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We report the results of high-resolution (~0.2 pc) CO(1-0) and CS(2-1)observations of the central regions of three star-forming molecular clouds inthe far-outer Galaxy (~16 kpc from the Galactic Center): WB89 85 (Sh 2-127),WB89 380, and WB89 437. We used the BIMA array in combination with IRAM 30-mand NRAO 12-m observations. The GMC's in which the regions are embedded werestudied by means of KOSMA 3-m CO(2-1) observations. The properties the CO andCS clumps are analyzed and compared with newly derived results of previouslypublished single-dish measurements of local clouds (OrionB South and Rosette).We find that the slopes of the clump mass distributions (-1.28 and -1.49, forWB89 85 and WB89 380, respectively) are somewhat less steep than found for mostlocal clouds, but similar to those of clouds which have been analyzed with thesame clumpfind program. We investigate the clump stability by using the virialtheorem, including all possible contributions (gravity, turbulence, magneticfields, and pressure due to the interclump gas). It appears that underreasonable assumptions a combination of these forces would render most clumpsstable. Comparing only gravity and turbulence, we find that in the far-outerGalaxy clouds, these forces are in equilibium (virial parameter alpha~1) forclumps down to the lowest masses found (a few Msol). For clumps in the localclouds alpha~1 only for clumps with masses larger than a few tens of Msol. Thusit appears that in these outer Galaxy clumps gravity is the dominant force downto a much lower mass than in local clouds, implying that gravitational collapseand star formation may occur more readily even in the smallest clumps. Althoughthere are some caveats, due to the inhomogeneity of the data used, this mightexplain the apparently steeper IMF found in the outer Galaxy.Comment: 29 pages, including 9 tables, 21 figures. Accepted for Astron.  Astrop

Clumpy outer Galaxy molecular clouds and the steepening of the IMF