A quantitative analysis of OCN^- formation in interstellar ice analogs

¹ Raymond and Beverly Sackler Laboratory for Astrophysics, Leiden Observatory, PO Box 9513, 2300 RA Leiden, The Netherlands
² NASA-Ames Research Center, Mail Stop 245-3, Moffett Field, CA 94035, USA

Corresponding author: F.A. van Broekhuizen, fvb@strw.leidenuniv.nl

Received: 5 August 2003
Accepted: 5 November 2003

Abstract

The 4.62 μm 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^-, which is readily formed by ultraviolet (UV) or ion-irradiation of ices containing H₂O, CO and NH₃. 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^- from ices composed of different combinations of H₂O, CO, CH₃OH, HNCO and NH₃ by UV- and thermally-mediated solid state chemistry. Our results show large implications for the use of the 4.62 μm feature as a diagnostic for energetic ice-processing. UV-mediated formation of OCN^- from H₂O/CO/NH₃ ice matrices falls short in reproducing the highest observed interstellar abundances. In this case, at most 2.7% OCN^- is formed with respect to H₂O 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 NH₃ are very efficient OCN^- formation mechanisms, converting 60%–85% and ~100%, respectively of the original HNCO. We propose that OCN^- 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.