KEYWORDS: X-rays, Analog electronics, Power supplies, Analog to digital converters, Field programmable gate arrays, X-ray imaging, X-ray detectors, Gamma radiation, Optical sensors
HiZ-GUNDAM is a candidate satellite mission for JAXA to promote time-domain and multi-messenger astronomy as the main targets of gamma-ray bursts. As the mission payload, one of the module of the wide field X-ray monitors consist of a lobster eye optics array and a focal imaging sensor. The field of view of the monitor covers ∼ 0.7 steradian of the sky in the soft X-ray band (0.4 − 4 keV). As the X-ray detector, the pnCCD detector fabricated by PNSensor Inc. can achieve our mission requirements. And we are developing an FPGA-based electronic system for the pnCCD.Our bread-board model of the electronic system consists of (1) a FPGA board, (2) an ADC and power supply board, (3) a pnCCD mounting board, and (4) a 96 × 192-pixel pnCCD read out by 4 CAMEX analog front-end ASICs. We have driven the front-end electronics of the pnCCD successfully by sending the test pulse. In this paper, we report the development status of our FPGA-based electronic system to control the pnCCD sensor.
KEYWORDS: Field programmable gate arrays, X-rays, Analog electronics, Power supplies, Image sensors, Analog to digital converters, CMOS sensors, X-ray imaging, Satellites, Charge-coupled devices
Gamma-ray bursts (GRBs) are the most luminous explosions in the universe, emitting energy on the order of 1052 to 1054 erg over several tens of milliseconds to a few hundred seconds. HiZ-GUNDAM is a future satellite mission designed to explore the early universe using GRBs as probes. It utilizes a wide-field X-ray monitor consisting of Lobster Eye Optics (LEO) and focal image sensors, which detect and determine the direction of GRBs. Two candidates for the focal plane detector are CMOS image sensors and pnCCD image sensors. In the past, we developed the CAPREO FPGA board for the high-speed readout and X-ray event extraction of CMOS image sensors. Currently, we are developing the drive and readout system for the pnCCD, the another candidate. PNSensor’s pnCCD detector, which features a fast readout, large area, and high sensitivity, meets the mission requirements, including an imaging area of 55 mm × 55 mm or larger, a frame rate of at least 10 fps, and a pixel size of approximately 100 μm. The pnCCD drive and readout system requires functions for generating the drive signals for the pnCCD and for AD conversion of the analog signals from the pnCCD. The CAPREO FPGA system can be adapted for high-speed readout and X-ray event extraction. To implement these functions, we developed the PHI driver board to generate charge transfer signals for the pnCCD, the ADC board to convert analog signals from the pnCCD, and a power supply board to power this system. In this paper, we first provide an overview of HiZ-GUNDAM and the mission requirements for the focal plane detector, followed by an introduction to the functions of the three electronic boards we developed.
Detectors with high energy and position resolution over a wide energy range are required for space telescopes in high energy astrophysics missions. By combining a low noise fully depleted pnCCD detector with a columnar CsI(Tl) scintillator, an energy dispersive spatially resolving detector can be realized with high quantum efficiency in the range from below 0.5 keV to above 150 keV. The detector is exposed to the photon source such that the X-rays first traverse the 450 μm sensitive pnCCD. If they are stopped through the photoelectric effect in the silicon detector, Fano-noiselimited energy resolution is achieved. This is true for X-rays from a few hundred eV up to approximately 15 keV. Above this energy the probability that the photon penetrates the pnCCD and converts in the CsI(Tl) scintillator is becoming higher. Due to the high atomic number of Cs (Z=55) and I (Z=53) hard X-rays are stopped efficiently in a 0.7 mm thick CsI(Tl) scintillator for photon energies up to 150 keV. The light from the scintillator is recorded with the same backilluminated pnCCD. For X-rays from a 57Co source with an energy of 122 keV and 136 keV we achieve an energy resolution of 0.7% (FWHM=850 eV) for the direct conversion in the silicon while the energy resolution for the conversion in the CsI(Tl) is 10% (12 keV). We have performed a knife-edge experiment at 122 keV and achieved a position precision of 27 μm at that energy. Monte Carlo simulations were showing similar, fully compatible results. In case the X-rays are converted directly in the silicon the position precision is better than 10 μm. This is close to the theoretical limit of the spatial resolution in such a system, which is given by the length of the tracks of the secondary electrons in the ionizing process in silicon and CsI. Spectra, images and the results of the GEANT4 simulations will be shown.
pnCCDs are a special type of charge coupled device (CCD) which were originally developed for applications in X-ray astronomy. At X-ray Free Electron Lasers (XFEL) pnCCDs are used as imaging X-ray spectrometers due to their outstanding characteristics like high readout speed, high and homogenous quantum efficiency, low readout noise, radiation hardness and a high pixel charge handling capacity. With pnCCDs it is possible to separate one photon from no photon and two photons as well as being able to measure up to up to 104 photons per pixel per frame. However, extremely high photon intensities can result in pixel saturation and charge spilling into neighboring pixels. Because of this charge blooming effect, spatial information is reduced. Due to the deep understanding of the internal potential distribution we can enhance the pixel full well capacity even more and improve the quality of the image. This paper describes the influence of the operation voltages and space charge distribution of the pnCCD on the electric potential profile by using 2D numerical device simulations. Experimental results with signal injection from an optical laser confirm the simulation models.
N. Loh, Dmitri Starodub, Lukas Lomb, Christina Hampton, Andrew Martin, Raymond Sierra, Anton Barty, Andrew Aquila, Joachim Schulz, Jan Steinbrener, Robert Shoeman, Stephan Kassemeyer, Christoph Bostedt, John Bozek, Sascha Epp, Benjamin Erk, Robert Hartmann, Daniel Rolles, Artem Rudenko, Benedikt Rudek, Lutz Foucar, Nils Kimmel, Georg Weidenspointner, Günther Hauser, Peter Holl, Emanuele Pedersoli, MengNing Liang, Mark Hunter, Lars Gumprecht, Nicola Coppola, Cornelia Wunderer, Heinz Graafsman, Filipe R. N. Maia, Tomas Ekeberg, Max Hantke, Holger Fleckenstein, Helmut Hirsemann, Karol Nass, Thomas White, Herbert Tobias, George Farquar, W. Henry Benner, Stefan Hau-Riege, Christian Reich, Andreas Hartmann, Heike Soltau, Stefano Marchesini, Sasa Bajt, Miriam Barthelmess, Lothar Strueder, Joachim Ullrich, Philip Bucksbaum, Keith Hodgson, Mathias Frank, Ilme Schlichting, Henry Chapman, Michael Bogan
Profiling structured beams produced by X-ray free-electron lasers (FELs) is crucial to both maximizing signal intensity for weakly scattering targets and interpreting their scattering patterns. Earlier ablative imprint studies describe how to infer the X-ray beam profile from the damage that an attenuated beam inflicts on a substrate. However, the beams in-situ profile is not directly accessible with imprint studies because the damage profile could be different from the actual beam profile. On the other hand, although a Shack-Hartmann sensor is capable of in-situ profiling, its lenses may be quickly damaged at the intense focus of hard X-ray FEL beams. We describe a new approach that probes the in-situ morphology of the intense FEL focus. By studying the translations in diffraction patterns from an ensemble of randomly injected sub-micron latex spheres, we were able to determine the non-Gaussian nature of the intense FEL beam at the Linac Coherent Light Source (SLAC National Laboratory) near the FEL focus. We discuss an experimental application of such a beam-profiling technique, and the limitations we need to overcome before it can be widely applied.
We developed a camera with a 264 × 264 pixel pnCCD of 48 μm size (thickness 450 μm) for X-ray and optical
applications. It has a high quantum efficiency and can be operated up to 400 / 1000 Hz (noise≈ 2:5 ē ENC
/ ≈4:0 ē ENC). High-speed astronomical observations can be performed with low light levels. Results of test
measurements will be presented. The camera is well suitable for ground based preparation measurements for
future X-ray missions. For X-ray single photons, the spatial position can be determined with significant sub-pixel
resolution.
Measurement campaigns of the Max-Planck Advanced Study Group (ASG) in cooperation with the Center for
Free Electron Laser Science (CFEL) at DESY-FLASH and SLAC-LCLS have established pnCCDs as universal
photon imaging spectrometers in the energy range from 90 eV to 2 keV. In the CFEL-ASG multi purpose
chamber (CAMP), pnCCD detector modules are an integral part of the design with the ability to detect photons
at very small scattering angles. In order to fully exploit the spectroscopic and intensity imaging capability of
pnCCDs, it is essentially important to translate the unprocessed raw data into units of photon counts for any
given position on the detection area.
We have studied the performance of pnCCDs in FEL experiments and laboratory test setups for the range
of signal intensities from a few X-ray photons per signal frame to 100 or more photons with an energy of 2 keV
per pixel. Based on these measurement results, we were able to characterize the response of pnCCDs over the
experimentally relevant photon energy and intensity range. The obtained calibration results are directly relevant
for the physics data analysis. The accumulated knowledge of the detector performance was implemented in
guidelines for detector calibration methods which are suitable for the specific requirements in photon science
experiments at Free Electron Lasers.
We discuss the achievable accuracy of photon energy and photon count measurements before and after the
application of calibration data. Charge spreading due to illumination of small spots with high photon rates is
discussed with respect to the charge handling capacity of a pixel and the effect of the charge spreading process
on the resulting signal patterns.
New generation synchrotron light sources, the X-ray free electron lasers, require a two dimensional focal plane
instrumentation to perform X-ray imaging from below 100eV up to 25keV. The instruments have to face the accelerator
bunch structure and energy bandwidth which is different for existing (FLASH, Hamburg and LCLS, Menlo Park) and
future photon sources (SACLA, Harima and XFEL, Hamburg). Within the frame of the Center for Free Electron Laser
Science (CFEL), a joint effort of the Max-Planck Society, DESY and the University of Hamburg, the MPI
semiconductor laboratory developed, produced and operated large area X-ray CCD detectors with a format of nearly
60cm2 image area. They show outstanding characteristics: a high readout speed due to a complete parallel signal
processing, high and homogeneous quantum efficiency, low signal noise, radiation hardness and a high pixel charge
handling capacitance. We will present measurement results which demonstrate the X-ray spectroscopic and imaging
capabilities of the fabricated devices.
We will also report on the concept and the anticipated properties of the full, large scale system. The implementation of
the detector into an experimental chamber to perform measurements e.g. of macromolecules in order to determine their
structure at atomic resolutions will be shown.
Andrew Martin, Jakob Andreasson, Andrew Aquila, Saša Bajt, Thomas R. Barends, Miriam Barthelmess, Anton Barty, W. Henry Benner, Christoph Bostedt, John Bozek, Phillip Bucksbaum, Carl Caleman, Nicola Coppola, Daniel DePonte, Tomas Ekeberg, Sascha Epp, Benjamin Erk, George Farquar, Holger Fleckenstein, Lutz Foucar, Matthias Frank, Lars Gumprecht, Christina Hampton, Max Hantke, Andreas Hartmann, Elisabeth Hartmann, Robert Hartmann, Stephan Hau-Riege, Günther Hauser, Peter Holl, André Hoemke, Olof Jönsson, Stephan Kassemeyer, Nils Kimmel, Maya Kiskinova, Faton Krasniqi, Jacek Krzywinski, Mengning Liang, Ne-Te Duane Loh, Lukas Lomb, Filipe R. N. Maia, Stefano Marchesini, Marc Messerschmidt, Karol Nass, Duško Odic, Emanuele Pedersoli, Christian Reich, Daniel Rolles, Benedikt Rudek, Artem Rudenko, Carlo Schmidt, Joachim Schultz, M. Marvin Seibert, Robert Shoeman, Raymond Sierra, Heike Soltau, Dmitri Starodub, Jan Steinbrener, Francesco Stellato, Lothar Strüder, Martin Svenda, Herbert Tobias, Joachim Ullrich, Georg Weidenspointner, Daniel Westphal, Thomas White, Garth Williams, Janos Hajdu, Ilme Schlichting, Michael Bogan, Henry Chapman
Results of coherent diffractive imaging experiments performed with soft X-rays (1-2 keV) at the Linac Coherent
Light Source are presented. Both organic and inorganic nano-sized objects were injected into the XFEL beam
as an aerosol focused with an aerodynamic lens. The high intensity and femtosecond duration of X-ray pulses
produced by the Linac Coherent Light Source allow structural information to be recorded by X-ray diffraction
before the particle is destroyed. Images were formed by using iterative methods to phase single shot diffraction
patterns. Strategies for improving the reconstruction methods have been developed. This technique opens
up exciting opportunities for biological imaging, allowing structure determination without freezing, staining or
crystallization.
The Max Planck Advanced Study Group (ASG) at the Center for Free Electron Laser Science (CFEL) has
designed the CFEL-ASG MultiPurpose (CAMP) instrument, which provides a unique combination of particle
and photon detectors for experiments at 4th generation light sources. In particular, CAMP includes two sets
of newly developed 1024 × 1024 pixel pnCCD imaging detector systems. The CAMP instrument has now been
successfully employed during the first three beam times at LCLS, and we report here on practical experience
gained for the operation of imaging pnCCD detectors at FEL facilities. We address a wide range of topics:
pnCCD gain and energy calibration during experiments; suppression of optical light contamination in pumpprobe
experiments; contamination of the pnCCD entrance window with sample material; effects of accidental
direct impact on the pnCCDs of particles generated by the FEL beam impinging on the experimental setup; and
the effect of accidental direct exposure of a pnCCD to the focused and unattenuated X-ray beam. These lessons
learned will help us to further improve operation of pnCCDs in future FEL experiments.
The new X-ray telescope eROSITA (extended ROentgen Survey with an Imaging Telescope Array) is the main
instrument on the Russian new Spectrum-RG satellite, scheduled for launch in 2012. The primary scientific goal
of eROSITA is the detection of about 100,000 clusters of galaxies in an all sky survey. This allows a systematic
study on the large scale structures in the universe and will give new information about the nature of dark energy.
The focal plane detector is a 5 cm × 3 cm framestore PNCCD, an advanced successor of the XMM-Newton
PNCCD, designed and fabricated at the MPI Halbleiterlabor. It has 384 × 384 pixels of 75 μm × 75 μm in the
image area and will provide high position, time and spectral resolution as well as a high quantum efficiency for
X-ray photons in the energy range from 0.2 keV up to 10 keV. The first flight-like CCDs have been finished in
2008. In order to extensively test these new PNCCDs we developed an electronic test-setup. It is very versatile,
allowing us to test the CCDs under many different conditions and is appropriate to show at the same time
excellent performance of the detector. In this contribution we present in detail the electronic test-setup, some
test results and the conclusions which can be drawn for the eROSITA flight modules.
For the eROSITA X-ray telescope, which is planned to be launched in 2012, detectors were developed and
fabricated at the MPI Semiconductor Laboratory. The fully depleted, back-illuminated pnCCDs have an ultrathin
pn-junction to improve the low-energy X-ray response function and quantum efficiency. The device thickness of
450 μm is fully sensitive to X-ray photons yielding high quantum efficiency of more than 90% at photon energies of
10 keV. An on-chip filter is deposited on top of the entrance window to suppress visible and UV light which would
interfere with the X-ray observations. The pnCCD type developed for the eROSITA telescope was characterized
in terms of quantum efficiency and spectral response function. The described measurements were performed in
2009 at the synchrotron radiation sources BESSY II and MLS as cooperation between the MPI Semiconductor
Laboratory and the Physikalisch-Technische Bundesanstalt (PTB). Quantum efficiency measurements over a
wide range of photon energies from 3 eV to 11 keV as well as spectral response measurements are presented. For
X-ray energies from 3 keV to 10 keV the quantum efficiency of the CCD including on-chip filter is shown to be
above 90% with an attenuation of visible light of more than five orders of magnitude. A detector response model
is described and compared to the measurements.
A special type of CCD, the so-called PNCCD, was originally developed for the focal plane camera of the XMMNewton
space telescope. After the satellite launch in 1999, the MPI Halbleiterlabor continued the detector development
for various ground-based applications. Finally, a new X-ray PNCCD was designed again for a space telescope named
eROSITA. The space telescope will be equipped with an array of seven parallel oriented X-ray mirror systems of
Wolter-I type and seven cameras, placed in their foci. This instrumentation will permit the exploration of the X-ray
universe in the energy band from 0.3 keV up to 10 keV with a time resolution of 50 ms for a full image comprising
384 x 384 pixels. eROSITA will be accommodated on the new Russian Spectrum-RG satellite. The mission was already
approved by the responsible German and Russian space agencies. The detector development is focussed to fulfil the
scientific specifications for detector performance under the constraints of all the mechanical, power, thermal and
radiation hardness issues for space instrumentation. This considers also the recent change of the satellite's orbit. The
Lagrange point L2 was decided as new destination of the satellite instead of a low-Earth orbit (LEO). We present a
detailed description of the detector system and the current development status. The most recent test results are reported
here. Essential steps for completion of the seven focal plane detectors until satellite launch in 2012 will be itemized.
Robert Hartmann, Sebastian Deires, Mark Downing, Hubert Gorke, Sven Herrmann, Sebastian Ihle, Gottfried Kanbach, Janis Papamastorakis, Heike Soltau, Alexander Stefanescu, Lothar Strüder
We present the design and optical imaging performance of a pnCCD detector system for highest frame rates and excellent
sensitivity over a wide wavelength range from the UV to near IR region. To achieve frame rates higher than one thousand
frames per second with an exceptionally low noise level, the devices are based on proven technology with column parallel
readout and operated in a split-frame transfer mode. The CCDs are back illuminated and coated with an Anti-Reflective-
Coating. The sensitivity over their full thickness of 450 &mgr;m allows for a quantum efficiency near 100% over a wide spectral
range.
At an optical test bench we determined the photon transfer curve, quantum efficiency and point-spread function within a
wavelength region between 300 nm to 1100 nm for various detector parameter. To demonstrate the ability of a pnCCD to
perform high-speed optical differential photometry, the crab nebula with the crab pulsar as central object were observed at
the 1.3m SKINAKAS telescope on crete. For these observations the pnCCD was operated at a speed of 2000 frames per
second.
The high speed, low noise and high quantum efficiency makes this detector an ideal instrument to be used as a wavefront
sensor in adaptive optics systems.
KEYWORDS: Sensors, Charge-coupled devices, Cameras, X-rays, Electronics, CCD cameras, Digital signal processing, Signal processing, CCD image sensors, Space telescopes
The German X-ray observatory eROSITA (extended ROentgen Survey with an Imaging Telescope Array) is the prime
instrument of the new Spectrum-RG mission. Launch of the Russian satellite is planned for the year 2011. The scientific
goal of eROSITA is primarily the detection and analysis of 100 thousand clusters of galaxies in order to study the large
scale structures in the Universe and to test cosmological models. The therefore required large effective area is obtained
by an array of seven identical and parallel aligned Wolter-I telescopes. In the focus of each mirror module, there is a
large frame store pnCCD detector, providing a field of view of 1° in diameter. The same X-ray detector type will also be
applied for ART-XC, another grazing-incidence telescope system aboard Spectrum-RG, which permits the detection of
heavily obscured X-ray sources. These scientific instruments allow the exploration of the X-ray Universe in the energy
band from 0.3 keV to 11 keV. During a mission time of at least five years, an all-sky survey, wide as well as deep
surveys and pointed observations will be performed. Approval and funding for eROSITA were granted by the German
space agency DLR in April 2007.
The conceptual design of the X-ray focal plane cameras is presented here comprising electrical, thermal, and mechanical
aspects. Key part of the camera is the pnCCD detector chip, which is developed and produced in our semiconductor
laboratory, the MPI Halbleiterlabor. The CCD was designed according to the specifications given by the scientific goals
of eROSITA. The eROSITA CCD differs apparently from all previously produced frame store pnCCDs by its larger
size and format. The CCD image area of the seven eROSITA cameras is in total 58 cm2 large and their number of pixels
is about seven times higher than that of the XMM-Newton pnCCD camera. First pnCCD devices were recently
produced and tested. Their performance measurements and results are of most importance for eROSITA because the
tested CCDs are the control sample of the flight detector production.
A pnCCD detector fulfils all typical requirement specifications to an X-ray detector optimally: The energy of the X-ray
photon is precisely measured, incidence position is determined even more accurate than the pixel size, and the arrival
time of the photon is very well defined by the high frame rate due to complete parallel signal processing. The
probability for detection of an X-ray photon is from 0.3 keV to 10 keV close to 100% and homogeneous over the image
area.
Such a detector has been developed for application in X-ray astronomy. The XMM-Newton space observatory is already
equipped with a pnCCD camera which performs since commissioning in 2000 till this day excellent measurements. For
the upcoming eROSITA telescope on the Spectrum-Roentgen-Gamma satellite, an advanced pnCCD detector system is
presently developed. Seven pnCCD cameras are placed in the foci of seven X-ray mirror systems researching the X-ray
sky during a mission time of 5 years.
For ground based instrumentation the X-ray fluxes can be extremely high, as it is the case in X-ray free electron lasers
(XFELs). The evolving XFELs will make it possible to capture three-dimensional images of the nanocosmos. Here the
focus is set on the measurement of X-ray intensities instead of spectroscopy, i.e. the number of monochromatic photons
per pixel (up to > 1000 photons) is counted at very high frame rates ( > 100/s).
Both projects have again in common the request for large image areas: in case of eROSITA seven times an image area
of 8 cm2 and for the XFEL experiment at LCLS we provide in a first step a 59 cm2 large image area. In a second step it
will be enlarged to even 236 cm2. We performed recently promising tests with the prototype detectors. Therefore we
started the production of the final devices for both applications in the MPI semiconductor laboratory.
An advanced pnCCD type has been developed, based on the concept of the XMM-Newton detector, which has been
performing spectroscopy and imaging since 2000. This new detector is designed according to the requirements of
eROSITA, a new X-ray astronomy mission, to be launched in 2010. The focal plane for each of the seven individual
Wolter telescopes will be equipped with one of these new-type X-ray pnCCDs. In addition to the eROSITA chips, we
have developed CCDs for other applications, e.g. for projects which require smaller pixel sizes. The devices that have
been produced in the semiconductor laboratory (MPI Halbleiterlabor) of the Max-Planck-Institut fur extraterrestrische
Physik are currently subject of systematic quality checks and spectroscopic tests. These tests are performed under
standardized conditions on a representative subset of the many devices we have produced. The aim of these tests is to
extract the key performance parameters of the individual CCDs like readout noise, energy resolution and the occurrence
of bad pixels. The analysis includes the CAMEX analog signal processor, which has been developed for the readout of
the CCD signals. After an introduction, we present the motivation for the detector development and give an overview
about our CCD design and production, as well as about the CAMEX ASIC. Then device tests, test setups and data
analysis are described. We report in detail about the performance of the tested devices. Failures that occurred during
device tests are subsequently discussed. Finally, we give a review of the results.
At MPI Halbleiterlabor, pnCCDs have been continuously developed to improve readout noise, readout speed, charge transfer efficiency and energy resolution. Pixel sizes of 75μm, 51μm and 36μm were realized in addition to the original 150μm pixel design. Reduction of the pixel size evidently changes the electric fields in the pixel structure. This leads to the question of how scaling of the pixel size affects the charge collection at subpixel dimensions. We used the "mesh-method" to measure the amount of signal charge deposited in a pixel depending on the position of X-Ray photon incidence within the pixel. In this experiment, a mesh with a rectangular hole pattern was mounted above the entrance window or structured front side of the detector. A slight rotation of the mesh ensures that every hole has a different position relative to the pixel below. It corresponds to scanning of a single pixel. Measurements were done with pnCCDs of 150μm, 75μm and 51μm pixel size at photon energies from 0.7keV to 5.4keV. We also used a setup with front side illumination of a pnCCD with 75μm pixel size to investigate the absorption of X-ray photons in the register structure of the device. Numerical simulations delivered results for signal charge distribution into pixels along the charge transfer direction. We analyzed the charge collection in a pixel and the absorption properties of the register structure with a spatial resolution below 5μm and could investigate the accuracy of numerical device simulations.
The CAST experiment at CERN (European Organization of Nuclear Research) searches for axions from the sun. The axion is a pseudoscalar particle that was motivated by theory thirty years ago, with the intention to solve the strong CP problem. Together with the neutralino, the axion is one of the most promising dark matter candidates. The CAST experiment has been taking data during the last two years, setting an upper limit on the coupling of axions to photons more restrictive than from any other solar axion search in the mass range below 10-1 eV. In 2005 CAST will enter a new experimental phase extending the sensitivity of the experiment to higher axion masses. The CAST experiment strongly profits from technology developed for high energy physics and for X-ray astronomy:
A superconducting prototype LHC magnet is used to convert potential axions to detectable X-rays in the 1-10 keV range via the inverse Primakoff effect. The most sensitive detector system of CAST is a spin-off from space technology, aWolter I type X-ray optics in combination with a prototype pn-CCD developed for ESA's XMM-Newton mission. As in other rare event searches, background suppression and a thorough shielding concept is essential to improve the sensitivity of the experiment to the best possible. In this context CAST offers the opportunity to study the background of pn-CCDs and its long term behavior in a terrestrial environment with possible implications for future space applications. We will present a systematic study of the detector background of the pn-CCD of CAST based on the data acquired since 2002 including preliminary results of our background simulations.
Fully depleted, backside illuminated pnCCDs with an integrated frame store area and an anti-reflective-coating for the optical and near infrared region have been fabricated. Measurement results of a 51 μm pixelsize device with an imaging area of 264 × 264 pixel will be presented. The devices, which feature a doublesided readout, allow to be operated at frame rates higher than 1000 frames per second. The electronic noise contribution of the entire detector system is slightly above two electrons at fastest readout modes.
We will also present the concept of a data acquisition system being able to handle pixel rates of more than 70 megapixel per second. Decentral data reduction and analysis units allow for a centroid determination of sub--images with a very low latency time.
The high speed, low noise and high quantum efficiency makes this camera system an ideal instrument for wavefront sensors in adaptive optics systems.
A new generation of pnCCDs has been developed for the proposed X-ray astronomy missions, DUO and ROSITA. The DUO/ROSITA CCD is a frame store pnCCD based on the concept of the XMM-Newton pnCCD and has both, improved performance and new features. This detector permits accurate spectroscopy of X-rays as well as imaging and high time resolution with high quantum efficiency in the energy band from 0.3 keV to 10 keV. Interfering electron-hole pair generation due to optical and UV light is prevented by a deposition of an on-chip filter. We describe the frame store pnCCDs developed and fabricated for the DUO and ROSITA missions in the semiconductor laboratory of the Max-Planck-Institut fuer extraterrestrische Physik. An overview about the CCD concept and design is given along with some details about the fabrication of the devices. In addition, we introduce a new analog signal processor which has been developed specifically for the readout of the frame store pnCCD signals. The main focus of this paper is to present the very first measurements with this CCD type and its analog signal processor. Towards this aim we report the operation of this new sensor and its key performance parameters. Finally we discuss ongoing and future tests with the DUO/ROSITA CCDs.
Dark Energy dominates the mass-energy content of the universe (about 73%) but we do not understand it. Most of the remainder of the Universe consists of Dark Matter (23%), made of an unknown particle. The problem of the origin of Dark Energy has become the biggest problem in astrophysics and one of the biggest problems in all of science. The major extant X-ray observatories, the Chandra X-ray Observatory and XMM-Newton, do not have the ability to perform large-area surveys of the sky. But Dark Energy is smoothly distributed throughout the universe and the whole universe is needed to study it. There are two basic methods to explore the properties of Dark Energy, viz. geometrical tests (supernovae) and studies of the way in which Dark Energy has influenced the large scale structure of the universe and its evolution. DUO will use the latter method, employing the copious X-ray emission from clusters of galaxies. Clusters of galaxies offer an ideal probe of cosmology because they are the best tracers of Dark Matter and their distribution on very large scales is dominated by the Dark Energy. In order to take the next step in understanding Dark Energy, viz. the measurement of the 'equation of state' parameter 'w', an X-ray telescope following the design of ABRIXAS will be accommodated into a Small Explorer mission in lowearth orbit. The telescope will perform a scan of 6,000 sq. degs. in the area of sky covered by the Sloan Digital Sky Survey (North), together with a deeper, smaller survey in the Southern hemisphere. DUO will detect 10.000 clusters of galaxies, measure the number density of clusters as a function of cosmic time, and the power spectrum of density fluctuations out to a redshift exceeding one. When combined with the spectrum of density fluctuations in the Cosmic Microwave Background from a redshift of 1100, this will provide a powerful lever arm for the crucial measurement of cosmological parameters.
KEYWORDS: Cameras, Mirrors, Charge-coupled devices, Telescopes, X-rays, Sensors, CCD cameras, Galaxy groups and clusters, Electronics, Digital signal processing
What is the nature of the Dark Energy that is driving the universe apart? Clusters of galaxies offer an ideal probe of cosmology because they are the best tracers of Dark Matter and their distribution on very large scales which is dominated by the Dark Energy. DUO will measure 10.000 clusters of galaxies, the power spectrum of density fluctuations of clusters and their number density as a function of cosmic time. Although designed long before the existence of Dark Energy was claimed, the ABRIXAS type X-ray telescope turns out to be ideally suited for this task: DUO is, in essence, a re-flight of the ABRIXAS X-ray telescope which some modifications of the focal plane instrumentation. First of all, we will use new CCDs which are improved versions of the pn-CCDs successfully flown on XMM-Newton. A modular concept having seven individual cameras in the foci of the seven mirror systems allows us to design the orientation of the seven telescopes with respect to each other matching the scientific needs of the DUO mission. Details of the concept including mechanical, electrical and thermal aspects are given.
The Cern Axion Solar Telescope - CAST - uses a prototype 9 Tesla LHC superconducting dipole magnet to search for a hypothetical pseudoscalar particle, the axion, which was proposed by theory in the 1980s to solve the strong CP problem and which could be a dark matter candidate. In CAST a strong magnetic field is used to convert the solar axions to detectable photons via inverse Primakoff effect. The resulting X-rays are thermally distributed in the energy range of 1-7 keV and can be observed with conventional X-ray detectors. The most sensitive detector system of CAST is a pn-CCD detector originally developed for XMM-Newton combined with a Wolter I type X-ray mirror system. The combination of a focusing X-ray optics and a state of the art pn-CCD detector which combines high quantum efficiency, good spacial and energy resolution, and low background improves the sensitivity of the CAST experiment such that for the first time the axion photon coupling constant can be probed beyond the best astrophysical constraints. In this paper we report on the performance and status of the X-ray telescope and pn-CCD detector of CAST.
DUO and ROSITA are two future X-ray astronomy missions observing in the energy band from about 0.3 keV to 10 keV. While the NASA satellite DUO will scan selected areas of the X-ray sky with high sensitivity, the German ROSITA mission shall perform an all-sky survey. Both missions apply an array of seven Wolter telescopes with separated field of views and seven dedicated PN-CCD focal plane detectors. The focal plane detectors are a further development of the flight-proven PN-CCD applied for the XMM-Newton observatory. The advanced device, called 'frame store PN-CCD', is designed and fabricated in the semiconductor laboratory of the Max-Planck-Institute for extraterrestrial physics. An introduction into the detector concept and design are presented as well as the promising results which have been achieved with the prototype devices. This includes an overview about the performance of the PN-CCD and in detail the recent measurements with the detector. An example is the low energy response of the optimized photon entrance window with integrated optical light filter. As the CAMEX analog signal processor chip is a main component of the detector module, we describe its development status. Furthermore, we report about the application of the mesh experiment to the PN-CCD which allows for a study of the electric potential characteristics in the detector bulk, in particular in the charge transfer depth. The information is of great importance for an accurate knowledge about the drift of the generated signal electrons into the potential wells of the pixels.
The fully depleted PN-CCD detector is meanwhile field-tested in several experiments on ground and in space. Its application as focal plane detector aboard ESA's XMM-Newton observatory can be considered as the most impressive one. The further development of this detector type including its readout chip in the MPI semiconductor laboratory is presented here. The new device, called frame store PN-CCD, shows substantial improvement of performance, in particular concerning the energy resolution and the probability of out of time event occurrence. Moreover, the detector offers features which are of great importance for its application in space. This is, besides the radiation hardness of the CCD, the variety of feasible pixel sizes and the high frame rates in combination with the small power consumption of the detector. Because of the thin radiation entrance window and the full depletion of the chip, the detector provides a high quantum efficiency for soft X-rays as well as for optical light and the near infrared. The frame store PN-CCD detector will be applied for the proposed X-ray astronomy missions DUO and ROSITA.
The pn-CCD was developed as focal plane detector for the XMM-Newton mission and operates successfully for more than 30 months in orbit without performance degradation. In order to match the new requirements of the future ROSITA mission which will perform a broad band X-ray all-sky survey, we propose an advanced type of pn-CCD. The concept and the new features of this frame store pn-CCD as part of the imaging X-ray spectrometer of ROSITA are described. First
measurements with prototype devices show the improvement of detector performance in comparison to the pn-CCD on XMM-Newton. We suggest as optical filter for the observations of the X-ray sky, a thin aluminum layer deposited on the photon entrance window of the device.
Active Pixel Sensors (APS) offer high-resolution imaging in combination with a fast and flexible readout. The MPI Halbleiterlabor develops and produces DEPFET (Depleted Field Effect Transistor) based APS devices. They are additionally characterized by enhanced sensitivity for X-ray photons in the range from 0.1 keV to 25 keV, spectroscopic energy resolution (below 1 electron r.m.s.) and radiation hardness. Moreover, the production process on high-ohmic silicon allows incorporating additional high-speed spectrometers based on silicon drift detectors. Such a detector system is proposed as a wide field imager for the XEUS (X-ray Evolving Universe Spectroscopy) mission. XEUS is a planned project within the European Space Agency's Horizon 2000+ program. We will present a focal plane concept for XEUS and measurement results from DEPFET-APS prototypes and high speed drift detectors.
The pn-CCD is the focal plane detector of one of the three X-ray
telescopes aboard the XMM-Newton observatory. During
revolution #156 more than 30 individual bright pixels lightened
up out of approximately 150,000 pixels of the 6 cm × 6 cm
large detector area. The amount of leakage current generated
in the pixels cannot be explained by single heavy ions impact,
however. We suggest that a micrometeoroid scattered off the
mirror surface under grazing incidence reached the focal plane
detector and produced the bright pixels. This proposal was
studied by us experimentally at the Heidelberg dust accelerator.
Micron-sized iron particles were accelerated to speeds of the
order of 5 km/s impinging on the surface of an X-ray mirror
under grazing incidence. Scatter products have been found with
detectors placed behind the mirror. They have been analyzed by
various methods to characterize their properties and the effects
produced by them in the pn-CCD. Micrometeoroid damage to
semiconductor detectors in the focus of grazing incidence optics
might be of concern for future space projects with very large
collecting area and are proposed to be studied in detail.
The main scientific objective of the ROSITA mission is to extend the X-ray all-sky survey of ROSAT to higher energies to gain an unbiased sample of all types of celestial X-ray sources in the medium energy band. During this mission the whole sky will be scanned by seven imaging X-ray telescopes. The telescopes have different viewing directions with an offset angle between 4 and 6 deg. The focal plane instrumentation of the telescopes is based on a novel type of pn-CCD with a frame store, an advanced version of the pn-CC operating quite successfully on XMM-Newton. The pixel size is adapted to the
mirror resolution and the fast readout time guaranties the required angular accuracy despite the scan motion. The X-ray camera carries seven separate CCDs arranged on a circle in the foci of the Wolter type I mirror systems of the seven telescopes. The CCDs are mounted on ceramic frames, which carry dedicated front-end electronics for each CCD. The CCDs are operated at a temperature of-80 deg C. Except for the entrance window, the CCDs are covered by graded shielding for suppression of fluorescent X-ray background, generated by cosmic rays in the surrounding materials. Filters in front of the the CCDs, inhibit optical and UV photons. For in-orbit calibration a radioactive
source producing fluorescent X-rays in the desired energy band is provided. We will give an overview of the mechanical, thermal and electrical concept of the camera system.
The pn-CCD camera on EPIC-XMM is the most advanced imaging X-ray spectrometer, as it combines high quantum efficiency, high speed readout and high energy resolution. The camera operates for almost two years as calibrated prior to launch. Future missions, like ESA's XEUS (X-ray Evolving Universe Spectroscopy) mission require higher spatial resolution, higher response at energies above 20 keV and most important a full frame readout rate increased by at least a factor of 20 for the first operational phase. XEUS represents a potential follow-on mission to the cornerstone XMM-Newton, currently in orbit. The XEUS mission is considered as part of ESA's Horizon 2000+ program within the context of the International Space Station (ISS.) In order to match the above requirements for the wide field imager of XEUS, we propose a frame store pn-CCD camera system based on the technology development of the EPIC (European Photon Imaging Camera) camera on XMM-Newton. Our goal is readout rate of 250 complete frames per second for 1024 x 1024 pixels with a pixel size of 75x75micrometers 2, monolithically integrated on a 6 inch wafer. The concept and the new features of the frame store pn-CCD camera will be described. The focal plane layout, the readout concept and the expected scientific performance will be introduced. The implementation of thin aluminum filters, monolithically grown on the pn-CCD entrance window, will be discussed as well as the integration of a very fast spectroscopic detector being able to record 106 counts per second with a FWHM of about 250 eV.
Based on the operational experience with the EPIC pn-CCD system on board of XMM-Newton, new imaging X-ray spectroscopic detector systems for future X-ray missions will be introduced in terms of energy, position and time resolving detectors. As the readout speed requirement in the case of single photon coating detectors increases drastically with the collecting area and improved angular resolution, but noise figures have to be on the lowest possible level, new detector schemes must be developed: Active pixel sensors (APS) for X-ray detection have the capability to randomly select areas of interest and to operate at noise levels below 1 electron (rms). About 1000 frames per second can be read out with a relatively low level of electric power with the proposed DEPFET arrays. One prominent candidate for the use of an APS is ESA's XEUS 0 the X-ray Evolving Universe Spectroscopy mission. It represents a potential follow-on mission to the cornerstone XMM-Newton, currently in orbit. The XEUS mission is considered as part of ESA's Horizon 2000+ program within the context of the International Space Station (ISS).
Silicon Drift Detectors (SDDs) with integrated readout transistors combine a large sensitive area with a small total readnode capacitance and are therefore well suited for high resolution, high count rate X-ray spectroscopy. The low leakage current level obtained by elaborated process technology makes it possible to operate them at room temperature or with moderate thermo-electric cooling. The monolithic combination of several SDDs to a multichannel drift detector solves the limited of size and allows for the realization of new physics experiments and systems. Up to 3 cm2 large SDDs for spectroscopic applications were fabricated and tested. Position sensitive X-ray systems are introduced. The description of the device principle is followed by the introduction of the multichannel drift detector concept. Layout, performance and examples of current and future applications are presented.
Fully depleted silicon pn-CCDs with an active thickness of 300 micrometers exhibit a quantum efficiency of 90 percent at a wavelength of 1 micrometers in the near IR. The multi-parallel readout architecture allows for a frame time shorter than 2 ms for a device having a format of 256 by 256 pixel. It can be operated in a full frame mode and in a frame store mode. The pixel size is 50 micrometers by 50 micrometers . The active area is then 12.8 by 12.8 mm2. Cooled down to -90 degrees C the electronic noise floor is below 5 electrons at 50 Megapixel per second. Quantum efficiency measurements will be shown as well as the physical models of the radiation entrance window. A camera system with comparable specifications - except for the pixel size - was already fabricated for ESA's XMM-NEWTON satellite mission, which was launched in early December 1999. The active size of the detector is 60 by 60 mm2 with a readout time of 4 ms. Future work includes the extension of the active area to 1000 by 1000 pixel, monolithically fabricated on a high resistivity 6 inch silicon wafer. The main driver for this development is ESA's planned XEUS mission, to be launched at the end of the next decade.
XMM-Newton, the most powerful X-ray telescope ever built was launched from the european space port Kourou on december 10 last year. Three large X-ray Wolter type mirror systems are focusing the incoming X-rays from 100 eV up to 15,000 eV onto the focal instruments: fully depleted backside illuminated pn-CCDs and frontside illuminated MOS-CCDs. The concept of the pn-CCD camera will be briefly described and its performance on ground and in orbit will be shown. Special emphasis will be given to the radiation hardening of the devices, to the instrument background and to the experience of charged particle background in space. A comparison of the performance on ground and after 5 months in space will be shown.
On 10th December 1999, the European X-ray satellite XMM, now called XMM-Newton, was successfully put into orbit. After initial commissioning of the satellite's subsystems, the EPIC-pn camera was switched on and tested thoroughly in the period Jan./Febr. 2000. After refining of some of the parameter settings and the on-board pn-computer programs, we started the Calibration and Performance Verification Phase, which will last until the end of May 2000. In this paper we report on the results of the EPIC-pn Commissioning Phase with respect to the in-orbit performance of the camera. We also show some of the early results with the pn-camera, the first light image of a region in the Large Magellanic Cloud, and an observation of the Crab Nebular.
Large format arrays covering a wide bandwidth from 1 eV to 25 keV will be used in the focal plane of X-ray telescopes as well as in adaptive optics systems. As the readout speed requirements increase drastically with the collecting area, but noise figures have to be on the lowest possible level, CCD-type detectors do not seem to be able to fulfill the experiment expectations. Active pixel sensors (APS) have the capability to randomly select areas of interest and to operate at noise levels below 1 electron (rms). One prominent candidate for the use of an APS is XEUS: The X-ray Evolving Universe Spectroscopy mission. It represents a potential follow-on mission to the ESA cornerstone XMM currently in orbit. The XEUS mission was considered as part of ESA's Horizon 2000+ within the context of the International Space Station.
Silicon Drift Detectors (SDDs) with integrated readout transistor combine a large sensitive area with a small value of the output capacitance and are therefore well suited for high resolution, high count rate X-ray spectroscopy. The low leakage current level obtained by the elaborated process technology makes it possible to operate them at room temperature or with moderate cooling. The monolithic combination of a number of SDDs to a Multichannel Drift Detector solves the limitation in size of the single device and allows the realization of new physics experiments and systems. The description of the device principle is followed by the introduction of the Multichannel Drift Detector concept. Layout, performance, and examples of current and future applications are given.
The concept of fully depleted, backside illuminated pn-CCD's with an integrated frame store area for high-speed applications will be presented. The device with a format of 128 by 256 pixel exhibits a readout time faster than 1000 frames per second with an electronic noise of less than 5 electrons. Due to the large sensitive volume of the detector and the development of an ultra-thin radiation entrance window, near theoretical quantum efficiencies are achieved from the ultra violet to the near infrared region. The high speed, low noise and high quantum efficiency makes these devices especially suited for the use as wavefront sensors in adaptive optics systems.
A 6 cm X 6 cm large monolithic charge coupled device has been developed and fabricated as focal plane x-ray detector for the European XMM satellite mission and the German ABRIXAS mission. This spectroscopic silicon detector is denominated pn-CCD because of its use of reverse biased pn- junctions as charge transfer registers, as ultra-thin homogeneous photon entrance window and for the on-chip electronics. Due tot he pn-CCD concept, the whole wafer thickness of 300 micrometers is sensitive to ionizing radiation. The read-out is performed in parallel and needs only 73 ms for the 36 cm2 large detector area. A uniform low noise performance is realized by on-chip integrated JFET electronics. The two best pn-CCDs have been integrated in the flight cameras for XMM and abrixas and extensively tested for the long term operation in space. The presentation comprises the basic concept of the detector, a short description of the flight device and its fabrication, test and operating as well as the key performance parameters. The concluding outlook describes methods of further development of the pn-CCD.
In the near future the European x-ray satellite XMM will be launched into orbit. The satellite is equipped with a PN-CCD camera with a sensitive area of 60 mm X 60 mm, integrated on a single silicon wafer. The same camera is on board of the German x-ray satellite ABRIXAS. The main feature of this camera type is the very good quantum efficiency of more than 90 percent in the energy range from 0.3 to 10 keV and the high time resolution, selectable between 7 microsecond(s) ec and 280 msec. All flight cameras are extensively calibrated, utilizing the long beam test facility Panter in Muenchen, the Synchrotron Radiation Facility beam lines at the Institut d'Astrophysique Spatiale in Orsay, and the PTB beam line at the Bessy Synchrotron in Berlin. We will give an overview of all the calibrations and calibration methods as well as some global results.
The quantum efficiency of the pn-CCD detector on the XMM satellite mission was determined in the spectral range between 150 eV and 15 keV. The unstructured entrance window of the device, which is formed by an ultrathin reverse biased pn-junction, results in an excellent spatial homogeneity with a good spectroscopic performance and high detection efficiency for low energy photons. The large sensitive thickness of the detector guarantees a high quantum efficiency for photons up to 10 keV. We give a review of the calibration techniques applied for quantum efficiency measurements at the Synchrotron Radiation Facility at the Institut d'Astrophysique Spatial in Orsay and the radiometry laboratory of the Physikalisch-Technische Bundesandstalt at the electron storage ring BESSY in Berlin. We summarize the applied data correction such as charge transfer loss and split event recognition and describe the data analysis to conclude in an absolute quantum efficiency of the pn-CCD.
ESA's future x-ray mission, the x-ray evolving ESA's future x-ray mission, the x-ray evolving universe spectroscopy mission (XEUS) is actually under study as a potential successor of the XMM satellite. Its collecting area for x- rays form 100 eV up to 20 eV will be about 200 times larger than compared to XMM. The angular resolution will be improved by a factor of five. The field of view will eventually be as large as 10 arcmin. Novel wide field images are needed to overcome the limitations by the state-of-the- art CCD type detectors, limited due to the high number of x- rays focused into the focal plane. To face the problem of high count rate and large formats with simultaneous good energy resolution and high quantum efficiency we have proposed two new focal plane x-ray detectors: (a) a back illuminated active pixel sensor and (b) a 200 readout channel back illuminated frame store pn-CCD. Both will be fabricated at the MPI semiconductor lab on 500 micrometers high resistivity silicon.
The concept and performance of the fully depleted pn- junction CCD system, developed for the European XMM- and the German ABRIXAS-satellite missions for soft x-ray imaging and spectroscopy in the 0.1 keV to 15 keV photon range, is presented. The 58 mm X 60 mm large pn-CCD array uses pn- junctions for registers and for the backside instead of MOS registers. This concept naturally allows to fully deplete the detector volume to make it an efficient detector to photons with energies up to 15 keV. For high detection efficiency in the soft x-ray region down to 100 eV, an ultrathin pn-CCD backside deadlayer has been realized. Each pn-CCD-channel is equipped with an on-chip JFET amplifier which, in combination with the CAMEX-amplifier and multiplexing chip, facilitates parallel readout with a pixel read rate of 3 MHz and an electronic noise floor of ENC < e-. With the complete parallel readout, very fast pn-CCD readout modi can be implemented in the system which allow for high resolution photon spectroscopy of even the brightest x-ray sources in the sky.
Monolithic arrays of 12 CCDs, 3 by 1 cm2 each, have been developed and produced for the focal plane instrumentation of the European photon imaging camera (EPIC) on XMM and the German ABRIXAS x-ray satellite mission. The design parameters have been optimized to match the properties of the x-ray imaging optics as well as the x-ray intensity, energy bandwidth and characteristic time constants of the objects to observe. The pixel size is 150 by 150 micrometer2; readout is performed in parallel; low noise, spectroscopic performance is realized by on-chip integrated JFET electronics; highohmic, ultrapure bulk material allows full depletion and enhances the efficiency for higher energy x-ray detection. The fabrication process, the layout topology and the operating conditions guarantee for a ten year operation in space without performance degradation.
The pn-charge coupled device (pn-CCD) detector system was developed as the focal plane instrument of an x-ray telescope for the European photon imaging camera (EPIC) on the x-ray multi mirror (XMM) mission. The second cornerstone mission of the European Space Agency's Horizon 2000 plan performs high throughput imaging and spectroscopy of the x- ray sky in the domain of 0.1 keV - 15 keV. The pn-charge coupled device will also be used for a German x-ray astronomy satellite mission, called ABRIXAS (a broad-band imaging x-ray all-sky survey). While XMM will perform pointed observations. ABRIXAS will carry out an all sky survey with imaging telescopes. Both projects are planned to be launched in 1999. The homogeneous coherent sensitive area of the detector consists of a 6 cm by 6 cm large array of 12 pn-CCDs which are monolithically integrated on a single silicon wafer together with the first stage of amplification. The pn-CCD detector has been optimized for high-resolution x-ray spectroscopy and its performance is close to the theoretical limits given by the Fano noise. High quantum efficiency essential for the investigation of faint objects is accomplished over the whole energy range by a thin photon entrance window and a full sensitive detector thickness. A fast readout achieves excellent time resolution for the observation of pulsed x-ray sources and avoids pile- up for bright objects. The relevant performance parameters reflecting the state of the detector development are presented. The radiation hardness of the pn-CCD was verified for the ten year satellite mission. No significant increases in the thermally generated current, charge transfer losses and transfer noise occurred in the temperature range planned for detector operation. A correction of the signal charge losses, which occur already before irradiation in all types of charge coupled devices during the charge transfer to the anodes, is necessary to achieve the highest energy resolution of the detector. Methods to reduce the signal charge losses which were successfully tested, are described.
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.