2017
DOI: 10.3847/1538-4357/835/1/108
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Kinematic Structure of Molecular Gas Around High-Mass Yso, Papillon Nebula, in N159 East in the Large Magellanic Cloud: A New Perspective With Alma

Abstract: -We present the ALMA Band 3 and Band 6 results of 12 CO(2-1), 13 CO(2-1), H30α recombination line, free-free emission around 98 GHz, and the dust thermal emission around 230 GHz toward the N159 East Giant Molecular Cloud (N159E) in the Large Magellanic Cloud (LMC). LMC is the nearest active highmass star forming face-on galaxy at a distance 50 kpc and is the best target for studing high-mass star formation. ALMA observations show that N159E is the complex of filamentary clouds with the width and length of ∼1 p… Show more

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Cited by 49 publications
(34 citation statements)
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“…N159, a pair of massive star forming clouds just to the south of 30 Doradus, has been observed with ALMA at similar angular resolution to the data presented here (Saigo et al (2017): resolution of 1.21 ×0.84 , Tokuda et al (2019): resolution of 0.29 ×0.25 , Fukui et al (2015):resolution of 1.3 ×0.8 , Fukui et al (2019): resolution of 0.28 ×0.25 ) dendrogram structures in N159 have a size-linewidth slope of 0.7±0.1, consistent with 30Dor-10, but the linewidth at a given scale is 0.33±0.05 dex lower. The molecular mass of N159 is significantly higher than 30Dor-10, so the enhanced linewidths in 30Dor cannot be explained by global equilibrium between gravitational and kinetic energy.…”
Section: Structure Analysis Result: Size-linewidth-flux Relationssupporting
confidence: 72%
“…N159, a pair of massive star forming clouds just to the south of 30 Doradus, has been observed with ALMA at similar angular resolution to the data presented here (Saigo et al (2017): resolution of 1.21 ×0.84 , Tokuda et al (2019): resolution of 0.29 ×0.25 , Fukui et al (2015):resolution of 1.3 ×0.8 , Fukui et al (2019): resolution of 0.28 ×0.25 ) dendrogram structures in N159 have a size-linewidth slope of 0.7±0.1, consistent with 30Dor-10, but the linewidth at a given scale is 0.33±0.05 dex lower. The molecular mass of N159 is significantly higher than 30Dor-10, so the enhanced linewidths in 30Dor cannot be explained by global equilibrium between gravitational and kinetic energy.…”
Section: Structure Analysis Result: Size-linewidth-flux Relationssupporting
confidence: 72%
“…Interferometry observations in millimeter have probed distributions of dense molecular gas at a clump scale (a few pc; e.g., Wong et al 2006;Seale et al 2012;Anderson et al 2014). The Atacama Large Millimeter/submillimeter Array (ALMA) has provided us with an unprecedented sensitivity and spatial resolution to study physical properties of dense molecular gas around young stellar objects (YSOs) at a subparsec scale (e.g., Indebetouw et al 2013;Fukui et al 2015;Saigo et al 2017;Nayak et al 2018). For solid state molecules, compositions of ice mantles have been probed by infrared spectroscopic observations towards embedded YSOs (e.g., van Loon et al 2005;Shimonishi et al 2008Shimonishi et al , 2010Shimonishi et al , 2016aOliveira et al 2009Oliveira et al , 2011Seale et al 2011) Chemistry of hot cores at low metallicity is now emerging with discoveries of extragalactic hot cores in the LMC with ALMA (Shimonishi et al 2016b;Sewiło et al 2018).…”
Section: Introductionmentioning
confidence: 99%
“…Several observational works on the CCC process are also available in the literature (e.g., Loren 1976;Miyawaki et al 1986Miyawaki et al , 2009Hasegawa et al 1994;Sato et al 2000;Okumura et al 2001;Furukawa et al 2009;Ohama et al 2010Ohama et al , 2017Ohama et al , 2018aShimoikura & Dobashi 2011;Torii et al 2011Torii et al , 2015Torii et al , 2017aTorii et al ,b, 2018aNakamura et al 2012Nakamura et al , 2014Shimoikura et al 2013;Dobashi et al 2014;Fukui et al 2014Fukui et al , 2015Fukui et al , 2016Fukui et al , 2017Fukui et al , 2018aHaworth et al 2015a,b;Tsuboi et al 2015;Baug et al 2016;Dewangan 2017;Dewangan & Ojha 2017;Dewangan et al 2017bDewangan et al , 2018aFujita et al 2017Fujita et al , 2018Gong et al 2017;Liu et al 2017;Nishimura et al 2017Nishimura et al , 2018Saigo et al 2017;Sano et al 2017Sano et al , 2018Tsutsumi et al 2017;Enokiya et al 2018;…”
Section: Discussionmentioning
confidence: 99%