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dc.contributor.advisorGebhardt, Karl
dc.creatorJee, Inhen
dc.date.accessioned2013-09-25T21:24:13Zen
dc.date.accessioned2017-05-11T22:34:00Z
dc.date.available2013-09-25T21:24:13Zen
dc.date.available2017-05-11T22:34:00Z
dc.date.issued2013-08en
dc.date.submittedAugust 2013en
dc.identifier.urihttp://hdl.handle.net/2152/21330en
dc.descriptiontexten
dc.description.abstractWe discuss two ways of measuring angular diameter distances in the Universe: (i) Baryon Acoustic Oscillation (BAO) , and (ii) strong gravitational lensing. For (i), we study the effects of survey geometry and selection functions on the 2-point correlation function of Lyman- alpha emitters in 1.9 < z < 3.5 for Hobby-Eberly Telescope Dark Energy Experiment (HETDEX). We develop a method to extract the BAO scale (hence a volume-averaged angular diameter distance D_V, which is a combination of the angular diameter distance and the Hubble expansion rate, i.e., [cz〖(1+z)〗^2 〖D_A〗^2 H^(-1) ]^(1/3)) from a spherically averaged 1-d correlation function. We quantify the statistical errors on such measurements. By using log-normal realizations of the HETDEX dataset, we show that we can determine DV from HETDEX at 2% accuracy using the 2-point correlation function. This study is complementary to the on-going effort to characterize the power spectrum using HETDEX. For (ii), a previous study (Para ficz and Hjorth 2009) looked at the case of a spherical lens following a singular isothermal distribution of matter and an isotropic velocity distribution, and found that combining measurements of the Einstein ring radius with the time delay of a strong lens system directly leads to a measurement of the angular diameter distance, D_A. Since this is a very new method, it requires more careful investigations of various real-world eff ects such as a realistic matter density pro file, an anisotropic velocity distribution, and external convergence. In more realistic lens confi gurations we find that the velocity dispersion is the dominant source of the uncertainty ; in order for this method to achieve competitive precision on measurements of DA, we need to constrain the velocity dispersion, down to the percent level. On the other hand, external convergence and velocity dispersion anisotropy have negligible e ect on our result. However, we also claim that the dominant source of the uncertainty depends largely on the image con figuration of the system, which leads us to the conclusion that studying the angular dependence of the lens mass distribution is a necessary component.en
dc.format.mediumelectronicen
dc.language.isoengen
dc.rightsCopyright is held by the author. Presentation of this material on the Libraries' web site by University Libraries, The University of Texas at Austin was made possible under a limited license grant from the author who has retained all copyrights in the works.en
dc.subjectAngular diameter distanceen
dc.subjectBaryon Acoustic Oscillationen
dc.subject2-point correlation functionen
dc.subjectHETDEXen
dc.subjectStrong gravitational lensingen
dc.subjectStandard ruleren
dc.titleMeasuring angular diameter distances in the universe by Baryon Acoustic Oscillation and strong gravitational lensingen
dc.typeThesisen
dc.description.departmentAstronomyen
dc.identifier.slug2152/21330en


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