The Roman Space Telescope will have the first advanced coronagraph in space, with deformable mirrors (DMs) for wavefront control (WFC), low-order wavefront sensing and maintenance, and a photon-counting detector. It is expected to be able to detect and characterize mature, giant exoplanets in reflected visible light. Over the past decade, the performance of the coronagraph in its flight environment has been simulated with increasingly detailed diffraction and structural/thermal finite-element modeling. With the instrument now being integrated in preparation for launch within the next few years, the present state of the end-to-end modeling, including the measured flight components such as DMs, is described. The coronagraphic modes, including characteristics most readily derived from modeling, are thoroughly described. The methods for diffraction propagation, WFC, and structural and thermal finite-element modeling are detailed. The techniques and procedures developed for the instrument will serve as a foundation for future coronagraphic missions, such as the Habitable Worlds Observatory.
NASA’s Nancy Grace Roman Space Telescope mission includes a Coronagraph Instrument (CGI) to demonstrate active Wavefront Sensing and Control (WFSC) for future direct imaging and characterization of exoplanets. CGI is in the instrument integration and testing phase and is scheduled to be delivered next year for integration into the Roman observatory. Key flight components, such as Deformable Mirrors (DMs) and detectors, have been recently characterized and integrated into the CGI optical system. A series of system level coronagraph requirement verifications in a vacuum chamber will take place starting later this year. Among them is the static raw contrast with a coronagraph stimulus source. This is the only time CGI will have the opportunity for dark hole digging before In-Orbit Commissioning (IOC). CGI High Order Wavefront Sensing and Control (HOWFSC) modeling has played an important role in assisting many engineering decisions and risk assessments and mitigations throughout the project phases, including when calibration data of key components and their imperfections became available. Here we present some of the latest modeling studies involving special use cases or properties of the DMs and detectors and give our current-best-estimates on static raw contrasts for the upcoming performance verification. Contrast performance for IOC phase WFSC with a typical reference star and its brightness is also provided. All evaluations are performed with the full features of HOWFSC modeling and extensive engineering details. This work is performed at the Jet Propulsion Laboratory / California Institute of Technology under contract to NASA.
The Astro2020 decadal survey recommended the Habitable Worlds Observatory (HWO), NASA’s direct imaging flagship mission, with a goal to achieve a statistically robust mission yield of 25 or more potentially habitable exoplanets. One way to achieve is to increase the instrument effectiveness by introducing additional bright, nearby targets. A majority of Sun-like stars have a stellar companion that can introduce additional noise into the field of view of any high-contrast imaging instrument and enabling exoplanet discovery around binary stars represents a path to increased coronagraphic instrument efficiency by increasing the available science target pool of bright nearby stars. This includes both of the Alpha Centauri A and B stars which would represent the top science target for direct imaging if companion leakage could be suppressed. Multi-Star Wavefront Control (MSWC) is a technique that removes stellar leakage from both stellar components, enabling direct imaging of exoplanets in many binary star systems which can potentially increase coronagraphic instrument effectiveness We present the latest testbed results obtained with MSWC as part of the technology development effort focusing on demonstrations conducted on the Occulting Mask Coronagraph (OMC) testbed at JPL during the vacuum test window last winter, with an additional vacuum test planned for this fall. The MSWC mask consists of a shaped pupil mask similar to the one used for the Wide-Field of View mode, but also includes a set of superimposed, regularly spaced dots that serve as a diffraction grating. OMC has a layout similar to the Roman Space Telescope coronagraph instrument and configured with a binary imaging mode with a MSWC mask using same design as the contributed mask for the Roman coronagraph. Our testbed results represent the first demonstrations of this technique using the recently installed full binary source. We present results demonstrating suppression in the Super-Nyquist regime for the third diffraction order reaching 8.7e-9 contrast with the Roman pupil. In addition, we present results obtained with a physical binary source and running MSWC in a binary star regime demonstrating 9.6e-8 contrast for a geometry matching potential Alpha Centauri observations in a 515 nm monochromatic wavelength (similar but bluer than for Band one) using the fifth diffraction order. Planned demonstrations in the upcoming vacuum window this fall will focus on Band 3d and Band 4 using the full MSWC mode for an Alpha Centauri geometry.
The Astro2020 Decadal Survey calls for a mission yield goal of 25 or more habitable zone planets detection and characterization in its recommendation of next NASA flagship mission, the Habitable World Observatory (HWO). Multi-Star Wavefront Control (MSWC) is a technique that enables simultaneous star light suppression of a binary or more star system. It has the potential to help achieve the goal by substantially increasing viable target samples to beyond single star systems. Technology development for MSWC has been ongoing for a number of years. Recently a better than 1e-7 monochromatic contrast was demonstrated at JPL’s High Contrast Imaging Testbed (HCIT) with a true binary source having similar Alpha Centauri star system separation for the first time. Here we present (High Order) Wavefront Sensing and Control (HOWFSC) modeling analysis of the testbed experiments for improving future performance. Our model is a modified extension of the HOWFSC engineering model that has proven to be a valuable tool for Roman Coronagraph Instrument (CGI) and was validated on the HCIT. It includes crucial engineering features and factors relevant to testbed (while omitting CGI specific elements) such as probing and sensing with detector noise and finite bandwidth used. The analysis provides important insight into and understanding of MSWC testbed experiments and identifies key performance-limiting factors that were not previously considered. Adjustments in both hardware and WFSC strategy and algorithm are discussed for next round testbed experiments to improve performance necessary for both Roman and HWO.
Optical diffraction and wavefront sensing and control (WFSC) models validated against the high-fidelity Roman Space Telescope Coronagraph Instrument (CGI) testbed play a key role in mask design selection and the verification of many requirements that cannot be accomplished until the observatory is in orbit. We have been steadily improving our model fidelity for the as-built CGI testbed system. We demonstrate recently good agreement between measurements and model predictions while validating the Hybrid Lyot Coronagraph’s (HLC) performance using the in-orbit high order wavefront sensing and control (HOWFSC) operational scenario. We present modeling and testbed validation results that explain the reason why many testbed WFSC iterations were needed for HLC in the past. A new, direct application of model-generated initial deformable mirror (DM) voltage pattern has since been successfully demonstrated on the testbed with significant speed and performance improvement. This opens up new model-based initial DM pattern WFSC approaches for CGI. This can greatly reduce flight risk from potentially insufficient ground DM pattern generation due to schedule or cost constraints or from unexpected post-delivery changes. This work was performed at the Jet Propulsion Laboratory, California Institute of Technology under contract to NASA.
High contrast imaging and characterization of faint exoplanets require a coronagraph instrument to efficiently suppress the host star light to 10-9 level contrast over a broad spectral bandwidth. The NASA WFIRST mission plan includes a coronagraph instrument to demonstrate the technology needed to image and characterize exoplanets. Lyot coronagraph masks designed to serve at the focal plane followed by a Lyot stop will be key elements in the WFIRST coronagraph and in future advanced missions such as LUVOIR (Bolcar (2019) and HabEx (Morgan 2019, Martin 2019)). Shaped pupil masks designed to work in reflective geometry are also employed in the WFIRST Coronagraph. High-contrast performance reaching much better than 10-9 contrast requires very tight design, fabrication tolerances, and material properties to meet a wide range of specifications, including precise shapes, micron-scale island features, ultra-low reflectivity regions, uniformity, wavefront quality, etc. In this paper, we present all the critical analytical and measured properties of materials and designs in relation to the results from our coronagraph testbeds.
Occulter mask fabrication for Hybrid Lyot Coronagraph (HLC) at JPL is a relatively mature technology as past successful testbed demonstrations can attest. Nevertheless, as NASA’s WFIRST mission moved into Phase B, new mask design space and fabrication process were explored for new requirements and for better performances for the CoronaGraph Instrument (CGI). To minimize the risks associated with the new explorations, CGI modeling team is tasked with assessing the viability of new designs. In this paper, we describe our HLC modeling effort and results, which identified the potential risks with early exploratory designs and modified fabrication processes. As a result, the traditional (proven) style design is kept for risk aversion. Along the way a standard procedure has been developed for systematic mask evaluation, mask baselining, and general flight performance prediction. In the second part, we describe our model validation effort for the chosen baseline mask’s testbed performance. The focus of the testbed demonstration is to address a major concern related to the CGI’s limited time for wavefront control (WFC) in flight. It includes two stages of WFC: ground seed generation WFC, and (simulated) in-orbit commissioning phase WFC. Good agreements have been achieved in both stages of WFC which affirms that the CGI is capable of digging a dark hole that meets raw contrast requirement within the required time allocation. It also represents a significant improvement in our HLC WFC modeling for an as-built real system.
KEYWORDS: Telescopes, Sun, Satellites, Large Synoptic Survey Telescope, Signal to noise ratio, Device simulation, Space telescopes, Large telescopes, Solar system, Photons
Large or even medium sized asteroids impacting the Earth can cause damage on a global scale. Existing and planned concepts for finding near-Earth objects (NEOs) with diameter of 140 m or larger would take ~15-20 years of observation to find ~90% of them. This includes both ground and space based projects. For smaller NEOs (~50-70 m in diameter), the time scale is many decades. The reason it takes so long to detect these objects is because most of the NEOs have highly elliptical orbits that bring them into the inner solar system once per orbit. If these objects cross the Earth's orbit when the Earth is on the other side of the Sun, they will not be detected by facilities on or around the Erath. A constellation of MicroSats in orbit around the Sun can dramatically reduce the time needed to find 90% of NEOs ~100-140 m in diameter.
A high-accuracy high-fidelity flight wavefront control (WFC) model is developed for detailed WFIRST-CGI raw contrast sensitivity analysis. Built upon features of recently testbed validated model, it is further refined to combine a full Fresnel propagation diffraction model for high accuracy contrast truth evaluation, and an economical compact model for WFC purposes. Extensive individual raw contrast error sensitivities are evaluated systematically, both as known imperfections and as unknown calibration errors, for two CGI modes: spectroscopy mode and wide field-of-view mode with shaped pupil coronagraph. More than 90 distinct error items were identified, including system aberrations, optical misalignment, component fabrication errors, telescope interface related errors, etc. The result forms the basis for raw contrast error budget flow down to a sub-system level, where detailed specifications needed to aid in component design and manufacturing, mechanical alignment and instrument integration, and verification and validation operations. Evaluations are automated, making it relatively easy for repeat runs of revised design or at new desired error quantity. Observations from the comprehensive analysis and top error sensitivities and contrast floor contributors are noted and discussed. Error budget flowdown process is also briefly described.
The Shaped Pupil Coronagraph (SPC) is one of the two operating modes of the WFIRST coronagraph instrument. The SPC provides starlight suppression in a pair of wedge-shaped regions over an 18% bandpass, and is well suited for spectroscopy of known exoplanets. To demonstrate this starlight suppression in the presence of expected onorbit input wavefront disturbances, we have recently built a dynamic testbed at JPL analogous to the WFIRST flight instrument architecture, with both Hybrid Lyot Coronagraph (HLC) and SPC architectures and a Low Order Wavefront Sensing and Control (LOWFS/C) subsystem to apply, sense, and correct dynamic wavefront disturbances. We present our best up-to-date results of the SPC mode demonstration from the testbed, in both static and dynamic conditions, along with model comparisons. HLC results will be reported separately.
KEYWORDS: Performance modeling, Wavefronts, Wavefront sensors, Control systems, Systems modeling, Exoplanets, Monte Carlo methods, Imaging systems, Space telescopes, Stars
NASA’s WFIRST mission includes a coronagraph instrument (CGI) for direct imaging of exoplanets. Significant improvement in CGI model fidelity has been made recently, alongside a testbed high contrast demonstration in a simulated dynamic environment at JPL. We present our modeling method and results of comparisons to testbed’s high order wavefront correction performance for the shaped pupil coronagraph. Agreement between model prediction and testbed result at better than a factor of 2 has been consistently achieved in raw contrast (contrast floor, chromaticity, and convergence), and with that comes good agreement in contrast sensitivity to wavefront perturbations and mask lateral shear.
To maintain the required performance of WFIRST Coronagraph in a realistic space environment, a Low Order Wavefront Sensing and Control (LOWFS/C) subsystem is necessary. The LOWFS/C uses a Zernike wavefront sensor (ZWFS) with the phase shifting disk combined with the starlight rejecting occulting mask. For wavefront error corrections, WFIRST LOWFS/C uses a fast steering mirror (FSM) for line-of-sight (LoS) correction, a focusing mirror for focus drift correction, and one of the two deformable mirrors (DM) for other low order wavefront error (WFE) correction. As a part of technology development and demonstration for WFIRST Coronagraph, a dedicated Occulting Mask Coronagraph (OMC) testbed has been built and commissioned. With its configuration similar to the WFIRST flight coronagraph instrument the OMC testbed consists of two coronagraph modes, Shaped Pupil Coronagraph (SPC) and Hybrid Lyot Coronagraph (HLC), a low order wavefront sensor (LOWFS), and an optical telescope assembly (OTA) simulator which can generate realistic LoS drift and jitter as well as low order wavefront error that would be induced by the WFIRST telescope’s vibration and thermal changes. In this paper, we will introduce the concept of WFIRST LOWFS/C, describe the OMC testbed, and present the testbed results of LOWFS sensor performance. We will also present our recent results from the dynamic coronagraph tests in which we have demonstrated of using LOWFS/C to maintain the coronagraph contrast with the presence of WFIRST-like line-of-sight and low order wavefront disturbances.
End-to-end numerical optical modeling of the WFIRST coronagraph incorporating wavefront sensing and control is used to determine the performance of the coronagraph with realistic errors, including pointing jitter and polarization. We present the performance estimates of the current flight designs as predicted by modeling. We also describe the release of a new version of the PROPER optical propagation library, our primary modeling tool, which is now available for Python and Matlab in addition to IDL.
Current coronagraph instrument design (CGI), as a part of a proposed NASA WFIRST (Wide-Field InfraRed Survey Telescope) mission, allocates two subband filters per full science band in order to contain system complexity and cost. We present our detailed investigation results on the adequacy of such limited number of finite subband filters in achieving full band dark hole contrast with shaped pupil coronagraph. The study is based on diffraction propagation modeling with realistic WFIRST optics, where each subband’s complex field estimation is obtained, using Electric Field Conjugation (EFC) wavefront sensing / control algorithm, from pairwise pupil plane deformable mirror (DM) probing and image plane intensity averaging of the resulting fields of multiple (subband) wavelengths. Multiple subband choices and probing and control strategies are explored, including standard subband probing; mixed wavelength and/or weighted Jacobian matrix; subband probing with intensity subtraction; and extended subband probing with intensity subtraction. Overall, the investigation shows that the achievable contrast with limited number of finite subband EFC probing is about 2~2.5x worse than the designed post-EFC contrast for current SPC design. The result suggests that for future shaped pupil design, slightly larger over intended full bandwidth should be considered if it will be used with limited subbands for probing.
JPL has recently passed an important milestone in its technology development for a proposed NASA WFIRST mission
coronagraph: demonstration of better than 1x10-8 contrast over broad bandwidth (10%) on both shaped pupil
coronagraph (SPC) and hybrid Lyot coronagraph (HLC) testbeds with the WFIRST obscuration pattern. Challenges
remain, however, in the technology readiness for the proposed mission. One is the discrepancies between the achieved
contrasts on the testbeds and their corresponding model predictions. A series of testbed diagnoses and modeling
activities were planned and carried out on the SPC testbed in order to close the gap. A very useful tool we developed
was a derived “measured” testbed wavefront control Jacobian matrix that could be compared with the model-predicted
“control” version that was used to generate the high contrast dark hole region in the image plane. The difference between
these two is an estimate of the error in the control Jacobian. When the control matrix, which includes both amplitude
and phase, was modified to reproduce the error, the simulated performance closely matched the SPC testbed behavior
in both contrast floor and contrast convergence speed. This is a step closer toward model validation for high contrast
coronagraphs. Further Jacobian analysis and modeling provided clues to the possible sources for the mismatch: DM
misregistration and testbed optical wavefront error (WFE) and the deformable mirror (DM) setting for correcting this
WFE. These analyses suggested that a high contrast coronagraph has a tight tolerance in the accuracy of its control
Jacobian. Modifications to both testbed control model as well as prediction model are being implemented, and future
works are discussed.
KEYWORDS: Wavefronts, Infrared telescopes, Space telescopes, Telescopes, Coronagraphy, Point spread functions, Exoplanets, Image analysis, Planets, Signal to noise ratio
For direct imaging and spectral characterization of cold exoplanets in reflected light, the proposed Wide-Field Infrared Survey Telescope (WFIRST) Coronagraph Instrument (CGI) will carry two types of coronagraphs. The High Contrast Imaging Testbed (HCIT) at the Jet Propulsion Laboratory has been testing both coronagraph types and demonstrated their abilities to achieve high contrast. Focal plane wavefront correction is used to estimate and mitigate aberrations. As the most time-consuming part of correction during a space mission, the acquisition of probed images for electric field estimation needs to be as short as possible. We present results from the HCIT of narrowband, low-signal wavefront estimation tests using a shaped pupil Lyot coronagraph (SPLC) designed for the WFIRST CGI. In the low-flux regime, the Kalman filter and iterated extended Kalman filter provide faster correction, better achievable contrast, and more accurate estimates than batch process estimation.
An Inverse Synthetic Aperture LADAR (ISAL) system is capable of providing high resolution surface mapping of near Earth objects which is an ability that has gained significant interest for both exploration and hazard assessment. The use of an ISAL system over these long distances often presents the need to operate the optical system in photon-starved conditions. This leads to a necessity to understand the implications of photon and detector noise in the system. Here a Carrier-to-Noise Ratio is derived which is similar to other optical imaging CNR definitions. The CNR value is compared to the quality of experimentally captured images recovered using the Phase Gradient Autofocus technique both with and without the presence of atmospheric turbulence. A minimum return signal CNR for the PGA to work is observed.
High quality linear laser frequency chirp of high chirp rate is critical to many laser ranging applications. In this paper, we describe a cost-effective chirp linearization approach implemented on our Inverse synthetic Aperture LADAR (ISAL) imaging testbed. Our approach uses a COTS PZT for external cavity laser frequency tuning and a common self-heterodyne fiber interferometer as a frequency monitor, with a two-step hardware and software chirp linearization procedure to achieve high quality chirp. First, the nominal triangle waveform input to PZT drive is modified through an iterative process prior to ISAL imaging acquisition. Several waveforms with chirp rates between 1 and 4THz/s have been acquired with residual chirp rate error ~ +/-2% in usable region. This process generally needs to be done only once for a typical PZT that has excellent repeatability but poor linearity. The modified waveform is then used during ISAL imaging acquisition without active control while the imperfection in transmitted frequency is monitored. The received imaging data is resampled digitally based on frequency error calculated from the frequency monitor data, effectively reduce chirp nonlinearity to ~+/- 0.2% in chirp rate error. The measured system impulse response from return signal shows near designed range resolution of a few mm, demonstrating the effectiveness of this approach.
NASA WFIRST-AFTA mission study includes a coronagraph instrument to find and characterize exoplanets. Various types of masks could be employed to suppress the host starlight to about 10−9 level contrast over a broad spectrum to enable the coronagraph mission objectives. Such masks for high-contrast internal coronagraphic imaging require various fabrication technologies to meet a wide range of specifications, including precise shapes, micron scale island features, ultralow reflectivity regions, uniformity, wave front quality, and achromaticity. We present the approaches employed at JPL to produce pupil plane and image plane coronagraph masks by combining electron beam, deep reactive ion etching, and black silicon technologies with illustrative examples of each, highlighting milestone accomplishments from the High Contrast Imaging Testbed at JPL and from the High Contrast Imaging Lab at Princeton University.
One of the two primary architectures being tested for the WFIRST-AFTA coronagraph instrument is the shaped pupil coronagraph, which uses a binary aperture in a pupil plane to create localized regions of high contrast in a subsequent focal plane. The aperture shapes are determined by optimization, and can be designed to work in the presence of secondary obscurations and spiders - an important consideration for coronagraphy with WFIRST-AFTA. We present the current performance of the shaped pupil testbed, including the results of AFTA Milestone 2, in which ≈ 6 × 10-9 contrast was achieved in three independent runs starting from a neutral setting.
Star light suppression technologies to find and characterize faint exoplanets include internal coronagraph instruments as well as external star shade occulters. Currently, the NASA WFIRST-AFTA mission study includes an internal coronagraph instrument to find and characterize exoplanets. Various types of masks could be employed to suppress the host star light to about 10-9 level contrast over a broad spectrum to enable the coronagraph mission objectives. Such masks for high contrast internal coronagraphic imaging require various fabrication technologies to meet a wide range of specifications, including precise shapes, micron scale island features, ultra-low reflectivity regions, uniformity, wave front quality, achromaticity, etc. We present the approaches employed at JPL to produce pupil plane and image plane coronagraph masks by combining electron beam, deep reactive ion etching, and black silicon technologies with illustrative examples of each, highlighting milestone accomplishments from the High Contrast Imaging Testbed (HCIT) at JPL and from the High Contrast Imaging Lab (HCIL) at Princeton University. We also present briefly the technologies applied to fabricate laboratory scale star shade masks.
The WFIRST/AFTA 2.4 m space telescope currently under study includes a stellar coronagraph for the imaging and spectral characterization of extrasolar planets. Based largely on performance predictions from end-to-end optical propagation modeling, promising coronagraphic methods were selected in late 2013 for further consideration for use on AFTA. Since those downselect analyses further modeling work has been done on evaluating refined coronagraph designs, wavefront sensing and control, detector representation, and time-dependent effects. Thermal, structural, ray trace, and diffraction propagation models are used in these studies. Presented here is the progress to date and plans for future analyses.
NASA’s WFIRST-AFTA mission concept includes the first high-contrast stellar coronagraph in space. This coronagraph will be capable of directly imaging and spectrally characterizing giant exoplanets similar to Neptune and Jupiter, and possibly even super-Earths, around nearby stars. In this paper we present the plan for maturing coronagraph technology to TRL5 in 2014-2016, and the results achieved in the first 6 months of the technology development work. The specific areas that are discussed include coronagraph testbed demonstrations in static and simulated dynamic environment, design and fabrication of occulting masks and apodizers used for starlight suppression, low-order wavefront sensing and control subsystem, deformable mirrors, ultra-low-noise spectrograph detector, and data post-processing.
Recent progress on developing a Grayscale Optical Correlator (GOC) is described. The development efforts have been simultaneously focused on the adoption of a composite correlation filter algorithm and the development and integration of high-resolution, high-speed, miniature GOC hardware system. We have selected the Optimum Trade-off Maximum Average Correlation Height (OT-MACH) filter synthesis algorithm due to its great target recognition performance and its suitability for optical implementation in a real-valued Spatial Light Modulator (SLM). We have, to date, participated in the development of the high
speed (1000 frames/sec) and high resolution (1024 pixel x 1024 pixel), small form factor (5 micron pixel pitch) Ferroelectric Liquid Crystal SLM. We have also developed a portable 512 x 512 GOC system and used it to various ATR applications such as target detection from surveillance data, sonar mine detection, etc. The status of our GOC hardware system and correlation filter synthesis status will be reported. Potential applications and system issues will also be discussed.
In real-world pattern recognition applications, multiple correlation filters can be synthesized to recognize broad variation of object classes, viewing angles, scale changes, and background clutters. Composite filters are used to reduce the number of filters needed for a particular target recognition task. Conventionally, the correlation peak is thresholded to determine if a target is present. Due to the complexity of the objects and the unpredictability of the environment, false positive or false negative identification often occur. In this paper we present the use of a radial basis function neural network (RBFNN) as a post-processor to assist the optical correlator to identify the objects and to reject false alarms. Image plane features near the correlation peaks are extracted and fed to the neural network for analysis. The approach is capable of handling large number of object variations and filter sets. Preliminary experimental results are presented and the performance is analyzed.
JPL is developing an Advanced Autonomous Target Recognition (AATR) technology to significantly reduce broad area search workload for imagery analysts. One of the algorithms to be delivered, as part of
JPL ATR Development and Evaluation (JADE) project, is the OT-MACH based ATR algorithm software package for grayscale optical correlator. In this paper we describe the basic features and functions of the software package as currently implemented. Automation of filter synthesis and test for GOC, particularly
the automation of OT-MACH parameter optimization, is discussed.
JPL has developed a compact portable 512 x 512 Grayscale Optical Correlator [1-4] by integrating a pair of 512 x 512 Ferroelectric Spatial Light Modulator (FLCSLM), a red diode laser, Fourier optics, a CMOS photodetector array. The system is designed to operate at the maximum speed of 1000 frames per second. A FPGA card was custom programmed to perform peak-detection post-processing to accommodate the system throughput rate. Custom mechanical mounting brackets were designed miniaturized the optics head of the GOC into a 6” x 3.5” x 2” volume. The device driver HW/SW is installed in a customized PC. The GOC system’s portability has been demonstrated by shipping it to various locations for target recognition testing.
JPL is developing a high resolution (512 pixel x 512 pixel), high-speed (1000 frames/sec), compact Automatic Target Recognition (ATR) processor for onboard target detection, identification and tracking. This ATR processor consists of a compact Grayscale Optical Correlator (GOC) for parallel wide area target-of-interest (TOI) detection and a hardware based self-learning neural network (NN) for target identification and adaptive monitoring. This processor can be tailored to meet specific system requirements for many ATR applications. Development includes simulation of key components in software including GOC simulation and NN simulation. Both simulation tools are discussed and demonstrated.
JPL and BNS Inc. are jointly developing a compact, low mass, Electro-Optic Imaging Fourier Transform Spectrometer (E-O IFTS) for hyperspectral imaging applications [6]. The spectral region of this spectrometer is in the near IR spectral band of 1 - 2.5 μm (1000 - 4000 cm-1) to allow high-resolution, high-speed hyperspectral imaging applications. The specific applications for NASA’s missions will focus on the measurement of a large number of different atmospheric gases simultaneously in the same airmass. Due to the use of a combination of birefringent phase retarders (YVO4) and multiple achromatic phase switches to achieve phase delay, this spectrometer is capable of hyperspectral measurements similar to that of the conventional Fourier transform spectrometer but without any moving parts. In this paper, the principle of operations, system architecture and recent technical progress will be presented.
JPL is developing a portable 512 x 512 Grayscale Optical Correlator (GOC) system for target data mining and identification applications. This GOC system will utilized a pair of 512 x 512 Ferroelectric Liquid Crystal Spatial Light Modulator (FLCSLM) to achieve 1000 frames/sec data throughput. Primary system design issues including: optics design to achieve compact system volume with fine tuning capability, photodetector array with onboard post-processing for peak detection and target identification. These issues and corresponding solutions will be discussed.
An Optical Processing for the Mining and Identification of Targets (OPMIT) system is being proposed to significantly reduce broad area search workload for NIMA imagery analysts. Central to the system is a Grayscale Optical Correlator (GOC), developed by JPL in recent years. In this paper we discuss some preliminary development of an important system component - the filter management module - that is critical for the success of GOC operation. The emphasis is on the streamlining the OT-MACH filter synthesis/testing procedure for effective and efficient filter design while maintaining filter performance.
JPL and BNS Inc. are jointly developing a compact, low mass, Electro-Optic Imaging Fourier Transform Spectrometer (E-O IFTS) for hyperspectral imaging applications. The spectral region of this spectrometer will be 1 - 2.5 μm (1000 - 4000 cm-1) to allow high-resolution, high-speed hyperspectral imaging applications. The specific applications for NASA's missions will focus on the measurement of a large number of different atmospheric gases simultaneously in the same airmass. Due to the use of a combination of birefringent phase retarders and multiple achromatic phase switches to achieve phase delay, this spectrometer is capable of hyperspectral measurements similar to that of the conventional Fourier transform spectrometer but without any moving parts. In this paper, the principle of operations, system architecture and recent experimental progress will be presented.
Future Mars/planets explorations call for precision and even pinpoint landing. Low cost optical correlator is one of the promising enabling technologies for pinpoint landing. JPL has developed a state-of-the-art miniature optical correlator (MOC) to demonstrate its feasibility. In this paper, we describe a simulation testbed under development for measuring MOC’s performance in a high-fidelity entry, descent, and landing environment, and provide our preliminary simulation result.
JPL has recently developed, for the first time, a compact (2” x 2” x 1”) Grayscale Optical Correlator (GOC) using a pair of 512 x 512 Ferroelectric Liquid Crystal Spatial Light Modulators. In this paper, we will discuss recent progress in the design and packaging technology to achieve a rugged portable GOC module to enable the real-time onboard applications of this miniature GOC. Several automatic target recognition applications will also be presented.
The precision of a radial basis function (RBF) neural network based tracking method has been assessed against real targets. Intensity profile feature extraction was used to build a model in real time, evolving with the target. Precision was assessed against traditionally measured frame-by-frame measurements from the recorded data set. The results show the potential limit for the technique and reveal intricacies associated with empirical data not necessarily observed in simulations.
An innovative compact holographic memory system will be presented. This system utilizes a new electro-optic (E-O) beam steering technology to achieve high-speed, high-density holographic data storage.
Real-time object recognition using a compact grayscale optical correlator will be introduced. A holographic memory module for storing a large bank of optimum correlation filters to accommodate large data throughput rate needed for many real-world applications has also been developed. System architecture of the optical processor and the holographic memory will be presented. Application examples of this object recognition technology will also be demonstrated.
Jet Propulsion Laboratory (JPL) has developed, for the first time, a matchbox-size 512 X 512 grayscale optical correlator (GOC) with the volume of 2 inch X 2 inch X 1 inch. This compact 512 X 512 GOC consists of a pair of newly developed ferroelectric liquid crystal spatial light modulator (FLC SLM) with a 7-micrometers pixel pitch, the smallest feature size developed to date. New system architecture has been designed that has greatly simplified the system alignment and relaxed the tolerance of the Fourier transform lenses. An experimental result of automatic target recognition (ATR) applications using this GOC has been accomplished. The high-quality correlation output has validated the superior quality of the FLC SLM and new GOC architecture.
In this paper, recent technical progress in developing a compact high-speed Grayscale Optical Correlator (GOC) for real-time pattern recognition at the Jet Propulsion Laboratory (JPL) will be presented. This GOC, under partial sponsorship by the Telecommunication and Mission Operation Directorate (TMOD) program at JPL, is being investigated for spacecraft navigation applications. All up-to-date hardware development, soft simulation and experimental demonstration of real-time landmark tracking during a lander descent sequence will be reported.
JPL is developing a high-density, nonvolatile Compact Holographic Data Storage (CHDS) system to enable large- capacity, high-speed, low power consumption, and read/write of data for commercial and space applications. This CHDS system consists of laser diodes, photorefractive crystal, spatial light modulator, photodetector array, and I/O electronic interface. In operation, pages of information would be recorded and retrieved with random access and high- speed. In this paper, recent technology progress in developing this CHDS at JPL will be presented. The recent applications of the CHDS to optical pattern recognition, as a high-density, high transfer rate memory bank will also be discussed.
Jet Propulsion Laboratory has been developing grayscale optical correlator (GOC) for a variety of automatic target recognition (ATR) applications. As reported in previous papers, a 128 X 128 camcorder-sized GOC has been demonstrated for real-time field ATR demos. In this paper, we will report the recent development of a prototype 512 X 512 GOC utilizing a new miniature ferroelectric liquid crystal spatial light modulator with a 7-micrometers pixel pitch. Experimental demonstration of ATR applications using this new GOC will be presented. The potential of developing a matchbox-sized GOC will also be discussed. A new application of synthesizing new complex-valued correlation filters using this real-axis 512 X 512 SLM will also be included.
Jet Propulsion Laboratory has developed a new 512 X 512 high-speed grayscale optical correlator (GOC) for real-time automatic target recognition (ATR) applications. As compared with a previous developed 128 X 128 grayscale optical correlator, the utilization of a pair of high-resolution input spatial light modulator (SLM) has increased the input field of view by 16 times. The use of a matching high- resolution filter SLM has increased the sharpness of the correlation peak. Key features of this GOC include: a grayscale input SLM (Kopin 640 X 480, 8-bit) to accommodate direct interface with the input imaging sensor. A real-valued (bipolar-amplitude) filter SLM (512 X 512, 4-bit) to enable use of a MACH (Maximum Average Correlation Height) composite correlation filter algorithm, compact and portable. This GOC architecture has greatly improve the system complexity by removing the need of preprocessing (binarization) the input, and the powerful MACH composite filter has greatly reduced the number of filter templates. In this paper, the criterion of selection of both input and filter SLM will be discussed. System analysis of building a compact correlator will also be provided. Experimental ATR verification of the 512 X 512 GOC will also be illustrated.
The projection slice filter is modified to include a noise cancellation algorithm for applications to real data with cluttered noise. The wavelet transform has been utilized in the color noise estimation process. The results of the application of these new techniques to the processing of real data with significant clutter components is reported. The techniques used here are part of an ongoing effort to improve the performance of correlation-based systems for fast recognition scenarios.
Current optimal filter projection methods either do not take explicit consideration of the limited dynamic range nature of the currently available SLMs or need complicated search and calculation process (for optimal gain and phase angle). To better utilize the limited dynamic range of the bipolar- amplitude SLM used in our recently developed grayscale optical correlator, we devise a simple and rather practical way to improve filter's dynamic range compression after using minimum Euclidean distance projection.
We have recently demonstrated a compact, high speed, gray- scale optical correlator for target detection. The capability of the direct gray-scale scene input and the gray-scale (real- valued) filter modulation enables us to implement a near- theoretical optimal filter on the optical correlator. This paper describes filter synthesizing algorithm for detecting targets in cluttered background input scene and the projection from the complex filter version to the real version for implementation on the gray-scale optical correlator. It is based on optimal-tradeoff MACH filter. It was found that using an appropriate simulated noise image to substitute the commonly used white noise in the filter design procedure is a very effective way to suppress clutter noise while maintain high tolerance for distortion. Both simulation and experimental results are provided.
Jet Propulsion Laboratory (JPL) has recently developed a camcorder-sized grayscale optical correlator (GOC) for real- time automatic target recognition applications. Key features of this GOC include: a grayscale input SLM to accommodate direct interface with the input imaging sensor, a real-valued (bipolar-amplitude) filter spatial light modulator to enable use of a MACH (Maximum Average Correlation Height) composite correlation filter algorithm, compact and portable. This GOC architecture has greatly improved the system complexity by removing the need of preprocess (binarization) the input, and the powerful MACH composite filter has greatly reduced the number of filter templates. Updating of the GOC system will be described in this paper, a recent real-time field demonstration for target recognition and tracking at Mojave Desert, CA will also be reported.
Volume holographic recording using nonlinear photorefractive crystals is characterized by, among other features, nonlinear beam coupling effect, erasure-recording dynamics, and crystal anisotropy and birefringency. In this paper we first investigate the spectral diffraction properties of a reflective-type volume hologram by considering photorefractive beam coupling and recording-erasure dynamics. We then investigate the spatial diffraction properties of a PR hologram as affected by crystal refractive-index anisotropy. Its effects on the fidelity of the hologram image and on multiplexing scheme are also discussed. Finally, the combined (intrasignal) beam coupling and crystal anisotropy effect are examined for PR LiNbO3 crystal.
Light-induced scattering in a Ce:Fe:LiNbO3 crystal is highly temperature dependent. By considering the effect due to thermally activated ions in a photorefractive crystal, we have shown that the photo-induced space-charge field is neutralized by the activated ions. This neutralization in turn leads to scattering noise reduction in the crystal. By raising the crystal temperature, we have observed a reduction in scattering noise, which is consistent with our prediction. The signal-to-noise ratio (SNR) in a two-wave mixing amplification due to thermal activation effect is analyzed. Experimental demonstrations using a Ce:Fe:LiNbO3 crystal are provided, in which we have shown that the SNR improves as the crystal temperature increases.
We describe a phase-difference prewhitening technique to improve the interclass discrimination capability for the case of one filter per multiobject. Conceptually, this is an extension of the magnitude- hitening operation in Yaroslavsky's optimal filter for the case of one filter per object. By introducing this technique into the filter synthesis procedure, the discrimination ability is increased significantly compared with previous methods. Computer simulation results by means of this technique are given.
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