The Ammonia Distribution on 4000 AU Scales Near S106FIR

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Session 82 -- HII Regions
Display presentation, Wednesday, 11, 1995, 9:20am - 6:30pm

[82.10] The Ammonia Distribution on 4000 AU Scales Near S106FIR

J. G. Mangum (SMTO), A. Wootten (NRAO)

The S106 HII region has been the subject of numerous observational investigations. The exciting star for the S106 bipolar HII region, called S106IR, has been studied at radio, infrared, and optical wavelengths. S106IR is buried within an $\sim$30\arcsec\ diameter dense molecular cloud, which produces an optical dark lane through the center of the HII region, and appears to be a pre-main sequence stellar object that may still be accreting matter. Several investigations have attempted to derive the structure of the dense molecular cloud surrounding S106IR. We present high spatial resolution ($\theta_b \sim 4\arcsec$) measurements of the NH$_3$ (1,1) and (2,2) emission toward S106FIR. On the larger scale these new measurements are consistent with early single antenna observations of the NH$_3$ structure toward this region, which show two clouds located on either side of S106IR. With these measurements we have further delineated these dense gas structures. We also derive the kinetic temperature over the small-scale structures in the S106IR/FIR region and find that T$_{ex}$(NH$_3$) $\sim$ 70 K toward S106FIR over a 10\arcsec\ $\times$ 6\arcsec\ region.

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