The JCMT BISTRO Survey: The magnetic field strength in the Orion A filament

We determine the magnetic field strength in the OMC 1 region of the Orion A filament via a new implementation of the Chandrasekhar-Fermi method using observations performed as part of the James Clerk Maxwell Telescope (JCMT) B-Fields In Star-Forming Region Observations (BISTRO) survey with the POL-2 instrument. We combine BISTRO data with archival SCUBA-2 and HARP observations to find a plane-of-sky magnetic field strength in OMC 1 of \(B_{\rm pos}=6.6\pm4.7\) mG, where \(\delta B_{\rm pos}=4.7\) mG represents a predominantly systematic uncertainty. We develop a new method for measuring angular dispersion, analogous to unsharp masking. We find a magnetic energy density of \(\sim1.7\times 10^{-7}\) Jm\(^{-3}\) in OMC 1, comparable both to the gravitational potential energy density of OMC 1 (\(\sim 10^{-7}\) Jm\(^{-3}\)), and to the energy density in the Orion BN/KL outflow (\(\sim 10^{-7}\) Jm\(^{-3}\)). We find that neither the Alfv\'{e}n velocity in OMC 1 nor the velocity of the super-Alfv\'{e}nic outflow ejecta is sufficiently large for the BN/KL outflow to have caused large-scale distortion of the local magnetic field in the \(\sim\)500-year lifetime of the outflow. Hence, we propose that the hour-glass field morphology in OMC 1 is caused by the distortion of a primordial cylindrically-symmetric magnetic field by the gravitational fragmentation of the filament and/or the gravitational interaction of the BN/KL and S clumps. We find that OMC 1 is currently in or near magnetically-supported equilibrium, and that the current large-scale morphology of the BN/KL outflow is regulated by the geometry of the magnetic field in OMC 1, and not vice versa.