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A sodium-layer laser guide star beacon with high-order adaptive optics at Lick Observatory (Mount Hamilton, California) produced a factor of 2.4 intensity increase and a factor of 2 decrease in full width at half maximum for an astronomical point source, compared with image motion compensation alone. The image full widths at half maximum were identical for laser and natural guide stars (0.3 arc second). The Strehl ratio with the laser guide star was 65 percent of that with a natural guide star. This technique should allow ground-based telescopes to attain the diffraction limit, by correcting for atmospheric distortions.

We screened 67 mutants in the O-helix of Thermus aquaticus (Taq) DNA polymerase I (pol I) for altered fidelity of DNA synthesis. These mutants were obtained (Suzuki, M., Baskin, D., Hood, L., and Loeb, L. A. (1996) Proc. Natl. Acad. Sci. U. S. A. 93, 9670-9675) by substituting an oligonucleotide containing random sequences for codons 659-671, and selecting for complementation of a growth defect in Escherichia coli caused by temperature-sensitive host pol I. Thirteen mutants decreased fidelity in a screen that employed primer extension reactions lacking one of four complementary deoxynucleoside triphosphates (dNTPs). Three mutants were purified and exhibited 29-68% of wild-type specific activity. Homogeneous polymerases A661E, A661P, and T664R extended primers further than the wild-type, synthesizing past template nucleotides for which the complementary dNTP was absent. The data indicate that both misinsertion of incorrect nucleotides and extension of mispaired primer termini were increased. In a lacZalpha forward mutation assay, A661E and T664R yielded mutation frequencies at least 7- and 25-fold greater, respectively, than that of the wild-type polymerase. These findings emphasize the importance of the O-helix in substrate recognition and are compatible with a role for pyrophosphate release in enhancing fidelity of DNA synthesis.

Programs at LLNL that involve large laser systems--ranging from the National Ignition Facility to new tactical laser weapons--depend on the maintenance of laser beam quality through precise control of the optical wavefront. This can be accomplished using adaptive optics, which compensate for time-varying aberrations that are often caused by heating in a high-power laser system. Over the past two decades, LLNL has developed a broad capability in adaptive optics technology for both laser beam control and high-resolution imaging. This adaptive optics capability has been based on thin deformable glass mirrors with individual ceramic actuators bonded to the back. In the case of high-power lasers, these adaptive optics systems have successfully improved beam quality. However, as we continue to extend our applications requirements, the existing technology base for wavefront control cannot satisfy them. To address this issue, this project studied improved modeling tools to increase our detailed understanding of the performance of these systems, and evaluated novel approaches to low-order wavefront control that offer the possibility of reduced cost and complexity. We also investigated improved beam control technology for high-resolution wavefront control. Many high-power laser systems suffer from high-spatial-frequency aberrations that require control of hundreds or thousands of phase points tomore » provide adequate correction. However, the cost and size of current deformable mirrors can become prohibitive for applications requiring more than a few tens of phase control points. New phase control technologies are becoming available which offer control of many phase points with small low-cost devices. The goal of this project was to expand our wavefront control capabilities with improved modeling tools, new devices that reduce system cost and complexity, and extensions to high spatial and temporal frequencies using new adaptive optics technologies. In FY 99, the second year of this project, work was performed in four areas (1) advanced modeling tools for deformable mirrors (2) low-order wavefront correctors with Alvarez lenses, (3) a direct phase measuring heterdyne wavefront sensor, and (4) high-spatial-frequency wavefront control using spatial light modulators.« less

The resolution of ground-based telescopes is typically limited to {approx}1 second of arc because of the blurring effects of atmospheric turbulence. Adaptive optics (AO) technology senses and corrects for the optical distortions due to turbulence hundreds of times per second using high-speed sensors, computers, deformable mirror, and laser technology. The goal of this project is to make AO systems widely useful astronomical tools providing resolutions up to an order of magnitude better than current, ground-based telescopes. Astronomers at the University of California Lick Observatory at Mt. Hamilton now routinely use the LLNL developed AO system for high resolution imaging of astrophysical objects. We report here on the instrument development progress and on the science observations made with this system during this 3-year ERI project.

The W.M. Keck Observatory, in collaboration with Lawrence Livermore National Laboratory (LLNL), is currently in the critical design phase of a natural guide star (NGS) and single laser guide star (LGS) adaptive optics (AO) user facility for the Nasmyth platform of the Keck II 10-m telescope.1 Two science instruments will accompany the AO facility: a near infrared camera (NIRC-2) being built at Caltech, and a near infrared spectrometer (NIRSPEC) being built at UCLA. NASA is planning to fund an interferometer between the Keck telescopes which will require a second NGS AO facility on Keck I.

A prototype adaptive optics system has been installed and tested on the 3 m Shane telescope at Lick Observatory. The adaptive optics system performance, using bright natural guide stars, is consistent with expectations based on theory. A sodium-layer laser guide star system has also been installed and tested on the Shane telescope. Operating at 15 W, the laser system produces a 9th magnitude guide star with seeing-limited size at 589 nm. Using the laser guide star, the adaptive optics system has reduced the wavefront phase variance on scales above 50 cm by a factor of 4. These results represent the first continuous wavefront phase correction using a sodium-layer laser guide star. Assuming tip-tilt is removed using a natural guide star, the measured control loop performance should produce images with a Strehl ratio of 0.4 at 2.2 {mu}m in 1 arc second seeing. Additional calibration procedures must be implemented in order to achieve these results with the prototype Lick adaptive optics system.

Laboratory targets have been imaged by a multi- sub -aperture, coherent receiver technique in which a common local oscillator illuminates the sub -aperture array to preserve both phase and intensityinformation. The target, receiver and range dimensions were chosen such that each sub -aperture was smaller than the speckle size. Various targets were illuminated by microsecond pulses from an e-beam pumped XeF power amplifier, which was seeded by a coherent ultraviolet beam generated with afrequency doubled visible dye laser. Data is presented showing comparisons between the coherent multi- sub -aperture approach and conventional, full aperture photography of the same target(s).INTRODUCTION Maxwell Laboratories, Inc. has been developing coherent ultraviolet technology for both velocity(Refs. 1, 2) and imaging applications. This paper deals with coherent, one dimensional, imaging utilizing a sub -aperture receiver in which the individual receiver apertures were smaller than the speckle