The Interaction Between the Supernova Remnant W41 and the Filamentary Infrared Dark Cloud G23.33-0.30

Abstract

G23.33-0.30 is a 600 $M_{\odot }$ infrared dark molecular filament that exhibits large NH${}_3$ velocity dispersions ($\sigma \sim 8\mathrm{km}{\mathrm{s}}^{-1}$) and bright, narrow NH${}_3$(3,3) line emission. We have probed G23.33-0.30 at the $<0.1$ pc scale and confirmed that the narrow NH${}_3$(3,3) line is emitted by four rare NH${}_3$(3,3) masers, which are excited by a large-scale shock impacting the filament. G23.33-0.30 also displays a velocity gradient along its length, a velocity discontinuity across its width, shock-tracing SiO(5-4) emission extended throughout the filament, broad turbulent line widths in NH${}_3$(1,1) through (6,6), CS(5-4), and SiO(5-4), as well as an increased NH${}_3$ rotational temperature ($T_{\mathrm{rot}}$) and velocity dispersion ($\sigma$) associated with the shocked, blueshifted component. The correlations among $T_{\mathrm{rot}}$, $\sigma$, and $V_{\mathrm{LSR}}$ implies that the shock is accelerating, heating, and adding turbulent energy to the filament gas. Given G23.33-0.30's location within the giant molecular cloud G23.0-0.4, we speculate that the shock and NH${}_3$(3,3) masers originated from the supernova remnant W41, which exhibits additional evidence of an interaction with G23.0-0.4. We have also detected the 1.3 mm dust continuum emission from at least three embedded molecular cores associated with G23.33-0.30. Although the cores have moderate gas masses ($M=7-10$ M${}_{\odot }$), their large virial parameters ($\alpha =4-9$) suggest that they will not collapse to form stars. The turbulent line widths of the cores may indicate negative feedback due to the SNR shock.

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