Weak gravitational lensing by large scale structure affects the number counts of faint galaxies through the “magnification bias” and thus affects the measurement of the angular two-point correlation function ω(θ). At faint magnitudes the clustering amplitude will decrease differently with limiting magnitude than expected from Limber’s equation. The amplitude will hit a minimum and then rise wit...

A massive foreground cluster lens changes the shapes (shear effect) and number density (magnification effect) of the faint background galaxy population. In this paper we investigate how the shear, magnification and combined information can be used to constrain cluster mass profiles in the weak lensing regime. We develop maximum likelihood techniques to make quantitative predictions for each of ...

This study is investigated the optimum parameters for a tuned mass damper (TMD) under the seismic excitation. Shuffled complex evolution (SCE) is a meta-heuristic optimization method which is used to find the optimum damping and tuning frequency ratio for a TMD. The efficiency of the TMD is evaluated by decreasing the structural displacement dynamic magnification factor (DDMF) and acceleration ...

A holographic projection system with optical zoom is demonstrated. By using a combination of a LC lens and an encoded Fresnel lens on the LCoS panel, we can control zoom in a holographic projector. The magnification can be electrically adjusted by tuning the focal length of the combination of the two lenses. The zoom ratio of the holographic projection system can reach 3.7:1 with continuous zoo...