February 2015

Hydroxylamine

Studies have suggested that hydroxylamine (NH2OH) should be formed under various astrophysical processing conditions, but a recent search for it by Pulliam et al. in 2012 toward a number of sources, including IRC+10216, Orion KL, Orion S, Sgr B2(N), Sgr B2(OH), W3IRS5, and W51M, was unsuccessful. Observations were made with the NRAO 12m telescope on Kitt Peak of 14 rotational transitions. A modeling study by Garrod, Widicus Weaver, and Herbst predicted that sufficient hydroxylamine should be produced by grain surface reactions, but upper detection limit determined by Pulliam et al. is about a million times less than the predicted abundance.

A preliminary report from 2013 suggested that hydroyxlamine had been detected toward the protostar L1157 with CARMA, but the subsequent publication by McGuire et al. only noted non-detection of multiple transitions.

UPDATE (2019): Yet another attempt to detect hydroxylamine, by Ligterink et al. reported late in 2018, failed to find the molecule toward the solar-like protostar IRAS 16293-2422B. On the basis of experiments, Jonusas & Krim observed that NH2OH may react before it can be desorbed from the ice surfaces where it is thought to be formed.


The Astrochymist homepage
Maintained by DE Woon
Links verified / updated 1 July 2019