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L. Magnani, S. Zelenik (University of Georgia), B. Engebreth (University of Colorado)
We present the most sensitive observations to date of the CH 3335 MHz line in the direction of the Galactic Center. A 3 x 3 map of the region was made at 9' resolution (21 pc at the distance of the Galactic Center) showing a velocity extent for the CH emission similar to that seen with the CO(1-0) transition. A narrow CH component at about 0 km/s present in all the CH spectra is most likely produced by molecular clouds in the Inner Galaxy and can be used to calculate the scale height of these objects (90 - 240 pc). This estimate is significantly larger than that for GMCs in the disk and possibly indicates a low-intensity, thick molecular disk component.
The author(s) of this abstract have provided an email address for comments about the abstract: loris@hal.physast.uga.edu
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Bulletin of the American Astronomical Society, 35#5
© 2003. The American Astronomical Soceity.