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Filamentary flows toward the centre of molecular clouds have been recognizedas a crucial process in the formation and evolution of stellar clusters. Inthis paper, we present a comprehensive observational study that investigatesthe gas properties and kinematics of the Giant Molecular Cloud G148.24+00.41using the observations of CO (1-0) isotopologues. We find that the cloud ismassive (10$^5$ M$_\odot$) and is one of the most massive clouds of the outerGalaxy. We identified six likely velocity coherent filaments in the cloudhaving length, width, and mass in the range of 14$-$38 pc, 2.5$-$4.2 pc, and(1.3$-$6.9) $\times$ 10$^3$ M$_\odot$, respectively. We find that the filamentsare converging towards the central area of the cloud, and the longitudinalaccretion flows along the filaments are in the range of $\sim$ 26$-$264M$_\odot$ Myr$^{-1}$. The cloud has fragmented into 7 clumps having mass in therange of $\sim$ 260$-$2100 M$_\odot$ and average size around $\sim$ 1.4 pc, outof which the most massive clump is located at the hub of the filamentarystructures, near the geometric centre of the cloud. Three filaments are foundto be directly connected to the massive clump and transferring matter at a rateof $\sim$ 675 M$_\odot$ Myr$^{-1}$. The clump hosts a near-infrared cluster.Our results show that large-scale filamentary accretion flows towards thecentral region of the collapsing cloud is an important mechanism for supplyingthe matter necessary to form the central high-mass clump and subsequent stellarcluster.

The Giant Molecular Cloud G148.24+00.41: Gas Properties, Kinematics, and Cluster Formation at the Nexus of Filamentary Flows