Negative and positive feedback from a supernova remnant with SHREC: a detailed study of the shocked gas in IC443

Supernova remnants (SNRs) contribute to regulate the star formationefficiency and evolution of galaxies. As they expand into the interstellarmedium (ISM), they transfer vast amounts of energy and momentum that displace,compress and heat the surrounding material. Despite the extensive work ingalaxy evolution models, it remains to be observationally validated to whatextent the molecular ISM is affected by the interaction with SNRs. We use thefirst results of the ESO-ARO Public Spectroscopic Survey SHREC, to investigatethe 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 SHRECtogether with SiO(1-0) observations obtained with the 40m telescope at theYebes Observatory. We find that the bulk of the SiO emission is arising fromthe ongoing shock interaction between IC443 and clump G. The shocked gas showsa well ordered kinematic structure, with velocities blue-shifted with respectto the central velocity of the SNR, similar to what observed toward otherSNR-cloud interaction sites. The shock compression enhances the molecular gasdensity, n(H$_2$), up to $>$10$^5$ cm$^{-3}$, a factor of >10 higher than theambient gas density and similar to values required to ignite star formation.Finally, we estimate that up to 50\% of the momentum injected by IC443 istransferred to the interacting molecular material. Therefore the molecular ISMmay represent an important momentum carrier in sites of SNR-cloud interactions.