  We use high-resolution hydrodynamical simulations of large-scale structure
formation to study the imprints of the local superclusters onto the full-sky
Sunyaev-Zel'dovich (SZ) signals. Following (Mathis et al. 2002), the initial
conditions have been statistically constrained to reproduce the density field
within a sphere of 110 Mpc around the Milky Way, as observed in the IRAS 1.2-Jy
all-sky redshift survey. As a result, the positions and masses of prominent
galaxy clusters and superclusters in our simulations coincide closely with
their real counterparts in the local universe. We present the results of two
different runs, one with adiabatic gas physics only, and one also including
cooling, star formation and feedback. By analysing the full-sky maps for the
thermal and kinetic SZ signals extracted from these simulations, we find that
for multipoles with l<100 the power spectrum is dominated by the prominent
local superclusters, and its amplitude at these scales is a factor of two
higher than that obtained from unconstrained simulations; at lower multipoles
(l<20) this factor can even reach one order of magnitude. We check the
influence of the SZ effect from local superclusters on the cosmic microwave
background (CMB) power spectrum at small multipoles and find it negligible and
with no signs of quadrupole-octopole alignment. However, performing simulations
of the CMB radiation including the experimental noise at the frequencies which
will be observed by the Planck satellite, we find results suggesting that an
estimate of the SZ power spectrum at large scales can be extracted.
