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

The Interaction between the Supernova Remnant W41 and the Filamentary Infrared Dark Cloud G23.33-0.30Hogge, Taylor G.Jackson, James M.Allingham, DavidGuzman, Andres E.Killerby-Smith, NicholasKraemer, Kathleen E.Sanhueza, PatricioStephens, Ian W.Whitaker, J. ScottDOI: info:10.3847/1538-4357/ab5180v. 88779
Hogge, Taylor G., Jackson, James M., Allingham, David, Guzman, Andres E., Killerby-Smith, Nicholas, Kraemer, Kathleen E., Sanhueza, Patricio, Stephens, Ian W., and Whitaker, J. Scott. 2019. "The Interaction between the Supernova Remnant W41 and the Filamentary Infrared Dark Cloud G23.33-0.30." The Astrophysical Journal 887:79. https://doi.org/10.3847/1538-4357/ab5180
ID: 154525
Type: article
Authors: Hogge, Taylor G.; Jackson, James M.; Allingham, David; Guzman, Andres E.; Killerby-Smith, Nicholas; Kraemer, Kathleen E.; Sanhueza, Patricio; Stephens, Ian W.; Whitaker, J. Scott
Abstract: G23.33-0.30 is a 600 M infrared dark molecular filament that exhibits large NH3 velocity dispersions (σ ∼ 8 km s−1) and bright, narrow NH3(3, 3) line emission. We have probed G23.33-0.30 at the (3, 3) line emission. We have probed G23.33-0.30 at the 3(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 (T rot) and velocity dispersion (σ) associated with the shocked, blueshifted component. The correlations among T rot, σ, and V LSR 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 (α = 4─9) suggest that they will not collapse to form stars. The turbulent line widths of the (α > 1) cores may indicate negative feedback due to the SNR shock.