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Molecular gas in high-mass filament WB673

Maria S. Kirsanova ; Svetlana V. Salii ; Andrej M. Sobolev ; Henrik Olofsson (Institutionen för rymd-, geo- och miljövetenskap, Onsala rymdobservatorium) ; Dmitry A. Ladeyschikov ; Magnus Thomasson (Institutionen för rymd-, geo- och miljövetenskap, Astronomi och plasmafysik)
Open Astronomy Vol. 26 (2017), 1, p. 99–105.
[Konferensbidrag, refereegranskat]

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 starforming regions. We observed CS (2-1), 13CO (1-0), C18O(1-0), and methanol lines at 96 GHz 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 104 M⊙ and mass-to-length ratio is 360M⊙ pc−1 from 13CO (1-0) data. Mass-to-length ratio for the dense gas is 3.4 − 34M⊙ 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.

Nyckelord: star formation, massive stars, H ɪɪ regions, bubbles



Denna post skapades 2018-01-12. Senast ändrad 2018-01-12.
CPL Pubid: 254443

 

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