Observational constraints on dark energy cosmological model parameters

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dc.contributor.author Farooq, Muhammad Omer
dc.date.accessioned 2013-10-09T17:30:51Z
dc.date.available 2013-10-09T17:30:51Z
dc.date.issued 2013-10-09
dc.identifier.uri http://hdl.handle.net/2097/16623
dc.description.abstract The expansion rate of the Universe changes with time, initially slowing (decelerating) when the universe was matter dominated, because of the mutual gravitational attraction of all the matter in it, and more recently speeding up (accelerating). A number of cosmological observations now strongly support the idea that the Universe is spatially flat (provided the dark energy density is at least approximately time independent) and is currently undergoing an accelerated cosmological expansion. A majority of cosmologists consider ``dark energy" to be the cause of this observed accelerated cosmological expansion. The ``standard" model of cosmology is the spatially-flat $\Lambda$CDM model. Although most predictions of the $\Lambda$CDM model are reasonably consistent with measurements, the $\Lambda$CDM model has some curious features. To overcome these difficulties, different Dark Energy models have been proposed. Two of these models, the XCDM parametrization and the slow rolling scalar field model $\phi$CDM, along with ``standard" $\Lambda$CDM, with the generalization of XCDM and $\phi$CDM in non-flat spatial geometries are considered here and observational data are used to constrain their parameter sets. In this thesis, we start with a overview of the general theory of relativity, Friedmann's equations, and distance measures in cosmology. In the following chapters we explain how we can constrain the three above mentioned cosmological models using three data sets: measurements of the Hubble parameter $H(z)$, Supernova (SN) apparent magnitudes, and the baryonic acoustic oscillations (BAO) peak length scale, as functions of redshift $z$. We then discuss constraints on the deceleration-acceleration transition redshift $z_{\rm da}$ using unbinned and binned $H(z)$ data. Finally, we incorporate the spatial curvature in the XCDM and $\phi$CDM model and determine observational constraints on the parameters of these expanded models. en_US
dc.language.iso en_US en_US
dc.publisher Kansas State University en
dc.subject Cosmology constraints en_US
dc.subject Dark energy en_US
dc.subject Constraints en_US
dc.title Observational constraints on dark energy cosmological model parameters en_US
dc.type Dissertation en_US
dc.description.degree Doctor of Philosophy en_US
dc.description.level Doctoral en_US
dc.description.department Department of Physics en_US
dc.description.advisor Bharat Ratra en_US
dc.subject.umi Astrophysics (0596) en_US
dc.subject.umi Physics (0605) en_US
dc.subject.umi Theoretical Physics (0753) en_US
dc.date.published 2013 en_US
dc.date.graduationmonth December en_US

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