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

G23.33-0.30 is a 600 M infrared dark molecular filament that exhibits large NH3 velocity dispersions ( ∼ 8 km s−1) and bright, narrow NH3(3, 3) line emission. We have probed G23.33-0.30 at the < 0.1 pc scale and confirmed that the narrow NH3(3, 3) line is emitted by four rare NH3(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, and broad turbulent line widths in NH3(1, 1) through (6, 6), CS(5-4), and SiO(5-4), as well as an increased NH3 rotational temperature (Trot) and velocity dispersion ( ) associated with the shocked, blueshifted component. The correlations among Trot, , and VLSR imply 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 NH3(3, 3) masers originated from the supernova remnant (SNR) 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 ), their large virial parameters ( = 4-9) suggest that they will not collapse to form stars. The turbulent line widths of the ( > 1) cores may indicate negative feedback due to the SNR shock.