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Solid state astrochemical reaction pathways have the potential to link theformation of small nitrogen-bearing species, like NH3 and HNCO, and prebioticmolecules, specifically amino acids. To date, the chemical origin of such smallnitrogen containing species is still not well understood, despite the fact thatammonia is an abundant constituent of interstellar ices toward young stellarobjects and quiescent molecular clouds. This is mainly because of the lack ofdedicated laboratory studies. The aim of the present work is to experimentallyinvestigate the formation routes of NH3 and HNCO through non-energetic surfacereactions in interstellar ice analogues under fully controlled laboratoryconditions and at astrochemically relevant temperatures. This study focuses onthe formation of NH3 and HNCO in CO-rich (non-polar) interstellar ices thatsimulate the CO freeze-out stage in dark interstellar cloud regions, wellbefore thermal and energetic processing start to become relevant. Wedemonstrate and discuss the surface formation of solid HNCO through theinteraction of CO molecules with NH radicals - one of the intermediates in theformation of solid NH3 upon sequential hydrogenation of N atoms. The importanceof HNCO for astrobiology is discussed.

Low Temperature Surface Formation of NH3 and HNCO: hydrogenation of nitrogen atoms in CO-rich interstellar ice analogues