Mathematics – Logic
Scientific paper
Aug 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003phdt.........2d&link_type=abstract
Thesis (PhD). THE JOHNS HOPKINS UNIVERSITY, Source DAI-B 64/02, p. 761, Aug 2003, 397 pages.
Mathematics
Logic
4
Scientific paper
It is impossible to understand the stars which make up our galaxy without understanding the properties and kinematics of the interstellar medium (ISM). I study the ISM of the Magellanic Clouds using three different, complementary datasets. The first is a set of 141 far- ultraviolet (FUV) spectra taken by the Far Ultraviolet Spectroscopic Explorer (FUSE ) satellite of sight lines toward hot, OB stars in the Large and Small Magellanic Clouds (LMC and SMC). I use these stars as background sources and study the absorption in the intervening ISM. FUSE data contain hundreds of transitions which probe a wide range of conditions in the ISM from cold, molecular gas to hot, ionized material. Secondly, I use a collection of emission-line images of the Magellanic Clouds in Hα light to provide a morphological context for the FUV absorption data. Finally, I present a set of 99 longslit echelle optical emission spectra to act as a bridge between the kinematics seen in the absorption spectra and the morphology seen in the images. These data lack the broad range of ISM diagnostics present in the FUSE data, but feature spatial resolution in one dimension. I use the combination of optical images and optical spectra to categorize each sight line by ISM morphology. The diagnostic power of this combined dataset is immense. I use these datasets to search for global patterns in the Magellanic ISM. In particular, I measure the velocities, widths, and column densities of the absorption features in five different FUV transitions and two optical transitions. Various other data from the literature are added to this collection and I search for correlations between different parameters. The picture that emerges is one of a three-phase ISM with cold, warm, and hot phases. The kinematics and distribution of each phase bear little resemblance to each other. Additionally, I use the high velocity resolution of the spectral data to perform two more focussed investigations on the global dataset. Finally, I carry out two investigations of specific ISM structures using small subsets of the emission and absorption data. (Abstract shortened by UMI.)
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