Molecular gas in high-mass filament WB 673
Journal article, 2017

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 WB 673. The clumps are high-mass and intermediate-mass star-forming regions. We observed CS (2–1), 13 CO (1–0), C 18 O (1–0), and methanol lines at 96 GHz toward WB 673 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 and mass-to-length ratio is 360 M pc 1 from 13 CO (1–0) data. Mass-to-length ratio for the dense gas is 3.4 34 M 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.

Massive stars

Star formation

Bubbles

H II regions

Author

M. S. Kirsanova

Ural Federal University

Svetlana V. Salii

Ural Federal University

A. M. Sobolev

Ural Federal University

Henrik Olofsson

Chalmers, Earth and Space Sciences, Onsala Space Observatory, Onsala Space Observatory, Observation Support

Dmitry A. Ladeyschikov

Ural Federal University

Magnus Thomasson

Chalmers, Earth and Space Sciences, Extragalactic Astrophysics

Open Astronomy

2543-6376 (ISSN)

Vol. 26 1 99-105

Subject Categories

Subatomic Physics

Meteorology and Atmospheric Sciences

Astronomy, Astrophysics and Cosmology

DOI

10.1515/astro-2017-0020

More information

Latest update

5/29/2018