Observational approach to molecular cloud evolution

Tomoharu Oka; Satoshi Yamamoto

doi:10.1016/j.asr.2003.04.038

Observational approach to molecular cloud evolution

Tomoharu Oka, Satoshi Yamamoto

Research output: Contribution to journal › Article › peer-review

Abstract

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.

Original language	English
Pages (from-to)	519-523
Number of pages	5
Journal	Advances in Space Research
Volume	34
Issue number	3
DOIs	https://doi.org/10.1016/j.asr.2003.04.038
Publication status	Published - 2004 Jan 1
Externally published	Yes

Keywords

Molecular cloud evolution
Submillimeter CI lines
Submillimeter wave telescope

ASJC Scopus subject areas

Aerospace Engineering
Astronomy and Astrophysics
Geophysics
Atmospheric Science
Space and Planetary Science
Earth and Planetary Sciences(all)

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10.1016/j.asr.2003.04.038

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@article{57ef96b12a934899bc3c56809aa43614,

title = "Observational approach to molecular cloud evolution",

abstract = " 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.",

keywords = "Molecular cloud evolution, Submillimeter CI lines, Submillimeter wave telescope",

author = "Tomoharu Oka and Satoshi Yamamoto",

year = "2004",

month = jan,

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doi = "10.1016/j.asr.2003.04.038",

language = "English",

volume = "34",

pages = "519--523",

journal = "Advances in Space Research",

issn = "0273-1177",

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number = "3",

}

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T1 - Observational approach to molecular cloud evolution

AU - Oka, Tomoharu

AU - Yamamoto, Satoshi

PY - 2004/1/1

Y1 - 2004/1/1

N2 - 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.

AB - 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.

KW - Molecular cloud evolution

KW - Submillimeter CI lines

KW - Submillimeter wave telescope

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SP - 519

EP - 523

JO - Advances in Space Research

JF - Advances in Space Research

IS - 3

ER -

Observational approach to molecular cloud evolution

Abstract

Keywords

ASJC Scopus subject areas

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