On the nature of star-forming filaments: I. Filament morphologies

TL;DR

This study uses high-resolution simulations to analyze star-forming filament structures, revealing their morphology, width variability, and sub-filament composition, aligning well with recent observations without requiring magnetic support.

Contribution

It provides a detailed simulation-based analysis of filament morphologies, widths, and sub-structures, challenging previous assumptions about magnetic support and filament formation processes.

Findings

Filaments fit well with Plummer-like profiles and have shallow power-law indices.

Average filament width is ~0.3 pc, with variations depending on the fitting method.

Filaments are composed of networks of short sub-filaments formed by cloud collapse.

Abstract

We use a suite of high resolution molecular cloud simulations carried out with the moving mesh code Arepo to explore the nature of star-forming filaments. The simulated filaments are identified and categorised from column density maps in the same manner as for recent Herschel observations. When fit with a Plummer-like profile the filaments are in excellent agreement with observations, and have shallow power-law profiles of p~2.2 without the need for magnetic support. When data within 1 pc of the filament centre is fitted with a Gaussian function, the average FWHM is ~0.3 pc, in agreement with predictions for accreting filaments. However, if the fit is constructed using only the inner regions, as in Herschel observations, the resulting FWHM is only ~0.2 pc. This value is larger than that measured in IC 5146 and Taurus, but is similar to that found in the Planck Galactic Cold Cores and in Cygnus X. The simulated filaments have a range of widths rather than a constant value. When the column density maps are compared to the 3D gas densities, the filaments seen in column density do not belong to a single structure. Instead, they are made up of a network of short ribbon-like sub-filaments reminiscent of those seen in Taurus. The sub-filaments are pre-existing within the simulated clouds, have radii similar to their Jeans radius, and are not primarily formed through fragmentation of the larger filament seen in column density. Instead, small filamentary clumps are swept together into a single column density structure by the large-scale collapse of the cloud.