Investigating high-mass star formation through chemical compositions of infrared dark clouds

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We have investigated the high-mass star formation on the basis of the chemical compositions of infrared dark clouds (IRDCs), which are thought to be in early evolutionary stages of high-mass star formation. For this purpose, we have carried out a survey of molecular lines toward massive clumps associated with infrared dark clouds (IRDCs) by using the Nobeyama Radio Observatory 45 m telescope and the ASTE 10 m telescope. We have found that the SiO and CH_3OH abundances relative to H^<13>CO^+ are enhanced in several IRDC clumps. Since SiO and CH_3OH are known as "shock tracers", this results means that an interaction between outflows and dense gas frequently occurs in early evolutionary stages of high-mass star formation. The data obtained are useful for future high-resolution observations.