Abstract:
We present the results of 850 μm polarization and C18O (3 − 2) line observations toward the western hub-filament
structure (W-HFS) of the dark Streamer in IC 5146 using the James Clerk Maxwell Telescope SCUBA-2/POL-2
and HARP instruments. We aim to investigate how the relative importance of the magnetic field, gravity, and
turbulence affects core formation in HFS by comparing the energy budget of this region. We identified four
850 μm cores and estimated the magnetic field strengths (Bpos) of the cores and the hub and filament using the
Davis–Chandrasekhar–Fermi method. The estimated Bpos is ∼80 to 1200 μG. From Wang et al., Bpos of E-47, a
core in the eastern hub (E-hub), and E-hub were reestimated to be 500 and 320 μG, respectively, with the same
method. We measured the gravitational (EG), kinematic (EK), and magnetic energies (EB) in the filament and hubs
and compared the relative importance among them. We found that an EB-dominant filament has aligned
fragmentation type, while EG-dominant hubs show no and clustered fragmentation types. In the EG dominant hubs,
it seems that the portion of EK determines whether the hub becomes to have clustered (the portion of EK ∼ 20%) or
no fragmentation type (∼10%). We propose an evolutionary scenario for the E- and W-HFSs, where the HFS
forms first by the collision of turbulent flows, and then the hubs and filaments can go into various types of
fragmentation depending on their energy balance of gravity, turbulence, and magnetic field.
