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Magnetic fields of molecular clouds in the Central Molecular Zone (CMZ) havebeen relatively underobserved at sub-parsec resolution. Here we reportJCMT/POL2 observations of polarized dust emission in the CMZ, which revealmagnetic field structures in dense gas at ~0.5 pc resolution. The elevenmolecular 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' amongthe 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 usingthe angular dispersion function method. The morphologies of magnetic fields inthe clouds suggest potential imprints of feedback from expanding H II regionsand young massive star clusters. A moderate correlation between the total viralparameter versus the star formation rate and the dense gas fraction of theclouds is found. A weak correlation between the mass-to-flux ratio and the starformation rate, and a weak anti-correlation between the magnetic field and thedense gas fraction are also found. Comparisons between magnetic fields andother dynamic components in clouds suggest a more dominant role of self-gravityand turbulence in determining the dynamical states of the clouds and affectingstar formation at the studied scales.

Magnetic Fields in the Central Molecular Zone Influenced by Feedback and Weakly Correlated with Star Formation