  We present the first analysis in NGC2071-North as a resolved hub-filament
featuring a double centre. This $\sim 1.5 \times 1.5$ parsec-scale filament hub
contains $\sim$500 $M_\odot$. Seen from Planck, magnetic field lines may have
facilitated the gathering of material at this isolated location. The energy
balance analysis, supported by infalling gas signatures, reveal that these
filaments are currently forming stars. Herschel 100 $\mu$m emission
concentrates in the hub, at IRAS 05451+0037 and LkH$\alpha$ 316, and presents
diffuse lobes and loops around them. We suggest that such a double centre could
be formed, because the converging locations of filament pairs are offset, by
2.3$'$ (0.27 pc). This distance also matches the diameter of a hub-ring, seen
in column density and molecular tracers, such as HCO$^+$(1$-$0) and HCN(1$-$0),
that may indicate a transition and the connection between the hub and the
radiating filaments. We argue that all of the three components of the emission
star LkH$\alpha$ 316 are in physical association. We find that a $\sim$0.06
pc-sized gas loop, attached to IRAS 05451+0037, can be seen at wavelengths all
the way from Pan-STARRS-i to Herschel-100 $\mu$m. These observations suggest
that both protostars at the double hub centre are interacting with the cloud
material. In our $^{13}$CO data, we do not seem to find the outflow of this
region that was identified in the 80s with much lower resolution.
