2022PASJ...74...24K

We have performed new large-scale ¹²CO, ¹³CO, and C¹⁸O J = 1-0 observations toward the Vulpecula OB association (l ∼ 60°) as part of the Nobeyama 45 m Local Spur CO survey project. Molecular clouds are distributed over ∼100 pc, with local peaks at the Sh 2-86, Sh 2-87, and Sh 2-88 high-mass star-forming regions in the Vulpecula complex. The molecular gas is associated with the Local Spur, which corresponds to the nearest inter-arm region located between the Local Arm and the Sagittarius Arm. We discovered new giant molecular filaments (GMFs) in Sh 2-86, with a length of ∼30 pc, width of ∼5 pc, and molecular mass of ∼4 ×10⁴ M_☉. We also found that Sh 2-86 contains the three velocity components at 22, 27, and 33 km s^–1. These clouds and GMFs are likely to be physically associated with Sh 2-86 because they have high ¹²CO J = 2-1 to J = 1-0 intensity ratios and coincide with the infrared dust emission. The open cluster NGC 6823 exists at the common intersection of these clouds. We argue that the multiple cloud interaction scenario, including GMFs, can explain cluster formation in the Vulpecula OB association.