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Title:
The magnetic field structure in W51A
Authors:
Chrysostomou, A.; Aitken, D. K.; Jenness, T.; Davis, C. J.; Hough, J. H.; Curran, R.; Tamura, M.
Affiliation:
AA(Dept of Physical Sciences, University of Hertfordshire, Hatfield, HERTS, AL10 9AB, UK ), AB(Dept of Physical Sciences, University of Hertfordshire, Hatfield, HERTS, AL10 9AB, UK ), AC(Joint Astronomy Centre, 660 N. A'ohoku Place, Hilo, HI 96720, USA ), AD(Joint Astronomy Centre, 660 N. A'ohoku Place, Hilo, HI 96720, USA ), AE(Dept of Physical Sciences, University of Hertfordshire, Hatfield, HERTS, AL10 9AB, UK ), AF(Dept of Physical Sciences, University of Hertfordshire, Hatfield, HERTS, AL10 9AB, UK ), AG(National Astronomical Observatory of Japan, Osawa, Mitaka, Tokyo 181-8588, Japan )
Publication:
Astronomy and Astrophysics, v.385, p.1014-1021 (2002) (A&A Homepage)
Publication Date:
04/2002
Origin:
A&A
A&A Keywords:
ISM: MAGNETIC FIELDS, ISM: INDIVIDUAL OBJECTS: W51A, STARS: FORMATION, TECHNIQUES: POLARIMETRIC, SUBMILLIMETER
DOI:
10.1051/0004-6361:20020154
Bibliographic Code:
2002A&A...385.1014C

Abstract

We present 850 mu m imaging polarimetry of the W51A massive star forming region performed with SCUBA on the JCMT. From the polarimetry we infer the column-averaged magnetic field direction, projected onto the plane of the sky. We find that the magnetic field geometry in the region is complicated. We compare the field geometry with 6 cm and CS J=7-6 emission and determine that the magnetic field must be relatively weak and plays a passive role, allowing itself to be shaped by pressure forces and dynamics in the ionised and neutral gases. Comparisons are drawn between our data and 1.3 mm BIMA interferometric polarimetry data, from which we conclude that the magnetic field must increase in importance as we move to smaller scales and closer to sites of active star formation. Table 2 is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/385/1014

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