Formation of OB clusters: W33 complex

Journal Article · Fri Apr 15 04:00:00 EST 1983 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/160900· OSTI ID:6120454

Haschick, A D; Ho, P T.P.

OB star formation in the W33 complex is studied using radio continuum interferometry and the spectral lines of the NH/sub 3/ molecule. Although OB star formation is extended on the scale of 10 pc, the most recent episode of star formation producing the most massive stars in the region is confined to a 1 pc core within the dense molecular gas. The clumpy appearance of the H II region is consistent with the interpretation that a cluster of OB stars has formed recently in the core of the molecular cloud. Although the radio structures are well correlated with observed 20 ..mu..m structures, the latter observation underestimates the intrinsic luminosities of the exciting sources. Far-infrared measurements, however, do provide a reliable indication of the total luminosity of the region. If a cluster of OB stars has formed in the core of W33, the observed total luminosity suggests that this cluster does not extend below O8. The location of the most massive and youngest stars toward the core of this region supports the traditional notion that star formation proceeds by a slow collection of the gas, followed by fragmentation, collisions, and subsequent coagulations.

• OSTI ID: 6120454
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 267:2; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
AMMONIA
COSMIC RADIO SOURCES
H2 REGIONS
HYDRIDES
HYDROGEN COMPOUNDS
INFRARED SPECTRA
INTERFEROMETRY
INTERSTELLAR GRAINS
MAPS
NITROGEN COMPOUNDS
NITROGEN HYDRIDES
PARTICLES
SPECTRA
STAR CLUSTERS
STAR EVOLUTION