Silicon monoxide and methanol emission from the NGC 2071 molecular outflow
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We report observations of emission in the J\3]2 and J\2]1 transitions of SiO and Jk\ 3k transitions of made with the Swedish-ESO Submillimeter Telescope (SEST), toward the ]2k CH3OH, high-velocity, collimated molecular outÑow in NGC 2071. Emission is detected from the lobes, as well as from the central core region, in both species. The spatial distribution of the SiO wing emission, which is detected over a velocity range of D50 km s~1, shows three distinct features : a blueshifted clump located toward the northeast, a redshifted clump located toward the southwest, and a central structure, with moderate redshifted velocities, located near the cluster of young stellar objects. The shape of the SiO proÐles from the northeast and southwest clumps are distinctly di erent. The SiO lines from the northeast clump exhibit a peak near the velocity of the ambient cloud and a gradual decline toward blueshifted velocities reaching Ñow velocities of up to [32 km s~1. On the other hand, the SiO proÐles from the southwest clump show a peak emission at a velocity that is redshifted by D8.5 km s~1 from the ambient gas velocity and a gradual decline in brightness toward the ambient cloud velocity. We suggest that the SiO emission from the clumps are signposts of working surfaces where a collimated jet is interacting with ambient material, and ascribe the di erences in line shape to di erences in the density of the environment under which the jet is propagating. The abundance of silicon monoxide in the outÑow lobes is found to be enhanced, with respect to that of quiescent ambient gas in dark globules, by at least 2 orders of magnitude (peak enhancement º500 in the southwest clump and º170 in the northeast clump). The abundance of methanol is considerably more enhanced in the southwest clump (peak enhancement of D500) than in the northwest clump (peak enhancement of D70). We suggest that the large enhancements of methanol and silicon monoxide in the outÑow clumps are most likely due to the release from grains of ice mantles and Si-bearing species via shocks produced by the interaction between the outÑow and dense ambient gas, and attribute the di erences in enhancements to the di erent shock velocities attained in the northeast clump (vsD45 km s~1) and southwest clump (vsD12 km s~1).
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