OBSERVATION OF THE C i 3P2.3P1 LINE TOWARD THE ORION KLEINMANN-LOW REGION

Material type: 文書・図像類

Author: YAMAMOTO, Satoshiほか

Publisher: University of Chicago Press

Publication date: 2001-02

Material Format: Digital

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Note (General)：: The 3P2-3P1fine-structure line of the neutral carbon atom (809 GHz) has been observed toward the Orion Kleinmann-Low (KL) region with the Mount Fuji s...

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Material Type: 文書・図像類
Title: OBSERVATION OF THE C i 3P2.3P1 LINE TOWARD THE ORION KLEINMANN-LOW REGION
Author/Editor: YAMAMOTO, Satoshi
MAEZAWA, Hiroyuki
IKEDA, Masafumi
ITO, Tetsuya
OKA, Tomoharu
SAITO, Gaku
IWATA, Mitsuhiro
KAMEGAI, Kazuhisa
SAKAI, Takeshi
SEKIMOTO, Yutaro
TATEMATSU, Ken-ichi
NOGUCHI, Takashi
SHI, Sheng-Cai
ARIKAWA, Yuji
ASO, Yoshiyuki
MIYAZAWA, Keisuke
SAITO, Shuji
FUJIWARA, Hideo
OHISHI, Masatoshi
OZEKI, Hiroyuki
INATANI, Junji
Author Heading: YAMAMOTO, Satoshi
MAEZAWA, Hiroyuki
IKEDA, Masafumi
ITO, Tetsuya
OKA, Tomoharu
SAITO, Gaku
IWATA, Mitsuhiro
KAMEGAI, Kazuhisa
SAKAI, Takeshi
SEKIMOTO, Yutaro
TATEMATSU, Ken-ichi
NOGUCHI, Takashi
SHI, Sheng-Cai
ARIKAWA, Yuji
ASO, Yoshiyuki
MIYAZAWA, Keisuke
SAITO, Shuji
FUJIWARA, Hideo
OHISHI, Masatoshi
OZEKI, Hiroyuki
INATANI, Junji
Publication, Distribution, etc.: University of Chicago Press
Publication Date: 2001-02
Publication Date (W3CDTF): 2001-02
Periodical title: Astrophysical Journal
No. or year of volume/issue: 547
Volume: 547
Pages: L165-L169
ISSN (Periodical Title): ISSN : 0004-637X
Text Language Code: eng
Subject Heading: ISM
atoms—ISM
clouds—ISM
individual (Orion Kleinmann-Low)
Target Audience: 一般
Note (General): The 3P2-3P1fine-structure line of the neutral carbon atom (809 GHz) has been observed toward the Orion Kleinmann-Low (KL) region with the Mount Fuji submillimeter-wave telescope. The 61×61area centered at Orion KL has been mapped with a grid spacing of 1:5. The intensity distribution of the3P2-3P1 line is found to be similar to that of the 3P1-3P0 line; these lines are rather weak toward Orion KL, while they are both bright at Orion KL's northern and southern positions. The excitation temperature determined from the intensity ratio between the 3P2-3P1 and 3P1-3P0 lines ranges from 40 to 110 K. The excitation temperature is not enhanced toward Orion KL, whereas it tends to be high in the vicinity of θ1 Orionis C. These results indicate that the C I emission arises from a photodissociation surface illuminated by strong UV radiation from θ1 Ori C. The relative reduction in the C I intensities toward Orion KL is found to originate from a relatively low excitation temperature rather than from the depletion of the C I column density. The origin of the low-excitation temperature of C I toward Orion KL is discussed in terms of a radiative transfer effect.
Access Restrictions: 限定公開
Rights (production): 〓 2001 The American Astronomical Society
Related Material (DOI): 10.1086/318901
Data Provider (Database): 国立情報学研究所 : 学術機関リポジトリデータベース（IRDB）（機関リポジトリ）
https://irdb.nii.ac.jp
Original Data Provider (Database): 福井大学 : 福井大学学術機関リポジトリ