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We present the results of $^{12}$CO($J$=1-0) mosaicing observations of the cDgalaxy NGC 1316 at kpc-resolution performed with the Morita Array of theAtacama Large Millimeter/submillimeter Array (ALMA). We reveal the detaileddistribution of the molecular gas in the central region for the first time: ashell structure in the northwest, a barely resolved blob in the southeast ofthe center and some clumps between them. The total molecular gas mass obtainedwith a standard Milky-Way CO-to-H$_2$ conversion factor is $(5.62 \pm0.53)\times10^8$ M$_\odot$, which is consistent with previous studies. Thedisturbed velocity field of the molecular gas suggests that the molecular gasis injected very recently ($<1$ Gyr) if it has an external origin and is in theprocess of settling into a rotating disk. Assuming that a low-mass gas-richgalaxy has accreted, the gas-to-dust ratio and H$_2$-to-HI ratio are unusuallylow ($\sim 28$) and high ($\sim 5.6$), respectively. To explain these ratios,additional processes should be taken into accounts such as an effective dustformation and conversion from atomic to molecular gas during the interaction.We also discuss the interaction between the nuclear jet and the molecular gas.

Complex distribution and velocity field of molecular gas in NGC 1316 as revealed by Morita Array of ALMA