  Sunyaev-Zeldovich decrements in the temperature of the Cosmic Microwave
Background (CMB) are produced by Thomson scattering of the CMB photons by the
confined hot electrons in the Intra-Cluster Medium encountered along the
line-of-sight. In this paper, we propose an alternate physical process that can
produce detectable thermal and kinematic Sunyaev-Zeldovich decrements around
quasars or quasar pairs in regions where no assembled, virialized clusters are
detected either in the optical or X-ray wave-band. Invoking quasar outflows, we
argue that both thermal and kinematic decrements can be produced by the baryons
swept up by the mechanical luminosity of quasars. In contrast to the case of
decrements produced by the hot electrons confined within the cluster potential,
the magnitude of these quasar-outflow induced effects depend primarily on the
luminosity of the QSO, and the physical scale of the outflow - which in turn
depends both on the mean local density and the density gradient in the vicinity
of the quasar. Quasar outflows produce (i) a frequency independent kinematic
decrement ${\Delta T/T} \sim {10^{-4}}$; (ii) a frequency dependent fluctuation
in the intensity ${\Delta {J_{\nu}}/{J_{\nu}}} \sim $ a 20% variation relative
to ${\Delta T/T}$, say at 15 GHz and 30 GHz; (iii) a temperature increment
${\Delta T/T} \sim {10^{-4}}$ on the opposite side of the QSO; (iv) a linear
polarization signal over 20'' at $\sim {10^{-7}}$ level; and therefore (v)
patches of signal ${\Delta T/T} \sim {10^{-4}}$ on degree scales.
