https://ogma.newcastle.edu.au/vital/access/ /manager/Index en-au 5 https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:43521 Wed 21 Sep 2022 11:25:22 AEST ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:38094 ⊙ 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 < 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 (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.]]> Tue 03 Aug 2021 18:28:28 AEST ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:41371 50 km), which are rather stationary. The methodology is deliberately chosen to highlight the locations of small-scale influences that are generally variable in both time and space. We may fortuitously find a potential new way to recognize bursts of irregular pulsations (Pi1B) using low-Earth orbit satellites.]]> Tue 02 Aug 2022 15:27:31 AEST ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:17377 Sat 24 Mar 2018 08:01:31 AEDT ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:24311 Sat 24 Mar 2018 07:14:39 AEDT ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:50741 Fri 04 Aug 2023 08:26:09 AEST ]]>