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Future Prospects

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CHAPTER 4. SUMMARY 103 higher (n(H2) > 2000 cm3) in the cloud edge facing to the HII region. These facts suggest the strong stellar wind and UV radiation from the surrounding massive stars are compressing the molecular gas.

6. The YSOs surface number density and the SFE are well positively correlated with the gas density. This fact indicates that the star formation is more effec-tively taking place in the denser environment.

104 4.2. FUTURE PROSPECTS provide us wealth of information of the density structure in the inner dense region.

For example, the combination of the C32S(J=2–1), C34S(J=1–0), and C34S(J=2–1) lines is possibly worthy for the analyses. These observations would provide us the significant perceptions for the whole picture of the evolution of molecular clouds.

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