  Magnetic fields of molecular clouds in the Central Molecular Zone (CMZ) have
been relatively underobserved at sub-parsec resolution. Here we report
JCMT/POL2 observations of polarized dust emission in the CMZ, which reveal
magnetic field structures in dense gas at ~0.5 pc resolution. The eleven
molecular clouds in our sample including two in the western part of the CMZ
(Sgr C and a far-side cloud candidate), four around the Galactic longitude 0
(the 50 km s-1 cloud, CO0.02-0.02, the `Stone' and the `Sticks & Straw' among
the Three Little Pigs), and five along the Dust Ridge (G0.253+0.016, clouds b,
c, d, and e/f), for each of which we estimate the magnetic field strength using
the angular dispersion function method. The morphologies of magnetic fields in
the clouds suggest potential imprints of feedback from expanding H II regions
and young massive star clusters. A moderate correlation between the total viral
parameter versus the star formation rate and the dense gas fraction of the
clouds is found. A weak correlation between the mass-to-flux ratio and the star
formation rate, and a weak anti-correlation between the magnetic field and the
dense gas fraction are also found. Comparisons between magnetic fields and
other dynamic components in clouds suggest a more dominant role of self-gravity
and turbulence in determining the dynamical states of the clouds and affecting
star formation at the studied scales.
