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  1. Maldives-NREL Cooperation | Open Energy Information

    Open Energy Info (EERE)

    Maldives-NREL Cooperation Jump to: navigation, search Logo: Maldives-NREL Cooperation Name Maldives-NREL Cooperation AgencyCompany Organization National Renewable Energy...

  2. Maldives: Energy Resources | Open Energy Information

    Open Energy Info (EERE)

    Country Profile Name Maldives Population 393,500 GDP 1,944,000,000 Energy Consumption 0.01 Quadrillion Btu 2-letter ISO code MV 3-letter ISO code MDV Numeric ISO...

  3. MagStar Technologies | Open Energy Information

    Open Energy Info (EERE)

    MagStar Technologies Jump to: navigation, search Name: MagStar Technologies Place: Hopkins, MN Information About Partnership with NREL Partnership with NREL Yes Partnership Type...

  4. EA-306 MAG Energy Solutions, Inc. | Department of Energy

    Energy Savers [EERE]

    MAG Energy Solutions, Inc. EA-306 MAG Energy Solutions, Inc. Order authorizing MAG Energy Solutions, Inc. to export electric energy to Canada PDF icon EA-306 MAG Energy Solutions, Inc. More Documents & Publications EA-306-B MAG Energy Solutions, Inc. EA-306-A MAG Energy Solutions, Inc. Application to Export Electric Energy OE Docket No. EA-306-A MAG Energy Solutions

  5. EA-306-B MAG Energy Solutions, Inc. | Department of Energy

    Energy Savers [EERE]

    -B MAG Energy Solutions, Inc. EA-306-B MAG Energy Solutions, Inc. Order authorizing MAG Energy Solutions (MAG E.S.) to export electric energy to Canada. PDF icon EA-306-B MAG ES (CN).pdf More Documents & Publications EA-306-A MAG Energy Solutions, Inc. EA-388 TEC Energy Inc. EA-257-D Emera Energy Services

  6. EA-306-A MAG Energy Solutions, Inc. | Department of Energy

    Energy Savers [EERE]

    -A MAG Energy Solutions, Inc. EA-306-A MAG Energy Solutions, Inc. Order authorizing MAG Energy Solutions to export electric energy to Canada. PDF icon EA-306-A MAG ES CN.pdf More Documents & Publications EA-306-B MAG Energy Solutions, Inc. Application to Export Electric Energy OE Docket No. EA-306-A MAG Energy Solutions, Inc. EA-264-C ENMAX Energy Marketing

  7. MagViz Bottled Liquid Scanner at Albuquerque International Sunport

    ScienceCinema (OSTI)

    Surko, Stephen; Dennis, Steve; Espy, Michelle

    2014-08-12

    The next-generation bottled liquid scanner, MagViz BLS, is demonstrated at the Albuquerque International Sunport, New Mexico

  8. Magnetized liner inertial fusion (MagLIF)

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

    Magnetized liner inertial fusion (MagLIF) [1] is an inertial confinement fusion (ICF) scheme using cylindrical compression of magnetized, preheated DT gas. A 10 - 30 T axial magnetic field reduces electron thermal conductivity allowing near-adiabatic compression at implosion velocities of order 100 km/s, much lower than the 300 km/s or more required for conventional ICF. Preheating to at least 100 eV ensures that keV temperatures are reached with a convergence ratio no greater than 30. The

  9. M 1 Partners | Open Energy Information

    Open Energy Info (EERE)

    Partners Jump to: navigation, search Name: M-1 Partners Place: New York Product: M-1 Partners is a joint venture between Peter Marshall and Robert Ott with the objective of...

  10. Application to Export Electric Energy OE Docket No. EA-306-A MAG Energy

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

    Solutions, Inc. | Department of Energy Solutions, Inc. Application to Export Electric Energy OE Docket No. EA-306-A MAG Energy Solutions, Inc. Application from MAG Energy Solutions, Inc. to export electric energy to Canada PDF icon Application to xport Electric Energy OE Docket No. EA-306-A MAG Energy Solutions, Inc. More Documents & Publications EA-306-A MAG Energy Solutions, Inc. EA-306 MAG Energy Solutions, Inc. Application to Export Electric Energy OE Docket No. EA-306-A MAG Energy

  11. Observation of 690 MV m^-1 Electron Accelerating Gradient with...

    Office of Scientific and Technical Information (OSTI)

    Observation of 690 MV m-1 Electron Accelerating Gradient with a Laser-Driven Dielectric Microstructure Citation Details In-Document Search Title: Observation of 690 MV m-1...

  12. Application to Export Electric Energy OE Docket No. EA-306-A MAG Energy

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

    Solutions: Federal Register Notice Volume 75, No. 237 - Dec. 10, 2010 | Department of Energy Solutions: Federal Register Notice Volume 75, No. 237 - Dec. 10, 2010 Application to Export Electric Energy OE Docket No. EA-306-A MAG Energy Solutions: Federal Register Notice Volume 75, No. 237 - Dec. 10, 2010 Application from MAG Energy Solutions to esport electric energy to Canada. Federal Register Notice. PDF icon Application to Export Electric Energy OE Docket No. EA-3060-A MAG Energy

  13. Analysis of substrate specificity of Schizosaccharomyces pombe Mag1 alkylpurine DNA glycosylase

    SciTech Connect (OSTI)

    Adhikary, Suraj; Eichman, Brandt F.

    2014-10-02

    DNA glycosylases specialized for the repair of alkylation damage must identify, with fine specificity, a diverse array of subtle modifications within DNA. The current mechanism involves damage sensing through interrogation of the DNA duplex, followed by more specific recognition of the target base inside the active site pocket. To better understand the physical basis for alkylpurine detection, we determined the crystal structure of Schizosaccharomyces pombe Mag1 (spMag1) in complex with DNA and performed a mutational analysis of spMag1 and the close homologue from Saccharomyces cerevisiae (scMag). Despite strong homology, spMag1 and scMag differ in substrate specificity and cellular alkylation sensitivity, although the enzymological basis for their functional differences is unknown. We show that Mag preference for 1,N{sup 6}-ethenoadenine ({var_epsilon}A) is influenced by a minor groove-interrogating residue more than the composition of the nucleobase-binding pocket. Exchanging this residue between Mag proteins swapped their {var_epsilon}A activities, providing evidence that residues outside the extrahelical base-binding pocket have a role in identification of a particular modification in addition to sensing damage.

  14. ARM - VAP Product - visstpx08m1rv4minnis

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

    8m1rv4minnis Documentation visst : XDC documentation Data Management Facility Plots (Quick Looks) ARM Data Discovery Browse Data Comments? We would love to hear from you! Send us a note below or call us at 1-888-ARM-DATA. Send VAP Output : VISSTPX08M1RV4MINNIS VISST-derived pixel-level products from satellite MTSAT, version 4 Active Dates 2008.05.01 - 2008.12.31 Originating VAP Process Minnis Cloud Products Using Visst Algorithm : VISST Measurements The measurements below provided by this

  15. A background correction algorithm for Van Allen Probes MagEIS electron flux measurements

    SciTech Connect (OSTI)

    Claudepierre, S. G.; O'Brien, T. P.; Blake, J. B.; Fennell, J. F.; Roeder, J. L.; Clemmons, J. H.; Looper, M. D.; Mazur, J. E.; Mulligan, T. M.; Spence, H. E.; Reeves, G. D.; Friedel, R. H. W.; Henderson, M. G.; Larsen, B. A.

    2015-07-14

    We describe an automated computer algorithm designed to remove background contamination from the Van Allen Probes Magnetic Electron Ion Spectrometer (MagEIS) electron flux measurements. We provide a detailed description of the algorithm with illustrative examples from on-orbit data. We find two primary sources of background contamination in the MagEIS electron data: inner zone protons and bremsstrahlung X-rays generated by energetic electrons interacting with the spacecraft material. Bremsstrahlung X-rays primarily produce contamination in the lower energy MagEIS electron channels (~30500 keV) and in regions of geospace where multi-M eV electrons are present. Inner zone protons produce contamination in all MagEIS energy channels at roughly L < 2.5. The background-corrected MagEIS electron data produce a more accurate measurement of the electron radiation belts, as most earlier measurements suffer from unquantifiable and uncorrectable contamination in this harsh region of the near-Earth space environment. These background-corrected data will also be useful for spacecraft engineering purposes, providing ground truth for the near-Earth electron environment and informing the next generation of spacecraft design models (e.g., AE9).

  16. A background correction algorithm for Van Allen Probes MagEIS electron flux measurements

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

    Claudepierre, S. G.; O'Brien, T. P.; Blake, J. B.; Fennell, J. F.; Roeder, J. L.; Clemmons, J. H.; Looper, M. D.; Mazur, J. E.; Mulligan, T. M.; Spence, H. E.; et al

    2015-07-14

    We describe an automated computer algorithm designed to remove background contamination from the Van Allen Probes Magnetic Electron Ion Spectrometer (MagEIS) electron flux measurements. We provide a detailed description of the algorithm with illustrative examples from on-orbit data. We find two primary sources of background contamination in the MagEIS electron data: inner zone protons and bremsstrahlung X-rays generated by energetic electrons interacting with the spacecraft material. Bremsstrahlung X-rays primarily produce contamination in the lower energy MagEIS electron channels (~30–500 keV) and in regions of geospace where multi-M eV electrons are present. Inner zone protons produce contamination in all MagEIS energymore » channels at roughly L < 2.5. The background-corrected MagEIS electron data produce a more accurate measurement of the electron radiation belts, as most earlier measurements suffer from unquantifiable and uncorrectable contamination in this harsh region of the near-Earth space environment. These background-corrected data will also be useful for spacecraft engineering purposes, providing ground truth for the near-Earth electron environment and informing the next generation of spacecraft design models (e.g., AE9).« less

  17. ARM - VAP Product - visstpx04m1rv3minnis

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

    rv3minnis Documentation visst : XDC documentation Data Management Facility Plots (Quick Looks) ARM Data Discovery Browse Data Comments? We would love to hear from you! Send us a note below or call us at 1-888-ARM-DATA. Send VAP Output : VISSTPX04M1RV3MINNIS VISST-derived pixel-level products from satellite MTSAT, version 3 Active Dates 2007.10.01 - 2007.12.31

  18. ARM - VAP Product - visstpx04m1rv4minnis

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

    rv4minnis Documentation visst : XDC documentation Data Management Facility Plots (Quick Looks) ARM Data Discovery Browse Data Comments? We would love to hear from you! Send us a note below or call us at 1-888-ARM-DATA. Send VAP Output : VISSTPX04M1RV4MINNIS VISST-derived pixel-level products from satellite MTSAT, version 4 Active Dates 2008.01.01 - 2008.04.30

  19. ARM - VAP Product - visstpx04m1rv1minnis

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

    rv1minnis Documentation visst : XDC documentation Data Management Facility Plots (Quick Looks) ARM Data Discovery Browse Data Comments? We would love to hear from you! Send us a note below or call us at 1-888-ARM-DATA. Send VAP Output : VISSTPX04M1RV1MINNIS VISST-derived pixel-level products from satellite MTSAT, version 1 Active Dates 2006.01.01 - 2006.02.28 Originating VAP Process Minnis Cloud Products Using Visst Algorithm : VISST Measurements The measurements below provided by this product

  20. A Novel MagPipe Pipeline transportation system using linear motor drives

    SciTech Connect (OSTI)

    Fang, J.R.; Montgomery, D.B.; Roderick, L.

    2009-11-15

    A novel capsule pipeline transportation system using linear motor drives, called Magplane MagPipe, is under development with the intention to replace trucks and railways for hauling materials from the mine to the rail head, power plant, or processing plant with reduced operating cost and energy consumption. The initial demonstration of a MagPipe line in Inner Mongolia will be a 500-m-long double-pipe coal transport system with the design transportation capacity of 3 Mega-Mg per year. The pipeline consists of 6-m-long plastic pipe modules with an I-beam suspension system inside the pipe to carry sets of five coupled capsules. The pipe will also contain noncontinuous motor winding modules spaced at 50-m intervals. A set of Halbach-arrayed permanent magnets on the bottom of the capsules interact with the linear motor windings to provide propulsion. The motor is driven by variable frequency drives outside the pipe to control the speed. This paper briefly describes the overall MagPipe pipeline transportation system, including the preliminary conclusions of the linear synchronous motor analysis.

  1. MagRad: A code to optimize the operation of superconducting magnets in a radiation environment

    SciTech Connect (OSTI)

    Yeaw, C.T.

    1995-12-31

    A powerful computational tool, called MagRad, has been developed which optimizes magnet design for operation in radiation fields. Specifically, MagRad has been used for the analysis and design modification of the cable-in-conduit conductors of the TF magnet systems in fusion reactor designs. Since the TF magnets must operate in a radiation environment which damages the material components of the conductor and degrades their performance, the optimization of conductor design must account not only for start-up magnet performance, but also shut-down performance. The degradation in performance consists primarily of three effects: reduced stability margin of the conductor; a transition out of the well-cooled operating regime; and an increased maximum quench temperature attained in the conductor. Full analysis of the magnet performance over the lifetime of the reactor includes: radiation damage to the conductor, stability, protection, steady state heat removal, shielding effectiveness, optimal annealing schedules, and finally costing of the magnet and reactor. Free variables include primary and secondary conductor geometric and compositional parameters, as well as fusion reactor parameters. A means of dealing with the radiation damage to the conductor, namely high temperature superconductor anneals, is proposed, examined, and demonstrated to be both technically feasible and cost effective. Additionally, two relevant reactor designs (ITER CDA and ARIES-II/IV) have been analyzed. Upon addition of pure copper strands to the cable, the ITER CDA TF magnet design was found to be marginally acceptable, although much room for both performance improvement and cost reduction exists. A cost reduction of 10-15% of the capital cost of the reactor can be achieved by adopting a suitable superconductor annealing schedule. In both of these reactor analyses, the performance predictive capability of MagRad and its associated costing techniques have been demonstrated.

  2. INSTALLATION MAG~NiX.ILRI DIVI8ION, CAN.fAN,CONN.

    Office of Legacy Management (LM)

    INSTALLATION MAG~NiX.ILRI DIVI8ION, CAN.fAN,CONN. .PERI,jD Aiq~+ 1, i950 TO: August 31, 195 .:\,.:. ,,., WORK SHEET FOR: I b WSIGNOR I. v DowChemical Go. Velasco, Texas ., Azlterprise Meetala cc Brooklyn, New York Meili $Worthin&m Hatboro, ?'a. LOT NO. '... I [ATERIAL SYnB,fJL KEASURED' NET WT. 100,007~ ( 4;020 I ! 19 ~, ANALYBIS % METAL/100 r, Noi. 23) METAL CONTENT INSTRUCTIONS: This sheet% will be Used.ln.preDarlng Haterlal Balance. 'The totals from the various ltams listed above ~111 be

  3. Role of mag-enhanced lime scrubbing in the FGD industry

    SciTech Connect (OSTI)

    Babu, M.; College, J.; Smith, K.; Stowe, D.H.

    1997-12-31

    The mag-enhanced lime scrubbing process has been in commercial use in the US since the early 1970`s. At present over 14,000 MW of coal-fired utility plants in the US burning high sulfur coal (2.5--4.0% S) utilize this process with an excellent emission compliance and cost performance record to date. Dravo Lime Company (DLC) being the largest supplier of lime to this industry continues to conduct extensive R and D in this area and provides technical support service to these users. The success of the mag-enhanced lime process is largely attributed to the dual alkali effect of the Mg-Ca ions with a very distinct role for the highly soluble Mg ion in the scrubber liquor. It is well known that the high solubility of the magnesium ions provides alkalinities in the scrubbing liquor far in excess of the limestone systems. As a result of this high alkalinity liquor the mag-lime scrubbers need a much lower liquid to gas ratio, have lower scrubber pressure drop, consume lower parasitic load, are able to handle very high inlet SO{sub 2} concentrations, show little scaling tendency, etc. The scrubbers, recirculation pumps, piping, etc., are much smaller and the systems have lower capital and operating costs over comparable limestone systems. This system typically has a high availability and the process is less severe mechanically on the scrubber, pumps, nozzles, piping than comparable limestone processes. DLC`s patented ThioClear{reg_sign} process is an improvement over the conventional Thiosorbic process in use today. The ThioClear process while providing all of the advantages of the Thiosorbic process uses a nearly clear liquor to scrub and can use an innovative Horizontal Scrubber at gas velocities of up to 7.62--9.14 m/s (25--30 FPS). This process produces an excellent quality gypsum for wall board, cement or other applications and can also produce valuable Mg(OH){sub 2} as by-product. This paper discusses the merits of Thiosorbic/ThioClear processes, innovations with respect to the scrubber design, cost advantages and the freedom to choose a lower cost higher S coal while easily meeting or exceeding the regulatory requirements in the industry.

  4. THE COS-HALOS SURVEY: KECK LRIS AND MAGELLAN MagE OPTICAL SPECTROSCOPY

    SciTech Connect (OSTI)

    Werk, Jessica K.; Prochaska, J. Xavier [UCO/Lick Observatory, University of California, Santa Cruz, CA (United States); Thom, Christopher; Tumlinson, Jason [Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD (United States); Tripp, Todd M.; Meiring, Joseph D. [Department of Astronomy, University of Massachusetts, Amherst, MA (United States); O'Meara, John M., E-mail: jwerk@ucolick.org [Department of Chemistry and Physics, Saint Michael's College, Colchester, VT (United States)

    2012-01-01

    We present high signal-to-noise optical spectra for 67 low-redshift (0.1 < z < 0.4) galaxies that lie within close projected distances (5 kpc < {rho} < 150 kpc) of 38 background UV-bright QSOs. The Keck LRIS and Magellan MagE data presented here are part of a survey that aims to construct a statistically sampled map of the physical state and metallicity of gaseous galaxy halos using the Cosmic Origins Spectrograph (COS) on the Hubble Space Telescope. We provide a detailed description of the optical data reduction and subsequent spectral analysis that allow us to derive the physical properties of this uniquely data-rich sample of galaxies. The galaxy sample is divided into 38 pre-selected L {approx} L*, z {approx} 0.2 'target' galaxies and 29 'bonus' galaxies that lie in close proximity to the QSO sightlines. We report galaxy spectroscopic redshifts accurate to {+-}30 km s{sup -1}, impact parameters, rest-frame colors, stellar masses, total star formation rates (SFRs), and gas-phase interstellar medium oxygen abundances. When we compare the distribution of these galaxy characteristics to those of the general low-redshift population, we find good agreement. The L {approx} L* galaxies in this sample span a diverse range of color (1.0 < u - r < 3.0), stellar mass (10{sup 9.5} < M/M{sub Sun} < 10{sup 11.5}), and SFRs (0.01-20 M{sub Sun} yr{sup -1}). These optical data, along with the COS UV spectroscopy, comprise the backbone of our efforts to understand how halo gas properties may correlate with their host galaxy properties, and ultimately to uncover the processes that drive gas outflow and/or are influenced by gas inflow.

  5. SECTION M EVALUATION FACTORS FOR AWARD TABLE OF CONTENTS M-1 EVALUATION OF PROPOSALS .....................................................................................2

    National Nuclear Security Administration (NNSA)

    TABLE OF CONTENTS M-1 EVALUATION OF PROPOSALS .....................................................................................2 M-2 BASIS FOR CONTRACT AWARD ...................................................................................3 M-3 TECHNICAL AND MANAGEMENT CRITERIA ..........................................................3 M-4 COST EVALUATION CRITERION .................................................................................5 Section M, Evaluation Factors Request for

  6. SECTION M EVALUATION FACTORS FOR AWARD TABLE OF CONTENTS M-1 EVALUATION OF PROPOSALS .....................................................................................2

    National Nuclear Security Administration (NNSA)

    M EVALUATION FACTORS FOR AWARD TABLE OF CONTENTS M-1 EVALUATION OF PROPOSALS .....................................................................................2 M-2 BASIS FOR CONTRACT AWARD ...................................................................................3 M-3 TECHNICAL AND MANAGEMENT CRITERIA ..........................................................3 M-4 COST CRITERION

  7. Mission hazard assessment for STARS Mission 1 (M1) in the Marshall Islands area

    SciTech Connect (OSTI)

    Outka, D.E.; LaFarge, R.A.

    1993-07-01

    A mission hazard assessment has been performed for the Strategic Target System Mission 1 (known as STARS M1) for hazards due to potential debris impact in the Marshall Islands area. The work was performed at Sandia National Laboratories as a result of discussion with Kwajalein Missile Range (KMR) safety officers. The STARS M1 rocket will be launched from the Kauai Test Facility (KTF), Hawaii, and deliver two payloads to within the viewing range of sensors located on the Kwajalein Atoll. The purpose of this work has been to estimate upper bounds for expected casualty rates and impact probability or the Marshall Islands areas which adjoin the STARS M1 instantaneous impact point (IIP) trace. This report documents the methodology and results of the analysis.

  8. Magnetic flux and heat losses by diffusive, advective, and Nernst effects in MagLIF-like plasma

    SciTech Connect (OSTI)

    Velikovich, A. L. Giuliani, J. L.; Zalesak, S. T.

    2014-12-15

    The MagLIF approach to inertial confinement fusion involves subsonic/isobaric compression and heating of a DT plasma with frozen-in magnetic flux by a heavy cylindrical liner. The losses of heat and magnetic flux from the plasma to the liner are thereby determined by plasma advection and gradient-driven transport processes, such as thermal conductivity, magnetic field diffusion and thermomagnetic effects. Theoretical analysis based on obtaining exact self-similar solutions of the classical collisional Braginskii's plasma transport equations in one dimension demonstrates that the heat loss from the hot plasma to the cold liner is dominated by the transverse heat conduction and advection, and the corresponding loss of magnetic flux is dominated by advection and the Nernst effect. For a large electron Hall parameter ?{sub e}?{sub e} effective diffusion coefficients determining the losses of heat and magnetic flux are both shown to decrease with ?{sub e}?{sub e} as does the Bohm diffusion coefficient, which is commonly associated with low collisionality and two-dimensional transport. This family of exact solutions can be used for verification of codes that model the MagLIF plasma dynamics.

  9. New probe of M1 and E1 strengths in GDR regions

    SciTech Connect (OSTI)

    Hayakawa, T. [Japan Atomic Energy Agency and National Astronomical Observatory in Japan (Japan); Ogata, K. [RCNP, Osaka University (Japan); Miyamoto, S.; Mochizuki, T.; Horikawa, K.; Amano, S. [University of Hyogo (Japan); Imazaki, K.; Li, D.; Izawa, Y. [Institute for Laser Technology (Japan); Chiba, S. [Tokyo Institute of Technology (Japan)

    2014-05-02

    The M1 strengths (or level density of 1{sup +} states) are of importance for estimation of interaction strengths between neutrinos and nuclei for the study of the supernova neutrino-process. In 1957, Agodi predicted theoretically angular distribution of neutrons emitted from states excited via dipole transitions with linearly polarized gamma-ray beam at the polar angle of ?=90 should be followed by a simple function, a + b cos(2?), where ?, is azimuthal angel. However, this theoretical prediction has not been verified over the wide mass region except for light nuclei as deuteron. We have measured neutron angular distributions with (polarized gamma, n) reactions on Au, Nal, and Cu. We have verified the Agodi's prediction for the first time over the wide mass region. This suggests that (polarized gamma, n) reactions may be useful tools to study M1 strengths in giant resonance regions.

  10. Surface Termination of M1 Phase and Rational Design of Propane Ammoxidation Catalysts

    SciTech Connect (OSTI)

    Guliants, Vadim

    2015-02-16

    This final report describes major accomplishments in this research project which has demonstrated that the M1 phase is the only crystalline phase required for propane ammoxidation to acrylonitrile and that a surface monolayer terminating the ab planes of the M1 phase is responsible for their activity and selectivity in this reaction. Fundamental studies of the topmost surface chemistry and mechanism of propane ammoxidation over the Mo-V-(Te,Sb)-(Nb,Ta)-O M1 and M2 phases resulted in the development of quantitative understanding of the surface molecular structure – reactivity relationships for this unique catalytic system. These oxides possess unique catalytic properties among mixed metal oxides, because they selectively catalyze three alkane transformation reactions, namely propane ammoxidation to acrylonitrile, propane oxidation to acrylic acid and ethane oxidative dehydrogenation, all of considerable economic significance. Therefore, the larger goal of this research was to expand this catalysis to other alkanes of commercial interest, and more broadly, demonstrate successful approaches to rational design of improved catalysts that can be applied to other selective (amm)oxidation processes.

  11. Search for 14.4 keV solar axions from M1 transition of Fe-57...

    Office of Scientific and Technical Information (OSTI)

    Search for 14.4 keV solar axions from M1 transition of Fe-57 with CUORE crystals Citation Details In-Document Search Title: Search for 14.4 keV solar axions from M1 transition of...

  12. Laser hazard analysis for LASIRIS Model MAG-501L-670M-1000-45[degree]-K diode laser associated with high resolution pulsed scanner.

    SciTech Connect (OSTI)

    Augustoni, Arnold L.

    2004-11-01

    A laser hazard analysis and safety assessment was performed for the LASIRISTM Model MAG-501L-670M-1000-45o-K diode laser associated with the High Resolution Pulse Scanner based on the ANSI Standard Z136.1-2000, American National Standard for the Safe Use of Lasers and the ANSI Standard Z136.6-2000, American National Standard for the Safe Use of Lasers Outdoors. The laser was evaluated for both indoor and outdoor use.

  13. The E2/M1 mixing ratio in the excitation of the {Delta} from polarized photo-reactions

    SciTech Connect (OSTI)

    The LEGS Collaboration

    1993-12-01

    In constituent quark models, a tensor interaction, mixing quark spins with their relative motion, is introduced to reproduce the observed baryon spectrum. This has a consequence completely analogous to the nuclear tensor force between the n and p in deuterium. A D state component is mixed into what would otherwise be a purely S-wave object. The D-wave component breaks spherical symmetry, resulting in a non-vanishing matrix element for the nucleon and a static quadrupole moment and deformation for its first excited state, the {Delta} resonance, at {approximately}325 MeV. The magnitude and sign of this D-state component are quite sensitive to the internal structure of the proton and have been of great interest in recent years. The intrinsic deformation of the spin 1/2 nucleon cannot be observed directly; it must be inferred from transition amplitudes such as N {yields} {Delta}. In a spherical bag model, the {Delta} is viewed as a pure quark-spin-flip transition proceeding only through M1 excitation. If there are D-state admixtures in the ground state of the nucleon and/or {Delta}, quadrupole excitation, in addition to spin-flip M1, is also allowed. The problem is to evaluate the relative magnitude of this E2 excitation in the presence of the dominant M1 transition. A variety of models predict this mixing ratio to be quite small, anywhere from {minus}0.9% to {minus}6%, so that a high degree of precision is demanded of experiment.

  14. Better Catalysts through Microscopy: Nanometer Scale M1/M2 Intergrown Heterostructure in Mo-V-M Complex Oxides

    SciTech Connect (OSTI)

    He, Qian [ORNL; Woo, Jungwon [University of Cincinnati; Belianinov, Alex [ORNL; Guliants, Vadim V. [University of Cincinnati; Borisevich, Albina Y [ORNL

    2015-01-01

    In recent decades, catalysis research has transformed from the predominantly empirical field to one where it is possible to control the catalytic properties via characterization and modification of the atomic-scale active centers. Many phenomena in catalysis, such as synergistic effect, however, transcend the atomic scale and also require the knowledge and control of the mesoscale structure of the specimen to harness. In this paper, we use our discovery of atomic-scale epitaxial interfaces in molybdenum vanadium based complex oxide catalysts systems (i.e., MoVMO, M = Ta, Te, Sb, Nb, etc.) to achieve control of the mesoscale structure of this complex mixture of very different active phases. We can now achieve true epitaxial intergrowth between the catalytically critical M1 and M2 phases in the system that are hypothesized to have synergistic interactions, and demonstrate that the resulting catalyst has improved selectivity in the initial studies. Finally, we highlight the crucial role atomic scale characterization and mesoscale structure control play in uncovering the complex underpinnings of the synergistic effect in catalysis.

  15. Maldives-Supporting the Zero Emissions Strategy | Open Energy...

    Open Energy Info (EERE)

    (GIZ) Partner Federal Ministry for the Environment, Nature Conservation and Nuclear Safety (BMU) Sector Energy Focus Area Energy Efficiency Topics Low emission...

  16. Safety Analysis Report for Packaging (SARP): Model AL-M1 nuclear packaging (DOE C of C No. USA/9507/BLF)

    SciTech Connect (OSTI)

    Coleman, H.L.; Whitney, M.A.; Williams, M.A.; Alexander, B.M.; Shapiro, A.

    1987-11-24

    This Safety Analysis Report for Packaging (SARP) satisfies the request of the US Department of Energy for a formal safety analysis of the shipping container identified as USA/9507/BLF, also called AL-M1, configuration 5. This report makes available to all potential users the technical information and the limits pertinent to the construction and use of the shipping containers. It includes discussions of structural integrity, thermal resistance, radiation shielding and radiological safety, nuclear criticality safety, and quality control. A complete physical and technical description of the package is presented. The package consists of an inner container centered within an insulated steel drum. The configuration-5 package contains tritiated water held on sorbent material. There are two other AL-M1 packages, designated configurations 1 and 3. These use the same insulated outer drum, but licensing of these containers will not be addressed in this SARP. Design and development considerations, the tests and evaluations required to prove the ability of the container to withstand normal transportation conditions, and the sequence of four hypothetical accident conditions (free drop, puncture, thermal, and water immersion) are discussed. Tables, graphs, dimensional sketches, photographs, technical references, loading and shipping procedures, Monsanto Research Corporation-Mound experience in using the containers, and a copy of the DOE/OSD/ALO Certificate of Compliance are included.

  17. Propane ammoxidation over the Mo-V-Te-Nb-O M1 phase: Reactivity of surface cations in hydrogen abstraction steps

    SciTech Connect (OSTI)

    Muthukumar, Kaliappan; Yu, Junjun; Xu, Ye; Guliants, Vadim V.

    2011-01-01

    Density functional theory calculations (GGA-PBE) have been performed to investigate the adsorption of C3 (propane, isopropyl, propene, and allyl) and H species on the proposed active center present in the surface ab planes of the bulk Mo-V-Te-Nb-O M1 phase in order to better understand the roles of the different surface cations in propane ammoxidation. Modified cluster models were employed to isolate the closely spaced V=O and Te=O from each other and to vary the oxidation state of the V cation. While propane and propene adsorb with nearly zero adsorption energy, the isopropyl and allyl radicals bind strongly to V=O and Te=O with adsorption energies, {Delta}E, being {le} -1.75 eV, but appreciably more weakly on other sites, such as Mo=O, bridging oxygen (Mo-O-V and Mo-O-Mo), and empty metal apical sites ({Delta}E > -1 eV). Atomic H binds more strongly to Te = O ({Delta}E {le} -3 eV) than to all the other sites, including V = O ({Delta}E = -2.59 eV). The reduction of surface oxo groups by dissociated H and their removal as water are thermodynamically favorable except when both H atoms are bonded to the same Te=O. Consistent with the strong binding of H, Te=O is markedly more active at abstracting the methylene H from propane (E{sub a} {le} 1.01 eV) than V = O (E{sub a} = 1.70 eV on V{sup 5+} = O and 2.13 eV on V{sup 4+} = O). The higher-than-observed activity and the loose binding of Te = O moieties to the mixed metal oxide lattice of M1 raise the question of whether active Te = O groups are in fact present in the surface ab planes of the M1 phase under propane ammoxidation conditions.

  18. STEM HAADF Image Simulation of the Orthorhombic M1 Phase in the Mo-V-Nb-Te-O Propane Oxidation Catalyst

    SciTech Connect (OSTI)

    D Blom; X Li; S Mitra; T Vogt; D Buttrey

    2011-12-31

    A full frozen phonon multislice simulation of high angle annular dark field scanning transmission electron microscopy (HAADF STEM) images from the M1 phase of the Mo-V-Nb-Te-O propane oxidation catalyst has been performed by using the latest structural model obtained using the Rietveld method. Simulated contrast results are compared with experimental HAADF images. Good agreement is observed at ring sites, however significant thickness dependence is noticed at the linking sites. The remaining discrepancies between the model based on Rietveld refinement and image simulations indicate that the sampling of a small volume element in HAADF STEM and averaging elemental contributions of a disordered site in a crystal slab by using the virtual crystal approximation might be problematic, especially if there is preferential Mo/V ordering near the (001) surface.

  19. Adsorption of propane, isopropyl, and hydrogen on cluster models of the M1 phase of Mo-V-Te-Nb-O mixed metal oxide catalyst

    SciTech Connect (OSTI)

    Govindasamy, Agalya; Muthukumar, Kaliappan; Yu, Junjun; Xu, Ye; Guliants, Vadim V.

    2010-01-01

    The Mo-V-Te-Nb-O mixed metal oxide catalyst possessing the M1 phase structure is uniquely capable of directly converting propane into acrylonitrile. However, the mechanism of this complex eight-electron transformation, which includes a series of oxidative H-abstraction and N-insertion steps, remains poorly understood. We have conducted a density functional theory study of cluster models of the proposed active and selective site for propane ammoxidation, including the adsorption of propane, isopropyl (CH{sub 3}CHCH{sub 3}), and H which are involved in the first step of this transformation, that is, the methylene C-H bond scission in propane, on these active site models. Among the surface oxygen species, the telluryl oxo (Te=O) is found to be the most nucleophilic. Whereas the adsorption of propane is weak regardless of the MO{sub x} species involved, isopropyl and H adsorption exhibits strong preference in the order of Te=O > V=O > bridging oxygens > empty Mo apical site, suggesting the importance of TeO{sub x} species for H abstraction. The adsorption energies of isopropyl and H and consequently the reaction energy of the initial dehydrogenation of propane are strongly dependent on the number of ab planes included in the cluster, which points to the need to employ multilayer cluster models to correctly capture the energetics of surface chemistry on this mixed metal oxide catalyst.

  20. EA-306_MAG_Canada.pdf

    Office of Environmental Management (EM)

  1. M1 Energy | Open Energy Information

    Open Energy Info (EERE)

    either solely or in partnership. Their project scope is focused on small to medium-sized oil, gas and electricity projects. Coordinates: 41.88415, -87.632409 Show Map Loading...

  2. Maldives-Program for Scaling Up Renewable Energy in Low Income...

    Open Energy Info (EERE)

    number of low income countries for energy efficiency, renewable energy and access to modern sustainable energy. The SREP stimulates economic growth through the scaled-up...

  3. Climate Mag_27JUN2013_ms07022013.indd

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

    ability to process and store carbon. 19 PartnersCollaborators Our partners include the United States Geological Survey, Michigan State University, the University of New Mexico,...

  4. Fine coal cleaning via the micro-mag process

    DOE Patents [OSTI]

    Klima, Mark S.; Maronde, Carl P.; Killmeyer, Richard P.

    1991-01-01

    A method of cleaning particulate coal which is fed with a dense medium slurry as an inlet feed to a cyclone separator. The coal particle size distribution is in the range of from about 37 microns to about 600 microns. The dense medium comprises water and ferromagnetic particles that have a relative density in the range of from about 4.0 to about 7.0. The ferromagnetic particles of the dense medium have particle sizes of less than about 15 microns and at least a majority of the particle sizes are less than about 5 microns. In the cyclone, the particulate coal and dense-medium slurry is separated into a low gravity product stream and a high gravity produce stream wherein the differential in relative density between the two streams is not greater than about 0.2. The low gravity and high gravity streams are treated to recover the ferromagnetic particles therefrom.

  5. Climate Mag_27JUN2013_ms07022013.indd

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

    CLIMATE AND IMPACT RESEARCH at Los Alamos National Laboratory Climate Research and National Security Los Alamos National Laboratory is truly a national security science laboratory, tackling some of the world's most challenging science and engineering issues. We are interested in the potential future impacts of climate change on global security, such as the coastal e ects of sea level rise, increased number of extreme storms, and the consequences of extensive regional tree mortality. Gaining a

  6. PPG and MAG Team Up for Turbine Blade Research

    Broader source: Energy.gov [DOE]

    Two companies work together to move forward in the industry, researching materials and processes that could lead to stronger, more reliable wind blades.

  7. New MagViz Airport Liquid Analysis System Undergoes Testing

    ScienceCinema (OSTI)

    None

    2010-01-08

    LOS ALAMOS, New Mexico, December 16, 2008?An innovative application of a technology first used for medical imaging may enhance airport security if Los Alamos National Laboratory scientists are successful. Los Alamos technologists have adapted Magnetic Res

  8. EA-306-A MAG ES CN.pdf

    Office of Environmental Management (EM)

  9. EA-306-B MAG ES (CN).pdf

    Office of Environmental Management (EM)

  10. Tritium on Z: The challenges and possibilities for MagLIF

    Broader source: Energy.gov [DOE]

    Presentation from the 36th Tritium Focus Group Meeting held in Los Alamos, New Mexico, November 3-5, 2015.

  11. The largest and highest powered magnet lab in the world - MagLab

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

    Magnet Time Search Staff Search Publications Search Site The National High Magnetic Field Laboratory Main Menu User Facilities DC Field Electron Magnetic Resonance High BT Ion...

  12. Asian Development Outlook 2010 | Open Energy Information

    Open Energy Info (EERE)

    Turkmenistan, Uzbekistan, China, South Korea, Mongolia, Afghanistan, Bangladesh, Bhutan, India, Maldives, Pakistan, Sri Lanka, Nepal, Cambodia, Indonesia, Malaysia, Laos, Vietnam,...

  13. C:\\MYDOCS\\FBSS-M~1\\HATTIE\\LAYOUT94.TXT

    U.S. Energy Information Administration (EIA) Indexed Site

    3. B4G Percent public order and safety PORDP5 52- 54 MISS3CH. 3. B4H Percent out-patient health care HCOUTP5 56- 58 MISS3CH. 3. B4I Percent industrial INDUSP5 60- 62 MISS3CH....

  14. Microsoft Word - Sandia-VT M-1 Summary Report_FINAL.docx

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

    ... President of the University of Vermont, Mary Powell, President and CEO of Green Mountain Power, and Marjorie Tatro, Director of Energy Technologies and System Solutions at Sandia. ...

  15. Search for 14.4 keV solar axions from M1 transition of Fe-57...

    Office of Scientific and Technical Information (OSTI)

    K. M. ; Huang, H. Z. ; Kadel, R. ; Kazkaz, K. ; Keppel, G. ; Kogler, L. ; Kolomensky, Yu. G. ; Lenz, D. ; Li, Y. L. ; Ligi, C. ; Liu, X. ; Ma, Y. G. ; Maiano, C. ; Maino, M. ;...

  16. ARM - Facility News Article

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

    ARM's two mobile facilities have completed field campaigns in the United States, Africa, Germany, the Azores, India, and the Maldives. They are currently preparing for yearlong...

  17. 1

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

    field experiment conducted during January and March 1999. As part of INDOEX, a new surface observatory was established in the Maldives. The Kaashidhoo Climate Observatory...

  18. ARM - Site Instruments

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

    2009-2010 Shouxian, China, 2008 Black Forest, Germany, 2007 Niamey, Niger, 2006 Point Reyes, California, 2005 Instruments : Gan Island, Maldives Active Retired Active instruments...

  19. Investigation of LaxSr1-xCoyM1-yO3-d (M = Mn Fe) perovskite materials as thermochemical energy storage media.

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

    Babiniec, Sean Michael; Ambrosini, Andrea; Coker, Eric Nicholas; Miller, James E.

    2015-06-23

    Materials in the LaxSr1–xCoyMn1–yO3–δ (LSCM) and LaxSr1–xCoyFe1–yO3–δ (LSCF) families are candidates for high-temperature thermochemical energy storage due to their facility for cyclic endothermic reduction and exothermic oxidation. A set of 16 LSCM and 21 LSCF compositions were synthesized by a modified Pechini method and characterized by powder X-ray diffraction and thermogravimetric analysis. All materials were found to be various symmetries of the perovskite phase. LSCM was indexed as tetragonal, cubic, rhombohedral, or orthorhombic as a function of increased lanthanum content. For LSCF, compositions containing low lanthanum content were indexed as cubic while materials with high lanthanum content were indexed asmore » rhombohedral. An initial screening of redox activity was completed by thermogravimetric analysis for each composition. The top three compositions with the greatest recoverable redox capacity for each family were further characterized in equilibrium thermogravimetric experiments over a range of temperatures and oxygen partial pressures. As a result, these equilibrium experiments allowed the extraction of thermodynamic parameters for LSCM and LSCF compositions operated in thermochemical energy storage conditions.« less

  20. Decontamination of hot cells K-1, K-3, M-1, M-3, and A-1, M-Wing, Building 200: Project final report Argonne National Laboratory-East

    SciTech Connect (OSTI)

    Cheever, C.L.; Rose, R.W.

    1996-09-01

    The purpose of this project was to remove radioactively contaminated materials and equipment from the hot cells, to decontaminate the hot cells, and to dispose of the radioactive waste. The goal was to reduce stack releases of Rn-220 and to place the hot cells in an emptied, decontaminated condition with less than 10 {micro}Sv/h (1 mrem/h) general radiation background. The following actions were needed: organize and mobilize a decontamination team; prepare decontamination plans and procedures; perform safety analyses to ensure protection of the workers, public, and environment; remotely size-reduce, package, and remove radioactive materials and equipment for waste disposal; remotely decontaminate surfaces to reduce hot cell radiation background levels to allow personnel entries using supplied air and full protective suits; disassemble and package the remaining radioactive materials and equipment using hands-on techniques; decontaminate hot cell surfaces to remove loose radioactive contaminants and to attain a less than 10 {micro}Sv/h (1 mrem/h) general background level; document and dispose of the radioactive and mixed waste; and conduct a final radiological survey.

  1. The effect of cigarette smoke and arsenic exposure on urothelial carcinoma risk is modified by glutathione S-transferase M1 gene null genotype

    SciTech Connect (OSTI)

    Chung, Chi-Jung [Department of Health Risk Management, College of Public Health, China Medical University, Taichung, Taiwan (China) [Department of Health Risk Management, College of Public Health, China Medical University, Taichung, Taiwan (China); Department of Medical Research, China Medical University Hospital, Taichung, Taiwan (China); Huang, Chao-Yuan; Pu, Yeong-Shiau [Department of Urology, National Taiwan University Hospital, Taipei, Taiwan (China)] [Department of Urology, National Taiwan University Hospital, Taipei, Taiwan (China); Shiue, Horng-Sheng [Department of Chinese Medicine, Chang Gung Memorial Hospital, Taipei, Taiwan (China)] [Department of Chinese Medicine, Chang Gung Memorial Hospital, Taipei, Taiwan (China); Su, Chien-Tien [Department of Family Medicine, Taipei Medical University Hospital, Taipei, Taiwan (China)] [Department of Family Medicine, Taipei Medical University Hospital, Taipei, Taiwan (China); Hsueh, Yu-Mei, E-mail: ymhsueh@tmu.edu.tw [Department of Public Health, School of Medicine, College of Medicine, Taipei Medical University, Taipei, Taiwan (China) [Department of Public Health, School of Medicine, College of Medicine, Taipei Medical University, Taipei, Taiwan (China); School of Public Health, College of Public Health and Nutrition, Taipei Medical University, Taipei, Taiwan (China)

    2013-01-15

    Inter-individual variation in the metabolism of xenobiotics, caused by factors such as cigarette smoking or inorganic arsenic exposure, is hypothesized to be a susceptibility factor for urothelial carcinoma (UC). Therefore, our study aimed to evaluate the role of geneenvironment interaction in the carcinogenesis of UC. A hospital-based casecontrol study was conducted. Urinary arsenic profiles were measured using high-performance liquid chromatographyhydride generator-atomic absorption spectrometry. Genotyping was performed using a polymerase chain reaction-restriction fragment length polymorphism technique. Information about cigarette smoking exposure was acquired from a lifestyle questionnaire. Multivariate logistic regression was applied to estimate the UC risk associated with certain risk factors. We found that UC patients had higher urinary levels of total arsenic, higher percentages of inorganic arsenic (InAs%) and monomethylarsonic acid (MMA%) and lower percentages of dimethylarsinic acid (DMA%) compared to controls. Subjects carrying the GSTM1 null genotype had significantly increased UC risk. However, no association was observed between gene polymorphisms of CYP1A1, EPHX1, SULT1A1 and GSTT1 and UC risk after adjustment for age and sex. Significant geneenvironment interactions among urinary arsenic profile, cigarette smoking, and GSTM1 wild/null polymorphism and UC risk were observed after adjustment for potential risk factors. Overall, geneenvironment interactions simultaneously played an important role in UC carcinogenesis. In the future, large-scale studies should be conducted using tag-SNPs of xenobiotic-metabolism-related enzymes for gene determination. -- Highlights: ? Subjects with GSTM1 null genotype had significantly increased UC risk. ? UC patients had poor arsenic metabolic ability compared to controls. ? GSTM1 null genotype may modify arsenic related UC risk.

  2. Scheuten SolarWorld Solizium GmbH | Open Energy Information

    Open Energy Info (EERE)

    search Name: Scheuten SolarWorld Solizium GmbH Place: Maldives Sector: Solar Product: Joint Venture of SolarWorld AG and Scheuten Solarholding for production of solar-grade...

  3. Workbook Contents

    U.S. Energy Information Administration (EIA) Indexed Site

    to Maldives of Crude Oil and Petroleum Products (Thousand Barrels)","U.S. Exports to Mali of Crude Oil and Petroleum Products (Thousand Barrels)","U.S. Exports to Malta of Crude...

  4. “Nodal Gap” induced by the incommensurate diagonal spin density modulation in underdoped high- Tc superconductors

    SciTech Connect (OSTI)

    Zhou, Tao; Gao, Yi; Zhu, Jian -Xin

    2015-03-07

    Recently it was revealed that the whole Fermi surface is fully gapped for several families of underdoped cuprates. The existence of the finite energy gap along the d-wave nodal lines (nodal gap) contrasts the common understanding of the d-wave pairing symmetry, which challenges the present theories for the high-Tcsuperconductors. Here we propose that the incommensurate diagonal spin-density-wave order can account for the above experimental observation. The Fermi surface and the local density of states are also studied. Our results are in good agreement with many important experiments in high-Tcsuperconductors.

  5. Lambda network having 2.sup.m-1 nodes in each of m stages with each node coupled to four other nodes for bidirectional routing of data packets between nodes

    DOE Patents [OSTI]

    Napolitano, Jr., Leonard M. (825 El Quanito Dr., Danville, CA 94526)

    1995-01-01

    The Lambda network is a single stage, packet-switched interprocessor communication network for a distributed memory, parallel processor computer. Its design arises from the desired network characteristics of minimizing mean and maximum packet transfer time, local routing, expandability, deadlock avoidance, and fault tolerance. The network is based on fixed degree nodes and has mean and maximum packet transfer distances where n is the number of processors. The routing method is detailed, as are methods for expandability, deadlock avoidance, and fault tolerance.

  6. Application to Export Electric Energy OE Docket No. EA-306-A...

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

    Solutions, Inc. Application to Export Electric Energy OE Docket No. EA-306-A MAG Energy Solutions, Inc. Application from MAG Energy Solutions, Inc. to export electric energy to...

  7. An accreting white dwarf near the Chandrasekhar limit in the Andromeda galaxy

    SciTech Connect (OSTI)

    Tang, Sumin; Bildsten, Lars; Wolf, William M.; Li, K. L.; Kong, Albert K. H.; Cao, Yi; Kulkarni, Shrinivas R.; Perley, Daniel A.; Prince, Thomas A.; Cenko, S. Bradley; De Cia, Annalisa; Kasliwal, Mansi M.; Laher, Russ R.; Surace, Jason; Nugent, Peter E.

    2014-05-01

    The intermediate Palomar Transient Factory (iPTF) detection of the most recent outburst of the recurrent nova (RN) system RX J0045.4+4154 in the Andromeda galaxy has enabled the unprecedented study of a massive (M > 1.3 M {sub ?}) accreting white dwarf (WD). We detected this nova as part of the near-daily iPTF monitoring of M31 to a depth of R ? 21 mag and triggered optical photometry, spectroscopy and soft X-ray monitoring of the outburst. Peaking at an absolute magnitude of M{sub R} = 6.6 mag, and with a decay time of 1 mag per day, it is a faint and very fast nova. It shows optical emission lines of He/N and expansion velocities of 1900-2600 km s{sup 1} 1-4 days after the optical peak. The Swift monitoring of the X-ray evolution revealed a supersoft source (SSS) with kT {sub eff} ? 90-110 eV that appeared within 5 days after the optical peak, and lasted only 12 days. Most remarkably, this is not the first event from this system, rather it is an RN with a time between outbursts of approximately 1 yr, the shortest known. Recurrent X-ray emission from this binary was detected by ROSAT in 1992 and 1993, and the source was well characterized as a M > 1.3 M {sub ?} WD SSS. Based on the observed recurrence time between different outbursts, the duration and effective temperature of the SS phase, MESA models of accreting WDs allow us to constrain the accretion rate to M-dot >1.710{sup ?7} M{sub ?} yr{sup ?1} and WD mass >1.30 M {sub ?}. If the WD keeps 30% of the accreted material, it will take less than a Myr to reach core densities high enough for carbon ignition (if made of C/O) or electron capture (if made of O/Ne) to end the binary evolution.

  8. ARM - Facility News Article

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

    14, 2012 [Facility News] Data Collection from Mobile Facility on Gan Island Suspended Bookmark and Share Local weather balloon launch volunteers pose with the AMF team on Gan Island after completing their training. Local weather balloon launch volunteers pose with the AMF team on Gan Island after completing their training. Due to sudden unrest in the Maldives in early February, operations of the ARM Mobile Facility on Gan Island were suspended on February 9, 2012, and all instruments have been

  9. ARM - Site Instruments

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

    FacilitiesInstruments AMF Information Science Architecture Baseline Instruments AMF1 AMF2 AMF3 MAOS Data Operations AMF Fact Sheet Images Contacts AMF Deployments McMurdo Station, Antarctica, 2015-2016 Pearl Harbor, Hawaii, to San Francisco, California, 2015 Hyytiälä, Finland, 2014 Manacapuru, Brazil, 2014 Oliktok Point, Alaska, 2013 Los Angeles, California, to Honolulu, Hawaii, 2012 Cape Cod, Massachusetts, 2012 Gan Island, Maldives, 2011 Ganges Valley, India, 2011 Steamboat Springs,

  10. ARM - Mobile Aerosol Observing System

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

    FacilitiesMobile Aerosol Observing System AMF Information Science Architecture Baseline Instruments AMF1 AMF2 AMF3 MAOS Data Operations AMF Fact Sheet Images Contacts AMF Deployments McMurdo Station, Antarctica, 2015-2016 Pearl Harbor, Hawaii, to San Francisco, California, 2015 Hyytiälä, Finland, 2014 Manacapuru, Brazil, 2014 Oliktok Point, Alaska, 2013 Los Angeles, California, to Honolulu, Hawaii, 2012 Cape Cod, Massachusetts, 2012 Gan Island, Maldives, 2011 Ganges Valley, India, 2011

  11. ARM - AMF1 Baseline Instruments

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

    FacilitiesAMF1 Baseline Instruments AMF Information Science Architecture Baseline Instruments AMF1 AMF2 AMF3 MAOS Data Operations AMF Fact Sheet Images Contacts AMF Deployments McMurdo Station, Antarctica, 2015-2016 Pearl Harbor, Hawaii, to San Francisco, California, 2015 Hyytiälä, Finland, 2014 Manacapuru, Brazil, 2014 Oliktok Point, Alaska, 2013 Los Angeles, California, to Honolulu, Hawaii, 2012 Cape Cod, Massachusetts, 2012 Gan Island, Maldives, 2011 Ganges Valley, India, 2011 Steamboat

  12. ARM - AMF2 Management and Operations

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

    Management and Operations AMF Information Science Architecture Baseline Instruments AMF1 AMF2 AMF3 MAOS Data Operations AMF Fact Sheet Images Contacts AMF Deployments McMurdo Station, Antarctica, 2015-2016 Pearl Harbor, Hawaii, to San Francisco, California, 2015 Hyytiälä, Finland, 2014 Manacapuru, Brazil, 2014 Oliktok Point, Alaska, 2013 Los Angeles, California, to Honolulu, Hawaii, 2012 Cape Cod, Massachusetts, 2012 Gan Island, Maldives, 2011 Ganges Valley, India, 2011 Steamboat Springs,

  13. ARM - AMF3 Baseline Instruments

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

    FacilitiesAMF3 Baseline Instruments AMF Information Science Architecture Baseline Instruments AMF1 AMF2 AMF3 MAOS Data Operations AMF Fact Sheet Images Contacts AMF Deployments McMurdo Station, Antarctica, 2015-2016 Pearl Harbor, Hawaii, to San Francisco, California, 2015 Hyytiälä, Finland, 2014 Manacapuru, Brazil, 2014 Oliktok Point, Alaska, 2013 Los Angeles, California, to Honolulu, Hawaii, 2012 Cape Cod, Massachusetts, 2012 Gan Island, Maldives, 2011 Ganges Valley, India, 2011 Steamboat

  14. Phase I A Phase I B Phase I C

    Office of Legacy Management (LM)

    Parcel 9 Parcel 8 Phase I A Phase I B Phase I C Parcel 7 Parcel 6 Parcel 4 Parcel 3 Parcel D Parcel H Parcel 6A T 61 87 3 105 2 OSE 63 28 126 45 COS OSW 100 GH 102 STP SST 301 300 Mag-82 Mag-81 Mag-80 Mag-83 Mag-84 Mound Closure Project - Current Parcels and Buildings FILE NAME: mnd_bldg_parcel_owner_c.mxd DATE: Legend Parcel - DOE Parcel - MMCIC Pond Building Ownership DOE Leased MMCIC Road - paved Railroad 200 0 200 100 Feet O:\Sites\OH\Mound\ProjectWorkArea\PawelS\mnd_bldg_parcel_owner_c.mxd

  15. PHYSICAL PROPERTIES OF MAIN-BELT COMET 176P/LINEAR

    SciTech Connect (OSTI)

    Hsieh, Henry H.; Ishiguro, Masateru; Lacerda, Pedro; Jewitt, David E-mail: p.lacerda@qub.ac.uk E-mail: jewitt@ucla.edu

    2011-07-15

    We present a physical characterization of comet 176P/LINEAR, the third discovered member of the new class of main-belt comets, which exhibit cometary activity but are dynamically indistinguishable from main-belt asteroids. Observations show the object exhibiting a fan-shaped tail for at least one month in late 2005, but then becoming inactive in early 2006. During this active period, we measure broadband colors of B - V = 0.63 {+-} 0.02, V - R = 0.35 {+-} 0.02, and R - I = 0.31 {+-} 0.04. Using data from when the object was observed to be inactive, we derive best-fit IAU phase function parameters of H = 15.10 {+-} 0.05 mag and G = 0.15 {+-} 0.10, and best-fit linear phase function parameters of m(1, 1, 0) = 15.35 {+-} 0.05 mag and {beta} = 0.038 {+-} 0.005 mag deg{sup -1}. From this baseline phase function, we find that 176P exhibits a mean photometric excess of {approx}30% during its active period, implying an approximate total coma dust mass of M{sub d} {approx} (7.2 {+-} 3.6) x 10{sup 4} kg. From inactive data obtained in early 2007, we find a rotation period of P{sub rot} = 22.23 {+-} 0.01 hr and a peak-to-trough photometric range of {Delta}m {approx} 0.7 mag. Phasing our photometric data from 176P's 2005 active period to this rotation period, we find that the nucleus exhibits a significantly smaller photometric range than in 2007 that cannot be accounted for by coma damping effects, and as such, are attributed by us to viewing geometry effects. A detailed analysis of these geometric effects showed that 176P is likely to be a highly elongated object with an axis ratio of 1.8 < b/a < 2.1, an orbital obliquity of {epsilon} {approx} 60{sup 0}, and a solstice position at a true anomaly of {nu}{sub o} = 20{sup 0} {+-} 20{sup 0}. Numerical modeling of 176P's dust emission found that its activity can only be reproduced by asymmetric dust emission, such as a cometary jet. We find plausible fits to our observations using models assuming {approx}10 {mu}m dust particles continuously emitted over the period during which 176P was observed to be active, and a jet direction of 180{sup 0} {approx}< {alpha}{sub jet} {approx}< 120{sup 0} and {delta}{sub jet} {approx} -60{sup 0}. We do not find good fits to our observations using models of impulsive dust emission, i.e., what would be expected if 176P's activity was an ejecta cloud resulting from an impact into non-volatile asteroid regolith. Since for a rotating body, the time-averaged direction of a non-equatorial jet is equivalent to the direction of the nearest rotation pole, we find an equivalent orbital obliquity of 50{sup 0} {approx}< {epsilon} {approx}< 75{sup 0}, consistent with the results of our light curve analysis. Furthermore, the results of both our light curve analysis and dust modeling analysis are consistent with the seasonal heating hypothesis used to explain the modulation of 176P's activity. Additional observations are highly encouraged to further characterize 176P's active behavior as the object approaches perihelion on 2011 July 1.

  16. The Nevada Test Site Development Corporations

    National Nuclear Security Administration (NNSA)

    1 8 1 2 2 m 1 .

  17. Tax Credits, Rebates & Savings | Department of Energy

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

    Standards In an effort to promote uniformity, the Maricopa Association of Governments (MAG) approved standard procedures for securing necessary electricalbuilding permits for...

  18. Application to Export Electric Energy OE Docket No. EA-306-A...

    Office of Environmental Management (EM)

    Solutions: Federal Register Notice Volume 75, No. 237 - Dec. 10, 2010 Application to Export Electric Energy OE Docket No. EA-306-A MAG Energy Solutions: Federal Register Notice...

  19. Maricopa Assn. of Governments- PV and Solar Domestic Water Heating Permitting Standards

    Broader source: Energy.gov [DOE]

    In an effort to promote uniformity, the Maricopa Association of Governments (MAG) approved standard procedures for securing necessary electrical/building permits for residential (single-family) and...

  20. Magwind LLC | Open Energy Information

    Open Energy Info (EERE)

    Texas Sector: Wind energy Product: Inventor of the Mag-Wind vertical axis wind turbine (VAWT) for building installations. The turbines are manufactured under contract at the...

  1. Sandia National Laboratories: Z Pulsed Power Facility: Z Research

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

    potential. With growing concerns about the health of our planet and escalating energy needs, the development of fusion technology is especially promising. Prototype Mag-Life...

  2. Maricopa Assn. of Governments - PV and Solar Domestic Water Heating...

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

    June 18, 2003, MAG passed permit submission requirements for residential solar domestic water heating systems. This is in addition to the existing standards for residential and...

  3. ARM - Feature Stories and Releases Article

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

    , 2011 [Feature Stories and Releases] AMIE, What You Wanna Do? Bookmark and Share Data spanning the Maldives to Papua New Guinea will help scientists analyze far-reaching tropical weather cycle This view shows a subset of the ARM Mobile Facility instruments operating at the Gan Island airport for the AMIE campaign. To see the complete collection, see the image set in Flickr. This view shows a subset of the ARM Mobile Facility instruments operating at the Gan Island airport for the AMIE campaign.

  4. ARM - Datastreams - tsiskyimage

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

    PVC M1 Browse Data Highland Center, Cape Cod MA; AMF1 retired PYE M1 Browse Data Point Reyes, CA retired SBS M1 Browse Data Steamboat Springs CO, Valley Site; AMF2 retired TMP M1...

  5. Carlsbad Field Office P. O

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

    Field Office Quality Assurance Director, Ava L. Holland , at (575) 234-7423. Enclosure CBFO:QA:DSM:MAG:l00571 :UFC 2300.00 Sincerely, David C. Moody Manager Original Signature...

  6. Microsoft Word - Transmittal of Final Audit Report A-13-02, SRS...

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

    DSM:MAG:13-1490:UFC 2300.00 Department of Energy Carlsbad Field Office P.O. Box 3090 Carlsbad, New Mexico 88221 August 6, 2013 Mr. John E. Kieling, Chief Hazardous Waste Bureau New...

  7. New airport liquid analysis system undergoes testing at Albuquerque...

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

    And sensors in the MRI machine detect these slightly different frequencies, which are in ... The fainter signals that MagViz teases out with a weaker magnet challenged the Los Alamos ...

  8. International Sunport

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

    And sensors in the MRI machine detect these slightly different frequencies, which are in ... The fainter signals that MagViz teases out with a weaker magnet challenged the Los Alamos ...

  9. Mr. Steve Zappe

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

    this audit report , please contact the CBFO Quality Assurance Director, Ava L. Holland, at (575) 234-7423. Enclosure CBFO:QA :OSM:MAG:09-1699:UFC 2300 .00 Sincerely, David C...

  10. Mr. Steve Zappe

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

    report , please contact the Carlsbad Field Office Quality Assurance Director, Ava L. Holland, at (575) 234-7423. Enclosure CBFO:QA:MPN :MAG:09 1679:UFC 2300.00 Sincerely, David C...

  11. Microsoft Word - 11-0702 _WRES 11-103 Att._ _Notification of...

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

    Enclosure cc: wenclosure S. Zappe, NMED *ED *ED denotes electronic distribution CBFO:OESH :GTB:MAG:11 -0702:UFC 5487.00 M. harif, General Manager Washington TRU Solutions, LLC...

  12. Microsoft Word - 11-0656 _signature on file_.docx

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

    RU:MAG:11-0656:UFC 2300.00 Department of Energy Carlsbad Field Office P. O. Box 3090 Carlsbad, New Mexico 88221 August 17, 2011 Mr. John Kieling, Acting Chief Hazardous Waste...

  13. Microsoft Word - 09-1690.doc

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

    MAG:09-1690:UFC 2300.00 Department of Energy Carlsbad Field Office P. O. Box 3090 Carlsbad, New Mexico 88221 September 22, 2009 Mr. Steve Zappe, Project Leader Hazardous Materials...

  14. YFTB_final_rep_FINAL2

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

    negative numbers are points above sea level. Magnitudes are from the PNSN. YEARMODA HRMN SECO LAT ( ') LON ( ') DEPTH MAG TYPE 19821030 2240 57.17 45 59.50 119 18.30 -0.20...

  15. Search for: All records | SciTech Connect

    Office of Scientific and Technical Information (OSTI)

    +- 0.21 mag. The integrated FUV and NUV photometry, compared with stellar population models, yields ages of the SF complexes up to a few hundred Myr, and masses from 2 x...

  16. MOxST Magnesium Recycling Concept Definition Project Final Report

    Office of Scientific and Technical Information (OSTI)

    ... of MagGen(tm) scale-up R&D. Synergies between ... He has authored 81 refereed journal articles and 83 other ... present Task 5 Project Management and Reporting. 3.1 ...

  17. Carlsbad Field Office

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

    of the CBFO Office of Quality Assurance, at (575) 234-7476. Sincerely, signature on file Jose R. Franco, Manager Carlsbad Field Office Enclosure CBFO:OQA:MPN:MAG:14-1052...

  18. --No Title--

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

    of the CBFO Office of Quality Assurance, at (575) 234-7476. Sincerely, signature on file Jose R. Franco, Manager Carlsbad Field Office Enclosure CBFO:OQA:DSM:MAG:14-1047...

  19. Optical and ultraviolet observations of the narrow-lined type...

    Office of Scientific and Technical Information (OSTI)

    m sub 15(B) 0.85 0.05 mag). Based on the UV and optical light curves, we derived that a sup 56Ni mass of about 0.88 M sub was synthesized in the explosion....

  20. DISCOVERY OF H? EMISSION FROM THE CLOSE COMPANION INSIDE THE GAP OF TRANSITIONAL DISK HD142527

    SciTech Connect (OSTI)

    Close, L. M.; Follette, K. B.; Males, J. R.; Apai, D.; Morzinski, K.; Rodigas, T. J.; Hinz, P.; Bailey, V.; Puglisi, A.; Xompero, M.; Briguglio, R.; Najita, J.; Weinberger, A. J.

    2014-02-01

    We utilized the new high-order 585 actuator Magellan Adaptive Optics system (MagAO) to obtain very high-resolution visible light images of HD142527 with MagAO's VisAO science camera. In the median seeing conditions of the 6.5m Magellan telescope (0.''50.''7), we find MagAO delivers 24%-19% Strehl at H? (0.656 ?m). We detect a faint companion (HD142527B) embedded in this young transitional disk system at just 86.3 1.9 mas (?12 AU) from the star. The companion is detected in both H? and a continuum filter (?mag = 6.33 0.20 mag at H? and 7.50 0.25 mag in the continuum filter). This provides confirmation of the tentative companion discovered by Biller and co-workers with sparse aperture masking at the 8m Very Large Telescope. The H? emission from the ?0.25 solar mass companion (EW = 180 ) implies a mass accretion rate of ?5.9 10{sup 10} M {sub sun} yr{sup 1} and a total accretion luminosity of 1.2% L {sub sun}. Assuming a similar accretion rate, we estimate that a 1 Jupiter mass gas giant could have considerably better (50-1000) planet/star contrasts at H? than at the H band (COND models) for a range of optical extinctions (3.4-0 mag). We suggest that ?0.5-5 M {sub jup} extrasolar planets in their gas accretion phase could be much more luminous at H? than in the NIR. This is the motivation for our new MagAO GAPplanetS survey for extrasolar planets.

  1. Protecting Against Nuclear Threats

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

    Protecting Against Nuclear Threats Protecting Against Nuclear Threats Los Alamos' mission is to solve national security challenges through scientific excellence. April 12, 2012 Los Alamos researchers use a magnetic field detector to screen carry-on liquids at airports Los Alamos researchers use a magnetic field detector to screen carry-on liquids at airports: MagViz project leader Michelle Espy demonstrates the MagViz liquid detection and analysis system in the Albuquerque International Sunport.

  2. A NEW LARGE SUPER-FAST ROTATOR: (335433) 2005 UW163

    SciTech Connect (OSTI)

    Chang, Chan-Kao; Lin, Hsing-Wen; Ip, Wing-Huen; Waszczak, Adam; Prince, Thomas A.; Kulkarni, Shrinivas R.; Laher, Russ; Surace, Jason

    2014-08-20

    Asteroids of size larger than 150m generally do not have rotation periods smaller than 2.2 hr. This spin cutoff is believed to be due to the gravitationally bound rubble-pile structures of the asteroids. Rotation with periods exceeding this critical value will cause asteroid breakup. Up until now, only one object, 2001 OE84, has been found to be an exception to this spin cutoff. We report the discovery of a new super-fast rotator, (335433) 2005 UW163, spinning with a period of 1.290 hr and a light curve variation of r' ? 0.8mag from the observations made at the P48 telescope and the P200 telescope of the Palomar Observatory. Its H{sub r{sup ?}}=17.690.27mag and multi-band colors (i.e., g' r' = 0.68 0.03mag, r' i' = 0.19 0.02mag and SDSS i z = 0.45mag) show it is a V-type asteroid with a diameter of 0.6 + 0.3/ 0.2 km. This indicates (335433) 2005 UW163 is a super-fast rotator beyond the regime of the small monolithic asteroid.

  3. ARM - VAP Process - sondeadjust

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

    retired HFE M1 Browse Data Shouxian, Anhui, China retired NIM M1 Browse Data Niamey, Niger retired PGH M1 Browse Data ARIES Observatory, Nainital, Uttarkhand, India; AMF1...

  4. ARM - VAP Product - sondeadjust

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

    retired HFE M1 Browse Data Shouxian, Anhui, China retired NIM M1 Browse Data Niamey, Niger retired PGH M1 Browse Data ARIES Observatory, Nainital, Uttarkhand, India; AMF1...

  5. ARM - Datastreams - skyrad20s

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

    retired PVC M1 Browse Data Highland Center, Cape Cod MA; AMF1 retired PYE M1 Browse Data Point Reyes, CA retired SBS M1 Browse Data Steamboat Springs CO, Valley Site; AMF2 retired...

  6. ARM - Instrument - gndrad

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

    Plots Highland Center, Cape Cod MA; AMF1 retired PYE M1 Browse Data Browse Plots Point Reyes, CA retired SBS M1 Browse Data Steamboat Springs CO, Valley Site; AMF2 retired TMP M1...

  7. A NEW CEPHEID DISTANCE TO THE GIANT SPIRAL M101 BASED ON IMAGE SUBTRACTION OF HUBBLE SPACE TELESCOPE/ADVANCED CAMERA FOR SURVEYS OBSERVATIONS

    SciTech Connect (OSTI)

    Shappee, Benjamin J.; Stanek, K. Z. E-mail: kstanek@astronomy.ohio-state.edu

    2011-06-01

    We accurately determine a new Cepheid distance to M101 (NGC 5457) using archival Hubble Space Telescope (HST)/Advanced Camera for Surveys V and I time series photometry of two fields within the galaxy. We make a slight modification to the ISIS image subtraction package to obtain optimal differential light curves from HST data. We discovered 827 Cepheids with periods between 3 and 80 days, the largest extragalactic sample of Cepheids observed with HST by a factor of two. With this large Cepheid sample, we find that the relative distance of M101 from the Large Magellanic Cloud is {Delta}{mu}{sub LMC} = 10.63 {+-} 0.04 (random) {+-} 0.06 (systematic) mag. If we use the geometrically determined maser distance to NGC 4258 as our distance anchor, the distance modulus of M101 is {mu}{sub 0} = 29.04 {+-} 0.05 (random) {+-} 0.18 (systematic) mag or D = 6.4 {+-} 0.2 (random) {+-} 0.5 (systematic) Mpc. The uncertainty is dominated by the maser distance estimate ({+-}0.15 mag), which should improve over the next few years. We determine a steep metallicity dependence, {gamma}, for our Cepheid sample through two methods, yielding {gamma} = -0.80 {+-} 0.21 (random) {+-} 0.06 (systematic) mag dex{sup -1} and {gamma} = -0.72{sup +0.22}{sub -0.25} (random) {+-} 0.06 (systematic) mag dex{sup -1}. We see marginal evidence for variations in the Wesenheit period-luminosity relation slope as a function of deprojected galactocentric radius. We also use the tip of the red giant branch method to independently determine the distance modulus to M101 of {mu}{sub 0} = 29.05 {+-} 0.06 (random) {+-} 0.12 (systematic) mag.

  8. ON THE DISTANCE OF THE MAGELLANIC CLOUDS USING CEPHEID NIR AND OPTICAL-NIR PERIOD-WESENHEIT RELATIONS

    SciTech Connect (OSTI)

    Inno, L.; Bono, G.; Buonanno, R.; Genovali, K.; Matsunaga, N.; Caputo, F.; Laney, C. D.; Marconi, M.; Piersimoni, A. M.; Primas, F.; Romaniello, M.

    2013-02-10

    We present the largest near-infrared (NIR) data sets, JHKs, ever collected for classical Cepheids in the Magellanic Clouds (MCs). We selected fundamental (FU) and first overtone (FO) pulsators, and found 4150 (2571 FU, 1579 FO) Cepheids for Small Magellanic Cloud (SMC) and 3042 (1840 FU, 1202 FO) for Large Magellanic Cloud (LMC). Current sample is 2-3 times larger than any sample used in previous investigations with NIR photometry. We also discuss optical VI photometry from OGLE-III. NIR and optical-NIR Period-Wesenheit (PW) relations are linear over the entire period range (0.0 < log P {sub FU} {<=} 1.65) and their slopes are, within the intrinsic dispersions, common between the MCs. These are consistent with recent results from pulsation models and observations suggesting that the PW relations are minimally affected by the metal content. The new FU and FO PW relations were calibrated using a sample of Galactic Cepheids with distances based on trigonometric parallaxes and Cepheid pulsation models. By using FU Cepheids we found a true distance moduli of 18.45 {+-} 0.02(random) {+-} 0.10(systematic) mag (LMC) and 18.93 {+-} 0.02(random) {+-} 0.10(systematic) mag (SMC). These estimates are the weighted mean over 10 PW relations and the systematic errors account for uncertainties in the zero point and in the reddening law. We found similar distances using FO Cepheids (18.60 {+-} 0.03(random) {+-} 0.10(systematic) mag (LMC) and 19.12 {+-} 0.03(random) {+-} 0.10(systematic) mag (SMC)). These new MC distances lead to the relative distance, {Delta}{mu} = 0.48 {+-} 0.03 mag (FU, log P = 1) and {Delta}{mu} = 0.52 {+-} 0.03 mag (FO, log P = 0.5), which agrees quite well with previous estimates based on robust distance indicators.

  9. Magellan Queues End November 30

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

    Magellan Queues End November 30 Magellan Queues End November 30 November 15, 2011 by Francesca Verdier Schedule and Status Mon, Nov 28 westmere queue drain - 08:00 - DONE remove - 10:20 - DONE serial queue add westmere nodes - 10:40 - DONE Tue, Nov 29 mag_xlmem queue drain - 08:00 - DONE remove - 09:15 - DONE reg_xlmem queue create - 14:00 - DONE enable - 17:00 Wed, Nov 30 no queue modifications Thu, Dec 1 magellan queue drain - 08:00 - DONE remove - 09:30 - DONE mag_serial queue drain - 08:00

  10. A 2.15 hr ORBITAL PERIOD FOR THE LOW-MASS X-RAY BINARY XB 1832-330 IN THE GLOBULAR CLUSTER NGC 6652

    SciTech Connect (OSTI)

    Engel, M. C.; Heinke, C. O.; Sivakoff, G. R.; Elshamouty, K. G.; Edmonds, P. D. E-mail: heinke@ualberta.ca

    2012-03-10

    We present a candidate orbital period for the low-mass X-ray binary (LMXB) XB 1832-330 in the globular cluster NGC 6652 using a 6.5 hr Gemini South observation of the optical counterpart of the system. Light curves in g' and r' for two LMXBs in the cluster, sources A and B in previous literature, were extracted and analyzed for periodicity using the ISIS image subtraction package. A clear sinusoidal modulation is evident in both of A's curves, of amplitude {approx}0.11 mag in g' and {approx}0.065 mag in r', while B's curves exhibit rapid flickering, of amplitude {approx}1 mag in g' and {approx}0.5 mag in r'. A Lomb-Scargle test revealed a 2.15 hr periodic variation in the magnitude of A with a false alarm probability less than 10{sup -11}, and no significant periodicity in the light curve for B. Though it is possible that saturated stars in the vicinity of our sources partially contaminated our signal, the identification of A's binary period is nonetheless robust.

  11. OVERVIEW OF THE SDSS-IV MaNGA SURVEY: MAPPING NEARBY GALAXIES...

    Office of Scientific and Technical Information (OSTI)

    2000. With a typical integration time of 3 hr, MaNGA reaches a target r-band signal-to-noise ratio of 4-8 (sup -1 per 2'' fiber) at 23 AB mag arcsecsup -2, which is typical...

  12. DISPLAYING THE HETEROGENEITY OF THE SN 2002cx-LIKE SUBCLASS OF TYPE Ia SUPERNOVAE WITH OBSERVATIONS OF THE Pan-STARRS-1 DISCOVERED SN 2009ku

    SciTech Connect (OSTI)

    Narayan, G.; Foley, R. J.; Berger, E.; Chornock, R.; Rest, A.; Soderberg, A. M.; Kirshner, R. P.; Botticella, M. T.; Smartt, S.; Valenti, S.; Huber, M. E.; Scolnic, D.; Grav, T.; Burgett, W. S.; Chambers, K. C.; Flewelling, H. A.; Gates, G.; Kaiser, N.; Magnier, E. A.; Morgan, J. S. E-mail: rfoley@cfa.harvard.edu

    2011-04-10

    SN 2009ku, discovered by Pan-STARRS-1, is a Type Ia supernova (SN Ia), and a member of the distinct SN 2002cx-like class of SNe Ia. Its light curves are similar to the prototypical SN 2002cx, but are slightly broader and have a later rise to maximum in g. SN 2009ku is brighter ({approx}0.6 mag) than other SN 2002cx-like objects, peaking at M{sub V} = -18.4 mag, which is still significantly fainter than typical SNe Ia. SN 2009ku, which had an ejecta velocity of {approx}2000 km s{sup -1} at 18 days after maximum brightness, is spectroscopically most similar to SN 2008ha, which also had extremely low-velocity ejecta. However, SN 2008ha had an exceedingly low luminosity, peaking at M{sub V} = -14.2 mag, {approx}4 mag fainter than SN 2009ku. The contrast of high luminosity and low ejecta velocity for SN 2009ku is contrary to an emerging trend seen for the SN 2002cx class. SN 2009ku is a counterexample of a previously held belief that the class was more homogeneous than typical SNe Ia, indicating that the class has a diverse progenitor population and/or complicated explosion physics. As the first example of a member of this class of objects from the new generation of transient surveys, SN 2009ku is an indication of the potential for these surveys to find rare and interesting objects.

  13. The calibration of the WISE W1 and W2 Tully-Fisher relation

    SciTech Connect (OSTI)

    Neill, J. D. [California Institute of Technology, 1200 East California Boulevard, MC 278-17, Pasadena, CA 91125 (United States); Seibert, Mark; Scowcroft, Victoria [The Observatories of the Carnegie Institute of Washington, 813 Santa Barbara Street, Pasadena, CA 91101 (United States); Tully, R. Brent [Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822 (United States); Courtois, Hlne; Sorce, Jenny G. [Institut de Physique Nucleaire, Universit Claude Bernard Lyon I, F-69100 Lyon (France); Jarrett, T. H. [University of Cape Town, Private Bag X3, Rondebosch 7701, Republic of South Africa (South Africa); Masci, Frank J. [Image Processing and Analysis Center (IPAC), California Institute of Technology, 1200 East California Boulevard, MC 100-22, Pasadena, CA 91125 (United States)

    2014-09-10

    In order to explore local large-scale structures and velocity fields, accurate galaxy distance measures are needed. We now extend the well-tested recipe for calibrating the correlation between galaxy rotation rates and luminositiescapable of providing such distance measuresto the all-sky, space-based imaging data from the Wide-field Infrared Survey Explorer (WISE) W1 (3.4 ?m) and W2 (4.6 ?m) filters. We find a correlation of line width to absolute magnitude (known as the Tully-Fisher relation, TFR) of M{sub W1}{sup b,i,k,a}=?20.35?9.56(log?W{sub mx}{sup i}?2.5) (0.54 mag rms) and M{sub W2}{sup b,i,k,a}=?19.76?9.74(log?W{sub mx}{sup i}?2.5) (0.56 mag rms) from 310 galaxies in 13 clusters. We update the I-band TFR using a sample 9% larger than in Tully and Courtois. We derive M{sub I}{sup b,i,k}=?21.34?8.95(log?W{sub mx}{sup i}?2.5) (0.46 mag rms). The WISE TFRs show evidence of curvature. Quadratic fits give M{sub W1}{sup b,i,k,a}=?20.48?8.36(log?W{sub mx}{sup i}?2.5)+3.60(log?W{sub mx}{sup i}?2.5){sup 2} (0.52 mag rms) and M{sub W2}{sup b,i,k,a}=?19.91?8.40(log?W{sub mx}{sup i}?2.5)+4.32(log?W{sub mx}{sup i}?2.5){sup 2} (0.55 mag rms). We apply an I-band WISE color correction to lower the scatter and derive M{sub C{sub W{sub 1}}}=?20.22?9.12(log?W{sub mx}{sup i}?2.5) and M{sub C{sub W{sub 2}}}=?19.63?9.11(log?W{sub mx}{sup i}?2.5) (both 0.46 mag rms). Using our three independent TFRs (W1 curved, W2 curved, and I band), we calibrate the UNION2 Type Ia supernova sample distance scale and derive H {sub 0} = 74.4 1.4(stat) 2.4(sys) km s{sup 1} Mpc{sup 1} with 4% total error.

  14. Search for: All records | SciTech Connect

    Office of Scientific and Technical Information (OSTI)

    De la Torre, Angeles G. (1) Leon-Reina, Laura (1) Losilla, Enrique R. (1) Martin-Sedeno, M. Carmen (1) Merlini, Marco (1) Ordonez, Luis M. (1) Porras-Vazquez, Jose M. (1) Save ...

  15. ARM - Datastreams - twrcam3m

    Office of Scientific and Technical Information (OSTI)

    Atqasuk AK retired ARM Mobile Facility FKB M1 Browse Data Browse Plots Black Forest, Germany retired GRW M1 Browse Data Browse Plots Graciosa Island, Azores, Portugal retired NIM...

  16. Clostridium thermocellum transcriptomic profiles after exposure...

    Office of Scientific and Technical Information (OSTI)

    Authors: Wilson, Charlotte M 1 ; Yang, Shihui 1 ; Ma, Qin 2 ; Johnson, Courtney M 1 ; Rodriguez Jr, Miguel 1 ; Dice, Lezlee T 1 ; Xu, Ying 2 ; Brown, Steven D 1 + ...

  17. ARM - Instrument - ccn

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

    PVC M1 Browse Data Highland Center, Cape Cod MA; AMF1 retired PYE M1 Browse Data Point Reyes, CA retired SBS S2 Browse Data Browse Plots Steamboat Springs CO, Christie Peak...

  18. ARM - Datastreams - nfov2ch

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

    Observatory, Nainital, Uttarkhand, India; AMF1 retired PVC M1 Browse Data Browse Plots Highland Center, Cape Cod MA; AMF1 retired PYE M1 Browse Data Browse Plots Point Reyes, CA...

  19. ARM - Datastreams - twrcam3m

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

    M1 Browse Data Highland Center, Cape Cod MA; AMF1 retired PYE M1 Browse Data Browse Plots Point Reyes, CA retired retired Originating instrument has been retired at this location...

  20. ARM - VAP Process - aip

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

    retired PVC M1 Browse Data Highland Center, Cape Cod MA; AMF1 retired PYE M1 Browse Data Point Reyes, CA retired retired Originating instrument has been retired at this location...

  1. ARM - Datastreams - mpl

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

    Browse Plots Central Facility, Darwin, Australia retired ARM Mobile Facility NIM M1 Browse Data Browse Plots Niamey, Niger retired PYE M1 Browse Data Browse Plots Point Reyes, CA...

  2. ARM - VAP Process - pblht

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

    ARIES Observatory, Nainital, Uttarkhand, India; AMF1 retired PYE M1 Browse Data Point Reyes, CA retired TMP M1 Browse Data U. of Helsinki Research Station (SMEAR II), Hyytiala,...

  3. ARM - Instrument - mpl

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

    Browse Plots Highland Center, Cape Cod MA; AMF1 PYE M1 Browse Data Browse Plots Point Reyes, CA retired SBS S1 Browse Data Steamboat Springs CO, Thunderhead Lodge TMP M1 Browse...

  4. ARM - VAP Process - aerinf

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

    PVC M1 Browse Data Highland Center, Cape Cod MA; AMF1 retired PYE M1 Browse Data Point Reyes, CA retired retired Originating instrument has been retired at this location...

  5. ARM - Instrument - mwr

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

    Plots ARIES Observatory, Nainital, Uttarkhand, India; AMF1 retired PVC M1 Browse Data Highland Center, Cape Cod MA; AMF1 retired PYE M1 Browse Data Browse Plots Point Reyes, CA...

  6. ARM - VAP Process - mergesonde

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

    Anhui, China retired NIM M1 Browse Data Niamey, Niger retired PYE M1 Browse Data Point Reyes, CA retired retired Originating instrument has been retired at this location...

  7. ARM - Instrument - aos

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

    M1 Browse Data Browse Plots Highland Center, Cape Cod MA; AMF1 PYE M1 Browse Data Point Reyes, CA retired SBS S2 Browse Data Steamboat Springs CO, Christie Peak retired TMP S1...

  8. ARM - Instrument - sonde

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

    Plots Highland Center, Cape Cod MA; AMF1 retired PYE M1 Browse Data Browse Plots Point Reyes, CA retired SBS M1 Browse Data Browse Plots Steamboat Springs CO, Valley Site; AMF2...

  9. ARM - Datastreams - sondewnpn

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

    Plots Highland Center, Cape Cod MA; AMF1 retired PYE M1 Browse Data Browse Plots Point Reyes, CA retired SBS M1 Browse Data Browse Plots Steamboat Springs CO, Valley Site; AMF2...

  10. ARM - Instrument - mfr

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

    Central Facility, Lamont, OK ARM Mobile Facility AWR M1 Browse Data McMurdo Station Ross Ice Shelf, Antarctica; AMF2 MAO M1 Browse Data Browse Plots Manacapuru, Amazonas,...

  11. LCLS CDR Appendix A - Parameter Tables

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

    ... size 109 96 m FWHM FEL mode & mode source 13 1.5 rad 1st harmonic rms FEL Rayleigh waist 32 28 m 1st harmonic FEL Rayleigh length 4.2 32 m 1st harmonic homogeneous bandwidth ...

  12. Sustainable Energy Resources for Consumers Fact Sheet July 2011

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

    Technology Estimated SERC Funds Estimated SERC Installations Solar Hot Water 20 M 2,500 Solar Photovoltaics 11 M 1,000 Solar Thermal Air Heating Panels 5.4 M 1,000 Heat Pump ...

  13. Diagnosing laser-preheated magnetized plasmas relevant to magnetized liner inertial fusion

    SciTech Connect (OSTI)

    Harvey-Thompson, Adam James; Sefkow, Adam B.; Nagayama, Taisuke N.; Wei, Mingsheng; Campbell, Edward Michael; Fiksel, Gennady; Chang, Po -Yu; Davies, Jonathan R.; Barnak, Daniel H.; Glebov, Vladimir Y.; Fitzsimmons, Paul; Fooks, Julie; Blue, Brent E.

    2015-12-22

    In this paper, we present a platform on the OMEGA EP Laser Facility that creates and diagnoses the conditions present during the preheat stage of the MAGnetized Liner Inertial Fusion (MagLIF) concept. Experiments were conducted using 9 kJ of 3? (355 nm) light to heat an underdense deuterium gas (electron density: 2.5 1020 cm-3 = 0.025 of critical density) magnetized with a 10 T axial field. Results show that the deuterium plasma reached a peak electron temperature of 670 140 eV, diagnosed using streaked spectroscopy of an argon dopant. The results demonstrate that plasmas relevant to the preheat stage of MagLIF can be produced at multiple laser facilities, thereby enabling more rapid progress in understanding magnetized preheat. Results are compared with magneto-radiation-hydrodynamics simulations, and plans for future experiments are described.

  14. Diagnosing laser-preheated magnetized plasmas relevant to magnetized liner inertial fusion

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

    Harvey-Thompson, Adam James; Sefkow, Adam B.; Nagayama, Taisuke N.; Wei, Mingsheng; Campbell, Edward Michael; Fiksel, Gennady; Chang, Po -Yu; Davies, Jonathan R.; Barnak, Daniel H.; Glebov, Vladimir Y.; et al

    2015-12-22

    In this paper, we present a platform on the OMEGA EP Laser Facility that creates and diagnoses the conditions present during the preheat stage of the MAGnetized Liner Inertial Fusion (MagLIF) concept. Experiments were conducted using 9 kJ of 3ω (355 nm) light to heat an underdense deuterium gas (electron density: 2.5 × 1020 cm-3 = 0.025 of critical density) magnetized with a 10 T axial field. Results show that the deuterium plasma reached a peak electron temperature of 670 ± 140 eV, diagnosed using streaked spectroscopy of an argon dopant. The results demonstrate that plasmas relevant to the preheatmore » stage of MagLIF can be produced at multiple laser facilities, thereby enabling more rapid progress in understanding magnetized preheat. Results are compared with magneto-radiation-hydrodynamics simulations, and plans for future experiments are described.« less

  15. PHOTOMETRY OF VARIABLE STARS FROM DOME A, ANTARCTICA: RESULTS FROM THE 2010 OBSERVING SEASON

    SciTech Connect (OSTI)

    Wang, Lingzhi; Zhu, Zonghong; Macri, Lucas M.; Wang, Lifan; Ashley, Michael C. B.; Lawrence, Jon S.; Luong-Van, Daniel; Storey, John W. V.; Cui, Xiangqun; Feng, Long-Long; Gong, Xuefei; Liu, Qiang; Shang, Zhaohui; Yang, Huigen; Yang, Ji; Yuan, Xiangyan; Zhou, Xu; Zhu, Zhenxi; Pennypacker, Carl R.; York, Donald G.

    2013-12-01

    We present results from a season of observations with the Chinese Small Telescope ARray, obtained over 183 days of the 2010 Antarctic winter. We carried out high-cadence time-series aperture photometry of 9125 stars with i ?< 15.3 mag located in a 23 deg{sup 2} region centered on the south celestial pole. We identified 188 variable stars, including 67 new objects relative to our 2008 observations, thanks to broader synoptic coverage, a deeper magnitude limit, and a larger field of view. We used the photometric data set to derive site statistics from Dome A. Based on two years of observations, we find that extinction due to clouds at this site is less than 0.1 and 0.4 mag during 45% and 75% of the dark time, respectively.

  16. Efficient One-Step Electrolytic Recycling of Low-Grade and Post-Consumer Magnesium Scrap

    SciTech Connect (OSTI)

    Adam C. Powell, IV

    2012-07-19

    Metal Oxygen Separation Technologies, Inc. (abbreviated MOxST, pronounced most) and Boston University (BU) have developed a new low-cost process for recycling post-consumer co-mingled and heavily-oxidized magnesium scrap, and discovered a new chemical mechanism for magnesium separations in the process. The new process, designated MagReGenTM, is very effective in laboratory experiments, and on scale-up promises to be the lowest-cost lowest-energy lowest-impact method for separating magnesium metal from aluminum while recovering oxidized magnesium. MagReGenTM uses as little as one-eighth as much energy as today's methods for recycling magnesium metal from comingled scrap. As such, this technology could play a vital role in recycling automotive non-ferrous metals, particularly as motor vehicle magnesium/aluminum ratios increase in order to reduce vehicle weight and increase efficiency.

  17. NEAR-INFRARED IMAGING OF A z = 6.42 QUASAR HOST GALAXY WITH THE HUBBLE SPACE TELESCOPE WIDE FIELD CAMERA 3

    SciTech Connect (OSTI)

    Mechtley, M.; Windhorst, R. A.; Cohen, S. H.; Jansen, R. A.; Scannapieco, E.; Ryan, R. E.; Koekemoer, A. M.; Schneider, G.; Fan, X.; Hathi, N. P.; Keel, W. C.; Roettgering, H.; Schneider, D. P.; Strauss, M. A.; Yan, H. J.

    2012-09-10

    We report on deep near-infrared F125W (J) and F160W (H) Hubble Space Telescope Wide Field Camera 3 images of the z = 6.42 quasar J1148+5251 to attempt to detect rest-frame near-ultraviolet emission from the host galaxy. These observations included contemporaneous observations of a nearby star of similar near-infrared colors to measure temporal variations in the telescope and instrument point-spread function (PSF). We subtract the quasar point source using both this direct PSF and a model PSF. Using direct subtraction, we measure an upper limit for the quasar host galaxy of m{sub J} > 22.8 and m{sub H} > 23.0 AB mag (2 {sigma}). After subtracting our best model PSF, we measure a limiting surface brightness from 0.''3 to 0.''5 radius of {mu}{sub J} > 23.5 and {mu}{sub H} > 23.7 AB mag arcsec{sup -2} (2 {sigma}). We test the ability of the model subtraction method to recover the host galaxy flux by simulating host galaxies with varying integrated magnitude, effective radius, and Sersic index, and conducting the same analysis. These models indicate that the surface brightness limit ({mu}{sub J} > 23.5 AB mag arcsec{sup -2}) corresponds to an integrated upper limit of m{sub J} > 22-23 AB mag, consistent with the direct subtraction method. Combined with existing far-infrared observations, this gives an infrared excess log (IRX) > 1.0 and corresponding ultraviolet spectral slope {beta} > -1.2 {+-} 0.2. These values match those of most local luminous infrared galaxies, but are redder than those of almost all local star-forming galaxies and z {approx_equal} 6 Lyman break galaxies.

  18. Los Alamos Team Demonstrates Bottle Scanner Technology

    ScienceCinema (OSTI)

    Espy, Michelle; Schultz, Larry

    2014-06-02

    Los Alamos scientists are demonstrating a Nuclear Magnetic Resonance Imaging (NMR) technology that may provide a breakthrough for screening liquids at airport security. By adding low-power X-ray data to the NMR mix, scientists believe they have unlocked a new detection technology. Funded in part by the Department of Homeland Security's Science and Technology Directorate, the new technology is called MagRay.

  19. A plausible (overlooked) super-luminous supernova in the Sloan digital sky survey stripe 82 data

    SciTech Connect (OSTI)

    Kostrzewa-Rutkowska, Zuzanna; Koz?owski, Szymon; Wyrzykowski, ?ukasz; Djorgovski, S. George; Mahabal, Ashish A.; Glikman, Eilat; Koposov, Sergey E-mail: simkoz@astrouw.edu.pl

    2013-12-01

    We present the discovery of a plausible super-luminous supernova (SLSN), found in the archival data of Sloan Digital Sky Survey (SDSS) Stripe 82, called PSN 000123+000504. The supernova (SN) peaked at m {sub g} < 19.4 mag in the second half of 2005 September, but was missed by the real-time SN hunt. The observed part of the light curve (17 epochs) showed that the rise to the maximum took over 30 days, while the decline time lasted at least 70 days (observed frame), closely resembling other SLSNe of SN 2007bi type. The spectrum of the host galaxy reveals a redshift of z = 0.281 and the distance modulus of ? = 40.77 mag. Combining this information with the SDSS photometry, we found the host galaxy to be an LMC-like irregular dwarf galaxy with an absolute magnitude of M{sub B} = 18.2 0.2 mag and an oxygen abundance of 12+log?[O/H]=8.30.2; hence, the SN peaked at M {sub g} < 21.3 mag. Our SLSN follows the relation for the most energetic/super-luminous SNe exploding in low-metallicity environments, but we found no clear evidence for SLSNe to explode in low-luminosity (dwarf) galaxies only. The available information on the PSN 000123+000504 light curve suggests the magnetar-powered model as a likely scenario of this event. This SLSN is a new addition to a quickly growing family of super-luminous SNe.

  20. Superluminous supernovae as standardizable candles and high-redshift distance probes

    SciTech Connect (OSTI)

    Inserra, C.; Smartt, S. J., E-mail: c.inserra@qub.ac.uk [Astrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN (United Kingdom)

    2014-12-01

    We investigate the use of type Ic superluminous supernovae (SLSN Ic) as standardizable candles and distance indicators. Their appeal as cosmological probes stems from their remarkable peak luminosities, hot blackbody temperatures, and bright rest-frame ultraviolet emission. We present a sample of 16 published SLSN, from redshifts 0.1 to 1.2, and calculate accurate K corrections to determine uniform magnitudes in 2 synthetic rest-frame filter bandpasses with central wavelengths at 400 nm and 520 nm. At 400 nm, we find an encouragingly low scatter in their uncorrected, raw mean magnitudes with M(400) = 21.86 0.35 mag for the full sample of 16 objects. We investigate the correlation between their decline rates and peak magnitude and find that the brighter events appear to decline more slowly. In a manner similar to the Phillips relation for type Ia SNe (SNe Ia), we define a ?M {sub 20} decline relation. This correlates peak magnitude and decline over 20 days and can reduce the scatter in standardized peak magnitudes to 0.22 mag. We further show that M(400) appears to have a strong color dependence. Redder objects are fainter and also become redder faster. Using this peak magnitudecolor evolution relation, a surprisingly low scatter of between 0.08 mag and 0.13 mag can be found in peak magnitudes, depending on sample selection. However, we caution that only 8 to 10 objects currently have enough data to test this peak magnitudecolor evolution relation. We conclude that SLSN Ic are promising distance indicators in the high-redshift universe in regimes beyond those possible with SNe Ia. Although the empirical relationships are encouraging, the unknown progenitor systems, how they may evolve with redshift, and the uncertain explosion physics are of some concern. The two major measurement uncertainties are the limited numbers of low-redshift, well-studied objects available to test these relationships and internal dust extinction in the host galaxies.

  1. TYPE Ia SUPERNOVA COLORS AND EJECTA VELOCITIES: HIERARCHICAL BAYESIAN REGRESSION WITH NON-GAUSSIAN DISTRIBUTIONS

    SciTech Connect (OSTI)

    Mandel, Kaisey S.; Kirshner, Robert P. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Foley, Ryan J., E-mail: kmandel@cfa.harvard.edu [Astronomy Department, University of Illinois at Urbana-Champaign, 1002 West Green Street, Urbana, IL 61801 (United States)

    2014-12-20

    We investigate the statistical dependence of the peak intrinsic colors of Type Ia supernovae (SNe Ia) on their expansion velocities at maximum light, measured from the Si II ?6355 spectral feature. We construct a new hierarchical Bayesian regression model, accounting for the random effects of intrinsic scatter, measurement error, and reddening by host galaxy dust, and implement a Gibbs sampler and deviance information criteria to estimate the correlation. The method is applied to the apparent colors from BVRI light curves and Si II velocity data for 79 nearby SNe Ia. The apparent color distributions of high-velocity (HV) and normal velocity (NV) supernovae exhibit significant discrepancies for B V and B R, but not other colors. Hence, they are likely due to intrinsic color differences originating in the B band, rather than dust reddening. The mean intrinsic B V and B R color differences between HV and NV groups are 0.06 0.02 and 0.09 0.02 mag, respectively. A linear model finds significant slopes of 0.021 0.006 and 0.030 0.009 mag (10{sup 3} km s{sup 1}){sup 1} for intrinsic B V and B R colors versus velocity, respectively. Because the ejecta velocity distribution is skewed toward high velocities, these effects imply non-Gaussian intrinsic color distributions with skewness up to +0.3. Accounting for the intrinsic-color-velocity correlation results in corrections to A{sub V} extinction estimates as large as 0.12 mag for HV SNe Ia and +0.06 mag for NV events. Velocity measurements from SN Ia spectra have the potential to diminish systematic errors from the confounding of intrinsic colors and dust reddening affecting supernova distances.

  2. Los Alamos Team Demonstrates Bottle Scanner Technology

    SciTech Connect (OSTI)

    Espy, Michelle; Schultz, Larry

    2014-05-06

    Los Alamos scientists are demonstrating a Nuclear Magnetic Resonance Imaging (NMR) technology that may provide a breakthrough for screening liquids at airport security. By adding low-power X-ray data to the NMR mix, scientists believe they have unlocked a new detection technology. Funded in part by the Department of Homeland Security's Science and Technology Directorate, the new technology is called MagRay.

  3. International Sunport

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

    airport liquid analysis system undergoes testing at Albuquerque International Sunport December 16, 2008 MagViz technology from Los Alamos sorts out liquids and gels LOS ALAMOS, New Mexico, December 16, 2008-An innovative application of a technology first used for medical imaging may enhance airport security if Los Alamos National Laboratory scientists are successful. Los Alamos technologists have adapted Magnetic Resonance Imaging (MRI) technology from the familiar medical device to create

  4. News | U.S. DOE Office of Science (SC)

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

    News News News Home Featured Articles Science Headlines Science Highlights Presentations & Testimony News Archives Communications and Public Affairs Contact Information Office of Science U.S. Department of Energy 1000 Independence Ave., SW Washington, DC 20585 P: (202) 586-5430 Nano Mag Flux Lines BNL Color-enhanced image of magnetic flux lines around individual nickel nanodots. (Brookhaven National Laboratory) Print Text Size: A A A Subscribe FeedbackShare Page The Office of Science has

  5. Decommissioning and PIE of the MEGAPIE spallation target

    SciTech Connect (OSTI)

    Latge, C.; Henry, J.; Wohlmuther, M.; Dai, Y.; Gavillet, D.; Hammer, B.; Heinitz, S.; Neuhausen, J.; Schumann, D.; Thomsen, K.; Tuerler, A.; Wagner, W.; Gessi, A.; Guertin, A.; Konstantinovic, M.; Lindau, R.; Maloy, S.; Saito, S.

    2013-07-01

    A key experiment in the Accelerated Driven Systems roadmap, the MEGAwatt PIlot Experiment (MEGAPIE) (1 MW) was initiated in 1999 in order to design and build a liquid lead-bismuth spallation target, then to operate it into the Swiss spallation neutron facility SINQ at Paul Scherrer Institute. The target has been designed, manufactured, and tested during integral tests, before irradiation carried out end of 2006. During irradiation, neutron and thermo hydraulic measurements were performed allowing deep interpretation of the experiment and validation of the models used during design phase. The decommissioning, Post Irradiation Examinations and waste management phases were defined properly. The phases dedicated to cutting, sampling, cleaning, waste management, samples preparation and shipping to various laboratories were performed by PSI teams: all these phases constitute a huge work, which allows now to perform post-irradiation examination (PIE) of structural material, irradiated in relevant conditions. Preliminary results are presented in the paper, they concern chemical characterization. The following radio-nuclides have been identified by ?-spectrometry: {sup 60}Co, {sup 101}Rh, {sup 102}Rh, {sup 108m}Ag, {sup 110m}Ag, {sup 133}Ba, {sup 172}Hf/Lu, {sup 173}Lu, {sup 194}Hg/Au, {sup 195}Au, {sup 207}Bi. For some of these nuclides the activities can be easily evaluated from ?-spectrometry results ({sup 207}Bi, {sup 194}Hg/Au), while other nuclides can only be determined after chemical separations ({sup 108m}Ag, {sup 110m}Ag, {sup 195}Au, {sup 129}I, {sup 36}Cl and ?-emitting {sup 208-210}Po). The concentration of {sup 129}I is lower than expected. The chemical analysis already performed on spallation and corrosion products in the lead-bismuth eutectic (LBE) are very relevant for further applications of LBE as a spallation media and more generally as a coolant.

  6. Microsoft Word - 09-1690.doc

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

    MAG:09-1690:UFC 2300.00 Department of Energy Carlsbad Field Office P. O. Box 3090 Carlsbad, New Mexico 88221 September 22, 2009 Mr. Steve Zappe, Project Leader Hazardous Materials Bureau New Mexico Environment Department 2905 E. Rodeo Park Drive, Building 1 Santa Fe, New Mexico 87502-6110 Subject: Transmittal of the Contact-Handled Waste Certification Audit Report for the Oak Ridge National Laboratory Central Characterization Project, Audit A-09-24 Dear Mr. Zappe: This letter transmits the

  7. Type Ia supernovae yielding distances with 3-4% precision (Journal Article)

    Office of Scientific and Technical Information (OSTI)

    | SciTech Connect Type Ia supernovae yielding distances with 3-4% precision Citation Details In-Document Search Title: Type Ia supernovae yielding distances with 3-4% precision The luminosities of Type Ia supernovae (SN), the thermonuclear explosions of white dwarf stars, vary systematically with their intrinsic color and light-curve decline rate. These relationships have been used to calibrate their luminosities to within ~0.14-0.20 mag from broadband optical light curves, yielding

  8. Cooperative Monitoring Center Occasional Paper/11: Cooperative Environmental Monitoring in the Coastal Regions of India and Pakistan

    SciTech Connect (OSTI)

    Rajen, Gauray

    1999-06-01

    The cessation of hostilities between India and Pakistan is an immediate need and of global concern, as these countries have tested nuclear devices, and have the capability to deploy nuclear weapons and long-range ballistic missiles. Cooperative monitoring projects among neighboring countries in South Asia could build regional confidence, and, through gradual improvements in relations, reduce the threat of war and the proliferation of weapons of mass destruction. This paper discusses monitoring the trans-border movement of flow and sediment in the Indian and Pakistani coastal areas. Through such a project, India and Pakistan could initiate greater cooperation, and engender movement towards the resolution of the Sir Creek territorial dispute in their coastal region. The Joint Working Groups dialogue being conducted by India and Pakistan provides a mechanism for promoting such a project. The proposed project also falls within a regional framework of cooperation agreed to by several South Asian countries. This framework has been codified in the South Asian Seas Action Plan, developed by Bangladesh, India, Maldives, Pakistan and Sri Lanka. This framework provides a useful starting point for Indian and Pakistani cooperative monitoring in their trans-border coastal area. The project discussed in this paper involves computer modeling, the placement of in situ sensors for remote data acquisition, and the development of joint reports. Preliminary computer modeling studies are presented in the paper. These results illustrate the cross-flow connections between Indian and Pakistani coastal regions and strengthen the argument for cooperation. Technologies and actions similar to those suggested for the coastal project are likely to be applied in future arms control and treaty verification agreements. The project, therefore, serves as a demonstration of cooperative monitoring technologies. The project will also increase people-to-people contacts among Indian and Pakistani policy makers and scientists. In the perceptions of the general public, the project will crystallize the idea that the two countries share ecosystems and natural resources, and have a vested interest in increased collaboration.

  9. The Gemini NICI planet-finding campaign: The companion detection pipeline

    SciTech Connect (OSTI)

    Wahhaj, Zahed; Liu, Michael C.; Nielsen, Eric L.; Chun, Mark; Ftaclas, Christ; Biller, Beth A.; Close, Laird M.; Hayward, Thomas L.; Hartung, Markus

    2013-12-10

    We present high-contrast image processing techniques used by the Gemini NICI Planet-Finding Campaign to detect faint companions to bright stars. The Near-Infrared Coronographic Imager (NICI) is an adaptive optics instrument installed on the 8 m Gemini South telescope, capable of angular and spectral difference imaging and specifically designed to image exoplanets. The Campaign data pipeline achieves median contrasts of 12.6 mag at 0.''5 and 14.4 mag at 1'' separation, for a sample of 45 stars (V = 4.3-13.9 mag) from the early phase of the campaign. We also present a novel approach to calculating contrast curves for companion detection based on 95% completeness in the recovery of artificial companions injected into the raw data, while accounting for the false-positive rate. We use this technique to select the image processing algorithms that are more successful at recovering faint simulated point sources. We compare our pipeline to the performance of the Locally Optimized Combination of Images (LOCI) algorithm for NICI data and do not find significant improvement with LOCI.

  10. A semi-analytic model of magnetized liner inertial fusion

    SciTech Connect (OSTI)

    McBride, Ryan D.; Slutz, Stephen A.

    2015-05-15

    Presented is a semi-analytic model of magnetized liner inertial fusion (MagLIF). This model accounts for several key aspects of MagLIF, including: (1) preheat of the fuel (optionally via laser absorption); (2) pulsed-power-driven liner implosion; (3) liner compressibility with an analytic equation of state, artificial viscosity, internal magnetic pressure, and ohmic heating; (4) adiabatic compression and heating of the fuel; (5) radiative losses and fuel opacity; (6) magnetic flux compression with Nernst thermoelectric losses; (7) magnetized electron and ion thermal conduction losses; (8) end losses; (9) enhanced losses due to prescribed dopant concentrations and contaminant mix; (10) deuterium-deuterium and deuterium-tritium primary fusion reactions for arbitrary deuterium to tritium fuel ratios; and (11) magnetized α-particle fuel heating. We show that this simplified model, with its transparent and accessible physics, can be used to reproduce the general 1D behavior presented throughout the original MagLIF paper [S. A. Slutz et al., Phys. Plasmas 17, 056303 (2010)]. We also discuss some important physics insights gained as a result of developing this model, such as the dependence of radiative loss rates on the radial fraction of the fuel that is preheated.

  11. Photospheric magnitude diagrams for type II supernovat: A promising tool to compute distances

    SciTech Connect (OSTI)

    Rodrguez, smar; Clocchiatti, Alejandro; Hamuy, Mario, E-mail: olrodrig@astro.puc.cl [Millennium Institute of Astrophysics, Casilla 36-D, Santiago (Chile)

    2014-12-01

    We develop an empirical color-based standardization for Type II supernovae (SNe II), equivalent to the classical surface brightness method given in Wesselink. We calibrate this standardization using SNe II with host galaxy distances measured using Cepheids, and a well-constrained shock breakout epoch and extinction due to the host galaxy. We estimate the reddening with an analysis of the B V versus V I color-color curves, similar to that of Natali et al. With four SNe II meeting the above requirements, we build a photospheric magnitude versus color diagram (similar to an H-R diagram) with a dispersion of 0.29 mag. We also show that when using time since shock breakout instead of color as the independent variable, the same standardization gives a dispersion of 0.09 mag. Moreover, we show that the above time-based standardization corresponds to the generalization of the standardized candle method of Hamuy and Pinto for various epochs throughout the photospheric phase. To test the new tool, we construct Hubble diagrams for different subsamples of 50 low-redshift (cz < 10{sup 4} km s{sup 1}) SNe II. For 13 SNe within the Hubble flow (cz {sub CMB} > 3000 km s{sup 1}) and with a well-constrained shock breakout epoch we obtain values of 68-69 km s{sup 1} Mpc{sup 1} for the Hubble constant and a mean intrinsic scatter of 0.12 mag or 6% in relative distances.

  12. FAINT TIDAL FEATURES IN GALAXIES WITHIN THE CANADA-FRANCE-HAWAII TELESCOPE LEGACY SURVEY WIDE FIELDS

    SciTech Connect (OSTI)

    Atkinson, Adam M.; Abraham, Roberto G.; Ferguson, Annette M. N.

    2013-03-01

    We present an analysis of the detectability of faint tidal features in galaxies from the wide-field component of the Canada-France-Hawaii Telescope Legacy Survey. Our sample consists of 1781 luminous (M{sub r{sup '}}<-19.3 mag) galaxies in the magnitude range 15.5 mag < r' < 17 mag and in the redshift range 0.04 < z < 0.2. Although we have classified tidal features according to their morphology (e.g., streams, shells, and tails), we do not attempt to interpret them in terms of their physical origin (e.g., major versus minor merger debris). Instead, we provide a catalog that is intended to provide raw material for future investigations which will probe the nature of low surface brightness substructure around galaxies. We find that around 12% of the galaxies in our sample show clear tidal features at the highest confidence level. This fraction rises to about 18% if we include systems with convincing, albeit weaker tidal features, and to 26% if we include systems with more marginal features that may or may not be tidal in origin. These proportions are a strong function of rest-frame color and of stellar mass. Linear features, shells, and fans are much more likely to occur in massive galaxies with stellar masses >10{sup 10.5} M {sub Sun }, and red galaxies are twice as likely to show tidal features than are blue galaxies.

  13. A search for fast optical transients in the Pan-STARRS1 medium-deep survey: M-dwarf flares, asteroids, limits on extragalactic rates, and implications for LSST

    SciTech Connect (OSTI)

    Berger, E.; Leibler, C. N.; Chornock, R.; Foley, R. J.; Soderberg, A. M.; Rest, A.; Price, P. A.; Burgett, W. S.; Chambers, K. C.; Flewelling, H.; Huber, M. E.; Magnier, E. A.; Tonry, J. L.; Metcalfe, N.; Stubbs, C. W.

    2013-12-10

    We present a search for fast optical transients (? ? 0.5 hr-1 day) using repeated observations of the Pan-STARRS1 Medium-Deep Survey (PS1/MDS) fields. Our search takes advantage of the consecutive g {sub P1} r {sub P1} observations (16.5 minutes in each filter), by requiring detections in both bands, with non-detections on preceding and subsequent nights. We identify 19 transients brighter than 22.5 AB mag (S/N ? 10). Of these, 11 events exhibit quiescent counterparts in the deep PS1/MDS templates that we identify as M4-M9 dwarfs at d ? 0.2-1.2 kpc. The remaining eight transients lack quiescent counterparts, exhibit mild but significant astrometric shifts between the g {sub P1} and r {sub P1} images, colors of (g r){sub P1} ? 0.5-0.8 mag, non-varying light curves, and locations near the ecliptic plane with solar elongations of about 130, which are all indicative of main-belt asteroids near the stationary point of their orbits. With identifications for all 19 transients, we place an upper limit of R {sub FOT}(? ? 0.5 hr) ? 0.12 deg{sup 2} day{sup 1} (95% confidence level) on the sky-projected rate of extragalactic fast transients at ? 22.5 mag, a factor of 30-50 times lower than previous limits; the limit for a timescale of ?1 day is R {sub FOT} ? 2.4 10{sup 3} deg{sup 2} day{sup 1}. To convert these sky-projected rates to volumetric rates, we explore the expected peak luminosities of fast optical transients powered by various mechanisms, and find that non-relativistic events are limited to M ? 10 to ? 14 mag for a timescale of ?0.5 hr to ?1 day, while relativistic sources (e.g., gamma-ray bursts, magnetar-powered transients) can reach much larger luminosities. The resulting volumetric rates are ? 13 Mpc{sup 3} yr{sup 1} (M ? 10 mag), ? 0.05 Mpc{sup 3} yr{sup 1} (M ? 14 mag), and ? 10{sup 6} Mpc{sup 3} yr{sup 1} (M ? 24 mag), significantly above the nova, supernova, and gamma-ray burst rates, respectively, indicating that much larger surveys are required to provide meaningful constraints. Motivated by the results of our search, we discuss strategies for identifying fast optical transients in the Large Synoptic Survey Telescope main survey, and reach the optimistic conclusion that the veil of foreground contaminants can be lifted with the survey data, without the need for expensive follow-up observations.

  14. The RR Lyrae stars: New perspectives

    SciTech Connect (OSTI)

    McNamara, D. H.; Barnes, J. E-mail: jonathan.barnes@slcc.edu

    2014-02-01

    We demonstrate that the Oosterhoff II (Oo II) RR Lyrae ab variables are hotter by ?270 K, at the same period, than Oo I variables. Or, at the same ((B) (V)){sub 0} value the Oo II variables have larger radii than Oo I variables. This accounts for the reason Oo II variables are brighter (0.12-0.20 mag) than Oo I variables. The dependence of the light amplitude of RR Lyrae variables on temperature is independent of Oo type. This makes it possible to derive an accurate set of equations to relate intrinsic (B V){sub 0} color indices to light amplitudes, which in turn can be used to determine the interstellar reddening (E (B V)). With just a few variables (?5), it is possible to determine the E (B V) to an accuracy of <0.01 mag in the absence of systematic photometric errors. We discuss the errors introduced in color excess determinations by including the Blazhko stars in a solution. A comparison of color excess values of 23 globular clusters and two regions of the Large Magellanic Cloud (LMC), determined with the aid of our newly developed equations, are found to compare favorably (?0.01 mag) with color excess values found in the literature. Four new Oo III variables, some found in metal-poor clusters, are discussed. An analysis of the galactic-field variables indicates the majority are Oo I and Oo II variables, but a few short-period (log P < 0.36) metal-strong variables, so far not found in galactic globular clusters are evidently ?0.30 mag fainter than Oo I variables. Oo III variables may also be present in the field. We conclude that the RR Lyrae ab variables are primarily restricted to four sequences or groups. If we assume that the Oo I variables' mean absolute magnitude is Mv = 0.61, the mean absolute magnitudes of the other three sequences are: short-period variables Mv ? 0.89 mag, Oo II Mv ? 0.43 mag, and Oo III Mv ? 0.29 mag. The Oo I fundamental RR Lyrae ab red edge (FRE) and fundamental blue edge (FBE) occur at approximately the following temperatures: FRE T ? 6180 K and FBE T ? 6750 K. There is a strong dependence of Mv on [Fe/H] as we proceed from the short-period variables to the Oo I variables and to the Oo II variables, but there seems to be little or no dependence of Mv on [Fe/H] for stars within a group, at least for the Oo I and Oo II groups. The Oo II variables exhibit a weak period luminosity relation in V in many globular clusters unlike the Oo II-like variables in Oo I clusters which do not exhibit a P-L relation. The properties of some intermediate LMC clusters are discussed.

  15. Everbrite Industries Inc | Open Energy Information

    Open Energy Info (EERE)

    Jump to: navigation, search Name: Everbrite Industries Inc. Place: Toronto, Ontario, Canada Zip: M1R 2T6 Sector: Solar Product: Everbrite Industries is an electrical contractor...

  16. Search for: All records | SciTech Connect

    Office of Scientific and Technical Information (OSTI)

    Godinez Vazquez, Humberto C. Los Alamos National Laboratory (1) Higdon, David M (1) Higdon, David M. Los Alamos National Laboratory (1) Higdon, David Mitchell (1) Hou, ...

  17. Search for: All records | DOE PAGES

    Office of Scientific and Technical Information (OSTI)

    Results Filter Results Filter by Author Bender, Carl M. (1) Comech, Andrew (1) Cooper, Fred (1) Cuevas-Maraver, Jesus (1) Kevrekidis, Panayotis G. (1) Khare, Avinash (1)...

  18. Search for: All records | DOE PAGES

    Office of Scientific and Technical Information (OSTI)

    Filtered Results Filter Results Filter by Author Khare, Avinash (4) Saxena, Avadh (4) Cooper, Fred (2) Kevrekidis, Panayotis G. (2) Bender, Carl M. (1) Christov, Ivan C. (1)...

  19. The Science of Battery Degradation. (Technical Report) | SciTech...

    Office of Scientific and Technical Information (OSTI)

    ... ; Nagasubramanian, Ganesan 1 ; Sugar, Joshua Daniel ; Talin, Albert Alec ; Tenney, Craig M 1 ; Zavadil, Kevin R. 1 + Show Author Affiliations Sandia National Laboratories, ...

  20. Nanoscale coherent intergrowths in a crystal ofLa?.?Ca?...

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    1 ; Tranquada, John M. 1 ; Billinge, Simon J. L. 2 + Show Author Affiliations Brookhaven National Lab. (BNL), Upton, NY (United States) Brookhaven National Lab. (BNL),...

  1. Search for: All records | SciTech Connect

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    ... with a magnitude m-1 which are placed in the immediate lower level of the hierarchy. ... ; Amaryan, Moscov ; Amaryan, Moskov ; Auerbach, Leonard ; Averett, Todd ; Berthot, J. ; ...

  2. Erratum: "Sensitivity of the interpretation of the experimental...

    Office of Scientific and Technical Information (OSTI)

    Authors: Stacey, W. M. 1 + Show Author Affiliations Georgia Tech Fusion Research Center, Atlanta, Georgia 30332 (United States) Georgia Tech Fusion Research Center, Atlanta, ...

  3. A new technique to measure tunneling barrier height in solid...

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    A 1 ; Dattelbaum, Andrew M 1 ; Mara, Nathan A 1 ; Kaschner, George C 1 ; Johnson, Oliver K 2 ; Seegmiller, Daniel 2 ; Fullwood, David T 2 + Show Author...

  4. "Title","Creator/Author","Publication Date","OSTI Identifier...

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    conditioning, series compensation, phase shifting, voltage balancing, fuel cell and photovoltaic utility systems interfacing, etc. The new M-level inverter consists of (M-1)2...

  5. A multilevel voltage-source inverter with separate dc sources...

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    conditioning, series compensation, phase shifting, voltage balancing, fuel cell and photovoltaic utility systems interfacing, etc. The new M-level inverter consists of (M-1)2...

  6. Bayesian approaches for combining computational model output...

    Office of Scientific and Technical Information (OSTI)

    for combining computational model output and physical observations Authors: Higdon, David M 1 ; Lawrence, Earl 1 ; Heitmann, Katrin 2 ; Habib, Salman 2 + Show Author...

  7. Quasiparticle dynamics across the full Brillouin zone of Bi2Sr2CaCu2O8...

    Office of Scientific and Technical Information (OSTI)

    Authors: Dakovski, Georgi L. 1 ; Durakiewicz, Tomasz 2 ; Zhu, Jian-Xin 3 ; Riseborough, Peter S. 4 ; Gu, Genda 5 ; Gilbertson, Steve M. 1 ; Taylor, Antoinette 6 ; ...

  8. Thermal And-Or Near Infrared At Coso Geothermal Area (2009) ...

    Open Energy Info (EERE)

    with elevation, on which temperature inversions appear superimposed as opposite trends. References Eneva, M.; Coolbaugh, M.; (1 January 2009) Importance of Elevation and...

  9. Order within disorder: The atomic structure of ion-beam sputtered...

    Office of Scientific and Technical Information (OSTI)

    Robert L. ; Route, Roger K. ; Fejer, Martin M. 1 ; Abernathy, Matthew R. ; Gustafson, Eric K. 2 ; Kim, Namjun ; Stebbins, Jonathan F. 3 ; Mehta, Apurva ; Shyam, Badri 4 ;...

  10. Slides presented by workshop participants at the International...

    Office of Scientific and Technical Information (OSTI)

    21 ; Higdon, David M. 1 ; Varet, Suzanne 22 ; Schnabel, Georg 18 ; Bauge, Eric 23 ; Koning, Arjan 24 ; Helgesson, Petter 25 ; Pomp, Stephan 25 ; Terranova, N....

  11. Piecewise moments method: Generalized Lanczos technique for nuclear...

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    Authors: Haxton, Wick C. ; Zurek, Kathryn M. 1 ; Nollett, Kenneth M. 2 + Show Author Affiliations Institute for Nuclear Theory and Department of Physics, University of ...

  12. Search for: All records | SciTech Connect

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    Zukoski, Charles F. (UIUC) (4) Hall, Lisa M. (1) Schweizer, Kenneth S. (1) Zukoski, ... So Youn ; Hall, Lisa M. ; Schweizer, Kenneth S. ; Zukoski, Charles F. September 2014 ...

  13. Teleseismic-Seismic Monitoring At Coso Geothermal Area (1998...

    Open Energy Info (EERE)

    for an earthquake of comparable magnitude at the Coso region. References Bhattacharyya, J.; Gross, S.; Lees, J.; Hastings, M. (1 June 1999) Recent earthquake sequences at Coso:...

  14. THE VEX RADIATION MODULE: 2D RADIATION TRANSPORT WITH MIMETIC...

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    the National Technical Information Service, Springfield, VA at www.ntis.gov. Authors: Powell, Devon M. 1 ; Lovegrove, Elizabeth G. 1 ; Fung, Jimmy 1 ; Kenamond, Mark A. 1...

  15. A 2D Radiation Transport Package with Mimetic Diffusion for ExaFlag...

    Office of Scientific and Technical Information (OSTI)

    the National Technical Information Service, Springfield, VA at www.ntis.gov. Authors: Powell, Devon M. 1 ; Lovegrove, Elizabeth G. 1 ; Kenamond, Mark A. 1 ; Fung, Jimmy 1...

  16. Search for: All records | SciTech Connect

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    Dehlinger, Dietrich (1) Dzenitis, John M. (1) Fisher, Karl A (1) Jung, Byoungsok (1) ... ; Dehlinger, Dietrich ; Shusteff, Maxim ; Jung, Byoungsok ; Ness, Kevin D An ultrasonic ...

  17. Table 1. Crude Oil Prices

    U.S. Energy Information Administration (EIA) Indexed Site

    from Table 24. Refiner acquisition costs -- Energy Information Administration, Form FEA-P110-M-1, "Refiners' Monthly Cost Allocation Report," January 1978 through June 1978;...

  18. X:\\L6046\\Data_Publication\\Pma\\current\\ventura\\pma.vp

    U.S. Energy Information Administration (EIA) Indexed Site

    from Table 24. Refiner acquisition costs -- Energy Information Administration, Form FEA-P110-M-1, "Refiners' Monthly Cost Allocation Report," January 1978 through June 1978;...

  19. Summary Statistics Table 1. Crude Oil Prices

    U.S. Energy Information Administration (EIA) Indexed Site

    from Table 24. Refiner acquisition costs -- Energy Information Administration, Form FEA-P110-M-1, "Refiners' Monthly Cost Allocation Report," January 1978 through June 1978;...

  20. Mechanical Behavior of the Near-field Host Rock Surrounding Excavation...

    Office of Scientific and Technical Information (OSTI)

    Service, Springfield, VA at www.ntis.gov. Authors: Kelkar, Sharad M. 1 ; Stauffer, Philip H. 1 ; Robinson, Bruce Alan 1 + Show Author Affiliations Los Alamos National...

  1. Search for: All records | DOE PAGES

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    Zhou, Miao (2) Zhou, Wu (2) Zou, Xiaolong (2) Ackerman, Thomas (1) Ajayan, Pullikel M (1) ... IN CRM Liu, Zheng ; Muhlbauer, Andreas ; Ackerman, Thomas November 2015 , Wiley Blackwell ...

  2. Spectroscopy of charmed baryons from lattice QCD (Conference...

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    well as spin-orbit coupling, are considered and those are also compared against similar energy splittings at other quark masses. Authors: Padmanath, M. 1 ; Edwards, Robert G....

  3. Targeted polypeptide degradation (Patent) | SciTech Connect

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    localization andor polypeptide degradation. The invention also provides research tools for the study of protein function. Authors: Church, George M. 1 ; Janse, Daniel M....

  4. A Framework for Integrated Modeling of Perturbations in Atmospheres...

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    David M. 1 ; Koller, Josef 1 ; Lawrence, Earl C. 1 ; Palmer, David 1 ; Thompson, David C. 1 ; Walker, Andrew C. 1 ; Wohlberg, Brendt E. 1 + Show Author ...

  5. Nanoscale coherent intergrowthlike defects in a crystal ofLa1...

    Office of Scientific and Technical Information (OSTI)

    1 ; Shi, Xiaoya 1 ; Li, Qiang 1 ; Zhong, Ruidan 1 ; Schneeloch, John A. 1 ; Gu, Genda 1 ; Tranquada, John M. 1 ; Billinge, Simon J. L. 2 + Show Author...

  6. Fundamentals of XAFS (Journal Article) | SciTech Connect

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    Journal Article: Fundamentals of XAFS Citation Details In-Document Search Title: Fundamentals of XAFS Authors: Newville, M. 1 + Show Author Affiliations (UC) Publication Date: ...

  7. X-ray absorption fine-structure spectroscopy (Book) | SciTech...

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    Authors: Newville, M. 1 + Show Author Affiliations (UC) Publication Date: 2014-12-22 OSTI Identifier: 1168410 Resource Type: Book Resource Relation: Related Information: CMS ...

  8. Introduction to computed microtomography and applications in...

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    Authors: Rivers, M. 1 + Show Author Affiliations (UC) Publication Date: 2014-12-22 OSTI Identifier: 1168409 Resource Type: Book Resource Relation: Related Information: CMS ...

  9. A CATALOG OF NEAR-IR SOURCES FOUND TO BE UNRESOLVED WITH MILLIARCSECOND RESOLUTION

    SciTech Connect (OSTI)

    Richichi, A.; Fors, O.; Cusano, F.; Moerchen, M.

    2012-12-15

    Calibration is one of the long-standing problems in optical interferometric measurements, particularly with long baselines which demand stars with angular sizes on the milliarcsecond scale and no detectable companions. While systems of calibrators have been generally established for the near-infrared in the bright source regime (K {approx}< 3 mag), modern large interferometers are sensitive to significantly fainter magnitudes. We aim to provide a list of sources found to be unresolved from direct observations with high angular resolution and dynamic range, which can be used to choose interferometric calibrators. To this purpose, we have used a large number of lunar occultations recorded with the ISAAC instrument at the Very Large Telescope to select sources found to be unresolved and without close companions. An algorithm has been used to determine the limiting angular resolution achieved for each source, taking into account a noise model built from occulted and unocculted portions of the light curves. We have obtained upper limits on the angular sizes of 556 sources, with magnitudes ranging from K{sub s} Almost-Equal-To 4 to 10, with a median of 7.2 mag. The upper limits on possible undetected companions (within Almost-Equal-To 0.''5) range from K{sub s} Almost-Equal-To 8 to 13, with a median of 11.5 mag. One-third of the sources have angular sizes {<=}1 mas, and two-thirds have sizes {<=}2 mas. This list of unresolved sources matches well the capabilities of current large interferometric facilities. We also provide available cross-identifications, magnitudes, spectral types, and other auxiliary information. A fraction of the sources are found to be potentially variable. The list covers parts of the Galactic Bulge and in particular the vicinity of the Galactic Center, where extinction is very significant and traditional lists of calibrators are often insufficient.

  10. EARLY OBSERVATIONS AND ANALYSIS OF THE TYPE Ia SN 2014J IN M82

    SciTech Connect (OSTI)

    Marion, G. H.; Vink, J. [University of Texas at Austin, 1 University Station C1400, Austin, TX 78712-0259 (United States); Sand, D. J. [Physics Department, Texas Tech University, Lubbock, TX 79409 (United States); Hsiao, E. Y. [Carnegie Observatories, Las Campanas Observatory, Colina El Pino, Casilla 601 (Chile); Banerjee, D. P. K.; Joshi, V.; Venkataraman, V.; Ashok, N. M. [Astronomy and Astrophysics Division, Physical Research Laboratory, Navrangapura, Ahmedabad - 380009, Gujarat (India); Valenti, S.; Howell, D. A. [Las Cumbres Observatory Global Telescope Network, 6740 Cortona Drive, Suite 102, Santa Barbara, CA 93117 (United States); Stritzinger, M. D. [Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C (Denmark); Amanullah, R.; Johansson, J. [The Oskar Klein Centre, Physics Department, Stockholm University, Albanova University Center, SE 106 91 Stockholm (Sweden); Binzel, R. P. [Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139 (United States); Bochanski, J. J. [Haverford College, 370 Lancaster Avenue, Haverford, PA 19041 (United States); Bryngelson, G. L. [Department of Physics and Astronomy, Francis Marion University, 4822 East Palmetto Street, Florence, SC 29506 (United States); Burns, C. R. [Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101 (United States); Drozdov, D. [Department of Physics and Astronomy, Clemson University, 8304 University Station, Clemson, SC 29634 (United States); Fieber-Beyer, S. K. [Department of Space Studies, University of North Dakota, University Stop 9008, ND 58202 (United States); Graham, M. L., E-mail: hman@astro.as.utexas.edu [Astronomy Department, University of California at Berkeley, Berkeley, CA 94720 (United States); and others

    2015-01-01

    We present optical and near infrared (NIR) observations of the nearby Type Ia SN 2014J. Seventeen optical and 23 NIR spectra were obtained from 10days before (10d) to 10days after (+10d) the time of maximum B-band brightness. The relative strengths of absorption features and their patterns of development can be compared at one day intervals throughout most of this period. Carbon is not detected in the optical spectra, but we identify C I?1.0693 in the NIR spectra. Mg II lines with high oscillator strengths have higher initial velocities than other Mg II lines. We show that the velocity differences can be explained by differences in optical depths due to oscillator strengths. The spectra of SN 2014J show that it is a normal SN Ia, but many parameters are near the boundaries between normal and high-velocity subclasses. The velocities for O I, Mg II, Si II, S II, Ca II, and Fe II suggest that SN 2014J has a layered structure with little or no mixing. That result is consistent with the delayed detonation explosion models. We also report photometric observations, obtained from 10d to +29d, in the UBVRIJH and K{sub s} bands. The template fitting package SNooPy is used to interpret the light curves and to derive photometric parameters. Using R{sub V} = 1.46, which is consistent with previous studies, SNooPy finds that A{sub V} = 1.80 for E(B V){sub host} = 1.23 0.06 mag. The maximum B-band brightness of 19.19 0.10 mag was reached on February 1.74 UT 0.13days and the supernova has a decline parameter, ?m {sub 15}, of 1.12 0.02 mag.

  11. Possible detection of the stellar donor or remnant for the type Iax supernova 2008ha

    SciTech Connect (OSTI)

    Foley, Ryan J. [Astronomy Department, University of Illinois at Urbana-Champaign, 1002 West Green Street, Urbana, IL 61801 (United States); McCully, Curtis; Jha, Saurabh W. [Department of Physics and Astronomy, Rutgers, The State University of New Jersey, 136 Frelinghuysen Road, Piscataway, NJ 08854 (United States); Bildsten, Lars [Department of Physics, University of California, Santa Barbara, CA 93106 (United States); Fong, Wen-fai [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Narayan, Gautham [National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719-4933 (United States); Rest, Armin [Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States); Stritzinger, Maximilian D. [Department of Physics and Astronomy, Aarhus University, Ny Munkegade, DK-8000 Aarhus C (Denmark)

    2014-09-01

    Type Iax supernovae (SNe Iax) are thermonuclear explosions that are related to SNe Ia, but are physically distinct. The most important differences are that SNe Iax have significantly lower luminosity (1%-50% that of typical SNe Ia), lower ejecta mass (?0.1-0.5 M {sub ?}), and may leave a bound remnant. The most extreme SN Iax is SN 2008ha, which peaked at M{sub V} = 14.2 mag, about 5 mag below that of typical SNe Ia. Here, we present Hubble Space Telescope (HST) images of UGC 12682, the host galaxy of SN 2008ha, taken 4.1 yr after the peak brightness of SN 2008ha. In these deep, high-resolution images, we detect a source coincident (0.86 HST pixels; 0.''043; 1.1?) with the position of SN 2008ha with M {sub F814W} = 5.4 mag. We determine that this source is unlikely to be a chance coincidence, but that scenario cannot be completely ruled out. If this source is directly related to SN 2008ha, it is either the luminous bound remnant of the progenitor white dwarf (WD) or its companion star. The source is consistent with being an evolved >3 M {sub ?} initial mass star, and is significantly redder than the SN Iax 2012Z progenitor system, the first detected progenitor system for a thermonuclear SN. If this source is the companion star for SN 2008ha, there is a diversity in SN Iax progenitor systems, perhaps related to the diversity in SN Iax explosions. If the source is the bound remnant of the WD, it must have expanded significantly. Regardless of the nature of this source, we constrain the progenitor system of SN 2008ha to have an age of <80 Myr.

  12. MAPPING THE INTERSTELLAR MEDIUM WITH NEAR-INFRARED DIFFUSE INTERSTELLAR BANDS

    SciTech Connect (OSTI)

    Zasowski, G.; Mnard, B.; Bizyaev, D.; Garca-Hernndez, D. A.; Prez, A. E. Garca; Majewski, S. R.; Hayden, M. R.; Holtzman, J.; Kinemuchi, K.; Johnson, J. A.; Wilson, J. C.; Nidever, D. L.; Shetrone, M.

    2015-01-01

    We map the distribution and properties of the Milky Way's interstellar medium as traced by diffuse interstellar bands (DIBs) detected in near-infrared stellar spectra from the SDSS-III/APOGEE survey. Focusing exclusively on the strongest DIB in the H band, at ? ? 1.527 ?m, we present a projected map of the DIB absorption field in the Galactic plane, using a set of about 60,000 sightlines that reach up to 15kpc from the Sun and probe up to 30mag of visual extinction. The strength of this DIB is linearly correlated with dust reddening over three orders of magnitude in both DIB equivalent width (W {sub DIB}) and extinction, with a power law index of 1.01 0.01, a mean relationship of W {sub DIB}/A{sub V} = 0.1 Šmag{sup 1} and a dispersion of ?0.05 Šmag{sup 1} at extinctions characteristic of the Galactic midplane. These properties establish this DIB as a powerful, independent probe of dust extinction over a wide range of A{sub V} values. The subset of about 14,000 robustly detected DIB features have a W {sub DIB} distribution that follows an exponential trend. We empirically determine the intrinsic rest wavelength of this transition to be ?{sub 0} = 15 272.42 Š and use it to calculate absolute radial velocities of the carrier, which display the kinematical signature of the rotating Galactic disk. We probe the DIB carrier distribution in three dimensions and show that it can be characterized by an exponential disk model with a scale height of about 100pc and a scale length of about 5kpc. Finally, we show that the DIB distribution also traces large-scale Galactic structures, including the Galactic long bar and the warp of the outer disk.

  13. THE HAWAII INFRARED PARALLAX PROGRAM. I. ULTRACOOL BINARIES AND THE L/T TRANSITION

    SciTech Connect (OSTI)

    Dupuy, Trent J.; Liu, Michael C.

    2012-08-01

    We present the first results from our high-precision infrared (IR) astrometry program at the Canada-France-Hawaii Telescope. We measure parallaxes for 83 ultracool dwarfs (spectral types M6-T9) in 49 systems, with a median uncertainty of 1.1 mas (2.3%) and as good as 0.7 mas (0.8%). We provide the first parallaxes for 48 objects in 29 systems, and for another 27 objects in 17 systems, we significantly improve upon published results, with a median (best) improvement of 1.7 times (5 times). Three systems show astrometric perturbations indicative of orbital motion; two are known binaries (2MASS J0518-2828AB and 2MASS J1404-3159AB) and one is spectrally peculiar (SDSS J0805+4812). In addition, we present here a large set of Keck adaptive optics imaging that more than triples the number of binaries with L6-T5 components that have both multi-band photometry and distances. Our data enable an unprecedented look at the photometric properties of brown dwarfs as they cool through the L/T transition. Going from Almost-Equal-To L8 to Almost-Equal-To T4.5, flux in the Y and J bands increases by Almost-Equal-To 0.7 mag and Almost-Equal-To 0.5 mag, respectively (the Y- and J-band 'bumps'), while flux in the H, K, and L' bands declines monotonically. This wavelength dependence is consistent with cloud clearing over a narrow range of temperature, since condensate opacity is expected to dominate at 1.0-1.3 {mu}m. Interestingly, despite more than doubling the near-IR census of L/T transition objects, we find a conspicuous paucity of objects on the color-magnitude diagram just blueward of the late-L/early-T sequence. This 'L/T gap' occurs at (J - H){sub MKO} 0.1-0.3 mag, (J - K){sub MKO} = 0.0-0.4 mag, and implies that the last phases of cloud evolution occur rapidly. Finally, we provide a comprehensive update to the absolute magnitudes of ultracool dwarfs as a function of spectral type using a combined sample of 314 objects.

  14. THE GALEX TIME DOMAIN SURVEY. I. SELECTION AND CLASSIFICATION OF OVER A THOUSAND ULTRAVIOLET VARIABLE SOURCES

    SciTech Connect (OSTI)

    Gezari, S.; Martin, D. C.; Forster, K.; Neill, J. D.; Morrissey, P.; Wyder, T. K.; Huber, M.; Burgett, W. S.; Chambers, K. C.; Kaiser, N.; Magnier, E. A.; Tonry, J. L.; Heckman, T.; Bianchi, L.; Neff, S. G.; Seibert, M.; Schiminovich, D.; Price, P. A.

    2013-03-20

    We present the selection and classification of over a thousand ultraviolet (UV) variable sources discovered in {approx}40 deg{sup 2} of GALEX Time Domain Survey (TDS) NUV images observed with a cadence of 2 days and a baseline of observations of {approx}3 years. The GALEX TDS fields were designed to be in spatial and temporal coordination with the Pan-STARRS1 Medium Deep Survey, which provides deep optical imaging and simultaneous optical transient detections via image differencing. We characterize the GALEX photometric errors empirically as a function of mean magnitude, and select sources that vary at the 5{sigma} level in at least one epoch. We measure the statistical properties of the UV variability, including the structure function on timescales of days and years. We report classifications for the GALEX TDS sample using a combination of optical host colors and morphology, UV light curve characteristics, and matches to archival X-ray, and spectroscopy catalogs. We classify 62% of the sources as active galaxies (358 quasars and 305 active galactic nuclei), and 10% as variable stars (including 37 RR Lyrae, 53 M dwarf flare stars, and 2 cataclysmic variables). We detect a large-amplitude tail in the UV variability distribution for M-dwarf flare stars and RR Lyrae, reaching up to |{Delta}m| = 4.6 mag and 2.9 mag, respectively. The mean amplitude of the structure function for quasars on year timescales is five times larger than observed at optical wavelengths. The remaining unclassified sources include UV-bright extragalactic transients, two of which have been spectroscopically confirmed to be a young core-collapse supernova and a flare from the tidal disruption of a star by dormant supermassive black hole. We calculate a surface density for variable sources in the UV with NUV < 23 mag and |{Delta}m| > 0.2 mag of {approx}8.0, 7.7, and 1.8 deg{sup -2} for quasars, active galactic nuclei, and RR Lyrae stars, respectively. We also calculate a surface density rate in the UV for transient sources, using the effective survey time at the cadence appropriate to each class, of {approx}15 and 52 deg{sup -2} yr{sup -1} for M dwarfs and extragalactic transients, respectively.

  15. S A N D I A T E C H N O L O G Y A Q UA RT E R LY R E S E A R

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

    Summer in Antarctica Ice in nanoseconds SUMMER 2007 S A N D I A T E C H N O L O G Y A Q UA RT E R LY R E S E A R C H & D E V E LO P M E N T MAG A Z I N E - VO LUM E 9 , N O. 2 Drought dilemmas Sandia Technology (ISSN: 1547-5190) is a quarterly magazine published by Sandia National Laboratories. Sandia is a mul- tiprogram engineering and science laboratory operated by Sandia Corporation, a Lockheed Martin company, for the U.S. Department of Energy. With main facilities in Albuquerque, New

  16. S A N D I A T E C H N O L O G Y A Q UA RT E R LY R E S E A R

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

    Closer to fusion Biofuels on tap FALL 2007 S A N D I A T E C H N O L O G Y A Q UA RT E R LY R E S E A R C H & D E V E LO P M E N T MAG A Z I N E - VO LUM E 9 , N O. 3 Simulation: Making engineers better Sandia Technology (ISSN: 1547-5190) is a quarterly maga- zine published by Sandia National Laboratories. Sandia is a multiprogram engineering and science laboratory operated by Sandia Corporation, a Lockheed Martin company, for the U.S. Department of Energy. With main facilities in

  17. Assessing

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

    dental disease in minutes Understanding climate change Keeping watch on the world SPRING 2007 S A N D I A T E C H N O L O G Y A Q UA RT E R LY R E S E A R C H & D E V E LO P M E N T MAG A Z I N E - VO LUM E 9 , N O. 1 Sandia Technology (ISSN: 1547-5190) is a quarterly maga- zine published by Sandia National Laboratories. Sandia is a multiprogram engineering and science laboratory operated by Sandia Corporation, a Lockheed Martin company, for the Department of Energy. With main facilities in

  18. MEASURING MICROLENSING USING SPECTRA OF MULTIPLY LENSED QUASARS

    SciTech Connect (OSTI)

    Motta, V.; Mediavilla, E.; Munoz, J. A. E-mail: emg@iac.es E-mail: jmunoz@uv.es

    2012-08-10

    We report on a program of spectroscopic observations of gravitationally lensed QSOs with multiple images. We seek to establish whether microlensing is occurring in each QSO image using only single-epoch observations. We calculate flux ratios for the cores of emission lines in image pairs to set a baseline for no microlensing. The offset of the continuum flux ratios relative to this baseline yields the microlensing magnification free from extinction, as extinction affects the continuum and the lines equally. When we find chromatic microlensing, we attempt to constrain the size of the QSO accretion disk. SDSSJ1004+4112 and HE1104-1805 show chromatic microlensing with amplitudes 0.2 < |{Delta}m| < 0.6 and 0.2 < |{Delta}m| < 0.4 mag, respectively. Modeling the accretion disk with a Gaussian source (I{proportional_to}exp (- R{sup 2}/2r{sup 2}{sub s})) of size r{sub s} {proportional_to}{lambda}{sup p} and using magnification maps to simulate microlensing, we find r{sub s} ({lambda}3363) = 7 {+-} 3 lt-day(18.1 {+-} 7.8 Multiplication-Sign 10{sup 15} cm) and p = 1.1 {+-} 0.4 for SDSS1004+4112, and r{sub s} ({lambda}3363) = 6 {+-} 2 lt-day(15.5 {+-} 5.2 Multiplication-Sign 10{sup 15} cm) and p = 0.7 {+-} 0.1 for HE1104-1805. For SDSSJ1029+2623, we find strong chromaticity of {approx}0.4 mag in the continuum flux ratio, which probably arises from microlensing, although not all the available data fit within this explanation. For Q0957+561, we measure B - A magnitude differences of 0.4 mag, much greater than the {approx}0.05 mag amplitude usually inferred from light-curve variability. It may substantially modify the current interpretations of microlensing in this system, likely favoring the hypothesis of smaller sources and/or larger microdeflectors. For HS0818+1227, our data yield possible evidence of microlensing.

  19. Slide 1

    Office of Environmental Management (EM)

    Tritium on Z: The challenges and possibilities for MagLIF D. C. Rovang, M. E. Cuneo, R. D. McBride, B. M. Jones, J. L. McKenney, H. C. Peebles, D. C. Spencer, K. N. Austin, D. B. Sinars, and G. A. Rochau Tritium Focus Group Meeting Los Alamos National Laboratory, Nov. 3- 5, 2015 Sandia National Laboratories SAND2015-9392 PE The Z facility combines the MJ-class Z pulsed-power accelerator with the TW-class Z Beamlet Laser (ZBL) Up to 22 MJ stored 15% coupling to load 1-3 MJ delivered to load

  20. HIGHLY VARIABLE OBJECTS IN THE PALOMAR-QUEST SURVEY: A BLAZAR SEARCH USING

    Office of Scientific and Technical Information (OSTI)

    OPTICAL VARIABILITY (Journal Article) | SciTech Connect HIGHLY VARIABLE OBJECTS IN THE PALOMAR-QUEST SURVEY: A BLAZAR SEARCH USING OPTICAL VARIABILITY Citation Details In-Document Search Title: HIGHLY VARIABLE OBJECTS IN THE PALOMAR-QUEST SURVEY: A BLAZAR SEARCH USING OPTICAL VARIABILITY We identify 3113 highly variable objects in 7200 deg{sup 2} of the Palomar-QUEST (PQ) Survey, which each varied by more than 0.4 mag simultaneously in two broadband optical filters on timescales from hours

  1. THE BROWN DWARF KINEMATICS PROJECT (BDKP). III. PARALLAXES FOR 70 ULTRACOOL DWARFS

    SciTech Connect (OSTI)

    Faherty, Jacqueline K.; Shara, Michael M.; Cruz, Kelle L.; Burgasser, Adam J.; Walter, Frederick M.; Van der Bliek, Nicole; Vrba, Frederick J.; Anglada-Escude, Guillem

    2012-06-10

    We report parallax measurements for 70 ultracool dwarfs (UCDs) including 11 late-M, 32 L, and 27 T dwarfs. In this sample, 14 M and L dwarfs exhibit low surface gravity features, 6 are close binary systems, and 2 are metal-poor subdwarfs. We combined our new measurements with 114 previously published UCD parallaxes and optical-mid-IR photometry to examine trends in spectral-type/absolute magnitude, and color-color diagrams. We report new polynomial relations between spectral type and M{sub JHK}. Including resolved L/T transition binaries in the relations, we find no reason to differentiate between a 'bright' (unresolved binary) and a 'faint' (single source) sample across the L/T boundary. Isolating early T dwarfs, we find that the brightening of T0-T4 sources is prominent in M{sub J} where there is a [1.2-1.4] mag difference. A similar yet dampened brightening of [0.3-0.5] mag happens at M{sub H} and a plateau or dimming of [-0.2 to -0.3] mag is seen in M{sub K} . Comparison with evolutionary models that vary gravity, metallicity, and cloud thickness verifies that for L into T dwarfs, decreasing cloud thickness reproduces brown dwarf near-IR color-magnitude diagrams. However we find that a near constant temperature of 1200 {+-}100 K along a narrow spectral subtype of T0-T4 is required to account for the brightening and color-magnitude diagram of the L-dwarf/T-dwarf transition. There is a significant population of both L and T dwarfs which are red or potentially 'ultra-cloudy' compared to the models, many of which are known to be young indicating a correlation between enhanced photospheric dust and youth. For the low surface gravity or young companion L dwarfs we find that 8 out of 10 are at least [0.2-1.0] mag underluminous in M{sub JH} and/or M{sub K} compared to equivalent spectral type objects. We speculate that this is a consequence of increased dust opacity and conclude that low surface gravity L dwarfs require a completely new spectral-type/absolute magnitude polynomial for analysis.

  2. DISCOVERY AND CHARACTERIZATION OF AN EXTREMELY DEEP-ECLIPSING CATACLYSMIC

    Office of Scientific and Technical Information (OSTI)

    VARIABLE: LSQ172554.8-643839 (Journal Article) | SciTech Connect DISCOVERY AND CHARACTERIZATION OF AN EXTREMELY DEEP-ECLIPSING CATACLYSMIC VARIABLE: LSQ172554.8-643839 Citation Details In-Document Search Title: DISCOVERY AND CHARACTERIZATION OF AN EXTREMELY DEEP-ECLIPSING CATACLYSMIC VARIABLE: LSQ172554.8-643839 We report the discovery of an eclipsing cataclysmic variable with eclipse depths >5.7 mag, orbital period 94.657 minutes, and peak brightness V {approx} 18 at J2000 position

  3. Exploring magnetized liner inertial fusion with a semi-analytic model

    Office of Scientific and Technical Information (OSTI)

    (Journal Article) | DOE PAGES Exploring magnetized liner inertial fusion with a semi-analytic model This content will become publicly available on January 13, 2017 « Prev Next » Title: Exploring magnetized liner inertial fusion with a semi-analytic model In this study, we explore magnetized liner inertial fusion (MagLIF) [S. A. Slutz et al., Phys. Plasmas 17, 056303 (2010)] using a semi-analytic model [R. D. McBride and S. A. Slutz, Phys. Plasmas 22, 052708 (2015)]. Specifically, we

  4. A first site of galaxy cluster formation: complete spectroscopy of a

    Office of Scientific and Technical Information (OSTI)

    protocluster at z = 6.01 (Journal Article) | SciTech Connect A first site of galaxy cluster formation: complete spectroscopy of a protocluster at z = 6.01 Citation Details In-Document Search Title: A first site of galaxy cluster formation: complete spectroscopy of a protocluster at z = 6.01 We performed a systematic spectroscopic observation of a protocluster at z = 6.01 in the Subaru Deep Field. We took spectroscopy for all 53 i' dropout galaxies down to z' = 27.09 mag in/around the

  5. Laboratory snags five R&D 100 awards

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

    R&D 100 awards Laboratory snags five R&D 100 awards Winning Laboratory projects are MagViz, the SIMTECHE CO2 Capture Process, Lasonix, TeraOps Software Radio, and the Artificial Retina Project. July 21, 2009 Los Alamos National Laboratory sits on top of a once-remote mesa in northern New Mexico with the Jemez mountains as a backdrop to research and innovation covering multi-disciplines from bioscience, sustainable energy sources, to plasma physics and new materials. Los Alamos National

  6. DWARF IRREGULAR GALAXY LEO A: SUPRIME-CAM WIDE-FIELD STELLAR PHOTOMETRY

    SciTech Connect (OSTI)

    Stonkut?, Rima; Narbutis, Donatas; Vansevi?ius, Vladas; Arimoto, Nobuo; Hasegawa, Takashi; Tamura, Naoyuki

    2014-10-01

    We have surveyed a complete extent of Leo Aan apparently isolated gas-rich low-mass dwarf irregular galaxy in the Local Group. The B, V, and I passband CCD images (typical seeing ?0.''8) were obtained with the Subaru Telescope equipped with the Suprime-Cam mosaic camera. The wide-field (20' 24') photometry catalog of 38,856 objects (V ? 16-26 mag) is presented. This survey is also intended to serve as ''a finding chart'' for future imaging and spectroscopic observation programs of Leo A.

  7. Carlsbad Field Office P. O. Box 3090 Carlsbad, New Mexico 88221

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

    MAG:13-1804:UFC 1410.00 Department of Energy Carlsbad Field Office P. O. Box 3090 Carlsbad, New Mexico 88221 May 7, 2013 Distribution Subject: Revised WIPP Tour Policy Visits to the U.S. Department of Energy's (DOE) Waste Isolation Pilot Plant (WIPP), which are highly valued by key decision-makers and centers of influence, directly benefit the mission and future of the WIPP project. For two decades, the WIPP tour program has been a vital component of community, state, national, and international

  8. Prospects for x-ray polarimetry measurements of magnetic fields in magnetized liner inertial fusion plasmas

    SciTech Connect (OSTI)

    Lynn, Alan G. Gilmore, Mark

    2014-11-15

    Magnetized Liner Inertial Fusion (MagLIF) experiments, where a metal liner is imploded to compress a magnetized seed plasma may generate peak magnetic fields ?10{sup 4} T (100 Megagauss) over small volumes (?10{sup ?10}m{sup 3}) at high plasma densities (?10{sup 28}m{sup ?3}) on 100 ns time scales. Such conditions are extremely challenging to diagnose. We discuss the possibility of, and issues involved in, using polarimetry techniques at x-ray wavelengths to measure magnetic fields under these extreme conditions.

  9. Los Alamos, New Mexico, July 21, 2009- Los Alamos National Laboratory scientists

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

    snags five R&D 100 awards July 21, 2009 "Oscars of Invention" recognize greatest innovations of 2009 Los Alamos, New Mexico, July 21, 2009- Los Alamos National Laboratory scientists won five of R&D Magazine's 2009 R&D 100 Awards. Recognized as the "Oscars of Invention" by the Chicago Tribune, these awards honor the top 100 proven technological advances of the past year. Winning Laboratory projects are MagViz, the SIMTECHE CO2 Capture Process, Lasonix, TeraOps

  10. Microsoft Word - Transmittal of Final Audit Report A-13-02, SRS-CCP.doc

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

    DSM:MAG:13-1490:UFC 2300.00 Department of Energy Carlsbad Field Office P.O. Box 3090 Carlsbad, New Mexico 88221 August 6, 2013 Mr. John E. Kieling, Chief Hazardous Waste Bureau New Mexico Environment Department 2905 Rodeo Park Drive East, Building 1 Santa Fe, New Mexico 87505 Subject: Transmittal of the Final Audit Report for Recertification Audit A-13-02, SRS/CCP Dear Mr. Kieling: This letter transmits the Final Audit Report for Carlsbad Field Office (CBFO) Recertification Audit A-13-02 of the

  11. Mr. James Bearzi, Chief Hazardous Waste Bureau

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

    8, 2010 New Mexico Environment Department 2905 E. Rodeo Park Dr. Bldg . 1 Santa Fe, New Mexico 87505-6303 Subject: Certification by a New Mexico Registered Professional Engineer in Support of TRUPACT-III References: United States Department Of Energy letter CBFO:OESH :GTB:MAG:11- 0702:UFC 5487.00 from Edward Ziemianski and M. F. Sharif to James Bearzi, dated January 10, 2011, subject: Notification of Planned Change to the Permitted Facility to Support TRUPACT-III United States Department Of

  12. Microsoft Word - 11-0656 _signature on file_.docx

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

    RU:MAG:11-0656:UFC 2300.00 Department of Energy Carlsbad Field Office P. O. Box 3090 Carlsbad, New Mexico 88221 August 17, 2011 Mr. John Kieling, Acting Chief Hazardous Waste Bureau New Mexico Environment Department 2905 Rodeo Park Drive East, Building 1 Santa Fe, New Mexico 87505-6303 Subject: Transmittal of the Final Audit Report for CBFO Audit A-11-13 of the INL/CCP Analytical Laboratories Dear Mr. Kieling: This letter transmits the Final Audit Report for Audit A-11-13 of the processes

  13. TO: FILE

    Office of Legacy Management (LM)

    FKW ~&%&k---- MEMORANDUM \ ' 5/3b i DATE--- __ --L+------- I . : ' I CITY: Caeasvl ~----------------_________ STATE: C-T -* *is- a' s h-2 Mag,~s;uun 3 hY;S iO* Of WNER~X IJE-LCOj Past:------__________________ Curre"t: ~~~~~~~~~----------_---~-- Owner contacted q yes ~$.a; if yes, date contacted ! IYPLOE-OPER!xION 9 Research & Development q Production scale testing I? Pilot Scale Bench Scale Process 0 Theoretical Studies 0 Sample & Analysis q Production Cl Disposal/Storage a

  14. SECTION M_Evaluation Factors

    National Nuclear Security Administration (NNSA)

    TABLE OF CONTENTS M-1 EVALUATION OF PROPOSALS......................................................................176 M-2 BASIS FOR CONTRACT AWARD...................................................................177 M-3 TECHNICAL AND MANAGEMENT CRITERIA..........................................177 M-4 COST CRITERION.............................................................................................179 Section M, Page 176 M-1 EVALUATION OF PROPOSALS (a) This acquisition will be

  15. FOUR NEW T DWARFS IDENTIFIED IN Pan-STARRS 1 COMMISSIONING DATA

    SciTech Connect (OSTI)

    Deacon, Niall R.; Liu, Michael C.; Magnier, Eugene A.; Bowler, Brendan P.; Burgett, W. S.; Chambers, K. C.; Flewelling, H.; Kaiser, N.; Morgan, J. S.; Sweeney, W. E.; Tonry, J. L.; Wainscoat, R. J.; Waters, C.; Goldman, Bertrand; Redstone, Joshua A.; Lupton, R. H.; Price, P. A.

    2011-09-15

    A complete well-defined sample of ultracool dwarfs is one of the key science programs of the Pan-STARRS 1 optical survey telescope (PS1). Here we combine PS1 commissioning data with the Two Micron All Sky Survey (2MASS) to conduct a proper motion search (0.''1-2.''0 yr{sup -1}) for nearby T dwarfs, using optical+near-IR colors to select objects for spectroscopic follow-up. The addition of sensitive far-red optical imaging from PS1 enables discovery of nearby ultracool dwarfs that cannot be identified from 2MASS data alone. We have searched 3700 deg{sup 2} of PS1 y-band (0.95-1.03 {mu}m) data to y {approx} 19.5 mag (AB) and J {approx} 16.5 mag (Vega) and discovered four previously unknown bright T dwarfs. Three of the objects (with spectral types T1.5, T2, and T3.5) have photometric distances within 25 pc and were missed by previous 2MASS searches due to more restrictive color selection criteria. The fourth object (spectral type T4.5) is more distant than 25 pc and is only a single-band detection in 2MASS. We also examine the potential for completing the census of nearby ultracool objects with the PS1 3{pi} survey.

  16. THE 2001-2003 LOW STATE OF NOVA LACERTAE 1950 (DK LAC)

    SciTech Connect (OSTI)

    Honeycutt, R. K.; Jacobson, H.; Hoffman, D.; Maxwell, T.; Croxall, K.; Kafka, S.; Henden, A. A.; Robertson, J. W. E-mail: jacob189@msu.edu E-mail: tmaxwell@astro.indiana.edu E-mail: skafka@dtm.ciw.edu E-mail: Jeff.Robertson@atu.edu

    2011-04-15

    We report on extensive photometry of DK Lac obtained during the interval 1990-2009, which includes a 2 mag low state during 2001-2003. Much of the photometry consists of exposures obtained with a typical spacing of several days, but also includes 26 sequences of continuous photometry each lasting 2-7 hr. We find no evidence for periodicities in our data. We do find that the random variations in the low state are approximately twice those in the high state, when expressed in magnitudes. The lack of orbital-timescale variations is attributed to the nearly face-on presentation of the disk. There is a 0.2 mag decline in the high-state brightness of the system over 19 years, which is consistent with the behavior of other old novae in the decades following outburst. High-state spectra are also presented and discussed. We find that the equivalent width of H{alpha} falls by about double from 1991 to 2008. The photometric properties are discussed in the context of the hibernation scenario for the behavior of novae between outbursts, in which we conclude that low states in old novae are probably unrelated to their possible entrance into hibernation.

  17. THE SIZE DISTRIBUTION OF THE NEPTUNE TROJANS AND THE MISSING INTERMEDIATE-SIZED PLANETESIMALS

    SciTech Connect (OSTI)

    Sheppard, Scott S.; Trujillo, Chadwick A.

    2010-11-10

    We present an ultra-deep survey for Neptune Trojans using the Subaru 8.2 m and Magellan 6.5 m telescopes. The survey reached a 50% detection efficiency in the R band at m{sub R} = 25.7 mag and covered 49 deg{sup 2} of sky. m{sub R} = 25.7 mag corresponds to Neptune Trojans that are about 16 km in radius (assuming an albedo of 0.05). A paucity of smaller Neptune Trojans (radii < 45 km) compared with larger ones was found. The brightest Neptune Trojans appear to follow a steep power-law slope (q = 5 {+-} 1) similar to the brightest objects in the other known stable reservoirs such as the Kuiper Belt, Jupiter Trojans, and main belt asteroids. We find a roll-over for the Neptune Trojans that occurs around a radius of r = 45 {+-} 10 km (m{sub R} = 23.5 {+-} 0.3), which is also very similar to the other stable reservoirs. All the observed stable regions in the solar system show evidence for Missing Intermediate-Sized Planetesimals (MISPs). This indicates a primordial and not collisional origin, which suggests that planetesimal formation proceeded directly from small to large objects. The scarcity of intermediate- and smaller-sized Neptune Trojans may limit them as being a strong source for the short period comets.

  18. The 1991-2012 light curve of the old nova HR Lyrae

    SciTech Connect (OSTI)

    Honeycutt, R. K.; Shears, J.; Kafka, S.; Robertson, J. W.; Henden, A. A. E-mail: bunburyobservatory@hotmail.com E-mail: Jeff.Robertson@atu.edu

    2014-05-01

    The 22 yr light curve of HR Lyr, acquired with a typical cadence of 2-6 days, is examined for periodic and quasi-periodic variations. No persistent periodicities are revealed. Rather, the light curve variations often take the form of nearly linear rises and falls having typical e-folding times of about 100 days. Occasional ?0.6 mag outbursts are also seen, with properties similar to those of small outbursts found in some nova-like cataclysmic variables. When the photometry is formed into yearly averages, a decline of 0.012 0.005 mag yr{sup 1} is apparent, consistent with the fading of irradiation-induced M-dot following the nova. The equivalent width of H? is tabulated at three epochs over the interval 1986-2008 in order to compare with a recent result for DK Lac in which H? was found to be fading 50 yr after the nova. However, our results for such a fading in HR Lyr are inconclusive.

  19. Optical and ultraviolet observations of the narrow-lined type Ia SN 2012fr in NGC 1365

    SciTech Connect (OSTI)

    Zhang, Ju-Jia; Bai, Jin-Ming; Wang, Bo; Liu, Zheng-Wei [Yunnan Observatories (YNAO), Chinese Academy of Sciences, Kunming 650011 (China); Wang, Xiao-Feng; Zhao, Xu-Lin; Chen, Jun-Cheng [Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing 100084 (China); Zhang, Tian-Meng, E-mail: jujia@ynao.ac.cn, E-mail: baijinming@ynao.ac.cn, E-mail: wang_xf@mail.tsinghua.edu.cn [National Astronomical Observatories of China (NAOC), Chinese Academy of Sciences, Beijing 100012 (China)

    2014-07-01

    Extensive optical and ultraviolet (UV) observations of the type Ia supernova (SN Ia) 2012fr are presented in this paper. It has a relatively high luminosity, with an absolute B-band peak magnitude of about 19.5 mag and a smaller post-maximum decline rate than normal SNe Ia (e.g., ?m {sub 15}(B) =0.85 0.05 mag). Based on the UV and optical light curves, we derived that a {sup 56}Ni mass of about 0.88 M {sub ?} was synthesized in the explosion. The earlier spectra are characterized by noticeable high-velocity features of Si II ?6355 and Ca II with velocities in the range of ?22, 000-25, 000 km s{sup 1}. At around the maximum light, these spectral features are dominated by the photospheric components which are noticeably narrower than normal SNe Ia. The post-maximum velocity of the photosphere remains almost constant at ?12,000 km s{sup 1} for about one month, reminiscent of the behavior of some luminous SNe Ia like SN 1991T. We propose that SN 2012fr may represent a subset of the SN 1991T-like SNe Ia viewed in a direction with a clumpy or shell-like structure of ejecta, in terms of a significant level of polarization reported in Maund et al. in 2013.

  20. Modeling transiting circumstellar disks: characterizing the newly discovered eclipsing disk system OGLE LMC-ECL-11893

    SciTech Connect (OSTI)

    Scott, Erin L.; Mamajek, Eric E.; Pecaut, Mark J.; Quillen, Alice C.; Moolekamp, Fred; Bell, Cameron P. M.

    2014-12-10

    We investigate the nature of the unusual eclipsing star OGLE LMC-ECL-11893 (OGLE J05172127-6900558) in the Large Magellanic Cloud recently reported by Dong et al. The eclipse period for this star is 468 days, and the eclipses exhibit a minimum of ?1.4 mag, preceded by a plateau of ?0.8 mag. Spectra and optical/IR photometry are consistent with the eclipsed star being a lightly reddened B9III star of inferred age ?150 Myr and mass ?4 M {sub ?}. The disk appears to have an outer radius of ?0.2 AU with predicted temperatures of ?1100-1400 K. We model the eclipses as being due to either a transiting geometrically thin dust disk or gaseous accretion disk around a secondary object; the debris disk produces a better fit. We speculate on the origin of such a dense circumstellar dust disk structure orbiting a relatively old low-mass companion, and on the similarities of this system to the previously discovered EE Cep.

  1. AN ACCURATE NEW METHOD OF CALCULATING ABSOLUTE MAGNITUDES AND K-CORRECTIONS APPLIED TO THE SLOAN FILTER SET

    SciTech Connect (OSTI)

    Beare, Richard; Brown, Michael J. I.; Pimbblet, Kevin

    2014-12-20

    We describe an accurate new method for determining absolute magnitudes, and hence also K-corrections, that is simpler than most previous methods, being based on a quadratic function of just one suitably chosen observed color. The method relies on the extensive and accurate new set of 129 empirical galaxy template spectral energy distributions from Brown et al. A key advantage of our method is that we can reliably estimate random errors in computed absolute magnitudes due to galaxy diversity, photometric error and redshift error. We derive K-corrections for the five Sloan Digital Sky Survey filters and provide parameter tables for use by the astronomical community. Using the New York Value-Added Galaxy Catalog, we compare our K-corrections with those from kcorrect. Our K-corrections produce absolute magnitudes that are generally in good agreement with kcorrect. Absolute griz magnitudes differ by less than 0.02 mag and those in the u band by ?0.04 mag. The evolution of rest-frame colors as a function of redshift is better behaved using our method, with relatively few galaxies being assigned anomalously red colors and a tight red sequence being observed across the whole 0.0 < z < 0.5 redshift range.

  2. Simulations of the OzDES AGN reverberation mapping project

    SciTech Connect (OSTI)

    King, Anthea L.; Martini, Paul; Davis, Tamara M.; Denney, K. D.; Kochanek, C. S.; Peterson, Bradley M.; Skielboe, Andreas; Vestergaard, Marianne; Huff, Eric; Watson, Darach; Banerji, Manda; McMahon, Richard; Sharp, Rob; Lidman, C.

    2015-08-26

    As part of the Australian spectroscopic dark energy survey (OzDES) we are carrying out a large-scale reverberation mapping study of ~500 quasars over five years in the 30 deg2 area of the Dark Energy Survey (DES) supernova fields. These quasars have redshifts ranging up to 4 and have apparent AB magnitudes between 16.8 mag < r < 22.5 mag. The aim of the survey is to measure time lags between fluctuations in the quasar continuum and broad emission-line fluxes of individual objects in order to measure black hole masses for a broad range of active galactic nuclei (AGN) and constrain the radiusluminosity (RL) relationship. Here we investigate the expected efficiency of the OzDES reverberation mapping campaign and its possible extensions. We expect to recover lags for ~3545 % of the quasars. AGN with shorter lags and greater variability are more likely to yield a lag measurement, and objects with lags ?6 months or ~1 yr are expected to be recovered the most accurately. The baseline OzDES reverberation mapping campaign is predicted to produce an unbiased measurement of the RL relationship parameters for H?, MgII?2798, and C IV?1549. As a result, extending the baseline survey by either increasing the spectroscopic cadence, extending the survey season, or improving the emission-line flux measurement accuracy will significantly improve the RL parameter constraints for all broad emission lines.

  3. Los Alamos Shows Airport Security Technology at Work

    ScienceCinema (OSTI)

    Espy, Michelle; Schultz, Larry; Hunter, James

    2014-06-24

    Los Alamos scientists have advanced a Magnetic Resonance Imaging (MRI) technology that may provide a breakthrough for screening liquids at airport security. They've added low-power X-ray data to the mix, and as a result have unlocked a new detection technology. Funded in part by the Department of Homeland Security's Science and Technology Directorate, the new system is named MagRay. The goal is to quickly and accurately distinguish between liquids that visually appear identical. For example, what appears to be a bottle of white wine could potentially be nitromethane, a liquid that could be used to make an explosive. Both are clear liquids, one would be perfectly safe on a commercial aircraft, the other would be strictly prohibited. How to tell them apart quickly without error at an airport security area is the focus of Michelle Espy, Larry Schultz and their team. In this video, Espy and the MagRay team explain how the new technology works, how they've developed an easy operator interface, and what the next steps might be in transitioning this technology to the private sector.

  4. Fine structure of the magnetic-dipole-strength distribution in {sup 208}Pb

    SciTech Connect (OSTI)

    Shizuma, T.; Kikuzawa, N.; Hayakawa, T.; Ohgaki, H.; Toyokawa, H.; Komatsubara, T.; Tamii, A.; Nakada, H.

    2008-12-15

    Spin-flip M1 strengths in {sup 208}Pb have been measured in photon scattering experiments with a quasi-monochromatic, linearly polarized photon beam. The data resolve an M1 giant resonance into at least seven, possibly eight, discrete transitions at excitation energies between 7.1 and 7.4 MeV below the neutron separation energy. The M1 strengths are measured with uncertainties considerably smaller than those in a previous study, which leads to a reexamination of the total strength. Experimental results are compared with an estimation of self-consistent random phase approximation using a semirealistic interaction.

  5. Methods and energy storage devices utilizing electrolytes having surface-smoothing additives

    DOE Patents [OSTI]

    Xu, Wu; Zhang, Jiguang; Graff, Gordon L; Chen, Xilin; Ding, Fei

    2015-11-12

    Electrodeposition and energy storage devices utilizing an electrolyte having a surface-smoothing additive can result in self-healing, instead of self-amplification, of initial protuberant tips that give rise to roughness and/or dendrite formation on the substrate and anode surface. For electrodeposition of a first metal (M1) on a substrate or anode from one or more cations of M1 in an electrolyte solution, the electrolyte solution is characterized by a surface-smoothing additive containing cations of a second metal (M2), wherein cations of M2 have an effective electrochemical reduction potential in the solution lower than that of the cations of M1.

  6. PHYSICAL PROPERTIES OF SPECTROSCOPICALLY CONFIRMED GALAXIES AT z {>=} 6. II. MORPHOLOGY OF THE REST-FRAME UV CONTINUUM AND Ly{alpha} EMISSION

    SciTech Connect (OSTI)

    Jiang Linhua; Windhorst, Rogier A.; Cohen, Seth H.; Mechtley, Matthew; Egami, Eiichi; Fan Xiaohui; Dave, Romeel; Finlator, Kristian; Kashikawa, Nobunari; Ouchi, Masami; Shimasaku, Kazuhiro

    2013-08-20

    We present a detailed structural and morphological study of a large sample of spectroscopically confirmed galaxies at z {>=} 6 using deep Hubble Space Telescope (HST) near-IR broad-band images and Subaru Telescope optical narrow-band images. The galaxy sample consists of 51 Ly{alpha} emitters (LAEs) at z {approx_equal} 5.7, 6.5, and 7.0, and 16 Lyman break galaxies (LBGs) at 5.9 {<=} z {<=} 6.5. These galaxies exhibit a wide range of rest-frame UV continuum morphology in the HST images, from compact features to multiple component systems. The fraction of merging/interacting galaxies reaches 40%-50% at the brightest end of M{sub 1500} {<=} -20.5 mag. The intrinsic half-light radii r{sub hl,in}, after correcting for point-spread function (PSF) broadening, are roughly between r{sub hl,in} {approx_equal} 0.''05 (0.3 kpc) and 0.''3 (1.7 kpc) at M{sub 1500} {<=} -19.5 mag. The median r{sub hl,in} value is 0.''16 ({approx}0.9 kpc). This is consistent with the sizes of bright LAEs and LBGs at z {>=} 6 found in previous studies. In addition, more luminous galaxies tend to be larger and exhibit a weak size-luminosity relation, r{sub hl,in}{proportional_to}L {sup 0.14} at M{sub 1500} {<=} -19.5 mag. The slope of 0.14 is significantly flatter than those in fainter LBG samples. We discuss the morphology of z {>=} 6 galaxies with nonparametric methods, including the concentration, asymmetry, and smoothness system and the Gini and M{sub 20} parameters, and demonstrate their validity through simulations. We search for extended Ly{alpha} emission halos around LAEs at z {approx_equal} 5.7 and 6.5 by stacking a number of narrow-band images. We do not find evidence of extended Ly{alpha} halos predicted by cosmological simulations. Such halos, if they exist, could be weaker than predicted. Finally, we investigate positional misalignment between the UV continuum and Ly{alpha} emissions in LAEs. While the two positions are generally consistent, several merging galaxies show significant positional differences. This is likely caused by a disturbed interstellar medium distribution due to merging activity.

  7. Towards tailoring the magnetocaloric response in FeRh-based ternary compounds

    SciTech Connect (OSTI)

    Barua, Radhika Jiménez-Villacorta, Félix; Lewis, L. H.

    2014-05-07

    In this work, we demonstrate that the magnetocaloric response of FeRh-based compounds may be tailored for potential magnetic refrigeration applications by chemical modification of the FeRh lattice. Alloys of composition Fe(Rh{sub 1−x}A{sub x}) or (Fe{sub 1−x}B{sub x})Rh (A = Cu, Pd; B = Ni; 0 < x < 0.06) were synthesized via arc-melting and subsequent annealing in vacuum at 1000 °C for 48 h. The magnetocaloric properties of the FeRh-based systems were determined using isothermal M(H) curves measured in the vicinity of the magnetostructural temperature (T{sub t}). It is found that the FeRh working temperature range (δT{sub FWHM}) may be chemically tuned over a wide temperature range, 100 K ≤ T ≤ 400 K. While elemental substitution consistently decreases the magnetic entropy change (ΔS{sub mag}) of the FeRh-based ternary alloys from that of the parent FeRh compound (ΔS{sub mag},{sub FeRh} ∼ 17 J/kg K; ΔS{sub mag,FeRh-ternary =} 7–14 J/kg K at H{sub app} = 2 T), the net refrigeration capacity (RC), defined as the amount of heat that can be transferred during one magnetic refrigeration cycle, of the modified systems is significantly higher (RC{sub FeRh} ∼ 150 J/kg; RC{sub FeRh-ternary =} 170–210 J/kg at H{sub app} = 2 T). These results are attributed to stoichiometry-induced changes in the FeRh electronic band structure and beneficial broadening of the magnetostructural transition due to local chemical disorder.

  8. Gander Energy | Open Energy Information

    Open Energy Info (EERE)

    Gander Energy Jump to: navigation, search Name: Gander Energy Place: Ontario, Canada Zip: M1R 2T6 Sector: Solar Product: Ontario based solar power project developer. References:...

  9. SHEAR ALFV

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

    ... . . . . . . 7 1.2 Coupling of poloidal harmonics to form TAE gap . . . . . . . . . . . . ... Figure 1.3 Cartoon showing the m and m + 1 poloidal harmonics coupled together to produce ...

  10. Agenda: Energy Infrastructure Finance | Department of Energy

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

    Sullivan, CEODirector of Investments, Grand River Dam Authority * Humayun Tai, Director, McKinsey Company * Steven J. Zucchet, SVP, Borealis Infrastructure 12:00 p.m. - 1:00 p.m. ...

  11. Search for: All records | DOE PAGES

    Office of Scientific and Technical Information (OSTI)

    Young -Min (1) Kinane, Christy J. (1) Kursumovic, Ahmed (1) Langridge, Sean (1) Lee, Jun -Sik (1) MacLaren, Ian (1) MacManus-Driscoll, Judith L. (1) Ramasse, Quentin M. (1)...

  12. Spin wave eigenmodes in single and coupled sub-150 nm rectangular...

    Office of Scientific and Technical Information (OSTI)

    ...anni.carlotti@fisica.unipg.it ; Madami, M. 1 ; Tacchi, S. 2 ; Gubbiotti, G. ; Dey, H. ; Csaba, G. ; Porod, W. 3 + Show Author Affiliations Dipartimento di Fisica e Geologia, ...

  13. Search for: All records | SciTech Connect

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    ... Testing Center, Casper, WY (United States) S. M. Stoller (United States) SLAC National ... Asara, John M (1) Begley, Michael J. (1) Cantley, Lewis C. (1) Coyle, Anthony J. (1) Eck, ...

  14. Microsoft Word - Armenian Cookbook.doc

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    January 24, 2013 Chez Leon 10:30 a.m - 1 p.m. Pauline Berberian, organizer and recipe source, assisted by Susan Kayser, Rose Moore and Mady Newfield 1 Appetizers and Salads...

  15. February 2013 pRad RMI experiments (Conference) | SciTech Connect

    Office of Scientific and Technical Information (OSTI)

    the National Technical Information Service, Springfield, VA at www.ntis.gov. Authors: Oro, David M. 1 ; Buttler, William T. 1 ; Cherne, Frank J. 1 ; Mariam, Fesseha G. 1...

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    Office of Scientific and Technical Information (OSTI)

    Roberts, Justin M. (1) Souza, Amanda (1) Winter, Georg E. (1) Save Results Save this search to My Library Excel (limit 2000) CSV (limit 5000) XML (limit 5000) Have feedback or ...

  17. Search for: All records | DOE Patents

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    Backhaus, Scott N. (1) Keolian, Robert (1) Keolian, Robert M. (1) Swift, Gregory W. (1) Save Results Excel (limit 2000) CSV (limit 5000) XML (limit 5000) Have feedback or ...

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    Shuman, Stewart (3) Sanchez, Ana M. (1) Schwer, Beate (1) Save Results Save this search to My Library Excel (limit 2000) CSV (limit 5000) XML (limit 5000) Have feedback or ...

  19. Search for: All records | DOE PAGES

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    Bassiri, Riccardo (1) Bi, Zhenxing (1) Blamire, Mark G. (1) Borisevich, Albina Y. (1) Byer, Robert L. (1) Choi, Eun -Mi (1) Fejer, Martin M. (1) Fix, Thomas (1) Gustafson, Eric K. ...

  20. Retooling Michigan: Tanks to Turbines

    Broader source: Energy.gov [DOE]

    A company that has manufactured geared systems for the M1 Abrams tank for more than 20 years is now part of the forces working toward energy security and independence.

  1. Search for: All records | SciTech Connect

    Office of Scientific and Technical Information (OSTI)

    ... Filter Results Filter by Subject materials science (3) energy storage (1) nanoscience and nanotechnology (1) Filter by Author Chen, L Q (3) Heo, T W (3) Tang, M (1) Wood, B C (1) ...

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    Gibbons, Sean M. (1) Gilbert, Jack A. (1) Hampton-Marcell, Jarrad T. (1) Lax, Simon (1) Smith, Daniel (1) Save Results Excel (limit 2000) CSV (limit 5000) XML (limit 5000) Have...

  3. CX-012096: Categorical Exclusion Determination

    Broader source: Energy.gov [DOE]

    M1 a and b Habitat Enhancement Project, Site 300 CX(s) Applied: B1.20 Date: 06/19/2013 Location(s): California Offices(s): Lawrence Livermore Site Office

  4. Graded-Refractive-Index Glass-based Antireflective Coatings:...

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    Ilia N 1 ; Liu, Tao 1 ; Wang, Peng 2 ; Menon, Rajesh 1 ; Trejo, Rosa M 1 ; Lara-Curzio, Edgar 1 ; Hunter, Scott Robert 1 ; Simpson, John T 1 ; Paranthaman, ...

  5. 04He

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

    . 4He level deduced admixture of symmetry; calculated (E), M1 transitions, Gaussian wave functions for 3,4He. 1979SU05: 3He(n, ), E thermal; measured for...

  6. Search for: All records | DOE PAGES

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    Dahl, Robert H. (1) Foo, Jee Loon (1) George, Kevin (1) Jensen, Heather M. (1) Keasling, Jay D. (1) Lee, Taek Soon (1) Leong, Susanna (1) Mukhopadhyay, Aindrila (1) Save Results...

  7. Scalable superhydrophobic coatings based on fluorinated diatomaceous...

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    Authors: Polyzos, Georgios 1 ; Winter, Kyle O 1 ; Lance, Michael J 1 ; Meyer III, Harry M 1 ; Armstrong, Beth L 1 ; Schaeffer, Daniel A 1 ; Simpson, John T 1 ; ...

  8. 1

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    1). Correspondingly, the absolute nadir radiance I( 5 ) at m 14 is 15.7 (radiance dimension is Wm -2 sr -1 m -1 ). This value I( 5 ) 15.7 was used here as a threshold...

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    ... results of ion and electron temperature pro le measurements from the x-ray imaging crystal ... average minor radius 0.32m, 1.2 le toroidal field (Bsub t) le 1.7 T, and ...

  10. Scientific Discovery through Advanced Computing (SciDAC-3) Partnership...

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    Authors: Hoffman, Forest M. 1 ; Bochev, Pavel B. 2 ; Cameron-Smith, Philip J.. 3 ; Easter, Richard C 4 ; Elliott, Scott M. 5 ; Ghan, Steven J. 4 ; Liu, Xiaohong 6 ; ...

  11. Approximate models for the ion-kinetic regime ininertial-confinement...

    Office of Scientific and Technical Information (OSTI)

    ... Authors: Hoffman, Nelson M. 1 Search SciTech Connect for author "Hoffman, Nelson M." Search SciTech Connect for ORCID "000000030178767X" Search orcid.org for ORCID ...

  12. YEAR

    National Nuclear Security Administration (NNSA)

    Asian American Pacific Islander Male (AAPI M) 1 Asian American Pacific Islander Female (AAPI F) 0 Hispanic Male (H M) 0 Hispanic Female (H F) 0 White Male (W M) 13 White Female (W ...

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    Jiang, J. Samuel (1) KC, Amit (1) Lederman, David (1) Pearson, John E. (1) Wu, Stephen M. (1) Zhang, Wei (1) Save Results Excel (limit 2000) CSV (limit 5000) XML (limit 5000) Have ...

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    Stanescu, Tudor D. (1) Tarafder, Kartick (1) Trappen, Robbyn (1) Wu, Stephen M. (1) Zhang, Wei (1) Save Results Excel (limit 2000) CSV (limit 5000) XML (limit 5000) Have feedback ...

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    Only0 Filtered Results Filter Results Filter by Author Biteen, Julie S. (1) Blainey, Paul C. (1) Cardon, Zoe G. (1) Chun, Miyoung (1) Church, George M. (1) Dorrestein, Pieter C....

  16. Principle Energy Limited | Open Energy Information

    Open Energy Info (EERE)

    Principle Energy Limited Place: Isle of Man, United Kingdom Zip: 1M1 1LB Sector: Renewable Energy Product: A UK-based renewable energy company focusing on bioethanol projects in...

  17. The unseen iceberg: Plant roots in arctic tundra (Journal Article...

    Office of Scientific and Technical Information (OSTI)

    ecosystems in the Arctic. Authors: Iversen, Colleen M 1 ; Sloan, Victoria L 1 ; Sullivan, Patrick F. 2 ; Euskirchen, Eugenie S 2 ; McGuire, A. David 2 ; Norby, Richard...

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    (1) wetlands (1) wetlands fine roots (1) Filter by Author Iversen, Colleen M (2) Sullivan, Patrick F. (2) Allen, Michael F. (1) Childs, Joanne (1) Eissenstat, David M. (1)...

  19. Micro-Earthquake At Coso Geothermal Area (2002-2005) | Open Energy...

    Open Energy Info (EERE)

    reservoir crack characterization: the Coso geothermal field Rial, J.A.; Elkibbi, M.; Yang, M. (1 January 2005) Shear-wave splitting as a tool for the characterization of...

  20. Search for: All records | SciTech Connect

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    ... Bozarth, Jeffrey M. (1) Cheney, Daniel L. (1) Choi, Hee-Jung (1) Fung, Juan Jos (1) ... Daniel M. ; Fung, Juan Jos ; Choi, Hee-Jung ; Thian, Foon Sun ; Kobilka, Tong Sun ; et ...

  1. Jefferson Lab Activities Group Invites Young and Not-So-Young...

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

    Holiday Events Holiday Party on Dec. 12 for Jefferson Lab Children and the Young at Heart The JAG Holiday Party is scheduled for Saturday, Dec. 12, 10 a.m.-1 p.m. in the CEBAF...

  2. Highly enhanced hard x-ray emission from oriented metal nanorod...

    Office of Scientific and Technical Information (OSTI)

    J. ; Sheng, Z.M. 1 ; Key Laboratory for Laser Plasmas of the Ministry of Education of China and Department of Physics, Shanghai Jiao Tong University, Shanghai 2 + Show Author...

  3. Working Together to Reduce Our Environmental Footprint

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

    computers, cell phones, TVs, printers, VCRs, cameras, and unwanted personally-owned electronic equipment. THURSDAY April 23 12:00 P.M. - 1:00 P.M. * Seasonal Landscapes at...

  4. Site Acquisition Description/ Category Contracting Office Solicitation

    Office of Environmental Management (EM)

    Laboratory Follow- On Procurements https:www.emcbc.doe. govSEBLANLPostFY1 6index.php EMCBC Full and Open Competition CPAF 500M-1B 2015 2016 2016 2016 2016 2016 Savannah...

  5. SAFL Channel | Open Energy Information

    Open Energy Info (EERE)

    University of Minnesota Hydrodynamics Hydrodynamic Testing Facility Type Channel Length(m) 84.0 Beam(m) 2.8 Depth(m) 1.8 Cost(per day) Contact POC Towing Capabilities Towing...

  6. MIT Tow Tank | Open Energy Information

    Open Energy Info (EERE)

    Institute of Technology Hydrodynamics Hydrodynamic Testing Facility Type Tow Tank Length(m) 36.6 Beam(m) 2.4 Depth(m) 1.2 Water Type Saltwater Cost(per day) 750 Towing...

  7. EPAct 1992 in U.S.C. | Department of Energy

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

    EPAct 1992 in U.S.C. CITE: 42USC6807a TITLE 42--THE PUBLIC HEALTH AND WELFARE CITE: 16USC831m-1 TITLE 16--CONSERVATION CITE: 42USC6348 TITLE 42--THE PUBLIC HEALTH AND WELFARE CITE: ...

  8. ARM - Instrument - twrcam

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    Data Highland Center, Cape Cod MA; AMF1 retired PYE M1 Browse Data Browse Plots Point Reyes, CA retired retired Originating instrument has been retired at this location...

  9. ARM - Instrument - nfov

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    Plots Highland Center, Cape Cod MA; AMF1 retired PYE M1 Browse Data Browse Plots Point Reyes, CA retired retired Originating instrument has been retired at this location...

  10. Search for: All records | DOE PAGES

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    Results Filter by Author Reichhardt, C. J. Olson (10) Reichhardt, C. (9) Ray, D. (5) Jia, X. (1) Johnson, P. A. (1) Libl, A. (1) Lopatina, L. M. (1) Save Results Excel (limit...

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    (1) Filter by Author Reichhardt, C. J. Olson (10) Reichhardt, C. (9) Ray, D. (5) Jia, X. (1) Johnson, P. A. (1) Libl, A. (1) Lopatina, L. M. (1) Save Results Save this...

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    Bauer, Eric D. (1) Baumbach, Ryan E. (1) Janka, Oliver (1) Kauzlarich, Susan M. (1) Shang, Tian (1) Thompson, Joe D. (1) Save Results Excel (limit 2000) CSV (limit 5000) XML (limit ...

  13. A=10B (59AJ76)

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

    eV, several times the single-particle value (ME57D). The relative weakness of the M1 transition may reflect the predicted inhibition of such transitions for Tz 0, T 0...

  14. 3M | Open Energy Information

    Open Energy Info (EERE)

    M Jump to: navigation, search Name: 3M Address: 3M Center Place: St. Paul, MN Zip: 55144-1000 Phone Number: 1-888-364-3577 Website: www.3m.com References: 3M1 Information About...

  15. Search for: All records | SciTech Connect

    Office of Scientific and Technical Information (OSTI)

    DelMoro, A. (1) Gandhi, P. (1) Hailey, C.J. (1) Harrison, F.A. (1) Koss, M. (1) Lansbury, ... ; Comastri, A. ; Bologna Observ. ; Harrison, F.A. ; Caltech ; Alexander, D.M. ; ...

  16. SECTION M_Evaluation Factors

    National Nuclear Security Administration (NNSA)

    SECTION M EVALUATION FACTORS FOR AWARD TABLE OF CONTENTS M-1 EVALUATION OF PROPOSALS .....................................................................................2 M-2 BASIS FOR CONTRACT AWARD ...................................................................................3 M-3 TECHNICAL AND MANAGEMENT CRITERIA ..........................................................3 M-4 COST CRITERION

  17. FOIA Request - January 2008

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

    ... who protect public health and safety of the ... Please provide us: AU;m1a CDMtiMIon A1lanIa Journal 001 AUl;lJn American ... importance to the public in understanding the ...

  18. CHS M | Open Energy Information

    Open Energy Info (EERE)

    CHS M Jump to: navigation, search Name: CHS & M Place: Germany Product: A local investment cooperative in Bosseborn, Germany. References: CHS & M1 This article is a stub. You can...

  19. Imaging the oblique propagation of electrons in germanium crystals at low

    Office of Scientific and Technical Information (OSTI)

    temperature and low electric field (Journal Article) | DOE PAGES Imaging the oblique propagation of electrons in germanium crystals at low temperature and low electric field This content will become publicly available on January 11, 2017 « Prev Next » Title: Imaging the oblique propagation of electrons in germanium crystals at low temperature and low electric field Authors: Moffatt, R. A. [1] ; Cabrera, B. [1] ; Corcoran, B. M. [1] ; Kreikebaum, J. M. [1] ; Redl, P. [1] ; Shank, B. [1] ;

  20. LC Recommendations for Data Transfer Nodes (Technical Report) | SciTech

    Office of Scientific and Technical Information (OSTI)

    Connect LC Recommendations for Data Transfer Nodes Citation Details In-Document Search Title: LC Recommendations for Data Transfer Nodes Abstract not provided. Authors: Harr, C. M. [1] ; Long, J. W. [1] ; Heer, T. M. [1] + Show Author Affiliations Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States) Publication Date: 2014-11-12 OSTI Identifier: 1178387 Report Number(s): LLNL-TR--664301 DOE Contract Number: AC52-07NA27344 Resource Type: Technical Report Research Org:

  1. A Framework for Integrated Modeling of Perturbations in Atmospheres for

    Office of Scientific and Technical Information (OSTI)

    Conjunction Tracking (IMPACT) (Conference) | SciTech Connect Framework for Integrated Modeling of Perturbations in Atmospheres for Conjunction Tracking (IMPACT) Citation Details In-Document Search Title: A Framework for Integrated Modeling of Perturbations in Atmospheres for Conjunction Tracking (IMPACT) Authors: Linares, Richard [1] ; Klimenko, Alexei V. [1] ; Brennan, Sean M. [1] ; Godinez Vazquez, Humberto C. [1] ; Higdon, David M. [1] ; Koller, Josef [1] ; Lawrence, Earl C. [1] ; Palmer,

  2. Clostridium thermocellum transcriptomic profiles after exposure to furfural

    Office of Scientific and Technical Information (OSTI)

    or heat stress (Journal Article) | SciTech Connect transcriptomic profiles after exposure to furfural or heat stress Citation Details In-Document Search Title: Clostridium thermocellum transcriptomic profiles after exposure to furfural or heat stress Authors: Wilson, Charlotte M [1] ; Yang, Shihui [1] ; Ma, Qin [2] ; Johnson, Courtney M [1] ; Rodriguez Jr, Miguel [1] ; Dice, Lezlee T [1] ; Xu, Ying [2] ; Brown, Steven D [1] + Show Author Affiliations ORNL [ORNL University of Georgia, Athens,

  3. Recent Results from the Excitation of Dipole States at the HI{gamma}S Facility

    SciTech Connect (OSTI)

    Tonchev, A. P.; Hutcheson, A.; Kwan, E.; Rusev, G.; Tornow, W.; Angell, C.; Hammond, S.; Karwowski, H. J.; Kelley, J. H.; Tsoneva, N.

    2009-01-28

    High-sensitivity studies of E1 and M1 excitations observed in the {sup 138}Ba({gamma},{gamma}') reaction at energies below the neutron emission threshold have been performed. The electric dipole character of the so-called 'pygmy' mode was experimentally verified for excitations from 4.0-8.6 MeV. The fine structure of the M1 'spin-flip' mode was observed for the first time in N = 82 nuclei.

  4. Thermophilic lignocellulose deconstruction (Journal Article) | SciTech

    Office of Scientific and Technical Information (OSTI)

    Connect Thermophilic lignocellulose deconstruction Citation Details In-Document Search Title: Thermophilic lignocellulose deconstruction Authors: Blumer-Schuette, Sara E. [1] ; Brown, Steven D [2] ; Sander, Kyle B [2] ; Bayer, Edward A [2] ; Kataeva, Irena [3] ; Zurawski, Jeffrey V [1] ; Conway, Jonathan M [1] ; Adams, Michael W. W. [3] ; Kelly, Robert M [1] + Show Author Affiliations North Carolina State University [North Carolina State University ORNL [ORNL University of Georgia, Athens,

  5. THE NUCLEUS OF MAIN-BELT COMET 259P/GARRADD

    SciTech Connect (OSTI)

    MacLennan, Eric M.; Hsieh, Henry H. E-mail: emaclenn@utk.edu

    2012-10-10

    We present observations of the main-belt comet 259P/Garradd, previously known as P/2008 R1 (Garradd), obtained in 2011 and 2012 using the Gemini North Telescope on Mauna Kea in Hawaii and the SOAR telescope at Cerro Pachon in Chile, with the goal of computing the object's phase function and nucleus size. We find an absolute magnitude of H{sub R} = 19.71 {+-} 0.05 mag and slope parameter of G{sub R} = -0.08 {+-} 0.05 for the inactive nucleus, corresponding to an effective nucleus radius of r{sub e} = 0.30 {+-} 0.02 km, assuming an R-band albedo of p{sub R} = 0.05. We also revisit observations reported for 259P while it was active in 2008 to quantify the dust mass loss and compare the object with other known main-belt comets.

  6. NEW BV(RI){sub C} PHOTOMETRY FOR PRAESEPE: FURTHER TESTS OF BROADBAND PHOTOMETRIC CONSISTENCY

    SciTech Connect (OSTI)

    Joner, Michael D.; Taylor, Benjamin J.; Laney, C. David; Van Wyk, Francois

    2011-11-15

    New BV(RI){sub C} measurements of Praesepe made at the South African Astronomical Observatory (SAAO) are presented. When those measurements are combined with those reported in previous papers in this series, it is found that they support previously determined V zero points for Praesepe, M67, and the Hyades. Support is also found for joint (V - R){sub C} and (R - I){sub C} zero points established previously for Praesepe and NGC 752. For the SAAO system of standard stars, a B - V correction to the Johnson system of about -9 mmag appears to be reasonably well established. The preferred (though not definitive) V correction is about +7 mmag. For the Landolt V system, zero-point identity with the Johnson system at a 2{sigma} level of 4.8 mmag is found, and no color term as large as 4 mmag (mag){sup -1} is detected. Updated CDS data files for Praesepe are briefly described.

  7. Land-use transition for bioenergy and climate stabilization: model comparison of drivers, impacts and interactions with other land use based mitigation options

    SciTech Connect (OSTI)

    Popp, Alexander; Rose, Steven K.; Calvin, Katherine V.; Van Vuuren, Detlef; Dietrich, Jan P.; Wise, Marshall A.; Stehfest, Eike; Humpenoder, Florian; Kyle, G. Page; Van Vliet, Jasper; Bauer, Nico; Lotze-Campen, Hermann; Klein, David; Kriegler, Elmar

    2014-04-01

    This study is a model comparison assessing the drivers and impacts of bioenergy production on the global land system and the interaction with other land use based mitigation options in the context of the EMF 27 project. We compare and evaluate results from three integrated assessment models (GCAM, IMAGE, and ReMIND/MAgPIE). All three models project that dedicated bioenergy crops and biomass residues are a potentially important and cost-effective component of the energy system. But bioenergy deployment levels and feedstock composition vary notably across models as do the implications for land-use and greenhouse gas emissions and the interaction with other land use based mitigation measures. Despite numerous model differences, we identify a few that are likely contributing to differences in land-use and emissions attributable to energy crop deployment.

  8. Properties OF M31. V. 298 eclipsing binaries from PAndromeda

    SciTech Connect (OSTI)

    Lee, C.-H.; Koppenhoefer, J.; Seitz, S.; Bender, R.; Riffeser, A.; Kodric, M.; Hopp, U.; Snigula, J.; Gssl, C.; Kudritzki, R.-P.; Burgett, W.; Chambers, K.; Hodapp, K.; Kaiser, N.; Waters, C.

    2014-12-10

    The goal of this work is to conduct a photometric study of eclipsing binaries in M31. We apply a modified box-fitting algorithm to search for eclipsing binary candidates and determine their period. We classify these candidates into detached, semi-detached, and contact systems using the Fourier decomposition method. We cross-match the position of our detached candidates with the photometry from Local Group Survey and select 13 candidates brighter than 20.5 mag in V. The relative physical parameters of these detached candidates are further characterized with the Detached Eclipsing Binary Light curve fitter (DEBiL) by Devor. We will follow up the detached eclipsing binaries spectroscopically and determine the distance to M31.

  9. S A N D I A T E C H N O L O G Y A Q UA RT E R LY R E S E A R

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

    Record-setting solar power Green jet fuel SUMMER 2008 In this issue: S A N D I A T E C H N O L O G Y A Q UA RT E R LY R E S E A R C H & D E V E LO P M E N T MAG A Z I N E - VO LUM E 1 0 , N O. 1 Energized Sandia Technology (ISSN: 1547-5190) is a quarterly maga- zine published by Sandia National Laboratories. Sandia is a multiprogram engineering and science laboratory operated by Sandia Corporation, a Lockheed Martin company, for the U.S. Department of Energy. With main facilities in

  10. X-ray Spectroscopy with Elliptical Crystals and Face-On Framing Cameras

    SciTech Connect (OSTI)

    Heeter, R; Emig, J; Fournier, K; Hansen, S; May, M; Young, B

    2004-04-16

    X-ray spectrometers using elliptically bent crystals have desirable properties for applications requiring broad spectral coverage, good spectral resolution, and minimized source broadening. Previous work used custom-positioned film or microchannel plate detectors. They find it is also useful and cost-effective to field elliptical crystals in existing snouts on the face-on gated microchannel plate framing cameras commonly used at many facilities. they numerically explored the full design space (spectral range and resolution) of elliptical crystals compatible with the new MSPEC multipurpose spectrometer snout. They have tested at the Omega laser an elliptical RAP crystal with 174 mm focal length, 0.9885 eccentricity, and 4.6 degree inclination, viewing from 1.0 to at least 1.7 keV with E/dE of 300-500. A slit (2x mag) images 3 mm sources with 70 um spatial resolution.

  11. BRORFELDE SCHMIDT CCD CATALOG

    SciTech Connect (OSTI)

    Zacharias, N.; Finch, C.; Wycoff, G. L.; Einicke, O. H.; Augustesen, K.; Clausen, J. V.; Hoeg, E.

    2010-08-15

    The Brorfelde Schmidt CCD Catalog (BSCC) contains about 13.7 million stars, north of +49{sup 0} decl. with precise positions and V, R photometry. The catalog has been constructed from the reductions of 18,667 CCD frames observed with the Brorfelde Schmidt Telescope between 2000 and 2007. The Tycho-2 catalog was used for astrometric and photometric reference stars. Errors of individual positions are about 20-200 mas for stars in the R = 10-18 mag range. External comparisons with the Two Micron All-Sky Survey (2MASS) and Sloan Digital Sky Survey reveal possible small systematic errors in the BSCC of up to about 30 mas. The catalog is supplemented with J, H, and K{sub s} magnitudes from the 2MASS catalog.

  12. THE MEMBERSHIP AND DISTANCE OF THE OPEN CLUSTER COLLINDER 419

    SciTech Connect (OSTI)

    Roberts, Lewis C.; Gies, Douglas R.; Parks, J. Robert; Grundstrom, Erika D.; McSwain, M. Virginia; Berger, David H.; Mason, Brian D.; Ten Brummelaar, Theo A.; Turner, Nils H. E-mail: gies@chara.gsu.ed E-mail: erika.grundstrom@vanderbilt.ed E-mail: dberger@sysplan.co E-mail: theo@chara-array.or

    2010-09-15

    The young open cluster Collinder 419 surrounds the massive O star, HD 193322, that is itself a remarkable multiple star system containing at least four components. Here we present a discussion of the cluster distance based upon new spectral classifications of the brighter members, UBV photometry, and an analysis of astrometric and photometric data from the third U. S. Naval Observatory CCD Astrograph Catalog and Two Micron All Sky Survey Catalog. We determine an average cluster reddening of E(B - V) = 0.37 {+-} 0.05 mag and a cluster distance of 741 {+-} 36 pc. The cluster probably contains some very young stars that may include a reddened M3 III star, IRAS 20161+4035.

  13. AN ENIGMATIC POINT-LIKE FEATURE WITHIN THE HD169142 TRANSITIONAL DISK ,

    SciTech Connect (OSTI)

    Biller, Beth A.; Males, Jared; Morzinski, Katie; Close, Laird M.; Follette, Katherine B.; Hinz, Philip M.; Rodigas, Timothy; Weinberger, Alycia; Juhsz, Attila; Lacour, Sylvestre; Henning, Thomas; Pott, Jrg-Uwe; Khler, Rainer; Bonnefoy, Mickal

    2014-09-01

    We report the detection of a faint point-like feature possibly related to ongoing planet-formation in the disk of the transition disk star HD169142. The point-like feature has a ?mag(L)? 6.4, at a separation of ?0.''11 and position angle ?0. Given its lack of an H or K{sub S} counterpart despite its relative brightness, this candidate cannot be explained by purely photospheric emission and must be a disk feature heated by an as yet unknown source. Its extremely red colors make it highly unlikely to be a background object, but future multi-wavelength follow up is necessary for confirmation and characterization of this feature.

  14. COSMOLOGICAL PARAMETERS FROM SUPERNOVAE ASSOCIATED WITH GAMMA-RAY BURSTS

    SciTech Connect (OSTI)

    Li, Xue; Hjorth, Jens; Wojtak, Rados?aw, E-mail: lixue@dark-cosmology.dk [Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen (Denmark)

    2014-11-20

    We report estimates of the cosmological parameters ? {sub m} and ?{sub ?} obtained using supernovae (SNe) associated with gamma-ray bursts (GRBs) at redshifts up to 0.606. Eight high-fidelity GRB-SNe with well-sampled light curves across the peak are used. We correct their peak magnitudes for a luminosity-decline rate relation to turn them into accurate standard candles with dispersion ? = 0.18mag. We also estimate the peculiar velocity of the low-redshift host galaxy of SN 1998bw using constrained cosmological simulations. In a flat universe, the resulting Hubble diagram leads to best-fit cosmological parameters of (?{sub m},?{sub ?})=(0.58{sub ?0.25}{sup +0.22},0.42{sub ?0.22}{sup +0.25}). This exploratory study suggests that GRB-SNe can potentially be used as standardizable candles to high redshifts to measure distances in the universe and constrain cosmological parameters.

  15. Integration of MHD load models with circuit representations the Z generator.

    SciTech Connect (OSTI)

    Jennings, Christopher A.; Ampleford, David J.; Jones, Brent Manley; McBride, Ryan D.; Bailey, James E.; Jones, Michael C.; Gomez, Matthew Robert.; Cuneo, Michael Edward; Nakhleh, Charles; Stygar, William A.; Savage, Mark Edward; Wagoner, Timothy C.; Moore, James K.

    2013-03-01

    MHD models of imploding loads fielded on the Z accelerator are typically driven by reduced or simplified circuit representations of the generator. The performance of many of the imploding loads is critically dependent on the current and power delivered to them, so may be strongly influenced by the generators response to their implosion. Current losses diagnosed in the transmission lines approaching the load are further known to limit the energy delivery, while exhibiting some load dependence. Through comparing the convolute performance of a wide variety of short pulse Z loads we parameterize a convolute loss resistance applicable between different experiments. We incorporate this, and other current loss terms into a transmission line representation of the Z vacuum section. We then apply this model to study the current delivery to a wide variety of wire array and MagLif style liner loads.

  16. Manipulating surface reactions in lithium-sulphur batteries using hybrid anode structures

    SciTech Connect (OSTI)

    Huang, C; Xiao, J; Shao, YY; Zheng, JM; Bennett, WD; Lu, DP; Saraf, LV; Engelhard, M; Ji, LW; Zhang, J; Li, XL; Graff, GL; Liu, J

    2014-01-09

    Lithium-sulphur batteries have high theoretical energy density and potentially low cost, but significant challenges such as severe capacity degradation prevent its widespread adoption. Here we report a new design of lithium-sulphur battery using electrically connected graphite and lithium metal as a hybrid anode to control undesirable surface reactions on lithium. Lithiated graphite placed in front of the lithium metal functions as an artificial, self-regulated solid electrolyte interface layer to actively control the electrochemical reactions and minimize the deleterious side reactions, leading to significant performance improvements. Lithium-sulphur cells incorporating this hybrid anodes deliver capacities of >800 mAhg(-1) for 400 cycles at a high rate of 1,737mAg(-1), with only 11% capacity fade and a Coulombic efficiency >99%. This simple hybrid concept may also provide scientific strategies for protecting metal anodes in other energy-storage devices.

  17. A LITHIUM-RICH RED GIANT BELOW THE CLUMP IN THE KEPLER CLUSTER, NGC 6819

    SciTech Connect (OSTI)

    Anthony-Twarog, Barbara J.; Rich, Evan; Twarog, Bruce A.; Deliyannis, Constantine P. E-mail: evan66210@gmail.com E-mail: con@astro.indiana.edu

    2013-04-10

    WIYN/HYDRA spectra in the Li 6708 A region have been obtained for 332 probable members of the old open cluster, NGC 6819. Preliminary analysis shows a pattern of Li depletion from the top of the turnoff to the base of the giant branch. Starting 1 mag below the level of the clump, all brighter giants have A(Li) below 1.0, with most having upper limits below 0.5. Star W007017, located below the first-ascent red giant bump is Li-rich with A(Li) = 2.3. As a highly probable single-star astrometric and radial-velocity cluster member, its discrepant asteroseismic membership could be a by-product of the processes that triggered Li enhancement. Its color-magnitude diagram location is consistent with only one proposed enhanced mixing process among first-ascent red giants.

  18. untitled

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

    petrol Witnessing a birth WINTER 2008 S A N D I A T E C H N O L O G Y A Q UA RT E R LY R E S E A R C H & D E V E LO P M E N T MAG A Z I N E - VO LUM E 9 , N O. 4 Sunshine to petrol Beauty, molecules deep A l l i a n c e s > Sandia Technology (ISSN: 1547-5190) is a quarterly maga- zine published by Sandia National Laboratories. Sandia is a multiprogram engineering and science laboratory operated by Sandia Corporation, a Lockheed Martin company, for the U.S. Department of Energy. With main

  19. Results from KamLAND-Zen

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

    Asakura, K.; Gando, A.; Gando, Y.; Hachiya, T.; Hayashida, S.; Ikeda, H.; Inoue, K.; Ishidoshiro, K.; Ishikawa, T.; Ishio, S.; et al

    2015-07-15

    KamLAND-Zen reports on a preliminary search for neutrinoless double-beta decay with 136Xe based on 114.8 live-days after the purification of the xenon loaded liquid scintillator. In this data, the problematic 110mAg background peak identified in previous searches is reduced by more than a factor of 10. By combining the KamLAND-Zen pre- and post-purification data, we obtain a preliminary lower limit on the 0νββ decay half-life of T0ν1/2 > 2.6×1025 yr at 90% C.L. The search sensitivity will be enhanced with additional low background data after the purification. As a result, prospects for further improvements with future KamLAND-Zen upgrades are alsomore » presented.« less

  20. PLANETARY CONSTRUCTION ZONES IN OCCULTATION: DISCOVERY OF AN EXTRASOLAR RING SYSTEM TRANSITING A YOUNG SUN-LIKE STAR AND FUTURE PROSPECTS FOR DETECTING ECLIPSES BY CIRCUMSECONDARY AND CIRCUMPLANETARY DISKS

    SciTech Connect (OSTI)

    Mamajek, Eric E.; Quillen, Alice C.; Pecaut, Mark J.; Moolekamp, Fred; Scott, Erin L.; Kenworthy, Matthew A.; Cameron, Andrew Collier; Parley, Neil R.

    2012-03-15

    The large relative sizes of circumstellar and circumplanetary disks imply that they might be seen in eclipse in stellar light curves. We estimate that a survey of {approx}10{sup 4} young ({approx}10 million year old) post-accretion pre-main-sequence stars monitored for {approx}10 years should yield at least a few deep eclipses from circumplanetary disks and disks surrounding low-mass companion stars. We present photometric and spectroscopic data for a pre-main-sequence K5 star (1SWASP J140747.93-394542.6 = ASAS J140748-3945.7), a newly discovered {approx}0.9 M{sub Sun} member of the {approx}16 Myr old Upper Centaurus-Lupus subgroup of Sco-Cen at a kinematic distance of 128 {+-} 13 pc. This star exhibited a remarkably long, deep, and complex eclipse event centered on 2007 April 29 (as discovered in Super Wide Angle Search for Planets (SuperWASP) photometry, and with portions of the dimming confirmed by All Sky Automated Survey (ASAS) data). At least five multi-day dimming events of >0.5 mag are identified, with a >3.3 mag deep eclipse bracketed by two pairs of {approx}1 mag eclipses symmetrically occurring {+-}12 days and {+-}26 days before and after. Hence, significant dimming of the star was taking place on and off over at least a {approx}54 day period in 2007, and a strong >1 mag dimming event occurring over a {approx}12 day span. We place a firm lower limit on the period of 850 days (i.e., the orbital radius of the eclipser must be >1.7 AU and orbital velocity must be <22 km s{sup -1}). The shape of the light curve is similar to the lopsided eclipses of the Be star EE Cep. We suspect that this new star is being eclipsed by a low-mass object orbited by a dense inner disk, further girded by at least three dusty rings of optical depths near unity. Between these rings are at least two annuli of near-zero optical depth (i.e., gaps), possibly cleared out by planets or moons, depending on the nature of the secondary. For possible periods in the range 2.33-200 yr, the estimated total ring mass is {approx}8-0.4 M{sub Moon} (if the rings have optical opacity similar to Saturn's rings), and the edge of the outermost detected ring has orbital radius {approx}0.4-0.09 AU. In the new era of time-domain astronomy opened by surveys like SuperWASP, ASAS, etc., and soon to be revolutionized by Large Synoptic Survey Telescope, discovering and characterizing eclipses by circumplanetary and circumsecondary disks will provide us with observational constraints on the conditions that spawn satellite systems around gas giant planets and planetary systems around stars.

  1. Optical BVRI photometry of common proper motion F/G/K+M wide separation binaries

    SciTech Connect (OSTI)

    Li, Ting; Marshall, Jennifer L.; Williams, Patrick; Chavez, Joy [Department of Physics and Astronomy, Texas A and M University, College Station, TX 77840 (United States); Lpine, Sbastien [Department of Physics and Astronomy, Georgia State University, Atlanta, GA 30302-4106 (United States)

    2014-10-01

    We present optical (BVRI) photometric measurements of a sample of 76 common proper motion wide separation main-sequence binary pairs. The pairs are composed of a F-, G-, or K-type primary star and an M-type secondary. The sample is selected from the revised NLTT catalog and the LSPM catalog. The photometry is generally precise to 0.03 mag in all bands. We separate our sample into two groups, dwarf candidates and subdwarf candidates, using the reduced proper motion diagram constructed with our improved photometry. The M subdwarf candidates in general have larger V R colors than the M dwarf candidates at a given V I color. This is consistent with an average metallicity difference between the two groups, as predicted by the PHOENIX/BT-Settl models. The improved photometry will be used as input into a technique to determine the metallicities of the M-type stars.

  2. Experimental observation of left polarized wave absorption near electron cyclotron resonance frequency in helicon antenna produced plasma

    SciTech Connect (OSTI)

    Barada, Kshitish K.; Chattopadhyay, P. K.; Ghosh, J.; Kumar, Sunil; Saxena, Y. C.

    2013-01-15

    Asymmetry in density peaks on either side of an m = +1 half helical antenna is observed both in terms of peak position and its magnitude with respect to magnetic field variation in a linear helicon plasma device [Barada et al., Rev. Sci. Instrum. 83, 063501 (2012)]. The plasma is produced by powering the m = +1 half helical antenna with a 2.5 kW, 13.56 MHz radio frequency source. During low magnetic field (B < 100 G) operation, plasma density peaks are observed at critical magnetic fields on either side of the antenna. However, the density peaks occurred at different critical magnetic fields on both sides of antenna. Depending upon the direction of the magnetic field, in the m = +1 propagation side, the main density peak has been observed around 30 G of magnetic field. On this side, the density peak around 5 G corresponding to electron cyclotron resonance (ECR) is not very pronounced, whereas in the m = -1 propagation side, very pronounced ECR peak has been observed around 5 G. Another prominent density peak around 12 G has also been observed in m = -1 side. However, no peak has been observed around 30 G on this m = -1 side. This asymmetry in the results on both sides is explained on the basis of polarization reversal of left hand polarized waves to right hand polarized waves and vice versa in a bounded plasma system. The density peaking phenomena are likely to be caused by obliquely propagating helicon waves at the resonance cone boundary.

  3. THE RED SUPERGIANT PROGENITOR OF SUPERNOVA 2012aw (PTF12bvh) IN MESSIER 95

    SciTech Connect (OSTI)

    Van Dyk, Schuyler D. [Spitzer Science Center/Caltech, Mailcode 220-6, Pasadena, CA 91125 (United States); Cenko, S. Bradley; Filippenko, Alexei V., E-mail: vandyk@ipac.caltech.edu, E-mail: cenko@berkeley.edu, E-mail: afilippenko@berkeley.edu [Department of Astronomy, University of California, Berkeley, CA 94720-3411 (United States); and others

    2012-09-10

    We report on the direct detection and characterization of the probable red supergiant (RSG) progenitor of the intermediate-luminosity Type II-Plateau (II-P) supernova (SN) 2012aw in the nearby (10.0 Mpc) spiral galaxy Messier 95 (M95; NGC 3351). We have identified the star in both Hubble Space Telescope images of the host galaxy, obtained 17-18 yr prior to the explosion, and near-infrared ground-based images, obtained 6-12 yr prior to the SN. The luminous supergiant showed evidence for substantial circumstellar dust, manifested as excess line-of-sight extinction. The effective total-to-selective ratio of extinction to the star was R'{sub V} Almost-Equal-To 4.35, which is significantly different from that of diffuse interstellar dust (i.e., R{sub V} = 3.1), and the total extinction to the star was therefore, on average, A{sub V} Almost-Equal-To 3.1 mag. We find that the observed spectral energy distribution for the progenitor star is consistent with an effective temperature of 3600 K (spectral type M3), and that the star therefore had a bolometric magnitude of -8.29. Through comparison with recent theoretical massive-star evolutionary tracks we can infer that the RSG progenitor had an initial mass 15 {approx}< M{sub ini}(M{sub Sun }) < 20. Interpolating by eye between the available tracks, we surmise that the star had initial mass {approx}17-18 M{sub Sun }. The circumstellar dust around the progenitor must have been destroyed in the explosion, as the visual extinction to the SN is found to be low (A{sub V} = 0.24 mag with R{sub V} = 3.1).

  4. A NEW H? EMISSION-LINE SURVEY IN THE ORION NEBULA CLUSTER

    SciTech Connect (OSTI)

    Szegedi-Elek, E.; Kun, M.; Pl, A.; Balzs, L. G.; Reipurth, B.; Willman, M.

    2013-10-01

    We present results from an H? emission line survey in a 1 deg{sup 2} area centered on the Orion Nebula Cluster, obtained with the Wide Field Grism Spectrograph 2 on the 2.2 m telescope of the University of Hawaii. We identified 587 stars with H? emission, 99 of which, located mainly in the outer regions of the observed area, have not appeared in previous H? surveys. We determined the equivalent width (EW) of the line and, based on this, classified 372 stars as classical T Tauri stars (CTTSs) and 187 as weak-line T Tauri stars (WTTSs). Simultaneous r', i' photometry indicates a limiting magnitude of r' ? 20 mag, but the sample is incomplete at r' > 17 mag. The surface distribution of the H? emission stars reveals a clustered population and a dispersed population, the former consisting of younger and more massive young stars than the latter. Comparison of the derived EWs with those found in the literature indicates variability of the H? line. We found that the typical amplitudes of the variability are not greater than a factor of two to three in most cases. We identified a subgroup of low-EW stars with infrared signatures indicative of optically thick accretion disks. We studied the correlations between the EW and other properties of the stars. Based on literature data, we examined several properties of our CTTS and WTTS subsamples and found significant differences in mid-infrared color indices, average rotational periods, and spectral energy distribution characteristics of the subsamples.

  5. A UV to mid-IR study of AGN selection

    SciTech Connect (OSTI)

    Chung, Sun Mi; Kochanek, Christopher S.; Assef, Roberto; Brown, Michael J. I.; Stern, Daniel; Jannuzi, Buell T.; Gonzalez, Anthony H.; Hickox, Ryan C.; Moustakas, John

    2014-07-20

    We classify the spectral energy distributions (SEDs) of 431,038 sources in the 9 deg{sup 2} Botes field of the NOAO Deep Wide-Field Survey (NDWFS). There are up to 17 bands of data available per source, including ultraviolet (GALEX), optical (NDWFS), near-IR (NEWFIRM), and mid-infrared (IRAC and MIPS) data, as well as spectroscopic redshifts for ?20,000 objects, primarily from the AGN and Galaxy Evolution Survey. We fit galaxy, active galactic nucleus (AGN), stellar, and brown dwarf templates to the observed SEDs, which yield spectral classes for the Galactic sources and photometric redshifts and galaxy/AGN luminosities for the extragalactic sources. The photometric redshift precision of the galaxy and AGN samples are ?/(1 + z) = 0.040 and ?/(1 + z) = 0.169, respectively, with the worst 5% outliers excluded. On the basis of the ?{sub ?}{sup 2} of the SED fit for each SED model, we are able to distinguish between Galactic and extragalactic sources for sources brighter than I = 23.5 mag. We compare the SED fits for a galaxy-only model and a galaxy-AGN model. Using known X-ray and spectroscopic AGN samples, we confirm that SED fitting can be successfully used as a method to identify large populations of AGNs, including spatially resolved AGNs with significant contributions from the host galaxy and objects with the emission line ratios of 'composite' spectra. We also use our results to compare with the X-ray, mid-IR, optical color, and emission line ratio selection techniques. For an F-ratio threshold of F > 10, we find 16,266 AGN candidates brighter than I = 23.5 mag and a surface density of ?1900 AGN deg{sup 2}.

  6. GRB 080503: IMPLICATIONS OF A NAKED SHORT GAMMA-RAY BURST DOMINATED BY EXTENDED EMISSION

    SciTech Connect (OSTI)

    Perley, D. A.; Metzger, B. D.; Butler, N. R.; Bloom, J. S.; Miller, A. A.; Filippenko, A. V.; Li, W.; Granot, J.; Sakamoto, T.; Gehrels, N.; Ramirez-Ruiz, E.; Bunker, A.; Chen, H.-W.; Glazebrook, K.; Hall, P. B.; Hurley, K. C.; Kocevski, D.; Norris, J.

    2009-05-10

    We report on observations of GRB 080503, a short gamma-ray burst (GRB) with very bright extended emission (about 30 times the gamma-ray fluence of the initial spike) in conjunction with a thorough comparison to other short Swift events. In spite of the prompt-emission brightness, however, the optical counterpart is extraordinarily faint, never exceeding 25 mag in deep observations starting at {approx}1 hr after the Burst Alert Telescope (BAT) trigger. The optical brightness peaks at {approx}1 day and then falls sharply in a manner similar to the predictions of Li and Paczynski (1998) for supernova-like emission following compact binary mergers. However, a shallow spectral index and similar evolution in X-rays inferred from Chandra observations are more consistent with an afterglow interpretation. The extreme faintness of this probable afterglow relative to the bright gamma-ray emission argues for a very low density medium surrounding the burst (a 'naked' GRB), consistent with the lack of a coincident host galaxy down to 28.5 mag in deep Hubble Space Telescope imaging. The late optical and X-ray peak could be explained by a slightly off-axis jet or by a refreshed shock. Our observations reinforce the notion that short GRBs generally occur outside regions of active star formation, but demonstrate that in some cases the luminosity of the extended prompt emission can greatly exceed that of the short spike, which may constrain theoretical interpretation of this class of events. This extended emission is not the onset of an afterglow, and its relative brightness is probably either a viewing-angle effect or intrinsic to the central engine itself. Because most previous BAT short bursts without observed extended emission are too faint for this signature to have been detectable even if it were present at typical level, conclusions based solely on the observed presence or absence of extended emission in the existing Swift sample are premature.

  7. VERY WIDE BINARIES AND OTHER COMOVING STELLAR COMPANIONS: A BAYESIAN ANALYSIS OF THE HIPPARCOS CATALOGUE

    SciTech Connect (OSTI)

    Shaya, Ed J.; Olling, Rob P.

    2011-01-15

    We develop Bayesian statistical methods for discovering and assigning probabilities to non-random (e.g., physical) stellar companions. These companions are either presently bound or were previously bound. The probabilities depend on similarities in corrected proper motion parallel and perpendicular to the brighter component's motion, parallax, and the local phase-space density of field stars. Control experiments are conducted to understand the behavior of false positives. The technique is applied to the Hipparcos Catalogue within 100 pc. This is the first all-sky survey to locate escaped companions still drifting along with each other. In the <100 pc distance range, {approx}220 high probability companions with separations between 0.01 and 1 pc are found. The first evidence for a population ({approx}300) of companions separated by 1-8 pc is found. We find these previously unnoticed naked-eye companions (both with V < 6th mag): Capella and 50 Per, {delta} Vel and HIP 43797, Alioth ({epsilon} UMa), Megrez ({delta} UMa) and Alcor, {gamma} and {tau} Cen, {phi} Eri and {eta} Hor, 62 and 63 Cnc, {gamma} and {tau} Per, {zeta} and {delta} Hya, {beta}{sup 01}, {beta}{sup 02} and {beta}{sup 03} Tuc, N Vel and HIP 47479, HIP 98174 and HIP 97646, and s Eri and HIP 14913. High probability fainter companions (>6th mag) of primaries with V < 4 are found for: Fomalhaut ({alpha} PsA), {gamma} UMa, {alpha} Lib, Alvahet ({iota} Cephi), {delta} Ara, {beta} Ser, {iota} Peg, {beta} Pic, {kappa} Phe, and {gamma} Tuc.

  8. The long-term light curve of the cataclysmic variable V794 Aquilae

    SciTech Connect (OSTI)

    Honeycutt, R. K.; Kafka, S.; Robertson, J. W. E-mail: skafka@aip.org

    2014-01-01

    The 1990-2012 light curve of the nova-like (NL) cataclysmic variable V794 Aql is studied in order to characterize and better understand the transitions to and from the faint state, and the variations within the bright state. Investigations of earlier portions of this data had concluded that the transitions to the low state were much slower than the rapid recovery, giving a sawtoothed appearance to the light curve. This behavior differs from that of most other VY Scl stars, which led to an interpretation of the large amplitude sawtooths as being due to an accretion disk (AD) instability. However, more recent photometry strongly suggests that the bright state itself has transitions of 1-1.5 mag, and that earlier studies had intermixed these bright state variations with the transitions to the low state. These newly recognized variations within the bright state sometimes appear as small outbursts (OBs) with typical amplitudes of 0.5-1.5 mag and spacings of ?15-50 days. The rise times of the OBs are 2-3 times faster than the decline times. We argue that the V794 Aql bright state variations are due to AD behavior similar to that seen in dwarf novae, but with varying degrees of stability. Similar regular small OBs have also been reported in other NL CVs, which we compare with V794 Aql. The true deep low states in V794 Aql appear to be normal, having transition speeds and shapes very similar to the transitions in other VY Scl stars.

  9. Optical and ultraviolet observations of a low-velocity type II plateau supernova 2013am in M65

    SciTech Connect (OSTI)

    Zhang, Jujia; Bai, Jinming; Fan, Yufeng; Wang, Jianguo; Yi, Weimin; Wang, Chuanjun; Xin, Yuxin; Liangchang; Zhang, Xiliang; Lun, Baoli; Wang, Xueli; He, Shousheng [Yunnan Observatories (YNAO), Chinese Academy of Sciences, Kunming 650216 (China); Wang, Xiaofeng; Huang, Fang; Mo, Jun [Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing 100084 (China); Mazzali, Paolo A.; Bersier, David [Astrophysics Research Institute, Liverpool John Moores University, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF (United Kingdom); Zhang, Tianmeng [National Astronomical Observatories of China (NAOC), Chinese Academy of Sciences, Beijing 100012 (China); Walker, Emma S., E-mail: jujia@ynao.ac.cn, E-mail: baijinming@ynao.ac.cn, E-mail: wang_xf@mail.tsinghua.edu.cn [Department of Physics, Yale University, New Haven, CT 06520-8121 (United States)

    2014-12-10

    Optical and ultraviolet observations for the nearby type II plateau supernova (SN IIP) 2013am in the nearby spiral galaxy M65 are presented in this paper. The early spectra are characterized by relatively narrow P-Cygni features, with ejecta velocities much lower than observed in normal SNe IIP (i.e., ?2000 km s{sup 1} versus ?5000 km {sup 1} in the middle of the plateau phase). Moreover, prominent Ca II absorptions are also detected in SN 2013am at relatively early phases. These spectral features are reminiscent of those seen in the low-velocity and low-luminosity SN IIP 2005cs. However, SN 2013am exhibits different photometric properties, having shorter plateau phases and brighter light curve tails if compared to SN 2005cs. Adopting R{sub V} = 3.1 and a mean value of total reddening derived from the photometric and spectroscopic methods (i.e., E(B V) = 0.55 0.19 mag), we find that SN 2013am may have reached an absolute V-band peak magnitude of 15.83 0.71 mag and produced an {sup 56}Ni mass of 0.016{sub ?0.006}{sup +0.010} M {sub ?} in the explosion. These parameters are close to those derived for SN 2008in and SN 2009N, which have been regarded as 'gap-filler' objects linking the faint SNe IIP to the normal ones. This indicates that some low-velocity SNe IIP may not necessarily result from the low-energetic explosions. The low expansion velocities could be due to a lower metallicity of the progenitor stars, a larger envelope mass ejected in the explosion, or the effect of viewing angle where these SNe were observed at an angle away from the polar direction.

  10. Systematic uncertainties associated with the cosmological analysis of the first Pan-STARRS1 type Ia supernova sample

    SciTech Connect (OSTI)

    Scolnic, D.; Riess, A.; Brout, D.; Rodney, S. [Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218 (United States); Rest, A. [Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States); Huber, M. E.; Tonry, J. L. [Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822 (United States); Foley, R. J.; Chornock, R.; Berger, E.; Soderberg, A. M.; Stubbs, C. W.; Kirshner, R. P.; Challis, P.; Czekala, I.; Drout, M. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Narayan, G. [Department of Physics, Harvard University, 17 Oxford Street, Cambridge, MA 02138 (United States); Smartt, S. J.; Botticella, M. T. [Astrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN (United Kingdom); Schlafly, E. [Max Planck Institute for Astronomy, Konigstuhl 17, D-69117 Heidelberg (Germany); and others

    2014-11-01

    We probe the systematic uncertainties from the 113 Type Ia supernovae (SN Ia) in the Pan-STARRS1 (PS1) sample along with 197 SN Ia from a combination of low-redshift surveys. The companion paper by Rest et al. describes the photometric measurements and cosmological inferences from the PS1 sample. The largest systematic uncertainty stems from the photometric calibration of the PS1 and low-z samples. We increase the sample of observed Calspec standards from 7 to 10 used to define the PS1 calibration system. The PS1 and SDSS-II calibration systems are compared and discrepancies up to ?0.02 mag are recovered. We find uncertainties in the proper way to treat intrinsic colors and reddening produce differences in the recovered value of w up to 3%. We estimate masses of host galaxies of PS1 supernovae and detect an insignificant difference in distance residuals of the full sample of 0.037 0.031 mag for host galaxies with high and low masses. Assuming flatness and including systematic uncertainties in our analysis of only SNe measurements, we find w =?1.120{sub ?0.206}{sup +0.360}(Stat){sub ?0.291}{sup +0.269}(Sys). With additional constraints from Baryon acoustic oscillation, cosmic microwave background (CMB) (Planck) and H {sub 0} measurements, we find w=?1.166{sub ?0.069}{sup +0.072} and ?{sub m}=0.280{sub ?0.012}{sup +0.013} (statistical and systematic errors added in quadrature). The significance of the inconsistency with w = 1 depends on whether we use Planck or Wilkinson Microwave Anisotropy Probe measurements of the CMB: w{sub BAO+H0+SN+WMAP}=?1.124{sub ?0.065}{sup +0.083}.

  11. MID-INFRARED HIGH-CONTRAST IMAGING OF HD 114174 B: AN APPARENT AGE DISCREPANCY IN A ''SIRIUS-LIKE'' BINARY SYSTEM

    SciTech Connect (OSTI)

    Matthews, Christopher T.; Crepp, Justin R.; Skemer, Andrew; Hinz, Philip M.; Bailey, Vanessa P.; Defrere, Denis; Leisenring, Jarron; Gianninas, Alexandros; Kilic, Mukremin; Skrutskie, Michael; Esposito, Simone; Puglisi, Alfio

    2014-03-10

    We present new observations of the faint ''Sirius-like'' companion discovered to orbit HD 114174. Previous attempts to image HD 114174 B at mid-infrared wavelengths using NIRC2 at Keck have resulted in a non-detection. Our new L'-band observations taken with the Large Binocular Telescope and L/M-band InfraRed Camera recover the companion (?L = 10.15 0.15mag, ? = 0.''675 0.''016) with a high signal-to-noise ratio (10?). This measurement represents the deepest L' high-contrast imaging detection at subarcsecond separations to date, including extrasolar planets. We confirm that HD 114174 B has near-infrared colors consistent with the interpretation of a cool white dwarf (WD; J L' = 0.76 0.19mag, K L' = 0.64 0.20). New model fits to the object's spectral energy distribution indicate a temperature T {sub eff} = 4260 360K, surface gravity log g = 7.94 0.03, a cooling age t{sub c} ? 7.8Gyr, and mass M = 0.54 0.01 M {sub ?}. We find that the cooling ages given by theoretical atmospheric models do not agree with the age of HD 114174 A derived from both isochronological and gyrochronological analyses. We speculate on possible scenarios to explain the apparent age discrepancy between the primary and secondary. HD114174B is a nearby benchmark WD that will ultimately enable a dynamical mass estimate through continued Doppler and astrometric monitoring. Efforts to characterize its physical properties in detail will test theoretical atmospheric models and improve our understanding of WD evolution, cooling, and progenitor masses.

  12. Simulations of the OzDES AGN reverberation mapping project

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

    King, Anthea L.; Martini, Paul; Davis, Tamara M.; Denney, K. D.; Kochanek, C. S.; Peterson, Bradley M.; Skielboe, Andreas; Vestergaard, Marianne; Huff, Eric; Watson, Darach; et al

    2015-08-26

    As part of the Australian spectroscopic dark energy survey (OzDES) we are carrying out a large-scale reverberation mapping study of ~500 quasars over five years in the 30 deg2 area of the Dark Energy Survey (DES) supernova fields. These quasars have redshifts ranging up to 4 and have apparent AB magnitudes between 16.8 mag < r < 22.5 mag. The aim of the survey is to measure time lags between fluctuations in the quasar continuum and broad emission-line fluxes of individual objects in order to measure black hole masses for a broad range of active galactic nuclei (AGN) and constrainmore » the radius–luminosity (R–L) relationship. Here we investigate the expected efficiency of the OzDES reverberation mapping campaign and its possible extensions. We expect to recover lags for ~35–45 % of the quasars. AGN with shorter lags and greater variability are more likely to yield a lag measurement, and objects with lags ≲6 months or ~1 yr are expected to be recovered the most accurately. The baseline OzDES reverberation mapping campaign is predicted to produce an unbiased measurement of the R–L relationship parameters for Hβ, MgIIλ2798, and C IVλ1549. As a result, extending the baseline survey by either increasing the spectroscopic cadence, extending the survey season, or improving the emission-line flux measurement accuracy will significantly improve the R–L parameter constraints for all broad emission lines.« less

  13. A P-loop Mutation in G[alpha] Subunits Prevents Transition to the Active State: Implications for G-protein Signaling in Fungal Pathogenesis

    SciTech Connect (OSTI)

    Bosch, Dustin E.; Willard, Francis S.; Ramanujam, Ravikrishna; Kimple, Adam J.; Willard, Melinda D.; Naqvi, Naweed I.; Siderovski, David P.

    2012-10-23

    Heterotrimeric G-proteins are molecular switches integral to a panoply of different physiological responses that many organisms make to environmental cues. The switch from inactive to active G{alpha}{beta}{gamma} heterotrimer relies on nucleotide cycling by the G{alpha} subunit: exchange of GTP for GDP activates G{alpha}, whereas its intrinsic enzymatic activity catalyzes GTP hydrolysis to GDP and inorganic phosphate, thereby reverting G{alpha} to its inactive state. In several genetic studies of filamentous fungi, such as the rice blast fungus Magnaporthe oryzae, a G42R mutation in the phosphate-binding loop of G{alpha} subunits is assumed to be GTPase-deficient and thus constitutively active. Here, we demonstrate that G{alpha}(G42R) mutants are not GTPase deficient, but rather incapable of achieving the activated conformation. Two crystal structure models suggest that Arg-42 prevents a typical switch region conformational change upon G{alpha}{sub i1}(G42R) binding to GDP {center_dot} AlF{sub 4}{sup -} or GTP, but rotameric flexibility at this locus allows for unperturbed GTP hydrolysis. G{alpha}(G42R) mutants do not engage the active state-selective peptide KB-1753 nor RGS domains with high affinity, but instead favor interaction with G{beta}{gamma} and GoLoco motifs in any nucleotide state. The corresponding G{alpha}{sub q}(G48R) mutant is not constitutively active in cells and responds poorly to aluminum tetrafluoride activation. Comparative analyses of M. oryzae strains harboring either G42R or GTPase-deficient Q/L mutations in the G{alpha} subunits MagA or MagB illustrate functional differences in environmental cue processing and intracellular signaling outcomes between these two G{alpha} mutants, thus demonstrating the in vivo functional divergence of G42R and activating G-protein mutants.

  14. PTF10nvg: AN OUTBURSTING CLASS I PROTOSTAR IN THE PELICAN/NORTH AMERICAN NEBULA

    SciTech Connect (OSTI)

    Covey, Kevin R.; Hillenbrand, Lynne A.; Kasliwal, Mansi M.; Ofek, Eran O.; Miller, Adam A.; Poznanski, Dovi; Cenko, S. Bradley; Silverman, Jeffrey M.; Bloom, Joshua S.; Butler, Nathaniel R.; Filippenko, Alexei V.; Fischer, William; Rayner, John; Rebull, Luisa M.; Law, Nicholas M.; Agueeros, Marcel; Dekany, Richard G.; Rahmer, Gustavo; Hale, David; Smith, Roger

    2011-02-15

    During a synoptic survey of the North American Nebula region, the Palomar Transient Factory (PTF) detected an optical outburst (dubbed PTF10nvg) associated with the previously unstudied flat or rising spectrum infrared source IRAS 20496+4354. The PTF R-band light curve reveals that PTF10nvg brightened by more than 5 mag during the current outburst, rising to a peak magnitude of R{sub PTF} {approx} 13.5 in 2010 September. Follow-up observations indicate that PTF10nvg has undergone a similar {approx}5 mag brightening in the K band and possesses a rich emission-line spectrum, including numerous lines commonly assumed to trace mass accretion and outflows. Many of these lines are blueshifted by {approx}175 km s{sup -1} from the North American Nebula's rest velocity, suggesting that PTF10nvg is driving an outflow. Optical spectra of PTF10nvg show several TiO/VO band heads fully in emission, indicating the presence of an unusual amount of dense (>10{sup 10} cm{sup -3}), warm (1500-4000 K) circumstellar material. Near-infrared spectra of PTF10nvg appear quite similar to a spectrum of McNeil's Nebula/V1647 Ori, a young star which has undergone several brightenings in recent decades, and 06297+1021W, a Class I protostar with a similarly reached near-infrared emission line spectrum. While further monitoring is required to fully understand this event, we conclude that the brightening of PTF10nvg is indicative of enhanced accretion and outflow in this Class-I-type protostellar object, similar to the behavior of V1647 Ori in 2004-2005.

  15. DIRECT IMAGING OF A COLD JOVIAN EXOPLANET IN ORBIT AROUND THE SUN-LIKE STAR GJ 504

    SciTech Connect (OSTI)

    Kuzuhara, M.; Tamura, M.; Kandori, R.; Hori, Y.; Suzuki, R.; Suenaga, T.; Takahashi, Y. H.; Kwon, J.; Kudo, T.; Janson, M.; Brandt, T. D.; Spiegel, D.; Burrows, A.; Turner, E. L.; Moro-Martin, A.; Thalmann, C.; Biller, B.; Henning, T.; Carson, J.; McElwain, M. W.; and others

    2013-09-01

    Several exoplanets have recently been imaged at wide separations of >10 AU from their parent stars. These span a limited range of ages (<50 Myr) and atmospheric properties, with temperatures of 800-1800 K and very red colors (J - H > 0.5 mag), implying thick cloud covers. Furthermore, substantial model uncertainties exist at these young ages due to the unknown initial conditions at formation, which can lead to an order of magnitude of uncertainty in the modeled planet mass. Here, we report the direct-imaging discovery of a Jovian exoplanet around the Sun-like star GJ 504, detected as part of the SEEDS survey. The system is older than all other known directly imaged planets; as a result, its estimated mass remains in the planetary regime independent of uncertainties related to choices of initial conditions in the exoplanet modeling. Using the most common exoplanet cooling model, and given the system age of 160{sup +350}{sub -60} Myr, GJ 504b has an estimated mass of 4{sup +4.5}{sub -1.0} Jupiter masses, among the lowest of directly imaged planets. Its projected separation of 43.5 AU exceeds the typical outer boundary of {approx}30 AU predicted for the core accretion mechanism. GJ 504b is also significantly cooler (510{sup +30}{sub -20} K) and has a bluer color (J - H = -0.23 mag) than previously imaged exoplanets, suggesting a largely cloud-free atmosphere accessible to spectroscopic characterization. Thus, it has the potential of providing novel insights into the origins of giant planets as well as their atmospheric properties.

  16. The 4.5 ?m full-orbit phase curve of the hot Jupiter HD 209458b

    SciTech Connect (OSTI)

    Zellem, Robert T.; Griffith, Caitlin A.; Showman, Adam P.; Lewis, Nikole K.; Knutson, Heather A.; Fortney, Jonathan J.; Laughlin, Gregory; Cowan, Nicolas B.; Agol, Eric; Burrows, Adam; Charbonneau, David; Deming, Drake; Langton, Jonathan

    2014-07-20

    The hot Jupiter HD 209458b is particularly amenable to detailed study as it is among the brightest transiting exoplanet systems currently known (V-mag = 7.65; K-mag = 6.308) and has a large planet-to-star contrast ratio. HD 209458b is predicted to be in synchronous rotation about its host star with a hot spot that is shifted eastward of the substellar point by superrotating equatorial winds. Here we present the first full-orbit observations of HD 209458b, in which its 4.5 ?m emission was recorded with Spitzer/IRAC. Our study revises the previous 4.5 ?m measurement of HD 209458b's secondary eclipse emission downward by ?35% to 0.1391%{sub ?0.0069%}{sup +0.0072%}, changing our interpretation of the properties of its dayside atmosphere. We find that the hot spot on the planet's dayside is shifted eastward of the substellar point by 40.9 6.0, in agreement with circulation models predicting equatorial superrotation. HD 209458b's dayside (T{sub bright} = 1499 15 K) and nightside (T{sub bright} = 972 44 K) emission indicate a day-to-night brightness temperature contrast smaller than that observed for more highly irradiated exoplanets, suggesting that the day-to-night temperature contrast may be partially a function of the incident stellar radiation. The observed phase curve shape deviates modestly from global circulation model predictions potentially due to disequilibrium chemistry or deficiencies in the current hot CH{sub 4} line lists used in these models. Observations of the phase curve at additional wavelengths are needed in order to determine the possible presence and spatial extent of a dayside temperature inversion, as well as to improve our overall understanding of this planet's atmospheric circulation.

  17. Kinetic investigation of catalytic disproportionation of superoxide ions in the non-aqueous electrolyte used in Li–air batteries

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

    Wang, Qiang; Zheng, Dong; McKinnon, Meaghan E.; Yang, Xiao -Qing; Qu, Deyang

    2014-10-28

    Superoxide reacts with carbonate solvents in Li–air batteries. Tris(pentafluorophenyl)borane is found to catalyze a more rapid superoxide (O2-) disproportionation reaction than the reaction between superoxide and propylene carbonate (PC). With this catalysis, the negative impact of the reaction between the electrolyte and O2-produced by the O2 reduction can be minimized. A simple kinetic study using ESR spectroscopy was reported to determine reaction orders and rate constants for the reaction between PC and superoxide, and the disproportionation of superoxide catalyzed by Tris(pentafluorophenyl)borane and Li ions. As a result, the reactions are found to be first order and the rate constants aremore »0.033 s-1 M-1, 0.020 s-1 M-1and 0.67 s-1M-1 for reactions with PC, Li ion and Tris(pentafluorophenyl)borane, respectively.« less

  18. Kinetic investigation of catalytic disproportionation of superoxide ions in the non-aqueous electrolyte used in Li-air batteries

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

    Wang, Qiang; Yang, Xiao -Qing; Zheng, Doug; McKinnon, Meaghan E.; Qu, Deyang

    2014-10-28

    Superoxide reacts with carbonate solvents in Liair batteries. Tris(pentafluorophenyl)borane is found to catalyze a more rapid superoxide (O2-) disproportionation reaction than the reaction between superoxide and propylene carbonate (PC). With this catalysis, the negative impact of the reaction between the electrolyte and O2-produced by the O2 reduction can be minimized. A simple kinetic study using ESR spectroscopy was reported to determine reaction orders and rate constants for the reaction between PC and superoxide, and the disproportionation of superoxide catalyzed by Tris(pentafluorophenyl)borane and Li ions. The reactions are found to be first order and the rate constants are 0.033 s-1 M-1,more0.020 s-1 M-1and 0.67 s-1M-1 for reactions with PC, Li ion and Tris(pentafluorophenyl)borane, respectively.less

  19. Scales in the fine structure of the magnetic dipole resonance: A wavelet approach to the shell model

    SciTech Connect (OSTI)

    Petermann, I.; Langanke, K.; Martinez-Pinedo, G.; Neumann-Cosel, P. von; Nowacki, F.; Richter, A.

    2010-01-15

    Wavelet analysis is applied as a tool for the examination of magnetic dipole (M1) strength distributions in pf-shell nuclei by the extraction of wavelet scales. Results from the analysis of theoretical M1 strength distributions calculated with the KB3G interaction are compared to experimental data from (e,e{sup '}) experiments and good agreement of the deduced wavelet scales is observed. This provides further insight into the nature of the scales from the model results. The influence of the number of Lanczos iterations on the development and stability of scales and the role of the model space in terms of the truncation level are studied. Moreover, differences in the scales of spin and orbital parts of the M1 strength are investigated, as is the use of different effective interactions (KB3G, GXPF1, and FPD6).

  20. Scissors mode of Gd nuclei studied from resonance neutron capture

    SciTech Connect (OSTI)

    Kroll, J.; Baramsai, B.; Becker, J. A.; and others

    2012-10-20

    Spectra of {gamma} rays following the neutron capture at isolated resonances of stable Gd nuclei were measured. The objectives were to get new information on photon strength of {sup 153,155-159}Gd with emphasis on the role of the M1 scissors-mode vibration. An analysis of the data obtained clearly indicates that the scissors mode is coupled not only to the ground state, but also to all excited levels of the nuclei studied. The specificity of our approach ensures unbiasedness in estimating the sumed scissors-mode strength {Sigma}B(M1){up_arrow}, even for odd product nuclei, for which conventional nuclear resonance fluorescence measurements yield only limited information. Our analysis indicates that for these nuclei the sum {Sigma}B(M1){up_arrow} increases with A and for {sup 157,159}Gd it is significantly higher compared to {sup 156,158}Gd.

  1. HUBBLE SPACE TELESCOPE ACS IMAGING OF THE GOALS SAMPLE: QUANTITATIVE STRUCTURAL PROPERTIES OF NEARBY LUMINOUS INFRARED GALAXIES WITH L{sub IR} > 10{sup 11.4} L{sub Sun}

    SciTech Connect (OSTI)

    Kim, D.-C.; Evans, A. S.; Privon, G. C. E-mail: aevans@virginia.edu; and others

    2013-05-10

    A Hubble Space Telescope/Advanced Camera for Surveys study of the structural properties of 85 luminous and ultraluminous (L{sub IR} > 10{sup 11.4} L{sub Sun }) infrared galaxies (LIRGs and ULIRGs) in the Great Observatories All-sky LIRG Survey (GOALS) sample is presented. Two-dimensional GALFIT analysis has been performed on F814W ''I-band'' images to decompose each galaxy, as appropriate, into bulge, disk, central point-spread function (PSF) and stellar bar components. The fraction of bulge-less disk systems is observed to be higher in LIRGs (35%) than in ULIRGs (20%), with the disk+bulge systems making up the dominant fraction of both LIRGs (55%) and ULIRGs (45%). Further, bulge+disk systems are the dominant late-stage merger galaxy type and are the dominant type for LIRGs and ULIRGs at almost every stage of galaxy-galaxy nuclear separation. The mean I-band host absolute magnitude of the GOALS galaxies is -22.64 {+-} 0.62 mag (1.8{sup +1.4}{sub -0.4} L{sup *}{sub I}), and the mean bulge absolute magnitude in GOALS galaxies is about 1.1 mag fainter than the mean host magnitude. Almost all ULIRGs have bulge magnitudes at the high end (-20.6 to -23.5 mag) of the GOALS bulge magnitude range. Mass ratios in the GOALS binary systems are consistent with most of the galaxies being the result of major mergers, and an examination of the residual-to-host intensity ratios in GOALS binary systems suggests that smaller companions suffer more tidal distortion than the larger companions. We find approximately twice as many bars in GOALS disk+bulge systems (32.8%) than in pure-disk mergers (15.9%) but most of the disk+bulge systems that contain bars are disk-dominated with small bulges. The bar-to-host intensity ratio, bar half-light radius, and bar ellipticity in GOALS galaxies are similar to those found in nearby spiral galaxies. The fraction of stellar bars decreases toward later merger stages and smaller nuclear separations, indicating that bars are destroyed as the merger advances. In contrast, the fraction of nuclear PSFs increases toward later merger stages and is highest in late-stage systems with a single nucleus. Thus, light from an active galactic nucleus or compact nuclear star cluster is more visible at I band as ULIRGs enter their latter stages of evolution. Finally, both GOALS elliptical hosts and nearby Sloan Digital Sky Survey (SDSS) ellipticals occupy the same part of the surface brightness versus half-light radius plot (i.e., the {sup K}ormendy Relation{sup )} and have similar slopes, consistent with the possibility that the GOALS galaxies belong to the same parent population as the SDSS ellipticals.

  2. HOPM1 mediated disease resistance to Pseudomonas syringae in Arabidopsis

    DOE Patents [OSTI]

    He, Sheng Yang (Okemos, MI); Nomura, Kinya (East Lansing, MI)

    2011-11-15

    The present invention relates to compositions and methods for enhancing plant defenses against pathogens. More particularly, the invention relates to enhancing plant immunity against bacterial pathogens, wherein HopM1.sub.1-300 mediated protection is enhanced, such as increased protection to Pseudomonas syringae pv. tomato DC3000 HopM1 and/or there is an increase in activity of an ATMIN associated plant protection protein, such as ATMIN7. Reagents of the present invention further provide a means of studying cellular trafficking while formulations of the present inventions provide increased pathogen resistance in plants.

  3. YEAR

    National Nuclear Security Administration (NNSA)

    9 YEAR 2014 Males 9 Females 10 YEAR 2014 SES 7 ED 1 EJ/EK 1 EN 05 1 NQ (Prof/Tech/Admin) 8 NU (Tech/Admin Support) 1 YEAR 2014 American Indian Alaska Native Male (AIAN M) 0 American Indian Alaskan Native Female (AIAN F) 1 African American Male (AA M) 1 African American Female (AA F) 5 Asian American Pacific Islander Male (AAPI M) 1 Asian American Pacific Islander Female (AAPI F) 0 Hispanic Male (H M) 0 Hispanic Female (H F) 3 White Male (W M) 7 White Female (W F) 1 PAY PLAN DIVERSITY TOTAL

  4. YEAR

    National Nuclear Security Administration (NNSA)

    17 Females 18 PAY PLAN YEAR 2014 SES 1 EJ/EK 3 NQ (Prof/Tech/Admin) 30 NU (Tech/Admin Support) 1 YEAR 2014 American Indian Alaska Native Male (AIAN M) 1 American Indian Alaskan Native Female (AIAN F) 2 African American Male (AA M) 3 African American Female (AA F) 7 Asian American Pacific Islander Male (AAPI M) 1 Asian American Pacific Islander Female (AAPI F) 0 Hispanic Male (H M) 2 Hispanic Female (H F) 6 White Male (W M) 10 White Female (W F) 3 DIVERSITY TOTAL WORKFORCE GENDER Associate

  5. Spectral Structure of the Pygmy Dipole Resonance

    SciTech Connect (OSTI)

    Tonchev, A. P.; Kwan, E.; Rusev, G.; Tornow, W.; Hammond, S. L.; Kelley, J. H.; Lenske, H.; Tsoneva, N.

    2010-02-19

    High-sensitivity studies of E1 and M1 transitions observed in the reaction {sup 138}Ba(gamma-vector,gamma{sup '}) at energies below the one-neutron separation energy have been performed using the nearly monoenergetic and 100% linearly polarized photon beams of the HIgamma-vectorS facility. The electric dipole character of the so-called 'pygmy' dipole resonance was experimentally verified for excitations from 4.0 to 8.6 MeV. The fine structure of the M1'spin-flip' mode was observed for the first time in N=82 nuclei.

  6. Synthesis of perylene-porphyrin building blocks and polymers thereof for the production of light-harvesting arrays

    DOE Patents [OSTI]

    Loewe, Robert S.; Tomizaki, Kin-ya; Lindsey, Jonathan S.

    2005-07-12

    The present invention provides methods, compounds, and compositions for the synthesis of light harvesting arrays, such arrays comprising: (a) a first substrate comprising a first electrode; and (b) a layer of light harvesting rods electrically coupled to said first electrode, each of said light harvesting rods comprising a polymer of Formula I: wherein m is at least 1; X.sup.1 is a charge separation group, and X.sup.2 through X.sup.m+1 are chromophores. At least one of X.sup.2 through X.sup.m+1 has at least one perylene group coupled thereto.

  7. Search for: All records | DOE PAGES

    Office of Scientific and Technical Information (OSTI)

    Switch to Detail View for this search DOE PAGES Search Results Page 1 of 1 Search for: All records Author ORCID ID is 0000000277555915 × Sort by Relevance Sort by Date (newest first) Sort by Date (oldest first) Sort by Relevance « Prev Next » Total Results1 Pub. Available Full TextPublicly Available Full Text1 Citation Only0 Filtered Results Filter Results Filter by Author Esteves, G. (1) Fancher, C. M. (1) Johnson-Wilke, R. L. (1) Jones, J. L. (1) Trolier-McKinstry, S. (1) Wallace, M. (1)

  8. Search for: All records | SciTech Connect

    Office of Scientific and Technical Information (OSTI)

    Switch to Detail View for this search SciTech Connect Search Results Page 1 of 1 Search for: All records Creators/Authors contains: "/Hawaii U./ETH, Zurich" × Sort by Relevance Sort by Date (newest first) Sort by Date (oldest first) Sort by Relevance « Prev Next » Everything1 Electronic Full Text1 Citations0 Multimedia0 Datasets0 Software0 Filter Results Filter by Subject astro, grqc (1) Filter by Author Alexander, D.M. (1) Ballantyne, D.R. (1) Balokovic, M. (1) Bauer, F.E. (1)

  9. Technical Assistance: Increasing Code Compliance

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

    Assistance: Increasing Code Compliance 2014 Building Technologies Office Peer Review Rosemarie Bartlett rosemarie.bartlett@pnnl.gov Pacific Northwest National Laboratory FY12 FY13 FY14 $3.9M $1.8M $1.8M Project Summary Timeline: Multi-year program in support of DOE statutory requirements Key Milestones: 1. REScheck Update Including Enhancements (Aug 2014) 2. 90.1-2013 Training Materials (Aug 2014) 3. Revised Compliance Methodology (Sept 2014) 4. 2015 IECC Training Materials (Dec 2014) 5.

  10. Pulsations and period changes of the non-Blazhko RR lyrae variable Y oct observed from Dome A, Antarctica

    SciTech Connect (OSTI)

    Zhihua, Huang; Jianning, Fu; Weikai, Zong; Lingzhi, Wang; Zonghong, Zhu; M, Macri Lucas; Lifan, Wang; Ashley, Michael C. B.; S, Lawrence Jon; Daniel, Luong-Van; Xiangqun, Cui; Long-Long, Feng; Xuefei, Gong; Qiang, Liu; Huigen, Yang; Xiangyan, Yuan; Xu, Zhou; Zhenxi, Zhu; R, Pennypacker Carl; G, York Donald

    2015-01-01

    During the operation of the Chinese Small Telescope Array (CSTAR) in Dome A of Antarctica in the years 2008, 2009, and 2010, large amounts of photometric data have been obtained for variable stars in the CSTAR field. We present here the study of one of six RR Lyrae variables, Y Oct, observed with CSTAR in Dome A, Antarctica. Photometric data in the i band were obtained in 2008 and 2010, with a duty cycle (defined as the fraction of time representing scientifically available data to CSTAR observation time) of about 44% and 52%, respectively. In 2009, photometric data in the g and r bands were gathered for this star, with a duty cycle of 65% and 60%, respectively. Fourier analysis of the data in the three bands only shows the fundamental frequency and its harmonics, which is characteristic of the non-Blazhko RR Lyrae variables. Values of the fundamental frequency and the amplitudes, as well as the total pulsation amplitude, are obtained from the data in the three bands separately. The amplitude of the fundamental frequency and the total pulsation amplitude in the g band are the largest, and those in the i band the smallest. Two-hundred fifty-one times of maximum are obtained from the three seasons of data, which are analyzed together with 38 maximum times provided in the GEOS RR Lyrae database. A period change rate of −0.96 ± 0.07 days Myr{sup −1} is then obtained, which is a surprisingly large negative value. Based on relations available in the literature, the following physical parameters are derived: [Fe/H] = −1.41 ± 0.14, M{sub V} = 0.696 ± 0.014 mag, V−K = 1.182 ± 0.028 mag, logT{sub eff} = 3.802 ± 0.003 K, logg = 2.705 ± 0.004, logL/L{sub ⊙} = 1.625 ± 0.013, and logM/M{sub ⊙} = −0.240 ± 0.019.

  11. PHOTOMETRIC REDSHIFTS IN THE HAWAII-HUBBLE DEEP FIELD-NORTH (H-HDF-N)

    SciTech Connect (OSTI)

    Yang, G.; Xue, Y. Q.; Kong, X.; Wang, J.-X.; Yuan, Y.-F.; Zhou, H. Y.; Luo, B.; Brandt, W. N.; Alexander, D. M.; Bauer, F. E.; Cui, W.; Lehmer, B. D.; Wu, X.-B.; Yuan, F. E-mail: xuey@ustc.edu.cn

    2015-01-01

    We derive photometric redshifts (z {sub phot}) for sources in the entire (?0.4deg{sup 2}) Hawaii-Hubble Deep Field-North (H-HDF-N) field with the EAzY code, based on point-spread-function-matched photometry of 15 broad bands from the ultraviolet (U band) to mid-infrared (IRAC 4.5 ?m). Our catalog consists of a total of 131,678sources. We evaluate the z {sub phot} quality by comparing z {sub phot} with spectroscopic redshifts (z {sub spec}) when available, and find a value of normalized median absolute deviation ?{sub NMAD} = 0.029 and an outlier fraction of 5.5% (outliers are defined as sources having |z{sub phot} z{sub spec} |/(1 + z{sub spec} ) > 0.15) for non-X-ray sources. More specifically, we obtain ?{sub NMAD}= 0.024 with 2.7% outliers for sources brighter than R = 23mag, ?{sub NMAD}= 0.035 with 7.4% outliers for sources fainter than R = 23mag, ?{sub NMAD}= 0.026 with 3.9% outliers for sources having z < 1, and ?{sub NMAD} = 0.034 with 9.0% outliers for sources having z > 1. Our z {sub phot} quality shows an overall improvement over an earlier z {sub phot} work that focused only on the central H-HDF-N area. We also classify each object as a star or galaxy through template spectral energy distribution fitting and complementary morphological parameterization, resulting in 4959 stars and 126,719 galaxies. Furthermore, we match our catalog with the 2Ms Chandra Deep Field-North main X-ray catalog. For the 462 matched non-stellar X-ray sources (281 having z {sub spec}), we improve their z {sub phot} quality by adding three additional active galactic nucleus templates, achieving ?{sub NMAD}= 0.035 and an outlier fraction of 12.5%. We make our catalog publicly available presenting both photometry and z {sub phot}, and provide guidance on how to make use of our catalog.

  12. 2007 TY430: A COLD CLASSICAL KUIPER BELT TYPE BINARY IN THE PLUTINO POPULATION

    SciTech Connect (OSTI)

    Sheppard, Scott S.; Ragozzine, Darin; Trujillo, Chadwick

    2012-03-15

    Kuiper Belt object 2007 TY430 is the first wide, equal-sized, binary known in the 3:2 mean motion resonance with Neptune. The two components have a maximum separation of about 1 arcsec and are on average less than 0.1 mag different in apparent magnitude with identical ultra-red colors (g - i = 1.49 {+-} 0.01 mag). Using nearly monthly observations of 2007 TY430 from 2007 to 2011, the orbit of the mutual components was found to have a period of 961.2 {+-} 4.6 days with a semi-major axis of 21000 {+-} 160 km and eccentricity of 0.1529 {+-} 0.0028. The inclination with respect to the ecliptic is 15.68 {+-} 0.22 deg and extensive observations have allowed the mirror orbit to be eliminated as a possibility. The total mass for the binary system was found to be 7.90 {+-} 0.21 Multiplication-Sign 10{sup 17} kg. Equal-sized, wide binaries and ultra-red colors are common in the low-inclination 'cold' classical part of the Kuiper Belt and likely formed through some sort of three-body interactions within a much denser Kuiper Belt. To date 2007 TY430 is the only ultra-red, equal-sized binary known outside of the classical Kuiper Belt population. Numerical simulations suggest 2007 TY430 is moderately unstable in the outer part of the 3:2 resonance and thus 2007 TY430 is likely an escaped 'cold' classical object that later got trapped in the 3:2 resonance. Similar to the known equal-sized, wide binaries in the cold classical population, the binary 2007 TY430 requires a high albedo and very low density structure to obtain the total mass found for the pair. For a realistic minimum density of 0.5 g cm{sup -3} the albedo of 2007 TY430 would be greater than 0.17. For reasonable densities, the radii of either component should be less than 60 km, and thus the relatively low eccentricity of the binary is interesting since no tides should be operating on the bodies at their large distances from each other. The low prograde inclination of the binary also makes it unlikely that the Kozai mechanism could have altered the orbit, making the 2007 TY430 binary orbit likely one of the few relatively unaltered primordial binary orbits known. Under some binary formation models, the low-inclination prograde orbit of the 2007 TY430 binary indicates formation within a relatively high velocity regime in the Kuiper Belt.

  13. ILLUMINATING THE DARKEST GAMMA-RAY BURSTS WITH RADIO OBSERVATIONS

    SciTech Connect (OSTI)

    Zauderer, B. A.; Berger, E.; Margutti, R.; Fong, W.; Laskar, T.; Chornock, R.; Soderberg, A. M. [Department of Astronomy, Harvard University, Cambridge, MA 02138 (United States); Levan, A. J. [Department of Physics, University of Warwick, Coventry CV4 7AL (United Kingdom); Olivares E, F.; Greiner, J. [Max-Planck-Institut fuer extraterrestrische Physik, Giessenbachstrasse, D-85748 Garching (Germany); Perley, D. A.; Horesh, A.; Carpenter, J. [Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91225 (United States); Updike, A. C. [Department of Chemistry and Physics, Roger Williams University, Bristol, RI 02809 (United States); Tanvir, N. R. [Department of Physics and Astronomy, University of Leicester, Leicester LE1 7RH (United Kingdom); Menten, K. M. [Max-Planck-Institut fuer Radioastronomie, D-53121 Bonn (Germany); Nakar, E. [Department of Astrophysics, Sackler School of Physics and Astronomy, Tel Aviv University, 69978 Tel Aviv (Israel); Chandra, P. [National Centre for Radio Astrophysics, Tata Institute of Fundamental Research, Pune University Campus, Ganeshkhind, Pune 411007 (India); Castro-Tirado, A. J. [Instituto de Astrofisica de Andalucia (IAA-CSIC), P.O. Box 03004, E-18080 Granada (Spain); Bremer, M. [Institut de Radioastronomie Millimetrique, 300 rue de la Piscine, F-38406 Saint Martin d'Heres (France); and others

    2013-04-20

    We present X-ray, optical, near-infrared (IR), and radio observations of gamma-ray bursts (GRBs) 110709B and 111215A, as well as optical and near-IR observations of their host galaxies. The combination of X-ray detections and deep optical/near-IR limits establish both bursts as ''dark''. Sub-arcsecond positions enabled by radio detections lead to robust host galaxy associations, with optical detections that indicate z {approx}< 4 (110709B) and z Almost-Equal-To 1.8-2.9 (111215A). We therefore conclude that both bursts are dark due to substantial rest-frame extinction. Using the radio and X-ray data for each burst we find that GRB 110709B requires A{sub V}{sup host}{approx}>5.3 mag and GRB 111215A requires A{sub V}{sup host}{approx}>8.5 mag (assuming z = 2). These are among the largest extinction values inferred for dark bursts to date. The two bursts also exhibit large neutral hydrogen column densities of N{sub H,{sub int}} {approx}> 10{sup 22} cm{sup -2} (z = 2) as inferred from their X-ray spectra, in agreement with the trend for dark GRBs. Moreover, the inferred values are in agreement with the Galactic A{sub V} -N{sub H} relation, unlike the bulk of the GRB population. Finally, we find that for both bursts the afterglow emission is best explained by a collimated outflow with a total beaming-corrected energy of E{sub {gamma}} + E{sub K} Almost-Equal-To (7-9) Multiplication-Sign 10{sup 51} erg (z = 2) expanding into a wind medium with a high density, M Almost-Equal-To (6-20) Multiplication-Sign 10{sup -5} M{sub Sun} yr{sup -1} (n Almost-Equal-To 100-350 cm{sup -3} at Almost-Equal-To 10{sup 17} cm). While the energy release is typical of long GRBs, the inferred density may be indicative of larger mass-loss rates for GRB progenitors in dusty (and hence metal rich) environments. This study establishes the critical role of radio observations in demonstrating the origin and properties of dark GRBs. Observations with the JVLA and ALMA will provide a sample with sub-arcsecond positions and robust host associations that will help to shed light on obscured star formation and the role of metallicity in GRB progenitors.

  14. The secret lives of Cepheids: evolutionary changes and pulsation-induced shock heating in the prototype classical Cepheid ? Cep

    SciTech Connect (OSTI)

    Engle, Scott G.; Guinan, Edward F. [Department of Astrophysics and Planetary Science, Villanova University, Villanova, PA 19085 (United States); Harper, Graham M. [School of Physics, Trinity College Dublin, College Green, Dublin 2 (Ireland); Neilson, Hilding R. [Department of Physics and Astronomy, East Tennessee State University, Box 70652, Johnson City, TN 37614 (United States); Evans, Nancy Remage, E-mail: scott.engle@villanova.edu [Smithsonian Astrophysical Observatory, MS 4, 60 Garden Street, Cambridge, MA 02138 (United States)

    2014-10-10

    Over the past decade, the Secret Lives of Cepheids (SLiC) program has been carried out at Villanova University to study aspects and behaviors of classical Cepheids that are still not well understood. In this, the first of several planned papers on program Cepheids, we report the current results for ? Cep, the Cepheid prototype. Ongoing photometry has been obtained to search for changes in the pulsation period, light-curve morphology, and amplitude. Combining our photometry with the times of maximum light compilation by Berdnikov et al. returns a small period change of dP/dt ?0.1006 0.0002 s yr{sup -1}. There is also evidence for a gradual light amplitude increase of ?0.011 mag (V band) and ?0.012 mag (B band) per decade over the last ?50 years. In addition, Hubble Space Telescope (HST) Cosmic Origins Spectrograph (COS) UV spectrophotometry and XMM-Newton X-ray data were carried out to investigate the high-temperature plasmas present above the Cepheid photospheres. In total, from the five visits (eight exposures) with XMM-Newton, ? Cep is found to be a soft X-ray source (L {sub X} (0.3-2 keV) ?4.5-13 10{sup 28} erg s{sup -1}) with peak flux at kT = 0.6-0.9 keV. The X-ray activity is found to vary, possibly in phase with the stellar pulsations. From 2010-2013, nine observations of ? Cep were carried out with HST-COS. The UV emissions are also variable and well phased with the stellar pulsations. Maximum UV line emissions occur near, or slightly before, maximum optical light, varying by as much as 20 times. This variability shows that pulsation-induced shock heating plays a significant role in Cepheid atmospheres, possibly in addition to a quiescent, magnetic heating. The results of this study show Cepheid atmospheres to be rather complex and dynamic.

  15. THE HST/ACS COMA CLUSTER SURVEY. II. DATA DESCRIPTION AND SOURCE CATALOGS

    SciTech Connect (OSTI)

    Hammer, Derek; Verdoes Kleijn, Gijs; Den Brok, Mark; Peletier, Reynier F.; Hoyos, Carlos; Balcells, Marc; Aguerri, Alfonso L.; Ferguson, Henry C.; Goudfrooij, Paul; Carter, David; Guzman, Rafael; Smith, Russell J.; Lucey, John R.; Graham, Alister W.; Trentham, Neil; Peng, Eric; Puzia, Thomas H.; Jogee, Shardha; Batcheldor, Dan; Bridges, Terry J.

    2010-11-15

    The Coma cluster, Abell 1656, was the target of an HST-ACS Treasury program designed for deep imaging in the F475W and F814W passbands. Although our survey was interrupted by the ACS instrument failure in early 2007, the partially completed survey still covers {approx}50% of the core high-density region in Coma. Observations were performed for 25 fields that extend over a wide range of cluster-centric radii ({approx}1.75 Mpc or 1{sup 0}) with a total coverage area of 274 arcmin{sup 2}. The majority of the fields are located near the core region of Coma (19/25 pointings) with six additional fields in the southwest region of the cluster. In this paper, we present reprocessed images and SEXTRACTOR source catalogs for our survey fields, including a detailed description of the methodology used for object detection and photometry, the subtraction of bright galaxies to measure faint underlying objects, and the use of simulations to assess the photometric accuracy and completeness of our catalogs. We also use simulations to perform aperture corrections for the SEXTRACTOR Kron magnitudes based only on the measured source flux and its half-light radius. We have performed photometry for {approx}73,000 unique objects; approximately one-half of our detections are brighter than the 10{sigma} point-source detection limit at F814W = 25.8 mag (AB). The slight majority of objects (60%) are unresolved or only marginally resolved by ACS. We estimate that Coma members are 5%-10% of all source detections, which consist of a large population of unresolved compact sources (primarily globular clusters but also ultra-compact dwarf galaxies) and a wide variety of extended galaxies from a cD galaxy to dwarf low surface brightness galaxies. The red sequence of Coma member galaxies has a color-magnitude relation with a constant slope and dispersion over 9 mag (-21 < M {sub F814W} < -13). The initial data release for the HST-ACS Coma Treasury program was made available to the public in 2008 August. The images and catalogs described in this study relate to our second data release.

  16. ULTRA STEEP SPECTRUM RADIO SOURCES IN THE LOCKMAN HOLE: SERVS IDENTIFICATIONS AND REDSHIFT DISTRIBUTION AT THE FAINTEST RADIO FLUXES

    SciTech Connect (OSTI)

    Afonso, J.; Bizzocchi, L.; Grossi, M.; Messias, H.; Fernandes, C. A. C.; Ibar, E.; Ivison, R. J.; Simpson, C.; Chapman, S.; Gonzalez-Solares, E.; Jarvis, M. J.; Rottgering, H.; Norris, R. P.; Dunlop, J.; Best, P.; Pforr, J.; Vaccari, M.; Seymour, N.; Farrah, D.; Huang, J.-S.; and others

    2011-12-20

    Ultra steep spectrum (USS) radio sources have been successfully used to select powerful radio sources at high redshifts (z {approx}> 2). Typically restricted to large-sky surveys and relatively bright radio flux densities, it has gradually become possible to extend the USS search to sub-mJy levels, thanks to the recent appearance of sensitive low-frequency radio facilities. Here a first detailed analysis of the nature of the faintest USS sources is presented. By using Giant Metrewave Radio Telescope and Very Large Array radio observations of the Lockman Hole at 610 MHz and 1.4 GHz, a sample of 58 USS sources, with 610 MHz integrated fluxes above 100 {mu}Jy, is assembled. Deep infrared data at 3.6 and 4.5 {mu}m from the Spitzer Extragalactic Representative Volume Survey (SERVS) are used to reliably identify counterparts for 48 (83%) of these sources, showing an average total magnitude of [3.6]{sub AB} = 19.8 mag. Spectroscopic redshifts for 14 USS sources, together with photometric redshift estimates, improved by the use of the deep SERVS data, for a further 19 objects, show redshifts ranging from z = 0.1 to z = 2.8, peaking at z {approx} 0.6 and tailing off at high redshifts. The remaining 25 USS sources, with no redshift estimate, include the faintest [3.6] magnitudes, with 10 sources undetected at 3.6 and 4.5 {mu}m (typically [3.6] {approx}> 22-23 mag from local measurements), which suggests the likely existence of higher redshifts among the sub-mJy USS population. The comparison with the Square Kilometre Array Design Studies Simulated Skies models indicates that Fanaroff-Riley type I radio sources and radio-quiet active galactic nuclei may constitute the bulk of the faintest USS population, and raises the possibility that the high efficiency of the USS technique for the selection of high-redshift sources remains even at the sub-mJy level.

  17. THE GEMINI/NICI PLANET-FINDING CAMPAIGN: THE FREQUENCY OF PLANETS AROUND YOUNG MOVING GROUP STARS

    SciTech Connect (OSTI)

    Biller, Beth A.; Ftaclas, Christ; Liu, Michael C.; Wahhaj, Zahed; Nielsen, Eric L.; Hayward, Thomas L.; Hartung, Markus; Chun, Mark; Clarke, Fraser; Thatte, Niranjan; Shkolnik, Evgenya L.; Reid, I. Neill; Boss, Alan; Lin, Douglas; Alencar, Silvia H. P.; De Gouveia Dal Pino, Elisabete; Gregorio-Hetem, Jane [Universidade de Sao Paulo, IAG and others

    2013-11-10

    We report results of a direct imaging survey for giant planets around 80 members of the β Pic, TW Hya, Tucana-Horologium, AB Dor, and Hercules-Lyra moving groups, observed as part of the Gemini/NICI Planet-Finding Campaign. For this sample, we obtained median contrasts of ΔH = 13.9 mag at 1'' in combined CH{sub 4} narrowband ADI+SDI mode and median contrasts of ΔH = 15.1 mag at 2'' in H-band ADI mode. We found numerous (>70) candidate companions in our survey images. Some of these candidates were rejected as common-proper motion companions using archival data; we reobserved with Near-Infrared Coronagraphic Imager (NICI) all other candidates that lay within 400 AU of the star and were not in dense stellar fields. The vast majority of candidate companions were confirmed as background objects from archival observations and/or dedicated NICI Campaign followup. Four co-moving companions of brown dwarf or stellar mass were discovered in this moving group sample: PZ Tel B (36 ± 6 M{sub Jup}, 16.4 ± 1.0 AU), CD–35 2722B (31 ± 8 M{sub Jup}, 67 ± 4 AU), HD 12894B (0.46 ± 0.08 M{sub ☉}, 15.7 ± 1.0 AU), and BD+07 1919C (0.20 ± 0.03 M{sub ☉}, 12.5 ± 1.4 AU). From a Bayesian analysis of the achieved H band ADI and ASDI contrasts, using power-law models of planet distributions and hot-start evolutionary models, we restrict the frequency of 1-20 M{sub Jup} companions at semi-major axes from 10-150 AU to <18% at a 95.4% confidence level using DUSTY models and to <6% at a 95.4% using COND models. Our results strongly constrain the frequency of planets within semi-major axes of 50 AU as well. We restrict the frequency of 1-20 M{sub Jup} companions at semi-major axes from 10-50 AU to <21% at a 95.4% confidence level using DUSTY models and to <7% at a 95.4% using COND models. This survey is the deepest search to date for giant planets around young moving group stars.

  18. THE GEMINI PLANET-FINDING CAMPAIGN: THE FREQUENCY OF GIANT PLANETS AROUND DEBRIS DISK STARS

    SciTech Connect (OSTI)

    Wahhaj, Zahed; Liu, Michael C.; Nielsen, Eric L.; Ftaclas, Christ; Chun, Mark; Biller, Beth A.; Hayward, Thomas L.; Thatte, Niranjan; Tecza, Matthias; Shkolnik, Evgenya L.; Kuchner, Marc; Reid, I. Neill; De Gouveia Dal Pino, Elisabete M.; Gregorio-Hetem, Jane; Boss, Alan; Lin, Douglas N. C.; and others

    2013-08-20

    We have completed a high-contrast direct imaging survey for giant planets around 57 debris disk stars as part of the Gemini NICI Planet-Finding Campaign. We achieved median H-band contrasts of 12.4 mag at 0.''5 and 14.1 mag at 1'' separation. Follow-up observations of the 66 candidates with projected separation <500 AU show that all of them are background objects. To establish statistical constraints on the underlying giant planet population based on our imaging data, we have developed a new Bayesian formalism that incorporates (1) non-detections, (2) single-epoch candidates, (3) astrometric and (4) photometric information, and (5) the possibility of multiple planets per star to constrain the planet population. Our formalism allows us to include in our analysis the previously known {beta} Pictoris and the HR 8799 planets. Our results show at 95% confidence that <13% of debris disk stars have a {>=}5 M{sub Jup} planet beyond 80 AU, and <21% of debris disk stars have a {>=}3 M{sub Jup} planet outside of 40 AU, based on hot-start evolutionary models. We model the population of directly imaged planets as d {sup 2} N/dMda{proportional_to}m {sup {alpha}} a {sup {beta}}, where m is planet mass and a is orbital semi-major axis (with a maximum value of a{sub max}). We find that {beta} < -0.8 and/or {alpha} > 1.7. Likewise, we find that {beta} < -0.8 and/or a{sub max} < 200 AU. For the case where the planet frequency rises sharply with mass ({alpha} > 1.7), this occurs because all the planets detected to date have masses above 5 M{sub Jup}, but planets of lower mass could easily have been detected by our search. If we ignore the {beta} Pic and HR 8799 planets (should they belong to a rare and distinct group), we find that <20% of debris disk stars have a {>=}3 M{sub Jup} planet beyond 10 AU, and {beta} < -0.8 and/or {alpha} < -1.5. Likewise, {beta} < -0.8 and/or a{sub max} < 125 AU. Our Bayesian constraints are not strong enough to reveal any dependence of the planet frequency on stellar host mass. Studies of transition disks have suggested that about 20% of stars are undergoing planet formation; our non-detections at large separations show that planets with orbital separation >40 AU and planet masses >3 M{sub Jup} do not carve the central holes in these disks.

  19. EXPLORING THE VARIABLE SKY WITH LINEAR. III. CLASSIFICATION OF PERIODIC LIGHT CURVES

    SciTech Connect (OSTI)

    Palaversa, Lovro; Eyer, Laurent; Rimoldini, Lorenzo; Ivezi?, eljko; Loebman, Sarah; Hunt-Walker, Nicholas; VanderPlas, Jacob; Westman, David; Becker, Andrew C.; Rudjak, Domagoj; Sudar, Davor; Boi?, Hrvoje; Galin, Mario; Kroflin, Andrea; Mesari?, Martina; Munk, Petra; Vrbanec, Dijana; Sesar, Branimir; Stuart, J. Scott; Srdo?, Gregor; and others

    2013-10-01

    We describe the construction of a highly reliable sample of ?7000 optically faint periodic variable stars with light curves obtained by the asteroid survey LINEAR across 10,000 deg{sup 2} of the northern sky. The majority of these variables have not been cataloged yet. The sample flux limit is several magnitudes fainter than most other wide-angle surveys; the photometric errors range from ?0.03 mag at r = 15 to ?0.20 mag at r = 18. Light curves include on average 250 data points, collected over about a decade. Using Sloan Digital Sky Survey (SDSS) based photometric recalibration of the LINEAR data for about 25 million objects, we selected ?200,000 most probable candidate variables with r < 17 and visually confirmed and classified ?7000 periodic variables using phased light curves. The reliability and uniformity of visual classification across eight human classifiers was calibrated and tested using a catalog of variable stars from the SDSS Stripe 82 region and verified using an unsupervised machine learning approach. The resulting sample of periodic LINEAR variables is dominated by 3900 RR Lyrae stars and 2700 eclipsing binary stars of all subtypes and includes small fractions of relatively rare populations such as asymptotic giant branch stars and SX Phoenicis stars. We discuss the distribution of these mostly uncataloged variables in various diagrams constructed with optical-to-infrared SDSS, Two Micron All Sky Survey, and Wide-field Infrared Survey Explorer photometry, and with LINEAR light-curve features. We find that the combination of light-curve features and colors enables classification schemes much more powerful than when colors or light curves are each used separately. An interesting side result is a robust and precise quantitative description of a strong correlation between the light-curve period and color/spectral type for close and contact eclipsing binary stars (? Lyrae and W UMa): as the color-based spectral type varies from K4 to F5, the median period increases from 5.9 hr to 8.8 hr. These large samples of robustly classified variable stars will enable detailed statistical studies of the Galactic structure and physics of binary and other stars and we make these samples publicly available.

  20. The hydrogen-poor superluminous supernova iPTF 13ajg and its host galaxy in absorption and emission

    SciTech Connect (OSTI)

    Vreeswijk, Paul M.; Gal-Yam, Avishay; De Cia, Annalisa; Rubin, Adam; Yaron, Ofer; Tal, David; Ofek, Eran O.; Savaglio, Sandra; Quimby, Robert M.; Sullivan, Mark; Cenko, S. Bradley; Filippenko, Alexei V.; Clubb, Kelsey I.; Perley, Daniel A.; Cao, Yi; Taddia, Francesco; Sollerman, Jesper; Leloudas, Giorgos; Arcavi, Iair; Kasliwal, Mansi M.; and others

    2014-12-10

    We present imaging and spectroscopy of a hydrogen-poor superluminous supernova (SLSN) discovered by the intermediate Palomar Transient Factory, iPTF 13ajg. At a redshift of z = 0.7403, derived from narrow absorption lines, iPTF 13ajg peaked at an absolute magnitude of M {sub u,} {sub AB} = 22.5, one of the most luminous supernovae to date. The observed bolometric peak luminosity of iPTF 13ajg is 3.2 10{sup 44} erg s{sup 1}, while the estimated total radiated energy is 1.3 10{sup 51} erg. We detect narrow absorption lines of Mg I, Mg II, and Fe II, associated with the cold interstellar medium in the host galaxy, at two different epochs with X-shooter at the Very Large Telescope. From Voigt profile fitting, we derive the column densities log N(Mg I) =11.94 0.06, log N(Mg II) =14.7 0.3, and log N(Fe II) =14.25 0.10. These column densities, as well as the Mg I and Mg II equivalent widths of a sample of hydrogen-poor SLSNe taken from the literature, are at the low end of those derived for gamma-ray bursts (GRBs) whose progenitors are also thought to be massive stars. This suggests that the environments of hydrogen-poor SLSNe and GRBs are different. From the nondetection of Fe II fine-structure absorption lines, we derive a lower limit on the distance between the supernova and the narrow-line absorbing gas of 50 pc. The neutral gas responsible for the absorption in iPTF 13ajg exhibits a single narrow component with a low velocity width, ?V = 76 km s{sup 1}, indicating a low-mass host galaxy. No host galaxy emission lines are detected, leading to an upper limit on the unobscured star formation rate (SFR) of SFR{sub [O} {sub II]}<0.07M{sub ?}yr{sup ?1}. Late-time imaging shows the iPTF 13ajg host galaxy to be faint, with g {sub AB} ? 27.0 and R {sub AB} ? 26.0 mag, corresponding to M {sub B,} {sub Vega} ? 17.7 mag.

  1. BPA-2013-01256-FOIA Request

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

    M1C1-Ti SSQcJTES, RC. AttojrneyN at.Law RECEIVED BY tWA FOIA OFFICE TillS DATE - 1143 DUE DATE: OF COUNS 6L 0014 5. KATES bATneonow4b. WA RuTh P HARING IL&Tri5w fri. HC'RDCZIcO Ws...

  2. Exceptional damage-tolerance of a medium-entropy alloy CrCoNi at cryogenic temperatures

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

    Gludovatz, Bernd; Hohenwarter, Anton; Thurston, Keli V. S.; Bei, Hongbin; Wu, Zhenggang; George, Easo P.; Ritchie, Robert O.

    2016-02-02

    The high-entropy alloys are an intriguing new class of metallic materials that derive their properties not from a single dominant constituent, such as iron in steels, nor from the presence of a second phase, such as in nickel-base superalloys, but rather comprise multi-element systems that crystallize as a single phase, despite containing high concentrations (~20 at.%) of five or more elements with different crystal structures. Indeed, we have recently reported on one such single-phase high-entropy alloy, NiCoCrFeMn, which displays exceptional strength and toughness at cryogenic temperatures. Here which displays unprecedented strength-toughness properties that exceed those of all high-entropy alloys andmore » most multi-phase alloys. With roomtemperature tensile strengths of almost 1 GPa and KJIc fracture-toughness values above 200 MPa.m 1/2 (with crack-growth toughnesses exceeding 300 MPa.m 1/2), the strength, ductility and toughness of the NiCoCr alloy actually improve at cryogenic temperatures to unprecedented levels of strengths above 1.3 GPa, failure strains up to 90% and KJIc values of 275 MPa.m 1/2 (with crackgrowth toughnesses above 400 MPa.m 1/2). These properties appear to result from continuous steady strain hardening, which acts to suppress plastic instability, resulting from pronounced dislocation activity and deformation-induced nano-twinning.« less

  3. Exceptional damage-tolerance of a medium-entropy alloy NiCoCr at cryogenic temperatures

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

    Gludovatz, Bernd; Hohenwarter, Anton; Thurston, Keli; Bei, Hongbin; Wu, Zhenggang; George, Easo

    2016-01-01

    High-entropy alloys1 3 are an intriguing new class of metallic materials that derive their properties not from a single dominant constituent, such as iron in steels, nor from the presence of a second phase, such as in nickel-base superalloys, but rather comprise multi-element systems that crystallize as a single phase4 7, despite containing high concentrations (~20 at.%) of five or more elements with different crystal structures5 7. Indeed, we have recently reported on one such single-phase high-entropy alloy, NiCoCrFeMn, which displays exceptional strength and toughness at cryogenic temperatures8. Here which displays unprecedented strength-toughness properties that exceed those of all high-entropymore »alloys and most multi-phase alloys. With roomtemperature tensile strengths of almost 1 GPa and KJIc fracture-toughness values above 200 MPa.m1/2 (with crack-growth toughnesses exceeding 300 MPa.m1/2), the strength, ductility and toughness of the NiCoCr alloy actually improve at cryogenic temperatures to unprecedented levels of strengths above 1.3 GPa, failure strains up to 90% and KJIc values of 275 MPa.m1/2 (with crackgrowth toughnesses above 400 MPa.m1/2). Such properties appear to result from continuous steady strain hardening, which acts to suppress plastic instability, resulting from pronounced dislocation activity and deformation-induced nano-twinning.« less

  4. Beamline 29-ID

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

    sided bounce Mirror (M1) 31.3 m Heat-sink, side bounce Monochromater (M2, LEG, MEG, HEG) 39.7 m In-Focus VLS-PGM Exit Slit 59.7 m Both RSXS and ARPES branchlines Mirror...

  5. Cours-VIII/Clavin2015.key

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

    instability u aI < u a < u aII acoustic velocity a kd L u a U L Re-stabilization tongue unstable wavelengths u 2 aI 2 b ( b + 1) ( b 1) 1 U Lc U L , k I k m 1 2 U Lc U L u...

  6. Property:AvgReservoirDepth | Open Energy Information

    Open Energy Info (EERE)

    yd + Amedee Geothermal Area + 213 m0.213 km 0.132 mi 698.819 ft 232.939 yd + B Bac-Man Laguna Geothermal Area + 1,500 m1.5 km 0.932 mi 4,921.26 ft 1,640.415 yd + Bad Blumau...

  7. 19_27_1995.tex

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

    ns g -0.296 0.003 4, 5, 7, 10, 11, 13, 14 0.27509 0.13 1 2 - 1 2 - m 61.4 3.0 ps 4, 5, 7, 10, 13 1.50756 0.3 5 2 - 1 2 - m 1.4 +0.5 -0.6 ps 4, 5,...

  8. 19_02_1995.tex

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

    3, 4, 7, 8, 9, 10 g -0.48 0.06 1.4717 0.4 1 2 + m 1.27 0.17 ps 3, 4, 7, 8 2.3715 1.0 9 2 + m > 3.5 ps 3, 4, 7 2.7790 0.9 7 2 + m 93 19...

  9. EGG-GTH-5775 J

    Office of Scientific and Technical Information (OSTI)

    r a t e can also be determined from a mass balance around the a i r stream: E (H2 - HI) G In this case, M 1.26 (H2 - H1) + .002 L 7 This second method of determining the...

  10. Soda Lake Geothermal Area | Open Energy Information

    Open Energy Info (EERE)

    of Reservoir: 1219 m1.219 km 0.757 mi 3,999.344 ft 1,333.111 yd 1 Average Depth to Reservoir: 762 m0.762 km 0.473 mi 2,500 ft 833.331 yd Use the "Edit with Form" button at...

  11. Section M: Evaluations Factors for Award

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

    V SECTION M EVALUATION FACTORS FOR AWARD Request for Proposal # DE-RP36-07GO97036 PART V SECTION M EVALUATION FACTORS FOR AWARD TABLE OF CONTENTS M.1 Evaluation of Proposals ..........................................................................................1 M.2 Evaluation Criteria..................................................................................................1 M.3 Basis For Award

  12. Search for: All records | SciTech Connect

    Office of Scientific and Technical Information (OSTI)

    S A (1) Montagna, J (1) Panek, A F (1) Parker, K M (1) Podolski, W F (1) Shearer, J (1) Smith, G W (1) Smyk, E B (1) Snyder, R (1) Swift, W (1) Save Results Save this search to My...

  13. 20_17_1998.tex

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

    2 + ; 0 0 + 1 m 1.05 0.06 ps g +0.54 0.04 3, 4, 8, 9, 12, 14, 16, 19, 20, 22, 23, 24, 27, 28, 29, 33, 34, 35, 36, 37, 39, 40, 46, 47, 48, 49, 52, 53, 55, 58, 59,...

  14. Silver (Ag) Transport Mechanisms in TRISO Coated Particles: A Critical Review

    SciTech Connect (OSTI)

    IJ van Rooyen; ML Dunzik-Gougar; PM van Rooyen

    2014-05-01

    Transport of 110mAg in the intact SiC layer of TRISO coated particles has been studied for approximately 30 years without arriving at a satisfactory explanation of the transport mechanism. In this paper the possible mechanisms postulated in previous experimental studies, both in-reactor and out-of reactor research environment studies are critically reviewed and of particular interest are relevance to very high temperature gas reactor operating and accident conditions. Among the factors thought to influence Ag transport are grain boundary stoichiometry, SiC grain size and shape, the presence of free silicon, nano-cracks, thermal decomposition, palladium attack, transmutation products, layer thinning and coated particle shape. Additionally new insight to nature and location of fission products has been gained via recent post irradiation electron microscopy examination of TRISO coated particles from the DOEs fuel development program. The combined effect of critical review and new analyses indicates a direction for investigating possible the Ag transport mechanism including the confidence level with which these mechanisms may be experimentally verified.

  15. Photometric and structural properties of NGC 6544: A combined VVV-Hubble space telescope study

    SciTech Connect (OSTI)

    Cohen, Roger E.; Mauro, Francesco; Geisler, Doug; Moni Bidin, Christian; Dotter, Aaron; Bonatto, Charles

    2014-07-01

    We combine archival Hubble Space Telescope imaging with wide-field near-infrared photometry to study the neglected metal-poor Galactic globular cluster NGC 6544. A high spatial resolution map of differential reddening over the inner portion of the cluster is constructed, revealing variations of up to half of the total reddening, and the resulting corrected color-magnitude diagrams reveal a sparse blue horizontal branch and centrally concentrated blue straggler population, verified via relative proper motions. Using the corrected photometry to investigate the cluster distance, reddening, and age via direct comparison to well-calibrated photometry of clusters with similar metallicities, we estimate (m M){sub 0} = 11.96, E(B V) = 0.79, and an age coeval with M13 to within the relevant uncertainties. Although our data are insufficient to place tight constraints on the reddening law toward NGC 6544, we find no strong evidence that it is non-standard at optical or near-infrared wavelengths. We also provide near-infrared fiducial sequences extending nearly 2 mag below the cluster main sequence turnoff, generated from a statistically decontaminated sample of cluster stars. Lastly, we redetermine the cluster center and construct a radial number density profile which is well fit by an atypically flat power law with a slope of about 1.7. We discuss this result, together with a flattened main sequence luminosity function and inverted mass function, in the context of mass segregation and tidal stripping via interactions with Milky Way potential.

  16. DOUBLE HORIZONTAL BRANCHES IN NGC 6440 AND NGC 6569 UNVEILED BY THE VVV SURVEY

    SciTech Connect (OSTI)

    Mauro, Francesco; Bidin, Christian Moni; Cohen, Roger; Geisler, Doug; Chene, Andre-Nicolas; Villanova, Sandro; Minniti, Dante; Catelan, Marcio

    2012-12-20

    We report the discovery of a peculiar horizontal branch (HB) in NGC 6440 and NGC 6569, two massive and metal-rich Galactic globular clusters (GGCs) located in the Galactic bulge, within 4 kpc from the Galactic center. In both clusters, two distinct clumps are detected at the level of the cluster HB, separated by only {approx}0.1 mag in the K{sub s} band. They were detected with IR photometric data collected with the 'VISTA Variables in the Via Lactea' Survey, and confirmed in independent IR catalogs available in the literature and Hubble Space Telescope optical photometry. Our analysis demonstrates that these clumps are real cluster features, not a product of field contamination or interstellar reddening. The observed split HBs could be a signature of two stellar sub-populations with different chemical composition and/or age, as recently found in Terzan 5, but it cannot be excluded that they are caused by evolutionary effects, in particular for NGC 6440. This interpretation, however, requires an anomalously high helium content (Y > 0.30). Our discovery suggests that such a peculiar HB morphology could be a common feature of massive, metal-rich bulge GGCs.

  17. Lipidomic Analysis of Endocannabinoid Signaling: Targeted Metabolite Identification and Quantification

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

    Keereetaweep, Jantana; Chapman, Kent D.

    2016-01-01

    The endocannabinoids N -arachidonoylethanolamide (or anandamide, AEA) and 2-arachidonoylglycerol (2-AG) belong to the larger groups of N -acylethanolamines (NAEs) and monoacylglycerol (MAG) lipid classes, respectively. They are biologically active lipid molecules that activate G-protein-coupled cannabinoid receptors found in various organisms. After AEA and 2-AG were discovered in the 1990s, they have been extensively documented to have a broad range of physiological functions. Along with AEA, several NAEs, for example, N -palmitoylethanolamine (PEA), N -stearoylethanolamine (SEA), and N -oleoylethanolamine (OEA) are also present in tissues, usually at much larger concentrations than AEA. Any perturbation that involves the endocannabinoid pathway maymore » subsequently alter basal level or metabolism of these lipid mediators. Further, the altered levels of these molecules often reflect pathological conditions associated with tissue damage. Robust and sensitive methodologies to analyze these lipid mediators are essential to understanding how they act as endocannabinoids. The recent advances in mass spectrometry allow researchers to develop lipidomics approaches and several methodologies have been proposed to quantify endocannabinoids in various biological systems.« less

  18. DISCOVERY OF A NEW MEMBER OF THE INNER OORT CLOUD FROM THE NEXT GENERATION VIRGO CLUSTER SURVEY

    SciTech Connect (OSTI)

    Chen, Ying-Tung; Ip, Wing-Huen; Kavelaars, J. J.; Gwyn, Stephen; Ferrarese, Laura; Ct, Patrick; Jordn, Andrs; Suc, Vincent; Cuillandre, Jean-Charles

    2013-09-20

    We report the discovery of 2010 GB{sub 174}, a likely new member of the Inner Oort Cloud (IOC). 2010 GB{sub 174} is 1 of 91 trans-Neptunian objects and Centaurs discovered in a 76 deg{sup 2} contiguous region imaged as part of the Next Generation Virgo Cluster Survey (NGVS)a moderate ecliptic latitude survey reaching a mean limiting magnitude of g' ? 25.5using MegaPrime on the 3.6 m Canada-France-Hawaii Telescope. 2010 GB{sub 174} is found to have an orbit with a semi-major axis of a ? 350.8 AU, an inclination of i ? 21.6, and a pericenter of q ? 48.5 AU. This is the second largest perihelion distance among known solar system objects. Based on the sky coverage and depth of the NGVS, we estimate the number of IOC members with sizes larger than 300 km (H{sub V} ? 6.2 mag) to be ? 11, 000. A comparison of the detection rate from the NGVS and the PDSSS (a characterized survey that 'rediscovered' the IOC object Sedna) gives, for an assumed a power-law luminosity function for IOC objects, a slope of ? ? 0.7 0.2. With only two detections in this region this slope estimate is highly uncertain.

  19. THE DISTRIBUTION OF FAINT SATELLITES AROUND CENTRAL GALAXIES IN THE CANADA-FRANCE-HAWAII TELESCOPE LEGACY SURVEY

    SciTech Connect (OSTI)

    Jiang, C. Y.; Jing, Y. P.; Li, Cheng

    2012-11-20

    We investigate the radial number density profile and the abundance distribution of faint satellites around central galaxies in the low-redshift universe using the Canada-France-Hawaii Telescope (CFHT) Legacy Survey. We consider three samples of central galaxies with magnitudes of M {sub r} = -21, -22, and -23 selected from the Sloan Digital Sky Survey group catalog of Yang et al. The satellite distribution around these central galaxies is obtained by cross-correlating these galaxies with the photometric catalog of the CFHT Legacy Survey. The projected radial number density of the satellites obeys a power-law form with the best-fit logarithmic slope of -1.05, independent of both the central galaxy luminosity and the satellite luminosity. The projected cross-correlation function between central and satellite galaxies exhibits a non-monotonic trend with satellite luminosity. It is most pronounced for central galaxies with M {sub r} = -21, where the decreasing trend of clustering amplitude with satellite luminosity is reversed when satellites are fainter than central galaxies by more than 2 mag. A comparison with the satellite luminosity functions in the Milky Way (MW) and M31 shows that the MW/M31 system has about twice as many satellites as around a typical central galaxy of similar luminosity. The implications for theoretical models are briefly discussed.

  20. OzDES multifibre spectroscopy for the Dark Energy Survey: First-year operation and results

    SciTech Connect (OSTI)

    Yuan, Fang

    2015-07-29

    The Australian Dark Energy Survey (OzDES) is a five-year, 100-night, spectroscopic survey on the Anglo-Australian Telescope, whose primary aim is to measure redshifts of approximately 2500 Type Ia supernovae host galaxies over the redshift range 0.1 < z < 1.2, and derive reverberation-mapped black hole masses for approximately 500 active galactic nuclei and quasars over 0.3 < z < 4.5. This treasure trove of data forms a major part of the spectroscopic follow-up for the Dark Energy Survey for which we are also targeting cluster galaxies, radio galaxies, strong lenses, and unidentified transients, as well as measuring luminous red galaxies and emission line galaxies to help calibrate photometric redshifts. Here, we present an overview of the OzDES programme and our first-year results. Between 2012 December and 2013 December, we observed over 10 000 objects and measured more than 6 000 redshifts. Our strategy of retargeting faint objects across many observing runs has allowed us to measure redshifts for galaxies as faint as mr = 25 mag. We outline our target selection and observing strategy, quantify the redshift success rate for different types of targets, and discuss the implications for our main science goals. In conclusion, we highlight a few interesting objects as examples of the fortuitous yet not totally unexpected discoveries that can come from such a large spectroscopic survey.

  1. Probing the f-state configuration of URu2Si2 with U LIII-edge resonant x-ray absorption spectroscopy

    SciTech Connect (OSTI)

    Medling, S. A.; Booth, C. H.; Tobin, J. G.; Baumbach, R. E.; Bauer, E. D.; Sokaras, D.; Nordlund, D.; Weng, T. C.

    2015-09-05

    It has often been said that the most interesting ph- syics occurs when competing interactions are of nearly the same magnitude. Such a situation is surely oc- curing at URu2Si2’s so-called “hidden-order transition”, which garners its name from the missing entropy at a 17.5 K phase transition relative to that expected for a conventional antiferromagnetic phase transition, de- spite the presence of only a very small ordered mag- netic moment.? Despite this discrepancy being identi- fied in 1985, the identification of the order parameter remains elusive, although progress toward understand- ing this transition has been steady since that time, and URu2Si2 remains an important research subject today.? The work described below provides measures of the 5f orbital occupancy and itinerancy using resonant x-ray emission spectroscopy (RXES) at the U LIII absorption edge and measuring U L 1 emission that potentially acts as a dividing line between different classes of “hidden- order” theories.

  2. FAST OPTICAL VARIABILITY OF A NAKED-EYE BURST-MANIFESTATION OF THE PERIODIC ACTIVITY OF AN INTERNAL ENGINE

    SciTech Connect (OSTI)

    Beskin, G.; Karpov, S.; Bondar, S.; Greco, G.; Guarnieri, A.; Bartolini, C.; Piccioni, A.

    2010-08-10

    We imaged the position of the naked-eye burst, GRB080319B, before, during, and after its gamma-ray activity with sub-second temporal resolution using the TORTORA wide-field camera. The burst optical prompt emission, which reached 5.3 mag, has been detected, and its periodic optical variability has been discovered in the form of four equidistant flashes with a duration of several seconds. We also detected a strong correlation (r {approx} 0.82) between optical and gamma-ray light curves with a 2 s delay of the optical emission with respect to the gamma-ray emission. The revealed temporal structure of the optical light curve in comparison with the gamma-ray light curve can be interpreted in the framework of the model of shell collisions in the ejecta containing a significant neutron component. All observed emission features reflect the non-stationary behavior of the burst internal engine-supposedly, a hyperaccreting solar-mass black hole formed in the collapse of a massive stellar core.

  3. PERSEUS I: A DISTANT SATELLITE DWARF GALAXY OF ANDROMEDA

    SciTech Connect (OSTI)

    Martin, Nicolas F.; Laevens, Benjamin P. M.; Schlafly, Edward F.; Rix, Hans-Walter; Slater, Colin T.; Bell, Eric F.; Bernard, Edouard J.; Ferguson, Annette M. N.; Finkbeiner, Douglas P.; Burgett, William S.; Chambers, Kenneth C.; Hodapp, Klaus W.; Kaiser, Nicholas; Kudritzki, Rolf-Peter; Magnier, Eugene A.; Morgan, Jeffrey S.; Tonry, John L.; Draper, Peter W.; Metcalfe, Nigel; Price, Paul A.; and others

    2013-12-10

    We present the discovery of a new dwarf galaxy, Perseus I/Andromeda XXXIII, found in the vicinity of Andromeda (M31) in stacked imaging data from the Pan-STARRS1 3? survey. Located 27.9 away from M31, Perseus I has a heliocentric distance of 785 65 kpc, compatible with it being a satellite of M31 at 374{sub ?10}{sup +14} kpc from its host. The properties of Perseus I are typical for a reasonably bright dwarf galaxy (M{sub V} = 10.3 0.7), with an exponential half-light radius of r{sub h} = 1.7 0.4 arcmin or r{sub h}=400{sub ?85}{sup +105} pc at this distance, and a moderate ellipticity (?=0.43{sub ?0.17}{sup +0.15}). The late discovery of Perseus I is due to its fairly low surface brightness (?{sub 0}=25.7{sub ?0.9}{sup +1.0}magarcsec{sup 2}), and to the previous lack of deep, high quality photometric data in this region. If confirmed to be a companion of M31, the location of Perseus I, far east from its host, could place interesting constraints on the bulk motion of the satellite system of M31.

  4. Properties of M31. IV. Candidate luminous blue variables from PAndromeda

    SciTech Connect (OSTI)

    Lee, C.-H.; Seitz, S.; Kodric, M.; Riffeser, A.; Koppenhoefer, J.; Bender, R.; Snigula, J.; Hopp, U.; Gssl, C.; Bianchi, L.; Price, P. A.; Fraser, M.; Burgett, W.; Chambers, K. C.; Flewelling, H.; Kaiser, N.; Kudritzki, R.-P.; Magnier, E. A.; Draper, P. W.

    2014-04-10

    We perform a study on the optical and infrared photometric properties of known luminous blue variables (LBVs) in M31 using a sample of LBV candidates from the Local Group Galaxy Survey by Masset et al. We find that M31 LBV candidates show photometric variability ranging from 0.375 to 1.576 mag in r {sub P1} during a 3 yr time span observed by the Pan-STARRS 1 Andromeda survey (PAndromeda). Their near-infrared colors also follow the distribution of Galactic LBVs as shown by Oksala et al. We use these features as selection criteria to search for unknown LBV candidates in M31. We thus devise a method to search for candidate LBVs using both optical color from the Local Group Galaxy Survey and infrared color from the Two Micron All Sky Survey, as well as photometric variations observed by PAndromeda. We find four sources exhibiting common properties of known LBVs. These sources also exhibit UV emission as seen from Galaxy Evolution Explorer, which is one of the previously adopted methods of searching for LBV candidates. The locations of the LBVs are well aligned with M31 spiral arms as seen in UV light, suggesting that they are evolved stars at a young age given their high-mass nature. We compare these candidates with the latest Geneva evolutionary tracks, which show that our new M31 LBV candidates are massive, evolved stars with ages of 10-100 Myr.

  5. OzDES multifibre spectroscopy for the Dark Energy Survey: First-year operation and results

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

    Yuan, Fang

    2015-07-29

    The Australian Dark Energy Survey (OzDES) is a five-year, 100-night, spectroscopic survey on the Anglo-Australian Telescope, whose primary aim is to measure redshifts of approximately 2500 Type Ia supernovae host galaxies over the redshift range 0.1 < z < 1.2, and derive reverberation-mapped black hole masses for approximately 500 active galactic nuclei and quasars over 0.3 < z < 4.5. This treasure trove of data forms a major part of the spectroscopic follow-up for the Dark Energy Survey for which we are also targeting cluster galaxies, radio galaxies, strong lenses, and unidentified transients, as well as measuring luminous red galaxiesmore » and emission line galaxies to help calibrate photometric redshifts. Here, we present an overview of the OzDES programme and our first-year results. Between 2012 December and 2013 December, we observed over 10 000 objects and measured more than 6 000 redshifts. Our strategy of retargeting faint objects across many observing runs has allowed us to measure redshifts for galaxies as faint as mr = 25 mag. We outline our target selection and observing strategy, quantify the redshift success rate for different types of targets, and discuss the implications for our main science goals. In conclusion, we highlight a few interesting objects as examples of the fortuitous yet not totally unexpected discoveries that can come from such a large spectroscopic survey.« less

  6. DISCOVERY OF A NEW FAINT DWARF GALAXY ASSOCIATED WITH NGC253

    SciTech Connect (OSTI)

    Sand, D. J.; Crnojevi?, D.; Strader, J.; Toloba, E.; Guhathakurta, P.; Caldwell, N.; McLeod, B.; Seth, A. C.

    2014-09-20

    We report the discovery of a new faint dwarf galaxy, which we dub Scl-MM-Dw1, at a projected distance of ?65kpc from the spiral galaxy NGC253. The discovery results from the Panoramic Imaging Survey of Centaurus and Sculptor (PISCeS), a program with the Magellan/Megacam imager to study faint substructure in resolved stellar light around massive galaxies outside of the Local Group. We measure a tip of the red giant branch distance to Scl-MM-Dw1 of D=3.90.5Mpc, consistent with that of NGC253, making their association likely. The new dwarf's stellar population is complex, with an old, metal-poor red giant branch (?10Gyr, [Fe/H]?2), and an asymptotic giant branch with an age of ?500Myr. Scl-MM-Dw1 has a half-light radius of r{sub h} =34050pc and an absolute magnitude of M{sub V} = 10.30.6mag, comparable to the Milky Way's satellites at the same luminosity. Once complete, our imaging survey of NGC253 and other nearby massive galaxies will provide a census of faint substructure in halos beyond the Local Group, both to put our own environment into context and to confront models of hierarchical structure formation.

  7. THE DISCOVERY OF PULSATING HOT SUBDWARFS IN NGC 2808

    SciTech Connect (OSTI)

    Brown, Thomas M.; Landsman, Wayne B.; Randall, Suzanna K.; Sweigart, Allen V.; Lanz, Thierry E-mail: Wayne.Landsman@nasa.gov E-mail: allen.sweigart@gmail.com

    2013-11-10

    We present the results of a Hubble Space Telescope program to search for pulsating hot subdwarfs in the core of NGC 2808. These observations were motivated by the recent discovery of such stars in the outskirts of ? Cen. Both NGC 2808 and ? Cen are massive globular clusters exhibiting complex stellar populations and large numbers of extreme horizontal branch stars. Our far-UV photometric monitoring of over 100 hot evolved stars has revealed six pulsating subdwarfs with periods ranging from 85 to 149 s and UV amplitudes of 2.0%-6.8%. In the UV color-magnitude diagram of NGC 2808, all six of these stars lie immediately below the canonical horizontal branch, a region populated by the subluminous 'blue-hook' stars. For three of these six pulsators, we also have low-resolution far-UV spectroscopy that is sufficient to broadly constrain their atmospheric abundances and effective temperatures. Curiously, and in contrast to the ? Cen pulsators, the NGC 2808 pulsators do not exhibit the spectroscopic or photometric uniformity one might expect from a well-defined instability strip, although they all fall within a narrow band (0.2 mag) of far-UV luminosity.

  8. Crystal Field Disorder in the Quantum Spin Ice Ground State of Tb2Sn2 xTixO7

    SciTech Connect (OSTI)

    Gaulin, Bruce D.; Zhang, J.; Dahlberg, M. L.; Matthews, Maria J.; Bert, F.; Kermarrec, E.; Fritsch, Katharina; Granroth, Garrett E; Jiramongkolchai, P.; Amato, A.; Baines, C.; Cava, R. J.; Mendels, P.; Schiffer, P

    2015-01-01

    Spin ice physics marries that of hydrogen disorder in water ice, first discussed almost 60 years ago by Pauling, and that of low temperature magnetism on certain networks of connected tetrahedra. Recently the classical spin ice mag- nets Ho2Ti2O7 and Dy2Ti2O7 have shown an emergent artificial magneto- statics , which manifests itself as Coulombic spin correlations and excitations behaving as diffusive magnetic monopoles. The related pyrochlore magnet, Tb2Ti2O7, has been proposed as a quantum variant of spin ice, stabilized by 1 virtual excitations between the crystal field (CF) ground state doublet appro- priate to Tb3+, and its low lying excited state doublet. Isostructural Tb2Sn2O7 displays soft spin ice order, and its Tb3+ ground and excited CF eigenstates are known to differ relative to those of Tb2Ti2O7. We present a comprehensive study of Tb2Sn2 xTixO7 showing a novel, dynamic spin liquid state for all x other than the end members (0, 2). This state is the result of disorder in the low lying Tb3+ CF environments which de-stabilizes the mechanism by which quantum fluctuations contribute to ground state selection in Tb2Sn2 xTixO7.

  9. THE DWARF NOVA OUTBURSTS OF NOVA HER 1960 (=V446 HER)

    SciTech Connect (OSTI)

    Honeycutt, R. K.; Robertson, J. W.; Kafka, S. E-mail: jrobertson@atu.edu

    2011-04-15

    V446 Her is the best example of an old nova which has developed dwarf nova (DN) eruptions in the post-nova state. We report on observed properties of the long-term light curve of V446 Her, using photometry over 19 years. Yearly averages of the outburst (OB) magnitudes show a decline of {approx}0.013 mag yr{sup -1}, consistent with the decline of other post-novae that do not have DN OBs. Previous suggestions of bimodal distributions of the amplitudes and widths of the OBs are confirmed. The OBs occur at a mean spacing of 18 days but the range of spacings is large (13-30 days). From simulations of DN OBs, it has been predicted that the OB spacing in V446 Her will increase as M-dot from the red dwarf companion slowly falls following the nova; however, the large intrinsic scatter in the spacings serves to hide any evidence of this effect. We do find a systematic change in the OB pattern in which the brighter, wider type of OBs disappeared after late 2003, and this phenomenon is suggested to be due to falling M-dot following the nova.

  10. SIX HIGH-PRECISION TRANSITS OF OGLE-TR-113b

    SciTech Connect (OSTI)

    Adams, E. R.; Elliot, J. L.; Seager, S.; Lopez-Morales, M.; Osip, D. J.

    2010-10-01

    We present six new transits of the hot Jupiter OGLE-TR-113b observed with MagIC on the Magellan Telescopes between 2007 January and 2009 May. We update the system parameters and revise the planetary radius to R{sub p} = 1.084 {+-} 0.029R{sub J} , where the error is dominated by stellar radius uncertainties. The new transit midtimes reveal no transit timing variations from a constant ephemeris of greater than 13 {+-} 28 s over two years, placing an upper limit of 1-2 M{sub +} on the mass of any perturber in a 1:2 or 2:1 mean-motion resonance with OGLE-TR-113b. Combining the new transit epochs with five epochs published between 2002 and 2006, we find hints that the orbital period of the planet may not be constant, with the best fit indicating a decrease of P-dot =-60{+-}15 ms yr{sup -1}. If real, this change in period could result from either a long-period (more than eight years) timing variation due to a massive external perturber or more intriguingly from the orbital decay of the planet. The detection of a changing period is still tentative and requires additional observations, but if confirmed it would enable direct tests of tidal stability and dynamical models of close-in planets.

  11. Discovery of the young L dwarf wise J174102.78-464225.5

    SciTech Connect (OSTI)

    Schneider, Adam C.; Cushing, Michael C.; Kirkpatrick, J. Davy; Mace, Gregory N.; Gelino, Christopher R.; Fajardo-Acosta, Sergio; Faherty, Jacqueline K.; Sheppard, Scott S.

    2014-02-01

    We report the discovery of the L dwarf WISE J174102.78464225.5, which was discovered as part of a search for nearby L dwarfs using the Wide-field Infrared Survey Explorer (WISE). The distinct triangular peak of the H-band portion of its near-infrared spectrum and its red near-infrared colors (J K{sub S} = 2.35 0.08 mag) are indicative of a young age. Via comparison to spectral standards and other red L dwarfs, we estimate a near-infrared spectral type of L7 2 (pec). From a comparison to spectral and low-mass evolutionary models, we determine self-consistent effective temperature, log g, age, and mass values of 1450 100 K, 4.0 0.25 (cm s{sup 2}), 10-100 Myr, and 4-21 M {sub Jup}, respectively. With an estimated distance of 10-30 pc, we explore the possibility that WISE J174102.78464225.5 belongs to one of the young nearby moving groups via a kinematic analysis and we find potential membership in the ? Pictoris or AB Doradus associations. A trigonometric parallax measurement and a precise radial velocity can help to secure its membership in either of these groups.

  12. A NEW COSMOLOGICAL DISTANCE MEASURE USING ACTIVE GALACTIC NUCLEUS X-RAY VARIABILITY

    SciTech Connect (OSTI)

    Franca, Fabio La; Bianchi, Stefano; Branchini, Enzo; Matt, Giorgio [Dipartimento di Matematica e Fisica, Universit Roma Tre, Via della Vasca Navale 84, I-00146, Roma (Italy); Ponti, Gabriele, E-mail: lafranca@fis.uniroma3.it [Max-Planck-Institut fr Extraterrestrische Physik, Giessenbachstrasse 1, D-85748 Garching bei Mnchen (Germany)

    2014-05-20

    We report the discovery of a luminosity distance estimator using active galactic nuclei (AGNs). We combine the correlation between the X-ray variability amplitude and the black hole (BH) mass with the single-epoch spectra BH mass estimates which depend on the AGN luminosity and the line width emitted by the broad-line region. We demonstrate that significant correlations do exist that allow one to predict the AGN (optical or X-ray) luminosity as a function of the AGN X-ray variability and either the H? or the Pa? line widths. In the best case, when the Pa? is used, the relationship has an intrinsic dispersion of ?0.6dex. Although intrinsically more disperse than supernovae Ia, this relation constitutes an alternative distance indicator potentially able to probe, in an independent way, the expansion history of the universe. With respect to this, we show that the new mission concept Athena should be able to measure the X-ray variability of hundreds of AGNs and then constrain the distance modulus with uncertainties of 0.1mag up to z ? 0.6. We also discuss how our estimator has the prospect of becoming a cosmological probe even more sensitive than the current supernovae Ia samples by using a new dedicated wide-field X-ray telescope able to measure the variability of thousands of AGNs.

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

    SciTech Connect (OSTI)

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

    2015-01-01

    The supernova (SN) impostor SN 2009ip has re-brightened several times since its initial discovery in 2009 August. During its last outburst in late 2012 September, it reached a peak brightness of m{sub v} ?13.5 (M{sub v} brighter than ?18), causing some to speculate that it had undergone a terminal core-collapse SN. Relatively high-cadence multi-wavelength photometry of the post-peak decline revealed bumps in brightness infrequently observed in other SNe IIn. These bumps occurred synchronously in all ultraviolet (UV) and optical bands with amplitudes of 0.10.4 mag at intervals of 1030 days. Episodic continuum brightening and dimming in the UV and optical with these characteristics is not easily explained within the context of models that have been proposed for the late September 2012 outburst of SN 2009ip. We also present evidence that the post-peak fluctuations in brightness occur at regular intervals and raise more questions about their origin.

  14. LIGHT ECHOES FROM ? CARINAE'S GREAT ERUPTION: SPECTROPHOTOMETRIC EVOLUTION AND THE RAPID FORMATION OF NITROGEN-RICH MOLECULES

    SciTech Connect (OSTI)

    Prieto, J. L.; Knapp, G. R. [Department of Astrophysical Sciences, Princeton University, 4 Ivy Lane, Princeton, NJ 08544 (United States); Rest, A.; Walborn, N. R. [Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States); Bianco, F. B. [Department of Physics, New York University, New York, NY 10012 (United States); Matheson, T. [National Optical Astronomy Observatory, Tucson, AZ 85719 (United States); Smith, N. [Steward Observatory, University of Arizona, Tucson, Arizona 85721 (United States); Hsiao, E. Y.; Campillay, A.; Contreras, C.; Gonzlez, C.; Morrell, N.; Phillips, M. M. [Las Campanas Observatory, Carnegie Observatories, Casilla 601, La Serena (Chile); Chornock, R. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Paredes lvarez, L.; James, D.; Smith, R. C. [Cerro Tololo Inter-American Observatory, Casilla 603, La Serena (Chile); Kunder, A. [Leibniz-Institut fr Astrophysik Potsdam, an der Sternwarte 16, D-14482, Potsdam (Germany); Margheim, S. [Gemini Observatory, Southern Operations Center, Casilla 603, La Serena (Chile); Welch, D. L. [Department of Physics and Astronomy, McMaster University, Hamilton, Ontario L8S 4M1 (Canada); and others

    2014-05-20

    We present follow-up optical imaging and spectroscopy of one of the light echoes of ? Carinae's nineteenth century Great Eruption discovered by Rest et al. By obtaining images and spectra at the same light echo position between 2011 and 2014, we follow the evolution of the Great Eruption on a 3yr timescale. We find remarkable changes in the photometric and spectroscopic evolution of the echo light. The i-band light curve shows a decline of ?0.9mag in ?1 yr after the peak observed in early 2011 and a flattening at later times. The spectra show a pure-absorption early G-type stellar spectrum at peak, but a few months after peak the lines of the Ca II triplet develop strong P-Cygni profiles and we see the appearance of [Ca II] 7291, 7324 doublet in emission. These emission features and their evolution in time resemble those observed in the spectra of some TypeIIn supernovae and supernova impostors. Most surprisingly, starting ?300days after peak brightness, the spectra show strong molecular transitions of CN at ? 6800 . The appearance of these CN features can be explained if the ejecta are strongly nitrogen enhanced, as is observed in modern spectroscopic studies of the bipolar Homunculus nebula. Given the spectroscopic evolution of the light echo, velocities of the main features, and detection of strong CN, we are likely seeing ejecta that contributes directly to the Homunculus nebula.

  15. GeOx/Reduced Graphene Oxide Composite as an Anode for Li-ion Batteries: Enhanced Capacity via Reversible Utilization of Li2O along with Improved Rate Performance

    SciTech Connect (OSTI)

    Lv, Dongping; Gordin, Mikhail; Yi, Ran; Xu, Terrence (Tianren); Song, Jiangxuan; Jiang, Yingbing; Choi, Daiwon; Wang, Donghai

    2014-09-01

    A self-assembled GeOx/reduced graphene oxide (GeOx/RGO) composite, where GeOx nanoparticles were grown directly on reduced graphene oxide sheets, was synthesized via a facile one-step reduction approach and studied by X-ray diffraction, transmission electron microscopy, energy dispersive X-ray spectroscopy, electron energy loss spectroscopy elemental mapping, and other techniques. Electrochemical evaluation indicates that incorporation of reduced graphene oxide enhances both the rate capability and reversible capacity of GeOx, with the latter being due to the RGO enabling reversible utilization of Li2O. The composite delivers a high reversible capacity of 1600 mAhg-1 at a current density of 100 mAg-1, and still maintains a capacity of 410 mAhg-1 at a high current density of 20 Ag-1. Owing to the flexible reduced graphene oxide sheets enwrapping the GeOx particles, the cycling stability of the composite was also improved significantly. To further demonstrate its feasibility in practical applications, the synthesized GeOx/RGO composite anode was successfully paired with a high voltage LiNi0.5Mn1.5O4 cathode to form a full cell, which showed good cycling and rate performance.

  16. Star formation relations in nearby molecular clouds

    SciTech Connect (OSTI)

    Evans, Neal J. II; Heiderman, Amanda; Vutisalchavakul, Nalin

    2014-02-20

    We test some ideas for star formation relations against data on local molecular clouds. On a cloud by cloud basis, the relation between the surface density of star formation rate and surface density of gas divided by a free-fall time, calculated from the mean cloud density, shows no significant correlation. If a crossing time is substituted for the free-fall time, there is even less correlation. Within a cloud, the star formation rate volume and surface densities increase rapidly with the corresponding gas densities, faster than predicted by models using the free-fall time defined from the local density. A model in which the star formation rate depends linearly on the mass of gas above a visual extinction of 8 mag describes the data on these clouds, with very low dispersion. The data on regions of very massive star formation, with improved star formation rates based on free-free emission from ionized gas, also agree with this linear relation.

  17. EIGHT HUNDRED NEW CANDIDATES FOR GLOBULAR CLUSTERS IN NGC 5128 (Centaurus A)

    SciTech Connect (OSTI)

    Harris, Gretchen L. H.; Johnston, Kyle; Kazemzadeh, Farnoud; Gomez, Matias; Harris, William E.; Kerzendorf, Wolfgang; Geisler, Doug; Woodley, Kristin A. E-mail: kyjohnston@rim.com E-mail: matiasgomez@unab.cl E-mail: wkerzend@mso.anu.edu.au E-mail: kwoodley@phas.ubc.ca

    2012-04-15

    We have used new wide-field imaging with the Magellan IMACS camera to search for globular cluster (GC) candidates around NGC 5128, the nearest giant E galaxy. The imaging data are in the B and R broadband filters and cover a 1.55 deg{sup 2} field centered on the galaxy, corresponding to an area about 90 Multiplication-Sign 90 kpc{sup 2} at the distance of NGC 5128. All the fields were taken under exceptionally high-quality seeing conditions (FWHM = 0.''4-0.''5 in R). Using this material we are able, for the first time in the literature, to construct a homogeneous list of GC candidates covering a wide span of the NGC 5128 halo and unusually free of field contaminants (foreground stars and faint background galaxies). Selecting the measured objects by color, magnitude, ellipticity, and profile size gives us a final catalog of 833 new high-quality GC candidates brighter than R = 21 (0.8 mag fainter than the standard GC luminosity function turnover point). The measured positions have better than 0.''2 precision in both coordinates. This list can be used as the basis for spectroscopic follow-up, leading to a more comprehensive kinematic and dynamic study of the halo.

  18. Eight new Milky Way companions discovered in first-year Dark Energy Survey data

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

    Bechtol, K.

    2015-06-30

    We report the discovery of eight new Milky Way companions inmore » $$\\sim 1800\\;{\\mathrm{deg}}^{2}$$ of optical imaging data collected during the first year of the Dark Energy Survey (DES). Each system is identified as a statistically significant over-density of individual stars consistent with the expected isochrone and luminosity function of an old and metal-poor stellar population. The objects span a wide range of absolute magnitudes (MV from $-2.2$ to $$-7.4\\;\\mathrm{mag}$$), physical sizes ($$10-170\\;\\mathrm{pc}$$), and heliocentric distances ($$30-330\\;\\mathrm{kpc}$$). Based on the low surface brightnesses, large physical sizes, and/or large Galactocentric distances of these objects, several are likely to be new ultra-faint satellite galaxies of the Milky Way and/or Magellanic Clouds. We introduce a likelihood-based algorithm to search for and characterize stellar over-densities, as well as identify stars with high satellite membership probabilities. As a result, we also present completeness estimates for detecting ultra-faint galaxies of varying luminosities, sizes, and heliocentric distances in the first-year DES data.« less

  19. OCCULTATION OF THE T TAURI STAR RW AURIGAE A BY ITS TIDALLY DISRUPTED DISK

    SciTech Connect (OSTI)

    Rodriguez, Joseph E.; Stassun, Keivan G.; Pepper, Joshua; Siverd, Robert J.; Cargile, Phillip; Beatty, Thomas G.; Gaudi, B. Scott

    2013-11-01

    RW Aur A is a classical T Tauri star, believed to have undergone a reconfiguration of its circumstellar environment as a consequence of a recent flyby of its stellar companion, RW Aur B. This interaction stripped away part of the circumstellar disk of RW Aur A, leaving a tidally disrupted ''arm'' and a short truncated circumstellar disk. We present photometric observations of the RW Aur system from the Kilodegree Extremely Little Telescope survey showing a long and deep dimming that occurred from 2010 September until 2011 March. The dimming has a depth of ?2 mag, a duration of ?180 days, and was confirmed by archival observations from American Association of Variable Star Observers. We suggest that this event is the result of a portion of the tidally disrupted disk occulting RW Aur A, specifically a fragment of the tidally disrupted arm. The calculated transverse linear velocity of the occulter is in excellent agreement with the measured relative radial velocity of the tidally disrupted arm. Using simple kinematic and geometric arguments, we show that the occulter cannot be a feature of the RW Aur A circumstellar disk, and we consider and discount other hypotheses. We also place constraints on the thickness and semimajor axis of the portion of the arm that occulted the star.

  20. OzDES multifibre spectroscopy for the Dark Energy Survey: First-year operation and results

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

    Yuan, Fang; Plazas, A. A.; Lidman, C.; Davis, T. M.; Childress, M.; Abdalla, F. B.

    2015-07-29

    OzDES is a five-year, 100-night, spectroscopic survey on the Anglo-Australian Telescope, whose primary aim is to measure redshifts of approximately 2,500 Type Ia supernovae host galaxies over the redshift range 0.1 morehelp calibrate photometric redshifts. Here we present an overview of the OzDES program and our first-year results. Between Dec 2012 and Dec 2013, we observed over 10,000 objects and measured more than 6,000 redshifts. Our strategy of retargeting faint objects across many observing runs has allowed us to measure redshifts for galaxies as faint as mr = 25 mag. We outline our target selection and observing strategy, quantify the redshift success rate for different types of targets, and discuss the implications for our main science goals. Finally, we highlight a few interesting objects as examples of the fortuitous yet not totally unexpected discoveries that can come from such a large spectroscopic survey.less

  1. Difference image analysis of defocused observations with CSTAR

    SciTech Connect (OSTI)

    Oelkers, Ryan J.; Macri, Lucas M.; Wang, Lifan; Ashley, Michael C. B.; Lawrence, Jon S.; Luong-Van, Daniel; Cui, Xiangqun; Gong, Xuefei; Qiang, Liu; Yang, Huigen; Yuan, Xiangyan; Zhou, Xu; Feng, Long-Long; Zhu, Zhenxi; Pennypacker, Carl R.; York, Donald G.

    2015-02-01

    The Chinese Small Telescope ARray carried out high-cadence time-series observations of 27 square degrees centered on the South Celestial Pole during the Antarctic winter seasons of 20082010. Aperture photometry of the 2008 and 2010 i-band images resulted in the discovery of over 200 variable stars. Yearly servicing left the array defocused for the 2009 winter season, during which the system also suffered from intermittent frosting and power failures. Despite these technical issues, nearly 800,000 useful images were obtained using g, r, and clear filters. We developed a combination of difference imaging and aperture photometry to compensate for the highly crowded, blended, and defocused frames. We present details of this approach, which may be useful for the analysis of time-series data from other small-aperture telescopes regardless of their image quality. Using this approach, we were able to recover 68 previously known variables and detected variability in 37 additional objects. We also have determined the observing statistics for Dome A during the 2009 winter season; we find the extinction due to clouds to be less than 0.1 and 0.4 mag for 40% and 63% of the dark time, respectively.

  2. NEW PRECISION ORBITS OF BRIGHT DOUBLE-LINED SPECTROSCOPIC BINARIES. V. THE AM STARS HD 434 AND 41 SEXTANTIS

    SciTech Connect (OSTI)

    Fekel, Francis C. [Kitt Peak National Observatory, National Optical Astronomy Observatory (United States); Williamson, Michael H., E-mail: fekel@evans.tsuniv.ed [Center of Excellence in Information Systems, Tennessee State University, 3500 John A. Merritt Boulevard, Box 9501, Nashville, TN 37209 (United States)

    2010-11-15

    We have detected the secondary component in two previously known spectroscopic binaries, HD 434 and 41 Sex, and for the first time determined double-lined orbits for them. Despite the relatively long period of 34.26 days and a moderate eccentricity of 0.32, combined with the components' rotationally broadened lines, measurement of the primary and secondary radial velocities of HD 434 has enabled us to obtain significantly improved orbital elements. While the 41 Sex system has a much shorter period of 6.167 days and a circular orbit, the estimated V mag difference of 3.2 between its components also makes this a challenging system. The new orbital dimensions (a{sub 1} sin i and a{sub 2} sin i) and minimum masses (m{sub 1} sin{sup 3} i and m{sub 2} sin{sup 3} i) of HD 434 have accuracies of 0.8% or better, while the same quantities for 41 Sex are good to 0.5% or better. Both components of HD 434 are Am stars while the Am star primary of 41 Sex has a late-F or early-G companion. All four stars are on the main sequence. The two components of HD 434 are rotating much faster than their predicted pseudosynchronous velocities, while both components of 41 Sex are synchronously rotating. For the primary of 41 Sex, the spectrum line depth changes noted by Sreedhar Rao et al. were not detected.

  3. DISCOVERY OF A BINARY BROWN DWARF AT 2 pc FROM THE SUN

    SciTech Connect (OSTI)

    Luhman, K. L.

    2013-04-10

    I am using multi-epoch astrometry from the Wide-field Infrared Survey Explorer (WISE) to search for new members of the solar neighborhood via their high proper motions. Through this work, I have identified WISE J104915.57-531906.1 as a high proper motion object and have found additional detections in images from the Digitized Sky Survey, the Two Micron All-Sky Survey, and the Deep Near-Infrared Survey of the Southern Sky. I have measured a parallax of 0.''496 {+-} 0.''037 (2.0 {+-} 0.15 pc) from the astrometry in these surveys, making WISE J104915.57-531906.1 the third closest system to the Sun. During spectroscopic observations with the Gemini Multi-Object Spectrograph at Gemini Observatory, an i-band acquisition image resolved it as a 1.''5 (3 AU) binary. A spectrum was collected for the primary, which I classify as L8 {+-} 1. The secondary is probably near the L/T transition as well given that it is only modestly fainter than the primary ({Delta}i = 0.45 mag).

  4. A SUPER-EARTH-SIZED PLANET ORBITING IN OR NEAR THE HABITABLE ZONE AROUND A SUN-LIKE STAR

    SciTech Connect (OSTI)

    Barclay, Thomas; Burke, Christopher J.; Howell, Steve B.; Rowe, Jason F.; Huber, Daniel; Jenkins, Jon M.; Quintana, Elisa V.; Still, Martin; Twicken, Joseph D.; Bryson, Stephen T.; Borucki, William J.; Caldwell, Douglas A.; Clarke, Bruce D.; Christiansen, Jessie L; Coughlin, Jeffrey L.; Ciardi, David; Fischer, Debra A.; and others

    2013-05-10

    We present the discovery of a super-Earth-sized planet in or near the habitable zone of a Sun-like star. The host is Kepler-69, a 13.7 mag G4V-type star. We detect two periodic sets of transit signals in the 3-year flux time series of Kepler-69, obtained with the Kepler spacecraft. Using the very high precision Kepler photometry, and follow-up observations, our confidence that these signals represent planetary transits is >99.3%. The inner planet, Kepler-69b, has a radius of 2.24{sup +0.44}{sub -0.29} R{sub Circled-Plus} and orbits the host star every 13.7 days. The outer planet, Kepler-69c, is a super-Earth-sized object with a radius of 1.7{sup +0.34}{sub -0.23} R{sub Circled-Plus} and an orbital period of 242.5 days. Assuming an Earth-like Bond albedo, Kepler-69c has an equilibrium temperature of 299 {+-} 19 K, which places the planet close to the habitable zone around the host star. This is the smallest planet found by Kepler to be orbiting in or near the habitable zone of a Sun-like star and represents an important step on the path to finding the first true Earth analog.

  5. Stellar metallicity of the extended disk and distance of the spiral galaxy NGC 3621

    SciTech Connect (OSTI)

    Kudritzki, Rolf-Peter; Bresolin, Fabio; Hosek, Matthew W. Jr.; Urbaneja, Miguel A.; Przybilla, Norbert E-mail: bresolin@ifa.hawaii.edu E-mail: Miguel.Urbaneja-Perez@uibk.ac.at

    2014-06-10

    Low resolution (?4.5 ) ESO VLT/FORS spectra of blue supergiant stars are analyzed to determine stellar metallicities (based on elements such as iron, titanium, and magnesium) in the extended disk of the spiral galaxy, NGC 3621. Mildly subsolar metallicity (0.30 dex) is found for the outer objects beyond 7 kpc, independent of galactocentric radius and compatible with the absence of a metallicity gradient, confirming the results of a recent investigation of interstellar medium H II region gas oxygen abundances. The stellar metallicities are slightly higher than those from the H II regions when based on measurements of the weak forbidden auroral oxygen line at 4363 but lower than the ones obtained with the R {sub 23} strong line method. It is shown that the present level of metallicity in the extended disk cannot be the result of chemical evolution over the age of the disk with the present rate of in situ star formation. Additional mechanisms must be involved. In addition to metallicity, stellar effective temperatures, gravities, interstellar reddening, and bolometric magnitudes are determined. After the application of individual reddening corrections for each target, the flux-weighted gravity-luminosity relationship of blue supergiant stars is used to obtain a distance modulus of 29.07 0.09 mag (distance D = 6.52 0.28 Mpc). This new distance is discussed in relation to Cepheid and the tip of the red giant branch distances.

  6. WIYN open cluster study. LX. Spectroscopic binary orbits in NGC 6819

    SciTech Connect (OSTI)

    Milliman, Katelyn E.; Mathieu, Robert D.; Gosnell, Natalie M.; Geller, Aaron M.; Meibom, Sren; Platais, Imants

    2014-08-01

    We present the current state of the WOCS radial-velocity (RV) survey for the rich open cluster NGC 6819 (2.5 Gyr) including 93 spectroscopic binary orbits with periods ranging from 1.5 to 8000 days. These results are the product of our ongoing RV survey of NGC 6819 using the Hydra Multi-Object Spectrograph on the WIYN 3.5 m telescope. We also include a detailed analysis of multiple prior sets of optical photometry for NGC 6819. Within a 1 field of view, our stellar sample includes the giant branch, the red clump, and blue straggler candidates, and extends to almost 2 mag below the main sequence (MS) turnoff. For each star observed in our survey we present all RV measurements, the average RV, and velocity variability information. Additionally, we discuss notable binaries from our sample, including eclipsing binaries (WOCS 23009, WOCS 24009, and WOCS 40007), stars noted in Kepler asteroseismology studies (WOCS 4008, WOCS 7009, and WOCS 8007), and potential descendants of past blue stragglers (WOCS 1006 and WOCS 6002). We find the incompleteness-corrected binary fraction for all MS binaries with periods less than 10{sup 4} days to be 22% 3% and a tidal circularization period of 6.2{sub ?1.1}{sup +1.1} days for NGC 6819.

  7. LEDA 074886: A REMARKABLE RECTANGULAR-LOOKING GALAXY

    SciTech Connect (OSTI)

    Graham, Alister W.; Spitler, Lee R.; Forbes, Duncan A.; Lisker, Thorsten; Janz, Joachim; Moore, Ben

    2012-05-10

    We report the discovery of an interesting and rare rectangular-shaped galaxy. At a distance of 21 Mpc, the dwarf galaxy LEDA 074886 has an absolute R-band magnitude of -17.3 mag. Adding to this galaxy's intrigue is the presence of an embedded, edge-on stellar disk (of extent 2 R{sub e,disk} = 12'' = 1.2 kpc) for which Forbes et al. reported v{sub rot}/{sigma} Almost-Equal-To 1.4. We speculate that this galaxy may be the remnant of two (nearly edge-on) merged disk galaxies in which the initial gas was driven inward and subsequently formed the inner disk, while the stars at larger radii effectively experienced a dissipationless merger event resulting in this 'emerald cut galaxy' having very boxy isophotes with a{sub 4}/a = -0.05 to -0.08 from 3 to 5 kpc. This galaxy suggests that knowledge from simulations of both 'wet' and 'dry' galaxy mergers may need to be combined to properly understand the various paths that galaxy evolution can take, with a particular relevance to blue elliptical galaxies.

  8. THE AKARI 2.5-5.0 ?m SPECTRAL ATLAS OF TYPE-1 ACTIVE GALACTIC NUCLEI: BLACK HOLE MASS ESTIMATOR, LINE RATIO, AND HOT DUST TEMPERATURE

    SciTech Connect (OSTI)

    Kim, Dohyeong; Im, Myungshin; Kim, Ji Hoon; Jun, Hyunsung David; Lee, Seong-Kook; Woo, Jong-Hak; Lee, Hyung Mok; Lee, Myung Gyoon; Nakagawa, Takao; Matsuhara, Hideo; Wada, Takehiko; Takagi, Toshinobu; Oyabu, Shinki; Ohyama, Youichi E-mail: mim@astro.snu.ac.kr

    2015-01-01

    We present 2.5-5.0?m spectra of 83 nearby (0.002 < z < 0.48) and bright (K < 14 mag) type-1 active galactic nuclei (AGNs) taken with the Infrared Camera on board AKARI. The 2.5-5.0?m spectral region contains emission lines such as Br? (2.63?m), Br? (4.05?m), and polycyclic aromatic hydrocarbons (3.3?m), which can be used for studying the black hole (BH) masses and star formation activity in the host galaxies of AGNs. The spectral region also suffers less dust extinction than in the ultra violet (UV) or optical wavelengths, which may provide an unobscured view of dusty AGNs. Our sample is selected from bright quasar surveys of Palomar-Green and SNUQSO, and AGNs with reverberation-mapped BH masses from Peterson etal. Using 11 AGNs with reliable detection of Brackett lines, we derive the Brackett-line-based BH mass estimators. We also find that the observed Brackett line ratios can be explained with the commonly adopted physical conditions of the broad line region. Moreover, we fit the hot and warm dust components of the dust torus by adding photometric data of SDSS, 2MASS, WISE, and ISO to the AKARI spectra, finding hot and warm dust temperatures of ?1100 K and ?220 K, respectively, rather than the commonly cited hot dust temperature of 1500 K.

  9. Eight new Milky Way companions discovered in first-year Dark Energy Survey data

    SciTech Connect (OSTI)

    Bechtol, K.; et al.

    2015-06-30

    We report the discovery of eight new Milky Way companions in $\\sim 1800\\;{\\mathrm{deg}}^{2}$ of optical imaging data collected during the first year of the Dark Energy Survey (DES). Each system is identified as a statistically significant over-density of individual stars consistent with the expected isochrone and luminosity function of an old and metal-poor stellar population. The objects span a wide range of absolute magnitudes (MV from $-2.2$ to $-7.4\\;\\mathrm{mag}$), physical sizes ($10-170\\;\\mathrm{pc}$), and heliocentric distances ($30-330\\;\\mathrm{kpc}$). Based on the low surface brightnesses, large physical sizes, and/or large Galactocentric distances of these objects, several are likely to be new ultra-faint satellite galaxies of the Milky Way and/or Magellanic Clouds. We introduce a likelihood-based algorithm to search for and characterize stellar over-densities, as well as identify stars with high satellite membership probabilities. As a result, we also present completeness estimates for detecting ultra-faint galaxies of varying luminosities, sizes, and heliocentric distances in the first-year DES data.

  10. NGC 4102: HIGH-RESOLUTION INFRARED OBSERVATIONS OF A NUCLEAR STARBURST RING

    SciTech Connect (OSTI)

    Beck, Sara C.; Lacy, John H.; Turner, Jean L.

    2010-10-20

    The composite galaxy NGC 4102 hosts a LINER nucleus and a starburst. We mapped NGC 4102 in the 12.8 {mu}m line of [Ne II], using the echelon spectrometer TEXES on the NASA IRTF, to obtain a data cube with 1.''5 spatial, and 25 km s{sup -1} spectral, resolution. Combining near-infrared, radio, and the [Ne II] data shows that the extinction to the starburst is substantial, more than 2 mag at the K band, and that the neon abundance is less than half solar. We find that the star formation in the nuclear region is confined to a rotating ring or disk of 4.''3 ({approx}300 pc) diameter, inside the inner Lindblad resonance. This region is an intense concentration of mass, with a dynamical mass {approx}3 x 10{sup 9} M{sub sun}, and of star formation. The young stars in the ring produce the [Ne II] flux reported by Spitzer for the entire galaxy. The mysterious blue component of line emission detected in the near-infrared is also seen in [Ne II]; it is not a normal active galactic nucleus outflow.

  11. On Techniques to Characterize and Correlate Grain Size, Grain Boundary Orientation and the Strength of the SiC Layer of TRISO Coated Particles: A Preliminary Study

    SciTech Connect (OSTI)

    I.J.van Rooyen; J.L. Dunzik Gougar; T. Trowbridge; Philip M van Rooyen

    2012-10-01

    The mechanical properties of the silicon carbide (SiC) layer of the TRi-ISOtropic (TRISO) coated particle (CP) for high temperature gas reactors (HTGR) are performance parameters that have not yet been standardized by the international HTR community. Presented in this paper are the results of characterizing coated particles to reveal the effect of annealing temperature (1000 to 2100C) on the strength and grain size of unirradiated coated particles. This work was further expanded to include possible relationships between the grain size and strength values. The comparative results of two strength measurement techniques and grain size measured by the Lineal intercept method are included. Preliminary grain boundary characterization results determined by electron backscatter diffraction (EBSD) are included. These results are also important for future fission product transport studies, as grain boundary diffusion is identified as a possible mechanism by which 110mAg, one of the fission activation products, might be released through intact SiC layers. Temperature is a parameter known to influence the grain size of SiC and therefore it is important to investigate the effect of high temperature annealing on the SiC grain size. Recommendations and future work will also be briefly discussed.

  12. Occupational health and environment research 1983: Health, Safety, and Environment Division. Progress report

    SciTech Connect (OSTI)

    Voelz, G.L.

    1985-05-01

    The primary responsibility of the Health, Safety, and Environment (HSE) Division at the Los Alamos National Laboratory is to provide comprehensive occupational health and safety programs, waste processing, and environmental protection. These activities are designed to protect the workers, the public, and the environment. Evaluation of respiratory protective equipment included the XM-30 and M17A1 military masks, use of MAG-1 spectacles in respirators, and eight self-contained units. The latter units were used in an evaluation of test procedures used for Bureau of Mines approval of breathing apparatuses. Analyses of air samples from field studies of a modified in situ oil shale retorting facility were performed for total cyclohexane extractables and selected polynuclear aromatic hydrocarbons. Aerosols generation and characterization of effluents from oil shale processing were continued as part of an inhalation toxicology study. Additional data on plutonium excretion in urine are presented and point up problems in using the Langham equation to predict plutonium deposition in the body from long-term excretion data. Environmental surveillance at Los Alamos during 1983 showed the highest estimated radiation dose from Laboratory operations to be about 26% of the natural background radiation dose. Several studies on radionuclides and their transport in the Los Alamos environment are described. The chemical quality of surface and ground water near the geothermal hot dry rock facility is described. Short- and long-term consequences to man from releases of radionuclides into the environment can be simulated by the BIOTRAN computer model, which is discussed brirfly.

  13. Ag Out-surface Diffusion In Crystalline SiC With An Effective SiO2 Diffusion Barrier

    SciTech Connect (OSTI)

    Xue, H.; Xiao, Haiyan Y.; Zhu, Zihua; Shutthanandan, V.; Snead, Lance L.; Boatner, Lynn A.; Weber, William J.; Zhang, Y.

    2015-09-01

    For applications of tristructural isotropic (TRISO) fuel particles in high temperature reactors, release of radioactive Ag isotope (110mAg) through the SiC coating layer is a safety concern. To understand the diffusion mechanism, Ag ion implantations near the surface and in the bulk were performed by utilizing different ion energies and energy-degrader foils. High temperature annealing was carried out on the as-irradiated samples to study the possible out-surface diffusion. Before and after annealing, Rutherford backscattering spectrometry (RBS) and secondary ion mass spectrometry (SIMS) measurements were employed to obtain the elemental profiles of the implanted samples. The results suggest little migration of buried Ag in the bulk, and an out-diffusion of the implanted Ag in the near-surface region of single crystal SiC. It is also found that a SiO2 layer, which was formed during annealing, may serve as an effective barrier to reduce or prevent Ag out diffusion through the SiC coating layer.

  14. Silver (Ag) Transport Mechanisms in TRISO coated particles: A Critical Review

    SciTech Connect (OSTI)

    I J van Rooyen; J H Neethling; J A A Engelbrecht; P M van Rooyen; G Strydom

    2012-10-01

    Transport of 110mAg in the intact SiC layer of TRISO coated particles has been studied for approximately 30 years without arriving at a satisfactory explanation of the transport mechanism. In this paper the possible mechanisms postulated in previous experimental studies, both in-reactor and out-of reactor research environment studies are critically reviewed and of particular interest are relevance to very high temperature gas reactor operating and accident conditions. Among the factors thought to influence Ag transport are grain boundary stoichiometry, SiC grain size and shape, the presence of free silicon, nano-cracks, thermal decomposition, palladium attack, transmutation products, layer thinning and coated particle shape. Additionally new insight to nature and location of fission products has been gained via recent post irradiation electron microscopy examination of TRISO coated particles from the DOEs fuel development program. The combined effect of critical review and new analyses indicates a direction for investigating possible the Ag transport mechanism including the confidence level with which these mechanisms may be experimentally verified.

  15. THE SLOAN DIGITAL SKY SURVEY QUASAR LENS SEARCH. IV. STATISTICAL LENS SAMPLE FROM THE FIFTH DATA RELEASE

    SciTech Connect (OSTI)

    Inada, Naohisa; Oguri, Masamune; Shin, Min-Su; Kayo, Issha; Fukugita, Masataka; Strauss, Michael A.; Gott, J. Richard; Hennawi, Joseph F.; Morokuma, Tomoki; Becker, Robert H.; Gregg, Michael D.; White, Richard L.; Kochanek, Christopher S.; Chiu, Kuenley; Johnston, David E.; Clocchiatti, Alejandro; Richards, Gordon T.; Schneider, Donald P.; Frieman, Joshua A.

    2010-08-15

    We present the second report of our systematic search for strongly lensed quasars from the data of the Sloan Digital Sky Survey (SDSS). From extensive follow-up observations of 136 candidate objects, we find 36 lenses in the full sample of 77,429 spectroscopically confirmed quasars in the SDSS Data Release 5. We then define a complete sample of 19 lenses, including 11 from our previous search in the SDSS Data Release 3, from the sample of 36,287 quasars with i < 19.1 in the redshift range 0.6 < z < 2.2, where we require the lenses to have image separations of 1'' < {theta} < 20'' and i-band magnitude differences between the two images smaller than 1.25 mag. Among the 19 lensed quasars, three have quadruple-image configurations, while the remaining 16 show double images. This lens sample constrains the cosmological constant to be {Omega}{sub {Lambda}} = 0.84{sup +0.06}{sub -0.08}(stat.){sup +0.09}{sub -0.07}(syst.) assuming a flat universe, which is in good agreement with other cosmological observations. We also report the discoveries of seven binary quasars with separations ranging from 1.''1 to 16.''6, which are identified in the course of our lens survey. This study concludes the construction of our statistical lens sample in the full SDSS-I data set.

  16. THE INFRARED SPECTRUM OF URANIUM HOLLOW CATHODE LAMPS FROM 850 nm to 4000 nm: WAVENUMBERS AND LINE IDENTIFICATIONS FROM FOURIER TRANSFORM SPECTRA

    SciTech Connect (OSTI)

    Redman, Stephen L.; Ramsey, Lawrence W.; Mahadevan, Suvrath [Department of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802 (United States); Lawler, James E. [Department of Physics, University of Wisconsin, 1150 University Avenue, Madison, WI 53706 (United States); Nave, Gillian [National Institute of Standards and Technology, Gaithersburg, MD 20899 (United States)

    2011-08-01

    We provide new measurements of wavenumbers and line identifications of 10, 100 U I and U II near-infrared (NIR) emission lines between 2500 cm{sup -1} and 12, 000 cm{sup -1} (4000-850 nm) using archival Fourier transform spectrometer spectra from the National Solar Observatory. This line list includes isolated uranium lines in the Y, J, H, K, and L bands (0.9-1.1 {mu}m, 1.2-1.35 {mu}m, 1.5-1.65 {mu}m, 2.0-2.4 {mu}m, and 3.0-4.0 {mu}m, respectively), and provides six times as many calibration lines as thorium in the NIR spectral range. The line lists we provide enable inexpensive, commercially available uranium hollow cathode lamps to be used for high-precision wavelength calibration of existing and future high-resolution NIR spectrographs.

  17. PPPL_Procurement_map_NJ_FY15

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

    8 Princeton Plasma Physics Laboratory Procured Materials and Services 2015 ($10.8M) # small business/ total firms 23.1k 27.2k 2 1 2 3 4 12 6 7 Hunterdon Somerset Middlesex Morris Warren Sussex Passaic Bergen Essex Hudson Union Monmouth Mercer Ocean Burlington Atlantic Camden Salem Gloucester Cumberland Cape May 5 11 9 52.4k 576k 1 426k 192k 394k 1.05M 4 1.63M 1.45M 1.69M 3 3.28M 2 / 2 1 / 1 1 / 3 10 / 11 18 / 20 4 / 4 7 / 9 24 / 25 6 / 8 18 / 20 7 / 8 28 / 32 10 8 5 9 6 11 7 12 District $

  18. Magnetic rotation (MR) band crossing in N=78 odd-Z nuclei: Tilted axis cranking (TAC) calculations to explore the role of nucleons

    SciTech Connect (OSTI)

    Kumar, Suresh

    2014-08-14

    Magnetic Rotation (MR) band crossing is studied systematically in N=78 isotones (La, Pr, Pm and Eu) using Tilted Axis Cranking (TAC) model. The observables such as I(h) vs h?, excitation energy E(MeV) vs spin I(h), and the B(M1)/B(E2) vs I(h) were considered to pinpoint MR crossing in these nuclei. The results of tilted axis cranking were compared with these experimental observables. The B(M1) and B(E2) values were also reported and used to understand the crossing behaviour of these MR bands. The systematic evolution of this phenomenon in N=78 odd-Z istotones leads to understand the role of nucleons in MR band crossing.

  19. Ternary metal-rich sulfide with a layered structure

    DOE Patents [OSTI]

    Franzen, Hugo F.; Yao, Xiaoqiang

    1993-08-17

    A ternary Nb-Ta-S compound is provided having the atomic formula, Nb.sub.1.72 Ta.sub.3.28 S.sub.2, and exhibiting a layered structure in the sequence S-M3-M2-M1-M2-M3-S wherein S represents sulfur layers and M1, M2, and M3 represent Nb/Ta mixed metal layers. This sequence generates seven sheets stacked along the [001] direction of an approximate body centered cubic crystal structure with relatively weak sulfur-to-sulfur van der Waals type interactions between adjacent sulfur sheets and metal-to-metal bonding within and between adjacent mixed metal sheets.

  20. Y YEAR

    National Nuclear Security Administration (NNSA)

    4 30 -11.76% ↓ YEAR 2013 2014 Males 16 14 -12.50% ↓ Females 18 16 -11.11% ↓ YEAR 2013 2014 SES 1 1 0% / EJ/EK 3 1 -66.67% ↓ NQ (Prof/Tech/Admin) 29 27 -6.90% ↓ NU (Tech/Admin Support) 1 1 0% / YEAR 2013 2014 American Indian Alaska Native Male (AIAN,M) 1 1 0% / American Indian Alaskan Native Female (AIAN,F) 2 2 0% / African American Male (AA,M) 3 3 0% / African American Female (AA,F) 7 6 -14.29% ↓ Asian American Pacific Islander Male (AAPI,M) 1 1 0% / Asian American Pacific Islander

  1. Light harvesting arrays

    DOE Patents [OSTI]

    Lindsey, Jonathan S. (Raleigh, NC)

    2002-01-01

    A light harvesting array useful for the manufacture of devices such as solar cells comprises: (a) a first substrate comprising a first electrode; and (b) a layer of light harvesting rods electrically coupled to the first electrode, each of the light harvesting rods comprising a polymer of Formula I: X.sup.1.paren open-st.X.sup.m+1).sub.m (I) wherein m is at least 1, and may be from two, three or four to 20 or more; X.sup.1 is a charge separation group (and preferably a porphyrinic macrocycle, which may be one ligand of a double-decker sandwich compound) having an excited-state of energy equal to or lower than that of X.sup.2, and X.sup.2 through X.sup.m+1 are chromophores (and again are preferably porphyrinic macrocycles).

  2. Convergent synthesis of multiporphyrin light-harvesting rods

    DOE Patents [OSTI]

    Lindsey, Jonathan S.; Loewe, Robert S.

    2003-08-05

    The present invention provides a convergent method for the synthesis of light harvesting rods. The rods are oligomers of the formula A.sup.1 (A.sup.b+1).sub.b, wherein b is at least 1, A.sup.1 through A.sup.b+1 are covalently coupled rod segments, and each rod segment A.sup.1 through A.sup.1+b comprises a compound of the formula X.sup.1 (X.sup.m+1).sub.m wherein m is at least 1 and X.sup.1 through X.sup.m+1 are covalently coupled porphyrinic macrocycles. Light harvesting arrays and solar cells containing such light harvesting rods are also described, along with intermediates useful in such methods and rods produced by such methods.

  3. A magnetically shielded room with ultra low residual field and gradient

    SciTech Connect (OSTI)

    Altarev, I.; Chesnevskaya, S.; Gutsmiedl, E.; Kuchler, F.; Lins, T.; Marino, M.; McAndrew, J.; Niessen, B.; Paul, S.; Petzoldt, G.; Singh, J.; Stoepler, R.; Stuiber, S.; Sturm, M.; Taubenheim, B. [Physikdepartment, Technische Universitt Mnchen, D-85748 Garching (Germany); Babcock, E. [Jlich Center for Neutron Science, Lichtenbergstrasse 1, D-85748 Garching (Germany); Beck, D.; Sharma, S. [Physics Department, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801 (United States); Burghoff, M.; Fan, I. [Physikalisch-Technische Bundesanstalt Berlin, D-10587 Berlin (Germany); and others

    2014-07-15

    A versatile and portable magnetically shielded room with a field of (700200) pT within a central volume of 1 m 1 m 1 m and a field gradient less than 300 pT/m, achieved without any external field stabilization or compensation, is described. This performance represents more than a hundredfold improvement of the state of the art for a two-layer magnetic shield and provides an environment suitable for a next generation of precision experiments in fundamental physics at low energies; in particular, searches for electric dipole moments of fundamental systems and tests of Lorentz-invariance based on spin-precession experiments. Studies of the residual fields and their sources enable improved design of future ultra-low gradient environments and experimental apparatus. This has implications for developments of magnetometry beyond the femto-Tesla scale in, for example, biomagnetism, geosciences, and security applications and in general low-field nuclear magnetic resonance (NMR) measurements.

  4. Low-energy magnetic radiation: Deviations from GOE

    SciTech Connect (OSTI)

    Frauendorf, S.; Schwengner, R.; Wimmer, K.

    2014-10-15

    A pronounced spike at low energy in the strength function for magnetic radiation (LEMAR) is found by means of Shell Model calculations, which explains the experimentally observed enhancement of the dipole strength. LEMAR originates from statistical low-energy M1-transitions between many excited complex states. Re-coupling of the proton and neutron high-j orbitals generates the strong magnetic radiation. LEMAR is closely related to Magnetic Rotation. LEMAR is predicted for nuclides participating in the r-process of element synthesis and is expected to change the reaction rates. An exponential decrease of the strength function and a power law for the size distribution of the B(M1) values are found, which strongly deviate from the ones of the GOE of random matrices, which is commonly used to represent complex compound states.

  5. Solar cells incorporating light harvesting arrays

    DOE Patents [OSTI]

    Lindsey, Jonathan S. (Raleigh, NC); Meyer, Gerald J. (Baltimore, MD)

    2002-01-01

    A solar cell incorporates a light harvesting array that comprises: (a) a first substrate comprising a first electrode; and (b) a layer of light harvesting rods electrically coupled to the first electrode, each of the light harvesting rods comprising a polymer of Formula I: X.sup.1.paren open-st.X.sup.m+1).sub.m (I) wherein m is at least 1, and may be from two, three or four to 20 or more; X.sup.1 is a charge separation group (and preferably a porphyrinic macrocycle, which may be one ligand of a double-decker sandwich compound) having an excited-state of energy equal to or lower than that of X.sup.2 ; and X.sup.2 through X.sup.m+1 are chromophores (and again are preferably porphyrinic macrocycles).

  6. RAP Committee Meeting - Transcribed Flipchart Notes

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

    May 8, 2013 Follow Up 1. Send 300 Area advice to committee for final consensus review 2. SAME ↑ for 100 F advice 3. SAME ↑ for LTS advice 4. Future discussion of GW questions in agenda (60+ min) 5. Email presentation to committee today - Susan H. Page 1 Call - Tues 1:30 p.m. 1. Update 3-month work plan 2. June meeting topics table Page

  7. News Media invited to interview Jefferson Lab summer science enrichment

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

    program participants; cover closing Poster Session | Jefferson Lab News Media invited to interview Jefferson Lab summer science enrichment program participants; cover closing Poster Session August 1, 2007 News Media representatives are invited to interview, photograph and/or film participants of Jefferson Lab's summer science enrichment programs as they share their summer experiences and projects with JLab staff during a Poster Session scheduled for Friday, Aug. 3, from 11:30 a.m.-1:30 p.m.

  8. Giant Nanocrystal Quantum Dots as Stable and Efficient Down-Conversion

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

    Phosphor for LED based Solid State Lighting (Technical Report) | SciTech Connect Technical Report: Giant Nanocrystal Quantum Dots as Stable and Efficient Down-Conversion Phosphor for LED based Solid State Lighting Citation Details In-Document Search Title: Giant Nanocrystal Quantum Dots as Stable and Efficient Down-Conversion Phosphor for LED based Solid State Lighting Authors: Kundu, Janardan [1] ; Ghosh, Yagnaseni [1] ; Dennis, Allison M. [1] ; Htoon, Han [1] ; Hollingsworth, Jennifer A

  9. Molecular details of a starch utilization pathway in the human gut symbiont

    Office of Scientific and Technical Information (OSTI)

    Eubacterium rectale (Journal Article) | SciTech Connect Molecular details of a starch utilization pathway in the human gut symbiont Eubacterium rectale Citation Details In-Document Search Title: Molecular details of a starch utilization pathway in the human gut symbiont Eubacterium rectale Authors: Cockburn, Darrell W. ; Orlovsky, Nicole I. ; Foley, Matthew H. ; Kwiatkowski, Kurt J. ; Bahr, Constance M. ; Maynard, Mallory ; Demeler, Borries ; Koropatkin, Nicole M. [1] ; UTSMC) [2] + Show

  10. Nondestructive Three–Dimensional Confocal Imaging and SXRF of Whole

    Office of Scientific and Technical Information (OSTI)

    Stardust Tracks in Aerogel (Conference) | SciTech Connect Conference: Nondestructive Three–Dimensional Confocal Imaging and SXRF of Whole Stardust Tracks in Aerogel Citation Details In-Document Search Title: Nondestructive Three–Dimensional Confocal Imaging and SXRF of Whole Stardust Tracks in Aerogel Authors: White, A.J. ; Ebel, D.S. ; Greenberg, M. [1] ; AMNH) [2] + Show Author Affiliations (NWU) [NWU ( Publication Date: 2014-02-26 OSTI Identifier: 1120954 Resource Type: Conference

  11. Preequilibrium Emission of Light Fragments in Spallation Reactions

    Office of Scientific and Technical Information (OSTI)

    (Conference) | SciTech Connect Conference: Preequilibrium Emission of Light Fragments in Spallation Reactions Citation Details In-Document Search Title: Preequilibrium Emission of Light Fragments in Spallation Reactions No abstract prepared. Authors: Kerby, Leslie M. [1] ; Mashnik, Stepan G. [1] ; Sierk, Arnold John [1] + Show Author Affiliations Los Alamos National Laboratory Publication Date: 2012-08-17 OSTI Identifier: 1049321 Report Number(s): LA-UR-12-22825 TRN: US1204458 DOE Contract

  12. Preliminary Results of Investigating Precompound Emission of Light

    Office of Scientific and Technical Information (OSTI)

    Fragments in Spallation Reactions, Summer 2012 (Technical Report) | SciTech Connect Preliminary Results of Investigating Precompound Emission of Light Fragments in Spallation Reactions, Summer 2012 Citation Details In-Document Search Title: Preliminary Results of Investigating Precompound Emission of Light Fragments in Spallation Reactions, Summer 2012 Authors: Kerby, Leslie M. [1] ; Mashnik, Stepan G. [1] ; Sierk, Arnold John [1] + Show Author Affiliations Los Alamos National Laboratory

  13. Reaction-in-Flight Neutrons and the Stopping Power in Cryogenic NIF

    Office of Scientific and Technical Information (OSTI)

    Capsules (Conference) | SciTech Connect Reaction-in-Flight Neutrons and the Stopping Power in Cryogenic NIF Capsules Citation Details In-Document Search Title: Reaction-in-Flight Neutrons and the Stopping Power in Cryogenic NIF Capsules Authors: Hayes-Sterbenz, Anna Catherine [1] ; Jungman, Gerard [1] ; Boswell, Melissa [1] ; Fowler, Malcolm M. [1] ; Grim, Gary P. [1] ; Klein, Andreas [1] ; Rundberg, Robert S. [1] ; Wilhelmy, Jerry B. [1] ; Wilson, Douglas Carl [1] ; Cerjan, Charles [2] ;

  14. Giant Nanocrystal Quantum Dots as Stable and Efficient Down-Conversion

    Office of Scientific and Technical Information (OSTI)

    Phosphor for LED based Solid State Lighting (Technical Report) | SciTech Connect Technical Report: Giant Nanocrystal Quantum Dots as Stable and Efficient Down-Conversion Phosphor for LED based Solid State Lighting Citation Details In-Document Search Title: Giant Nanocrystal Quantum Dots as Stable and Efficient Down-Conversion Phosphor for LED based Solid State Lighting Authors: Kundu, Janardan [1] ; Ghosh, Yagnaseni [1] ; Dennis, Allison M. [1] ; Htoon, Han [1] ; Hollingsworth, Jennifer A

  15. Hydrothermal corrosion of SiC in LWR coolant environments in the absence of

    Office of Scientific and Technical Information (OSTI)

    irradiation (Journal Article) | SciTech Connect Journal Article: Hydrothermal corrosion of SiC in LWR coolant environments in the absence of irradiation Citation Details In-Document Search Title: Hydrothermal corrosion of SiC in LWR coolant environments in the absence of irradiation Authors: Terrani, Kurt A [1] ; Yang, Ying [1] ; Kim, Young-Jin [2] ; Rebak, Raul [2] ; Meyer III, Harry M [1] ; Gerczak, Tyler J [1] + Show Author Affiliations ORNL General Electric (GE) Publication Date:

  16. Mechanical Behavior of the Near-field Host Rock Surrounding Excavations

    Office of Scientific and Technical Information (OSTI)

    (Technical Report) | SciTech Connect Technical Report: Mechanical Behavior of the Near-field Host Rock Surrounding Excavations Citation Details In-Document Search Title: Mechanical Behavior of the Near-field Host Rock Surrounding Excavations Authors: Kelkar, Sharad M. [1] ; Stauffer, Philip H. [1] ; Robinson, Bruce Alan [1] + Show Author Affiliations Los Alamos National Laboratory Publication Date: 2015-01-09 OSTI Identifier: 1167232 Report Number(s): LA-UR-14-27717 DOE Contract Number:

  17. Petascale, Adaptive CFD (ALCF ESP Technical Report): ALCF-2 Early Science

    Office of Scientific and Technical Information (OSTI)

    Program Technical Report (Technical Report) | SciTech Connect Petascale, Adaptive CFD (ALCF ESP Technical Report): ALCF-2 Early Science Program Technical Report Citation Details In-Document Search Title: Petascale, Adaptive CFD (ALCF ESP Technical Report): ALCF-2 Early Science Program Technical Report Authors: Jansen, K.E. ; Rasquin, M. [1] ; University of Colorado Boulder) [2] + Show Author Affiliations (LCF) ( Publication Date: 2013-05-13 OSTI Identifier: 1079768 Report Number(s):

  18. Comparison of Expanded Preequilibrium CEM Model with CEM03.03 and

    Office of Scientific and Technical Information (OSTI)

    Experimental Data, FY2013 (Technical Report) | SciTech Connect Comparison of Expanded Preequilibrium CEM Model with CEM03.03 and Experimental Data, FY2013 Citation Details In-Document Search Title: Comparison of Expanded Preequilibrium CEM Model with CEM03.03 and Experimental Data, FY2013 Authors: Kerby, Leslie M. [1] ; Mashnik, Stepan G. [1] ; Sierk, Arnold John [1] + Show Author Affiliations Los Alamos National Laboratory [Los Alamos National Laboratory Publication Date: 2013-11-26 OSTI

  19. Developing County-level Water Footprints of Biofuel Produced from

    Office of Scientific and Technical Information (OSTI)

    Switchgrass and Miscanthus x Giganteus in the United States (Technical Report) | SciTech Connect Technical Report: Developing County-level Water Footprints of Biofuel Produced from Switchgrass and Miscanthus x Giganteus in the United States Citation Details In-Document Search Title: Developing County-level Water Footprints of Biofuel Produced from Switchgrass and Miscanthus x Giganteus in the United States Authors: Wu, May M. [1] ; Chiu, Yi-Wen [1] + Show Author Affiliations Argonne National

  20. Fabrication and Hydrothermal Corrosion of NITE-SiC with Various Sintering

    Office of Scientific and Technical Information (OSTI)

    Additives (Conference) | SciTech Connect Conference: Fabrication and Hydrothermal Corrosion of NITE-SiC with Various Sintering Additives Citation Details In-Document Search Title: Fabrication and Hydrothermal Corrosion of NITE-SiC with Various Sintering Additives Authors: Terrani, Kurt A [1] ; Katoh, Yutai [1] ; Parish, Chad M [1] ; Kim, Young-Jin [2] + Show Author Affiliations ORNL General Electric (GE) Publication Date: 2016-01-01 OSTI Identifier: 1237151 DOE Contract Number:

  1. Flow and Thermal Behavior of an EGS Reservoir - Geothermal Code

    Office of Scientific and Technical Information (OSTI)

    Comparison Study (Conference) | SciTech Connect Conference: Flow and Thermal Behavior of an EGS Reservoir - Geothermal Code Comparison Study Citation Details In-Document Search Title: Flow and Thermal Behavior of an EGS Reservoir - Geothermal Code Comparison Study Authors: Kelkar, Sharad M. [1] ; Mclure, Mark [2] ; Ghassemi, Ahmad [3] + Show Author Affiliations Los Alamos National Laboratory University of Texas Austin University of Oklahoma Publication Date: 2015-01-26 OSTI Identifier:

  2. Implementation of micro-ball nanodiamond anvils for high-pressure studies

    Office of Scientific and Technical Information (OSTI)

    above 6Mbar (Journal Article) | SciTech Connect SciTech Connect Search Results Journal Article: Implementation of micro-ball nanodiamond anvils for high-pressure studies above 6Mbar Citation Details In-Document Search Title: Implementation of micro-ball nanodiamond anvils for high-pressure studies above 6Mbar Authors: Dubrovinsky, Leonid ; Dubrovinskaia, Natalia ; Prakapenka, Vitali B. ; Abakumov, Artem M. [1] ; Bayreuth) [2] ; UC) [2] + Show Author Affiliations (Antwerp) ( Publication Date:

  3. In situ measurement of increased ferroelectric/ferroelastic domain wall

    Office of Scientific and Technical Information (OSTI)

    motion in declamped tetragonal lead zirconate titanate thin films (Journal Article) | DOE PAGES DOE PAGES Search Results Publisher's Accepted Manuscript: In situ measurement of increased ferroelectric/ferroelastic domain wall motion in declamped tetragonal lead zirconate titanate thin films Title: In situ measurement of increased ferroelectric/ferroelastic domain wall motion in declamped tetragonal lead zirconate titanate thin films Authors: Wallace, M. [1] Search DOE PAGES for author

  4. Introduction to computed microtomography and applications in Earth science

    Office of Scientific and Technical Information (OSTI)

    (Book) | SciTech Connect Introduction to computed microtomography and applications in Earth science Citation Details In-Document Search Title: Introduction to computed microtomography and applications in Earth science Authors: Rivers, M. [1] + Show Author Affiliations (UC) Publication Date: 2014-12-22 OSTI Identifier: 1168409 Resource Type: Book Resource Relation: Related Information: CMS Workshop Lectures, Advanced Applications of Synchrotron Radiation in Clay Science Publisher: 2014; Tha

  5. tomoRecon : High-speed tomography reconstruction on workstations using

    Office of Scientific and Technical Information (OSTI)

    multi-threading (Conference) | SciTech Connect tomoRecon : High-speed tomography reconstruction on workstations using multi-threading Citation Details In-Document Search Title: tomoRecon : High-speed tomography reconstruction on workstations using multi-threading Authors: Rivers, M. [1] + Show Author Affiliations (UC) [UC Publication Date: 2014-03-11 OSTI Identifier: 1122284 Resource Type: Conference Resource Relation: Conference: Developments in X-Ray Tomography VIII;August 13-15, 2012;San

  6. A new technique to measure tunneling barrier height in solid media

    Office of Scientific and Technical Information (OSTI)

    (Conference) | SciTech Connect A new technique to measure tunneling barrier height in solid media Citation Details In-Document Search Title: A new technique to measure tunneling barrier height in solid media Authors: Mason, Thomas A [1] ; Dattelbaum, Andrew M [1] ; Mara, Nathan A [1] ; Kaschner, George C [1] ; Johnson, Oliver K [2] ; Seegmiller, Daniel [2] ; Fullwood, David T [2] + Show Author Affiliations Los Alamos National Laboratory BYU Publication Date: 2011-05-24 OSTI Identifier:

  7. A statistical perspective of validation and UQ (Conference) | SciTech

    Office of Scientific and Technical Information (OSTI)

    Connect statistical perspective of validation and UQ Citation Details In-Document Search Title: A statistical perspective of validation and UQ Authors: Higdon, David M [1] + Show Author Affiliations Los Alamos National Laboratory [Los Alamos National Laboratory Publication Date: 2011-10-24 OSTI Identifier: 1114420 Report Number(s): LA-UR-11-06111; LA-UR-11-6111 DOE Contract Number: AC52-06NA25396 Resource Type: Conference Resource Relation: Conference: Workshop on Verification and

  8. Bayesian approaches for combining computational model output and physical

    Office of Scientific and Technical Information (OSTI)

    observations (Conference) | SciTech Connect Bayesian approaches for combining computational model output and physical observations Citation Details In-Document Search Title: Bayesian approaches for combining computational model output and physical observations Authors: Higdon, David M [1] ; Lawrence, Earl [1] ; Heitmann, Katrin [2] ; Habib, Salman [2] + Show Author Affiliations Los Alamos National Laboratory ANL Publication Date: 2011-07-25 OSTI Identifier: 1084581 Report Number(s):

  9. Electro-Magnetic Dipole Properties of The Even-Even {sup 160}Gd Nucleus in The Spectroscopic Region

    SciTech Connect (OSTI)

    Ertugral, Filiz; Kuliev, Ali; Guliyev, Ekber

    2008-11-11

    In this study result of calculations using rotational, translational and Galilean invariant quasiparticle random-phase approximation is presented for the low lying dipole excitations in the even-even {sup 60}Gd nucleus. To make detail structure analysis for electric and magnetic dipole states, calculations carried out for both {delta}K = 1 and {delta}K = 0 branches. The analysis shows that almost all transitions with {delta}K = 1 are magnetic character in 2.4 divide 4 MeV energy interval. However, the calculations indicate the presence of a few prominent negative parity K{sup {pi}} = 1 states in the investigated energy interval, one of them with rather high E1 strength B(E1) = 7.1{center_dot}10{sup -3} e{sup 2} fm{sup 2} at energy 3.2 MeV. Calculated M1 dipole strength of the scissors mode K{sup {pi}} = 1{sup +} excitations clustered in two groups around 2.7 and 3.3 MeV. A similar situation arises for the experimentally obtained states two bumps around {omega}{sub i} = 2.7 MeV and {omega}{sub i} = 3.3 MeV. It has been shown that main part of spin-1 states, observed at energy 2.4 divide 4 MeV in {sup 160}Gd may be attributed to have M1 character and may be interpreted as main fragments of the scissors mode. However, it is apparent that the experimental data exceeds the calculation results for the summed B(M1) by a factor of 1.13 for M1 transitions.

  10. liu-99.PDF

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

    Calibration of the Passive Cavity Aerosol Spectrometer Probe, Estimation of Refractive Index, and Closure of Light-Scattering Coefficients Y. Liu and P. H. Daum Brookhaven National Laboratory Environmental Chemistry Division Upton, New York Introduction Optical counters such as the Passive Cavity Aerosol Spectrometer Probe (PCASP) (PMS, Inc., Boulder, Colorado) are often calibrated with latex particles having a refractive index m = 1.588. Because refractive indices of ambient aerosols are often

  11. ARM - VAP Process - masc

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    Productsmasc Documentation & Plots Data Management Facility Plots (Quick Looks) ARM Data Discovery Browse Data Comments? We would love to hear from you! Send us a note below or call us at 1-888-ARM-DATA. Send VAP : Multi-Angle Snowflake Camera (MASC) Instrument Categories Surface Meteorology Primary Measurements The following measurements are those considered scientifically relevant. Hydrometeor fall velocity Locations ARM Mobile Facility OLI M1 Browse Data Olikiok Point, Alaska; AMF3

  12. ARM - Instrument - masc

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    govInstrumentsmasc Documentation ARM Data Discovery Browse Data Comments? We would love to hear from you! Send us a note below or call us at 1-888-ARM-DATA. Send Instrument : Multi-Angle Snowflake Camera (MASC) Instrument Categories Surface Meteorology Output Datastreams masc : Multi-angle Snowflake Camera Primary Measurements The following measurements are those considered scientifically relevant. Hydrometeor fall velocity Locations ARM Mobile Facility OLI M1 Browse Data Olikiok Point, Alaska;

  13. Volttron Technical meeting

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

    VOLTTRON Technical Meeting Virginia Tech Advanced Research Institute July 2015 Our mission * Accelerate clean energy technologies, companies and projects * Create high-quality jobs and long-term economic growth * Support municipal clean energy projects * Invest in residential and commercial renewable energy installations * Cultivate a robust marketplace for innovation Wind Turbine Testing Facility Boston, Massachusetts Mass Energy Landscape/Challenges * M! #1 in energy efficiency but ... *

  14. Scalable superhydrophobic coatings based on fluorinated diatomaceous earth

    Office of Scientific and Technical Information (OSTI)

    (Journal Article) | SciTech Connect Scalable superhydrophobic coatings based on fluorinated diatomaceous earth Citation Details In-Document Search Title: Scalable superhydrophobic coatings based on fluorinated diatomaceous earth Authors: Polyzos, Georgios [1] ; Winter, Kyle O [1] ; Lance, Michael J [1] ; Meyer III, Harry M [1] ; Armstrong, Beth L [1] ; Schaeffer, Daniel A [1] ; Simpson, John T [1] ; Hunter, Scott Robert [1] ; Datskos, Panos G [1] ; Demko, Jonathan A [1] + Show Author

  15. Structures of two distinct conformations of holo-non-ribosomal peptide

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    synthetases (Journal Article) | SciTech Connect Structures of two distinct conformations of holo-non-ribosomal peptide synthetases Citation Details In-Document Search Title: Structures of two distinct conformations of holo-non-ribosomal peptide synthetases Authors: Drake, Eric J. ; Miller, Bradley R. ; Shi, Ce ; Tarrasch, Jeffrey T. ; Sundlov, Jesse A. ; Allen, C. Leigh ; Skiniotis, Georgios ; Aldrich, Courtney C. ; Gulick, Andrew M. [1] ; UMM) [2] ; HWMRI) [2] + Show Author Affiliations

  16. Synchrotron x-Ray Spectroscopic Analysis (Book) | SciTech Connect

    Office of Scientific and Technical Information (OSTI)

    Book: Synchrotron x-Ray Spectroscopic Analysis Citation Details In-Document Search Title: Synchrotron x-Ray Spectroscopic Analysis Authors: Sutton, S.R. ; Newville, M. [1] + Show Author Affiliations (UC) [UC Publication Date: 2014-02-26 OSTI Identifier: 1120008 Resource Type: Book Resource Relation: Related Information: Treatise on Geochemistry Publisher: 2014; Elsevier;Cambridge, MA ;H. Holland, K. Turekian, eds.;213-230 Research Org: Advanced Photon Source (APS), Argonne National Laboratory

  17. THE VEX RADIATION MODULE: 2D RADIATION TRANSPORT WITH MIMETIC DIFFUSION FOR

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    EXAFLAG (Conference) | SciTech Connect THE VEX RADIATION MODULE: 2D RADIATION TRANSPORT WITH MIMETIC DIFFUSION FOR EXAFLAG Citation Details In-Document Search Title: THE VEX RADIATION MODULE: 2D RADIATION TRANSPORT WITH MIMETIC DIFFUSION FOR EXAFLAG Authors: Powell, Devon M. [1] ; Lovegrove, Elizabeth G. [1] ; Fung, Jimmy [1] ; Kenamond, Mark A. [1] + Show Author Affiliations Los Alamos National Laboratory Publication Date: 2013-08-16 OSTI Identifier: 1090702 Report Number(s): LA-UR-13-26513

  18. The Community Climate System Model Version 4 (Journal Article) | SciTech

    Office of Scientific and Technical Information (OSTI)

    Connect Authors: Gent, Peter [1] ; Donner, Leo [2] ; Holland, Markia [1] ; Hunke, Elizabeth [3] ; Jayne, Steve [4] ; Lawrence, David M. [1] ; Neale, Richard B. [1] ; Rasch, Philip J. [5] ; Vertenstein, Mariana [1] ; Worley, Patrick H [6] ; Yang, Zong-Liang [7] ; Zhang, Minghua [8] + Show Author Affiliations National Center for Atmospheric Research (NCAR) NOAA Geophysical Fluid Dynamics Laboratory (GFDL), Princeton, NJ Los Alamos National Laboratory (LANL) Woods Hole Oceanographic Institution

  19. The Red Storm Architecture and Early Experiences With Multi-Core Processors

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    (Journal Article) | SciTech Connect With Multi-Core Processors Citation Details In-Document Search Title: The Red Storm Architecture and Early Experiences With Multi-Core Processors Authors: Tomkins, James L [1] ; Brightwell, Ron [1] ; Camp, William J [1] ; Dosanjh, Sudip [1] ; Kelly, Suzanne M [1] ; Lin, Paul T. [1] ; Vaughan, Courtenay T. [1] ; Levesque, John [2] ; Tipparaju, Vinod [3] + Show Author Affiliations Sandia National Laboratories (SNL) Cray, Inc. ORNL Publication Date:

  20. The SWIFT Tilearchy (Conference) | SciTech Connect

    Office of Scientific and Technical Information (OSTI)

    The SWIFT Tilearchy Citation Details In-Document Search Title: The SWIFT Tilearchy Authors: Nelson, Eric Michael [1] ; Aulwes, Robbie Tuan [1] ; Bement, Matthew Thomas [1] ; Campbell, Joann Marie [1] ; Ferenbaugh, Charles Roger [1] ; Fung, Jimmy [1] ; Jean, Brian Altom [1] ; Kelley, Timothy M. [1] ; Lally, Bryan Richard [1] ; Kenamond, Mark Andrew [1] + Show Author Affiliations Los Alamos National Laboratory [Los Alamos National Laboratory Publication Date: 2014-07-31 OSTI Identifier: 1148940

  1. The effects of dilution on turbulence and transport in C-Mod ohmic plasmas

    Office of Scientific and Technical Information (OSTI)

    and comparisons with gyrokinetic simulations (Journal Article) | SciTech Connect The effects of dilution on turbulence and transport in C-Mod ohmic plasmas and comparisons with gyrokinetic simulations Citation Details In-Document Search This content will become publicly available on July 13, 2016 Title: The effects of dilution on turbulence and transport in C-Mod ohmic plasmas and comparisons with gyrokinetic simulations Authors: Ennever, P. [1] ; Porkolab, M. [1] ; Candy, J. [2] ; Staebler,

  2. Time-resolved carrier distributions in graphene (Conference) | SciTech

    Office of Scientific and Technical Information (OSTI)

    Connect Conference: Time-resolved carrier distributions in graphene Citation Details In-Document Search Title: Time-resolved carrier distributions in graphene Authors: Gilbertson, Steve Michael [1] ; Durakiewicz, Tomasz [1] ; Zhu, Jian - Xin [1] ; Mohite, Aditya D [1] ; Dattelbaum, Andrew M [1] ; Rodtiguez, George [1] ; Dakovski, Georgi [2] ; Dani, Keshav M [3] + Show Author Affiliations Los Alamos National Laboratory SLAC OKINAWA INSTITUTE OF SCIENCE AND TECHNOLOGY Publication Date:

  3. Media Advisory: Poster Session Highlights Projects, Research Carried Out by

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

    Summer Interns at Jefferson Lab | Jefferson Lab Aug. 1, 2014 Time: 11:45 a.m. - 1 p.m. Place: The CEBAF Center lobby at Jefferson Lab, 12000 Jefferson Avenue, Newport News, VA 23606 Event: More than 40 high school students and college undergraduates who participated in summer science internship programs at the Department of Energy's Thomas Jefferson National Accelerator Facility, or Jefferson Lab, will share with invited guests and members of the lab community results from their respective

  4. Ultrafast Laser Fabrication: a Rapid Prototyping Capability for CINT

    Office of Scientific and Technical Information (OSTI)

    (Technical Report) | SciTech Connect Technical Report: Ultrafast Laser Fabrication: a Rapid Prototyping Capability for CINT Citation Details In-Document Search Title: Ultrafast Laser Fabrication: a Rapid Prototyping Capability for CINT Authors: McCulloch, Quinn [1] ; Dattelbaum, Andrew M. [1] ; Nath, Pulak [1] + Show Author Affiliations Los Alamos National Laboratory Publication Date: 2013-03-04 OSTI Identifier: 1067392 Report Number(s): LA-UR-13-21541 DOE Contract Number: AC52-06NA25396

  5. Using vanadium in spinel as a sensor of oxygen fugacity in meteorites:

    Office of Scientific and Technical Information (OSTI)

    Applications to Mars, Vesta, and other asteroids (Conference) | SciTech Connect Using vanadium in spinel as a sensor of oxygen fugacity in meteorites: Applications to Mars, Vesta, and other asteroids Citation Details In-Document Search Title: Using vanadium in spinel as a sensor of oxygen fugacity in meteorites: Applications to Mars, Vesta, and other asteroids Authors: Righter, K. ; Sutton, S. ; Danielson, L. ; Pando, K. ; Le, L. ; Newville, M. [1] ; NASA JSC) [2] ; Hamilton Sundstrand) [2]

  6. PHASE II REMEDIAL INVESTlGATlOE FORMER AMCHITKA ARMY AIR BASE

    Office of Legacy Management (LM)

    lWE&PREENING MEMORANDUL PHASE II REMEDIAL INVESTlGATlOE FORMER AMCHITKA ARMY AIR BASE AMCHITKA ISLAND, ALAS0 February 199: 111 IIllllllllllllllllllllll1111 AMC 0001 08 Submitted To: Department of the Army Alaska District, Corps of Engineers By: Shannon &Wilson, Inc. 2055 Hill Road Fairbanks, Alaska 997094244 TABLE OF CONTENTS m 1.0 INTRODUCTION .............................................................................................................. 1-1 2.0 SCOPE OF THE REMEDIAL

  7. Title FREEDOM OF INFORMATION ACT REQUEST (FOT

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

    ... 3c - 40 woM 4- 0) LI 0i 4W. U .- 0 o .)(-' gg -bI- C) .0 vC cc >0 Aau- C 4-1. 0 0 n cvJ ... Cu > d > .OE -00G a) M 4- toWa . c S- m +1GG)L o 4-) (2 0 00 4- I -M 4al ch -) 1 S- ...

  8. Office of Secure Transportation Ten-Year Site Plan

    National Nuclear Security Administration (NNSA)

    Secure Transportation Ten-Year Site Plan Fiscal Year 2016 OST M 1.02 Prepared by Facilities Management Branch NOTICE This report was prepared as an account of work sponsored by an agency of the United States Government. Neither the United States Government, nor any agency thereof, nor any of their employees makes any warranty, express or implied, or assumes any legal liability or responsibility for the accuracy, completeness, or usefulness of any information, apparatus, product, or process

  9. Section J

    Energy Savers [EERE]

    M-1 Section J Appendix M Key Design, Licensing and Site Management M&O Milestone Chart Activity Planned Date Develop and Submit CD-2 (25%-30%) 08/2009 Submission of Construction Performance Specifications - Balance of Plant Support Facilities (OCRWM Start of Construction 3/2012) TBD Submission of Construction Performance Specifications - Initial Handling Facility (IHF) (OCRWM Start of Construction for IHF: 9/2013) TBD Submission of Construction Performance Specifications - Wet Handling

  10. Sustainable Nano-Materials: What is happening at the cellular level?

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

    Nano-Materials What is happening at the cellular level? Art J. Ragauskas, Institute of Paper Science and Technology Georgia Institute of Technology Advanced Materials: Cellular Level Chemicals Enzymes Mechanical 1 cm 10 m 1 m 10 nm 100 m mm nm Micro Fibrillated Cellulose NanoCellulose Balls Cellulose Whiskers Composite Whisker Films Water Based polymer + Whiskers>> Easy Dispersions Matrix = hydrosoluble polymers Water evaporation nanocomposite film Poly(oxyethylene) Xylans; Hemis

  11. NO reduction using sublimation of cyanuric acid

    DOE Patents [OSTI]

    Perry, R.A.

    1996-05-21

    A method of reducing the NO content of a gas stream comprises contacting the gas stream with an amount of HNCO at a temperature effective for heat-induced decomposition of cyanuric acid, said amount and temperature being effective for the resultant lowering of the NO content of the gas stream, said cyanuric acid being particulate and having a particle size of less than 90 {micro}m. 1 fig.

  12. DOE-STD-1153-2002; A Graded Approach for Evaluating Radiation Doses to Aquatic and Terrestrial Biota

    Office of Environmental Management (EM)

    1 PRINCIPLES AND APPLICATION MODULE 1: PRINCIPLES AND APPLICATION DOE-STD-1153-2002 INTENTIONALLY BLANK DOE-STD-1153-2002 M1-1 1 Introduction The U.S. Department of Energy (DOE) is accountable to Congress and the public for the safe conduct of its activities, including facility operation, waste management and disposal activities, and remediation of environmental contamination. These routine activities may result in releases of radionuclides to the air and water, accumulation of radionuclides in

  13. Document

    Office of Environmental Management (EM)

    279 Federal Register / Vol. 71, No. 13 / Friday, January 20, 2006 / Notices ACTION: Notice of public meeting agenda. DATE AND TIME: Thursday, February 2, 2006, 10 a.m.-1 p.m. PLACE: Hyatt Regency (Valley Forge Room), 400 New Jersey Avenue, NW., Washington, DC 20001. (Metro Stop: Union Station). AGENDA: The Commission will receive the following reports: Title II Requirements Payments Update; and updates on other administrative matters. The Commission will receive presentations on the following

  14. DOE-STD-1153-2002; A Graded Approach for Evaluating Radiation Doses to Aquatic and Terrestrial Biota

    National Nuclear Security Administration (NNSA)

    STD-1153-2002 A Graded Approach for Evaluating Radiation Doses to Aquatic and Terrestrial Biota MODULE 1 PRINCIPLES AND APPLICATION MODULE 1: PRINCIPLES AND APPLICATION DOE-STD-1153-2002 INTENTIONALLY BLANK DOE-STD-1153-2002 M1-1 1 Introduction The U.S. Department of Energy (DOE) is accountable to Congress and the public for the safe conduct of its activities, including facility operation, waste management and disposal activities, and remediation of environmental contamination. These routine

  15. Microsoft Word - 03-11-09 Agenda FINAL.doc

    National Nuclear Security Administration (NNSA)

    AGENDA CAB FULL BOARD MEETING Atomic Testing Museum, Frank Rogers Auditorium 755 East Flamingo Road, Las Vegas, NV 89119 March 11, 2009 - 5:00 p.m. 1. Open Meeting / Agenda Review Denise Rupp, Facilitator 2. Chair's Opening Remarks: Dave Hermann, Board Chair Agenda Approval 3. Public Comment Denise Rupp, Facilitator 4. Presentation: Cultural Resources at the NTS Linda Cohn, NNSA/NV 5. Committee Updates: Budget Committee Jack Ramsey, Committee Chair Committee's recommendation letter for Board

  16. Nuclear Material Transaction Report nrc741_1

    National Nuclear Security Administration (NNSA)

    A A M 1 1 1 1 COMPANY NAME COMPANY ADDRESS CITY, STATE ZIP CODE CONTACT COMPANY NAME COMPANY ADDRESS CITY, STATE ZIP CODE CONTACT 2 1 32 50 -1042.00 2 32 50 1002.00 03 31 2008 004 A01 1 2 NP NP PRODUCTION PRODUCTION 50 50 309 309 J J -105736.00 105736.00 13.2962 13.2962 -88991.00 88905.00 Example 2-m-a

  17. BRIGHTEST CLUSTER GALAXIES AT THE PRESENT EPOCH

    SciTech Connect (OSTI)

    Lauer, Tod R.; Postman, Marc; Strauss, Michael A.; Graves, Genevieve J.; Chisari, Nora E.

    2014-12-20

    We have obtained photometry and spectroscopy of 433 z ? 0.08 brightest cluster galaxies (BCGs) in a full-sky survey of Abell clusters to construct a BCG sample suitable for probing deviations from the local Hubble flow. The BCG Hubble diagram over 0 < z < 0.08 is consistent to within 2% of the Hubble relation specified by a ? {sub m} = 0.3, ? = 0.7 cosmology. This sample allows us to explore the structural and photometric properties of BCGs at the present epoch, their location in their hosting galaxy clusters, and the effects of the cluster environment on their structure and evolution. We revisit the L{sub m} -? relation for BCGs, which uses ?, the log-slope of the BCG photometric curve of growth, to predict the metric luminosity in an aperture with 14.3kpc radius, L{sub m} , for use as a distance indicator. Residuals in the relation are 0.27mag rms. We measure central stellar velocity dispersions, ?, of the BCGs, finding the Faber-Jackson relation to flatten as the metric aperture grows to include an increasing fraction of the total BCG luminosity. A three-parameter ''metric plane'' relation using ? and ? together gives the best prediction of L{sub m} , with 0.21mag residuals. The distribution of projected spatial offsets, r{sub x} of BCGs from the X-ray-defined cluster center is a steep ? = 2.33 power law over 1 < r{sub x} < 10{sup 3}kpc. The median offset is ?10kpc, but ?15% of the BCGs have r{sub x} > 100kpc. The absolute cluster-dispersion normalized BCG peculiar velocity |?V {sub 1}|/? {sub c} follows an exponential distribution with scale length 0.39 0.03. Both L{sub m} and ? increase with ? {sub c}. The ? parameter is further moderated by both the spatial and velocity offset from the cluster center, with larger ? correlated with the proximity of the BCG to the cluster mean velocity or potential center. At the same time, position in the cluster has little effect on L{sub m} . Likewise, residuals from the metric plane show no correlation with either the spatial or velocity offset from the cluster center. The luminosity difference between the BCG and second-ranked galaxy, M2, increases as the peculiar velocity of the BCG within the cluster decreases. Further, when M2 is a close luminosity ''rival'' of the BCG, the galaxy that is closest to either the velocity or X-ray center of the cluster is most likely to have the larger ?. We conclude that the inner portions of the BCGs are formed outside the cluster, but interactions in the heart of the galaxy cluster grow and extend the envelopes of the BCGs.

  18. Magnetism and magnetocaloric effect in multicomponent Laves-phase compounds: Study and comparative analysis

    SciTech Connect (OSTI)

    Ćwik, J.

    2014-01-15

    This paper presents a review and results of comparative study of the influence of Gd on some physical properties of (R{sub 0.9}R′{sub 0.1}){sub 1−x}Gd{sub x}Co{sub 2} solid solutions with R=Dy, Ho and R′=Er, Ho and x varied from 0.05 to 0.15. Powder X-ray diffraction analysis performed at room temperature revealed that all studied solid solutions solidify with the formation of a Laves-phase MgCu{sub 2}-type structure (space group Fd−3m). The magnetization behavior and the magnetic transition are analyzed in terms of the Landau theory. The studies of magnetic properties and heat capacity showed that a relatively small Gd addition significantly increases T{sub C} of the compounds. The maximum percentage increase in T{sub C}, namely, ∼43% was observed for (Ho{sub 0.9}Er{sub 0.1}){sub 1−x}Gd{sub x}Co{sub 2}. However, the highest temperature was noted for the (Dy{sub 0.9}Ho{sub 0.1}){sub 0.85}Gd{sub 0.15}Co{sub 2} solid solution; it is T{sub C}=183.4 K. Below the ordering temperature, all samples are ferrimagnetically ordered; at high temperatures, they are Curie–Weiss paramagnets. Moreover, a small Gd addition eliminates the field-induced magnetic transition near T{sub C} and, as consequence, transforms the nature of magnetic transition from the first- to second-order. The magnetocaloric effect has been estimated in terms of both isothermal magnetic entropy and adiabatic temperature changes. The highest adiabatic temperature change ΔT{sub ad}=3 K and highest isothermal entropy change ΔS{sub mag}=12.1 J/kg K were observed for (Ho{sub 0.9}Er{sub 0.1}){sub 0.95}Gd{sub 0.05}Co{sub 2} at ∼90 K in magnetic fields of 2 T and 3 T, respectively. A decrease in the entropy change has been observed with increasing Gd content in all studied samples. The smallest values of ΔS{sub mag} were observed for the (Dy{sub 0.9}Ho{sub 0.1}){sub 1−x}Gd{sub x}Co{sub 2} solid solutions. Under an external field change of from 0 to 3 T, the maximum entropy change for (Dy{sub 0.9}Ho{sub 0.1}){sub 1−x}Gd{sub x}Co{sub 2} compounds decreases from 6.9 at x=0.05–4.3 J/kg K at x=0.15. The refrigerant capacity for all solid solutions (with 0.05≤x≤0.15) is reported. The effect of increasing Gd content in the solid solutions on their magnetic and magnetocaloric properties is discussed. - Graphical abstract: Temperature dependencies of ΔT{sub ad} induced by µ{sub 0}H=1 and 2 T in (a) (Ho{sub 0.9}Er{sub 0.1}){sub 1−x}Gd{sub x}Co{sub 2} and (b) (Dy{sub 0.9}Er{sub 0.1}){sub 1−x}Gd{sub x}Co{sub 2} solid solutions. Display Omitted.

  19. DEMOGRAPHICS OF THE GALAXIES HOSTING SHORT-DURATION GAMMA-RAY BURSTS

    SciTech Connect (OSTI)

    Fong, W.; Berger, E.; Chornock, R.; Margutti, R.; Czekala, I.; Zauderer, B. A.; Laskar, T.; Servillat, M. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Levan, A. J.; Tunnicliffe, R. L. [Department of Physics, University of Warwick, Coventry CV4 7AL (United Kingdom); Tanvir, N. R. [Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH (United Kingdom); Fox, D. B. [Department of Astronomy and Astrophysics, 525 Davey Laboratory, Pennsylvania State University, University Park, PA 16802 (United States); Perley, D. A. [Cahill Center for Astronomy and Astrophysics, Room 232, California Institute of Technology, Pasadena, CA 91125 (United States); Cenko, S. B. [Department of Astronomy, University of California, Berkeley, CA 94720-3411 (United States); Persson, S. E.; Monson, A. J.; Kelson, D. D.; Birk, C.; Murphy, D. [Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101 (United States); Anglada, G. [Institut fuer Astrophysik, Friedrich-Hund-Platz 1, Universitaet Goettingen, D-37077 Goettingen (Germany)

    2013-05-20

    We present observations of the afterglows and host galaxies of three short-duration gamma-ray bursts (GRBs): 100625A, 101219A, and 110112A. We find that GRB 100625A occurred in a z = 0.452 early-type galaxy with a stellar mass of Almost-Equal-To 4.6 Multiplication-Sign 10{sup 9} M{sub Sun} and a stellar population age of Almost-Equal-To 0.7 Gyr, and GRB 101219A originated in a star-forming galaxy at z = 0.718 with a stellar mass of Almost-Equal-To 1.4 Multiplication-Sign 10{sup 9} M{sub Sun }, a star formation rate of Almost-Equal-To 16 M{sub Sun} yr{sup -1}, and a stellar population age of Almost-Equal-To 50 Myr. We also report the discovery of the optical afterglow of GRB 110112A, which lacks a coincident host galaxy to i {approx}> 26 mag, and we cannot conclusively identify any field galaxy as a possible host. From afterglow modeling, the bursts have inferred circumburst densities of Almost-Equal-To 10{sup -4}-1 cm{sup -3} and isotropic-equivalent gamma-ray and kinetic energies of Almost-Equal-To 10{sup 50}-10{sup 51} erg. These three events highlight the diversity of galactic environments that host short GRBs. To quantify this diversity, we use the sample of 36 Swift short GRBs with robust associations to an environment ({approx}1/2 of 68 short bursts detected by Swift to 2012 May) and classify bursts originating from four types of environments: late-type ( Almost-Equal-To 50%), early-type ( Almost-Equal-To 15%), inconclusive ( Almost-Equal-To 20%), and ''host-less'' (lacking a coincident host galaxy to limits of {approx}> 26 mag; Almost-Equal-To 15%). To find likely ranges for the true late- and early-type fractions, we assign each of the host-less bursts to either the late- or early-type category using probabilistic arguments and consider the scenario that all hosts in the inconclusive category are early-type galaxies to set an upper bound on the early-type fraction. We calculate most likely ranges for the late- and early-type fractions of Almost-Equal-To 60%-80% and Almost-Equal-To 20%-40%, respectively. We find no clear trend between gamma-ray duration and host type. We also find no change to the fractions when excluding events recently claimed as possible contaminants from the long GRB/collapsar population. Our reported demographics are consistent with a short GRB rate driven by both stellar mass and star formation.

  20. PLANETS AROUND LOW-MASS STARS (PALMS). IV. THE OUTER ARCHITECTURE OF M DWARF PLANETARY SYSTEMS

    SciTech Connect (OSTI)

    Bowler, Brendan P.; Liu, Michael C.; Shkolnik, Evgenya L.; Tamura, Motohide

    2015-01-01

    We present results from a high-contrast adaptive optics imaging search for giant planets and brown dwarfs (≳1 M {sub Jup}) around 122 newly identified nearby (≲40 pc) young M dwarfs. Half of our targets are younger than 135 Myr and 90% are younger than the Hyades (620 Myr). After removing 44 close stellar binaries (implying a stellar companion fraction of >35.4% ± 4.3% within 100 AU), 27 of which are new or spatially resolved for the first time, our remaining sample of 78 single M dwarfs makes this the largest imaging search for planets around young low-mass stars (0.1-0.6 M {sub ☉}) to date. Our H- and K-band coronagraphic observations with Keck/NIRC2 and Subaru/HiCIAO achieve typical contrasts of 12-14 mag and 9-13 mag at 1'', respectively, which correspond to limiting planet masses of 0.5-10 M {sub Jup} at 5-33 AU for 85% of our sample. We discovered four young brown dwarf companions: 1RXS J235133.3+312720 B (32 ± 6 M {sub Jup}; L0{sub −1}{sup +2}; 120 ± 20 AU), GJ 3629 B (64{sub −23}{sup +30} M {sub Jup}; M7.5 ± 0.5; 6.5 ± 0.5 AU), 1RXS J034231.8+121622 B (35 ± 8 M {sub Jup}; L0 ± 1; 19.8 ± 0.9 AU), and 2MASS J15594729+4403595 B (43 ± 9 M {sub Jup}; M8.0 ± 0.5; 190 ± 20 AU). Over 150 candidate planets were identified; we obtained follow-up imaging for 56% of these but all are consistent with background stars. Our null detection of planets enables strong statistical constraints on the occurrence rate of long-period giant planets around single M dwarfs. We infer an upper limit (at the 95% confidence level) of 10.3% and 16.0% for 1-13 M {sub Jup} planets between 10-100 AU for hot-start and cold-start (Fortney) evolutionary models, respectively. Fewer than 6.0% (9.9%) of M dwarfs harbor massive gas giants in the 5-13 M {sub Jup} range like those orbiting HR 8799 and β Pictoris between 10-100 AU for a hot-start (cold-start) formation scenario. The frequency of brown dwarf (13-75 M {sub Jup}) companions to single M dwarfs between 10-100 AU is 2.8{sub −1.5}{sup +2.4}%. Altogether we find that giant planets, especially massive ones, are rare in the outskirts of M dwarf planetary systems. Although the first directly imaged planets were found around massive stars, there is currently no statistical evidence for a trend of giant planet frequency with stellar host mass at large separations as predicted by the disk instability model of giant planet formation.

  1. Dipole strength in the {sup 235}U(gamma,gamma{sup '}) reaction up to 2.8 MeV

    SciTech Connect (OSTI)

    Yevetska, O.; Enders, J.; Fritzsche, M.; Neumann-Cosel, P. von; Romig, C.; Savran, D.; Sonnabend, K.; Oberstedt, S.; Richter, A.

    2010-04-15

    Spectra of the {sup 235}U(gamma,gamma{sup '}) reaction were measured at the S-DALINAC at bremsstrahlung end-point energies E{sub 0}=3.5 and 4.4 MeV and scattering angles of 90 deg. and 135 deg. with respect to the beam axis. Discrete transitions are observed at excitation energies below 2.3 MeV only. The deduced cross sections are in rough agreement with the findings of Bertozzi et al. [Phys. Rev. C 78, 041601(R) (2008)] except for the most prominent transition, where the present result is lower by a factor of about 2. Evidence for unresolved dipole strength is found in the spectra by means of a fluctuation analysis, which was carried out up to an excitation energy of 2.8 MeV. If this unresolved strength exhibits the same ratio of E1/M1 cross sections as observed in the even-mass neighbor {sup 236}U, then the energy centroid E{sub x}=2.5(3) MeV and total strength SIGMAB(M1)arrow up=3.6(1.3)mu{sub N}{sup 2} of the M1 part are in good agreement with the systematics of the scissors mode in even-even actinide nuclei.

  2. Magnetic dipole sequences in {sup 83}Rb

    SciTech Connect (OSTI)

    Schwengner, R.; Schnare, H.; Wagner, A.; Doenau, F.; Rainovski, G.; Frauendorf, S.; Jungclaus, A.; Hausmann, M.; Lieb, K. P.; Yordanov, O.; Napoli, D. R.; De Angelis, G.; Axiotis, M.; Marginean, N.; Brandolini, F.; Alvarez, C. Rossi

    2009-10-15

    High-spin states in {sup 83}Rb were populated in the reaction {sup 11}B+{sup 76}Ge at beam energies of 45 and 50 MeV. {gamma} rays were detected with the spectrometer GASP. The level scheme of {sup 83}Rb was extended up to 13.9 MeV. Mean lifetimes of 23 levels were determined using the Doppler-shift-attenuation method. Among the bands newly established is a sequence comprising intense M1 transitions and crossover E2 transitions. This sequence turns out to be irregular and thus shows that magnetic rotation as observed in the neighboring odd-odd isotopes is not realized in this odd-even nuclide. Excited states in {sup 83}Rb were interpreted in terms of the shell model using the model space {pi}(0f{sub 5/2},1p{sub 3/2},1p{sub 1/2},0g{sub 9/2}) {nu}(1p{sub 1/2},0g{sub 9/2}). The configurations predicted for the negative-parity M1 sequence reproduce the M1 transition strengths fairly well.

  3. Glass-ceramic joint and method of joining

    DOE Patents [OSTI]

    Meinhardt, Kerry D [Richland, WA; Vienna, John D [West Richland, WA; Armstrong, Timothy R [Clinton, TN; Pederson, Larry R [Kennewick, WA

    2003-03-18

    The present invention is a glass-ceramic material and method of making useful for joining a solid ceramic component and at least one other solid component. The material is a blend of M1-M2-M3, wherein M1 is BaO, SrO, CaO, MgO, or combinations thereof, M2 is Al.sub.2 O.sub.3, present in the blend in an amount from 2 to 15 mol %, M3 is SiO.sub.2 with up to 50 mol % B.sub.2 O.sub.3 that substantially matches a coefficient of thermal expansion of the solid electrolyte. According to the present invention, a series of glass ceramics in the M1-Al.sub.2 O.sub.3 -M3 system can be used to join or seal both tubular and planar solid oxide fuel cells, oxygen electrolyzers, and membrane reactors for the production of syngas, commodity chemicals and other products.

  4. Crystal structure and hydrogenation properties of pseudo-binary Mg{sub 6}Pd{sub 0.5}Ni{sub 0.5} complex metallic alloy

    SciTech Connect (OSTI)

    Cuevas, F.; Latroche, M.

    2009-10-15

    The crystal structure of the Ni-substituted Mg{sub 6.10(2)}Pd{sub 0.52(2)}Ni{sub 0.41(2)} complex metallic alloy has been determined by X-ray and neutron powder diffraction. The reaction of this compound at 573 K towards deuterium absorption for pressures up to 23 bar has also been studied. The crystal structure of Mg{sub 6.10(2)}Pd{sub 0.52(2)}Ni{sub 0.41(2)} compound was determined in the light of Samson's [Acta Crystallogr. B 28 (1972) 936) and Makongo's (Philos. Mag. 86 (2006) 427] models for the binary Mg{sub 6}Pd compound. It crystallizes in F4-bar3m space group with lattice parameter 20.13331(7) A. The refined unit-cell composition is Mg{sub 342(1)}Pd{sub 29(1)}Ni{sub 23(1)} with Z=56. Nickel by palladium substitution is not fully random. Nickel atoms preferentially locate on Pd sites with low coordination number due to steric effects. Deuterium uptake is 9.6 D/f.u. under the given conditions of pressure and temperature. Upon absorption, the intermetallic compound disproportionates into MgD{sub 2}, Mg{sub 5}Pd{sub 2} and Mg{sub 2}NiD{sub 4} phases. The Mg{sub 2}NiD{sub 4} phase is observed to crystallize in the orthorhombic LT2 modification for which an averaged crystal structure in the Pcc2 space group is proposed. - Graphical abstract: Coordination polyhedron around site Mg14 in pseudobinary Mg{sub 6}(Pd,Ni) compounds.

  5. Variable accretion processes in the young binary-star system UY Aur

    SciTech Connect (OSTI)

    Stone, Jordan M.; Eisner, J. A.; Kulesa, Craig; McCarthy, Don; Salyk, Colette E-mail: jeisner@as.arizona.edu E-mail: dmccarthy@as.arizona.edu

    2014-09-01

    We present new K-band spectroscopy of the UY Aur binary star system. Our data are the first to show H{sub 2} emission in the spectrum of UY Aur A and the first to spectrally resolve the Br? line in the spectrum of UY Aur B. We see an increase in the strength of the Br? line in UY Aur A and a decrease in Br? and H{sub 2} line luminosity for UY Aur B compared to previous studies. Converting Br? line luminosity to accretion rate, we infer that the accretion rate onto UY Aur A has increased by 2 10{sup 9} M {sub ?} yr{sup 1} per year since a rate of zero was observed in 1994. The Br? line strength for UY Aur B has decreased by a factor of 0.54 since 1994, but the K-band flux has increased by 0.9 mag since 1998. The veiling of UY Aur B has also increased significantly. These data evince a much more luminous disk around UY Aur B. If the lower Br? luminosity observed in the spectrum of UY Aur B indicates an intrinsically smaller accretion rate onto the star, then UY Aur A now accretes at a higher rate than UY Aur B. However, extinction at small radii or mass pile-up in the circumstellar disk could explain decreased Br? emission around UY Aur B even when the disk luminosity implies an increased accretion rate. In addition to our scientific results for the UY Aur system, we discuss a dedicated pipeline we have developed for the reduction of echelle-mode data from the ARIES spectrograph.

  6. The allwise motion survey and the quest for cold subdwarfs

    SciTech Connect (OSTI)

    Kirkpatrick, J. Davy; Fajardo-Acosta, Sergio; Gelino, Christopher R.; Fowler, John W.; Cutri, Roc M.; Schneider, Adam; Cushing, Michael C.; Mace, Gregory N.; Wright, Edward L.; Logsdon, Sarah E.; McLean, Ian S.; Skrutskie, Michael F.; Eisenhardt, Peter R.; Stern, Daniel; Balokovi?, Mislav; Burgasser, Adam J.; Faherty, Jacqueline K.; Lansbury, George B.; Rich, J. A.; Skrzypek, Nathalie; and others

    2014-03-10

    The AllWISE processing pipeline has measured motions for all objects detected on Wide-field Infrared Survey Explorer (WISE) images taken between 2010 January and 2011 February. In this paper, we discuss new capabilities made to the software pipeline in order to make motion measurements possible, and we characterize the resulting data products for use by future researchers. Using a stringent set of selection criteria, we find 22,445 objects that have significant AllWISE motions, of which 3525 have motions that can be independently confirmed from earlier Two Micron All Sky Survey (2MASS) images, yet lack any published motions in SIMBAD. Another 58 sources lack 2MASS counterparts and are presented as motion candidates only. Limited spectroscopic follow-up of this list has already revealed eight new L subdwarfs. These may provide the first hints of a 'subdwarf gap' at mid-L types that would indicate the break between the stellar and substellar populations at low metallicities (i.e., old ages). Another object in the motion listWISEA J154045.67510139.3is a bright (J ? 9 mag) object of type M6; both the spectrophotometric distance and a crude preliminary parallax place it ?6 pc from the Sun. We also compare our list of motion objects to the recently published list of 762 WISE motion objects from Luhman. While these first large motion studies with WISE data have been very successful in revealing previously overlooked nearby dwarfs, both studies missed objects that the other found, demonstrating that many other nearby objects likely await discovery in the AllWISE data products.

  7. TWENTY-FIVE SUBARCSECOND BINARIES DISCOVERED BY LUNAR OCCULTATIONS

    SciTech Connect (OSTI)

    Richichi, A.; Fors, O.; Cusano, F.; Moerchen, M.

    2013-09-15

    We report on 25 subarcsecond binaries, detected for the first time by means of lunar occultations in the near-infrared (near-IR) as part of a long-term program using the ISAAC instrument at the ESO Very Large Telescope. The primaries have magnitudes in the range K = 3.8-10.4, and the companions in the range K = 6.4-12.1. The magnitude differences have a median value of 2.8, with the largest being 5.4. The projected separations are in the range 6-748 mas and with a median of 18 mas, or about three times less than the diffraction limit of the telescope. Among our binary detections are a pre-main-sequence star and an enigmatic Mira-like variable previously suspected to have a companion. Additionally, we quote an accurate first-time near-IR detection of a previously known wider binary. We discuss our findings on an individual basis as far as made possible by the available literature, and we examine them from a statistical point of view. We derive a typical frequency of binarity among field stars of Almost-Equal-To 10%, in the resolution and sensitivity range afforded by the technique ( Almost-Equal-To 0.''003 to Almost-Equal-To 0.''5, and K Almost-Equal-To 12 mag, respectively). This is in line with previous results using the same technique but we point out interesting differences that we can trace up to sensitivity, time sampling, and average distance of the targets. Finally, we discuss the prospects for further follow-up studies.

  8. Final Technical Report

    SciTech Connect (OSTI)

    Juan Camilo Serrano

    2011-12-16

    New and novel material and process technologies applied in wind blade designs and production are critical to increasing the competitiveness of wind power generation against traditional sources of energy. In this project, through collaboration between PPG Industries and MAG Industrial Automation Systems, the potential of using automated manufacturing for the production of fiber glass composite wind blades was evaluated from both technical and economic points of view. Further, it was demonstrated that by modifying the standard blade raw material forms through the use of cost effective pre-impregnated rovings coupled with using an automated fiber placement machine to lay up the parts, it is possible to produce state of the art composite laminates with significantly improved mechanical performance and with higher processing rates than standard blade production technology allows for today, thereby lowering the cost of energy over turbine blades made using traditional processes and materials. In conformity with the scope of work of the submitted proposal, the project team completed each task and documented and reported its findings on the appropriate quarterly report submitted to the DOE project team. The activities and this report are divided into 5 subtasks: (1) Material Investigation - Reviews traditional materials and key specifications and testing methods; (2) Manufacturing and Automation - Identifies new candidate material forms and automated layup processes; (3) Process Development - Performs trials of candidate materials and processes; (4) Predictive Analysis - Assesses impact of new material forms and automated processes on a model blade design; and (5) Feasibility Assessment - Compares traditional manufacturing processes and materials to new candidate material forms and automated processes.

  9. EXTINCTION AND DUST GEOMETRY IN M83 H II REGIONS: AN HUBBLE SPACE TELESCOPE/WFC3 STUDY

    SciTech Connect (OSTI)

    Liu, Guilin; Calzetti, Daniela; Hong, Sungryong; Whitmore, Bradley; Chandar, Rupali; O'Connell, Robert W.; Blair, William P.; Cohen, Seth H.; Kim, Hwihyun; Frogel, Jay A.

    2013-12-01

    We present Hubble Space Telescope/WFC3 narrow-band imaging of the starburst galaxy M83 targeting the hydrogen recombination lines (H?, H?, and Pa?), which we use to investigate the dust extinction in the H II regions. We derive extinction maps with 6pc spatial resolution from two combinations of hydrogen lines (H?/H? and H?/Pa?), and show that the longer wavelengths probe larger optical depths, with A{sub V} values larger by ?1mag than those derived from the shorter wavelengths. This difference leads to a factor ?2 discrepancy in the extinction-corrected H? luminosity, a significant effect when studying extragalactic H II regions. By comparing these observations to a series of simple models, we conclude that a large diversity of absorber/emitter geometric configurations can account for the data, implying a more complex physical structure than the classical foreground ''dust screen'' assumption. However, most data points are bracketed by the foreground screen and a model where dust and emitters are uniformly mixed. When averaged over large (?100-200pc) scales, the extinction becomes consistent with a ''dust screen'', suggesting that other geometries tend to be restricted to more local scales. Moreover, the extinction in any region can be described by a combination of the foreground screen and the uniform mixture model with weights of 1/3 and 2/3 in the center (?2kpc), respectively, and 2/3 and 1/3 for the rest of the disk. This simple prescription significantly improves the accuracy of the dust extinction corrections and can be especially useful for pixel-based analyses of galaxies similar to M83.

  10. Eight ultra-faint galaxy candidates discovered in year two of the Dark Energy Survey

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

    Drlica-Wagner, A.

    2015-11-04

    We report the discovery of eight new ultra-faint dwarf galaxy candidates in the second year of optical imaging data from the Dark Energy Survey (DES). Six of these candidates are detected at high confidence, while two lower-confidence candidates are identified in regions of non-uniform survey coverage. The new stellar systems are found by three independent automated search techniques and are identified as overdensities of stars, consistent with the isochrone and luminosity function of an old and metal-poor simple stellar population. The new systems are faint (MV > -4.7 ) and span a range of physical sizes (17 pc < r1/2more » < 181pc) and heliocentric distances (25 kpc < D⊙ < 214 kpc). All of the new systems have central surface brightnesses consistent with known ultra-faint dwarf galaxies (μ 27.5 mag arcsec -2). Roughly half of the DES candidates are more distant, less luminous, and/or have lower surface brightnesses than previously known Milky Way satellite galaxies. Most of the candidates are found in the southern part of the DES footprint close to the Magellanic Clouds. We find that the DES data alone exclude (p < 10-3) a spatially isotropic distribution of Milky Way satellites and that the observed distribution can be well, though not uniquely, described by an association between several of the DES satellites and the Magellanic system. Furthermore, our model predicts that the full sky may hold ~100 ultra-faint galaxies with physical properties comparable to the DES satellites and that 20%–30% of these would be spatially associated with the Magellanic Clouds.« less

  11. DISSECTING PHOTOMETRIC REDSHIFT FOR ACTIVE GALACTIC NUCLEUS USING XMM- AND CHANDRA-COSMOS SAMPLES

    SciTech Connect (OSTI)

    Salvato, M.; Hasinger, G.; Ilbert, O.; Rau, A.; Brusa, M.; Bongiorno, A.; Civano, F.; Elvis, M.; Zamorani, G.; Vignali, C.; Comastri, A.; Bardelli, S.; Bolzonella, M.; Cappelluti, N.; Aussel, H.; Le Floc'h, E.; Mainieri, V.; Capak, P.; Caputi, K.; and others

    2011-12-01

    In this paper, we release accurate photometric redshifts for 1692 counterparts to Chandra sources in the central square degree of the Cosmic Evolution Survey (COSMOS) field. The availability of a large training set of spectroscopic redshifts that extends to faint magnitudes enabled photometric redshifts comparable to the highest quality results presently available for normal galaxies. We demonstrate that morphologically extended, faint X-ray sources without optical variability are more accurately described by a library of normal galaxies (corrected for emission lines) than by active galactic nucleus (AGN) dominated templates, even if these sources have AGN-like X-ray luminosities. Preselecting the library on the bases of the source properties allowed us to reach an accuracy {sigma}{sub {Delta}z/(1+z{sub s{sub p{sub e{sub c)}}}}}{approx}0.015 with a fraction of outliers of 5.8% for the entire Chandra-COSMOS sample. In addition, we release revised photometric redshifts for the 1735 optical counterparts of the XMM-detected sources over the entire 2 deg{sup 2} of COSMOS. For 248 sources, our updated photometric redshift differs from the previous release by {Delta}z > 0.2. These changes are predominantly due to the inclusion of newly available deep H-band photometry (H{sub AB} = 24 mag). We illustrate once again the importance of a spectroscopic training sample and how an assumption about the nature of a source together, with the number and the depth of the available bands, influences the accuracy of the photometric redshifts determined for AGN. These considerations should be kept in mind when defining the observational strategies of upcoming large surveys targeting AGNs, such as eROSITA at X-ray energies and the Australian Square Kilometre Array Pathfinder Evolutionary Map of the Universe in the radio band.

  12. NEW CONSTRAINTS ON THE FAINT END OF THE UV LUMINOSITY FUNCTION AT z ? 7-8 USING THE GRAVITATIONAL LENSING OF THE HUBBLE FRONTIER FIELDS CLUSTER A2744

    SciTech Connect (OSTI)

    Atek, Hakim; Kneib, Jean-Paul; Richard, Johan; Clement, Benjamin; Jauzac, Mathilde; Schaerer, Daniel; Limousin, Marceau; Jullo, Eric; Natarajan, Priyamvada; Egami, Eiichi; Ebeling, Harald

    2015-02-10

    Exploiting the power of gravitational lensing, the Hubble Frontier Fields (HFF) program aims at observing six massive galaxy clusters to explore the distant universe far beyond the limits of blank field surveys. Using the complete Hubble Space Telescope observations of the first HFF cluster A2744, we report the detection of 50 galaxy candidates at z ? 7 and eight candidates at z ? 8 in a total survey area of 0.96arcmin{sup 2} in the source plane. Three of these galaxies are multiply imaged by the lensing cluster. Using an updated model of the mass distribution in the cluster we were able to calculate the magnification factor and the effective survey volume for each galaxy in order to compute the ultraviolet galaxy luminosity function (LF) at both redshifts 7 and 8. Our new measurements reliably extend the z ? 7 UV LF down to an absolute magnitude of M {sub UV} ? 15.5. We find a characteristic magnitude of M{sub UV}{sup ?}=?20.90{sub ?0.73}{sup +0.90}mag and a faint-end slope ?=?2.01{sub ?0.28}{sup +0.20}, close to previous determinations in blank fields. We show here for the first time that this slope remains steep down to very faint luminosities of 0.01 L {sup *}. Although prone to large uncertainties, our results at z ? 8 also seem to confirm a steep faint-end slope below 0.1 L {sup *}. The HFF program is therefore providing an extremely efficient way to study the faintest galaxy populations at z > 7 that would otherwise be inaccessible with current instrumentation. The full sample of six galaxy clusters will provide even better constraints on the buildup of galaxies at early epochs and their contribution to cosmic reionization.

  13. DETECTION OF A DISTINCT METAL-POOR STELLAR HALO IN THE EARLY-TYPE GALAXY NGC3115

    SciTech Connect (OSTI)

    Peacock, Mark B.; Strader, Jay; Romanowsky, Aaron J.; Brodie, Jean P.

    2015-02-10

    We present the resolved stellar populations in the inner and outer halo of the nearby lenticular galaxy NGC3115. Using deep Hubble Space Telescope observations, we analyze stars 2 mag fainter than the tip of the red giant branch (TRGB). We study three fields along the minor axis of this galaxy, 19, 37, and 54kpc from its centercorresponding to 7, 14, and 21 effective radii (r{sub e} ). Even at these large galactocentric distances, all of the fields are dominated by a relatively enriched population, with the main peak in the metallicity distribution decreasing with radius from [Z/H] ? 0.5 to 0.65. The fraction of metal-poor stars ([Z/H] < 0.95) increases from 17% at 16-37 kpc to 28% at ?54kpc. We observe a distinct low-metallicity population (peaked at [Z/H] ? 1.3 and with total mass 2 10{sup 10} M {sub ?} ? 14% of the galaxy's stellar mass) and argue that this represents the detection of an underlying low-metallicity stellar halo. Such halos are generally predicted by galaxy formation theories and have been observed in several late-type galaxies, including the Milky Way and M31. The metallicity and spatial distribution of the stellar halo of NGC3115 are consistent with the galaxy's globular cluster system, which has a similar low-metallicity population that becomes dominant at these large radii. This finding supports the use of globular clusters as bright chemodynamical tracers of galaxy halos. These data also allow us to make a precise measurement of the magnitude of the TRGB, from which we derive a distance modulus of NGC3115 of 30.05 0.05 0.10{sub sys} (10.2 0.2 0.5{sub sys}Mpc)

  14. A NOVEL APPROACH TO CONSTRAIN THE MASS RATIO OF MINOR MERGERS IN ELLIPTICAL GALAXIES: APPLICATION TO NGC 4889, THE BRIGHTEST CLUSTER GALAXY IN COMA

    SciTech Connect (OSTI)

    Gu Meng; Huang Song; Ho, Luis C.; Peng, Chien Y.

    2013-08-10

    Minor mergers are thought to be important for the buildup and structural evolution of massive elliptical galaxies. In this work, we report the discovery of a system of four shell features in NGC 4889, one of the brightest members of the Coma cluster, using optical images taken with the Hubble Space Telescope and the Sloan Digital Sky Survey. The shells are well aligned with the major axis of the host and are likely to have been formed by the accretion of a small satellite galaxy. We have performed a detailed two-dimensional photometric decomposition of NGC 4889 and of the many overlapping nearby galaxies in its vicinity. This comprehensive model allows us not only to firmly detect the low-surface brightness shells, but, crucially, also to accurately measure their luminosities and colors. The shells are bluer than the underlying stars at the same radius in the main galaxy. We make use of the colors of the shells and the color-magnitude relation of the Coma cluster to infer the luminosity (or mass) of the progenitor galaxy. The shells in NGC 4889 appear to have been produced by the minor merger of a moderate-luminosity (M{sub I} Almost-Equal-To -18.7 mag) disk (S0 or spiral) galaxy with a luminosity (mass) ratio of {approx}90:1 with respect to the primary galaxy. The novel methodology presented in this work can be exploited to decode the fossil record imprinted in the photometric substructure of other nearby early-type galaxies.

  15. JELLYFISH: EVIDENCE OF EXTREME RAM-PRESSURE STRIPPING IN MASSIVE GALAXY CLUSTERS

    SciTech Connect (OSTI)

    Ebeling, H.; Stephenson, L. N.; Edge, A. C.

    2014-02-01

    Ram-pressure stripping by the gaseous intracluster medium has been proposed as the dominant physical mechanism driving the rapid evolution of galaxies in dense environments. Detailed studies of this process have, however, largely been limited to relatively modest examples affecting only the outermost gas layers of galaxies in nearby and/or low-mass galaxy clusters. We here present results from our search for extreme cases of gas-galaxy interactions in much more massive, X-ray selected clusters at z > 0.3. Using Hubble Space Telescope snapshots in the F606W and F814W passbands, we have discovered dramatic evidence of ram-pressure stripping in which copious amounts of gas are first shock compressed and then removed from galaxies falling into the cluster. Vigorous starbursts triggered by this process across the galaxy-gas interface and in the debris trail cause these galaxies to temporarily become some of the brightest cluster members in the F606W passband, capable of outshining even the Brightest Cluster Galaxy. Based on the spatial distribution and orientation of systems viewed nearly edge-on in our survey, we speculate that infall at large impact parameter gives rise to particularly long-lasting stripping events. Our sample of six spectacular examples identified in clusters from the Massive Cluster Survey, all featuring M {sub F606W} < 21 mag, doubles the number of such systems presently known at z > 0.2 and facilitates detailed quantitative studies of the most violent galaxy evolution in clusters.

  16. Source-plane reconstruction of the giant gravitational arc in A2667: A candidate Wolf-Rayet galaxy at z ? 1

    SciTech Connect (OSTI)

    Cao, Shuo; Zhu, Zong-Hong; Covone, Giovanni; Jullo, Eric; Richard, Johan; Izzo, Luca

    2015-01-01

    We present a new analysis of Hubble Space Telescope, Spitzer Space Telescope, and Very Large Telescope imaging and spectroscopic data of a bright lensed galaxy at z = 1.0334 in the lensing cluster A2667. Using this high-resolution imaging, we present an updated lens model that allows us to fully understand the lensing geometry and reconstruct the lensed galaxy in the source plane. This giant arc gives a unique opportunity to view the structure of a high-redshift disk galaxy. We find that the lensed galaxy of A2667 is a typical spiral galaxy with a morphology similar to the structure of its counterparts at higher redshift, z ? 2. The surface brightness of the reconstructed source galaxy in the z {sub 850} band reveals the central surface brightness I(0) = 20.28 0.22 mag arcsec{sup 2} and a characteristic radius r{sub s} = 2.01 0.16 kpc at redshift z ? 1. The morphological reconstruction in different bands shows obvious negative radial color gradients for this galaxy. Moreover, the redder central bulge tends to contain a metal-rich stellar population, rather than being heavily reddened by dust due to high and patchy obscuration. We analyze the VIMOS/integral field unit spectroscopic data and find that, in the given wavelength range (?1800-3200 ), the combined arc spectrum of the source galaxy is characterized by a strong continuum emission with strong UV absorption lines (Fe II and Mg II) and shows the features of a typical starburst Wolf-Rayet galaxy, NGC 5253. More specifically, we have measured the equivalent widths of Fe II and Mg II lines in the A2667 spectrum, and obtained similar values for the same wavelength interval of the NGC 5253 spectrum. Marginal evidence for [C III] 1909 emission at the edge of the grism range further confirms our expectation.

  17. A LOW ESCAPE FRACTION OF IONIZING PHOTONS OF L > L* LYMAN BREAK GALAXIES AT z = 3.3

    SciTech Connect (OSTI)

    Boutsia, K.; Grazian, A.; Giallongo, E.; Fontana, A.; Pentericci, L.; Castellano, M.; Fiore, F.; Gallozzi, S.; Testa, V.; Paris, D.; Santini, P.; Zamorani, G.; Mignoli, M.; Vanzella, E.; Lilly, S. J.

    2011-07-20

    We present an upper limit for the relative escape fraction (f{sup rel}{sub esc}) of ionizing radiation at z {approx} 3.3 using a sample of 11 Lyman break galaxies (LBGs) with deep imaging in the U band obtained with the Large Binocular Camera, mounted on the prime focus of the Large Binocular Telescope. We selected 11 LBGs with secure redshifts in the range 3.27 < z < 3.35, from three independent fields. We stacked the images of our sources in the R and U bands, which correspond to an effective rest-frame wavelength of 1500 A and 900 A, respectively, obtaining a limit in the U band image of {>=}30.7 mag (AB) at 1{sigma}. We derive a 1{sigma} upper limit of f{sup rel}{sub esc} {approx} 5%, which is one of the lowest values found in the literature so far at z {approx} 3.3. Assuming that the upper limit for the escape fraction that we derived from our sample holds for all galaxies at this redshift, the hydrogen ionization rate that we obtain ({Gamma}{sub -12} < 0.3 s{sup -1}) is not enough to keep the intergalactic medium ionized and a substantial contribution to the UV background by faint active galactic nuclei is required. Since our sample is clearly still limited in size, larger z {approx} 3 LBG samples at similar or even greater depths are necessary to confirm these results on a more firm statistical basis.

  18. OVERVIEW OF THE SDSS-IV MaNGA SURVEY: MAPPING NEARBY GALAXIES AT APACHE POINT OBSERVATORY

    SciTech Connect (OSTI)

    Bundy, Kevin; Bershady, Matthew A.; Wake, David A.; Tremonti, Christy; Diamond-Stanic, Aleksandar M.; Law, David R.; Cherinka, Brian; Yan, Renbin; Snchez-Gallego, Jos R.; Drory, Niv; MacDonald, Nicholas; Weijmans, Anne-Marie; Thomas, Daniel; Masters, Karen; Coccato, Lodovico; Aragn-Salamanca, Alfonso; Avila-Reese, Vladimir; Badenes, Carles; Falcn-Barroso, Jsus; Belfiore, Francesco; and others

    2015-01-01

    We present an overview of a new integral field spectroscopic survey called MaNGA (Mapping Nearby Galaxies at Apache Point Observatory), one of three core programs in the fourth-generation Sloan Digital Sky Survey (SDSS-IV) that began on 2014 July 1. MaNGA will investigate the internal kinematic structure and composition of gas and stars in an unprecedented sample of 10,000 nearby galaxies. We summarize essential characteristics of the instrument and survey design in the context of MaNGA's key science goals and present prototype observations to demonstrate MaNGA's scientific potential. MaNGA employs dithered observations with 17 fiber-bundle integral field units that vary in diameter from 12'' (19 fibers) to 32'' (127 fibers). Two dual-channel spectrographs provide simultaneous wavelength coverage over 3600-10300 at R ? 2000. With a typical integration time of 3 hr, MaNGA reaches a target r-band signal-to-noise ratio of 4-8 ({sup 1} per 2'' fiber) at 23 AB mag arcsec{sup 2}, which is typical for the outskirts of MaNGA galaxies. Targets are selected with M {sub *} ? 10{sup 9} M {sub ?} using SDSS-I redshifts and i-band luminosity to achieve uniform radial coverage in terms of the effective radius, an approximately flat distribution in stellar mass, and a sample spanning a wide range of environments. Analysis of our prototype observations demonstrates MaNGA's ability to probe gas ionization, shed light on recent star formation and quenching, enable dynamical modeling, decompose constituent components, and map the composition of stellar populations. MaNGA's spatially resolved spectra will enable an unprecedented study of the astrophysics of nearby galaxies in the coming 6yr.

  19. The infrared medium-deep survey. II. How to trigger radio AGNs? Hints from their environments

    SciTech Connect (OSTI)

    Karouzos, Marios; Im, Myungshin; Kim, Jae-Woo; Lee, Seong-Kook; Jeon, Yiseul; Choi, Changsu; Hong, Jueun; Hyun, Minhee; Jun, Hyunsung David; Kim, Dohyeong; Kim, Yongjung; Kim, Ji Hoon; Kim, Duho; Park, Won-Kee; Taak, Yoon Chan; Yoon, Yongmin; Chapman, Scott; Pak, Soojong; Edge, Alastair

    2014-12-10

    Activity at the centers of galaxies, during which the central supermassive black hole is accreting material, is nowadays accepted to be rather ubiquitous and most probably a phase of every galaxy's evolution. It has been suggested that galactic mergers and interactions may be the culprits behind the triggering of nuclear activity. We use near-infrared data from the new Infrared Medium-Deep Survey and the Deep eXtragalactic Survey of the VIMOS-SA22 field and radio data at 1.4 GHz from the FIRST survey and a deep Very Large Array survey to study the environments of radio active galactic nuclei (AGNs) over an area of ?25 deg{sup 2} and down to a radio flux limit of 0.1 mJy and a J-band magnitude of 23 mag AB. Radio AGNs are predominantly found in environments similar to those of control galaxies at similar redshift, J-band magnitude, and (M{sub u} M{sub r} ) rest-frame color. However, a subpopulation of radio AGNs is found in environments up to 100 times denser than their control sources. We thus preclude merging as the dominant triggering mechanism of radio AGNs. By fitting the broadband spectral energy distribution of radio AGNs in the least and most dense environments, we find that those in the least dense environments show higher radio-loudness, higher star formation efficiencies, and higher accretion rates, typical of the so-called high-excitation radio AGNs. These differences tend to disappear at z > 1. We interpret our results in terms of a different triggering mechanism for these sources that is driven by mass loss through winds of young stars created during the observed ongoing star formation.

  20. Determination of low-level radioactivity in environmental samples by gamma spectroscopy at Argonne National Laboratory

    SciTech Connect (OSTI)

    Streets, W.E.; Heinrich, R.R.; Lamoureux, L.L.

    1988-01-01

    We currently have six Ge/Ge(Li) detectors that are being used for gamma counting of environmental samples (three with horizontal geometry, three with vertical geometry). The detectors were calibrated for close-geometry efficiency by counting standards in a set configuration (a height of 6.4 cm in a 4-oz. wide-mouthed Naglene bottle) immediately adjacent to the cryostat face. This configuration was chosen so that the standards would be symmetrical to the centers of both the horizontal and vertical detectors. Two solid standards were prepared by adding a known amount of Standard Reference Material NBL No. 6-A (Pitchblende) and NBL No. 7-A (Monazite Sand) to a blanked soil and mixing. Homogeneity of the standards was checked by counting each standard at each quadrant (on a horizontal detector). The final mixtures showed less than 1% deviation between the high and low quadrant counts. Two liquid secondary standards were prepared from stock solutions of /sup 137/Cs, /sup 131/I, and /sup 110m/Ag, which has been characterized as point sources using several detector efficiency curves. These efficiencies were determined using point source standards from the National Bureau of Standards (NBS) and International Atomic Energy Agency (IAEA). All standards had activity levels that allowed less than 1% counting statistics to be obtained on the major peaks (i.e., those with stronger branching ratio) within two hours. Analysis of the resulting data yield smooth efficiency curves for each of the six detectors. Although the standard compositions varied, solid and liquid, the densities were all approx. =1.0 g/cm/sup 3/. 3 refs.

  1. Deep z-band observations of the coolest Y dwarf

    SciTech Connect (OSTI)

    Kopytova, Taisiya G.; Crossfield, Ian J. M.; Deacon, Niall R.; Brandner, Wolfgang; Buenzli, Esther; Bayo, Amelia; Schlieder, Joshua E.; Manjavacas, Elena; Kopon, Derek; Biller, Beth A.

    2014-12-10

    WISE J085510.83-071442.5 (hereafter, WISE 0855-07) is the coolest Y dwarf known to date and is located at a distance of 2.31 0.08 pc, giving it the fourth largest parallax of any known star or brown dwarf system. We report deep z-band observations of WISE 0855-07 using FORS2 on UT1/Very Large Telescope. We do not detect any counterpart to WISE 0855-07 in our z-band images and estimate a brightness upper limit of AB mag > 24.8 (F {sub ?} < 0.45 ?Jy) at 910 65 nm with 3? confidence. We combine our z-band upper limit with previous near- and mid-infrared photometry to place constraints on the atmospheric properties of WISE 0855-07 via comparison to models which implement water clouds in the atmospheres of T {sub eff} < 300 K substellar objects. We find that none of the available models that implement water clouds can completely reproduce the observed spectral energy distribution of WISE 0855-07. Every model significantly disagrees with the (3.6 ?m/4.5 ?m) flux ratio and at least one other bandpass. Since methane is predicted to be the dominant absorber at 3-4 ?m, these mismatches might point to an incorrect or incomplete treatment of methane in current models. We conclude that (a) WISE0855-07 has T {sub eff} ? 200-250 K, (b) <80% of its surface is covered by clouds, and (c) deeper observations, and improved models of substellar evolution, atmospheres, clouds, and opacities will be necessary to better characterize this object.

  2. A population of relic intermediate-mass black holes in the halo of the Milky Way

    SciTech Connect (OSTI)

    Rashkov, Valery; Madau, Piero

    2014-01-10

    If 'seed' central black holes were common in the subgalactic building blocks that merged to form present-day massive galaxies, then relic intermediate-mass black holes (IMBHs) should be present in the Galactic bulge and halo. We use a particle tagging technique to dynamically populate the N-body Via Lactea II high-resolution simulation with black holes, and assess the size, properties, and detectability of the leftover population. The method assigns a black hole to the most tightly bound central particle of each subhalo at infall according to an extrapolation of the M {sub BH}-?{sub *} relation, and self-consistently follows the accretion and disruption of Milky Way progenitor dwarfs and their holes in a cosmological 'live' host from high redshift to today. We show that, depending on the minimum stellar velocity dispersion, ? {sub m}, below which central black holes are assumed to be increasingly rare, as many as ?2000 (? {sub m} = 3 km s{sup 1}) or as few as ?70 (? {sub m} = 12 km s{sup 1}) IMBHs may be left wandering in the halo of the Milky Way today. The fraction of IMBHs forced from their hosts by gravitational recoil is ? 20%. We identify two main Galactic subpopulations, 'naked' IMBHs, whose host subhalos were totally destroyed after infall, and 'clothed' IMBHs residing in dark matter satellites that survived tidal stripping. Naked IMBHs typically constitute 40%-50% of the total and are more centrally concentrated. We show that, in the ? {sub m} = 12 km s{sup 1} scenario, the clusters of tightly bound stars that should accompany naked IMBHs would be fainter than m{sub V} = 16 mag, spatially resolvable, and have proper motions of 0.1-10 mas yr{sup 1}. Their detection may provide an observational tool to constrain the formation history of massive black holes in the early universe.

  3. MONSTER IN THE DARK: THE ULTRALUMINOUS GRB 080607 AND ITS DUSTY ENVIRONMENT

    SciTech Connect (OSTI)

    Perley, D. A.; Morgan, A. N.; Miller, A. A.; Bloom, J. S.; Cenko, S. B.; Li, W.; Filippenko, A. V.; Butler, N. R.; Christian, P.; Updike, A.; Hartmann, D. H.; Yuan, F.; Akerlof, C. W.; Prochaska, J. X.; Tanvir, N. R.; Levan, A. J.; Milne, P.; Rujopakarn, W.; Rykoff, E. S.

    2011-02-15

    We present early-time optical through infrared photometry of the bright Swift gamma-ray burst (GRB) 080607, starting only 6 s following the initial trigger in the rest frame. Complemented by our previously published spectroscopy, this high-quality photometric data set allows us to solve for the extinction properties of the redshift 3.036 sightline, giving perhaps the most detailed information to date on the ultraviolet continuum absorption properties of any sightline outside our Local Group. The extinction properties are not adequately modeled by any ordinary extinction template (including the average Milky Way, Large Magellanic Cloud, and Small Magellanic Cloud curves), partially because the 2175 A feature (while present) is weaker by about a factor of two than when seen under similar circumstances locally. However, the spectral energy distribution is exquisitely fitted by the more general Fitzpatrick and Massa parameterization of Local-Group extinction, putting it in the same family as some peculiar Milky Way extinction curves. After correcting for this (considerable, A{sub V} = 3.3 {+-} 0.4 mag) extinction, GRB 080607 is revealed to have been among the most optically luminous events ever observed, comparable to the naked-eye burst GRB 080319B. Its early peak time (t{sub rest} < 6 s) indicates a high initial Lorentz factor ({Gamma}>600), while the extreme luminosity may be explained in part by a large circumburst density. Only because of its early high luminosity could the afterglow of GRB 080607 be studied in such detail in spite of the large attenuation and great distance, making this burst an excellent prototype for the understanding of other highly obscured extragalactic objects, and of the class of 'dark' GRBs in particular.

  4. A RARE EARLY-TYPE STAR REVEALED IN THE WING OF THE SMALL MAGELLANIC CLOUD

    SciTech Connect (OSTI)

    Evans, C. J.; Hainich, R.; Oskinova, L. M.; Hamann, W.-R.; Todt, H.; Gallagher III, J. S.; Chu, Y.-H.; Gruendl, R. A.; Henault-Brunet, V.

    2012-07-10

    Sk 183 is the visually brightest star in the N90 nebula, a young star-forming region in the Wing of the Small Magellanic Cloud (SMC). We present new optical spectroscopy from the Very Large Telescope which reveals Sk 183 to be one of the most massive O-type stars in the SMC. Classified as an O3-type dwarf on the basis of its nitrogen spectrum, the star also displays broadened He I absorption, which suggests a later type. We propose that Sk 183 has a composite spectrum and that it is similar to another star in the SMC, MPG 324. This brings the number of rare O2- and O3-type stars known in the whole of the SMC to a mere four. We estimate physical parameters for Sk 183 from analysis of its spectrum. For a single-star model, we estimate an effective temperature of 46 {+-} 2 kK, a low mass-loss rate of {approx}10{sup -7} M{sub Sun} yr{sup -1}, and a spectroscopic mass of 46{sup +9}{sub -8} M{sub Sun} (for an adopted distance modulus of 18.7 mag to the young population in the SMC Wing). An illustrative binary model requires a slightly hotter temperature ({approx}47.5 kK) for the primary component. In either scenario, Sk 183 is the earliest-type star known in N90 and will therefore be the dominant source of hydrogen-ionizing photons. This suggests Sk 183 is the primary influence on the star formation along the inner edge of the nebula.

  5. Measuring distances and reddenings for a billion stars: Toward a 3D dust map from Pan-STARRS 1

    SciTech Connect (OSTI)

    Green, Gregory Maurice; Finkbeiner, Douglas P.; Schlafly, Edward F.; Rix, Hans-Walter; Juri?, Mario; Burgett, Will; Chambers, Kenneth C.; Flewelling, Heather; Kudritzki, Rolf Peter; Magnier, Eugene; Tonry, John; Wainscoat, Richard; Waters, Christopher; Draper, Peter W.; Metcalfe, Nigel; Martin, Nicolas

    2014-03-10

    We present a method to infer reddenings and distances to stars based only on their broad-band photometry, and show how this method can be used to produce a three-dimensional (3D) dust map of the Galaxy. Our method samples from the full probability density function of distance, reddening, and stellar type for individual stars, as well as the full uncertainty in reddening as a function of distance in the 3D dust map. We incorporate prior knowledge of the distribution of stars in the Galaxy and the detection limits of the survey. For stars in the Pan-STARRS 1 (PS1) 3? survey, we demonstrate that our reddening estimates are unbiased and accurate to ?0.13 mag in E(B V) for the typical star. Based on comparisons with mock catalogs, we expect distances for main-sequence stars to be constrained to within ?20%-60%, although this range can vary, depending on the reddening of the star, the precise stellar type, and its position on the sky. A later paper will present a 3D map of dust over the three quarters of the sky surveyed by PS1. Both the individual stellar inferences and the 3D dust map will enable a wealth of Galactic science in the plane. The method we present is not limited to the passbands of the PS1 survey but may be extended to incorporate photometry from other surveys, such as the Two Micron All Sky Survey, the Sloan Digital Sky Survey (where available), and in the future, LSST and Gaia.

  6. Pan-STARRS1 DISCOVERY OF TWO ULTRALUMINOUS SUPERNOVAE AT z Almost-Equal-To 0.9

    SciTech Connect (OSTI)

    Chomiuk, L.; Chornock, R.; Soderberg, A. M.; Berger, E.; Foley, R. J.; Kirshner, R. P.; Czekala, I.; Chevalier, R. A.; Huber, M. E.; Gezari, S.; Riess, A.; Rodney, S. A.; Narayan, G.; Stubbs, C. W.; Rest, A.; Smartt, S. J.; Tonry, J. L.; Burgett, W. S.; Chambers, K. C.; Wood-Vasey, W. M.; and others

    2011-12-20

    We present the discovery of two ultraluminous supernovae (SNe) at z Almost-Equal-To 0.9 with the Pan-STARRS1 Medium Deep Survey. These SNe, PS1-10ky and PS1-10awh, are among the most luminous SNe ever discovered, comparable to the unusual transients SN 2005ap and SCP 06F6. Like SN 2005ap and SCP 06F6, they show characteristic high luminosities (M{sub bol} Almost-Equal-To -22.5 mag), blue spectra with a few broad absorption lines, and no evidence for H or He. We have constructed a full multi-color light curve sensitive to the peak of the spectral energy distribution in the rest-frame ultraviolet, and we have obtained time series spectroscopy for these SNe. Given the similarities between the SNe, we combine their light curves to estimate a total radiated energy over the course of explosion of (0.9-1.4) Multiplication-Sign 10{sup 51} erg. We find photospheric velocities of 12,000-19,000 km s{sup -1} with no evidence for deceleration measured across {approx}3 rest-frame weeks around light curve peak, consistent with the expansion of an optically thick massive shell of material. We show that, consistent with findings for other ultraluminous SNe in this class, radioactive decay is not sufficient to power PS1-10ky, and we discuss two plausible origins for these events: the initial spin-down of a newborn magnetar in a core-collapse SN, or SN shock breakout from the dense circumstellar wind surrounding a Wolf-Rayet star.

  7. A SEARCH FOR L/T TRANSITION DWARFS WITH Pan-STARRS1 AND WISE: DISCOVERY OF SEVEN NEARBY OBJECTS INCLUDING TWO CANDIDATE SPECTROSCOPIC VARIABLES

    SciTech Connect (OSTI)

    Best, William M. J.; Liu, Michael C.; Magnier, Eugene A.; Aller, Kimberly M.; Burgett, W. S.; Chambers, K. C.; Hodapp, K. W.; Kaiser, N.; Kudritzki, R.-P.; Morgan, J. S.; Tonry, J. L.; Wainscoat, R. J.; Deacon, Niall R.; Dupuy, Trent J.; Redstone, Joshua; Price, P. A.

    2013-11-10

    We present initial results from a wide-field (30,000 deg{sup 2}) search for L/T transition brown dwarfs within 25 pc using the Pan-STARRS1 and Wide-field Infrared Survey Explorer (WISE) surveys. Previous large-area searches have been incomplete for L/T transition dwarfs, because these objects are faint in optical bands and have near-infrared (near-IR) colors that are difficult to distinguish from background stars. To overcome these obstacles, we have cross-matched the Pan-STARRS1 (optical) and WISE (mid-IR) catalogs to produce a unique multi-wavelength database for finding ultracool dwarfs. As part of our initial discoveries, we have identified seven brown dwarfs in the L/T transition within 9-15 pc of the Sun. The L9.5 dwarf PSO J140.2308+45.6487 and the T1.5 dwarf PSO J307.6784+07.8263 (both independently discovered by Mace et al.) show possible spectroscopic variability at the Y and J bands. Two more objects in our sample show evidence of photometric J-band variability, and two others are candidate unresolved binaries based on their spectra. We expect our full search to yield a well-defined, volume-limited sample of L/T transition dwarfs that will include many new targets for study of this complex regime. PSO J307.6784+07.8263 in particular may be an excellent candidate for in-depth study of variability, given its brightness (J = 14.2 mag) and proximity (11 pc)

  8. A PAN-STARRS + UKIDSS SEARCH FOR YOUNG, WIDE PLANETARY-MASS COMPANIONS IN UPPER SCORPIUS

    SciTech Connect (OSTI)

    Aller, Kimberly M.; Kraus, Adam L.; Liu, Michael C.; Burgett, William S.; Chambers, Kenneth C.; Hodapp, Klaus W.; Kaiser, Nick; Magnier, Eugene A.; Price, Paul A.

    2013-08-10

    We have combined optical and NIR photometry from Pan-STARRS 1 and UKIDSS to search the young (5-10 Myr) star-forming region of Upper Scorpius for wide ( Almost-Equal-To 400-4000 AU) substellar companions down to {approx}5 M{sub Jup}. Our search is Almost-Equal-To 4 mag deeper than previous work based on the Two Micron All Sky Survey. We identified several candidates around known stellar members using a combination of color selection and spectral energy distribution fitting. Our follow-up spectroscopy has identified two new companions as well as confirmed two companions previously identified from photometry, with spectral types of M7.5-M9 and masses of {approx}15-60 M{sub Jup}, indicating a frequency for such wide substellar companions of {approx}0.6% {+-} 0.3%. Both USco 1610-1913B and USco 1612-1800B are more luminous than expected for their spectral type compared with known members of Upper Sco. HIP 77900B has an extreme mass ratio (M{sub 2}/M{sub 1} Almost-Equal-To 0.005) and an extreme separation of 3200 AU. USco 1602-2401B also has a very large separation of 1000 AU. We have also confirmed a low-mass stellar companion, USco 1610-2502B (730 AU, M5.5). Our substellar companions appear both non-coeval with their primary stars according to evolutionary models and, as a group, are systematically more luminous than the Upper Sco cluster sequence. One possible reason for these luminosity discrepancies could be different formation processes or accretion histories for these objects.

  9. LACERTA I AND CASSIOPEIA III. TWO LUMINOUS AND DISTANT ANDROMEDA SATELLITE DWARF GALAXIES FOUND IN THE 3{pi} PAN-STARRS1 SURVEY

    SciTech Connect (OSTI)

    Martin, Nicolas F.; Laevens, Benjamin P. M.; Slater, Colin T.; Bell, Eric F.; Schlafly, Edward F.; Morganson, Eric; Rix, Hans-Walter; Bernard, Edouard J.; Ferguson, Annette M. N.; Finkbeiner, Douglas P.; Burgett, William S.; Chambers, Kenneth C.; Hodapp, Klaus W.; Kaiser, Nicholas; Kudritzki, Rolf-Peter; Magnier, Eugene A.; Morgan, Jeffrey S.; Tonry, John L.; Wainscoat, Richard J.; Price, Paul A.

    2013-07-20

    We report the discovery of two new dwarf galaxies, Lacerta I/Andromeda XXXI (Lac I/And XXXI) and Cassiopeia III/Andromeda XXXII (Cas III/And XXXII), in stacked Pan-STARRS1 r{sub P1}- and i{sub P1}-band imaging data. Both are luminous systems (M{sub V} {approx} -12) located at projected distances of 20. Degree-Sign 3 and 10. Degree-Sign 5 from M31. Lac I and Cas III are likely satellites of the Andromeda galaxy with heliocentric distances of 756{sup +44}{sub -28} kpc and 772{sup +61}{sub -56} kpc, respectively, and corresponding M31-centric distances of 275 {+-} 7 kpc and 144{sup +6}{sub -4} kpc. The brightest of recent Local Group member discoveries, these two new dwarf galaxies owe their late discovery to their large sizes (r{sub h} = 4.2{sup +0.4}{sub -0.5} arcmin or 912{sup +124}{sub -93} pc for Lac I; r{sub h} = 6.5{sup +1.2}{sub -1.0} arcmin or 1456 {+-} 267 pc for Cas III) and consequently low surface brightness ({mu}{sub 0} {approx} 26.0 mag arcsec{sup -2}), as well as to the lack of a systematic survey of regions at large radii from M31, close to the Galactic plane. This latter limitation is now alleviated by the 3{pi} Pan-STARRS1 survey, which could lead to the discovery of other distant Andromeda satellite dwarf galaxies.

  10. EXTREME CORONAL LINE EMITTERS: TIDAL DISRUPTION OF STARS BY MASSIVE BLACK HOLES IN GALACTIC NUCLEI?

    SciTech Connect (OSTI)

    Wang Tinggui; Zhou Hongyan; Wang Huiyuan; Yang Chenwei; Komossa, S.

    2012-04-20

    Tidal disruption of stars by supermassive black holes at the centers of galaxies is expected to produce unique emission-line signatures, which have not yet been explored adequately. Here we report the discovery of extremely strong coronal lines from [Fe X] up to [Fe XIV] in a sample of seven galaxies (including two recently reported cases), which we interpret as such signatures. This is the first systematic search for objects of this kind, by making use of the immense database of the Sloan Digital Sky Survey. The galaxies, which are non-active as evidenced by the narrow line ratios, show broad emission lines of complex profiles in more than half of the sample. Both the high-ionization coronal lines and the broad lines are fading on timescales of years in objects observed with spectroscopic follow-ups, suggesting their transient nature. Variations of inferred non-stellar continua, which have absolute magnitudes of at least -16 to -18 mag in the g band, are also detected in more than half of the sample. The coronal line emitters reside in sub-L{sub *} disk galaxies (-21.3 < M{sub i} < -18.5) with small stellar velocity dispersions. The sample seems to form two distinct types based on the presence or absence of the [Fe VII] lines, with the latter having relatively low luminosities of [O III], [Fe XI], and the host galaxies. These characteristics can most naturally be understood in the context of transient accretion onto intermediate-mass black holes at galactic centers following tidal disruption of stars in a gas-rich environment. We estimate the incidence of such events to be around 10{sup -5} yr{sup -1} for a galaxy with -21.3 < M{sub i} < -18.5.

  11. LOW-MASS ECLIPSING BINARIES IN THE INITIAL KEPLER DATA RELEASE

    SciTech Connect (OSTI)

    Coughlin, J. L.; Harrison, T. E.; Ule, N.; Lopez-Morales, M.; Hoffman, D. I.

    2011-03-15

    We identify 231 objects in the newly released Cycle 0 data set from the Kepler Mission as double-eclipse, detached eclipsing binary systems with T{sub eff} < 5500 K and orbital periods shorter than {approx}32 days. We model each light curve using the JKTEBOP code with a genetic algorithm to obtain precise values for each system. We identify 95 new systems with both components below 1.0 M{sub sun} and eclipses of at least 0.1 mag, suitable for ground-based follow-up. Of these, 14 have periods less than 1.0 day, 52 have periods between 1.0 and 10.0 days, and 29 have periods greater than 10.0 days. This new sample of main-sequence, low-mass, double-eclipse, detached eclipsing binary candidates more than doubles the number of previously known systems and extends the sample into the completely heretofore unexplored P > 10.0 day period regime. We find preliminary evidence from these systems that the radii of low-mass stars in binary systems decrease with period. This supports the theory that binary spin-up is the primary cause of inflated radii in low-mass binary systems, although a full analysis of each system with radial-velocity and multi-color light curves is needed to fully explore this hypothesis. Also, we present seven new transiting planet candidates that do not appear among the list of 706 candidates recently released by the Kepler team, or in the Kepler False Positive Catalog, along with several other new and interesting systems. We also present novel techniques for the identification, period analysis, and modeling of eclipsing binaries.

  12. HD106906b: A PLANETARY-MASS COMPANION OUTSIDE A MASSIVE DEBRIS DISK

    SciTech Connect (OSTI)

    Bailey, Vanessa; Reiter, Megan; Morzinski, Katie; Males, Jared; Su, Kate Y. L.; Hinz, Philip M.; Stark, Daniel; Close, Laird M.; Follette, Katherine B.; Rodigas, Timothy; Meshkat, Tiffany; Kenworthy, Matthew; Mamajek, Eric; Briguglio, Runa; Puglisi, Alfio; Xompero, Marco; Weinberger, Alycia J.

    2014-01-01

    We report the discovery of a planetary-mass companion, HD106906 b, with the new Magellan Adaptive Optics (MagAO) + Clio2 system. The companion is detected with Clio2 in three bands: J, K{sub S} , and L', and lies at a projected separation of 7.''1 (650 AU). It is confirmed to be comoving with its 13 2 Myr F5 host using Hubble Space Telescope Advanced Camera for Surveys astrometry over a time baseline of 8.3 yr. DUSTY and COND evolutionary models predict that the companion's luminosity corresponds to a mass of 11 2 M {sub Jup}, making it one of the most widely separated planetary-mass companions known. We classify its Magellan/Folded-Port InfraRed Echellette J/H/K spectrum as L2.5 1; the triangular H-band morphology suggests an intermediate surface gravity. HD106906 A, a pre-main-sequence Lower Centaurus Crux member, was initially targeted because it hosts a massive debris disk detected via infrared excess emission in unresolved Spitzer imaging and spectroscopy. The disk emission is best fit by a single component at 95 K, corresponding to an inner edge of 15-20 AU and an outer edge of up to 120 AU. If the companion is on an eccentric (e > 0.65) orbit, it could be interacting with the outer edge of the disk. Close-in, planet-like formation followed by scattering to the current location would likely disrupt the disk and is disfavored. Furthermore, we find no additional companions, though we could detect similar-mass objects at projected separations >35 AU. In situ formation in a binary-star-like process is more probable, although the companion-to-primary mass ratio, at <1%, is unusually small.

  13. A multi-wavelength investigation of the radio-loud supernova PTF11qcj and its circumstellar environment

    SciTech Connect (OSTI)

    Corsi, A.; Ofek, E. O.; Gal-Yam, A.; Xu, D.; Frail, D. A.; Kulkarni, S. R.; Horesh, A.; Carpenter, J.; Arcavi, I.; Cao, Y.; Mooley, K.; Sesar, B.; Fox, D. B.; Kasliwal, M. M.; Sullivan, M.; Maguire, K.; Pan, Y.-C.; Cenko, S. B.; Sternberg, A.; Bersier, D.; and others

    2014-02-10

    We present the discovery, classification, and extensive panchromatic (from radio to X-ray) follow-up observations of PTF11qcj, a supernova (SN) discovered by the Palomar Transient Factory (PTF). Our observations with the Karl G. Jansky Very Large Array show that this event is radio-loud: PTF11qcj reached a radio peak luminosity comparable to that of the famous gamma-ray-burst-associated SN 1998bw (L {sub 5} {sub GHz} ? 10{sup 29} erg s{sup 1} Hz{sup 1}). PTF11qcj is also detected in X-rays with the Chandra Observatory, and in the infrared band with Spitzer. Our multi-wavelength analysis probes the SN interaction with circumstellar material. The radio observations suggest a progenitor mass-loss rate of ?10{sup 4} M {sub ?} yr{sup 1} (v{sub w} /1000 km s{sup 1}), and a velocity of ?0.3-0.5 c for the fastest moving ejecta (at ?10 days after explosion). However, these estimates are derived assuming the simplest model of SN ejecta interacting with a smooth circumstellar wind, and do not account for possible inhomogeneities in the medium and asphericity of the explosion. The radio data show deviations from such a simple model, as well as a late-time re-brightening. The X-ray flux from PTF11qcj is compatible with the high-frequency extrapolation of the radio synchrotron emission (within the large uncertainties). A light echo from pre-existing dust is in agreement with our infrared data. Our pre-explosion data from the PTF suggest that a precursor eruption of absolute magnitude M{sub r} ? 13 mag may have occurred ?2.5 yr prior to the SN explosion. Overall, PTF11qcj fits the expectations from the explosion of a Wolf-Rayet star. Precursor eruptions may be a feature characterizing the final pre-explosion evolution of such stars.

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

    SciTech Connect (OSTI)

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

    2011-10-15

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

  15. Radio-optical reference frame link using the U.S. Naval observatory astrograph and deep CCD imaging

    SciTech Connect (OSTI)

    Zacharias, N.; Zacharias, M. I.

    2014-05-01

    Between 1997 and 2004 several observing runs were conducted, mainly with the CTIO 0.9 m, to image International Celestial Reference Frame (ICRF) counterparts (mostly QSOs) in order to determine accurate optical positions. Contemporary to these deep CCD images, the same fields were observed with the U.S. Naval Observatory astrograph in the same bandpass. They provide accurate positions on the Hipparcos/Tycho-2 system for stars in the 10-16 mag range used as reference stars for the deep CCD imaging data. Here we present final optical position results of 413 sources based on reference stars obtained by dedicated astrograph observations that were reduced following two different procedures. These optical positions are compared to radio very long baseline interferometry positions. The current optical system is not perfectly aligned to the ICRF radio system with rigid body rotation angles of 3-5 mas (= 3? level) found between them for all three axes. Furthermore, statistically, the optical-radio position differences are found to exceed the total, combined, known errors in the observations. Systematic errors in the optical reference star positions and physical offsets between the centers of optical and radio emissions are both identified as likely causes. A detrimental, astrophysical, random noise component is postulated to be on about the 10 mas level. If confirmed by future observations, this could severely limit the Gaia to ICRF reference frame alignment accuracy to an error of about 0.5 mas per coordinate axis with the current number of sources envisioned to provide the link. A list of 36 ICRF sources without the detection of an optical counterpart to a limiting magnitude of about R = 22 is provided as well.

  16. The Gemini NICI planet-finding campaign: the orbit of the young exoplanet ? Pictoris b

    SciTech Connect (OSTI)

    Nielsen, Eric L.; Liu, Michael C.; Chun, Mark; Ftaclas, Christ; Wahhaj, Zahed; Biller, Beth A.; Hayward, Thomas L.; Kuchner, Marc J.; Rodigas, Timothy J.; Toomey, Douglas W.

    2014-10-20

    We present new astrometry for the young (12-21 Myr) exoplanet ? Pictoris b taken with the Gemini/NICI and Magellan/MagAO instruments between 2009 and 2012. The high dynamic range of our observations allows us to measure the relative position of ? Pic b with respect to its primary star with greater accuracy than previous observations. Based on a Markov Chain Monte Carlo analysis, we find the planet has an orbital semi-major axis of 9.1{sub ?0.5}{sup +5.3} AU and orbital eccentricity <0.15 at 68% confidence (with 95% confidence intervals of 8.2-48 AU and 0.00-0.82 for semi-major axis and eccentricity, respectively, due to a long narrow degenerate tail between the two). We find that the planet has reached its maximum projected elongation, enabling higher precision determination of the orbital parameters than previously possible, and that the planet's projected separation is currently decreasing. With unsaturated data of the entire ? Pic system (primary star, planet, and disk) obtained thanks to NICI's semi-transparent focal plane mask, we are able to tightly constrain the relative orientation of the circumstellar components. We find the orbital plane of the planet lies between the inner and outer disks: the position angle (P.A.) of nodes for the planet's orbit (211.8 0.3) is 7.4? greater than the P.A. of the spine of the outer disk and 3.2? less than the warped inner disk P.A., indicating the disk is not collisionally relaxed. Finally, for the first time we are able to dynamically constrain the mass of the primary star ? Pic to 1.76{sub ?0.17}{sup +0.18} M {sub ?}.

  17. THE SUBARU HIGH-z QUASAR SURVEY: DISCOVERY OF FAINT z ? 6 QUASARS

    SciTech Connect (OSTI)

    Kashikawa, Nobunari; Furusawa, Hisanori; Niino, Yuu [Optical and Infrared Astronomy Division, National Astronomical Observatory, Mitaka, Tokyo 181-8588 (Japan); Ishizaki, Yoshifumi; Onoue, Masafusa; Toshikawa, Jun; Ishikawa, Shogo [Department of Astronomy, School of Science, Graduate University for Advanced Studies, Mitaka, Tokyo 181-8588 (Japan); Willott, Chris J. [Herzberg Institute of Astrophysics, National Research Council, 5071 West Saanich Road, Victoria, BC V9E 2E7 (Canada); Im, Myungshin [Center for the Exploration of the Origin of the Universe (CEOU), Astronomy Program, Department of Physics and Astronomy, Seoul National University, 1 Gwanak-rho, Gwanak-gu, Seoul 151-742 (Korea, Republic of); Shimasaku, Kazuhiro [Department of Astronomy, University of Tokyo, Hongo, Tokyo 113-0033 (Japan); Ouchi, Masami [Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582 (Japan); Hibon, Pascale, E-mail: n.kashikawa@nao.ac.jp [Gemini Observatory, La Serena (Chile)

    2015-01-01

    We present the discovery of one or two extremely faint z ? 6 quasars in 6.5 deg{sup 2} utilizing a unique capability of the wide-field imaging of the Subaru/Suprime-Cam. The quasar selection was made in (i'-z{sub B} ) and (z{sub B} -z{sub R} ) colors, where z{sub B} and z{sub R} are bandpasses with central wavelengths of 8842 and 9841 , respectively. The color selection can effectively isolate quasars at z ? 6 from M/L/T dwarfs without the J-band photometry down to z{sub R} < 24.0, which is 3.5 mag deeper than the Sloan Digital Sky Survey (SDSS). We have selected 17 promising quasar candidates. The follow-up spectroscopy for seven targets identified one apparent quasar at z = 6.156 with M {sub 1450} = 23.10. We also identified one possible quasar at z = 6.041 with a faint continuum of M {sub 1450} = 22.58 and a narrow Ly? emission with HWHM =427 km s{sup 1}, which cannot be distinguished from Lyman ? emitters. We derive the quasar luminosity function at z ? 6 by combining our faint quasar sample with the bright quasar samples by SDSS and CFHQS. Including our data points invokes a higher number density in the faintest bin of the quasar luminosity function than the previous estimate employed. This suggests a steeper faint-end slope than lower z, though it is yet uncertain based on a small number of spectroscopically identified faint quasars, and several quasar candidates still remain to be diagnosed. The steepening of the quasar luminosity function at the faint end does increase the expected emission rate of the ionizing photon; however, it only changes by a factor of approximately two to six. This was found to still be insufficient for the required photon budget of reionization at z ? 6.

  18. WEAK GALACTIC HALO-DWARF SPHEROIDAL CONNECTION FROM RR LYRAE STARS

    SciTech Connect (OSTI)

    Fiorentino, Giuliana [INAF-Osservatorio Astronomico di Bologna, via Ranzani 1, I-40127 Bologna (Italy); Bono, Giuseppe [Dipartimento di Fisica, Universit di Roma Tor Vergata, Via della Ricerca Scientifica 1, I-00133 Roma (Italy); Monelli, Matteo; Gallart, Carme; Martnez-Vsquez, Clara E. [Instituto de Astrofsica de Canarias, Calle Via Lactea s/n, E-38205 La Laguna, Tenerife (Spain); Stetson, Peter B. [National Research Council, 5071 West Saanich Road, Victoria, BC V9E 2E7 (Canada); Tolstoy, Eline [Kapteyn Astronomical Institute, University of Groningen, Postbus 800, 9700 AV Groningen (Netherlands); Salaris, Maurizio [Astrophysics Research Institute, Liverpool John Moores University IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L35RF (United Kingdom); Bernard, Edouard J., E-mail: giuliana.fiorentino@oabo.inaf.it [SUPA, Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ (United Kingdom)

    2015-01-01

    We discuss the role that dwarf galaxies may have played in the formation of the Galactic halo (Halo) using RR Lyrae stars (RRL) as tracers of their ancient stellar component. The comparison is performed using two observables (periods, luminosity amplitudes) that are reddening and distance independent. Fundamental mode RRL in 6 dwarf spheroidals (dSphs) and 11 ultra faint dwarf galaxies (?1300) show a Gaussian period distribution well peaked around a mean period of (Pab) =0.6100.001days (? = 0.03). The Halo RRL (?15,000) are characterized by a broader period distribution. The fundamental mode RRL in all the dSphs apart from Sagittarius are completely lacking in High Amplitude Short Period (HASP) variables, defined as those having P ?0.48days and A{sub V} ?0.75mag. Such variables are not uncommon in the Halo and among the globular clusters and massive dwarf irregulars. To further interpret this evidence, we considered 18 globulars covering a broad range in metallicity (2.3?[Fe/H]? 1.1) and hosting more than 35 RRL each. The metallicity turns out to be the main parameter, since only globulars more metal-rich than [Fe/H]? 1.5 host RRL in the HASP region. This finding suggests that dSphs similar to the surviving ones do not appear to be the major building-blocks of the Halo. Leading physical arguments suggest an extreme upper limit of ?50% to their contribution. On the other hand, massive dwarfs hosting an old population with a broad metallicity distribution (Large Magellanic Cloud, Sagittarius) may have played a primary role in the formation of the Halo.

  19. Clues to the nature of SN 2009ip from photometric and spectroscopic evolution to late times

    SciTech Connect (OSTI)

    Graham, M. L. [Astronomy Department, University of California, Berkeley, CA 94720 (United States); Sand, D. J. [Physics Department, Texas Tech University, Lubbock, TX 79409 (United States); Valenti, S.; Howell, D. A.; Parrent, J. [Las Cumbres Observatory Global Telescope Network, Goleta, CA 93117 (United States); Halford, M.; Zaritsky, D. [Astronomy Department, University of Arizona, Tucson, AZ 85721 (United States); Bianco, F. [Department of Physics, New York University, 4 Washington Place, New York, NY 10003 (United States); Rest, A. [Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States); Dilday, B., E-mail: melissagraham@berkeley.edu [North Idaho College, 1000 W. Garden Avenue, Coeur d'Alene, ID 83814 (United States)

    2014-06-01

    We present time series photometric and spectroscopic data for the transient SN 2009ip from the start of its outburst in 2012 September until 2013 November. These data were collected primarily with the new robotic capabilities of the Las Cumbres Observatory Global Telescope Network, a specialized facility for time domain astrophysics, and includes supporting high-resolution spectroscopy from the Southern Astrophysical Research Telescope, Kitt Peak National Observatory, and Gemini Observatory. Based on our nightly photometric monitoring, we interpret the strength and timing of fluctuations in the light curve as interactions between fast-moving ejecta and an inhomogeneous circumstellar material (CSM) produced by past eruptions of this massive luminous blue variable (LBV) star. Our time series of spectroscopy in 2012 reveals that, as the continuum and narrow H? flux from CSM interactions declines, the broad component of H? persists with supernova (SN)-like velocities that are not typically seen in LBVs or SN impostor events. At late times, we find that SN 2009ip continues to decline slowly, at ? 0.01 mag day{sup 1}, with small fluctuations in slope similar to Type IIn supernovae (SNe IIn) or SN impostors but no further LBV-like activity. The late-time spectrum features broad calcium lines similar to both late-time SNe and SN impostors. In general, we find that the photometric and spectroscopic evolution of SN 2009ip is more similar to SNe IIn than either continued eruptions of an LBV star or SN impostors but we cannot rule out a nonterminal explosion. In this context, we discuss the implications for episodic mass loss during the late stages of massive star evolution.

  20. Hydrogen-poor superluminous supernovae and long-duration gamma-ray bursts have similar host galaxies

    SciTech Connect (OSTI)

    Lunnan, R.; Chornock, R.; Berger, E.; Laskar, T.; Fong, W.; Sanders, N. E.; Challis, P. M.; Drout, M. R.; Foley, R. J.; Kirshner, R. P.; Leibler, C.; Marion, G. H.; Milisavljevic, D.; Narayan, G. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Rest, A. [Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States); Huber, M. E. [Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822 (United States); McCrum, M.; Smartt, S. J.; Smith, K. W. [Astrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, Belfast BT7 1NN (United Kingdom); Scolnic, D., E-mail: rlunnan@cfa.harvard.edu [Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218 (United States); and others

    2014-06-01

    We present optical spectroscopy and optical/near-IR photometry of 31 host galaxies of hydrogen-poor superluminous supernovae (SLSNe), including 15 events from the Pan-STARRS1 Medium Deep Survey. Our sample spans the redshift range 0.1 ? z ? 1.6, and is the first comprehensive host galaxy study of this specific subclass of cosmic explosions. Combining the multi-band photometry and emission-line measurements, we determine the luminosities, stellar masses, star formation rates, and metallicities. We find that, as a whole, the hosts of SLSNe are a low-luminosity ((M{sub B} ) ? 17.3 mag), low stellar mass ((M {sub *}) ? 2 10{sup 8} M {sub ?}) population, with a high median specific star formation rate ((sSFR) ? 2 Gyr{sup 1}). The median metallicity of our spectroscopic sample is low, 12 + log (O/H) ? 8.35 ? 0.45 Z {sub ?}, although at least one host galaxy has solar metallicity. The host galaxies of H-poor SLSNe are statistically distinct from the hosts of GOODS core-collapse SNe (which cover a similar redshift range), but resemble the host galaxies of long-duration gamma-ray bursts (LGRBs) in terms of stellar mass, SFR, sSFR, and metallicity. This result indicates that the environmental causes leading to massive stars forming either SLSNe or LGRBs are similar, and in particular that SLSNe are more effectively formed in low metallicity environments. We speculate that the key ingredient is large core angular momentum, leading to a rapidly spinning magnetar in SLSNe and an accreting black hole in LGRBs.