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The distribution of interstellar medium in the Scd galaxy NGC 6946 and in a sample of dwarf irregular galaxies

Thesis/Dissertation ·
OSTI ID:5095982
The author has compared the atomic and molecular hydrogen distributions in the spiral galaxy NGC 6946 and in 15 dwarf irregular galaxies. He made observations of the CO J = 1 {yields} 0 transition to obtain a fully sampled map to a radium of 10 kpc in NGC 6946, using the 14-meter telescope of the Five College Radio Astronomy Observatory, and also completely mapped the 21-cm line of neutral hydrogen with the Very Large Array. He has also made CO observations at FCRAO in 15 dwarf irregular galaxies spanning a wide range of infrared luminosity and color. In NGC 6946 the CO HI maps were used to investigate the radial and azimuthal variations in the atomic and molecular gas. The H{sub 2} mass is found to dominate the ISM in the inner disk of this galaxy. The H{sub 2}, H{alpha}, radio continuum, and blue light radial profiles are found to be centrally peaked with exponential falloffs, while the HI distribution is much flatter, with a central depression. He infers a constant efficiency of star formation with radium in NGC 6946 and suggest that HI plays only a passive role in the star formation process of this galaxy. Spiral arm enhancements in the H{sub 2} surface densities, H{alpha} surface brightnesses, and {sigma} (H{sub 2})/{mu}(H{alpha}) ratios are observed. The presence of these arm enhancements, as well as enhancements in the gas surface densities in interarm regions is consistent with a picture in which cloud-cloud collisions play an important role in the star formation process in NGC 6946. For the dwarf galaxies, high observed L{sub IR}/L{sub CO} ratios in the blue systems are indicative of a present burst of star formation, while the red systems exhibit low L{sub IR}/L{sub CO} ratios.
Research Organization:
Massachusetts Univ., Amherst, MA (USA)
OSTI ID:
5095982
Country of Publication:
United States
Language:
English