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

Abstract

We present the first 850 $\hat{I}¼$m polarization observations in the most active star-forming site of the Rosette Molecular Cloud (RMC, $d\sim$1.6 kpc) in the wall of the Rosette Nebula, imaged with the SCUBA-2/POL-2 instruments of the JCMT, 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 decreases with the 850 $\hat{I}¼$m continuum intensity with $\hat{I}\pm$ = 0.49 $\pm$ 0.08 in the $p\propto I^{-\hat{\mathrm{I}}\pm }$ relation, which suggests that some fraction of the dust grains remain aligned at high densities. The north of our 850 $\hat{I}¼$m image reveals a "gemstone ring" morphology, which is a $\sim$1 pc-diameter ring-like structure with extended emission in the "head" to the south-west. We hypothesize that it might have been blown by feedback in its interior, while the B-field is parallel to its circumference in most places. In the south of our SCUBA-2 field the clumps are apparently connected with filaments which follow Infrared Dark Clouds (IRDCs). Here, the POL-2 magnetic field orientations appear bimodal with respect to the large-scale Planck field. The mass of our effective mapped area is $\sim$ 174 $M_{\odot }$ that we calculate from 850 $\hat{I}¼$m flux densities. We compare our results with masses from large-scale emission-subtracted Herschel 250 $\hat{I}¼$m data, and find agreement within 30%. We estimate the POS B-field strength in one typical subregion using the Davis-Chandrasekhar-Fermi (DCF) technique and find 80 $\pm$ 30 $\hat{I}¼$G toward a clump and its outskirts. The estimated mass-to-flux ratio of $\hat{I}»$ = 2.3 $\pm$ 1.0 suggests that the B-field is not sufficiently strong to prevent gravitational collapse in this subregion.

15 pages (12+3), 9 figures, 1 table. Accepted for publication in the Astrophysical Journal