Extended ammonia observations towards the 'Integral-Shaped Filament'

Abstract

Recent observations suggest a scenario in which filamentary structures in the ISM represent the first step towards clumps/cores and eventually star formation. The densest filaments would then fragment into prestellar cores owing to gravitational instability. We seek to understand the roles filamentary structures play in high-mass star formation. We mapped the integral-shaped filament (ISF) in NH3 (1, 1) and (2, 2). The whole filamentary structure is uniformly and fully sampled. We find that the morphology revealed by the map of velocity-integrated intensity of the NH3 (1, 1) line is closely associated with the dust ridge. We identify 6 "clumps" related to the well known OMC-1 to 5 and 11 "sub-clumps" within the map and they are separated not randomly but in roughly equal intervals along the ISF. The average spacing of clumps is 11.30'$\pm$1.31' (1.36$\pm$0.16 pc ) and the average spacing of sub-clumps is 7.18'$\pm$1.19' (0.86$\pm$0.14 pc). These spacings agree well with the predicted values of the thermal (0.86 pc) and turbulent sausage instability (1.43 pc) by adopting a cylindric geometry of the ISF with an inclination of $60^{\circ }$ with respect to the line of sight. We also find a velocity gradient of about 0.6 km s-1 pc-1 that runs along the ISF which likely arises from an overall rotation of the Orion A molecular cloud. The inferred ratio between rotational and gravitational energy is well below unity. Furthermore, fluctuations are seen in the centroid velocity diagram along the ISF. The OMC-1 to 5 clouds are located close to the local extrema of the fluctuations, which suggests that there exist gas flows associated with these clumps in the ISF. The derived NH3 (1, 1) and (2, 2) rotation temperatures in the OMC-1 are about 30-40 K. In OMC-2, OMC-3, and the northern part of OMC-4, we find higher and lower temperatures at the boundaries and in the interior, respectively.

arXiv commentAccepted by A&A. 14 pages, 14 figures

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• OMC-2 FIR 4 under the microscope: Shocks, filaments, and a highly collimated jet at 100 au scales
• Molecular environs and triggered star formation around the large Galactic infrared bubble N 24
• Evidence for dense gas heated by the explosion in Orion KL
• NH${}_3$ (1,1) hyperfine intensity anomalies in the Orion A molecular cloud
• Ammonia observations towards the Aquila Rift cloud complex
• NH${}_3$ Observations of the S235 Star Forming Region: Dense Gas in Inter-core Bridges
• Filaments in the OMC-3 cloud and uncertainties in estimates of filament profiles
• Cloud-cloud collision and star formation in G013.313+0.193
• NH3 (1,1) hyperfine intensity anomalies in infall sources