A quantitative analysis of OCN super(-) formation in interstellar ice analogs

The 4.62 mu m absorption band, observed along the line-of-sight towards various young stellar objects, is generally used as a qualitative indicator for energetic processing of interstellar ice mantles. This interpretation is based on the excellent fit with OCN super(-), which is readily formed by ultraviolet (UV) or ion-irradiation of ices containing H sub(2)O, CO and NH sub(3). However, the assignment requires both qualitative and quantitative agreement in terms of the efficiency of formation as well as the formation of additional products. Here, we present the first quantitative results on the efficiency of laboratory formation of OCN super(-) from ices composed of different combinations of H sub(2)O, CO, CH sub(3)OH, HNCO and NH sub(3) by UV- and thermally-mediated solid state chemistry. Our results show large implications for the use of the 4.62 mu m feature as a diagnostic for energetic ice-processing. UV-mediated formation of OCN super(-) from H sub(2)O/CO/NH sub(3) ice matrices falls short in reproducing the highest observed interstellar abundances. In this case, at most 2.7% OCN super(-) is formed with respect to H sub(2)O under conditions that no longer apply to a molecular cloud environment. On the other hand, photoprocessing and in particular thermal processing of solid HNCO in the presence of NH sub(3) are very efficient OCN super(-) formation mechanisms, converting 60%-85% and similar to 100%, respectively of the original HNCO. We propose that OCN super(-) is most likely formed thermally from HNCO given the ease and efficiency of this mechanism. Upper limits on solid HNCO and the inferred interstellar ice temperatures are in agreement with this scenario.