High Excitation Molecular Gas in the Galactic Center Loops; 12CO(J =2-1 and J =3-2) Observations

@article{Kudo2010HighEM,
  title={High Excitation Molecular Gas in the Galactic Center Loops; 12CO(J =2-1 and J =3-2) Observations},
  author={Natsuko Kudo and Kazufumi Torii and Mami Machida and Timothy A. Davis and Kazuki Tsutsumi and M. Fujishita and Nayuta Moribe and Hiroaki Yamamoto and Takeshi Okuda and Akiko Kawamura and Norikazu Mizuno and Toshikazu Onishi and Hiroyuki Maezawa and Akira Mizuno and Kunihiko Tanaka and Nobuyuki Yamaguchi and Hajime Ezawa and Kunio Takahashi and Satoshi Nozawa and Ryoji Matsumoto and Yasuo Fukui},
  journal={arXiv: Astrophysics of Galaxies},
  year={2010}
}
We have carried out 12CO(J =2-1) and 12CO(J =3-2) observations at spatial resolutions of 1.0-3.8 pc toward the entirety of loops 1 and 2 and part of loop 3 in the Galactic center with NANTEN2 and ASTE. These new results revealed detailed distributions of the molecular gas and the line intensity ratio of the two transitions, R3-2/2-1. In the three loops, R3-2/2-1 is in a range from 0.1 to 2.5 with a peak at ~ 0.7 while that in the disk molecular gas is in a range from 0.1 to 1.2 with a peak at 0… 
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Recent large-area, deep CO surveys in the Galactic disk have revealed the formation of ~50 high-mass stars or clusters triggered by cloud–cloud collisions (CCCs). Although the Galactic Center
DETAILED MOLECULAR OBSERVATIONS TOWARD THE DOUBLE HELIX NEBULA
The Double Helix Nebula (DHN), located 100 pc above Sgr A* in the Galactic center (GC), is a unique structure whose morphology suggests it is a magnetic feature. Recent molecular observations toward
Using CO line ratios to trace compressed areas in bubble N131
Aims. N131 is a typical infrared dust bubble showing an expanding ring-like shell. We study the CO line ratios that can be used to trace the interaction in the expanding bubble. Methods. We carried
Formation of Galactic Prominence in the Galactic Central Region
We carried out 2.5-dimensional resistive MHD simulations to study the formation mechanism of molecular loops observed by Fukui et al. in the Galactic central region. Since it is hard to form
Hidden Star Formation in High-Velocity Gas Clouds in Clump 2 near the Edge of the CMZ
  • V. Tolls, H. Smith
  • Physics, Environmental Science
    Proceedings of the International Astronomical Union
  • 2016
Abstract We present a snapshot of our ongoing investigation of molecular clouds in Clump 2 located in the Galactic Bar region at a projected distance of ~400pc from the Galactic Center. We show that
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