Abstract
CS observations with resolutions of 1-2 arcmin of low-mass molecular cloud cores are presented. The results are compared with those of previous NH3 observations. In comparison with the NH3 emission, the CS emission comes from a larger region and has a larger velocity dispersion. The mass and density derived from the CS data are also larger by 1-2 orders of magnitude than those derived from the NH3 data. On the other hand, both CS and NH3 emission lines are at the same velocity, and statistically both CS and NH3 lines have wider line widths toward cores with associated IRAS sources. This seems to indicate that CS and NH3 are probing regions closely related to star formation in the dense cores in spite of some differences in their properties. 31 refs.
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