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1

Energy All-Stars Shine Bright at Inaugural Lecture Series | Department...  

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

CEO of Bloomberg New Energy Finance, highlighted the impressive growth of investments in renewable energy around the world, while also cautioning of the challenges that lie ahead....

2

Jennifer Granholm (Energy All Stars Presentation)  

Broader source: Energy.gov [DOE]

Former Michigan Governor Jennifer Granholm delivered this presentation advocating for an energy Race to the Top competition between the states at the Energy All Stars event on January 19, 2013, at...

3

Bill Nye (Energy All Stars Presentation)  

Broader source: Energy.gov [DOE]

Bill Nye the Science Guy delivered this presentation on space and the lessons about climate change that can be gleaned from the other planets in our solar system at the Energy All Stars event on...

4

All-Star Nanocrystals | The Ames Laboratory  

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr MayAtmospheric Optical Depth (AOD)ProductssondeadjustsondeadjustAbout theOFFICE OF RESEARCHThermal Solar ThermalAll-Star Nanocrystals

5

Collaboration Shines in Materials Project Success  

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

Collaboration Shines in Materials Project Success Collaboration Shines in Materials Project Success Many Hands at Lab Lift 'World-Changing Idea' to New Heights December 12, 2013 |...

6

NA61/SHINE ion program  

E-Print Network [OSTI]

The Super Proton Synchrotron (SPS) at CERN covers one of the most interesting regions of the phase diagram (T - \\mu_{B}) of strongly interacting matter. The study of central Pb+Pb collisions by NA49 indicate that the threshold for deconfinement is reached already at the low SPS energies. Theoretical considerations predict a critical point of strongly interacting matter at energies accessible at the SPS. The NA61/SHINE experiment, a successor of the NA49 project, will study hadron production in p+p, p+A, h+A, and A+A reactions at various energies. The broad physics program includes the investigation of the properties of strongly interacting matter, as well as precision measurements of hadron spectra for the T2K neutrino experiment and for the Pierre Auger Observatory and KASCADE cosmic-ray projects. The main physics goals of the NA61/SHINE ion program are to study the properties of the onset of deconfinement at low SPS energies and to find signatures of the critical point of strongly interacting matter. To achieve these goals a broad range in the (T - \\mu_{B}) phase diagram will be covered by performing an energy (10A-158A GeV/c) and system size (p+p, B+C, Ar+Ca, Xe+La) scan. The first data for this 2-D scan were taken in 2009, i.e. p+p interactions at 20, 30, 40, 80, 158 GeV/c beam energy. This contribution will summarize physics arguments for the NA61/SHINE ion program, show the detector performance and present the current status of the experiment and plans for the next years.

Maja Mackowiak for the NA61 Collaboration

2010-09-06T23:59:59.000Z

7

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

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

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

8

New OLED Lighting Systems Shine Bright, Save 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 RankCombustion | Department ofT ib l L d F S iPartnership Program | Department ofMembraneofDepartment

9

SHINE Vacuum Pump Test Verification  

SciTech Connect (OSTI)

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.

Morgan, Gregg A; Peters, Brent

2013-09-30T23:59:59.000Z

10

Virginia Tech Shines Light on Home Efficiency | Department of...  

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

Virginia Tech Shines Light on Home Efficiency Virginia Tech Shines Light on Home Efficiency July 9, 2010 - 10:54am Addthis Virginia Tech's solar-powered Lumenhaus was designed for...

11

LET THE SUN SHINE: OPTIMAL DEPLOYMENT OF PHOTOVOLTAICS IN GERMANY  

E-Print Network [OSTI]

/kWh, depending on its location as well as on the size and type of PV system used (EPIA Report, 2011). InvestmentLET 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

Paris-Sud XI, Université de

12

A high brightness field emission display  

SciTech Connect (OSTI)

The military requirement for avionics display performance requires that displays be legible with 10,000 foot-candles (fc) bright light shining into the pilot`s eyes, or 10,000 fc shining directly on the display. The contrast ratio under these conditions must be at least 4.66:1. In addition, instant-on operation is sought for temperatures as low as {minus}54 C. Currently these specifications can barely be met by monochrome CRTs whose use is counter-indicated by other factors. No color display can achieve optimum performance in the areas mentioned, nor do any current contenders, primarily AMLCD`s, have any prospects of achieving full compliance. The FED being developed by Raytheon shows strong promise of being able to achieve the brightness and contrast ratios desired. The FED is also inherently able to provide instant-on functionality at any terrestrial temperature and does not require any heating at low temperatures. The technical objective of the Raytheon development program is to develop a high performance, full color, FED Panel that meets the performance and environmental operating condition requirements specified for military and other high performance display applications.

Palevsky, A. [Raytheon Co., Quincy, MA (United States)

1996-12-31T23:59:59.000Z

13

Shining Light in Dark Places: Understanding the Tor Network  

E-Print Network [OSTI]

Shining Light in Dark Places: Understanding the Tor Network Damon McCoy1 , Kevin Bauer1 , Dirk-used? (3) Who is using Tor? To sample the results, we show that web traffic makes up the ma- jority latency and high throughput, it is ideal for interac- tive applications such as web browsing, file sharing

14

Metamaterials Shine Bright as New Terahertz Source | U.S. DOE...  

Office of Science (SC) Website

than conventional materials that are presently used for these applications. Detailed analysis of the directionality and polarization of the emitted radiation reveals the...

15

New OLED Lighting Systems Shine Bright, Save Energy | 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:Year in3.pdfEnergy HealthCommentsAugustNationalMarkets withCohen |DepartmentofCyber

16

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

E-Print Network [OSTI]

Fusion energy · Fusion powers the Sun, and all stars, in which light nuclei fuse together at high in excess of 100 million degrees, much higher than in the Sun. The hot hydrogen gas (known as a `plasma

17

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

Office of Environmental Management (EM)

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May Jun Jul(Summary) "of EnergyEnergy Cooperation |South Valley ResponsibleSubmissionof Energy 5ofA2011EnergyA Shining

18

EM Shines with Five DOE Sustainability Awards | Department of Energy  

Office of Environmental Management (EM)

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May Jun Jul(Summary) "of Energy Power SystemsResources DOE ZeroThreeEnergyDepartment0: DOE512:Shines with Five DOE

19

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May JunDatastreamsmmcrcalgovInstrumentsrucLas Conchas recovery challenge fund Las Conchas recoveryNuclear energyInstrument to shine

20

Shining Light on Catalysis | Stanford Synchrotron Radiation Lightsource  

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May JunDatastreamsmmcrcalgovInstrumentsrucLas ConchasPassiveSubmitted forHighlightsSeminars SeminarsO'Leary d3j906Sheng Dai (2011)Shining

Note: This page contains sample records for the topic "all-stars shine bright" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


21

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

E-Print Network [OSTI]

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

Walter, Frederick M.

22

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

E-Print Network [OSTI]

FPL's solar stars shine at new 500-acre array By SUSAN SALISBURY Palm Beach Post Staff Writer and water, Florida Power & Light Co. workers finished cleaning the mirrors at its new Martin County solar's dedication of the one-of-a-kind hybrid solar energy center, it's nice that the 5-by-5-foot mirrors

Belogay, Eugene A.

23

Why Does the Sun Shine? What is the source of solar  

E-Print Network [OSTI]

Why Does the Sun Shine? #12;What is the source of solar luminosity? There were three plausible contraction #12;Fire Suppose the Sun were a mixture of carbon and oxygen on fire. ·Each chemical reaction releases an energy of about 10-11 ergs. ·The mass of the Sun could contain 3x1055 Carbon atoms plus twice

Walter, Frederick M.

24

The Old New Frontier: Studying the CERN-SPS Energy Range with NA61/SHINE  

E-Print Network [OSTI]

With the Large Hadron Collider entering its third year of granting us insight into the highest collision energies to date, one should nevertheless keep in mind the unexplored physics potential of lower energies. A prime example here is the NA61/SHINE experiment at the CERN Super Proton Synchrotron. Using its large-acceptance hadronic spectrometer, SHINE aims to accomplish a number of physics goals: measuring spectra of identified hadrons in hadron-nucleus collisions to provide reference for accelerator neutrino experiments and cosmic-ray observatories, investigating particle properties in the large transverse-momentum range for hadron+hadron and hadron+nucleus collisions for studying the nuclear modification factor at SPS energies, and measuring hadronic observables in a particularly interesting region of the phase diagram of strongly-interacting matter to study the onset of deconfinement and search for the critical point of strongly-interacting matter with nucleus-nucleus collisions. This contribution shall summarise results obtained so far by NA61/SHINE, as well as present the current status and plans of its experimental programme.

Marek Szuba; for the NA61/SHINE Collaboration

2012-09-26T23:59:59.000Z

25

AN ALL-SKY CATALOG OF BRIGHT M DWARFS  

SciTech Connect (OSTI)

We present an all-sky catalog of M dwarf stars with apparent infrared magnitude J < 10. The 8889 stars are selected from the ongoing SUPERBLINK survey of stars with proper motion {mu} > 40 mas yr{sup -1}, supplemented on the bright end with the Tycho-2 catalog. Completeness tests which account for kinematic (proper motion) bias suggest that our catalog represents {approx}75% of the estimated {approx}11, 900 M dwarfs with J < 10 expected to populate the entire sky. Our catalog is, however, significantly more complete for the northern sky ({approx}90%) than it is for the south ({approx}60%). Stars are identified as cool, red M dwarfs from a combination of optical and infrared color cuts, and are distinguished from background M giants and highly reddened stars using either existing parallax measurements or, if such measurements are lacking, using their location in an optical-to-infrared reduced proper motion diagram. These bright M dwarfs are all prime targets for exoplanet surveys using the Doppler radial velocity or transit methods; the combination of low-mass and bright apparent magnitude should make possible the detection of Earth-size planets on short-period orbits using currently available techniques. Parallax measurements, when available, and photometric distance estimates are provided for all stars, and these place most systems within 60 pc of the Sun. Spectral type estimated from V - J color shows that most of the stars range from K7 to M4, with only a few late M dwarfs, all within 20 pc. Proximity to the Sun also makes these stars good targets for high-resolution exoplanet imaging searches, especially if younger objects can be identified on the basis of X-ray or UV excess. For that purpose, we include X-ray flux from ROSAT and FUV/NUV ultraviolet magnitudes from GALEX for all stars for which a counterpart can be identified in those catalogs. Additional photometric data include optical magnitudes from Digitized Sky Survey plates and infrared magnitudes from the Two Micron All Sky Survey.

Lepine, Sebastien [Department of Astrophysics, Division of Physical Sciences, American Museum of Natural History, Central Park West at 79th Street, New York, NY 10024 (United States); Gaidos, Eric [Department of Geology and Geophysics, University of Hawaii, 1680 East-West Road, Honolulu, HI 96822 (United States)

2011-10-15T23:59:59.000Z

26

Bright Future NW Energy Coalition  

E-Print Network [OSTI]

Getting To a Bright Future 1. Cap global-warming emissions. President Obama and the U.S. Congress should Climate Initiative: 15% reduction from 1990 levels by 2020, 80% or larger reduction by 2050. While

27

Probing braneworld hypothesis with a "neutron-shining-through-a-wall" experiment  

E-Print Network [OSTI]

The possibility for our visible world to be a 3-brane embedded in a multidimensional bulk is at the heart of many theoretical edifices in high energy physics. Probing the braneworld hypothesis is then a major experimental challenge. Following recent theoretical works showing that matter swapping can occur between braneworlds, we propose a "neutron-shining-through-a-wall" experiment. We first show that an intense neutron source such as a nuclear reactor core can induce a hidden neutron flux in an adjacent hidden braneworld. We then describe how a low background detector can detect neutrons arising from the hidden world and we quantify the expected sensitivity to the swapping probability. As a proof of concept, a constraint is derived from previous experiments.

Sarrazin, Michael; Lamblin, Jacob; Petit, Fabrice; Terwagne, Guy; Nesvizhevsky, Valery V

2015-01-01T23:59:59.000Z

28

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.

29

A Bright Idea: New Efficiency Standards for Incandescent and...  

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

A Bright Idea: New Efficiency Standards for Incandescent and Fluorescent Lights A Bright Idea: New Efficiency Standards for Incandescent and Fluorescent Lights July 21, 2009 -...

30

Discovery of a GeV Blazar Shining Through the Galactic Plane  

SciTech Connect (OSTI)

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.

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.

2011-08-11T23:59:59.000Z

31

Massive Disks in Low Surface Brightness Galaxies  

E-Print Network [OSTI]

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.

B. Fuchs

2002-09-09T23:59:59.000Z

32

A brightness exceeding simulated Langmuir limit  

SciTech Connect (OSTI)

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.

Nakasuji, Mamoru [2-15-11, Serigaya-chou, Kounan-ku, Yokohama-shi, Kanagawa-ken (Japan)] [2-15-11, Serigaya-chou, Kounan-ku, Yokohama-shi, Kanagawa-ken (Japan)

2013-08-15T23:59:59.000Z

33

Surface brightness in plasma-redshift cosmology  

E-Print Network [OSTI]

In 2001 Lori M. Lubin and Allan Sandage, using big-bang cosmology for interpreting the data, found the surface brightness of galaxies to be inversely proportional to about the third power of (1+z), while the contemporary big-bang cosmology predicts that the surface brightness is inversely proportional to the fourth power of (1+z). In contrast, these surface brightness observations are in agreement with the predictions of the plasma-redshift cosmology. Lubin and Sandage (2001) and Barden et al. (2005), who surmised the big-bang expansion, interpreted the observations to indicate that the diameters of galaxies are inversely proportional to (1+z). In contrast, when assuming plasma-redshift cosmology, the diameters of galaxies are observed to be constant independent of redshift and any expansion. Lubin and Sandage (2001) and Barden et al. (2005), when using big-bang cosmology, observed the average absolute magnitude of galaxies to decrease with redshift; while in plasma redshift cosmology it is a constant. Lubin and Sandage and Barden et al. suggested that a coherent evolution could explain the discrepancy between the observed relations and those predicted in the big-bang cosmology. We have failed to find support for this explanation. We consider the observed relations between the redshift and the surface-brightness, the galaxy diameter, and the absolute magnitude to be robust confirmations of plasma-redshift cosmology.

Ari Brynjolfsson

2006-05-31T23:59:59.000Z

34

Technical Assistance Application Bright Schools Program  

E-Print Network [OSTI]

audit ­ evaluate energy efficiency opportunities at existing facilities Evaluate opportunitiesTechnical Assistance Application Bright Schools Program C a l i f o r n i a E n e r g y C o m m i: Zip: Contact Person: Title: Department: Phone Number: Email: * Name of K-12 school/ District 2. Attach

35

Laser Power Meter Large, bright, backlit LCD  

E-Print Network [OSTI]

Laser Power Meter FEATURES · Large, bright, backlit LCD display · Digital accuracy with analog-like movement for laser tuning · Works with thermopile and optical sensors · Intuitive button-driven user COMPATIBILITY · PowerMax® thermal sensors · Optical sensors FieldMaxII-TO Coherent Laser Measurement and Control

Woodall, Jerry M.

36

Business Honors Program A Bright Business Future  

E-Print Network [OSTI]

Business Honors Program Achieve! #12;2page A Bright Business Future If you are a talented no further. The Business Honors Program at Mihaylo College of Business and Economics provides a socially and professionally stimulating academic environment to a select group of business administration students. As you

de Lijser, Peter

37

High-brightness H/sup -/ accelerators  

SciTech Connect (OSTI)

Neutral particle beam (NPB) devices based on high-brightness H/sup -/ accelerators are an important component of proposed strategic defense systems. The basic rationale and R and D program are outlined and examples given of the underlying technology thrusts toward advanced systems. Much of the research accomplished in the past year is applicable to accelerator systems in general; some of these activities are discussed.

Jameson, R.A.

1987-01-01T23:59:59.000Z

38

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 Office of InspectorConcentrating SolarElectricEnergyCTBarre BiomassTHISBrickyard Energy Partners LLCBridgewaterBright

39

EECBG Success Story: Bright Green Spot: Fort Worth Library |...  

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

Bright Green Spot: Fort Worth Library EECBG Success Story: Bright Green Spot: Fort Worth Library September 30, 2010 - 9:53am Addthis Fort Worth's Central Library is seeing...

40

Bright Green Spot: Fort Worth Library | Department of Energy  

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

Bright Green Spot: Fort Worth Library Bright Green Spot: Fort Worth Library September 30, 2010 - 4:07pm Addthis Lindsay Gsell Fort Worth's Central Library is seeing tremendous...

Note: This page contains sample records for the topic "all-stars shine bright" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


41

Search for bright stars with infrared excess  

SciTech Connect (OSTI)

Bright stars, stars with visual magnitude smaller than 6.5, can be studied using small telescope. In general, if stars are assumed as black body radiator, then the color in infrared (IR) region is usually equal to zero. Infrared data from IRAS observations at 12 and 25?m (micron) with good flux quality are used to search for bright stars (from Bright Stars Catalogues) with infrared excess. In magnitude scale, stars with IR excess is defined as stars with IR color m{sub 12}?m{sub 25}>0; where m{sub 12}?m{sub 25}?=??2.5log(F{sub 12}/F{sub 25})+1.56, where F{sub 12} and F{sub 25} are flux density in Jansky at 12 and 25?m, respectively. Stars with similar spectral type are expected to have similar color. The existence of infrared excess in the same spectral type indicates the existence of circum-stellar dust, the origin of which is probably due to the remnant of pre main-sequence evolution during star formation or post AGB evolution or due to physical process such as the rotation of those stars.

Raharto, Moedji, E-mail: moedji@as.itb.ac.id [Astronomy Research Division, Faculty of Mathematics and Natural Sciences, Institut Teknologi Bandung, Jl. Ganesha 10, Bandung 40132 (Indonesia)

2014-03-24T23:59:59.000Z

42

The Bright Side of Dark Matter  

E-Print Network [OSTI]

We show that it is not possible in the absence of dark matter to construct a four-dimensional metric that explains galactic observations. In particular, by working with an effective potential it is shown that a metric which is constructed to fit flat rotation curves in spiral galaxies leads to the wrong sign for the bending of light i.e. repulsion instead of attraction. Hence, without dark matter the motion of particles on galactic scales cannot be explained in terms of geodesic motion on a four- dimensional metric. This reveals a new bright side to dark matter: it is indispensable if we wish to retain the cherished equivalence principle.

A. Edery

1999-05-27T23:59:59.000Z

43

The IRAS Revised Bright Galaxy Sample (RBGS)  

E-Print Network [OSTI]

IRAS flux densities, redshifts, and infrared luminosities are reported for all sources identified in the IRAS Revised Bright Galaxy Sample (RBGS), a complete flux-limited survey of all extragalactic objects with total 60 micron flux density greater than 5.24 Jy, covering the entire sky surveyed by IRAS at Galactic latitude |b| > 5 degrees. The RBGS includes 629 objects, with a median (mean) sample redshift of 0.0082 (0.0126) and a maximum redshift of 0.0876. The RBGS supersedes the previous two-part IRAS Bright Galaxy Samples, which were compiled before the final ("Pass 3") calibration of the IRAS Level 1 Archive in May 1990. The RBGS also makes use of more accurate and consistent automated methods to measure the flux of objects with extended emission. Basic properties of the RBGS sources are summarized, including estimated total infrared luminosities, as well as updates to cross-identifications with sources from optical galaxy catalogs established using the NASA/IPAC Extragalactic Database (NED). In addition...

Sanders, D B; Kim, D C; Surace, J A; Soifer, B T

2003-01-01T23:59:59.000Z

44

Internetwork chromospheric bright grains observed with IRIS  

E-Print Network [OSTI]

The Interface Region Imaging Spectrograph (IRIS) reveals small-scale rapid brightenings in the form of bright grains all over coronal holes and the quiet sun. These bright grains are seen with the IRIS 1330 \\AA, 1400 \\AA\\ and 2796 \\AA\\ slit-jaw filters. We combine coordinated observations with IRIS and from the ground with the Swedish 1-m Solar Telescope (SST) which allows us to have chromospheric (Ca II 8542 \\AA, Ca II H 3968 \\AA, H\\alpha, and Mg II k 2796 \\AA), and transition region (C II 1334 \\AA, Si IV 1402) spectral imaging, and single-wavelength Stokes maps in Fe I 6302 \\AA at high spatial (0.33"), temporal and spectral resolution. We conclude that the IRIS slit-jaw grains are the counterpart of so-called acoustic grains, i.e., resulting from chromospheric acoustic waves in a non-magnetic environment. We compare slit-jaw images with spectra from the IRIS spectrograph. We conclude that the grain intensity in the 2796 \\AA\\ slit-jaw filter comes from both the Mg II k core and wings. The signal in the C II ...

Martnez-Sykora, Juan; Carlsson, Mats; De Pontieu, Bart; Pereira, Tiago M D; Boerner, Paul; Hurlburt, Neal; Kleint, Lucia; Lemen, James; Tarbell, Ted D; Title, Alan; Wuelser, Jean-Pierre; Hansteen, Viggo H; Golub, Leon; McKillop, Sean; Reeves, Kathy K; Saar, Steven; Testa, Paola; Tian, Hui; Jaeggli, Sarah; Kankelborg, Charles

2015-01-01T23:59:59.000Z

45

automated local bright: Topics by E-print Network  

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

with the penumbral features. The bright points are not uniformly distributed over the umbra but preferentially located around the penumbral boundary and in the fast decaying...

46

artificial sky brightness: Topics by E-print Network  

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

with the penumbral features. The bright points are not uniformly distributed over the umbra but preferentially located around the penumbral boundary and in the fast decaying...

47

area telescope bright: Topics by E-print Network  

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

with the penumbral features. The bright points are not uniformly distributed over the umbra but preferentially located around the penumbral boundary and in the fast decaying...

48

albeit ultraviolet bright: Topics by E-print Network  

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

with the penumbral features. The bright points are not uniformly distributed over the umbra but preferentially located around the penumbral boundary and in the fast decaying...

49

High Brightness Neutron Source for Radiography  

SciTech Connect (OSTI)

This research and development program was designed to improve nondestructive evaluation of large mechanical objects by providing both fast and thermal neutron sources for radiography. Neutron radiography permits inspection inside objects that x-rays cannot penetrate and permits imaging of corrosion and cracks in low-density materials. Discovering of fatigue cracks and corrosion in piping without the necessity of insulation removal is possible. Neutron radiography sources can provide for the nondestructive testing interests of commercial and military aircraft, public utilities and petrochemical organizations. Three neutron prototype neutron generators were designed and fabricated based on original research done at the Lawrence Berkeley National Laboratory (LBNL). The research and development of these generators was successfully continued by LBNL and Adelphi Technology Inc. under this STTR. The original design goals of high neutron yield and generator robustness have been achieved, using new technology developed under this grant. In one prototype generator, the fast neutron yield and brightness was roughly 10 times larger than previously marketed neutron generators using the same deuterium-deuterium reaction. In another generator, we integrate a moderator with a fast neutron source, resulting in a high brightness thermal neutron generator. The moderator acts as both conventional moderator and mechanical and electrical support structure for the generator and effectively mimics a nuclear reactor. In addition to the new prototype generators, an entirely new plasma ion source for neutron production was developed. First developed by LBNL, this source uses a spiral antenna to more efficiently couple the RF radiation into the plasma, reducing the required gas pressure so that the generator head can be completely sealed, permitting the possible use of tritium gas. This also permits the generator to use the deuterium-tritium reaction to produce 14-MeV neutrons with increases of yield of two orders of magnitude. The first fast neutron radiographic images were obtained using neutron cameras and a new fast neutron generator. These early images demonstrated the feasibility of using fast neutrons for imaging and penetrating thick objects of high density and imaging. Fast neutrons can be used to image low atomic number materials (e.g. plastics, explosives, lubricants and ceramics) that are shielded by high density materials (e.g. lead, tungsten and uranium). Fast neutron radiography could be used as a means to screen weapons for flaws and chemical stability. X-ray radiography can not easily do this. Fast neutron imaging is technically difficult and, consequently, a completely undeveloped market. Two of the generators were designed to have small source size and high brightness, ideal for fast-neutron imaging. With these generators we successfully used two fast neutron cameras: one developed by us, and another developed by a collaborator, Commonwealth Scientific and Industrial Research Organization, CSIRO. We have successfully used these cameras to obtain low resolution images of various objects such as pipe fittings filled with water and other mechanical objects. Higher resolution and contrast images are expected by decreasing the source size and increasing generator yield.

Cremer, J. T.; Piestrup, Melvin, A.; Gary, Charles, K.; Harris, Jack, L. Williams, David, J.; Jones, Glenn, E.; Vainionpaa, J. , H.; Fuller, Michael, J.; Rothbart, George, H.; Kwan, J., W.; Ludewigt, B., A.; Gough, R.., A..; Reijonen, Jani; Leung, Ka-Ngo

2008-12-08T23:59:59.000Z

50

SPITZER 24 {mu}m EXCESSES FOR BRIGHT GALACTIC STARS IN BOOeTES AND FIRST LOOK SURVEY FIELDS  

SciTech Connect (OSTI)

Optically bright Galactic stars (V {approx}< 13 mag) having f {sub {nu}}(24 {mu}m) > 1 mJy are identified in Spitzer mid-infrared surveys within 8.2 deg{sup 2} for the Booetes field of the NOAO Deep Wide-Field Survey and within 5.5 deg{sup 2} for the First Look Survey (FLS). One hundred and twenty-eight stars are identified in Booetes and 140 in the FLS, and their photometry is given. (K - [24]) colors are determined using K magnitudes from the Two Micron All Sky Survey for all stars in order to search for excess 24 {mu}m luminosity compared to that arising from the stellar photosphere. Of the combined sample of 268 stars, 141 are of spectral types F, G, or K, and 17 of these 141 stars have 24 {mu}m excesses with (K - [24]) > 0.2 mag. Using limits on absolute magnitude derived from proper motions, at least eight of the FGK stars with excesses are main-sequence stars, and estimates derived from the distribution of apparent magnitudes indicate that all 17 are main-sequence stars. These estimates lead to the conclusion that between 9% and 17% of the main-sequence FGK field stars in these samples have 24 {mu}m infrared excesses. This result is statistically similar to the fraction of stars with debris disks found among previous Spitzer targeted observations of much brighter, main-sequence field stars.

Hovhannisyan, L. R.; Mickaelian, A. M. [Byurakan Astrophysical Observatory and Isaac Newton Institute of Chile Armenian Branch, 378433, Byurakan, Aragatzotn Province (Armenia); Weedman, D. W.; Houck, J. R. [Astronomy Department, Cornell University, Ithaca, NY 14853 (United States); Le Floc'h, E. [Steward Observatory, University of Arizona, Tucson, AZ, 85721 (United States); Soifer, B. T. [Spitzer Science Center, California Institute of Technology, 220-6, Pasadena, CA 91125 (United States); Brand, K. [Space Telescope Science Institute, 3700 San Martin Dr., Baltimore, MD 21218 (United States); Dey, A.; Jannuzi, B. T. [National Optical Astronomy Observatory, 950 N. Cherry Ave., Tucson, AZ 85719 (United States)], E-mail: lilithov11@yahoo.com, E-mail: dweedman@isc.astro.cornell.edu

2009-07-15T23:59:59.000Z

51

High output lamp with high brightness  

DOE Patents [OSTI]

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.

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)

2002-01-01T23:59:59.000Z

52

Dim Matter in the Disks of Low Surface Brightness Galaxies  

E-Print Network [OSTI]

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.

B. Fuchs

2002-04-23T23:59:59.000Z

53

Ashland Electric Utility- Bright Way to Heat Water Loan  

Broader source: Energy.gov [DOE]

The City of Ashland Conservation Division offers a solar water heating program to residential electric customers who currently use an electric water heater. Under "The Bright Way to Heat Water...

54

Ashland Electric Utility- Bright Way to Heat Water Rebate  

Broader source: Energy.gov [DOE]

The City of Ashland Conservation Division offers a solar water heating program to its residential electric customers who currently use an electric water heater. Under "The Bright Way to Heat Water...

55

Proposal for a High-Brightness Pulsed Electron Source  

SciTech Connect (OSTI)

We propose a novel scheme for a high-brightness pulsedelectron source, which has the potential for many useful applications inelectron microscopy, inverse photo-emission, low energy electronscattering experiments, and electron holography. A description of theproposed scheme is presented.

Zolotorev, Max; Commins, Eugene D.; Heifets, Sam; Sannibale,Fernando

2006-03-15T23:59:59.000Z

56

Infrared Brightness Temperature of Mars, 1983-2103  

E-Print Network [OSTI]

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.

E. L. Wright

2007-03-25T23:59:59.000Z

57

Template for project inclusion for Remote Sensing Systems' MSU/AMSU brightness temperatures in the C  

E-Print Network [OSTI]

Template for project inclusion for Remote Sensing Systems' MSU/AMSU brightness temperatures- Quality control procedures, including ongoing improvements. Brightness temperatures and geolocation data

58

High-brightness, high-current ion sources  

SciTech Connect (OSTI)

Several existing high-current dc ion sources are presented that yield positive ions and are based on gas discharges. Their common features are then outlined: extraction systems, required plasma qualities, and the production of ions from solid materials. Finally, from well-established laws, scaling rules for high-brightness ion beams are derived taking one specific case to determine the numerical constants. These rules predict that the current values of transportable beams scale proportionally to the 3/2 power of the extraction voltage, whereas the brightness strongly decreases with rising voltage.

Keller, R.

1985-01-01T23:59:59.000Z

59

SC-RISE LECTURE SERIES BRIGHT HORIZONS IN SOLAR ENERGY  

E-Print Network [OSTI]

SC-RISE LECTURE SERIES BRIGHT HORIZONS IN SOLAR ENERGY Sustainable Energy Opportunities, Options are being developed including biomass, geothermal, hydropower, ocean thermal energy conversion, solar electric, solar thermal, and wind. However, such aspects as low energy density, siting, and temporal

60

Data Integrity in a Distributed Storage System Jonathan D. Bright  

E-Print Network [OSTI]

Data Integrity in a Distributed Storage System Jonathan D. Bright Sigma Storage Corporation of Connecticut Storrs, CT, U.S.A. Abstract Distributed storage systems must provide highly available access, fault-tolerant algorithms, storage systems, distributed locking 1 Introduction The traditional storage

Chandy, John A.

Note: This page contains sample records for the topic "all-stars shine bright" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


61

class rooms H.R. Bright Building 1st  

E-Print Network [OSTI]

Cao Cheng Cao Yixin Choi Jinho Chung Jiryang Creel James Crosby Ralph Duncan Brittany Fan Jia-hao Guo Elena Rodriguez #12;115 129 423D 423C 115 115 423B 423A (Welch) 115 115 419D 419C H.R. Bright Building

62

RESEARCH Open Access Directed evolution of bright mutants of an  

E-Print Network [OSTI]

very limited brightness, which restricts their utility as biological imaging probes. Results: To increase the scope and utility of flavin-binding fluorescent proteins as practical fluorescent reporters Biology, University of Illinois at Urbana-Champaign, Urbana, IL 61801, USA Full list of author information

Schroeder, Charles

63

Proposal for a High-Brightness Pulsed Electron Source  

SciTech Connect (OSTI)

We propose a novel scheme for 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. A description of the proposed scheme is presented.

Zolotorev, M.; Commins, E.D.; Heifets, S.; Sannibale, F.; /LBL, Berkeley /UC, Berkeley /SLAC

2006-10-16T23:59:59.000Z

64

New Near-Infrared Surface Brightness Fluctuation Models  

E-Print Network [OSTI]

We present new theoretical models for surface brightness fluctuations in the near-infrared. We show the time evolution of near-infrared brightness fluctuation properties over large age and metallicity ranges, i.e., from 12 Myr to 16 Gyr, and from Z/Zsun=1/50 to Z/Zsun=2.5, for single age, single metallicity stellar populations. All the stellar models are followed from the zero age main sequence to the central carbon ignition for massive stars, or to the end of the thermally pulsing regime of the asymptotic giant branch phase for low and intermediate mass stars. The new models are compared with observed near-infrared fluctuation absolute magnitudes and colours for a sample of Magellanic Cloud star clusters and Fornax Cluster galaxies. For star clusters younger than ~3 Gyr, the predicted near-infrared fluctuation properties are in a satisfactory agreement with observed ones over a wide range of stellar population metallicities. However, for older star clusters, the agreement between the observed and predicted near-IR brightness fluctuations depends on how the surface brightness absolute magnitudes are estimated. The computed set of models are not able to match the observed near-IR fluctuation absolute magnitudes and colours simultaneously. We argue that the observed discrepancies between the predicted and observed properties of old MC superclusters are more likely due to observational reasons.

M. Mouhcine; R. A. Gonzalez; M. C. Liu

2005-11-30T23:59:59.000Z

65

Bright Spots in the South Carolina the Economy  

E-Print Network [OSTI]

Bright Spots in the South Carolina the Economy 2012 African American Economic Summit Doug Woodward Professor of Economics #12;Overview · Why we should worry. ­ Global economy and financial contagion. ­ U.S. economy and political uncertainty. · Why we should be happy. ­ South Carolina economy healing. · Robust

Almor, Amit

66

Ultra-bright pulsed electron beam with low longitudinal emittance  

DOE Patents [OSTI]

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.

Zolotorev, Max (Oakland, CA)

2010-07-13T23:59:59.000Z

67

Extremely High Current, High-Brightness Energy Recovery Linac  

SciTech Connect (OSTI)

Next generation ERL light-sources, high-energy electron coolers, high-power Free-Electron Lasers, powerful Compton X-ray sources and many other accelerators were made possible by the emerging technology of high-power, high-brightness electron beams. In order to get the anticipated performance level of ampere-class currents, many technological barriers are yet to be broken. BNL's Collider-Accelerator Department is pursuing some of these technologies for its electron cooling of RHIC application, as well as a possible future electron-hadron collider. We will describe work on CW, high-current and high-brightness electron beams. This will include a description of a superconducting, laser-photocathode RF gun and an accelerator cavity capable of producing low emittance (about 1 micron rms normalized) one nano-Coulomb bunches at currents of the order of one ampere average.

I. Ben-Zvi; D.S. Barton; D.B. Beavis; M. Blaskiewicz; J.M. Brennan; A. Burrill; R. Calaga; P. Cameron; X.Y. Chang; R. Connolly; D.M. Gassner; J.G. Grimes; H. Hahn; A. Hershcovitch; H.-C. Hseuh; P.D.J. Johnson; D. Kayran; J. Kewisch; R.F. Lambiase; V. Litvinenko; G.T. McIntyre; W. Meng; T.C.N. Nehring; T. Nicoletti; B. Oerter; D. Pate; J. Rank; T. Rao; T. Roser; T. Russo; J. Scaduto; Z. Segalov; K. Smith; N.W.W. Williams; K.-C. Wu; V. Yakimenko; K. Yip; A. Zaltsman; Y. Zhao; H. Bluem; A. Burger; M.D. Cole; A.J. Favale; D. Holmes; J. Rathke; T. Schultheiss; A.M.M. Todd; J.R. Delayen; L. W. Funk; P. Kneisel; H.L. Phillips; J.P. Preble

2005-05-16T23:59:59.000Z

68

Microwave generated electrodeless lamp for producing bright output  

SciTech Connect (OSTI)

A microwave generated electrodeless light source for producing a bright output comprising a lamp structure including a microwave chamber and a plasma medium-containing lamp envelope having a maximum dimension which is substantially less than a wavelength disposed therein. To provide the desired radiation output the interior of the chamber is coated with a UV-reflective material and the chamber has an opening for allowing UV radiation to exit, which is covered with a metallic mesh. The chamber is arranged to be near-resonant at a single wavelength, and the lamp envelope has a fill including mercury at an operating pressure of 1-2 atmospheres, while a power density of at least 250-300 (watts/cm/sup 3/) is coupled to the envelope to result in a relatively high deep UV output at a relatively high brightness.

Wood, Ch. H.; Ury, M. G.

1985-03-26T23:59:59.000Z

69

A statistical study of bright spot reflection parameters  

E-Print Network [OSTI]

cal Study of Bright Spot Reflection Parameters. (December 1981) David Lee Godwin, B. S. , Pepperdine University Chairman of Adv1sory Committee: Dr. T. W. Spencer A data set consisting of two seismic lines served as the basis of study... obtained from each of the seismic lines were compared to deter- mine if the presence of commercial quantities of gas could be identified. The measurement process revealed that the interval travel time measurements between the marker horizons...

Godwin, David Lee

1981-01-01T23:59:59.000Z

70

On the relationship between brightness temperature and thunderstorm evolution  

E-Print Network [OSTI]

ACKNOWLEDGEMENTS . TABLE OF CONTENTS LIST OF FIGURES . V1 INTRODUCTION DATA CONCEPTUAL MODEL OF THUNDERSTORM. . . . . BRIGHTNESS TEMPERATURE OVERVIEW . . . 10 THUNDERSTORM OVERVIEW 13 ANALYSIS k METHODS . . RESULTS . . . . . 20 CONCLUSIONS 32 REFERENCES... Introduction The impact of tropical precipitation on the global energy budget has long been a topic of investigation. Riehl and Malkus (1958) determined that latent heat released in tropical convection provided the balance of poleward transport of energy...

Rapp, Anita Denise

2013-02-22T23:59:59.000Z

71

High-Throughput, High-Precision Hot Testing Tool for High-Brightness...  

Energy Savers [EERE]

Throughput, High-Precision Hot Testing Tool for High-Brightness Light-Emitting Diode Testing High-Throughput, High-Precision Hot Testing Tool for High-Brightness Light-Emitting...

72

Structure of Bright 2MASS Galaxies: 2D Fits to the Ks-band Surface Brightness Profiles  

E-Print Network [OSTI]

The unprecedented sky coverage and photometric uniformity of the Two Micron All Sky Survey (2MASS) provides a rich resource for obtaining a detailed understanding of the galaxies populating our local (z<0.1) Universe. A full characterization of the physical structure of nearby galaxies is essential for theoretical and observational studies of galaxy evolution and structure formation. We have begun a quantified description of the internal structure and morphology of 10,000 bright (10brightness profiles using GIM2D. From our initial Monte Carlo tests on 77 galaxies drawn at random from the RC3, we find that the model derived structural parameter errors due to sky uncertainies are typically less than 10%.

Daniel H. McIntosh; Ari H. Maller; Neal Katz; Martin D. Weinberg

2002-09-01T23:59:59.000Z

73

Shining light through the Sun  

E-Print Network [OSTI]

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.

Malcolm Fairbairn; Timur Rashba; Sergey Troitsky

2007-05-19T23:59:59.000Z

74

The redshifts of bright sub-mm sources  

E-Print Network [OSTI]

One of the key goals in observational cosmology over the next few years will be to establish the redshift distribution of the recently-discovered sub-mm source population. In this brief review I discuss and summarize the redshift information which has been gleaned to date for the ~ 50 bright sub-mm sources which have been uncovered via the six main classes of survey performed with SCUBA on the JCMT over the last 2-3 years. Despite the biases inherent in some of these surveys, and the crudeness of the redshift information available in others, I conclude that all current information suggests that only 10-15 % of luminous sub-mm sources lie at z < 2, and that the median redshift of this population is z ~ 3. I suggest that such a high median redshift is arguably not unexpected given current theories designed to explain the correlation between black-hole mass and spheroid mass found at low redshift. In such scenarios, peak AGN emission is expected to correspond to, or even to cause termination of major star-formation activity in the host spheroid. In contrast, maximum dust emission is expected to occur roughly half-way through the star-formation process. Given that optical emission from bright quasars peaks at z = 2.5, dust-emission from massive ellipticals might be reasonably expected to peak at some point in the preceding ~ 1 Gyr, at z ~ 3. Confirmation or refutation of this picture requires significantly-improved redshift information on bright samples of SCUBA sources.

James S. Dunlop

2001-01-17T23:59:59.000Z

75

The Spectral Energy Distribution of Fermi bright blazars  

E-Print Network [OSTI]

(Abridged) We have conducted a detailed investigation of the broad-band spectral properties of the \\gamma-ray selected blazars of the Fermi LAT Bright AGN Sample (LBAS). By combining our accurately estimated Fermi gamma-ray spectra with Swift, radio, infra-red, optical and other hard X-ray/gamma-ray data, collected within three months of the LBAS data taking period, we were able to assemble high-quality and quasi-simultaneous Spectral Energy Distributions (SED) for 48 LBAS blazars.The SED of these gamma-ray sources is similar to that of blazars discovered at other wavelengths, clearly showing, in the usual Log $\

Abdo, A A; Ajello, M; Axelsson, M; Baldini, L; Ballet, J; Barbiellini, G; Bastieri, D; Baughman, B M; Bechtol, K; Bellazzini, R; Berenji, B; Blandford, R D; Bloom, E D; Bonamente, E; Borgland, A; Bregeon, J; Brez, A; Brigida, M; Bruel, P; Burnett, T H; Buson, S; Caliandro, G A; Cameron, R A; Caraveo, P A; Casandjian, J M; Cavazzuti, E; Cecchi, C; Celik, O; Charles, E; Chaty, S; Chekhtman, A; Chiang, J; Ciprini, S; Claus, R; Cohen-Tanugi, J; Colafrancesco, S; Cominsky, L R; Conrad, J; Costamante, L; Cutini, S; Dermer, C D; de Angelis, A; de Palma, F; Digel, S W; Silva, E do Couto e; Drell, P S; Dubois, R; Dumora, D; Farnier, C; Favuzzi, C; Fegan, S J; Focke, W B; Fortin, P; Frailis, M; Fuhrmann, L; Fukazawa, Y; Funk, S; Fusco, P; Gargano, F; Gasparrini, D; Gehrels, N; Germani, S; Giebels, B; Giglietto, N; Giommi, P; Giordano, F; Glanzman, T; Godfrey, G; Grenier, I A; Grove, J E; Guillemot, L; Guiriec, S; Hadasch, D; Hanabata, Y; Harding, A K; Hayashida, M; Hays, E; Healey, S E; Horan, D; Hughes, R E; Itoh, R; Jackson, M S; Johannesson, G; Johnson, A S; Johnson, W N; Kadler, M; Kamae, T; Katagiri, H; Kataoka, J; Kawai, N; Kerr, M; Knodlseder, J; Kocian, M L; Kuss, M; Lande, J; Latronico, L; Longo, F; Loparco, F; Lott, B; Lovellette, M N; Lubrano, P; Madejski, G M; Makeev, A; Max-Moerbeck, W; Mazziotta, M N; McConville, W; McEnery, J E; Meurer, C; Michelson, P F

2009-01-01T23:59:59.000Z

76

The Future is bright for Y-12 … 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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr MayAtmosphericNuclear SecurityTensile Strain Switched Ferromagnetism in Layered NbS2 and NbSe2DifferentThe Five FastestFuture is bright for

77

Michael Liebreich (Energy All Stars Presentation) | 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 Office of Inspector General Office0-72.pdfGeorgeDoesn't32 Master EM ProjectMemoDepartmentFY 2010 Methane(June

78

BRIGHT SOURCE SUBTRACTION REQUIREMENTS FOR REDSHIFTED 21 cm MEASUREMENTS  

SciTech Connect (OSTI)

The H I 21 cm transition line is expected to be an important probe into the cosmic dark ages and epoch of reionization. Foreground source removal is one of the principal challenges for the detection of this signal. This paper investigates the extragalactic point source contamination and how accurately bright sources ({approx}>1 Jy) must be removed in order to detect 21 cm emission with upcoming radio telescopes such as the Murchison Widefield Array. We consider the residual contamination in 21 cm maps and power spectra due to position errors in the sky model for bright sources, as well as frequency-independent calibration errors. We find that a source position accuracy of 0.1 arcsec will suffice for detection of the H I power spectrum. For calibration errors, 0.05% accuracy in antenna gain amplitude is required in order to detect the cosmic signal. Both sources of subtraction error produce residuals that are localized to small angular scales, k{sub perpendicular} {approx}> 0.05 Mpc{sup -1}, in the two-dimensional power spectrum.

Datta, A. [New Mexico Tech, Socorro, NM 87801 (United States); Bowman, J. D. [California Institute of Technology, Pasadena, CA 91125 (United States); Carilli, C. L., E-mail: adatta@nrao.ed [National Radio Astronomy Observatory, Socorro, NM 87801 (United States)

2010-11-20T23:59:59.000Z

79

Comparative Analysis of a Transition Region Bright Point with a Blinker and Coronal Bright Point Using Multiple EIS Emission Lines  

E-Print Network [OSTI]

Since their discovery twenty year ago, transition region bright points (TRBPs) have never been observed spectroscopically. Bright point properties have not been compared with similar transition region and coronal structures. In this work we have investigated three transient quiet Sun brightenings including a TRBP, a coronal BP (CBP) and a blinker. We use time-series observations of the extreme ultraviolet emission lines of a wide range of temperature T (log T = 5.3 - 6.4) from the EUV imaging spectrometer (EIS) onboard the Hinode satellite. We present the EIS temperature maps and Doppler maps, which are compared with magnetograms from the Michelson Doppler Imager (MDI) onboard the SOHO satellite. Doppler velocities of the TR BP and blinker are <,25 km s$^{-1}$, which is typical of transient TR phenomena. The Dopper velocities of the CBP were found to be < 20 km s^{-1} with exception of those measured at log T = 6.2 where a distinct bi-directional jet is observed. From an EM loci analysis we find evidenc...

Orange, N Brice; Chesny, David L; Patel, Maulik; Hesterly, Katie; Preuss, Lauren; Neira, Chantale; Turner, Niescja E

2015-01-01T23:59:59.000Z

80

Statistical isotropy violation of the CMB brightness fluctuations  

SciTech Connect (OSTI)

Certain anomalies at large angular scales in the cosmic microwave background (CMB) measured by WMAP have been suggested as possible evidence of breakdown of statistical isotropy (SI). SI violation of cosmological perturbations is a generic feature of ultralarge scale structure of the cosmos and breakdown of global symmetries. Most CMB photons free-stream to the present from the surface of last scattering. It is thus reasonable to expect statistical isotropy violation in the CMB photon distribution observed now to have originated from SI violation in the baryon-photon fluid at last scattering, in addition to anisotropy of the primordial power spectrum studied earlier in the literature. We consider the generalized anisotropic brightness distribution fluctuations, {Delta}(k-vector, n-circumflex, {tau}) (at conformal time {tau}) in contrast to the SI case where it is simply a function of |k-vector| and k-circumflex{center_dot}n-circumflex. The brightness fluctuations expanded in bipolar spherical harmonic (BipoSH) series can then be written as {Delta}{sub l{sub 1}}{sub l{sub 2}}{sup LM}(k,{tau}), where L>0 terms encode deviations from statistical isotropy. Violation of SI encoded in the present off-diagonal elements of the harmonic space correlation , equivalently, the BipoSH coefficients A{sub ll}{sup 'LM}, are then related to the generalized BipoSH brightness fluctuation terms at present. We study the evolution of {Delta}{sub l{sub 1}}{sub l{sub 2}}{sup LM}(k,{tau}) from nonzero terms {Delta}{sub l{sub 3}}{sub l{sub 4}}{sup LM}(k,{tau}{sub s}) at last scattering, in the free-streaming regime. We show that the terms with given BipoSH multipole LM evolve independently. Moreover, similar to the SI case, power at small spherical harmonic (SH) multipoles of {Delta}{sub l{sub 3}}{sub l{sub 4}}{sup LM}(k,{tau}{sub s}) at the last scattering is transferred to {Delta}{sub l{sub 1}}{sub l{sub 2}}{sup LM}(k,{tau}) at larger SH multipoles. The structural similarity is more apparent in the asymptotic expression for large values of the final SH multipoles. This formalism allows an elegant identification of any SI violation observed today to a possible origin in SI violating physics present in the baryon-photon fluid. This is illustrated for the known result of SI violating angular correlations due to the presence of a homogeneous magnetic field in the baryon-photon fluid.

Aich, Moumita; Souradeep, Tarun [Inter-University Centre for Astronomy and Astrophysics, Post Bag 4, Ganeshkhind, Pune 411 007 (India)

2010-04-15T23:59:59.000Z

Note: This page contains sample records for the topic "all-stars shine bright" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
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81

High Brightness Plasmon-Enhanced Nanostructured Gold Photoemitters  

SciTech Connect (OSTI)

Plasmonic nanohole arrays are fabricated in gold thin films by focused ion beam (FIB) lithography. Subsequent heat treatment creates sub 100 nm nanometric structures including tips, rods and flakes, all localized in the nanohole array region. The combined nanohole array and nanostructured surface comprise an efficient photoemitter. High brightness photoemission is observed from this construct using photoemission electron microscopy (PEEM), following 780 nm femtosecond (fs) laser irradiation. By comparing our observables to results of finite difference time domain (FDTD) calculations, we demonstrate that photoemission from the sub-100 nm structures is enhanced in the region of propagating surface plasmons launched from the nanohole arrays. Additionally, by tuning hole diameter and separation in the nanohole array, the photoemission intensity of nanostructured photoemitters can be controlled. We observe a photoemission enhancement of over 108, relative to photoemission from the flat region of the gold substrate at laser intensities well below the ablation threshold.

Gong, Yu; Joly, Alan G.; Kong, Lingmei; El-Khoury, Patrick Z.; Hess, Wayne P.

2014-12-30T23:59:59.000Z

82

High-current-density, high brightness cathodes for free electron laser applications  

SciTech Connect (OSTI)

This report discusses the following topics: brightness and emittance of electron beams and cathodes; general requirements for cathodes in high brightness electron guns; candidate cathode types; plasma and field emission cathodes; true field emission cathodes; oxide cathodes; lanthanum hexaborides cathodes; laser driven thermionic cathodes; laser driven photocathodes; impregnated porous tungsten dispenser cathodes; and choice of best performing cathode types.

Green, M.C. (Varian Associates, Palo Alto, CA (USA). Palo Alto Microwave Tube Div.)

1987-06-01T23:59:59.000Z

83

DUST TEMPERATURES IN THE INFRARED SPACE OBSERVATORY ATLAS OF BRIGHT SPIRAL GALAXIES1  

E-Print Network [OSTI]

DUST TEMPERATURES IN THE INFRARED SPACE OBSERVATORY ATLAS OF BRIGHT SPIRAL GALAXIES1 George J Space Observatory Atlas of Bright Spiral Galaxies. For the 71 galaxies where we had complete 60­180 lm Facility (IRTF) with IRAS far-infrared data to conclude that spiral galaxies have cold dust components

Joseph, Robert D.

84

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

E-Print Network [OSTI]

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

Tretiak, Sergei

85

Graphical Methods for Quantifying Macromolecules through Bright Field Imaging  

SciTech Connect (OSTI)

Bright ?eld imaging of biological samples stained with antibodies and/or special stains provides a rapid protocol for visualizing various macromolecules. However, this method of sample staining and imaging is rarely employed for direct quantitative analysis due to variations in sample fixations, ambiguities introduced by color composition, and the limited dynamic range of imaging instruments. We demonstrate that, through the decomposition of color signals, staining can be scored on a cell-by-cell basis. We have applied our method to Flbroblasts grown from histologically normal breast tissue biopsies obtained from two distinct populations. Initially, nuclear regions are segmented through conversion of color images into gray scale, and detection of dark elliptic features. Subsequently, the strength of staining is quanti?ed by a color decomposition model that is optimized by a graph cut algorithm. In rare cases where nuclear signal is significantly altered as a result of samplepreparation, nuclear segmentation can be validated and corrected. Finally, segmented stained patterns are associated with each nuclear region following region-based tessellation. Compared to classical non-negative matrix factorization, proposed method (i) improves color decomposition, (ii) has a better noise immunity, (iii) is more invariant to initial conditions, and (iv) has a superior computing performance

Chang, Hang; DeFilippis, Rosa Anna; Tlsty, Thea D.; Parvin, Bahram

2008-08-14T23:59:59.000Z

86

Exploring Infrared Properties of Giant Low Surface Brightness Galaxies  

E-Print Network [OSTI]

Abridged: We present analysis of Spitzer Space Telescope observations of the three low surface brightness (LSB) optical giant galaxies Malin 1, UGC 6614 and UGC 9024. Mid- and far-infrared morphology, spectral energy distributions, and integrated colors are used to derive the dust mass, dust-to-gas mass ratio, total infrared luminosity, and star formation rate (SFR). The 8 micron images indicate that polycyclic aromatic hydrocarbon molecules are present in the central regions of all three metal-poor LSB galaxies. The diffuse optical disks of Malin 1 and UGC 9024 remain undetected at mid- and far-infrared wavelengths. The dustiest of the three LSB galaxies, UGC 6614, has infrared morphology that varies significantly with wavelength. The 8 and 24 micron emission is co-spatial with H\\alpha emission previously observed in the outer ring of UGC 6614. The estimated dust-to-gas ratios, from less than 10^{-3} to 10^{-2}, support previous indications that the LSB galaxies are relatively dust poor compared to the HSB galaxies. The total infrared luminosities are approximately 1/3 to 1/2 the blue band luminosities, suggesting that old stellar populations are the primary source of dust heating in these LSB objects. The SFR estimated from the infrared data ranges ~0.01-0.88 M_sun yr^{-1}, consistent with results from optical studies.

Nurur Rahman; Justin H. Howell; George Helou; Joseph M. Mazzarella; Brent Buckalew

2007-04-11T23:59:59.000Z

87

Low Cost Lithography Tool for High Brightness LED Manufacturing  

SciTech Connect (OSTI)

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.

Andrew Hawryluk; Emily True

2012-06-30T23:59:59.000Z

88

Emission Line Properties of the Large Bright Quasar Survey  

E-Print Network [OSTI]

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.

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

2000-11-20T23:59:59.000Z

89

Numerical Optimization of Electron Beams for High Brightness x- and {gamma}-Ray Production  

SciTech Connect (OSTI)

Production of high-brightness x- and {gamma}-ray beams using Compton-scattering schemes requires high-brightness electron beams; to minimize the output photon bandwidth, the electron beam emittance must also be minimized. This emittance minimization is in conflict with the desire to increase the electron bunch charge and maximize the number of scatterers at the interaction point. We study here, using a combination of PARMELA and well-benchmarked, Compton-scattering codes, the impact of laser temporal and spatial profiles on the emittance produced in a photoinjector, and the trade-off between charge and emittance in scattered photon brightness and flux.

Gibson, David J.; Anderson, Scott G.; Hartemann, Frederic V.; Siders, Craig W.; Tremaine, Aaron M.; Barty, Christopher P. J. [Lawrence Livermore National Laboratory, Livermore, CA 94550 (United States)

2006-11-27T23:59:59.000Z

90

Batse observations of gamma-ray burst spectra; 2, peak energy evolution in bright, long bursts  

E-Print Network [OSTI]

Abstract We investigate spectral evolution in 37 bright, long gamma-ray bursts observed with the BATSE Spectroscopy Detectors. High resolution spectra are characterized by the energy of the peak of \

Ford, L A; Matteson, J L; Briggs, M S; Pendleton, G N; Preece, R D; Paciesas, W S; Teegarden, B J; Palmer, D M; Schaefer, B E; Cline, T L; Fishman, G J; Kouveliotou, C; Meegan, C A; Wilson, R B; Lestrade, J P

1994-01-01T23:59:59.000Z

91

Progress in bright ion beams for industry, medicine and fusion at LBNL  

E-Print Network [OSTI]

HI FAN 1160 LBNL-50492 Progress in Bright Ion BeamsMedicine and Fusion at LBNL Joe W. Kwan Lawrence BerkeleyAbstract Recent progresses at LBNL in developing ion beams

Kwan, Joe W.

2002-01-01T23:59:59.000Z

92

Axial Ratio of Edge-On Spiral Galaxies as a Test For Extended Bright Radio Halos  

E-Print Network [OSTI]

We use surface brightness contour maps of nearby edge-on spiral galaxies to determine whether extended bright radio halos are common. In particular, we test a recent model of the spatial structure of the diffuse radio continuum by Subrahmanyan and Cowsik which posits that a substantial fraction of the observed high-latitude surface brightness originates from an extended Galactic halo of uniform emissivity. Measurements of the axial ratio of emission contours within a sample of normal spiral galaxies at 1500 MHz and below show no evidence for such a bright, extended radio halo. Either the Galaxy is atypical compared to nearby quiescent spirals or the bulk of the observed high-latitude emission does not originate from this type of extended halo.

Singal, J; Jones, E; Dunlap, H

2015-01-01T23:59:59.000Z

93

The Acute Side Effects of Bright Light Therapy: A Placebo-Controlled Investigation  

E-Print Network [OSTI]

Despite the emergence of numerous clinical and non-clinical applications of bright light therapy (LT) in recent decades, the prevalence and severity of LT side effects have not yet been fully explicated. A few adverse LT ...

Botanov, Yevgeny; Ilardi, Stephen S.

2013-09-24T23:59:59.000Z

94

Bright High Average Power Table-top Soft X-Ray Lasers  

SciTech Connect (OSTI)

We have demonstrated the generation of bright soft x-ray laser pulses with record-high average power from compact plasma amplifiers excited by ultrafast solid state lasers. These lasers have numerous applications in nanoscience and nanotechnology.

Rocca, Jorge [Colorado State University, Fort Collins; Reagan, Brendon [Colorado State University, Fort Collins; Wernsing, Keith [Colorado State University, Fort Collins; Luther, Brad [Colorado State University, Fort Collins; Curtis, Alden [Colorado State University, Fort Collins; Nichols,, Anthony [Colorado State University, Fort Collins; Wang, Yong [Colorado State University, Fort Collins; Alessi, David [Colorado State University, Fort Collins; Martz, Dale [Colorado State University, Fort Collins; Yin, Liang [Colorado State University, Fort Collins; Wang, Shoujun [Colorado State University, Fort Collins; Berrill, Mark A [ORNL; Furch, Federico [Colorado State University, Fort Collins; Woolston, Mark [Colorado State University, Fort Collins; Patel, Dinesh [Colorado State University, Fort Collins; Marconi, Mario [Colorado State University, Fort Collins; Menoni, Carmen [Colorado State University, Fort Collins

2012-01-01T23:59:59.000Z

95

Proceedings of the third ICFA mini-workshop on high intensity, high brightness hadron accelerators  

SciTech Connect (OSTI)

The third mini-workshop on high intensity, high brightness hadron accelerators was held at Brookhaven National Laboratory on May 7-9, 1997 and had about 30 participants. The workshop focussed on rf and longitudinal dynamics issues relevant to intense and/or bright hadron synchrotrons. A plenary session was followed by four sessions on particular topics. This document contains copies of the viewgraphs used as well as summaries written by the session chairs.

Roser, T.

1997-11-01T23:59:59.000Z

96

The Deconvolution of Lunar Brightness Temperature based on Maximum Entropy Method using Chang'E-2 Microwave Data  

E-Print Network [OSTI]

A passive and multi-channel microwave sounder onboard Chang'E-2 orbiter has successfully performed microwave observation of the lunar surface and subsurface structure. Compared with Chang'E-1 orbiter, Chang'E-2 orbiter obtained more accurate and comprehensive microwave brightness temperature data which is helpful for further research. Since there is a close relationship between microwave brightness temperature data and some related properties of the lunar regolith, such as the thickness, temperature and dielectric constant, so precise and high resolution brightness temperature is necessary for such research. However, through the detection mechanism of the microwave sounder, the brightness temperature data acquired from the microwave sounder is weighted by the antenna radiation pattern, so the data is the convolution of the antenna radiation pattern and the lunar brightness temperature. In order to obtain the real lunar brightness temperature, a deconvolution method is needed. The aim of this paper is to solve...

Xing, Shuguo; Feng, Jianqing; Li, Chunlai

2014-01-01T23:59:59.000Z

97

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

E-Print Network [OSTI]

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.

M. Coleman Miller

1999-04-08T23:59:59.000Z

98

Record high-average current from a high-brightness photoinjector  

SciTech Connect (OSTI)

High-power, high-brightness electron beams are of interest for many applications, especially as drivers for free electron lasers and energy recovery linac light sources. For these particular applications, photoemission injectors are used in most cases, and the initial beam brightness from the injector sets a limit on the quality of the light generated at the end of the accelerator. At Cornell University, we have built such a high-power injector using a DC photoemission gun followed by a superconducting accelerating module. Recent results will be presented demonstrating record setting performance up to 65 mA average current with beam energies of 4-5 MeV.

Dunham, Bruce; Barley, John; Bartnik, Adam; Bazarov, Ivan; Cultrera, Luca; Dobbins, John; Hoffstaetter, Georg; Johnson, Brent; Kaplan, Roger; Karkare, Siddharth; Kostroun, Vaclav; Li Yulin; Liepe, Matthias; Liu Xianghong; Loehl, Florian; Maxson, Jared; Quigley, Peter; Reilly, John; Rice, David; Sabol, Daniel [Cornell Laboratory for Accelerator-Based Sciences and Education, Cornell University, Ithaca, New York 14853 (United States)] [Cornell Laboratory for Accelerator-Based Sciences and Education, Cornell University, Ithaca, New York 14853 (United States); and others

2013-01-21T23:59:59.000Z

99

White light emitting diode as liquid crystal display backlight ; High brightness light emitting diode as liquid crystal display backlight .  

E-Print Network [OSTI]

??The discovery of high brightness (white) light emitting diode (LED) is considered as a real threat to the current lighting industry in various applications. One (more)

Soon, Chian Myau

2007-01-01T23:59:59.000Z

100

Bright broad-band afterglows of gravitational wave bursts from mergers of binary neutron stars  

E-Print Network [OSTI]

If double neutron star mergers leave behind a massive magnetar rather than a black hole, a bright early afterglow can follow the gravitational wave burst (GWB) even if there is no short gamma-ray burst (SGRB) - GWB association or there is an association but the SGRB does not beam towards earth. Besides directly dissipating the proto-magnetar wind as suggested by Zhang, we here 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 broad-band 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 lightcurves usually peak around the magnetar spindown time scale (10^3-10^5s), reaching brightness 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 broad-band afterglows, if detected and combined with GWBs in the future, would be a probe of massive millisecond magnetars and stiff equation-of-state for nuclear matter.

He Gao; Xuan Ding; Xue-Feng Wu; Bing Zhang; Zi-Gao Dai

2013-01-03T23:59:59.000Z

Note: This page contains sample records for the topic "all-stars shine bright" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


101

Improving the photostability of bright monomeric orange and red fluorescent proteins  

E-Print Network [OSTI]

Improving the photostability of bright monomeric orange and red fluorescent proteins Nathan C illumination. Although fluorescent proteins typically bleach at a substantially slower rate than many small-molecule dyes, in many cases the lack of sufficient photostability remains an important limiting factor

Tsien, Roger Y.

102

23 Figure 3.1: Color transition from purple/maroon argillites into bright red  

E-Print Network [OSTI]

;#12;#12;#12;#12;#12;#12;#12;#12;23 Figure 3.1: Color transition from purple/maroon argillites into bright red argillites. This transition weathering, possibly sideritic layer in the lower part of the picture. The fine grained overlying red Island Section, lower maroon and purple part in red unit (level: 9 meter; Figure 3.3); south shore Gull

Kidd, William S. F.

103

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

104

Power Minimization in a Backlit TFT-LCD Display by Concurrent Brightness and Contrast Scaling  

E-Print Network [OSTI]

Brightness and Contrast Scaling (CBCS) technique for a cold cathode fluorescent lamp (CCFL) backlit TFT out that the cold cathode fluorescent lamp (CCFL) backlight of an LCD display dominates the energy be used to characterize the optical power emitted from a spot light source, such as a light bulb

Pedram, Massoud

105

Power Minimization in a Backlit TFT-LCD Display by Concurrent Brightness and Contrast Scaling  

E-Print Network [OSTI]

Brightness and Contrast Scaling (CBCS) technique for a cold cathode fluorescent lamp (CCFL) backlit TFT fluorescent lamp (CCFL) backlight of an LCD display dominates the energy consumption of the whole system [1 be used to characterize the optical power emitted from a spot light source, such as a light bulb

Pedram, Massoud

106

This bright top floor accommodation comprises: -hall with shelved storage cupboard  

E-Print Network [OSTI]

This bright top floor accommodation comprises: - hall with shelved storage cupboard - fully oak flooring in the living/dining room and varnished floorboards in the hall and double bedroom regarded restaurants and a Waitrose supermarket. Recreational facilities can be found at Warrender Swimming

Edinburgh, University of

107

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

E-Print Network [OSTI]

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

Hansen, James E.

108

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

E-Print Network [OSTI]

METHANE AND ETHANE ON THE BRIGHT KUIPER BELT OBJECT 2005 FY9 M. E. Brown,1 K. M. Barkume,1 G. A regime and by absorption due to methane in the near-infrared. The solid methane absorption lines through the methane. These long path lengths can be parameterized as a methane grain size of approximately

Brown, Michael E.

109

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

SciTech Connect (OSTI)

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.

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)

2013-07-10T23:59:59.000Z

110

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

111

The SDSS view of the Palomar-Green bright quasar survey  

SciTech Connect (OSTI)

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.

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.

2005-02-01T23:59:59.000Z

112

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

E-Print Network [OSTI]

SWIFT PANCHROMATIC OBSERVATIONS OF THE BRIGHT GAMMA-RAY BURST GRB 050525a A. J. Blustin,1 D. Band,2 ABSTRACT The bright gamma-ray burst GRB 050525a has been detected with the Swift observatory, providing. This jet break time combined with the total gamma-ray energy of the burst constrains the opening angle

Zhang, Bing

113

AN INFRARED SPACE OBSERVATORY ATLAS OF BRIGHT SPIRAL GALAXIES1 George J. Bendo,2,3,4  

E-Print Network [OSTI]

AN INFRARED SPACE OBSERVATORY ATLAS OF BRIGHT SPIRAL GALAXIES1 George J. Bendo,2,3,4 Robert D in a series we present an atlas of infrared images and photometry from 1.2 to 180 lm for a sample of bright galaxies. Using the Infrared Space Observatory (ISO), we have obtained 12 lm images and photometry at 60

Joseph, Robert D.

114

Lasers will shine in future warfare  

SciTech Connect (OSTI)

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

Kramer, David

2014-07-01T23:59:59.000Z

115

Flying on Sun Shine: Sailing in Space  

SciTech Connect (OSTI)

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.

Alhorn, Dean (NASA, Marshall Space Flight Center) [NASA, Marshall Space Flight Center

2012-03-28T23:59:59.000Z

116

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May JunDatastreamsmmcrcalgovInstrumentsruc DocumentationP-Series to User Group and Userof

117

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 CenterFranconia, Virginia:FAQ < RAPID Jump to:Seadov Pty LtdSteen, Minnesota:36052°, -97.6114217° LoadingEnergy Group LLCSun RiverSun

118

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr MayAtmosphericNuclear Security Administrationcontroller systemsBiSiteNeutron Scattering Facilities5:68 SpecialAgreementsSpecial

119

Modeling Bright Gamma-ray and Radio Emission at Fast Cloud Shocks  

E-Print Network [OSTI]

Recent observations by the Large Area Telescope (LAT) onboard the Fermi satellite have revealed bright gamma-ray emission from middle-aged supernova remnants (SNRs) inside our Galaxy. These remnants, which also possess bright non-thermal radio shells, are often found to be interacting directly with surrounding gas clouds. We explore the non-thermal emission mechanism at these dynamically evolved SNRs by constructing a hydrodynamical model. Two scenarios of particle acceleration, either a re-acceleration of Galactic cosmic rays (CRs) or an efficient nonlinear diffusive shock acceleration (NLDSA) of particles injected from downstream, are considered. Using parameters inferred from observations, our models are contrasted with the observed spectra of SNR W44. For the re-acceleration case, we predict a significant enhancement of radio and GeV emission as the SNR undergoes a transition into the radiative phase. If sufficiently strong magnetic turbulence is present in the molecular cloud, the re-acceleration scenari...

Lee, Shiu-Hang; Raymond, John C; Nagataki, Shigehiro; Slane, Patrick O; Ellison, Donald C

2015-01-01T23:59:59.000Z

120

Study of microwave/gamma-ray properties for Fermi-LAT bright AGNs  

E-Print Network [OSTI]

Blazars are a small fraction of all extragalactic sources but, unlike other objects, they are strong emitters across the entire electromagnetic spectrum. Recent data in the microwave region of the electromagnetic spectrum have become available to allow for systematic studies of blazars over large cosmological volumes. This frequency band is indeed particularly suited for the selection of blazars since at these frequencies the contamination from radio extended components with steep spectra is no longer present and the emission from the accretion process is negligible. During the first 3 months of scientific operations Fermi-LAT detected 106 bright, high-galactic latitude (| b |> 10 deg) AGNs with high significance. In this study we investigate the possible relations between the microwave and the gamma-ray emissions for Fermi-LAT detected AGNs belonging to WMAP 5th year bright source catalog.

Gasparrini, D; Giommi, P; Pittori, C; Colafrancesco, S

2009-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "all-stars shine bright" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


121

Controlling a superconducting nanowire single-photon detector using tailored bright illumination  

E-Print Network [OSTI]

We experimentally demonstrate that a superconducting nanowire single-photon detector is deterministically controllable by bright illumination. We found that bright light can temporarily make a large fraction of the nanowire length normally-conductive, can extend deadtime after a normal photon detection, and can cause a hotspot formation during the deadtime with a highly nonlinear sensitivity. In result, although based on different physics, the superconducting detector turns out to be controllable by virtually the same techniques as avalanche photodiode detectors. As demonstrated earlier, when such detectors are used in a quantum key distribution system, this allows an eavesdropper to launch a detector control attack to capture the full secret key without being revealed by to many errors in the key.

Lars Lydersen; Mohsen K. Akhlaghi; A. Hamed Majedi; Johannes Skaar; Vadim Makarov

2011-11-16T23:59:59.000Z

122

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

DOE Patents [OSTI]

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.

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

2014-02-18T23:59:59.000Z

123

$?$--PhotoZ: Photometric Redshifts by Inverting the Tolman Surface Brightness Test  

E-Print Network [OSTI]

Surface brightness is a fundamental observational parameter of galaxies. We show, for the first time in detail, how it can be used to obtain photometric redshifts for galaxies, the $\\mu$-PhotoZ method. We demonstrate that the Tolman surface brightness relation, $\\mu \\propto (1+z)^{-4}$, is a powerful tool for determining galaxy redshifts from photometric data. We develop a model using $\\mu$ and a color percentile (ranking) measure to demonstrate the $\\mu$-PhotoZ method. We apply our method to a set of galaxies from the SHELS survey, and demonstrate that the photometric redshift accuracy achieved using the surface brightness method alone is comparable with the best color-based methods. We show that the $\\mu$-PhotoZ method is very effective in determining the redshift for red galaxies using only two photometric bands. We discuss the properties of the small, skewed, non-gaussian component of the error distribution. We calibrate $\\mu_r, (r-i)$ from the SDSS to redshift, and tabulate the result, providing a simple, but accurate look up table to estimate the redshift of distant red galaxies.

Michael J. Kurtz; Margaret J. Geller; Daniel G. Fabricant; William F. Wyatt; Ian P. Dell'Antonio

2007-07-03T23:59:59.000Z

124

THE PANCHROMATIC HUBBLE ANDROMEDA TREASURY. I. BRIGHT UV STARS IN THE BULGE OF M31  

SciTech Connect (OSTI)

As part of the Panchromatic Hubble Andromeda Treasury multi-cycle program, we observed a 12' Multiplication-Sign 6.'5 area of the bulge of M31 with the WFC3/UVIS filters F275W and F336W. From these data we have assembled a sample of {approx}4000 UV-bright, old stars, vastly larger than previously available. We use updated Padova stellar evolutionary tracks to classify these hot stars into three classes: Post-AGB stars (P-AGB), Post-Early AGB (PE-AGB) stars, and AGB-manque stars. P-AGB stars are the end result of the asymptotic giant branch (AGB) phase and are expected in a wide range of stellar populations, whereas PE-AGB and AGB-manque (together referred to as the hot post-horizontal branch; HP-HB) stars are the result of insufficient envelope masses to allow a full AGB phase, and are expected to be particularly prominent at high helium or {alpha} abundances when the mass loss on the red giant branch is high. Our data support previous claims that most UV-bright sources in the bulge are likely hot (extreme) horizontal branch (EHB) stars and their progeny. We construct the first radial profiles of these stellar populations and show that they are highly centrally concentrated, even more so than the integrated UV or optical light. However, we find that this UV-bright population does not dominate the total UV luminosity at any radius, as we are detecting only the progeny of the EHB stars that are the likely source of the UV excess. We calculate that only a few percent of main-sequence stars in the central bulge can have gone through the HP-HB phase and that this percentage decreases strongly with distance from the center. We also find that the surface density of hot UV-bright stars has the same radial variation as that of low-mass X-ray binaries. We discuss age, metallicity, and abundance variations as possible explanations for the observed radial variation in the UV-bright population.

Rosenfield, Philip; Johnson, L. Clifton; Dalcanton, Julianne J.; Williams, Benjamin F.; Gilbert, Karoline M. [Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195 (United States); Girardi, Leo [Osservatorio Astronomico di Padova-INAF, Vicolo dell'Osservatorio 5, I-35122 Padova (Italy); Bressan, Alessandro [SISSA, Via Bonomea 265, 34136 Trieste (Italy); Lang, Dustin [Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544 (United States); Guhathakurta, Puragra; Dorman, Claire E. [UCO/Lick Observatory and Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064 (United States); Howley, Kirsten M. [Lawrence Livermore National Laboratory, 7000 East Avenue, Livermore, CA 94550 (United States); Lauer, Tod R.; Olsen, Knut A. G. [National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719 (United States); Bell, Eric F. [Department of Astronomy, University of Michigan, 500 Church St., Ann Arbor, MI 48109 (United States); Bianchi, Luciana [Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218 (United States); Caldwell, Nelson [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street Cambridge, MA 02138 (United States); Dolphin, Andrew [Raytheon Company, 1151 East Hermans Road, Tucson, AZ 85756 (United States); Kalirai, Jason [Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States); Larsen, Soren S. [Astronomical Institute, University of Utrecht, Princetonplein 5, 3584 CC Utrecht (Netherlands); Rix, Hans-Walter [Max Planck Institute for Astronomy, Koenigstuhl 17, D-69117 Heidelberg (Germany); and others

2012-08-20T23:59:59.000Z

125

Resilience of gated avalanche photodiodes against bright illumination attacks in quantum cryptography  

E-Print Network [OSTI]

Semiconductor avalanche photodiodes (APDs) are commonly used for single photon detection in quantum key distribution. Recently, many attacks using bright illumination have been proposed to manipulate gated InGaAs APDs. In order to devise effective counter-measures, careful analysis of these attacks must be carried out to distinguish between incorrect operation and genuine loopholes. Here, we show that correctly-operated, gated APDs are immune to continuous-wave illumination attacks, while monitoring the photocurrent for anomalously high values is a straightforward counter-measure against attacks using temporally tailored light.

Z. L. Yuan; J. F. Dynes; A. J. Shields

2011-06-14T23:59:59.000Z

126

Computational and experimental characterization of high-brightness beams for femtosecond electron imaging and spectroscopy  

SciTech Connect (OSTI)

Using a multilevel fast multipole method, coupled with the shadow imaging of femtosecond photoelectron pulses for validation, we quantitatively elucidate the photocathode, space charge, and virtual cathode physics, which fundamentally limit the spatiotemporal and spectroscopic resolution and throughput of ultrafast electron microscope (UEM) systems. We present a simple microscopic description to capture the nonlinear beam dynamics based on a two-fluid picture and elucidate an unexpected dominant role of image potential pinning in accelerating the emittance growth process. These calculations set theoretical limits on the performance of UEM systems and provide useful guides for photocathode design for high-brightness electron beam systems.

Portman, J.; Zhang, H.; Tao, Z.; Makino, K.; Berz, M.; Duxbury, P. M.; Ruan, C.-Y. [Physics and Astronomy Department, Michigan State University, East Lansing, Michigan 48824 (United States)] [Physics and Astronomy Department, Michigan State University, East Lansing, Michigan 48824 (United States)

2013-12-16T23:59:59.000Z

127

Bright Young Minds for a Clean Energy Future | 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 Delicious RankCombustion |Energyon ArmedWaste andAccess toSustainable Transportation »BiomassBrandonBrianBright Young

128

Sliding Mode Pulsed Averaging IC Drivers for High Brightness Light Emitting Diodes  

SciTech Connect (OSTI)

This project developed new Light Emitting Diode (LED) driver ICs associated with specific (uniquely operated) switching power supplies that optimize performance for High Brightness LEDs (HB-LEDs). The drivers utilize a digital control core with a newly developed nonlinear, hysteretic/sliding mode controller with mixed-signal processing. The drivers are flexible enough to allow both traditional microprocessor interface as well as other options such as on the fly adjustment of color and brightness. Some other unique features of the newly developed drivers include AC Power Factor Correction; High power efficiency; Substantially fewer external components should be required, leading to substantial reduction of Bill of Materials (BOM). Thus, the LED drivers developed in this research : optimize LED performance by increasing power efficiency and power factor. Perhaps more remarkably, the LED drivers provide this improved performance at substantially reduced costs compared to the present LED power electronic driver circuits. Since one of the barriers to market penetration for HB-LEDs (in particular white light LEDs) is cost/lumen, this research makes important contributions in helping the advancement of SSL consumer acceptance and usage.

Dr. Anatoly Shteynberg, PhD

2006-08-17T23:59:59.000Z

129

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

E-Print Network [OSTI]

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.

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

2012-02-14T23:59:59.000Z

130

A serendipitous all sky survey for bright objects in the outer solar system  

E-Print Network [OSTI]

We use seven year's worth of observations from the Catalina Sky Survey and the Siding Spring Survey covering most of the northern and southern hemisphere at galactic latitudes higher than 20 degrees to search for serendipitously imaged moving objects in the outer solar system. These slowly moving objects would appear as stationary transients in these fast cadence asteroids surveys, so we develop methods to discover objects in the outer solar system using individual observations spaced by months, rather than spaced by hours, as is typically done. While we independently discover 8 known bright objects in the outer solar system, the faintest having $V=19.8\\pm0.1$, no new objects are discovered. We find that the survey is nearly 100% efficient at detecting objects beyond 25 AU for $V\\lesssim 19.1$ ($V\\lesssim18.6$ in the southern hemisphere) and that the probability that there is one or more remaining outer solar system object of this brightness left to be discovered in the unsurveyed regions of the galactic plan...

Brown, M E; Schmidt, B P; Drake, A J; Djorgovski, S G; Graham, M J; Mahabal, A; Donalek, C; Larson, S; Christensen, E; Beshore, E; McNaught, R

2015-01-01T23:59:59.000Z

131

Bright and fast voltage reporters across the visible spectrum via electrochromic FRET (eFRET)  

E-Print Network [OSTI]

We present a palette of brightly fluorescent genetically encoded voltage indicators (GEVIs) with excitation and emission peaks spanning the visible spectrum, sensitivities from 6 - 10% Delta F/F per 100 mV, and half-maximal response times from 1 - 7 ms. A fluorescent protein is fused to an Archaerhodopsin-derived voltage sensor. Voltage-induced shifts in the absorption spectrum of the rhodopsin lead to voltage-dependent nonradiative quenching of the appended fluorescent protein. Through a library screen, we identified linkers and fluorescent protein combinations which reported neuronal action potentials in cultured rat hippocampal neurons with a single-trial signal-to-noise ratio from 6.6 to 11.6 in a 1 kHz imaging bandwidth at modest illumination intensity. The freedom to choose a voltage indicator from an array of colors facilitates multicolor voltage imaging, as well as combination with other optical reporters and optogenetic actuators.

Zou, Peng; Douglass, Adam D; Hochbaum, Daniel R; Brinks, Daan; Werley, Christopher A; Harrison, D Jed; Campbell, Robert E; Cohen, Adam E

2014-01-01T23:59:59.000Z

132

Homogeneous spectroscopic parameters for bright planet host stars from the northern hemisphere  

E-Print Network [OSTI]

Aims. In this work we derive new precise and homogeneous parameters for 37 stars with planets. For this purpose, we analyze high resolution spectra obtained by the NARVAL spectrograph for a sample composed of bright planet host stars in the northern hemisphere. The new parameters are included in the SWEET-Cat online catalogue. Methods. To ensure that the catalogue is homogeneous, we use our standard spectroscopic analysis procedure, ARES+MOOG, to derive effective temperatures, surface gravities, and metallicities. These spectroscopic stellar parameters are then used as input to compute the stellar mass and radius, which are fundamental for the derivation of the planetary mass and radius. Results. We show that the spectroscopic parameters, masses, and radii are generally in good agreement with the values available in online databases of exoplanets. There are some exceptions, especially for the evolved stars. These are analyzed in detail focusing on the effect of the stellar mass on the derived planetary mass. ...

Sousa, S G; Mortier, A; Tsantaki, M; Adibekyan, V; Mena, E Delgado; Israelian, G; Rojas-Ayala, B; Neves, V

2015-01-01T23:59:59.000Z

133

Hipparcos calibration of the peak brightness of four SNe Ia and the value of Ho  

E-Print Network [OSTI]

Hipparcos geometrical parallaxes allowed us to calibrate the Cepheid Period-Luminosity relation and to compute the true distance moduli of 17 galaxies. Among these 17 galaxies, we selected those which generated type Ia Supernovae (SNe Ia). We found NGC 5253, parent galaxy of 1895B and 1972E, IC 4182 and NGC 4536 parents of 1937C and 1981B, respectively. We used the available B-band photometry to determine the peak brightness of these four SNe Ia. We obtained = -19.65 \\pm 0.09. Then, we built a sample of 57 SNe Ia in order to plot the Hubble diagram and determine its zero-point. Our result (ZP_{B} = -3.16 \\pm 0.10) is in agreement with other determinations and allows us to derive the following Hubble constant : Ho = 50 \\pm 3 (internal) km.s^-1.Mpc^-1.

P. Lanoix

1997-12-10T23:59:59.000Z

134

Beyond the Hubble Deep Field Limiting Magnitude: Faint Galaxy Number Counts from Surface-Brightness Fluctuations  

E-Print Network [OSTI]

The faint end of the differential galaxy number counts, n(m), in the Hubble Deep Field (HDF) North has been determined for the F450W, F606W, and F814W filters by means of surface-brightness fluctuation (SBF) measurements. This technique allows us to explore n(m) beyond the limiting magnitude of the HDF, providing new, stronger constraints on the faint end of n(m). This has allowed us to test the validity of previous number count studies and to produce a new determination of the faint end of n(m) for magnitudes fainter than 28.8 in the AB system and to extend this estimate down to 31. This value represents an extension of more than two magnitudes beyond the limits of previous photometric studies. The obtained n(m) slopes are \\gamma=0.27, 0.21, and 0.26 in B_{450}, V_{606}, and I_{814}, respectively.

A. Marin-Franch; A. Aparicio

2003-05-16T23:59:59.000Z

135

The early X-ray afterglows of optically bright and dark Gamma-Ray Bursts  

E-Print Network [OSTI]

A systematical study on the early X-ray afterglows of both optically bright and dark gamma-ray bursts (B-GRBs and D-GRBs) observed by Swift has been presented. Our sample includes 25 GRBs. Among them 13 are B-GRBs and 12 are D-GRBs. Our results show that the distributions of the X-ray afterglow fluxes ($F_{X}$), the gamma-ray fluxes ($S_{\\gamma}$), and the ratio ($R_{\\gamma, X}$) for both the D-GRBs and B-GRBs are similar. The differences of these distributions for the two kinds of GRBs should be statistical fluctuation. These results indicate that the progenitors of the two kinds of GRBs are the same population. Their total energy explosions are comparable. The suppression of the optical emissions from D-GRBs should results from circumburst but not their central engine.

Yi-Qing Lin

2006-04-08T23:59:59.000Z

136

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

DOE Patents [OSTI]

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.

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

2009-10-27T23:59:59.000Z

137

4-H All-Star Constitution (Revised 3-22-14)  

E-Print Network [OSTI]

be associated with the 4-H Program of Virginia Cooperative Extension of Virginia individual and cooperative efforts. ARTICLE III - Membership The membership-economic condition, disability, or political affiliation. ARTICLE IV - Officers and Election

Liskiewicz, Maciej

138

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May Jun Jul(Summary) "of EnergyEnergyENERGYWomentheATLANTA,Fermi NationalBusinessDepartment ofEnergyDepartment of

139

STEM Women All-Stars Hit the Road | 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 Office of Inspector GeneralDepartment of Energy fromCommentsRevolving STATEMENT OF MELANIE KENDERDINE DIRECTORSTEM

140

An Atlas of H-alpha and R Images and Radial Profiles of 29 Bright Isolated Spiral Galaxies  

E-Print Network [OSTI]

Narrow-band H-alpha+[NII] and broadband R images and surface photometry are presented for a sample of 29 bright (M_B < -18) isolated S0-Scd galaxies within a distance of 48 Mpc. These galaxies are among the most isolated nearby spiral galaxies of their Hubble classifications as determined from the Nearby Galaxies Catalog (Tully 1987a).

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

2005-11-22T23:59:59.000Z

Note: This page contains sample records for the topic "all-stars shine bright" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


141

The bright Gamma-Ray Burst of February 10, 2000: a case study of an optically dark GRB  

E-Print Network [OSTI]

The bright Gamma-Ray Burst of February 10, 2000: a case study of an optically dark GRB L. Piro 1 in GRBs with optical afterglows. Subject headings: cosmology: observations | gamma-rays: bursts 1 searches of these events, known variously as \\dark GRBs", \\failed optical afterglows" (FOA), or \\gamma

Fynbo, Johan

142

THE SLOAN BRIGHT ARCS SURVEY: DISCOVERY OF SEVEN NEW STRONGLY LENSED GALAXIES FROM z = 0.66-2.94  

SciTech Connect (OSTI)

We report the discovery of seven new, very bright gravitational lens systems from our ongoing gravitational lens search, the Sloan Bright Arcs Survey (SBAS). Two of the systems are confirmed to have high source redshifts z = 2.19 and z = 2.94. Three other systems lie at intermediate redshift with z = 1.33, 1.82, 1.93 and two systems are at low redshift z = 0.66, 0.86. The lensed source galaxies in all of these systems are bright, with i-band magnitudes ranging from 19.73 to 22.06. We present the spectrum of each of the source galaxies in these systems along with estimates of the Einstein radius for each system. The foreground lens in most systems is identified by a red sequence based cluster finder as a galaxy group; one system is identified as a moderately rich cluster. In total, SBAS has now discovered 19 strong lens systems in the SDSS imaging data, 8 of which are among the highest surface brightness z {approx_equal} 2-3 galaxies known.

Kubo, Jeffrey M.; Allam, Sahar S.; Drabek, Emily; Lin, Huan; Tucker, Douglas; Buckley-Geer, Elizabeth J.; Diehl, H. Thomas; Soares-Santos, Marcelle; Hao Jiangang; Kubik, Donna; Annis, James; Frieman, Joshua A. [Center for Particle Astrophysics, Fermi National Accelerator Laboratory, Batavia, IL 60510 (United States); Wiesner, Matthew [Department of Physics, Northern Illinois University, DeKalb, IL 60115 (United States); West, Anderson [The Illinois Math and Science Academy, Aurora, IL 60506 (United States)

2010-12-01T23:59:59.000Z

143

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

E-Print Network [OSTI]

#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

Christian, Eric

144

TRIGGERED STAR FORMATION IN A BRIGHT-RIMMED CLOUD (BRC 5) OF IC 1805  

SciTech Connect (OSTI)

We report recent optical, near-infrared (NIR), and millimeter observations which have revealed some new features of the bright-rimmed cloud BRC 5 associated with W4. With slitless spectroscopy, we detected 17 H{alpha} emission stars around the cloud; 4 are near the surface of the cloud, and 1 is toward IRAS 02252+6120. NIR photometry shows that the central H{alpha} emission star, together with one bright infrared source, has large NIR excesses and Class I spectral energy distributions. These two Class I objects are associated with the 2.9 mm continuum peaks and with a bipolar outflow, and are in between two separate, elongated C{sup 18}O(J = 1-0) cores. The C{sup 18}O cores and the two Class I sources are aligned along a line at position angle {approx}240 Degree-Sign , somewhat less than perpendicular to the direction of UV radiation from the OB stars. Most of the detected H{alpha} emission stars, all T Tauri candidates, are located within {approx}3' of the cloud on the exciting star side. An estimate of the age of the stars based on a color-magnitude diagram suggests that these T Tauri candidates have ages of {approx}1 Myr or less, but are more evolved objects than the central young stellar objects. This age sequence suggests sequential star formation within the BRC 5 cloud. The {sup 13}CO(J = 1-0) emission shows three elongated structures, which indicates the asymmetric structure toward the UV incident axis. We present our exploratory simulation results by using a smoothed particle hydrodynamic code that suggests that the asymmetrical BRC 5 structure could possibly result from the evolution of a preexisting prolate molecular cloud subject to radiation-driven implosion (RDI). Our best-fit prolate cloud has an initial mass of {approx}400 M{sub Sun }, an axial ratio of {approx}1.7, and a semi-major axis of {approx}1.6 pc, pointing away from the ionization flux by an angle of 15 Degree-Sign . The simulated cloud structure not only closely matches the observed asymmetric morphological structure of BRC 5, but also reveals the possibility of the development of two major cores at the head of BRC 5. For the first time, the possibility of forming two stars by an RDI mechanism in a BRC is investigated.

Fukuda, Naoya [Faculty of Biosphere-Geosphere Science, Okayama University of Science, 1-1 Ridai-chou, Okayama 700-0005 (Japan); Miao, Jingqi [Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR (United Kingdom); Sugitani, Koji [Graduate School of Natural Sciences, Nagoya City University, Mizuho-ku, Nagoya 467-8501 (Japan); Kawahara, Kentaro [Faculty of Informatics, Okayama University of Science, 1-1 Ridai-chou, Okayama 700-0005 (Japan); Watanabe, Makoto [Department of Cosmosciences, Hokkaido University, Kita 10, Nishi 8, Kita-ku, Sapporo, Hokkaido 060-0810 (Japan); Nakano, Makoto [Faculty of Education and Welfare Science, Oita University, Oita 870-1192 (Japan); Pickles, Andrew J., E-mail: fukudany@big.ous.ac.jp [Las Cumbres Observatory Global Telescope Network, 6740 Cortona Drive, Goleta, CA 93117 (United States)

2013-08-20T23:59:59.000Z

145

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]

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

Machel, Hans

146

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]

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

White, Andrew G.

147

The HI Companions of HII Galaxies and Low Surface Brightness Dwarf Galaxies  

E-Print Network [OSTI]

I study the VLA HI survey of HII galaxies by Taylor et al. (1995, ApJS, 99, 427; 1996, ApJS, 102, 189) and the VLA HI survey of low surface brightness (LSB) dwarf galaxies by Taylor et al. (1996, ApJS, in press) to investigate the role of galaxy interactions in triggering the bursts of massive star formation seen in HII galaxies. I find that the companion rate for HII galaxies is more than twice that of LSB dwarfs (p[HII] = 0.57 p[LSB] = 0.24). I examine the completeness of the companion samples detected by the two surveys, finding that because they were observed in identical fashions, there are no relative biases to cause one sample or the other to have more companions. Thus I conclude that the difference in the number of HI rich companions is genuine, and signifies a difference in the local, small scale environments between the two types of galaxy. I search through published galaxy catalogs to study the large scale environments of the two samples, finding that at large separations, the two samples exist in very similar environments on average. The difference in companion rates between HII galaxies and LSB dwarfs supports the idea that the bursts of star formation are triggered by galaxy interactions.

Christopher L. Taylor

1996-11-18T23:59:59.000Z

148

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

DOE Patents [OSTI]

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.

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

2001-01-01T23:59:59.000Z

149

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

E-Print Network [OSTI]

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...

Abdo, A A; Aune, T; Berley, D; Chen, C; Christopher, G E; DeYoung, T; Dingus, B L; Ellsworth, R W; Gonzlez, 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; Nmethy, 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

2009-01-01T23:59:59.000Z

150

Sub-GeV flashes in $?-$ray burst afterglows as probes of underlying bright UV flares  

E-Print Network [OSTI]

Bright optical and X-ray flares have been observed in many Gamma-ray Burst (GRB) afterglows. These flares have been attributed to late activity of the central engine. In most cases the peak energy is not known and it is possible and even likely that there is a significant far-ultraviolet component. These far-ultraviolet photons escape our detection because they are absorbed by the neutral hydrogen before reaching Earth. However, these photons cross the blast wave produced by the ejecta that have powered the initial GRB. They can be inverse Compton upscattered by hot electrons within this blast wave. This process will produce a strong sub-GeV flare that follows the high energy (soft X-ray) tail of the far-UV flare but lasts much longer and can be detected by the upcoming {\\em Gamma-Ray Large Area Telescope} (GLAST) satellite. This signature can be used to probe the spectrum of the underlying far-ultraviolet flare. The extra cooling produced by this inverse Compton process can lower the X-ray emissivity of the forward shock and explain the unexpected low early X-ray flux seen in many GRBs.

Yizhong Fan; Tsvi Piran

2006-04-17T23:59:59.000Z

151

DETECTION OF AN ULTRA-BRIGHT SUBMILLIMETER GALAXY BEHIND THE SMALL MAGELLANIC CLOUD  

SciTech Connect (OSTI)

We report the discovery of a new ultra-bright submillimeter galaxy (SMG) behind the Small Magellanic Cloud (SMC). This SMG is detected as a 43.3 {+-} 8.4 mJy point source (MM J01071-7302, hereafter MMJ0107) in the 1.1 mm continuum survey of the SMC by AzTEC on the ASTE telescope. MMJ0107 is also detected in the radio (843 MHz), Herschel/SPIRE, Spitzer MIPS 24 {mu}m, all IRAC bands, Wide-field Infrared Survey Explorer, and near-infrared (J, H, K{sub S} ). We find an optical (U, B, V) source, which might be the lensing object, at a distance of 1.''4 from near-infrared and IRAC sources. Photometric redshift estimates for the SMG using representative spectral energy distribution templates show the redshifts of 1.4-3.9. We estimate total far-infrared luminosity of (0.3-2.2) Multiplication-Sign 10{sup 14} {mu}{sup -1} L{sub Sun} and a star formation rate of 5600-39, 000 {mu}{sup -1} M{sub Sun} yr{sup -1}, where {mu} is the gravitational magnification factor. This apparent extreme star formation activity is likely explained by a highly magnified gravitational lens system.

Takekoshi, Tatsuya; Minamidani, Tetsuhiro; Sorai, Kazuo; Habe, Asao [Department of Cosmosciences, Graduate School of Science, Hokkaido University, Sapporo 060-0810 (Japan); Tamura, Yoichi; Kohno, Kotaro [Institute of Astronomy, University of Tokyo, Osawa, Mitaka, Tokyo 181-0015 (Japan); Oogi, Taira [Department of Physics, Faculty of Science, Hokkaido University, Sapporo 060-0810 (Japan); Ezawa, Hajime; Komugi, Shinya; Mizuno, Norikazu; Muller, Erik; Kawamura, Akiko [Chile Observatory, National Astronomical Observatory, Mitaka, Tokyo 181-8588 (Japan); Oshima, Tai [Nobeyama Radio Observatory, National Astronomical Observatory of Japan, Minamimaki, Minamisaku, Nagano 384-1305 (Japan); Scott, Kimberly S. [North American ALMA Science Center, National Radio Astronomy Observatory, Charlottesville, VA 22903 (United States); Austermann, Jason E. [Center for Astrophysics and Space Astronomy, University of Colorado, Boulder, CO 80309 (United States); Tosaki, Tomoka [Joetsu University of Education, Joetsu, Niigata 943-8512 (Japan); Onishi, Toshikazu [Department of Physical Science, Osaka Prefecture University, Gakuen 1-1, Sakai, 599-8531 Osaka (Japan); Fukui, Yasuo [Department of Astrophysics, Nagoya University, Chikusa-ku, Nagoya 464-8602 (Japan); Matsuo, Hiroshi [Advanced Technology Center, National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588 (Japan); Aretxaga, Itziar [Instituto Nacional de Astrofisica, Optica y Electronica (INAOE), 72000 Puebla (Mexico); and others

2013-09-10T23:59:59.000Z

152

STUDIES OF THE Be STAR X PERSEI DURING A BRIGHT INFRARED PHASE  

SciTech Connect (OSTI)

We present multi-epoch photometric and spectroscopic near-infrared observations of the Be star X Persei in the JHK bands covering the wavelength range 1.08-2.35 {mu}m. Combining results from our earlier studies with the present observations, it is shown that the equivalent widths and line fluxes of the prominent H I and He I lines anti-correlate with the strength of the adjacent continuum. That is, during the span of the observations, the JHK broadband fluxes increase while the emission equivalent width values of the H I and He I lines decrease (the lines under consideration being the Paschen and Brackett lines of hydrogen and the 1.7002 {mu}m and 2.058 {mu}m lines of helium). Such an anti-correlation effect is not commonly observed in Be stars in the optical; in the infrared, this may possibly be the first reported case of such behavior. We examine different mechanisms that could possibly cause it and suggest that it could originate due to a radiatively warped, precessing circumstellar disk. It is also shown that during the course of our studies, X Per evolved to an unprecedented state of high near-IR brightness with J, H, K magnitudes of 5.20, 5.05, and 4.84, respectively.

Mathew, Blesson; Banerjee, D. P. K.; Naik, Sachindra; Ashok, N. M., E-mail: blessonmathew@gmail.com [Astronomy and Astrophysics Division, Physical Research Laboratory, Navrangapura, Ahmedabad 380 009, Gujarat (India)

2013-06-15T23:59:59.000Z

153

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

E-Print Network [OSTI]

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.

T. J. Davidge

1994-10-13T23:59:59.000Z

154

Active Detection and Imaging of Nuclear Materials with High-Brightness Gamma Rays  

SciTech Connect (OSTI)

A Compton scattering {gamma}-ray source, capable of producing photons with energies ranging from 0.1 MeV to 0.9 MeV has been commissioned and characterized, and then used to perform nuclear resonance fluorescence (NRF) experiments. The performances of the two laser systems (one for electron production, one for scattering), the electron photoinjector, and the linear accelerator are also detailed, and {gamma}-ray results are presented. The key source parameters are the size (0.01 mm{sup 2}), horizontal and vertical divergence (6 x 10 mrad{sup 2}), duration (10 ps), spectrum and intensity (10{sup 5} photons/shot). These parameters are summarized by the peak brightness, 1.5 x 10{sup 15} photons/mm{sup 2}/mrad{sup 2}/s/0.1% bandwidth, measured at 478 keV. Additional measurements of the flux as a function of the timing difference between the drive laser pulse and the relativistic photo-electron bunch, {gamma}-ray beam profile, and background evaluations are presented. These results are systematically compared to theoretical models and computer simulations. NRF measurements performed on {sup 7}Li in LiH demonstrate the potential of Compton scattering photon sources to accurately detect isotopes in situ.

Barty, C J; Gibson, D J; Albert, F; Anderson, S G; Anderson, G G; Betts, S M; Berry, R D; Fisher, S E; Hagmann, C A; Johnson, M S; Messerly, M J; Phan, H H; Semenov, V A; Shverdin, M Y; Tremaine, A M; Hartemann, F V; Siders, C W; McNabb, D P

2009-02-26T23:59:59.000Z

155

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

E-Print Network [OSTI]

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.

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

1997-02-24T23:59:59.000Z

156

SPECTRAL VARIABILITY OF FIRST BRIGHT QSOs WITH SLOAN DIGITAL SKY SURVEY OBSERVATIONS  

SciTech Connect (OSTI)

For some samples, it has been shown that spectra of QSOs with low redshift are bluer during their brighter phases. For the FIRST bright QSO sample, we assemble their spectra from Sloan Digital Sky Survey Data Release 7 (SDSS DR7) to investigate variability between the spectra from White et al. and from the SDSS for a long rest-frame time lag, up to 10 years. There are 312 radio-loud (RL) QSOs and 232 radio-quiet (RQ) QSOs in this sample, up to z {approx} 3.5. With two-epoch variation, it is found that the spectra of half of the QSOs appear redder during their brighter phases. There is no obvious difference in slope variability between subsamples of RQ and RL QSOs. This result implies that the presence of a radio jet does not affect the slope variability on 10 year timescales. The arithmetic composite difference spectrum for variable QSOs is steep blueward of {approx}2500 A. The variability for the region blueward of 2500 A is different to that for the region redward of 2500 A.

Bian Weihao; Zhang Li [Department of Physics and Institute of Theoretical Physics, Nanjing Normal University, Nanjing 210097 (China); Green, Richard [LBT Observatory, AZ 85721 (United States); Hu Chen [Key Laboratory for Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100039 (China)

2012-11-10T23:59:59.000Z

157

IDENTIFYING BREAKS AND CURVATURE IN THE FERMI SPECTRA OF BRIGHT FLAT SPECTRUM RADIO QUASARS  

SciTech Connect (OSTI)

Knowing the site of {gamma}-ray emission in active galactic nucleus jets will do much for our understanding of the physics of the source. In particular, if the emission region is close to the black hole then absorption of {gamma}-rays with photons from the broad-line region could become significant. Such absorption is predicted to produce two specific spectral breaks in the {gamma}-ray spectra of Flat Spectrum Radio Quasars (FSRQs). We test this hypothesis using three years of Fermi observations of nine bright FSRQs. A simple power-law fit to the spectrum of each source can be significantly improved by introducing a break, but the break energies are inconsistent with those predicted by the double-absorber model. In some cases the fit can be further improved by a log-parabola. In addition, by dividing the data from each source into two equal epochs we find that the best description of an object's spectrum often varies between a log-parabola and a broken power law.

Harris, J.; Daniel, M. K.; Chadwick, P. M., E-mail: j.d.harris@durham.ac.uk [Department of Physics, Durham University, South Road, Durham DH1 3LE (United Kingdom)

2012-12-10T23:59:59.000Z

158

VERITAS OBSERVATIONS OF SIX BRIGHT, HARD-SPECTRUM FERMI-LAT BLAZARS  

SciTech Connect (OSTI)

We report on VERITAS very high energy (VHE; E {>=} 100 GeV) observations of six blazars selected from the Fermi Large Area Telescope First Source Catalog (1FGL). The gamma-ray emission from 1FGL sources was extrapolated up to the VHE band, taking gamma-ray absorption by the extragalactic background light into account. This allowed the selection of six bright, hard-spectrum blazars that were good candidate TeV emitters. Spectroscopic redshift measurements were attempted with the Keck Telescope for the targets without Sloan Digital Sky Survey spectroscopic data. No VHE emission is detected during the observations of the six sources described here. Corresponding TeV upper limits are presented, along with contemporaneous Fermi observations and non-concurrent Swift UVOT and X-Ray Telescope data. The blazar broadband spectral energy distributions (SEDs) are assembled and modeled with a single-zone synchrotron self-Compton model. The SED built for each of the six blazars shows a synchrotron peak bordering between the intermediate- and high-spectrum-peak classifications, with four of the six resulting in particle-dominated emission regions.

Aliu, E.; Errando, M. [Department of Physics and Astronomy, Barnard College, Columbia University, NY 10027 (United States); Archambault, S. [Physics Department, McGill University, Montreal, QC H3A 2T8 (Canada); Arlen, T. [Department of Physics and Astronomy, University of California, Los Angeles, CA 90095 (United States); Aune, T.; Bouvier, A. [Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064 (United States); Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R. [Department of Physics, Washington University, St. Louis, MO 63130 (United States); Benbow, W. [Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645 (United States); Boettcher, M. [Astrophysical Institute, Department of Physics and Astronomy, Ohio University, Athens, OH 45701 (United States); Cesarini, A.; Connolly, M. P. [School of Physics, National University of Ireland Galway, University Road, Galway (Ireland); Ciupik, L. [Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605 (United States); Collins-Hughes, E. [School of Physics, University College Dublin, Belfield, Dublin 4 (Ireland); Cui, W. [Department of Physics, Purdue University, West Lafayette, IN 47907 (United States); Duke, C. [Department of Physics, Grinnell College, Grinnell, IA 50112-1690 (United States); Dumm, J. [School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455 (United States); Falcone, A., E-mail: afurniss@ucsc.edu, E-mail: pafortin@cfa.harvard.edu, E-mail: deirdre@llr.in2p3.fr [Department of Astronomy and Astrophysics, 525 Davey Lab, Pennsylvania State University, University Park, PA 16802 (United States); Collaboration: VERITAS Collaboration; and others

2012-11-10T23:59:59.000Z

159

Atmospheric Imaging Assembly Response Functions: Solving the Fe VIII Problems with Hinode EIS Bright Point Data  

E-Print Network [OSTI]

The Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory is a state-of-the-art imager with the potential to do unprecedented time-dependent multi-thermal analysis at every pixel on scales short compared to the radiative and conductive cooling times. Recent results, however, have identified missing spectral lines in the CHIANTI atomic physics data base, which is used to construct the instrument response functions. We have done differential emission measure analysis using simultaneous AIA and Hinode/EIS observations of six X-ray bright points. Our results not only support the conclusion that CHIANTI is incomplete near 131 angstroms, but more importantly, suggest that the peak temperature of the Fe VIII emissivity/response is likely to be closer to log T = 5.8 than to the current value of log T = 5.7. Using a revised emissivity/response calculation for Fe VIII, we find that the observed AIA 131-angstrom flux can be underestimated by about 1.25, which is smaller than previous comparisons.

Schmelz, Joan T; Kimble, Jason A; 10.1007/s11207-012-0208-1

2013-01-01T23:59:59.000Z

160

High-brightness electron beam evolution following laser-based cleaning of a photocathode  

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

Laser-based techniques have been widely used for cleaning metal photocathodes to increase quantum efficiency (QE). However, the impact of laser cleaning on cathode uniformity and thereby on electron beam quality are less understood. We are evaluating whether this technique can be applied to revive photocathodes used for high-brightness electron sources in advanced x-ray free-electron laser (FEL) facilities, such as the Linac Coherent Light Source (LCLS) at the SLAC National Accelerator Laboratory. The laser-based cleaning was applied to two separate areas of the current LCLS photocathode on July 4 and July 26, 2011, respectively. The QE was increased by 810 times upon the laser cleaning. Since the cleaning, routine operation has exhibited a slow evolution of the QE improvement and comparatively rapid improvement of transverse emittance, with a factor of 3 QE enhancement over five months, and a significant emittance improvement over the initial 23 weeks following the cleaning. Currently, the QE of the LCLS photocathode is holding constant at about 1.210?4 , with a normalized injector emittance of about 0.3???m for a 150-pC bunch charge. With the proper procedures, the laser-cleaning technique appears to be a viable tool to revive the LCLS photocathode. We present observations and analyses for the QE and emittance evolution in time following the laser-based cleaning of the LCLS photocathode, and comparison to the previous studies, the measured thermal emittance versus the QE and comparison to the theoretical model.

Zhou, F.; Brachmann, A.; Decker, F-J.; Emma, P.; Gilevich, S.; Iverson, R.; Stefan, P.; Turner, J.

2012-09-01T23:59:59.000Z

Note: This page contains sample records for the topic "all-stars shine bright" from the National Library of EnergyBeta (NLEBeta).
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to obtain the most current and comprehensive results.


161

The stellar content of the XMM-Newton Bright Serendipitous Survey  

E-Print Network [OSTI]

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.

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

2006-10-12T23:59:59.000Z

162

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

E-Print Network [OSTI]

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.

Beverly J. Smith; P. M. Harvey

1996-05-06T23:59:59.000Z

163

CONCEPTUAL DESIGN OF A BRIGHT ELECTRON INJECTOR BASED ON A LASER-DRIVEN PHOTOCATHODE RF ELECTRON GUN  

SciTech Connect (OSTI)

Conceptual design of a bright electron injector for the 1 GeV high gradient test experiment. envisaged by the LLNL-SLAC-LBL collaboration on the Relativistic Klystron is presented. The design utilizes a high-brightness laser-driven RF photocathode electron gun, similar to the pioneering LANL early studies in concept (different parametrically however), together with achromatic magnetic bunching and transport systems and diagnostics. The design is performed with attention to possible use in an FEL as well. A simple but realistic analytic model including longitudinal and transverse space-charge and RF effects and extensive computer simulation form the basis of the parametric choice for the source. These parameters are used as guides for the design of the pico-second laser system and magnetic bunching section.

Chattopadhyay, S.; Chen, Y.J.; Hopkins, D.; Kim, K.J.; Kung, A.; Miller, R.; Sessler, a.; Young, T.

1988-09-01T23:59:59.000Z

164

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

SciTech Connect (OSTI)

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.

Portman, J.; Zhang, H.; Makino, K.; Ruan, C. Y.; Berz, M.; Duxbury, P. M. [Physics and Astronomy Department, Michigan State University, East Lansing, Michigan 48824 (United States)

2014-11-07T23:59:59.000Z

165

The angular size of the Cepheid L Car: a comparison of the interferometric and surface brightness techniques  

E-Print Network [OSTI]

Recent interferometric observations of the brightest and angularly largest classical Cepheid, L Carinae, with ESO's VLT Interferometer (VLTI) have resolved with high precision the variation of its angular diameter with phase. We compare the measured angular diameter curve to the one we derive by an application of the Baade-Wesselink type infrared surface brightness technique, and find a near-perfect agreement between the two curves. The mean angular diameters of L Car from the two techniques agree very well within their total error bars (1.5 %), as do the derived distances (4 %). This result is an indication that the calibration of the surface brightness relations used in the distance determination of far away Cepheids is not affected by large biases.

P. Kervella; P. Fouque; J. Storm; W. P. Gieren; D. Bersier; D. Mourard; N. Nardetto; V. Coude du Foresto

2004-02-11T23:59:59.000Z

166

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

SciTech Connect (OSTI)

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.

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)

2013-09-15T23:59:59.000Z

167

Experimental investigation of bright spots in broadband, gated x-ray images of ignition-scale implosions on the National Ignition Facility  

SciTech Connect (OSTI)

Bright spots in the hot spot intensity profile of gated x-ray images of ignition-scale implosions at the National Ignition Facility [G. H. Miller et al., Opt. Eng. 443, (2004)] are observed. X-ray images of cryogenically layered deuterium-tritium (DT) and tritium-hydrogen-deuterium (THD) ice capsules, and gas filled plastic shell capsules (Symcap) were recorded along the hohlraum symmetry axis. Heterogeneous mixing of ablator material and fuel into the hot spot (i.e., hot-spot mix) by hydrodynamic instabilities causes the bright spots. Hot-spot mix increases the radiative cooling of the hot spot. Fourier analysis of the x-ray images is used to quantify the evolution of bright spots in both x- and k-space. Bright spot images were azimuthally binned to characterize bright spot location relative to known isolated defects on the capsule surface. A strong correlation is observed between bright spot location and the fill tube for both Symcap and cryogenically layered DT and THD ice targets, indicating the fill tube is a significant seed for the ablation front instability causing hot-spot mix. The fill tube is the predominant seed for Symcaps, while other capsule non-uniformities are dominant seeds for the cryogenically layered DT and THD ice targets. A comparison of the bright spot power observed for Si- and Ge-doped ablator targets shows heterogeneous mix in Symcap targets is mostly material from the doped ablator layer.

Barrios, M. A.; Suter, L. J.; Glenn, S.; Benedetti, L. R.; Bradley, D. K.; Collins, G. W.; Hammel, B. A.; Izumi, N.; Ma, T.; Scott, H.; Smalyuk, V. A. [Lawrence Livermore National Laboratory, Livermore, California 94550 (United States)] [Lawrence Livermore National Laboratory, Livermore, California 94550 (United States); Regan, S. P.; Epstein, R. [Laboratory for Laser Energetics, University of Rochester 250 East River Road, Rochester, New York 14623-199 (United States)] [Laboratory for Laser Energetics, University of Rochester 250 East River Road, Rochester, New York 14623-199 (United States); Kyrala, G. A. [Los Alamos National Laboratory, Los Alamos, New Mexico 87545 (United States)] [Los Alamos National Laboratory, Los Alamos, New Mexico 87545 (United States)

2013-07-15T23:59:59.000Z

168

V and R-band Galaxy Luminosity Functions and Low Surface Brightness Galaxies in the Century Survey  

E-Print Network [OSTI]

We use 64 square degrees of deep V and R CCD images to measure the local V and R band luminosity function of galaxies. The V_0<16.7 and R_0<16.2 redshift samples contain 1250 galaxies and are 98% complete. We apply k-corrections before the magnitude selection so that the completeness is to the same depth for all spectral types. The V and R faint end slopes are surprisingly identical: alpha = -1.07+-0.09. Representative Schechter function parameters for H_0=100 are: M^*_R = -20.88+-0.09, phi^*_R = 0.016+-0.003 Mpc^-3 and M^*_V = -20.23+-0.09, phi^*_V = 0.020+-0.003 Mpc^-3. The V and R local luminosity densities, j_R = (1.9+-0.6)x10^8 and j_V = (2.2+-0.7)x10^8 L_sun, are in essential agreement with the recent 2dF and SDSS determinations. All low surface brightness (LSB) galaxies fall in the large scale structure delineated by high surface brightness galaxies. The properties and surface number density of our LSB galaxies are consistent with the LSB galaxy catalog of O'Neil, Bothun & Cornell, suggesting that our samples are complete for LSB galaxies to the magnitude limits. We measure colors, surface brightnesses, and luminosities for our samples, and find strong correlations among these galaxy properties.

Warren R. Brown; Margaret J. Geller; Daniel G. Fabricant; Michael J. Kurtz

2001-05-11T23:59:59.000Z

169

Steps toward a high precision solar rotation profile: Results from SDO/AIA coronal bright point data  

E-Print Network [OSTI]

Coronal bright points (CBP) are ubiquitous small brightenings in the solar corona associated with small magnetic bipoles. We derive the solar differential rotation profile by tracing the motions of CBPs detected by the Atmospheric Imaging Assembly (AIA) instrument aboard the Solar Dynamics Observatory (SDO). We also investigate problems related to detection of coronal bright points resulting from instrument and detection algorithm limitations. To determine the positions and identification of coronal bright points we used a segmentation algorithm. A linear fit of their central meridian distance and latitude versus time was utilised to derive velocities. We obtained 906 velocity measurements in a time interval of only 2 days. The differential rotation profile can be expressed as $\\omega_{rot} = (14.47\\pm 0.10 + (0.6\\pm 1.0)\\sin^{2}(b) + (-4.7\\pm 1.7)\\sin^{4}(b))$\\degr day$^{-1}$. Our result is in agreement with other work and it comes with reasonable errors in spite of the very short time interval used. This wa...

Sudar, Davor; Braja, Roman; Saar, Steven H

2015-01-01T23:59:59.000Z

170

DISCOVERING BRIGHT QUASARS AT INTERMEDIATE REDSHIFTS BASED ON OPTICAL/NEAR-INFRARED COLORS  

SciTech Connect (OSTI)

The identification of quasars at intermediate redshifts (2.2 < z < 3.5) has been inefficient in most previous quasar surveys since the optical colors of quasars are similar to those of stars. The near-IR K-band excess technique has been suggested to overcome this difficulty. Our recent study also proposed to use optical/near-IR colors for selecting z < 4 quasars. To verify the effectiveness of this method, we selected a list of 105 unidentified bright targets with i ? 18.5 from the quasar candidates of SDSS DR6 with both SDSS ugriz optical and UKIDSS YJHK near-IR photometric data, which satisfy our proposed Y K/g z criterion and have photometric redshifts between 2.2 and 3.5 estimated from the nine-band SDSS-UKIDSS data. We observed 43 targets with the BFOSC instrument on the 2.16 m optical telescope at Xinglong station of the National Astronomical Observatory of China in the spring of 2012. We spectroscopically identified 36 targets as quasars with redshifts between 2.1 and 3.4. The high success rate of discovering these quasars in the SDSS spectroscopic surveyed area further demonstrates the robustness of both the Y K/g z selection criterion and the photometric redshift estimation technique. We also used the above criterion to investigate the possible stellar contamination rate among the quasar candidates of SDSS DR6, and found that the rate is much higher when selecting 3 < z < 3.5 quasar candidates than when selecting lower redshift candidates (z < 2.2). The significant improvement in the photometric redshift estimation when using the nine-band SDSS-UKIDSS data over the five-band SDSS data is demonstrated and a catalog of 7727 unidentified quasar candidates in SDSS DR6 selected with optical/near-IR colors and having photometric redshifts between 2.2 and 3.5 is provided. We also tested the Y K/g z selection criterion with the recently released SDSS-III/DR9 quasar catalog and found that 96.2% of 17,999 DR9 quasars with UKIDSS Y- and K-band data satisfy our criterion. With some available samples of red quasars and type II quasars, we find that 88% and 96.5% of these objects can be selected by the Y K/g z criterion, respectively, which supports our claim that using the Y K/g z criterion efficiently selects both unobscured and obscured quasars. We discuss the implications of our results on the ongoing and upcoming large optical and near-IR sky surveys.

Wu, Xue-Bing; Zuo, Wenwen; Yang, Jinyi; Yang, Qian; Wang, Feige, E-mail: wuxb@pku.edu.cn [Department of Astronomy, Peking University, Beijing 100871 (China)

2013-10-01T23:59:59.000Z

171

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

SciTech Connect (OSTI)

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.

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)

2012-12-01T23:59:59.000Z

172

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

E-Print Network [OSTI]

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.

T. J. Davidge

1998-03-24T23:59:59.000Z

173

Comparison of heliospheric current sheet structure obtained from potential magnetic field computations and from observed polarization coronal brightness  

SciTech Connect (OSTI)

The report compares the structure of the heliospheric current sheet early in Sunspot Cycle 21 as computed from the observed photospheric magnetic field with a potential field approximation, and as inferred from synoptic maps of the observed coronal polarization brightness. On most of the solar rotations compared, the two methods give essentially the same results; the basic shape of the warped current sheet and the amplitude (in solar latitude) of the displacements of the sheet from the solar equator are similar. On one rotation the current sheet computed with the potential field approximation appears to be distorted by a large photospheric region of unbalanced magnetic flux.

Wilcox, J.M.; Hundhausen, A.J.

1983-02-01T23:59:59.000Z

174

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

E-Print Network [OSTI]

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...

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

2008-01-01T23:59:59.000Z

175

HerMES: A DEFICIT IN THE SURFACE BRIGHTNESS OF THE COSMIC INFRARED BACKGROUND DUE TO GALAXY CLUSTER GRAVITATIONAL LENSING  

SciTech Connect (OSTI)

We have observed four massive galaxy clusters with the SPIRE instrument on the Herschel Space Observatory and measure a deficit of surface brightness within their central region after removing detected sources. We simulate the effects of instrumental sensitivity and resolution, the source population, and the lensing effect of the clusters to estimate the shape and amplitude of the deficit. The amplitude of the central deficit is a strong function of the surface density and flux distribution of the background sources. We find that for the current best fitting faint end number counts, and excellent lensing models, the most likely amplitude of the central deficit is the full intensity of the cosmic infrared background (CIB). Our measurement leads to a lower limit to the integrated total intensity of the CIB of I{sub 250{mu}m}>0.69{sub -0.03}{sup +0.03}(stat.){sub -0.06}{sup +0.11}(sys.) MJy sr{sup -1}, with more CIB possible from both low-redshift sources and from sources within the target clusters. It should be possible to observe this effect in existing high angular resolution data at other wavelengths where the CIB is bright, which would allow tests of models of the faint source component of the CIB.

Zemcov, M.; Cooray, A.; Bock, J.; Dowell, C. D.; Nguyen, H. T. [California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125 (United States); Blain, A. [Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH (United Kingdom); Bethermin, M. [Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu-CNRS-Universite Paris Diderot, CE-Saclay, pt courrier 131, F-91191 Gif-sur-Yvette (France); Clements, D. L. [Astrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London SW7 2AZ (United Kingdom); Conley, A.; Glenn, J. [Center for Astrophysics and Space Astronomy 389-UCB, University of Colorado, Boulder, CO 80309 (United States); Conversi, L. [Herschel Science Centre, European Space Astronomy Centre, Villanueva de la Canada, E-28691 Madrid (Spain); Farrah, D.; Oliver, S. J.; Roseboom, I. G. [Astronomy Centre, Department of Physics and Astronomy, University of Sussex, Brighton BN1 9QH (United Kingdom); Griffin, M. [School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff CF24 3AA (United Kingdom); Halpern, M.; Marsden, G. [Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1 (Canada); Jullo, E.; Kneib, J.-P. [Aix-Marseille Universite, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR7326, F-13388 Marseille (France); Richard, J., E-mail: zemcov@caltech.edu [Centre de Recherche Astronomique de Lyon, Universite Lyon 1, 9 avenue Charles Andre, F-69230 Saint-Genis Laval (France); and others

2013-06-01T23:59:59.000Z

176

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

SciTech Connect (OSTI)

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.

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)

2012-04-10T23:59:59.000Z

177

SPECTROSCOPIC CONFIRMATION OF UV-BRIGHT WHITE DWARFS FROM THE SANDAGE TWO-COLOR SURVEY OF THE GALACTIC PLANE  

SciTech Connect (OSTI)

We present spectroscopic observations confirming the identification of hot white dwarfs among UV-bright sources from the Sandage Two-color Survey of the Galactic Plane and listed in the Lanning (Lan) catalog of such sources. A subsample of 213 UV-bright Lan sources have been identified as candidate white dwarfs based on the detection of a significant proper motion. Spectroscopic observations of 46 candidates with the KPNO 2.1 m telescope confirm 30 sources to be hydrogen white dwarfs with subtypes in the DA1-DA6 range, and with one of the stars (Lan 161) having an unresolved M dwarf as a companion. Five more sources are confirmed to be helium white dwarfs, with subtypes from DB3 to DB6. One source (Lan 364) is identified as a DZ 3 white dwarf, with strong lines of calcium. Three more stars are found to have featureless spectra (to within detection limits) and are thus classified as DC white dwarfs. In addition, three sources are found to be hot subdwarfs: Lan 20 and Lan 480 are classified as sdOB, and Lan 432 is classified sdB. The remaining four objects are found to be field F star interlopers. Physical parameters of the DA and DB white dwarfs are derived from model fits.

Lepine, Sebastien [Department of Astrophysics, Division of Physical Sciences, American Museum of Natural History, Central Park West at 79th Street, New York, NY 10024 (United States); Bergeron, P. [Departement de Physique, Universite de Montreal, C.P. 6128, Succursale Centre-Ville, Montreal, QC H3C 3J7 (Canada); Lanning, Howard H., E-mail: lepine@amnh.org [National Optical Astronomical Observatories, 940 North Cherry Avenue, Tucson, AZ (United States)

2011-03-15T23:59:59.000Z

178

BRIGHT POINTS AND JETS IN POLAR CORONAL HOLES OBSERVED BY THE EXTREME-ULTRAVIOLET IMAGING SPECTROMETER ON HINODE  

SciTech Connect (OSTI)

We present observations of polar coronal hole bright points (BPs) made with the Extreme-ultraviolet Imaging Spectrometer (EIS) on the Hinode spacecraft. The data consist of raster images of BPs in multiple spectral lines from mostly coronal ions, e.g., Fe X-Fe XV. The BPs are observed for short intervals and thus the data are snapshots of the BPs obtained during their evolution. The images reveal a complex unresolved temperature structure (EIS resolution is about 2''), with the highest temperature being about 2 x 10{sup 6} K. Some BPs appear as small loops with temperatures that are highest near the top. But others are more point-like with surrounding structures. However, the thermal time evolution of the BPs is an important factor in their appearance. A BP may appear quite different at different times. We discuss one BP with an associated jet that is bright enough to allow statistically meaningful measurements. The jet Doppler speed along the line of sight is about 15-20 km s{sup -1}. Electron densities of the BPs and the jet are typically near 10{sup 9} cm{sup -3}, which implies path lengths along the line of sight on the order of a few arcsec. We also construct differential emission measure curves for two of the best observed BPs. High spatial resolution (significantly better than 1'') is required to fully resolve the BP structures.

Doschek, G. A.; Landi, E.; Warren, H. P. [Space Science Division, Naval Research Laboratory, Washington, DC 20375 (United States); Harra, L. K., E-mail: george.doschek@nrl.navy.mi [Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey, RH5 6NT (United Kingdom)

2010-02-20T23:59:59.000Z

179

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

Office of Environmental Management (EM)

emissions that cause climate change. The utility-scale PV solar story gets to the heart of what we aim to do at LPO - help launch new markets. To provide more details on this...

180

Relativistic Jets Shine through Shocks or Magnetic Reconnection?  

E-Print Network [OSTI]

Observations of gamma-ray-bursts and jets from active galactic nuclei reveal that the jet flow is characterized by a high radiative efficiency and that the dissipative mechanism must be a powerful accelerator of non-thermal particles. Shocks and magnetic reconnection have long been considered as possible candidates for powering the jet emission. Recent progress via fully-kinetic particle-in-cell simulations allows us to revisit this issue on firm physical grounds. We show that shock models are unlikely to account for the jet emission. In fact, when shocks are efficient at dissipating energy, they typically do not accelerate particles far beyond the thermal energy, and vice versa. In contrast, we show that magnetic reconnection can deposit more than 50% of the dissipated energy into non-thermal leptons as long as the energy density of the magnetic field in the bulk flow is larger than the rest mass energy density. The emitting region, i.e., the reconnection downstream, is characterized by a rough energy equipa...

Sironi, Lorenzo; Giannios, Dimitrios

2015-01-01T23:59:59.000Z

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181

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.

182

Cosmos incognito : Vera Rubin shines light on dark matter  

E-Print Network [OSTI]

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 ...

Yeager, Ashley

2008-01-01T23:59:59.000Z

183

1366 Technologies Shines a Light on American Innovation  

Broader source: Energy.gov [DOE]

An inside look at 1366 Technologies' innovative approach to solar manufacturing. Documenting how a $4 million grant from the Advanced Research Projects Agency-Energy (ARPA-E), through the Recovery Act is helping to make their ambitious goal of producing solar at the cost of coal a reality.

184

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

E-Print Network [OSTI]

. · Total chemical potential would be 1045 ergs. · This is the solar luminosity for 4000 years. = 5 x 1044 A gigantic nuclear furnace where hydrogen is built into helium at a temperature of millions of degrees Yo ho of incandescent gas A gigantic nuclear furnace where hydrogen is built into helium at a temperature of millions

Walter, Frederick M.

185

Galaxies that Shine: radiation-hydrodynamical simulations of disk galaxies  

E-Print Network [OSTI]

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 ...

Rosdahl, Joakim; Teyssier, Romain; Agertz, Oscar

2015-01-01T23:59:59.000Z

186

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

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

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

187

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 Office of InspectorConcentrating Solar PowerstoriesNrelPartnerTypePonsa, Mallorca:upGuidebook Jump to:Smarr EMCSmart

188

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

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May Jun Jul(Summary) "ofEarly Career Scientists'Montana.Program - LibbyofThisStatement ||More Emphasis onEnergy One Systemof

189

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May JunDatastreamsmmcrcalgovInstrumentsruc DocumentationP-SeriesFlickrinformationPostdocs & GraduatesReducing Dimensions:

190

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May Jun Jul(Summary) "ofEarly Career Scientists'Montana. DOCUMENTS AVAILABLEReport 2009 activitiesofHomemade blankets can make easyThe

191

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 Office of Inspector GeneralDepartment of Energyof the Americas |DOEEnergy Smooth BromeSoftwareWake ofDecathlon:

192

HAT-P-7b: An Extremely Hot Massive Planet Transiting a Bright Star in the Kepler Field  

E-Print Network [OSTI]

We report on the latest discovery of the HATNet project; a very hot giant planet orbiting a bright (V = 10.5) star with a small semi-major axis of a = 0.0377 +/- 0.0005 AU. Ephemeris for the system is P = 2.2047299 +/- 0.0000040 days, mid-transit time E = 2,453,790.2593 +/- 0.0010 (BJD). Based on the available spectroscopic data on the host star and photometry of the system, the planet has a mass of Mp = 1.78+/-^{0.08}_{0.05} MJup and radius of Rp = 1.36+/-^{0.20}_{0.09} RJup. The parent star is a slightly evolved F6 star with M = 1.47+/-^{0.08}_{-0.05} Msun,R = 1.84+/-^{0.23}_{0.11} Rsun, Teff = 6350 +/- 80 K, and metallicity [Fe/H] = +0.26 +/- 0.08. The relatively hot and large host star, combined with the close orbit of the planet, yield a very high planetary irradiance of (4.71+/-^{1.44}_{0.05}) 10^9 erg cm^{-2}s^{-1}, which places the planet near the top of the pM class of irradiated planets as defined by Fortney et al. (2007). If as predicted by Fortney et al. (2007) the planet re-radiates its absorbed energy before distributing it to the night side, the day-side temperature should be about (2730+/-^{150}_{100}) K. Because the host star is quite bright, measurement of the secondary eclipse should be feasible for ground-based telescopes, providing a good opportunity to compare the predictions of current hot Jupiter atmospheric models with the observations. Moreover, the host star falls in the field of the upcoming Kepler mission; hence extensive space-borne follow-up, including not only primary transit and secondary eclipse observations but also asteroseismology, will be possible.

A. Pal; G. A. Bakos; G. Torres; R. W. Noyes; D. W. Latham; Geza Kovacs; G. W. Marcy; D. A. Fischer; R. P. Butler; D. D. Sasselov; B. Sipocz; G. A. Esquerdo; Gabor Kovacs; R. Stefanik; J. Lazar; I. Papp; P. Sari

2008-03-05T23:59:59.000Z

193

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

E-Print Network [OSTI]

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.

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

2008-01-12T23:59:59.000Z

194

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

SciTech Connect (OSTI)

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.

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)

2010-07-20T23:59:59.000Z

195

WHAT ASTEROSEISMOLOGY CAN DO FOR EXOPLANETS: KEPLER-410A b IS A SMALL NEPTUNE AROUND A BRIGHT STAR, IN AN ECCENTRIC ORBIT CONSISTENT WITH LOW OBLIQUITY  

E-Print Network [OSTI]

We confirm the Kepler planet candidate Kepler-410A b (KOI-42b) as a Neptune-sized exoplanet on a 17.8 day, eccentric orbit around the bright (K p = 9.4) star Kepler-410A (KOI-42A). This is the third brightest confirmed ...

Van Eylen, V.

196

Quinn for New York campaign Come and intern with the Quinn for New York campaign. The campaign is looking for bright, energetic  

E-Print Network [OSTI]

Quinn for New York campaign Come and intern with the Quinn for New York campaign. The campaign is looking for bright, energetic individuals who want to learn the nuts and bolts of how a campaign works, and help elect the next Mayor of New York City. Hours are completely flexible with a small requirement

Patel, Aniruddh D.

197

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

E-Print Network [OSTI]

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

Fynbo, Johan

198

CARMA SURVEY TOWARD INFRARED-BRIGHT NEARBY GALAXIES (STING): MOLECULAR GAS STAR FORMATION LAW IN NGC 4254  

SciTech Connect (OSTI)

This study explores the effects of different assumptions and systematics on the determination of the local, spatially resolved star formation law. Using four star formation rate (SFR) tracers (H{alpha} with azimuthally averaged extinction correction, mid-infrared 24 {mu}m, combined H{alpha} and mid-infrared 24 {mu}m, and combined far-ultraviolet and mid-infrared 24 {mu}m), several fitting procedures, and different sampling strategies, we probe the relation between SFR and molecular gas at various spatial resolutions (500 pc and larger) and surface densities ({Sigma}{sub H{sub 2}})approx. 10-245 M{sub sun} pc{sup -2}) within the central {approx}6.5 kpc in the disk of NGC 4254. We explore the effect of diffuse emission using an unsharp masking technique with varying kernel size. The fraction of diffuse emission, f{sub DE}, thus determined is a strong inverse function of the size of the filtering kernel. We find that in the high surface brightness regions of NGC 4254 the form of the molecular gas star formation law is robustly determined and approximately linear ({approx}0.8-1.1) and independent of the assumed fraction of diffuse emission and the SFR tracer employed. When the low surface brightness regions are included, the slope of the star formation law depends primarily on the assumed fraction of diffuse emission. In such a case, results range from linear when the fraction of diffuse emission in the SFR tracer is f{sub DE} {approx}< 30% (or when diffuse emission is removed in both the star formation and the molecular gas tracer) to super-linear ({approx}1.4) when f{sub DE} {approx}> 50%. We find that the tightness of the correlation between gas and star formation varies with the choice of star formation tracer. The 24 {mu}m SFR tracer by itself shows the tightest correlation with the molecular gas surface density, whereas the H{alpha} corrected for extinction using an azimuthally averaged correction shows the highest dispersion. We find that for R < 0.5R{sub 25} the local star formation efficiency is constant and similar to that observed in other large spirals, with a molecular gas depletion time {tau}{sub dep} {approx} 2 Gyr.

Rahman, Nurur; Bolatto, Alberto D.; Herrera-Camus, Rodrigo; Jameson, Katherine; Vogel, Stuart N. [Department of Astronomy, University of Maryland, College Park, MD 20742 (United States); Wong, Tony; Xue Rui [Department of Astronomy, University of Illinois, Urbana-Champaign, IL 61801 (United States); Leroy, Adam K. [National Radio Astronomy Observatory, Charlottesville, VA (United States); Walter, Fabian [Max-Planck-Institute fur Astronomie, Konigstuhl 17, 69117 Heidelberg (Germany); Rosolowsky, Erik [I. K. Barber School of the Arts and Science, University of British Columbia, Kelowna, BC V1V1V7 (Canada); West, Andrew A. [Department of Astronomy, Boston University, Boston, MA 02215 (United States); Bigiel, Frank; Blitz, Leo [Department of Astronomy, University of California, Berkeley, CA 94720 (United States); Ott, Juergen, E-mail: nurur@astro.umd.edu [National Radio Astronomy Observatory, Socorro, NM 87801 (United States)

2011-04-01T23:59:59.000Z

199

With more than 90% of all stars sharing fates similar to that of the Sun, more mas-  

E-Print Network [OSTI]

al. monitored the -Cephei star HD 129929 (with a mass of 9.5 solar mass- es) for more than 21 years of convection in its central nuclear furnace drives mixing of material beyond the "classi- cal" limits cooling track--the last part of this evolution for stars of less than ~8 solar masses (M

Melbourne, Timothy

200

Detection of significant cm to sub-mm band radio and gamma-ray correlated variability in Fermi bright blazars  

E-Print Network [OSTI]

The exact location of the gamma-ray emitting region in blazars is still controversial. In order to attack this problem we present first results of a cross-correlation analysis between radio (11 cm to 0.8 mm wavelength, F-GAMMA program) and gamma-ray (0.1-300 GeV) ~ 3.5 year light curves of 54 Fermi-bright blazars. We perform a source stacking analysis and estimate significances and chance correlations using mixed source correlations. Our results reveal: (i) the first highly significant multi-band radio and gamma-ray correlations (radio lagging gamma rays) when averaging over the whole sample, (ii) average time delays (source frame: 76+/-23 to 7+/-9 days), systematically decreasing from cm to mm/sub-mm bands with a frequency dependence tau_r,gamma (nu) ~ nu^-1, in good agreement with jet opacity dominated by synchrotron self-absorption, (iii) a bulk gamma-ray production region typically located within/upstream of the 3 mm core region (tau_3mm,gamma=12+/-8 days), (iv) mean distances between the region of gamma-...

Fuhrmann, L; Chiang, J; Angelakis, E; Zensus, J A; Nestoras, I; Krichbaum, T P; Ungerechts, H; Sievers, A; Pavlidou, V; Readhead, A C S; Max-Moerbeck, W; Pearson, T J

2014-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "all-stars shine bright" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


201

Bright X-ray flares in XRF 050406 and GRB 050502B provide evidence for extended central engine activity  

E-Print Network [OSTI]

Gamma-ray bursts (GRBs) are the most powerful explosions since the Big Bang, with typical energies around 10**51 ergs. Long GRBs (duration > 2 s) are thought to signal the creation of black holes, most likely by collapse of massive stars. The detected signals from the resulting highly relativistic fireball consist of prompt gamma-ray emission (from internal shocks in the fireball) lasting for several seconds to minutes, followed by afterglow emission (from external shocks as the fireball encounters surrounding material) covering a broad range of frequencies from radio through X-rays. Because of the time needed to determine the GRB position, most afterglow measurements have been made hours after the burst, and little is known about the characteristics of afterglows in the minutes following a burst, when the afterglow emission is actively responding to inhomogeneities in both the fireball and the circumburst environment. Here we report our discovery of two bright X-ray flares peaking a few minutes after the bur...

Burrows, D N; Falcone, A; Kobayashi, S; Zhang, B; Moretti, A; O'Brien, P T; Goad, M R; Campana, S; Page, K L; Angelini, L; Barthelmy, S D; Beardmore, A P; Capalbi, M; Chincarini, G; Cummings, J; Cusumano, G; Fox, D; Giommi, P; Hill, J E; Kennea, J A; Krimm, H; Mangano, V; Marshall, F; Mszros, P; Morris, D C; Nousek, J A; Osborne, J P; Pagani, C; Perri, M; Tagliaferri, G; Wells, A A; Woosley, S; Gehrels, N

2005-01-01T23:59:59.000Z

202

MILAGRO OBSERVATIONS OF MULTI-TeV EMISSION FROM GALACTIC SOURCES IN THE FERMI BRIGHT SOURCE LIST  

SciTech Connect (OSTI)

We present the result of a search of the 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 eight-year Milagro data set. Milagro is sensitive to gamma rays with energy from 1 to 100 TeV with a peak sensitivity from 10 to 50 TeV depending on the source spectrum and declination. These results extend the observation of these sources far above the Fermi energy band. With the new analysis and additional data, multi-TeV emission is definitively observed associated with the Fermi pulsar, J2229.0+6114, in the Boomerang pulsar wind nebula (PWN). Furthermore, an extended region of multi-TeV emission is associated with the Fermi pulsar, J0634.0+1745, the Geminga pulsar.

Abdo, A. A.; Linnemann, J. T. [Department of Physics and Astronomy, Michigan State University, 3245 BioMedical Physical Sciences Building, East Lansing, MI 48824 (United States); Allen, B. T.; Chen, C. [Department of Physics and Astronomy, University of California, Irvine, CA 92697 (United States); Aune, T. [Santa Cruz Institute for Particle Physics, University of California, 1156 High Street, Santa Cruz, CA 95064 (United States); Berley, D.; Goodman, J. A. [Department of Physics, University of Maryland, College Park, MD 20742 (United States); Christopher, G. E.; Kolterman, B. E.; Mincer, A. I.; Nemethy, P. [Department of Physics, New York University, 4 Washington Place, New York, NY 10003 (United States); DeYoung, T. [Department of Physics, Pennsylvania State University, University Park, PA 16802 (United States); Dingus, B. L.; Hoffman, C. M. [Group P-23, Los Alamos National Laboratory, P.O. Box 1663, Los Alamos, NM 87545 (United States); Ellsworth, R. W. [Department of Physics and Astronomy, George Mason University, 4400 University Drive, Fairfax, VA 22030 (United States); Gonzalez, M. M. [Instituto de AstronomIa, Universidad Nacional Autonoma de Mexico, 04510 Mexico, D.F. (Mexico); Hays, E.; McEnery, J. E. [NASA Goddard Space Flight Center, Greenbelt, MD 20771 (United States); Huentemeyer, P. H. [Department of Physics, University of Utah, Salt Lake City, UT 84112 (United States); Morgan, T. [Department of Physics, University of New Hampshire, Morse Hall, Durham, NH 03824 (United States)] (and others)

2009-08-01T23:59:59.000Z

203

Sub-GeV flashes in $\\gamma-$ray burst afterglows as probes of underlying bright UV flares  

E-Print Network [OSTI]

Bright optical and X-ray flares have been observed in many Gamma-ray Burst (GRB) afterglows. These flares have been attributed to late activity of the central engine. In most cases the peak energy is not known and it is possible and even likely that there is a significant far-ultraviolet component. These far-UV photons escape our detection because they are absorbed by the neutral hydrogen before reaching Earth. However, these photons cross the blast wave produced by the ejecta that have powered the initial GRB. They can be inverse Compton upscattered by hot electrons within this blast wave. This process will produce a strong sub-GeV flare that can be detected by the upcoming {\\em Gamma-Ray Large Area Telescope} (GLAST) satellite. This signature can be used to probe the spectrum of the underlying far-ultraviolet flare. The extra cooling produced by this inverse Compton process can lower the X-ray emissivity of the forward shock and explain the unexpected low early X-ray flux seen in many GRBs.

Fan, Y; Fan, Yizhong; Piran, Tsvi

2006-01-01T23:59:59.000Z

204

Resolved Massive Star Clusters in the Milky Way and its Satellites: Brightness Profiles and a Catalogue of Fundamental Parameters  

E-Print Network [OSTI]

[Abridged]: We present a database of structural and dynamical properties for 153 spatially resolved star clusters (50 "young massive clusters" and 103 old globulars) in the Milky Way, the Large and Small Magellanic Clouds, and the Fornax dwarf spheroidal. This database complements and extends others in the literature, such as those of Harris, and Mackey & Gilmore. By fitting a number of models to the clusters' density profiles, we derive various characteristic surface brightnesses and radii; central potentials, velocity dispersions, and escape velocities; total luminosities, masses, and binding energies; phase-space densities and relaxation timescales; and ``kappa-space'' parameters. Population-synthesis models are used to predict intrinsic (B-V) colors, reddenings, and V-band mass-to-light ratios for the same 153 clusters plus another 63 globulars in the Milky Way, and we compare these predictions to the observed quantities where available. These results are intended to serve as the basis for future investigations of structural correlations and the fundamental plane of massive star clusters, including especially comparisons between the systemic properties of young and old clusters. We also address the question of what structural model fits each cluster best, and argue that the extended halos known to characterize many Magellanic Cloud clusters may be examples of the generic envelope structure of self-gravitating star clusters, not just transient features associated strictly with young age.

Dean E. McLaughlin; Roeland P. van der Marel

2006-05-04T23:59:59.000Z

205

Testing Models of Intrinsic Brightness Variations in Type Ia Supernovae, and their Impact on Measuring Cosmological Parameters  

E-Print Network [OSTI]

For spectroscopically confirmed type Ia supernovae we evaluate models of intrinsic brightness variations with detailed data/Monte-Carlo comparisons of the dispersion in the following quantities: Hubble-diagram scatter, color difference (B-V-c) between the true B-V color and the fitted color (c) from the SALT-II light curve model, and photometric redshift residual. The data sample includes 251 ugriz light curves from the 3-season Sloan Digital Sky Survey-II, and 191 griz light curves from the Supernova Legacy Survey 3-year data release. We find that the simplest model of a wavelength independent (coherent) scatter is not adequate, and that to describe the data the intrinsic scatter model must have wavelength-dependent variations. We use Monte Carlo simulations to examine the standard approach of adding a coherent scatter term in quadrature to the distance-modulus uncertainty in order to bring the reduced chi2 to unity when fitting a Hubble diagram. If the light curve fits include model uncertainties with the c...

Kessler, Richard; Marriner, John; Betoule, Marc; Brinkmann, Jon; Cinabro, David; El-Hage, Patrick; Frieman, Joshua; Jha, Saurabh; Mosher, Jennifer; Schneider, Donald P

2012-01-01T23:59:59.000Z

206

The SCUBA Local Universe Galaxy Survey II. 450 micron data - evidence for cold dust in bright IRAS Galaxies  

E-Print Network [OSTI]

This is the second in a series of papers presenting results from the SCUBA Local Universe Galaxy Survey. In our first paper we provided 850 micron flux densities for 104 galaxies selected from the IRAS Bright Galaxy Sample and we found that the 60, 100 micron (IRAS) and 850 micron (SCUBA) fluxes could be adequately fitted by emission from dust at a single temperature. In this paper we present 450 micron data for the galaxies. With the new data, the spectral energy distributions of the galaxies can no longer be fitted with an isothermal dust model - two temperature components are now required. Using our 450 micron data and fluxes from the literature, we find that the 450/850 micron flux ratio for the galaxies is remarkably constant and this holds from objects in which the star formation rate is similar to our own Galaxy, to ultraluminous infrared galaxies (ULIRGS) such as Arp 220. The only possible explanation for this is if the dust emissivity index for all of the galaxies is ~2 and the cold dust component has a similar temperature in all galaxies (20-21 K). The dust masses estimated using the new temperatures are higher by a factor ~2 than those determined previously using a single temperature. This brings the gas-to-dust ratios of the IRAS galaxies into agreement with those of the Milky Way and other spiral galaxies which have been intensively studied in the submm.

Loretta Dunne; Stephen Eales

2001-06-20T23:59:59.000Z

207

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

E-Print Network [OSTI]

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.

Tod E. Strohmayer; Craig B. Markwardt

1999-03-03T23:59:59.000Z

208

High brightness microwave lamp  

DOE Patents [OSTI]

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.

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

2003-09-09T23:59:59.000Z

209

Bright Lights, Black Leather  

E-Print Network [OSTI]

?" The older man paused, smoothing his fingers over his mustache. "Mike Orgell," he said simply. Sonny froze at the mention of that name. Mike Orgell. Five months had passed since the last time he'd heard it spoken; hearing it again now was like reopening...'re lovers." "Yeah? So?" Sonny demanded. "Whats that got to do with Mike Orgell?" "You made your feelings known about Orgell, and Evan Freed... their sexual orientations." Martin held the detective's stare. "Your reaction to Henderson, to what he said...

LaSalle, R.

1995-01-01T23:59:59.000Z

210

BRIGHT 22 ?m EXCESS CANDIDATES FROM THE WISE ALL-SKY CATALOG AND THE HIPPARCOS MAIN CATALOG  

SciTech Connect (OSTI)

In this paper, we present a catalog that includes 141 bright candidates (?10.27 mag, V band) showing an excess of infrared (IR) at 22 ?m. Of these 141 candidates, 38 stars are known IR-excess stars or disks, 23 stars are double or multiple stars, and 4 are Be stars while the remaining more than 70 stars are identified as 22 ?m excess candidates in our work. The criterion for selecting candidates is K{sub s} [22]{sub ?m}. All these candidates are selected from the Wide-field Infrared Survey Explorer all-sky data cross-correlated with the Hipparcos main catalog and the likelihood-ratio technique is employed. Considering the effect of background, we introduce the IRAS 100 ?m level to exclude the high background. We also estimate the coincidence probability of these sources. In addition, we present the optical to mid-IR spectral energy distributions and optical images for all the candidates, and give the observed optical spectra of six stars with the National Astronomical Observatories, Chinese Academy of Sciences' 2.16 m telescope. To measure for the amount of dust around each star, the fractional luminosity is also provided. We also test whether our method of selecting IR-excess stars can be used to search for extra-solar planets; we cross-match our catalog with known IR-excess stars with planets but found no matches. Finally, we give the fraction of stars showing excess IR for different spectral types of main-sequence stars.

Wu, Chao-Jian; Wu, Hong; Lam, Man-I; Yang, Ming; Gao, Liang [National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012 (China); Wen, Xiao-Qing [Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012 (China); Li, Shuo [Department of Astronomy, Peking University, Beijing 100871 (China); Zhang, Tong-Jie [Department of Astronomy, Beijing Normal University, Beijing 100875 (China)

2013-10-01T23:59:59.000Z

211

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

SciTech Connect (OSTI)

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.

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)

2013-10-20T23:59:59.000Z

212

A COMPREHENSIVE STUDY OF GAMMA-RAY BURST OPTICAL EMISSION. III. BRIGHTNESS DISTRIBUTIONS AND LUMINOSITY FUNCTIONS OF OPTICAL AFTERGLOWS  

SciTech Connect (OSTI)

We continue our systematic statistical study on optical afterglow data of gamma-ray bursts (GRBs). We present the apparent magnitude distributions of early optical afterglows at different epochs (t = 10{sup 2} s, 10{sup 3} s, and 1 hr) for the optical light curves of a sample of 93 GRBs (the global sample) and for sub-samples with an afterglow onset bump or a shallow decay segment. For the onset sample and shallow decay sample we also present the brightness distribution at the peak time t{sub p} and break time t{sub b}, respectively. All the distributions can be fit with Gaussian functions. We further perform Monte Carlo simulations to infer the luminosity function of GRB optical emission at the rest-frame time 10{sup 3} s, t{sub p}, and t{sub b}. Our results show that a single power-law luminosity function is adequate to model the data with indices -1.40 {+-} 0.10, -1.06 {+-} 0.16, and -1.54 {+-} 0.22. Based on the derived rest-frame 10{sup 3} s luminosity function, we generate the intrinsic distribution of the R-band apparent magnitude M{sub R} at the observed time 10{sup 3} s post-trigger, which peaks at M{sub R} = 22.5 mag. The fraction of GRBs whose R-band magnitude is fainter than 22 mag and 25 mag and at the observer time 10{sup 3} s are {approx}63% and {approx}25%, respectively. The detection probabilities of the optical afterglows with ground-based robotic telescopes and the UV-Optical Telescope on board Swift are roughly consistent with that inferred from this intrinsic M{sub R} distribution, indicating that the variations of the dark GRB fraction among the samples with different telescopes may be due to the observational selection effect, although the existence of an intrinsically dark GRB population cannot be ruled out.

Wang Xianggao; Liang Enwei; Li Liang; Lu Ruijing [Department of Physics and GXU-NAOC Center for Astrophysics and Space Sciences, Guangxi University, Nanning 530004 (China); Wei Jianyan [National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012 (China); Zhang Bing, E-mail: lew@gxu.edu.cn [Department of Physics and Astronomy, University of Nevada, Las Vegas, NV 89154 (United States)

2013-09-10T23:59:59.000Z

213

TESTING MODELS OF INTRINSIC BRIGHTNESS VARIATIONS IN TYPE Ia SUPERNOVAE AND THEIR IMPACT ON MEASURING COSMOLOGICAL PARAMETERS  

SciTech Connect (OSTI)

For spectroscopically confirmed Type Ia supernovae we evaluate models of intrinsic brightness variations with detailed data/Monte Carlo comparisons of the dispersion in the following quantities: Hubble-diagram scatter, color difference (B - V - c) between the true B - V color and the fitted color (c) from the SALT-II light curve model, and photometric redshift residual. The data sample includes 251 ugriz light curves from the three-season Sloan Digital Sky Survey-II and 191 griz light curves from the Supernova Legacy Survey 3 year data release. We find that the simplest model of a wavelength-independent (coherent) scatter is not adequate, and that to describe the data the intrinsic-scatter model must have wavelength-dependent variations resulting in a {approx}0.02 mag scatter in B - V - c. Relatively weak constraints are obtained on the nature of intrinsic scatter because a variety of different models can reasonably describe this photometric data sample. We use Monte Carlo simulations to examine the standard approach of adding a coherent-scatter term in quadrature to the distance-modulus uncertainty in order to bring the reduced {chi}{sup 2} to unity when fitting a Hubble diagram. If the light curve fits include model uncertainties with the correct wavelength dependence of the scatter, we find that this approach is valid and that the bias on the dark energy equation-of-state parameter w is much smaller ({approx}0.001) than current systematic uncertainties. However, incorrect model uncertainties can lead to a significant bias on the distance moduli, with up to {approx}0.05 mag redshift-dependent variation. This bias is roughly reduced in half after applying a Malmquist bias correction. For the recent SNLS3 cosmology results, we estimate that this effect introduces an additional systematic uncertainty on w of {approx}0.02, well below the total uncertainty. This uncertainty depends on the choice of viable scatter models and the choice of supernova (SN) samples, and thus this small w-uncertainty is not guaranteed in future cosmology results. For example, the w-uncertainty for SDSS+SNLS (dropping the nearby SNe) increases to {approx}0.04.

Kessler, Richard; Frieman, Joshua A. [Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637 (United States)] [Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637 (United States); Guy, Julien; Betoule, Marc; El-Hage, Patrick [Laboratoire de Physique Nucleaire et des Hautes Energies, UPMC Univ. Paris 6, UPD Univ. Paris 7, CNRS IN2P3, 4 place Jussieu, F-75005 Paris (France)] [Laboratoire de Physique Nucleaire et des Hautes Energies, UPMC Univ. Paris 6, UPD Univ. Paris 7, CNRS IN2P3, 4 place Jussieu, F-75005 Paris (France); Marriner, John [Center for Particle Astrophysics, Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510 (United States)] [Center for Particle Astrophysics, Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510 (United States); Brinkmann, Jon [Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349 (United States)] [Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349 (United States); Cinabro, David [Department of Physics, Wayne State University, Detroit, MI 48202 (United States)] [Department of Physics, Wayne State University, Detroit, MI 48202 (United States); Jha, Saurabh [Department of Physics and Astronomy, Rutgers University, 136 Frelinghuysen Road, Piscataway, NJ 08854 (United States)] [Department of Physics and Astronomy, Rutgers University, 136 Frelinghuysen Road, Piscataway, NJ 08854 (United States); Mosher, Jennifer [Department of Physics and Astronomy, University of Pennsylvania, 203 South 33rd Street, Philadelphia, PA 19104 (United States)] [Department of Physics and Astronomy, University of Pennsylvania, 203 South 33rd Street, Philadelphia, PA 19104 (United States); Schneider, Donald P., E-mail: kessler@kicp.uchicago.edu [Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802 (United States)

2013-02-10T23:59:59.000Z

214

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

SciTech Connect (OSTI)

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.

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

2013-09-10T23:59:59.000Z

215

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

E-Print Network [OSTI]

We reanalyze Fermi/LAT gamma-ray spectra of bright blazars with a higher photon statistics than in previous works and with new Pass 7 data representation. In the spectra of the brightest blazar 3C 454.3 and possibly of 4C +21.35 we detect breaks at 5 GeV (in the rest frame) associated with the photon-photon pair production absorption by He II Lyman continuum (LyC). We also detect confident breaks at 20 GeV associated with hydrogen LyC both in the individual spectra and in 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 hydrogen Ly complex over He II, rather small detected optical depth, and the break energy consistent with the head-on collisions with LyC photons imply that the gamma-ray emission site is located within the BLR, but most of the BLR emission comes from a flat disk-like structure ...

Stern, Boris E

2014-01-01T23:59:59.000Z

216

HAT-P-34b-HAT-P-37b: FOUR TRANSITING PLANETS MORE MASSIVE THAN JUPITER ORBITING MODERATELY BRIGHT STARS  

SciTech Connect (OSTI)

We report the discovery of four transiting extrasolar planets (HAT-P-34b-HAT-P-37b) with masses ranging from 1.05 to 3.33 M{sub J} and periods from 1.33 to 5.45 days. These planets orbit relatively bright F and G dwarf stars (from V = 10.16 to V = 13.2). Of particular interest is HAT-P-34b which is moderately massive (3.33 M{sub J}), has a high eccentricity of e = 0.441 {+-} 0.032 at a period of P = 5.452654 {+-} 0.000016 days, and shows hints of an outer component. The other three planets have properties that are typical of hot Jupiters.

Bakos, G. A.; Hartman, J. D.; Csubry, Z.; Penev, K. [Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544 (United States); Torres, G.; Beky, B.; Latham, D. W.; Bieryla, A.; Quinn, S.; Szklenar, T.; Esquerdo, G. A.; Noyes, R. W. [Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (United States); Buchhave, L. A. [Niels Bohr Institute, University of Copenhagen, DK-2100, Denmark, and Centre for Star and Planet Formation, Natural History Museum of Denmark, DK-1350 Copenhagen (Denmark); Kovacs, G. [Konkoly Observatory, Budapest (Hungary); Shporer, A. [LCOGT, 6740 Cortona Drive, Santa Barbara, CA (United States); Fischer, D. A. [Astronomy Department, Yale University, New Haven, CT (United States); Johnson, J. A. [California Institute of Technology, Department of Astrophysics, MC 249-17, Pasadena, CA (United States); Howard, A. W.; Marcy, G. W. [Department of Astronomy, University of California, Berkeley, CA (United States); Sato, B., E-mail: gbakos@astro.princeton.edu [Department of Earth and Planetary Sciences, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551 (Japan); and others

2012-07-15T23:59:59.000Z

217

Metal Abundances and Kinematics of Bright Metal-Poor Giants Selected from the LSE Survey: Implications for the Metal-Weak Thick Disk  

E-Print Network [OSTI]

We report medium-resolution (1-2 A) spectroscopy and broadband (UBV) photometry for a sample of 39 bright stars (the majority of which are likely to be giants) selected as metal-deficient candidates from an objective-prism survey concentrating on Galactic latitudes below |b| = 30 deg, the LSE survey of Drilling & Bergeron. Although the primary purpose of the LSE survey was to select OB stars (hence the concentration on low latitudes), the small number of bright metal-deficient giant candidates noted during this survey provide interesting information on the metal-weak thick disk (MWTD) population. The kinematics of the LSE giants indicate the presence of a rapidly rotating population, even at quite low metallicity. We consider the distribution of orbital eccentricity of the LSE giants as a function of [Fe/H], and conclude that the local fraction (i.e., within 1 kpc from the Sun) of metal-poor stars that might be associated with the MWTD is on the order of 30%-40% at abundances below [Fe/H] = -1.0. Contrary to recent analyses of previous (much larger) samples of non-kinematically selected metal-poor stars, we find that this relatively high fraction of local metal-poor stars associated with the MWTD may extend to metallicities below [Fe/H] = -1.6, much lower than had been considered before. We identify a subsample of 11 LSE stars that are very likely to be members of the MWTD, based on their derived kinematics; the lowest metallicity among these stars is [Fe/H] = -2.35. Implications of these results for the origin of the MWTD and for the formation of the Galaxy are considered. (abridged)

Timothy C. Beers; John S. Drilling; Silvia Rossi; Masashi Chiba; Jaehyon Rhee; Birgit Fuhrmeister; John E. Norris; Ted von Hippel

2002-04-19T23:59:59.000Z

218

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]

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

219

RESONANCES IN THE PHOTOIONIZATION CROSS SECTIONS OF ATOMIC NITROGEN SHAPE THE FAR-ULTRAVIOLET SPECTRUM OF THE BRIGHT STAR IN 47 TUCANAE  

SciTech Connect (OSTI)

The far-ultraviolet spectrum of the Bright Star (B8 III) in 47 Tuc (NGC 104) shows a remarkable pattern: it is well fit by local thermodynamic equilibrium models at wavelengths longer than Ly{beta}, but at shorter wavelengths it is fainter than the models by a factor of two. A spectrum of this star obtained with the Far Ultraviolet Spectroscopic Explorer shows broad absorption troughs with sharp edges at 995 and 1010 A and a deep absorption feature at 1072 A; none of which are predicted by the models. We find that these features are caused by resonances in the photoionization cross sections of the first and second excited states of atomic nitrogen (2s {sup 2} 2p {sup 3} {sup 2} D {sup 0} and {sup 2} P {sup 0}). Using cross sections from the Opacity Project, we can reproduce these features, but only if we use the cross sections at their full resolution, rather than the resonance-averaged cross sections usually employed to model stellar atmospheres. These resonances are strongest in stellar atmospheres with enhanced nitrogen and depleted carbon abundances, a pattern typical of post-asymptotic giant branch stars.

Dixon, William V.; Chayer, Pierre, E-mail: dixon@stsci.edu, E-mail: chayer@stsci.edu [Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States)

2013-08-10T23:59:59.000Z

220

Resonances in the Photoionization Cross Sections of Atomic Nitrogen Shape the Far-Ultraviolet Spectrum of the Bright Star in 47 Tucanae  

E-Print Network [OSTI]

The far-ultraviolet (FUV) spectrum of the Bright Star (B8 III) in 47 Tuc (NGC 104) shows a remarkable pattern: it is well fit by LTE models at wavelengths longer than Lyman beta, but at shorter wavelengths it is fainter than the models by a factor of two. A spectrum of this star obtained with the Far Ultraviolet Spectroscopic Explorer (FUSE) shows broad absorption troughs with sharp edges at 995 and 1010 A and a deep absorption feature at 1072 A, none of which are predicted by the models. We find that these features are caused by resonances in the photoionization cross sections of the first and second excited states of atomic nitrogen (2s$^2$ 2p$^3$ $^2$D$^0$ and $^2$P$^0$). Using cross sections from the Opacity Project, we can reproduce these features, but only if we use the cross sections at their full resolution, rather than the resonance-averaged cross sections usually employed to model stellar atmospheres. These resonances are strongest in stellar atmospheres with enhanced nitrogen and depleted carbon ab...

Dixon, William V

2013-01-01T23:59:59.000Z

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221

XMM-Newton Data Processing for Faint Diffuse Emission: Proton Flares, Exposure Maps and Report on EPIC MOS1 Bright CCDs Contamination  

E-Print Network [OSTI]

We present a study of the in-flight performance of the XMM-Newton EPIC MOS and pn detectors, with focus on the influence of proton flares and vignetting on the data. The very wide range in the conditions of our sample of observations, in terms of exposure length and background intensities, allows the detection of a wide range in the spectra of the proton flares, in contrast to the hard-spectrum flares proposed by Lumb et al.(2002) or Read et al.(2003) We also find an up to now unreported contamination in the low energy regime (E<0.5 keV) of the MOS1 observations, consisting of a significant increase in the measured intensities in two CCDs at the edges of the detector. This contamination yields in "bright CCDs" in the observations. Its effect must be taken into account for the study of sources detected in the affected CCDs. With respect to vignetting, we present in-flight exposure maps and we propose a method to repeat this calculation for user-definable energy bands. All the results presented here, have the goal to enable the study of very faint extended sources with XMM-Newton, like nearby galactic X-ray halos or the soft X-ray background.

J. Pradas; J. Kerp

2005-08-04T23:59:59.000Z

222

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

SciTech Connect (OSTI)

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.

Wong, Tony; Xue, Rui [Department of Astronomy, University of Illinois, Urbana, IL 61801 (United States)] [Department of Astronomy, University of Illinois, Urbana, IL 61801 (United States); Bolatto, Alberto D.; Fisher, David B.; Vogel, Stuart N. [Department of Astronomy, University of Maryland, College Park, MD 20742 (United States)] [Department of Astronomy, University of Maryland, College Park, MD 20742 (United States); Leroy, Adam K. [National Radio Astronomy Observatory, Charlottesville, VA 22903 (United States)] [National Radio Astronomy Observatory, Charlottesville, VA 22903 (United States); Blitz, Leo [Department of Astronomy, University of California, Berkeley, CA 94720 (United States)] [Department of Astronomy, University of California, Berkeley, CA 94720 (United States); Rosolowsky, Erik [Department of Physics, University of Alberta, Edmonton, AB T6G 2E1 (Canada)] [Department of Physics, University of Alberta, Edmonton, AB T6G 2E1 (Canada); Bigiel, Frank [Institut fr theoretische Astrophysik, Zentrum fr Astronomie der Universitt Heidelberg, Albert-Ueberle Str. 2, D-69120 Heidelberg (Germany)] [Institut fr theoretische Astrophysik, Zentrum fr Astronomie der Universitt Heidelberg, Albert-Ueberle Str. 2, D-69120 Heidelberg (Germany); Ott, Jrgen [National Radio Astronomy Observatory, Socorro, NM 87801 (United States)] [National Radio Astronomy Observatory, Socorro, NM 87801 (United States); Rahman, Nurur [Department of Physics, C1 Lab 140, University of Johannesburg, P.O. Box 524, Auckland Park, Johannesburg 2006 (South Africa)] [Department of Physics, C1 Lab 140, University of Johannesburg, P.O. Box 524, Auckland Park, Johannesburg 2006 (South Africa); Walter, Fabian [Max-Planck-Institut fr Astronomie, Konigstuhl 17, D-69117 Heidelberg (Germany)] [Max-Planck-Institut fr Astronomie, Konigstuhl 17, D-69117 Heidelberg (Germany)

2013-11-01T23:59:59.000Z

223

KEPLER-21b: A 1.6 R{sub Earth} PLANET TRANSITING THE BRIGHT OSCILLATING F SUBGIANT STAR HD 179070  

SciTech Connect (OSTI)

We present Kepler observations of the bright (V = 8.3), oscillating star HD 179070. The observations show transit-like events which reveal that the star is orbited every 2.8 days by a small, 1.6 R{sub Earth} object. Seismic studies of HD 179070 using short cadence Kepler observations show that HD 179070 has a frequency-power spectrum consistent with solar-like oscillations that are acoustic p-modes. Asteroseismic analysis provides robust values for the mass and radius of HD 179070, 1.34 {+-} 0.06 M{sub Sun} and 1.86 {+-} 0.04 R{sub Sun }, respectively, as well as yielding an age of 2.84 {+-} 0.34 Gyr for this F5 subgiant. Together with ground-based follow-up observations, analysis of the Kepler light curves and image data, and blend scenario models, we conservatively show at the >99.7% confidence level (3{sigma}) that the transit event is caused by a 1.64 {+-} 0.04 R{sub Earth} exoplanet in a 2.785755 {+-} 0.000032 day orbit. The exoplanet is only 0.04 AU away from the star and our spectroscopic observations provide an upper limit to its mass of {approx}10 M{sub Earth} (2{sigma}). HD 179070 is the brightest exoplanet host star yet discovered by Kepler.

Howell, Steve B. [National Optical Astronomy Observatory, Tucson, AZ 85719 (United States); Rowe, Jason F.; Bryson, Stephen T. [NASA Ames Research Center, Moffett Field, CA 94035 (United States); Quinn, Samuel N. [Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138 (United States); Marcy, Geoffrey W.; Isaacson, Howard [Department of Astronomy, University of California, Berkeley, CA 94720 (United States); Ciardi, David R. [NASA Exoplanet Science Institute/Caltech, Pasadena, CA 91125 (United States); Chaplin, William J.; Elsworth, Yvonne [School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT (United Kingdom); Metcalfe, Travis S. [High Altitude Observatory and Scientific Computing Division, National Center for Atmospheric Research, Boulder, CO 80307 (United States); Monteiro, Mario J. P. F. G. [Centro de Astrofisica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto (Portugal); Appourchaux, Thierry [Institut d'Astrophysique Spatiale, Universite Paris XI-CNRS (UMR8617), Batiment 121, 91405 Orsay Cedex (France); Basu, Sarbani [Department of Astronomy, Yale University, New Haven, CT 06520-8101 (United States); Creevey, Orlagh L. [Departamento de Astrofisica, Universidad de La Laguna, E-38206 La Laguna, Tenerife (Spain); Gilliland, Ronald L. [Space Telescope Science Institute, Baltimore, MD 21218 (United States); Quirion, Pierre-Olivier [Canadian Space Agency, 6767 Boulevard de l'Aeroport, Saint-Hubert, QC, J3Y 8Y9 (Canada); Stello, Denis [Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006 (Australia); Kjeldsen, Hans; Christensen-Dalsgaard, Joergen [Department of Physics and Astronomy, Aarhus University, DK-8000 Aarhus C (Denmark); Garcia, Rafael A. [Laboratoire AIM, CEA/DSM-CNRS-Universite Paris Diderot-IRFU/SAp, 91191 Gif-sur-Yvette Cedex (France); and others

2012-02-20T23:59:59.000Z

224

Low surface brightness galaxies rotation curves in the low energy limit of $R^n$ gravity : no need for dark matter?  

E-Print Network [OSTI]

We investigate the possibility that the observed flatness of the rotation curves of spiral galaxies is not an evidence for the existence of dark matter haloes, but rather a signal of the breakdown of General Relativity. To this aim, we consider power - law fourth order theories of gravity obtained by replacing the scalar curvature $R$ with $f(R) = f_0 R^n$ in the gravity Lagrangian. We show that, in the low energy limit, the gravitational potential generated by a pointlike source may be written as $\\Phi(r) \\propto r^{-1} \\left [ 1 + (r/r_c)^{\\beta} \\right ]$ with $\\beta$ a function of the slope $n$ of the gravity Lagrangian and $r_c$ a scalelength depending on the gravitating system properties. In order to apply the model to realistic systems, we compute the modified potential and the rotation curve for spherically symmetric and for thin disk mass distributions. It turns out that the potential is still asymptotically decreasing, but the corrected rotation curve, although not flat, is higher than the Newtonian one thus offering the possibility to fit rotation curves without dark matter. To test the viability of the model, we consider a sample of 15 low surface brightness (LSB) galaxies with combined HI and H$\\alpha$ measurements of the rotation curve extending in the putative dark matter dominated region. We find a very good agreement between the theoretical rotation curve and the data using only stellar disk and interstellar gas.

S. Capozziello; V. F. Cardone; A. - Troisi

2006-12-13T23:59:59.000Z

225

spring 2013research scholarship, Collaboration, and Outreach at northwestern University Centerpiece  

E-Print Network [OSTI]

Office for Research, 633 Clark Street Evanston, Illinois 60208 This publication is available online atVolume 12, Number 2 CONTENTS 2 Connecting the Dots Between Art and Science 20 Solar: Shingle Style 6 Science-field infrared view of an "emission" nebula that shines by its own light. The bright orange nebula is situated

Shahriar, Selim

226

Bright Ideas in Solar Energy  

E-Print Network [OSTI]

like fossil fuels or hydrogen, storage is impractical justenergy as hydrogen gas (a common energy storage mechanism,rich hydrogen provides a good solution to energy storage

Melville, Jo

2014-01-01T23:59:59.000Z

227

Bright prospects for lighting retrofits  

SciTech Connect (OSTI)

Great potential for energy savings can be found in the alleys, hallways and stairwells of multifamily buildings, but this potential is not always easy to realize. This article discusses the solution to common problems, retrofitting mistakes, retrofitting for savings, replacements for incandescent bulbs, better exit lights. 1 fig., 1 tab.

Hasterok, L. [Wisconsin Energy Conservation Corp., Madison, WI (United States)

1995-09-01T23:59:59.000Z

228

Bright Ideas in Solar Energy  

E-Print Network [OSTI]

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.

Melville, Jo

2014-01-01T23:59:59.000Z

229

Bright Ideas in Solar Energy  

E-Print Network [OSTI]

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,

Melville, Jo

2014-01-01T23:59:59.000Z

230

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

E-Print Network [OSTI]

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 measured bias of an LBG sample. Comparing this against recent results in the literature at fainter (sub-$L_{*}$) limiting magnitudes, and with simple models describing the relationship between LBGs and dark matter haloes, we discuss the implications on the implied environments and nature of LBGs. It seems that the brightest LBGs (in contrast with the majority sub-$L_{*}$ population), have clustering properties, and host dark matter halo masses, that are consistent with them being progenitors of the most massive galaxies today.

Paul D. Allen; Leonidas A. Moustakas; Gavin Dalton; Emily MacDonald; Chris Blake; Lee Clewley; Catherine Heymans; Gary Wegner

2005-05-02T23:59:59.000Z

231

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

SciTech Connect (OSTI)

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.

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

2014-01-01T23:59:59.000Z

232

Sir --Your Editorial "Time for Japan to shine?" (Nature 427, 763; 2004) clearly  

E-Print Network [OSTI]

that the United States and Japan refuse a direct and objective comparison of the technical assets of the European the necessity of building ITER, formerly the International Thermonuclear Experimental Reactor. But I must say of the JT-60 tokamak to achieve critical science on the way to Demo, the engineering prototype reactor

233

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

E-Print Network [OSTI]

installations. This California Solar Initiative has the2. CALIFORNIAS SOLAR PROGRAMS Californias PV market isramifications, both for Californias new solar programs and

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

2006-01-01T23:59:59.000Z

234

NOAH WARDRIP-FRUIN, JOSH CARROLL, ROBERT COOVER, SHAWN GREENLEE, ANDREW MCCLAIN E BEN "SASCHA" SHINE  

E-Print Network [OSTI]

that cut across the field from the art world through com- mercial video games. It does this by unfolding

California at Santa Cruz, University of

235

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

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

was on integrated devices for solar fuels. Solar fuels devices are akin to photovoltaics (solar cells), except instead of light being converted to electricity in an external...

236

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

SciTech Connect (OSTI)

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].

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

2006-01-01T23:59:59.000Z

237

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

E-Print Network [OSTI]

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.

E. T. Vishniac

1993-09-28T23:59:59.000Z

238

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

Energy Savers [EERE]

Energy-Saving LEDs on Utah Starry Nights June 11, 2010 - 4:27pm Addthis Thanks to an Energy Efficiency and Conservation Block Grant (EECBG), Utah is replacing streetlights...

239

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

SciTech Connect (OSTI)

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.

Wallace,B.

2005-01-01T23:59:59.000Z

240

Fuel Cells Shine a Light on the Last Endeavour Space Shuttle 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:YearRound-UpHeatMulti-Dimensional ElectricalEnergy FrozenNovember 10, 2014 2014

Note: This page contains sample records for the topic "all-stars shine bright" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


241

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

Office of Environmental Management (EM)

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May Jun Jul(Summary) " ,"ClickPipelinesProvedDecember 2005Department ofDOE AccidentWasteZoneEnergy

242

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 Fuels DataCombinedDepartment2015Services »of(BENEFIT) -Archived EACFailures |

243

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:YearRound-Up from the Gridwise Global1WasteRecoveryAwardsFacilityEnergy SharedSherryEnergy

244

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May Jun Jul(Summary) "ofEarly Careerlumens_placard-green.epsEnergy1.pdfMarket | Department ofSecretaryMarch 26,Researcha

245

Shining Stars of Solar: Meet Three SunShot Postdoctoral Award Recipients  

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 Office of Inspector GeneralDepartment of Energyof the Americas |DOE Former Worker/EnergyFractureSheratonWho Are Making

246

Axion mechanism of Sun luminosity and TSI variations: light shining through the solar radiation zone  

E-Print Network [OSTI]

It is shown that the hypothesis of the axion mechanism of Sun luminosity suggesting that the solar axion-like particles are born in the core of the Sun and may be efficiently converted back into $\\gamma$-quanta in the magnetic field of the solar overshoot tachocline is physically relevant. As a result, it is also shown that the intensity variations of the $\\gamma$-quanta of axion origin, induced by the magnetic field variations in the tachocline, directly cause the Sun luminosity and total solar irradiance (TSI) variations and eventually characterize the active and quiet states of the Sun. Within the framework of this mechanism estimations of the strength of the axion coupling to a photon ($g_{a \\gamma} = 7.2 \\cdot 10^{-11} GeV^{-1}$) and the axion-like particle mass ($m_a \\sim 10^{-5} eV$) have been obtained. It is also shown that the claimed axion parameters do not contradict any known experimental and theoretical model-independent limitations.

Rusov, V D; Sharf, I V; Eingorn, M V; Smolyar, V P; Vlasenko, D S; Zelentsova, T N; Linnik, E P; Beglaryan, M E

2014-01-01T23:59:59.000Z

247

Weatherization Shines in California: Weatherization Assistance Close-Up Fact Sheet  

SciTech Connect (OSTI)

California demonstrates its commitment to technology and efficiency through the Weatherization Program. Weatherization uses advanced technologies and techniques to reduce energy costs for low-income families by increasing the energy efficiency of their homes.

D& R International

2001-10-10T23:59:59.000Z

248

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

E-Print Network [OSTI]

INVESTIGATION OF PHOTOVOLTAIC COST TRENDS IN CALIFORNIA RyanInvestigation of Photovoltaic Cost Trends in California,cost of customer-sited, grid-connected solar photovoltaic (

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

2006-01-01T23:59:59.000Z

249

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 Rank EERE:YearRound-UpHeatMulti-Dimensionalthe10IO1OP001 Letter Report:Life-CycleDuty Vehicle Pathways

250

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:YearRound-UpHeat Pump Models |Conduct,Final9: DraftPlant,Community'Into SavingsStudents |Department

251

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:YearRound-UpHeat Pump Models |Conduct,Final9:Department of Energy at 24/7

252

Shining Energy-saving LEDs on Utah Starry Nights | 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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May Jun Jul(Summary) "ofEarlyEnergyDepartment of Energy U.S. DepartmentCommitment for aIn this update,Sherry Stout -Stephen

253

Sandia National Laboratories: producing power when the sun isn't shining  

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr MayAtmosphericNuclear Security Administration the1developmentturbine bladelifetimepower-to-gasproduce and deliver

254

Shining Light on the Fleeting Interactions of Single Molecules | U.S. DOE  

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr MayAtmosphericNuclear SecurityTensile Strain Switched5 IndustrialIsadore Perlman,BiosScience (SC) RegionalRegionals »

255

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr MayAtmosphericNuclear SecurityTensile Strain Switched5 IndustrialIsadore Perlman,BiosScience (SC) RegionalRegionals »Office ofOfficeof

256

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)

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.

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)

2013-09-01T23:59:59.000Z

257

The XMM-Newton X-ray Spectra of the Most X-ray Luminous Radio-quiet ROSAT Bright Survey-QSOs: A Reference Sample for the Interpretation of High-redshift QSO Spectra  

E-Print Network [OSTI]

We present the broadband X-ray properties of four of the most X-ray luminous (L_X >= 10^{45} erg/s in the 0.5-2 keV band) radio-quiet QSOs found in the ROSAT Bright Survey. This uniform sample class, which explores the extreme end of the QSO luminosity function, exhibits surprisingly homogenous X-ray spectral properties: a soft excess with an extremely smooth shape containing no obvious discrete features, a hard power law above 2 keV, and a weak narrow/barely resolved Fe K-alpha fluorescence line for the three high signal-to-noise ratio (S/N) spectra. The soft excess can be well fitted with only a soft power law. No signatures of warm or cold intrinsic absorbers are found. The Fe K-alpha centroids and the line widths indicate emission from neutral Fe (E=6.4 keV) originating from cold material from distances of only a few light days or further out. The well-constrained equivalent widths (EW) of the neutral Fe lines are higher than expected from the X-ray Baldwin effect which has been only poorly constrained at...

Krumpe, Mirko; Markowitz, Alex; Corral, Amalia; 10.1088/0004-637X/725/1/1

2010-01-01T23:59:59.000Z

258

High Brightness Beam Applications: Energy Recovered Linacs  

SciTech Connect (OSTI)

In the first part of the paper some general statements are made regarding applications suitable for utilizing energy recovered linacs (ERLs) by contrasting their potential performance to that of single pass linacs and storage rings. As a result of their potential for extremely good beam quality in combination with high average beam current, ERLs have been used and considered as drivers of both free electron laser and partially coherent photon sources, from THz through X-rays; as a suitable technology for high energy electron cooling; and as a continuous or semi-continuous electron beam source for high energy colliders. At present, beam requirements tend to be highly matched to end use requirements. By reviewing some of the many examples which have either been reduced to practice, or are being explored presently, one can develop an appreciation for the wide range of parameters being considered in ERL applications.

Geoffrey A. Krafft

2005-09-01T23:59:59.000Z

259

Bright and dark sides of computational intelligence  

E-Print Network [OSTI]

positive and negative values and the resulted neuron excitation net is calculated as a sum of products mapping and both systems internally operate within a limited signal range between zero and one. In general of incoming signals multiplied by weights: xw=net ii n =1i (1) k net out netk-+1 1 =f(net)=out exp Fig. 2

Wilamowski, Bogdan Maciej

260

Sustainable > DI BrightGreen January 2010  

E-Print Network [OSTI]

Management > Intelligent Buildings > IT Systems > Plug-in and Electric Vehicles > Smart Grids and Meters Heat and Power Plants > District Heating and Cooling > Energy Efficient Building Materials > Energy > Heat Pumps > Industrial Equipment and Processes > Lighting > Low-Energy Water Supply > Material

Note: This page contains sample records for the topic "all-stars shine bright" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


261

Bright Center of the Universe Issue 9  

E-Print Network [OSTI]

to the individual authors or artists on publication SB BO BPI r Table of Contents The Boy Who's Worth a Ship 1 Z. P. Florian-Art by Horian Cup, Candle and Life 12 Marti Bcnidick-filk Sun Jumper 13 Marti Benedict (Filk) Chivalry '. M4 Kate Bickcl-art by Tara Ludmcr... Siobhan DG Silver Bell 106 Marti Benidict (Filk) The Slavers 107 Marti Benedict (Filk) The Woven Ocean 108 Selinthia Avenchesca The Glitter and the Glory 109 Jason ClarkeArt by Florian Sea of Stars 124 Marti Benedict (Filk) The Star Weaver 125 Marti...

Multiple Contributors

1999-01-01T23:59:59.000Z

262

Bright Center of the Universe Issue 3  

E-Print Network [OSTI]

Schneider 1 Art By Z.P Florian What Child Is This? M.Treleaven 7 Corellian WordPuzzle Wendy Schwartz 13 The (Not Quite) Complete History of Red Flight LouiseTurner 14 The Journey Back Marcia Brin 17 Being There (Poem) YvetteGhilan 23 Call It aTie Z. P.... Florian 25 Art by Z.P. Florian Tercel Marty nn 31 You Love Him, Don't You? C. Anson 32 Art by Z.P. Florian Three Stories (Poem) YvetteGhilan 56 Art by Z.P. Florian Trial Run Chris Callahan 57 Art by Z.P. Florian Talisman Carolyn Gollcdge 62 Art by Martynn...

Multiple Contributors

1993-01-01T23:59:59.000Z

263

PublicationsmailagreementNo.40014024 Bright minds and  

E-Print Network [OSTI]

with the study. See story page 8. PHOTO: UVic PHOTO SerViceS New report sounds the alarm on climate change that use innovative en- gineering, data communications and sensor technologies to gather continuous real

Victoria, University of

264

Bright Center of the Universe Issue 8  

E-Print Network [OSTI]

Threepio's weight already?" "Well, I think they can only manage so much when they work together. Fierell is a very good Jedi tutor but even she seemed a little taken aback. Han?" "Mmm?" The sound was muffled as he muzzled at her throat. "You know...

Multiple Contributors

1998-01-01T23:59:59.000Z

265

The Future Looks Bright for Teraflop Computing  

SciTech Connect (OSTI)

Wouldnt 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 Nvidias 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 dont exist in todays market. The development of Matlab plug-ins is a very positive sign for the future of GPGPUs and is indicative of Nvidias sense of where the market is headed.

Farber, Rob

2007-11-01T23:59:59.000Z

266

PublicationsmailagreementNo.40014024 Bright minds and  

E-Print Network [OSTI]

Microfluidics and Nanofluid- ics, describes the focus of his research as "plumbing, but not on the conventional

Victoria, University of

267

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May JunDatastreamsmmcrcalgovInstrumentsruc Documentation RUC : XDCResearch Relatedcontent ARM Data Discovery Browse Datanarrowband

268

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May JunDatastreamsmmcrcalgovInstrumentsruc Documentation RUC : XDCResearch Relatedcontent ARM Data Discovery Browsenarrowband

269

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May JunDatastreamsmmcrcalgovInstrumentsruc Documentation RUC : XDCResearch Relatedcontent ARM Data DiscoverygovMeasurementsMicrowave

270

average brightness of moonlight as a function  

E-Print Network [OSTI]

figures from Roach & Gordon: `The Light of the Night Sky' (1973) #12;many different reactions contribute to nightglow: tables from Roach & Gordon: `The Light of the Night Sky' (1973) nightglow lines can be very upper atmosphere emissions (Roach & Gordon 1973) aurora is transient emission driven by high

Peletier, Reynier

271

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 Home5b9fcbce19 NoPublic Utilities Address: 160Benin: EnergyBoston Area SolarConnecticut: EnergyVermont: EnergyBrigham CityEnergy

272

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 Home5b9fcbce19 NoPublic Utilities Address: 160Benin: EnergyBoston Area SolarConnecticut: EnergyVermont: EnergyBrigham

273

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 Office of InspectorConcentrating SolarElectricEnergyCTBarre BiomassTHIS PAGE ISJump to:Blackfeet Nation Wind

274

Sandia National Laboratories: high-brightness LED  

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr MayAtmosphericNuclear Security Administration the1development Sandia,evaluatingfull moduleresources gridstandbyhigh

275

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 Office of Inspector GeneralDepartmentAUDIT REPORT Americium/CuriumSunways JV JumpBraselco Jump to:

276

Sandia National Laboratories: BrightSource  

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr MayAtmosphericNuclear Security Administration the1 -the Mid-Infrared0Energy Advanced NuclearBASFBoeing Patent Awarded

277

THE XMM-NEWTON X-RAY SPECTRA OF THE MOST X-RAY LUMINOUS RADIO-QUIET ROSAT BRIGHT SURVEY-QSOs: A REFERENCE SAMPLE FOR THE INTERPRETATION OF HIGH-REDSHIFT QSO SPECTRA  

SciTech Connect (OSTI)

We present the broadband X-ray properties of four of the most X-ray luminous (L{sub X} {>=} 10{sup 45} erg s{sup -1} in the 0.5-2 keV band) radio-quiet QSOs found in the ROSAT Bright Survey. This uniform sample class, which explores the extreme end of the QSO luminosity function, exhibits surprisingly homogenous X-ray spectral properties: a soft excess with an extremely smooth shape containing no obvious discrete features, a hard power law above 2 keV, and a weak narrow/barely resolved Fe K{alpha} fluorescence line for the three high signal-to-noise ratio (S/N) spectra. The soft excess can be well fitted with only a soft power law. No signatures of warm or cold intrinsic absorbers are found. The Fe K{alpha} centroids and the line widths indicate emission from neutral Fe (E = 6.4 keV) originating from cold material from distances of only a few light days or further out. The well-constrained equivalent widths (EW) of the neutral Fe lines are higher than expected from the X-ray Baldwin effect which has been only poorly constrained at very high luminosities. Taking into account our individual EW measurements, we show that the X-ray Baldwin effect flattens above L{sub X} {approx} 10{sup 44} erg s{sup -1} (2-10 keV band) where an almost constant (EW) of {approx}100 eV is found. We confirm the assumption of having very similar X-ray active galactic nucleus properties when interpreting stacked X-ray spectra. Our stacked spectrum serves as a superb reference for the interpretation of low S/N spectra of radio-quiet QSOs with similar luminosities at higher redshifts routinely detected by XMM-Newton and Chandra surveys.

Krumpe, M.; Markowitz, A. [University of California, San Diego, Center for Astrophysics and Space Sciences, 9500 Gilman Drive, La Jolla, CA 92093-0424 (United States); Lamer, G. [Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam (Germany); Corral, A., E-mail: mkrumpe@ucsd.ed [INAF-Osservatorio Astronomico di Brera, via Brera 28, 20121 Milan (Italy)

2010-12-20T23:59:59.000Z

278

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)

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.

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)

2009-10-19T23:59:59.000Z

279

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

E-Print Network [OSTI]

Force. The Task Force is comprised of representatives from local and federal government agencies (USDA on electricity costs). Because of increasing population and urban sprawl trends (1,100 inhabitants per mi2

Gilbes, Fernando

280

Searching for life where the sun don't shine : explorations to the seafloors of Earth and Europa  

E-Print Network [OSTI]

Hydrothermal vents on Earth's seafloor host entire ecosystems that live off energy from chemosynthesis rather than photosynthesis. This energy process uses chemical reactions between metals and hot gases from inside Earth's ...

Fitzpatrick, Garret R

2012-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "all-stars shine bright" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


281

Growing Cutting-edge X-ray Optics  

SciTech Connect (OSTI)

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

Ray Conley

2012-11-30T23:59:59.000Z

282

Growing Cutting-edge X-ray Optics  

ScienceCinema (OSTI)

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

Ray Conley

2013-07-17T23:59:59.000Z

283

SUSTAINABLE AND HOLISTIC INTEGRATION OF ENERGY STORAGE AND SOLAR...  

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

SUSTAINABLE AND HOLISTIC INTEGRATION OF ENERGY STORAGE AND SOLAR PV (SHINES) SUSTAINABLE AND HOLISTIC INTEGRATION OF ENERGY STORAGE AND SOLAR PV (SHINES) Funding Number:...

284

High brightness diode-pumped organic solid-state laser  

E-Print Network [OSTI]

High-power, diffraction-limited organic solid-state laser operation has been achieved in a vertical external cavity surface-emitting organic laser (VECSOL), pumped by a low-cost compact blue laser diode. The diode-pumped VECSOLs were demonstrated with various dyes in a polymer matrix, leading to laser emissions from 540 nm to 660 nm. Optimization of both the pump pulse duration and output coupling leads to a pump slope efficiency of 11% for a DCM based VECSOLs. We report output pulse energy up to 280 nJ with 100 ns long pump pulses, leading to a peak power of 3.5 W in a circularly symmetric, diffraction-limited beam.

Zhao, Zhuang; Nafa, Malik; Chnais, Sbastien; Forget, Sbastien

2015-01-01T23:59:59.000Z

285

Light Wars: The Bright Future of Laser Weapons  

E-Print Network [OSTI]

currently the highest power solid-state laser in the world,funding the Joint High Power Solid-State Laser (JHPSSL)Solid-state lasers and chemical lasers have certain limitations on the power

Mistry, Hemma

2009-01-01T23:59:59.000Z

286

High brightness photocathode injector for BNL Accelerator Test Facility  

SciTech Connect (OSTI)

An analysis of the BNL photocathode (1-1/2 cell) Gun'' operating at 2856 MHZ, is presented. The beam parameters including beam energy, and emittance are calculated. A review of the Gun parameters and full input and output of our analysis with program PARMELA, is given in Section 2, some of our results, are tabulated. The phase plots and the beam parameters, at downstream ends of the elements, from cathode through the cavity, first cell is labeled as element 2; and second cell is labeled as element to the exit of the GUN. The analysis was made for 3 cases, using three different initial values (EO) for the average accelerating gradient (MV/m), for comparison with previous works. For illustration, the field obtained with program SUPERFISH is given, and conclusion including shunt impedances obtained for the cells and the cavity are given in Section 6. PARMELA is used as a standard design program at ATF. At the request of some of the users of program PARMELA, this request of some of the users of program PARMELA, this report include and illustrates some of our data, in the input and output format of the program PARMELA. 5 refs., 7 figs., 3 tabs.

Parsa, Z.; Young, L.

1990-01-01T23:59:59.000Z

287

Bright-White Beetle Scales Optimise Multiple Scattering of Light  

E-Print Network [OSTI]

-linear Spectroscopy (LENS), Universita` di Firenze, 50019 Sesto Fiorentino (FI), Italy, 2Istituto Nazionale di Ottica (CNR-INO), Largo Fermi 6, 50125 Firenze (FI), Italy, 3Universita` di Firenze, Dipartimento di Fisica e Astronomia, 50019 Sesto Fiorentino (FI), Italy...

Burresi, Matteo; Cortese, Lorenzo; Pattelli, Lorenzo; Kolle, Mathias; Vukusic, Peter; Wiersma, Diederik S.; Steiner, Ullrich; Vignolini, Silvia

2014-08-15T23:59:59.000Z

288

Bright Light-Emitting Diodes based on Organometal Halide Perovskite  

E-Print Network [OSTI]

this class of materials to be excellent semiconductors for optoelectronic devices.1-7 Their primary advantages lie in the fact that they can be easily solution processed, require no high temperature heating, and they possess an optical bandgap which...

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.

2014-08-03T23:59:59.000Z

289

Sensor Switch's Bright Manufacturing Future | Department of Energy  

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

spaces are vacant. They also make devices that dim or turn off lights when sufficient daylight is present. Both types of products provide cost effective energy savings in indoor...

290

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.

291

Bright-White Beetle Scales Optimise Multiple Scattering of Light  

E-Print Network [OSTI]

Whiteness arises from diffuse and broadband reflection of light typically achieved through optical scattering in randomly structured media. In contrast to structural colour due to coherent scattering, white appearance ...

Burresi, Matteo

292

Wireless Power Transmission: An Obscure History, Possibly a Bright Future.  

E-Print Network [OSTI]

the use of microwaves because of the economic and energy efficiency that can be leveraged by products) and James F. Trimer (NASA) announced the development of a thin-film plastic rectenna using printed

La Rosa, Andres H.

293

Bright Water- hydrosols, water conservation and climate change  

E-Print Network [OSTI]

Since air-water and water-air interfaces are equally refractive, cloud droplets and microbubbles dispersed in bodies of water reflect sunlight in much the same way. The lifetime of sunlight-reflecting microbubbles, and hence the scale on which they may be applied, depends on Stokes Law and the influence of ambient or added surfactants. Small bubbles backscatter light more efficiently than large ones, opening the possibility of using highly dilute micron-radius hydrosols to substantially brighten surface waters. Such microbubbles can noticeably increase water surface reflectivity, even at volume fractions of parts per million and such loadings can be created at an energy cost as low as J m-2 to initiate and milliwatts m-2 to sustain. Increasing water albedo in this way can reduce solar energy absorption by as much as 100 W m-2, potentially reducing equilibrium temperatures of standing water bodies by several Kelvins. While aerosols injected into the stratosphere tend to alter climate globally, hydrosols can be...

Seitz, Russell

2010-01-01T23:59:59.000Z

294

NREL Success Stories - SkyFuel Partnership Reflects Bright Future  

ScienceCinema (OSTI)

NREL Scientists and SkyFuel share a story about how their partnership has resulted in a revolutionary concentrating solar power technology ReflecTech Mirror Film.

Jorgensen, Gary; Gee, Randy

2013-05-29T23:59:59.000Z

295

Schmidt modes in the angular spectrum of bright squeezed vacuum  

E-Print Network [OSTI]

We study the spatial properties of high-gain parametric down-conversion (PDC). From the Hamiltonian we find the Schmidt modes, apply the Bloch-Messiah reduction, and calculate analytically the measurable quantities, such as the angular distributions of photon numbers and photon-number correlations. Our approach shows that the Schmidt modes of PDC radiation can be considered the same as for the low-gain (biphoton) case while the Schmidt eigenvalues strongly depend on the parametric gain. Its validity is confirmed by comparison with several experimental results, obtained by us and by other groups.

Polina R. Sharapova; Angela M. Perez; Olga V. Tikhonova; Maria V. Chekhova

2014-10-24T23:59:59.000Z

296

A BRIGHT IMPULSIVE SOLAR BURST DETECTED AT 30 THz  

SciTech Connect (OSTI)

Ground- and space-based observations of solar flares from radio wavelengths to gamma-rays have produced considerable insights but raised several unsolved controversies. The last unexplored wavelength frontier for solar flares is in the range of submillimeter and infrared wavelengths. Here we report the detection of an intense impulsive burst at 30 THz using a new imaging system. The 30 THz emission exhibited remarkable time coincidence with peaks observed at microwave, mm/submm, visible, EUV, and hard X-ray wavelengths. The emission location coincides with a very weak white-light feature, and is consistent with heating below the temperature minimum in the atmosphere. However, there are problems in attributing the heating to accelerated electrons. The peak 30 THz flux is several times larger than the usual microwave peak near 9 GHz, attributed to non-thermal electrons in the corona. The 30 THz emission could be consistent with an optically thick spectrum increasing from low to high frequencies. It might be part of the same spectral component found at sub-THz frequencies whose nature remains mysterious. Further observations at these wavelengths will provide a new window for flare studies.

Kaufmann, P.; Fernandes, L. O. T.; Kudaka, A. S.; De Souza, R. V.; Valio, A.; Raulin, J.-P. [Center of Radio Astronomy and Astrophysics, Engineering School, Mackenzie Presbyterian University, Sao Paulo, SP (Brazil); White, S. M. [Air Force Research Laboratories, Space Vehicles Directorate, Albuquerque, NM 87117 (United States); Freeland, S. L. [Lockheed Martin Solar and Astrophysics Laboratory, Palo Alto, CA 94304 (United States); Marcon, R. [''Gleb Wataghin'' Physics Institute, State University of Campinas, Campinas, SP (Brazil); Aballay, J. L.; Fernandez, G.; Godoy, R.; Marun, A.; Gimenez de Castro, C. G. [El Leoncito Astronomical Complex, CONICET, San Juan (Argentina)

2013-05-10T23:59:59.000Z

297

Photo of the Week: Bright Ideas | Department of Energy  

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

two of history's most important energy-related engineers: Thomas Edison and Nikola Tesla. Edison and Tesla's developments in electric power generation and distribution made...

298

Wireless Power Transmission An Obscure History and a Bright Future?  

E-Print Network [OSTI]

to the distant rectenna site over a distance of 1.6 km. The dc output was 30 kW." [2] [5] #12;Solar Power 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

La Rosa, Andres H.

299

Bright Lights From Dark Places | 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 Delicious RankCombustion |Energy UsageAUDITVehiclesTankless orA BRIEFApril 2015CommerceDepartmentBlowerBreaking

300

Bright Lights and Even Brighter Ideas | 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 Delicious RankCombustion |Energy UsageAUDITVehiclesTankless orA BRIEFApril 2015CommerceDepartmentBlowerBreakingand Even

Note: This page contains sample records for the topic "all-stars shine bright" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


301

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:Year in Review: Top Five EEREDepartmentFebruary 4,Brent Nelson About Us Brent Nelson,From

302

Photoswitchable Nanoprobes Offer Unlimited Brightness in Frequency-Domain  

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr MayAtmosphericNuclear Security Administration the1 - September 2006 TheStevenAdministrationPhotometric(dmpe =PhotosImaging. |

303

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr MayAtmosphericNuclear Security Administration the1 - September 2006PhotovoltaicSeptember 22, 2014SocietyJ. Dudhia51 Posters A5941736191

304

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr MayAtmosphericNuclear Security Administration the1 - September 2006 TheSteven Ashby Dr. Steven Ashbystation |projectdiagnostic tool

305

PROGRESS AND FUTURE DIRECTIONS IN BRIGHTNESS ELECTRON BEAM SOURCES*  

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr MayAtmosphericNuclear Security Administration the1 - September 2006 TheSteven Ashby Dr. Steven Para buscar una publicación,PROGRESS

306

Bright and dark helices of light Ole Steuernagel  

E-Print Network [OSTI]

. A: Pure Appl. Opt. 1, 750­768 (1999). 6. J. Leach, S. Keen, M. J. Padgett, C. Saunter, and G. D. Staliunas, "Vortex Creation in Bose-Einstein Condensates by Diffraction on a Helical Light Grating," http anisotropic media," Phys. Rev. Lett. 96, 163905 (2006). 19. J. Leach, M. R. Dennis, J. Courtial, and M. J

Kaye, Paul

307

INTERPRETATION OF THE ARCADE 2 ABSOLUTE SKY BRIGHTNESS MEASUREMENT  

SciTech Connect (OSTI)

We use absolutely calibrated data between 3 and 90 GHz from the 2006 balloon flight of the ARCADE 2 instrument, along with previous measurements at other frequencies, to constrain models of extragalactic emission. Such emission is a combination of the cosmic microwave background (CMB) monopole, Galactic foreground emission, the integrated contribution of radio emission from external galaxies, any spectral distortions present in the CMB, and any other extragalactic source. After removal of estimates of foreground emission from our own Galaxy, and an estimated contribution of external galaxies, we present fits to a combination of the flat-spectrum CMB and potential spectral distortions in the CMB. We find 2{sigma} upper limits to CMB spectral distortions of {mu} < 6 x 10{sup -4} and |Y{sub ff}| < 1 x 10{sup -4}. We also find a significant detection of a residual signal beyond that, which can be explained by the CMB plus the integrated radio emission from galaxies estimated from existing surveys. This residual signal may be due to an underestimated galactic foreground contribution, an unaccounted for contribution of a background of radio sources, or some combination of both. The residual signal is consistent with emission in the form of a power law with amplitude 18.4 {+-} 2.1 K at 0.31 GHz and a spectral index of -2.57 {+-} 0.05.

Seiffert, M.; Levin, S. M. [Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109 (United States); Fixsen, D. J.; Kogut, A.; Wollack, E. [University of Maryland, Code 665, Goddard Space Flight Center, Greenbelt, MD 20771 (United States); Limon, M. [Columbia Astrophysics Laboratory, 550W 120th St., Mail Code 5247, New York, NY 10027-6902 (United States); Lubin, P. M. [Physics Department, University of California, Santa Barbara, CA (United States); Mirel, P. [Wyle Informations Systems, Code 665, Goddard Space Flight Center, Greenbelt, MD 20771 (United States); Singal, J. [Kavli Institute for Particle Astrophysics and Cosmology, SLAC National Accelerator Laboratory, Menlo Park, CA 94025 (United States); Villela, T.; Wuensche, C. A., E-mail: Michael.D.Seiffert@jpl.nasa.gov [Instituto Nacional de Pesquisas Espaciais, Divisao de Astrofisica, Caixa Postal 515, 12245-970-Sao Jose dos Campos, SP (Brazil)

2011-06-10T23:59:59.000Z

308

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 Office of InspectorConcentrating SolarElectricEnergyCTBarre BiomassTHISBrickyard Energy Partners

309

Department Announces Loan Guarantee for BrightSource Energy Inc. |  

Office of Environmental Management (EM)

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May Jun Jul(Summary) "of EnergyEnergy CooperationRequirements Matrix U.S. Department of Energy | December Washington, DC

310

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 CenterFranconia, Virginia: Energy Resources Jump to:46 -Energieprojekte3Informationof Energy Calculator29 JumpNamaNanjing

311

NRG Energy, Inc. (BrightSource) | 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 Office of Inspector General Office0-72.pdfGeorgeDoesn't32Department ofMovingJanuary1 |DepartmentNRG Energy, Inc.

312

Solar Generation Has a Bright 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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May Jun Jul(Summary) "of EnergyEnergyENERGYWomenthe House Committee on Energy andDepartment ofAnShare yourA NewGrowth of Solar

313

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May Jun Jul(Summary) "of EnergyEnergyENERGYWomenthe HouseStudents Heal the LandRemarks asFact Sheet, April 20152:45PMBrian Deese

314

The Problem Conventional office lighting typically consists of bright fluo-  

E-Print Network [OSTI]

and undercabinet lights combined with incandescent or fluorescent task lights. This approach is not very energy-friendly, high-quality light- ing with a number of benefits. Reduced waste from fluorescent lights. Fluorescent, an already-efficient lighting system can save even more energy. If an employee leaves the office and forgets

315

July 17-19, 2013 Paul Sabatier University, Toulouse, France  

E-Print Network [OSTI]

Applications Usage of Biofuel to Mitigate the Current Environmental Impact of Aviation Shine Jude Hamilton

316

Thermal benefits of artificial shelters in snakes: A radiotelemetric study of two sympatric colubrids  

E-Print Network [OSTI]

successfully for conservation (Webb and Shine, 2000; Arida and Bull, 2008; Grillet et al., 2010). Artificial

Blouin-Demers, Gabriel

317

The Gaia Project - technique, performance and status  

E-Print Network [OSTI]

Gaia is a satellite mission of the ESA, aiming at absolute astrometric measurements of about one billion stars (all stars down to 20th magnitude, with unprecedented accuracy. Additionally, magnitudes and colors will be obtained for all these stars, while radial-velocities and spectral properties will be determined only for bright objects (V<17.5). At 15th magnitude Gaia aims at an angular accuracy of 20 microarcseconds (muas). This goal can only be reached if the geometry of the telescopes, the detectors, and the pointing of Gaia at each moment ("attitude") can be inferred from the Gaia measurements itself with muas accuracy.

Stefan Jordan

2008-11-14T23:59:59.000Z

318

OOTOBEB,1913. MONTHLY WEATHER REVIEW. 1615 A METEOROLOGICAL STlJDY OF PARKS AND T-ERED AREAS IN THE WESTERN YELLOW-PINE FORESTS OF  

E-Print Network [OSTI]

variations in precipitation, atmos heric moisture, and wind movement. The percentage oHsun- shine is very

319

JGGB EXECUTIVE COMMITTEE MEETING MINUTES | AUGUST 6, 2012 Attendance: Sanjay Kumar (Co-Chair), Shuvo Roy (Co-Chair), Sri Nagarajan, SarahJane Taylor, Amy  

E-Print Network [OSTI]

students who shined through who could benefit from program · Have a group of ppl on admissions committee

Healy, Kevin Edward

320

I.V. Ptashnik and K.P. Shine Vol. 16, No. 3 /March 2003/ Atmos. Oceanic Opt. 251 0235-6880/03/03 251-05 $02.00 2003 Institute of Atmospheric Optics  

E-Print Network [OSTI]

Academy of Science, Russia Received January 13, 2003 Line-by-line calculations in the spectral region 2 remains an important concern for global climate modeling. It was shown more then 10 years ago in Ref. 1 in the different models. This factor has become more important recently as significant changes have taken place

Hogan, Robin

Note: This page contains sample records for the topic "all-stars shine bright" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


321

High-brightness single photon source from a quantum dot in a directional-emission  

E-Print Network [OSTI]

, Stanford University, Stanford CA 94305 2 Sony Corporation, Shinagawa-ku, Tokyo, Japan, 141-0001 3, Stanford University, Stanford CA 94305 a mitsuru.toishi@jp.sony.com, b englund@fas.harvard.edu, c jela

Vuckovic, Jelena

322

THE CATALOG OF POSITIONS OF OPTICALLY BRIGHT EXTRAGALACTIC RADIO SOURCES OBRS-2  

SciTech Connect (OSTI)

Future space-borne astrometry missions, such as Gaia, will be able to determine the optical positions of hundreds of quasars with submilliarcsecond accuracies comparable to those achieved in radio by very long baseline interferometry (VLBI). Comparisons of coordinate systems from space-borne missions and VLBI will be very important, first for investigations of possible systematic errors and second for investigations of possible shifts between centroids of radio and optical emissions in active galactic nuclei. In order to make such a comparison more robust, a program for densification of the grid of radio sources detectable with both VLBI and Gaia was launched in 2006. Program sources are 398 quasars with declinations > - 10 Degree-Sign that are brighter than 18 mag at the V band. The first two observing campaigns were run in 2007-2008. In the third campaign, a set of 291 objects from that list was observed with the VLBA+EVN in 2010-2011 with the primary goal of producing their images with milliarcsecond resolution. In this paper, following the method of absolute astrometry, coordinates of observed sources have been derived with milliarcsecond accuracies from analysis of these observations. The catalog of positions of 295 target sources, estimates of their correlated flux densities at 2.2 and 8.4 GHz, and their images are presented. The accuracies of source coordinates are in a range of 2-200 mas, with a median of 3.2 mas.

Petrov, L., E-mail: Leonid.Petrov@lpetrov.net [Astrogeo Center, Falls Church, VA 22043 (United States)

2013-07-01T23:59:59.000Z

323

November 16, 2006 Spectral properties of X-ray bright variable sources in the Taurus  

E-Print Network [OSTI]

Code 5247, 550 West 120th Street, New York, NY 10027, USA 5 INAF - Osservatorio Astrofisico di Arcetri of flares to derive the size of the flaring loops. Results. The light curves of the selected sources show to solar flares, or of slow modulation due e.g. to rotation (Feigelson & Montmerle 1999; Wolk et al. 2005

324

Visualizing individual microtubules by bright field microscopy Braulio Gutirrez-Medinaa  

E-Print Network [OSTI]

structure and organization. Individual microtubules have been visualized via fluorescence imaging of dye polymers using sensitive CCD cameras. We demonstrate the imaging of unstained microtubules using cells. The spatial resolution of light mi- croscopy is traditionally limited by diffraction

Block, Steven

325

Development of a High-Brightness VHF Electron Source at LBNL  

E-Print Network [OSTI]

VHF ELECTRON SOURCE AT LBNL* S. Lidia # , F. Sannibale, J.S. Virostek, R. Wells, LBNL, Berkeley, CA, USA Abstract

Lidia, Steven M.; Sannibale, Fernando; Staples, John W.; Virostek, Steve P.; Wells, Russell P.

2008-01-01T23:59:59.000Z

326

A bright idea? : the promise and peril of a memory drug  

E-Print Network [OSTI]

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 ...

Dowd, William (William Michael)

2007-01-01T23:59:59.000Z

327

Horizon brightness revisited: measurements and a model of clear-sky radiances  

E-Print Network [OSTI]

from solar energy engineering2 ,3 to atmospheric optics4'5 have repeatedly measured and modeled. Second, before the advent of narrow field-of-view (FOV) radiometers8 and photographic analysis tech explanation of the phenomenon. High-Resolution Measurements of Clear-Sky Radiances We beginby electronically

Lee Jr., Raymond L.

328

Veeco Develops a Tool to Reduce Epitaxy Costs and Increase LED Brightness  

Broader source: Energy.gov [DOE]

With the help of DOE funding, Veeco is working on reducing epitaxy costs and increasing LED efficiency by developing a physical vapor deposition (PVD) tool for depositing aluminum nitride buffer layers on LED substrates. PVD, also known as "sputtering," is an alternative to metal-organic chemical vapor deposition (MOCVD). PVD is a purely physical process that involves plasma sputter bombardment rather than a chemical reaction at the surface to be coated, as in MOCVD.

329

Sleep, mood, and circadian responses to bright green light during sleep  

E-Print Network [OSTI]

Groups .96 Figure 9: ESS Baseline and EndEpworth Sleepiness Scale (ESS; Johns, 1991), The PittsburghEpworth Sleepiness Scale (ESS; Johns, 1991) is a commonly-

Grandner, Michael Andrew

2007-01-01T23:59:59.000Z

330

1RXSJ062518.2+733433: A bright, soft intermediate polar  

E-Print Network [OSTI]

We present the results of 50 hours time-resolved R-band photometry of the ROSAT all-sky survey source 1RXSJ062518.2+733433. The source was identified by Wei et al. (1999) as a cataclysmic variable. Our photometry, performed in 10 nights between February 11, 2003, and March 21, 2003, reveals two stable periodicities at 19.7874 and 283.118 min, which are identified as probable spin and orbital periods of the binary. We therefore classify 1RXSJ062518.2+733433 as an intermediate polar. Analysis of the RASS X-ray observations reveal a variability of 100% in the X-ray flux and a likely soft X-ray excess. The new IP thus joins the rare group of soft IPs with only four members so far.

A. Staude; A. D. Schwope; M. Krumpe; V. Hambaryan; R. Schwarz

2003-04-17T23:59:59.000Z

331

1RXSJ062518.2+733433: A bright, soft intermediate polar  

E-Print Network [OSTI]

We present the results of 50 hours time-resolved R-band photometry of the ROSAT all-sky survey source 1RXSJ062518.2+733433. The source was identified by Wei et al. (1999) as a cataclysmic variable. Our photometry, performed in 10 nights between February 11, 2003, and March 21, 2003, reveals two stable periodicities at 19.7874 and 283.118 min, which are identified as probable spin and orbital periods of the binary. We therefore classify 1RXSJ062518.2+733433 as an intermediate polar. Analysis of the RASS X-ray observations reveal a variability of 100% in the X-ray flux and a likely soft X-ray excess. The new IP thus joins the rare group of soft IPs with only four members so far.

Staude, A; Krumpe, M; Hambaryan, V; Schwarz, R

2003-01-01T23:59:59.000Z

332

Space-charged-induced emittance growth in the transport of high-brightness electron beams  

SciTech Connect (OSTI)

The emittance induced by space charge in a drifting beam of finite length has been investigated, and a scaling law has been obtained from simple considerations of the different rates of expansion of different portions of the beam. The scaling law predicts the initial rate of emittance growth, before the beam shape has distorted significantly, and thus represents an upper bound on the rate of emittance increase. This scaling law has been substantiated by particle-in-cell simulation and the dependence on geometric factors evaluated for specific choices of the beam profile. For long, axially nonuniform beams, the geometric factors have been evaluated explicitly for Gaussian profiles, and other shapes.

Jones, M.E.; Carlsten, B.E.

1987-03-01T23:59:59.000Z

333

SunShot Grand Challenge Summit: Bright Outlook to Achieve SunShot Goal  

Office of Energy Efficiency and Renewable Energy (EERE)

Last week, hundreds of solar energy leaders gathered in southern California to participate in SunShots biennial Grand Challenge Summit. Read a recap of the four-day event, which focused on making solar energy fully cost-competitive with traditional forms of energy by 2020.

334

Lecture 2. Instrumentation Is the Sun very bright so we can never be photon hungry?  

E-Print Network [OSTI]

a secondary flat, so images are not rotated. Coelostats #12;12 Turret Altazimuth mirror arrangement Kitt Peak;9 Consideration of telescope focal length Diameter of solar image in the focal plane: f : focal length A : Sun to generate effective focal length. Arfd /2 B) Long Primary Focus Instrument #12;10 Heliostat primary mirror

335

The GMRT EoR Experiment: Limits on Polarized Sky Brightness at 150 MHz  

E-Print Network [OSTI]

The GMRT reionization effort aims to map out the large scale structure of the Universe during the epoch of reionization (EoR). Removal of polarized Galactic emission is a difficult part of any 21 cm EoR program, and we present new upper limits to diffuse polarized foregrounds at 150 MHz. We find no high significance evidence of polarized emission in our observed field at mid galactic latitude (J2000 08h26m+26). We find an upper limit on the 2-dimensional angular power spectrum of diffuse polarized foregrounds of [l^2 C_l/(2 PI)]^{1/2}EoR observations, is [k^3 P_p(k)/(2 PI^2)]^{1/2} 0.03 h/Mpc, k EoR signal in total intensity of [k^3 P(k)/ (2 PI^2) ]^{1/2} ~ 10 mK. We find polarized structure is substantially weaker than suggested by extrapolation from higher frequency observations, so the new low upper limits reported here reduce the anticipated impact of these foregrounds on EoR experiments. We discuss Faraday beam and depth depolarization models and compare predictions of these models to our data. We report on a new technique for polarization calibration using pulsars, as well as a new technique to remove broadband radio frequency interference. Our data indicate that, on the edges of the main beam at GMRT, polarization squint creates ~ 3% leakage of unpolarized power into polarized maps at zero rotation measure. Ionospheric rotation was largely stable during these solar minimum night time observations.

Ue-Li Pen; Tzu-Ching Chang; Christopher M. Hirata; Jeffrey B. Peterson; Jayanta Roy; Yashwant Gupta; Julia Odegova; Kris Sigurdson

2009-05-05T23:59:59.000Z

336

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

E-Print Network [OSTI]

are considering radiation, the electric fields detected areof synchrotron radiation from the General Electric syn-by the null in the electric dipole radiation pattern in the

O'Shea, Finn Henry

2012-01-01T23:59:59.000Z

337

Sleep, mood, and circadian responses to bright green light during sleep  

E-Print Network [OSTI]

white light from fluorescent bulbs, as point sources mightthan incandescent bulbs. Also, fluorescent light is easier

Grandner, Michael Andrew

2007-01-01T23:59:59.000Z

338

E-Print Network 3.0 - all-sky survey bright Sample Search Results  

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

All-Sky Survey. Since the simulated light curve is quite stable... .1. All-Sky Survey FIS is primarily designed ... Source: Pak, Soojong - Department of Astronomy and Space...

339

Critical issues for high-brightness heavy-ion beams -- prioritized  

E-Print Network [OSTI]

National Ignition Facility (NIF) will provide motivation toobtaining funding for the NIF, the Large Hadron Collider (

2007-01-01T23:59:59.000Z

340

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

E-Print Network [OSTI]

. Table 1 shows how three different instruments in the same area (Toronto, Canada) can give quite different values for the same periods. Toronto gives a much lower reading than Toronto-Scarborough or Toronto Meteorological Research Station. Since all... of instrument 15 and the positioning of the instrument can affect the results obtained. Table 1. Variation statistics for three distinct ground-based instru- ments located in the same area. All instruments are in Toronto, Canada, and are less than 20 mi...

Kolczynski, Edward Franklin

1971-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "all-stars shine bright" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


341

Looking on bright side of losing ITER Risa Kato and Tetsuro Yamada / Yomiuri Shimbun Staff Writers  

E-Print Network [OSTI]

to have a remote-controlled ITER experiment unit, and one for the development of super heat candidate to have a remote-control facility is of especially high significance, according to experts. The remote-control facility is envisaged as playing a key role in the ITER project, as it will be able

342

E-Print Network 3.0 - average brightness thomson Sample Search...  

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

the first polarizing beamsplitter, 0 200 2N... for Thomson scattering J Howard Plasma Research Laboratory, Australian National University, Canberra, ACT 0200... birefringent...

343

How Many CASTLE Bulbs Would You Need To Match the Brightness of the Sun?  

E-Print Network [OSTI]

;Suppose that you have two household incandescent bulbs: one is labeled "60W," the other "100W." If you try incandescent bulb and a 9W fluorescent bulb. Which one makes your room brighter? It's not what you might expect... in fact, they look about the same! The incandescent bulb emits a broad spectrum of visible and infrared

Collar, Juan I.

344

Detecting Sound-Wave-Like Surface Brightness Ripples in Cluster Cores  

E-Print Network [OSTI]

We investigate the observational requirements for the detection of sound-wave-like features in galaxy cluster cores. We calculate the effect of projection on the observed wave amplitude, and find that the projection factor depends only weakly on the underlying cluster properties but strongly on the wavelength of the sound waves, with the observed amplitude being reduced by a factor ~5 for 5 kpc waves but only by a factor ~ 2 for 25 kpc waves. We go on to estimate the time needed to detect ripples similar to those previously detected in the Perseus cluster in other clusters. We find that the detection time scales most strongly with the flux of the cluster and the amplitude of the ripples. By connecting the ripple amplitude to the heating power in the system, we estimate detection times for a selection of local clusters and find that several may have ripples detected with ~1Ms Chandra time.

J. Graham; A. C. Fabian; J. S. Sanders

2008-08-18T23:59:59.000Z

345

Generation, transport and focusing of high-brightness heavy ion beams  

E-Print Network [OSTI]

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 ...

Henestroza, Enrique

2006-01-01T23:59:59.000Z

346

Homogeneity of bright radio sources at 15 GHz on the sky and in the space  

E-Print Network [OSTI]

A revised sample of the 2 cm Very Long Baseline Array (VLBA) survey is studied to test the isotropic distribution of radio sources on the sky and their uniform distribution in space. The revised sample is complete to flux-density limits of 1.5 Jy for positive declinations and 2 Jy for declinations between 0 and -20 degrees. At present the active galactic nuclei sample comprises 122 members. Application of the two-dimensional Kolmogorov-Smirnov (K-S) test shows that there is no significant deviation from the homogenous distribution in the sky, while the V/Vmax test shows that the space distribution of active nuclei is not uniform at high confidence level (99.9%). This is indicative of a strong luminosity and/or density evolution implying that active nuclei (or jet activity phenomena) were more populous at high redshifts, z~2.

Arshakian, T G; Zensus, J A; Lister, M L

2003-01-01T23:59:59.000Z

347

Theoretical ecology: a successful first year and a bright future for a new journal  

E-Print Network [OSTI]

6 EDITORIAL Theoretical ecology: a successful first year andvolume 2 of Theoretical Ecology. Looking back, this has beenfocusing on theoretical ecology can play an expanding role

Hastings, Alan

2009-01-01T23:59:59.000Z

348

Radio Observations of the AGN and Gas in Low Surface Brightness Galaxies  

E-Print Network [OSTI]

Abstract. LSB galaxies have low metallicities, diffuse stellar disks, and massive HI disks. We have detected molecular gas in two giant LSB galaxies, UGC 6614 and F568-6. A millimeter continuum source has been detected in UGC 6614 as well. At centimeter wavelengths we have detected and mapped the continuum emission from the giant LSB galaxy 1300+0144. The emission is extended about the nucleus and is most likely originating from the AGN in the galaxy. The HI gas distribution and velocity field in 1300+0144 was also mapped. The HI disk extends well beyond the optical disk and appears lopsided in the intensity maps.

F. Combes; J. Palous; M. Das; N. Kantharia; S. N. Vogel; S. S. Mcgaugh

2006-01-01T23:59:59.000Z

349

Perception, 1993, volume 22, pages 343-351 Colour pools, brightness pools, assimilation,  

E-Print Network [OSTI]

varies according to the colours involved. For red-cyan and green-magenta complementary pairs colour vision are discussed in the light of these findings. 1 Introduction The purpose of this communication the preparation of this communication we found that we were the rein- ventors, not the originators

Kingdom, Frederick A. A.

350

A bright thermonuclear X-ray burst simultaneously observed with Chandra and RXTE  

E-Print Network [OSTI]

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) ...

in t Zand, J. J. M.

351

E-Print Network 3.0 - australia telescope low-brightness Sample...  

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

Blue Bump BL Lac: BL Lacert26; object CASPIR: Cryogenic Array... SpectrometerImager near-infrared detector on the Australian National University's 2.3m telescope EGRET... :...

352

Development of a High-Brightness VHF Electron Source at LBNL  

E-Print Network [OSTI]

voltage DC or microwave RF guns, each with its particularinjection system utilizing a gun resonant in the VHF band.driven by a VHF band gun. This gun may present an attractive

Lidia, Steven M.; Sannibale, Fernando; Staples, John W.; Virostek, Steve P.; Wells, Russell P.

2008-01-01T23:59:59.000Z

353

Overview of Recent Progres on High Repetition Rate, High Brightness Electron Guns  

E-Print Network [OSTI]

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

Sannibale, F.

2014-01-01T23:59:59.000Z

354

106Rotation Velocity of a Galaxy Spiral galaxy M-101 showing its bright nucleus and  

E-Print Network [OSTI]

V(x)/dx = 0. 1 3 2 24 4 3 2 2 ( ) (350 )(3/ 4)(1 ) (2 ) 350(1 ) (1 ) dV x x x x x dx x - + - + = + so after=1 the physical distance is 10,000 light years. How many years does it take a star to complete one the physical distance is 10,000 light years. How many years does it take a star to complete one circular orbit

355

High-brightness single photon source from a quantum dot in a directional-emission nanocavity  

E-Print Network [OSTI]

We analyze a single photon source consisting of an InAs quantum dot coupled to a directional-emission photonic crystal (PC) cavity implemented in GaAs. On resonance, the dot's lifetime is reduced by more than 10 times, to 45ps. Compared to the standard three-hole defect cavity, the perturbed PC cavity design improves the collection efficiency into an objective lens (NA=0.75) by factor 6, and improves the coupling efficiency of the collected light into a single mode fiber by factor 1.9. The emission frequency is determined by the cavity mode, which is antibunched to g(2)=0.05. The cavity design also enables efficient coupling to a higher-order cavity mode for local optical excitation of cavity-coupled quantum dots.

Mitsuru Toishi; Dirk Englund; Andrei Faraon; Jelena Vuckovic

2009-04-08T23:59:59.000Z

356

Statistical Correlations between Parameters of Photospheric Magnetic Fields and Coronal Soft X-ray Brightness  

E-Print Network [OSTI]

07102 USA 2. Big Bear Solar Observatory, 40386 North Shore Lane, Big Bear City, CA 92314 USA 3. National) the magnetic energy dissipation, , (3) the unsigned line-of-sight magnetic flux, , (4) the area,2 , Haimin Wang1,2 1. Center for Solar-Terrestrial Research , New Jersey Institute of Technology, Newark, NJ

357

The Bright Lights in New York Could Be Solar | 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 Delicious RankCombustion |Energy UsageAUDITVehiclesTankless or Demand-Type Water Heaters Tankless orNationalCareersThe

358

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May Jun Jul(Summary) "of EnergyEnergyENERGYWomenthe HouseStudents2.2at Multipleorder supplies or Department ofDepartment of

359

Cracking Molecular Structures with Bright Lights - and a Few Good Eggs |  

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 Delicious RankCombustion |Energy UsageAUDITVehiclesTankless orAChief MedicalDepartmentWorkingCookingDepartment of

360

New Family of Tiny Crystals Glow Bright in LED Lights | Advanced Photon  

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr MayAtmosphericNuclear Security Administration the Contributions andDataNational Library of1,Department ofNewof NO2: Key Role

Note: This page contains sample records for the topic "all-stars shine bright" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


361

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 RankCombustion | Department ofT ib l L d F SSalesOE0000652 Srivastava,Pacific1of PageHYDROGEN H 25Energyof

362

New family of tiny crystals glow bright in LED lights | ornl.gov  

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May JunDatastreamsmmcrcalgovInstrumentsrucLas Conchas recoveryLaboratory | NationalJohn CyberNeutrons usedDOENewNew exhibit highlightsNew

363

LIMITATIONS ON THE RESOLUTION OF YAG:CE BEAM PROFILE MONITOR FOR HIGH BRIGHTNESS ELECTRON BEAM  

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr MayAtmospheric Optical Depth7-1D: VegetationEquipment Surfaces and Interfaces Sample Environment: Magnet and6ledp/ The

364

Design, conditioning, and performance of a high voltage, high brightness dc photoelectron gun with variable gap  

SciTech Connect (OSTI)

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.

Maxson, Jared; Bazarov, Ivan; Dunham, Bruce; Dobbins, John; Liu, Xianghong; Smolenski, Karl [Cornell Laboratory for Accelerator-Based Sciences and Education, Cornell University, Ithaca, New York 14853 (United States)

2014-09-15T23:59:59.000Z

365

Turbulent Diffusion in the Photosphere as Derived from Photospheric Bright Point Motion  

E-Print Network [OSTI]

, Vecchio, A.2 1 - Big Bear Solar Observatory, 40386 N. Shore Lane, Big Bear City, CA 92314, USA; 2 of Physics & Astronomy, Michigan State University, East Lansing, MI 48824, USA Received ; accepted #12;­ 2 ­ ABSTRACT On the basis of observations of solar granulation obtained with the New Solar Telescope (NST

366

A Program Full of Bright Ideas for Kentucky: Weatherization Assistance Close-Up Fact Sheet  

SciTech Connect (OSTI)

Kentucky demonstrates its commitment to technology and efficiency through the Weatherization Program. Weatherization uses advanced technologies and techniques to reduce energy costs for low-income families by increasing the energy efficiency of their homes.

D& R International

2001-10-10T23:59:59.000Z

367

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

368

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 Home5b9fcbce19 NoPublic Utilities Address: 160Benin: EnergyBoston Area SolarConnecticut: EnergyVermont: EnergyBrigham CityEnergy Inc

369

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:Year in3.pdfEnergy Health and Productivity QuestionnaireSingle Emitter |VolumeEnergyR

370

ITP Glass: A Clear Vision for a Bright Future | 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:YearRound-UpHeatMulti-Dimensionalthe U.S. Department ofIOWA1999) | Department2009 | UC ENERGYA

371

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr MayAtmosphericNuclear Security Administration the Contributions and Achievements of Women |hits 21Species.4 Leads NREL4 FS-6A42-62241

372

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr MayAtmosphericNuclear Security Administration the Contributions andData and ResourcesOther FederalNiche Innovative WayFuture for

373

Plastic Solar Cells See Bright Future | ANSER Center | Argonne-Northwestern  

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May JunDatastreamsmmcrcalgovInstrumentsrucLas ConchasPassive Solar Home Design Passive SolarCenterYou are here: SN

374

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May JunDatastreamsmmcrcalgovInstrumentsrucLas ConchasPassiveSubmittedStatus TomAbout »Lab (NewportSuccess StoriesNERSC

375

Synthetic properties of bright metal-poor variables. II. BL Her stars  

E-Print Network [OSTI]

We investigate the properties of the so-called BL Her stars, i.e., Population II Cepheids with periods shorter than 8 days, using updated pulsation models and evolutionary tracks computed adopting a metal abundance in the range of Z=0.0001 to Z=0.004. We derive the predicted Period-Magnitude (PM) and Period-Wesenheit (PW) relations at the various photometric bands and we show that the slopes of these relations are in good agreement with the slopes determined by observed variables in Galactic globular clusters, independently of the adopted M_V(RR)-[Fe/H] relation to get the cluster RR Lyrae-based distance. Moreover, we show that also the distances provided by the predicted PM and PW relations for BL Her stars agree within the errors with the RR Lyrae based values. The use of the predicted relations with W Vir stars, which are Population II Cepheids with periods longer than 8 days, provides no clear evidence for or against a change in the PM and PW slopes around P~10 days.

M. Di Criscienzo; F. Caputo; M. Marconi; S. Cassisi

2007-05-18T23:59:59.000Z

376

Bright x-ray sources from laser irradiation of foams with high concentration of Ti  

SciTech Connect (OSTI)

Low-density foams irradiated by a 20 kJ laser at the Omega laser facility (Laboratory for Laser Energetics, Rochester, NY, USA) are shown to convert more than 5% of the laser energy into 4.6 to 6.0?keV x rays. This record 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 obtained in a foam with a total density of 5?mg/cm{sup 3}. The dynamics of the ionization front through these foams were investigated at the 1 kJ laser of the Gekko XII facility (Institute for Laser Engineering, Osaka, Japan). Hydrodynamic simulations can reproduce the average electron temperature but fail to predict accurately the heat front velocity in the foam. This discrepancy is shown to be unrelated to the possible water adsorbed in the foam but could be attributed to effects of the foam micro-structure.

Prez, F., E-mail: perez75@llnl.gov; Patterson, J. R.; May, M.; Colvin, J. D.; Biener, M. M.; Wittstock, A.; Kucheyev, S. O.; Charnvanichborikarn, S.; Satcher, J. H.; Gammon, S. A.; Poco, J. F.; Fournier, K. B. [Lawrence Livermore National Laboratory, 7000 East Ave., Livermore, California 94550 (United States)] [Lawrence Livermore National Laboratory, 7000 East Ave., Livermore, California 94550 (United States); Fujioka, S.; Zhang, Z.; Ishihara, K.; Tanaka, N.; Ikenouchi, T.; Nishimura, H. [Institute of Laser Engineering, Osaka University, 2-6 Yamada-Oka, Suita, Osaka 565-0871 (Japan)] [Institute of Laser Engineering, Osaka University, 2-6 Yamada-Oka, Suita, Osaka 565-0871 (Japan)

2014-02-15T23:59:59.000Z

377

CX-000546: Categorical Exclusion Determination | Department of...  

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

Environmental Management, Savannah River Operations Office A Kaiser Optic Fourier Transform Raman (FT-Raman) spectrometer will be use to shine a weak (0 to 400 megawatts) laser...

378

IT TalkJanuary / February 2011 Issue 1 Improved Security, Efficiency,  

E-Print Network [OSTI]

on the IT Infrastructure Library (ITIL), which is a British invention. IT Talk was designed to shine a light on all

379

E-Print Network 3.0 - atoms technical progress Sample Search...  

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

innovations... Shining Light on Ultracold Atoms: Illuminating Complex Matters "The Cold Front" The First Lecture... of the last century, the discrete frequencies of...

380

Solar | Department of Energy  

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

for more World Cup Action | Photo courtesy of Renato CobucciImprensaMG Shining Some Light on the World Cup's Efficiency Efforts Brazil strives for energy efficiency with...

Note: This page contains sample records for the topic "all-stars shine bright" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


381

E-Print Network 3.0 - adult toad model Sample Search Results  

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

Shine, Rick - School of Biological Sciences, University of Sydney Collection: Environmental Sciences and Ecology ; Biology and Medicine 2 2006 NORTHEASTERN NATURALIST 13( I...

382

Tax Credits, Rebates & Savings | Department of Energy  

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

to solar, while the permitting laws... Eligibility: Construction Savings Category: Photovoltaics, Solar Water Heat City of Milwaukee- Milwaukee Shines Solar Financing Beginning...

383

Solar | Department of Energy  

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

Research Award Program work on. | Photo by Dennis Schroeder, National Renewable Energy Laboratory Shining Stars of Solar: Meet Three SunShot Postdoctoral Award Recipients...

384

CX-000270: Categorical Exclusion Determination | Department of...  

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

CX-000270: Categorical Exclusion Determination Recovery Act: Milwaukee Shines for a Sustainable Solar Economy CX(s) Applied: A9, A11 Date: 12282009 Location(s): Wisconsin...

385

E-Print Network 3.0 - anopheles fluviatilis diptera Sample Search...  

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

but could not get Anopheles maculipennis 1. Present address: Dept. Biology Source: Shine, Rick - School of Biological Sciences, University of Sydney Collection: Environmental...

386

E-Print Network 3.0 - adult type alport Sample Search Results  

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

adult body size. (1) This dimorphism is determined mainly by the direction Source: Shine, Rick - School of Biological Sciences, University of Sydney Collection: Environmental...

387

E-Print Network 3.0 - anopheles nuneztovari diptera Sample Search...  

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

but could not get Anopheles maculipennis 1. Present address: Dept. Biology Source: Shine, Rick - School of Biological Sciences, University of Sydney Collection: Environmental...

388

E-Print Network 3.0 - anopheles braziliensis diptera Sample Search...  

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

but could not get Anopheles maculipennis 1. Present address: Dept. Biology Source: Shine, Rick - School of Biological Sciences, University of Sydney Collection: Environmental...

389

E-Print Network 3.0 - anopheles aconitus diptera Sample Search...  

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

but could not get Anopheles maculipennis 1. Present address: Dept. Biology Source: Shine, Rick - School of Biological Sciences, University of Sydney Collection: Environmental...

390

Blast-furnace ironmaking -- Existing capital and continued improvements are a winning formula for a bright future  

SciTech Connect (OSTI)

Throughout the years the blast-furnace process has been improved upon significantly. Increases to the hot-blast temperature, improvements to the physical, chemical, and metallurgical properties of coke and burden materials, the use of more fuel injectants, and improvements to the design of the furnace facilities have led to significant decreases in furnace coke rate, increases in productivity, and increases in furnace campaign life. As a result, many of the alternative cokeless reduction processes have not replaced blast-furnace hot-metal production in North America. In the future, these continued blast-furnace improvements will potentially result in coke rates decreasing to 400 pounds per net ton of hot metal (lb/NTHM) as more pulverized coal is injected. These improvements, coupled with the fact that existing blast furnaces and coke plants can be refurbished for approximately $110 per annual ton of hot metal [$100 per annual net ton of hot metal (NTHM)], will result in extending the life of the North American blast furnaces well into the twenty-first century.

Oshnock, T.W.; Colinear, J.A. [U.S. Steel, Monroeville, PA (United States)

1995-12-01T23:59:59.000Z

391

No excess of bright galaxies around the redshift 7.1 quasar ULAS J1120+0641  

E-Print Network [OSTI]

to facilitate studies of the Universe in the first billion years after the big bang in two ways. First, since they are the most luminous non-transient objects, it is possible to measure the opacity of the intergalactic medium (IGM) along the line of sight due... whether this was due to flat-fielding errors by constructing a corrective flat-field from our pipelined images. All 25 ACS images were scaled to the same sky level, and this stack was median filtered before the small-scale structure was removed...

Simpson, Chris; Mortlock, Daniel; Warren, Stephen; Cantalupo, Sebastiano; Hewett, Paul; McLure, Ross; McMahon, Richard; Venemans, Bram

2014-07-02T23:59:59.000Z

392

SPIE International Conference, Denver CO, July 1999 1 Relevance Of The Modified Model For The Microwave Brightness Temperature To The  

E-Print Network [OSTI]

of low wind conditions. The radiosonde profiles are used to compute the upwelling and downwelling numerous advantages over ship and buoy data. Some of these advantages include the vast coverage of global seas, including locations where radiosonde or buoys cannot be afforded, relatively low power

Cruz-Pol, Sandra L.

393

Search for gamma-rays from the unusually bright GRB 130427A with the HAWC Gamma-ray Observatory  

E-Print Network [OSTI]

The long gamma-ray burst (GRB) 130427A was the most powerful burst ever detected with a redshift $z\\lesssim0.5$, featuring the highest energy photon so far detected from a GRB and the longest lasting emission above 100 MeV. The HAWC Gamma-ray Observatory is a new extensive air shower detector currently under construction in central Mexico. It features two data acquisition (DAQ) systems - one designed to readout full air-shower events (main DAQ) and the other one counting the signals in each photomultiplier tube (scaler DAQ). The burst occurred at a zenith angle of $57^\\circ$, when HAWC was running 10% of the final detector and collecting data with the scaler DAQ only. Based on the observed light curve at MeV-GeV energies, 8 different time periods have been searched for prompt and delayed emission from this GRB. In all cases, no statistically significant excess of counts has been found and upper limits have been placed. It is shown that a similar GRB close to zenith would be easily detected by the full HAWC de...

Abeysekara, A U; Alvarez, C; Arceo, R; Arteaga-Velzquez, J C; Solares, H A Ayala; Barber, A S; Baughman, B M; Bautista-Elivar, N; BenZvi, S Y; Rosales, M Bonilla; Braun, J; Caballero-Mora, K S; Carramiana, A; Castillo, M; Cotti, U; Cotzomi, J; de la Fuente, E; De Len, C; DeYoung, T; Hernandez, R Diaz; Dingus, B L; DuVernois, M A; Ellsworth, R W; Fiorino, D W; Fraija, N; Galindo, A; Gonzlez, M M; Goodman, J A; Gussert, M; Hampel-Arias, Z; Harding, J P; Hui, C M; Hntemeyer, P; Imran, A; Iriarte, A; Karn, P; Kieda, D; Kunde, G J; Lara, A; Lauer, R J; Lee, W H; Lennarz, D; Vargas, H Len; Linnemann, J T; Longo, M; Luna-Garca, R; Malone, K; Marinelli, A; Marinelli, S S; Martinez, H; Martinez, O; Martnez-Castro, J; Matthews, J A J; Torres, E Mendoza; Miranda-Romagnoli, P; Moreno, E; Mostaf, M; Nellen, L; Newbold, M; Noriega-Papaqui, R; Oceguera-Becerra, T O; Patricelli, B; Pelayo, R; Ponce, E; Pretz, J; Prez-Prez, E G; Rivire, C; Rosa-Gonzlez, D; Salazar, H; Greus, F Salesa; Sandoval, A; Schneider, M; Sinnis, G; Smith, A J; Woodle, K Sparks; Springer, R W; Taboada, I; Tollefson, K; Torres, I; Ukwatta, T N; Villaseor, L; Weisgarber, T; Westerhoff, S; Wisher, I G; Wood, J; Yodh, G B; Younk, P W; Zaborov, D; Zepeda, A; Zhou, H; lvarez, J D

2014-01-01T23:59:59.000Z

394

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

E-Print Network [OSTI]

a charge generation layer into an electron only device to form an n-i-p-i-n structure. It is shown that an electron only device (EOD), which can be considered as an n-i-n structure. The low injection barrier with a negative bias across the device while the holes are blocked at the other electrode. Therefore, the electron

Demir, Hilmi Volkan

395

tales from the high-rise P8 Universe found to be twice as bright P17  

E-Print Network [OSTI]

of Canberra is the site of research investigating how extreme winds generate monster waves in the open ocean

Liley, David

396

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

E-Print Network [OSTI]

that geoscientists are in demand and increasing demand is forecast. A recent report pursuing an education in geology or a geoscience related field as demand for geoscientists is high and the opportunities are diverse. With increasing global demand

Walker, Lawrence R.

397

A compact streak camera for 150 fs time resolved measurement of bright pulses in ultrafast electron diffraction  

SciTech Connect (OSTI)

We have developed a compact streak camera suitable for measuring the duration of highly charged subrelativistic femtosecond electron bunches with an energy bandwidth in the order of 0.1%, as frequently used in ultrafast electron diffraction (UED) experiments for the investigation of ultrafast structural dynamics. The device operates in accumulation mode with 50 fs shot-to-shot timing jitter, and at a 30 keV electron energy, the full width at half maximum temporal resolution is 150 fs. Measured durations of pulses from our UED gun agree well with the predictions from the detailed charged particle trajectory simulations.

Kassier, G. H.; Haupt, K.; Erasmus, N.; Rohwer, E. G.; Bergmann, H. M. von; Schwoerer, H. [Laser Research Institute, University of Stellenbosch, Private Bag X1, 7602 Matieland (South Africa); Coelho, S. M. M.; Auret, F. D. [Department of Physics, University of Pretoria, Pretoria 0002 (South Africa)

2010-10-15T23:59:59.000Z

398

CONCEPTUAL DESIGN OF A BRIGHT ELECTRON INJECTOR BASED ON A LASER-DRIVEN PHOTOCATHODE RF ELECTRON GUN  

E-Print Network [OSTI]

Photocathode RF Electron Gun S. Chattopadhyay, Y.J. Chen, D.PHOTOCATHODE RF ELECTRON GUN' S. Chnttopndhyny. Y.J. Chen (Photocathode RF Electron Gun S. Chattopadhyay, Y.I. Chen, D.

Chattopadhyay, S.

2010-01-01T23:59:59.000Z

399

Posters Brightness Fields of Broken Clouds V. E. Zuev, G. A. Titov, E. I. Kasyanov, and D. A. Zimin  

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr MayAtmosphericNuclear Security Administration the1 - September 2006PhotovoltaicSeptember 22, 2014SocietyJ. Dudhia51 Posters A59

400

Nanoscale optical positioning of single quantum dots for bright, pure, and on-demand single-photon emission  

E-Print Network [OSTI]

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 (minimum) position uncertainty efficiency (48 % +/- 5 % into a 0.4 numerical aperture lens, close to the theoretically predicted value of 50 %), low multiphoton prob...

Sapienza, Luca; Badolato, Antonio; Srinivasan, Kartik

2015-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "all-stars shine bright" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


401

Through a window, brightly : modulating daylight and solar radiation in commercial and institutional buildings through the use of architectural elements  

E-Print Network [OSTI]

Natural lighting serves several important functions in buildings. The visual power of a shaft of sunlight penetrating a dark space or the visual beauty of a stained window has long been recognized by architects and designers. ...

Schlereth, Hans-Joachim

1982-01-01T23:59:59.000Z

402

Oregon's Rocky Shore Species: Anemones Giant Green Anemones get their bright coloration from symbiotic, single-celled  

E-Print Network [OSTI]

" (blobs on rocks that look like paint or tar) is a different stage in the life cycle of this red alga snails, and barnacles A common species, the finger limpet A small, colorful lined chiton A lemon

Wright, Dawn Jeannine

403

Solar Policy Environment: Milwaukee  

Broader source: Energy.gov [DOE]

The City of Milwaukees SAC Initiative, Milwaukee Shines, works to reduce informational, economic and procedural barriers to the widespread adoption of solar energy systems. While the City of Milwaukee and its partners have demonstrated commitment and experience in implementing solar technologies, Milwaukee Shines aims to enhance these efforts and make solar a viable alternative throughout the region.

404

"A 4-H tradition that has been maintained  

E-Print Network [OSTI]

Virginia 4-H All Stars "A 4-H tradition that has been maintained for over 80 years." Becoming an All Star By being active in your home 4-H community and maintaining a high interest in "Making the Best Better," you can apply to become a 4- H All Star in Virginia. Applications must be filled out

Liskiewicz, Maciej

405

X-ray Properties of Low-Mass Pre-Main Sequence Stars in the Orion Trapezium Cluster  

E-Print Network [OSTI]

The Chandra High Energy Transmission Gratings (HETG) Orion Legacy Project (HOLP) is the first comprehensive set of observations of a very young massive stellar cluster which provides high resolution X-ray spectra of very young stars over a wide mass range (0.7 - 2.3 Msun). In this paper, we focus on the six brightest X-ray sources with T Tauri stellar counterparts which are well-characterized at optical and infra-red wavelengths. All stars show column densities which are substantially smaller than expected from optical extinction indicating that the sources are located on the near side of the cluster with respect to the observer as well as that these stars are embedded in more dusty environments. Stellar X-ray luminosities are well above $10^{31}$ erg/s, in some cases exceeding $10^{32}$ erg/s for a substantial amount of time. The stars during these observations show no flares but are persistently bright. The spectra can be well fit with two temperature plasma components of 10 MK and 40 MK, of which the latte...

Schulz, Norbert S; Guenther, Moritz; Testa, Paola; Canizares, Claude R

2015-01-01T23:59:59.000Z

406

--No Title--  

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

A Kaiser Optic Fourier Transform Raman (FT-Raman) spectrometer will be use to shine a weak (0 - 400 mWatts) laser (785 nm) to 0.25 mm2 area of sample and then observed the...

407

U.S. Department of Energy Categorical Exclusion ...  

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

and Inorganics Savannah River Site AikenAikenSouth Carolina A Kaiser Optic Fourier Transform Raman (FT-Raman) spectrometer will be used to shine a weak (0-400 mWatts) laser (785...

408

CX-010650: Categorical Exclusion Determination | Department of...  

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

South Carolina Offices(s): Savannah River Operations Office A Kaiser Optic Fourier Transform Raman (FT-Raman) spectrometer will be used to shine a weak (0-400 mWatts) laser (785...

409

Energy Blog | Department of Energy  

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

Rain and Shine Friday marked the end of the Solar Decathlon competition. Team Germany won (for the second time) in a very competitive field, in a ceremony marked by gray...

410

Sandia National Laboratories: utility-scale alternative energy...  

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

produce energy as predictably as generating plants powered by oil, coal, or natural gas. Solar panels only produce electricity when the sun is shining, and wind turbines are only...

411

Energy 101: Solar PV  

SciTech Connect (OSTI)

Solar photovoltaic (PV) systems can generate clean, cost-effective power anywhere the sun shines. This video shows how a PV panel converts the energy of the sun into renewable electricity to power homes and businesses.

None

2011-01-01T23:59:59.000Z

412

FREE TRIAL WEEK! We will offer many of our classes free of charge from Monday, September 19 Sunday, Sep-  

E-Print Network [OSTI]

FREE TRIAL WEEK! We will offer many of our classes free of charge from Monday, September 19 ­Sunday intensity style program us- ing free weights, resistance and body weight. RISE AND SHINE INTERVAL

413

NATURE MEDICINE VOLUME 7 NUMBER 5 MAY 2001 525 BOOK REVIEW  

E-Print Network [OSTI]

a fascinating story. There is an old saying to the effect that truth is like daylight shining behind a curtain seems a good solution. Folkman was clearly capable of that type of thinking and he showed, even early

Nowak, Martin A.

414

DOE Announces up to $52.5 Million for Concentrating Solar Power...  

Office of Environmental Management (EM)

include low-cost energy storage, which allows them to provide electricity even when the sun is not shining. CSP technologies currently used in utility-scale power plants typically...

415

Secretary Chu Announces up to $62 Million for Concentrating Solar...  

Office of Environmental Management (EM)

can include low-cost energy storage, allowing them to provide electricity even when the sun is not shining. Boosting these technologies today will generate the clean-technology...

416

Energy Department Announces New Concentrating Solar Power Technology...  

Office of Environmental Management (EM)

their ability to store energy as heat so that consumer demand can be met even when the sun is not shining, including during the night. These systems can be combined with existing...

417

Photovoltaic Cell Quantum Efficiency Basics | Department of Energy  

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

carriers collected by a photovoltaic (PV) cell to the number of photons-or packets of light-of a given energy shining on the solar cell. Quantum efficiency therefore relates to...

418

Energy 101: Solar PV  

ScienceCinema (OSTI)

Solar photovoltaic (PV) systems can generate clean, cost-effective power anywhere the sun shines. This video shows how a PV panel converts the energy of the sun into renewable electricity to power homes and businesses.

None

2013-05-29T23:59:59.000Z

419

PI Research Organisation Project Title NE/J024678/1 Dr Christopher Davis University of Reading Driving space weather forecasts with real data  

E-Print Network [OSTI]

Lead Grant Reference PI Research Organisation Project Title NE/J024678/1 Dr Christopher Davis Troposphere and the Routing of Aircraft (EXTRA)Professor Keith Shine University of Reading NE/J023760

420

Neutrino Theory  

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

operators in the Lagrangian (Majorana mass terms), or both. The ongoing neutrinoless double-beta decay searches may be able to shine light on the matter. But the neutrino sector...

Note: This page contains sample records for the topic "all-stars shine bright" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


421

Subwavelength optical microscopy in the far field  

E-Print Network [OSTI]

We present a procedure for subwavelength optical microscopy. The identical atoms are distributed on a plane and shined with a standing wave. We rotate the plane to different angles and record the resonant fluorescence spectra in the far field, from...

Sun, Qingqing; Al-Amri, M.; Scully, Marlan O.; Zubairy, M. Suhail.

2011-01-01T23:59:59.000Z

422

On the role of Mn(IV) vacancies in the photoreductive dissolution of hexagonal birnessite  

E-Print Network [OSTI]

2005) Perovskites - Oxygen vacancies shine blue. Nat. Mater.Ciccacci F. (2007) Oxygen vacancies and induced changes inTiO 2 doped by N, Nd, and vacancy. Solid State Commun. 136,

Kwon, K.D.

2009-01-01T23:59:59.000Z

423

Energy 101: Solar PV | Department of Energy  

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

Solar PV Energy 101: Solar PV Addthis Description Solar photovoltaic (PV) systems can generate clean, cost-effective power anywhere the sun shines. This video shows how a PV panel...

424

Development of an asynchronous solar-powered cooker  

E-Print Network [OSTI]

One reason that solar cookers have not gained widespread acceptance is because their use has proved inconvenient and impractical. Users are restricted to cooking when, and where, the sun is shining. Furthermore, the cooking ...

Akinwale, P. Femi (Pamela Femi)

2006-01-01T23:59:59.000Z

425

E-Print Network 3.0 - aspect ratio hydrogen Sample Search Results  

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

Summary: of fuel cells is an extremely important aspect in the production of hydrogen. Fuel cells function... HYDROGEN There is a good chance that hydrogen will be the shining...

426

The Year of Concentrating Solar Power: Five New Plants to Power...  

Office of Environmental Management (EM)

a power block to generate electricity. The technology can generate energy even when the sun isn't shining, helping to provide clean power at times of peak demand. We recently...

427

Surface modification of indium tin oxide by plasma treatment: An effective method to improve the efficiency, brightness, and reliability of organic  

E-Print Network [OSTI]

Surface modification of indium tin oxide by plasma treatment: An effective method to improve; accepted for publication 7 January 1997 We demonstrate the improvement of an indium tin oxide anode contact conductivity, and effi- ciency as a hole injector into organic materials, indium tin oxide ITO has been widely

428

Astron. Nachr. / AN 329, No. 7, 1 7 (2008) / DOI 10.1002/asna.2008xxxxx High-resolution observations of extremely bright penumbral grains  

E-Print Network [OSTI]

-located with the cluster is displaced from the middle penumbra closer towards the umbra and that the radial outflow it is well known that about three quarters of the penum- bral grains move towards the umbra whereas

429

The Bright Gamma-Ray Burst 991208 - Tight Constraints on Afterglow Models from Observations of the Early-Time Radio Evolution  

E-Print Network [OSTI]

The millimeter wavelength emission from GRB 991208 is the second brightest ever detected, yielding a unique data set. We present here well-sampled spectra and light curves over more than two decades in frequency for a two-week period. This data set has allowed us for the first time to trace the evolution of the characteristic synchrotron self-absorption frequency nu_a and peak frequency nu_m, and the peak flux density F_m: we obtain nu_a \\propto t^{-0.15 +- 0.12}, nu_m \\propto t^{-1.7 +- 0.4}, and $_m \\propto t^{-0.47 +- 0.11}. From the radio data we find that models of homogeneous or wind-generated ambient media with a spherically symmetric outflow can be ruled out. A model in which the relativistic outflow is collimated (a jet) can account for the observed evolution of the synchrotron parameters, the rapid decay at optical wavelengths, and the observed radio to optical spectral flux distributions that we present here, provided that the jet transition has not been fully completed in the first two weeks after the event. These observations provide additional evidence that rapidly decaying optical/X-ray afterglows are due to jets and that such transitions either develop very slowly or perhaps never reach the predicted asymptotic decay F(t) \\propto t^{-p}.

T. J. Galama; M. Bremer; F. Bertoldi; K. M. Menten; U. Lisenfeld; D. S. Shepherd; B. Mason; F. Walter; G. G. Pooley; D. A. Frail; R. Sari; S. R. Kulkarni; E. Berger; J. S. Bloom; A. J. Castro-Tirado; J. Granot

2000-06-14T23:59:59.000Z

430

Time-dependent, x-ray spectral unfolds and brightness temperatures for intense Li{sup +} ion beam-driven hohlraums  

SciTech Connect (OSTI)

X-ray-producing hohlraums are being studied as indirect drives for inertial confinement fusion targets. In a 1994 target series on the PBFAII accelerator, cylindrical hohlraum targets were heated by an intense Li{sup +} ion beam and viewed by an array of 13 time-resolved, filtered x-ray detectors (XRDs). The unfold operator (UFO) code and its suite of auxiliary functions were used extensively in obtaining time-resolved x-ray spectra and radiation temperatures from this diagnostic. The UFO was also used to obtain fitted response functions from calibration data, to simulate data from blackbody x-ray spectra of interest, to determine the suitability of various unfolding parameters (e.g., energy domain, energy partition, smoothing conditions, and basis functions), to interpolate the XRD signal traces, and to unfold experimental data. The simulation capabilities of the code were useful in understanding an anomalous feature in the unfolded spectra at low photon energies ({le}100 eV). Uncertainties in the differential and energy-integrated unfolded spectra were estimated from uncertainties in the data. The time{endash}history of the radiation temperature agreed well with independent calculations of the wall temperature in the hohlraum. {copyright} {ital 1997 American Institute of Physics.}

Fehl, D.L.; Chandler, G.A.; Biggs, F.; Dukart, R.J.; Moats, A.R.; Leeper, R.J. [Sandia National Laboratories Albuquerque, New Mexico 87185 (United States)] [Sandia National Laboratories Albuquerque, New Mexico 87185 (United States)

1997-01-01T23:59:59.000Z

431

Time-dependent, x-ray spectral unfolds and brightness temperatures for intense Li{sup +} ion beam-driven hohlraums  

SciTech Connect (OSTI)

X-ray-producing hohlraums are being studied as indirect drives for Inertial Confinement Fusion targets. In a 1994 target series on the PBFAII accelerator, cylindrical hohlraum targets were heated by an intense Li{sup +} ion beam and viewed by an array of 13 time-resolved, filtered x-ray detectors (XRDs). The UFO unfold code and its suite of auxiliary functions were used extensively in obtaining time- resolved x-ray spectra and radiation temperatures from this diagnostic. UFO was also used to obtain fitted response functions from calibration data, to simulate data from blackbody x-ray spectra of interest, to determine the suitability of various unfolding parameters (e.g., energy domain, energy partition, smoothing conditions, and basis functions), to interpolate the XRD signal traces, and to unfold experimental data. The simulation capabilities of the code were useful in understanding an anomalous feature in the unfolded spectra at low photon energies ({le} 100 eV). Uncertainties in the differential and energy-integrated unfolded spectra were estimated from uncertainties in the data. The time-history of the radiation temperature agreed well with independent calculations of the wall temperature in the hohlraum.

Fehl, D.L.; Chandler, G.A.; Biggs, F.; Dukart, R.J.; Moats, A.R.; Leeper, R.J.

1996-07-01T23:59:59.000Z

432

1FGL J1417.7-4407: A gamma-ray bright binary with a massive neutron star and a giant secondary  

E-Print Network [OSTI]

We present multiwavelength observations of the persistent Fermi-LAT unidentified gamma-ray source 1FGL J1417.7-4407, showing it is likely to be associated with a newly discovered X-ray binary containing a massive neutron star (nearly 2 M_sun) and a ~ 0.4 M_sun giant secondary with a 5.4 day period. SOAR optical spectroscopy at a range of orbital phases reveals variable double-peaked H-alpha emission, consistent with the presence of an accretion disk. The lack of radio emission and evidence for a disk suggests the gamma-ray emission is unlikely to originate in a pulsar magnetosphere, but could instead be associated with a pulsar wind, relativistic jet, or could be due to synchrotron self-Compton at the disk/magnetosphere boundary. Assuming a wind or jet, the high ratio of gamma-ray to X-ray luminosity (~ 20) suggests efficient production of gamma-rays, perhaps due to the giant companion. The system appears to be a low-mass X-ray binary that has not yet completed the pulsar recycling process. This system is a g...

Strader, Jay; Cheung, C C; Sand, David J; Donato, Davide; Corbet, Robin; Koeppe, Dana; Edwards, Philip G; Stevens, Jamie; Petrov, Leonid; Salinas, Ricardo; Peacock, Mark; Finzell, Thomas; Reichart, Daniel; Haislip, Joshua

2015-01-01T23:59:59.000Z

433

Low surface brightness galaxies rotation curves in the low energy limit of $R^n$ gravity no need for dark matter?  

E-Print Network [OSTI]

We investigate the possibility that the observed flatness of the rotation curves of spiral galaxies is not an evidence for the existence of dark matter haloes, but rather a signal of the breakdown of General Relativity. To this aim, we consider power - law fourth order theories of gravity obtained by replacing the scalar curvature $R$ with $f(R) = f_0 R^n$ in the gravity Lagrangian. We show that, in the low energy limit, the gravitational potential generated by a pointlike source may be written as $\\Phi(r) \\propto r^{-1} \\left [ 1 + (r/r_c)^{\\beta} \\right ]$ with $\\beta$ a function of the slope $n$ of the gravity Lagrangian and $r_c$ a scalelength depending on the gravitating system properties. In order to apply the model to realistic systems, we compute the modified potential and the rotation curve for spherically symmetric and for thin disk mass distributions. It turns out that the potential is still asymptotically decreasing, but the corrected rotation curve, although not flat, is higher than the Newtonian...

Capozziello, S; Troisi, A

2006-01-01T23:59:59.000Z

434

Eclipsing binaries observed with the WIRE satellite I. Discovery and photometric analysis of the new bright A0IV eclipsing binary Psi Centauri  

E-Print Network [OSTI]

Determinations of stellar mass and radius with realistic uncertainties at the level of 1% provide important constraints on models of stellar structure and evolution. We present a high-precision light curve of the A0IV star Psi Centauri, from the star tracker on board the WIRE satellite and the Solar Mass Ejection Imager camera on the Coriolis spacecraft. The data show that Psi Cen is an eccentric eclipsing binary system with a relatively long orbital period. The WIRE light curve extends over 28.7 nights and contains 41334 observations with 2 mmag point-to-point scatter. The eclipse depths are 0.28 and 0.16 mag, and show that the two eclipsing components of Psi Cen have very different radii. As a consequence, the secondary eclipse is total. We find the eccentricity to be e=0.55 with an orbital period of 38.8 days from combining the WIRE light curve with data taken over two years from the Solar Mass Ejection Imager camera. We have fitted the light curve with EBOP and have assessed the uncertainties of the resulting parameters using Monte Carlo simulations. The fractional radii of the stars and the inclination of the orbit have random errors of only 0.1% and 0.01 degrees, respectively, but the systematic uncertainty in these quantities may be somewhat larger. We have used photometric calibrations to estimate the effective temperatures of the components of Psi Cen to be 10450+-300 and 8800+-300 K, indicating masses of about 3.1 and 2.0 Msun. There is evidence in the WIRE light curve for g-mode pulsations in the primary star.

H. Bruntt; J. Southworth; G. Torres; A. J. Penny; J. V. Clausen; D. L. Buzasi

2006-06-22T23:59:59.000Z

435

Published in: Journal of Geophysical ResearchVOL.100E10 21,119--21,234, October 25, 1995. Low brightness temperatures of Martian Polar caps : CO 2  

E-Print Network [OSTI]

to the condensation of CO 2 in the atmosphere. We have used a combination of data analysis and modeling to compare to the frost point of CO 2 gas, CO 2 condenses, and polar ice caps are formed. The surface temperature which have directly condensed on the ground could have an emissivity close to unity and in any case much

Forget, François

436

Published in: Journal of Geophysical ResearchVOL.100-E10 21,11921,234, October 25, 1995. Low brightness temperatures of Martian Polar caps : CO  

E-Print Network [OSTI]

to the condensation of CO¢ in the atmosphere. We have used a combination of data analysis and modeling to compare to the frost point of CO¤ gas, CO¤ condenses, and polar ice caps are formed. The surface temperature which have directly condensed on the ground could have an emissivity close to unity and in any case much

Forget, François

437

Multi-wavelength observations of 3C 279 during the extremely bright gamma-ray flare in 2014 March-April  

E-Print Network [OSTI]

The well studied blazar 3C 279 underwent a giant $\\gamma$-ray outburst in 2014 March-April. The measured $\\gamma$-ray flux (1.21 $\\pm$ 0.10 $\\times$ 10$^{-5}$ ph cm$^{-2}$ s$^{-1}$ in 0.1-300 GeV energy range) is the highest detected from 3C 279 by Fermi Large Area Telescope. Hour scale $\\gamma$-ray flux variability are observed, with a flux doubling time as short as 1.19 $\\pm$ 0.36 hours detected during one flare. The $\\gamma$-ray spectrum is found to be curved at peak of the flare suggesting low probability of detecting very high energy (VHE; E $>$ 100 GeV) emission, which is further confirmed by the Very Energetic Radiation Imaging Telescope Array System observations. The $\\gamma$-ray flux increased by more than an order in comparison to low activity state and the flare consists of multiple sub-structures having fast rise and slow decay profile. The flux enhancement is seen in all the wavebands though at a lesser extent compared to $\\gamma$-rays. During the flare, a considerable amount of the kinetic jet p...

Paliya, Vaidehi S; Stalin, C S

2015-01-01T23:59:59.000Z

438

Submm-bright X-ray absorbed QSOs at z~2: insights into the co-evolution of AGN and star-formation  

E-Print Network [OSTI]

We have assembled a sample of 5 X-ray-absorbed and submm-luminous type 1 QSOs at $z \\sim 2$ which are simultaneously growing their central black holes through accretion and forming stars copiously. We present here the analysis of their rest-frame UV to submm Spectral Energy Distributions (SEDs), including new Herschel data. Both AGN (direct and reprocessed) and Star Formation (SF) emission are needed to model their SEDs. From the SEDs and their UV-optical spectra we have estimated the masses of their black holes $M_{BH}\\sim 10^{9}-10^{10}\\,M_{\\odot}$, their intrinsic AGN bolometric luminosities $L_{BOL}\\sim(0.8 - 20)\\times 10^{13} L_{\\odot}$, Eddington ratios $L_{BOL}/L_{Edd}\\sim 0.1 - 1.1$ and bolometric corrections $L_{BOL}/L_{X,2-10}\\sim 30 - 500$. These values are common among optically and X-ray-selected type 1 QSOs (except for RX~J1249), except for the bolometric corrections, which are higher. These objects show very high far-infrared luminosities $L_{FIR}\\sim$ (2 - 8)$\\times10^{12}\\,M_{\\odot}$ and Star...

Khan-Ali, A; Page, M J; Stevens, J A; Mateos, S; Symeonidis, M; Orjales, J M Cao

2015-01-01T23:59:59.000Z

439

The Complete Census of 70-um-Bright Debris Disks within the FEPS (Formation and Evolution of Planetary Systems) Spitzer Legacy Survey of Sun-like Stars  

E-Print Network [OSTI]

(abbreviated) We report detection with the Spitzer Space Telescope of cool dust surrounding solar type stars. The observations were performed as part of the Legacy Science Program, ``Formation and Evolution of Planetary Systems'' (FEPS). From the overall FEPS sample (Meyer et al. 2006) of 328 stars having ages ~0.003-3 Gyr we have selected sources with 70 um flux densities indicating excess in their spectral energy distributions above expected photospheric emission........ .....The rising spectral energy distributions towards - and perhaps beyond - 70 um imply dust temperatures T_dust temperature, location, fractional luminosity, and mass of the dust from fitted single temperature blackbody models. For >1/3 of the debris sources we find that multiple temperature components are suggested, implying a spatial distribution of dust extending over many tens of AU. Because the disks are dominated by collisional processes, the parent body (planetesimal) belts may be extended as well. Preliminary assessment of the statistics of cold debris around sun-like stars shows that ~10% of FEPS targets with masses between 0.6 and 1.8 Msun and ages between 30 Myr and 3 Gyr exhibit 70 um emission in excess of the expected photospheric flux density. We find that fractional excess amplitudes appear higher for younger stars and that there may be a trend in 70 um excess frequency with stellar mass.

Lynne A. Hillenbrand; John M. Carpenter; Jinyoung Serena Kim; Michael R. Meyer; Dana E. Backman; Amaya Moro-Martin; David J. Hollenbach; Dean C. Hines; Ilaria Pascucci; Jeroen Bouwman

2007-12-30T23:59:59.000Z

440

On the Results of Measurements of the Direct Sun Radiation Flux by Actinometer and of Maximal Polarization of Sky Brightness in the Solar Almucantar  

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:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr MayAtmosphericNuclear Security Administration the1 - September 2006 The 2002 WholesaleEnergy's 1000 acres of landJune 2013|

Note: This page contains sample records for the topic "all-stars shine bright" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


441

Morphological diversity of cell types in macaque monkey visual system  

E-Print Network [OSTI]

MicroBrightField, Williston, VT). Shrinkage correction,software (MicroBrightField, Williston, VT). Quantificationssoftware (MicroBrightField, Williston, VT) to examine the

Nhan, Hoang Luat

2010-01-01T23:59:59.000Z

442

Contributions of early parallel pathways to extrastriate visual cortex in macaque monkey  

E-Print Network [OSTI]

MicroBrightField, Williston, VT). For the fluorescentsoftware (MicroBrightField, Williston, VT). Only cell bodiessoftware (MicroBrightField, Williston, VT). Reconstructions

Nassi, Jonathan J.

2007-01-01T23:59:59.000Z

443

The architecture of the mouse trigeminal-facial brainstem : disynaptic circuitry, genomic organization, and follicle mechanics  

E-Print Network [OSTI]

MicroBrightField Inc. , Williston, VT). Brain traces wereMicroBrightField, Inc. , Williston, VT) according to the

Matthews, David William; Matthews, David William

2012-01-01T23:59:59.000Z

444

Social behavior from a comparative neuroanatomical perspective : the amygdala in human evolution  

E-Print Network [OSTI]

software (MicroBrightField,Williston, VT) using the 1x andsuite (MicroBrightField,Williston, VT). The anatomical

Barger, Nicole L.

2012-01-01T23:59:59.000Z

445

Notice of Intent to Issue Funding Opportunity for Integrated PV and Energy Storage Systems  

Broader source: Energy.gov [DOE]

As solar power plants proliferate, the variability and uncertainty of the solar resource poses challenges for integrating PV with electric power systems at both the distribution and bulk system levels. In response to these challenges, the U.S. Department of Energy Office of Energy Efficiency and Renewable Energy (EERE) has issued a notice of intent (NOI) to release the SunShot Sustainable and Holistic IntegratioN of Energy storage and Solar (SHINES) funding opportunity. SHINES will enable the holistic design, development, and widespread sustainable deployment of low-cost, flexible, and reliable energy storage solutions, and will strive to successfully integrate these solutions into PV power plants. SHINES projects can also focus on demand response and load management to achieve target metrics.

446

Hadron Production at Fixed Target Energies and Extensive Air Showers  

E-Print Network [OSTI]

NA61/SHINE is a fixed-target experiment to study hadron production in hadron-nucleus and nucleus-nucleus collisions at the CERN SPS. Due to the very good acceptance and particle identification in forward direction, NA61/SHINE is well suited for measuring particle production to improve the reliability of air shower simulations. Data with proton and pion beams have been taken in 2007 and 2009. First analysis results for the pion yield in proton-carbon interactions at 31 GeV will be shown and compared to predictions from models used in air shower simulations.

M. Unger; for the NA61/SHINE Collaboration

2010-12-12T23:59:59.000Z

447

UV-BRIGHT NEARBY EARLY-TYPE GALAXIES OBSERVED IN THE MID-INFRARED: EVIDENCE FOR A MULTI-STAGE FORMATION HISTORY BY WAY OF WISE AND GALEX IMAGING  

SciTech Connect (OSTI)

In the local universe, 10% of massive elliptical galaxies are observed to exhibit a peculiar property: a substantial excess of ultraviolet emission than what is expected from their old, red stellar populations. Several origins for this ultraviolet excess (UVX) have been proposed including a population of hot young stars and a population of old, blue horizontal branch or extended horizontal branch (BHB or EHB) stars that have undergone substantial mass loss from their outer atmospheres. We explore the radial distribution of UVX in a selection of 49 nearby E/S0-type galaxies by measuring their extended photometry in the UV through mid-infrared (mid-IR) with the Galaxy Evolution Explorer (GALEX), the Sloan Digital Sky Survey, and the Wide-field Infrared Survey Explorer (WISE). We compare UV/optical and UV/mid-IR colors with the Flexible Stellar Population Synthesis models, which allow for the inclusion of EHB stars. We find that combined WISE mid-IR and GALEX UV colors are more effective in distinguishing models than optical colors, and that the UV/mid-IR combination is sensitive to the EHB fraction. There are strong color gradients, with the outer radii bluer than the inner half-light radii by {approx}1 mag. This color difference is easily accounted for with an increase in the BHB fraction of 0.25 with radius. We estimated that the average ages for the inner and outer radii are 7.0 {+-} 0.3 Gyr, and 6.2 {+-} 0.2 Gyr, respectively, with the implication that the outer regions are likely to have formed {approx}1 Gyr after the inner regions. Additionally, we find that metallicity gradients are likely not a significant factor in the color difference. The separation of color between the inner and outer regions, which agrees with a specific stellar population difference (e.g., higher EHB populations), and the {approx}0.5-2 Gyr age difference suggests multi-stage formation. Our results are best explained by inside-out formation: rapid star formation within the core at early epochs (>4 Gyr ago) and at least one later stage starburst event coinciding with z {approx} 1.

Petty, S. M.; Farrah, D. G. [Department of Physics, Virginia Tech, Blacksburg, VA 24061 (United States); Neill, J. D.; Bridge, C. R. [Division of Physics, Math, and Astronomy, California Institute of Technology, Pasadena, CA 91125 (United States); Jarrett, T. H.; Tsai, C.-W. [Astronomy Department, University of Cape Town, Rondebosch 7701 (South Africa); Blain, A. W. [Department of Physics and Astronomy, University of Leicester, Leicester LE1 7RH (United Kingdom); Rich, R. M.; Lake, S. E.; Wright, E. L. [Department of Physics and Astronomy, University of California, Los Angeles, CA 90095 (United States); Benford, D. J. [NASA, Goddard Space Flight Center, Greenbelt, MD 20771 (United States); Masci, F. J. [IPAC, California Institute of Technology, Pasadena, CA 91125 (United States)

2013-10-01T23:59:59.000Z

448

This paper presents the realization and comprehensive characterization of a compact bright source of ultrafast synchrotron radiation with appreciable degree of spatial coherence. It has been drawn to our attention that we had inadvertently neglected to ci  

E-Print Network [OSTI]

of synchrotron X-ray radiation from relativistic laser-plasma interaction and laser-accelerated electrons. Phys oscillations of electrons accelerated in laser wakefields characterized by spectral X-ray analysis. Phys. Rev measurement based on Fresnel diffraction from laser-based synchrotron radiation demonstrating the resolution

Loss, Daniel

449

Synthesis and photoluminescence properties of the high-brightness Eu{sup 3+}-doped M{sub 2}Gd{sub 4}(MoO{sub 4}){sub 7} (M=Li, Na) red phosphors  

SciTech Connect (OSTI)

A series of red-emitting phosphors Eu{sup 3+}-doped M{sub 2}Gd{sub 4}(MoO{sub 4}){sub 7} (M=Li, Na) have been successfully synthesized at 850 Degree-Sign C by solid state reaction. The excitation spectra of the two phosphors reveal two strong excitation bands at 396 nm and 466 nm, respectively, which match well with the two popular emissions from near-UV and blue light-emitting diode chips. The intensity of the emission from {sup 5}D{sub 0} to {sup 7}F{sub 2} of M{sub 2}(Gd{sub 1-x}Eu{sub x}){sub 4}(MoO{sub 4}){sub 7} phosphors with the optimal compositions of x=0.85 for Li or x=0.70 for Na is about five times higher than that of Y{sub 2}O{sub 3}:Eu{sup 3+}. The quantum efficiencies of the entitled phosphors excited under 396 nm and 466 nm are also investigated and compared with commercial phosphors Sr{sub 2}Si{sub 5}N{sub 8}:Eu{sup 2+} and Y{sub 3}A{sub 5}O{sub 12}:Ce{sup 3+}. The experimental results indicate that the Eu{sup 3+}-doped M{sub 2}Gd{sub 4}(MoO{sub 4}){sub 7} (M=Li, Na) phosphors are promising red-emitting phosphors pumped by near-UV and blue light. - Graphical Abstract: The intensity of the red emission of M{sub 2}(Gd{sub 1-x}Eu{sub x}){sub 4}(MoO{sub 4}){sub 7} (M=Li, Na) phosphors with the optimal compositions is about five times higher than that of Y{sub 2}O{sub 3}:Eu{sup 3+}. Highlights: Black-Right-Pointing-Pointer Two novel Eu{sup 3+}-doped red phosphors (Na{sub 2}Gd{sub 4}(MoO{sub 4}){sub 2}, Li{sub 2}Gd{sub 4}(MoO{sub 4}){sub 7}) were synthesized. Black-Right-Pointing-Pointer Their emission intensities are about five times higher than that of Y{sub 2}O{sub 3}:Eu{sup 3+}. Black-Right-Pointing-Pointer Their quantum efficiencies are higher than that of commercial red phosphor Sr{sub 2}Si{sub 5}N{sub 8}:Eu{sup 2+}.

Zhao Chengchun [Key Laboratory of Materials for High Power Laser, Shanghai Institute of Optics and Fine Mechanics, Chinese Academy of Sciences, Shanghai 201800 (China); Graduate School of Chinese Academy of Sciences, Beijing 100039 (China); Yin Xin [CAS Key Laboratory of Materials for Energy Conversion, Shanghai Institute of Ceramics, Chinese Academy of Sciences, Shanghai 200050 (China); Huang Fuqiang, E-mail: huangfq@mail.sic.ac.cn [CAS Key Laboratory of Materials for Energy Conversion, Shanghai Institute of Ceramics, Chinese Academy of Sciences, Shanghai 200050 (China); Hang Yin, E-mail: yhang@siom.ac.cn [Key Laboratory of Materials for High Power Laser, Shanghai Institute of Optics and Fine Mechanics, Chinese Academy of Sciences, Shanghai 201800 (China)

2011-12-15T23:59:59.000Z

450

EXPLORING THE CENTRAL SUB-PARSEC REGION OF THE {gamma}-RAY BRIGHT RADIO GALAXY 3C 84 WITH VLBA AT 43 GHz IN THE PERIOD OF 2002-2008  

SciTech Connect (OSTI)

Following the discovery of a new radio component right before the GeV {gamma}-ray detection since 2008 August by the Fermi Gamma-ray Space Telescope, we present a detailed study of the kinematics and light curve on the central sub-parsec scale of 3C 84 using the archival Very Long Baseline Array 43 GHz data covering the period between 2002 January and 2008 November. We find that the new component 'C3', previously reported by the observations with the Very Long Baseline Interferometer Exploration of Radio Astrometry, was already formed in 2003. The flux density of C3 increases moderately until 2008, and then it becomes brighter rapidly after 2008. The radio core, C1, also shows a similar trend. The apparent speed of C3 with reference to the core C1 shows moderate acceleration from 0.10c to 0.47c between 2003 November and 2008 November, but is still sub-relativistic. We further try to fit the observed broadband spectrum by the one-zone synchrotron self-Compton model using the measured apparent speed of C3. The fit can reproduce the observed {gamma}-ray emission, but does not agree with the observed radio spectral index between 22 and 43 GHz.

Suzuki, Kenta [Institute of Astronomy, University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015 (Japan); Nagai, Hiroshi; Kino, Motoki; Kobayashi, Hideyuki [National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 (Japan); Kataoka, Jun [Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555 (Japan); Asada, Keiichi; Inoue, Makoto [Institute of Astronomy and Astrophysics, Academia Sinica, P.O. Box 23-141, Taipei 10617, Taiwan, R.O.C. (China); Doi, Akihiro [Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Yoshinodai 3-1-1, Chuo-ku, Sagamihara 252-5210 (Japan); Orienti, Monica; Giovannini, Gabriele; Giroletti, Marcello [INAF Istituto di Radioastronomia, via Gobetti 101, 40129 Bologna (Italy); Laehteenmaeki, Anne; Tornikoski, Merja; Leon-Tavares, Jonathan [Aalto University Metsaehovi Radio Observatory, Metsaehovintie 114, FIN-02540 Kylmaelae (Finland); Bach, Uwe [Max-Planck-Institut fuer Radioastronomie, Auf dem Huegel 69, 53121 Bonn (Germany); Kameno, Seiji [Faculty of Science, Kagoshima University, 1-21-35 Korimoto, Kagoshima 890-0065 (Japan)

2012-02-20T23:59:59.000Z

451

Renewable Energy Economic Development  

E-Print Network [OSTI]

Renewable Energy Economic Development Dick Sheehy & Nate Monosoff, CH2M HILL March, 2010 #12;Contents 1. Who is CH2M HILL? 2. Why Do We Need Renewables? 3. Where Is The Wind Blowing? 4. Where Is The Sun Shining? 5. How To Catch Some Rays? 6. Renewable Related 2 Proprietary & Confidential #12;Where

452

Global warming and its implications for conservation. 3. How does it work? Part two: atmospheric science and the layer model  

E-Print Network [OSTI]

that energy comes in from the sun and shines back out to space as IR. The main points are: 1. The outflow of IR energy from a planet must balance heating from the sun. 2. The planet accomplishes this balance warms the surface of the planet as it moves toward an equilibrium of energy fluxes in and out. The layer

Creel, Scott

453

New High-Temperature Superconductors  

E-Print Network [OSTI]

much of each gets made. Water to Burn RENEWABLE ENERGY SOURCES, SUCH AS WIND AND SOLAR POWER, have plenty going for them. They're abundant and carbon-free, and their prices are dropping. But they're part-timers. Even when the sun is shining and the wind is blowing, there is no good way to store excess electricity

Heller, Eric

454

RESEARCH REPORT 2012 ResearchResearchResearch  

E-Print Network [OSTI]

's `smoking gun' PARTNERSHIPS 18 Community heals itself through university partnership 19 Supply chain 26 Thirsty for global water solutions 28 Building peace from big picture to leverage point 29 Spotlight, praise shine on filmmakers 30 Hometown global manufacturing 31 Metal heavy with meaning 32

Saldin, Dilano

455

RESEARCH REPORT 2012 On the cover: Junhong Chen, a professor of mechanical engineering at  

E-Print Network [OSTI]

's `smoking gun' PARTNERSHIPS 18 Community heals itself through university partnership 19 Supply chain 26 Thirsty for global water solutions 28 Building peace from big picture to leverage point 29 Spotlight, praise shine on filmmakers 30 Hometown global manufacturing 31 Metal heavy with meaning 32

Saldin, Dilano

456

Feasibility of a Small Scale Intensity Correlation Interferometer  

E-Print Network [OSTI]

double slit image. The interferometer consists of 2 avalanche photo-diodes connected to a data acquisition computer. The image is produced by shining light through the double slit image an image containment system. The sensors are placed at the far end...

Kelderman, Gregory Peter

2013-04-29T23:59:59.000Z

457

Published: September 13, 2011 r 2011 American Chemical Society 1601 dx.doi.org/10.1021/tx200316x |Chem. Res. Toxicol. 2011, 24, 16011609  

E-Print Network [OSTI]

applica- tions including fire-fighting foam, additives in self-shine floor polishes, cement, lubricants, and oil repellants in food packages.1 Two classes of perfluor- oalkyl chemicals that are commonly measured effects, tumorigenesis, developmental toxicity, and immunotoxicity,4?6 there remains considerable interest

Omiecinski, Curtis

458

Photovoltaic Crystalline Silicon Cell Basics  

Broader source: Energy.gov [DOE]

To separate electrical charges, crystalline silicon cells must have a built-in electric field. Light shining on crystalline silicon may free electrons within the crystal lattice, but for these electrons to do useful worksuch as provide electricity to a light bulbthey must be separated and directed into an electrical circuit.

459

Storing Renewable Energy in Chemical Bonds  

ScienceCinema (OSTI)

With nearly 7 billion people, the world's population is demanding more electricity every year. Improved technologies are bringing wind and solar power to our electrical grid. However, wind turbines and solar panels only work when the wind blows or the sun shines. PNNL scientists discuss catalysis approaches for storing and releasing energy on demand.

Helm, Monte; Bullock, Morris

2014-06-13T23:59:59.000Z

460

Storing Renewable Energy in Chemical Bonds  

SciTech Connect (OSTI)

With nearly 7 billion people, the world's population is demanding more electricity every year. Improved technologies are bringing wind and solar power to our electrical grid. However, wind turbines and solar panels only work when the wind blows or the sun shines. PNNL scientists discuss catalysis approaches for storing and releasing energy on demand.

Helm, Monte; Bullock, Morris

2013-03-27T23:59:59.000Z

Note: This page contains sample records for the topic "all-stars shine bright" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


461

WIND TOMOGRAPHY IN BINARY SYSTEMS O.Knill, R.Dgani and M.Vogel  

E-Print Network [OSTI]

WIND TOMOGRAPHY IN BINARY SYSTEMS O.Knill, R.Dgani and M.Vogel ETH-Zurich, CH-8092, Switzerland method is particularly suitable for determining the velocity laws of stellar winds. 1. WIND TOMOGRAPHY AND ABEL'S INTEGRAL Binary systems in which a compact, point-like radiation source shines through the wind

Knill, Oliver

462

argentina preliminary results: Topics by E-print Network  

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

argentina preliminary results First Page Previous Page 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 Next Page Last Page Topic Index 1 Delaware Will Shine...

463

THE STRATOSPHERETROPOSPHERE ANALYSES OF REGIONAL  

E-Print Network [OSTI]

, kenneth P. Bowman, elliot l. atlas, steVe c. wofsy, fUQing Zhang, James f. Bresch, Brian a. ridley, Jasna balance (e.g., Forster and Shine1997;Shepherd 2007). Because many trace con- stituents have relatively trace species distributions. Many meteorological phenom- ena such as Rossby waves, gravity waves (GWs

464

The Sun -II Alexei Gilchrist  

E-Print Network [OSTI]

The Sun - II Alexei Gilchrist #12;Some resources · http://www.nineplanets.org/sol.html · "The Universe: Secrets of the Sun" video ­ Search on youtube (references are to clips here http in these slides Secrets of the Sun #12;Why does the sun shine? Long and fascinating history involving - geology

Wardle, Mark

465

This is a typical amateur-astronomer's green laser pointer, shown with a  

E-Print Network [OSTI]

arrested the preceding week after allegedly shining a green laser at a private jet on approach to a nearby airport and then at a police helicopter dispatched to search for the culprit. According to the criminal on the Use ... 8/19/10 9:32 AM http://www.printthis.clickability.com/pt/cpt?action=cpt&title=S... 1 of 5 #12

Barnes, Joshua Edward

466

Volume 10, No. 1 Decade of the Brain  

E-Print Network [OSTI]

Winter 2014 Volume 10, No. 1 SHINING A LIGHT ON BRAIN INJURY Decade of the Brain #12;ALSO of traumatic brain injury in children 14 "Hypoxia in a box" may reveal hidden concussion damage 18 Diabetes Clark, MSN'11, builds hope and health in Uganda Decade of the BRAIN #12;From 1990 through 2000, the U

Dolbow, John

467

Magnetotransport in low dimensional semiconductor structures  

E-Print Network [OSTI]

bias to the gate, one may capacitively induce carriers into the 2DEG. The carrier density in a GaAs-AIGaAs heterostructure, at low temper ature, can also be enhanced by shining an red light emitting diode (LED) onto the device. This has the effect...

Kim, Gil-Ho

1998-06-16T23:59:59.000Z

468

Center for Biotechnology Prof. Dr.-Ing. Gerhard Sagerer  

E-Print Network [OSTI]

developed innovative new courses of study which attract gifted students from all over the world. The CeBiTec not only shines in the international world of science; it also has important cooperation partners in many such as the application of biofuels, and for new microscope techniques, to name just a few. The CeBiTec has continually

Moeller, Ralf

469

Volume 130, Number 16 tech.mit.edu Friday, April 2, 2010 Oldest and Largest  

E-Print Network [OSTI]

of the health reform bill have yet to be felt, the passage of the bill shined a hard light on health care who has worked extensively with Democrats on health care reform. "The U.S. government now takes health's conse- quences by conducting new research and looking for new ways to fix health care ineffi- ciencies

Ishii, Hiroshi

470

110 NATURE PHYSICS | VOL 8 | FEBRUARY 2012 | www.nature.com/naturephysics news & views  

E-Print Network [OSTI]

the coupling between the movable mirror and the light2,3 . The resonator is displaced by forces generated expect that exciting the electrons in a piece of semiconductor by shining a laser on it would simply heat electrons do cause local heating of the semiconductor, they can also produce a dramatic cooling down

Loss, Daniel

471

The Long Way Home  

E-Print Network [OSTI]

'. They have a CB, I think." Ray opened his mouth and then closed it. "See you in about an hour, Benny." Ray reached for the flashlight kept under the stove and clicked it on. Shining the light, he saw the newspaper racks and grabbed a handful. They came...

Dawn, M.; Bennett, J.

2002-01-01T23:59:59.000Z

472

JOURNAL OF GEOPHYSICAL RESEARCH, VOL. ???, XXXX, DOI:10.1029/, Isotopic Fractionations in the TTL in cloud-resolving  

E-Print Network [OSTI]

. The results suggest that the sublimation of relatively enriched ice associated with deep convection affects and chemistry of the stratosphere and also of the earth as a whole [e.g., Forster and Shine, 1999; Kirk], hydration by overshooting deep convection through the in- jection and subsequent sublimation of ice [e

Blossey, Peter

473

THE DISCOVERY OF www.sciam.com Updated from the April 2000 issue 27  

E-Print Network [OSTI]

by the thermonuclear radiation from hydrogen fusion; once it begins, the star's size and luminosity stay constant. A star shines because of the thermonuclear reactions in its core, which release enormous amounts of energy by fusing hy- drogen into helium. For the fusion reactions to oc- cur, though, the temperature

Backer, Don

474

Atmos. Chem. Phys., 12, 69696982, 2012 www.atmos-chem-phys.net/12/6969/2012/  

E-Print Network [OSTI]

dioxide (CO2) forc- ing, and the influence of remote forcings often outweighs that of local forcings- tion and type. Aerosol and ozone forcings typically induce larger responses than equivalent carbon trading schemes or evaluation of mitigation scenarios use metrics based on global mean forc- ing (Shine et

Meskhidze, Nicholas

475

CORONAL ABUNDANCES IN ORION NEBULA CLUSTER STARS A. Maggio,1  

E-Print Network [OSTI]

pattern of abundances for all stars, although a weak dependence on flare loop size may be present. The abundance of calcium is the only one which appears to vary substantially between stars, but this quantity

Micela, Giusi

476

Draft version March 16, 2007 Preprint typeset using L A T E X style emulateapj v. 03/07/07  

E-Print Network [OSTI]

pattern of abundances for all stars, although a weak dependence on flare loop size may be present. The abundance of calcium is the only one which appears to vary substantially between stars, but this quantity

477

Lauren Andersen | Department of Energy  

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

Lauren Andersen About Us Lauren Andersen - Policy Advisor at White House Office of Science and Technology Policy Most Recent STEM Women All-Stars Hit the Road April 30...

478

Local functional input to neurons in deep layers of rat visual cortex  

E-Print Network [OSTI]

MicroBrightField, Inc. , Williston, VT; see Figs. 2.1B,MicroBrightField, Williston, VT). Each reconstructionsystem (MicroBrightField, Williston, VT). Each neuronal

Zarrinpar, Amir

2006-01-01T23:59:59.000Z

479

Compensatory Paracrine Mechanisms That Define The Urothelial Response to Injury in Partial Bladder Outlet Obstruction  

E-Print Network [OSTI]

3.19, MicroBrightField, Williston, Vermont). The application3.19, MicroBrightField, Williston, Vermont). The application

Lendvay,, Thomas S.

2008-01-01T23:59:59.000Z

480

Intrinsic and extrinsic mechanisms of corticospinal axon regeneration  

E-Print Network [OSTI]

MicroBrightField, Inc, Williston, VT). Random fields of viewMicroBrightField, Inc, Williston, VT) to estimate the total

Hollis, Edmund Roy

2008-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "all-stars shine bright" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


481

Microglial and neuronal abnormalities in the autistic brain  

E-Print Network [OSTI]

MicroBrightField, Williston, VT). In the density assessment,MicroBrightField, Williston, VT), on a Nikon Eclipse 80i

Morgan, John T.

2009-01-01T23:59:59.000Z

482

E-Print Network 3.0 - automatic fuzzy rule Sample Search Results  

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

PROCESSING TO PREDICT PULP BRIGHTNESS USING FUZZY LOGICPULP BRIGHTNESS USING FUZZY LOGIC Summary: Decision Support System (FuzzyFlou) Automatic Generation of Fuzzy Knowledge...

483

Paul Murdin how we discovered the cosMos  

E-Print Network [OSTI]

galaxies and therefore rather faint. The appearance of a bright, nearby supernova like Tycho Brahe's `new

McReynolds, Ben

484

Pion Production Cross-section Measurements in p+C Collisions at the CERN SPS for Understanding Extensive Air Showers  

E-Print Network [OSTI]

An important approach to studying high-energy cosmic rays is the investigation of the properties of extensive air showers; however, the lateral distribution of particles in simulations of such showers strongly depends on the applied model of low-energy hadronic interactions. It has been shown that many constraints to be applied to these models can be obtained by studying identified-particle spectra from accelerator collisions, in the energy range of the CERN Super Proton Synchrotron. Here we present measurements of the pion production cross-section obtained by the NA61/SHINE experiment at the SPS, in proton-carbon collisions at the beam energy of 31 GeV from the year 2007. Further analyses of identified-particle yields in SHINE, in particular with a pion beam, are in preparation.

Marek Szuba; for the NA61/SHINE Collaboration

2010-09-16T23:59:59.000Z

485

Two particle correlations from the energy scan with p+p interactions  

E-Print Network [OSTI]

The NA61/Shine experiment aims to discover the critical point of strongly interacting matter and study the properties of the onset of deconfinement. These goals are to be achieved by performing a two dimensional phase diagram T-mu_B scan by measurements of hadron production properties in proton-proton, proton-nucleus and nucleus-nucleus interactions as a function of collision energy and system size. Close to the phase transition and/or close to the critical point large fluctuations are predicted. In this contribution preliminary results on two-particle correlations in pseudorapidity and azimuthal angle will be presented for p+p interactions at beam momenta: 20, 31, 40, 80 and 158 GeV/c. The NA61/Shine results will be compared with the corresponding data of other experiments and model predictions. A striking evolution with collision energy is observed.

Maksiak, Bartosz

2015-01-01T23:59:59.000Z

486

Method of measuring a liquid pool volume  

DOE Patents [OSTI]

A method of measuring a molten metal liquid pool volume and in particular molten titanium liquid pools, including the steps of (a) generating an ultrasonic wave at the surface of the molten metal liquid pool, (b) shining a light on the surface of a molten metal liquid pool, (c) detecting a change in the frequency of light, (d) detecting an ultrasonic wave echo at the surface of the molten metal liquid pool, and (e) computing the volume of the molten metal liquid.

Garcia, Gabe V. (Las Cruces, NM); Carlson, Nancy M. (Idaho Falls, ID); Donaldson, Alan D. (Idaho Falls, ID)

1991-01-01T23:59:59.000Z

487

Laser cooling of solids  

SciTech Connect (OSTI)

We present an overview of solid-state optical refrigeration also known as laser cooling in solids by fluorescence upconversion. The idea of cooling a solid-state optical material by simply shining a laser beam onto it may sound counter intuitive but is rapidly becoming a promising technology for future cryocooler. We chart the evolution of this science in rare-earth doped solids and semiconductors.

Epstein, Richard I [Los Alamos National Laboratory; Sheik-bahae, Mansoor [UNM

2008-01-01T23:59:59.000Z

488

Rosencrantz & Guildenstern Are Dead and Obscured by Language  

E-Print Network [OSTI]

changes around them without their knowledge or consent; and the events happening around them are not only beyond their control, but beyond even their understanding. The result is an acrobatic display of linguistic pyrotechnics as well as a provocative.... The moving lights will be used for specials and for gobo washes all over the stage. I found that doing my lighting storyboard by photographing the models with actual lights and gels shining on them greatly influenced my color choices. I knew which...

Banks, Elizabeth

2010-04-27T23:59:59.000Z

489

A review of "Anne Conway: A Woman Philosopher." by Sarah Hutton  

E-Print Network [OSTI]

of a circle of great thinkers. Hutton claims that Conway led this group and set its agenda. Hutton also utilizes ?reconstructive archae- ology,? which Hutton defines as ?the history of her [Conway?s] philosophical activities ? pieced together ? from... Hutton remembers to bring Conway back into the analysis and shows the reader how Conway directly influenced a particular philosopher, her book shines. The historical approach that Hutton employed also led to limited success. Hutton rightly acknowledges...

Karol K. Weaver

2006-01-01T23:59:59.000Z

490

Effect of dietary protein level and source on reproductive performance and progeny development in swine fed sorghum-based diets  

E-Print Network [OSTI]

EFFECT OF DIETARY PROTEIN LE'i ~ L AND SOURCE ON REPRODUCTIVE PERFORMANCE AND PROGENY DEVELOPMENT IN SHINE FED SORGHUM-BASED DIETS A Thesis DOPRANCE GALEN HAUGHT Submitted to the Graduate College of Texas ASM University in partial fulfillment... of the requir ment for the degree of MASTER OF SCIENCE May 1974 Major Subject. Animal Nutrition EFFECT OF DIETARY PROTEIN LEVEL AND SOURCE ON REPRODUCTIVE PERFORMANCE AND PROGENY DEVELOPMENT IN SWINE FED SORGHUM-BASED DIETS A Thesis by DORRANCE GALEN...

Haught, Dorrance Galen

1974-01-01T23:59:59.000Z

491

Field emission from organic materials  

E-Print Network [OSTI]

Field emission displays (FEDs) show great promise as high performance flat panel displays. The light emission process is efficient, long lifetimes are possible with high brightness, and bright passive matrix displays can ...

Kymissis, Ioannis, 1977-

2003-01-01T23:59:59.000Z

492

APS Upgrade | Advanced Photon Source  

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

APS View Larger The brightness and energy of x-ray beams are critical properties for research. Higher brightness means more x-rays can be focused onto a smaller, laser-like spot,...

493

07/05/2013 21:46Evolution Of Black Holes Compared To Evolution Of Flight -Space News -redOrbit Page 1 of 3http://www.redorbit.com/news/space/1112839583/evolutionary-biology-applied-to-black-hole-manifestation-050713/  

E-Print Network [OSTI]

-long Gamma-Ray Bursts Dying Supergiant Stars Implicated in Hours-long Gamma-Ray Bursts NASA\\'s Fermi, Swift See \\'Shockingly Bright\\' Burst NASA\\'s Fermi, Swift See \\'Shockingly Bright\\' Burst Long Day

Reece, Sarah

494

firstchoiceF O R I N F O R M A T I O N , E D U C A T I O N A N D E N T E R T A I N M E N T M A Y 2 0 13 National Memorial Day  

E-Print Network [OSTI]

) and Gary Sinise (CSI: New York) for a night of remembrance, featuring an all-star line-up performing: Cologne to Zell" 9:00pm This Old House "Cambridge Project" Part 4 of 15 9:30m Hometime "Creekside Home Into Deep Space: The Birth of the Alma Observatory Monday 6th 8:00pm Rick Steves' Europe "Burgundy: Profound

Meyers, Steven D.

495

Type IIP supernovae as cosmological probes: A SEAM distance to SN 1999em  

E-Print Network [OSTI]

Type IIP Supernovae as Cosmological Probes: A SEAM Distanceintrinsic brightness, supernovae make excellent cosmologicalstars: atmospheres supernovae: 1999em Distances from

Baron, E.; Nugent, Peter E.; Branch, David; Hauschildt, Peter H.

2004-01-01T23:59:59.000Z

496

MBA CAREER CONNECTIONS CLASS OF 2011: CAREER EMPLOYMENT  

E-Print Network [OSTI]

Theranostics, Inc. * Booz Allen Hamilton, Inc. BrightScope, Inc. BumbleBee LLC California Center for Sustainable

Russell, Lynn

497

Tax Credits, Rebates & Savings | Department of Energy  

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

Eligibility: Agricultural, Commercial, Industrial, Nonprofit Savings Category: Heat Pumps, Lighting Residential Energy Efficiency Rebates (Offered by 11 Utilities) Bright...

498

Added JWST Science Cases for the Timeframe 2012-2015 A SAR Study  

E-Print Network [OSTI]

role in their application. Observations of the brightness of type Ia supernovae provided the first empirical indication for dark energ

Sirianni, Marco

499

E-Print Network 3.0 - advanced magnetic resonance Sample Search...  

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

(Namikawa, 1985; Gibbs, 1988) channels. These include studies... weak, synchrotron radiation brightness, together with resonant ... Source: Haskel, Daniel - Advanced Photon...

500

Impairments in experience-dependent cortical plasticity in aged animals  

E-Print Network [OSTI]

Neurolucida (MBF Bioscience, Williston, VT) and analyzedMicroBrightField Bioscience, Williston, VT). The area of the

Rickert, Jessica Louise

2009-01-01T23:59:59.000Z