National Library of Energy BETA

Sample records for all-stars shine bright

  1. Energy All-Stars Shine Bright at Inaugural Lecture Series

    Broader source: Energy.gov [DOE]

    Last Saturday, the Energy Department held its first Energy All-Stars event -- an afternoon of TED-style talks from America's energy leaders.

  2. Michael Liebreich (Energy All Stars Presentation)

    Office of Energy Efficiency and Renewable Energy (EERE)

    Michael Liebreich, CEO of Bloomberg New Energy Finance, delivered this presentation on the energy economy at the Energy All Stars event on January 19, 2013, at the US Department of Energy in...

  3. Sue Tierney (Energy All Stars Presentation)

    Broader source: Energy.gov [DOE]

    Sue Tierney delivered this presentation" The Future of Energy: Toward the 21st Century Energy System We Need (With an Eye on the Rear View Mirror)" at the Energy All Stars event on January 19, 2013...

  4. All-Star Nanocrystals | The Ames Laboratory

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

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  5. New OLED Lighting Systems Shine Bright, Save Energy

    Office of Energy Efficiency and Renewable Energy (EERE)

    Case study that describes how Universal Display Corporation received SBIR funding to adapt its PHOLED lighting technology for high-end commercial and institutional building applications.

  6. New OLED Lighting Systems Shine Bright, Save Energy

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    entered into business agreements with leading manufacturers in the U.S., Japan, Korea, Taiwan, China, and Europe. Cumulative Estimated Savings by 2018 1 Energy Estimated potential...

  7. SHINE Vacuum Pump Test Verification

    SciTech Connect (OSTI)

    Morgan, Gregg A; Peters, Brent

    2013-09-30

    Normetex pumps used world-wide for tritium service are no longer available. DOE and other researchers worldwide have spent significant funds characterizing this pump. Identification of alternate pumps is required for performance and compatibility with tritium gas. Many of the pumps that could be used to meet the functional performance requirements (e.g. pressure and flow conditions) of the Normetex pump have features that include the use of polymers or oils and greases that are not directly compatible with tritium service. This study assembles a test system to determine the flow characteristics for candidate alternate pumps. These tests are critical to the movement of tritium through the SHINE Tritium Purification System (TPS). The purpose of the pump testing is two-fold: (1) obtain baseline vacuum pump characteristics for an alternate (i.e. ''Normetex replacement'') pump intended for use in tritium service; and (2) verify that low pressure hydrogen gas can be transported over distances up to 300 feet by the candidate pumps. Flow rates and nominal system pressures have been identified for the SHINE Mo-99 production process Tritium Purification System (TPS). To minimize the line sizes for the transfer of low pressure tritium from the Neutron Driver Accelerator System (NDAS) to the primary processing systems in the TPS, a ''booster'' pump has been located near the accelerator in the design. A series of pump tests were performed at various configurations using hydrogen gas (no tritium) to ensure that this concept is practical and maintains adequate flow rates and required pressures. This report summarizes the results of the tests that have been performed using various pump configurations. The current design of the Tritium Purification System requires the ''booster'' pump to discharge to or to be backed by another vacuum pump. Since Normetex pumps are no longer manufactured, a commercially available Edwards scroll pump will be used to back the booster pump. In this case the ''booster pump'' is an Adixen Molecular Drag Pump (MDP 5011) and the backing pump is an Edwards (nXDS15iC) scroll pump. Various configurations of the two pumps and associated lengths of 3/4 inch tubing (0 feet to 300 feet) were used in combination with hydrogen and nitrogen flow rates ranging from 25-400 standard cubic centimeters per minute (sccm) to determine whether the proposed pump configuration meets the design criteria for SHINE. The results of this study indicate that even under the most severe conditions (300 feet of tubing and 400 sccm flow rate) the Adixen 5011 MDP can serve as a booster pump to transport gases from the accelerator (NDAS) to the TPS. The Target Gas Receiving System pump (Edwards nXDS15iC) located approximately 300 feet from the accelerator can effectively back the Adixen MDP. The molecular drag pump was able to maintain its full rotational speed even when the flow rate was 400 sccm hydrogen or nitrogen and 300 feet of tubing was installed between the drag pump and the Edwards scroll pump. In addition to maintaining adequate rotation, the pressure in the system was maintained below the target pressure of 30 torr for all flow rates, lengths of tubing, and process gases. This configuration is therefore adequate to meet the SHINE design requirements in terms of flow and pressure.

  8. Argonne Researchers Shine "Light" on Origins of Wind Turbine...

    Office of Environmental Management (EM)

    Researchers Shine "Light" on Origins of Wind Turbine Bearing Failures Argonne Researchers Shine "Light" on Origins of Wind Turbine Bearing Failures September 12, 2014 - 11:34am...

  9. Desert Sunlight is Shining Example of How DOE Loan Guarantees...

    Energy Savers [EERE]

    Sunlight is Shining Example of How DOE Loan Guarantees Helped Launch Utility-scale PV Solar Market Desert Sunlight is Shining Example of How DOE Loan Guarantees Helped Launch...

  10. Bright Ideas

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

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  11. Light-shining-through-walls with lasers

    E-Print Network [OSTI]

    Friederike Januschek

    2014-10-07

    Light-shining-through-walls experiments are the search experiments for weakly interacting slim particles (WISPs) with the smallest model dependence. They have the advantage that not only the detection, but also the production of the WISPs takes place in the laboratory and can thus be controlled. Using lasers is the preferred option for most of the mass region and has led to the world's most stringent laboratory limits (ALPS I) there. At CERN, OSQAR promises to surpass these and at DESY ALPS II is currently set up, which is planning to probe the axion-like particle to photon coupling down to $|g_{a\\gamma}|\\gtrsim 2\\cdot10^{-11}$ GeV$^{-1}$, which is in a region favored by many astrophysical hints.

  12. A Shining Example of Dr. King's legacy | Department of Energy

    Broader source: Energy.gov (indexed) [DOE]

    A Shining Example of Dr. Kings legacy Kathy Chambers Senior Science and Technical Information Specialist, OSTI Editor's Note: This blog was originally posted on OSTI's blog....

  13. LET THE SUN SHINE: OPTIMAL DEPLOYMENT OF PHOTOVOLTAICS IN GERMANY

    E-Print Network [OSTI]

    Paris-Sud XI, Université de

    LET THE SUN SHINE: OPTIMAL DEPLOYMENT OF PHOTOVOLTAICS IN GERMANY Anna CRETI Jérôme JOAUG Cahier n:chantal.poujouly@polytechnique.edu hal-00751743,version1-14Nov2012 #12;Let the sun shine: optimal deployment of photovoltaics in Germany-in tari¤s to foster the di¤usion of photovoltaics is recently being rediscussed in several countries

  14. September 24, 2014 Delaware Will Shine Strategic Planning Initiative

    E-Print Network [OSTI]

    Firestone, Jeremy

    1 September 24, 2014 Delaware Will Shine Strategic Planning: CONCEPT PAPER NOTE: The goal of this strategic planning working group CORE VALUES are offered by this strategic planning working group

  15. Why Does the Sun Shine? Is the Sun on Fire?

    E-Print Network [OSTI]

    Walter, Frederick M.

    Why Does the Sun Shine? #12;Is the Sun on Fire? Fire (oxidation) produces light and heat, just like the Sun. Source: chemical potential energy Suppose the Sun were made of carbon and oxygen. ·The Sun could) * mp N = M / MCO2 = 2.6 X 1055 (number of reactions possible) #12;Is the Sun on Fire? Fire produces

  16. Why Does the Sun Shine? Is the Sun on Fire?

    E-Print Network [OSTI]

    Walter, Frederick M.

    Why Does the Sun Shine? #12;Is the Sun on Fire? Fire (oxidation) produces light and heat, just like the Sun. Source: chemical potential energy Suppose the Sun were made of carbon and oxygen. · The Sun could) * mp N = M¤ / MCO2 = 2.6 X 1055 (number of reactions possible) #12;Is the Sun on Fire? Fire produces

  17. Shining Light in Dark Places: Understanding the Tor Network

    E-Print Network [OSTI]

    Washington at Seattle, University of

    Shining Light in Dark Places: Understanding the Tor Network Damon McCoy1 , Kevin Bauer1 , Dirk used? (2) How is Tor being mis-used? (3) Who is using Tor? To sample the results, we show that web such as web browsing, file sharing, and instant messaging. Since its initial development, researchers have

  18. ALS X-Rays Shine a New Light on Catalysis

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

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  19. Shining Light on Opacity (Journal Article) | SciTech Connect

    Office of Scientific and Technical Information (OSTI)

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  20. Shining Light on Opacity (Journal Article) | SciTech Connect

    Office of Scientific and Technical Information (OSTI)

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  1. Shining Light on Catalysis | Stanford Synchrotron Radiation Lightsource

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

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  2. Rain or Shine: We Cycle for Science | Department of Energy

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

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  3. Mass map shines light on dark matter | Argonne National Laboratory

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

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  4. SHINE Tritium Nozzle Design: Activity 6, Task 1 Report

    SciTech Connect (OSTI)

    Okhuysen, Brett S.; Pulliam, Elias Noel

    2015-11-05

    In FY14, we studied the qualitative and quantitative behavior of a SHINE/PNL tritium nozzle under varying operating conditions. The result is an understanding of the nozzle’s performance in terms of important flow features that manifest themselves under different parametric profiles. In FY15, we will consider nozzle design with a focus on nozzle geometry and integration. From FY14 work, we will understand how the SHINE/PNL nozzle behaves under different operating scenarios. The first task for FY15 is to evaluate the FY14 model as a predictor of the actual flow. Considering different geometries is more time-intensive than parameter studies, therefore we recommend considering any relevant flow features that were not included in the FY14 model. In the absence of experimental data, it is particularly important to consider any sources of heat in the domain or boundary conditions that may affect the flow and incorporate these into the simulation if they are significant. Additionally, any geometric features of the beamline segment should be added to the model such as the orifice plate. The FY14 model works with hydrogen. An improvement that can be made for FY15 is to develop CFD properties for tritium and incorporate those properties into the new models.

  5. Sustainable and Holistic Integration of Energy Storage and Solar PV (SHINES) Funding Opportunity

    Office of Energy Efficiency and Renewable Energy (EERE)

    The Sustainable and Holistic Integration of Energy Storage and Solar PV (SHINES) solution as envisioned by SunShot will have the following features:

  6. Letting The Sun Shine On Solar Costs: An Empirical Investigation Of Photovoltaic Cost Trends In California

    E-Print Network [OSTI]

    Wiser, Ryan; Bolinger, Mark; Cappers, Peter; Margolis, Robert

    2006-01-01

    THE SUN SHINE ON SOLAR COSTS: AN EMPIRICAL INVESTIGATION OFWe find that: (1) solar costs have declined substantially2004 $/W AC . 4. SOLAR COSTS HAVE DECLINED SUBSTANTIALLY In

  7. arXiv:astro-ph/0009259v219Sep2000 How the Sun Shines

    E-Print Network [OSTI]

    Walter, Frederick M.

    arXiv:astro-ph/0009259v219Sep2000 How the Sun Shines John N. Bahcall What makes the sun shine? How does the sun produce the vast amount of energy necessary to support life on earth? These questions 1833 Treatise on Astronomy: The sun's rays are the ultimate source of almost every motion which takes

  8. LED Record Efficacy and Brightness

    Broader source: Energy.gov [DOE]

    Designed for general lighting applications such as street, industrial, and parking garage lighting, the Cree XLamp® power LED sets new records for LED brightness and efficacy, up to 85 lm/W at 350 mA. The XLamp utilizes Cree's performance breakthrough EZBright™ LED chip; both products include technology that was developed in part with R&D funding support from DOE.

  9. Available online at www.sciencedirect.com Plant cuticles shine: advances in wax biosynthesis and export

    E-Print Network [OSTI]

    Kunst, Ljerka

    Available online at www.sciencedirect.com Plant cuticles shine: advances in wax biosynthesis stresses. It is composed of cutin polymer matrix and waxes, produced and secreted by epidermal cells involved in fatty acid elongation and biosynthesis of wax components, as well as transporters required

  10. Shining Energy-saving LEDs on Utah Starry Nights | Department of Energy

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Delicious RankADVANCED MANUFACTURINGEnergy BillsNo.Hydrogen4 » Searchwith Ultra-Deepwater AdvisoryShining

  11. Light Shines on Better Budget for Glendale, Arizona | Department of Energy

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Delicious RankADVANCED MANUFACTURING OFFICE INDUSTRIALU.S.Leadership on Clean Energys oElectrical EnergyDOEDutyShines

  12. NA61-SHINE: Hadron Production Measurements for Cosmic Ray and Neutrino Experiments

    E-Print Network [OSTI]

    Nicolas Abgrall

    2010-05-25

    As neutrino long baseline experiments enter a new domain of precision, important systematic errors due to poor knowledge of production cross-sections for pions and kaons require more dedicated measurements for precise neutrino flux predictions. The cosmic ray experiments require dedicated hadron production measurements to tune simulation models used to describe air shower profiles. Among other goals, the NA61-SHINE (SPS Heavy Ion and Neutrino Experiment) experiment at the CERN SPS aims at precision measurements (5% and below) for both neutrino and cosmic ray experiments: those will improve the prediction of the neutrino flux for the T2K experiment at J-PARC and the prediction of muon production in the propagation of air showers for the Auger and KASCADE experiments. Motivations for new hadron production measurements are briefly discussed. NA61-SHINE took data during a pilot run in 2007 and in 2009 with different Carbon targets. The NA61-SHINE setup and preliminary spectra for positive and negative pions obtained with the 2007 thin (4% interaction length) Carbon target data are presented. The use of the NA61 data for the T2K neutrino flux predictions is finally discussed in further details.

  13. Black hole variability and the star formation-active galactic nucleus connection: Do all star-forming galaxies host an active galactic nucleus?

    SciTech Connect (OSTI)

    Hickox, Ryan C.; Chen, Chien-Ting J.; Civano, Francesca M.; Hainline, Kevin N.; Mullaney, James R.; Alexander, David M.; Goulding, Andy D.

    2014-02-10

    We investigate the effect of active galactic nucleus (AGN) variability on the observed connection between star formation and black hole accretion in extragalactic surveys. Recent studies have reported relatively weak correlations between observed AGN luminosities and the properties of AGN hosts, which has been interpreted to imply that there is no direct connection between AGN activity and star formation. However, AGNs may be expected to vary significantly on a wide range of timescales (from hours to Myr) that are far shorter than the typical timescale for star formation (?100 Myr). This variability can have important consequences for observed correlations. We present a simple model in which all star-forming galaxies host an AGN when averaged over ?100 Myr timescales, with long-term average AGN accretion rates that are perfectly correlated with the star formation rate (SFR). We show that reasonable prescriptions for AGN variability reproduce the observed weak correlations between SFR and L {sub AGN} in typical AGN host galaxies, as well as the general trends in the observed AGN luminosity functions, merger fractions, and measurements of the average AGN luminosity as a function of SFR. These results imply that there may be a tight connection between AGN activity and SFR over galaxy evolution timescales, and that the apparent similarities in rest-frame colors, merger rates, and clustering of AGNs compared to 'inactive' galaxies may be due primarily to AGN variability. The results provide motivation for future deep, wide extragalactic surveys that can measure the distribution of AGN accretion rates as a function of SFR.

  14. NPR: Particles From The Edge Of Space Shine A Light On Fukushima

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

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  15. Rain or Shine, Students Keep Their Race Cars Going - News Feature | NREL

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

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  16. Bright Star Astrometry with URAT

    E-Print Network [OSTI]

    Zacharias, Norbert

    2015-01-01

    The U.S. Naval Observatory Robotic Astrometric Telescope (URAT) is observing the northern sky since April 2012 for an astrometric survey. Multiple overlaps per year are performed in a single bandpass (680$-$750 nm) using the "redlens" 20 cm aperture astrograph and a mosaic of large CCDs. Besides the regular, deep survey to magnitude 18.5, short exposures with an objective grating are taken to access stars as bright as 3rd magnitude. A brief overview of the program, observing and reductions is given. Positions on the 8 to 20 mas level are obtained of 66,202 Hipparcos stars at current epochs. These are compared to the Hipparcos Catalog to investigate its accuracy. About 20\\% of the observed Hipparcos stars are found to have inconsitent positions with the Hipparcos Catalog prediction on the 3 sigma level or over (about 75 mas or more discrepant position offsets). Some stars are now seen at an arcsec (or 25 sigma) off their Hipparcos Catalog predicted position.

  17. Corrosion Assessment of Candidate Materials for the SHINE Subcritical Assembly Vessel and Components FY14 Report

    SciTech Connect (OSTI)

    Pawel, Steven J.

    2014-10-01

    Laboratory corrosion testing of candidate alloys—including Zr-4 and Zr-2.5Nb representing the target solution vessel, and 316L, 2304, 304L, and 17-4 PH stainless steels representing process piping and balance-of-plant components—was performed in support of the proposed SHINE process to produce 99Mo from low-enriched uranium. The test solutions used depleted uranyl sulfate in various concentrations and incorporated a range of temperatures, excess sulfuric acid concentrations, nitric acid additions (to simulate radiolysis product generation), and iodine additions. Testing involved static immersion of coupons in solution and in the vapor above the solution, and was extended to include planned-interval tests to examine details associated with stainless steel corrosion in environments containing iodine species. A large number of galvanic tests featuring couples between a stainless steel and a zirconium-based alloy were performed, and limited vibratory horn testing was incorporated to explore potential erosion/corrosion features of compatibility. In all cases, corrosion of the zirconium alloys was observed to be minimal, with corrosion rates based on weight loss calculated to be less than 0.1 mil/year with no change in surface roughness. The resulting passive film appeared to be ZrO2 with variations in thickness that influence apparent coloration (toward light brown for thicker films). Galvanic coupling with various stainless steels in selected exposures had no discernable effect on appearance, surface roughness, or corrosion rate. Erosion/corrosion behavior was the same for zirconium alloys in uranyl sulfate solutions and in sodium sulfate solutions adjusted to a similar pH, suggesting there was no negative effect of uranium resulting from fluid dynamic conditions aggressive to the passive film. Corrosion of the candidate stainless steels was similarly modest across the entire range of exposures. However, some sensitivity to corrosion of the stainless steels was observed in solutions with 50 wppm iodine (the actual SHINE process expects 0.1–1 wppm) with the highest corrosion rates (up to ~6 mil/year) observed on specimens exposed in the vapor phase. Lower concentrations of iodine species (5 or 28 wppm) proved much less corrosive, and the planned-interval data indicated that metal corrodibility decreased with time for all immersed exposures and, with one minor exception, all vapor exposures. Little change in susceptibility to corrosion was observed as a result of nitric acid additions to the test environment (simulating radiolysis products). The trend toward reduced corrosion (immersion and vapor phase) with decreasing iodine concentration suggests that, at the expected conditions in the SHINE process, it is unlikely that iodine species will generate a general corrosion concern for the candidate stainless steels.

  18. Mississippi State Axion Search: A Light Shining though a Wall ALP Search

    E-Print Network [OSTI]

    Mohanmurthy, Prajwal; Formaggio, Joseph; Fowler, Nicholas; Gaerlan, Mikhail; Jiang, Yipeng; Madsen, John; Oblath, Noah; Powers, Adam; Ray, Amy; Riehle, Robertson

    2015-01-01

    The elegant solutions to the strong CP problem predict the existence of a particle called axion. Thus, the search for axion like particles (ALP) has been an ongoing endeavor. The possibility that these axion like particles couple to photons in presence of magnetic field gives rise to a technique of detecting these particles known as light shining through a wall (LSW). Mississippi State Axion Search (MASS) is an experiment employing the LSW technique in search for axion like particles. The apparatus consists of two radio frequency (RF) cavities, both under the influence of strong magnetic field and separated by a lead wall. While one of the cavities houses a strong RF generator, the other cavity houses the detector systems. The MASS apparatus looks for excesses in RF photons that tunnel through the wall as a signature of candidate axion-like particles. The concept behind the experiment as well as the projected sensitivities are presented here.

  19. Resonant laser power build-up in ALPS -- a "light-shining-through-walls" experiment

    E-Print Network [OSTI]

    Klaus Ehret; Maik Frede; Samvel Ghazaryan; Matthias Hildebrandt; Ernst-Axel Knabbe; Dietmar Kracht; Axel Lindner; Jenny List; Tobias Meier; Niels Meyer; Dieter Notz; Javier Redondo; Andreas Ringwald; Günter Wiedemann; Benno Willke

    2009-05-26

    The ALPS collaboration runs a light-shining-through-walls (LSW) experiment to search for photon oscillations into "weakly interacting sub-eV particles" (WISPs) inside of a superconducting HERA dipole magnet at the site of DESY. In this paper we report on the first successful integration of a large-scale optical cavity to boost the available power for WISP production in this type of experiments. The key elements are a frequency tunable narrow line-width continuous wave laser acting as the primary light source and an electronic feed-back control loop to stabilize the power build-up. We describe and characterize our apparatus and demonstrate the data analysis procedures on the basis of a brief exemplary run.

  20. Mississippi State Axion Search: A Light Shining though a Wall ALP Search

    E-Print Network [OSTI]

    Prajwal Mohanmurthy; Dipangkar Dutta; Joseph Formaggio; Nicholas Fowler; Mikhail Gaerlan; Yipeng Jiang; John Madsen; Noah Oblath; Adam Powers; Amy Ray; Robertson Riehle

    2015-03-08

    The elegant solutions to the strong CP problem predict the existence of a particle called axion. Thus, the search for axion like particles (ALP) has been an ongoing endeavor. The possibility that these axion like particles couple to photons in presence of magnetic field gives rise to a technique of detecting these particles known as light shining through a wall (LSW). Mississippi State Axion Search (MASS) is an experiment employing the LSW technique in search for axion like particles. The apparatus consists of two radio frequency (RF) cavities, both under the influence of strong magnetic field and separated by a lead wall. While one of the cavities houses a strong RF generator, the other cavity houses the detector systems. The MASS apparatus looks for excesses in RF photons that tunnel through the wall as a signature of candidate axion-like particles. The concept behind the experiment as well as the projected sensitivities are presented here.

  1. Updated Spitzer emission spectroscopy of bright transiting hot...

    Office of Scientific and Technical Information (OSTI)

    Updated Spitzer emission spectroscopy of bright transiting hot Jupiter HD 189733b Citation Details In-Document Search Title: Updated Spitzer emission spectroscopy of bright...

  2. Light Pollution in the Shining Star of the Caribbean: Recovering the nightscape for future generations in island of Puerto Rico

    E-Print Network [OSTI]

    Gilbes, Fernando

    Light Pollution in the Shining Star of the Caribbean: Recovering the nightscape for future@fs.fed.us Other authors: Members of the Light Pollution Task Force representing the following entities: Puerto pollution consequences, most people reacted positively to the prominence of the island's artificial

  3. Massive Disks in Low Surface Brightness Galaxies

    E-Print Network [OSTI]

    B. Fuchs

    2002-09-09

    An update of the set of low surface brightness galaxies is presented which can be used to set constraints on the otherwise ambiguous decompositions of their rotation curves into contributions due to the various components of the galaxies. The selected galaxies show all clear spiral structure and arguments of density wave theory of galactic spiral arms are used to estimate the masses of the galactic disks. Again these estimates seem to indicate that the disks of low surface brightness galaxies might be much more massive than currently thought. This puzzling result contradicts stellar population synthesis models. This would mean also that low surface brightness galaxies are not dominated by dark matter in their inner parts.

  4. A brightness exceeding simulated Langmuir limit

    SciTech Connect (OSTI)

    Nakasuji, Mamoru

    2013-08-15

    When an excitation of the first lens determines a beam is parallel beam, a brightness that is 100 times higher than Langmuir limit is measured experimentally, where Langmuir limits are estimated using a simulated axial cathode current density which is simulated based on a measured emission current. The measured brightness is comparable to Langmuir limit, when the lens excitation is such that an image position is slightly shorter than a lens position. Previously measured values of brightness for cathode apical radii of curvature 20, 60, 120, 240, and 480 ?m were 8.7, 5.3, 3.3, 2.4, and 3.9 times higher than their corresponding Langmuir limits, respectively, in this experiment, the lens excitation was such that the lens and the image positions were 180 mm and 400 mm, respectively. From these measured brightness for three different lens excitation conditions, it is concluded that the brightness depends on the first lens excitation. For the electron gun operated in a space charge limited condition, some of the electrons emitted from the cathode are returned to the cathode without having crossed a virtual cathode. Therefore, method that assumes a Langmuir limit defining method using a Maxwellian distribution of electron velocities may need to be revised. For the condition in which the values of the exceeding the Langmuir limit are measured, the simulated trajectories of electrons that are emitted from the cathode do not cross the optical axis at the crossover, thus the law of sines may not be valid for high brightness electron beam systems.

  5. Bright and dark sides of computational intelligence

    E-Print Network [OSTI]

    Wilamowski, Bogdan Maciej

    Bright and dark sides of computational intelligence Bogdan M. Wilamowski Auburn University positive and negative values and the resulted neuron excitation net is calculated as a sum of products of incoming signals multiplied by weights: xw=net ii n =1i (1) k net out netk-+1 1 =f(net)=out exp Fig. 2

  6. Discovery of a GeV Blazar Shining Through the Galactic Plane

    SciTech Connect (OSTI)

    Vandenbroucke, J.; Buehler, R.; Ajello, M.; Bechtol, K.; /Stanford U., HEPL /KIPAC, Menlo Park /SLAC; Bellini, A.; /Padua U., Astron. Dept. /Baltimore, Space Telescope Sci.; Bolte, M.; /UC, Santa Cruz; Cheung, C.C.; /Naval Research Lab, Wash., D.C. /NAS, Washington, D.C.; Civano, F.; /Smithsonian Astrophys. Observ.; Donato, D.; /NASA, Goddard; Fuhrmann, L.; /Bonn, Max Planck Inst., Radioastron.; Funk, S.; Healey, S.E.; /Stanford U., HEPL /KIPAC, Menlo Park /SLAC; Hill, A.B.; /Joseph Fourier U.; Knigge, C.; /Southampton U.; Madejski, G.M.; Romani, R.W.; /Stanford U., HEPL /KIPAC, Menlo Park /SLAC; Santander-Garcia, M.; /IAC, La Laguna /Isaac Newton Group /Laguna U., Tenerife; Shaw, M.S.; /Stanford U., HEPL /KIPAC, Menlo Park /SLAC; Steeghs, D.; /Warwick U.; Torres, M.A.P.; /Smithsonian Astrophys. Observ.; Van Etten, A.; /Stanford U., HEPL /KIPAC, Menlo Park /SLAC /Texas U., Astron. Dept.

    2011-08-11

    The Fermi Large Area Telescope (LAT) discovered a new gamma-ray source near the Galactic plane, Fermi J0109+6134, when it flared brightly in 2010 February. The low Galactic latitude (b = -1.2{sup o}) indicated that the source could be located within the Galaxy, which motivated rapid multi-wavelength follow-up including radio, optical, and X-ray observations. We report the results of analyzing all 19 months of LAT data for the source, and of X-ray observations with both Swift and the Chandra X-ray Observatory. We determined the source redshift, z = 0.783, using a Keck LRIS observation. Finally, we compiled a broadband spectral energy distribution (SED) from both historical and new observations contemporaneous with the 2010 February flare. The redshift, SED, optical line width, X-ray obsorption, and multi-band variability indicate that this new Gev source is a blazar seen through the Galactic plane. Because several of the optical emission lines have equivalent width > 5 {angstrom}, this blazar belongs in the flat-spectrum radio quasar category.

  7. Raman beam combining for laser brightness enhancement

    DOE Patents [OSTI]

    Dawson, Jay W; Allen, Grahan S; Pax, Paul H; Heebner, John E; Sridharan, Arun K; Rubenchik, Alexander M; Barty, Christopher B.J

    2015-11-05

    An optical source capable of enhanced scaling of pulse energy and brightness utilizes an ensemble of single-aperture fiber lasers as pump sources, with each such fiber laser operating at acceptable pulse energy levels. Beam combining involves stimulated Raman scattering using a Stokes' shifted seed beam, the latter of which is optimized in terms of its temporal and spectral properties. Beams from fiber lasers can thus be combined to attain pulses with peak energies in excess of the fiber laser self-focusing limit of 4 MW while retaining the advantages of a fiber laser system of high average power with good beam quality.

  8. Raman beam combining for laser brightness enhancement

    DOE Patents [OSTI]

    Dawson, Jay W.; Allen, Graham S.; Pax, Paul H.; Heebner, John E.; Sridharan, Arun K.; Rubenchik, Alexander M.; Barty, Chrisopher B. J.

    2015-10-27

    An optical source capable of enhanced scaling of pulse energy and brightness utilizes an ensemble of single-aperture fiber lasers as pump sources, with each such fiber laser operating at acceptable pulse energy levels. Beam combining involves stimulated Raman scattering using a Stokes' shifted seed beam, the latter of which is optimized in terms of its temporal and spectral properties. Beams from fiber lasers can thus be combined to attain pulses with peak energies in excess of the fiber laser self-focusing limit of 4 MW while retaining the advantages of a fiber laser system of high average power with good beam quality.

  9. BrightSource Energy | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIX E LIST OFAMERICA'SHeavy Electricals Ltd BHEL Jump to:Bottomline EnergyBrightSource

  10. Are Low Surface Brightness Discs Young?

    E-Print Network [OSTI]

    Paolo Padoan; Raul Jimenez; Vincenzo Antonuccio-Delogu

    1996-09-12

    We reconsider the problem of the age of the stellar discs of late-type Low Surface Brightness (LSB) galaxies by making use of a new IMF recently derived from numerical fluid dynamical simulations (Padoan, Nordlund and Jones, 1997). While a Miller-Scalo IMF cannot adequately describe the photometric properties of LSBs, when we apply the new Padoan et al. (1997) IMF to a simple exponential disc model with parameters appropriate to LSBs, we get excellent fits of the colors and color gradients. We then conclude that: a) The star formation history of LSB disc galaxies can be described by an initial burst of a few times $10^7$ yr followed by a quiescent period with only sporadic star formation; b) LSBs' discs are not young. The age of the LSB disc galaxies for which colors have been measured are all larger than about 10 Gyr$.

  11. Concepts for Phosphorescent Organic LEDs at High Brightness ...

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    Concepts for Phosphorescent Organic LEDs at High Brightness May 24, 2010 at 3pm36-428 Sebastian Reineke Institut fr Angewandte Photophysik, Dresden reineke001 abstract: Organic...

  12. Ultra Bright LED Light Injection Calibration System for MINOS

    E-Print Network [OSTI]

    B. Anderson; A. Anjomshoaa; P. Dervan; J. A. Lauber; J. Thomas

    1998-10-26

    We describe here a proposal for a light injection calibration system for the MINOS detectors based on ultra bright blue LEDs as the light source. We have shown that these LEDs are bright enough to span over two orders of magnitude in light intensity, commensurate with that expected in a single scintillator strip in the MINOS neutrino detectors.

  13. High output lamp with high brightness

    DOE Patents [OSTI]

    Kirkpatrick, Douglas A. (Great Falls, VA); Bass, Gary K. (Mt. Airy, MD); Copsey, Jesse F. (Germantown, MD); Garber, Jr., William E. (Poolesville, MD); Kwong, Vincent H. (Vancouver, CA); Levin, Izrail (Silver Spring, MD); MacLennan, Donald A. (Gaithersburg, MD); Roy, Robert J. (Frederick, MD); Steiner, Paul E. (Olney, MD); Tsai, Peter (Olney, MD); Turner, Brian P. (Damascus, MD)

    2002-01-01

    An ultra bright, low wattage inductively coupled electrodeless aperture lamp is powered by a solid state RF source in the range of several tens to several hundreds of watts at various frequencies in the range of 400 to 900 MHz. Numerous novel lamp circuits and components are disclosed including a wedding ring shaped coil having one axial and one radial lead, a high accuracy capacitor stack, a high thermal conductivity aperture cup and various other aperture bulb configurations, a coaxial capacitor arrangement, and an integrated coil and capacitor assembly. Numerous novel RF circuits are also disclosed including a high power oscillator circuit with reduced complexity resonant pole configuration, parallel RF power FET transistors with soft gate switching, a continuously variable frequency tuning circuit, a six port directional coupler, an impedance switching RF source, and an RF source with controlled frequency-load characteristics. Numerous novel RF control methods are disclosed including controlled adjustment of the operating frequency to find a resonant frequency and reduce reflected RF power, controlled switching of an impedance switched lamp system, active power control and active gate bias control.

  14. Dim Matter in the Disks of Low Surface Brightness Galaxies

    E-Print Network [OSTI]

    B. Fuchs

    2002-04-23

    An attempt is made to set constraints on the otherwise ambiguous decomposition of the rotation curves of low surface brightness galaxies into contributions due to the various components of the galaxies. For this purpose galaxies are selected which show clear spiral structure. Arguments of density wave theory of galactic spiral arms are then used to estimate the masses of the galactic disks. These estimates seem to indicate that the disks of low surface brightness galaxies might be much more massive than currently thought. This unexpected result contradicts stellar population synthesis models. This would also mean that low surface brightness galaxies are not dominated by dark matter in their inner parts.

  15. The Effect of Acute Bright Light Exposure on Social Affiliation

    E-Print Network [OSTI]

    Botanov, Yevgeny

    2014-08-31

    In recent decades, bright light has emerged as a useful tool in numerous clinical and non-clinical applications, with the potential to influence circadian rhythms, sleep, mood, and several other functional domains. However, ...

  16. Induction effects for heterochromatic brightness matching, heterochromatic flicker photometry,

    E-Print Network [OSTI]

    Dobkins, Karen R.

    Induction effects for heterochromatic brightness matching, heterochromatic flicker photometry flicker photometry (HFP), and minimally distinct border (MDB). For HBM, subjects varied the relative compared with those obtained on two other tasks: hetero- chromatic flicker photometry (HFP) and minimally

  17. Infrared Brightness Temperature of Mars, 1983-2103

    E-Print Network [OSTI]

    E. L. Wright

    2007-03-25

    The predicted infrared brightness temperature of Mars using the 1976 model of Wright is tabulated here for the period 1983 to 2103. This model was developed for far-infrared calibration, and is still being used for JCMT calibration.

  18. Bright Light-Emitting Diodes based on Organometal Halide Perovskite

    E-Print Network [OSTI]

    Tan, Zhi-Kuang; Moghaddam, Reza Saberi; Lai, May Ling; Docampo, Pablo; Higler, Ruben; Deschler, Felix; Price, Michael; Sadhanala, Aditya; Pazos, Luis M.; Credgington, Dan; Hanusch, Fabian; Bein, Thomas; Snaith, Henry J.; Friend, Richard H.

    2014-08-03

    temperature and high vacuum processes, rendering them uneconomical for use in large area displays. Here, we report high brightness light-emitting diodes based on solution-processed organometal halide perovskites. We demonstrate electroluminescence in the near...

  19. A high-brightness source of polarization-entangled photons

    E-Print Network [OSTI]

    Weinfurter, Harald

    A high-brightness source of polarization-entangled photons optimized for applications in free space for Quantum Computing and Department of Physics and Astronomy, University of Waterloo, Ontario N2L 3G1, Canada 3, 1090 Wien, Austria 7 Department of Electrical and Electronic Engineering, University of Bristol

  20. Ultra-bright pulsed electron beam with low longitudinal emittance

    DOE Patents [OSTI]

    Zolotorev, Max (Oakland, CA)

    2010-07-13

    A high-brightness pulsed electron source, which has the potential for many useful applications in electron microscopy, inverse photo-emission, low energy electron scattering experiments, and electron holography has been described. The source makes use of Cs atoms in an atomic beam. The source is cycled beginning with a laser pulse that excites a single Cs atom on average to a band of high-lying Rydberg nP states. The resulting valence electron Rydberg wave packet evolves in a nearly classical Kepler orbit. When the electron reaches apogee, an electric field pulse is applied that ionizes the atom and accelerates the electron away from its parent ion. The collection of electron wave packets thus generated in a series of cycles can occupy a phase volume near the quantum limit and it can possess very high brightness. Each wave packet can exhibit a considerable degree of coherence.

  1. Bright x-ray sources from laser irradiation of foams with high...

    Office of Scientific and Technical Information (OSTI)

    Bright x-ray sources from laser irradiation of foams with high concentration of Ti Citation Details In-Document Search Title: Bright x-ray sources from laser irradiation of foams...

  2. Bright Skies Ahead for Moapa | Department of Energy

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Delicious Rank EERE:FinancingPetroleum Based Fuels ResearchofDerivative Classifiers Should KnowLandfillBright Skies

  3. South African night sky brightness during high aerosol epochs

    E-Print Network [OSTI]

    Winkler, Hartmut; Marang, Fred

    2014-01-01

    Sky conditions in the remote, dry north-western interior of South Africa are now the subject of considerable interest in view of the imminent construction of numerous solar power plants in this area. Furthermore, the part of this region in which the core of the SKA is to be located (which includes SALT) has been declared an Astronomical Advantage Zone, for which sky brightness monitoring will now be mandatory. In this project we seek to characterise the sky brightness profile under a variety of atmospheric conditions. Key factors are of course the lunar phase and altitude, but in addition the sky brightness is also significantly affected by the atmospheric aerosol loading, as that influences light beam scattering. In this paper we chose to investigate the sky characteristics soon after the Mount Pinatubo volcanic eruption in 1991, which resulted in huge ash masses reaching the stratosphere (where they affected solar irradiance for several years). We re-reduced photometric sky measurements from the South Afric...

  4. Inverse Free Electron Laser Interactions with Sub-Picosecond High Brightness Electron Beams

    E-Print Network [OSTI]

    Moody, Joshua Timothy

    2014-01-01

    Accelerated Electron Beam Spectrum . . . . . . . . . . . .2 High Brightness Electron Beams Produced in thetion of Uniformly Filled Ellipsoidal Electron Beam: Method-

  5. vol. 181, no. 5 the american naturalist may 2013 Warning Signal Brightness Variation: Sexual Selection

    E-Print Network [OSTI]

    Cummings, Molly E.

    and females are exceptionally bright, this population is also sexually dimorphic in terms of aposemvol. 181, no. 5 the american naturalist may 2013 E-Note Warning Signal Brightness Variation: Sexual) and conspecifics but not to the presumed major predator (birds). This study thus suggests that signal brightness

  6. PPPL: Great story, Bright Future | Princeton Plasma Physics Lab

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass mapSpeeding access| Department ofStephen P riceawards |PPPL: Great story, Bright

  7. The Future is bright for Y-12 Â… and diverse

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power AdministrationRobust,Field-effectWorking With U.S.Week Day Year(active tab) 2016TheTheFuture is bright for Y-12

  8. Statistical Properties of Bright Galaxies in the SDSS Photometric System

    E-Print Network [OSTI]

    Shimasaku, K; Doi, M; Hamabe, M; Ichikawa, T; Okamura, S; Sekiguchi, M; Yasuda, N

    2001-01-01

    We investigate the photometric properties of 456 bright galaxies using imaging data recorded during the commissioning phase of the Sloan Digital Sky Survey (SDSS). Morphological classification is carried out by correlating results of several human classifiers. Our purpose is to examine the statistical properties of color indices, scale lengths, and concentration indices as functions of morphology for the SDSS photometric system. We find that $u'-g'$, $g'-r'$, and $r'-i'$ colors of SDSS galaxies match well with those expected from the synthetic calculation of spectroscopic energy distribution of template galaxies and with those transformed from $UBVR_CI_C$ color data of nearby galaxies. The agreement is somewhat poor, however, for $i'-z'$ color band with a discrepancy of $0.1-0.2$ mag. With the aid of the relation between surface brightness and radius obtained by Kent (1985), we estimate the averages of the effective radius of early type galaxies and the scale length of exponential disks both to be 2.6 kpc for...

  9. Robust difference imaging of high surface brightness targets

    E-Print Network [OSTI]

    Kerins, E; Duke, J P; Gould, A; Han, C; Newsam, A; Park, B -G; Street, R

    2010-01-01

    Over the last two decades the Andromeda Galaxy (M31) has been something of a test-bed for methods aimed at obtaining accurate time-domain relative photometry within highly crowded fields. Difference imaging methods, originally pioneered towards M31, have evolved into sophisticated methods, such as the Optimal Image Subtraction (OIS) method of Alard & Lupton (1998), that today are most widely used to survey variable stars, transients and microlensing events in our own Galaxy. We show that modern difference image (DIA) algorithms such as OIS, whilst spectacularly successful towards the Milky Way bulge, may perform badly towards high surface brightness targets such as the M31 bulge. Poor results typically occur in the presence of common data systematics that scale with image flux such as internal reflections, scattered light, flat field errors or fringing. Using data from the Angstrom Project microlensing survey of the M31 bulge, we show that very good results are usually obtainable by first performing caref...

  10. Hacking commercial quantum cryptography systems by tailored bright illumination

    E-Print Network [OSTI]

    Lydersen, Lars; Wittmann, Christoffer; Elser, Dominique; Skaar, Johannes; Makarov, Vadim; 10.1038/NPHOTON.2010.214

    2010-01-01

    The peculiar properties of quantum mechanics allow two remote parties to grow a private, secret key, even if the eavesdropper can do anything permitted by the laws of nature. In quantum key distribution (QKD) the parties exchange non-orthogonal or entangled quantum states to generate quantum correlated classical data. Consequently, QKD implementations always rely on detectors to measure the relevant quantum property of the signal states. However, practical detectors are not only sensitive to quantum states. Here we show how an eavesdropper can exploit such deviations from the ideal behaviour: We demonstrate experimentally how the detectors in two commercially available QKD systems can be fully remote controlled using specially tailored bright illumination. This makes it possible to acquire the full secret key without leaving any trace; we propose an eavesdropping apparatus built of off-the-shelf components. The loophole is likely to be present in most QKD systems using avalanche photo diodes (APDs) to detect ...

  11. Hacking commercial quantum cryptography systems by tailored bright illumination

    E-Print Network [OSTI]

    Lars Lydersen; Carlos Wiechers; Christoffer Wittmann; Dominique Elser; Johannes Skaar; Vadim Makarov

    2011-03-04

    The peculiar properties of quantum mechanics allow two remote parties to communicate a private, secret key, which is protected from eavesdropping by the laws of physics. So-called quantum key distribution (QKD) implementations always rely on detectors to measure the relevant quantum property of single photons. Here we demonstrate experimentally that the detectors in two commercially available QKD systems can be fully remote-controlled using specially tailored bright illumination. This makes it possible to tracelessly acquire the full secret key; we propose an eavesdropping apparatus built of off-the-shelf components. The loophole is likely to be present in most QKD systems using avalanche photodiodes to detect single photons. We believe that our findings are crucial for strengthening the security of practical QKD, by identifying and patching technological deficiencies.

  12. Statistical Properties of Bright Galaxies in the SDSS Photometric System

    E-Print Network [OSTI]

    K. Shimasaku; M. Fukugita; M. Doi; M. Hamabe; T. Ichikawa; S. Okamura; M. Sekiguchi; N. Yasuda

    2001-05-23

    We investigate the photometric properties of 456 bright galaxies using imaging data recorded during the commissioning phase of the Sloan Digital Sky Survey (SDSS). Morphological classification is carried out by correlating results of several human classifiers. Our purpose is to examine the statistical properties of color indices, scale lengths, and concentration indices as functions of morphology for the SDSS photometric system. We find that $u'-g'$, $g'-r'$, and $r'-i'$ colors of SDSS galaxies match well with those expected from the synthetic calculation of spectroscopic energy distribution of template galaxies and with those transformed from $UBVR_CI_C$ color data of nearby galaxies. The agreement is somewhat poor, however, for $i'-z'$ color band with a discrepancy of $0.1-0.2$ mag. With the aid of the relation between surface brightness and radius obtained by Kent (1985), we estimate the averages of the effective radius of early type galaxies and the scale length of exponential disks both to be 2.6 kpc for $L^*$ galaxies. We find that the half light radius of galaxies depends slightly on the color bands, consistent with the expected distribution of star-forming regions for late type galaxies and with the known color gradient for early type galaxies. We also show that the (inverse) concentration index, defined by the ratio of the half light Petrosian radius to the 90% light Petrosian radius, correlates tightly with the morphological type; this index allows us to classify galaxies into early (E/S0) and late (spiral and irregular) types, allowing for a 15-20% contamination from the opposite class compared with eye-classified morphology.

  13. Bright and dark excitons in semiconductor carbon nanotubes: insights from electronic structure calculations

    E-Print Network [OSTI]

    Tretiak, Sergei

    Bright and dark excitons in semiconductor carbon nanotubes: insights from electronic structure Article on the web 23rd March 2009 DOI: 10.1039/b818473a We review electronic structure calculations (bright) and optically forbidden (dark) states from the lowest excitonic band of the nanotubes

  14. Emission Line Properties of the Large Bright Quasar Survey

    E-Print Network [OSTI]

    Karl Forster; Paul J. Green; Thomas L. Aldcroft; Marianne Vestergaard; Craig B. Foltz; Paul C. Hewett

    2000-11-20

    We present measurements of the optical/UV emission lines for a large homogeneous sample of 993 quasars from the Large Bright Quasar Survey. Our largely automated technique accounts for continuum breaks and galactic reddening, and we perform multicomponent fits to emission line profiles, including the effects of blended iron emission, and of absorption lines both galactic and intrinsic. Here we describe the fitting algorithm and present the results of line fits to the LBQS sample, including upper limits to line equivalent widths when warranted. The distribution of measured line parameters, principally equivalent width and FWHM, are detailed for a variety of lines, including upper limits. We thus initiate a large-scale investigation of correlations between the high energy continuum and emission lines in quasars, to be extended to complementary samples using similar techniques. High quality, reproducible measurements of emission lines for uniformly selected samples will advance our understanding of active galaxies, especially in a new era of large surveys selected by a variety of complementary methods.

  15. Magnitude-range brightness variations of overactive K giants

    E-Print Network [OSTI]

    Oláh, K; K?vári, Zs; Granzer, T; Strassmeier, K G; Kriskovics, L; Vida, K

    2014-01-01

    We study three representative, overactive spotted K giants (IL Hya, XX Tri, and DM UMa) known to exhibit V-band light variations between 0.65-1.05 mags. Our aim is to find the origin of their large brightness variation. We employ long-term phase-resolved multicolor photometry, mostly from automatic telescopes, covering 42 yr for IL Hya, 28 yr for XX Tri, and 34 yr for DM UMa. For one target, IL Hya, we present a new Doppler image from NSO data taken in late 1996. Effective temperatures for our targets are determined from all well-sampled observing epochs and are based on a V-I_C color-index calibration. The effective temperature change between the extrema of the rotational modulation for IL Hya and XX Tri is in the range 50-200 K. The bolometric flux during maximum of the rotational modulation, i.e., the least spotted states, varied by up to 39% in IL Hya and up to 54% in XX Tri over the course of our observations. We emphasize that for IL Hya this is just about half of the total luminosity variation that can...

  16. Low Cost Lithography Tool for High Brightness LED Manufacturing

    SciTech Connect (OSTI)

    Andrew Hawryluk; Emily True

    2012-06-30

    The objective of this activity was to address the need for improved manufacturing tools for LEDs. Improvements include lower cost (both capital equipment cost reductions and cost-ofownership reductions), better automation and better yields. To meet the DOE objective of $1- 2/kilolumen, it will be necessary to develop these highly automated manufacturing tools. Lithography is used extensively in the fabrication of high-brightness LEDs, but the tools used to date are not scalable to high-volume manufacturing. This activity addressed the LED lithography process. During R&D and low volume manufacturing, most LED companies use contact-printers. However, several industries have shown that these printers are incompatible with high volume manufacturing and the LED industry needs to evolve to projection steppers. The need for projection lithography tools for LED manufacturing is identified in the Solid State Lighting Manufacturing Roadmap Draft, June 2009. The Roadmap states that Projection tools are needed by 2011. This work will modify a stepper, originally designed for semiconductor manufacturing, for use in LED manufacturing. This work addresses improvements to yield, material handling, automation and throughput for LED manufacturing while reducing the capital equipment cost.

  17. Stellar Populations and Surface Brightness Fluctuations: New Observations and Models

    E-Print Network [OSTI]

    John P. Blakeslee; Alexandre Vazdekis; Edward A. Ajhar

    2000-08-15

    We examine the use of surface brightness fluctuations (SBF) for both stellar population and distance studies. New V-band SBF data are reported for five Fornax cluster galaxies and combined with literature data to define a new V-band SBF distance indicator. We use new stellar population models, based on the latest Padua isochrones transformed empirically to the observational plane, to predict SBF magnitudes and integrated colours for a wide range of population ages and metallicities. We examine the sensitivity of the predictions to changes in the isochrones, transformations, and IMF. The new models reproduce the SBF data for globular clusters fairly well, especially if higher metallicity globulars are younger. The models also give a good match to the "fluctuation colors" of elliptical galaxies. In order to obtain theoretical calibrations of the SBF distance indicators, we combine our single-burst models into composite population models. These models reproduce the observed behavior of the SBF magnitudes as a function of stellar population parameters, including the steep colour dependence found for HST/WFPC2 F814W SBF data. Because the theoretical SBF calibrations are fairly sensitive to uncertain details of stellar evolution, the empirical calibrations are more secure. However, the sensitivity of SBF to these finer details potentially makes it a powerful constraint for stellar evolution and population synthesis. [abbridged

  18. The dearth of nuclear star clusters in bright galaxies

    E-Print Network [OSTI]

    Arca-Sedda, Manuel; Spera, Mario

    2015-01-01

    We investigate the interaction of a massive globular cluster (GC) with a super massive black hole (SMBH), located at the centre of its host galaxy, by means of direct $N$-body simulations. The results show that tidal distortions induced by the stellar background and the SMBH act on a time shorter than that of dynamical friction decay for a $10^6$ M$_\\odot$ GC whenever the SMBH mass exceeds $\\sim 10^8$ M$_\\odot$. This implies an almost complete dissolution of the infalling GC before it reaches the inner region ($\\lesssim 5$ pc) of the parent galaxy. The generalization of this result to a larger sample of infalling GCs shows that such destructive process may prevent the formation and growth of a bright galactic nucleus. Another interesting, serendipitous, result we obtained is that the close interaction between the SMBH and the GC produces a ``wave'' of stars that escape from the cluster and, in a fraction, even from the whole galaxy.

  19. Bright Transients from Black Hole - Neutron Star Mergers

    E-Print Network [OSTI]

    D'Orazio, Daniel J; Murray, Norman W; Price, Larry

    2016-01-01

    Direct detection of black hole-neutron star (BHNS) pairs is anticipated with the advent of aLIGO. Electromagnetic counterparts may be crucial for a confident gravitational-wave detection as well as for extraction of astronomical information. Yet BHNS star pairs are notoriously dark and so inaccessible to telescopes. Contrary to this expectation, a bright electromagnetic transient can occur in the final moments before merger as long as the neutron star is highly magnetized. The orbital motion of the neutron star magnet creates a Faraday flux and corresponding power available for luminosity. A spectrum of curvature radiation ramps up until the rapid injection of energy ignites a fireball, which would appear as an energetic blackbody peaking in the X-ray to gamma-rays for neutron star field strengths ranging from $10^{12}$G to $10^{16}$G respectively and a $10M_{\\odot}$ black hole. The fireball event may last from a few milliseconds to a few seconds depending on the NS magnetic field strength, and may be observa...

  20. Shining light through the Sun

    E-Print Network [OSTI]

    Malcolm Fairbairn; Timur Rashba; Sergey Troitsky

    2007-05-19

    It is shown that the Sun can become partially transparent to high energy photons in the presence of a pseudo-scalar. In particular, if the axion interpretation of the PVLAS result were true then up to 2% of GeV energy gamma rays might pass through the Sun, while an even stronger effect is expected for some axion parameters. We discuss the possibilities of observing this effect. Present data are limited to the observation of the solar occultation of 3C 279 by EGRET in 1991; 98% C.L. detection of a non-zero flux of gamma rays passing through the Sun is not yet conclusive. Since the same occultation happens every October, future experiments, e.g. GLAST, are expected to have better sensitivity.

  1. Measured Properties of the DUVFEL High Brightness, Ultrashort Electron Beam

    SciTech Connect (OSTI)

    Emma, Paul J

    2002-08-20

    The DUVFEL electron linac is designed to produce sub-picosecond, high brightness electron bunches to drive an ultraviolet FEL. The accelerator consists of a 1.6 cell S-band photoinjector, variable pulse length Ti:Sapp laser, 4 SLAC-type S-band accelerating sections, and 4-dipole chicane bunch compressor. In preparation for FEL operation, the compressed electron beam has been fully characterized. Measurement of the beam parameters and simulation of the beam are presented. The properties of the laser and photoinjector are summarized in Table 1. In typical running, 10 mJ of IR light is produced by the Spectraphyics Tsunami Ti:Sapphire oscillator and TSA50 amplifier, which is frequency tripled to produce 450 uJ of UV light. After spatial filtering and aperturing of the gaussian mode to produce a nearly uniform laser spot, about 200-300 uJ is delivered to the cathode. This produces 300 pC of charge at the accelerating phase of 30 degrees. The RF cavity is a Gun IV [1] with copper cathode that has been modified for better performance [2]. In principle, the laser pulse length may be adjusted from 100 fs to 10 ps, however there are practical limitations on the range of adjustment due to dispersion characteristics and efficiency of the BBO crystals. The thickness of the harmonic crystals is optimized for pulse lengths from 1-5 ps. Within this range of pulse lengths there is evidence [3] of variations in the time profile of the UV light that are sensitive to the phase-matching angle of the crystal.

  2. Visualizing individual microtubules by bright field microscopy Braulio Gutirrez-Medinaa

    E-Print Network [OSTI]

    Block, Steven

    a microscope with conventional bright field optics in conjunction with a webcam-type camera and a light-emitting diode illuminator. The light scattered by microtubules is image-processed to remove the background

  3. Compact radiation sources for increased access to high brightness x-rays

    E-Print Network [OSTI]

    O'Shea, Finn Henry

    2012-01-01

    results for the 4.5 GeV LCLS beam. . . . . . . . . . .148 Simulation of a 13.65 GeV LCLS beam . . . . . . . . . .142 LCLS ultra-low charge, high brightness beam

  4. THE STABILITY OF LOW SURFACE BRIGHTNESS DISKS BASED ON MULTI-WAVELENGTH MODELING

    E-Print Network [OSTI]

    MacLachlan, J. M.

    To investigate the structure and composition of the dusty interstellar medium (ISM) of low surface brightness (LSB) disk galaxies, we have used multi-wavelength photometry to construct spectral energy distributions for ...

  5. NREL and SkyFuel Partnership Reflects Bright Future for Solar Energy -

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shines light on771/6/14 Contact:News Releases |NREL Technology6 NewAutomotive

  6. NREL: Technology Transfer - NREL and SkyFuel Partnership Reflects Bright

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shines lightGeospatial ToolkitSMARTS -BeingFuture for Solar Energy NREL and

  7. Asymmetric Surface Brightness Distribution of Altair Observed with the Navy Prototype Optical Interferometer

    E-Print Network [OSTI]

    Naoko Ohishi; Tyler E. Nordgren; Donald J. Hutter

    2004-05-16

    An asymmetric surface brightness distribution of the rapidly rotating A7IV-V star, Altair, has been measured by the Navy Prototype Optical Interferometer (NPOI). The observations were recorded simultaneously using a triangle of three long baselines of 30m, 37m, and 64m, on 19 spectral channels, covering the wavelength range of 520nm to 850nm. The outstanding characteristics of these observations are (a) high resolution with the minimum fringe spacing of 1.7mas, easily resolving the 3-milliarcsecond (mas) stellar disk, and (b) the measurement of closure phase which is a sensitive indicator to the asymmetry of the brightness distribution of the source. Uniform disk diameters fit to the measured squared visibility amplitudes confirms the Altair's oblate shape due to its rapid rotation. The measured observables of Altair showed two features which are inconsistent with both the uniform-disk and limb-darkened disk models, while the measured observable of the comparison star, Vega, are consistent with the limb-darkened disk model. The first feature is that measured squared visibility amplitudes at the first minimum do not reach 0.0 but rather remain at about 0.02, indicating the existence of a small bright region on the stellar disk. The other is that the measured closure phases show non-zero/180 degrees at all spectral channels, which requires an asymmetric surface brightness distribution. We fitted the measured observables to a model with a bright spot on a limb-darkened disk and found the observations are well reproduced by a bright spot, which has relative intensity of 4.7%, on a 3.38 mas limb-darkened stellar disk. Rapid rotation of Altair indicates that this bright region is a pole, which is brighter than other part of the star owing to gravity darkening.

  8. Bright tunable femtosecond x-ray emission from laser irradiated micro-droplets

    SciTech Connect (OSTI)

    Yu, Tong-Pu Hu, Li-Xiang; Yin, Yan; Shao, Fu-Qiu; Zhuo, Hong-Bin; Ma, Yan-Yun; Yang, Xiao-Hu; Luo, Wen; Pukhov, Alexander

    2014-09-15

    It is demonstrated that bright femtosecond X-rays can be obtained by irradiating a moderate laser onto a helium micro-droplet. The laser ponderomotive force continuously sweeps electrons from the droplets and accelerates them forward. The electrons exposed in the outrunning laser field oscillate transversely and emit photons in the forward direction. The total flux of photons with energies above 1?keV is as high as 10{sup 9}/shot which is about 10-fold enhancement compared with betatron oscillation under similar laser conditions. The maximum achieved peak brightness is up to 10{sup 21} photons/s/mm{sup 2}/mrad{sup 2}/0.1%BW. By adjusting laser and droplet parameters, we can get tunable X-rays with required brightness and energy.

  9. The Search for Cosmological Black Holes: A Surface Brightness Variability Test

    E-Print Network [OSTI]

    Geraint F. Lewis; Rodrigo A. Ibata

    2000-04-04

    Recently it has been suggested that the majority of dark matter in the universe resides in the form of Jupiter mass black holes distributed cosmologically. This population makes itself apparent by microlensing high redshift quasars and introducing pronounced variability into their observed light curves. While several arguments dismissing this hypothesis have been presented, a conclusive observational test is, alas, sadly lacking. In this paper we investigate the effect of a cosmologically distributed population of microlensing masses on galaxies at low to intermediate redshift. The magnification of bright stars in these galaxies leads to small, but observable, fluctuations in their surface brightness. The variability time scale for Jupiter-mass lensing objects is of the order of a few months and this population may be detected through a future space-based monitoring campaign of a field containing $z \\sim 0.5$ galaxies. The monitoring of galactic surface brightness will provide an effective test of the nature of dark matter on cosmological scales.

  10. SOLAR POLAR X-RAY JETS AND MULTIPLE BRIGHT POINTS: EVIDENCE FOR SYMPATHETIC ACTIVITY

    SciTech Connect (OSTI)

    Pucci, Stefano; Romoli, Marco; Poletto, Giannina; Sterling, Alphonse C.

    2012-02-15

    We present an analysis of X-ray bright points (BPs) and X-ray jets observed by Hinode/X-Ray Telescope on 2007 November 2-4, within the solar northern polar coronal hole. After selecting small subregions that include several BPs, we followed their brightness evolution over a time interval of a few hours, when several jets were observed. We find that most of the jets occurred in close temporal association with brightness maxima in multiple BPs: more precisely, most jets are closely correlated with the brightening of at least two BPs. We suggest that the jets result from magnetic connectivity changes that also induce the BP variability. We surmise that the jets and implied magnetic connectivity we describe are small-scale versions of the active-region-scale phenomenon, whereby flares and eruptions are triggered by interacting bipoles.

  11. A Characterization of the Brightness Oscillations During Thermonuclear Bursts From 4U 1636-536

    E-Print Network [OSTI]

    M. Coleman Miller

    1999-04-08

    The discovery of nearly coherent brightness oscillations during thermonuclear X-ray bursts from six neutron-star low-mass X-ray binaries has opened up a new way to study the propagation of thermonuclear burning, and may ultimately lead to greater understanding of thermonuclear propagation in other astrophysical contexts, such as in Type Ia supernovae. Here we report detailed analyses of the ~580 Hz brightness oscillations during bursts from 4U 1636-536. We investigate the bursts as a whole and, in more detail, the initial portions of the bursts. We analyze the ~580 Hz oscillations in the initial 0.75 seconds of the five bursts that were used in a previous search for a brightness oscillation at the expected ~290 Hz spin frequency, and find that if the same frequency model describes all five bursts there is insufficient data to require more than a constant frequency or, possibly, a frequency plus a frequency derivative. Therefore, although it is appropriate to use an arbitrarily complicated model of the ~580 Hz oscillations to generate a candidate waveform for the ~290 Hz oscillations, models with more than two parameters are not required by the data. For the bursts as a whole we show that the characteristics of the brightness oscillations vary greatly from burst to burst. We find, however, that in at least one of the bursts, and possibly in three of the four that have strong brightness oscillations throughout the burst, the oscillation frequency reaches a maximum several seconds into the burst and then decreases. This behavior has not been reported previously for burst brightness oscillations, and it poses a challenge to the standard burning layer expansion explanation for the frequency changes.

  12. The Threat to the Planet* Dark & Bright Sides of Global Warming

    E-Print Network [OSTI]

    Hansen, James E.

    The Threat to the Planet* Dark & Bright Sides of Global Warming Jim Hansen 3 October 2007 presented provides most important information on global warming. Recorded human history occurs within the Holocene for these large climate change is perturbations of Earth's orbit. #12;Continental Drift Fig. 1 "Global Warming

  13. Technical Evaluation Report "ND2 Attenuation of the COS Bright Object Aperture"

    E-Print Network [OSTI]

    Colorado at Boulder, University of

    Technical Evaluation Report "ND2 Attenuation of the COS Bright Object Aperture" Date: 30 June 2000 Document Number: COS-11-0019 Revision: Initial Release Contract No.: NAS5-98043 CDRL No.: N/A Prepared By: J. Morse, COS Project Scientist, CU/CASA Date Reviewed By: J. Green, COS Principal Investigator, CU

  14. A Probabilistic Approach of Designing Driving Circuits for Strings of High-Brightness Light

    E-Print Network [OSTI]

    Lehman, Brad

    Email : abhattac@ece.neu.edu Abstract-Often, High Brightness LEDs (HB-LED) are connected in series to create strings. According to their data sheets, the HB-LEDs have a variation in their forward voltage in parallel. This paper proposes a probabilistic approach for modeling the forward voltage drop across the HB-LEDs

  15. KEEPING THE FUTURE BRIGHT 2004 Canadian Electricity Human Resource Sector Study

    E-Print Network [OSTI]

    supply 8 Electricity consumption 9 Supply and demand projections 9 Electricity exports and importsKEEPING THE FUTURE BRIGHT 2004 Canadian Electricity Human Resource Sector Study #12;This project Electricity Association The Canadian Electricity Association (CEA), founded in 1891, is the national forum

  16. Cell Cycle Regulation of Cyclin-Dependent Kinases in Tobacco Cultivar Bright Yellow-2 Cells1

    E-Print Network [OSTI]

    Murray, J.A.H.

    Cell Cycle Regulation of Cyclin-Dependent Kinases in Tobacco Cultivar Bright Yellow-2 Cells1 David different regulation during the cell cycle. CdkA mRNA and protein accumulate during G1 in cells re, although CdkA mRNA and protein levels are not significantly regulated. In contrast, CdkB1 transcripts

  17. DEVELOPMENT OF A HIGH BRIGHTNESS ELECTRON GUN FOR THE ACCELERATOR TEST FACILITY AT BROOKHAVEN NATIONAL LABORATORY*

    E-Print Network [OSTI]

    McDonald, Kirk

    954 DEVELOPMENT OF A HIGH BRIGHTNESS ELECTRON GUN FOR THE ACCELERATOR TEST FACILITY AT BROOKHAVEN, New York 11973 and K. McDonald Princeton [Jniversity Abstract An electron gun utilizing a radio). Here we report on the de;$n of the electron gun which will provide r.f. bunches of up to 10 electrons

  18. Observational difference between gamma and X-ray properties of optically dark and bright GRBs

    SciTech Connect (OSTI)

    Balazs, L. G. [Konkoly Observatory, Budapest (Hungary); Horvath, I. [Bolyai Military University, Budapest (Hungary); Bagoly, Zs.; Veres, P. [Eoetvoes University, Budapest (Hungary); Meszaros, A. [Charles University, Prague (Czech Republic)

    2008-05-22

    Using the discriminant analysis of the multivariate statistical analysis we compared the distribution of the physical quantities of the optically dark and bright GRBs, detected by the BAT and XRT on board of the Swift Satellite. We found that the GRBs having detected optical transients (OT) have systematically higher peak fluxes and lower HI column densities than those without OT.

  19. METHANE AND ETHANE ON THE BRIGHT KUIPER BELT OBJECT 2005 FY9 M. E. Brown,1

    E-Print Network [OSTI]

    Brown, Michael E.

    METHANE AND ETHANE ON THE BRIGHT KUIPER BELT OBJECT 2005 FY9 M. E. Brown,1 K. M. Barkume,1 G. A indicates the clear presence of ethane, an expected product of UV photolysis of methane. No evidence for N2 of 2005 FY9 that leads to large methane grains, abundant sites for ethane formation through UV photolysis

  20. Special Sensor Microwave Imager and Sounder (SSMIS) Antenna Brightness Temperature Data Record (TDR)

    E-Print Network [OSTI]

    Special Sensor Microwave Imager and Sounder (SSMIS) Antenna Brightness Temperature Data Record (TDR/NESDIS/Center for Satellite Applications and Research Contributors from: Banghua Yan (Lead), QSS/JCSDA Ninghai Sun, IMSG, Metoffice, UK Yong Han, STAR/JCSDA Mark Liu, QSS/JCSDA Distribution to: Ralph Ferrrao, STAR Tom Schott, OSD

  1. BRIGHT BROADBAND AFTERGLOWS OF GRAVITATIONAL WAVE BURSTS FROM MERGERS OF BINARY NEUTRON STARS

    SciTech Connect (OSTI)

    Gao He; Ding Xuan; Wu Xuefeng [Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008 (China); Zhang Bing [Department of Physics and Astronomy, University of Nevada, Las Vegas, NV 89154 (United States); Dai Zigao, E-mail: xfwu@pmo.ac.cn, E-mail: zhang@physics.unlv.edu, E-mail: dzg@nju.edu.cn [School of Astronomy and Space Science, Nanjing University, Nanjing 210093 (China)

    2013-07-10

    If double neutron star mergers leave behind a massive magnetar rather than a black hole, then a bright early afterglow can follow the gravitational wave burst (GWB) even if there is no short gamma-ray burst (SGRB)-GWB association or if there is an association but the SGRB does not beam toward Earth. Besides directly dissipating the proto-magnetar wind, as suggested by Zhang, here we suggest that the magnetar wind could push the ejecta launched during the merger process and, under certain conditions, would reach a relativistic speed. Such a magnetar-powered ejecta, when interacting with the ambient medium, would develop a bright broadband afterglow due to synchrotron radiation. We study this physical scenario in detail and present the predicted X-ray, optical, and radio light curves for a range of magnetar and ejecta parameters. We show that the X-ray and optical light curves usually peak around the magnetar spin-down timescale ({approx}10{sup 3}-10{sup 5} s), reaching brightnesses readily detectable by wide-field X-ray and optical telescopes, and remain detectable for an extended period. The radio afterglow peaks later, but is much brighter than the case without a magnetar energy injection. Therefore, such bright broadband afterglows, if detected and combined with GWBs in the future, would be a probe of massive millisecond magnetars and stiff equations of state for nuclear matter.

  2. An Hi selected sample of galaxies ---The Hi mass function and the surface brightness distribution

    E-Print Network [OSTI]

    Zwaan, Martin

    An Hi selected sample of galaxies --- The Hi mass function and the surface brightness distribution from the Arecibo Hi Strip Survey, an unbiased extragalactic Hi survey, combined with optical and 21cm follow­up observations, determine the Hi Mass Function and the cosmological mass density of Hi

  3. Planetary Nebula Planetary Nebula Planetary Nebula The bright glowing outer layers of gas

    E-Print Network [OSTI]

    Bechtold, Jill

    produced by fusion and in the heat of the explosion are scattered into space. Mass: 3 - 60 SM Star from a red giant star. The explosion occurs when the hydrogen fuel in the core is depleted. Mass: 0.5 - 1.0 SM StarPower Points: 5 The bright glowing outer layers of gas ejected from a red giant star

  4. Interpretation of electron holographic phase images and defocused bright-field images of nanocarbon field emitters

    E-Print Network [OSTI]

    Dunin-Borkowski, Rafal E.

    a corresponding out-of-focus image recorded from a similar wire [2]. These images cannot be interpreted usingInterpretation of electron holographic phase images and defocused bright-field images of nanocarbon field, image simulation Electron holography is well suited to the investigation of electric and magnetic

  5. Personal audio with a planar bright zone Philip Coleman,a)

    E-Print Network [OSTI]

    Jackson, Philip JB

    Kingdom Jan Abildgaard Pedersenb) Bang & Olufsen A/S, Peter Bangs Vej 15, DK7600, Struer, Denmark 1 #12 re- production do not consider control of the bright zone phase, which may lead to self. Single-zone approaches have considered plane wave reproduction by focusing the sound energy in to a point

  6. A Spectromicroscopic Study of 3d Transition Metal Interactions with Humic Acid; A bright

    E-Print Network [OSTI]

    Sparks, Donald L.

    A Spectromicroscopic Study of 3d Transition Metal Interactions with Humic Acid; A bright future for Humic Acid Research? (S02- nachtegaal174813-Oral) Abstract: It is important to understand groups of humic acid. Soft X-ray microscopy was applied to map the distribution of carbon containing

  7. The SDSS view of the Palomar-Green bright quasar survey

    SciTech Connect (OSTI)

    Jester, Sebastian; Schneider, Donald P.; Richards, Gordon T.; Green, Richard F.; Schmidt, Maarten; Hall, Patrick B.; Strauss, Michael A.; Vanden Berk, Daniel E.; Stoughton, Chris; Gunn, James E.; Brinkmann, Jon; Kent, Stephen M.; Smith, J.Allyn; Tucker, Douglas, L.; Yanny, Brian; /Fermilab /Penn State U., Astron. Astrophys. /Princeton U.

    2005-02-01

    The author investigates the extent to which the Palomar-Green (PG) Bright Quasar Survey (BQS) is complete and representative of the general quasar population by comparing with imaging and spectroscopy from the Sloan Digital Sky Survey. A comparison of SDSS and PG photometry of both stars and quasars reveals the need to apply a color and magnitude recalibration to the PG data. Using the SDSS photometric catalog, they define the PG's parent sample of objects that are not main-sequence stars and simulate the selection of objects from this parent sample using the PG photometric criteria and errors. This simulation shows that the effective U-B cut in the PG survey is U-B < -0.71, implying a color-related incompleteness. As the color distribution of bright quasars peaks near U-B = -0.7 and the 2-{sigma} error in U-B is comparable to the full width of the color distribution of quasars, the color incompleteness of the BQS is approximately 50% and essentially random with respect to U-B color for z < 0.5. There is however, a bias against bright quasars at 0.5 < z < 1, which is induced by the color-redshift relation of quasars (although quasars at z > 0.5 are inherently rare in bright surveys in any case). They find no evidence for any other systematic incompleteness when comparing the distributions in color, redshift, and FIRST radio properties of the BQS and a BQS-like subsample of the SDSS quasar sample. However, the application of a bright magnitude limit biases the BQS toward the inclusion of objects which are blue in g-i, in particular compared to the full range of g-i colors found among the i-band limited SDSS quasars, and even at i-band magnitudes comparable to those of the BQS objects.

  8. SWIFT PANCHROMATIC OBSERVATIONS OF THE BRIGHT GAMMA-RAY BURST GRB 050525a A. J. Blustin,1

    E-Print Network [OSTI]

    Zhang, Bing

    SWIFT PANCHROMATIC OBSERVATIONS OF THE BRIGHT GAMMA-RAY BURST GRB 050525a A. J. Blustin,1 D. Band,2 S. Barthelmy,2 P. Boyd,2 M. Capalbi,3 S. T. Holland,2 F. E. Marshall,2 K. O. Mason,1 M. Perri,3 T ABSTRACT The bright gamma-ray burst GRB 050525a has been detected with the Swift observatory, providing

  9. AC-driven, color-and brightness-tunable organic light-emitting diodes constructed from an electron only device

    E-Print Network [OSTI]

    Demir, Hilmi Volkan

    - and brightness-tunable organic light-emitting diode (OLED) is reported. This OLED was realized by inserting emission from an organic light- emitting diode (OLED) [1] results from the electron/hole recombinationAC-driven, color- and brightness-tunable organic light-emitting diodes constructed from an electron

  10. Rotation of the Trajectories of Bright soliton and Realignment of Intensity Distribution in the Coupled Nonlinear Schrodinger Equation

    E-Print Network [OSTI]

    Radha, R; Porsezian, K

    2013-01-01

    We revisit the collisional dynamics of bright solitons in the coupled Nonlinear Schrodinger equation. We observe that apart from the intensity redistribution in the interaction of bright solitons, one also witnesses a rotation of the trajectories of bright solitons . The angle of rotation can be varied by suitably manipulating the Self-Phase Modulation (SPM) or Cross Phase Modulation (XPM) parameters.The rotation of the trajectories of the bright solitons arises due to the excess energy that is injected into the dynamical system through SPM or XPM. This extra energy not only contributes to the rotation of the trajectories, but also to the realignment of intensity distribution between the two modes. We also notice that the angular separation between the bright solitons can also manouvred suitably. The above results which exclude quantum superposition for the field vectors may have wider ramifications in nonlinear optics, Bose-Einstein condensates, Left Handed (LH) and Right Handed (RH) meta materials.

  11. Bright Blue

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity ofkandz-cm11 OutreachProductswsicloudwsiclouddenDVA N C E D B L OBransen Plasma Asher An O2 RFand112001

  12. Millimeter Wavelength Brightness Fluctuations of the Atmosphere Above the South Pole

    E-Print Network [OSTI]

    Bussmann, R S; Kuo, C L

    2004-01-01

    We report measurements of the millimeter wavelength brightness fluctuations produced by the atmosphere above the South Pole made with the Arcminute Cosmology Bolometer Array Receiver (ACBAR). The data span the 2002 Austral winter during which ACBAR was mounted on the Viper telescope at the South Pole. We recover the atmospheric signal in the presence of instrument noise by calculating the correlation between signals from distinct elements of the ACBAR bolometer array. With this method, it is possible to measure atmospheric brightness fluctuations with high SNR even under the most stable atmospheric conditions. The observed atmospheric signal is characterized by the parameters of the Komolgorov-Taylor (KT) model, which are the amplitude and power law exponent describing the atmospheric power spectrum, and the two components of the wind angular velocity at the time of the observation. The KT model is typically a good description of the observed fluctuations, and fits to the data produce values of the Komolgorov...

  13. Magnification 3x -1,000,000x Electron Gun High brightness Schottky

    E-Print Network [OSTI]

    Damm, Werner

    SEM Column Magnification 3x - 1,000,000x Electron Gun High brightness Schottky Emitter Resolution Current 1 pA to 40 nA Accelerating Voltage 1 kV to 5 kV, 10kV to 30 kV Gun Vacuum Magnification 150x to 1,000,000x Resolution (SE) Gun Ga liquid metal ion source Chamber

  14. Volume-scalable high-brightness three-dimensional visible light source

    DOE Patents [OSTI]

    Subramania, Ganapathi; Fischer, Arthur J; Wang, George T; Li, Qiming

    2014-02-18

    A volume-scalable, high-brightness, electrically driven visible light source comprises a three-dimensional photonic crystal (3DPC) comprising one or more direct bandgap semiconductors. The improved light emission performance of the invention is achieved based on the enhancement of radiative emission of light emitters placed inside a 3DPC due to the strong modification of the photonic density-of-states engendered by the 3DPC.

  15. The Distribution of Star Formation and Metals in the Low Surface Brightness Galaxy UGC 628

    E-Print Network [OSTI]

    Young, J E; Wang, Sharon X

    2015-01-01

    We introduce the MUSCEL Program (MUltiwavelength observations of the Structure, Chemistry and Evolution of LSB galaxies), a project aimed at determining the star-formation histories of low surface brightness galaxies. MUSCEL utilizes ground-based optical spectra and space-based UV and IR photometry to fully constrain the star-formation histories of our targets with the aim of shedding light on the processes that led low surface brightness galaxies down a different evolutionary path from that followed by high surface brightness galaxies, such as our Milky Way. Here we present the spatially-resolved optical spectra of UGC 628, observed with the VIRUS-P IFU at the 2.7-m Harlen J. Smith Telescope at the McDonald Observatory, and utilize emission-line diagnostics to determine the rate and distribution of star formation as well as the gas-phase metallicity and metallicity gradient. We find highly clustered star formation throughout UGC 628, excluding the core regions, and a log(O/H) metallicity around -4.2, with mo...

  16. Beyond 31 mag/arcsec^2: the low surface brightness frontier with the largest optical telescopes

    E-Print Network [OSTI]

    Trujillo, Ignacio

    2015-01-01

    The detection of optical surface brightness structures in the sky with magnitudes fainter than 30 mag/arcsec^2 (3sigma in 10x10 arcsec boxes; r-band) has remained elusive in current photometric deep surveys. Here we show how present-day 10 meter class telescopes can provide broadband imaging 1.5-2 mag deeper than most previous results within a reasonable amount of time (i.e. <10h on source integration). In particular, we illustrate the ability of the 10.4 m Gran Telescopio de Canarias (GTC) telescope to produce imaging with a limiting surface brightness of 31.5 mag/arcsec^2 (3sigma in 10x10 arcsec boxes; r-band) using 8.1 hours on source. We apply this power to explore the stellar halo of the galaxy UGC00180, a galaxy analogous to M31 located at ~150 Mpc, by obtaining a surface brightness radial profile down to mu_r~33 mag/arcsec^2. This depth is similar to that obtained using star counts techniques of Local Group galaxies, but is achieved at a distance where this technique is unfeasible. We find that the ...

  17. NEAR-IR IMAGING POLARIMETRY TOWARD A BRIGHT-RIMMED CLOUD: MAGNETIC FIELD IN SFO 74

    SciTech Connect (OSTI)

    Kusune, Takayoshi; Sugitani, Koji [Graduate School of Natural Sciences, Nagoya City University, Mizuho-ku, Nagoya 467-8501 (Japan); Miao, Jingqi [Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR (United Kingdom); Tamura, Motohide; Kwon, Jungmi [Department of Astronomy, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033 (Japan); Sato, Yaeko [National Astronomical Observatory, 2-21-1 Osawa, Mikata, Tokyo 181-8588 (Japan); Watanabe, Makoto [Department of Cosmosciences, Hokkaido University, Kita 10, Nishi 8, Kita-ku, Sapporo, Hokkaido 060-0810 (Japan); Nishiyama, Shogo [Faculty of Education, Miyagi University of Education, Sendai 980-0845 (Japan); Nagayama, Takahiro [Department of Physics, Kagoshima University, 1-21-35 Korimoto, Kagoshima 890-0065 (Japan); Sato, Shuji [Department of Astrophysics, Nagoya University, Chikusa-ku, Nagoya 464-8602 (Japan)

    2015-01-01

    We have made near-infrared (JHK {sub s}) imaging polarimetry of a bright-rimmed cloud (SFO 74). The polarization vector maps clearly show that the magnetic field in the layer just behind the bright rim is running along the rim, quite different from its ambient magnetic field. The direction of the magnetic field just behind the tip rim is almost perpendicular to that of the incident UV radiation, and the magnetic field configuration appears to be symmetric as a whole with respect to the cloud symmetry axis. We estimated the column and number densities in the two regions (just inside and far inside the tip rim) and then derived the magnetic field strength, applying the Chandrasekhar-Fermi method. The estimated magnetic field strength just inside the tip rim, ?90 ?G, is stronger than that far inside, ?30 ?G. This suggests that the magnetic field strength just inside the tip rim is enhanced by the UV-radiation-induced shock. The shock increases the density within the top layer around the tip and thus increases the strength of the magnetic field. The magnetic pressure seems to be comparable to the turbulent one just inside the tip rim, implying a significant contribution of the magnetic field to the total internal pressure. The mass-to-flux ratio was estimated to be close to the critical value just inside the tip rim. We speculate that the flat-topped bright rim of SFO 74 could be formed by the magnetic field effect.

  18. A Survey of UV Bright Sources Behind the Halo of M31

    E-Print Network [OSTI]

    Fittingoff, Andrew; Kalirai, Jasonjot S; Strader, Jay; Guhathakurta, Puragra; Kaplan, Kyle F

    2009-01-01

    We have performed a wide-area ultraviolet (UV) imaging survey using the GALaxy Evolution eXplorer (GALEX) to search for bright, point-like UV sources behind M31's extended halo. Our survey consisted of 46 pointings covering an effective area of ~50 deg^2, in both the far-UV and near-UV channels. We combined these data with optical R-band observations acquired with the WIYN Mosaic-1 imager on the Kitt Peak National Observatory 0.9m WIYN telescope. An analysis of the brightness and colors of sources matched between our photometric catalogs yielded ~100 UV-bright quasar candidates. We have obtained discovery spectra for 76 of these targets with the Kast spectrometer on the Lick 3m telescope and confirm 30 active galactic nuclei and quasars, 29 galaxies at z > 0.02 including several early-type systems, 16 Galactic stars (hot main-sequence stars), and one featureless source previously identified as a BL Lac object. Future UV spectroscopy of the brightest targets with the Cosmic Origins Spectrograph on the Hubble S...

  19. Night-sky brightness monitoring in Hong Kong - a city-wide light pollution assessment

    E-Print Network [OSTI]

    Pun, Chun Shing Jason

    2011-01-01

    Results of the first comprehensive light pollution survey in Hong Kong are presented. The night-sky brightness was measured and monitored around the city using a portable light sensing device called the Sky Quality Meter over a 15-month period beginning in March 2008. A total of 1,957 data sets were taken at 199 distinct locations, including urban and rural sites covering all 18 Administrative Districts of Hong Kong. The survey shows that the environmental light pollution problem in Hong Kong is severe - the urban night-skies (sky brightness at 15.0 mag per arcsec square) are on average ~100 times brighter than at the darkest rural sites (20.1 mag per arcsec square), indicating that the high lighting densities in the densely populated residential and commercial areas lead to light pollution. In the worst polluted urban location studied, the night-sky at 13.2 mag per arcsec square can be over 500 times brighter than the darkest sites in Hong Kong. The observed night-sky brightness is found to be affected by hu...

  20. New bright optical spectrophotometric standards: A-type stars from the STIS Next Generation Spectral Library

    E-Print Network [OSTI]

    Prieto, Carlos Allende

    2015-01-01

    Exoplanets have sparked interest in extremely high signal-to-noise ratio spectroscopic observations of very bright stars, in a regime where flux calibrators, in particular DA white dwarfs, are not available. We argue that A-type stars offer a useful alternative and reliable space-based spectrophotometry is now available for a number of bright ones in the range 3model fluxes, we identify 18 new very-bright trustworthy A-type flux standards for the optical range (400-800 nm), and provide scaled model fluxes for them. Our tests suggest that the absolute fluxes for these stars in the optical are reliable to within 3%. We limit the spectral range to 400-800 nm, since our models have difficulties to reproduce the observed fluxes in the near-infrared and, especially, in the near-UV, where the discrepancies rise up to ~ 10%. Based on our model fits, we derive angular diameters with an estimated accuracy of about 1%.

  1. Cloning Hubble Deep Fields II: Models for Evolution by Bright Galaxy Image Transformation

    E-Print Network [OSTI]

    Rychard J. Bouwens; Tom Broadhurst; Joseph Silk

    1998-10-29

    In a companion paper we outlined a methodology for generating parameter-free, model-independent ``no-evolution'' fields of faint galaxy images, demonstrating the need for significant evolution in the HDF at faint magnitudes. Here we incorporate evolution into our procedure, by transforming the input bright galaxy images with redshift, for comparison with the HDF at faint magnitudes. Pure luminosity evolution is explored assuming that galaxy surface brightness evolves uniformly, at a rate chosen to reproduce the I-band counts. This form of evolution exacerbates the size discrepancy identified by our no-evolution simulations, by increasing the area of a galaxy visible to a fixed isophote. Reasonable dwarf-augmented models are unable to generate the count excess invoking moderate rates of stellar evolution. A plausible fit to the counts and sizes is provided by `mass-conserving' density-evolution, consistent with small-scale hierarchical growth, where the product of disk area and space density is conserved with redshift. Here the increased surface brightness generated by stellar evolution is accomodated by the reduced average galaxy size, for a wide range of geometries. These models are useful for assessing the limitations of the HDF images, by calculating their rates of incompleteness and the degree of over-counting. Finally we demonstrate the potential for improvement in quantifying evolution at fainter magnitudes using the HST Advanced Camera, with its superior UV and optical performance.

  2. Careers Bachelor if Sciences in The future is bright for those pursuing an education in geology or a geoscience

    E-Print Network [OSTI]

    Walker, Lawrence R.

    Careers ­ Bachelor if Sciences in Geology The future is bright for those pursuing an education in geology or a geoscience related field as demand and gas industry (median $125,350). Forbes recently ranked Geology #7 in its "15

  3. Abundance gradients in low surface brightness spirals: clues on the origin of common gradients in galactic discs

    E-Print Network [OSTI]

    Bresolin, Fabio

    2015-01-01

    We acquired spectra of 141 HII regions in ten late-type low surface brightness galaxies (LSBGs). The analysis of the chemical abundances obtained from the nebular emission lines shows that metallicity gradients are a common feature of LSBGs, contrary to previous claims concerning the absence of such gradients in this class of galaxies. The average slope, when expressed in units of the isophotal radius, is found to be significantly shallower in comparison to galaxies of high surface brightness. This result can be attributed to the reduced surface brightness range measured across their discs, when combined with a universal surface mass density-metallicity relation. With a similar argument we explain the common abundance gradient observed in high surface brightness galaxy (HSBG) discs and its approximate dispersion. This conclusion is reinforced by our result that LSBGs share the same common abundance gradient with HSBGs, when the slope is expressed in terms of the exponential disc scale length.

  4. A SOUTHERN SKY AND GALACTIC PLANE SURVEY FOR BRIGHT KUIPER BELT OBJECTS

    SciTech Connect (OSTI)

    Sheppard, Scott S.; Udalski, Andrzej; Kubiak, Marcin; Pietrzynski, Grzegorz; Poleski, Radoslaw; Soszynski, Igor; Szymanski, Michal K.; Ulaczyk, Krzysztof; Trujillo, Chadwick

    2011-10-15

    About 2500 deg{sup 2} of sky south of declination -25{sup 0} and/or near the Galactic Plane were surveyed for bright outer solar system objects. This survey is one of the first large-scale southern sky and Galactic Plane surveys to detect dwarf planets and other bright Kuiper Belt Objects in the trans-Neptunian region. The survey was able to obtain a limiting R-band magnitude of 21.6. In all, 18 outer solar system objects were detected, including Pluto which was detected near the Galactic center using optimal image subtraction techniques to remove the high stellar density background. Fourteen of the detections were previously unknown trans-Neptunian objects, demonstrating that the southern sky had not been well searched to date for bright outer solar system objects. Assuming moderate albedos, several of the new discoveries from this survey could be in hydrostatic equilibrium and thus could be considered dwarf planets. Combining this survey with previous surveys from the northern hemisphere suggests that the Kuiper Belt is nearly complete to around 21st magnitude in the R band. All the main dynamical classes in the Kuiper Belt are occupied by at least one dwarf-planet-sized object. The 3:2 Neptune resonance, which is the innermost well-populated Neptune resonance, has several large objects while the main outer Neptune resonances such as the 5:3, 7:4, 2:1, and 5:2 do not appear to have any large objects. This indicates that the outer resonances are either significantly depleted in objects relative to the 3:2 resonance or have a significantly different assortment of objects than the 3:2 resonance. For the largest objects (H < 4.5 mag), the scattered disk population appears to have a few times more objects than the main Kuiper Belt (MKB) population, while the Sedna population could be several times more than that of the MKB.

  5. EMPIRICAL DETERMINATION OF EINSTEIN A-COEFFICIENT RATIOS OF BRIGHT [Fe II] LINES

    SciTech Connect (OSTI)

    Giannini, T.; Antoniucci, S.; Nisini, B.; Lorenzetti, D.; Alcalá, J. M.; Bacciotti, F.; Podio, L.; Bonito, R.; Stelzer, B.

    2015-01-01

    The Einstein spontaneous rates (A-coefficients) of Fe{sup +} lines have been computed by several authors with results that differ from each other by up to 40%. Consequently, models for line emissivities suffer from uncertainties that in turn affect the determination of the physical conditions at the base of line excitation. We provide an empirical determination of the A-coefficient ratios of bright [Fe II] lines that would represent both a valid benchmark for theoretical computations and a reference for the physical interpretation of the observed lines. With the ESO-Very Large Telescope X-shooter instrument between 3000 Å and 24700 Å, we obtained a spectrum of the bright Herbig-Haro object HH 1. We detect around 100 [Fe II] lines, some of which with a signal-to-noise ratios ?100. Among these latter lines, we selected those emitted by the same level, whose dereddened intensity ratios are direct functions of the Einstein A-coefficient ratios. From the same X-shooter spectrum, we got an accurate estimate of the extinction toward HH 1 through intensity ratios of atomic species, H I  recombination lines and H{sub 2} ro-vibrational transitions. We provide seven reliable A-coefficient ratios between bright [Fe II] lines, which are compared with the literature determinations. In particular, the A-coefficient ratios involving the brightest near-infrared lines (?12570/?16440 and ?13209/?16440) are in better agreement with the predictions by the Quinet et al. relativistic Hartree-Fock model. However, none of the theoretical models predict A-coefficient ratios in agreement with all of our determinations. We also show that literature data of near-infrared intensity ratios better agree with our determinations than with theoretical expectations.

  6. Origin of the bright prompt optical emission in the naked eye burst

    SciTech Connect (OSTI)

    Hascoeet, R.; Daigne, F.; Mochkovitch, R.

    2010-10-15

    The huge optical brightness of GRB 080319B (the 'Naked Eye Burst') makes this event really challenging for models of the prompt GRB emission. In the framework of the internal shock model, we investigate a scenario where the dominant radiative process is synchrotron emission and the high optical flux is due to the dynamical properties of the relativistic outflow : if the initial Lorentz factor distribution in the jet is highly variable, many internal shocks will form within the outflow at various radii. The most violent shocks will produce the main gamma-ray component while the less violent ones will contribute at lower energy, including the optical range.

  7. Bright Integrated Photon-Pair Source for Practical Passive Decoy-State Quantum Key Distribution

    E-Print Network [OSTI]

    Stephan Krapick; Michael Stefszky; Michal Jachura; Benjamin Brecht; Malte Avenhaus; Christine Silberhorn

    2014-01-28

    We report on a bright, nondegenerate type-I parametric down-conversion source, which is well suited for passive decoy-state quantum key distribution. We show the photon-number-resolved analysis over a broad range of pump powers and we prove heralded higher-order $n$-photon states up to $n=4$. The inferred photon click statistics exhibit excellent agreements to the theoretical predictions. From our measurement results we conclude that our source meets the requirements to avert photon-number-splitting attacks.

  8. Correlation analysis of mean global radiation values with mean brightness values for one year 

    E-Print Network [OSTI]

    Kolczynski, Edward Franklin

    1971-01-01

    quantities of global radiation, = kb. sin h i oi where i denotes the number of the month (1 to 12), Q. is the individual monthly quantity of global radiation, h . is the solar altitude relat- oi ed to noon of the middle day of the month, and k is the coei... which now exists in the data bank of this field. B. ~Db' t' The objective of the proposed research is to investigate a pos- sible relationship between global radiation, as measured from ground- based instruments, and mean brightness values...

  9. Bright Young Minds for a Clean Energy Future | Department of Energy

    Broader source: Energy.gov (indexed) [DOE]

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of Natural GasAdjustmentsShirley Ann JacksonDepartment of EnergyResearchers atDayWhenBethanyOnAristides Patrinos,Bright Young

  10. Asymmetric Surface Brightness Distribution of Altair Observed with the Navy Prototype Optical Interferometer

    E-Print Network [OSTI]

    Ohishi, N; Hutter, D J; Ohishi, Naoko; Nordgren, Tyler E.; Hutter, Donald J.

    2004-01-01

    An asymmetric surface brightness distribution of the rapidly rotating A7IV-V star, Altair, has been measured by the Navy Prototype Optical Interferometer (NPOI). The observations were recorded simultaneously using a triangle of three long baselines of 30m, 37m, and 64m, on 19 spectral channels, covering the wavelength range of 520nm to 850nm. The outstanding characteristics of these observations are (a) high resolution with the minimum fringe spacing of 1.7mas, easily resolving the 3-milliarcsecond (mas) stellar disk, and (b) the measurement of closure phase which is a sensitive indicator to the asymmetry of the brightness distribution of the source. Uniform disk diameters fit to the measured squared visibility amplitudes confirms the Altair's oblate shape due to its rapid rotation. The measured observables of Altair showed two features which are inconsistent with both the uniform-disk and limb-darkened disk models, while the measured observable of the comparison star, Vega, are consistent with the limb-darke...

  11. The Dark Bursts population in a complete sample of bright Swift Long Gamma-Ray Bursts

    E-Print Network [OSTI]

    A. Melandri; B. Sbarufatti; P. D'Avanzo; R. Salvaterra; S. Campana; S. Covino; S. D. Vergani; L. Nava; G. Ghisellini; G. Ghirlanda; D. Fugazza; V. Mangano; M. Capalbi; G. Tagliaferri

    2012-02-14

    We study the properties of the population of optically dark events present in a carefully selected complete sample of bright Swift long gamma-ray bursts. The high level of completeness in redshift of our sample (52 objects out of 58) allow us to establish the existence of a genuine dark population and we are able to estimate the maximum fraction of dark burst events (~30%) expected for the whole class of long gamma-ray burst. The redshift distribution of this population of dark bursts is similar to the one of the whole sample. Interestingly, the rest-frame X-ray luminosity (and the de-absorbed X-ray flux) of the sub-class of dark bursts is slightly higher than the average luminosity of the non-dark events. At the same time the prompt properties do not differ and the optical flux of dark events is at the lower tail of the optical flux distribution, corrected for Galactic absorption. All these properties suggest that dark bursts events generate in much denser environments with respect to normal bright events. We can therefore exclude the high-z and the low-density scenarios and conclude that the major cause of the origin of optically dark events is the dust extinction.

  12. SN1994D in NGC4526: a normally bright type Ia supernova

    E-Print Network [OSTI]

    Georg Drenkhahn; Tom Richtler

    1999-09-07

    SN1994D of type Ia has been suspected not to fit into the relation between decline rate, colour, and brightness. However, an individual distance of its host galaxy, NGC4526, other than that of the Virgo cluster, has not yet been published. We determined the distance by the method of globular cluster luminosity functions on the basis of HST archive data. A maximum-likelihood fit returns apparent turn-over magnitudes of 23.16+-0.16mag in V and 21.96+-0.09mag in I. The corresponding distance modulus is 30.4+-0.3mag, where the error reflects our estimation of the absolute distance scale. The absolute magnitudes (not corrected for decline rate and colour) are -18.67+-0.30mag, -18.62+-0.30mag, and -18.40+-0.30mag for B, V, and I, respectively. The corrected magnitudes are -18.69+-0.31mag, -18.69+-0.31mag, and -18.44+-0.31mag. Compared with other supernovae with reliably determined distances, SN1994D fits within the errors. It is therefore not a counter-example against a uniform decline-rate-colour-brightness relation.

  13. Much Ado about Microbunching: Coherent Bunching in High Brightness Electron Beams

    SciTech Connect (OSTI)

    Ratner, Daniel; /Stanford U. /SLAC

    2012-05-25

    The push to provide ever brighter coherent radiation sources has led to the creation of correspondingly bright electron beams. With billions of electrons packed into normalized emittances (phase space) below one micron, collective effects may dominate both the preservation and use of such ultra-bright beams. An important class of collective effects is due to density modulations within the bunch, or microbunching. Microbunching may be deleterious, as in the case of the Microbunching Instability (MBI), or it may drive radiation sources of unprecedented intensity, as in the case of Free Electron Lasers (FELs). In this work we begin by describing models of microbunching due to inherent beam shot noise, which sparks both the MBI as well as SLAC's Linac Coherent Light Source, the world's first hard X-ray laser. We first use this model to propose a mechanism for reducing the inherent beam shot noise as well as for predicting MBI effects. We then describe experimental measurements of the resulting microbunching at LCLS, including optical radiation from the MBI, as well as the first gain length and harmonic measurements from a hard X-ray FEL. In the final chapters, we describe schemes that use external laser modulations to microbunch light sources of the future. In these sections we describe coherent light source schemes for both both linacs and storage rings.

  14. EM Shines with Five DOE Sustainability Awards

    Broader source: Energy.gov [DOE]

    WASHINGTON, D.C. – EM was selected for five DOE 2013 Sustainability Awards that recognize individual and group efforts at the Oak Ridge, Savannah River and Portsmouth sites.

  15. Virginia Tech Shines Light on Home Efficiency

    Broader source: Energy.gov [DOE]

    Collegiate teams from around the world came to Madrid this month to present their solar-powered houses in the first biennial Solar Decathlon Europe, a competition modeled after the Energy Department's Solar Decathlon in Washington, D.C.

  16. The Dark Penguin Shines Light at Colliders

    E-Print Network [OSTI]

    Primulando, Reinard; Tsai, Yuhsin

    2015-01-01

    Collider experiments are one of the most promising ways to constrain Dark Matter (DM) interactions. For several types of DM-Standard Model couplings, a meaningful interpretation of the results requires to go beyond effective field theory, considering simplified models with light mediators. This is especially important in the case of loop-mediated interactions. In this paper we perform the first simplified model study of the magnetic dipole interacting DM, by including the one-loop momentum-dependent form factors that mediate the coupling -- given by the Dark Penguin -- in collider processes. We compute bounds from the monojet, monophoton, and diphoton searches at the $8$ and $14$ TeV LHC, and compare the results to those of direct and indirect detection experiments. Future searches at the $100$ TeV hadron collider and at the ILC are also addressed. We find that the optimal search strategy requires loose cuts on the missing transverse energy, to capture the enhancement of the form factors near the threshold fo...

  17. Collaboration Shines in Materials Project Success

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    its December cover as a top world-changing idea of 2013. The Materials Project, an open, web-hosted service, allows scientists using supercomputers and quantum mechanical...

  18. Lasers will shine in future warfare

    SciTech Connect (OSTI)

    Kramer, David

    2014-07-01

    High-power radio and microwave beams join cost-effective, solid-state lasers on US military’s horizon.

  19. Flying on Sun Shine: Sailing in Space

    SciTech Connect (OSTI)

    Alhorn, Dean

    2012-03-28

    On January 20th, 2011, NanoSail-D successfully deployed its sail in space. It was the first solar sail vehicle to orbit the earth and the second sail ever unfurled in space. The 10m2 sail, deployment mechanism and electronics were packed into a 3U CubeSat with a volume of about 3500cc. The NanoSail-D mission had two objectives: eject a nanosatellite from a minisatellite; deploy its sail from a highly compacted volume to validate large structure deployment and potential de-orbit technologies. NanoSail-D was jointly developed by NASA's Marshall Space Flight Center and Ames Research Center. The ManTech/NeXolve Corporation provided key sail design support. NanoSail-D is managed by Marshall and jointly sponsored by the Army Space and Missile Defense Command, the Space Test Program, the Von Braun Center for Science and Innovation and Dynetics Inc. The presentation will provide insights into sailcraft advances and potential missions enabled by this emerging in-space propulsion technology.

  20. Shining a spotlight on intact proteins

    SciTech Connect (OSTI)

    Pasa-Tolic, Ljiljana; Masselon, Christophe

    2014-05-01

    Cells react to cues from their environment using various mechanisms that include changes in metabolites, gene expression, protein binding partners, protein localization, and protein posttranslational modifications (PTMs), all of which contribute to altered cellular signatures that enable appropriate cellular responses. Given the seemingly infinite number of mechanisms available to affect protein function and modulate biological processes, the question arises as to how cells manage to interpret protein readouts to accomplish the appropriate cell-type specific response to a particular stimulus.

  1. Sun Shine Solar | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page| Open Energy Information Serbia-Enhancing CapacityVectren)Model for the EntireOpenSumpter,Energy Group LLCCoop,

  2. Collaboration Shines in Materials Project Success

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity ofkandz-cm11 Outreach Home Room News PublicationsAuditsCluster Compatibility Mode Cluster

  3. Special announcement: Building 9731 shines again

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power AdministrationRobust,Field-effect Photovoltaics -7541C.3 Special Report: OAS-RA-14-03

  4. High brightness--multiple beamlets source for patterned X-ray production

    DOE Patents [OSTI]

    Leung, Ka-Ngo (Hercules, CA); Ji, Qing (Albany, CA); Barletta, William A. (Oakland, CA); Jiang, Ximan (El Cerrito, CA); Ji, Lili (Albany, CA)

    2009-10-27

    Techniques for controllably directing beamlets to a target substrate are disclosed. The beamlets may be either positive ions or electrons. It has been shown that beamlets may be produced with a diameter of 1 .mu.m, with inter-aperture spacings of 12 .mu.m. An array of such beamlets, may be used for maskless lithography. By step-wise movement of the beamlets relative to the target substrate, individual devices may be directly e-beam written. Ion beams may be directly written as well. Due to the high brightness of the beamlets from extraction from a multicusp source, exposure times for lithographic exposure are thought to be minimized. Alternatively, the beamlets may be electrons striking a high Z material for X-ray production, thereafter collimated to provide patterned X-ray exposures such as those used in CAT scans. Such a device may be used for remote detection of explosives.

  5. A bright on-demand source of indistinguishable single photons at telecom wavelengths

    E-Print Network [OSTI]

    Kim, Je-Hyung; Richardson, Christopher J K; Leavitt, Richard P; Waks, Edo

    2015-01-01

    Long-distance quantum communication relies on the ability to efficiently generate and prepare single photons at telecom wavelengths. In many applications these photons must also be indistinguishable such that they exhibit interference on a beamsplitter, which implements effective photon-photon interactions. However, deterministic generation of indistinguishable single photons with high brightness remains a challenging problem. We demonstrate a telecom wavelength source of indistinguishable single photons using an InAs/InP quantum dot in a nanophotonic cavity. The cavity enhances the quantum dot emission, resulting in a nearly Gaussian transverse mode profile with high out-coupling efficiency exceeding 46%, leading to detected photon count rates that would exceed 1.5 million counts per second. We also observe Purcell enhanced spontaneous emission rate as large as 4. Using this source, we generate linearly polarized, high purity single photons at telecom-wavelength and demonstrate the indistinguishable nature o...

  6. EUV light source with high brightness at 13.5 nm

    SciTech Connect (OSTI)

    Borisov, V M; Prokof'ev, A V; Khristoforov, O B [State Research Center of Russian Federation 'Troitsk Institute for Innovation and Fusion Research', Troitsk, Moscow Region (Russian Federation); Koshelev, K N [Institute of Spectroscopy, Russian Academy of Sciences, Troitsk, Moscow (Russian Federation); Khadzhiyskiy, F Yu [EUV Labs, Ltd., Troitsk, Moscow (Russian Federation)

    2014-11-30

    The results of the studies on the development of a highbrightness radiation source in the extreme ultraviolet (EUV) range are presented. The source is intended for using in projection EUV lithography, EUV mask inspection, for the EUV metrology, etc. Novel approaches to creating a light source on the basis of Z-pinch in xenon allowed the maximal brightness [130 W(mm{sup 2} sr){sup -1}] to be achieved in the vicinity of plasma for this type of radiation sources within the 2% spectral band centred at the wavelength of 13.5 nm that corresponds to the maximal reflection of multilayer Mo/Si mirrors. In this spectral band the radiation power achieves 190 W in the solid angle of 2? at a pulse repetition rate of 1.9 kHz and an electric power of 20 kW, injected into the discharge. (laser applications and other topics in quantum electronics)

  7. Bright microwave pulses from PSR B0531+21 observed with a prototype transient survey receiver

    SciTech Connect (OSTI)

    O'Dea, J. Andrew; Cheng, Tsan-Huei; Buu, Chau M.; Asmar, Sami W.; Armstrong, J. W.; Jenet, F. A.; Beroiz, Martin

    2014-05-01

    Recent discoveries of transient radio events have renewed interest in time-variable astrophysical phenomena. Many radio transient events are rare, requiring long observing times for reliable statistical study. The National Aeronautics and Space Administration/Jet Propulsion Laboratory's Deep Space Network (DSN) tracks spacecraft nearly continuously with 13 large-aperture, low system temperature radio antennas. During normal spacecraft operations, the DSN processes only a small fraction of the pre-detection bandwidth available from these antennas; any information in the remaining bandwidth, e.g., from an astronomical source in the same antenna beam as the spacecraft, is currently ignored. As a firmware modification to the standard DSN tracking receiver, we built a prototype receiver that could be used for astronomical transient surveys. Here, we demonstrate the receiver's utility through observations of bright pulses from the Crab pulsar and describe attributes of potential transient survey observations piggybacking on operational DSN tracks.

  8. Selective excitation of bright and dark plasmonic resonances of single gold nanorods

    E-Print Network [OSTI]

    Demichel, O; Francs, G Colas des; Bouhelier, A; Hertz, E; Billard, F; de Fornel, F; Cluzel, B

    2015-01-01

    Plasmonic dark modes are pure near-field resonances since their dipole moments are vanishing in far field. These modes are particularly interesting to enhance nonlinear light-matter interaction at the nanometer scale because radiative losses are mitigated therefore increasing the intrinsic lifetime of the resonances. However, the excitation of dark modes by standard far field approaches is generally inefficient because the symmetry of the electromagnetic near-field distribution has a poor overlap with the excitation field. Here, we demonstrate the selective optical excitation of bright and dark plasmonic modes of single gold nanorods by spatial phase-shaping the excitation beam. Using two-photon luminescence measurements, we unambiguously identify the symmetry and the order of the emitting modes and analyze their angular distribution by Fourier-space imaging.

  9. Modeling solar coronal bright point oscillations with multiple nanoflare heated loops

    E-Print Network [OSTI]

    Chandrashekhar, K

    2015-01-01

    Intensity oscillations of coronal bright points (BPs) have been studied for past several years. It has been known for a while that these BPs are closed magnetic loop like structures. However, initiation of such intensity oscillations is still an enigma. There have been many suggestions to explain these oscillations, but modeling of such BPs have not been explored so far. Using a multithreaded nanoflare heated loop model we study the behavior of such BPs in this work. We compute typical loop lengths of BPs using potential field line extrapolation of available data (Chandrashekhar et al. 2013), and set this as the length of our simulated loops. We produce intensity like observables through forward modeling and analyze the intensity time series using wavelet analysis, as was done by previous observers. The result reveals similar intensity oscillation periods reported in past observations. It is suggested these oscillations are actually shock wave propagations along the loop. We also show that if one considers di...

  10. Thermometric- and Acoustic-Based Beam Power Monitor for Ultra-Bright X-Rays

    SciTech Connect (OSTI)

    Bentsen, Gregory; /Rochester U. /SLAC

    2010-08-25

    A design for an average beam power monitor for ultra-bright X-ray sources is proposed that makes simultaneous use of calorimetry and radiation acoustics. Radiation incident on a solid target will induce heating and ultrasonic vibrations, both of which may be measured to give a fairly precise value of the beam power. The monitor is intended for measuring ultra-bright Free-Electron Laser (FEL) X-ray beams, for which traditional monitoring technologies such as photo-diodes or scintillators are unsuitable. The monitor consists of a Boron Carbide (B{sub 4}C) target designed to absorb most of the incident beam's energy. Resistance temperature detectors (RTD) and piezoelectric actuators are mounted on the outward faces of the target to measure the temperature changes and ultrasonic vibrations induced by the incident beam. The design was tested using an optical pulsed beam (780 nm, 120 and 360 Hz) from a Ti:sapphire oscillator at several energies between 0.8 and 2.6 mJ. The RTDs measured an increase in temperature of about 10 K over a period of several minutes. The piezoelectric sensors recorded ringing acoustic oscillations at 580 {+-} 40 kHz. Most importantly, the amplitude of the acoustic signals was observed to scale linearly with beam power up to 2 mJ of pulse energy. Above this pulse energy, the vibrational signals became nonlinear. Several causes for this nonlinearity are discussed, including amplifier saturation and piezoelectric saturation. Despite this nonlinearity, these measurements demonstrate the feasibility of such a beam power measurement device. The advantage of two distinct measurements (acoustic and thermometric) provides a useful method of calibration that is unavailable to current LCLS diagnostics tools.

  11. Millimeter Wavelength Brightness Fluctuations of the Atmosphere Above the South Pole

    E-Print Network [OSTI]

    R. S. Bussmann; W. L. Holzapfel; C. L. Kuo

    2004-12-02

    We report measurements of the millimeter wavelength brightness fluctuations produced by the atmosphere above the South Pole made with the Arcminute Cosmology Bolometer Array Receiver (ACBAR). The data span the 2002 Austral winter during which ACBAR was mounted on the Viper telescope at the South Pole. We recover the atmospheric signal in the presence of instrument noise by calculating the correlation between signals from distinct elements of the ACBAR bolometer array. With this method, it is possible to measure atmospheric brightness fluctuations with high SNR even under the most stable atmospheric conditions. The observed atmospheric signal is characterized by the parameters of the Komolgorov-Taylor (KT) model, which are the amplitude and power law exponent describing the atmospheric power spectrum, and the two components of the wind angular velocity at the time of the observation. The KT model is typically a good description of the observed fluctuations, and fits to the data produce values of the Komolgorov exponent that are consistent with theoretical expectations. By combining the wind angular velocity results with measurements of the wind linear velocity, we find that the altitude of the observed atmospheric fluctuations is consistent with the distribution of water vapor determined from radiosonde data. For data corresponding to frequency passbands centered on 150, 219, and 274 GHz, we obtain median fluctuation power amplitudes of [10, 38, 74] mK^{2} rad^{-5/3} in Rayleigh-Jeans temperature units. Comparing with previous work, we find that these median amplitudes are approximately an order of magnitude smaller than those found at the South Pole during the Austral summer and at least 30 times lower than found at the ALMA site in the Atacama desert.

  12. Bright solitons in defocusing media with spatial modulation of the quintic nonlinearity

    E-Print Network [OSTI]

    Jianhua Zeng; Boris A. Malomed

    2012-09-04

    It has been recently demonstrated that self-defocusing (SDF) media with the cubic nonlinearity, whose local coefficient grows from the center to periphery fast enough, support stable bright solitons, without the use of any linear potential. Our objective is to test the genericity of this mechanism for other nonlinearities, by applying it to one- and two-dimensional (1D and 2D) quintic SDF media. The models may be implemented in optics (in particular, in colloidal suspensions of nanoparticles), and the 1D model may be applied to the description of the Tonks-Girardeau gas of ultracold bosons. In 1D, the nonlinearity-modulation function is taken as $% g_{0}+\\sinh ^{2}(\\beta x) $. This model admits a subfamily of exact solutions for fundamental solitons. Generic \\ soliton solutions are constructed in a numerical form, and also by means of the Thomas-Fermi and variational approximations (TFA and VA). In particular, a new ansatz for the VA is proposed, in the form of "raised $\\mathrm{sech}$", which provides for an essentially better accuracy than the usual Gaussian ansatz. The stability of all the fundamental (nodeless) 1D solitons is established through the computation of the corresponding eigenvalues for small perturbations, and also verified by direct simulations. Higher-order 1D solitons with two nodes have a limited stability region, all the modes with more than two nodes being unstable. It is concluded that the recently proposed "anti-VK" stability criterion for fundamental bright solitons in systems with SDF nonlinearities holds here too. Particular exact solutions for 2D solitons are produced as well.

  13. Bright, Coherent, Ultrafast Soft X-Ray Harmonics Spanning the Water Window from a Tabletop Light Source

    E-Print Network [OSTI]

    M. C. Chen; P. Arpin; T. Popmintchev; M. Gerrity; B. Zhang; M. Seaberg; M. M. Murnane; H. C. Kapteyn

    2010-06-20

    We demonstrate fully phase matched high-order harmonic generation with emission spanning the water window spectral region important for bio- and nano-imaging and a breadth of materials and molecular dynamics studies. We also generate the broadest bright coherent bandwidth (~300eV) to date obtained from any light source, small or large. The harmonic photon flux at 0.5 keV is 10^3 higher than demonstrated previously, making it possible for the first time to demonstrate spatial coherence in the water window. The continuum emission is consistent with a single attosecond burst, that extends bright attosecond pulses into the soft x-ray region.

  14. ARM: G-band (183 GHz) Vapor Radiometer profiler: 15 microwave brightness temperatures from 170.0 to 183.3 GHz

    DOE Data Explorer [Office of Scientific and Technical Information (OSTI)]

    Maria Cadeddu

    G-band (183 GHz) Vapor Radiometer profiler: 15 microwave brightness temperatures from 170.0 to 183.3 GHz

  15. Optical Wireless based on High Brightness Visible LEDs Grantham Pang, Thomas Kwan, Hugh Liu, Chi-Ho Chan

    E-Print Network [OSTI]

    Pang, Grantham

    tolerance to humidity, low power consumption and minimal heat generation. Light-emitting diodes (LEDsOptical Wireless based on High Brightness Visible LEDs Grantham Pang, Thomas Kwan, Hugh Liu, Chi use of lighting or signaling devices constructed by light-emitting diodes (LEDs). The idea

  16. An Atlas of Halpha and R Images and Radial Profiles of 63 Bright Virgo Cluster Spiral Galaxies

    E-Print Network [OSTI]

    R. A. Koopmann; J. D. P. Kenney; J. Young

    2001-06-19

    Narrow-band Halpha and broadband R images and radial profiles are presented for 63 bright spiral galaxies in the Virgo Cluster. The sample is complete for Sb-Scd galaxies with B magnitude less than 12 and inclination less than 75 degrees. Isophotal radii, disk scalelengths, concentration parameters, and integrated fluxes are derived for the sample galaxies.

  17. Vol. 9,No. 5/May 1992/J. Opt. Soc. Am. A 643 Why is snow so bright?

    E-Print Network [OSTI]

    DeCarlo, Doug

    Vol. 9,No. 5/May 1992/J. Opt. Soc. Am. A 643 Why is snow so bright? J. J. Koenderink Utrecht November 22, 1991; accepted December 3, 1991 Snow seen against an overcast sky typically appears much. INTRODUCTION The albedo of snow typically ranges between 80% (old snow) and 95% (fresh snow), whereas most

  18. P-55 / J. X. Sun P-55: Bright and Efficient Stacked White Organic Light-emitting Diodes

    E-Print Network [OSTI]

    P-55 / J. X. Sun P-55: Bright and Efficient Stacked White Organic Light-emitting Diodes J. X. Sun N mCP N NN N N N TPBi FirPic Alq3 N O N O N O Al EuroDisplay 2005 · 397 #12;P-55 / J. X. Sun

  19. A close-up of the Sun (shown in ultraviolet light) reveals a mottled surface, bright flares,

    E-Print Network [OSTI]

    Christian, Eric

    #12;#12;A close-up of the Sun (shown in ultraviolet light) reveals a mottled surface, bright flares, and tongues of hot gas leaping into space. Though they look like burns in the face of the Sun, sunspots circle in the center of the photo--allows scientists to see the solar wind streaming away from the Sun

  20. Generation of Dark and Bright Spin Wave Envelope Soliton Trains through Self-Modulational Instability in Magnetic Films

    E-Print Network [OSTI]

    Patton, Carl

    Generation of Dark and Bright Spin Wave Envelope Soliton Trains through Self-Modulational spin wave envelope soliton trains from a continuous wave input signal due to spontaneous modulational instability has been observed for the first time. The dark soliton trains were formed from high dispersion

  1. P-107 / C.F. Qiu P-107: Very Bright and Efficient Phosphorescent Organic Light-Emitting

    E-Print Network [OSTI]

    . Introduction Organic-light emitting diodes (OLEDs) as pixels for flat- panel displays are being hotly pursuedP-107 / C.F. Qiu P-107: Very Bright and Efficient Phosphorescent Organic Light-Emitting Diode and Technology Clear Water Bay, Kowloon, Hong Kong Abstract The characteristics of an organic light

  2. All-Star Nanocrystals | U.S. DOE Office of Science (SC)

    Office of Science (SC) Website

    F. Zhu, L. Men, Y. Guo, Q. Zhu, U. Bhattacharjee, P.M. Goodwin, J.W. Petrich, E.A. Smith, J. Vela, "Shape evolution and single particle luminescence of organometal halide...

  3. Introducing the All-Star Geeks of SoSTEM 2014! | Department of...

    Broader source: Energy.gov (indexed) [DOE]

    invention for the President at the White House Science Fair, and Tyrone Davis, a third-year law student who, in 2010, devised innovative ways for a college in North...

  4. Article for The Virginia Star May 2015 "All Stars in the Star City"

    E-Print Network [OSTI]

    Virginia Tech

    , and industrial elements and fixtures. The shop is full of interesting furniture and decorations. We'll try! Virginia Museum of Transportation Its collection has expanded to automotive, aviation, transit, and other

  5. STEM Women All-Stars Hit the Road | Department of Energy

    Broader source: Energy.gov (indexed) [DOE]

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of Natural GasAdjustmentsShirleyEnergyTher i nAandSummaryDIST OFMEAG, Dalton System:Energy< prev nextKarina Edmonds,

  6. Introducing the All-Star Geeks of SoSTEM 2014! | Department of Energy

    Broader source: Energy.gov (indexed) [DOE]

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of Natural GasAdjustmentsShirleyEnergy A plug-inPPLforLDRDEnergy Copyrights ASiteas PreparedDepartment of

  7. arXiv:1404.3440v1[astro-ph.IM]13Apr2014 CCD photometry of bright stars using objective wire mesh

    E-Print Network [OSTI]

    Masci, Frank

    arXiv:1404.3440v1[astro-ph.IM]13Apr2014 CCD photometry of bright stars using objective wire mesh ; accepted #12;­ 2 ­ ABSTRACT Obtaining accurate photometry of bright stars from the ground remains tricky for precision CCD photometry of such stars. Our tests on Cep and its comparison star differing by 5 magnitudes

  8. Generation of continuouswave bright squeezed light S. Schiller, G. Breitenbach, S. F. Pereira, R. Paschotta, A. G. White, and J. Mlynek

    E-Print Network [OSTI]

    White, Andrew G.

    Generation of continuous­wave bright squeezed light S. Schiller, G. Breitenbach, S. F. Pereira, R approaches to the generation of bright amplitude­squeezed light using second­order non­ linear effects in optical cavities. A 0.2 mW beam at 1064 nm exhibiting 4 dB squeezing has been generated using a phase

  9. Mineral hints at bright blue rocks deep in the Earth 12 March 2014 Last updated at 21:16 ET | By Simon Redfern Science writer

    E-Print Network [OSTI]

    Machel, Hans

    Mineral hints at bright blue rocks deep in the Earth 12 March 2014 Last updated at 21:16 ET | By Simon Redfern Science writer Minerals preserved in diamond have revealed hints of the bright blue and back, which it has." Blue planet Prof Joseph Smyth of the University of Colorado has spent many

  10. 29.3 / X. L. Zhu 29.3: Very Bright and Efficient Top-Emitting OLED with Ultra-Thin Yb as

    E-Print Network [OSTI]

    29.3 / X. L. Zhu 29.3: Very Bright and Efficient Top-Emitting OLED with Ultra-Thin Yb as Effective, Kowloon, Hong Kong Abstract Very bright and efficient top-emitting organic light-emitting diodes (TOLEDs OLEDs have attracted much interest due to its potential application in flat-panel displays [1

  11. Suppression of fiber modal noise induced radial velocity errors for bright emission-line calibration sources

    SciTech Connect (OSTI)

    Mahadevan, Suvrath; Halverson, Samuel; Ramsey, Lawrence; Venditti, Nick

    2014-05-01

    Modal noise in optical fibers imposes limits on the signal-to-noise ratio (S/N) and velocity precision achievable with the next generation of astronomical spectrographs. This is an increasingly pressing problem for precision radial velocity spectrographs in the near-infrared (NIR) and optical that require both high stability of the observed line profiles and high S/N. Many of these spectrographs plan to use highly coherent emission-line calibration sources like laser frequency combs and Fabry-Perot etalons to achieve precision sufficient to detect terrestrial-mass planets. These high-precision calibration sources often use single-mode fibers or highly coherent sources. Coupling light from single-mode fibers to multi-mode fibers leads to only a very low number of modes being excited, thereby exacerbating the modal noise measured by the spectrograph. We present a commercial off-the-shelf solution that significantly mitigates modal noise at all optical and NIR wavelengths, and which can be applied to spectrograph calibration systems. Our solution uses an integrating sphere in conjunction with a diffuser that is moved rapidly using electrostrictive polymers, and is generally superior to most tested forms of mechanical fiber agitation. We demonstrate a high level of modal noise reduction with a narrow bandwidth 1550 nm laser. Our relatively inexpensive solution immediately enables spectrographs to take advantage of the innate precision of bright state-of-the art calibration sources by removing a major source of systematic noise.

  12. KIC 4768731: a bright long-period roAp star in the Kepler Field

    E-Print Network [OSTI]

    Smalley, B; Murphy, S J; Lehmann, H; Kurtz, D W; Holdsworth, D L; Cunha, M S; Balona, L A; Briquet, M; Bruntt, H; de Cat, P; Lampens, P; Thygesen, A O; Uytterhoeven, K

    2015-01-01

    We report the identification of 61.45 d^-1 (711.2 mu Hz) oscillations, with amplitudes of 62.6-mu mag, in KIC 4768731 (HD 225914) using Kepler photometry. This relatively bright (V=9.17) chemically peculiar star with spectral type A5 Vp SrCr(Eu) has previously been found to exhibit rotational modulation with a period of 5.21 d. Fourier analysis reveals a simple dipole pulsator with an amplitude that has remained stable over a 4-yr time span, but with a frequency that is variable. Analysis of high-resolution spectra yields stellar parameters of T_eff = 8100 +/- 200 K, log g = 4.0 +/- 0.2, [Fe/H] = +0.31 +/- 0.24 and v sin i = 14.8 +/- 1.6 km/s. Line profile variations caused by rotation are also evident. Lines of Sr, Cr, Eu, Mg and Si are strongest when the star is brightest, while Y and Ba vary in anti-phase with the other elements. The abundances of rare earth elements are only modestly enhanced compared to other roAp stars of similar T_eff and log g. Radial velocities in the literature suggest a significant...

  13. A bright on-demand source of indistinguishable single photons at telecom wavelengths

    E-Print Network [OSTI]

    Je-Hyung Kim; Tao Cai; Christopher J. K. Richardson; Richard P. Leavitt; Edo Waks

    2015-11-17

    Long-distance quantum communication relies on the ability to efficiently generate and prepare single photons at telecom wavelengths. In many applications these photons must also be indistinguishable such that they exhibit interference on a beamsplitter, which implements effective photon-photon interactions. However, deterministic generation of indistinguishable single photons with high brightness remains a challenging problem. We demonstrate a telecom wavelength source of indistinguishable single photons using an InAs/InP quantum dot in a nanophotonic cavity. The cavity enhances the quantum dot emission, resulting in a nearly Gaussian transverse mode profile with high out-coupling efficiency exceeding 46%, leading to detected photon count rates that would exceed 1.5 million counts per second. We also observe Purcell enhanced spontaneous emission rate as large as 4. Using this source, we generate linearly polarized, high purity single photons at telecom-wavelength and demonstrate the indistinguishable nature of the emission using a two-photon interference measurement. Our results provide a promising approach to generate on-demand indistinguishable single photons at telecom wavelength for applications in quantum networking and quantum communication.

  14. V and I Photometry of Bright Giants in the Central Regions of NGC 147

    E-Print Network [OSTI]

    T. J. Davidge

    1994-10-13

    Deep V and I CCD images with sub-arcsec spatial resolution are used to investigate the stellar content of the central regions of the Local Group dwarf elliptical galaxy NGC147. Red giant branch (RGB) stars are resolved over the entire field, and the RGB-tip occurs at I ~ 20.5, suggesting that the distance modulus is 24.3. A comparison with globular cluster sequences indicates that the center of NGC147 is moderately metal-poor, with [Fe/H] ~ -1. This is not significantly different from what was found in the outer regions of the galaxy by Mould, Kristian & Da Costa (1983, ApJ, 270, 471). Moreover, the width of the V-I color distribution at I = 21.0 indicates that a spread in metallicity is present, with sigma[Fe/H] ~ +/- 0.3. There is no evidence of a component more metal-poor than [Fe/H] ~ -1.3. A small population of moderately bright asymptotic giant branch (AGB) stars has also been detected, and the AGB-tip occurs near M{bol} ~ -5.0, indicating that an intermediate-age population is present. It is estimated that the intermediate-age population contributes ~ 2-3% of the V light from NGC147.

  15. Bright X-ray source from a laser-driven micro-plasma-waveguide

    E-Print Network [OSTI]

    Yi, Longqing; Thanh, Phuc Luu; Shen, Baifei

    2015-01-01

    Bright tunable x-ray sources have a number of applications in basic science, medicine and industry. The most powerful sources are synchrotrons, where relativistic electrons are circling in giant storage rings. In parallel, compact laser-plasma x-ray sources are being developed. Owing to the rapid progress in laser technology, very high-contrast femtosecond laser pulses of relativistic intensities become available. These pulses allow for interaction with micro-structured solid-density plasma without destroying the structure by parasitic pre-pulses. The high-contrast laser pulses as well as the manufacturing of materials at micro- and nano-scales open a new realm of possibilities for laser interaction with photonic materials at the relativistic intensities. Here we demonstrate, via numerical simulations, that when coupling with a readily available 1.8 Joule laser, a micro-plasma-waveguide (MPW) may serve as a novel compact x-ray source. Electrons are extracted from the walls by the laser field and form a dense ...

  16. Evidence Against BALS in the X-ray Bright QSO PG1416-129

    E-Print Network [OSTI]

    Paul J. Green; Thomas L. Aldcroft; Smita Mathur; Norbert Schartel

    1997-02-24

    Recent results from the ROSAT All Sky Survey, and from deep ROSAT pointings reveal that broad absorption line quasars (BALQSOs) are weak in the soft X-ray bandpass (with optical-to-X-ray spectral slope alpha_{ox}>1.8) in comparison to QSOs with normal OUV spectra (mean alpha_{ox}=1.4). One glaring exception appeared to be the nearby BALQSO PG1416-129, which is a bright ROSAT source showing no evidence for intrinsic soft X-ray absorption. We present here our new HST FOS spectrum of PG1416-129, in which we find no evidence for BALs. We show that the features resulting in the original BAL classification, based on IUE spectra, were probably spurious. On the basis of UV, X-ray and optical evidence, we conclude that PG1416-129, is not now, and has never been a BALQSO. Our result suggests that weak soft X-ray emission is a defining characteristic of true BALQSOs. If BALQSOs indeed harbor normal intrinsic spectral energy distributions, their observed soft X-ray weakness is most likely the result of absorption. The ubiquitous occurrence of weak soft X-ray emission with UV absorption (BALs) thus suggests absorbers in each energy regime that are physically associated, if not identical.

  17. Detection of the Transverse Proximity Effect: Radiative Feedback from Bright QSOs

    E-Print Network [OSTI]

    T. S. Goncalves; C. C. Steidel; M. Pettini

    2007-11-26

    Measuring the response of the intergalactic medium to a blast of ionizing radiation allows one to infer the physical properties of the medium and, in principle, the lifetime and isotropy of the radiating source. The most sensitive such measurements can be made if the source of radiation is near the line of sight to a bright background QSO. We present results based on deep Keck/HIRES observations of the QSO triplet KP76, KP77 and KP78 at z ~2.5, with separations of 2-3 arcmin on the plane of the sky. Using accurate systemic redshifts of the QSOs from near-IR spectroscopy, we quantify the state of the IGM gas in the proximity regions where the expected ionizing flux from the foreground QSOs exceeds that of the metagalactic background by factors of 10-200, assuming constant and isotropic emission. Based on the unusual ionization properties of the absorption systems with detected HI, CIV, and OVI, we conclude that the gas has been significantly affected by the UV radiation from the nearby QSOs. Aided by observations of the galaxy density near the foreground QSOs, we discuss several effects that may explain why the transverse proximity effect has eluded most previous attempts to detect it. Our observations suggest that the luminosities of KP76 and KP77 have remained comparable to current values over timescales of, respectively, Delta t > 25 Myr and 16 Myr radiation from either QSO was significantly anisotropic during these intervals.

  18. Bright Fireballs Associated with the Potentially Hazardous Asteroid 2007LQ19

    E-Print Network [OSTI]

    Madiedo, Jose M; Ortiz, Jose L; Castro-Tirado, Alberto J; Cabrera-Caño, Jesus

    2014-01-01

    We analyze here two very bright fireballs produced by the ablation in the atmosphere of two large meteoroids in 2009 and 2010. These slow-moving and deep-penetrating events were observed over Spain in the framework of our Spanish Fireball Network continuous meteor monitoring campaign. The analysis of the emission spectrum imaged for one of these fireballs has provided the first clues about the chemical nature of the progenitor meteoroids. The orbital parameters of these particles suggests a likely association with the recently identified July rho-Herculid meteoroid stream. In addition, considerations about the likely parent body of this stream are also made on the basis of orbital dissimilarity criteria. This orbital analysis reveals that both meteoroids and PHA 2007LQ19 exhibit a similar evolution during a time period of almost 8,000 years, which suggests that either this NEO is the potential parent of these particles or that this NEO and both meteoroids had a common progenitor in the past.

  19. GRB 061121: Broadband spectral evolution through the prompt and afterglow phases of a bright burst

    E-Print Network [OSTI]

    Page, K L; Osborne, J P; Zhang, B; Godet, O; Marshall, F E; Melandri, A; Norris, J P; O'Brien, P T; Palshin, V; Rol, E; Romano, P; Starling, R L C; Schady, P; Yost, S A; Barthelmy, S D; Beardmore, A P; Cusumano, G; Burrows, D N; De Pasquale, M; Ehle, M; Evans, P A; Gehrels, N; Goad, M R; Golenetskii, S; Guidorzi, C; Mundell, C; Page, M J; Ricker, G; Sakamoto, T; Schaefer, B E; Stamatikos, M; Troja, E; Ulanov, M; Yuan, F; Ziaeepour, H

    2007-01-01

    Swift triggered on a precursor to the main burst of GRB 061121 (z=1.314), allowing observations to be made from the optical to gamma-ray bands. Many other telescopes, including Konus-Wind, XMM-Newton, ROTSE and the Faulkes Telescope North, also observed the burst. The gamma-ray, X-ray and UV/optical emission all showed a peak ~75s after the trigger, although the optical and X-ray afterglow components also appear early on - before, or during, the main peak. Spectral evolution was seen throughout the burst, with the prompt emission showing a clear positive correlation between brightness and hardness. The Spectral Energy Distribution (SED) of the prompt emission, stretching from 1eV up to 1MeV, is very flat, with a peak in the flux density at ~1keV. The optical-to-X-ray spectra at this time are better fitted by a broken, rather than single, power-law, similar to previous results for X-ray flares. The SED shows spectral hardening as the afterglow evolves with time. This behaviour might be a symptom of self-Compto...

  20. Swift panchromatic observations of the bright gamma-ray burst GRB050525a

    E-Print Network [OSTI]

    Blustin, A J; Barthelmy, S; Boyd, P; Capalbi, M; Holland, S T; Marshall, F E; Mason, K O; Perri, M; Poole, T; Roming, P; Rosen, S; Schady, P; Still, M; Zhang, B; team, for the Swift

    2006-01-01

    The bright gamma-ray burst GRB050525a has been detected with the Swift observatory, providing unique multiwavelength coverage from the very earliest phases of the burst. The X-ray and optical/UV afterglow decay light curves both exhibit a steeper slope ~0.15 days after the burst, indicative of a jet break. The timing of the jet break combined with the total gamma-ray energy of the burst constrains the opening angle of the jet to be 2.5 degrees. We derive an empirical `time-lag' redshift from the BAT data of z_hat = 0.69 +/- 0.02, in good agreement with the spectroscopic redshift of 0.61. Prior to the jet break, the X-ray data can be modelled by a simple power law with index alpha = -1.2. However after 300s the X-ray flux brightens by about 30% compared to the power-law fit. The optical/UV data have a more complex decay, with evidence of a rapidly falling reverse shock component that dominates in the first minute or so, giving way to a flatter forward shock component at later times. The multiwavelength X-ray/U...

  1. Preparation of brightness stabilization agent for lignin containing pulp from biomass pyrolysis oils

    DOE Patents [OSTI]

    Agblevor, Foster A. (Blacksburg, VA); Besler-Guran, Serpil (Flemington, NJ)

    2001-01-01

    A process for producing a brightness stabilization mixture of water-soluble organic compounds from biomass pyrolysis oils comprising: a) size-reducing biomass material and pyrolyzing the size-reduced biomass material in a fluidized bed reactor; b) separating a char/ash component while maintaining char-pot temperatures to avoid condensation of pyrolysis vapors; c) condensing pyrolysis gases and vapors, and recovering pyrolysis oils by mixing the oils with acetone to obtain an oil-acetone mixture; d) evaporating acetone and recovering pyrolysis oils; e) extracting the pyrolysis oils with water to obtain a water extract; f) slurrying the water extract with carbon while stirring, and filtering the slurry to obtain a colorless filtrate; g) cooling the solution and stabilizing the solution against thermally-induced gelling and solidification by extraction with ethyl acetate to form an aqueous phase lower layer and an organic phase upper layer; h) discarding the upper organic layer and extracting the aqueous layer with ethyl acetate, and discarding the ethyl acetate fraction to obtain a brown-colored solution not susceptible to gelling or solidification upon heating; i) heating the solution to distill off water and other light components and concentrating a bottoms fraction comprising hydroxyacetaldehyde and other non-volatile components having high boiling points; and j) decolorizing the stabilized brown solution with activated carbon to obtain a colorless solution.

  2. Milagro Observations of TeV Emission from Galactic Sources in the Fermi Bright Source List

    E-Print Network [OSTI]

    Abdo, A A; Aune, T; Berley, D; Chen, C; Christopher, G E; DeYoung, T; Dingus, B L; Ellsworth, R W; González, M M; Goodman, J A; Hays, E; Hoffman, C M; Huentemeyer, P H; Kolterman, B E; Linnemann, J T; McEnery, J E; Morgan, T; Mincer, A I; Némethy, P; Pretz, J; Ryan, J M; Parkinson, P M Saz; Shoup, A; Sinnis, G; Smith, A J; Vasileiou, V; Walker, G P; Williams, D A; Yodh, G B

    2009-01-01

    We present the result of a search of Milagro sky map for spatial correlations with sources from a subset of the recent Fermi Bright Source List (BSL). The BSL consists of the 205 most significant sources detected above 100 MeV by the Fermi Large Area Telescope. We select sources based on their categorization in the BSL, taking all confirmed or possible Galactic sources in the field of view of Milagro. Of the 34 Fermi sources selected, 14 are observed by Milagro at a significance of 3 standard deviations or more. We conduct this search with a new analysis which employs newly-optimized gamma-hadron separation and utilizes the full 8-year Milagro dataset. Milagro is sensitive to gamma rays above 1 TeV and these results extend the observation of these sources far above the Fermi energy band. With the new analysis and additional data, TeV emission is definitively observed associated with the Fermi pulsar J2229.0+6114, in the the Boomerang Pulsar Wind Nebula (PWN). Furthermore, an extended region of TeV emission is...

  3. Low emittance pion beams generation from bright photons and relativistic protons

    E-Print Network [OSTI]

    Serafini, L; Petrillo, V

    2015-01-01

    Present availability of high brilliance photon beams as those produced by X-ray Free Electron Lasers in combination with intense TeV proton beams typical of the Large Hadron Collider makes it possible to conceive the generation of pion beams via photo-production in a highly relativistic Lorentz boosted frame: the main advantage is the low emittance attainable and a TeV-class energy for the generated pions, that may be an interesting option for the production of low emittance muon and neutrino beams. We will describe the kinematics of the two classes of dominant events, i.e. the pion photo-production and the electron/positron pair production, neglecting other small cross-section possible events like Compton and muon pair production. Based on the phase space distributions of the pion and muon beams we will analyze the pion beam brightness achievable in three examples, based on advanced high efficiency high repetition rate FELs coupled to LHC or Future Circular Collider (FCC) proton beams, together with the stud...

  4. The Outer Disks of Early-Type Galaxies. I. Surface-Brightness Profiles of Barred Galaxies

    E-Print Network [OSTI]

    Erwin, Peter; Beckman, John E

    2007-01-01

    We present a study of 66 barred, early-type (S0-Sb) disk galaxies, focused on the disk surface brightness profile outside the bar region and the nature of Freeman Type I and II profiles, their origins, and their possible relation to disk truncations. This paper discusses the data and their reduction, outlines our classification system, and presents $R$-band profiles and classifications for all galaxies in the sample. The profiles are derived from a variety of different sources, including the Sloan Digital Sky Survey (Data Release 5). For about half of the galaxies, we have profiles derived from more than one telescope; this allows us to check the stability and repeatability of our profile extraction and classification. The vast majority of the profiles are reliable down to levels of mu_R ~ 27 mag arcsec^-2; in exceptional cases, we can trace profiles down to mu_R > 28. We can typically follow disk profiles out to at least 1.5 times the traditional optical radius R_25; for some galaxies, we find light extendin...

  5. Bright Lyman Break Galaxies in the Sloan Digital Sky Survey First Data Release

    E-Print Network [OSTI]

    Bentz, M C; Weinberg, D H; Bentz, Misty C.; Osmer, Patrick S.; Weinberg, David H.

    2003-01-01

    We report the discovery of six compact, starburst galaxies with redshifts 2.3 < z < 2.8 and r-band magnitudes 19.8-20.5 in the Quasar Catalog of the Sloan Digital Sky Survey First Data Release (SDSS DR1). The SDSS spectra of these objects resemble the composite spectrum of Lyman Break Galaxies (LBGs) at z \\approx 3, but the galaxies are 4-5 magnitudes brighter than an ``L*'' LBG and 2-3 magnitudes brighter than the most luminous objects in typical LBG spectroscopic surveys. Star formation rates inferred from the UV continuum luminosities are about 300-1000 M_sun yr^-1 with no correction for dust extinction. Such rates are similar to those inferred for ultraluminous infrared galaxies, but in these UV-bright objects the star formation is evidently not obscured by high dust column densities. The SDSS images show no evidence of multiple imaging or foreground lensing structures, but amplification by gravitational lensing (as in the case of MS 1512-cB58) cannot be ruled out with the present data. Assuming tha...

  6. Transitions from order to disorder in multiple dark and multiple dark-bright soliton atomic clouds

    DOE Public Access Gateway for Energy & Science Beta (PAGES Beta)

    Wang, Wenlong; Kevrekidis, P. G.

    2015-03-09

    We have performed a systematic study quantifying the variation of solitary wave behavior from that of an ordered cloud resembling a “crystalline” configuration to that of a disordered state that can be characterized as a soliton “gas.” As our illustrative examples, we use both one-component, as well as two-component, one-dimensional atomic gases very close to zero temperature, where in the presence of repulsive interatomic interactions and of a parabolic trap, a cloud of dark (dark-bright) solitons can form in the one- (two-) component system. We corroborate our findings through three distinct types of approaches, namely a Gross-Pitaevskii type of partialmore »differential equation, particle-based ordinary differential equations describing the soliton dynamical system, and Monte Carlo simulations for the particle system. In addition, we define an “empirical” order parameter to characterize the order of the soliton lattices and study how this changes as a function of the strength of the “thermally” (i.e., kinetically) induced perturbations. As may be anticipated by the one-dimensional nature of our system, the transition from order to disorder is gradual without, apparently, a genuine phase transition ensuing in the intermediate regime.« less

  7. BRIGHT HOT IMPACTS BY ERUPTED FRAGMENTS FALLING BACK ON THE SUN: UV REDSHIFTS IN STELLAR ACCRETION

    SciTech Connect (OSTI)

    Reale, F.; Orlando, S.; Testa, P.; Landi, E.; Schrijver, C. J.

    2014-12-10

    A solar eruption after a flare on 2011 June 7 produced EUV-bright impacts of fallbacks far from the eruption site, observed with the Solar Dynamics Observatory. These impacts can be taken as a template for the impact of stellar accretion flows. Broad redshifted UV lines have been commonly observed in young accreting stars. Here we study the emission from the impacts in the Atmospheric Imaging Assembly's UV channels and compare the inferred velocity distribution to stellar observations. We model the impacts with two-dimensional hydrodynamic simulations. We find that the localized UV 1600 Å emission and its timing with respect to the EUV emission can be explained by the impact of a cloud of fragments. The first impacts produce strong initial upflows. The following fragments are hit and shocked by these upflows. The UV emission comes mostly from the shocked front shell of the fragments while they are still falling, and is therefore redshifted when observed from above. The EUV emission instead continues from the hot surface layer that is fed by the impacts. Fragmented accretion can therefore explain broad redshifted UV lines (e.g., C IV 1550 Å) to speeds around 400 km s{sup –1} observed in accreting young stellar objects.

  8. Probing the Cosmic Star Formation History by Brightness Distribution of Gamma-Ray Bursts

    E-Print Network [OSTI]

    Tomonori Totani

    1998-08-20

    Brightness distribution of Gamma-Ray Bursts (GRBs) is studied in detail under the assumption that GRB rate is related to cosmic star formation rate. The two populations of the long- and short-duration bursts in the 4B BATSE catalog are analyzed separately. Taking account of current uncertainties in the observational estimate of star formation rate (SFR), we have tried various models of the cosmic star formation history and we find that the SFR evolution in $z$ = 0--1 is strongly constrained by the GRB distribution if the standard candle approximation is valid. The strong SFR evolution by a factor of $\\sim$ 15 from $z$ = 0 to 1 inferred from UV observations is too steep to be consistent with the GRB distribution for any distance scale of GRBs. Some possibilities to reconcile this discrepancy are discussed, including the intrinsic luminosity dispersion of GRBs and/or modification of star formation history estimated by UV observations. We argue that SFR increase factor from $z$ = 0 to 1 may be as low as about 4 if we choose different sets of cosmological parameters and/or take account of the evolution of metallicity and dust extinction in the UV data, and this would significantly remedy the discrepancy.

  9. Investigation of intergranular bright points from the New Vacuum Solar Telescope

    E-Print Network [OSTI]

    Ji, Kai-Fan; Xiang, Yong-yuan; Feng, Song; Deng, Hui; Wang, Feng; Yang, Yun-Fei

    2015-01-01

    Six high-resolution TiO-band image sequences from the New Vacuum Solar Telescope (NVST) are used to investigate the properties of intergranular bright points (igBPs). We detect the igBPs using a Laplacian and morphological dilation algorithm (LMD) and track them using a three-dimensional segmentation algorithm automatically, and then investigate the morphologic, photometric and dynamic properties of igBPs, in terms of equivalent diameter, the intensity contrast, lifetime, horizontal velocity, diffusion index, motion range and motion type. The statistical results confirm the previous studies based on G-band or TiO-band igBPs from the other telescopes. It illustrates that the TiO data from the NVST have a stable and reliable quality, which are suitable for studying the igBPs. In addition, our method is feasible to detect and track the igBPs in the TiO data from the NVST. With the aid of the vector magnetograms obtained from the Solar Dynamics Observatory /Helioseismic and Magnetic Imager, the properties of igBP...

  10. Untangling the contributions of image charge and laser profile for optimal photoemission of high-brightness electron beams

    SciTech Connect (OSTI)

    Portman, J.; Zhang, H.; Makino, K.; Ruan, C. Y.; Berz, M.; Duxbury, P. M.

    2014-11-07

    Using our model for the simulation of photoemission of high brightness electron beams, we investigate the virtual cathode physics and the limits to spatio-temporal and spectroscopic resolution originating from the image charge on the surface and from the profile of the exciting laser pulse. By contrasting the effect of varying surface properties (leading to expanding or pinned image charge), laser profiles (Gaussian, uniform, and elliptical), and aspect ratios (pancake- and cigar-like) under different extraction field strengths and numbers of generated electrons, we quantify the effect of these experimental parameters on macroscopic pulse properties such as emittance, brightness (4D and 6D), coherence length, and energy spread. Based on our results, we outline optimal conditions of pulse generation for ultrafast electron microscope systems that take into account constraints on the number of generated electrons and on the required time resolution.

  11. Ultra-bright, ultra-broadband hard x-ray driven by laser-produced energetic electron beams

    SciTech Connect (OSTI)

    Shi, Yin; Shen, Baifei; Zhang, Xiaomei; Wang, Wenpeng; Ji, Liangliang; Zhang, Lingang; Xu, Jiancai; Yu, Yahong; Zhao, Xueyan; Wang, Xiaofeng; Yi, Longqing; Xu, Tongjun; Xu, Zhizhan [State Key Laboratory of High Field Laser Physics, Shanghai Institute of Optics and Fine Mechanics, Chinese Academy of Sciences, P.O. Box 800-211, Shanghai 201800 (China)] [State Key Laboratory of High Field Laser Physics, Shanghai Institute of Optics and Fine Mechanics, Chinese Academy of Sciences, P.O. Box 800-211, Shanghai 201800 (China)

    2013-09-15

    We propose a new method of obtaining a compact ultra-bright, ultra-broadband hard X-ray source. This X-ray source has a high peak brightness in the order of 10{sup 22} photons/(s mm{sup 2} mrad{sup 2} 0.1\\%BW), an ultrashort duration (10 fs), and a broadband spectrum (flat distribution from 0.1 MeV to 4 MeV), and thus has wide-ranging potential applications, such as in ultrafast Laue diffraction experiments. In our scheme, laser-plasma accelerators (LPAs) provide driven electron beams. A foil target is placed oblique to the beam direction so that the target normal sheath field (TNSF) is used to provide a bending force. Using this TNSF-kick scheme, we can fully utilize the advantages of current LPAs, including their high charge, high energy, and low emittance.

  12. Contributions of artificial lighting sources on light pollution in Hong Kong measured through a night sky brightness monitoring network

    E-Print Network [OSTI]

    Pun, Chun Shing Jason; Leung, Wai Yan; Wong, Chung Fai

    2014-01-01

    Light pollution is a form of environmental degradation in which excessive artificial outdoor lighting, such as street lamps, neon signs, and illuminated signboards, affects the natural environment and the ecosystem. Poorly designed outdoor lighting not only wastes energy, money, and valuable Earth resources, but also robs us of our beautiful night sky. Effects of light pollution on the night sky can be evaluated by the skyglow caused by these artificial lighting sources, through measurements of the night sky brightness (NSB). The Hong Kong Night Sky Brightness Monitoring Network (NSN) was established to monitor in detail the conditions of light pollution in Hong Kong. Monitoring stations were set up throughout the city covering a wide range of urban and rural settings to continuously measure the variations of the NSB. Over 4.6 million night sky measurements were collected from 18 distinct locations between May 2010 and March 2013. This huge dataset, over two thousand times larger than our previous survey, for...

  13. High Spatial Resolution KAO Far-Infrared Observations of the Central Regions of Infrared-Bright Galaxies

    E-Print Network [OSTI]

    Beverly J. Smith; P. M. Harvey

    1996-05-06

    We present new high spatial resolution Kuiper Airborne Observatory 50 micron and/or 100 micron data for 11 infrared-bright galaxies. We also tabulate previously published KAO data for 11 other galaxies, along with the IRAS data for the bulges of M 31 and M 81. We find that L(FIR)/L(B) and L(FIR)/L(H) correlate with CO (1 - 0) intensity and tau(100). Galaxies with optical or near-infrared signatures of OB stars in their central regions have higher values of I(CO) and tau(100), as well as higher far-infrared surface brightnesses and L(FIR)/L(B) and L(FIR)/L(H) ratios. L(FIR)/L(H(alpha)) does not correlate strongly with CO and tau(100). These results support a scenario in which OB stars dominate dust heating in the more active galaxies and older stars are important in quiescent bulges.

  14. The stellar content of the XMM-Newton Bright Serendipitous Survey

    E-Print Network [OSTI]

    J. Lopez-Santiago; G. Micela; S. Sciortino; F. Favata; A. Caccianiga; R. Della Ceca; P. Severgnini; V. Braito

    2006-10-12

    Context: The comparison of observed counts in a given sky direction with predictions by Galactic models yields constraints to the spatial distribution and the stellar birthrate of young stellar populations. In this work we present the results of the analysis of the stellar content of the XMM-Newton Bright Serendipitous Survey (XBSS). This unbiased survey includes a total of 58 stellar sources selected in the 0.5 -- 4.5 keV energy band, having a limiting sensitivity of $10^{-2}$ cnt s$^{-1}$ and covering an area of 28.10 sq. deg. Aims: Our main goal is to understand the recent star formation history of the Galaxy in the vicinity of the Sun. Methods: We compare the observations with the predictions obtained with XCOUNT, a model of the stellar X-ray content of the Galaxy. The model predicts the number and properties of the stars to be observed in terms of magnitude, colour, population and $f_\\mathrm{x}/f_\\mathrm{v}$ ratio distributions of the coronal sources detected with a given instrument and sensitivity in a specific sky direction. Results: As in other shallow surveys, we observe an excess of stars not predicted by our Galaxy model. Comparing the colours of the identified infrared counterparts with the model predictions, we observe that this excess is produced by yellow (G+K) stars. The study of the X-ray spectrum of each source reveals a main population of stars with coronal temperature stratification typical of intermediate-age stars. As no assumptions have been made for the selection of the sample, our results must be representative of the entire Solar Neighbourhood. Some stars show excess circumstellar absorption indicative of youth.

  15. Reconciliation of the Surface Brightness Fluctuations and Type Ia Supernovae Distance Scales

    E-Print Network [OSTI]

    Edward A. Ajhar; John L. Tonry; John P. Blakeslee; Adam G. Riess; Brian P. Schmidt

    2001-05-21

    We present Hubble Space Telescope measurements of surface brightness fluctuations (SBF) distances to early-type galaxies that have hosted Type Ia supernovae (SNIa). The agreement in the relative SBF and SNIa multicolor light curve shape and delta-m_15 distances is excellent. There is no systematic scale error with distance, and previous work has shown that SBF and SNIa give consistent ties to the Hubble flow. However, we confirm a systematic offset of about 0.25 mag in the distance zero points of the two methods, and we trace this offset to their respective Cepheid calibrations. SBF has in the past been calibrated with Cepheid distances from the H_0 Key Project team, while SNIa have been calibrated with Cepheid distances from the team composed of Sandage, Saha, and collaborators. When the two methods are calibrated in a consistent way, their distances are in superb agreement. Until the conflict over the ``long'' and ``short'' extragalactic Cepheid distances among many galaxies is resolved, we cannot definitively constrain the Hubble constant to better than about 10%, even leaving aside the additional uncertainty in the distance to the Large Magellanic Cloud, common to both Cepheid scales. However, recent theoretical SBF predictions from stellar population models favor the Key Project Cepheid scale, while the theoretical SNIa calibration lies between the long and short scales. In addition, while the current SBF distance to M31/M32 is in good agreement with the RR Lyrae and red giant branch distances, calibrating SBF with the longer Cepheid scale would introduce a 0.3 mag offset with respect to the RR Lyrae scale.

  16. GRB 061121: Broadband spectral evolution through the prompt and afterglow phases of a bright burst

    E-Print Network [OSTI]

    K. L. Page; R. Willingale; J. P. Osborne; B. Zhang; O. Godet; F. E. Marshall; A. Melandri; J. P. Norris; P. T. O'Brien; V. Pal'shin; E. Rol; P. Romano; R. L. C. Starling; P. Schady; S. A. Yost; S. D. Barthelmy; A. P. Beardmore; G. Cusumano; D. N. Burrows; M. De Pasquale; M. Ehle; P. A. Evans; N. Gehrels; M. R. Goad; S. Golenetskii; C. Guidorzi; C. Mundell; M. J. Page; G. Ricker; T. Sakamoto; B. E. Schaefer; M. Stamatikos; E. Troja; }; M. Ulanov; F. Yuan; H. Ziaeepour

    2007-04-12

    Swift triggered on a precursor to the main burst of GRB 061121 (z=1.314), allowing observations to be made from the optical to gamma-ray bands. Many other telescopes, including Konus-Wind, XMM-Newton, ROTSE and the Faulkes Telescope North, also observed the burst. The gamma-ray, X-ray and UV/optical emission all showed a peak ~75s after the trigger, although the optical and X-ray afterglow components also appear early on - before, or during, the main peak. Spectral evolution was seen throughout the burst, with the prompt emission showing a clear positive correlation between brightness and hardness. The Spectral Energy Distribution (SED) of the prompt emission, stretching from 1eV up to 1MeV, is very flat, with a peak in the flux density at ~1keV. The optical-to-X-ray spectra at this time are better fitted by a broken, rather than single, power-law, similar to previous results for X-ray flares. The SED shows spectral hardening as the afterglow evolves with time. This behaviour might be a symptom of self-Comptonisation, although circumstellar densities similar to those found in the cores of molecular clouds would be required. The afterglow also decays too slowly to be accounted for by the standard models. Although the precursor and main emission show different spectral lags, both are consistent with the lag-luminosity correlation for long bursts. GRB 061121 is the instantaneously brightest long burst yet detected by Swift. Using a combination of Swift and Konus-Wind data, we estimate an isotropic energy of 2.8x10^53 erg over 1keV - 10MeV in the GRB rest frame. A probable jet break is detected at ~2x10^5s, leading to an estimate of ~10^51 erg for the beaming-corrected gamma-ray energy.

  17. The Outer Disks of Early-Type Galaxies. I. Surface-Brightness Profiles of Barred Galaxies

    E-Print Network [OSTI]

    Peter Erwin; Michael Pohlen; John E. Beckman

    2007-09-21

    We present a study of 66 barred, early-type (S0-Sb) disk galaxies, focused on the disk surface brightness profile outside the bar region and the nature of Freeman Type I and II profiles, their origins, and their possible relation to disk truncations. This paper discusses the data and their reduction, outlines our classification system, and presents $R$-band profiles and classifications for all galaxies in the sample. The profiles are derived from a variety of different sources, including the Sloan Digital Sky Survey (Data Release 5). For about half of the galaxies, we have profiles derived from more than one telescope; this allows us to check the stability and repeatability of our profile extraction and classification. The vast majority of the profiles are reliable down to levels of mu_R ~ 27 mag arcsec^-2; in exceptional cases, we can trace profiles down to mu_R > 28. We can typically follow disk profiles out to at least 1.5 times the traditional optical radius R_25; for some galaxies, we find light extending to ~ 3 R_25. We classify the profiles into three main groups: Type I (single-exponential), Type II (down-bending), and Type III (up-bending). The frequencies of these types are approximately 27%, 42%, and 24%, respectively, plus another 6% which are combinations of Types II and III. We further classify Type II profiles by where the break falls in relation to the bar length, and in terms of the postulated mechanisms for breaks at large radii ("classical trunction" of star formation versus the influence of the Outer Lindblad Resonance of the bar). We also classify the Type III profiles by the probable morphology of the outer light (disk or spheroid). Illustrations are given for all cases. (Abridged)

  18. Inter- and Intra-Observer Variability in Prostate Definition With Tissue Harmonic and Brightness Mode Imaging

    SciTech Connect (OSTI)

    Sandhu, Gurpreet Kaur, E-mail: Gurpreet.Sandhu2@albertahealthservices.ca [Department of Medical Physics, Tom Baker Cancer Centre, Calgary, Alberta (Canada); Department of Physics and Astronomy, University of Calgary, Calgary, Alberta (Canada); Dunscombe, Peter [Department of Medical Physics, Tom Baker Cancer Centre, Calgary, Alberta (Canada); Department of Physics and Astronomy, University of Calgary, Calgary, Alberta (Canada); Department of Oncology, Faculty of Medicine, University of Calgary, Calgary, Alberta (Canada); Meyer, Tyler [Department of Medical Physics, Tom Baker Cancer Centre, Calgary, Alberta (Canada); Department of Physics and Astronomy, University of Calgary, Calgary, Alberta (Canada); Pavamani, Simon [Department of Oncology, Faculty of Medicine, University of Calgary, Calgary, Alberta (Canada); Department of Radiation Oncology, Christian Medical College, Vellore (India); Khan, Rao [Department of Medical Physics, Tom Baker Cancer Centre, Calgary, Alberta (Canada); Department of Physics and Astronomy, University of Calgary, Calgary, Alberta (Canada); Department of Oncology, Faculty of Medicine, University of Calgary, Calgary, Alberta (Canada)

    2012-01-01

    Purpose: The objective of this study was to compare the relative utility of tissue harmonic (H) and brightness (B) transrectal ultrasound (TRUS) images of the prostate by studying interobserver and intraobserver variation in prostate delineation. Methods and Materials: Ten patients with early-stage disease were randomly selected. TRUS images of prostates were acquired using B and H modes. The prostates on all images were contoured by an experienced radiation oncologist (RO) and five equally trained observers. The observers were blinded to information regarding patient and imaging mode. The volumes of prostate glands and areas of midgland slices were calculated. Volumes contoured were compared among the observers and between observer group and RO. Contours on one patient were repeated five times by four observers to evaluate the intraobserver variability. Results: A one-sample Student t-test showed the volumes outlined by five observers are in agreement (p > 0.05) with the RO. Paired Student t-test showed prostate volumes (p = 0.008) and midgland areas (p = 0.006) with H mode were significantly smaller than that with B mode. Two-factor analysis of variances showed significant interobserver variability (p < 0.001) in prostate volumes and areas. Inter- and intraobserver consistency was quantified as the standard deviation of mean volumes and areas, and concordance indices. It was found that for small glands ({<=}35 cc) H mode provided greater interobserver consistency; however, for large glands ({>=}35 cc), B mode provided more consistent estimates. Conclusions: H mode provided superior inter- and intraobserver agreement in prostate volume definition for small to medium prostates. In large glands, H mode does not exhibit any additional advantage. Although harmonic imaging has not proven advantageous for all cases, its utilization seems to be judicious for small prostates.

  19. Production of high brightness H- beam by charge exchange of hydrogen atom beam in sodium jet

    SciTech Connect (OSTI)

    Davydenko, V.; Zelenski, A.; Ivanov, A.; Kolmogorov, A.

    2010-11-16

    Production of H{sup -} beam for accelerators applications by charge exchange of high brightness hydrogen neutral beam in a sodium jet cell is experimentally studied in joint BNL-BINP experiment. In the experiment, a hydrogen-neutral beam with 3-6 keV energy, equivalent current up to 5 A and 200 microsecond pulse duration is used. The atomic beam is produced by charge exchange of a proton beam in a pulsed hydrogen target. Formation of the proton beam is performed in an ion source by four-electrode multiaperture ion-optical system. To achieve small beam emittance, the apertures in the ion-optical system have small enough size, and the extraction of ions is carried out from the surface of plasma emitter with a low transverse ion temperature of {approx}0.2 eV formed as a result of plasma jet expansion from the arc plasma generator. Developed for the BNL optically pumped polarized ion source, the sodium jet target with recirculation and aperture diameter of 2 cm is used in the experiment. At the first stage of the experiment H{sup -} beam with 36 mA current, 5 keV energy and {approx}0.15 cm {center_dot} mrad normalized emittance was obtained. To increase H{sup -} beam current ballistically focused hydrogen neutral beam will be applied. The effects of H{sup -} beam space-charge and sodium-jet stability will be studied to determine the basic limitations of this approach.

  20. REX, a 5-MV pulsed-power source for driving high-brightness electron beam diodes

    SciTech Connect (OSTI)

    Carlson, R.L.; Kauppila, T.J.; Ridlon, R.N.

    1991-01-01

    The Relativistic Electron-beam Experiment, or REX accelerator, is a pulsed-power source capable of driving a 100-ohm load at 5 MV, 50 kA, 45 ns (FWHM) with less than a 10-ns rise and 15-ns fall time. This paper describes the pulsed-power modifications, modelling, and extensive measurements on REX to allow it to drive high impedance (100s of ohms) diode loads with a shaped voltage pulse. A major component of REX is the 1.83-m-diam {times} 25.4-cm-thick Lucite insulator with embedded grading rings that separates the output oil transmission line from the vacuum vessel that contains the re-entrant anode and cathode assemblies. A radially tailored, liquid-based resistor provides a stiff voltage source that is insensitive to small variations of the diode current and, in addition, optimizes the electric field stress across the vacuum side of the insulator. The high-current operation of REX employs both multichannel peaking and point-plane diverter switches. This mode reduces the prepulse to less than 2 kV and the postpulse to less than 5% of the energy delivered to the load. Pulse shaping for the present diode load is done through two L-C transmission line filters and a tapered, glycol-based line adjacent to the water PFL and output switch. This has allowed REX to drive a diode producing a 4-MV, 4.5-kA, 55-ns flat-top electron beam with a normalized Lapostolle emittance of 0.96 mm-rad corresponding to a beam brightness in excess of 4.4 {times} 10{sup 8} A/m{sup 2} {minus}rad{sup 2}. 6 refs., 13 figs.

  1. ACTIVITY-BRIGHTNESS CORRELATIONS FOR THE SUN AND SUN-LIKE STARS

    SciTech Connect (OSTI)

    Preminger, D. G.; Chapman, G. A.; Cookson, A. M.

    2011-10-01

    We analyze the effect of solar features on the variability of the solar irradiance in three different spectral ranges. Our study is based on two solar-cycles' worth of full-disk photometric images from the San Fernando Observatory, obtained with red, blue, and Ca II K-line filters. For each image we measure the photometric sum, {Sigma}, which is the relative contribution of solar features to the disk-integrated intensity of the image. The photometric sums in the red and blue continuum, {Sigma}{sub r} and {Sigma}{sub b}, exhibit similar temporal patterns: they are negatively correlated with solar activity, with strong short-term variability, and weak solar-cycle variability. However, the Ca II K-line photometric sum, {Sigma}{sub K}, is positively correlated with solar activity and has strong variations on solar-cycle timescales. We show that we can model the variability of the Sun's bolometric flux as a linear combination of {Sigma}{sub r} and {Sigma}{sub K}. We infer that, over solar-cycle timescales, the variability of the Sun's bolometric irradiance is directly correlated with spectral line variability, but inversely correlated with continuum variability. Our blue and red continuum filters are quite similar to the Stroemgren b and y filters used to measure stellar photometric variability. We conclude that active stars whose visible continuum brightness varies inversely with activity, as measured by the Ca HK index, are displaying a pattern that is similar to that of the Sun, i.e., radiative variability in the visible continuum that is spot-dominated.

  2. TURBULENT DIFFUSION IN THE PHOTOSPHERE AS DERIVED FROM PHOTOSPHERIC BRIGHT POINT MOTION

    SciTech Connect (OSTI)

    Abramenko, V. I.; Yurchyshyn, V.; Goode, P. R.; Carbone, V.; Lepreti, F.; Capparelli, V.; Vecchio, A.; Stein, R. F.

    2011-12-20

    On the basis of observations of solar granulation obtained with the New Solar Telescope of Big Bear Solar Observatory, we explored proper motion of bright points (BPs) in a quiet-sun area, a coronal hole, and an active region plage. We automatically detected and traced BPs and derived their mean-squared displacements as a function of time (starting from the appearance of each BP) for all available time intervals. In all three magnetic environments, we found the presence of a super-diffusion regime, which is the most pronounced inside the time interval of 10-300 s. Super-diffusion, measured via the spectral index, {gamma}, which is the slope of the mean-squared displacement spectrum, increases from the plage area ({gamma} = 1.48) to the quiet-sun area ({gamma} = 1.53) to the coronal hole ({gamma} = 1.67). We also found that the coefficient of turbulent diffusion changes in direct proportion to both temporal and spatial scales. For the minimum spatial scale (22 km) and minimum time scale (10 s), it is 22 and 19 km{sup 2} s{sup -1} for the coronal hole and the quiet-sun area, respectively, whereas for the plage area it is about 12 km{sup 2} s{sup -1} for the minimum time scale of 15 s. We applied our BP tracking code to three-dimensional MHD model data of solar convection and found the super-diffusion with {gamma} = 1.45. An expression for the turbulent diffusion coefficient as a function of scales and {gamma} is obtained.

  3. Sparkling extreme-ultraviolet bright dots observed with Hi-C

    SciTech Connect (OSTI)

    Régnier, S.; Alexander, C. E.; Walsh, R. W.; Winebarger, A. R.; Cirtain, J.; Golub, L.; Korreck, K. E.; Weber, M.; Mitchell, N.; Platt, S.; De Pontieu, B.; Title, A.; Kobayashi, K.; Kuzin, S.; DeForest, C. E.

    2014-04-01

    Observing the Sun at high time and spatial scales is a step toward understanding the finest and fundamental scales of heating events in the solar corona. The high-resolution coronal (Hi-C) instrument has provided the highest spatial and temporal resolution images of the solar corona in the EUV wavelength range to date. Hi-C observed an active region on 2012 July 11 that exhibits several interesting features in the EUV line at 193 Å. One of them is the existence of short, small brightenings 'sparkling' at the edge of the active region; we call these EUV bright dots (EBDs). Individual EBDs have a characteristic duration of 25 s with a characteristic length of 680 km. These brightenings are not fully resolved by the SDO/AIA instrument at the same wavelength; however, they can be identified with respect to the Hi-C location of the EBDs. In addition, EBDs are seen in other chromospheric/coronal channels of SDO/AIA, which suggests a temperature between 0.5 and 1.5 MK. Based on their frequency in the Hi-C time series, we define four different categories of EBDs: single peak, double peak, long duration, and bursty. Based on a potential field extrapolation from an SDO/HMI magnetogram, the EBDs appear at the footpoints of large-scale, trans-equatorial coronal loops. The Hi-C observations provide the first evidence of small-scale EUV heating events at the base of these coronal loops, which have a free magnetic energy of the order of 10{sup 26} erg.

  4. A closer look at the fluctuations in the brightness of SN 2009IP during its late 2012 eruption

    SciTech Connect (OSTI)

    Martin, J. C. [Barber Observatory, University of Illinois Springfield, Springfield, IL 62704 (United States); Hambsch, F.-J. [Remote Observatory, Atacama Desert, Chile Vereniging Voor Sterrenkunde (VVS), Oude Bleken 12, B-2400 Mol (Belgium); Margutti, R.; Soderberg, A. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02318 (United States); Tan, T. G. [Perth Exoplanet Survey Telescope, Perth (Australia); Curtis, I., E-mail: jmart5@uis.edu [Adelaide (Australia)

    2015-01-01

    The supernova (SN) impostor SN 2009ip has re-brightened several times since its initial discovery in 2009 August. During its last outburst in late 2012 September, it reached a peak brightness of m{sub v} ?13.5 (M{sub v} brighter than ?18), causing some to speculate that it had undergone a terminal core-collapse SN. Relatively high-cadence multi-wavelength photometry of the post-peak decline revealed bumps in brightness infrequently observed in other SNe IIn. These bumps occurred synchronously in all ultraviolet (UV) and optical bands with amplitudes of 0.1–0.4 mag at intervals of 10–30 days. Episodic continuum brightening and dimming in the UV and optical with these characteristics is not easily explained within the context of models that have been proposed for the late September 2012 outburst of SN 2009ip. We also present evidence that the post-peak fluctuations in brightness occur at regular intervals and raise more questions about their origin.

  5. The Near-Infrared Photometric Properties of Bright Giants in the Central Regions of the Galactic Bulge

    E-Print Network [OSTI]

    T. J. Davidge

    1998-03-24

    Images recorded through broad (J, H, K), and narrow (CO, and 2.2micron continuum) band filters are used to investigate the photometric properties of bright (K < 13.5) stars in a 6 x 6 arcmin field centered on the SgrA complex. The giant branch ridgelines in the (K, J-K) and (K, H-K) color-magnitude diagrams are well matched by the Baade's Window (BW) M giant sequence if the mean extinction is A_K ~ 2.8 mag. Extinction measurements for individual stars are estimated using the M_K versus infrared color relations defined by M giants in BW, and the majority of stars have A_K between 2.0 and 3.5 mag. The extinction is locally high in the SgrA complex, where A_K ~ 3.1 mag. Reddening-corrected CO indices, CO_o, are derived for over 1300 stars with J, H, and K brightnesses, and over 5300 stars with H and K brightnesses. The distribution of CO_o values for stars with K_o between 11.25 and 7.25 can be reproduced using the M_K versus CO_o relation defined by M giants in BW. The data thus suggest that the most metal-rich giants in the central regions of the bulge and in BW have similar photometric properties and 2.3micron CO strengths. Hence, it appears that the central region of the bulge does not contain a population of stars that are significantly more metal-rich than what is seen in BW.

  6. BRIGHTNESS AND FLUCTUATION OF THE MID-INFRARED SKY FROM AKARI OBSERVATIONS TOWARD THE NORTH ECLIPTIC POLE

    SciTech Connect (OSTI)

    Pyo, Jeonghyun; Jeong, Woong-Seob [Korea Astronomy and Space Science Institute (KASI), Daejeon 305-348 (Korea, Republic of); Matsumoto, Toshio [Department of Physics and Astronomy, Seoul National University, Seoul 151-742 (Korea, Republic of); Matsuura, Shuji, E-mail: jhpyo@kasi.re.kr [Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210 (Japan)

    2012-12-01

    We present the smoothness of the mid-infrared sky from observations by the Japanese infrared astronomical satellite AKARI. AKARI monitored the north ecliptic pole (NEP) during its cold phase with nine wave bands covering from 2.4 to 24 {mu}m, out of which six mid-infrared bands were used in this study. We applied power-spectrum analysis to the images in order to search for the fluctuation of the sky brightness. Observed fluctuation is explained by fluctuation of photon noise, shot noise of faint sources, and Galactic cirrus. The fluctuations at a few arcminutes scales at short mid-infrared wavelengths (7, 9, and 11 {mu}m) are largely caused by the diffuse Galactic light of the interstellar dust cirrus. At long mid-infrared wavelengths (15, 18, and 24 {mu}m), photon noise is the dominant source of fluctuation over the scale from arcseconds to a few arcminutes. The residual fluctuation amplitude at 200'' after removing these contributions is at most 1.04 {+-} 0.23 nW m{sup -2} sr{sup -1} or 0.05% of the brightness at 24 {mu}m and at least 0.47 {+-} 0.14 nW m{sup -2} sr{sup -1} or 0.02% at 18 {mu}m. We conclude that the upper limit of the fluctuation in the zodiacal light toward the NEP is 0.03% of the sky brightness, taking 2{sigma} error into account.

  7. The effect of the fifth-order nonlinearity on the existence of bright solitons below the modulation instability threshold

    E-Print Network [OSTI]

    Gandzha, I S

    2015-01-01

    We analyze three different high-order nonlinear Schr\\"{o}dinger equation (HONLSE) models that have been used in the literature to describe the evolution of slowly modulated gravity waves on the surface of ideal finite-depth fluid. We demonstrate that the inclusion of the fifth-order nonlinear term to the HONLSE model introduces only a small correction to the amplitude of the bright HONLSE soliton solutions obtained without this term. Such soliton slutions behave as quasi-solitons in this more general case.

  8. Broadband Spectral Properties of Bright High-Energy Gamma-Ray Bursts Observed with BATSE and EGRET

    E-Print Network [OSTI]

    Kaneko, Y; Preece, R; Dingus, B L; Briggs, M S

    2008-01-01

    We present the spectral analysis of duration-integrated broadband spectra (in $\\sim30 $keV$-200 $MeV) of 15 bright BATSE gamma-ray bursts (GRBs). Some GRB spectra are very hard, with their spectral peak energies being above the BATSE LAD passband limit of $\\sim$2 MeV. In such cases, their high-energy spectral parameters (peak energy and high-energy power-law indices) cannot be adequately constrained by BATSE LAD data alone. A few dozen bright BATSE GRBs were also observed with EGRET's calorimeter, TASC, in multi-MeV energy band, with a large effective area and fine energy resolution. Combining the BATSE and TASC data, therefore, affords spectra that span four decades of energy ($30 $keV$-200 $MeV), allowing for a broadband spectral analysis with good statistics. Studying such broadband high-energy spectra of GRB prompt emission is crucial, as they provide key clues to understanding its gamma-ray emission mechanism. Among the 15 GRB spectra, we found two cases with a significant high-energy excess, and another...

  9. A COMPLETE SAMPLE OF BRIGHT SWIFT LONG GAMMA-RAY BURSTS. I. SAMPLE PRESENTATION, LUMINOSITY FUNCTION AND EVOLUTION

    SciTech Connect (OSTI)

    Salvaterra, R. [INAF, IASF Milano, via E. Bassini 15, I-20133 Milano (Italy); Campana, S.; Vergani, S. D.; Covino, S.; D'Avanzo, P.; Fugazza, D.; Ghirlanda, G.; Ghisellini, G.; Melandri, A.; Sbarufatti, B.; Tagliaferri, G. [INAF, Osservatorio Astronomico di Brera, via E. Bianchi 46, I-23807 Merate (Saint Lucia) (Italy); Nava, L. [SISSA, via Bonomea 265, I-34136 Trieste (Italy); Flores, H. [Laboratoire GEPI, Observatoire de Paris, CNRS-UMR8111, Univ. Paris-Diderot 5 place Jules Janssen, 92195 Meudon (France); Piranomonte, S., E-mail: ruben@lambrate.inaf.it [INAF, Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monte Porzio Catone, Rome (Italy)

    2012-04-10

    We present a carefully selected sub-sample of Swift long gamma-ray bursts (GRBs) that is complete in redshift. The sample is constructed by considering only bursts with favorable observing conditions for ground-based follow-up searches, which are bright in the 15-150 keV Swift/BAT band, i.e., with 1-s peak photon fluxes in excess to 2.6 photons s{sup -1} cm{sup -2}. The sample is composed of 58 bursts, 52 of them with redshift for a completeness level of 90%, while another two have a redshift constraint, reaching a completeness level of 95%. For only three bursts we have no constraint on the redshift. The high level of redshift completeness allows us for the first time to constrain the GRB luminosity function and its evolution with cosmic times in an unbiased way. We find that strong evolution in luminosity ({delta}{sub l} = 2.3 {+-} 0.6) or in density ({delta}{sub d} = 1.7 {+-} 0.5) is required in order to account for the observations. The derived redshift distributions in the two scenarios are consistent with each other, in spite of their different intrinsic redshift distributions. This calls for other indicators to distinguish among different evolution models. Complete samples are at the base of any population studies. In future works we will use this unique sample of Swift bright GRBs to study the properties of the population of long GRBs.

  10. KELT-7b: A hot Jupiter transiting a bright V=8.54 rapidly rotating F-star

    E-Print Network [OSTI]

    Bieryla, Allyson; Beatty, Thomas G; Eastman, Jason; Siverd, Robert J; Pepper, Joshua; Gaudi, B Scott; Stassun, Keivan G; Canas, Caleb; Latham, David W; Buchhave, Lars A; Sanchis-Ojeda, Roberto; Winn, Joshua N; Jensen, Eric L N; Kielkopf, John F; McLeod, Kim K; Gregorio, Joao; Colon, Knicole D; Street, Rachel; Ross, Rachel; Penny, Matthew; Mellon, Samuel N; Oberst, Thomas E; Fulton, Benjamin J; Wang, Ji; Berlind, Perry; Calkins, Michael L; Esquerdo, Gilbert A; DePoy, Darren L; Gould, Andrew; Marshall, Jennifer; Pogge, Richard; Trueblood, Mark; Trueblood, Patricia

    2015-01-01

    We report the discovery of KELT-7b, a transiting hot Jupiter with a mass of $1.28 \\pm 0.18$ MJ, radius of $1.53_{-0.047}^{+0.046}$ RJ, and an orbital period of $2.7347749 \\pm 0.0000039$ days. The bright host star (HD33643; KELT-7) is an F-star with $V=8.54$, Teff $=6789_{-49}^{+50}$ K, [Fe/H] $=0.139_{-0.081}^{+0.075}$, and $\\log{g}=4.149 \\pm 0.019$. It has a mass of $1.535_{-0.054}^{+0.066}$ Msun, a radius of $1.732_{-0.045}^{+0.043}$ Rsun, and is the fifth most massive, fifth hottest, and the ninth brightest star known to host a transiting planet. It is also the brightest star around which KELT has discovered a transiting planet. Thus, KELT-7b is an ideal target for detailed characterization given its relatively low surface gravity, high equilibrium temperature, and bright host star. The rapid rotation of the star ($73 \\pm 0.5$ km/s) results in a Rossiter-McLaughlin effect with an unusually large amplitude of several hundred m/s. We find that the orbit normal of the planet is likely to be well-aligned with ...

  11. A correlation between intrinsic brightness and average decay rate of Swift UVOT GRB optical/UV light curves

    E-Print Network [OSTI]

    Oates, S R; De Pasquale, M; Schady, P; Breeveld, A A; Holland, S T; Kuin, N P M; Marshall, F E

    2012-01-01

    We examine a sample of 48 Swift/UVOT long Gamma-ray Burst light curves and find a correlation between the logarithmic luminosity at 200s and average decay rate determined from 200s onwards, with a Spearman rank coefficient of -0.58 at a significance of 99.998% (4.2 sigma). We discuss the causes of the log L_200s - alpha_>200s correlation, finding it to be an intrinsic property of long GRBs, and not resulting from the selection criteria. We find two ways to produce the correlation. One possibility is that there is some property of the central engine, outflow or external medium that affects the rate of energy release so that the bright afterglows release their energy more quickly and decay faster than the fainter afterglows. Alternatively, the correlation may be produced by variation of the observers viewing angle, with observers at large viewing angles observing fainter and slower decaying light curves.

  12. Broadband Spectral Properties of Bright High-Energy Gamma-Ray Bursts Observed with BATSE and EGRET

    E-Print Network [OSTI]

    Y. Kaneko; M. M. Gonzalez; R. Preece; B. L. Dingus; M. S. Briggs

    2008-01-12

    We present the spectral analysis of duration-integrated broadband spectra (in $\\sim30 $keV$-200 $MeV) of 15 bright BATSE gamma-ray bursts (GRBs). Some GRB spectra are very hard, with their spectral peak energies being above the BATSE LAD passband limit of $\\sim$2 MeV. In such cases, their high-energy spectral parameters (peak energy and high-energy power-law indices) cannot be adequately constrained by BATSE LAD data alone. A few dozen bright BATSE GRBs were also observed with EGRET's calorimeter, TASC, in multi-MeV energy band, with a large effective area and fine energy resolution. Combining the BATSE and TASC data, therefore, affords spectra that span four decades of energy ($30 $keV$-200 $MeV), allowing for a broadband spectral analysis with good statistics. Studying such broadband high-energy spectra of GRB prompt emission is crucial, as they provide key clues to understanding its gamma-ray emission mechanism. Among the 15 GRB spectra, we found two cases with a significant high-energy excess, and another case with a extremely high peak energy (\\epeak $\\gtrsim$ 170 MeV). There have been very limited number of GRBs observed at MeV energies and above, and only a few instruments have been capable of observing GRBs in this energy band with such high sensitivity. Thus, our analysis results presented here should also help predict GRB observations with current and future high-energy instruments such as AGILE and GLAST, as well as with ground-based very-high-energy telescopes.

  13. GRB 090926A AND BRIGHT LATE-TIME FERMI LARGE AREA TELESCOPE GAMMA-RAY BURST AFTERGLOWS

    SciTech Connect (OSTI)

    Swenson, C. A.; Roming, P. W. A.; Vetere, L.; Kennea, J. A. [Pennsylvania State University, 525 Davey Lab, University Park, PA 16802 (United States); Maxham, A.; Zhang, B. B.; Zhang, B. [University of Nevada, Las Vegas, Box 454002, 4505 Maryland Parkway, Las Vegas, NV 89154 (United States); Schady, P. [Max-Planck-Institut fuer extraterrestrische Physik, Garching (Germany); Holland, S. T. [Universities Space Research Association, 10227 Wincopin Circle, Suite 500, Columbia, MD 21044 (United States); Kuin, N. P. M.; Oates, S. R.; De Pasquale, M. [The UCL Mullard Space Science Laboratory, Holmbury St Mary, Surrey, RH5 6NT (United Kingdom); Page, K. L., E-mail: cswenson@astro.psu.ed [Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH (United Kingdom)

    2010-07-20

    GRB 090926A was detected by both the Gamma-ray Burst Monitor and Large Area Telescope (LAT) instruments on board the Fermi Gamma-ray Space Telescope. Swift follow-up observations began {approx}13 hr after the initial trigger. The optical afterglow was detected for nearly 23 days post trigger, placing it in the long-lived category. The afterglow is of particular interest due to its brightness at late times, as well as the presence of optical flares at T0+10{sup 5} s and later, which may indicate late-time central engine activity. The LAT has detected a total of 16 gamma-ray bursts; nine of these bursts, including GRB 090926A, also have been observed by Swift. Of the nine Swift-observed LAT bursts, six were detected by UVOT, with five of the bursts having bright, long-lived optical afterglows. In comparison, Swift has been operating for five years and has detected nearly 500 bursts, but has only seen {approx}30% of bursts with optical afterglows that live longer than 10{sup 5} s. We have calculated the predicted gamma-ray fluence, as would have been seen by the Burst Alert Telescope (BAT) on board Swift, of the LAT bursts to determine whether this high percentage of long-lived optical afterglows is unique, when compared to BAT-triggered bursts. We find that, with the exception of the short burst GRB 090510A, the predicted BAT fluences indicate that the LAT bursts are more energetic than 88% of all Swift bursts and also have brighter than average X-ray and optical afterglows.

  14. AS102 -Day Laboratory Exercise #2: Luminosity and Brightness _ Page 1 Introduction -How do we determine the value of the Sun's luminosity or the luminosity of other

    E-Print Network [OSTI]

    Opher, Merav

    : light bulbs, meter sticks, calculators, wax blocks, aluminum foil Methods: · Mask light from a bulb consists of two wax blocks and a piece of aluminum foil located between the wax blocks. When viewed from the edge, this photometer will allow you to judge when the two wax blocks are equally bright. Then, if we

  15. Bright six-partite continuous variable entanglement using cascaded four-wave mixing processes in a four-level atomic system

    E-Print Network [OSTI]

    Guangqiang He; Xufei Wu; Yi Gu

    2011-09-10

    We theoretically show that bright six-partite continuous-variable entanglement can be generated using cascaded four-wave mixing effects of third-order nonlinearity atomic systems above threshold. The six-partite continuous-variable entanglement among the six cavity fields with different frequencies is analyzed by applying optimized inseparability criteria proposed by Van Loock and Furusawa.

  16. European Particle Accelerator Conference -Rome, Italy -June 7-12, 1988 DEVELOPMENT OFA HIGH BRIGHTNESS ELECTRON GUN FOR THE ACCELERATOR TEST FACILITY AT

    E-Print Network [OSTI]

    McDonald, Kirk

    BRIGHTNESS ELECTRON GUN FOR THE ACCELERATOR TEST FACILITY AT BROOKHAVEN NATIONAL LABORATORY* K. Batchelor, HDonald Princeton University At innBNL--41767 DE89 002179 Abstract An electron gun utilizing aradio frequency on the design of (he electron gun which will provide r.f. bunches of upto 101 electrons synchronized

  17. Fifteen years of XMM-Newton and Chandra monitoring of Sgr A*: Evidence for a recent increase in the bright flaring rate

    E-Print Network [OSTI]

    Ponti, G; Morris, M R; Merloni, A; Munoz-Darias, T; Clavel, M; Haggard, D; Zhang, S; Nandra, K; Gillessen, S; Mori, K; Neilsen, J; Rea, N; Degenaar, N; Terrier, R; Goldwurm, A

    2015-01-01

    We present a study of the X-ray flaring activity of Sgr A* during all the 150 XMM-Newton and Chandra observations pointed at the Milky Way center over the last 15 years. This includes the latest XMM-Newton and Chandra campaigns devoted to monitoring the closest approach of the very red Br-Gamma emitting object called G2. The entire dataset analysed extends from September 1999 through November 2014. We employed a Bayesian block analysis to investigate any possible variations in the characteristics (frequency, energetics, peak intensity, duration) of the flaring events that Sgr A* has exhibited since their discovery in 2001. We observe that the total bright-or-very bright flare luminosity of Sgr A* increased between 2013-2014 by a factor of 2-3 (~3.5 sigma significance). We also observe an increase (~99.9% significance) from 0.27+-0.04 to 2.5+-1.0 day^-1 of the bright-or-very bright flaring rate of Sgr A*, starting in late summer 2014, which happens to be about six months after G2's peri-center passage. This mi...

  18. Spectrally bright and broad fiber-based heralded single-photon source E. A. Goldschmidt, M. D. Eisaman, J. Fan,* S. V. Polyakov, and A. Migdall

    E-Print Network [OSTI]

    Migdall, Alan

    , such a spectrally bright and broad fiber-based heralded single-photon source is suitable for a variety of quantum-information into two categories: on-demand sources whose operation is ideally deterministic, and heralded sources-based heralded single-photon sources is suitable for future quantum-information applications. In the experiment

  19. THE BRIGHT GAMMA-RAY BURST OF 2000 FEBRUARY 10: A CASE STUDY OF AN OPTICALLY DARK GAMMA-RAY BURST

    E-Print Network [OSTI]

    Fynbo, Johan

    THE BRIGHT GAMMA-RAY BURST OF 2000 FEBRUARY 10: A CASE STUDY OF AN OPTICALLY DARK GAMMA-RAY BURST L Received 2002 January 16; accepted 2002 June 8 ABSTRACT The gamma-ray burst GRB 000210 had the highest: observations -- gamma-rays: bursts 1. INTRODUCTION It is observationally well established that about half

  20. Bright and dark singlet excitons via linear and two-photon spectroscopy in monolayer transition metal dichalcogenides

    DOE Public Access Gateway for Energy & Science Beta (PAGES Beta)

    Berkelbach, Timothy C.; Hybertsen, Mark S.; Reichmann, David R.

    2015-08-10

    We discuss the linear and two-photon spectroscopic selection rules for spin-singlet excitons in monolayer transition-metal dichalcogenides. Our microscopic formalism combines a fully k-dependent few-orbital band structure with a many-body Bethe-Salpeter equation treatment of the electron-hole interaction, using a model dielectric function. We show analytically and numerically that the single-particle, valley-dependent selection rules are preserved in the presence of excitonic effects. Furthermore, we definitively demonstrate that the bright (one-photon allowed) excitons have s-type azimuthal symmetry and that dark p-type excitons can be probed via two-photon spectroscopy. Thus, the screened Coulomb interaction in these materials substantially deviates from the 1/??r form; thismore »breaks the “accidental” angular momentum degeneracy in the exciton spectrum, such that the 2p exciton has a lower energy than the 2s exciton by at least 50 meV. We compare our calculated two-photon absorption spectra to recent experimental measurements.« less

  1. Impulsive and Long Duration High-Energy Gamma-ray Emission From the Very Bright 2012 March 7 Solar Flares

    E-Print Network [OSTI]

    ,

    2013-01-01

    The Fermi Large Area Telescope (LAT) observed two bright X-class solar flares on 2012 March 7, and detected gamma-rays up to 4 GeV. We detected gamma-rays both during the impulsive and temporally-extended emission phases, with emission above 100 MeV lasting for approximately 20 hours. Accurate localization of the gamma-ray production site(s) coincide with the solar active region from which X-ray emissions associated with these flares originated. Our analysis of the >100 MeV gamma-ray emission shows a relatively rapid monotonic decrease in flux during the first hour of the impulsive phase, and a much slower, almost monotonic decrease in flux for the next 20 hours. The spectra can be adequately described by a power law with a high energy exponential cutoff, or as resulting from the decay of neutral pions produced by accelerated protons and ions with an isotropic power-law energy distribution. The required proton spectrum has a number index ~3, with minor variations during the impulsive phase, while during the t...

  2. UV-Bright Stellar Populations and Their Evolutionary Implications in the Collapsed-Core Cluster M15

    E-Print Network [OSTI]

    Haurberg, Nathalie C; Cohn, Haldan N; Lugger, Phyllis M; Anderson, Jay; Cool, Adrienne M; Serenelli, Aldo; 10.1088/0004-637X/722/1/158

    2010-01-01

    We performed deep photometry of the central region of Galactic globular cluster M15 from archival Hubble Space Telescope data taken on the High Resolution Channel and Solar Blind Channel of the Advanced Camera for Surveys. Our data set consists of images in far-UV (FUV$_{140}$; F140LP), near-UV (NUV$_{220}$; F220W), and blue (B$_{435}$; F435W) filters. The addition of an optical filter complements previous UV work on M15 by providing an additional constraint on the UV-bright stellar populations. Using color-magnitude diagrams (CMDs) we identified several populations that arise from non-canonical evolution including candidate blue stragglers, extreme horizontal branch stars, blue hook stars (BHks), cataclysmic variables (CVs), and helium-core white dwarfs (He WDs). Due to preliminary identification of several He WD and BHk candidates, we add M15 as a cluster containing a He WD sequence and suggest it be included among clusters with a BHk population. We also investigated a subset of CV candidates that appear in...

  3. On the Frequency Evolution of X-ray Brightness Oscillations During Thermonuclear X-ray Bursts: Evidence for Coherent Oscillations

    E-Print Network [OSTI]

    Tod E. Strohmayer; Craig B. Markwardt

    1999-03-03

    We investigate the time dependence of the frequency of X-ray brightness oscillations during thermonuclear bursts from several neutron star low mass X-ray binaries. We find that the oscillation frequencies in the cooling tails of X-ray bursts from 4U 1702-429 and 4U 1728-34 are well described by an exponential "chirp" model. With this model we demonstrate that the pulse trains in the cooling tails of many bursts are highly phase coherent, having oscillation quality factors as high as Q ~ 4000. We use this model of the frequency evolution to search sensitively for significant power at the harmonics and first sub-harmonic of the 330 and 363 Hz signals in bursts from 4U 1702-429 and 4U 1728-34, respectively, but find not evidence for significant power at any harmonic or the sub-harmonic. We argue that the high coherence favors stellar rotation as the source of the oscillations. We briefly discuss the frequency evolution in terms of rotational motion of an angular momentum conserving thermonuclear shell. we discuss how the limits on harmonic content can be used to infer properties of the neutron star.

  4. The behaviour of dark matter associated with 4 bright cluster galaxies in the 10kpc core of Abell 3827

    E-Print Network [OSTI]

    Richard Massey; Liliya Williams; Renske Smit; Mark Swinbank; Thomas Kitching; David Harvey; Mathilde Jauzac; Holger Israel; Douglas Clowe; Alastair Edge; Matt Hilton; Eric Jullo; Adrienne Leonard; Jori Liesenborgs; Julian Merten; Irshad Mohammed; Daisuke Nagai; Johan Richard; Andrew Robertson; Prasenjit Saha; Rebecca Santana; John Stott; Eric Tittley

    2015-04-13

    Galaxy cluster Abell 3827 hosts the stellar remnants of four almost equally bright elliptical galaxies within a core of radius 10kpc. Such corrugation of the stellar distribution is very rare, and suggests recent formation by several simultaneous mergers. We map the distribution of associated dark matter, using new Hubble Space Telescope imaging and VLT/MUSE integral field spectroscopy of a gravitationally lensed system threaded through the cluster core. We find that each of the central galaxies retains a dark matter halo, but that (at least) one of these is spatially offset from its stars. The best-constrained offset is 1.62+/-0.48kpc, where the 68% confidence limit includes both statistical error and systematic biases in mass modelling. Such offsets are not seen in field galaxies, but are predicted during the long infall to a cluster, if dark matter self-interactions generate an extra drag force. With such a small physical separation, it is difficult to definitively rule out astrophysical effects operating exclusively in dense cluster core environments - but if interpreted solely as evidence for self-interacting dark matter, this offset implies a cross-section sigma/m=(1.7+/-0.7)x10^{-4}cm^2/g x (t/10^9yrs)^{-2}, where t is the infall duration.

  5. Fusion energy Fusion powers the Sun, and all stars, in which light nuclei fuse together at high temperatures

    E-Print Network [OSTI]

    would provide the UK's per capita electricity production for 30 years. · Fusion is environmentally. · The estimated cost of electricity generated by fusion is similar to the cost of electricity produced in other). ITER's expected lifetime cost is less than the amount being spent on the London Olympics. #12;

  6. High brightness microwave lamp

    DOE Patents [OSTI]

    Kirkpatrick, Douglas A.; Dolan, James T.; MacLennan, Donald A.; Turner, Brian P.; Simpson, James E.

    2003-09-09

    An electrodeless microwave discharge lamp includes a source of microwave energy, a microwave cavity, a structure configured to transmit the microwave energy from the source to the microwave cavity, a bulb disposed within the microwave cavity, the bulb including a discharge forming fill which emits light when excited by the microwave energy, and a reflector disposed within the microwave cavity, wherein the reflector defines a reflective cavity which encompasses the bulb within its volume and has an inside surface area which is sufficiently less than an inside surface area of the microwave cavity. A portion of the reflector may define a light emitting aperture which extends from a position closely spaced to the bulb to a light transmissive end of the microwave cavity. Preferably, at least a portion of the reflector is spaced from a wall of the microwave cavity. The lamp may be substantially sealed from environmental contamination. The cavity may include a dielectric material is a sufficient amount to require a reduction in the size of the cavity to support the desired resonant mode.

  7. Bright Lights, Black Leather 

    E-Print Network [OSTI]

    LaSalle, R.

    1995-01-01

    My research is a qualitative study about the Asian American experience. Studies have shown that Asian Americans obtain high levels of educational attainment and household income, but these figures are misleading. Asian ...

  8. Hubble space telescope observations of the afterglow, supernova, and host galaxy associated with the extremely bright GRB 130427A

    SciTech Connect (OSTI)

    Levan, A. J. [Department of Physics, University of Warwick, Coventry, CV4 7AL (United Kingdom); Tanvir, N. R.; Wiersema, K. [Department of Physics and Astronomy, University of Leicester, University Road, Leicester, LE1 7RH (United Kingdom); Fruchter, A. S.; Hounsell, R. A.; Graham, J. [Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States); Hjorth, J.; Fynbo, J. P. U. [Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen (Denmark); Pian, E. [INAF, Trieste Astronomical Observatory, via G.B. Tiepolo 11, I-34143 Trieste (Italy); Mazzali, P. [Astrophysics Research Institute, Liverpool John Moores University, IC2 Liverpool Science Park 146 Brownlow Hill, Liverpool L3 5RF (United Kingdom); Perley, D. A. [Department of Astronomy, California Institute of Technology, MC 249-17, 1200 East California Blvd., Pasadena, CA 91125 (United States); Cano, Z. [Centre for Astrophysics and Cosmology, Science Institute, University of Iceland, Dunhagi 5, 107 Reykjavik (Iceland); Cenko, S. B. [Astrophysics Science Division, NASA Goddard Space Flight Center, Mail Code 661, Greenbelt, MD 20771 (United States); Kouveliotou, C. [Science and Technology Office, ZP12, NASA/Marshall Space Flight Center, Huntsville, AL 35812 (United States); Pe'er, A. [Department of Physics, University College Cork, Cork (Ireland); Misra, K., E-mail: a.j.levan@warwick.ac.uk [Aryabhatta Research Institute of Observational Sciences, Manora Peak, Nainital-263 002 (India)

    2014-09-10

    We present Hubble Space Telescope (HST) observations of the exceptionally bright and luminous Swift gamma-ray burst (GRB), GRB 130427A. At z = 0.34, this burst affords an excellent opportunity to study the supernova (SN) and host galaxy associated with an intrinsically extremely luminous burst (E {sub iso} > 10{sup 54} erg): more luminous than any previous GRB with a spectroscopically associated SN. We use the combination of the image quality, UV capability, and invariant point-spread function of HST to provide the best possible separation of the afterglow, host, and SN contributions to the observed light ?17 rest-frame days after the burst, utilizing a host subtraction spectrum obtained one year later. Advanced Camera for Surveys grism observations show that the associated SN, SN 2013cq, has an overall spectral shape and luminosity similar to SN 1998bw (with a photospheric velocity, v {sub ph} ? 15, 000 km s{sup –1}). The positions of the bluer features are better matched by the higher velocity SN 2010bh (v {sub ph} ? 30, 000 km s{sup –1}), but this SN is significantly fainter and fails to reproduce the overall spectral shape, perhaps indicative of velocity structure in the ejecta. We find that the burst originated ?4 kpc from the nucleus of a moderately star forming (1 M {sub ?} yr{sup –1}), possibly interacting disk galaxy. The absolute magnitude, physical size, and morphology of this galaxy, as well as the location of the GRB within it, are also strikingly similar to those of GRB 980425/SN 1998bw. The similarity of the SNe and environment from both the most luminous and least luminous GRBs suggests that broadly similar progenitor stars can create GRBs across six orders of magnitude in isotropic energy.

  9. Observations of Ultraluminous Infrared Galaxies with the Infrared Spectrograph on the Spitzer Space Telescope II: The IRAS Bright Galaxy Sample

    E-Print Network [OSTI]

    L. Armus; V. Charmandaris; J. Bernard-Salas; H. W. W. Spoon; J. A. Marshall; S. J. U Higdon; V. Desai; H. I. Teplitz; L. Hao; D. Devost; B. R. Brandl; Y. Wu; G. C. Sloan; B. T. Soifer; J. R. Houck; T. L. Herter

    2006-10-06

    We present spectra taken with the Infrared Spectrograph on Spitzer covering the 5-38 micron region of the ten Ultraluminous Infrared Galaxies (ULIRGs) found in the IRAS Bright Galaxy Sample. Among the BGS ULIRGs, we find a factor of 50 spread in the rest-frame mid to far-infrared spectral slope. The 9.7 micron silicate optical depths range from less than 0.4 more than 4.2, implying line of sight extinctions of A(V) ~ 8 - 78 mag. There is evidence for water ice and hydrocarbon absorption and C2H2 and HCN absorption features in four and possibly six of the 10 BGS ULIRGs, indicating shielded molecular clouds and a warm, dense ISM. We have detected [NeV] emission in three of the ten BGS ULIRGs, at flux levels of 5-18E-14 erg/cm^2/sec and [NeV] 14.3/[NeII] 12.8 line flux ratios of 0.12-0.85. The remaining BGS ULIRGs have limits on their [NeV]/[NeII] line flux ratios which range from less than 0.15 to less than 0.01. Among the BGS ULIRGs, the AGN fractions implied by either the [NeV]/[NeII] or [OIV]/[NeII] line flux ratios (or their upper limits) are significantly lower than implied by the MIR slope or EQW of the 6.2 micron PAH feature. Fitting the SEDs, we see evidence for hot (T > 300K) dust in five of the BGS ULIRGs, with the fraction of hot dust to total dust luminosity ranging from ~1-23%, before correcting for extinction. When integrated over the IRAC-8, IRS blue peakup, and MIPS-24 filter bandpasses, the IRS spectra imply very blue colors for some ULIRGs at z ~ 1.3. This is most extreme for sources with significant amounts of warm dust and deep silicate absorption.

  10. The Outer Disks of Early-Type Galaxies. II. Surface-Brightness Profiles of Unbarred Galaxies and Trends with Hubble Type

    E-Print Network [OSTI]

    Gutierrez, Leonel; Aladro, Rebeca; Beckman, John E

    2011-01-01

    We present azimuthally averaged radial profiles of R-band surface brightness for a complete sample of 47 early-type, unbarred galaxies, as a complement to our previous study of early-type barred galaxies. Following very careful sky subtraction, the profiles can typically be determined down to brightness levels well below 27 mag arcsec^{-2} and in the best cases below 28 mag arcsec^{-2}. We classified the profiles according to the scheme used previously for the barred sample: Type I profiles are single unbroken exponential radial declines in brightness; Type II profiles ("truncations") have an inner shallow slope (usually exponential) which changes at a well defined break radius to a steeper exponential; and Type III profiles ("antitruncations") have an inner exponential that is steeper, giving way to a shallower outer (usually exponential) decline. By combining these profiles with previous studies, we can make the first clear statements about the trends of outer-disk profile types along the Hubble sequence (i...

  11. BRIGHT 'MERGER-NOVA' FROM THE REMNANT OF A NEUTRON STAR BINARY MERGER: A SIGNATURE OF A NEWLY BORN, MASSIVE, MILLISECOND MAGNETAR

    SciTech Connect (OSTI)

    Yu, Yun-Wei [Institute of Astrophysics, Central China Normal University, Wuhan 430079 (China)] [Institute of Astrophysics, Central China Normal University, Wuhan 430079 (China); Zhang, Bing; Gao, He, E-mail: yuyw@mail.ccnu.edu.cn, E-mail: zhang@physics.unlv.edu [Department of Physics and Astronomy, University of Nevada, Las Vegas, NV 89154 (United States)] [Department of Physics and Astronomy, University of Nevada, Las Vegas, NV 89154 (United States)

    2013-10-20

    A massive millisecond magnetar may survive the merger of a neutron star (NS) binary, which would continuously power the merger ejecta. We develop a generic dynamic model for the merger ejecta with energy injection from the central magnetar. The ejecta emission (the {sup m}erger-nova{sup )} powered by the magnetar peaks in the UV band and the peak of the light curve, progressively shifts to an earlier epoch with increasing frequency. A magnetar-powered merger-nova could have an optical peak brightness comparable to a supernova, which is a few tens or hundreds times brighter than the radioactive-powered merger-novae (the so-called macro-nova or kilo-nova). On the other hand, such a merger-nova would peak earlier and have a significantly shorter duration than that of a supernova. An early collapse of the magnetar could suppress the brightness of the optical emission and shorten its duration. Such millisecond-magnetar-powered merger-novae may be detected from NS-NS merger events without an observed short gamma-ray burst, and could be a bright electromagnetic counterpart for gravitational wave bursts due to NS-NS mergers. If detected, it suggests that the merger leaves behind a massive NS, which has important implications for the equation-of-state of nuclear matter.

  12. Fewer lights, Brighter Shine in New Hampshire County

    Broader source: Energy.gov [DOE]

    The parking lot to the county courthouse and nursing home facility in Strafford County, New Hampshire needed new lights. And thanks to an Energy Efficiency and Conservation Block Grant from the Energy Department, Strafford got what it needed and more.

  13. Cosmos incognito : Vera Rubin shines light on dark matter

    E-Print Network [OSTI]

    Yeager, Ashley

    2008-01-01

    This thesis, a profile of astronomer Vera Rubin, highlights her scientific achievements, most notably the irrefutable evidence she gathered to persuade the astronomical community that galaxies spin at a faster speed than ...

  14. ALS X-Rays Shine a New Light on Catalysis

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    times science has used high-brilliance x-rays to look so closely at these reactions. Lead author Dr. David Mueller at the ALS using x-rays to characterize working fuel cells....

  15. Shining Light on the Fleeting Interactions of Single Molecules...

    Office of Science (SC) Website

    However, watching these molecular encounter events is not easy due to the perpetual thermal agitation of the surrounding water molecules, and nanometer-sized biomolecules...

  16. Making (and Saving) Money While the Sun Shines

    Broader source: Energy.gov [DOE]

    This presentation summarizes the information given by Tydings and Rosenberg during the DOE SunShot Grand Challenge: Summit and Technology Forum, June 13-14, 2012.

  17. NREL: News Feature - Rain or Shine, Students Keep Their Race...

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    always work," he said. One of his teams, Astler said, wanted to use a hinge so that the solar panel could be adjusted to more directly receive the sun. But the hinge added too...

  18. ALS X-Rays Shine a New Light on Catalysis

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    ALS in a novel way to observe the behavior of electrons during technologically important chemical reactions in metal oxide electrocatalysts. What they learned has upended...

  19. ALS X-Rays Shine a New Light on Catalysis

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    were able to directly observe redox processes in thin-film iron and cobalt perovskite oxide electrocatalysts using surface-sensitive, x-ray absorption spectroscopy while...

  20. Shining Some Light on the World Cup's Efficiency Efforts | Department...

    Broader source: Energy.gov (indexed) [DOE]

    The Mineiro Stadium, with its six thousand solar panels, is ready for more World Cup Action | Photo courtesy of Renato CobucciImprensaMG The Mineiro Stadium, with its six...

  1. Galaxies that Shine: radiation-hydrodynamical simulations of disk galaxies

    E-Print Network [OSTI]

    Rosdahl, Joakim; Teyssier, Romain; Agertz, Oscar

    2015-01-01

    Radiation feedback is typically implemented using subgrid recipes in hydrodynamical simulations of galaxies. Very little work has so far been performed using radiation-hydrodynamics (RHD), and there is no consensus on the importance of radiation feedback in galaxy evolution. We present RHD simulations of isolated galaxy disks of different masses with a resolution of 18 pc. Besides accounting for supernova feedback, our simulations are the first galaxy-scale simulations to include RHD treatments of photo-ionisation heating and radiation pressure, from both direct optical/UV radiation and multi-scattered, re-processed infrared (IR) radiation. Photo-heating smooths and thickens the disks and suppresses star formation about as much as the inclusion of ("thermal dump") supernova feedback does. These effects decrease with galaxy mass and are mainly due to the prevention of the formation of dense clouds, as opposed to their destruction. Radiation pressure, whether from direct or IR radiation, has little effect, but ...

  2. Desert Sunlight is Shining Example of How DOE Loan Guarantees...

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    (EIA) forecasted in 2008 that just 140 MW of total utility-scale PV solar capacity would be installed by 2015. Now we're in 2015 and Desert Sunlight itself represents...

  3. Shining Light on Catalysis | Stanford Synchrotron Radiation Lightsourc...

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    A. van Bokhoven, Professor for Heterogeneous Catalysis Institute for Chemical and Bioengineering ETH Zurich Head of Laboratory for Catalysis and Sustainable Chemistry (LSK) Swiss...

  4. ALS X-Rays Shine a New Light on Catalysis

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity ofkandz-cm11 Outreach HomeA Better Anode Design to Improve4AJ01) (See Energy Level79AJ01)19^ U N ISpectrum PrintUsers'ALS

  5. ALS X-Rays Shine a New Light on Catalysis

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity ofkandz-cm11 Outreach HomeA Better Anode Design to Improve4AJ01) (See Energy Level79AJ01)19^ U N ISpectrum PrintUsers'ALSALS

  6. ALS X-Rays Shine a New Light on Catalysis

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity ofkandz-cm11 Outreach HomeA Better Anode Design to Improve4AJ01) (See Energy Level79AJ01)19^ U N ISpectrum PrintUsers'ALSALSALS

  7. ALS X-Rays Shine a New Light on Catalysis

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity ofkandz-cm11 Outreach HomeA Better Anode Design to Improve4AJ01) (See Energy Level79AJ01)19^ U N ISpectrum

  8. National Laboratories Shine at World's Largest Hydropower Event |

    Broader source: Energy.gov (indexed) [DOE]

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of Natural GasAdjustmentsShirleyEnergy AEnergy Managing SwimmingMicrosoftPolicy, on May 28, 2014,

  9. ALS X-Rays Shine a New Light on Catalysis

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of NaturalDukeWakefieldSulfateSciTechtail.TheoryTuesday, August 10, 20102016 NewsUsers' Executive Committee ALSALS X-Rays

  10. ALS X-Rays Shine a New Light on Catalysis

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of NaturalDukeWakefieldSulfateSciTechtail.TheoryTuesday, August 10, 20102016 NewsUsers' Executive Committee ALSALS X-RaysALS

  11. Smart Grid Shines after California Earthquake | OpenEI Community

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIX ECoop Inc JumpHeter Battery Technology CoWanpingSilveiraSmallSmarr EMC Jump to:CoSmart

  12. EM Waste Isolation Pilot Plant Team's Holiday Spirit Shines | Department

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Delicious Rank EERE:FinancingPetroleum Based|DepartmentStatementof EnergyQuality AssuranceTop1 EMEMUtilityof

  13. Solar Decathlon: Rain and Shine | Department of Energy

    Energy Savers [EERE]

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIX E LIST OF APPLICABLE DIRECTIVES PursuantEnergy Small|EnergyWake of

  14. LANL Instrument to Shine Light on Mars Habitability | National Nuclear

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity ofkandz-cm11 Outreach Home Room NewsInformationJesse Bergkamp Graduate student Subtask2 J.N. Shadid,1 Hany4-22379LAMMPSSecurity

  15. A Shining Example of Dr. King's legacy | Department of Energy

    Broader source: Energy.gov (indexed) [DOE]

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of Natural GasAdjustmentsShirley Ann JacksonDepartment| Department ofApplianceU.S.Department of5thAThePROCEDURALThe

  16. Los Alamos instrument to shine light on Mars habitability

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity ofkandz-cm11 Outreach Home Room NewsInformationJesse BergkampCentermillion to local Unitedto STEMLANLTeam honoredInstrument to

  17. Crayola's True Color Shines Through: Green | Department of Energy

    Broader source: Energy.gov (indexed) [DOE]

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of Natural GasAdjustmentsShirleyEnergy A plug-in electric vehicle (PEV)Day-June2012 |DepartmentRemarksHomemade blankets

  18. GALAXY HALO TRUNCATION AND GIANT ARC SURFACE BRIGHTNESS RECONSTRUCTION IN THE CLUSTER MACSJ1206.2-0847

    SciTech Connect (OSTI)

    Eichner, Thomas; Seitz, Stella; Monna, Anna [Universitaets-Sternwarte Muenchen, Scheinerstr. 1, D-81679 Muenchen (Germany); Suyu, Sherry H. [Department of Physics, University of California, Santa Barbara, CA 93106 (United States); Halkola, Aleksi [Institute of Medical Engineering, University of Luebeck, Ratzeburger Allee 160 23562 Luebeck (Germany); Umetsu, Keiichi [Institute of Astronomy and Astrophysics, Academia Sinica, P.O. Box 23-141, Taipei 10617, Taiwan (China); Zitrin, Adi [Institut fuer Theoretische Astrophysik, ZAH, Albert-Ueberle-Strasse 2, D-69120 Heidelberg (Germany); Coe, Dan; Postman, Marc; Koekemoer, Anton; Bradley, Larry [Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21208 (United States); Rosati, Piero [ESO-European Southern Observatory, D-85748 Garching bei Muenchen (Germany); Grillo, Claudio; Host, Ole [Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen (Denmark); Balestra, Italo [Max-Planck-Institut fuer Extraterrestrische Physik, Giessenbachstrasse, D-85748 Garching (Germany); Zheng, Wei; Lemze, Doron [Department of Physics and Astronomy, The Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218 (United States); Broadhurst, Tom [Department of Theoretical Physics, University of the Basque Country, P.O. Box 644, E-48080 Bilbao (Spain); Moustakas, Leonidas [Jet Propulsion Laboratory, California Institute of Technology, MS 169-327, Pasadena, CA 91109 (United States); Molino, Alberto [Instituto de Astrofisica de Andalucia (CSIC), C/Camino Bajo de Huetor 24, Granada E-18008 (Spain); and others

    2013-09-10

    In this work, we analyze the mass distribution of MACSJ1206.2-0847, particularly focusing on the halo properties of its cluster members. The cluster appears relaxed in its X-ray emission, but has a significant amount of intracluster light that is not centrally concentrated, suggesting that galaxy-scale interactions are still ongoing despite the overall relaxed state. The cluster lenses 12 background galaxies into multiple images and one galaxy at z = 1.033 into a giant arc and its counterimage. The multiple image positions and the surface brightness (SFB) distribution of the arc, which is bent around several cluster members, are sensitive to the cluster galaxy halo properties. We model the cluster mass distribution with a Navarro-Frenk-White profile and the galaxy halos with two parameters for the mass normalization and the extent of a reference halo assuming scalings with their observed near-infrared light. We match the multiple image positions at an rms level of 0.''85 and can reconstruct the SFB distribution of the arc in several filters to a remarkable accuracy based on this cluster model. The length scale where the enclosed galaxy halo mass is best constrained is about 5 effective radii-a scale in between those accessible to dynamical and field strong-lensing mass estimates on the one hand and galaxy-galaxy weak-lensing results on the other hand. The velocity dispersion and halo size of a galaxy with m{sub 160W,AB} = 19.2 and M{sub B,Vega} = -20.7 are {sigma} = 150 km s{sup -1} and r Almost-Equal-To 26 {+-} 6 kpc, respectively, indicating that the halos of the cluster galaxies are tidally stripped. We also reconstruct the unlensed source, which is smaller by a factor of {approx}5.8 in area, demonstrating the increase in morphological information due to lensing. We conclude that this galaxy likely has star-forming spiral arms with a red (older) central component.

  19. Scale Lengths in Disk Surface Brightness as probes of Dust Extinction in 3 Spiral Galaxies: M 51, NGC 3631 and M 100

    E-Print Network [OSTI]

    J. E. Beckman; R. F. Peletier; J. H. Knapen; R. L. M. Corradi; L. J. Gentet

    1996-02-19

    We have measured the radial brightness distributions in the disks of three nearby face-on spirals: M 51, NGC 3631, and NGC 4321 (M 100) in the photometric bands B through I, with the addition of the K band for M 51 only. The measurements were made by averaging azimuthally, in three modes, the two-dimensional surface brightness over the disks in photometric images of the objects in each band: (a) over each disk as a whole, (b) over the spiral arms alone, and (c) over the interarm zones alone. From these profiles scale-lengths were derived for comparison with schematic exponential disk models incorporating interstellar dust. These models include both absorption and scattering in their treatment of radiative transfer. The model fits show that the arms exhibit greater optical depth in dust than the interarm zones. The average fraction of emitted stellar light in V which is extinguished by dust within 3 scale-lengths of the center of each galaxy does not rise above 20% in any of them. We show that this conclusion is also valid for models with similar overall quantities of dust, but where this is concentrated in lanes. These can also account for the observed scale-lengths, and their variations.

  20. The mystery of spectral breaks: Lyman continuum absorption by photon-photon pair production in the Fermi GeV spectra of bright blazars

    SciTech Connect (OSTI)

    Stern, Boris E. [Institute for Nuclear Research, Russian Academy of Sciences, Prospekt 60-letiya Oktyabrya 7a, Moscow 117312 (Russian Federation); Poutanen, Juri, E-mail: stern.boris@gmail.com, E-mail: juri.poutanen@utu.fi [Tuorla Observatory, University of Turku, Väisäläntie 20, FI-21500 Piikkiö (Finland)

    2014-10-10

    We re-analyze Fermi/LAT ?-ray spectra of bright blazars using the new Pass 7 version of the detector response files and detect breaks at ?5 GeV in the rest-frame spectra of 3C 454.3 and possibly also 4C +21.35, associated with the photon-photon pair production absorption by the He II Lyman continuum (LyC). We also detect significant breaks at ?20 GeV associated with hydrogen LyC in both the individual spectra and the stacked redshift-corrected spectrum of several bright blazars. The detected breaks in the stacked spectra univocally prove that they are associated with atomic ultraviolet emission features of the quasar broad-line region (BLR). The dominance of the absorption by the hydrogen Ly complex over He II, a small detected optical depth, and break energy consistent with head-on collisions with LyC photons imply that the ?-ray emission site is located within the BLR, but most of the BLR emission comes from a flat disk-like structure producing little opacity. Alternatively, the LyC emission region size might be larger than the BLR size measured from reverberation mapping, and/or the ?-ray emitting region is extended. These solutions would resolve the long-standing issue of how the multi-hundred GeV photons can escape from the emission zone without being absorbed by softer photons.

  1. XID: Cross-Association of ROSAT/Bright Source Catalog X-ray Sources with USNO A2 Optical Point Sources

    E-Print Network [OSTI]

    Robert E. Rutledge; Robert J. Brunner; Thomas A. Prince; Carol Lonsdale

    2000-04-04

    We quantitatively cross-associate the 18811 ROSAT Bright Source Catalog (RASS/BSC) X-ray sources with optical sources in the USNO-A2 catalog, calculating the the probability of unique association (Pid) between each candidate within 75 arcsec of the X-ray source position, on the basis of optical magnitude and proximity. We present catalogs of RASS/BSC sources for which the probability of association is >98%, >90%, and >50%, which contain 2705, 5492, and 11301 unique USNO-A2 optical counterparts respectively down to the stated level of significance. We include in this catalog a list of objects in the SIMBAD database within 10 arcsec of the USNO position, as an aid to identification and source classification. The catalog is more useful than previous catalogs which either rely on plausibility arguments for association, or do not aid in selecting a counterpart between multiple off-band sources in the field. We find that a fraction ~65.8% of RASS/BSC sources have an identifiable optical counterpart, down to the magnitude limit of the USNO catalog which could be identified by their spatial proximity and high optical brightness.

  2. VERITAS detection of $\\gamma$-ray flaring activity from the BL Lac object 1ES 1727+502 during bright moonlight observations

    E-Print Network [OSTI]

    Archambault, S; Beilicke, M; Benbow, W; Bird, R; Biteau, J; Bouvier, A; Bugaev, V; Cardenzana, J V; Cerruti, M; Chen, X; Ciupik, L; Connolly, M P; Cui, W; Dickinson, H J; Dumm, J; Eisch, J D; Errando, M; Falcone, A; Feng, Q; Finley, J P; Fleischhack, H; Fortin, P; Fortson, L; Furniss, A; Gillanders, G H; Griffin, S; Griffiths, S T; Grube, J; Gyuk, G; Håkansson, N; Hanna, D; Holder, J; Humensky, T B; Johnson, C A; Kaaret, P; Kar, P; Kertzman, M; Khassen, Y; Kieda, D; Krause, M; Krennrich, F; Kumar, S; Lang, M J; Maier, G; McArthur, S; McCann, A; Meagher, K; Millis, J; Moriarty, P; Mukherjee, R; Nieto, D; de Bhróithe, A O'Faoláin; Ong, R A; Otte, A N; Park, N; Pohl, M; Popkow, A; Prokoph, H; Pueschel, E; Quinn, J; Ragan, K; Reyes, L C; Reynolds, P T; Richards, G T; Roache, E; Santander, M; Sembroski, G H; Shahinyan, K; Smith, A W; Staszak, D; Telezhinsky, I; Tucci, J V; Tyler, J; Varlotta, A; Vincent, S; Wakely, S P; Weinstein, A; Welsing, R; Wilhelm, A; Williams, D A; Zitzer, B; Hughes, Z D

    2015-01-01

    During moonlit nights, observations with ground-based Cherenkov telescopes at very high energies (VHE, $E>100$ GeV) are constrained since the photomultiplier tubes (PMTs) in the telescope camera are extremely sensitive to the background moonlight. Observations with the VERITAS telescopes in the standard configuration are performed only with a moon illumination less than 35$\\%$ of full moon. Since 2012, the VERITAS collaboration has implemented a new observing mode under bright moonlight, by either reducing the voltage applied to the PMTs (reduced-high-voltage configuration, RHV), or by utilizing UV-transparent filters. While these operating modes result in lower sensitivity and increased energy thresholds, the extension of the available observing time is useful for monitoring variable sources such as blazars and sources requiring spectral measurements at the highest energies. In this paper we report the detection of $\\gamma$-ray flaring activity from the BL Lac object 1ES 1727+502 during RHV observations. Thi...

  3. Production, formation, and transport of high-brightness atomic hydrogen beam studies for the relativistic heavy ion collider polarized source upgrade

    SciTech Connect (OSTI)

    Kolmogorov, A. Stupishin, N.; Atoian, G.; Ritter, J.; Zelenski, A.; Davydenko, V.; Ivanov, A.; Novosibirsk State University, Novosibirsk

    2014-02-15

    The RHIC polarized H{sup ?} ion source had been successfully upgraded to higher intensity and polarization by using a very high brightness fast atomic beam source developed at BINP, Novosibirsk. In this source the proton beam is extracted by a four-grid multi-aperture ion optical system and neutralized in the H{sub 2} gas cell downstream from the grids. The proton beam is extracted from plasma emitter with a low transverse ion temperature of ?0.2 eV which is formed by plasma jet expansion from the arc plasma generator. The multi-hole grids are spherically shaped to produce “geometrical” beam focusing. Proton beam formation and transport of atomic beam were experimentally studied at test bench.

  4. EPIC 204129699b, a grazing transiting hot Jupiter on an 1.26-day orbit around a bright solar like star

    E-Print Network [OSTI]

    Grziwa, S; Csizmadia, Sz; Fridlund, M; Parviainen, H; Deeg, H J; Cabrera, J; Djupvik, A A; Albrecht, S; Palle, E B; Pätzold, M; Béjar, V J S; Arranz, J P; Eigmüller, P; Erikson, A; Fynbo, J P U; Guenther, E W; Hatzes, A P; Kiilerich, A; Korth, J; Kuutma, T; Montanés-Rodríguez, P; Nespral, D; Nowak, G; Rauer, H; Saario, J; Sebastian, D; Slumstrup, D

    2015-01-01

    We report the discovery of EPIC 204129699b, the first confirmed transiting hot Jupiter detected by the K2 space mission. We combined K2 photometry with FastCam lucky imaging and FIES and HARPS high-resolution spectroscopy to confirm the planetary nature of the transiting object and derived the system parameters. EPIC 204129699b is a 1.8-Jupiter-mass planet on an 1.26-day-orbit around a G7V star (M* = 0.91 Msun, R* = 0.78 Rsun). The planetary radius is poorly constrained (0.7 < Rp < 1.4 RJup ), owing to the grazing transit and the low sampling rate of the K2 photometry. The short orbital period and the brightness of the host star (V = 10.8 mag) make the system amenable to atmospheric characterization.

  5. THE RADIO SURFACE-BRIGHTNESS-TO-DIAMETER RELATION FOR GALACTIC SUPERNOVA REMNANTS: SAMPLE SELECTION AND ROBUST ANALYSIS WITH VARIOUS FITTING OFFSETS

    SciTech Connect (OSTI)

    Pavlovic, M. Z.; Urosevic, D.; Arbutina, B. [Department of Astronomy, Faculty of Mathematics, University of Belgrade, Studentski trg 16, 11000 Belgrade (Serbia); Vukotic, B. [Astronomical Observatory, Volgina 7, 11060 Belgrade 38 (Serbia); Goeker, Ue. D., E-mail: marko@math.rs [Physics Department, Bogazici University, Bebek 34342, Istanbul (Turkey)

    2013-01-15

    In this paper, we present new empirical radio surface-brightness-to-diameter ({Sigma}-D) relations for supernova remnants (SNRs) in our Galaxy. We also present new theoretical derivations of the {Sigma}-D relation based on equipartition or on a constant ratio between cosmic rays and magnetic field energy. A new calibration sample of 60 Galactic SNRs with independently determined distances is created. Instead of (standard) vertical regression, used in previous papers, different fitting procedures are applied to the calibration sample in the log {Sigma}-log D plane. Non-standard regressions are used to satisfy the requirement that values of parameters obtained from the fitting of {Sigma}-D and D-{Sigma} relations should be invariant within estimated uncertainties. We impose symmetry between {Sigma}-D and D-{Sigma} due to the existence of large scatter in both D and {Sigma}. Using four fitting methods that treat {Sigma} and D symmetrically, different {Sigma}-D slopes {beta} are obtained for the calibration sample. Monte Carlo simulations verify that the slopes of the empirical {Sigma}-D relation should be determined by using orthogonal regression because of its good performance in data sets with severe scatter. The slope derived here ({beta} = 4.8) is significantly steeper than those derived in previous studies. This new slope is closer to the updated theoretically predicted surface-brightness-diameter slope in the radio range of the Sedov phase. We also analyze the empirical {Sigma}-D relations for SNRs in a dense environment of molecular clouds and for SNRs evolving in the lower-density interstellar medium. Applying new empirical relations to estimate distances of Galactic SNRs results in a dramatically changed distance scale.

  6. Jetting into the Moments after the Big Bang | U.S. DOE Office...

    Office of Science (SC) Website

    shining brightly at temperatures more than 100,000 times hotter than the center of the Sun. To explore the properties of this plasma of quarks and gluons as it expands and cools,...

  7. 1998 - 06 | Jefferson Lab

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    June 1998 Sun, 06281998 - 11:00pm FEL Shines Bright in Debut (Virginia Business Observer) Sat, 06201998 - 11:00pm Laser Breaks Record (Richmond Times-Dispatch) Thu, 06181998...

  8. Analysis and Identification of Biomarkers and Origin of Color in a Bright Blue Crude Oil Juyal, P.; McKenna, A. M.; Yen, A.; Rodgers, R. P.; Reddy, C. M.; Nelson, R. K.; Andrews, A. B.;

    E-Print Network [OSTI]

    Analysis and Identification of Biomarkers and Origin of Color in a Bright Blue Crude Oil Juyal, P School, Woods Hole A key step in crude oil production is injection of monoethyene glycol (MEG) to prevent. Strikingly blue crude oil from a Gulf of Mexico drillingg y , p of Mexico platform, the recovery of MEG from

  9. Estimating 13.8-GHz path-integrated attenuation from 10.7-GHz brightness temperatures for the TRMM combined PR-TMI precipitation algorithm

    SciTech Connect (OSTI)

    Smith, E.A.; Farrar, M.R.; Xiang, X. [Florida State Univ., Tallahassee, FL (United States)] [Florida State Univ., Tallahassee, FL (United States); Turk, F.J. [Naval Research Lab., Monterey, CA (United States)] [Naval Research Lab., Monterey, CA (United States); Mugnai, A. [Instituto di Fisica dell`Atmosfera-CNR, Frascati (Italy)] [Instituto di Fisica dell`Atmosfera-CNR, Frascati (Italy)

    1997-04-01

    This study presents research in support of the design and implementation of a combined radar-radiometer algorithm to be used for precipitation retrieval during the Tropical Rainfall Measuring Mission (TRMM). The combined algorithm approach is expected to overcome various difficulties that arise with a radar-only approach, particularly related to estimates of path-integrated attenuation (PIA)along the TRMM radar beam. A technique is described for estimating PIA at the 13.8-GHz frequency of the TRMM precipitation radar (PR) from 10.7-GHz brightness temperature T{sub B} measurements obtained from the TRMM microwave imager. Through the use of variational or probabilistic techniques, the independent PIA calculations provide a means to adjust for errors that accumulate in estimates of range-dependent rain rates at progressively increasing range positions from radar reflectivity vectors. The accepted radar approach for obtaining PIA from ocean-viewing radar reflectivity measurements is called the surface reference technique, a scheme based on the difference in ocean surface cross sections between cloud-free and raining radar pixels. This technique has encountered problems, which are discussed and analyzed with the aid of coordinated aircraft radar (Airborne Rain Mapping Radar) and radiometer (Advanced Microwave Precipitation Radiometer) measurements obtained during the west Pacific Tropical Ocean Global Atmosphere Coupled Ocean-Atmosphere Response Experiment in 1993. 97 refs., 12 figs., 5 tabs.

  10. CARMA SURVEY TOWARD INFRARED-BRIGHT NEARBY GALAXIES (STING). III. THE DEPENDENCE OF ATOMIC AND MOLECULAR GAS SURFACE DENSITIES ON GALAXY PROPERTIES

    SciTech Connect (OSTI)

    Wong, Tony; Xue, Rui; Bolatto, Alberto D.; Fisher, David B.; Vogel, Stuart N.; Leroy, Adam K.; Blitz, Leo; Rosolowsky, Erik; Bigiel, Frank; Ott, Jürgen; Rahman, Nurur; Walter, Fabian

    2013-11-01

    We investigate the correlation between CO and H I emission in 18 nearby galaxies from the CARMA Survey Toward IR-Bright Nearby Galaxies (STING) at sub-kpc and kpc scales. Our sample, spanning a wide range in stellar mass and metallicity, reveals evidence for a metallicity dependence of the H I column density measured in regions exhibiting CO emission. Such a dependence is predicted by the equilibrium model of McKee and Krumholz, which balances H{sub 2} formation and dissociation. The observed H I column density is often smaller than predicted by the model, an effect we attribute to unresolved clumping, although values close to the model prediction are also seen. We do not observe H I column densities much larger than predicted, as might be expected were there a diffuse H I component that did not contribute to H{sub 2} shielding. We also find that the H{sub 2} column density inferred from CO correlates strongly with the stellar surface density, suggesting that the local supply of molecular gas is tightly regulated by the stellar disk.

  11. The Young and Bright Type Ia Supernova ASASSN-14lp: Discovery, Early-Time Observations, First-Light Time, Distance to NGC 4666, and Progenitor Constraints

    E-Print Network [OSTI]

    Shappee, B J; Holoien, T W -S; Prieto, J L; Contreras, C; Itagaki, K; Burns, C R; Kochanek, C S; Stanek, K Z; Alper, E; Basu, U; Beacom, J F; Bersier, D; Brimacombe, J; Conseil, E; Danilet, A B; Dong, Subo; Falco, E; Grupe, D; Hsiao, E Y; Kiyota, S; Morrell, N; Nicolas, J; Phillips, M M; Pojmanski, G; Simonian, G; Stritzinger, M; Szczygie?, D M; Thompson, T A; Thorstensen, J; Wagner, M; Wo?niak, P R

    2015-01-01

    On 2014 Dec. 9.61, the All-Sky Automated Survey for SuperNovae (ASAS-SN or "Assassin") discovered ASASSN-14lp just $\\sim2$ days after first light using a global array of 14-cm diameter telescopes. ASASSN-14lp went on to become a bright supernova ($V = 11.94$ mag), second only to SN 2014J for the year. We present prediscovery photometry (with a detection less than a day after first light) and ultraviolet through near-infrared photometric and spectroscopic data covering the rise and fall of ASASSN-14lp for more than 100 days. We find that ASASSN-14lp had a broad light curve ($\\Delta m_{15}(B) = 0.796 \\pm 0.001_{\\textrm{stat}}$), a $B$-band maximum at $2457015.823 \\pm 0.030_{\\textrm{stat}}$, a rise time of $16.94^{+ 0.11 }_{- 0.11 }$ days, and moderate host--galaxy extinction ($E(B-V)_{\\textrm{host}} = 0.329 \\pm 0.001_{\\textrm{stat}}$). Using ASASSN-14lp we derive a distance modulus for NGC 4666 of $\\mu = 30.834 \\pm 0.003_{\\textrm{stat}} \\pm 0.16_{\\textrm{syst}}$ corresponding to a distance of $14.68 \\pm 0.02_{\\...

  12. Galaxies in X-ray Selected Clusters and Groups in Dark Energy Survey Data: Stellar Mass Growth of Bright Central Galaxies Since z~1.2

    E-Print Network [OSTI]

    Zhang, Y; Mckay, T; Rooney, P; Evrard, A E; Romer, A K; Perfecto, R; Song, J; Desai, S; Mohr, J; Wilcox, H; Bermeo, A; Jeltema, T; Hollowood, D; Bacon, D; Capozzi, D; Collins, C; Das, R; Gerdes, D; Hennig, C; Hilton, M; Hoyle, B; Kay, S; Liddle, A; Mann, R G; Mehrtens, N; Nichol, R C; Papovich, C; Sahlén, M; Soares-Santos, M; Stott, J; Viana, P T; Abbott, T; Abdalla, F B; Banerji, M; Bauer, A H; Benoit-Lévy, A; Bertin, E; Brooks, D; Buckley-Geer, E; Burke, D L; Rosell, A Carnero; Castander, F J; Diehl, H T; Doel, P; Cunha, C E; Eifler, T F; Neto, A Fausti; Fernandez, E; Flaugher, B; Fosalba, P; Frieman, J; Gaztanaga, E; Gruen, D; Gruendl, R A; Honscheid, K; James, D; Kuehn, K; Kuropatkin, N; Lahav, O; Maia, M A G; Makler, M; Marshall, J L; Martini, Paul; Miquel, R; Ogando, R; Plazas, A A; Roodman, A; Rykoff, E S; Sako, M; Sanchez, E; Scarpine, V; Schubnell, M; Sevilla, I; Smith, R C; Sobreira, F; Suchyta, E; Swanson, M E C; Tarle, G; Thaler, J; Tucker, D; Vikram, V; Da Costa, L N

    2015-01-01

    Using the science verification data of the Dark Energy Survey (DES) for a new sample of 106 X-Ray selected clusters and groups, we study the stellar mass growth of Bright Central Galaxies (BCGs) since redshift 1.2. Compared with the expectation in a semi-analytical model applied to the Millennium Simulation, the observed BCGs become under-massive/under-luminous with decreasing redshift. We incorporate the uncertainties associated with cluster mass, redshift, and BCG stellar mass measurements into analysis of a redshift-dependent BCG-cluster mass relation, $m_{*}\\propto(\\frac{M_{200}}{1.5\\times 10^{14}M_{\\odot}})^{0.24\\pm 0.08}(1+z)^{-0.19\\pm0.34}$, and compare the observed relation to the simulation prediction. We estimate the average growth rate since z = 1.0 for BCGs hosted by clusters of $M_{200, z}=10^{13.8}M_{\\odot}$, at $z=1.0$: $m_{*, BCG}$ appears to have grown by $0.13\\pm0.11$ dex, in tension at $\\sim 2.5 \\sigma$ significance level with the 0.4 dex growth rate expected in the simulation. We show that...

  13. The SW Sex-type star 2MASS J01074282+4845188: an unusual bright accretion disk with non-steady emission and a hot white dwarf

    E-Print Network [OSTI]

    Khruzina, T; Kjurkchieva, D; 10.1051/0004-6361/201220385

    2013-01-01

    We present new photometric and spectral observations of the newly discovered nova-like eclipsing star 2MASS J01074282+4845188. To obtain a light curve solution we used model of a nova-like star whose emission sources are a white dwarf surrounded by an accretion disk, a secondary star filling its Roche lobe, a hot spot and a hot line. 2MASS J01074282+4845188 shows the deepest permanent eclipse among the known nova-like stars. It is reproduced by covering the very bright accretion disk by the secondary component. The luminosity of the disk is much bigger than that of the rest light sources. The determined high temperature of the disk is typical for that observed during the outbursts of CVs. The primary of 2MASS J01074282+4845188 is one of the hottest white dwarfs in CVs. The temperature of 5090 K of its secondary is also quite high and more appropriate for a long-period SW Sex star. It might be explained by the intense heating from the hot white dwarf and the hot accretion disk of the target. The high mass accr...

  14. The Oxford-Dartmouth Thirty Degree Survey II: Clustering of Bright Lyman Break Galaxies - Strong Luminosity Dependent Bias at z=4

    E-Print Network [OSTI]

    Allen, P D; Dalton, G; MacDonald, E; Blake, C; Clewley, L; Heymans, C; Wegner, G; Allen, Paul D.; Moustakas, Leonidas A.; Dalton, Gavin; Donald, Emily Mac; Blake, Chris; Clewley, Lee; Heymans, Catherine; Wegner, Gary

    2005-01-01

    We present measurements of the clustering properties of bright ($L>L_{*}$) z$\\sim$4 Lyman Break Galaxies (LBGs) selected from the Oxford-Dartmouth Thirty Degree Survey (ODT). We describe techniques used to select and evaluate our candidates and calculate the angular correlation function which we find best fitted by a power law, $\\omega(\\theta)=A_{w}\\theta^{-\\beta}$ with $A_{w}=15.4$ (with $\\theta$ in arcseconds), using a constrained slope of $\\beta=0.8$. Using a redshift distribution consistent with photometric models, we deproject this correlation function and find a comoving $r_{0}=11.4_{-1.9}^{+1.7}$ h$_{100}^{-1}$ Mpc in a $\\Omega_m=0.3$ flat $\\Lambda$ cosmology for $i_{AB}\\leq24.5$. This corresponds to a linear bias value of $b=8.1_{-2.6}^{+2.0}$ (assuming $\\sigma_{8}=0.9$). These data show a significantly larger $r_{0}$ and $b$ than previous studies at $z\\sim4$. We interpret this as evidence that the brightest LBGs have a larger bias than fainter ones, indicating a strong luminosity dependence for the m...

  15. Bright Ideas in Solar Energy

    E-Print Network [OSTI]

    Melville, Jo

    2014-01-01

    of the renewable energy pie in the very near future. In therenewable energies like solar power help us prepare for the future,

  16. Bright Ideas in Solar Energy

    E-Print Network [OSTI]

    Melville, Jo

    2014-01-01

    en.wikipedia.org/wiki/File:Solar_two.jpg 18 • B erkeley SMolten Nitrate Salt for Solar Energy Storage. Retrieved fromK. (2008). More-Efficient Solar Cells. Retrieved from

  17. Sensor Switch's Bright Manufacturing Future

    Broader source: Energy.gov [DOE]

    The switch helps with cost effective energy savings by turning off the lights when an occupancy sensor says the room is empty.

  18. Bright Ideas in Solar Energy

    E-Print Network [OSTI]

    Melville, Jo

    2014-01-01

    nuclear energy in this regard (Quiggin, 2008). With the help of carbon taxes and additional government subsidies,

  19. Bright Ideas in Solar Energy

    E-Print Network [OSTI]

    Melville, Jo

    2014-01-01

    www.popularmechanics.com/science/energy/solar-wind/3-clever-Molten Nitrate Salt for Solar Energy Storage. Retrieved fromKrisch, J. (2014). 3 Clever New Ways to Store Solar Energy.

  20. Bright Future NW Energy Coalition

    E-Print Network [OSTI]

    as coal or natural-gas generation. Wind and biomass nearly twice as many. Solar PV job potential is huge on natural gas. Energy Efficiency 3¢/kWh Energy Efficiency 3¢/kWh RPS 2020 10¢/kWh RPS 2020 10¢/kWh New Natural Gas 10¢/kWh Repower Existing Coal Plants 6¢/kWh New Renewables 2020-2050 10¢/kWh Repower

  1. Bright Future for CPV (Presentation)

    SciTech Connect (OSTI)

    Kurtz, S.

    2009-02-03

    Concentrator photovoltaics may play significant role in growth of solar electricity because of scalability. Need to take a bird?s eye view for the design and a worm?s eye view for diagnosis.

  2. Bright Ideas in Solar Energy

    E-Print Network [OSTI]

    Melville, Jo

    2014-01-01

    output of 300 megawatts, though Solar Thermal Energy (STE).Solar Thermal Energy is solar it is expected to reach 550This class of solar thermal energy collection, known as a

  3. Bright Ideas in Solar Energy

    E-Print Network [OSTI]

    Melville, Jo

    2014-01-01

    Molten Nitrate Salt for Solar Energy Storage. Retrieved fromNew Ways to Store Solar Energy. Retrieved from http://new-ways-to-store-solar-energy-16407404 Lenert, Andrej,

  4. COMET C/2011 W3 (LOVEJOY): ORBIT DETERMINATION, OUTBURSTS, DISINTEGRATION OF NUCLEUS, DUST-TAIL MORPHOLOGY, AND RELATIONSHIP TO NEW CLUSTER OF BRIGHT SUNGRAZERS

    SciTech Connect (OSTI)

    Sekanina, Zdenek; Chodas, Paul W. E-mail: Paul.W.Chodas@jpl.nasa.gov

    2012-10-01

    We describe the physical and orbital properties of C/2011 W3. After surviving perihelion passage, the comet was observed to undergo major physical changes. The permanent loss of the nuclear condensation and the formation of a narrow spine tail were observed first at Malargue, Argentina, on December 20 and then systematically at Siding Spring, Australia. The process of disintegration culminated with a terminal fragmentation event on December 17.6 UT. The postperihelion dust tail, observed for {approx}3 months, was the product of activity over <2 days. The nucleus' breakup and crumbling were probably caused by thermal stress due to the penetration of the intense heat pulse deep into the nucleus' interior after perihelion. The same mechanism may be responsible for cascading fragmentation of sungrazers at large heliocentric distances. The delayed response to the hostile environment in the solar corona is at odds with the rubble-pile model, since the residual mass of the nucleus, estimated at {approx}10{sup 12} g (equivalent to a sphere 150-200 m across) just before the terminal event, still possessed nontrivial cohesive strength. The high production rates of atomic oxygen, observed shortly after perihelion, are compatible with a subkilometer-sized nucleus. The spine tail-the product of the terminal fragmentation-was a synchronic feature, whose brightest part contained submillimeter-sized dust grains, released at velocities of up to 30 m s{sup -1}. The loss of the nuclear condensation prevented an accurate orbital-period determination by traditional techniques. Since the missing nucleus must have been located on the synchrone, whose orientation and sunward tip have been measured, we compute the astrometric positions of this missing nucleus as the coordinates of the points of intersection of the spine tail's axis with the lines of forced orbital-period variation, derived from the orbital solutions based on high-quality preperihelion astrometry from the ground. The resulting orbit gives 698 {+-} 2 yr for the osculating orbital period, showing that C/2011 W3 is the first member of the expected new, 21st-century cluster of bright Kreutz-system sungrazers, whose existence was predicted by these authors in 2007. From the spine tail's evolution, we determine that its measured tip, populated by dust particles 1-2 mm in diameter, receded antisunward from the computed position of the missing nucleus. The bizarre appearance of the comet's dust tail in images taken only hours after perihelion with the coronagraphs on board the SOHO and STEREO spacecraft is readily understood. The disconnection of the comet's head from the tail released before perihelion and an apparent activity attenuation near perihelion have a common cause-sublimation of all dust at heliocentric distances smaller than about 1.8 solar radii. The tail's brightness is strongly affected by forward scattering of sunlight by dust. From an initially broad range of particle sizes, the grains that were imaged the longest had a radiation-pressure parameter {beta} {approx_equal} 0.6, diagnostic of submicron-sized silicate grains and consistent with the existence of the dust-free zone around the Sun. The role and place of C/2011 W3 in the hierarchy of the Kreutz system and its genealogy via a 14th-century parent suggest that it is indirectly related to the celebrated sungrazer X/1106 C1, which, just as the first-generation parent of C/2011 W3, split from a common predecessor during the previous return to perihelion.

  5. Cavity Light-Emitting Diode for Durable, High-Brightness and High-Efficiency Lighting Applications: First Budget Period Technical Report

    SciTech Connect (OSTI)

    Yijian Shi

    2009-09-30

    A COLED device consists of a top electrode (anode) and a bottom electrode (cathode) separated by a thin dielectric layer. In this metal/dielectric stack, numerous small wells, or cavities, are etched through the top electrode and the dielectric layer. These cavities are subsequently filled with LEP molecules. When a voltage is applied between the top and bottom electrodes, holes (from the top electrode) and electrons (from the bottom electrode) are injected into the polymer. Light emission is generated upon recombination of holes and electrons within the polymer along the perimeters of cavities. Figure 1 compares the structures of the COLED and the traditional OLED. The existing COLED fabrication process flow is illustrated in Figure 2. A COLED can potentially be 5 times more efficient and can operate at as much as 100 times higher current density with much longer lifetime than an OLED. To fully realize these potential advantages, the COLED technology must overcome the following technical barriers, which were the technical focused points for Years 1 and 2 (Phase I) of this project: (1) Construct optimum thickness dielectric layer: In the traditional OLED structure, the optimal thickness of the LEP film is approximately 80-100 nm. In a COLED device, the effective LEP thickness roughly equals the thickness of the dielectric layer. Therefore, the optimal dielectric thickness for a COLED should also be roughly equal to 80-100 nm. Generally speaking, it is technically challenging to produce a defect-free dielectric layer at this thickness with high uniformity, especially over a large area. (2) Develop low-work-function cathode: A desired cathode should have a low work function that matches the lowest unoccupied molecular orbital (LUMO) level of the LEP molecules. This is usually achieved by using a low-work-function metal such as calcium, barium, lithium, or magnesium as the cathode. However, these metals are very vulnerable to oxygen and water. Since the cathode of the COLED will be exposed to air and processing chemicals during the COLED fabrication process, these low-work-function metals cannot be used directly in the COLED structure. Thus, new materials with low work function and better chemical stability are needed for the COLED cathode. (3) Increase active device area: Since photons are only generated from perimeters of the cavities, the actual active area in a COLED device is smaller than the device surface area. The cavity diameter and cavity spacing of the COLED devices previously produced at SRI by conventional photolithography processing are typically in the range of 3 to 7 {mu}m with an estimated active area of 2-3%. To achieve the same brightness of a traditional OLED at the same applied voltage, the active device area of a COLED should be at least 20% (1/5) of the device surface area, provided the COLED has 5 times higher EQE. This requires reducing the cavity diameter and cavity spacing to the sub-micrometer region, which can be achieved by electron-beam lithography or nanoimprint lithography. (4) Improve metal/polymer interfaces: The polymer/metal interfaces are critical issues to improve and optimize since they directly affect the effectiveness and balance of hole and electron injection, and consequently the device performance. Conventional approaches for improving a metal/polymer interface include deposition of a special interfacial material on the selected electrode surface or applying a proper surface treatment prior to deposition of the LEP. Since these approaches are generally nonselective to the cathode and anode, they cannot be directly adopted for COLED devices. Generally, the interface integration in current OLED technology still needs a better chemical approach. Hence, advanced methodology developed for the COLED technology as promoted in this project may be also suitable for other OLED devices.

  6. Planck cold clumps in the $\\lambda$ Orionis complex: I. Discovery of an extremely young Class 0 protostellar object and a proto-brown dwarf candidate in a bright rimmed clump PGCC G192.32-11.88

    E-Print Network [OSTI]

    Liu, Tie; Kim, Kee-Tae; Wu, Yuefang; Lee, Chang Won; Lee, Jeong-Eun; Tatematsu, Kenichi; Choi, Minho; Juvela, Mika; Thompson, Mark; Goldsmith, Paul F; Liu, Sheng-yuan; Naomi, Hirano; Koch, Patrick; Henkel, Christian; Sanhueza, Patricio; He, JinHua; Rivera-Ingraham, Alana; Wang, Ke; Cunningham, Maria R; Tang, Ya-Wen; Lai, Shih-Ping; Yuan, Jinghua; Li, Di; Fuller, Gary; Kang, Miju; Luong, Quang Nguyen; Liu, Hauyu Baobab; Ristorcelli, Isabelle; Yang, Ji; Xu, Ye; Hirota, Tomoya; Mardones, Diego; Qin, Sheng-Li; Chen, Huei-Ru; Kwon, Woojin; Meng, FanYi; Zhang, Huawei; Kim, Mi-Ryang; Yi, Hee-Weon

    2015-01-01

    We are performing a series of observations with ground-based telescopes toward Planck Galactic cold clumps (PGCCs) in the $\\lambda$ Orionis complex in order to systematically investigate the effects of stellar feedback. In the particular case of PGCC G192.32-11.88, we discovered an extremely young Class 0 protostellar object (G192N) and a proto-brown dwarf candidate (G192S). G192N and G192S are located in a gravitationally bound bright-rimmed clump. The velocity and temperature gradients seen in line emission of CO isotopologues indicate that PGCC G192.32-11.88 is externally heated and compressed. G192N probably has the lowest bolometric luminosity ($\\sim0.8$ L$_{\\sun}$) and accretion rate (6.3$\\times10^{-7}$ M$_{\\sun}$~yr$^{-1}$) when compared with other young Class 0 sources (e.g. PACS Bright Red sources (PBRs)) in the Orion complex. It has slightly larger internal luminosity ($0.21\\pm0.01$ L$_{\\sun}$) and outflow velocity ($\\sim$14 km~s$^{-1}$) than the predictions of first hydrostatic cores (FHSCs). G192N...

  7. THE LBT BOOeTES FIELD SURVEY. I. THE REST-FRAME ULTRAVIOLET AND NEAR-INFRARED LUMINOSITY FUNCTIONS AND CLUSTERING OF BRIGHT LYMAN BREAK GALAXIES AT Z {approx} 3

    SciTech Connect (OSTI)

    Bian Fuyan; Fan Xiaohui; Jiang Linhua; McGreer, Ian; Dave, Romeel [Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721 (United States); Dey, Arjun [National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719 (United States); Green, Richard F. [Large Binocular Telescope Observatory and Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721 (United States); Maiolino, Roberto [Cavendish Laboratory, University of Cambridge, 19 J. J. Thomson Ave., Cambridge CB3 0HE (United Kingdom); Walter, Fabian [Max-Planck-Institut fuer Astronomie, Koenigstuhl 17, D-69117 Heidelberg (Germany); Lee, Kyoung-Soo [Department of Physics, Purdue University, West Lafayette, IN 47906 (United States)

    2013-09-01

    We present a deep LBT/LBC U{sub spec}-band imaging survey (9 deg{sup 2}) covering the NOAO Booetes field. A total of 14,485 Lyman break galaxies (LBGs) at z {approx} 3 are selected, which are used to measure the rest-frame UV luminosity function (LF). The large sample size and survey area reduce the LF uncertainties due to Poisson statistics and cosmic variance by {>=}3 compared to previous studies. At the bright end, the LF shows excess power compared to the best-fit Schechter function, which can be attributed to the contribution of z {approx} 3 quasars. We compute the rest-frame near-infrared LF and stellar mass function (SMF) of z {approx} 3 LBGs based on the R-band and [4.5 {mu}m]-band flux relation. We investigate the evolution of the UV LFs and SMFs between z {approx} 7 and z {approx} 3, which supports a rising star formation history in the LBGs. We study the spatial correlation function of two bright LBG samples and estimate their average host halo mass. We find a tight relation between the host halo mass and the galaxy star formation rate (SFR), which follows the trend predicted by the baryonic accretion rate onto the halo, suggesting that the star formation in LBGs is fueled by baryonic accretion through the cosmic web. By comparing the SFRs with the total baryonic accretion rates, we find that cosmic star formation efficiency is about 5%-20% and it does not evolve significantly with redshift, halo mass, or galaxy luminosity.

  8. FPL's solar stars shine at new 500-acre array By SUSAN SALISBURY

    E-Print Network [OSTI]

    Fernandez, Eduardo

    , it is the world's largest and oldest. Building solar in a hurricane zone is different. "We had to temper the glass legislation allowed the company to build its 110 megawatts of solar. Since solar plants are more expensive like to build an additional 300 to 500 megawatts of solar. "We believe that solar is a great addition

  9. Formulation and Analysis of Compliant Grouted Waste Forms for SHINE Waste Streams

    SciTech Connect (OSTI)

    Ebert, William; Pereira, Candido; Heltemes, Thad A.; Youker, Amanda; Makarashvili, Vakhtang; Vandegrift, George F.

    2014-01-01

    Optional grouted waste forms were formulated for waste streams generated during the production of 99Mo to be compliant with low-level radioactive waste regulations. The amounts and dose rates of the various waste form materials that would be generated annually were estimated and used to determine the effects of various waste processing options, such as the of number irradiation cycles between uranium recovery operations, different combinations of waste streams, and removal of Pu, Cs, and Sr from waste streams for separate disposition (which is not evaluated in this report). These calculations indicate that Class C-compliant grouted waste forms can be produced for all waste streams. More frequent uranium recovery results in the generation of more chemical waste, but this is balanced by the fact that waste forms for those waste streams can accommodate higher waste loadings, such that similar amounts of grouted waste forms are required regardless of the recovery schedule. Similar amounts of grouted waste form are likewise needed for the individual and combined waste streams. Removing Pu, Cs, and Sr from waste streams lowers the waste form dose significantly at times beyond about 1 year after irradiation, which may benefit handling and transport. Although these calculations should be revised after experimentally optimizing the grout formulations and waste loadings, they provide initial guidance for process development.

  10. Welfare reform shines a light on work-force development challenges

    E-Print Network [OSTI]

    Campbell, David

    2000-01-01

    Butte, Kern, Sacramento and Tulare) lag behind the statewideMidwest or North Carolina. In Tulare County, where unemploy-and Salt Lake City. The Tulare County MOVE (More Opportunity

  11. NPR: Particles From The Edge Of Space Shine A Light On Fukushima

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    space. The Fukushima accident was broadcast around the world. On March 11, 2011, an earthquake and tsunami struck the plant, knocking out cooling in three working reactors. The...

  12. NPR: Particles From The Edge Of Space Shine A Light On Fukushima

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    the world. On March 11, 2011, an earthquake and tsunami struck the plant, knocking out cooling in three working reactors. The uranium fuel inside melted down. But nobody's quite...

  13. Why Disks Shine: the Transport of Angular Momentum in Hot, Thin Disks

    E-Print Network [OSTI]

    E. T. Vishniac

    1993-09-28

    I review recent work on the radial transport of angular momentum in ionized, Keplerian accretion disks. Proposed mechanisms include hydrodynamic and MHD local instabilities and long range effects mediated by wave transport. The most promising models incorporate the Velikhov-Chandrasekhar instability, caused by an instability of the magnetic field embedded in a differentially rotating disk. This has the important feature that the induced turbulent motions necessarily transport angular momentum outward. By contrast, convective modes may transport angular momentum in either direction. Combining the magnetic field instability with an $\\alpha-\\Omega$ dynamo driven by internal waves leads to a model in which the dimensionless viscosity scales as $(H/r)^{4/3}$. However, this model has a phenomenology which is quite different from the $\\alpha$ disk model. For example, an active disk implies some source of excitation for the internal waves. In binary systems with a mass ratio of order unity the most likely exciting mechanism is a parametric instability due to tidal forces. This implies that in systems where the accretion stream is intermittent, like MV Lyrae or TT Ari, epochs when the mass flow is absent or very small will be epochs in which the disk shrinks and becomes relatively inactive and dark. This model also implies that forced vertical mixing is important, even in convectively stable disks. I discuss various observational tests of this model and the focus of current theoretical work.

  14. Letting the Sun Shine on Solar Costs: An Empirical Investigation of Photovoltaic Cost Trends in California

    SciTech Connect (OSTI)

    Wiser, R.; Bolinger, M.; Cappers, P.; Margolis, R.

    2006-01-01

    This report provides a comprehensive analysis of grid-connected solar photovoltaic (PV) cost trends in California, which is by far the largest PV market in the United States. The findings of this work may help stakeholders to understand important trends in the California PV market, and policymakers to design more effective solar incentive programs--a particularly important objective given the recent announcement from the California Public Utilities Commission (CPUC) to establish an 11-year, $3.2 billion incentive program for customer-sited solar. The study statistically analyzes the installed cost of grid-connected PV systems funded by the state's two largest solar rebate programs, overseen by the California Energy Commission (CEC) [operating since 1998] and the CPUC [operating since 2001].

  15. Letting The Sun Shine On Solar Costs: An Empirical Investigation Of Photovoltaic Cost Trends In California

    E-Print Network [OSTI]

    Wiser, Ryan; Bolinger, Mark; Cappers, Peter; Margolis, Robert

    2006-01-01

    incentives have impacted pre-rebate installed costs, andMost prominent are capital cost rebates offered to PV systemtwo most significant current rebate programs are overseen by

  16. Letting The Sun Shine On Solar Costs: An Empirical Investigation Of Photovoltaic Cost Trends In California

    E-Print Network [OSTI]

    Wiser, Ryan; Bolinger, Mark; Cappers, Peter; Margolis, Robert

    2006-01-01

    infrastructure. Though PV cost reductions in California areworldwide. Data on PV capacity and costs are expresseddepth statistical analysis of PV system costs in California.

  17. Shine: A Step Towards Distributed Multi-Hop Visible Light Communication

    E-Print Network [OSTI]

    Kuzmanov, Georgi

    allows our platform to be connected to many experimental boards such as Arduino, Beaglebone, Raspberry Pi

  18. Shining Stars of Solar: Meet Three SunShot Postdoctoral Award...

    Broader source: Energy.gov (indexed) [DOE]

    Professor, Department of Chemistry, with a joint appointment in the Department of Chemical Engineering & Materials Science How would you describe your experience as an EERE...

  19. Letting The Sun Shine On Solar Costs: An Empirical Investigation Of Photovoltaic Cost Trends In California

    E-Print Network [OSTI]

    Wiser, Ryan; Bolinger, Mark; Cappers, Peter; Margolis, Robert

    2006-01-01

    Total Cost (CPUC) Module Cost Index (CEC, CPUC) CEC CPUC *an external index of worldwide module costs from Strategies

  20. Shining New Light on Protein Structure and Function thru Synchrotron Radiation Circular Dichroism (SRCD) Spectroscopy

    SciTech Connect (OSTI)

    Wallace,B.

    2005-01-01

    Circular dichroism (CD) spectroscopy has been employed for more than 50 years for the study of the structure and dynamics of proteins. It is now a workhorse of structural biology, finding applications in the determination of protein secondary structures, monitoring and deciphering protein folding, examining macromolecular interactions, and defining and quantitating protein-ligand binding. For the most part, CD studies have used laboratory-based instruments to measure electronic transitions in the far (190-250 nm), near ultraviolet (UV) (250-300 nm) and visible (> 400 nm) wavelength ranges, which have enabled studies of polypeptide backbones, aromatic amino acids and colored chromophores, respectively. Additional transitions exist at lower wavelengths in the vacuum ultraviolet (VUV) region (<190 nm); however, these transitions tend to be inaccessible to conventional CD instruments, due to the low intensity of their Xenon arc lamp light sources at wavelengths below190 nm. In 1980, the first synchrotron-based CD instruments were constructed, which took advantage of the high photon flux available from synchrotron light sources at these wavelengths. However, the technique of synchrotron radiation circular dichroism (SRCD) did not really take off until enabling studies had been done to show that additional data were obtainable for proteins in the VUV region, that these data were readily accessible with modern beamlines, and most importantly, that new applications of these data existed in structural molecular biology.

  1. EECBG Success Story: Shining Energy-Saving LEDs on Utah Starry...

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    LEDs across 14 rural communities. About 2,500 streetlights will be replaced and could save the town 20% to 50% on electricity bills. Learn more. Addthis Related Articles A...

  2. Letting The Sun Shine On Solar Costs: An Empirical Investigation Of Photovoltaic Cost Trends In California

    E-Print Network [OSTI]

    Wiser, Ryan; Bolinger, Mark; Cappers, Peter; Margolis, Robert

    2006-01-01

    in the largest solar market in the United States:CALIFORNIA’S SOLAR PROGRAMS California’s PV market is driven

  3. 2014 Winners of the Prudential Productivity Awards Florida State shines in annual productivity competition!

    E-Print Network [OSTI]

    but would also allow both schools to share the access license thereby lowering the cost per book productivity and promotes innovation to improve the delivery of state services while saving money for Florida taxpayers and businesses. This year, the competition attracted over 500 nominations for innovations

  4. August 4, 2006 Eco-lights shine new hope on `gorillas in the mist'

    E-Print Network [OSTI]

    Calgary, University of

    -developed solar cellular phone chargers. By training community members to manufacture the devices, the project and Sri Lankan refugee camps among new Light Up The World Foundation projects The cloud forests deep in the heart of Africa are the last refuge of the endangered mountain gorilla. Unfortunately, they are also one

  5. Photo of the Week: Rain or Shine, Preparing for the 2013 Hurricane Season |

    Broader source: Energy.gov (indexed) [DOE]

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of Natural GasAdjustmentsShirleyEnergyTher i nAandSummary Areas ofEnergy OnPeter B. LyonsDepartmentofa Future

  6. Shining Some Light on the World Cup's Efficiency Efforts | Department of

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Delicious Rank EERE:Financing Tool FitsProjectDataSecretary Moniz'sSeparation ProgramsFellowshipsShannonSherry

  7. Shining Stars of Solar: Meet Three SunShot Postdoctoral Award Recipients

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Delicious Rank EERE:Financing Tool FitsProjectDataSecretary Moniz'sSeparation ProgramsFellowshipsShannonSherryWho Are

  8. Fuel Cells Shine a Light on the Last Endeavour Space Shuttle Launch |

    Broader source: Energy.gov (indexed) [DOE]

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of Natural GasAdjustmentsShirleyEnergyTher i nA Guide to Tapping intoand David To:KamraSackPSTViewsafety,FactDepartment of

  9. Shining LUX on isospin-violating dark matter beyond leading order (Journal

    Office of Scientific and Technical Information (OSTI)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of NaturalDukeWakefieldSulfateSciTechtail. (Conference) |Janka,FerraraTechnologies

  10. Spins and Heat in Nanoscale Electronic Systems (SHINES) | U.S. DOE Office

    Office of Science (SC) Website

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power AdministrationRobust,Field-effectWorkingLosThe 26thIWalter H.4Office of Science (SC) Solid-StateOffice ofof

  11. EECBG Success Story: Light Shines on Better Budget for Glendale, Arizona |

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Delicious Rank EERE:FinancingPetroleum Based|Department of EnergyDepartment ofDepartment of Energy

  12. EECBG Success Story: Shining Energy-Saving LEDs on Utah Starry Nights |

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Delicious Rank EERE:FinancingPetroleum Based|Department of EnergyDepartmentDepartment ofResidential Energy

  13. NPR: Particles From The Edge Of Space Shine A Light On Fukushima

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity ofkandz-cm11 Outreach Home Room NewsInformationJessework usesof EnergyY-12 NationalNO FEAR Act Notice NONP UserNPR:

  14. Argonne Researchers Shine "Light" on Origins of Wind Turbine Bearing

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Delicious Rank EERE: Alternative FuelsofProgram:Y-12Power, Inc | Department ofMarketing, LLCorArea

  15. Desert Sunlight is Shining Example of How DOE Loan Guarantees Helped Launch

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Delicious Rank EERE: Alternative Fuels DataEnergy Webinar:IAbout Us|of EnergySmall Business Forum|Utility-scale

  16. Rise and Shine: Lighting the World with 10 Billion LED Bulbs | Department

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Delicious Rank EERE: Alternative Fuels Data CenterFinancialInvesting inServicesRecoveryRhode Island Schools

  17. Technical Assistance Application Bright Schools Program

    E-Print Network [OSTI]

    the energy cost and detailed usage information for each facility listed in Item 4 (above). Any past energy construction only: Schematic drawings (if available) 3. Project Description Type of assistance needed: Energy for proposed energy project New construction ­ evaluation of new facility Other Discuss your proposed project

  18. PublicationsmailagreementNo.40014024 Bright minds and

    E-Print Network [OSTI]

    Victoria, University of

    of protons at the highest energies ever reached by a particle accelerator.Times- Colonist story: http' remained in the common recreational and circulation space in front of the McPherson Library. Due a public meeting to enable all interested members of the campus community to receive accurate information

  19. Bright Center of the Universe Issue 3 

    E-Print Network [OSTI]

    Multiple Contributors

    1993-01-01

    Dark potential. The thought of him being more powerful than Vader if he turned raises interesting possibilities. I did find myself having to stop several time to figure out sentence structure, and typos are really distracting in a story like this... great love of language and control over words was evident in phrases like "My pure dark isvital now" and "his lightside litany stubbornly lectures over his pique." She captures these men with strokes ofcarefully chosen words and brings them to life...

  20. Solar Generation Has a Bright Future

    Broader source: Energy.gov [DOE]

    The amount of electricity the United States generates from solar power has started to grow rapidly and is projected to reach 18,000 megawatt hours per day in 2013.

  1. PublicationsmailagreementNo.40014024 Bright minds and

    E-Print Network [OSTI]

    Victoria, University of

    2009 The University of Victoria's community newspaper ring.uvic.ca Student's research helps promote eco-friendly

  2. PublicationsmailagreementNo.40014024 Bright minds and

    E-Print Network [OSTI]

    Victoria, University of

    @uvic.ca CLEAN ENERGY FutureGrid forum outlines BC's energy options Climate change is expected to boost the performance of BC Hydro's main reservoirs through increased water flows, and smart-grid technology promises sterilized animals, to be limited to areas within Ring Road. Keep up to date on the issue at http

  3. PublicationsmailagreementNo.40014024 Bright minds and

    E-Print Network [OSTI]

    Victoria, University of

    on the world through documentary film and photography: two things he is very pas- sionate about. He started p.3 CONVOCATION PROFILE Anthropology grad follows passion for film, photography & helping others to study documentary filmmaking and qualitative methodology at the University of Copenhagen. Tepleski

  4. Bright Center of the Universe Issue 8 

    E-Print Network [OSTI]

    Multiple Contributors

    1998-01-01

    This project established an in vivo method to identify and manipulate expression of markers of osteoarthritis (OA). Specifically, strategies that predictably induce joint inflammation to evaluate dietary methods of OA prevention in young horses have...

  5. Brightness masking is modulated by disparity structure

    E-Print Network [OSTI]

    Pelekanos, Vassilis; Ban, Hiroshi; Welchman, Andrew E.

    2015-03-24

    –O’Brien–Cornsweet effect are consistent with ‘filling-in’. Vision Research, 38(13), 2037–2046. De Weerd, P., Gattass, R., Desimone, R., & Ungerleider, L. G. (1995). Responses of cells in monkey visual cortex during perceptual filling-in of an artificial scotoma. Nature... stream_source_info Pelekanos et al 2015 Vision Research.pdf.txt stream_content_type text/plain stream_size 30883 Content-Encoding UTF-8 stream_name Pelekanos et al 2015 Vision Research.pdf.txt Content-Type text/plain; charset=UTF-8...

  6. PublicationsmailagreementNo.40014024 Bright minds and

    E-Print Network [OSTI]

    Victoria, University of

    of Canada (RSC), the country's senior national body of distinguished Canadian scholars. In the historyNt or former uVic faculty members who are fellows of the royal society of caNada SEPTEMBER 2010 The University person in three inVictoria is assisted by a UnitedWay-funded agency or program.Visit the website

  7. A Bright Year for Tidal Disruptions?

    E-Print Network [OSTI]

    Metzger, Brian D

    2015-01-01

    When a star is tidally disrupted by a supermassive black hole (BH), roughly half of its mass falls back to the BH at super-Eddington rates. Being tenuously gravitationally bound and unable to cool radiatively, only a small fraction f_in few 1e4 K, converting the emission to optical/near-UV wavelengths where photons more readily escape due to the lower opacity. This can explain the unexpectedly low and temporally constant effective temperatures of optically-discovered TDE flares. For BHs with relatively high masses M_BH > 1e7 M_sun the ejecta can become ionized at an earlier stage, or for a wider range of viewing angles, producing a TDE flare which is instead dominated by thermal X-ray emission. We predict total radiated energies consistent with those of observed TDE flares, and ejecta velocities that agree with the measured emission line widths. The peak optical luminosity for M_BH wind, possibly contributing to the unexpected dearth of o...

  8. Sustainable > DI BrightGreen January 2010

    E-Print Network [OSTI]

    of the publication is available from our webshop di.dk/english ISO 14001 ISO 14001 is an international standard FSC Controlled Wood certification ensures that responsible forest management has been used. Printed by

  9. The Future Looks Bright for Teraflop Computing

    SciTech Connect (OSTI)

    Farber, Rob

    2007-11-01

    Wouldn’t it be great to have a teraflop of computing power sitting in your lab, desktop workstation, or remote instrument server? Talk about simplifying workflows, eliminating competition for HPC resources, and allowing more scientists and technicians to get more work done! Well, the computer industry is marketing that capability now in the form of high-end video cards – and for a bargain price – with more and better technology on the market horizon. As the industry evolves to become more oriented toward multi-core and multi-threaded hardware; video card manufacturers are attempting to transition from a niche to multi-purpose market. One of the products currently getting attention is the Nvidia Tesla family of products based on the Tesla GPGPU (general purpose graphics processing unit). This card contains 128 processor computing core engines advertised as having the ability to deliver an aggregate 518 billion single-precision floating operations per second (518 Gflop), which is being introduced at a $1499 MSRP price-point. Nvidia also offers other commodity graphics cards, such as the GeForce 8800, which appear on paper to have roughly the same performance for roughly half the price – although with half the memory (768M vs the Tesla 1.5 GB). This highlights how the Tesla GPGPUs are essentially redesigned graphics cards (with no video capability, increased memory, and clock changes) that fit into PCI-Express slots in your motherboard. If you believe Nvidia’s claims, two Tesla cards will - for the right applications - turn your lab workstation into a teraflop capable supercomputer. Double-precision versions are projected for a late 2007 introduction with expected 2008 delivery. The Nvidia Tesla GPGPU is one step forward in the many-core revolution that is happening in the computer industry. Instead of making two or four processing cores available to the user, many-core processors offer tens or hundreds of processing cores. Many-core processors promise to provide very high performance-per-dollar and performance-per-watt for many computational workloads. Intel is working on their version of many-core processors but delivery dates appear to be several years in the future. Last year Intel made a large splash with their proof-of-concept teraflop 80-core chip, which they announced might be available sometime in 2011. Intel is also working on something similar to the Nvidia Tesla – codename Larrabee – which will perform in the teraflop range and has a release date of sometime around 2009 or 2010. Larrabee is supposed to have 16 – 24 cores and several nice features. Bottom line: A teraflop lab computer is feasible today as the programmable Nvidia GeForce 8 and Quadro family of graphics cards are available now, Tesla cards will be shipping, and exciting many-core architectures are on the horizon from a number of vendors. Definitely, the potential for parallel processing systems is huge, and GPGPUs certainly provide parallel processing, but are there enough applications out there to take them mainstream and make it more appealing to businesses other than just research firms? Only time will tell as more applications are developed to utilize this computational capability. Right now, programming is required. Recently Google purchased PeakStream, a firm that engaged in abstracting the task of running multiple threads to software with specific GPGPU applicability. However, Google is a visionary software company. Instrument vendors and much of the software industry are still in the early stages of the transition to multi-threaded many-core data processing. Applications that exploit the full potential of parallel processing systems, and GPGPUs in particular, really don’t exist in today’s market. The development of Matlab plug-ins is a very positive sign for the future of GPGPUs and is indicative of Nvidia’s sense of where the market is headed.

  10. Bright 30 THz Impulsive Solar Bursts

    E-Print Network [OSTI]

    Kaufmann, P; Marcon, R; Kudaka, A S; Cabezas, D P; Cassiano, M M; Francile, C; Fernandes, L O T; Ramirez, R F Hidalgo; Luoni, M; Marun, A; Pereyra, P; de Souza, R V

    2015-01-01

    Impulsive 30 THz continuum bursts have been recently observed in solar flares, utilizing small telescopes with a unique and relatively simple optical setup concept. The most intense burst was observed together with a GOES X2 class event on October 27, 2014, also detected at two sub-THz frequencies, RHESSI X-rays and SDO/HMI and EUV. It exhibits strikingly good correlation in time and in space with white light flare emission. It is likely that this association may prove to be very common. All three 30 THz events recently observed exhibited intense fluxes in the range of 104 solar flux units, considerably larger than those measured for the same events at microwave and sub-mm wavelengths. The 30 THz burst emission might be part of the same spectral burst component found at sub-THz frequencies. The 30 THz solar bursts open a promising new window for the study of flares at their origin

  11. ARM - Measurement - Longwave narrowband brightness temperature

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity ofkandz-cm11 Comments?govInstrumentsnoaacrnBarrow, Alaska Outreach Home Roomparticlecontent ARM Data Discoverynarrowband

  12. ARM - Measurement - Longwave spectral brightness temperature

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity ofkandz-cm11 Comments?govInstrumentsnoaacrnBarrow, Alaska Outreach Home Roomparticlecontent ARM Datanarrowband

  13. ARM - Measurement - Microwave narrowband brightness temperature

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity ofkandz-cm11 Comments?govInstrumentsnoaacrnBarrow, Alaska Outreach Home Roomparticlecontent ARM Datanarrowbandspectralflux

  14. Bright Automotive Inc | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIX E LISTStar Energy LLC JumpBiossence JumpJerseyEconomyBridger Valley Elec Assn,Automotive

  15. BrightPhase Energy | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION JEnvironmentalBowerbank, Maine: Energy ResourcesCounty, Texas:Brewer,Iowa:Brigantine, NewEnergy

  16. BrightSource | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION JEnvironmentalBowerbank, Maine: Energy ResourcesCounty, Texas:Brewer,Iowa:Brigantine,

  17. Blight-to-Bright | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIX ECoop IncIowaWisconsin:Pontiac Biomass Facility JumpII JumpBlackfeet

  18. Bright Power Inc | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIX ECoop IncIowaWisconsin:PontiacInformation Forest ServiceBridgewater2 Jump to:Power

  19. Bright three-band white light generated from CdSe/ZnSe quantum dot-assisted Sr{sub 3}SiO{sub 5}:Ce{sup 3+},Li{sup +}-based white light-emitting diode with high color rendering index

    SciTech Connect (OSTI)

    Jang, Ho Seong; Kwon, Byoung-Hwa; Jeon, Duk Young [Department of Materials Science and Engineering, Korea Advanced Institute of Science and Technology, 373-1, Guseong-dong, Yuseong-gu, Daejeon 305-701 (Korea, Republic of); Yang, Heesun [Department of Materials Science and Engineering, Hongik University, 72-1, Sangsu-dong, Mapo-gu, Seoul 121-791 (Korea, Republic of)

    2009-10-19

    In this study, bright three-band white light was generated from the CdSe/ZnSe quantum dot (QD)-assisted Sr{sub 3}SiO{sub 5}:Ce{sup 3+},Li{sup +}-based white light-emitting diode (WLED). The CdSe/ZnSe core/shell structure was confirmed by energy dispersive x-ray spectroscopy and x-ray photoelectron spectroscopy. The CdSe/ZnSe QDs showed high quantum efficiency (79%) and contributed to the high luminous efficiency ({eta}{sub L}) of the fabricated WLED. The WLED showed bright natural white with excellent color rendering property ({eta}{sub L}=26.8 lm/W, color temperature=6140 K, and color rendering index=85) and high stability against the increase in forward bias currents from 20 to 70 mA.

  20. Reducing stray light in Opto-Mechanical Systems Michael A. Gauvin and Edward R. Freniere

    E-Print Network [OSTI]

    Bechtold, Jill

    Reducing stray light in Opto-Mechanical Systems Michael A. Gauvin and Edward R. Freniere Lambda Research Corporation Abstract Almost every optical imaging system suffers from stray light or unwanted light. In an optical imaging system, stray light is caused by light from a bright source shining

  1. A review of "Rubens, Velazquez, and the King of Spain" by Aneta Georgievska-Shine and Larry Silver 

    E-Print Network [OSTI]

    Stoenescu, Livia

    2015-01-01

    . As part of this arsenal of bestial instincts, the love theme is predominately depicted by Rubens as a scene of the rape of either Ganymede or Europa (58). By divesting love of the enchanting dimension that the myth typically presents to the viewer...

  2. New Exclusion Limits for the Search of Scalar and Pseudoscalar Axion-Like Particles from " Light Shining Through a Wall "

    E-Print Network [OSTI]

    at the low energy frontier in the sub-eV range. The OSQAR photon regeneration experiment looks for "Light an 18.5 W continuous wave laser emitting in the green spectral regime (532 nm). No regenerated photons- ticle physics are not restricted to the high energy fron- tier. Therefore, researchers are increasingly

  3. Adapting High Brightness Relativistic Electron Beams for Ultrafast Science

    E-Print Network [OSTI]

    Scoby, Cheyne Matthew

    2012-01-01

    111 Transverse electron beamfemtosecond relativistic electron beams . . Organization offields of a relativistic electron beam. Phys. Rev. Lett. ,

  4. ITP Glass: A Clear Vision for a Bright Future

    Office of Energy Efficiency and Renewable Energy (EERE)

    This document presents perspectives on the glass industry's past, present and future, with special attention to competitive challenges now facing the industry and technological responses that will reinforce its continuing contribution...

  5. SC-RISE LECTURE SERIES BRIGHT HORIZONS IN SOLAR ENERGY

    E-Print Network [OSTI]

    are being developed including biomass, geothermal, hydropower, ocean thermal energy conversion, solar in technology development. The high capital costs typical of sustainable technologies coupled with the cyclic Time: 3:00 PM Location: A265 Bourns Hall Abstract: Low cost energy is critical to our lifestyles

  6. Wireless Power Transmission An Obscure History and a Bright Future?

    E-Print Network [OSTI]

    La Rosa, Andres H.

    the primary circuit energized by the oscillator (Century Magazine, June 1900). The building of a global transmission. Solar Power Satellite to Earth Terminal. Desert Solar Power Farm to Civilization. Earth Terminal solution to the coming power shortage . . . Solar Power Satellites (SPS) (4) #12;Solar Power Satellites (5

  7. High Average Brightness Photocathode Development for FEL Applications...

    Office of Scientific and Technical Information (OSTI)

    Laser Conference, FEL 2013; Manhattan, NY; 20130826 through 20130830 Research Org: Brookhaven National Laboratory (BNL) Sponsoring Org: USDOE SC OFFICE OF SCIENCE (SC) Country of...

  8. The Problem Conventional office lighting typically consists of bright fluo-

    E-Print Network [OSTI]

    by delamping--result in lower power consump- tion. The PLS, which features light-emitting diode (LED lighting is reduced and three light-emitting diode (LED) task lights (two desk lamps and one undercabinet

  9. Cree Sets New Benchmarks for LED Efficacy and Brightness

    Broader source: Energy.gov [DOE]

    Cree has successfully created a cool white LED prototype that delivers 107 lm/W at 350mA. This achievement builds on the Cree EZBright® LED chip platform, developed in part with prior funding support from DOE. Cree made the prototype LED under their DOE project focused on developing LED chips incorporating photonic crystal elements for improved light extraction and novel package technology for higher down-conversion efficiency compared to conventional LEDs. Based on a 1 millimeter-square chip, the new prototype LED produces white light with a CCT of 5500K and a CRI of 73. Integration of four of these prototype LEDs can produce luminous flux of more than 450 lumens.

  10. INTRODUCTION Carotenoid pigments are responsible for many bright yellow, orange

    E-Print Network [OSTI]

    Bortolotti, Gary R.

    Cinegéticos, IREC (CSIC, UCLM, JCCM), Ciudad Real, Spain, 2 School of Biological Sciences, University

  11. Micro moon versus macro moon: Brightness and size

    E-Print Network [OSTI]

    Agrawal, Dulli Chandra

    2015-01-01

    The moon, moonlight, phases of the moon and its relatively simple recurring cycle has been of interest since time immemorial to the human beings, navigators, astronomers and astrologers. The fact that its orbit is elliptical as well its plane is inclined with the plane of rotation of the earth gives rise to new moon to full moon and solar and lunar eclipses. During the phase of the full moon, the luminous flux and its apparent size will depend on its distance from the earth. In case it is at farthest point known as lunar apogee causes smallest full moon or micro full moon and if it is closest to us termed as lunar perigee will result in macro full moon, also known as super moon, a term coined by astrologer Richard Nolle in 1979. The theoretical expressions for the lunar luminous fluxes on the earth representing the power of lunar light the earth intercepts in the direction normal to the incidence over an area of one square meter are derived for two extreme positions lunar apogee and lunar perigee. The express...

  12. New water masers in Seyfert and FIR bright galaxies. II

    E-Print Network [OSTI]

    P. Castangia; A. Tarchi; C. Henkel; K. M. Menten

    2007-12-05

    Recently, a relationship between the water maser detection rate and far infrared (FIR) flux density has been found as a result of a 22 GHz maser survey in a sample comprised of northern galaxies with 100 micron flux density > 50 Jy and a declination >-30 degrees. The survey has been extended toward galaxies with lower FIR flux densities in order to confirm this correlation and to discover additional maser sources for relevant follow-up interferometric studies. A sample of 41 galaxies with 30 Jy -30 degrees was observed with the 100-m telescope at Effelsberg in a search for the 22 GHz water vapor line. The average 3-sigma noise level of the survey is 40 mJy for a 1 km/s channel, corresponding to a detection threshold for the isotropic maser luminosity of about 0.5 solar luminosities at a distance of 25 Mpc. Two detections are reported: a megamaser with an isotropic luminosity of approximately 35 solar luminosities in the Seyfert/HII galaxy NGC613 and a kilomaser of approximately 1 solar luminosity in the merger system NGC520.[abridged

  13. Adapting High Brightness Relativistic Electron Beams for Ultrafast Science

    E-Print Network [OSTI]

    Scoby, Cheyne Matthew

    2012-01-01

    Hastings, F. M. Rudakov, D. H. Dowell, J. F. Schmerge, J. D.F. -J. Decker, Y. Ding, D. Dowell, P. Emma, J. Frisch, Z.Brachmann, F. -J. Decker, D. Dowell, P. Emma, J. Frisch, S.

  14. VARIATIONAL MODELS FOR IMAGE COLORIZATION VIA CHROMATICITY AND BRIGHTNESS DECOMPOSITION

    E-Print Network [OSTI]

    regions with color are given. We propose a couple of variational models using chromaticity color component algorithm using weighted distance image blending technique is studied in [49]. The authors utilize Dijkstra, and YCbCr (Luminance,two color-difference components) widely used for digital video; nonlinear color

  15. Adapting High Brightness Relativistic Electron Beams for Ultrafast Science

    E-Print Network [OSTI]

    Scoby, Cheyne Matthew

    2012-01-01

    LCLSprobe experiments at the lcls. Opt. Express, 18(17):17620–probe experiments at the LCLS. Optics express, 18(17):17620–

  16. Coiled tubing technology advances to a bright future

    SciTech Connect (OSTI)

    Ghiselin, R.

    1998-07-01

    This supplement contains six short articles on coiled tubing, its advantages, performance, and materials. The articles are: Coiled Tubing--On the Brink of a New Millennium; CT Advances Promise a Broad, Dynamic Future; Performance, Safety and Cost Make the Case for HPCT; Fast and Accurate, CTD Helps Drillers Hit Their Targets; Composite Tubing Rapidly Proves Advantages in the Field; and People and Performance are Key to Coiled Tubing Growth.

  17. Phosphorescent organic light emitting diodes with high efficiency and brightness

    DOE Patents [OSTI]

    Forrest, Stephen R; Zhang, Yifan

    2015-11-12

    An organic light emitting device including a) an anode; b) a cathode; and c) an emissive layer disposed between the anode and the cathode, the emissive layer comprising an organic host compound and a phosphorescent compound exhibiting a Stokes Shift overlap greater than 0.3 eV. The organic light emitting device may further include a hole transport layer disposed between the emissive layer and the anode; and an electron transport layer disposed between the emissive layer and the cathode. In some embodiments, the phosphorescent compound exhibits a phosphorescent lifetime of less than 10 .mu.s. In some embodiments, the concentration of the phosphorescent compound ranges from 0.5 wt. % to 10 wt. %.

  18. Dust properties of UV bright galaxies at z ~ 2

    E-Print Network [OSTI]

    S. Noll; D. Pierini

    2005-08-25

    We investigate the properties of the extinction curve in the rest-frame UV for a sample of 34 UV-luminous galaxies at 2 energy distribution is adopted; its sensitivity to properties of the stellar populations or of dust attenuation is established with the use of combined stellar population and radiative transfer models. The distribution of the z ~ 2 UV-luminous FDF galaxies in several diagnostic diagrams shows that their extinction curves range between those typical of the Small and Large Magellanic Clouds (SMC and LMC, respectively). For the majority of strongly reddened objects having a UV continuum slope beta > -0.4 a significant 2175 A absorption feature is inferred, indicating an LMC-like extinction curve. On the other hand, the UV continua of the least reddened objects are mostly consistent with SMC-like extinction curves, lacking a significant 2175 A bump, as for the Calzetti et al. sample of local starbursts. Furthermore, the most opaque (beta ~ 0) UV-luminous galaxies tend to be among the most metal rich, most massive, and largest systems at z ~ 2. The presence of the UV bump does not seem to depend on the total metallicity, as given by the equivalent width (EW) of the C IV doublet. Conversely, it seems to be associated with large EWs of prominent interstellar low-ionisation absorption lines, suggesting a link between the strength of the UV bump and the topology of the interstellar medium of the most evolved UV-luminous, massive galaxies at z ~ 2.

  19. RESEARCH Open Access Directed evolution of bright mutants of an

    E-Print Network [OSTI]

    Schroeder, Charles

    saturation mutagenesis to isolate brighter variants of a flavin-binding fluorescent protein, which is a first], a wide range of emission wavelengths [11,12], enhanced thermal tolerance [13], and improved efficiency of Förster resonance energy transfer (FRET) [14]. However, the available palette of GFP-based fluor- escent

  20. NREL Success Stories - SkyFuel Partnership Reflects Bright Future

    ScienceCinema (OSTI)

    Jorgensen, Gary; Gee, Randy

    2013-05-29

    NREL Scientists and SkyFuel share a story about how their partnership has resulted in a revolutionary concentrating solar power technology ReflecTech Mirror Film.

  1. Bright vigorous winds as signposts of supermassive black hole birth

    E-Print Network [OSTI]

    Fiacconi, Davide

    2015-01-01

    The formation of supermassive black holes is still an outstanding question. In the quasi-star scenario, black hole seeds experience an initial super-Eddington growth, that in less than a million years may leave a $10^4-10^5$ M$_{\\odot}$ black hole at the centre of a protogalaxy at $z \\sim 20-10$. Super-Eddington accretion, however, may be accompanied by vigorous mass loss that can limit the amount of mass that reaches the black hole. In this paper, we critically assess the impact of radiative driven winds, launched from the surface of the massive envelopes from which the black hole accretes. Solving the full wind equations coupled with the hydrostatic structure of the envelope, we find mass outflows with rates between a few tens and $10^4$ M$_{\\odot}$ yr$^{-1}$, mainly powered by advection luminosity within the outflow. We therefore confirm the claim by Dotan, Rossi & Shaviv (2011) that mass losses can severely affect the black hole seed early growth within a quasi-star. In particular, seeds with mass $>1...

  2. Bright Ideas for Chemical Biology Luke D. Lavis,

    E-Print Network [OSTI]

    Nielsen, Steven O.

    product quinine (1), an im- portant compound for both medicinal and organic chemistry (15). The visible emission from an aqueous quinine solution was reported by Herschel in 1845 (16). Stokes showed that this phenomenon was due to the absorption and then emission of light by quinine and coined the term "fluorescence

  3. Bright Lights and Even Brighter Ideas | Department of Energy

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    which could one day be used to create "greener" and more efficient paints, fiber optics and solar cells. In this photo, the iridescent scales of an emerald-patched...

  4. Adapting High Brightness Relativistic Electron Beams for Ultrafast Science

    E-Print Network [OSTI]

    Scoby, Cheyne Matthew

    2012-01-01

    field lines as the electromagnetic pulse travels into thepulses 117 Femtosecond probing of transient electromagneticlaser pulses and the evolution of electromagnetic fields in

  5. Bright-White Beetle Scales Optimise Multiple Scattering of Light

    E-Print Network [OSTI]

    Burresi, Matteo; Cortese, Lorenzo; Pattelli, Lorenzo; Kolle, Mathias; Vukusic, Peter; Wiersma, Diederik S.; Steiner, Ullrich; Vignolini, Silvia

    2014-08-15

    -resolved measurements were performed by overlapping the probe pulse with a gate pulse at 1550 nm from a parametric oscillator on a b-Barium Borate (BBO) crystal in time, space and in reciprocal space. Electromagnetic radiation with a frequency equal to the sum... the time-of-flight of a light pulse through single scales. These measure- ments separate the ‘early’ light, which undergoes only few scattering events, from the ‘late’ light, characteristic for multiple scattering25,26. An ultra-fast time...

  6. High brightness symmetric emittance rf photoinjector preliminary design report

    SciTech Connect (OSTI)

    Colby, E.R.; Ostiguy, J.F. [Fermi National Accelerator Lab., Batavia, IL (United States); Rosenzweig, J.B. [California Univ., Los Angeles, CA (United States). Dept. of Physics

    1994-08-01

    A preliminary design for a high bunch charge (8 nC), low emittance (< 20 mm-mr) radiofrequency electron photoinjector matched to the requirements of the Tesla Test Facility is presented. A 1.5 cell iris coupled {pi}mode structure with high average accelerating gradient is chosen for its high shunt impedance, simplicity, and ability to accommodate an externally mounted solenoid for simultaneous beam divergence control and emittance compensation. Beam optics are optimized for an overall injector consisting of the electron gun followed by one linac capture section, a dipole chicane for magnetic bunch compression to achieve a bunch length corresponding to {sigma}{sub z} = 1 mm. Electrical and beam dynamical aspects of the photoinjector design are presented. A description of the proposed experimental program is included.

  7. NanoBright Technologies Pte Ltd | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QAsource History ViewMayo, Maryland:NPI Ventures Ltd Jump to: navigation, search59Naknek,C Jump to:

  8. BrightView Systems Ltd | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIX E LISTStar Energy LLC JumpBiossence JumpJerseyEconomyBridger Valley Elec

  9. A Bright Idea: New Efficiency Standards for Incandescent and Fluorescent

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Delicious Rank EERE:Financing ToolInternationalReportOffice | DepartmentVery1, in: Statement of Dr.26Former|A

  10. Posters Comparisons of Brightness Temperature Measurements and Calculations Obtained

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass mapSpeedingProgram Guidelines This document outlines the majorL.Posters9 Posters1

  11. BrightPath Energy LLC | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIX ECoop IncIowaWisconsin:PontiacInformation Forest ServiceBridgewater2 Jump

  12. Brightness and Coherence of Synchrotron Radiation and FELs (Conference) |

    Office of Scientific and Technical Information (OSTI)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of NaturalDukeWakefieldSulfate Reducing Bacteria (Technical Report) |concentration of Ti (Journal Article) |SciTech Connect

  13. Brightness and Coherence of Synchrotron Radiation and FELs (Conference) |

    Office of Scientific and Technical Information (OSTI)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of NaturalDukeWakefieldSulfate Reducing Bacteria (Technical Report) |concentration of Ti (Journal Article) |SciTech

  14. High Average Brightness Photocathode Development for FEL Applications

    Office of Scientific and Technical Information (OSTI)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of NaturalDukeWakefieldSulfate Reducing(Journal Article)lasers (Journal Article) |different|(Journal

  15. High Average Brightness Photocathode Development for FEL Applications

    Office of Scientific and Technical Information (OSTI)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of NaturalDukeWakefieldSulfate Reducing(Journal Article)lasers (Journal Article) |different|(Journal(Conference) | SciTech

  16. Updated Spitzer emission spectroscopy of bright transiting hot Jupiter HD

    Office of Scientific and Technical Information (OSTI)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of NaturalDukeWakefieldSulfateSciTechtail.Theory of rare Kaonfor Direct Measurement of Plutonium in

  17. Department Announces Loan Guarantee for BrightSource Energy Inc. |

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Delicious Rank EERE:FinancingPetroleum Based| Department8, 20153Daniel BoffDepartmentbeginsGeothermalDemonstrations

  18. Bright Lights From Dark Places | Department of Energy

    Broader source: Energy.gov (indexed) [DOE]

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of Natural GasAdjustmentsShirley Ann JacksonDepartment of EnergyResearchers atDayWhenBethanyOnAristides Patrinos, DeputyCharles

  19. Bright Lights and Even Brighter Ideas | Department of Energy

    Broader source: Energy.gov (indexed) [DOE]

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of Natural GasAdjustmentsShirley Ann JacksonDepartment of EnergyResearchers atDayWhenBethanyOnAristides Patrinos,

  20. Bright Skies Ahead for Moapa | Department of Energy

    Broader source: Energy.gov (indexed) [DOE]

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of Natural GasAdjustmentsShirley Ann JacksonDepartment|Marketing, LLC |Energycurrently providesDepartment ofAwardsTo jumpIn

  1. SAFETY, GUIDELINES & ETIQUETTE Most programs will be held rain or shine. We assume you will come unless we hear from you.

    E-Print Network [OSTI]

    Lawrence, Deborah

    to use the recycling bins (located in Picnic Area and at Peetwood Pavilion) for plastic, glass, and cans. Reduce, Reuse, and RECYCLE! #12;

  2. Tracking the Sun: The Installed Cost of Photovoltaics in the U.S. from 1998-2007

    E-Print Network [OSTI]

    Wiser, Ryan

    2009-01-01

    the Sun Shine on Solar Costs: An Empirical Investigation ofthe Sun Shine on Solar Costs: An Empirical Investigation ofthe Sun Shine on Solar Costs: An Empirical Investigation of

  3. Growing Cutting-edge X-ray Optics

    ScienceCinema (OSTI)

    Ray Conley

    2013-07-17

    Ever imagined that an Xbox controller could help open a window into a world spanning just one billionth of a meter? Brookhaven Lab's Ray Conley grows cutting-edge optics called multilayer Laue lenses (MLL) one atomic layer at a time to focus high-energy x-rays to within a single nanometer. To achieve this focusing feat, Ray uses a massive, custom-built atomic deposition device, an array of computers, and a trusty Xbox controller. These lenses will be deployed at the Lab's National Synchrotron Light Source II, due to begin shining super-bright light on pressing scientific puzzles in 2015

  4. News Item

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright Future for Protein

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    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright Future for ProteinNewly

  6. News Item

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright Future for ProteinNewlyA

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright Future for

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright Future forDiscovery of

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright Future forDiscovery of4

  10. News Item

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright Future forDiscovery

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright Future forDiscovery4

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright Future

  13. News Item

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright Future4 Weber-Bargioni

  14. News Item

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright Future4

  15. News Item

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright Future4Organic Facility

  16. News Item

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright Future4Organic FacilityA

  17. News Item

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright Future4Organic

  18. News Item

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright Future4OrganicXiang Zhang

  19. News Item

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright Future4OrganicXiang

  20. News Item

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright

  1. News Item

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright4 Toyota's Battery

  2. News Item

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright4 Toyota's

  3. News Item

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright4 Toyota'sShaping the

  4. News Item

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright4 Toyota'sShaping

  5. News Item

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright4

  6. News Item

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright4Foundry Helps Capture

  7. News Item

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright4Foundry Helps

  8. News Item

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright4Foundry HelpsOn the Road

  9. News Item

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright4Foundry HelpsOn the

  10. News Item

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright4Foundry HelpsOn

  11. News Item

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright4Foundry HelpsOnDispelling

  12. News Item

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright4Foundry

  13. News Item

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright4FoundryStudy Reveals

  14. News Item

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright4FoundryStudy

  15. News Item

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shinesSolarNew scholarshipThree Foundry ScientistsBright4FoundryStudyOutsmarting

  16. Field trials identify more native plants suited to urban landscaping

    E-Print Network [OSTI]

    Reid, S. Karrie; Oki, Lorence R

    2008-01-01

    developed All-Stars plant lists to help visitors identifyat arboretum plant sales. From the All-Stars list as well as

  17. Solid-State Lighting with High Brightness, High Efficiency, and Low Cost

    E-Print Network [OSTI]

    Gilchrist, James F.

    -emitting diode (LED) is the most popular technique due to its advantages of small volume, long lifetime, high reliability, low power consumption, and nonpollution. The progress in solid-state lighting has been driven to the progress in visible InGaN-based light-emitting diodes (LEDs) based on III-nitride based semiconductor

  18. A Calibrated Measurement of the Near-IR Continuum Sky Brightness Using Magellan/FIRE

    E-Print Network [OSTI]

    Sullivan, Peter William

    We characterize the near-IR sky background from 308 observations with the Folded-port InfraRed Echellette (FIRE) spectrograph at Magellan. A subset of 105 observations selected to minimize lunar and thermal effects gives ...

  19. Spatial resolution enhancement of terrestrial features using deconvolved SSM/K microwave brightness temperatures

    SciTech Connect (OSTI)

    Farrar, M.R.; Smith, E.A. (Dept. of Meteorology and Supercomputer Computations Research Inst., Florida State Univ., Tallahassee, FL (US))

    1992-03-01

    In this paper a method for enhancing the 19, 22 and 37 GHz measurements of the SSM/I (Special Sensor Microwave/Imager) to the spatial resolution and sampling density of the high resolution 85-GHz channel is presented. An objective technique for specifying the tuning parameter, which balances the tradeoff between resolution and noise, is developed in terms of maximizing cross-channel correlations. Various validation procedures are performed to demonstrate the effectiveness of the method, which hopefully will provide researchers with a valuable tool in multispectral applications of satellite radiometer data.

  20. New family of tiny crystals glow bright in LED lights | ornl...

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    Minuscule crystals that glow different colors may be the missing ingredient for white LED lighting that illuminates homes and offices as effectively as natural sunlight....

  1. Sleep, mood, and circadian responses to bright green light during sleep

    E-Print Network [OSTI]

    Grandner, Michael Andrew

    2007-01-01

    mouth or teeth,” “nose or throat,” “chest,” “heart,” “stomach or abdomen,” “bowel movements,” “appetite,” “urination,” “genitals or sexual functioning,” “muscles,

  2. Titan's bright spots: Multiband spectroscopic measurement of surface diversity and hazes

    E-Print Network [OSTI]

    Adamkovics, Mate

    in a methane- based meteorological cycle that is similar to the Earth's hydrological cycle [Toon et al., 1988 initiates a series of chemical reactions that result in the formation of condensible hydrocarbons aerosols settle into the tropo- sphere, they can serve as condensation nuclei for Titan's methane

  3. Nanoscale optical positioning of single quantum dots for bright and pure single-photon emission

    E-Print Network [OSTI]

    Luca Sapienza; Marcelo Davanco; Antonio Badolato; Kartik Srinivasan

    2015-08-05

    Self-assembled, epitaxially-grown InAs/GaAs quantum dots are promising semiconductor quantum emitters that can be integrated on a chip for a variety of photonic quantum information science applications. However, self-assembled growth results in an essentially random in-plane spatial distribution of quantum dots, presenting a challenge in creating devices that exploit the strong interaction of single quantum dots with highly confined optical modes. Here, we present a photoluminescence imaging approach for locating single quantum dots with respect to alignment features with an average position uncertainty technology for the creation of optimized single quantum dot devices. To that end, we create quantum dot single-photon sources, based on a circular Bragg grating geometry, that simultaneously exhibit high collection efficiency (48 % +/- 5 % into a 0.4 numerical aperture lens, close to the theoretically predicted value of 50 %), low multiphoton probability (g(2)(0) <1 %), and a significant Purcell enhancement factor (~ 3).

  4. Sparkling extreme-ultraviolet bright dots observed with Hi-C...

    Office of Scientific and Technical Information (OSTI)

    Technial Information About OSTI Mission Organization Chart Achievements Alliances OSTI History Feedback DOE STI Program Scientific and Technical Information Program (STIP)...

  5. UBV stellar photometry of bright stars in GC M5. II. Physical parameters of HB stars

    E-Print Network [OSTI]

    P. V. Baev; H. Markov; N. Spassova

    2001-08-09

    The physical parameters of the stars in the central region of the globular cluster M5 (NGC 5904) were determined from UBV photometry using Kurucz (1992) synthetic flux distributions and some empirical relations. It is found that the bluest horizontal branch stars have higher luminosities than predicted by canonical zero-age horizontal branch models. Parameters of the mass distribution on the HB stars are determined. It is shown that the gap in the blue HB previously reported (Markov et al. 1999) is probably a statistical fluctuation.

  6. Evolution of bright star-forming galaxies in the first billion years 

    E-Print Network [OSTI]

    Bowler, Rebecca Alison Andrews

    2015-07-01

    , and that the stars can be effectively removed by fitting standard stellar spectra to the observed photometry. The galaxy surface density in the UltraVISTA/COSMOS field exceeds that in the UDS/SXDS by a factor of ?1.4, indicating strong cosmic variance between the two...

  7. The Formation of Submillimetre-Bright Galaxies from Gas Infall over a Billion Years

    E-Print Network [OSTI]

    Narayanan, Desika; Feldmann, Robert; Robitaille, Thomas; Hopkins, Philip; Thompson, Robert; Hayward, Christopher; Ball, David; Faucher-Giguere, Claude-Andre; Keres, Dusan

    2015-01-01

    Submillimetre-luminous galaxies at high-redshift are the most luminous, heavily star-forming galaxies in the Universe, and are characterised by prodigious emission in the far-infrared at 850 microns (S850 > 5 mJy). They reside in halos ~ 10^13Msun, have low gas fractions compared to main sequence disks at a comparable redshift, trace complex environments, and are not easily observable at optical wavelengths. Their physical origin remains unclear. Simulations have been able to form galaxies with the requisite luminosities, but have otherwise been unable to simultaneously match the stellar masses, star formation rates, gas fractions and environments. Here we report a cosmological hydrodynamic galaxy formation simulation that is able to form a submillimetre galaxy which simultaneously satisfies the broad range of observed physical constraints. We find that groups of galaxies residing in massive dark matter halos have rising star formation histories that peak at collective rates ~ 500-1000 Msun/yr at z=2-3, by wh...

  8. On the Nature of X-ray Surface Brightness Fluctuations in M87

    E-Print Network [OSTI]

    Arévalo, P; Zhuravleva, I; Forman, W R; Jones, C

    2015-01-01

    X-ray images of galaxy clusters and gas-rich elliptical galaxies show a wealth of small-scale features which reflect fluctuations in density and/or temperature of the intra-cluster medium. In this paper we study these fluctuations in M87/Virgo, to establish whether sound waves/shocks, bubbles or uplifted cold gas dominate the structure. We exploit the strong dependence of the emissivity on density and temperature in different energy bands to distinguish between these processes. Using simulations we demonstrate that our analysis recovers the leading type of fluctuation even in the presence of projection effects and temperature gradients. We confirm the isobaric nature of cool filaments of gas entrained by buoyantly rising bubbles, extending to 7' to the east and south-west, and the adiabatic nature of the weak shocks at 40" and 3' from the center. For features of 5--10 kpc, we show that the central 4'x 4' region is dominated by cool structures in pressure equilibrium with the ambient hotter gas while up to 30 ...

  9. Many patients with spinal cord inju-ries didn't have a bright future in

    E-Print Network [OSTI]

    Bedwell, David M.

    prices doesn't change the need to aggressively pursue alternative fuel sources, says UAB researcher Fouad-powered transit bus that is expected to be operational in Birmingham next summer. The Birmingham Hydrogen Fuel receive hands-on experience Diana Marin, an occupational therapist in the Spain Rehabilitation Center

  10. High-Throughput, High-Precision Hot Testing Tool for High-Brightness...

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    Diode Testing Lead Performer: KLA-Tencor Corporation - Milpitas, CA Partners: Ocean Optics - Dunedin, FL DOE Total Funding: 3,994,729 Cost Share: 4,626,422 Project Term: 815...

  11. Inverse Free Electron Laser Interactions with Sub-Picosecond High Brightness Electron Beams

    E-Print Network [OSTI]

    Moody, Joshua Timothy

    2014-01-01

    the OAP chamber, goes through a periscope that preserves itsthe OAP chamber, goes through a periscope that preserves itsPolarization Preserving Periscope Periscope with Window 500

  12. Lecture 2. Instrumentation Is the Sun very bright so we can never be photon hungry?

    E-Print Network [OSTI]

    through 60cm telescope; exposure time 1ms. "3.0"3.0 %1efficiency,A10,A5000 m Results: Only 400 photons

  13. Design, conditioning, and performance of a high voltage, high brightness dc photoelectron gun with variable gap

    SciTech Connect (OSTI)

    Maxson, Jared; Bazarov, Ivan; Dunham, Bruce; Dobbins, John; Liu, Xianghong; Smolenski, Karl

    2014-09-15

    A new high voltage photoemission gun has been constructed at Cornell University which features a segmented insulator and a movable anode, allowing the cathode-anode gap to be adjusted. In this work, we describe the gun's overall mechanical and high voltage design, the surface preparation of components, as well as the clean construction methods. We present high voltage conditioning data using a 50 mm cathode-anode gap, in which the conditioning voltage exceeds 500 kV, as well as at smaller gaps. Finally, we present simulated emittance results obtained from a genetic optimization scheme using voltage values based on the conditioning data. These results indicate that for charges up to 100 pC, a 30 mm gap at 400 kV has equal or smaller 100% emittance than a 50 mm gap at 450 kV, and also a smaller core emittance, when placed as the source for the Cornell energy recovery linac photoinjector with bunch length constrained to be <3 ps rms. For 100 pC up to 0.5 nC charges, the 50 mm gap has larger core emittance than the 30 mm gap, but conversely smaller 100% emittance.

  14. Overview of Recent Progres on High Repetition Rate, High Brightness Electron Guns

    E-Print Network [OSTI]

    Sannibale, F.

    2014-01-01

    Ceramic DC Electron Gun for the Jefferson Laboratory FEL.ALICE (ERLP) DC Photoinjector Gun Commissioning, Proc. ofa 500-kV Photo- cathode DC Gun for the ERL Light Sources in

  15. The unexpectedly bright comet C/2012 F6 (Lemmon) unveiled at near-infrared wavelengths

    SciTech Connect (OSTI)

    Paganini, Lucas; DiSanti, Michael A.; Mumma, Michael J.; Villanueva, Geronimo L.; Bonev, Boncho P.; Keane, Jacqueline V.; Meech, Karen J.; Gibb, Erika L.; Boehnhardt, Hermann

    2014-01-01

    We acquired near-infrared spectra of the Oort cloud comet C/2012 F6 (Lemmon) at three different heliocentric distances (R {sub h}) during the comet's 2013 perihelion passage, providing a comprehensive measure of the outgassing behavior of parent volatiles and cosmogonic indicators. Our observations were performed pre-perihelion at R {sub h} = 1.2 AU with CRIRES (on 2013 February 2 and 4), and post-perihelion at R {sub h} = 0.75 AU with CSHELL (on March 31 and April 1) and R {sub h} = 1.74 AU with NIRSPEC (on June 20). We detected 10 volatile species (H{sub 2}O, OH* prompt emission, C{sub 2}H{sub 6}, CH{sub 3}OH, H{sub 2}CO, HCN, CO, CH{sub 4}, NH{sub 3}, and NH{sub 2}), and obtained upper limits for two others (C{sub 2}H{sub 2} and HDO). One-dimensional spatial profiles displayed different distributions for some volatiles, confirming either the existence of polar and apolar ices, or of chemically distinct active vents in the nucleus. The ortho-para ratio for water was 3.31 ± 0.33 (weighted mean of CRIRES and NIRSPEC results), implying a spin temperature >37 K at the 95% confidence limit. Our (3?) upper limit for HDO corresponds to D/H < 2.45 × 10{sup –3} (i.e., <16 Vienna Standard Mean Ocean Water, VSMOW). At R {sub h} = 1.2 AU (CRIRES), the production rate for water was Q(H{sub 2}O) = 1.9 ± 0.1 × 10{sup 29} s{sup –1} and its rotational temperature was T {sub rot} ? 69 K. At R {sub h} = 0.75 AU (CSHELL), we measured Q(H{sub 2}O) = 4.6 ± 0.6 × 10{sup 29} s{sup –1} and T {sub rot} = 80 K on March 31, and 6.6 ± 0.9 × 10{sup 29} s{sup –1} and T {sub rot} = 100 K on April 1. At R {sub h} = 1.74 AU (NIRSPEC), we obtained Q(H{sub 2}O) = 1.1 ± 0.1 × 10{sup 29} s{sup –1} and T {sub rot} ? 50 K. The measured volatile abundance ratios classify comet C/2012 F6 as rather depleted in C{sub 2}H{sub 6} and CH{sub 3}OH, while HCN, CH{sub 4}, and CO displayed abundances close to their median values found among comets. H{sub 2}CO was the only volatile showing a relative enhancement. The relative paucity of C{sub 2}H{sub 6} and CH{sub 3}OH (with respect to H{sub 2}O) suggests formation within warm regions of the nebula. However, the normal abundance of HCN and hypervolatiles CH{sub 4} and CO, and the enhancement of H{sub 2}CO, may indicate a possible heterogeneous nucleus of comet C/2012 F6 (Lemmon), possibly as a result of radial mixing within the protoplanetary disk.

  16. Dedicated to the memory of Paul Green (1931{1998) Tyger! Tyger! burning bright

    E-Print Network [OSTI]

    Carbone, Alessandra

    retain the framework of physics and look at patterns such as clouds in the sky, water owing in a river;usion of several inter- acting chemical substances might cause mosaic patterns on animals, from zebras since chemical reactions and di#11;usion drive the system down an energy well towards equilibrium, and

  17. Sleep, mood, and circadian responses to bright green light during sleep

    E-Print Network [OSTI]

    Grandner, Michael Andrew

    2007-01-01

    Rhythms. 15(5), 437-46. Dijk, D. J. , & Czeisler, C. A. (by others (Achermann, Dijk, Brunner & Borbély, 1993;Benington & Heller, 1994; 1995; Dijk & Czeisler, 1995), have

  18. Digital Sliding Mode Pulsed Current Averaging IC Drivers for High Brightness Light Emitting Diodes

    E-Print Network [OSTI]

    Lehman, Brad

    to the load. A variable frequency boost converter in Discontinuous Conduction Mode (DCM) has been used algorithm of the inductor current variations for a digitally controlled DC-DC boost converter operating in Continuous Conduction Mode. [10] describes a microcontroller based digital boost converter for a RGB

  19. 'DisrupTech' event to highlight bright ideas from Los Alamos

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    DisrupTech will feature eight technology presentations in the areas of sustainable fracking, solar cell materials, biofuels, tamper forensics, neutralization of toxic chemicals,...

  20. HIA 2015 DOE Zero Energy Ready Home Case Study: BrightLeaf Homes...

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    cold * Completion: October 2014 * Category: Production Modeled Performance Data: * HERS Index: without PV 38 * Projected Annual Utility Costs: without PV 1,362 * Projected...

  1. GRB 060607A: A GRB with Bright Asynchronous Early $X$-ray and Optical Emissions

    E-Print Network [OSTI]

    Houri Ziaeepour; Stephen T. Holland; Patricia T. Boyd; Kim L. Page; Samantha Oates; Craig B. Markwardt; Peter Meszaros; Neil Gehrels; Francis E. Marshall; Jay Cummings; Mike Goad

    2007-12-19

    The early optical emission of the moderately high redshift ($z=3.08$) GRB 060607A shows a remarkable broad and strong peak with a rapid rise and a relatively slow power-law decay. It is not coincident with the strong early-time flares seen in the X-ray and gamma-ray energy bands. There is weak evidence for variability superposed on this dominant component in several optical bands that can be related to flares in high energy bands. While for a small number of GRBs, well-sampled optical flares have been observed simultaneously with X-ray and gamma ray pulses, GRB 060607A is one of the few cases where the early optical emission shows no significant evidence for correlation with the prompt emission. In this work we first report in detail the broad band observations of this burst by Swift. Then by applying a simple model for the dynamics and the synchrotron radiation of a relativistic shock, we show that the dominant component of the early emissions in optical wavelengths has the same origin as the tail emission produced after the main gamma ray activity. The most plausible explanation for the peak in the optical light curve seems to be the cooling of the prompt after the main collisions, shifting the characteristic synchrotron frequency to the optical bands. It seems that the cooling process requires a steepening of the electron energy distribution and/or a break in this distribution at high energies. The sharp break in the X-ray light curve at few thousands of seconds after the trigger, is not observed in the IR/optical/UV bands, and therefore can not be a jet break. Either the X-ray break is due to a change in the spectrum of the accelerated electrons or the lack of an optical break is due to the presence of a related delayed response component (Abbreviated).

  2. GRB 061121: BROADBAND SPECTRAL EVOLUTION THROUGH THE PROMPT AND AFTERGLOW PHASES OF A BRIGHT BURST

    E-Print Network [OSTI]

    Zhang, Bing

    K. L. Page,1 R. Willingale,1 J. P. Osborne,1 B. Zhang,2 O. Godet,1 F. E. Marshall,3 A. Melandri,4 J. Yuan,11 and H. Ziaeepour9 Received 2006 December 22; accepted 2007 April 12 ABSTRACT Swift triggered- stantaneously brightest long burst yet detected by Swift. Using a combination of Swift and Konus-Wind data, we

  3. GRB 060607A: A GRB with Bright Asynchronous Early $X$-ray and Optical Emissions

    E-Print Network [OSTI]

    Ziaeepour, Houri; Boyd, Patricia T; Page, Kim L; Oates, Samantha; Markwardt, Craig B; Meszaros, Peter; Gehrels, Neil; Marshall, Francis E; Cummings, Jay; Goad, Mike

    2007-01-01

    The early optical emission of the moderately high redshift ($z=3.08$) GRB 060607A shows a remarkable broad and strong peak with a rapid rise and a relatively slow power-law decay. It is not coincident with the strong early-time flares seen in the X-ray and gamma-ray energy bands. There is weak evidence for variability superposed on this dominant component in several optical bands that can be related to flares in high energy bands. While for a small number of GRBs, well-sampled optical flares have been observed simultaneously with X-ray and gamma ray pulses, GRB 060607A is one of the few cases where the early optical emission shows no significant evidence for correlation with the prompt emission. In this work we first report in detail the broad band observations of this burst by Swift. Then by applying a simple model for the dynamics and the synchrotron radiation of a relativistic shock, we show that the dominant component of the early emissions in optical wavelengths has the same origin as the tail emission p...

  4. Supplementary Information Stephen J. Royle, Nicholas A. Bright & Leon Lagnado "Clathrin is required for the function

    E-Print Network [OSTI]

    , as shown in Supplementary Fig. S1a. During interphase, GFP-tagged clathrin light chain a (GFP-LCa to localise with microtubules invading the nuclear space during prometaphase (Supplementary Fig. S1a chain (Supplementary Figs. S2,S3). Clathrin at the mitotic spindle could be labelled with GFP-LCa, GFP-nLCa

  5. Three-dimensional analysis of free-electron laser performance using brightness scaled variables

    E-Print Network [OSTI]

    Gullans, M.

    2008-01-01

    to the Linac Coherent Light Source (LCLS) design, ESASEon the LCLS, and the optimal gain for a ?xed emittance.The parameters for LCLS used here are a beam energy of 13.64

  6. DYNAMICAL STABILITY AND ENVIRONMENTAL INFLUENCES IN LOW SURFACE BRIGHTNESS DISK GALAXIES

    E-Print Network [OSTI]

    McGaugh, Stacy

    and starburst activity in these galaxies. Subject heading: galaxies: evolution -- galaxies: interactions in their lifetimes. Indeed, sufficient tidally induced star formation in LSB disks may drive evolution from LSB are significantly different (de Blok & McGaugh 1996, hereafter dBM). In particular, LSB galaxies have lower disk

  7. New Family of Tiny Crystals Glow Bright in LED Lights | Advanced...

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    crystals that glow different colors may be the missing ingredient for white light-emitting diode (LED) lighting that illuminates homes and offices as effectively as natural...

  8. High-intensity, high-brightness polarized and unpolarized beam production in charge-exchange collisions

    SciTech Connect (OSTI)

    Zelenski, A.; Ritter, J.; Zubets, V.; Steski, D.; Atoian, G.; Davydenko, V.; Ivanov, A.; Kolmogorov, A.

    2011-03-28

    Basic limitations on the high-intensity H{sup -} ion beam production were experimentally studied in charge-exchange collisions of the neutral atomic hydrogen beam in the Na-vapour jet ionizer cell. These studies are the part of the polarized source upgrade (to 10 mA peak current and 85% polarization) project for RHIC. In the source the atomic hydrogen beam of a 5-10 keV energy and total (equivalent) current up to 5 A is produced by neutralization of proton beam in pulsed hydrogen gas target. Formation of the proton beam (from the surface of the plasma emitter with a low transverse ion temperature {approx}0.2 eV) is produced by four-electrode spherical multi-aperture ion-optical system with geometrical focusing. The hydrogen atomic beam intensity up to 1.0 A/cm{sup 2} (equivalent) was obtained in the Na-jet ionizer aperture of a 2.0 cm diameter. At the first stage of the experiment H-beam with 36 mA current, 5 keV energy and {approx}1.0 cm {center_dot} mrad normalized emittance was obtained using the flat grids and magnetic focusing.

  9. High efficiency and brightness fluorescent organic light emitting diode by triplet-triplet fusion

    DOE Patents [OSTI]

    Forrest, Stephen; Zhang, Yifan

    2015-02-10

    A first device is provided. The first device further comprises an organic light emitting device. The organic light emitting device further comprises an anode, a cathode, and an emissive layer disposed between the anode and the cathode. The emissive layer may include an organic host compound and at least one organic emitting compound capable of fluorescent emission at room temperature. Various configurations are described for providing a range of current densities in which T-T fusion dominates over S-T annihilation, leading to very high efficiency fluorescent OLEDs.

  10. Current Trends in Peptide Science Quantum Dots and Peptides: A Bright Future Together

    E-Print Network [OSTI]

    Ghosh, Indraneel

    be generated for any emission wave- length with an *30 nm of Full-width half-maximum. The typically broad materials, such as quantum nano- rods,3 magnetic nanocrystals,4 QD-based solar cells, and light, and long luminescent lifetimes. These remarkable properties of QDs have resulted in their use

  11. GE Bright Mind: Dr. John Schenck and the forefront of MRI research...

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    particular knowledge of the technology, but several staff members - particularly Howard Hart and Richard Likes - had been investigating MR on a part-time basis. They had become...

  12. Looking on bright side of losing ITER Risa Kato and Tetsuro Yamada / Yomiuri Shimbun Staff Writers

    E-Print Network [OSTI]

    the French site the green light later this month. The Japanese government has bowed to the inevitable would become the world's leader in nuclear fusion energy. The Finance Ministry, however, was skeptical at the Japan Atomic Energy Research Institute for plasma experiments, for building an experimental fusion

  13. A bright thermonuclear X-ray burst simultaneously observed with Chandra and RXTE

    E-Print Network [OSTI]

    in't Zand, J. J. M.

    The prototypical accretion-powered millisecond pulsar SAX J1808.4?3658 was observed simultaneously with Chandra-LETGS and RXTE-PCA near the peak of a transient outburst in November 2011. A single thermonuclear (type-I) ...

  14. Bright tripartite entanglement in triply concurrent parametric oscillation A. S. Bradley and M. K. Olsen

    E-Print Network [OSTI]

    Queensland, University of

    , University of Virginia, 382 McCormick Road, Charlottesville, Virginia 22904-4714, USA Received 17 May 2005 number s : 42.50.Dv, 03.65.Ud, 03.67.Mn, 42.65.Lm Entanglement is a central property of quantum mechanics

  15. Internet as Teenager In Higher Education: Rapid Growth, Transformation, Uncertain but Bright Future

    E-Print Network [OSTI]

    Matkin, Gary

    2007-01-01

    religious beliefs, the Internet is challenging higherimportant contribution of the Internet to education to datePaper Series Gary Matkin, INTERNET AS TEENAGER IN HIGHER

  16. Bright x-ray sources from laser irradiation of foams with high...

    Office of Scientific and Technical Information (OSTI)

    efficiency with foam targets is due to novel fabrication techniques based on atomic-layer-deposition of Ti atoms on an aerogel scaffold. A Ti concentration of 33 at. % was...

  17. AEGIS: The Diversity of Bright Near-IR Selected Distant Red Galaxies

    E-Print Network [OSTI]

    2006-01-01

    tra of DRGs in the Extended Groth Strip (EGS). We study 1010with K s EGS, and two other ?elds that arebetween the ACS imaging in the EGS and our NIR survey. We ?

  18. South Florida Sun-Sentinel.com Some bright spots behind the Census' dark economic

    E-Print Network [OSTI]

    Fernandez, Eduardo

    of the Great Recession in 2009. The Census stats also showed poverty and the numbers of the uninsured were up

  19. n a bright spring morning in Pasadena, California, the air is rich with the smells

    E-Print Network [OSTI]

    Napp, Nils

    solution." CATCHING RAYS The concept of artificial photosynthesis goes back to 1912, but the push than a plant cell. Their gleam- ing new labs are the headquarters of the Joint Center for Artificial Photosynthesis (JCAP), a 190-person research programme funded by SPRINGTIMEFORTHE ARTIFICIALLEAFResearchers make

  20. Power Minimization in a Backlit TFT-LCD Display by Concurrent Brightness and Contrast Scaling

    E-Print Network [OSTI]

    Pedram, Massoud

    energy corrected for the standardized spectral response of human vision. Luminous intensity (candela out that the cold cathode fluorescent lamp (CCFL) backlight of an LCD display dominates the energy conservative to deliver great energy savings. In this paper, we propose using the image contrast as a metric

  1. Power Minimization in a Backlit TFT-LCD Display by Concurrent Brightness and Contrast Scaling

    E-Print Network [OSTI]

    Pedram, Massoud

    around a backlit TFT-LCD display in Fig. 1. Luminous flux (lumen) is the emission rate of light energy fluorescent lamp (CCFL) backlight of an LCD display dominates the energy consumption of the whole system [1 energy savings. In this paper, we propose using the image contrast as a metric to measure the image

  2. Bibliography Adelson, E. H. (1993). Perceptual organization and the judgment of brightness. Science, 262,

    E-Print Network [OSTI]

    Kersten, Dan

    1993-01-01

    Vision and Pattern Recognition. Champaign, Illinois. The Institute of Electrical and Electronics of the Stereo Correspondence Problem Using Half-Occluded Regions. IEEE Computer Society Conference on Computer Engineers, Inc., 506-512. Bell, A. J., & Sejnowski, T. J. (1997). The "independent components" of natural

  3. but variations of brightness with time allow astronomers to detect light echoes through

    E-Print Network [OSTI]

    star and eventually reaches the critical Chandrasekhar mass (1.4 solar masses), a thermonuclear explosion disrupts the star, releasing materials that are the product of the stellar nuclear fusion (mostly G-type companion star14 (a star just like our Sun) all suggested a thermonuclear supernova rather

  4. On the Brightness of Surviving Companions in Type Ia Supernova Remnants

    E-Print Network [OSTI]

    Noda, Kazuhiro; Shigeyama, Toshikazu

    2015-01-01

    The progenitor systems for type Ia supernovae are still controversial. One of the methods to test the proposed scenario for the progenitor systems is to identify companions that are supposed to survive according to the so-called single degenerate scenario. These companions might be affected by supernova ejecta. We present several numerical simulations of surviving red-giant companions whose envelopes were stripped and heated. We find that red-giants with less-massive helium cores ($\\lesssim0.30\\,M_{\\odot}$) can be so faint after the supernovae that we cannot detect them. In addition, we apply the results to the case of SNR 0509-67.5, and put constraints on the helium core mass, envelope stripping, and energy injection under the single degenerate scenario for type Ia supernovae.

  5. Different Characteristics of the Bright Branches of the Globular Clusters M3 and M13

    E-Print Network [OSTI]

    Dong-Hwan Cho; Sang-Gak Lee; Young-Beom Jeon; Kyung Jin Sim

    2005-02-17

    We carried out wide-field BVI CCD photometric observations of the GCs M3 and M13 using the BOAO 1.8 m telescope equipped with a 2K CCD. We present CMDs of M3 and M13. We have found AGB bumps at V = 14.85 for M3 at V = 14.25 for M13. It is found that AGB stars in M3 are more concentrated near the bump, while those in M13 are scattered along the AGB sequence. We identified the RGB bump of M3 at V = 15.50 and that of M13 at V = 14.80. We have estimated the ratios R and R2 for M3 and M13 and found that of R for M3 is larger than that for M13 while R2's for M3 and M13 are similar when only normal HB stars are used in R and R2 for M13. However, we found that R's for M3 and M13 are similar while R2 for M3 is larger than that for M13 when all the HB stars are included in R and R2 for M13. We have compared the observed RGB LFs of M3 and M13 with the theoretical RGB LF of Bergbusch & VandenBerg at the same radial distances from the cluster centers as used in R and R2 for M3 and M13. We found "extra stars" belonging to M13 in the comparison of the observed RGB LF of M13 and the theoretical RGB LF of Bergbusch & VandenBerg. In the original definition of R of Buzzoni et al., N(HB) corresponds to the lifetime of HB stars in the RR Lyrae instability strip at log T_eff = 3.85. So, the smaller R value resulting for M13 compared with that for M3 in the case where only normal HB stars are included in R and R2 for M13 may be partially caused by "extra stars", and the similar R's for M3 and M13 in the case where the all HB stars are included in R and R2 for M13 may be caused by "extra stars" in the upper RGB of M13. If "extra stars" in the upper RGB of M13 are caused by an effective "deep mixing" these facts support the contention that an effective "deep mixing" could lead to different HB morphologies between M3 and M13 and subsequent sequences.

  6. BLAST05: Power Spectra of Bright Galactic Cirrus at Submillimeter Wavelengths

    E-Print Network [OSTI]

    Roy, Arabindo; Bock, James J; Chapin, Edward L; Devlin, Mark J; Dicker, Simon R; Griffin, Matthew; Gundersen, Joshua O; Halpern, Mark; Hargrave, Peter C; Hughes, David H; Klein, Jeff; Marsden, Gaelen; Martin, Peter G; Mauskopf, Philip; Miville-Deschenes, Marc-Antoine; Netterfield, Calvin B; Olmi, Luca; Pascale, Enzo; Patanchon, Guillaume; Rex, Marie; Scott, Douglas; Semisch, Christopher; Truch, Matthew D P; Tucker, Carole; Tucker, Gregory S; Viero, Marco P; Wiebe, Donald V

    2009-01-01

    We report multi-wavelength power spectra of diffuse Galactic dust emission from BLAST observations at 250, 350, and 500 microns in Galactic Plane fields in Cygnus X and Aquila. These submillimeter power spectra statistically quantify the self-similar structure observable over a broad range of scales and can be used to assess the cirrus noise which limits the detection of faint point sources. The advent of submillimeter surveys with the Herschel Space Observatory makes the wavelength dependence a matter of interest. We show that the observed relative amplitudes of the power spectra can be related through a spectral energy distribution (SED). Fitting a simple modified black body to this SED, we find the dust temperature in Cygnus X to be 19.9 +/- 1.3 K and in the Aquila region 16.9 +/- 0.7 K. Our empirical estimates provide important new insight into the substantial cirrus noise that will be encountered in forthcoming observations.

  7. Envisioning a Bright Future for New Braunfels Children: A Community-Based Approach to School Readiness 

    E-Print Network [OSTI]

    Fanomezantsoa, Herilala; Hopkins, Elizabeth; Tooley, Kathryn

    2015-05-20

    Consulting Capstone Group (MCCG) mission was to provide the McKenna Foundation with informed recommendations regarding school readiness, so that they could effectively serve and advance the well-being of the New Braunfels community....

  8. The Bright Lights in New York Could Be Solar | Department of...

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    a solar potential of 5,800 megawatts peak output-more that 40 percent of the city's electrical demand at peak times if all the rooftops were fully outfitted with solar. About...

  9. A bright idea? : the promise and peril of a memory drug

    E-Print Network [OSTI]

    Dowd, William (William Michael)

    2007-01-01

    In the MIT lab of neuropharmacologist Richard Wurtman, rodents that received a new Alzheimer's drug have shown a marked improvement in learning and memory. They are able to master elaborate mazes in half the time of their ...

  10. Generation, transport and focusing of high-brightness heavy ion beams

    E-Print Network [OSTI]

    Henestroza, Enrique

    2006-01-01

    The Neutralized Transport Experiment (NTX) has been built at the Heavy Ion Fusion Virtual National Laboratory. NTX is the first successful integrated beam system experiment that explores various physical phenomena, and ...

  11. A brightly colored starfish with a voracious appetite for mussels occupies a key niche in

    E-Print Network [OSTI]

    Bertness, Mark D.

    by a monotone of mussels. Paine called the starfish a "keystone" species be- cause, like a keystone in architecture, it is crucial for maintaining structure. Since then, Paine's notion of keystone species has be, the so-called keystone, was absent, says Bertness. "The classic keystone species example is wrong," he

  12. Internet as Teenager In Higher Education: Rapid Growth, Transformation, Uncertain but Bright Future

    E-Print Network [OSTI]

    Matkin, Gary

    2007-01-01

    that the history of the application of Internet technologythis new Internet technology. The Lessons of History aboutthis history. I conclude with an assertion that the Internet

  13. DOE Zero Energy Ready Home Case Study: BrightLeaf Homes, McCormick...

    Energy Savers [EERE]

    Innovation Award winning production home in the cold climate that got a HERS 38 without PV, with staggered 2x4 studs every 8"on a 2x6 plate with dense-packed R-25 cellulose,...

  14. Inner disc rearrangement revealed by dramatic brightness variations in the young star PV Cep

    E-Print Network [OSTI]

    Kun, M; Moór, A; Kóspál, Á; Ábrahám, P; Apai, D; Kiss, Z T; Klagyivik, P; Magakian, T Yu; Mez\\Ho, Gy; Movsessian, T A; Pál, A; Rácz, M; Rogers, J

    2011-01-01

    Young Sun-like stars at the beginning of the pre-main sequence (PMS) evolution are surrounded by accretion discs and remnant protostellar envelopes. Photometric and spectroscopic variations of these stars are driven by interactions of the star with the disc. Time scales and wavelength dependence of the variability carry information on the physical mechanisms behind these interactions. We conducted multi-epoch, multi-wavelength study of PV Cep, a strongly variable, accreting PMS star. By combining our own observations from 2004-2010 with archival and literature data, we show that PV Cep started a spectacular fading in 2005, reaching an I_C-band amplitude of 4 mag. Analysis of variation of the optical and infrared fluxes, colour indices, and emission line fluxes suggests that the photometric decline in 2005-2009 resulted from an interplay between variable accretion and circumstellar extinction: since the central luminosity of the system is dominated by accretion, a modest drop in the accretion rate could induce...

  15. Physical nature of the [S II]-bright shell nebulae N70 and N185

    SciTech Connect (OSTI)

    Zhang, Ning-Xiao; Jiang, Bing; Chen, Yang; Chu, You-Hua; Gruendl, R. A.; Williams, R. M.

    2014-09-01

    N70 and N185 are two large (?100 pc in diameter) shell nebulae in the Large Magellanic Cloud (LMC). Their high [S II]/H? ratios rival those of supernova remnants (SNRs), but they are not confirmed as SNRs. To study their physical nature, we have obtained XMM-Newton X-ray observations and high-dispersion long-slit echelle spectroscopic observations of these two nebulae. The X-ray spectra of both nebulae can be well interpreted with an optically thin thermal (?0.2 keV) plasma with the average LMC abundance in a collisional ionization equilibrium. N70 encompasses the OB association LH114. Although N70 has a modest expansion velocity and essentially thermal radio emission, its diffuse X-ray luminosity (?6.1 × 10{sup 35} erg s{sup –1}) is higher than that from a quiescent superbubble with N70's density, size, and expansion velocity; thus, N70 is most likely a superbubble that is recently energized by an interior SNR. N185 does not contain any known OB association, and its X-ray luminosity is an order of magnitude lower than expected if it is a quiescent superbubble. N185 has nonthermal radio emission and has high-velocity material expanding at nearly 200 km s{sup –1}, similar to many known SNRs in the LMC. Its X-ray luminosity (?1.9 × 10{sup 35} erg s{sup –1}) is also consistent with that of an evolved SNR. We therefore suggest that N185 is energized by a recent supernova.

  16. High-Throughput, High-Precision Hot Testing Tool for High-Brightness

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Delicious Rank EERE:Financing Tool Fits the Bill Financing ToolSustainableSecurityHighDepartment ofLight-Emitting Diode

  17. Supernovae of the Same Brightness, Cut From Vastly Different Cosmic Cloth

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity ofkandz-cm11 Outreach Home RoomPreservationBio-Inspired Solar Fuel Production 1: Totalof EnergyWind

  18. 'DisrupTech' event to highlight bright ideas from Los Alamos

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of NaturalDukeWakefieldSulfateSciTechtail.Theory ofDidDevelopmentatabout WhoQUESTIONS",#LabSpotlight'Data

  19. Panel Discussion: The SunShot Initiative: The Future is Bright | Department

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Delicious RankADVANCED MANUFACTURINGEnergy Bills andOrder 422.1, CONDUCT P - .EnergyHYDROGEN ENERGY H 25Energyofof

  20. SunShot Grand Challenge Summit: Bright Outlook to Achieve SunShot Goal |

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power AdministrationRobust,Field-effect PhotovoltaicsStructureInnovationEnergy ConversionLansof18 and985 1 2 3

  1. BrightPhase Energy Inc formerly Solar Focus | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION JEnvironmentalBowerbank, Maine: Energy ResourcesCounty, Texas:Brewer,Iowa:Brigantine, NewEnergy Inc

  2. DOE Tour of Zero: McCormick Avenue by BrightLeaf Homes | Department of

    Broader source: Energy.gov (indexed) [DOE]

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of Natural GasAdjustmentsShirleyEnergyTher i n c i pStateDOE FederalTheof Energy2,408-square-foot zero energy home

  3. DOE Zero Energy Ready Home Case Study: BrightLeaf Homes, McCormick Avenue,

    Broader source: Energy.gov (indexed) [DOE]

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of Natural GasAdjustmentsShirleyEnergyTher i n c i pStateDOE FederalTheofHeyeck, AEP, Sr.Energy ofBrookfield, IL |

  4. AN EMERGING CLASS OF BRIGHT, FAST-EVOLVING SUPERNOVAE WITH LOW-MASS EJECTA

    Office of Scientific and Technical Information (OSTI)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of NaturalDukeWakefield MunicipalTechnicalInformation4563 LLNL(Technicalentanglements forusing LSSTConnect

  5. Bright x-ray sources from laser irradiation of foams with high

    Office of Scientific and Technical Information (OSTI)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of NaturalDukeWakefieldSulfate Reducing Bacteria (Technical Report) |

  6. Bright x-ray sources from laser irradiation of foams with high

    Office of Scientific and Technical Information (OSTI)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of NaturalDukeWakefieldSulfate Reducing Bacteria (Technical Report) |concentration of Ti (Journal Article) | SciTech

  7. Bright x-ray sources from laser irradiation of foams with high

    Office of Scientific and Technical Information (OSTI)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of NaturalDukeWakefieldSulfate Reducing Bacteria (Technical Report) |concentration of Ti (Journal Article) |

  8. High-Ti-concentration aerogels for bright x-ray sources (Technical Report)

    Office of Scientific and Technical Information (OSTI)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of NaturalDukeWakefieldSulfate Reducing(Journal Article)lasers (Journal Article)SciTech ConnectMicrofabricated| SciTech

  9. High-Ti-concentration aerogels for bright x-ray sources (Technical Report)

    Office of Scientific and Technical Information (OSTI)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of NaturalDukeWakefieldSulfate Reducing(Journal Article)lasers (Journal Article)SciTech ConnectMicrofabricated| SciTech|

  10. High-Z Non-Equilibrium Physics and Bright X-ray Sources with New Laser

    Office of Scientific and Technical Information (OSTI)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of NaturalDukeWakefieldSulfate Reducing(Journal Article)lasers (Journal Article)SciTech ConnectMicrofabricated|Targets

  11. High-Z Non-Equilibrium Physics and Bright X-ray Sources with New Laser

    Office of Scientific and Technical Information (OSTI)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of NaturalDukeWakefieldSulfate Reducing(Journal Article)lasers (Journal Article)SciTech

  12. DOE Tour of Zero Floorplans: McCormick Avenue by BrightLeaf Homes |

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Delicious Rank EERE:FinancingPetroleum Based| Department8, 2015 GATEWAY Takes onandField |ofDepartment

  13. GE Bright Mind: Dr. John Schenck and the forefront of MRI research | GE

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity ofkandz-cm11 Outreach Home Room NewsInformation Current HABFESOpportunities Nuclear Physics (NP)about a majorHKL-2000Global

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    Broader source: Energy.gov (indexed) [DOE]

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of Natural GasAdjustmentsShirley Ann JacksonDepartment|Marketing, LLC | Department ofApps forLynn talked aboutEnergy

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    Broader source: Energy.gov (indexed) [DOE]

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of Natural GasAdjustmentsShirley Ann JacksonDepartment|Marketing, LLC | Department ofApps forLynn talked

  16. Cracking Molecular Structures with Bright Lights - and a Few Good Eggs |

    Broader source: Energy.gov (indexed) [DOE]

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of Natural GasAdjustmentsShirley Ann JacksonDepartment of EnergyResearchersOctoberCharles DOEJungleWinter (Part 2) |

  17. DOE Tour of Zero: McCormick Avenue by BrightLeaf Homes | Department of

    Broader source: Energy.gov (indexed) [DOE]

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of Natural GasAdjustmentsShirley Ann JacksonDepartment ofOffice of Headquarters AccountingDOEEnergyHumanAddisonEnergy

  18. Plastic Solar Cells See Bright Future | ANSER Center | Argonne-Northwestern

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

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  19. The Bright Lights in New York Could Be Solar | Department of Energy

    Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

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  20. DOE Finalizes $1.6 Billion Loan Guarantee for BrightSource Energy Inc. |

    Broader source: Energy.gov (indexed) [DOE]

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of Natural GasAdjustmentsShirleyEnergy A plug-in electric vehicle10nominate an employee forThis formis