Statistics
Scientific paper
Jan 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000phdt........71t&link_type=abstract
PhD Thesis, Department of Astronomy, Faculty of Science, Kyoto University, Japan. VIII+117 pp. (2000)
Statistics
1
Galaxies, Evolution, Statistics
Scientific paper
In this thesis, we explore the history of the galaxy evolution through the statistical properties of galaxies, especially through their infrared emission. We use the infrared galaxy number count as a probe of the evolutionary status of galaxies, because it is known that the infrared emission of galaxies is generated mainly from the dust in star-forming regions, heated by ultraviolet photon from young massive stars. Thus the term "galaxy evolution" is nearly equal to the star formation history of galaxies in this thesis. In order to understand the entire history of the evolution of galaxies, there are roughly two approaches: one is based on the fundamental physical processes and deducing the phenomena (we call it the forward approach), and the other is based on the observations of (relatively) nearby galaxies and induce their early properties (backward or empirical approach). Both of them are important and they should interact and stimulate each other. At present, many observational projects are now in progress, whose results expected to give great impacts to various fields. For direct comparison of the prediction with these forthcoming new observation, we prefer the empirical approach in this thesis. We conclude that the evolution of galaxies from z=0 to 2 is much stronger than previously estimated from the IRAS survey. Considering our SED ingredients we suggest that the evolving population is starburst-like galaxy. Redshift estimation using galaxy FIR colors can be practicable using sets of bandpasses 50, 70, and 150 μm with the aid of present and future optical surveys. The concepts of FIR-sub-mm color-color diagram is now regarded as a strong tool for finding distant galaxies. Thus, our predictions will be used to construct the strategy of future observations of young galaxies.
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