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G23.33-0.30 is a 600 $M_{\odot}$ infrared dark molecular filament thatexhibits large NH$_3$ velocity dispersions ($\sigma \sim 8 \ \rm{km \ s^{-1}}$)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 byfour rare NH$_3$(3,3) masers, which are excited by a large-scale shockimpacting the filament. G23.33-0.30 also displays a velocity gradient along itslength, a velocity discontinuity across its width, shock-tracing SiO(5-4)emission extended throughout the filament, broad turbulent line widths inNH$_3$(1,1) through (6,6), CS(5-4), and SiO(5-4), as well as an increasedNH$_3$ rotational temperature ($T_{\rm{rot}}$) and velocity dispersion($\sigma$) associated with the shocked, blueshifted component. The correlationsamong $T_{\rm{rot}}$, $\sigma$, and $V_{\rm{LSR}}$ implies that the shock isaccelerating, heating, and adding turbulent energy to the filament gas. GivenG23.33-0.30's location within the giant molecular cloud G23.0-0.4, we speculatethat the shock and NH$_3$(3,3) masers originated from the supernova remnantW41, which exhibits additional evidence of an interaction with G23.0-0.4. Wehave also detected the 1.3 mm dust continuum emission from at least threeembedded molecular cores associated with G23.33-0.30. Although the cores havemoderate gas masses ($M = 7-10$ M$_{\odot}$), their large virial parameters($\alpha=4-9$) suggest that they will not collapse to form stars. The turbulentline widths of the cores may indicate negative feedback due to the SNR shock.

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