Fourier Telescopy (FT) is an active imaging method which interferes spatially diverse, frequency-encoded laser beams
on a distant target, and records a time history of the reflected intensity measured by a single photodetector on a large
receiver. FT has been studied extensively for imaging Geostationary objects, using high-energy pulsed lasers to project
triplets of laser beams, by gradually stepping over time through the multitude of u,v-plane baselines required for accurate
object reconstruction. Phase closure among the received triplets plays a key role in canceling out random atmospheric
phase errors between laser beams. A new method has been devised to apply FT to rapidly moving targets, such as LEO
space objects. In order to implement the thousands of baselines in a short engagement time, approximately 20
continuous-wave laser beams are simultaneously broadcast, and the baseline configurations are rapidly changed through
a dynamic optical element. In order to eliminate unknown atmospheric errors, a new type of global phase closure has
been developed, which allows image reconstruction from the time history of measured total reflected intensity,
originating from the complex 20-beam interference patterns. In this paper, we summarize the new FT LEO method, and
give a detailed derivation of the phase closure and image reconstruction algorithms that will lead to ultra-high resolution
images of fast-moving space objects.
Software has been developed for the SAINT program that simulates the operation of a Fourier Telescopy imaging system that could potentially be used to create images of a satellite in low earth orbit. Fourier telescopy uses multiple beams that illuminate the target with a fringe pattern that sweeps across it due to frequency differences between beams. In this way the target spatial frequency components are encoded in the temporal signal that is reflected from the target. The software simulates the propagation effects and target interaction effects that would be present in a real system. This enables the creation of a simulated received signal as a function of time. A particular problem was accurately modeling the appearance of the target as its aspect changes during a rapid transit over the transmitter and receiver. A novel reconstructor has been developed that compensates for atmospheric phase fluctuations affecting the large number of beams transmitted simultaneously (~10). The reconstructor solves for hundreds of image Fourier components simultaneously, permitting rapid reconstruction of the image.
Fourier telescopy (FT) is an active imaging technique that is a candidate for high resolution imaging systems which can be used to obtain satellite images out to geosynchronous target ranges. Fourier telescopy uses multiple beams that illuminate the target with a fringe pattern that sweeps across it due to a set frequency difference between beams. In this way the target spatial frequency components are encoded in the temporal signal that is reflected from the target. The FT receiver can then be composed of a large area "light bucket" collector, since only the integrated temporal signal is necessary to reconstruct the target image. The GEO Light Imaging National Testbed (GLINT) system was previously designed to obtain satellite images at geosynchronous ranges by using this technique. The "light bucket" receiver was designed use forty heliostats, each having a collection area of ten meters square, and composed of a 16 x 16 grid of two foot square mirrors. The heliostats would redirect the return light from the target onto a large spherical concentrator array composed of hexagonal mirror segments. This concentrator would then focus the return light onto a photomultiplier tube (PMT) detector. The FT Field experiment presented in this paper uses one 10-meter square heliostat and a single PMT, plus a scaled down secondary array to provide the optical elements of the receiver for the FT field experiment. In this paper, we will describe the performance characteristics of the heliostat, secondary, and PMT detector. Performance characteristics include optical wavefront, alignment, and alignment stability of the optical elements. Finally, results will be presented after the receiver was integrated with a transmitter system that provided the modulated FT signal from various targets. Image reconstructions will show that even using low quality "Light bucket" receiver optics and a 1.5 km horizontal path through the atmosphere, the modulated signal can still produce good image quality of the targets. Image reconstruction will also be presented for different SNR values in the received signal.
Fourier telescopy (FT) is an active imaging technique that is a good candidate for high resolution imaging systems that can be used to obtain satellite images out to geosynchronous target ranges. Fourier telescopy uses multiple beams that illuminate the target with a fringe pattern that sweeps across it due to frequency differences between beams. In this way the target spatial frequency components are encoded in the temporal signal that is reflected from the target. The FT receiver can then be composed of a large area "light bucket" collector, since only the integrated temporal signal is necessary to reconstruct the target image. The GEO Light Imaging National Testbed (GLINT) system was previously designed to obtain satellite images at geosynchronous ranges by using this technique. Laboratory experiments by several groups have demonstrated the validity of this technique to produce images from simulated targets. In this paper we expand upon these previous experiments to present results from both a FT laboratory and field experimental setup that simulated realistic photon noise, speckle noise, and atmospheric turbulence that will be encountered in an actual FT imaging system. To obtain the scaling for the FT experiment, we have used the GLINT system design parameters for our experimental setup. We will also discuss the phase closure process used to eliminate the random phase differences between the beams from the target spatial frequency measurements and the basic reconstruction algorithm used to produce the target image. Results will also be given that demonstrate the phase closure variance is reduced by averaging a small number of high SNR measurements together, as compared to averaging a larger number of low SNR measurements. Target reconstruction improvements obtained by "unbiasing" the average of the individual low SNR phase closure measurements will also be discussed.
The objective of this project is to develop a liquid-cooled window to transmit a high-energy laser beam. The window is to be used with continuous wave lasers with wavelengths between 1.0-1.4 micrometers and is to be 20 more centimeters in diameter. The window must transmit the beam with only small phase and amplitude distortions. The goal is less than 1/20 wave distortion across the beam at 1.315 micrometers that is the primary wavelength of interest. A prototype window will be built at a later data. In this paper results are presented of research into a) techniques for bonding two pieces of fused silica to from the window and b) suitable coolants.
KEYWORDS: Mirrors, Distortion, Interferometers, Temperature metrology, Optical coatings, Electron beams, Cameras, High power lasers, Glasses, Raster graphics
The thermal distortion test facility (TDTF) at Phillips Laboratory provides precise measurements of the distortion of mirrors that occurs when their surfaces are heated. The TDTF has been used for several years to evaluate mirrors being developed for high-power lasers. The facility has recently undergone some significant upgrades to improve the accuracy with which mirrors can be heated and the resulting distortion measured. The facility and its associated instrumentation are discussed.
The Thermal Distortion Test Facility (TDTF) provides precise measurements of the distortion of laser mirrors which occurs when their surfaces are heated. The TDTF has been used for several years to evaluate mirrors being developed for high power lasers. The facility has recently undergone some significant upgrades to improve the accuracy with which mirrors can be heated and the resulting distortion measured. The facility and its associated instrumentation are discussed.
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