Observational approach to molecular cloud evolution

Tomoharu Oka, Satoshi Yamamoto

研究成果: Article査読


We have constructed a 1.2-m submillimeter-wave telescope at the summit of Mt. Fuji to observe molecular clouds in two CI lines, 3 P 1 - 3 P 0 (492 GHz) and 3 P 2 - 3 P 1 (809 GHz). The telescope has been operated successfully for four observing seasons since the installation on 1998. We have obtained large-scale CI 492 GHz distributions of many molecular clouds, including Orion MC, Taurus MC, DR15, ρ-Oph, DR21, NGC2264, M17, W3, W44, W51, Rosette MC, covering more than 40 square degrees of the sky. The distribution of CI 492 GHz emission is found to be different from those of the 13 CO or C 18 O emission in some clouds. We found C 0 -rich areas (C/CO ∼ 1) in several dark clouds without strong UV sources. Away from UV sources the spatial sequence appears to be C + /CO/C 0 . This seems to be inconsistent with the standard photodissociation region picture. These results are discussed in relation to formation processes of molecular clouds and dense cloud cores.

ジャーナルAdvances in Space Research
出版ステータスPublished - 2004 1月 1

ASJC Scopus subject areas

  • 航空宇宙工学
  • 天文学と天体物理学
  • 地球物理学
  • 大気科学
  • 宇宙惑星科学
  • 地球惑星科学(全般)


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