Giant molecular cloud G18.1-0.3+51 associated with HII regions and supernova remnant in the 3-kpc expanding ring

Analyzing the high-resolution CO-line survey of the Galactic plane with the Nobeyama 45-m telescope (FUGIN), we show that the star-forming complex G18.15-0.30+51 (G18) at radial velocity of 51 \kms is {a tight triple association of a giant molecular cloud (GMC), HII regions, and a supernova remnant (SNR).} The kinematical distance of G18 is determined to be $d=3.9\pm 0.2$ kpc for near solution for circular rotation, $12\pm 0.2$ kpc for far solution, or $d=6.1\pm 0.1$, if it is in the 3-kpc expanding ring. The HI-line absorption of radio continuum from the HII regions constrains the distance to $5.6\lesssim d_{\mathrm{S}\mathrm{N}\mathrm{R}}\le 7.6$ kpc. The $\mathrm{\Sigma }-D$ (radio brightness-diameter) relation yields the distance to the SNR of $d_{\mathrm{S}\mathrm{N}\mathrm{R}}=10.1_{-4.7}^{+11.5}$ kpc, allowing for a minimum distance of 5.4 kpc. From these we uniquely determined the distance of G18 to be $6.07\pm 0.13$ kpc in the 3-kpc expanding ring with the SNR being physically associated. The molecular mass of the GMC is estimated to be $M_{\mathrm{m}\mathrm{o}\mathrm{l}}\sim 3\times {10}^5{M}_{\odot }$. The ratio of Virial to luminous molecular masses is greater than unity in the central region and decreases outward to $\lesssim 0.2$ at the cloud edge, indicating that the central region is dynamic, while the entire cloud is stable. We discuss the origin of the G18 triple system and propose a sustainable GMC model with continuous star formation.