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We present the first 850 $\mu$m polarization observations in the most activestar-forming site of the Rosette Molecular Cloud (RMC, $d\sim$1.6 kpc) in thewall of the Rosette Nebula, imaged with the SCUBA-2/POL-2 instruments of theJCMT, as part of the B-Fields In Star-Forming Region Observations 2 (BISTRO-2)survey. From the POL-2 data we find that the polarization fraction decreaseswith the 850 $\mu$m continuum intensity with $\alpha$ = 0.49 $\pm$ 0.08 in the$p \propto I^{\rm -\alpha}$ relation, which suggests that some fraction of thedust grains remain aligned at high densities. The north of our 850 $\mu$m imagereveals a "gemstone ring" morphology, which is a $\sim$1 pc-diameter ring-likestructure with extended emission in the "head" to the south-west. Wehypothesize that it might have been blown by feedback in its interior, whilethe B-field is parallel to its circumference in most places. In the south ofour SCUBA-2 field the clumps are apparently connected with filaments whichfollow Infrared Dark Clouds (IRDCs). Here, the POL-2 magnetic fieldorientations appear bimodal with respect to the large-scale Planck field. Themass of our effective mapped area is $\sim$ 174 $M_\odot$ that we calculatefrom 850 $\mu$m flux densities. We compare our results with masses fromlarge-scale emission-subtracted Herschel 250 $\mu$m data, and find agreementwithin 30%. We estimate the POS B-field strength in one typical subregion usingthe Davis-Chandrasekhar-Fermi (DCF) technique and find 80 $\pm$ 30 $\mu$Gtoward a clump and its outskirts. The estimated mass-to-flux ratio of $\lambda$= 2.3 $\pm$ 1.0 suggests that the B-field is not sufficiently strong to preventgravitational collapse in this subregion.

The JCMT BISTRO-2 Survey: The Magnetic Field in the Center of the Rosette Molecular Cloud