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We want to investigate the influence of the powerful outflow driven by thehot core Sgr B2(N1) on the gas molecular inventory of the surrounding medium.We used the data taken as part of the 3 mm imaging spectral-line survey ReMoCA(Re-exploring Molecular Complexity with ALMA). Integrated intensity maps of SOand SiO emission reveal a bipolar structure with blue-shifted emissiondominantly extending to the SE from the centre of the hot core and red-shiftedemission to the NW. This is also prominently observed in emission of otherS-bearing molecules and species that only contain N as a heavy element,including COMs, but also CH3OH, CH3CHO, HNCO, and NH2CHO. For a selection ofCOMs and simpler species, spectra were modelled under the assumption of LTE andpopulation diagrams were derived at two positions, one in each outflow lobe.From this analysis, we obtained rotational temperatures, which are in a rangeof ~100-200K, and column densities. Abundances were subsequently compared topredictions of astrochemical models and to observations of L1157-B1, a positionlocated in the well-studied outflow of the low-mass protostar L1157, and thesource G+0.693-0.027, located in the Sgr B2 molecular cloud complex. Given theshort distance of the analysed outflow positions to the centre of Sgr B2(N1),we propose a scenario in which a phase of hot-core chemistry (i.e. thermaldesorption of ice species and high-temperature gas-phase chemistry) preceded ashock wave. The subsequent compression and further heating of the materialresulted in the accelerated destruction of (mainly O-bearing) molecules.Gas-phase formation of cyanides seems to be able to compete with theirdestruction in the post-shock gas. Abundances of HCnN (n=3,5) are enhanced inthe outflow component pointing to (additional) gas-phase formation. To confirmsuch a scenario, appropriate chemical shock models need to be run.

Shocking Sgr B2(N1) with its own outflow: A new perspective on segregation between O- and N-bearing molecules