Cluster-forming site AFGL 5157: colliding filamentary clouds and star formation

Abstract

We observationally investigate star formation (SF) process occurring in AFGL 5157 (area ~13.5 pc X 13.5 pc) using a multi-wavelength approach. Embedded filaments are seen in the {\it Herschel} column density map, and one of them is identified as an elongated filamentary feature (FF) (length ~8.3 pc; mass ~1170 Msun). Five Herschel clumps (Mclump ~45-300 Msun) are traced in the central part of FF, where an extended temperature structure (Td ~13.5-26.5 K) is observed. In the direction of the central part of FF, the warmer region at Td ~20-26.5 K spatially coincides with a mid-infrared (MIR) shell surrounding a previously known evolved infrared cluster. Diffuse H-alpha 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 FF, and are distributed around the infrared shell. Previously detected H2O masers, H2 knots, massive protostar candidates, and HII region are also seen toward the embedded clusters. Using the 12CO and 13CO line data, the central part of FF is observed at the overlapping zones of two filamentary molecular clouds (length ~12.5 pc) around -20 and -17 km/s, 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.

21 pages, 14 figures, Accepted for publication in The Astrophysical Journal

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• Simulation of Head-on Collisions Between Filamentary Molecular Clouds Threaded by a Lateral Magnetic Field and Subsequent Evolution
• Instability and Evolution of Shocked Clouds Formed by Orthogonal Collisions between Magnetized Filamentary Molecular Clouds
• HI Narrow-Line Self-Absorptions Toward the High-Mass Star-Forming Region G176.51+00.20
• Kronberger 55: A Candidate for End-dominated Collapse Scenario
• Evolution of compressed clouds formed by filament coalescence. I. Oblique collisions
• Neutral Stellar Winds Toward the High-Mass Star-Forming Region G176.51+00.20