The Maddalena Thaddeus (MT) cloud is a relatively nearby (2.2 kpc), outer galaxy molecular cloud which exhibits no evidence for recent OB star formation. MT proposed that it is a rare example of a young GMC before the onset of massive star formation. Using the SEST telescope, we mapped the central region of peak (12) CO temperatures. We detected emission from 3 clumps which were previously detected in (13) CO mapping by Williams et al. (1994 ApJ 428, 693). The CS emission of the clumps is less extended and shows much more substructure than the (13) CO emission. We compare the relative masses, densities derived from the (13) CO and CS data and present a linewidth vs. source size relationship. Near--infrared images taken from Calar Alto of one of the clumps show no evidence for stellar density enhancements or nebulosity - features commonly found towards active star forming regions. Finally, we present a pictorial comparison of K--band, IRAS, and CS maps from a number of regions to compare the MT cloud to other "well studied" molecular clouds.
American Astronomical Society Meeting Abstracts #188
- Pub Date:
- May 1996