Detection of Magnetic Fields in M17 through the HI Zeeman Effect

Details Detection of Magnetic Fields in M17 through the HI Zeeman Effect Detection of Magnetic Fields in M17 through the HI Zeeman Effect

May 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aas...190.0611b&link_type=abstract

American Astronomical Society, 190th AAS Meeting, #06.11; Bulletin of the American Astronomical Society, Vol. 29, p.785

Astronomy and Astrophysics

Astronomy

Scientific paper

We have carried out VLA Zeeman observations of \ion {H} {2} absorption lines toward the \ion {H} {2} region in the M17 giant molecular cloud complex. The resulting maps have 45''/x60''/ spatial resolution and 0.64 kms(-1) velocity resolution. M17 provides a unique opportunity to investigate the interaction of an \ion {H} {2} region-molecular cloud interface due its edge-on geometry. The \ion {H} {1} absorption lines toward M17 show between 5 and 8 distinct velocity components. We explore possible physical connections between these components and the M17 region based on calculations of \ion {H} {1} column densities, line of sight magnetic field strengths, as well as comparisons with a wide array of previous optical, infrared, and radio observations. These analyses have led us to adopt a model in which at least two of these \ion {H} {1} components originate from \ion {H} {1} gas in the PDR which has formed at the southwestern \ion {H} {2} region-molecular cloud boundary. In particular, a component at the same velocity as the M17 molecular cloud ~ 20 kms(-1) seems to originate from the edge-on interface between the \ion {H} {2} region and molecular cloud in the southwestern part of the source. For this component we have detected a steep peaking up of both the \ion {H} {1} column density divided by spin temperature (>=5.6x10(19) cm(-2) /K) and line of sight magnetic field strengths (Blos ~ -450 mu G) toward this boundary. In addition, we believe that the blended component at velocities between 12 to 16 kms(-1) originates from the front side of the PDR which has formed between the \ion {H} {2} region and a lip of molecular gas which is believed to have curved around like a bowl to obscure the Southern bar of the \ion {H} {2} region. The peak \ion {H} {1} column density divided by spin temperature and Blos for this component is >=4.4x10(19) cm(-2) /K and ~ 550 mu G respectively. Magnetic field detections were also made at 4, 6, and 25 kms(-1) .

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