  Supernova remnants (SNRs) contribute to regulate the star formation
efficiency and evolution of galaxies. As they expand into the interstellar
medium (ISM), they transfer vast amounts of energy and momentum that displace,
compress and heat the surrounding material. Despite the extensive work in
galaxy evolution models, it remains to be observationally validated to what
extent the molecular ISM is affected by the interaction with SNRs. We use the
first results of the ESO-ARO Public Spectroscopic Survey SHREC, to investigate
the shock interaction between the SNR IC443 and the nearby molecular clump G.
We use high sensitivity SiO(2-1) and H$^{13}$CO$^+$(1-0) maps obtained by SHREC
together with SiO(1-0) observations obtained with the 40m telescope at the
Yebes Observatory. We find that the bulk of the SiO emission is arising from
the ongoing shock interaction between IC443 and clump G. The shocked gas shows
a well ordered kinematic structure, with velocities blue-shifted with respect
to the central velocity of the SNR, similar to what observed toward other
SNR-cloud interaction sites. The shock compression enhances the molecular gas
density, n(H$_2$), up to $>$10$^5$ cm$^{-3}$, a factor of >10 higher than the
ambient gas density and similar to values required to ignite star formation.
Finally, we estimate that up to 50\% of the momentum injected by IC443 is
transferred to the interacting molecular material. Therefore the molecular ISM
may represent an important momentum carrier in sites of SNR-cloud interactions.
