Total linear polarization in the OH maser W75N: VLBA polarization structure.

Details Total linear polarization in the OH maser W75N: VLBA polarization structure. Total linear polarization in the OH maser W75N: VLBA polarization structure.

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aas...19915504m&link_type=abstract

American Astronomical Society, 199th AAS Meeting, #155.04; Bulletin of the American Astronomical Society, Vol. 34, p.562

Astronomy and Astrophysics

Astronomy

Scientific paper

W75N is a star-forming region containing various ultra-compact HII regions and OH, H2O, and CH3OH maser emission. Our VLBA map shows that the OH masers are located in a thin disk rotating around an O-star which is the exciting star of the ultra-compact HII region VLA1. A separate set of maser spots is connected with the ultra-compact HII region VLA2. The radial velocity of OH maser spots varies across the disc from 3.7 km s-1 to 10.9 km s-1. The diameter of the disk is 4000 A.U. All maser spots are strongly polarized. This are the first OH masers showing nearly 100 per cent linear polarization in several spots. Two maser spots seem to be Zeeman pairs corresponding to a magnetic field of 5.2 mgauss and 7.7 mgauss and in one case we tentatively found a Zeeman pair consisting of two linearly polarized components. The linearly polarized maser spots are shown to be from σ -components which is the case of the magnetic field being perpendicular to the line of sight. The direction of the magnetic field as determined from linearly polarized spots is perpendicular to the plane of the disk, although the galactic Faraday rotation may significantly affect this conclusion.

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