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We present IRAM 30m observations of molecular lines of CO and itsisotopologues from the massive spiral galaxy NGC 5908 selected from theCGM-MASS sample. $^{12}$CO $J=1-0$, $^{12}$CO $J=2-1$, and $^{13}$CO $J=1-0$lines have been detected in most of the positions along the galactic disk. Thetotal molecular gas mass of NGC 5908 is $\sim7\times10^9\rm~M_\odot$ and thetotal cool gas mass adding atomic hydrogen is$\sim1.3\times10^{10}\rm~M_\odot$, comparable to the upper limit of the mass ofthe X-ray emitting hot gas in the halo. Modeling the rotation curvesconstructed with all three CO lines indicates that NGC 5908 has a dark matterhalo mass of $M_{\rm vir}\sim10^{13}\rm~M_{\rm \odot}$, putting it among themost massive isolated spiral galaxies. The $^{12}$CO/$^{13}$CO $J=1-0$,$^{12}$CO $J=2-1$/$J=1-0$ line ratios and the estimated molecular gastemperature all indicate normal but non-negligible star formation in thisfairly gas-rich massive isolated spiral galaxy, consistent with the measuredstar formation intensity and surface densities. The galaxy is probably at anearly evolutionary stage after a fast growth stage with mergers and/orstarbursts, with plenty of leftover cool gas, relatively high SFR, low hot CGMcooling rate, and low X-ray emissivity.

Molecular Gas of the Most Massive Spiral Galaxies I: a Case Study of NGC 5908