H II region--molecular cloud complex W 3: A model derived from molecular observations

Journal Article · Sun Jun 15 04:00:00 EDT 1980 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/158044· OSTI ID:5002984

Dickel, H R

A model of the W3 molecular cloud is constructed from the analysis of /sup 12/CO, /sup 13/CO, CS, HCN, and H/sub 2/CO molecular data. Originally an initial cloud of mass approx.5 x 10/sup 4/ M/sub sun/ started to fragment and collapse after passage through the spiral density-wave shock of the Perseus arm. The open cluster (Ocl 352) which excites the present W4 H II region formed at the head of the cloud a few million years ago. The ionization front with its associated shock is expanding into the remaining W3 molecular cloud where its effects are seen in the velocities of W3(OH) and the infrared source AFGL 333. The bright dense ''core'' of the W3 molecular cloud which contains six embedded compact H II regions, eight near-infrared sources, and three H/sub 2/O masers is collapsing and possibly rotating.

• Research Organization: Astronomy Department, University of Illinois; and Sterrewacht, Leiden
• OSTI ID: 5002984
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 238:3; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640105* -- Astrophysics & Cosmology-- Galaxies
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ABUNDANCE
CHEMICAL COMPOSITION
COSMIC GASES
COSMIC RADIO SOURCES
FLUIDS
FUNCTIONS
GASES
GRAVITATIONAL COLLAPSE
H2 REGIONS
IONIZATION
MOLECULES
NEBULAE
RADIAL VELOCITY
SHOCK WAVES
SPECTRAL DENSITY
SPECTRAL FUNCTIONS
STAR CLUSTERS
VELOCITY