  In order to develop a more comprehensive picture of star formation, it is
essential to understand the physical relationship between dense cores and the
filaments embedding them. There is evidence that magnetic fields play a crucial
role in this context. We aim to understand how magnetic fields influence the
properties and kinematics of an isolated filament located east of the Barnard
59 clump, belonging to the Pipe Nebula. We use near infrared polarization
observations to determine the magnetic field configuration, and we apply the
Davis Chandrasekhar Fermi method to infer the magnetic field strength in the
plane of the sky. Furthermore, we use complementary data from the James Clerk
Maxwell Submillimetre Telescope (JCMT) of C18O and 13CO J=3-2 transition to
determine the filament's kinematics. Finally, we model the radial density
profile of the filament with polytropic cylindrical models. Our results
indicate that the filament is stable to radial collapse and is radially
supported by agents other than thermal pressure. In addition, based on previous
observations of emission lines on this source, we suggest that gas is flowing
toward the hub, while C18O (3-2) non-thermal motions indicate that the cloud is
in a quiescent state.
