Physics & Astronomy ETDs

Publication Date



In Chapter 1, I outline the methods of making ground-based infrared observations. I concentrate on the observational procedures rather than the instrumental design. Near-infrared observations of S 156A, _S 158A, S 159A, S 162A1, S 228, and G 45. 5 + 0 .1 (#2) made with a beam size of ̴1 are used to estimate the total near infrared flux. After correcting for the line of sight extinction the near infrared luminosities are greater than the Lyman-α luminosities inferred from radio observations. A strong double peaked infrared source was discovered near the region of G 25.3-0.1. The infrared source and the radio source previously reported in this region seem to be two separate sources. Peak A of the infrared source seems to be a late M star with a circumstellar dust and ice shell. Peak B seems to be an HII region with a massive ( ̴ 5-10 M0) Pre-Main Sequence exciting star. I present near infrared observations of W 49 CC#l, W 49 CC#6, W 40, G 24.8 + 0.1, G 25.4 - 0.2 and W 52. These observations were made with 46" and 63" beam sizes. Only W 49 CC#6 has been previously observed in the near infrared, and these observations were made with a 7" beam. I compute extinction coefficients for the sources that have radio observations. In Chapter 5, I present near infrared broad band and medium resolution spectral observations of Comet West (1975n). The observations show color temperatures higher than would be expected from solar heating of a grey body. This temperature difference can be explained by the emissivity of the particles in the comet varying with the wavelength.

Degree Name


Level of Degree


Department Name

Physics & Astronomy

First Committee Member (Chair)

Michael Zeilik II

Second Committee Member

David Solomon King

Third Committee Member

Colston Chandler



Document Type