|
1.INTRODUCTIONDetectors form a cornerstone in the measurement capabilities of space missions, and consequently the European Space Agency (ESA) is always concerned to have the highest possible detector performance available to instrument developers. In this overview we report on the present and future detector development activities for the European Space Agency Science and Earth Observation Program, focusing on the developments in the visible to infrared wavelength range. These developments cover entire new detector developments, evaluation of existing detectors under environmental conditions, and modifications of existing designs. The overall strategic approach uses both technology-push and technology-pull. For example, a new detector development can be linked to a specific mission and therefore, its requirements are based on the mission needs. On the other hand, a detector development can be initiated to increase the TRL of a technology and show that basic performances can be achieved. Currently, three roadmaps have been defined and cover:
The ALFA-NIR and ALFA-Controller roadmap is shown in Figure 1 where the ALFA-N phase 1 and 2 are finished and phase 3 is on-going. For the ALFA-Controller, the phase 1 is finished and the phase 2 is kicked-off. The MWIR/LWIR detector development roadmap is shown in Figure 2. Figure 2Coordinated development activities related to MWIR/LWIR/VLWIR MCT detector developments for both Earth Observation and Science missions ![]() The European CMOS development roadmap initially pursued two themes:
Science/astronomy applications – low noise Following changes in the European foundry landscape, only the low flux development is now on-on-going. However, the remit of the low flux CIS development has been expanded to cover both higher and lower signal applications. The next chapter presents both the detector developments in support of these roadmaps and strategic developments that are in addition. They are sorted as much as possible by wavelength, going from the visible to the infrared. 2.DETECTOR DEVELOPMENTS2.1European low flux CMOS image sensorThe low-flux CIS activity began in early 2016 led by Caeleste (Belgium). Caeleste is responsible for the design of the chip and LFoundry (Italy) for the manufacturing. The goal of the activity is to develop a radiation hard, charge domain global shutter, high dynamic range pixel for low flux / high flux space applications. The initial sensor design (see Figure 3) is back-thinned and has the following specification:
Figure 3Left: Frontside chip of the European Low-Flux CIS packaged on chip-on-board. Right: detector architecture ![]() In 2017, first images were acquired using the first front side illuminated samples. However, unexpected high pining voltages were measured on test structures. As a result, a second run of wafers with optimized implantations started and currently the backside thinning of those new wafers is taking place. First backside packaged samples are expected to be ready by end of 2018. 2.2High-performance silicon visible hybrid CMOS image sensorIn addition to monolithic CMOS image sensors, the Agency seeks for developing a hybrid CMOS visible image sensor. Being hybrid, the manufactured detector is less sensitive to parasitic light and allows for separate optimization of the ROIC and the photodiode layer. The goal of the activity is to demonstrate the potential of hybrid technology for high-performance silicon visible CMOS image sensors. The activity was granted to Teledyne-e2v (UK) and Leonardo (UK). The design of a dedicated ROIC was considered to be out of the scope of this activity. Efforts are instead focused on the photodiode design and the hybridization. The requirements are defined as follows: The first run of manufacturing of the photodiode wafer, the post processing of ROIC wafer and the hybridization are completed (see Figure 4). The first packaged samples are under test and the first image was acquired. The second manufacturing run implementing small corrections on the design and process is currently taking place. The new batch of wafers are in progress and wafers are at the backthinning step. In October 2018 first packaged devices will be available. 2.3Performance characterization and comparison of P-channel and N-channel CCD devicesThis study explores the defects created in both N- and P-channel CCD204s when irradiated by protons, looking at defect type and mobility post-irradiation. Two irradiations were performed under cryogenic conditions (at 153K and 203K), with the devices held at mid-point temperature (173K) between irradiations. The performance characterization was held for three weeks at each temperature. The study was led by the Open University and the results are presented in [1]. The devices were tested pre- and post-proton irradiation for opto-electronic performance and showed comparable results. The study indicates that P-channel CCDs are superior in post-irradiation performance to N-channel CCDs for certain in-flight operating conditions and could increase operational mission lifetime due to their robustness against radiation damage (see Figure 5). Additionally, the activity brought new knowledge of trap species and densities in both N- and P-channel CCDs, which are an important asset for the design of future scientific instruments. 2.4Curved detectorsCurved focal plane detectors offer a well-known method for simplifying the optical design without sacrificing performance for many applications. The reduction in mass and volume offered by the utilization of such detector arrays can clearly help in achieving these key objectives of space instrument design. The aim of this activity is to demonstrate that existing, high-performance 2D detector arrays (CCD or CIS), already used in space applications, can be successfully curved and still meet both performance and environmental requirements. This activity encompasses the following tasks:
The contract is currently under negotiation, will start in Q3 2018 and is foreseen to be finished mid 2019. 2.5The ALFA programIn 2010, the Agency initiated an ambitious, multi-activity program to develop a large-format (2k × 2k pixels) NIR detector array and associated control ASIC (application specific integrated circuit). The key aims of this program are to develop a photon to space wire system according to the roadmap shown in Figure 1. The detector tested [2] at the end of phase two (see Figure 1) showed very promising results (see Figure 7). The best detector, the CEA/LETI (FR) LPE device (640*512 pixels, 15μm pitch), has been proton and then gamma irradiated. The results after the proton radiation are presented in [3] and show an increase of only 24% of the dark current after irradiation up to a fluence of 2.27e11p+ .cm-2. The program is at present in phase three led by Sofradir (FR) [4] and has the goal to design, manufacture and characterize a large format 2D array MCT array (shown in Figure 6) with the following parameters:
The detailed design review has been completed successfully and the ROIC is under manufacture with the foundry. It is expected to be delivered in July this year with first ROIC level results available in the autumn. Control ASIC developmentsThe Agency is supporting the development of versatile control ASICs to be able to control and read out a CMOS based detector. In this context, two separate activities are on-going. The first one targets Earth Observation applications and the second one Science/Astronomy applications and in particular the ALFA-N detector as shown in Figure 1. The Earth Observation targeted activity is run by Ideas (Norway) developing the NIRCA mkII. This ASIC shall be (see Figure 8) capable of providing clocks and bias voltages to operate the detector as well as providing video processing and digitisation (16 channels, 14 bit, up to 12 Msps), leading to a two-chip detection system (ASIC + detector). The NIRCA mkII is designed to be interface-compatible as a minimum with the Sofradir NGP detector and the Leonardo ME950. The critical design review is planned for November 2018. The Science oriented activity aims to further develop a cryogenic, control and digitization application specific integrated circuit predominantly for optimized large area NIR/SWIR detector hybrids. After the phase 1 of the activity a prototype ASIC developed by Caeleste (BE) has been tested [5] using a dedicated test setup at ESTEC (see Figure 9). For the second phase, after reissue, the activity is run by Caeleste with a kick-off in June 2018. It shall contain 36 video channels at a read-out speed of 100kHz at 16-bit/5MHz at 12-bit. It foresees a programmable seqencer for clocks and bias. The completion of the activity is scheduled for end of 2019. 2.6Optimization of long, modular linear InGaAs imagers.This activity aims to develop the next generation of long-linear InGaAs arrays with improved noise performance for commercial applications. This activity was granted to Xenics in Belgium. The specifications are the following:
The heritage of this activity is the previous successful development for the Proba-V sensor with 3000 pixels, 25μm pitch and wire bonded. In the on-going activity, where the flip chip approach is replacing the wire bonding, currently a demonstrator with one 2k linear InGaAs chip wire bonded on a PCB is successfully fabricated. An appropriate custom ceramic package has been developed (see Figure 10). The noise optimization of the camera hardware/software and full characterization is on-going. 2.7Development of Low Dark Current MWIR/LWIR detectorsThis development runs with two parallel contracts. The first one is led by AIM (DE) with Caeleste (BE) designing the ROIC and University of Cardiff (UK) for the characterization. The second one is led by Sofradir (FR) with CEA-LETI and CEA-SAP (FR) for design and characterization of the detectors. The study is performance oriented and does not focus on any specific MCT technology or and specific ROIC architecture. The key requirements for the activities are:
Sofradir have manufactured the detectors and started the characterizations of the chosen ROIC. In order to reach the 40K operating temperature, the setup has been updated and the characterization of the hybrid will start in the coming months. In the AIM activity, also a design of a new ROIC with 4 read out segments (7T-CTIA, 5T-CTIA non-rad, 5T-CTIA rad-hard, SFD) has been developed. Characterization of the final demonstrators (n-on-p and p-on-n MCT materials) is on-going in Cardiff University. First results are very promising for the improvement of the dark current. 2.8Low Dark current VLWIR T2SL Infrared detectorsThe goal of the activity is to evaluate T2SL (type-II superlattice) detectors for space applications through the design, manufacture and test of high performance, low dark current VLWIR detector arrays using COTS ROIC and compare them with established technology. The tested devices from IRNOVA (SE) have the following specifications:
The growth development, process development and detector fabrication/evaluation are in progress (see Figure 11). Figure 11Left: FLIR Indigo ISC0208 ROIC mounted on a LCC68 socket, before integration in ADS test set-up for electrical functional test. Right: Schematic depicting the band structure of the absorption region in a GaSb-InAs type II strained superlattice device. ![]() The detailed design review took place in November 2017, but the best design option requires non-standard ROIC, therefore additional funding will be injected in the activity. 2.9Evaluation of MCT APD Detectors for future space applicationsFuture astronomy missions require a low dark current, but in particular a very low noise contribution from the readout noise. In the standard photodiode architecture, the readout noise main contributor is coming from the first stage of the amplification. The technology offered by Avalanche Photodiode (APD) allows reducing the readout noise by creating an internal amplification where the photoelectrons are created under a high electric field. Current APD application are targeted to ground base astronomy [6], but this technology is also promising for future space missions. The goal of the activity is to test and characterize existing European MCT APD arrays in a radiation environment. The selected device is the ‘Saphira’ from Leonardo (UK) (see Figure 12) with the following performances: A total of two irradiation campaigns have been performed: The analysis of results is concluded and no degradation in performance has been observed for TID up to 28 krad (biased) and 56 krad (unbiased). Although some technical difficulties with the proton test occurred, no degradation was observed for irradiation up to 5.92E10 p/cm2 at 62 MeV. 2.10Copernicus pre-developmentsIn the frame of the “Copernicus Space Component Expansion” programme new missions have been identified by the European Commission (EC) as priorities for implementation in the coming years by providing additional capabilities in support of current emerging user needs. As part of the preparatory activities for the evolution of Copernicus, Phase A/B1 studies are being undertaken for 6 high priority candidate Expansion Sentinels, namely:
Each of the three optical candidate missions is accompanied by a dedicated detector pre-development programme. It is initiated in order to support the fulfillment of the mission goals, but also to build up future capabilities. CHIME detector pre-developmentThe Copernicus Hyperspectral Imaging Mission for the Environment (CHIME) [8] aims to augment the Copernicus space component with precise spectroscopic measurements to derive quantitative surface characteristics supporting the monitoring, implementation and improvement of a range of policies in the domain of raw materials, agriculture, soils, food security, biodiversity, environmental degradation and hazards, inland and coastal waters, snow, forestry and the urban environment. The pre-development of a detector optimised for meeting the mission needs of the Hyperspectral Imaging Mission is being initiated. The major improvement required with respect to existing detectors is the development of large detector arrays covering the visible to short-wave infrared while supporting a high frame rate. Such detectors with performance optimised for this mission are currently not available from European suppliers. Key requirements of the CHIME detector pre-development are:
The contract has been awarded to AIM (DE), the kick-off took place begin of August 2018. The requirements review is foreseen for end of August 2018. The overall planned duration of the baseline activity is 24 months. CO2M detector pre-developmentThe Anthropogenic CO2 monitoring (CO2M) mission aims to analyse through the use of CO2 satellite imagers the man-made CO2 emissions and overall CO2 budget at country and regional/megacity scales. Key requirements of the CO2M detector pre-development are:
The activity is expected to kick-off in November 2018 and the overall planned duration of the baseline activity is 24 months. LSTM detector pre-developmentThe High Spatio-Temporal Resolution Land Surface Temperature (LST) Monitoring Mission shall be able to complement the current visible (VIS) and near-infrared (NIR) Copernicus observations with high spatio-temporal resolution Thermal Infrared observations over land and coastal regions. Key requirements of the LSTM detector pre-development are:
The pre-development is expected to kick-off in September/October 2018 and the overall planned duration of the baseline activity is 24 months. 3.CONCLUSIONSThe European Space Agency recognizes the importance of not only improving and optimizing the performance of detectors but also in supporting their continued availability. To this end, ESA continues to develop and maintain its strategic approach to detector developments, using both technology-push and technology-pull, through both internal and external consultation, resulting in the initiation of targeted detector development activities across the waveband. REFERENCESNathan L. Bush, et al.,
“A comparison of proton damage effects on P- and N-Channel CCDs I: performance following cryogenic irradiation,”
in SPIE Astronomical Telescopes + Instrumentation,
(2018). https://doi.org/10.1117/12.2313447 Google Scholar
P-E. Crouzet, et al.,
“First characterization of the NIR European Large Format Array detectors at ESTEC,”
in SPIE,
(2015). Google Scholar
D. Gooding et al.,
“Large format array NIR detectors for future ESA astronomy missions: characterization and comparison,”
in Proceedings,
(2016). https://doi.org/10.1117/12.2231179 Google Scholar
Bruno Fièque, et al.,
“Development of astronomy large focal plane array “ALFA” at Sofradir and CEA,”
in SPIE Astronomical Telescopes + Instrumentation,
(2018). https://doi.org/10.1117/12.2311713 Google Scholar
F. Lemmel et al.,
“Large format array controller (aLFA-C): tests and characterisation at ESA,”
in Proceedings,
(2016). Google Scholar
Dani Atkinson; Donald Hall; Christoph Baranec; Ian Baker; Shane Jacobson and Reed Riddle,
“Observatory deployment and characterization of SAPHIRA HgCdTe APD arrays,”
in Proc. SPIE,
(2014). https://doi.org/10.1117/12.2056807 Google Scholar
Peter R. Roelfsema, et al.,
“SPICA: a joint infrared space observatory,”
in SPIE Astronomical Telescopes + Instrumentation,
(2018). Google Scholar
Nieke, J. and M. Rast,
“Towards the Copernicus Hyperspectral Imaging Mission (CHIME),”
(2018). https://doi.org/10.1109/IGARSS.2018.8518384 Google Scholar
|