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Observations of the molecular gas in galaxies are vital to understanding theevolution and star-forming histories of galaxies. However, galaxies withmolecular gas maps of their whole discs having sufficient resolution todistinguish galactic structures are severely lacking. Millimeter wavelengthstudies at a high angular resolution across multiple lines and transitions areparticularly needed, severely limiting our ability to infer the universalproperties of molecular gas in galaxies. Hence, we conducted a legacy projectwith the 45 m telescope of the Nobeyama Radio Observatory, called the COMulti-line Imaging of Nearby Galaxies (COMING), which simultaneously observed147 galaxies with high far-infrared flux in $^{12}$CO, $^{13}$CO, and C$^{18}$O$J=1-0$ lines. The total molecular gas mass was derived using the standardCO-to-H$_2$ conversion factor and found to be positively correlated with thetotal stellar mass derived from the WISE $3.4 \mu$m band data. The fraction ofthe total molecular gas mass to the total stellar mass in galaxies does notdepend on their Hubble types nor the existence of a galactic bar, although whengalaxies in individual morphological types are investigated separately, thefraction seems to decrease with the total stellar mass in early-type galaxiesand vice versa in late-type galaxies. No differences in the distribution of thetotal molecular gas mass, stellar mass, and the total molecular gas to stellarmass ratio was observed between barred and non-barred galaxies, which is likelythe result of our sample selection criteria, in that we prioritized observingFIR bright (and thus molecular gas-rich) galaxies.

CO Multi-line Imaging of Nearby Galaxies (COMING) IV. Overview of the Project