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AirMSPI verison 6 terrain-projected georegistered radiance product acquired during the RADEX flight campaign

AirMSPI_RADEX_Terrain-projected_Georegistered_Radiance_Data is an AirMSPI terrain-projected georegistered radiance product acquired during the Radar Definition Experiment (RADEX) flight campaign.AirMSPI Level 1B2 products contain radiometric and polarimetric images of clouds, aerosols, and the surface of the Earth. In particular, products contain map-projected data at 8 wavelengths: 355, 380, 445, 470, 555, 660, 865, and 935 nm. The data products include radiance, time, solar zenith, solar azimuth, view zenith, and view azimuth for all spectral bands. Wavelengths for which polarization information is available (470, 660, and 865 nm) and include the Stokes parameters Q and U, as well as degree of linear polarization (DOLP) and angle of linear polarization (AOLP). Q, U, and AOLP are reported relative to both the scattering and view meridian planes. Files are distributed in HDF-EOS-5 format.This release of AirMSPI data contains all targets acquired during the Radar Definition Experiment (RADEX) flight campaign, which was based out of Joint Base Lewis-McChord, Washington. The campaign focused on characterizing new radar instruments being tested for future NASA satellite missions with AirMSPI providing additional cloud characterization. AirMSPI data were acquired from November 10 through December 13, 2015.

Investigation of the Chromosphere-Corona Interface with the Upgraded Very high angular Resolution ULtraviolet Telescope (VAULT2.0) Project

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&rsquo;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: ? What is the role of Type-II spicules in the transfer of energy and mass across the chromosphere-corona interface? ? Does neutral plasma absorption of the EUV emission from active region moss explain the discrepancies in the models of coronal loop heating? ? Where are the photospheric footpoints of coronal loops? ? What is the structure of coronal holes in the Lyman-alpha temperature range? ? What is the absolute abundance of H I at the base of the solar wind? 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 &lsquo;transition region&rsquo;, 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. Both theoretical and observational considerations point to the importance of tracing the mass and energy on small spatial scales through the upper chromosphere and transition region (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 H&alpha;) 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 (&le; 10,000K). The forthcoming IRIS satellite will partially cover the gap between chromosphere and transition region by obtaini

Last of the Wild Project, Version 1, 2002 (LWP-1): Last of the Wild Dataset (IGHP)

The Last of the Wild Dataset of the Last of the Wild Project, Version 1, 2002 (LWP-1) is derived from the LWP-1 Human Footprint Dataset. The gridded data are classified according to their raster value (wild = 0-10; not wild >10). The ten largest polygons of more than 5 square kilometers within each biome by realm are selected and identified. The dataset in Interrupted Goode Homolosine Projection (IGHP) is produced by the Wildlife Conservation Society (WCS) and Columbia University Center for International Earth Science Information Network (CIESIN).

Global One-Eighth Degree Population Base Year and Projection Grids Based on the Shared Socioeconomic Pathways, Revision 01

The Global One-Eighth Degree Population Base Year and Projection Grids Based on the Shared Socioeconomic Pathways, Revision 01, data set consists of global urban, rural, and total population data for the base year 2000, and population projections at ten-year intervals for 2010-2100 at a resolution of one-eighth degree (7.5 arc-minutes), consistent both quantitatively and qualitatively with the SSPs. Spatial demographic data are key inputs for the analysis of land use, energy use, and emissions, as well as for the assessment of climate change vulnerability, impacts, and adaptation. The SSPs are developed to support future climate and global change research and the Intergovernmental Panel on Climate Change (IPCC) Sixth Assessment Report (AR6).

Emission Line Astronomy - Coronagraphic Tunable Narrow Band Imaging and Integral Field Spectroscopy. Project

We propose to continue our program of emission line astronomy featuring three areas of emphasis: 1) The distribution and nature of high redshift emission line galaxies, using the Lyman alpha and other rest-frame UV lines; and the study of planetary systems in formation in the first 10 Myrs, with the interplay of circumstellar disks and jets; and spectral differencing of transiting planets. 2) We are extending the capability of our Goddard Fabry-Perot Imager by incorporating a Coronagraphic Integral Field Spectrograph (CIFS), and will continue our observations with the improved instrument. We request support for completing the commissioning of the instrument, and for its maintenance and operation. The CIFS, which has been delivered to the Apache Point Observatory's 3.5-m telescope, consists of a custom microlens array and magnifier section, a grating wheel assembly, and a photon-counting electron-multiplying CCD (EMCCD), within the optical train of the Fabry-Perot. The instrument is switchable between Fabry-Perot and IFS modes. It provides observational support to interpret data from the HST, Spitzer, Chandra, Herschel and soon JWST space observatories with capabilities not available on them, and will be used to develop technology for future NASA flight programs such as WFIRST, and NWO, THEIA, ATLAST and other planet-finding missions. In this period we propose to extend the wavelength coverage of the CIFS, by extending the format of the EMCCD.

The Focusing Optics X-ray Solar Imager (FOXSI): Update & Second Launch Project

Particle acceleration in solar flares and its contribution to coronal heating are among the main&nbsp; unsolved problems in heliophysics. Accelerated electrons in a plasma radiate hard X-ray (HXR)&nbsp; emission through the well-known process of bremsstrahlung. HXR observations therefore are a&nbsp; powerful diagnostic tool, providing quantitative measurements of flare-accelerated electrons. Since&nbsp; bremsstrahlung emission depends on the density of the ambient medium, solar HXR emission is&nbsp; usually brightest from below the transition region, where the density increases rapidly towards the&nbsp; photosphere. Electron beams entering the chromosphere lose energy quickly through collisions and&nbsp; produce relatively intense HXR emission at the footpoints of magnetic field lines. Electron beams&nbsp; moving in the relatively tenuous corona suffer very few collisions, losing little energy and producing&nbsp; only faint HXR emission. Present-day HXR instrumentation does not have the sensitivity to see&nbsp; faint HXR emission from electrons traveling in the corona, nor the dynamic range to see such&nbsp; faint emission in the presence of bright HXR footpoint emission in the chromosphere. Existing&nbsp; observations therefore show us only where energetic electrons are stopped, but not where they&nbsp; are accelerated, nor along what path they escape from the acceleration site. The most sensitive&nbsp; solar HXR observations so far are provided by the Reuven Ramaty High Energy Spectroscopic&nbsp; Imager (RHESSI) (Lin et al. 2002). These measurements are obtained with a non-focusing rotation&nbsp; modulation collimator (RMC) imaging technique (Hurford et al. 2002). RMCs and other types&nbsp; of non-focusing imaging, however, have intrinsically limited dynamic range and sensitivity. HXR&nbsp; focusing optics can overcome both of these limitations (Section 1.2.2).&nbsp; The Focusing Optics X-ray Solar Imager (FOXSI) is a sounding rocket payload funded under the&nbsp; NASA Low Cost Access to Space (LCAS) program to test HXR focusing optics combined with&nbsp; silicon strip detectors for solar observations (Krucker et al. 2009). The FOXSI program is being led&nbsp; by the Space Sciences Laboratory at UC Berkeley in collaboration with the Marshall Space Flight&nbsp; Center (MSFC) and the Japan Aerospace Exploration Agency (JAXA). FOXSI is on schedule&nbsp; and on budget for a launch in October 2010. FOXSI will offer imaging spectroscopy and&nbsp; unprecedented HXR sensitivity and dynamic range. FOXSI will be !100 times more sensitive than&nbsp; RHESSI at 10 keV, and, for the first time, detect the non-thermal counterparts of quiet sun network&nbsp; flares (Section 1.2.4).&nbsp; Here we propose a continuation of the FOXSI program which includes data analysis&nbsp; and a second flight with an upgraded version of FOXSI. At moderate cost, we propose to&nbsp; enhance the effective area, in particular at higher energies (by a factor of !4 at 15 keV), by adding&nbsp; 3 more shells to the existing 7-shell optics (see Figure 9). Furthermore, our Japanese collaborators&nbsp; will provide, at no cost, newly available double-sided cadmium telluride (CdTe) detectors as&nbsp; a replacement for the Si detectors to allow us to take full advantage of the effective area at higher&nbsp; energies. A second flight will therefore not only allow us to continue testing HXR focusing&nbsp; optics for solar observations and also test newly developed CdTe strip detectors&nbsp; in flight but is also expected to provide a significant increase in scientific return. In&nbsp; this two year proposal, the first year (2011) will be used to upgrade the FOXSI payload and to&nbsp; analyze data from the first flight, while the second flight is planned for the midd

Advanced W-Band Gallium Nitride Monolithic Microwave Integrated Circuits (MMICs) for Cloud Doppler Radar Supporting ACE Project

Develop W-band Gallium Nitride (GaN) MMICs to enable the advanced cross-track scanning, dual-frequency Doppler cloud radar concept in support of the Aerosol-Cloud-Ecosystem (ACE) mission. Targeted GaN MMIC component performance goals are: Power amplifier (PA): 1 Watt with 12 dB gain. Low noise amplifier (LNA): &lt;6 dB noise figure with&nbsp;&nbsp;&nbsp;&nbsp; 17 dB gain. Single pole double throw switch (SPDT): &lt;3 dB insertion loss. Phase shifter: 4 bit resolution and &lt;8 dB insertion loss. Integrated MMIC chip with all transceiver front end functions. &nbsp;

Last of the Wild Project, Version 2, 2005 (LWP-2): Global Human Influence Index (HII) Dataset (IGHP)

The Global Human Influence Index Dataset of the Last of the Wild Project, Version 2, 2005 (LWP-2) is a global dataset of 1-kilometer grid cells, created from nine global data layers covering human population pressure (population density), human land use and infrastructure (built-up areas, nighttime lights, land use/land cover), and human access (coastlines, roads, railroads, navigable rivers). The dataset in Interrupted Goode Homolosine Projection (IGHP) is produced by the Wildlife Conservation Society (WCS) and Columbia University Center for International Earth Science Information Network (CIESIN).

Free Form Mirrors for Ultra Compact High Speed Optical Systems Project

This task is to collaboratively design and fabricate the free-form WIRIS telescope primary mirror with our partner Zygo as a technology demonstration. Fabricating the primary is challenging as it has 865 um of aspheric departure and is not rotationally symmetric.

Yup'ik Environmental Knowledge Project (Community Page), Version 1

Since 2000, the Calista Elders Council (CEC) staff has worked with elders from Bering Sea coastal communities to document Yup'ik place names. Elders have been eager to teach young people their rich history and named places of their homeland, including camp and settlement sites, rivers, sloughs, rocks, ponds, even sandbars and underwater channels. More than 3,000 names have been identified with Yup'ik views on the importance of place names, the land, values, and language.Supporting Yup’ik EducationOne area of growth stemming from the Yup’ik Environmental Knowledge Project has been collaboration with the Lower Kuskokwim School District. Teachers and their students have participated in training sessions on atlas technology and how to add content. As part of the district’s curriculum development, high school students collect and share the history and culture of the Yup’ik way of life.

Last of the Wild Project, Version 2, 2005 (LWP-2): Global Human Influence Index (HII) Dataset (Geographic)

The Global Human Influence Index Dataset of the Last of the Wild Project, Version 2, 2005 (LWP-2) is a global dataset of 1-kilometer grid cells, created from nine global data layers covering human population pressure (population density), human land use and infrastructure (built-up areas, nighttime lights, land use/land cover), and human access (coastlines, roads, railroads, navigable rivers). The dataset in Clarke 1866 Geographic Coordinate System is produced by the Wildlife Conservation Society (WCS) and the Columbia University Center for International Earth Science Information Network (CIESIN).

AirMSPI verison 6 ellipsoid-projected georegistered radiance product acquired during the NASA ORACLES flight campaign Jul-Oct 2016

AirMSPI_ORACLES_Ellipsoid-projected_Georegistered_Radiance_Data are AirMSPI Ellipsoid-projected georegistered radiance product acquired during the NASA ObseRvations of Aerosols above CLouds and their intEractionS (ORACLES) flight campaign.AirMSPI Level 1B2 products contain radiometric and polarimetric images of clouds, aerosols, and the surface of the Earth. In particular, products contain map-projected data at 8 wavelengths: 355, 380, 445, 470, 555, 660, 865, and 935 nm. The data products include radiance, time, solar zenith, solar azimuth, view zenith, and view azimuth for all spectral bands. Wavelengths for which polarization information is available (470, 660, and 865 nm) also include the Stokes parameters Q and U, as well as degree of linear polarization (DOLP) and angle of linear polarization (AOLP). Q, U, and AOLP are reported relative to both the scattering and view meridional planes. Files are distributed in HDF-EOS-5 format.This release of AirMPSI data contains all targets acquired during the ObseRvations of Aerosols above CLouds and their intEractionS (ORACLES) flight campaign, including the check-out and transit flights. ORACLES was based out of Walvis Bay, Namibia and focused on the South Atlantic Ocean off the coast of Namibia and Angola. AirMSPI was acquired from July 28 to October 6, 2016. More details about the ORACLES campaign and AirMSPI participation can be found at https://espo.nasa.gov/oracles (link is external).

Smart Sensing Using Wavelets Project

Further refinements to the FOSS technologies are focusing on &ldquo;smart&rdquo; sensing techniques that adjust sensing parameters as needed in real time so that only the necessary amount of data is acquired &ndash; no more, no less. Traditional FOSS signal processing is based on Fourier transforms that break up the length of the fiber into analysis sections that are equal in length along the whole fiber. If high resolution is required along one portion of the fiber, the whole fiber must be processed at that resolution. Wavelet transforms make it possible to efficiently break up the length of the fiber into analysis sections that vary in length. If high resolution is required along one portion of the fiber, only that portion is processed at high resolution, and the rest of the fiber can be processed at the lower resolution.Work to date: The team has developed a C language prototype of a wavelet-based signal processing algorithm. This static form currently operates at half the speed of the Fourier-based algorithm but it will be able to operate 3-4 times faster when optimized.&nbsp;The team has also developed a LabVIEW prototype of the adaptive form of the algorithm. This form provides real-time adaptive spatial resolution.&nbsp;For example: when strain on a wing increases during flight, the software will automatically increase the resolution on the part of the fiber that is under strain.Looking ahead: Next steps involve optimizing the code and implementing it on a digital signal processing (DSP) chip.&nbsp;A patent application for the wavelet algorithm has been filed with the USPTO.Benefits<ul><li>Improved efficiency: Offers precision measurement only where it is needed rather than on the entire fiber</li><li>Faster signal processing: Data can be processed at different resolutions at different fiber segments</li><li>Adaptive: Automatically selects optimum resolution based on data received</li></ul>Applications<ul><li>Strain sensing</li><li>Temperature measurements</li></ul>

Ocean Margin Exchange Phase II (OMEX II) Project

Measurements made under the OMEX-II project were made along the Northwest European continental shelf between 1997 and 1999.

Transformational Tools and Technologies Project

The Transformational Tools and Technologies (TTT) Project advances state-of-the-art computational and experimental tools and technologies that are vital to aviation applications in the six strategic thrusts. The project develops new computer-based tools, computational fluid dynamics models, and associated scientific knowledge that will provide first-of-a-kind capabilities to analyze, understand, and predict aviation concept performance. These revolutionary tools will be applied to accelerate NASA&rsquo;s research and the community&rsquo;s design and introduction of advanced concepts. The Project also explores technologies that are broadly-critical to advancing ARMD strategic outcomes.&nbsp; Such technologies include the understanding of new types of strong and lightweight materials, innovative controls techniques, and experimental methods.&nbsp; TTT also develops improved MDAO and systems analysis tools to enable multi-disciplinary integration. All of these technologies will support and enable concept development and benefits assessment across multiple ARMD programs and disciplines.&nbsp;The tools and technologies of interest span many disciplines.&nbsp; The Fluid Mechanics Discipline encompasses advanced turbulence modeling, boundary layer transition prediction and modeling, numerical methods, and flow control development and prediction for a wide range of airframe and propulsion system flow problems of interest.&nbsp; Canonical data is developed and used to validate the modeling improvements developed in this discipline.&nbsp; Development of more accurate physics-based methods such as large eddy simulation (LES) is emphasized.The Structures and Materials Discipline emphasizes improved multifunctional and high temperature materials for airframe and engine application, as well as modeling and simulation tool development to improve validated first-principles materials and structural modeling.&nbsp; Development of ceramic matrix composite (CMC) materials for high-temperature engine application is of particular emphasis in the discipline.The MDAO (Multi-Disciplinary Design, Analysis &amp; Optimization) and Systems Analysis Discipline develops MDAO and aircraft system-level tools to improve integration of discipline-based technologies and enable improved assessment of system-level benefits.&nbsp; An open-source framework is emphasized to better leverage external partners and increase interaction and benefit to the community.The Combustion Discipline is developing more accurate physics-based models for complex multi-species reacting flows representative of aircraft engine combustors.&nbsp; This is done through a combination of high-fidelity benchmark experiments and the use of advanced unsteady turbulence modeling and large eddy simulation (LES) methods.&nbsp; Advanced concepts such as active combustion control and pressure-gain combustion cycles are also investigated.The Controls Discipline encompasses work across aircraft flight controls and advanced propulsion controls.&nbsp; Development of technologies to enable distributed engine control systems are an area of emphasis in this discipline.The Innovative Measurements Discipline conducts research to advance the state-of-the-art in cross-cutting sensing and measurement technologies for aircraft and propulsion systems.&nbsp; Areas of development include advanced optical measurements, enhanced sensing, and improved data acquisition.

Superconducting Resonator Spectrometer for Millimeter- and Submillimeter-Wave Astrophysics Project

"We propose to develop a novel ultra-compact spectrograph-on-a-chip for the submillimeter and millimeter waveband. SuperSpec uses planar lithographed superconducting transmission-line filters to sort incident radiation by frequency to an array of direct detectors such as MKIDs. The system is naturally wideband and can be very low loss, enabling background-limited spectroscopy on the ground and in space, as is currently done with a diffraction grating spectrographs. But while moderate-resolution grating systems for the mm and submm bands have sizes measured in tens of centimeters, SuperSpec can have a size measured in millimeters. If successful, SuperSpec will pave the way for a new kind of astronomical instrument for the submm/mm: a 2-D array of hundreds to thousands of individual spectrometers, each simultaneously measuring a separate spectrum. With the possible exception of polarization, such an instrument extracts all available information from the light at a telescope focal plane. SuperSpec thus offers the potential to revolutionize astrophysics in the far-IR through millimeter, an important spectral regime for which the the Astro2010 Decadal Survey made two specific recommendations for this decade: 1) Participate in the Japanese-led SPICA space telescope with a spectrometer instrument such as BLISS, and 2) Construct CCAT and its associated instrumentation. Depending on SPICA's schedule, SuperSpec technology could be injected and would enhance and extend the long-wavelength capability of BLISS or a similar instrument. Whether or not SPICA moves ahead quickly, our demonstration will position SuperSpec to be used in on CCAT and suborbital platforms this decade, paving the way for optimal science return with future NASA-led cryogenic far-IR space missions on the drawing board for the next decade: CALISTO/SAFIR and SPIRIT. SuperSpec is based on propagation on a superconducting transmission line (TL). As radiation propagates along the line, it encounters a seri

Coastal High Acquisition Rate Radiometers for Innovative Environmental Research Project

Measurements from the C-HARRIER (Coastal High Acquisition Rate Radiometers for Innovative Environmental Research) project, which aims to study the coastal atmospheric and acquatic environments of Monterey Bay, Pinto Lake, and Lake Tahoe.

PATagonia EXperiment (PATEX) Project

PATagonia EXperiment (PATEX) Project is a Brazilian research project, which has the overall objective of characterizing the environmental constraints, phytoplankton assemblages, primary production rates, bio-optical characteristics, and air-sea CO2 fluxes waters along the Argentinean shelf-break during austral spring and summer. A set of seven PATEX cruises were conducted from 2004 to 2009. Garcia et al., 2011 (doi:10.1029/2010JC006595)

Development of a Robust Low-Power Pressure Transducer for Thermospheric Applications Project

The Earth&rsquo;s ionosphere is home to a number of phenomena that are regularly observed but still unpredictable; obvious examples include equatorial spread F, tidal ion layers, and sporadic E. The fundamental connection between these disparate events is that all three are strongly influenced by coupling between ionized and neutral particles. Most of what we know about these phenomena comes from plasma diagnostics &ndash; we can accurately measure electric fields, plasma density, and plasma temperatures in the ionosphere using in-situ probes, ground-based radars, and optical remote sensing techniques. Our ability to measure the neutral temperatures, densities, and motions at ionospheric altitudes is significantly less mature. We therefore propose to develop a low-power transducer system that will enable accurate measurements of neutral pressure and winds when assimilated into existing instrumentation systems. The low power aspect of this transducer concept is particularly important, since it is compatible with very small satellite platforms such as CubeSats. When deployed on constellations of small satellites in different orbit planes, instruments built around the small sensors we develop will be capable of providing simultaneous global measurements of neutral pressures and winds. These measurements will produce marked improvements in our predictive models, and bring us one step closer to forecasting the diverse phenomena that arise due to ion-neutral interactions in the upper atmosphere.

The High resolution Coronal Imager Project

The telescope design is a direct continuation of the development from NIXT to TRACE and AIA: we propose a Ritchey-Chr&acute;etien with plate scale sufficient to provide 0.1 arcsec pixel size, and multilayer coatings on two D-shaped halves, so that there are two wavelength channels available. The detector is a large-format back-illuminated CCD, providing high quan tum efficiency and rapid readout for high im age cadence. Channel selection is made via selectable focal plane filters. An H-telescope with NTSC (TV) output is included for real-time pointing verification during the flight. Major components of this new payload have been developed and qualified for the Hinode XRT instrument, SDO program (AIA &amp; HMI) and for the Solar Ultraviolet Magnetograph Investigation (SUMI) sounding rocket. This has helped keep the development costs for Hi-C sig nificantly lower than they otherwise would have been. The vehicle layout includes all major components needed for the flight demonstration. . It has a to total length of 108.9 inches and a launch weight of 562.9 pounds. The vehicle is the standard NASA 22-inch diameter shell. The proposed experiment design is based on the SAO NIXT and TXI instrument designs. A detailed weight breakdown is provided in Figure 5. As evidenced by Table 1, every component in the proposed mission has heritage in multiple successful instruments. Now we propose to ex tend the telescope magnification to the diffrac tion limit. AIA chose to extend the TRACE resolution to a full-sun field of view and now we are proposing to extend TRACE by increasing the magnification on the secondary mirror. The technologies required to build AIA are identical to that for Hi-C and every major contribution to the development of Hi-C is performed by the teams that built AIA (SAO, LMSAL) &nbsp; &nbsp;