Hydroxyl maser disc and outflow in the Orion-BN/KL region

• Published in: Monthly notices of the Royal Astronomical Society Vol. 367; no. 2; pp. 541 - 552
• Main Authors: Cohen, R. J., Gasiprong, N., Meaburn, J., Graham, M. F.
• Format: Journal Article
• Language: English
• Published: Oxford, UK Blackwell Science Ltd 01-04-2006; Blackwell Science; Oxford University Press
• Subjects: Astronomy; Astrophysics; Data analysis; Earth, ocean, space; Exact sciences and technology; ISM: individual: Orion-BN/KL; ISM: jets and outflows; Kinematics; magnetic fields; masers; polarization; Radio astronomy; stars: formation; stars: formation; ISM: jets and outflows; polarization; magnetic fields; masers; ISM: individual: Orion-BN/KL; Runaway stars; Polarization; Compact radiosource; Molecular flow; Radiowave interferometers; Rotation axis; Shock front; Continuum; Star formation; Tori; Rotating disk; Masers; Kinematics; Cosmic radio sources; Jets; Radial velocity; Position angle; Magnetic fields; Diameter; Proper motion
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1111/j.1365-2966.2006.10021.x

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 +42 km s−1. 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 16.3 mG, with a possible reversal. No OH masers were found associated with even the most prominent proplyds within 10 arcsec of θ1 Ori C.