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We present the results of dust emission polarization measurements ofOphiuchus-B (Oph-B) carried out using the Submillimetre Common-User BolometerArray 2 (SCUBA-2) camera with its associated polarimeter (POL-2) on the JamesClerk Maxwell Telescope (JCMT) in Hawaii. This work is part of the B-fields InStar-forming Region Observations (BISTRO) survey initiated to understand therole of magnetic fields in star formation for nearby star-forming molecularclouds. We present a first look at the geometry and strength of magnetic fieldsin Oph-B. The field geometry is traced over $\sim$0.2 pc, with clear detectionof both of the sub-clumps of Oph-B. The field pattern appears significantlydisordered in sub-clump Oph-B1. The field geometry in Oph-B2 is more ordered,with a tendency to be along the major axis of the clump, parallel to thefilamentary structure within which it lies. The degree of polarizationdecreases systematically towards the dense core material in the two sub-clumps.The field lines in the lower density material along the periphery are smoothlyjoined to the large scale magnetic fields probed by NIR polarizationobservations. We estimated a magnetic field strength of 630$\pm$410 $\mu$G inthe Oph-B2 sub-clump using a Davis-Chandeasekhar-Fermi analysis. With thismagnetic field strength, we find a mass-to-flux ratio $\lambda$= 1.6$\pm$1.1,which suggests that the Oph-B2 clump is slightly magnetically supercritical.

Magnetic fields towards Ophiuchus-B derived from SCUBA-2 polarization measurements