  We show that clusters of galaxies induce step-like wiggles on top of the
cosmic microwave background (CMB). The direction of the wiggle is parallel to
the large scale gradient of CMB allowing one to isolate the effect from other
small scale fluctuations. The effect is sensitive to the deflection angle
rather than its derivative (shear or magnification) and is thus tracing outer
parts of the cluster with higher sensitivity than some other methods. A typical
amplitude of the effect is $10\mu K (\sigma_v/1400 kms^{-1})^2$ where
$\sigma_v$ is the velocity dispersion of the cluster and several $\mu K$
signals extend out to a fraction of a degree. We derive the expressions for the
temperature profile for several simple parameterized cluster models and
identify some degeneracies between parameters. Finally, we discuss how to
separate this signal from other imprints on CMB using custom designed filters.
Detection of this effect is within reach of the next generation of small scale
CMB telescopes and could provide information about the cluster density profile
beyond the virial radius.
