Molecular gas in high-mass filament WB673

Abstract

We studied the distribution of dense gas in a filamentary molecular cloud containing several dense clumps. The center of the filament is given by the dense clump WB673. The clumps are high-mass and intermediate-mass star-forming regions. We observed CS(2-1), 13CO(1-0), C18O(1-0) and methanol lines at 96GHz toward WB673 with the Onsala Space Observatory 20-m telescope. We found CS(2-1) emission in the inter-clump medium so the clumps are physically connected and the whole cloud is indeed a filament. Its total mass is $10^4$ M${}_{\odot }$ and mass-to-length ratio is 360 M${}_{\odot }$pc${}^{-1}$ from 13CO(1-0) data. Mass-to-length ratio for the dense gas is $3.4-34$ M${}_{\odot }$pc${}^{-1}$ from CS(2-1) data. The PV-diagram of the filament is V-shaped. We estimated physical conditions in the molecular gas using methanol lines. Location of the filament on the sky between extended shells suggests that it could be a good example to test theoretical models of formation of the filaments via multiple compression of interstellar gas by supersonic waves.

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Cited by in corpus (6)

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• The warm-up phase in massive star-forming cores around RCW 120
• Filamentary Structures and Star Formation Activities in the Sites S234, V582, and IRAS 05231+3512
• Study of the filamentary infrared dark cloud G192.76+00.10 in the S254-S258 OB complex
• NH${}_3$ Observations of the S235 Star Forming Region: Dense Gas in Inter-core Bridges
• Star formation timescale in the molecular filament WB 673