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We performed new large-scale $^{12}$CO, $^{13}$CO, and C$^{18}$O $J=$1--0observations of the W43 giant molecular cloud complex in the tangentialdirection of the Scutum arm ($l\sim {30^\circ}$) as a part of the FUGINproject. The low-density gas traced by $^{12}$CO is distributed over 150 pc$\times$ 100 pc ($l \times b$), and has a large velocity dispersion (20-30 kms$^{-1}$). However, the dense gas traced by C$^{18}$O is localized in the W43Main, G30.5, and W43 South (G29.96-0.02) high-mass star-forming regions in theW43 GMC complex, which have clumpy structures. We found at least two cloudswith a velocity difference of $\sim$ 10-20 km s$^{-1}$, both of which arelikely to be physically associated with these high-mass star-forming regionsbased on the results of high $^{13}$CO $J=$ 3-2 to $J =$ 1-0 intensity ratioand morphological correspondence with the infrared dust emission. The velocityseparation of these clouds in W43 Main, G30.5, and W43 South is too large foreach cloud to be gravitationally bound. We also revealed that the dense gas inthe W43 GMC has a high local column density, while "the current SFE" of entirethe GMC is low ($\sim 4\%$) compared with the W51 and M17 GMC. We argue thatthe supersonic cloud-cloud collision hypothesis can explain the origin of thelocal mini-starbursts and dense gas formation in the W43 GMC complex.

publications of the astronomical society of japan

FOREST Unbiased Galactic plane Imaging survey with the Nobeyama 45 m  telescope (FUGIN). VI. Dense gas and mini-starbursts in the W43 giant  molecular cloud complex