must. We derive similar expressions for
bulk flow velocity in terms of $\xi$ and $J_3$. One interesting result that
emerges directly from this analysis is that, for angles $\theta$, there is a
substantial contribution to the correlation function from a wide range of
distance $r$ and that the radial shape of this contribution does not vary
greatly with angle.
