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We present the results of C18O(J=1-0) mapping observations of a 20'x18' areain the Lynds 1204 molecular cloud associated with the Sharpless 2-140 (S140) HII region. The C18O cube (alpha-delta-vLSR) data shows that there are threeclumps with sizes of \sim 1 pc in the region. Two of them have peculiar redshifted velocity components at their edges, which can be interpreted as theresults of the interaction between the cloud and the Cepheus Bubble. From theC18O cube data, the clumpfind identified 123 C18O cores, which have meanradius, velocity width in FWHM, and LTE mass of 0.36\pm0.07 pc, 0.37\pm0.09 kms-1, and 41\pm29 Msun, respectively. All the cores in S140 are most likely tobe gravitationally bound by considering the uncertainty in the C18O abundance.We derived a C18O core mass function (CMF), which shows a power-law-likebehavior above a turnover at 30 Msun. The best-fit power-law index of-2.1\pm0.2 is quite consistent with those of the IMF and the C18O CMF in theOMC-1 region by Ikeda & Kitamura (2009). Kramer et al. (1998) estimated thepower-law index of -1.65 in S140 from the C18O(J=2-1) data, which isinconsistent with this study. However, the C18O(J=2-1) data are spatiallylimited to the central part of the cloud and are likely to be biased towardhigh-mass cores, leading to the flatter CMF. Consequently, this study and ourprevious one strongly support that the power-law form of the IMF has beenalready determined at the density of \sim 10^{3-4} cm^{-3}, traced by theC18O(J=1-0) line.

Similarity between the C18O (J=1-0) core mass function and the IMF in the S 140 region