The MSTAR sensor (Modulation Sideband Technology for Absolute Ranging) is a new system for measuring absolute distance, capable of resolving the integer cycle ambiguity of standard interferometers, and making it possible to measure distance with subnanometer accuracy. The sensor uses a single laser in conjunction with fast phase modulators and low frequency detectors. We describe the design of the system - the principle of operation, the metrology source, beam-launching optics, and signal processing - and show results for target distances up to 1 meter. We then demonstrate how the system can be scaled to kilometer-scale distances and used for space-based applications.
Deep, stable starlight suppression is needed for the direct interferometric detection of Earth-like planets and
requires careful control of the intensity and phase of the beams that are being combined. We have
developed a novel compensator for the Terrestrial Planet Finder Interferometer based on a deformable
mirror to correct the intensity and phase at each wavelength across the bandwidth of 8 to 12 microns
wavelength. This paper will discuss the results of using the adaptive nuller to achieve deep broadband
nulling in the mid-IR.
KEYWORDS: Mirrors, Simulation of CCA and DLA aggregates, Cameras, Camera shutters, Optical alignment, Staring arrays, Interferometry, Metrology, Mechanical engineering, Off axis mirrors
The Astrometric Beam Combiner (ABC) is a critical element of the Space Interferometry Mission (SIM) that
performs three key functions: coherently combine starlight from two siderostats; individually detect starlight for
angle tracking; and disperse and detect the interferometric fringes. In addition, the ABC contains: a stimulus,
cornercubes and shutters for in-orbit calibration; several tip/tilt mirror mechanisms for in-orbit alignment; and
internal metrology beam launcher for pathlength monitoring. The detailed design of the brassboard ABC (which
has the form, fit and function of the flight unit) is complete, procurement of long-lead items is underway, and
assembly and testing is expected to be completed in Spring 2009. In this paper, we present the key requirements
for the ABC, details of the completed optical and mechanical design as well as plans for assembly and alignment.
We present an overview of the ongoing progress towards flight readiness of the SIM project. We summarize the
engineering milestones that have been completed in the last two years, namely: the Brass-Board Internal and
External Metrology Beam Launchers, the Brass-Board Metrology Source, and the Instrument Communication
Hardware/Software Architecture Demonstration. We also show other progress such as: the life test of the bass-screw
and PZT actuators, building the Metrology Fiducials and the Single Strut Test Article. We status the
ongoing work on the Brass-Board Fast Steering Mirror and the Brass-Board Astrometric Beam Combiner. We
end with a proposed path towards finishing the Brass-Board suite.
Deep, stable starlight nulls are needed for the direct detection of Earth-like planets and require careful
control of the intensity and phase of the beams that are being combined. We have tested a novel
compensator based on a deformable mirror to correct the intensity and phase at each wavelength across the
bandwidth of 8 to 12 microns wavelength. This paper will cover the results of the adaptive nuller tests
performed in the mid-IR.
Deep, stable starlight nulls are needed for the direct detection of Earth-like planets and require careful control of the intensity and phases of the beams that are being combined. We are testing a novel compensator based on a deformable mirror to correct the intensity and phase at each wavelength and polarization across the nulling bandwidth. We have successfully demonstrated intensity and phase control using a deformable mirror across a 100nm wide band in the near-IR, and are in the process of conducting experiments in the mid-IR wavelengths. This paper covers the current results and in the mid-IR.
Deep, stable starlight nulls are needed for the direct detection of Earth-like planets and require careful control of the intensity and phases of the beams that are being combined. We are testing a novel compensator based on a deformable mirror to correct the intensity and phase at each wavelength and polarization across the nulling bandwidth. We have successfully demonstrated intensity and phase control using a deformable mirror across a 100nm wide band in the near-IR, and are in the process of building the phase 2 experiment operating at mid-IR wavelengths. This paper covers the results of our demonstration in the near-IR, as well as our current progress in the mid-IR.
Deep, stable nulling of starlight requires careful control of the amplitudes and phases of the beams that are being combined. The detection of earth-like planets using the interferometer architectures currently being considered require that the electric field amplitudes are balanced at the level of ~ 0.1% and the phases are controlled at the level of 1 mrad (corresponding to ~ 1.5 nm for a wavelength of 10 microns). These conditions must be met simultaneously at all wavelengths across the science band and for both polarization states, imposing unrealistic tolerances on the symmetry between the optical beamtrains. Lay et. al. proposed the concept of a compensator that is inserted into the beamtrain, which can adaptively correct for the mismatches across the spectrum enabling deep nulls with realistic, imperfect optics. This proposed design uses a deformable mirror to adjust the amplitude and phase of the electric field that couples into the single-mode spatial filter. We have demonstrated amplitude and phase control at a single wavelength in the near-IR. We are preparing to demonstrate control with our deformable mirror actuator in the near-IR and in parallel are preparing a demonstration in the mid-IR where the compensator will be required to operate.
Absolute metrology measures the actual distance between two optical fiducials. A number of methods have been employed, including pulsed time-of-flight, intensity-modulated optical beam, and two-color interferometry. The rms accuracy is currently limited to ~5 microns. Resolving the integer number of wavelengths requires a 1-sigma range accuracy of ~0.1 microns. Closing this gap has a large pay-off: the range (length measurement) accuracy can be increased substantially using the unambiguous optical phase.
The MSTAR sensor (Modulation Sideband Technology for Absolute Ranging) is a new system for measuring absolute distance, capable of resolving the integer cycle ambiguity of standard interferometers, and making it possible to measure distance with sub-nanometer accuracy. In this paper, we present recent experiments that use dispersed white light interferometry to independently validate the zero-point of the system. We also describe progress towards reducing the size of optics, and stabilizing the laser wavelength for operation over larger target ranges.
MSTAR is a general-purpose tool for conveniently measuring length with much greater accuracy than was previously possible, and has a wide range of possible applications.
Deep, stable nulling of starlight requires careful control of the amplitudes and phases of the beams that are being combined. The detection of earth-like planets using the interferometer architectures currently being considered for the Terrestrial Planet Finder mission require that the E-field amplitudes are balanced at the level of ~ 0.1%, and the phases are controlled at the level of 1 mrad (corresponding to ~ 1.5 nm for a wavelength of 10 μm). These conditions must be met simultaneously at all wavelengths across the science band, and for both polarization states, imposing unrealistic
tolerances on the symmetry between the optical beamtrains. We introduce the concept of a compensator that is inserted into the beamtrain, which can adaptively correct for the mismatches across the spectrum, enabling deep nulls with realistic, imperfect optics. The design presented uses a deformable mirror to adjust the amplitude and phase of each beam as an arbitrary function of wavelength and polarization. A proof-of-concept experiment will be conducted at visible / near-IR wavelengths, followed by a system operating in the Mid-IR band.
We report on the laboratory demonstration of an active linear metrology scheme using two separate lasers. In `active' metrology, the passive retroreflector in one arm of a typical heterodyne interferometer is replaced with an active optical transponder. The Transponder can dramatically boost the returned signal strength, thereby providing a way to perform metrology and pathlength control over long (> km) distances. Two Lightwave Electronics non-planar ring oscillator lasers at a wavelength of 1.319 micrometers were used as the Source and Transponder. The frequency of the Transponder is offset locked to the signal received from the Source using the Lightwave Laser Offset Locking Accessory, and the Transponder beam is sent back to the Source. The phases of the beat signals are measured locally at the Source and Transponder by appropriately demodulating the signal, and post-processed to determine displacement. In initial experiments, the standard deviation of the measurement errors was less than three nanometers.
We present a preliminary design for a tracking and pointing subsystem for the optical communication link between the International Space Station and a ground receiver at Table Mountain Facility. The link is intended to demonstrate high rate downlink capability of rates up to 2.5 Gbps. The design objective of tracking and pointing subsystem is to limit the pointing loss to within 4 dB to ensure the maximum downlink capability with 3 dB link margin. We will show the underlying tracking and pointing subsystem design and present analysis that shows the allocated error budget can be met.
A high data rate laser transmitter assembly (LTA) has been designed as the source for an optical free-space communication link between the International Space Station and the 1-meter Optical Communication Telescope Laboratory (OCTL) to be built at the Table Mountain Facility (TMF, Wrightwood, CA). the transmitter design concept uses a fiber-based master oscillator power amplifier (MOPA) configuration with an average output power of 200 mW at a 1550 nm transmit wavelength. This transmitter source is also designed to provide a signal at 980 nm to the silicon-based focal plane array for the point-ahead beam control function. This novel integration of a 980 nm boresight signal allows the use of silicon based imagers for the acquisition/tracking and point- ahead functions, yet permits the transmit signal to be at any wavelength outside the silicon sensitivity. The LTA, a sub- system of the Flight Terminal, has been designed to have a selectable data rate from 155 - 2500 Mbps in discrete steps. It also incorporates a 2.5 Gbps pseudo-random bit sequence (PRBS) generator for complete link testing and diagnostics. The design emphasizes using commercial off the shelf components (COTS).
This paper presents an overview of the preliminary design of both the flight and ground systems of the Optical Communication Demonstration and High-rate Link Facility which will demonstrate optical communication from the International Space Station to ground after its deployment in October 2002. The overview of the preliminary design of the Flight System proceeds by contrasting it with the design of the laboratory- model unit, emphasizing key changes and the rationale behind the design choices. After presenting the preliminary design of the Ground System, the timetable for the construction and deployment of the flight and ground systems is outlined.
The Atmospheric Visibility Monitoring (AVM) project gathers data on the transmission of light through the atmosphere. These data are measured and collected at autonomous observatories using stellar photometric techniques. The information gathered is used to build statistical models that assess the quality of future space-to-ground optical communication links. The first of the three currently running AVM observatories became operational in 1994. Jet Propulsion Laboratory (JPL) is upgrading all three observatories. The upgrade includes new Charge Coupled Device (CCD) imagers, Windows NT-based computers and new control software. The new CCDs improve the following: near IR performance, daylight photometry, pixel field-of-view, intensity resolution and signal-to-noise ratios. Employing these new CCDs requires upgrading the CPU, operating system and control software. Together these changes improve the quality of future data obtained and processed by the AVM system.
Mountain-top to mountain-top optical link experiments have been initiated at JPL, in order to perform a systems level evaluation of optical communications. Progress made so far is reported. The NASA, JPL developed optical communications demonstrator (OCD) is used to transmit a laser signal from Strawberry Peak (SP), located in the San Bernadino mountains of California. This laser beam is received by a 0.6 m aperture telescope at JPL's Table Mountain Facility (TMF), located in Wrightwood, California. The optical link is bi-directional with the TMF telescope transmitting a continuous 4-wave (cw) 780 nm beacon and the OCD sending back an 840 nm, 100 - 500 Mbps pseudo noise (PN) modulated, laser beam. The optical link path is at an average altitude of 2 Km above sea level, covers a range of 46.8 Km and provides an atmospheric channel equivalent to approximately 4 air masses. Average received power measured at either end fall well within the uncertainties predicted by link analysis. The reduction in normalized intensity variance ((sigma) I2) for the 4- beam beacon, compared to each individual beam, at SP, was from approximately 0.68 to 0.22. With some allowance for intra-beam mis-alignment, this is consistent with incoherent averaging. The (sigma) I2 measured at TMF approximately 0.43 plus or minus 0.22 exceeded the expected aperture averaged value of less than 0.1, probably because of beam wander. The focused spot sizes of approximately 162 plus or minus 6 micrometer at the TMF Coude and approximately 64 plus or minus 3 micrometer on the OCD compare to the predicted size range of 52 - 172 micrometer and 57 - 93 micrometer, respectively. This is consistent with 4 - 5 arcsec of atmospheric 'seeing.' The preliminary evaluation of OCD's fine tracking indicates that the uncompensated tracking error is approximately 3.3 (mu) rad compared to approximately 1.7 (mu) rad observed in the laboratory. Fine tracking performance was intermittent, primarily due to beacon fades on the OCD tracking sensor. The best bit error rates observed while tracking worked were 1E - 5 to 1E - 6.
The Optical Communications Demonstrator (OCD) is a laboratory based lasercom terminal that was developed to validate several key technologies such as precision beam pointing, high bandwidth beacon tracking and beacon acquisition. The unique architecture of OCD uses a single focal plane array (FPA) and a single fine steering mirror (FSM) for beacon acquisition, beacon tracking and point-ahead compensation. A fiber-coupled laser transmitter further reduces the complexity of the terminal. Over the last year, system level integration, test and characterization of the terminal were conducted. Here we present results from the integration and test (I&T) of the terminal with the Lasercom Terminal Evaluation Station (LTES), with particular emphasis on the fine tracking performance. Furthermore, we will describe lessons learnt from the implementation and testing of OCD that are relevant to the design of future flight optical communication terminals. The completed OCD is now being used in a series of ground-ground experiments to understand atmospheric effects and to gain experience operating the OCD.
The Optical Communications Demonstrator (OCD), under development at the Jet Propulsion Laboratory (JPL), is a laboratory-based lasercomm terminal designed to validate several key technologies, primarily precision beam pointing, high bandwidth tracking, and beacon acquisition. The novelty of the instrument is that it uses a single CCD array detector for both beacon acquisition and tracking, and a fiber-coupled laser transmitter. The resulting reduction in design complexity can lead to a reduced system cost and an improved system reliability. In this paper, we describe recent progress on the development of the OCD terminal, particularly the electronics packaging and optical characterization with the Lasercom Test and Evaluation Station (LTES).
The Free-space Optical Communication Analysis Software (FOCAS) was developed at the Jet Propulsion Laboratory (JPL) to provide mission planners, systems engineers and communications engineers with an easy to use tool to analyze direct-detection optical communication links. The FOCAS program, implemented in Microsoft Excel, gives it all the power and flexibility built into the spreadsheet. An easy-to-use interface, developed using Visual Basic for Applications (VBA), to the spreadsheet allows easy input of data and parameters. A host of pre- defined components allow an analyst to configure a link without having to know the details of the components. FOCAS replaces the over-a-decade-old FORTRAN program called OPTI widely used previously at JPL. This paper describes the features and capabilities of the Excel-spreadsheet-based FOCAS program.
The Atmospheric Visibility Monitoring (AVM) program at the Jet Propulsion Laboratory has been in place for the last few years to obtain atmospheric transmission statistics data to support free-space optical communications experiments and missions. Atmospheric transmission data is collected through a set of three autonomous systems, all located in the south-western U.S., that observe selected stars throughout the year. Data from these three sites are collected and processed on a regular basis to obtain cumulative distribution functions of atmospheric attenuation for different spectral windows of interest. In This paper, we describe recent work on creation of a database using Microsoft Access to analyze atmospheric transmission data collected by the AVM project. The database, which replaces time-consuming Matlab programs, offers a rapid and extremely easy way to extract and analyze AVM data.
Analyses of uplink and downlink data from recent free-space optical communications experiments carried out between Table Mountain Facility and the Japanese ETS-VI satellite are presented. Fluctuations in signal power collected by the satellite's laser communication experiment due to atmospheric scintillation and its amelioration using multiple uplink beams are analyzed and compared to experimental data. Downlink data was analyzed to determine the cause of a larger than expected variation in signal strength. In spite of the difficulty in deconvolving atmospheric effects from pointing errors and spacecraft vibration, experimental data clearly indicate significant improvement in signal reception on the uplink with multiple beams, and the need for stable pointing to establish high data rate optical communications.
The objective of the Atmospheric VIsibility Monitoring (AVM) program at the JPL is to obtain atmospheric transmission statistics data to support free-space optical communications experiments and missions. Atmospheric transmission data is collected through a set of three autonomous systems, all located in the south-western US, that observe the stars throughout the year. Data from the three sites are collected and processed on a regular basis to obtain cumulative distribution functions of atmospheric attenuation at different spectral regions. These data will be used to determine site diversity information. In addition, work is underway to build a database of atmospheric transmission data collected by the AVM program and to upgrade the AVM systems to obtain improved data at the important 1.06 micrometers wavelength.
The Optical Communications Demonstrator (OCD) is a laboratory-based lasercom demonstration terminal designed to validate several key technologies, including beacon acquisition, high bandwidth tracking, precision beam pointing, and point-ahead compensation functions. It has been under active development over the past few years. The instrument uses a CCD array detector for both spatial acquisition and high-bandwidth tracking, and a fiber coupled laser transmitter. The array detector tracking concept provides wide field-of-view acquisition and permits effective platform jitter compensation and point-ahead control using only one steering mirror. The use of a fiber- coupled transmitter modularizes the transmitter design and de-couples its thermal management problems from the main system optics. The reduction in design complexity can lead to a reduced system cost and an improved system reliability. This paper describes recent progress on the development of the OCD terminal.
KEYWORDS: Receivers, Sensors, Optical tracking, Optical communications, Space operations, Point spread functions, Transmitters, Signal to noise ratio, Spatial resolution, Telecommunications
The problem of acquiring and tracking a sun-lit earth, which poses a rather stringent demand on the design of the pointing acquisition and tracking subsystem for a deep-space optical communication package, is addressed. The acquisition subsystem must be capable of locating and tracking the receiver location based on a sun-lit earth image that is blurred by the point spread function of the imaging optics and spatially quantized by the detector pixels. Spatial tracking must be performed at bandwidths in excess of 1 kHz to effectively reject platform jitters. A simple solution of locating the earth limb shows a great potential for providing the necessary acquisition and tracking accuracy. By using separate acquisition and tracking detectors, the system can be implemented without extensive technology development. The slow bandwidth required for the acquisition process can be readily accomplished with an available CCD array, and an analog tracking loop can be implemented using a quadrant tracker and calibrated centroid tracking without the excessive computing overhead of the array detector-based spatial tracker.
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