CN line emission from the molecular clouds assoiated with S106 and NGC 7538

Journal Article · Thu Jul 15 04:00:00 EDT 1982 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/160103· OSTI ID:6849025

Churchwell, E; Bieging, J H

The line intensity distributions of the N = 1--0 transition of CN are presented for the molecular clouds associated with S106 and NGC 7538. In S106, CN line emission is largely proportional to the column density of CN; the temperature and density structure of S106 are fairly complex and clearly influence the CN line intensities, but generally the CN column density and line intensity vary together. The CN emission in S106 appears to be a disk of molecular gas in which an 08 or 09 star has formed, ionized, and dispersed the central part of the disk, and left a molecular torus with an expanding double-lobed H II region approximately perpendicular to the plane of the torus. In NGC 7538 the CN column density is essentially constant over the whole mapped region, and the CN line intensities vary with the excitation temperature. Thus the CN emission toward NGC 7538 outlines a region of enhanced H/sub 2/ density, or kinetic temperature, or both. At least three regions of successive star formation are apparent toward NGC 7538. The most recent star formation appears to be occuring in the region of maximum CN emission.

• Research Organization: Washburn Observatory, University of Wisconsin-Madison
• OSTI ID: 6849025
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 258:2; 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 RADIO SOURCES
CYANOGEN
EMISSION SPECTRA
ENERGY-LEVEL TRANSITIONS
EXCITATION
H2 REGIONS
INTERSTELLAR GRAINS
NEBULAE
PARTICLES
SPECTRA