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<p>The main objective was to design and manufacture a multi-channel high resolution analog-digital converter for digitizing a CCD image signal. The tasks included schematic capture, simulation, layout and verification leading to a GDSII foundry ready database. The chip was sent for manufacture in August 2012 and silicon was received in October 2012.</p>

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"We propose to develop a revolutionary x-ray camera for astrophysical imaging spectroscopy. High-resolution x-ray spectroscopy is a powerful tool for studying the evolving universe. Emission line ratios (e.g. within the He-like triplet) provide density and temperature diagnostics. Emission and absorption line energies identify ions and determine their velocities, and the shape of the lines can be used to study turbulence or the relativistic effects of a supermassive black hole. The grating spectrometers on the XMM and Chandra satellites demonstrated the power of high-resolution x-ray spectroscopy for astrophysics, but there remains a need for instrumentation that can provide higher spectral resolution with high throughput in the Fe-K band and that can enable spatial/spectral investigations of extended sources, such as supernova remnants and galaxy clusters. The instrumentation needed is a broad-band imaging spectrometer - basically an x-ray camera that can precisely resolve x-ray energies and fluxes over a large field-of-view. While we do not claim that in 3 years we will have developed such detectors, we advocate developing the technology that has the greatest potential for achieving this. Theoretically, magnetically-coupled microcalorimeters are best equipped to achieve sub-eV energy resolution in very large formats. We propose to build upon the work carried out by our group on metallic magnetic calorimeters (MMC) in the antecedent program. The great promise of MMCs for sub-eV energy resolution has been recognized for years. During our current research program, an accident in detector fabrication produced devices that derived their sensitivity from a different operating principle - the temperature dependence of a superconduc

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MODIS (or Moderate Resolution Imaging Spectroradiometer) is a key instrument aboard the Terra (EOS AM) and Aqua (EOS PM) satellites. Terra's orbit around the Earth is timed so that it passes from north to south across the equator in the morning, while Aqua passes south to north over the equator in the afternoon. Terra MODIS and Aqua MODIS are viewing the entire Earth's surface every 1 to 2 days, acquiring data in 36 spectral bands, or groups of wavelengths (see MODIS Technical Specifications). These data will improve our understanding of global dynamics and processes occurring on the land, in the oceans, and in the lower atmosphere. MODIS is playing a vital role in the development of validated, global, interactive Earth system models able to predict global change accurately enough to assist policy makers in making sound decisions concerning the protection of our environment.

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We propose the development of a physical-vapor-deposition coating technique to correct residual figure errors in grazing-incidence optics. The process involves selectively depositing a filler material to smooth out the low-to-mid-spatial-frequency errors that typically dominate the performance of x-ray optics. We have demonstrated proof-of-concept on small (few-cm scale) full-shell optics intended for medical imaging. We propose here to scale the process up to larger mirrors applicable to astronomy. Simulations indicate that given adequate metrology, substantial improvements in angular resolution are possible through application of the technique. The process is applicable to full shell or segmented optics, either mounted or unmounted, and can in principal also be used to figure short reflectors. Examples of programs that could benefit from this technique include the large mission IXO and smaller explorer-class missions such as WFXT.

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<p> We propose a three-year effort to upgrade our existing sub-arcsecond Lyman-alpha telescope payload to improve the observing cadence by a factor of 2, increase the signal-to-ratio by a factor of 4, and launch the payload twice. With this upgraded performance, we will be able to investigate a number of scientific questions regarding the structure and heating of the solar atmosphere that address NASA’s Strategic Goal to understand the Sun and its effects on Earth and the Solar System. Specifically, the ultra-high resolution and high-temporal cadence VAULT2.0 science program and associated launch campaigns will answer the following five questions:</p> <p> ? <em>What is the role of Type-II spicules in the transfer of energy and mass across the chromosphere-corona interface? </em></p> <p> ? <em>Does neutral plasma absorption of the EUV emission from active region moss explain the discrepancies in the models of coronal loop heating? </em></p> <p> ? <em>Where are the photospheric footpoints of coronal loops? </em></p> <p> ? <em>What is the structure of coronal holes in the Lyman-alpha temperature range? </em></p> <p> ? <em>What is the absolute abundance of H I at the base of the solar wind? </em></p> <p> Despite decades of ground-based observations, the chromosphere remains one of the least understood layers of the solar atmosphere because of our limited understanding of the physical processes that govern it. In the last few years, the chromosphere has been propelled to the forefront of solar physics research thanks to spectacular new observations from space (Hinode/SOT and VAULT), and ground (e.g., SOUP, IBIS, DOT, SST), and the advent of sophisticated numerical simulations which are beginning to address the complex physics of the optically thick chromospheric plasmas and are opening up the interpretation of the observations. With these new capabilities come exciting new ideas regarding the role of the chromosphere in supplying the mass and energy to heat the corona, the nature of filaments, and the contribution of chromospheric jets to the solar wind. These ideas are challenging our traditional views of coronal heating (a long-standing mystery of solar physics), the existence of the ‘transition region’, the role of neutral plasmas in coronal emission and even the dominance of magnetic fields at coronal heights. The recent SMEX selection of a chromosphere-oriented mission, IRIS, is further evidence for the renewed importance of chromospheric physics. Observational limitations, however, are impeding further development and validation of these ideas. <strong>Both theoretical and observational considerations point to the importance of tracing the mass and energy on <em>small spatial scales through the upper chromosphere and transition region </em></strong>(e.g., De Pontieu et al. 2007a, 2009, 2011; Vourlidas et al. 2010). This layer corresponds roughly to the temperature range from 10,000K (ground-based Hα) to 80,000K (space-based HeI). The requirement for high spatial- and temporal-resolution observations in this temperature range cannot be met fully by current instrumentation. Narrow-band, high-resolution images from TRACE, Hinode, STEREO and SOHO have inadequate temperature coverage or poor resolution. The SDO/AIA observations are skewed towards higher temperature plasmas. The SOHO spectrometers CDS and SUMER have good temperature coverage and fidelity, but limited spatial and temporal resolution and more importantly, limited operational lifetime. Hinode/EIS observations are mostly confined to the upper solar atmosphere while SOT observations are confined to the lower chromosphere (≤ 10,000K). The forthcoming IRIS satellite will partially cover the gap between chromosphere and transition region by obtaining high resolution spectra of selected Mg II (< 14,000K), C II (~30,000 K) and Si IV (~80,000 K)</p>

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MODIS (or Moderate Resolution Imaging Spectroradiometer) is a key instrument aboard the Terra (EOS AM) and Aqua (EOS PM) satellites. Terra's orbit around the Earth is timed so that it passes from north to south across the equator in the morning, while Aqua passes south to north over the equator in the afternoon. Terra MODIS and Aqua MODIS are viewing the entire Earth's surface every 1 to 2 days, acquiring data in 36 spectral bands, or groups of wavelengths (see MODIS Technical Specifications). These data will improve our understanding of global dynamics and processes occurring on the land, in the oceans, and in the lower atmosphere. MODIS is playing a vital role in the development of validated, global, interactive Earth system models able to predict global change accurately enough to assist policy makers in making sound decisions concerning the protection of our environment.

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<p>The existing HDWLT (pictured) contoured composite structure design, its analyses and manufacturing tools, will be used to validate key analyses inputs through structure manufacturing, collecting relevant test data and assessing the performance parameters.</p>

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MODIS (or Moderate Resolution Imaging Spectroradiometer) is a key instrument aboard the Terra (EOS AM) and Aqua (EOS PM) satellites. Terra's orbit around the Earth is timed so that it passes from north to south across the equator in the morning, while Aqua passes south to north over the equator in the afternoon. Terra MODIS and Aqua MODIS are viewing the entire Earth's surface every 1 to 2 days, acquiring data in 36 spectral bands, or groups of wavelengths (see MODIS Technical Specifications). These data will improve our understanding of global dynamics and processes occurring on the land, in the oceans, and in the lower atmosphere. MODIS is playing a vital role in the development of validated, global, interactive Earth system models able to predict global change accurately enough to assist policy makers in making sound decisions concerning the protection of our environment.

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AMMOS Technology tasks include: - Enhance mission planning and sequence generation tools with constraint based automated planning and scheduling techniques to enable greater levels of ground automation. - Demonstration of automated mission planning for tactical surface operations - Developing a multi-objective optimization tool for use in science planning for complex observatory scheduling. - An automated method to diagnose spacecraft systems from telemetry, generating models from standard test data and system documentation only - Develop Level 2 data product creation framework for producing atmospheric profiles. The framework will be multimission and will allow subsequent missions to leverage on the implementations of previous missions - Automatic analysis discovers near-invisible signals and rapidly drafts maps of surface materials Develop Orbital stability analysis algorithms, mean element orbit control/sizing algorithms - Develop flexible, reactive, multimission b??smartb? executive for AutoNav/AutoGNC - Develop algorithms to optimize the time of finite burns within a multi-body gravity field. - Develop tools and a handbook to quickly survey and generate low-energy transfers between the Earth and Moon, including transfers to low lunar orbits and three-body orbits. - Develop a strategy using an optimal sequence of flybys and observations to do rapid characterization (shape, gravity, and environment) of small bodies (including binaries) without entering orbit or placing the S/C into an unstable state

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In collaboration with other Directorates and agencies, ASTEP supports investigations focused on exploring the Earth?s extreme environments in order to develop a sound technical and scientific basis to conduct astrobiological research on other solar system bodies. ASTEP is a science-driven exploration program that results in new science and operational/technological capabilities to enable the next generation of planetary exploration. A unique feature that is central to ASTEP is the use of terrestrial field campaigns to further science and technology and NASA?s exploration capabilities. Proposals that integrate science, technology, and field campaign objectives are given priority. In addition to science: - ASTEP seeks the development and application of technologies that support science investigations by enabling remote searches for, and identification of, life and life- related chemistry in extreme environments (including lunar and planetary surfaces). These technologies include, but are not limited to, sample acquisition and handling techniques, sample manipulation, and the use of mobile science platforms (including planetary rovers and astronauts) including techniques for autonomous operations and self-contained deployment systems. (Science instrument technology proposals are supported through ASTID). - ASTEP seeks systems-level terrestrial field campaigns designed to address astrobiology science goals and demonstrate and validate related technologies in remote and/or extreme environments on Earth. Field campaigns are conducted with complete systems and in a manner that approximates operations during an actual planetary mission, providing an opportunity to understand the performance, capabilities, and efficiencies associated with the tested systems while enabling human participants to gain operational experience with those systems in the field. The ASTEP R&A Lead estimates approximately 20% of the funded effort is technology-related ($1.8M of $9M in FY12)

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PPR supports research to improve NASA's understanding of the potential for both forward and backward contamination, how to minimize it, and to set standards in these areas for spacecraft preparation and operating procedures. Improvements in technologies and methods for evaluating the potential for life in returned samples are supported. The PPR R&A Lead estimates that approximately 40% of the effort funded through PPR is technology related, particularly in the following areas: ? The development or adaptation of modern molecular analytical methods to rapidly detect, classify, and/or enumerate the widest possible spectrum of Earth microbes carried by spacecraft (on surfaces and/or in bulk materials, especially at low densities) before, during, and after assembly and launch processing. Of particular interest are methods capable of identifying microbes with high potential for surviving spacecraft flight or planetary environmental conditions (e.g., anaerobes, psychrophiles, radiation-resistant organisms); and ? New or improved methods, technologies, and procedures for spacecraft sterilization that are compatible with spacecraft materials and assemblies. PPR's research areas derive directly from recent National Research Council (NRC) recommendations on planetary protection for solar system exploration missions (see http://planetaryprotection.nasa.gov/documents/ for online reports and a list of publications).