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dc.contributor.authorSano, H.-
dc.contributor.authorEnokiya, R.-
dc.contributor.authorHayashi, K.-
dc.contributor.authorYamagishi, M.-
dc.contributor.authorSaeki, S.-
dc.contributor.authorOkawa, K.-
dc.contributor.authorTsuge, K.-
dc.contributor.authorTsutsumi, D.-
dc.contributor.authorKohno, M.-
dc.contributor.authorHattori, Y.-
dc.contributor.authorYoshiike, S.-
dc.contributor.authorFujita, S.-
dc.contributor.authorNishimura, A.-
dc.contributor.authorOhama, A.-
dc.contributor.authorTachihara, K.-
dc.contributor.authorTorii, K.-
dc.contributor.authorHasegawa, Y.-
dc.contributor.authorKimura, K.-
dc.contributor.authorOgawa, H.-
dc.contributor.authorWong, G.-
dc.contributor.authoret al.-
dc.identifier.citationPublications of Astronomical Society of Japan, 2018; 70(SP2):1-13-
dc.description.abstractA collision between two molecular clouds is one possible candidate for high-mass star formation. The Hii region RCW 36, located in the Vela molecular ridge, contains a young star cluster (~1Myr 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 9kms -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 5kms -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 0.3pc assuming the collision angle to be 45degrees relative to the line-of-sight. We estimate the collision timescale to be ~105yr. 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.-
dc.description.statementofresponsibilityHidetoshi Sano, Rei Enokiya, Katsuhiro Hayashi, Mitsuyoshi Yamagishi, Shun Saeki, Kazuki Okawa, Kisetsu Tsuge, Daichi Tsutsumi, Mikito Kohno, Yusuke Hattori, Satoshi Yoshiike, Shinji Fujita, Atsushi Nishimura, Akio Ohama, Kengo Tachihara, Kazufumi Torii, Yutaka Hasegawa, Kimihiro Kimura, Hideo Ogawa, Graeme F Wong, Catherine Braiding, Gavin Rowell, Michael G Burton, Yasuo Fukui-
dc.publisherOxford University Press-
dc.rights© The Author(s) 2018. Published by Oxford University Press on behalf of the Astronomical Society of Japan.-
dc.titleRCW 36 in the Vela Molecular Ridge: evidence for high-mass star-cluster formation triggered by cloud-cloud collision-
dc.typeJournal article-
dc.identifier.orcidRowell, G. [0000-0002-9516-1581]-
Appears in Collections:Aurora harvest 8
IPAS publications
Physics publications

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