Adelberger, Kurt L. (2002) Star formation and structure formation at redshifts 1 < z < 4. Dissertation (Ph.D.), California Institute of Technology. http://resolver.caltech.edu/CaltechETD:etd-09252008-090426
NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document. The universe of galaxies beyond redshift one has finally become relatively easy to observe. While only a handful of galaxies with redshifts z > 1 were known 10 years ago, more than 2000 have spectroscopic redshifts today. These surveys are beginning to provide us with a detailed view of the first half of cosmic history. Their creation and interpretation is the subject of this thesis. Chapter 1 describes efficient techniques that can be used to locate galaxies at 1 [...] z [...] 5 among the numerous foreground and background objects in deep optical images. Chapter 2 characterizes the effects of dust obscuration on the resulting large high-redshift samples. The remainder of the thesis attemtps to place star-forming high-redshift galaxies into a larger cosmological context. Chapter 3 investigates the spatial clustering of galaxies at z ~ 3, finds it to be strong, and shows that this suggests a close link between rapidly star-forming galaxies and massive virialized objects in the underlying distribution of dark matter. Chapter 4 analyses the curious spatial association of high-redshift galaxies with inter-galactic hydrogen and metals, and finds some evidence that the numerous supernova explosions in young galaxies may profoundly affect the evolution of the universe's baryons.
|Item Type:||Thesis (Dissertation (Ph.D.))|
|Degree Grantor:||California Institute of Technology|
|Division:||Physics, Mathematics and Astronomy|
|Thesis Availability:||Restricted to Caltech community only|
|Defense Date:||22 February 2001|
|Default Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Imported from ETD-db|
|Deposited On:||07 Oct 2008|
|Last Modified:||29 Jan 2014 23:39|
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