2026-09-19T22:35:15Zhttps://dspace.mit.edu/server/oai/requestoai:dspace.mit.edu:1721.1/327372022-01-13T07:54:41Zcom_1721.1_7582com_1721.1_7581col_1721.1_131024
Jacqueline N. Hewitt.
Dorsher, Susan E. (Susan Elaine), 1982-
Massachusetts Institute of Technology. Dept. of Physics.
Massachusetts Institute of Technology. Department of Physics
2006-05-15T20:26:26Z
2006-05-15T20:26:26Z
2004
2004
http://hdl.handle.net/1721.1/32737
56729405
Thesis (S.B.)--Massachusetts Institute of Technology, Dept. of Physics, 2004.
Includes bibliographical references (leaves 69-73).
We develop a technique for measuring cosmological parameters ([omega]M and w) using gravitational lens geometry, source and lens redshifts, and the velocity dispersion of the lensing galaxy. This technique makes use of the relation [theta][sub]E = 4[pi]... where the critical radius [theta][sub]E and the one-dimensional velocity dispersion of the lensing galaxy [sigma]v are observable and the angular diameter distance ratio D[sub]LS/D[sub]S is related to the source and lens redshifts Z[source] and Z[lens] through the cosmological model. We assess the feasibility of this technique by examining the dependence of that ratio on cosmological parameters, doing a Monte Carlo simulation with a singular isothermal sphere lens galaxy, and estimating the error due to the asymmetry of real lenses. We conclude that the method is feasible with a large lens sample and a nearly circular projected mass distribution. We expect errors of less than 0.1 in [omega]M for a flat universe with a cosmological constant and a lens sample selected so that the axial ratio f > 0.8 for each lens.
by Susan E. Dorsher.
S.B.
73 leaves
2770905 bytes
2773672 bytes
application/pdf
application/pdf
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Massachusetts Institute of Technology
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http://dspace.mit.edu/handle/1721.1/7582
Physics.
Using gravitational lens geometry to measure cosmological parameters
Thesis
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<Abstract>We develop a technique for measuring cosmological parameters ([omega]M and w) using gravitational lens geometry, source and lens redshifts, and the velocity dispersion of the lensing galaxy. This technique makes use of the relation [theta][sub]E = 4[pi]... where the critical radius [theta][sub]E and the one-dimensional velocity dispersion of the lensing galaxy [sigma]v are observable and the angular diameter distance ratio D[sub]LS/D[sub]S is related to the source and lens redshifts Z[source] and Z[lens] through the cosmological model. We assess the feasibility of this technique by examining the dependence of that ratio on cosmological parameters, doing a Monte Carlo simulation with a singular isothermal sphere lens galaxy, and estimating the error due to the asymmetry of real lenses. We conclude that the method is feasible with a large lens sample and a nearly circular projected mass distribution. We expect errors of less than 0.1 in [omega]M for a flat universe with a cosmological constant and a lens sample selected so that the axial ratio f > 0.8 for each lens.</Abstract>
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