Ariel (Atmospheric Remote Sensing Infrared Exoplanet Large Survey) [1] [2] is the fourth Mission (M4) of the ESA’s Cosmic Vision Program 2015-2025, selected in March 2018 and officially adopted in November 2020 by the Agency, whose aim is to characterize the atmospheres of hundreds of diverse exoplanets orbiting nearby different types of stars and to identify the key factors affecting the formation and evolution of planetary systems. The Mission will have a nominal duration of four years and a possible extension of two years at least. Its launch is presently scheduled for mid 2029 from the French Guiana Space Centre in Kourou on board an Ariane 6.2 launcher in a dual launch configuration with Comet Interceptor. The baseline operational orbit of the Ariel is a large amplitude halo orbit around the second Lagrangian (L2) virtual point located along the line joining the Sun and the Earth-Moon system at about 1.5 million km (~236 RE) from the Earth in the anti-Sun direction. Ariel’s halo orbit is designed to be an eclipse-free orbit as it offers the possibility of long uninterrupted observations in a fairly stable environment (thermal, radiation, etc.). An injection trajectory is foreseen with a single passage through the Van Allen radiation belts (LEO, MEO and GEO near-Earth environments). This is approximated by a worst-case half orbit, prior the injection and transfer to L2, with a duration of 10.5 hours, a perigee of 300 km (LEO), an apogee of 64000 km (GEO and beyond), and an inclination close to 0 degrees. During both the injection trajectory and the final orbit around L2, Ariel will encounter and interact mainly with the Sun radiation and the space plasma environment. In L2 the Ariel spacecraft will spend most of its time in the direct solar wind and the Earth’s magnetosheath with passages through the magnetotail. These three environments, along with LEO and GEO, can lead to the build-up of a net electric charge on the spacecraft and payload conductive and dielectric surfaces leading to the risk of Electro Static Discharges (ESD), potentially endangering the whole Payload integrity and telecommunications to Ground.
ARIEL (Atmospheric Remote-sensing InfraRed Large-survey) is a medium-class mission of the European Space Agency, part of the Cosmic Vision program, whose launch is foreseen by early 2029. ARIEL aims to study the composition of exoplanet atmospheres, their formation and evolution. The ARIEL’s target will be a sample of about 1000 planets observed with one or more of the following methods: transit, eclipse and phase-curve spectroscopy, at both visible and infrared wavelengths simultaneously. The scientific payload is composed by a reflective telescope having a 1m-class elliptical primary mirror, built in solid Aluminium, and two focal-plane instruments: FGS and AIRS. FGS (Fine Guidance System)1 has the double purpose, as suggested by its name, of performing photometry (0.50-0.55 μm) and low resolution spectrometry over three bands (from 0.8 to 1.95 µm) and, simultaneously, to provide data to the spacecraft AOCS (Attitude and Orbit Control System) with a cadence of 10 Hz and contributing to reach a 0.02 arcsec pointing accuracy for bright targets. AIRS (ARIEL InfraRed Spectrometer) instrument will perform IR spectrometry in two wavelength ranges: between 1.95 and 3.9 μm (with a spectral resolution R < 100) and between 3.9 and 7.8 μm with a spectral resolution R < 30. This paper provides the status of the ICU (Instrument Control Unit), an electronic box whose purpose is to command and supply power to AIRS (as well as acquire science data from its two channels) and to command and control the TCU (Telescope Control Unit).
KEYWORDS: Field programmable gate arrays, Electronics, Data processing, Power supplies, Image processing, Infrared imaging, Space telescopes, Exoplanets, Infrared spectroscopy, Photometry
ARIEL is an ESA mission whose scientific goal is to investigate exoplanetary atmospheres. The payload is composed by two instruments: AIRS (ARIEL IR Spectrometer) and FGS (Fine Guidance System). The FGS detection chain is composed by two HgCdTe detectors and by the cold Front End Electronics (SIDECAR), kept at cryogenic temperatures, interfacing with the F-DCU (FGS Detector Control Unit) boards that we will describe thoroughly in this paper. The F-DCU are situated in the warm side of the payload in a box called FCU (FGS Control Unit) and contribute to the FGS VIS/NIR imaging and NIR spectroscopy. The F-DCU performs several tasks: drives the detectors, processes science data and housekeeping telemetries, manages the commands exchange between the FGS/DPU (Data Processing Unit) and the SIDECARs and provides high quality voltages to the detectors. This paper reports the F-DCU status, describing its architecture, the operation and the activities, past and future necessary for its development.
Ariel [1] is the M4 mission of the ESA’s Cosmic Vision Program 2015-2025, whose aim is to characterize by lowresolution transit spectroscopy the atmospheres of over one thousand warm and hot exoplanets orbiting nearby stars. The operational orbit of the spacecraft is baselined as a large amplitude halo orbit around the Sun-Earth L2 Lagrangian point, as it offers the possibility of long uninterrupted observations in a fairly stable radiative and thermo-mechanical environment. A direct escape injection with a single passage through the Earth radiation belts and no eclipses is foreseen. The space environment around Earth and L2 presents significant design challenges to all spacecraft, including the effects of interactions with Sun radiation and charged particles owning to the surrounding plasma environment, potentially leading to dielectrics charging and unwanted electrostatic discharge (ESD) phenomena endangering the Payload operations and its data integrity. Here, we present some preliminary simulations and analyses about the Ariel Payload dielectrics and semiconductors charging along the transfer orbit from launch to L2 included.
One of the advantages of arrays with aperiodic distributed elements is their ability to mitigate the detrimental mutual coupling effects on the radiation pattern. However, we show that the mutual coupling inside a random array can still generate undesired structures in the frequency response although the single antenna features a spectral smooth response. For small subsets (a couple of SKALA4.1 antennas and a 16-element array) of a low-frequency instrument station of the Square Kilometre Array, the combination of large mutual coupling and antenna geometry creates systematic distortions in the element frequency responses. This phenomenon compromises the station spectral smoothness response versus frequency. However, we demonstrate that it is possible to partially mitigate these frequency structures by reconfiguring the antenna distribution based on exclusion zones.
We summarize the activities conducted since 2019 in the numerical electromagnetic analysis of one prototype station of the SKA-Low telescope. Working closely with the SKA Observatory, two teams based in Australia and Italy have collaborated effectively in modeling and analyzing AAVS2, which is the most recent prototype of an SKA-Low station installed in Western Australia. A comprehensive overview of the main electromagnetic parameters at element and array level obtained with two different commercial solvers is presented. Results for scattering parameters, individual element patterns, and station beams are shown; all these fully incorporate mutual coupling effects. Sensitivity of the station is addressed, as the cross-polarization performance. Finally, we also address some lessons learned and their impact on the project.
Giulia Macario, Giuseppe Pupillo, Gianni Bernardi, Pietro Bolli, Paola Di Ninni, Giovanni Comoretto, Andrea Mattana, Jader Monari, Federico Perini, Marco Schiaffino, Marcin Sokolowski, Randall Wayth, Jess Broderick, Mark Waterson, Maria Grazia Labate, Riccardo Chiello, Alessio Magro, Tom Booler, Andrew McPhail, Dave Minchin, Raunaq Bhushan
The low frequency component of the Square Kilometre Array (SKA1-Low) will be an aperture phased array located at the Murchison Radio-astronomy Observatory (MRO) site in Western Australia. It will be composed of 512 stations, each consisting of 256 log-periodic dual-polarized antennas, and will operate in the low frequency range (50 to 350 MHz) of the SKA bandwidth. The Aperture Array Verification System 2 (AAVS2), operational since late 2019, is the last full-size engineering prototype station deployed at the MRO site before the start of the SKA1-Low construction phase. The aim of this paper is to characterize the station performance through commissioning observations at six different frequencies (55, 70, 110, 160, 230, and 320 MHz) collected during its first year of activities. We describe the calibration procedure, present the resulting all-sky images and their analysis, and discuss the station calibratability and system stability. Using the difference imaging method, we also derive estimates of the SKA1-Low sensitivity for the same frequencies and compare them with those obtained through electromagnetic simulations across the entire telescope bandwidth, finding good agreement (within 13%). Moreover, our estimates exceed the SKA1-Low requirements at all considered frequencies by up to a factor of ∼2.3. Our results are very promising and allow for an initial validation of the AAVS2 prototype station performance, which is an important step toward the coming SKA1-Low telescope construction and science.
An unmanned aerial vehicle (UAV) is exploited to characterize in situ the high-band antennas (HBAs) of the low-frequency array (LOFAR) CS302 station located in Exloo, The Netherlands. The size of an HBA array is about 30 m. The Fraunhofer distance (a few kilometers) is not reachable in the frequency band (120 to 240 MHz) within the flight regulation limits. Therefore, far-field patterns cannot be directly measured. The UAV, equipped with an radio frequency synthesizer and a dipole antenna, flies in the near-field region of the considered array. Measurement of three different frequencies (124, 150, and 180 MHz) is efficiently made during the same UAV flight. The near-field focusing method is exploited to validate the far-field pattern of the array under test within an angular range around the beam axis. Such a technique avoids both the time consuming λ / 2 sampling of the aperture field and the further application of computationally heavy near-field to far-field transformations. The array beam is well reconstructed in the main lobe and first sidelobes within a 2D scan plane sampled with a radial raster. A further postprocessing technique is proposed and validated on a subarray of HBAs. It suggests efficient ways for the future characterization of regular aperture arrays for SKA-MID Phase 2.
The Square Kilometre Array telescope at low-frequency (SKA-Low) will be a phased array telescope supporting a wide range of science cases covering the frequency band 50 - 350 MHz, while at the same time asking for high sensitivity and excellent characteristics. These extremely challenging requirements resulted in a design using 512 groups of 256 log periodic dual polarized antennas each (where each group is called “station”), for a total of 131072 antennas. The 512 stations are randomly distributed mostly within a dense area around the centre of the SKA-Low, and then in 3 arms having 16 station clusters each. In preparation for the SKA Phase 1 (SKA1) System Critical Design Review (CDR), prototype stations were deployed at the Murchison Radio-astronomy Observatory (MRO) site (Western Australia) near the Murchison Widefield Array (MWA) radio telescope. The project involved multiple parties in an International collaboration building and testing different prototypes of the SKA1-Low station near the actual site. This resulted in both organisational and logistic challenges typical of a deployment of the actual telescope. The test set-up involved a phased build-up of the complex station of log-periodic antennas, by starting from the deployment of 48 antennas and related station signal processing (called AAVS1.5, where AAVS stands for Aperture Array Verification System), followed by expansion to a full station (AAVS2.0). As reference a station with dipole antennas EDA2 (EDA: Engineering Development Array) was deployed. This test set-up was used for an extensive test and evaluation programme. All test antenna configurations were simulated in detail by electromagnetic (EM) models, and the prediction of the models was further verified by appropriate tests with a drone-based radio frequency source. Astronomical observations on Sun and galaxy transit were performed with calibrated stations of both EDA2, AAVS1.5 and AAVS2.0. All 3 configurations were calibrated. EM modelling and calibration results for the full station AAVS2.0 and EM verification for the AAVS1.5 station are presented. The comparisons between the behaviour of the log-periodic antennas and the dipoles have advanced our understanding the calibration quality and the technological maturity of the future SKA1-Low array.
Using the long-established Cardiff metal-mesh filter technology, we have exploited our ability to artificially manipulate the phase of a wavefront across a device in order to produce a dielectric-based Toraldo pupil working at millimeter wavelengths. The use of a Toraldo pupil to push the angular resolution of an optical imaging system beyond the classical diffraction limit is yet to be realized in the millimeter regime, but is an exciting prospect. Here we present the design and measured performance of a prototype Toraldo pupil, based on a 5 annuli design.
The concept of super-resolution refers to various methods for improving the angular resolution of an optical imaging system beyond the classical diffraction limit. In optical microscopy, several techniques have been developed with the aim of narrowing the central lobe of the illumination Point Spread Function (PSF). In Astronomy a few methods have been proposed to achieve reflector telescopes and antennas with resolution significantly better than the diffraction limit but, to our best knowledge, no working system is in operation. A possible practical approach consists of using the so-called "Toraldo Pupils" (TPs) or variable transmittance filters. These pupils were introduced by G. Toraldo di Francia in 1952,1 and consist of a series of discrete, concentric circular coronae providing specific optical transparency and dephasing in order to engineer the required PSF. The first successful laboratory test of TPs in the microwaves was achieved in 2003,2 and in the present work we build upon these initial measurements to perform electromagnetic (EM) numerical simulations of TPs, using a commercial full-wave software tool. These simulations were used to study various EM effects that can mask and/or affect the performance of the pupils and to analyze the near-field as well as the far-field response. Our EM analysis confirms that at 20 GHz the width of the central lobe in the far-field generated by a TP significantly decreases compared to a clear circular aperture with the same diameter.
Low frequency aperture array technology requires advanced ad-hoc tools for performing antenna and array pattern characterization and instrumental calibration. A micro Unmanned Aerial Vehicle (UAV) mounting a radio-frequency transmitting system developed in Italy has demonstrated to satisfy the challenging characteristics of these tasks. Therefore, a measurement campaign by means of this UAV system has been planned to one Dutch station of the Low Frequency Array (LOFAR) with the main goal to improve the LOFAR antenna and array models. In preparation for this campaign, some initial tests applying the UAV system to one low-frequency antenna of LOFAR were performed in Italy. This contribution describes this measurement session and shows that the measured antenna gain patterns at different frequencies between 40 and 70 MHz agree very well with the electromagnetic models.
KEYWORDS: Receivers, Radio telescopes, Cryogenics, Polarization, Oscillators, Waveguides, Interference (communication), Electronic filtering, Linear filtering, L band
In this article, we present the design and performances of the radio receiver system installed at the Sardinia Radio
Telescope (SRT). The three radio receivers planned for the first light of the Sardinian Telescope have been installed in
three of the four possible focus positions. A dual linear polarization coaxial receiver that covers two frequency bands,
the P-band (305-410 MHz) and the L-band (1.3-1.8 GHz) is installed at the primary focus. A mono-feed that covers the
High C-band (5.7-7.7 GHz) is installed at the beam waveguide foci. A multi-beam (seven beams) K-band receiver (18-
26.5 GHz) is installed at the Gregorian focus. Finally, we give an overview about the radio receivers, which under test
and under construction and which are needed for expanding the telescope observing capabilities.
M. Murgia, G. Bianchi, P. Bolli, G. Comoretto, D. Dallacasa, M. Farooqui, F. Gaudiomonte, L. Gregorini, F. Govoni, K-H. Mack, M. Massardi, A. Mattana, A. Melis, J. Monari, L. Mureddu, G. Naldi, F. Paonessa, F. Perini, A. Poddighe, I. Porceddu, I. Prandoni, G. Pupillo, M. Schiaffino, F. Schillirò, G. Serra, A. Tibaldi, T. Venturi, G. Virone, A. Zanichelli
We present a project aimed at realizing an Italian aperture array demonstrator constituted by prototypical Vivaldi antennas designed to operate at radio frequencies below 500 MHz. We focus on an array composed of a core plus a few satellite phased-array stations to be installed at the Sardinia Radio Telescope (SRT) site. The antenna elements are mobile and thus it will be possible to investigate the performance in terms of both uv-coverage and synthesized resolution resulting from different configurations of the array.
KEYWORDS: Holography, Antennas, Satellites, Reflectors, Receivers, Radio telescopes, Signal to noise ratio, Field programmable gate arrays, Microwave radiation, Calibration
Microwave holography is a well-established technique for mapping surface errors of large reflector antennas, particularly those designed to operate at high frequencies.
We present here a holography system based on the interferometric method for mapping the primary reflector surface of the Sardinia Radio Telescope (SRT). SRT is a new 64-m-diameter antenna located in Sardinia, Italy, equipped with an
active surface and designed to operate up to 115 GHz.
The system consists mainly of two radio frequency low-noise coherent channels, designed to receive Ku-band digital TV signals from geostationary satellites. Two commercial prime focus low-noise block converters are installed on the radio telescope under test and on a small reference antenna, respectively. Then the signals are amplified, filtered and downconverted to baseband. An innovative digital back-end based on FPGA technology has been implemented to digitize two 5 MHz-band signals and calculate their cross-correlation in real-time. This is carried out by using a 16-bit resolution ADCs and a FPGA reaching very large amplitude dynamic range and reducing post-processing time. The final
holography data analysis is performed by CLIC data reduction software developed within the Institut de Radioastronomie Millimétrique (IRAM, Grenoble, France).
The system was successfully tested during several holography measurement campaigns, recently performed at the
Medicina 32-m radio telescope. Two 65-by-65 maps, using an on-the-fly raster scan with on-source phase calibration,
were performed pointing the radio telescope at 38 degrees elevation towards EUTELSAT 7A satellite. The high SNR
(greater than 60 dB) and the good phase stability led to get an accuracy on the surface error maps better than 150 μm
RMS.
Claudio Pernechele, Carlo Barbieri, Pietro Bolli, Franco Buffa, Tonino Pisanu, Sergio Poppi, Giampaolo Serra, Marco Morsiani, Juri Roda, Giampaolo Zacchiroli, Carlo Nocita, Mario Paternò
The Sardinia Radio Telescope (SRT) is a 64 meters (diameter) single dish radioantenna which is in the building phase in
Italy. One of the most challenging characteristics of SRT is its capability to observe up to a frequency of 100 GHz thanks
to its main reflector active surface. The active surface is composed by 1008 panels and 1116 mechanical actuators which
may modify the segmented shape of the main reflector making possible the correction for wavefront distortions induced
by the gravitational and thermal deformations.
In order to observe at a frequency of 100 GHz the surface shape must be accurate below of a value of 150 μm r.m.s..
This value may be reached during the initial alignement phase using the microwave holography but it cannot be
maintained during the scientific operations because of the (dynamical) deformations. In order to permit the observations
at any time, a system able to measure the surface deformations with the necessary accuracy and a time-response of few
minutes (the time-scale of the deformations) must be operative.
We propose here three simple and robust methods to measure the relative deformations of the segmented panels with
respect to an initial aligned surface (reference surface). The ultimate choice on which one of the three systems will
operate on SRT will be taken after final testing on all of them. Prototypes of each system have been realized and two of
them have been also successfully tested on the active optics radiotelescope of Noto (Italy). The test on the third system
will be done in the next few months.
We present the design of the passive feed system of the dual-band receiver for the prime focus of the Sardinia Radio
Telescope (SRT), a new 64 m diameter radio telescope which is being built in Sardinia, Italy. The feed system operates
simultaneously in P-band (305-410 MHz) and L-band (1300-1800 MHz). The room temperature illuminators are
arranged in coaxial configuration with an inner circular waveguide for L-band (diameter of 19 cm) and an outer coaxial
waveguide for P-band (diameter of 65 cm). Choke flanges are used outside the coaxial section to improve the crosspolarization
performance and the back scattering of the P-band feed. The geometry was optimized for compactness and
high antenna efficiency in both bands using commercial electromagnetic simulators. Four probes arranged in
symmetrical configuration are used in both the P and the L-band feeds to extract dual-linearly polarized signals and to
combine them, through phased-matched coaxial cables, into 180 deg hybrid couplers. A vacuum vessel encloses the two
P-band hybrids and the two L-band hybrids which are cooled, respectively at 15 K and 77 K. For the P-Band, four low
loss coaxial feedthroughs are used to cross the vacuum vessel, while for the L-Band a very low loss large window is
employed. The P-band hybrids are based on a microstrip rat-race design with fractal geometry. The L-band hybrids are
based on an innovative double-ridged waveguide design that also integrates a band-pass filter for Radio Frequency
Interference (RFI) mitigation.
Iqueye is a single photon counting very high speed photometer built for the ESO 3.5m New Technology Telescope
(NTT) in La Silla (Chile) as prototype of a 'quantum' photometer for the 42m European Extremely Large Telescope (E-ELT).
The optics of Iqueye splits the telescope pupil into four portions, each feeding a Single Photon Avalanche Diode
(SPAD) operated in Geiger mode. The SPADs sensitive area has a diameter of 100 μm, with a quantum efficiency better
than 55% at 500 nm, and a dark count less than 50 Hz. The quenching circuit and temperature control are integrated in
each module. A time-to-digital converter (TDC) board, controlled by a rubidium oscillator plus a GPS receiver, time tags
the pulses from the 4 channels. The individual times are stored in a 2 TeraByte memory. Iqueye can run continuously for
hours, handling count rates up to 8 MHz, with a final absolute accuracy of each time tag better that 0.5 ns. A first very
successful run was performed in Jan 2009; both very faint and very bright stars were observed, demonstrating the high
photometric quality of the instrument. The first run allowed also to identify some opto-mechanical improvements, which
have been implemented for a second run performed in Dec 2009. The present paper will describe the first version, the
improvements implemented in the second one, and some of the obtained astronomical results.
Almost all astronomical instruments detect and analyze the first order spatial and/or temporal coherence properties
of the photon stream coming from celestial sources. Additional information might be hidden in the second
and higher order coherence terms, as shown long ago by Hanbury-Brown and Twiss with the Narrabri Intensity
Interferometer. The future Extremely Large Telescopes and in particular the 42 m telescope of the European
Southern Observatory (ESO) could provide the high photon flux needed to extract this additional information.
To put these expectations (which we had already developed at the conceptual level in the QuantEYE study for the
100 m OverWhelmingly Large Telescope to experimental test in the real astronomical environment, we realized
a small prototype (Aqueye) for the Asiago 182 cm telescope. This instrument is the fastest photon counting
photometer ever built. It has 4 parallel channels operating simultaneously, feeding 4 Single Photon-Avalanche
Diodes (SPADs), with the ability to push the time tagging capabilities below the nano-second region for hours
of continuous operation. Aqueye has been extensively used to acquire photons from a variety of variable stars,
in particular from the pulsar in the Crab Nebula. Following this successful realization, a larger version, named
Iqueye, has been built for the 3.5 m New Technology Telescope (NTT) of ESO. Iqueye follows the same optical
solution of dividing the telescope pupil in 4 sub-pupils, imaged on new generation SPADs having useful diameters
of 100 micrometers, time jitter less than 50 picoseconds and dark-count noise less than 50 counts/second. The
spectral efficiency of the system peaks in the visible region of the spectrum. Iqueye operated very successfully at
the NTT in January 2009. The present paper describes the main features of the two photometers and present
some of the astronomical results already obtained.
KEYWORDS: Receivers, Antennas, Mirrors, Telescopes, Radio astronomy, Control systems, Space telescopes, Radio telescopes, Astronomy, Electromagnetic coupling
We present the status of the Sardinia Radio Telescope (SRT) project, a new general purpose, fully steerable 64 m
diameter parabolic radiotelescope capable to operate with high efficiency in the 0.3-116 GHz frequency range. The
instrument is the result of a scientific and technical collaboration among three Structures of the Italian National Institute
for Astrophysics (INAF): the Institute of Radio Astronomy of Bologna, the Cagliari Astronomy Observatory (in
Sardinia,) and the Arcetri Astrophysical Observatory in Florence. Funding agencies are the Italian Ministry of Education
and Scientific Research, the Sardinia Regional Government, and the Italian Space Agency (ASI,) that has recently
rejoined the project. The telescope site is about 35 km North of Cagliari.
The radio telescope has a shaped Gregorian optical configuration with a 7.9 m diameter secondary mirror and
supplementary Beam-WaveGuide (BWG) mirrors. With four possible focal positions (primary, Gregorian, and two
BWGs), SRT will be able to allocate up to 20 remotely controllable receivers. One of the most advanced technical
features of the SRT is the active surface: the primary mirror will be composed by 1008 panels supported by electromechanical
actuators digitally controlled to compensate for gravitational deformations. With the completion of the
foundation on spring 2006 the SRT project entered its final construction phase. This paper reports on the latest advances
on the SRT project.
This contribution gives a description of the Sardinia Radio Telescope (SRT), a new general purpose, fully steerable antenna proposed by the Institute of Radio Astronomy (IRA) of the National Institute for Astrophysics. The radio telescope is under construction near Cagliari (Sardinia) and it will join the two existing antennas of Medicina (Bologna) and Noto (Siracusa) both operated by the IRA. With its large antenna size (64m diameter) and its active surface, SRT, capable of operations up to about 100GHz, will contribute significantly to VLBI networks and will represent a powerful single-dish radio telescope for many science fields. The radio telescope
has a Gregorian optical configuration with a supplementary beam-waveguide (BWG), which provides additional focal points. The Gregorian surfaces are shaped to minimize the spill-over and the standing wave between secondary mirror and feed. After the start of the contract for the radio telescope structural and mechanical fabrication in 2003, in the present year the foundation construction will be completed. The schedule foresees the radio telescope inauguration in late 2006.
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.