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RCW 36 in the Vela Molecular Ridge: Evidence for high-mass star-cluster formation triggered by cloud–cloud collision
http://hdl.handle.net/2237/00028577
http://hdl.handle.net/2237/0002857758930118-f50d-40bd-9625-ea9bee6020e6
名前 / ファイル | ライセンス | アクション |
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Item type | 学術雑誌論文 / Journal Article(1) | |||||
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公開日 | 2018-09-13 | |||||
タイトル | ||||||
タイトル | RCW 36 in the Vela Molecular Ridge: Evidence for high-mass star-cluster formation triggered by cloud–cloud collision | |||||
言語 | en | |||||
著者 |
Sano, Hidetoshi
× Sano, Hidetoshi× Enokiya, Rei× Hayashi, Katsuhiro× Yamagishi, Mitsuyoshi× Saeki, Shun× Okawa, Kazuki× Tsuge, Kisetsu× Tsutsumi, Daichi× Kohno, Mikito× Hattori, Yusuke× Yoshiike, Satoshi× Fujita, Shinji× Nishimura, Atsushi× Ohama, Akio× Tachihara, Kengo× Torii, Kazufumi× Hasegawa, Yutaka× Kimura, Kimihiro× Ogawa, Hideo× Wong, Graeme F× Braiding, Catherine× Rowell, Gavin× Burton, Michael G× Fukui, Yasuo |
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アクセス権 | ||||||
アクセス権 | open access | |||||
アクセス権URI | http://purl.org/coar/access_right/c_abf2 | |||||
権利 | ||||||
言語 | en | |||||
権利情報 | This is a pre-copyedited, author-produced version of an article accepted for publication in [Publications of the Astronomical Society of Japan] following peer review. The version of record [Publications of the Astronomical Society of Japan. v.70, n.SP2, 2018, p.S43] is available online at: http://doi.org/10.1093/pasj/psy006. | |||||
抄録 | ||||||
内容記述タイプ | Abstract | |||||
内容記述 | A collision between two molecular clouds is one possible candidate for high-mass star formation. The H ii region RCW 36, located in the Vela molecular ridge, contains a young star cluster (∼ 1 Myr old) and two O-type stars. We present new CO observations of RCW 36 made with NANTEN2, Mopra, and ASTE using 12CO(J = 1–0, 2–1, 3–2) and 13CO(J = 2–1) emission lines. We have discovered two molecular clouds lying at the velocities VLSR ∼ 5.5 and 9 km s^−1. Both clouds are likely to be physically associated with the star cluster, as verified by the good spatial correspondence among the two clouds, infrared filaments, and the star cluster. We also found a high intensity ratio of ∼ 0.6–1.2 for CO J = 3–2/1–0 toward both clouds, indicating that the gas temperature has been increased due to heating by the O-type stars. We propose that the O-type stars in RCW 36 were formed by a collision between the two clouds, with a relative velocity separation of 5 km s^−1. The complementary spatial distributions and the velocity separation of the two clouds are in good agreement with observational signatures expected for O-type star formation triggered by a cloud–cloud collision. We also found a displacement between the complementary spatial distributions of the two clouds, which we estimate to be 0.3 pc assuming the collision angle to be 45° relative to the line-of-sight. We estimate the collision timescale to be ∼ 10^5 yr. It is probable that the cluster age found by Ellerbroek et al. (2013b, A&A, 558, A102) is dominated by the low-mass members which were not formed under the triggering by cloud–cloud collision, and that the O-type stars in the center of the cluster are explained by the collisional triggering independently from the low-mass star formation. | |||||
言語 | en | |||||
内容記述 | ||||||
内容記述タイプ | Other | |||||
内容記述 | ファイル公開:2019-05-01 | |||||
言語 | ja | |||||
出版者 | ||||||
出版者 | Oxford University Press | |||||
言語 | en | |||||
言語 | ||||||
言語 | eng | |||||
資源タイプ | ||||||
資源タイプ識別子 | http://purl.org/coar/resource_type/c_6501 | |||||
資源タイプ | journal article | |||||
出版タイプ | ||||||
出版タイプ | AM | |||||
出版タイプResource | http://purl.org/coar/version/c_ab4af688f83e57aa | |||||
DOI | ||||||
関連タイプ | isVersionOf | |||||
識別子タイプ | DOI | |||||
関連識別子 | https://doi.org/10.1093/pasj/psy006 | |||||
ISSN(print) | ||||||
収録物識別子タイプ | PISSN | |||||
収録物識別子 | 0004-6264 | |||||
ISSN(Online) | ||||||
収録物識別子タイプ | EISSN | |||||
収録物識別子 | 2053-051X | |||||
書誌情報 |
en : Publications of the Astronomical Society of Japan 巻 70, 号 SP2, p. S43, 発行日 2018-05 |
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著者版フラグ | ||||||
値 | author |