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2011
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The SpaceCube 2.0 is a compact, highperformance, low-power onboard processing system that takes advantage of cutting-edge hybrid (CPU/FPGA/DSP) processing elements. The SpaceCube 2.0 design concept includes two commercial Virtex-5 field-programmable gate array (FPGA) parts protected by "radiation hardened by software" technology, and possesses exceptional size, weight, and power characteristics [5×5×7 in., 3.5 lb (≈12.7×12.7×17.8 cm, 1.6 kg) 5-25 W, depending on the application's required clock rate]. The two Virtex-5 FPGA parts are implemented in a unique back-toback configuration to maximize data transfer and computing performance. Draft computing power specifications for the SpaceCube 2.0 unit include four PowerPC 440s (1100 DMIPS each), 500+ DSP48Es (2×580 GMACS), 100+ LVDS high-speed serial I/Os (1.25 Gbps each), and 2×190 GFLOPS single-precision (65 GFLOPS double-precision) floating point performance. The SpaceCube 2.0 includes PROM memory for CPU boot, health and safety, and basic command and telemetry functionality; RAM memory for program execution; and FLASH/EEPROM memory to store algorithms and application code for the CPU, FPGA, and DSP processing elements. Program execution can be reconfigured in real time and algorithms can be updated, modified, and/or replaced at any point during the mission. Gigabit Ethernet, Spacewire, SATA and highspeed LVDS serial/parallel I/O channels are available for instrument/sensor data ingest, and mission-unique instrument interfaces can be accommodated using a compact PCI (cPCI) expansion card interface. The SpaceCube 2.0 can be utilized in NASA Earth Science, Helio/Astrophysics and Exploration missions, and Department of Defense satellites for onboard data processing. It can also be used in commercial communication and mapping satellites.
Space Telescopes and Instrumentation 2010: Ultraviolet to Gamma Ray, 2010
The Wide Field Imager (WFI) of the International X-ray Observatory (IXO) is an X-ray imaging spectrometer based on a large monolithic DePFET (Depleted P-channel Field Effect Transistor) Active Pixel Sensor. Filling an area of 10 x 10 cm² with a format of 1024 x 1024 pixels it will cover a field of view of 18 arcmin. The pixel size of 100 x 100 µm² corresponds to a fivefold oversampling of the telescope's expected 5 arcsec point spread function. The WFI's basic DePFET structure combines the functionalities of sensor and integrated amplifier with nearly Fano-limited energy resolution and high efficiency from 100 eV to 15 keV. The development of dedicated control and amplifier ASICs allows for high frame rates up to 1 kHz and flexible readout modes. Results obtained with representative prototypes with a format of 256 x 256 pixels are presented.
2010
The Wide Field Imager (WFI) of the International X-ray Observatory (IXO) is an X-ray imaging spectrometer based on a large monolithic DePFET (Depleted P-channel Field Effect Transistor) Active Pixel Sensor. Filling an area of 10 x 10 cm 2 with a format of 1024 x ...
ACM Computing Surveys
Physical Unclonable Function (PUF) has recently attracted interest from both industry and academia as a potential alternative approach to secure Internet of Things (IoT) devices from the more traditional computational-based approach using conventional cryptography. PUF is a promising solution for lightweight security, where the manufacturing fluctuation process of IC is used to improve the security of IoT as it provides low complexity design and preserves secrecy. PUF provides a low-cost low-power solution and can be implemented in both Field Programmable Gate Arrays (FPGA) and Application-Specific Integrated Circuits (ASICs). In this survey, we provide a comprehensive review of the state-of-the-art of PUF, its architectures, protocols and security for IoT.
2018
The Euclid space mission, approved by the European Space Agency, is planned to perform an extensive survey over a 6 years period, beginning end of 2020. The satellite will be equipped with two instruments, a visible imager and a near-infrared spectro-photometer (NISP). These instruments will allow to measure the shape and redshift of galaxies over a large fraction of the extragalactic sky in order to study the evolution of cosmic structures, the accelerated expansion of the Universe and the nature of dark matter. This thesis has been carried out in the context of the INFN team participating in Euclid. I have contributed to the development of a software simulating the Euclid Spacecraft commanding and responding towards the NISP Instrument Control Unit. By this simulator the testing and validation of the functionalities of the Control Unit Application Software are made possible. My PhD activity abroad (6 months) was done at the CPPM Lab in Marseille collaborating with the local group ...
The Scientific World Journal, 2013
The Communications Interface Board (CIB) is an improved communications architecture that was demonstrated on the International Space Station (ISS). ISS communication interfaces allowing for real-time telemetry and health monitoring require a significant amount of development. The CIB simplifies the communications interface to the ISS for real-time health monitoring, telemetry, and control of resident sensors or experiments. With a simpler interface available to the telemetry bus, more sensors or experiments may be flown. The CIB accomplishes this by acting as a bridge between the ISS MIL-STD-1553 low-rate telemetry (LRT) bus and the sensors allowing for two-way command and telemetry data transfer. The CIB was designed to be highly reliable and radiation hard for an extended flight in low Earth orbit (LEO) and has been proven with over 40 months of flight operation on the outside of ISS supporting two sets of flight experiments. Since the CIB is currently operating in flight on the ISS, recent results of operations will be provided. Additionally, as a vehicle health monitoring enabling technology, an overview and results from two experiments enabled by the CIB will be provided. Future applications for vehicle health monitoring utilizing the CIB architecture will also be discussed.
2020
Stratospheric ozone represents only a tiny fraction of the atmosphere, yet is vitally important for life on Earth. Measurements from satellites provided data on the initial decline of ozone in the late 1970s and early 1980s that supported the adoption of the Montreal Protocol, and current observations hint at a potential recovery. Adequate determination of that recovery requires continuous and, in the case of multiple instruments, overlapping data records. However, most current satellite systems are well beyond their expected lifetimes, and are large and expensive to build and launch. A new measurement paradigm is needed to enable cost-effective, sustainable measurements of atmospheric ozone into the 2040s when ozone is expected to recover. The Stratospheric Aerosol and Gas Experiment IV (SAGE IV) is an example of an innovative mission that can sustain a crucial science measurement at a fraction of the costs of traditional, larger missions. SAGE IV is a solar occultation imager capable of measuring ozone, aerosol, and other trace gas species with the same quality as previous SAGE instruments (including SAGE III currently on International Space Station (ISS)), yet takes advantage of recent technological advancements to reduce its overall size, fitting inside a 6U CubeSat bus. This paper describes the SAGE IV instrument.
ПриPONTийский меняла: деньги местного рынка. XI Международный Нумизматический Симпозиум. Материалы научной конференции / Отв. ред. Н. А. Алексеенко. – Симферополь : ИТ «АРИАЛ», 2024.
VUE (Voices in Urban Education)
Revista Brasileira de Farmacognosia, 2014
Prosiding Konferensi Nasional Pengabdian Kepada Masyarakat dan Corporate Social Responsibility (PKM-CSR), 2021
Journal of Neuro-Ophthalmology, 2014
Enfermería Investiga Investigación Vinculación Docencia y Gestión, 2019
Chemosphere, 2009
IEEJ Transactions on Sensors and Micromachines, 2001
Kontakt, 2018