Millimeter observations of isothiocyanic acid (HNCS) and its higher energy isomer, thiocyanic acid (HSCN), have been carried out toward Sgr?B2 and TMC-1 using the 12?m telescope of the Arizona Radio Observatory. For both species, the JKa,Kc ?= 80,8?? 70,7 and 90,9?? 80,8 transitions near 91-93?GHz and 103-106?GHz were mapped across a 6'?? 3' region, centered near Sgr?B2(M). Comparative mapping observations were also done for the JKa,Kc ?= 40,4?? 30,3 line of HNCO and HOCN near 84-87?GHz. In addition, the JKa,Kc ?= 70,7?? 60,6 and 80,8?? 70,7 transitions of both HNCS and HSCN were detected in TMC-1, the first identification of either molecule in a cold, dark cloud. Emission from HNCS and HSCN was found to be extended over the Sgr?B2 cloud, with a single velocity component and a linewidth of ~20-25?km?s?1. Column densities derived for HSCN in Sgr?B2 are typically N tot ~ (0.2-1)?? 1013?cm?2, with N tot ~ (0.8-5)?? 1013?cm?2 for the more stable isomer, HNCS. In TMC-1, these species have similar column densities of (6-8)?? 1010?cm?2. The [HNCS]/[HSCN] abundance ratio ranges from 2 to 7 in Sgr?B2, with a value of ~1 in TMC-1. In contrast, the [HNCO]/[HOCN] ratio in Sgr?B2 is ~110-250. Gas-grain chemical models do not reproduce the observed abundances of the sulfur isomers in either source. Given the energy difference of over 3200?K between HNCS and HSCN, these observations suggest that both molecules are produced from gas-phase, ion-molecule chemistry with a common precursor, HNCSH+. The oxygen analogs, in contrast, probably have a more complex chemical network, perhaps involving the H2NCO+ precursor, which preferentially leads to HNCO.
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