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AUSTRALIA TELESCOPE OBSERVATIONS
OF THE CTB 33 COMPLEX

A. P. SARMA
Physics & Astronomy Department, University of Kentucky, Lexington, KY 40506
sarma@pa.uky.edu

W. M. GOSS
National Radio Astronomy Observatory, P. O. Box 0, Socorro, NM 87801
mgoss@nrao.edu

A. J. GREEN
School of Physics, University of Sydney, NSW 2006, Australia
agreen@Physics.usyd.edu.au

D. A. FRAIL
National Radio Astronomy Observatory, P. O. Box 0, Socorro, NM 87801
dfrail@nrao.edu

(accepted Feb 21 1997, scheduled for publication, July 1997, ApJ, 483)


We present high resolution radio continuum, \ion{H}{1} absorption and H90$\alpha$ recombination line observations of the CTB 33 complex and nearby sources (l=337$\arcdeg$, b=0$\arcdeg$) taken with the Australia Telescope Compact Array. We estimate distances to several discrete sources based on \ion{H}{1} absorption. Radio recombination lines are detected for two sources in the field. The compact source G337.0$-$0.1 in the CTB 33 complex, whose nature was previously in doubt, is identified as a supernova remnant with a diameter of $\sim$ 5 pc. This classification is based on several contributing features, a non-thermal spectral index ($-$0.6), a shell structure and the absence of detectable recombination lines. In addition a 1720 MHz OH maser is probably associated with G337.0$-$0.1. We conclude that the CTB 33 region is a SNR-\ion{H}{2} complex at a distance of $\sim$ 11 kpc.


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