From theory to observation: understanding filamentary flows in high-mass star-forming clusters

Abstract

Here we use data from multi-scale galactic MHD simulations to observe filaments and star forming clumps on 10's of pc scales and investigate flow rate relationships along, and onto filaments as well as flows towards the clumps. Using the FilFinderPPV identification technique, we identify the prominent filamentary structures in each data cube. Each filament and its corresponding clump are analysed by calculating flow rates along each filament towards the clump, onto each filament from increasing distances, and radially around each clump. This analysis is conducted for two cubes, one feedback dominated region, and one with less feedback. Looking at the face-on inclination of the simulations (0 degrees), we observe different trends depending on the environmental conditions (more or less feedback). The median flow rate in the region with more feedback is 8.9$\times$10${}^{-5}$ M${}_{sun}{\mathrm{yr}}^{-1}$ and we see that flow rates along the filaments toward the clumps generally decrease in these regions. In the region with less feedback we have a median flow rate of 2.9$\times$10${}^{-4}$ M${}_{sun}{\mathrm{yr}}^{-1}$ and when looking along the filaments here we see the values either increase or remain constant. We find that the flow rates from the environments onto the primary filaments are of an order of magnitude sufficient to sustain the flow rates along these filaments. When discussing the effects of galactic and filamentary inclination, we also observe that viewing the filaments from different galactic inclinations can reveal the presence of feeder structures (smaller filamentary structures aiding in the flow of material). The method used to estimate these flow rates, which has been previously applied to observational data, produced results consistent with those obtained from the simulations themselves, providing high confidence in the flow rate calculation method.

13 pages, 14 figures, accepted for publication in A&A

References in corpus (15)

• Filamentary structure of star-forming complexes
• ATLASGAL --- properties of a complete sample of Galactic clumps
• The link between turbulence, magnetic fields, filaments, and star formation in the Central Molecular Zone cloud G0.253+0.016
• A Galactic-scale gas wave in the Solar Neighborhood
• The dynamical properties of dense filaments in the infrared dark cloud G035.39-00.33
• ALMA observations of massive molecular gas filaments encasing radio bubbles in the Phoenix cluster
• On the Three-Dimensional Structure of Local Molecular Clouds
• The Hi-GAL catalogue of dusty filamentary structures in the Galactic Plane
• Magnetized interstellar molecular clouds: II. The Large-Scale Structure and Dynamics of Filamentary Molecular Clouds
• Dynamical cloud formation traced by atomic and molecular gas
• Dynamical Accretion Flows -- ALMAGAL: Flows along filamentary structures in high-mass star-forming clusters
• Necessary conditions for the formation of filaments and star clusters in the cold neutral medium
• Emergence of high-mass stars in complex fiber networks (EMERGE) V. From filaments to spheroids: the origin of the hub-filament systems
• Rotation of Two Micron All Sky Survey Clumps in Molecular Clouds
• The Milky Way atlas for linear filaments II. clump rotation versus filament orientation

Cited by in corpus (1)

• From inter-filamentary gas to filaments and hubs: gas flows in the Mon R2 hub-filament system