A portable differential image motion sensor (DIMS) has been developed and field demonstrated to measure the
atmospheric coherence diameter, or Fried parameter, r0, both at daytime and at night. The hardware design was
developed using system requirements and performance analysis. A graphical user interface (GUI) and software were
developed to automatically measure r0 from collected imagery data. The DIMS system uses a short wave infrared
(SWIR) camera, IR telescope with custom environmental enclosure, a rack-mount computer accessed remotely through a
laptop, and an equatorial mount and tripod for accurate pointing at a selected star. The system is two-man portable. The
sensor continuously measures r0 from star imagery during clear weather at any time of day or night, with an update rate
of 10 minutes. A continuously nutating optical wedge moves the star image in a circle allowing automatic background
subtraction. Data output is provided at the SWIR 1.6 μm wavelength and scaled to 0.55 μm and pointing at zenith. Valid
r0 measurements range is from 1 cm to 20 cm (in the visible waveband). The r0 measurements over time were performed
at daytime at sea level in San Diego. The largest values of r0 were observed near and after the sunset. This approach
provides a straight-forward path to sea-based seeing measurements with an addition of a stabilized platform.
A laboratory demonstration of two novel tactical beam control methods for correcting the effects of strong turbulence
including Beacon Anisoplanatism, and the combined effects of Beacon Anisoplanatism and Thermal Blooming,
respectively, were performed in SAIC's Tactical Beam Control Test-Bed. Both systems were tested with ratio of
aperture diameter to Fried parameter, D/r0, of up to 7, and ratio of beam spot size at the target to isoplanatic angle, θB/θo,
of up to 10. The first method was implemented in a Wavefront-based Stochastic Parallel Gradient Decent (WSPGD)
adaptive optics (AO) system, which uses an off-axis wavefront sensor (WFS) to provide feedback for a multi-dithering
beam control algorithm. The second method was implemented in a Hybrid WSPGD AO system, which incorporates the
WSPGD AO system with a conventional Phase Conjugate (PC) AO system. The Hybrid system uses an on-axis WFS to
generate initial deformable mirror commands and an off-axis WFS to generate additional commands that account for the
high frequency phase components removed from the wavefront of a laser return by Beacon Anisoplanatism. We
developed a low speed PC-based WSPGD controller, implemented designs of the WSPGD and Hybrid WSPGD AO
systems in SAIC's Test-Bed, and tested both AO systems in static and dynamic turbulence over a wide range of
turbulence conditions. A target-plane tracker was used to stabilize the line-of-sight in the AO corrected beam. Test
results show that the WSPGD AO system efficiently compensates the effects of Beacon Anisoplanatism for both static
and dynamic turbulence, providing a mean performance gain of 1.8 averaged over multiple turbulent realizations. We
also found in testing that the Hybrid WSPGD system efficiently compensates for Beacon Anisoplanatism in the presence
of Thermal Blooming - providing improved compensation for both Thermal Blooming and turbulence. In the presence
of strong Beacon Anisoplanatism with θB/θo of up to 10, the maximum performance gain is 4.9 and the mean
performance gain for multiple turbulence realizations is 2.1.
KEYWORDS: Point spread functions, Turbulence, Stars, Atmospheric propagation, Sensors, Telescopes, Atmospheric optics, Scintillation, Atmospheric sensing, Signal to noise ratio
Turbulence inner scale affects scintillation in laser projection and laser communication systems especially in strong
scintillation regime. Analytical and numerical models are used for performance analysis and design of these systems.
Turbulence inner scale is critically important to anchor theoretical predictions to an experiment. However, the inner scale
is usually not measured in the experiments along extended atmospheric paths. Commercial scintillometer commonly
operates over the range of a few hundreds meters and requires an optical transmitter and receiver at different ends of the
propagation path. We introduced a concept for turbulence inner scale sensor, which is based on phase related
phenomenon and can operate along arbitrary atmospheric paths including the strong scintillation regime both during
daytime and nighttime. We evaluated the feasibility of this approach. We developed an analytical model for a tilt-corrected
point spread function (PSF) of a distant source that enables turbulence inner scale sensor determination from
optical measurements, evaluated the PSF sensitivity to the inner scale variations for ground-to-ground and space-to-ground
engagement scenarios, designed and built a sensor breadboard prototype Finally, for the first time we performed
turbulence inner scale measurements along space-to-ground propagation paths by imaging stars. We found that the
turbulence inner scale on space-to-ground paths is in the range from 1 cm to 3 cm, whereas it is in the range from 0.2 cm
to 1.2 cm near the ground. Thus, initial inner scale measurements by imaging stars revealed that turbulence inner scale
on extended elevated paths exceeds that value near the ground.
GLINT (Geo Light Imaging National Testbed) is a program to image geo-synchronous satellites using Fourier telescopy. The design of the GLINT system requires knowledge of the reflectance properties of the satellites in certain specific wavelength ranges. Calibrated measurements of satellite brightness due to solar illumination can be made with a telescope. This report details such measurements and the data processing necessary to yield curves of normalized satellite return versus phase angle in given wavelength ranges. These measurements can be used to check the accuracy of satellite reflectivity models.
KEYWORDS: Wavefronts, National Ignition Facility, Control systems, Sensors, Actuators, Deformable mirrors, Mirrors, Wavefront sensors, Control systems design, Near field optics
A wavefront control system will be employed on NIF to correct beam aberrations that otherwise would limit the minimum target focal spot size. For most applications, NIF requires a focal spot that is a few times the diffraction limit. Sources of aberrations that must be corrected include prompt pump-induced distortions in the laser slabs, thermal distortions in the laser slabs from previous shots, manufacturing figure errors in the optics, beam off-axis effects, gas density variations, and gravity, mounting, and coating-induced optic distortions.
The Multiple Mirror Telescope (MMT) is now being replaced by a single 6.5m telescope which will have an integral adaptive optics system optimized for near IR operation. We illustrate key results obtained with low-order adaptive optics at the MMT and report on progress on the major components of the system for the new telescope. We also give a brief update on the status of the telescope itself. First light for the adaptive system is expected in mid 1999.
We report the latest progress on the design, fabrication and testing of the adaptive secondary mirror to be used in the adaptive optics system to for the 6.5m upgrade to the Steward Observatory's MMT. The adaptive secondary will use electromagnetic force actuators is conjunction with a rigid reference structure to deform a thin and flexible glass facesheet. The facesheet is fabricated with figure accuracy comparable to the surface of a traditional static secondary mirror. The flexible facesheet can however, be deformed by the actuators to conjugate the changing atmospheric aberration. Capacitive position sensor are placed at each actuators and are used to rapidly measure the position of the glass facesheet relative to the rigid reference structure. These measurements are used as feedback in a servo control-loop which maintains the desired figure of the adaptive secondary facesheet. In the proposed design the mechanical interface between the facesheet and the reference structure is limited to a small hub in the center of the facesheet. Due to heat dissipation in the electromagnetic voice-coils a temperature control system is required to maintain the facesheet of the adaptive secondary near the ambient temperature of the atmosphere. We report on laboratory test of a nearly full size 60 actuator adaptive secondary prototype. We include test of actuator stroke and position accuracy, control-loop stability, and closed-loop bandwidth.
We report the latest progress on the design, fabrication and testing of the adaptive secondary mirror to be used in the adaptive optics system to for the 6.5m upgrade to the Steward Observatory's MMT. The adaptive secondary will use electromagnetic force actuators in conjunction with a rigid reference structure to deformed a thin and flexible glass facesheet. The facesheet is fabricate with figure accuracy comparable to the surface of a traditional static secondary mirror. The flexible facesheet can however, be deformed by the actuators to conjugate the changing atmospheric aberration. Capacitive position sensors are placed at each actuator and are used to rapidly measure the position of the glass facesheet relative to the rigid reference structure. These measurements are used as feedback in a servo control- loop which maintains the desired figure of the adaptive secondary facesheet. In the proposed design the mechanical interface between the facesheet and the reference structure is limited to a small hub in the center of the facesheet. Due to heat dissipation in the electromagnetic voice-coils a temperature control system is required to maintain the facesheet of the adaptive secondary near the ambient temperature of the atmosphere. We report on laboratory test of a nearly full size 60 actuator adaptive secondary prototype. We include test of actuator stroke and position accuracy, control-loop stability, and closed-loop bandwidth.
The Multiple Mirror Telescope on Mt. Hopkins will soon be upgraded to a single 6.5 m primary mirror.An adaptive- optical system, featuring a thin-shell, adaptive-secondary mirror with 330 voice-coil actuators is being developed for this new telescope. The thin-shell mirror is supported by a thick, concave aluminum substrate which also holds the actuator control and monitoring electronics and serves as the reference surface. With the actuator electronics dissipating heat into the substrate, the thermal behavior of the aluminum reference plate becomes as important issue. This paper presents results form tow experiments designed to determine the thermal behavior of the reference plate.
The upgraded 6.5 m MMT in Arizona will use an adaptive secondary to optimize performance in the near infrared spectral region. The secondary mirror is a 2 mm thick, 640 mm diameter Zerodur shell suspended only by a flexible center hub. Three hundred voice coil actuators installed in an aluminum reference surface deform the shell according to commands from a wavefront sensor. Capacitor position sensors surrounding each actuator provide feedback in an inner servo loop, much faster than the exterior wavefront sensor control bandwidth. A 60 actuator prototype, nearly identical to the final adaptive secondary size, has been built and is currently being tested.
ThermoTrex Corporation has designed and built a prototype of the fast steering mirror to be used for image motion control in the TNG adaptive optics system. The principal characteristic of this mirror is the use of voice coil actuators whose positions are controlled with closed loops based on capacitive sensors. Here we report the main features of the mirror assembly and laboratory measurements done to characterize the mirror behavior. The Bode diagram of the mirror is reported and discussed.
The new 6.5 m single mirror multiple mirror telescope (MMT) will be equipped with adaptive optics capabilities to enhance high resolution infrared astronomy. Before we build the 64 cm diameter adaptive secondary, we fabricated a smaller prototype mirror. The adaptive secondary uses voice coil force actuators with an average spacing of 30 mm. Surrounding each actuator is an analog capacitor position sensor operating in a digital closed loop at 10 kHz. This allows the force actuators to be controlled as if they were position actuators. The adaptive secondary configuration and performance test results are presented, followed by the changes to be incorporated into the next curved shell prototype.
An unusual dual-aperture 28.5-inch, f/21 Ritchey-Chretien telescope has been completed and will be installed in the recently upgraded University of Denver extreme high altitude observatory facility, atop 14,268 ft. Mount Evans in Colorado. Designed to optimize high spatial resolution imaging, the Meyer binocular telescope incorporates active thermal management of the telescope structure. The secondary mirror support elements are fabricated from INVAR and permit active tip-tilt and focusing capability. The optics were fabricated from Zerodur by Contraves USA, and each system has a measured total wavefront error less than 0.050 lambda at 633 nm. All optical surfaces are coated with a multi- layer dielectric enhanced silver, providing high reflectance from below 350 nm to beyond 26 micrometer. The telescope control system has been designed to allow initial operation from an insulated control room. Long-term plans call for totally remote operation from the University of Denver campus via direct microwave radio link. Instrumentation planned for the telescope at first light includes: (1) a low order 400 nm to 1,000 nm band adaptive optics system (AO5: adaptive optics, 5 mode) equipped with a large format CCD camera; (2) a mid-infrared array camera (TNTCAM: ten and twenty micron camera); and (3) a mid-IR moderate dispersion spectrometer (TGIRS: two grating IR spectrometer). Some of the science problems the dual aperture telescope is uniquely situated to tackle include the study of planetary atmosphere, detection of planetary systems around nearby stars and the analysis of evolutionary changes in stars. The Mount Evans site (at 4,303 meters elevation, the highest operating astronomical facility in the world) is located 70 km west of Denver and can be reached via a paved state highway which extends all the way to the summit. The observatory is currently under construction with installation of the telescope planned for late summer 1996.
A new adaptive optics system has been constructed for moderately high resolution in the near infrared at the Multiple Mirror Telescope (MMT). The system, called FASTTRAC II, has been designed to combine the highest throughput with the lowest possible background emission by making the adaptive optical element be an existing and necessary part of the telescope, and by eliminating all warm surfaces between the telescope and the science camera's dewar. At present, only natural guide stars are supported, but by the end of 1995, we will add the capability to use a single sodium resonance beacon derived from a laser beam projected nearly coaxially with the telescope. In this paper, we present a description of FASTTRAC II, and show results from its first test run at the telescope in April 1995.
We present an overview of the new adaptive system under development for the conversion of the Multiple Mirror Telescope (MMT) to a 6.5 m continuous primary mirror. The system is optimized for diffraction-limited imaging from 1.6 to 2.2 micrometer wavelength, using an adaptive secondary mirror which directly feeds an infrared science detector at f/15 Cassegrain focus. Nearly full sky coverage will be obtained using a low-power, continuous wave (cw) sodium laser beacon to sense high-order wavefront errors, with image motion sensing using a quadrant detector sensitive to infrared field star photons in the 1.2 - 1.6 micrometer band. Components are currently under development, so that the adaptive instrument can be integrated with the new 6.5 m telescope soon after first light.
In 1996, the Multiple Mirror Telescope will be replaced with a 6.5 m single primary mirror. Development is currently underway on a sodium laser guide star adaptive optical system for the new telescope. One unique feature will be an adaptive secondary mirror, consisting of 320 individually controlled voice coil actuators on the back side of a thin, 64 cm diameter mirror. This paper describes initial tests on a 15 cm diameter, thin, flat prototype mirror with a single actuator. The thin mirror is held near a thick substrate which also serves as an immovable reference surface. A novel voice coil actuator connects the two glass parts. A custom capacitance sensor surrounding the voice coil actuator measures the absolute distance between the mirror back side and the reference surface. This prototype provides detailed performance measurements, including temporal and spatial actuator response functions. Assembly, alignment, and calibration techniques for the 64 cm mirror will be debugged. The data will help optimize the design and performance of the adaptive secondary.
We present a novel, high performance, and economical design for tip-tilt mirrors. The two- dimensional tilt of each mirror is sensed through capacitive displacement sensors sensitive to approximately 1 nm rms out to 10 KHz. An analogue PID circuit utilizes this positional feedback to lock the mirrors to the commanded tilt via voice coil drivers. These mirrors achieve a 10 - 90% risetime of 3.0 ms and have a critically damped response at 100 - 150 Hz update rates. We have incorporated six of these tip-tilt mirrors to adaptively combine all six beams from the MMT. During first light of the instrument in April 1995, individual beams improved from 1.1 inch to 0.6 inch FWHM in 60 s exposures corrected with 60 Hz update rates.
An adaptive optics system for small to medium astronomical telescopes has been designed and is under construction. This adaptive optics system corrects the five lowest order Zernike wavefront aberrations, providing near diffraction-limited performance for telescope diameters smaller than about 5*ro, and useful correction up to about 10*ro. This adaptive optics system design consists of a lens-based wavefront aberrator, a CCD-based Shack-Hartmann wavefront sensor, and a personal computer-based feedback loop.
Access to the requested content is limited to institutions that have purchased or subscribe to SPIE eBooks.
You are receiving this notice because your organization may not have SPIE eBooks access.*
*Shibboleth/Open Athens users─please
sign in
to access your institution's subscriptions.
To obtain this item, you may purchase the complete book in print or electronic format on
SPIE.org.
INSTITUTIONAL Select your institution to access the SPIE Digital Library.
PERSONAL Sign in with your SPIE account to access your personal subscriptions or to use specific features such as save to my library, sign up for alerts, save searches, etc.