Submillimeter-wave C I spectral lines from the NGC 1333 region

Tomoharu Oka, Mitsuhiro Iwata, Hiroyuki Maezawa, Masafumi Ikeda, Tetsuya Ito, Kazuhisa Kamegai, Takeshi Sakai, Satoshi Yamamoto

研究成果: Article

9 引用 (Scopus)

抄録

We present large (30′ × 40′) maps in the C0 3P0-3P0 ([C I]; 492 GHz) and CO J = 3-2 (346 GHz) spectral lines of the NGC 1333 star-forming complex. We also report detections of the C0 3P2- 3P1 (809 GHz) spectral line from 3 × 3 positions centered on HH 12. The overall extents of [C I] and CO J = 3-2 emission are similar to those of 13CO and C18O J = 1-0 emission. The CO J = 3-2 intensity peak is adjacent to the illuminating star SVS 3, while the [C I] intensity peaks at 5′ southwest of the reflection nebula, filling a hollow surrounded by a C-shaped dense molecular shell. We suggest that the observed [C I] distributions might be the result of nonequilibrium chemistry on the basis of the time-dependent chemical simulation. A huge expanding H I shell associated with the NGC 1333 cloud lends further support to this notion.

元の言語English
ページ(範囲)803-815
ページ数13
ジャーナルAstrophysical Journal
602
発行部数2 I
DOI
出版物ステータスPublished - 2004 2 20
外部発表Yes

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submillimeter waves
line spectra
shell
reflection nebulae
stars
illuminating
hollow
chemistry
simulation
detection
distribution
chemical

ASJC Scopus subject areas

  • Space and Planetary Science

これを引用

Oka, T., Iwata, M., Maezawa, H., Ikeda, M., Ito, T., Kamegai, K., ... Yamamoto, S. (2004). Submillimeter-wave C I spectral lines from the NGC 1333 region. Astrophysical Journal, 602(2 I), 803-815. https://doi.org/10.1086/381082

Submillimeter-wave C I spectral lines from the NGC 1333 region. / Oka, Tomoharu; Iwata, Mitsuhiro; Maezawa, Hiroyuki; Ikeda, Masafumi; Ito, Tetsuya; Kamegai, Kazuhisa; Sakai, Takeshi; Yamamoto, Satoshi.

:: Astrophysical Journal, 巻 602, 番号 2 I, 20.02.2004, p. 803-815.

研究成果: Article

Oka, T, Iwata, M, Maezawa, H, Ikeda, M, Ito, T, Kamegai, K, Sakai, T & Yamamoto, S 2004, 'Submillimeter-wave C I spectral lines from the NGC 1333 region', Astrophysical Journal, 巻. 602, 番号 2 I, pp. 803-815. https://doi.org/10.1086/381082
Oka T, Iwata M, Maezawa H, Ikeda M, Ito T, Kamegai K その他. Submillimeter-wave C I spectral lines from the NGC 1333 region. Astrophysical Journal. 2004 2 20;602(2 I):803-815. https://doi.org/10.1086/381082
Oka, Tomoharu ; Iwata, Mitsuhiro ; Maezawa, Hiroyuki ; Ikeda, Masafumi ; Ito, Tetsuya ; Kamegai, Kazuhisa ; Sakai, Takeshi ; Yamamoto, Satoshi. / Submillimeter-wave C I spectral lines from the NGC 1333 region. :: Astrophysical Journal. 2004 ; 巻 602, 番号 2 I. pp. 803-815.
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AU - Oka, Tomoharu

AU - Iwata, Mitsuhiro

AU - Maezawa, Hiroyuki

AU - Ikeda, Masafumi

AU - Ito, Tetsuya

AU - Kamegai, Kazuhisa

AU - Sakai, Takeshi

AU - Yamamoto, Satoshi

PY - 2004/2/20

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N2 - We present large (30′ × 40′) maps in the C0 3P0-3P0 ([C I]; 492 GHz) and CO J = 3-2 (346 GHz) spectral lines of the NGC 1333 star-forming complex. We also report detections of the C0 3P2- 3P1 (809 GHz) spectral line from 3 × 3 positions centered on HH 12. The overall extents of [C I] and CO J = 3-2 emission are similar to those of 13CO and C18O J = 1-0 emission. The CO J = 3-2 intensity peak is adjacent to the illuminating star SVS 3, while the [C I] intensity peaks at 5′ southwest of the reflection nebula, filling a hollow surrounded by a C-shaped dense molecular shell. We suggest that the observed [C I] distributions might be the result of nonequilibrium chemistry on the basis of the time-dependent chemical simulation. A huge expanding H I shell associated with the NGC 1333 cloud lends further support to this notion.

AB - We present large (30′ × 40′) maps in the C0 3P0-3P0 ([C I]; 492 GHz) and CO J = 3-2 (346 GHz) spectral lines of the NGC 1333 star-forming complex. We also report detections of the C0 3P2- 3P1 (809 GHz) spectral line from 3 × 3 positions centered on HH 12. The overall extents of [C I] and CO J = 3-2 emission are similar to those of 13CO and C18O J = 1-0 emission. The CO J = 3-2 intensity peak is adjacent to the illuminating star SVS 3, while the [C I] intensity peaks at 5′ southwest of the reflection nebula, filling a hollow surrounded by a C-shaped dense molecular shell. We suggest that the observed [C I] distributions might be the result of nonequilibrium chemistry on the basis of the time-dependent chemical simulation. A huge expanding H I shell associated with the NGC 1333 cloud lends further support to this notion.

KW - Astrochemistry

KW - ISM: atoms

KW - ISM: individual (NGC 1333)

KW - ISM: molecules

KW - Reflection nebulae

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