# JCMT BISTRO survey: Magnetic Fields within the Hub-Filament Structure in IC 5146

## TL;DR

This study uses polarization observations at 850 μm to map magnetic fields in the IC 5146 hub-filament structure, revealing a curved magnetic field morphology, estimating its strength, and analyzing the role of magnetic fields in star formation.

## Contribution

It provides the first detailed magnetic field morphology and strength measurement within a core-scale hub-filament structure in IC 5146, using Bayesian analysis and the DCF method.

## Key findings

- Magnetic field shows a curved morphology possibly influenced by filament contraction.
- Magnetic field strength is estimated at 0.5±0.2 mG in the core region.
- Gravity and magnetic fields are of comparable importance, with turbulence playing a lesser role.

## Abstract

We present the 850 $\mu$m polarization observations toward the IC5146 filamentary cloud taken using the Submillimetre Common-User Bolometer Array 2 (SCUBA-2) and its associated polarimeter (POL-2), mounted on the James Clerk Maxwell Telescope (JCMT), as part of the B-fields In STar forming Regions Observations (BISTRO). This work is aimed at revealing the magnetic field morphology within a core-scale ($\lesssim 1.0$ pc) hub-filament structure (HFS) located at the end of a parsec-scale filament. To investigate whether or not the observed polarization traces the magnetic field in the HFS, we analyze the dependence between the observed polarization fraction and total intensity using a Bayesian approach with the polarization fraction described by the Rice likelihood function, which can correctly describe the probability density function (PDF) of the observed polarization fraction for low signal-to-noise ratio (SNR) data. We find a power-law dependence between the polarization fraction and total intensity with an index of 0.56 in $A_V\sim$ 20--300 mag regions, suggesting that the dust grains in these dense regions can still be aligned with magnetic fields in the IC5146 regions. Our polarization maps reveal a curved magnetic field, possibly dragged by the contraction along the parsec-scale filament. We further obtain a magnetic field strength of 0.5$\pm$0.2 mG toward the central hub using the Davis-Chandrasekhar-Fermi method, corresponding to a mass-to-flux criticality of $\sim$ $1.3\pm0.4$ and an Alfv\'{e}nic Mach number of $<$0.6. These results suggest that gravity and magnetic field is currently of comparable importance in the HFS, and turbulence is less important.