M ost of the perceptual cues we use to visualize 3D structures are available in 2D projections. This is why we can make sense of photographs and images on a television screen, at the cinema, or on a computer monitor. Such cues include occlusion, perspective, familiar size, and atmospheric haze. Four cues are missing from 2D media: stereo parallax—seeing a different image with each eye; movement...

This paper presents a method for relative orientation using the feature based matching techniques. The interest operator and feature based matching are use to select points and measure parallax for relative orientation automatically. After the feature based matching, a fine least square matching is preformed to achieve high precision. The matched points are then used for the relative orientatio...

We show that binary microlensing events with three well-measured peaks (two caustic crossings plus a cusp approach) can yield determinations of both the projected Einstein radius r̃E and the angular Einstein radius θE, and so the lens mass M = c2(4G)−1r̃EθE. To a certain extent, rotation of the binary can mimic the effects of parallax, but should often be possible to disentangle parallax from rot...

The most powerful tool for measuring distances within our Galaxy is the annual parallax. We carried out phase-referencing VLBI observations of H2O masers in the star forming region W3(OH) with respect to the extragalactic continuum source ICRF 0244+624 to measure their absolute proper motions. The measured annual parallax is 0.484 ± 0.004 milli-arcseconds which corresponds to a distance of 2.07...

We study the first microlensing event toward the Carina spiral arm discovered by the OGLE collaboration. We demonstrate that this long duration event exhibits strong parallax signatures. Additional information from the parallax effect allows us to determine the lens transverse velocity projected onto the Sun-source line to be ∼ 145 km s. We also estimate the optical depth, event rate and durati...

The results obtained by two algorithms of statistical parallaxes applied to a large sample of RR Lyrae stars are compared. They show no significant difference and confirm the validity of the earlier approach based on the principle of maximum likelihood.