Detectors are very often a performance-limiting component for space instrumentation – the better the detector, the better the instrument performance. Consequently, the European Space Agency (ESA) invests significant resources into the development of high-performance detector solutions for current and future missions. While technology developments span the full electromagnetic spectrum, infrared (and visible) wavebands are of particular interest and this paper presents a detailed overview of infrared detector development activities currently being undertaken by ESA in collaboration with European industrial partners.
The exposure of Charge-Coupled Devices (CCD) to high-energy particles in space leads to a degradation of their performances. One of the observed mechanisms is the creation of defects in the CCD silicon lattice by displacement damage, inducing a reduction of the Charge Transfer Efficiency (CTE), i.e. the ability of the device to efficiently transfer the photo-induced charge to the read-out output node. Hence a reduction of the imaging quality of the detector. We present here a comparison of the modelled and measured optical quality of the FLEX CCD exposed to a high energy proton flux. The optical quality was directly measured on an irradiated flight representative device. A physical model of the detector, including an accurate modelling of the charge trapping dynamic, is used to generate synthetic scenes affected by CTE degradation from which the optical quality is assessed and compared to the measurement. Eventually the correlation of the model and the measurement will allow to accurately assess the performances of a detector exposed to space radiation environment.
Detectors play a crucial role for the instrument design and the achievable instrument performance. The wavebands of interest for remote sensing are the visible and the infrared. Therefore, the European Space Agency has a strong interest in the performance enhancement of detector arrays in those spectral ranges. The Agency follows a continuous development strategy to enhance the capabilities for future Earth observation and astronomy missions. This paper presents the technical and planning status of these detector technology development activities.
The European Space Agency strongly supports detector development in Europe from the gamma ray up to the far-infrared wavelengths. The requirements associated to these detector developments are linked to the spatial environment and the needed instrument performance. This paper reports on the status of these developments, the roadmap and the actual performance of the manufactured devices.
The ESA EarthCARE satellite mission objective is the observation of clouds and aerosols from low Earth orbit. The key spatial context providing instrument within the payload suite of 4 instruments is the Multi- Spectral Imager (MSI). This paper discusses the test program developed and implemented at SSTL for the formal qualification of the COTS micro-bolometer detectors for the TIR camera of the MSI. The comprehensive test campaign for the qualification of the detectors covered full electro-optical characterisation, life tests, environmental testing (thermal and mechanical), Particle Impact Noise Detection (PIND) tests, destructive physical analysis (DPA) and radiation tolerance assessment. Testing was undertaken at the specialist detector test facilities at SSTL. External facilities were called on for aspects of the programme. We describe the microbolometer arrays tested, the test benches developed for the program, test facilities, the test procedures and a summary of the test results. The qualification programme was completed in May 2014.
Frédéric Lemmel, Jörg ter Haar, John van der Biezen, Ludovic Duvet, Nick Nelms, Sander Blommaert, Bart Butler, Cornelis van der Luijt, Jerko Heijnen, Hans Smit, Ivo Visser
KEYWORDS: Sensors, Cryogenics, Prototyping, Calibration, Clocks, Control systems, Video, Digital clocks, Signal detection, Field programmable gate arrays
For future near infrared astronomy missions, ESA is developing a complete detection and conversion chain (photon to SpaceWire chain system):
Large Format Array (aLFA-N) based on MCT type detectors.
aLFA-C (Astronomy Large Format Array Controller): a versatile cryogenic detector controller.
An aLFA-C prototype was developed by Caeleste (Belgium) under ESA contract (400106260400). To validate independently the performances of the aLFA-C prototype and consolidate the definition of the follow-on activity, a dedicated test bench has been designed and developed in ESTEC/ESA within the Payload Technology Validation group. This paper presents the test setup and the performance validation of the first prototype of this controller at room and cryogenic temperature. Test setup and software needed to test the HAWAII-2RG and aLFA-N detectors with the aLFA-C prototype at cryogenic temperature will be also presented.
The European Space Agency has a very strong interest in the performance enhancement of detector arrays for future scientific and astronomy missions. Improvements in Visible and Infrared wavelengths are of particular interest and the Agency undertakes a programme of continuous development aimed at enhancing the capability of detectors in these wavebands. This paper presents the status of these detector technology development activities.
Remote sensing is a priority activity for the European Space Agency and detector performance is a crucial factor in determining how well this role is performed. Consequently, the Agency has a strong interest in continuous improvement of both detector capabilities and availability within Europe. To this end, ESA maintains a number of strategic detector development plans combining both technology-push and technology-pull. The visible and infrared wavebands are of particular interest for remote sensing activities and this paper sets out the requirements for current and future missions and presents details of the Agency’s current and planned detector developments.
We report on the present and future detector development activities for the European Space Agency Science Programme. The development of European technology in that field is a key mission enabler for the program, which requires TRL6 (ISO scale) by end of the definition phase, so called "mission adoption". This is particularly true for Astronomy and fundamental physics type missions. Current activities are in particular targeting large format and p-channel CCD, NIR and MWIR, LWIR wavelength ranges as well as related ASIC controller. For the longer term future mission plan (so called M4, M5 and L2 missions, M3 being PLATO and L1 JUICE), the extreme ends of the spectrum will be addressed. An overview of the detector status for the Earth Observation program is given in appendix, as most of the technologies are directly applicable to some extent to science missions, in particular for Planetary missions. The specific validation activities in place in the future mission preparation office in support to the space science program will be eventually briefly detailed.
The Geostationary Earth Radiation Budget (GERB) instrument is an Earth observing scientific payload launched on-board the European Space Agency Meteosat Second Generation (MSG) satellite in September 2002. The instrument measures reflected and emitted radiation in two wavebands, 0.3 - 4 μm and 4 - 30 μm. The focal plane consists of a 256-element thermoelectric linear array operating at ~300 K and four application specific integrated circuits (ASIC) providing parallel amplification, filtering and digitisation. This paper describes in detail the design, operation and performance of the GERB focal plane array.
We have fabricated a new experimental pixel array using 2mm-thick CdZnTe. The trial arrays have been bump-bonded to the Rockwell PICNIC readout IC which provides low noise read out of pixel signals. First measurements are presented from the detector characterisation, which in particular, demonstrate that a very high bond yield (>99%) was
achieved. It is envisaged that these detectors will be suitable for future X-ray astronomy and planetary missions as well as ground based applications such as non-destructive testing, threat detection and baggage scanning.
Mark Sims, D. Pullan, George Fraser, S. Whitehead, J. Sykes, J. Holt, Gillian Butcher, Nick Nelms, J. Dowson, D. Ross, C. Bicknell, M. Crocker, B. Favill, Alan Wells, L. Richter, H. Kochan, Hans Hamacher, L. Ratke, Andrew Griffiths, A. Coates, N. Phillips, A. Senior, John Zarnecki, M. Towner, M. Leese, M. Patel, C. Wilson, Nicolas Thomas, S. Hviid, Jean-Luc Josset, G. Klingelhoefer, B. Bernhardt, P. van Duijn, G. Sims, K. Yung
The performance of the PAW instrumentation on the 60kg Beagle 2 lander for ESA’s 2003 Mars Express mission will be described. Beagle 2 will search for organic material on and below the surface of Mars in addition to a study of the inorganic chemistry and mineralogy of the landing site. The lander will utilize acquisition and preparation tools to obtain samples from below the surface, and both under and inside rocks. In situ analysis will include examination of samples with an optical microscope, Mossbauer and fluorescent X-ray spectrometers. Extracted samples will be returned to the lander for analysis, in particular a search for organics and a measurement of their isotopic composition. The PAW experiment performance data will be described along with the status of the project.
The Geostationary Earth Radiation Budget (GERB) instrument employs a 256 element thermoelectric linear array. As part of the read-out electronics, a custom ASIC has been developed which provides parallel signal processing and digitization for 64 detector pixels. Four of these ASICs combine to provide complete detector read-out, culminating in a single serial digital interface for data output. We present details of the operation and performance of the ASIC achieved as part of the GERB focal plane assembly (FPA).
The construction and testing of the detector system for the Geostationary Earth Radiation Budget (GERB) instrument has proved to be technically challenging in a number of areas. The detector system consists of an uncooled linear array of 256 thermoelectric pixels with 4 Application Specific Integrated Circuits (ASICs) to perform front end analogue signal processing, A/D conversion and multiplexing. The design of the detector and of the ASICs represents considerable development effort to meet, in particular, requirements of low noise and broad band spectral response and the designs have been presented in previous papers. The assembly and integration of the components into a suitably packaged flight focal plane assembly (FPA) has also been challenging, requiring a solution which would allow for individual testing of components before commitment to assembly into the focal plane package. Having assembled and qualified several detector systems, the characterization and performance of the flight detector system is presented in this paper.
D. Anagnostopoulos, M. Augsburger, Gunther Borchert, D. Chatellard, Michael Daum, J.-P. Egger, Detlev Gotta, P. Hauser, P. Indelicato, E. Jeannet, K. Kirch, Nick Nelms, O. Schult, T. Siems, Leopold Simons, Alan Wells
An experiment is described which aims to determine the pion mass to 1 ppm or better, from which a new determination of the upper limit of the muon neutrino mass is anticipated. The approach utilizes spectroscopy of X-ray emissions from pionic atoms formed in gaseous targets. The spectroscopy is performed with a Bragg crystal spectrometer, with an energy resolution of approximately 300 meV, using an array of X-ray CCDs mounted at the focus to measure the spectral line structure of the 4 keV pionic nitrogen transition. To achieve sub-ppm accuracy, as energy calibration a muonic oxygen transition is used. It is known with a precision of 0.3 ppm and almost coincides in energy with the pionic transition.
The Geostationary Earth radiation Budget (GERB) instrument will play an important role in Earth Observation Science, when it is launched on ESA's Meteosat Second Generation (MSG) satellite in 2000. The purpose of the instrument is to measure the reflected and emitted radiation of the Earth over at least a five year period, to an accuracy better than 1% within a 15 minute observation period. These scientific requirements have resulted in a detector system comprising several technological advances. The detector chosen for this instrument is a 256 pixel linear array of thermoelectric (TE) elements operating at room temperature. Based on an existing commercial design, the detector has pushed micromachined thermoelectric arrays to its limits to achieve the noise requirements. The spectral requirements of the instrument to give a flat spectral response over the 0.32 - 30 micrometer range has necessitated the blacking of the TE array. Blacking such small area arrays is a novel application and presented several problems during the course of the development. The signal conditioning electronics, consisting of 4 Application Specific Integrated Circuits, performs front end analogue signal processing, A/D conversion and multiplexing. The design of the detector system is presented in this paper, with the packaging, signal processing and blacking described in some detail.
The Geostationary Earth Radiation Budget (GERB) instrument is to be flown on ESA's Meteosat Second Generation (MSG) satellite in 2000. The purpose of the instrument is to measure accurately the daily cycle of the reflected and emitted radiation of the Earth over at least a five year period. The measurements will be made from geostationary orbit and will complement those planned from instruments in low Earth polar orbits. The data from GERB will provide the first consistent measurements of the hour-by-hour variation of clouds and simultaneous measurements of the radiation balance, and will allow climate models to be further developed and validated. The instrument will accumulate images of the Earth disc every 15 minutes in wavebands of 0.32 - 4.0 pm and 0.32 - 30 im with a nadir resolution of 50 km. The detector for this instrument consists of a 256 pixel linear array of thermoelectric (TE) elements. The TB array operates at room temperature and is blacked to give a flat spectral response over the 0.32 - 30 im band. The detector hybrid consists of the 256pixel detector plus 4 Application Specific Integrated Circuits (ASICs), comprising 64 channels each, which perform front end analogue signal processing, A/D conversion and multiplexing. As the MSG platform is spin-stabilised, the Earth image is stabilised on the detector using a de-spin mirror and is only present on the detector for 40 ms. Integration of the signal over the 40 ms and taken over a 15 minute observation period enables the radiance in both long and short wavebands to be measured to an accuracy better than 1%. The detector concept is described and test results of a prototype system are presented. Keywords: JR detectors, thermoelectric, gold black, EOS
The x-ray mirror calibration program for the JET-X telescope on spectrum-X has recently been carried out at the 130 m long Panter x-ray beam line of the Max Plank Institute fur Extraterrestriche Physik. The excellent spatial resolution achieved with these mirrors, 15 arcsec half energy width (HEW) at 1.5 keV and 19 arcseconds at 8 keV, has proved to be difficult to measure precisely using previously established calibration methods (involving either slit detectors or the ROSAT PSPC imaging proportional counter). New diagnostic techniques have, therefore, been developed using a CCD imaging camera which utilized newly available x- ray CCD technology. Details of the calibration technique and the performance of the camera are provided and results are compared with those obtained from the slit and PSPC detectors.
The microelectronics and photonics test bed (MPTB) operated by NRL is intended to provide an experimental platform for the evaluation of the effects of radiation damage on advanced microelectronic circuits and photonic devices. While several systems exist to monitor the accumulation of dose from ionizing radiation in space, little attention has been given to the accumulation of bulk damage in semiconductors. This is of increasing concern when using sensitive detectors for example for astronomical imaging or star-sensing. The bulk damage monitor experiment is designed as a prototype module to monitor the accumulation of bulk damage and uses a sensitive linear charge coupled device in a system designed to accurately monitor the effect of non- ionizing radiation. The experiment, which is light weight, with very low average power consumption and telemetry volume, may form one element in future dosimetry systems on- board spacecraft.
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