Analyses show that astronomical occultation methods may be used to determine the silhouettes of satellites at geostationary distances, a result few other techniques can achieve. Specifically, an array of photon-counting detectors is positioned in the path of the target shadow from one star. Reduction of the received star intensity vs. time can yield silhouette resolution of less than a meter. In this paper, we address the critical issues of a) the limited density of useable stars, b) positioning of the detector array into the path of the shadow, and c) undoing the effects of diffraction. A conceptual design for an imaging station is presented.
The results of an investigation into beam shaping techniques for generating near field Gaussian intensity patterns from uniform intensity ("flat top") laser beams are presented. The motivation for this study was the desire to produce realistic High Energy Laser (HEL) far field intensity profiles for laser effects testing, without propagating the large distances necessary to obtain the true far field pattern and beam size typical of HEL target engagement scenarios. To minimize cost, maximize wavelength diversity, and provide a high laser damage threshold capability, an all reflective optical system was preferred.
Though beam shaping systems are commonly used to convert Gaussian beams to flat tops beams, the reverse problem, that of converting flat tops to Gaussians, appears to be new territory. Most beam shaping approaches, particularly those that do not preserve phase, are not reversible. Two simple approaches that use segmented mirrors for converting flat tops to Gaussians are described here. While beam integrators, commonly used to convert Gaussians to flat tops do not work in reverse, the approaches presented use segmented mirrors resembling beam integrators, and have some similar benefits.
Geometric and physical optics analyses are presented to illustrate the performance characteristics of the different approaches at wavelengths of 1.315 and 3.8 microns. A simple method to reduce interference effects in the reshaped beam, that are present when a coherent source is used, are discussed.
The use of a "Field Mapping" beam shaping technique for generating near field Gaussian intensity patterns from uniform intensity ("flat top") laser beams is described. The design objective was to simulate realistic High Energy Laser (HEL) far field intensity patterns for laser effects testing purposes, without having to propagate the large distances necessary to obtain the true far field intensity profile and beam size typical of realistic target engagement scenarios.
The field mapping approach presented uses a continuous surface mirror with a figure designed to redistribute the energy into a Gaussian distribution at the target plane. The use of a reflective system was desired to minimize cost and maximize wavelength diversity and laser damage threshold capability. Physical optics analyses are presented to illustrate the performance characteristics of a totally passive reflective field mapping beam shaper.
Fourier telescopy offers the capability to obtain images of geosynchronous satellites by trading the need for a high power laser and a very large high optical quality receiver for a very large collecting aperture of lower optical quality. The GLINT Program is managed by the US Air Force Research Laboratory and is funded by a congressional add and completion requires continued support. The proposed collector consists of 40 heliostats, each 10m2. The optical quality of the heliostats is not a major issue as the images are obtained by demodulating a received time-series signal. Even with a 4,000m2 collector the energy requirements dictate that as many as 200 pulses must be averaged for each triple product to be obtained. With a laser operating at several Hertz, the collection of data for a single triple product will take minutes and the collection of the full set of triplets for a modest system, will take several hours.
This paper studies strategies for dealing with dynamic solar panels. During an engagement, the body of the satellite will remain fixed relative to the ground site; however the solar panels will turn to point at the sun. Data collected for a full night will be corrupted. One approach is to take data for a short period over many nights at the same solar time. Examples are presented of image quality versus length of time of data collection. The analysis makes uses of the Air Force Research Laboratory’s Time-Domain Analysis and Simulation for Active Tracking (TASAT) code. The amount of time that data may be collected on a given night is compared to the quality of the image recovered. A successful laboratory demonstration of Fourier telescopy is also described.
Many laser imaging applications produce as outputs the phase differences between adjacent points in the digital 2-D image spatial frequency domain. A wavefront reconstruction algorithm must then be used to convert phase difference arrays to a spatial frequency global phase array. The spatial frequency domain for most applications (for example, Sheared Beam Imaging) is contained in a regular square grid. For other applications such as Fourier Telescopy, the spatial frequency domain grid points depend upon the placement of the laser illuminators. Additionally, off-axis viewing angles introduce a skew into the u-v sample space, so we need to be able to reconstruct wavefronts on non-square grid arrays. In this work we will demonstrate use of standard square grid reconstructors to reconstruct non-square grid arrays. Additionally, we compare the relative accuracy between a complex exponential wavefront reconstruction algorithm and a modified least- squares wavefront reconstruction algorithm in recovering the global phase from regular square and non-square grid arrays.
KEYWORDS: Satellites, Motion measurement, Satellite imaging, 3D modeling, Signal to noise ratio, Data modeling, Motion models, Transmitters, Fourier transforms, Switches
GLINT is a program to image geosynchronous satellites using Fourier telescopy. The standard method of creating an image takes some time requiring the satellite to be stationary for an hour or more. Important information about the satellite's motion and orientation can be obtained by measuring a small subset of the u-v sample space. These measurements can be taken relatively quickly and can be used even if the object is moving. These motion estimates can be useful in themselves -- for instance as an aid to regaining control of the satellite. They can also be used as inputs to alternate imaging schemes that map out the u-v space synchronously with the rotating satellite.
Fourier telescopy is an imaging technique in which the Fourier spectrum of an object is built up by sweeping fringe patterns of varying spatial frequency and orientation over the object. The modulated scattered radiation that results is collected by an nonimaging detector. We have performed a laboratory demonstration of Fourier telescopy in order to confirm the validity of the fundamental measurement concept and the image reconstruction method. We show experimentally obtained images and compare them to simulated images. On- going experiments will characterize the consequences of less-than-ideal measurement conditions, such as fringe- spacing errors and less-than-unity fringe modulation. Our ultimate application is the imaging of geosynchronous satellites.
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