Unveiling the role of magnetic fields in a filament accreting onto a young protocluster

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Table 2

Physical parameters for the three regions of the filament from Eq. (9).

Region	δB/B₀	m (rad pc⁻¹)	B_pos (μG)	$B_{p o s}^{* (a)} (μ G)$ $\[B_{\mathrm{pos}}^{*(a)}(\mu \mathrm{G})\]$	N(H₂)(cm⁻²)	λ^(b)
R1	0.39 ± 0.02	1.6 ± 0.2	151 ± 6	66 ± 1	4.1 ×10²¹	0.27 ± 0.04
R2	0.26 ± 0.01	3.57 ± 0.06	222 ± 9	80 ± 1	3.9 ×10²¹	0.13 ± 0.02
R3	0.25 ± 0.06	13.5 ± 0.2	234 ± 6	83 ± 8	3.9 ×10²¹	0.13 ± 0.02

Notes. ^(a) $B_{pos}^{*}$ $\[B_{\text {pos }}^*\]$ is the B-field strength calculated from Skalidis & Tassis (2021). ^(b)λ is cloud stability; see Sect. 4.3. In all computations, we considered δ = 10 mpc, obtained from Franco et al. (2010).

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