We present large-scale (2° × 2°) observations toward the molecular cloud M120.1+3.0, using CO, CO and CO (J = 1 − 0) data from the Purple Mountain Observatory 13.7 m millimeter telescope. The distance of the cloud is measured to be ∼1.1 kpc. Using the CO data, we identify a main filament F1 and two sub-filaments F2 and F3 in the cloud, which together show a “hub-filament” structure. Filaments F1 and F2 are thermally supercritical. Furthermore, F1 displays clear localized systematic motions in the CO position–velocity diagram, which could be explained by accretion along the filament. The mean estimated accretion rate is ∼132 M Myr. Approximately 150 CO clumps are identified in the cloud, of which 39 are gravitationally bound. Most of these virialized clumps are well distributed along the supercritical filaments F1 and F2. Based on the complementary infrared and optical data, we identify ∼186 young stellar objects in the observed area and extract five clusters within the dense ridge of F1. The calculated star formation rate (SFR) surface densities (Σ) in the clusters range from 1.4 to 2.5 M Myr pc, with a mean value of ∼2.0 M Myr pc. We therefore regard them as mini-starburst cluster candidates. The comparison between Σ and column density N along the skeleton of F1 suggests that star formation is closely related to the dense gas in the cloud. Along the main filament F1, five bipolar outflows are also found. All these results indicate intense star-forming activities in the M120.1+3.0 molecular cloud.
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