Spatial Light Modulator (SLM) technologies are well established in many application fields over the last decades. Addressing challenging operational conditions, a special class of high-speed SLMs has emerged over the past 20 years, namely Micromirror Array (MMA) devices. Fraunhofer IPMS MMA technology has enabled several ultraviolet photolithography applications at industrial scale. Given the fact that these devices are available for scientific testing, we proposed to explore for the first time their functionality and performance with respect to the space application requirements for the European framework cooperation. Previous studies strongly support this approach with the investigation of several SLM technologies for space instrumentation. In this study, the key parameters of an already available 256 x 256 pixel MMA device have been assessed and its performance has been evaluated under environmental constraints of a future space mission, in terms of temperature (from -40 °C to 80 °C), vacuum (< 10-5 mbar) and vibrations in X-, Y- and Z-axes, showing zero failure rate for the MMA device after all tests. These experimental findings, together with simulations results, confirm the robustness of the MMA technology, especially against temperature changes, and encourage further activities for the development of a space-customized spatial light modulator technology.
Earth Observation (EO) systems are generating an ever-increasing amount of data to be handled on board yet with limited resources, which sometimes hinders a full exploitation of the information content. In this paper, we present a demonstrator of a super-resolved compressive imager operating in whiskbroom mode in the Visible-Near Infrared (VISNIR) and Medium Infrared (MIR) spectral ranges. The demonstrator, which is under development in the frame of the EU H2020 funded SURPRISE project, is based on the use of a Digital MicroMirror Device (DMD) as a core element of its architecture and it is inspired by a single-pixel camera in order to avoid the use of large focal plane arrays. The demonstrator has 10 channels in the VNIR and two channels in the MIR and it can reach a super-resolution factor from 4 x 4 to 32 x 32, that is the ratio between the number of pixels of the image reconstructed at the end of the process and the number of pixels of the detector. Besides, on the grounds of the results obtained by image reconstruction tests on simulated datasets by using Deep Learning based algorithms, data are expected to be natively compressed with a Compression Ratio up to 50%. The study is expected to provide valuable insight for the future development of a novel class of EO instruments with improved performances in terms of ground sampling distance, native compression and on-board processing capabilities. Additional presentation content can be accessed on the supplemental content page.
MAJIS (Moons And Jupiter Imaging Spectrometer) is the VIS-IR imaging spectrometer of the ESA/JUICE mission that will explore the Jovian system. It covers the spectral range 0.5 to 2.35 μm and 2.26 to 5.56 μm using two channels. The MAJIS Optical Head (OH) consists in a TMA telescope shared between the two channels, as well as a slit and collimator, then a dichroic filter that splits the light between the channels, each one being equipped with its own grating and focusing lens. The same type of detector is used for both spectrometers (apart from the order sorting filter), being a 400 pixels × 508 spectels with 36 µm pitch. We will present the characterization of the OH performed at Leonardo Company at cold operational temperatures (from 110K to 150K). The test set-up with a specific emphasis of the Optical Ground Support Equipment (OGSE) used during that characterization campaign will be shortly described. Then, the main performances (spatial, spectral) of the OH will be presented and a comparison with the requirements will be provided.
The need of high-resolution Earth Observation (EO) images for scientific and commercial exploitation has led to the generation of an increasing amount of data with a material impact on the resources needed to handle data on board of satellites. In this respect, Compressive Sensing (CS) can offer interesting features in terms of native compression, onboard processing and instrumental architecture. In CS instruments the data are acquired natively compressed by leveraging on the concept of sparsity, while on-board processing is offered at low computational cost by information extraction directly from CS data. In addition, instrument’s architecture can enjoy super-resolution capabilities that ensure a higher number of pixels in the reconstructed image with respect to that natively provided by the detector. In this paper, we present the working principle and main features of a CS demonstrator of a super-resolved instrument for EO applications with ten channels in the visible and two channels in the medium infrared. Besides the feature of merging in a single step the acquisition and compression phases of the image generation, its architecture allows to reach a superresolution factor of at least 4x4 in the images reconstructed at the end of process. The outcome of the research can open the way to the development of a novel class of EO instruments with improved Ground Sampling Distance (GSD) - with respect to that one provided natively by the number of sensing elements of the detector - and impact EO applications thanks to native compression, on-board processing capabilities and increased GSD.
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