  Understanding the initial conditions of star formation requires both
observational studies and theoretical works taking into account the magnetic
field, which plays an important role in star formation processes. Herein, we
study the young nearby dense cloud core L1521 F ($n$(H$_2$) $\sim 10^{4-6}$
cm$^{-3}$) in the Taurus Molecular Cloud. This dense core hosts a 0.2 $M_\odot$
protostar, categorized as a Very Low Luminosity Objects with complex velocity
structures, particularly in the vicinity of the protostar. To trace the
magnetic field within the dense core, we conducted high sensitivity
submillimeter polarimetry of the dust continuum at $\lambda$= 850 $\mu$m and
450 $\mu$m using the POL-2 polarimeter situated in front of the SCUBA-2
submillimeter bolometer camera on James Clerk Maxwell Tetescope. This was
compared with millimeter polarimetry taken at $\lambda$= 3.3 mm with ALMA. The
magnetic field was detected at $\lambda$= 850 $\mu$m in the peripheral region,
which is threaded in a north-south direction, while the central region traced
at $\lambda$= 450 $\mu$m shows a magnetic field with an east-west direction,
i.e., orthogonal to that of the peripheral region. Magnetic field strengths are
estimated to be $\sim$70 $\mu$G and 200 $\mu$G in the peripheral- and
central-regions, respectively, using the Davis-Chandrasekhar-Fermi method. The
resulting mass-to-flux ratio of 3 times larger than that of magnetically
critical state for both regions indicates that L1521 F is magnetically
supercritical, i.e., gravitational forces dominate over magnetic turbulence
forces. Combining observational data with MHD simulations, detailed parameters
of the morphological properties of this puzzling object are derived for the
first time.
