Dispersed fringe sensor for the Giant Magellan Telescope.

The Giant Magellan Telescope (GMT) consists of seven 8.365 m segments, with gaps of 0.345 m between adjacent segments.

The dark side of the rings of Uranus.

The rings of Uranus are oriented edge-on to Earth in 2007 for the first time since their 1977 discovery. This event provides a rare opportunity to observe their dark (unlit) side, where dense rings darken to near invisibility, but faint rings become much brighter. We present a ground-based infrared image of the unlit side of the rings that shows that the system has changed dramatically since previous views.

Modeling low order aberrations in laser guide star adaptive optics systems.

When using a laser guide star (LGS) adaptive optics (AO) system, quasi-static aberrations are observed between the measured wavefronts from the LGS wavefront sensor (WFS) and the natural guide star (NGS) WFS. These LGS aberrations, which can be as much as 1200 nm RMS on the Keck II LGS AO system, arise due to the finite height and structure of the sodium layer. The LGS aberrations vary significantly between nights due to the difference in sodium structure.

Quasi-static aberrations induced by laser guide stars in adaptive optics.

Laser Guide Star Adaptive Optics (LGS AO) systems use the return from an artificial guide star to measure the wavefront aberrations in the direction of the science object. We observe quasi-static differences between the measured wavefront and the wavefront aberration of the science object. This paper quantifies and explains the source of the difference between the wavefronts measured using an LGS and a natural guide star at the W.

A low density of 0.8 g cm(-3) for the Trojan binary asteroid 617 Patroclus.

The Trojan population consists of two swarms of asteroids following the same orbit as Jupiter and located at the L4 and L5 stable Lagrange points of the Jupiter-Sun system (leading and following Jupiter by 60 degrees ). The asteroid 617 Patroclus is the only known binary Trojan. The orbit of this double system was hitherto unknown.

Measuring the centroid gain of a Shack-Hartmann quad-cell wavefront sensor by using slope discrepancy.

Shack-Hartmann wavefront sensors (SH WFS) are used by many adaptive optics (AO) systems to measure the wavefront. In this WFS, the centroid of the spots is proportional to the wavefront slope. If the detectors consist of 2 x 2 quad cells, as is the case in most astronomical AO systems, then the centroid measurement is proportional to the centroid gain.

Performance of the Keck Observatory adaptive-optics system.

The adaptive-optics (AO) system at the W. M. Keck Observatory is characterized.

Atmospheric turbulence characterization with the Keck adaptive optics systems. I. Open-loop data.

We present a detailed investigation of different methods of the characterization of atmospheric turbulence with the adaptive optics systems of the W. M. Keck Observatory.

Wave-front sensing from defocused images by use of wave-front slopes.

We describe a novel technique for deriving wave-front aberrations from two defocused intensity measurements. The intensity defines a probability density function, and the method is based on the evolution of the cumulative density function of the intensity with light propagation. In one dimension, the problem is easily solved with a histogram specification procedure, with a linear relationship between the wave-front slope and the difference in the abscissas of the histograms.

Extended analysis of curvature sensing.

Curvature sensors are used in adaptive optics to measure the wave-front aberrations. In practice, their performance is limited by their nonlinear behavior, which we characterize by solving simultaneously the irradiance transport equation and the accompanying wave-front transport equation. We show how the presence of nonlinear geometric terms limits the accuracy of the sensor and how diffraction effects limit the spatial resolution.