Mon. Not. R. Astron. Soc., 367, 541-552 (2006/April-1)
Hydroxyl maser disc and outflow in the Orion-BN/KL region.
COHEN R.J., GASIPRONG N., MEABURN J. and GRAHAM M.F.
Abstract (from CDS):
Multi Element Radio Linked Interferometer Network (MERLIN) measurements of 1.6-GHz hydroxyl (OH) masers associated with Orion-Becklin-Neugebauer/Kleinmann-Low (Orion-BN/KL) are presented, and the data are compared with data on other masers, molecular lines, compact radio continuum sources and infrared sources in the region. OH masers are detected over an area of 30 arcsec in diameter, with the majority lying along an approximately E-W structure that extends for ∼18 arcsec, encompassing the infrared sources IRc2, IRc6 and IRc7. Radial velocities range from -13 to +42km/s. The system of OH masers shows a velocity gradient together with non-circular motions. The kinematics are modelled in terms of an expanding and rotating disc or torus. The rotation axis is found to be in the same direction as the molecular outflow. There is an inner cavity of radius ∼1300 au with no OH masers. The inner cavity, like the H2O `shell' masers and SiO masers, is centred on radio source I. Some of the OH masers occur in velocity-coherent strings or arcs that are longer than 5 arcsec (2250 au). One such feature, Stream A, is a linear structure at position angle ∼45°, lying between IRc2 and BN. We suggest that these masers trace shock fronts, and have appeared, like a vapour trail, 200 yr after the passage of the runaway star BN. The radio proper motions of BN, source I and source n project back to a region near the base of Stream A that is largely devoid of OH masers. The 1612-MHz masers are kinematically distinct from the other OH masers. They are also more widely distributed and appear to be associated with the outflow as traced by H2O masers and by the 2.12-µm emission from shocked H2. The magnetic field traced by the OH masers ranges from 1.8 to 16.3mG, with a possible reversal. No OH masers were found associated with even the most prominent proplyds within 10 arcsec of θ1 Ori C.
2006 The Authors. Journal compilation © 2006 RAS
magnetic fields - masers - polarization - stars: formation - ISM: individual: Orion-BN/KL - ISM: jets and outflows
Table 1: [CGM2006] 1612L NN (Nos 1-10), [CGM2006] 1612R N (No. 1), [CGM2006] 1665L NNN (Nos 1-204), [CGM2006] 1665R NNN (Nos 1-226), [CGM2006] 1667L N (Nos 1-3). Fig.1: [CGM2006] Stream A (No. A), [CGM2006] Arc B N=1.
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