The Cluster-forming Site AFGL 5157: Colliding Filamentary Clouds and Star Formation

Abstract

Abstract We observationally investigate star formation process occurring in AFGL 5157 (area ∼13.5 pc × 13.5 pc) using a multi-wavelength approach. Embedded filaments are seen in the Herschel column density map, and one of them is identified as an elongated filamentary feature (FF) (length ∼8.3 pc; mass ∼1170 M ⊙). Five Herschel clumps (M clump ∼45–300 M ⊙) are traced in the central part of the FF, where an extended temperature structure (T d ∼13.5–26.5 K) is observed. In the direction of the central part of the FF, the warmer region at T d ∼20–26.5 K spatially coincides with a mid-infrared shell surrounding a previously known evolved infrared cluster. Diffuse Hα emission is traced inside the infrared shell, suggesting the presence of massive stars in the evolved cluster. Based on the surface density analysis of young stellar objects (YSOs), embedded clusters of YSOs are traced toward the central part of the FF, and are distributed around the infrared shell. Previously detected H2O masers, H2 knots, massive protostar candidates, and an H ii region are also seen toward the embedded clusters. Using the 12CO and 13CO line data, the central part of the FF is observed at the overlapping zones of two filamentary molecular clouds (length ∼12.5 pc) around −20 and −17 km s−1, which are also connected in velocity. Our observational results suggest that the formation of massive stars appears to be triggered by a collision of two filamentary molecular clouds, which might have also influenced the birth of YSOs in AFGL 5157.