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Sample records for apache point observatory

  1. Infrared Spectroscopic Data from the Apache Point Observatory Galactic Evolution Experiment (APOGEE), SDSS-III Data Release 10

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

    Sloan Digital Sky Survey (SDSS) Data Release 10 is the first spectroscopic release from the Apache Point Observatory Galactic Evolution Experiment (APOGEE), including spectra and derived stellar parameters for more than 50,000 stars. APOGEE is an ongoing survey of ~100,000 stars accessing all parts of the Milky Way. By operating in the infrared (H-band) portion of the electromagnetic spectrum, APOGEE is better able to detect light from stars lying in dusty regions of the Milky Way than surveys conducted in the optical, making this survey particularly well-suited for exploring the Galactic disk and bulge. APOGEE's high resolution spectra provide detailed information about the stellar atmospheres; DR10 provides derived effective temperatures, surface gravities, overall metallicities, and information on the abundances of several chemical elements. [copied from http://www.sdss3.org/dr10/irspec/

  2. 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; Sánchez-Gallego, José R.; Drory, Niv; MacDonald, Nicholas; Weijmans, Anne-Marie; Thomas, Daniel; Masters, Karen; Coccato, Lodovico; Aragón-Salamanca, Alfonso; Avila-Reese, Vladimir; Badenes, Carles; Falcón-Barroso, Jésus; 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 Å at R ? 2000. With a typical integration time of 3 hr, MaNGA reaches a target r-band signal-to-noise ratio of 4-8 (Å{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 6 yr.

  3. Apache Point Observatory

    E-Print Network [OSTI]

    Johnson, Eric E.

    around the globe by astronomers using the Internet and a unique software program. Originally used objects. Utilizing many of the successful design technology of the ARC 3.5-m telescope, New Mexico State in the Sacramento Mountains of south-central New Mexico. Four telescopes are currently operated: The Sloan

  4. NEW ATLAS9 AND MARCS MODEL ATMOSPHERE GRIDS FOR THE APACHE POINT OBSERVATORY GALACTIC EVOLUTION EXPERIMENT (APOGEE)

    SciTech Connect (OSTI)

    Meszaros, Sz.; Allende Prieto, C.; De Vicente, A.; Edvardsson, B.; Gustafsson, B.; Castelli, F.; Garcia Perez, A. E.; Majewski, S. R.; Plez, B.; Schiavon, R.; Shetrone, M.

    2012-10-01

    We present a new grid of model photospheres for the SDSS-III/APOGEE survey of stellar populations of the Galaxy, calculated using the ATLAS9 and MARCS codes. New opacity distribution functions were generated to calculate ATLAS9 model photospheres. MARCS models were calculated based on opacity sampling techniques. The metallicity ([M/H]) spans from -5 to 1.5 for ATLAS and -2.5 to 0.5 for MARCS models. There are three main differences with respect to previous ATLAS9 model grids: a new corrected H{sub 2}O line list, a wide range of carbon ([C/M]) and {alpha} element [{alpha}/M] variations, and solar reference abundances from Asplund et al. The added range of varying carbon and {alpha}-element abundances also extends the previously calculated MARCS model grids. Altogether, 1980 chemical compositions were used for the ATLAS9 grid and 175 for the MARCS grid. Over 808,000 ATLAS9 models were computed spanning temperatures from 3500 K to 30,000 K and log g from 0 to 5, where larger temperatures only have high gravities. The MARCS models span from 3500 K to 5500 K, and log g from 0 to 5. All model atmospheres are publicly available online.

  5. Design of a telescope pointing and tracking subsystem for the Big Bear Solar Observatory New Solar Telescope

    E-Print Network [OSTI]

    Design of a telescope pointing and tracking subsystem for the Big Bear Solar Observatory New Solar Telescope J. R. Varsika and G.Yangb aBig Bear Solar Observatory, 40386 North Shore Lane, Big Bear City, California, U.S.A.; bNew Jersey Institute of Technology, Newark, New Jersey, U.S.A. ABSTRACT The New Solar

  6. Solar Feasibility Study May 2013 - San Carlos Apache Tribe

    SciTech Connect (OSTI)

    Rapp, Jim; Duncan, Ken; Albert, Steve

    2013-05-01

    The San Carlos Apache Tribe (Tribe) in the interests of strengthening tribal sovereignty, becoming more energy self-sufficient, and providing improved services and economic opportunities to tribal members and San Carlos Apache Reservation (Reservation) residents and businesses, has explored a variety of options for renewable energy development. The development of renewable energy technologies and generation is consistent with the Tribe’s 2011 Strategic Plan. This Study assessed the possibilities for both commercial-scale and community-scale solar development within the southwestern portions of the Reservation around the communities of San Carlos, Peridot, and Cutter, and in the southeastern Reservation around the community of Bylas. Based on the lack of any commercial-scale electric power transmission between the Reservation and the regional transmission grid, Phase 2 of this Study greatly expanded consideration of community-scale options. Three smaller sites (Point of Pines, Dudleyville/Winkleman, and Seneca Lake) were also evaluated for community-scale solar potential. Three building complexes were identified within the Reservation where the development of site-specific facility-scale solar power would be the most beneficial and cost-effective: Apache Gold Casino/Resort, Tribal College/Skill Center, and the Dudleyville (Winkleman) Casino.

  7. V-185: Apache OpenOffice SDK Oracle Java JavaDoc Spoofing Vulnerabilit...

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

    Apache OpenOffice SDK Oracle Java JavaDoc Spoofing Vulnerability PLATFORM: Apache OpenOffice SDK 3.x ABSTRACT: Apache has acknowledged a vulnerability in Apache OpenOffice SDK...

  8. U-255: Apache Wicket Input Validation Flaw Permits Cross-Site...

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

    Wicket Input Validation Flaw Permits Cross-Site Scripting Attacks PLATFORM: Apache Software Foundation Apache Wicket 1.5.5 Apache Software Foundation Apache Wicket 1.5-RC5.1...

  9. Three-Year Global Survey of Coronal Null Points from Potential-Field-Source-Surface (PFSS) Modeling and Solar Dynamics Observatory (SDO) Observations

    E-Print Network [OSTI]

    Freed, Michael; McKenize, David

    2014-01-01

    This article compiles and examines a comprehensive coronal magnetic-null-point survey created by potential-field-source-surface (PFSS) modeling and Solar Dynamics Observatory/Atmospheric Imaging Assembly (SDO/AIA) observations. The locations of 582 potential magnetic null points in the corona were predicted from the PFSS model between Carrington Rotations (CR) 2098 (June 2010) and 2139 (July 2013). These locations were manually inspected, using contrast-enhanced SDO/AIA images in 171 angstroms at the east and west solar limb, for structures associated with nulls. A Kolmogorov--Smirnov (K--S) test showed a statistically significant difference between observed and predicted latitudinal distributions of null points. This finding is explored further to show that the observability of null points could be affected by the Sun's asymmetric hemisphere activity. Additional K--S tests show no effect on observability related to eigenvalues associated with the fan and spine structure surrounding null points or to the orie...

  10. Optimizing CMS build infrastructure via Apache Mesos

    E-Print Network [OSTI]

    David Abdurachmanov; Alessandro Degano; Peter Elmer; Giulio Eulisse; David Mendez; Shahzad Muzaffar

    2015-07-28

    The Offline Software of the CMS Experiment at the Large Hadron Collider (LHC) at CERN consists of 6M lines of in-house code, developed over a decade by nearly 1000 physicists, as well as a comparable amount of general use open-source code. A critical ingredient to the success of the construction and early operation of the WLCG was the convergence, around the year 2000, on the use of a homogeneous environment of commodity x86-64 processors and Linux. Apache Mesos is a cluster manager that provides efficient resource isolation and sharing across distributed applications, or frameworks. It can run Hadoop, Jenkins, Spark, Aurora, and other applications on a dynamically shared pool of nodes. We present how we migrated our continuos integration system to schedule jobs on a relatively small Apache Mesos enabled cluster and how this resulted in better resource usage, higher peak performance and lower latency thanks to the dynamic scheduling capabilities of Mesos.

  11. San Carlos Apache Tribe - Energy Organizational Analysis

    SciTech Connect (OSTI)

    Rapp, James; Albert, Steve

    2012-04-01

    The San Carlos Apache Tribe (SCAT) was awarded $164,000 in late-2011 by the U.S. Department of Energy (U.S. DOE) Tribal Energy Program's "First Steps Toward Developing Renewable Energy and Energy Efficiency on Tribal Lands" Grant Program. This grant funded: ? The analysis and selection of preferred form(s) of tribal energy organization (this Energy Organization Analysis, hereinafter referred to as "EOA"). ? Start-up staffing and other costs associated with the Phase 1 SCAT energy organization. ? An intern program. ? Staff training. ? Tribal outreach and workshops regarding the new organization and SCAT energy programs and projects, including two annual tribal energy summits (2011 and 2012). This report documents the analysis and selection of preferred form(s) of a tribal energy organization.

  12. Search for TeV Gamma-Ray Emission from Point-like Sources in the Inner Galactic Plane with a Partial Configuration of the HAWC Observatory

    E-Print Network [OSTI]

    Abeysekara, A U; Alvarez, C; Álvarez, J D; Arceo, R; Arteaga-Velázquez, J C; Solares, H A Ayala; Barber, A S; Baughman, B M; Bautista-Elivar, N; Reyes, A D Becerril; Belmont, E; BenZvi, S Y; Bernal, A; Braun, J; Caballero-Mora, K S; Capistrán, T; Carramiñana, A; Casanova, S; Castillo, M; Cotti, U; Cotzomi, J; de León, S Coutiño; de la Fuente, E; De León, C; DeYoung, T; Dingus, B L; DuVernois, M A; Ellsworth, R W; Enriquez-Rivera, O; Fiorino, D W; Fraija, N; Garfias, F; González, M M; Goodman, J A; Gussert, M; Hampel-Arias, Z; Harding, J P; Hernandez, S; Hüntemeyer, P; Hui, C M; Imran, A; Iriarte, A; Karn, P; Kieda, D; Lara, A; Lauer, R J; Lee, W H; Lennarz, D; Vargas, H León; Linnemann, J T; Longo, M; Raya, G Luis; Malone, K; Marinelli, A; Marinelli, S S; Martinez, H; Martinez, O; Martínez-Castro, J; Matthews, J A J; Miranda-Romagnoli, P; Moreno, E; Mostafá, M; Nellen, L; Newbold, M; Noriega-Papaqui, R; Patricelli, B; Pelayo, R; Pérez-Pérez, E G; Pretz, J; Ren, Z; Rivière, C; Rosa-González, D; Salazar, H; Greus, F Salesa; Sandoval, A; Schneider, M; Sinnis, G; Smith, A J; Woodle, K Sparks; Springer, R W; Taboada, I; Tibolla, O; Tollefson, K; Torres, I; Ukwatta, T N; Villaseñor, L; Vrabel, K; Weisgarber, T; Westerhoff, S; Wisher, I G; Wood, J; Yapici, T; Yodh, G B; Younk, P W; Zaborov, D; Zepeda, A; Zhou, H

    2015-01-01

    A survey of the inner Galaxy region of Galactic longitude l in [+15, +50] degree and latitude b in [-4,+4] degree is performed using one-third of the High Altitude Water Cherenkov (HAWC) Observatory operated during its construction phase. To address the ambiguities arising from unresolved sources in the data, we use a maximum likelihood technique to identify point source candidates. Ten sources and candidate sources are identified in this analysis. Eight of these are associated with known TeV sources but not all have differential fluxes compatible with previous measurements. Three sources are detected with significances $>5\\,\\sigma$ after accounting for statistical trials, and are associated with known TeV sources.

  13. Project Reports for San Carlos Apache Tribe- 2012 Project

    Broader source: Energy.gov [DOE]

    Under this project, the San Carlos Apache Tribe will study the feasibility of solar energy projects within the reservation with the potential to generate a minimum of 1 megawatt (MW).

  14. SEARCH FOR POINT-LIKE SOURCES OF ULTRA-HIGH ENERGY NEUTRINOS AT THE PIERRE AUGER OBSERVATORY AND IMPROVED LIMIT ON THE DIFFUSE FLUX OF TAU NEUTRINOS

    SciTech Connect (OSTI)

    Abreu, P.; Andringa, S. [LIP and Instituto Superior Tecnico, Technical University of Lisbon (Portugal); Aglietta, M. [Istituto di Fisica dello Spazio Interplanetario (INAF), Universita di Torino and Sezione INFN, Torino (Italy); Ahlers, M. [University of Wisconsin, Madison, WI (United States); Ahn, E. J. [Fermilab, Batavia, IL (United States); Albuquerque, I. F. M. [Universidade de Sao Paulo, Instituto de Fisica, Sao Paulo, SP (Brazil); Allard, D. [Laboratoire AstroParticule et Cosmologie (APC), Universite Paris 7, CNRS-IN2P3, Paris (France); Allekotte, I. [Centro Atomico Bariloche and Instituto Balseiro (CNEA-UNCuyo-CONICET), San Carlos de Bariloche (Argentina); Allen, J. [New York University, New York, NY (United States); Allison, P. [Ohio State University, Columbus, OH (United States); Almela, A. [Universidad Tecnologica Nacional - Facultad Regional Buenos Aires, Buenos Aires (Argentina); Alvarez Castillo, J. [Universidad Nacional Autonoma de Mexico, Mexico, D.F. (Mexico); Alvarez-Muniz, J. [Universidad de Santiago de Compostela (Spain); Alves Batista, R. [Universidade Estadual de Campinas, IFGW, Campinas, SP (Brazil); Ambrosio, M.; Aramo, C. [Universita di Napoli 'Federico II' and Sezione INFN, Napoli (Italy); Aminaei, A. [IMAPP, Radboud University Nijmegen (Netherlands); Anchordoqui, L. [University of Wisconsin, Milwaukee, WI (United States); Antici'c, T. [Rudjer Boskovi'c Institute, 10000 Zagreb (Croatia); Collaboration: Pierre Auger Collaboration; and others

    2012-08-10

    The surface detector array of the Pierre Auger Observatory can detect neutrinos with energy E{sub {nu}} between 10{sup 17} eV and 10{sup 20} eV from point-like sources across the sky south of +55 Degree-Sign and north of -65 Degree-Sign declinations. A search has been performed for highly inclined extensive air showers produced by the interaction of neutrinos of all flavors in the atmosphere (downward-going neutrinos), and by the decay of tau leptons originating from tau neutrino interactions in Earth's crust (Earth-skimming neutrinos). No candidate neutrinos have been found in data up to 2010 May 31. This corresponds to an equivalent exposure of {approx}3.5 years of a full surface detector array for the Earth-skimming channel and {approx}2 years for the downward-going channel. An improved upper limit on the diffuse flux of tau neutrinos has been derived. Upper limits on the neutrino flux from point-like sources have been derived as a function of the source declination. Assuming a differential neutrino flux k{sub PS} {center_dot} E {sup -2}{sub {nu}} from a point-like source, 90% confidence level upper limits for k{sub PS} at the level of Almost-Equal-To 5 Multiplication-Sign 10{sup -7} and 2.5 Multiplication-Sign 10{sup -6} GeV cm{sup -2} s{sup -1} have been obtained over a broad range of declinations from the searches for Earth-skimming and downward-going neutrinos, respectively.

  15. Mescalero Apache Tribe Monitored Retrievable Storage (MRS)

    SciTech Connect (OSTI)

    Peso, F.

    1992-03-13

    The Nuclear Waste Policy Act of 1982, as amended, authorizes the siting, construction and operation of a Monitored Retrievable Storage (MRS) facility. The MRS is intended to be used for the temporary storage of spent nuclear fuel from the nation's nuclear power plants beginning as early as 1998. Pursuant to the Nuclear Waste Policy Act, the Office of the Nuclear Waste Negotiator was created. On October 7, 1991, the Nuclear Waste Negotiator invited the governors of states and the Presidents of Indian tribes to apply for government grants in order to conduct a study to assess under what conditions, if any, they might consider hosting an MRS facility. Pursuant to this invitation, on October 11, 1991 the Mescalero Apache Indian Tribe of Mescalero, NM applied for a grant to conduct a phased, preliminary study of the safety, technical, political, environmental, social and economic feasibility of hosting an MRS. The preliminary study included: (1) An investigative education process to facilitate the Tribe's comprehensive understanding of the safety, environmental, technical, social, political, and economic aspects of hosting an MRS, and; (2) The development of an extensive program that is enabling the Tribe, in collaboration with the Negotiator, to reach an informed and carefully researched decision regarding the conditions, (if any), under which further pursuit of the MRS would be considered. The Phase 1 grant application enabled the Tribe to begin the initial activities necessary to determine whether further consideration is warranted for hosting the MRS facility. The Tribe intends to pursue continued study of the MRS in order to meet the following objectives: (1) Continuing the education process towards a comprehensive understanding of the safety, environmental, technical, social and economic aspects of the MRS; (2) Conducting an effective public participation and information program; (3) Participating in MRS meetings.

  16. V-140: Apache ActiveMQ Bugs Let Remote Users Conduct Cross-Site...

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

    0: Apache ActiveMQ Bugs Let Remote Users Conduct Cross-Site Scripting Attacks, Deny Service, and Obtain Potentially Sensitive Information V-140: Apache ActiveMQ Bugs Let Remote...

  17. RIO GRANDE FLOODWAY SAN ACACIA TO BOSQUE DEL APACHE UNIT

    E-Print Network [OSTI]

    US Army Corps of Engineers

    REEVALUATION REPORT AND SUPPLEMENTAL ENVIRONMENTAL IMPACT STATEMENT II FINAL U.S. Army Corps of Engineers Report and Supplemental Environmental Impact Statement II (GRR/SEIS II) as well as supporting#12;RIO GRANDE FLOODWAY SAN ACACIA TO BOSQUE DEL APACHE UNIT SOCORRO COUNTY, NEW MEXICO GENERAL

  18. Independent External Peer Review Rio Grande Floodway, San Acacia to Bosque Del Apache,

    E-Print Network [OSTI]

    US Army Corps of Engineers

    Flood Risk Management General Reevaluation Report and Supplemental Environmental Impact Statement (Rev Diversion Dam SEIS Supplemental Environmental Impact Statement SOW Scope of Work SWILFPDC Southwest Illinois Apache, New Mexico Flood Risk Management General Reevaluation Report (GRR) and Supplemental Environmental

  19. EA-2002: Right-of-Way Application for the Tucson-Apache 115-kV...

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

    the potential environmental impacts of a proposal for BIA to grant Western a 150-foot right-of-way across tribal land along the existing Tucson-Apache Transmission Line to...

  20. Jicarilla Apache Utility Authority Renewable Energy and Energy Efficiency Strategic Planning

    SciTech Connect (OSTI)

    Rabago, K.R.

    2008-06-28

    The purpose of this Strategic Plan Report is to provide an introduction and in-depth analysis of the issues and opportunities, resources, and technologies of energy efficiency and renewable energy that have potential beneficial application for the people of the Jicarilla Apache Nation and surrounding communities. The Report seeks to draw on the best available information that existed at the time of writing, and where necessary, draws on new research to assess this potential. This study provides a strategic assessment of opportunities for maximizing the potential for electrical energy efficiency and renewable energy development by the Jicarilla Apache Nation. The report analyzes electricity use on the Jicarilla Apache Reservation in buildings. The report also assesses particular resources and technologies in detail, including energy efficiency, solar, wind, geothermal, biomass, and small hydropower. The closing sections set out the elements of a multi-year, multi-phase strategy for development of resources to the maximum benefit of the Nation.

  1. Sensors for Environmental Observatories

    E-Print Network [OSTI]

    Hamilton, Michael P.

    Sensors for Environmental Observatories Report of the NSF-Sponsored Workshop December 2004 #12 States of America. 2005. #12;Sensors for Environmental Observatories Report of the NSF Sponsored Workshop Evaluation Center (WTEC), Inc. 4800 Roland Avenue Baltimore, Maryland 21210 #12;In recent years

  2. Using Entrez Utilities Web Service with Apache Axis2 for Java Creating a Web Service Client Application

    E-Print Network [OSTI]

    Levin, Judith G.

    Using Entrez Utilities Web Service with Apache Axis2 for Java Creating a Web Service Client Entrez Utilities Web Service using Axis2 for Java. Preinstalled Software You should have Apache Axis2.sh shell script file on Linux) in the bin directory of Axis2 installation. You will use it to generate Web

  3. THE TENTH DATA RELEASE OF THE SLOAN DIGITAL SKY SURVEY: FIRST...

    Office of Scientific and Technical Information (OSTI)

    Journal Article: THE TENTH DATA RELEASE OF THE SLOAN DIGITAL SKY SURVEY: FIRST SPECTROSCOPIC DATA FROM THE SDSS-III APACHE POINT OBSERVATORY GALACTIC EVOLUTION EXPERIMENT Citation...

  4. Sommers-Bausch Observatory

    E-Print Network [OSTI]

    Stowell, Michael

    Sommers-Bausch Observatory Handbook Ninth Edition, Fall 2013 DEPARTMENT OF ASTROPHYSICAL of the early years of SBO. Thanks also to the Denver Library for information and photos of Elmer Sommers, Ed here at Sommers-Bausch: Kelsey Johnson, Cori Krauss, John Weiss, James Roberts, Quyen Hart, Colin

  5. Sommers-Bausch Observatory

    E-Print Network [OSTI]

    Stowell, Michael

    The Sommers-Bausch Observatory Handbook Eighth Edition, Fall 2012 DEPARTMENT OF ASTROPHYSICAL to the Denver Library for information and photos of Elmer Sommers, Ed Kosmicki of Summit Magazine for the 16 the educational mission here at Sommers-Bausch: Kelsey Johnson, Cori Krauss, John Weiss, James Roberts, Quyen Hart

  6. The National Virtual Observatory

    E-Print Network [OSTI]

    Robert J. Brunner; S. George Djorgovski; Thomas A. Prince; Alex S. Szalay

    2001-08-23

    As a scientific discipline, Astronomy is rather unique. We only have one laboratory, the Universe, and we cannot, of course, change the initial conditions and study the resulting effects. On top of this, acquiring Astronomical data has historically been a very labor-intensive effort. As a result, data has traditionally been preserved for posterity. With recent technological advances, however, the rate at which we acquire new data has grown exponentially, which has generated a Data Tsunami, whose wave train threatens to overwhelm the field. In this conference proceedings, we present and define the concept of virtual observatories, which we feel is the only logical answer to this dilemma.

  7. Controls for a Pulsed Ion Accelerator Using Apache Cassandra (No-SQL) and ZMQ

    E-Print Network [OSTI]

    Persaud, A; Stettler, M W; Vytla, V K

    2015-01-01

    We report on updates to the accelerator controls for the Neutral Drift Compression Experiment II, a pulsed accelerator for heavy ions. The control infrastructure is built around a LabVIEW interface combined with an Apache Cassandra (No-SQL) backend for data archiving. Recent upgrades added the storing and retrieving of device settings into the database, as well as adding ZMQ as a message broker that replaces LabVIEW's shared variables. Converting to ZMQ also allows easy access using other programming languages, such as Python.

  8. CHILBOLTON OBSERVATORY The Chilbolton Observatory in Hampshire is at the

    E-Print Network [OSTI]

    's energy balance. Scientists use CFARR's sophisticated RADAR (Radio Detection And Ranging), LIDAR (LIghtCHILBOLTON OBSERVATORY The Chilbolton Observatory in Hampshire is at the cutting-edge of world Monitoring Facility. CFARR CFARR is one of the world's most advanced experimental meteorological remote

  9. The Enriched Xenon Observatory

    SciTech Connect (OSTI)

    Dolinski, M. J. [Stanford University Physics Department, 382 Via Pueblo Mall, Stanford, CA 94305-4060 (United States)

    2009-12-17

    The Enriched Xenon Observatory (EXO) experiment will search for neutrinoless double beta decay of {sup 136}Xe. The EXO Collaboration is actively pursuing both liquid-phase and gas-phase Xe detector technologies with scalability to the ton-scale. The search for neutrinoless double beta decay of {sup 136}Xe is especially attractive because of the possibility of tagging the resulting Ba daughter ion, eliminating all sources of background other than the two neutrino decay mode. EXO-200, the first phase of the project, is a liquid Xe time projection chamber with 200 kg of Xe enriched to 80% in {sup 136}Xe. EXO-200, which does not include Ba-tagging, will begin taking data in 2009, with two-year sensitivity to the half-life for neutrinoless double beta decay of 6.4x10{sup 25} years. This corresponds to an effective Majorana neutrino mass of 0.13 to 0.19 eV.

  10. Space Telescope Programs Hubble Observatory

    E-Print Network [OSTI]

    Colorado at Boulder, University of

    Certifications required for all raw materials ­ Shelf Life (Polymerics) materials date controlled by QA · DesignsSpace Telescope Programs Hubble Observatory HST-COS FUV PER 11/8/00 FUV Detector System Materials;Space Telescope Programs Hubble Observatory HST-COS FUV PER 11/8/00 Materials and Processes · Materials

  11. PRECIPITATION AT ARMAGH OBSERVATORY 18381997

    E-Print Network [OSTI]

    PRECIPITATION AT ARMAGH OBSERVATORY 1838­1997 C.J. Butler, A.D.S. Coughlin and D.T. Fee ABSTRACT the longest in the British Isles. Here we present the monthly mean daily precipitation recorded at Armagh with the compilation and calibration of one such body of data, namely the precipitation recorded at Armagh Observatory

  12. Jiangmen Underground Neutrino Observatory

    E-Print Network [OSTI]

    Miao He; for the JUNO collaboration

    2014-12-13

    The Jiangmen Underground Neutrino Observatory (JUNO) is a multipurpose neutrino-oscillation experiment designed to determine the neutrino mass hierarchy and to precisely measure oscillation parameters by detecting reactor antineutrinos, observe supernova neutrinos, study the atmospheric, solar neutrinos and geo-neutrinos, and perform exotic searches, with a 20 kiloton liquid scintillator detector of unprecedented $3\\%$ energy resolution (at 1 MeV) at 700-meter deep underground and to have other rich scientific possibilities. Currently MC study shows a sensitivity of the mass hierarchy to be $\\overline{\\Delta\\chi^2}\\sim 11$ and $\\overline{\\Delta\\chi^2}\\sim 16$ in a relative and an absolute measurement, respectively. JUNO has been approved by Chinese Academy of Sciences in 2013, and an international collaboration was established in 2014. The civil construction is in preparation and the R$\\&$D of the detectors are ongoing. A new offline software framework was developed for the detector simulation, the event reconstruction and the physics analysis. JUNO is planning to start taking data around 2020.

  13. Unsaturated fractured rock characterization methods and data sets at the Apache Leap Tuff Site

    SciTech Connect (OSTI)

    Rasmussen, T.C.; Evans, D.D.; Sheets, P.J.; Blanford, J.H. [Arizona Univ., Tucson, AZ (USA). Dept. of Hydrology and Water Resources

    1990-08-01

    Performance assessment of high-level nuclear waste containment feasibility requires representative values of parameters as input, including parameter moments, distributional characteristics, and covariance structures between parameters. To meet this need, characterization methods and data sets for interstitial, hydraulic, pneumatic and thermal parameters for a slightly welded fractured tuff at the Apache Leap Tuff Site situated in central Arizona are reported in this document. The data sets include the influence of matric suction on measured parameters. Spatial variability is investigated by sampling along nine boreholes at regular distances. Laboratory parameter estimates for 105 core segments are provided, as well as field estimates centered on the intervals where the core segments were collected. Measurement uncertainty is estimated by repetitively testing control samples. 31 refs., 10 figs., 21 tabs.

  14. FEASIBILITY STUDY FOR A PETROLEUM REFINERY FOR THE JICARILLA APACHE TRIBE

    SciTech Connect (OSTI)

    John D. Jones

    2004-10-01

    A feasibility study for a proposed petroleum refinery for the Jicarilla Apache Indian Reservation was performed. The available crude oil production was identified and characterized. There is 6,000 barrels per day of crude oil production available for processing in the proposed refinery. The proposed refinery will utilize a lower temperature, smaller crude fractionation unit. It will have a Naphtha Hydrodesulfurizer and Reformer to produce high octane gasoline. The surplus hydrogen from the reformer will be used in a specialized hydrocracker to convert the heavier crude oil fractions to ultra low sulfur gasoline and diesel fuel products. The proposed refinery will produce gasoline, jet fuel, diesel fuel, and a minimal amount of lube oil. The refinery will require about $86,700,000 to construct. It will have net annual pre-tax profit of about $17,000,000. The estimated return on investment is 20%. The feasibility is positive subject to confirmation of long term crude supply. The study also identified procedures for evaluating processing options as a means for American Indian Tribes and Native American Corporations to maximize the value of their crude oil production.

  15. Space Telescope Programs Hubble Observatory

    E-Print Network [OSTI]

    Colorado at Boulder, University of

    Functional Test Pre-Vibration Functional BATC Acceptance Review · Verify Mechanical Integrity Only · Static Observatory HST-COS FUV PER 11/8/00 FUV Detector System Test Flow Vibration Test Post-Vibration Functional EMI Acceleration · Random Vibration · Sine Survey FUV detector Performance tests ·Long-Form Detector Functional

  16. Carnegie Mellon Opens Data Center Observatory

    E-Print Network [OSTI]

    Carnegie Mellon Opens Data Center Observatory :: CyLab Press Releases In the News CSO Council INI Home > Media Center > In the News > Carnegie Mellon Opens Data Center Observatory Carnegie Mellon Opens Data Center Observatory On May 23, 2006 Carnegie Mellon University held a lab dedication ceremony

  17. Mescalero Apache Tribe Monitored Retrievable Storage (MRS). Phase 1 feasibility study report

    SciTech Connect (OSTI)

    Peso, F.

    1992-03-13

    The Nuclear Waste Policy Act of 1982, as amended, authorizes the siting, construction and operation of a Monitored Retrievable Storage (MRS) facility. The MRS is intended to be used for the temporary storage of spent nuclear fuel from the nation`s nuclear power plants beginning as early as 1998. Pursuant to the Nuclear Waste Policy Act, the Office of the Nuclear Waste Negotiator was created. On October 7, 1991, the Nuclear Waste Negotiator invited the governors of states and the Presidents of Indian tribes to apply for government grants in order to conduct a study to assess under what conditions, if any, they might consider hosting an MRS facility. Pursuant to this invitation, on October 11, 1991 the Mescalero Apache Indian Tribe of Mescalero, NM applied for a grant to conduct a phased, preliminary study of the safety, technical, political, environmental, social and economic feasibility of hosting an MRS. The preliminary study included: (1) An investigative education process to facilitate the Tribe`s comprehensive understanding of the safety, environmental, technical, social, political, and economic aspects of hosting an MRS, and; (2) The development of an extensive program that is enabling the Tribe, in collaboration with the Negotiator, to reach an informed and carefully researched decision regarding the conditions, (if any), under which further pursuit of the MRS would be considered. The Phase 1 grant application enabled the Tribe to begin the initial activities necessary to determine whether further consideration is warranted for hosting the MRS facility. The Tribe intends to pursue continued study of the MRS in order to meet the following objectives: (1) Continuing the education process towards a comprehensive understanding of the safety, environmental, technical, social and economic aspects of the MRS; (2) Conducting an effective public participation and information program; (3) Participating in MRS meetings.

  18. DISCOVERY OF A DYNAMICAL COLD POINT IN THE HEART OF THE SAGITTARIUS dSph GALAXY WITH OBSERVATIONS FROM THE APOGEE PROJECT

    SciTech Connect (OSTI)

    Majewski, Steven R.; Hasselquist, Sten; Nidever, David L. E-mail: sh6cy@virginia.edu; and others

    2013-11-01

    The dynamics of the core of the Sagittarius (Sgr) dwarf spheroidal (dSph) galaxy are explored using high-resolution (R ? 22, 500), H-band, near-infrared spectra of over 1000 giant stars in the central 3 deg{sup 2} of the system, of which 328 are identified as Sgr members. These data, among some of the earliest observations from the Sloan Digital Sky Survey III/Apache Point Observatory Galactic Evolution Experiment (APOGEE) and the largest published sample of high resolution Sgr dSph spectra to date, reveal a distinct gradient in the velocity dispersion of Sgr from 11 to 14 km s{sup –1} for radii >0.°8 from center to a dynamical cold point of 8 km s{sup –1} in the Sgr center—a trend differing from that found in previous kinematical analyses of Sgr over larger scales that suggests a more or less flat dispersion profile at these radii. Well-fitting mass models with either cored and cusped dark matter distributions can be found to match the kinematical results, although the cored profile succeeds with significantly more isotropic stellar orbits than required for a cusped profile. It is unlikely that the cold point reflects an unusual mass distribution. The dispersion gradient may arise from variations in the mixture of populations with distinct kinematics within the dSph; this explanation is suggested (e.g., by detection of a metallicity gradient across similar radii), but not confirmed, by the present data. Despite these remaining uncertainties about their interpretation, these early test data (including some from instrument commissioning) demonstrate APOGEE's usefulness for precision dynamical studies, even for fields observed at extreme airmasses.

  19. EA-2002: Right-of-Way Application for the Tucson-Apache 115-kV Transmission Line, Pima County, Arizona

    Broader source: Energy.gov [DOE]

    Western Area Power Administration (Western) and the Bureau of Indian Affairs (BIA), as joint lead agencies, prepared an EA that evaluates the potential environmental impacts of a proposal for BIA to grant Western a 150-foot right-of-way across tribal land along the existing Tucson-Apache Transmission Line to replace the previous 100-foot right-of-way, which has expired.

  20. Great Salt Lake Basin Hydrologic Observatory

    E-Print Network [OSTI]

    Tarboton, David

    Great Salt Lake Basin Hydrologic Observatory Contact Information David Tarboton Utah State University of Utah 135 South 1460 East Rm 719 Salt Lake City, Utah (801) 581-5033 wjohnson. The Great Salt Lake Basin Hydrologic Observatory development team is highly committed to this concept

  1. The Pierre Auger Cosmic Ray Observatory

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

    Aab, Alexander

    2015-07-08

    The Pierre Auger Observatory, located on a vast, high plain in western Argentina, is the world's largest cosmic ray observatory. The objectives of the Observatory are to probe the origin and characteristics of cosmic rays above 1017 eV and study the interactions of these, the most energetic particles observed in nature. The Auger design features an array of 1660 water Cherenkov particle detector stations spread over 3000 km2 overlooked by 24 air fluorescence telescopes. Additionally, three high elevation fluorescence telescopes overlook a 23.5 km2, 61-detector infilled array with 750 m spacing. The Observatory has been in successful operation since completionmore »in 2008 and has recorded data from an exposure exceeding 40,000 km2 sr yr. This paper describes the design and performance of the detectors, related subsystems and infrastructure that make up the Observatory.« less

  2. The Pierre Auger Cosmic Ray Observatory

    E-Print Network [OSTI]

    ,

    2015-01-01

    The Pierre Auger Observatory, located on a vast, high plain in western Argentina, is the world's largest cosmic ray observatory. The objectives of the Observatory are to probe the origin and characteristics of cosmic rays above $10^{17}$ eV and to study the interactions of these, the most energetic particles observed in nature. The Auger design features an array of 1660 water-Cherenkov particle detector stations spread over 3000 km$^2$ overlooked by 24 air fluorescence telescopes. In addition, three high elevation fluorescence telescopes overlook a 23.5 km$^2$, 61 detector infill array. The Observatory has been in successful operation since completion in 2008 and has recorded data from an exposure exceeding 40,000 km$^2$ sr yr. This paper describes the design and performance of the detectors, related subsystems and infrastructure that make up the Auger Observatory.

  3. The Pierre Auger Cosmic Ray Observatory

    SciTech Connect (OSTI)

    Aab, Alexander

    2015-07-08

    The Pierre Auger Observatory, located on a vast, high plain in western Argentina, is the world's largest cosmic ray observatory. The objectives of the Observatory are to probe the origin and characteristics of cosmic rays above 1017 eV and study the interactions of these, the most energetic particles observed in nature. The Auger design features an array of 1660 water Cherenkov particle detector stations spread over 3000 km2 overlooked by 24 air fluorescence telescopes. Additionally, three high elevation fluorescence telescopes overlook a 23.5 km2, 61-detector infilled array with 750 m spacing. The Observatory has been in successful operation since completion in 2008 and has recorded data from an exposure exceeding 40,000 km2 sr yr. This paper describes the design and performance of the detectors, related subsystems and infrastructure that make up the Observatory.

  4. The Princeton Tritium Observatory for Light, Early Universe,...

    Office of Environmental Management (EM)

    The Princeton Tritium Observatory for Light, Early Universe, Massive Neutrino Yield (PTOLEMY) The Princeton Tritium Observatory for Light, Early Universe, Massive Neutrino Yield...

  5. Virtual Global Magnetic ObservatoryVirtual Global Magnetic Observatory Network in Africa:Network in Africa

    E-Print Network [OSTI]

    Michigan, University of

    Virtual Global Magnetic ObservatoryVirtual Global Magnetic Observatory Network in Africa:Network in Africa: Capacity Building for ElectronicCapacity Building for Electronic Geophysical YearGeophysical Year · VGMO.NET is a middleware architecture that provides a new way for the worldwide geomagnetic community

  6. Hybrid Performance of the Pierre Auger Observatory

    E-Print Network [OSTI]

    B. R. Dawson; for the Pierre Auger Collaboration

    2007-06-08

    A key feature of the Pierre Auger Observatory is its hybrid design, in which ultra high energy cosmic rays are detected simultaneously by fluorescence telescopes and a ground array. The two techniques see air showers in complementary ways, providing important cross-checks and measurement redundancy. Much of the hybrid capability stems from the accurate geometrical reconstruction it achieves, with accuracy better than either the ground array detectors or a single telescope could achieve independently. We have studied the geometrical and longitudinal profile reconstructions of hybrid events. We present the results for the hybrid performance of the Observatory, including trigger efficiency, energy and angular resolution, and the efficiency of the event selection.

  7. Status of the Milagro $\\gamma$ Ray Observatory

    E-Print Network [OSTI]

    Atkins, R; Berley, D; Chen, M L; Coyne, D G; Delay, R S; Dingus, B L; Dorfan, D E; Ellsworth, R W; Evans, D; Falcone, A D; Fleysher, L; Fleysher, R; Gisler, G; Goodman, J A; Haines, T J; Hoffman, C M; Hugenberger, S; Kelley, L A; Leonor, I; Macri, J R; McConnell, M; McCullough, J F; McEnery, J E; Miller, R S; Mincer, A I; Morales, M F; Némethy, P; Ryan, J M; Schneider, M; Shen, B; Shoup, A L; Sinnis, G; Smith, A J; Sullivan, G W; Thompson, T N; Tümer, T O; Wang, K; Wascko, M O; Westerhoff, S; Williams, D A; Yang, T; Yodh, G B

    2001-01-01

    The Milagro Gamma Ray Observatory is the world's first large-area water Cherenkov detector capable of continuously monitoring the sky at TeV energies. Located in northern New Mexico, Milagro will perform an all sky survey of the Northern Hemisphere at energies between ~250 GeV and 50 TeV. With a high duty cycle, large detector area (~5000 square meters), and a wide field-of-view (~1 sr), Milagro is uniquely capable of searching for transient and DC sources of high-energy gamma-ray emission. Milagro has been operating since February, 1999. The current status of the Milagro Observatory and initial results will be discussed.

  8. Status of the Milagro Gamma Ray Observatory

    E-Print Network [OSTI]

    R. Atkins; W. Benbow; D. Berley; M. -L. Chen; D. G. Coyne; R. S. Delay; B. L. Dingus; D. E. Dorfan; R. W. Ellsworth; D. Evans; A. Falcone; L. Fleysher; R. Fleysher; G. Gisler; J. A. Goodman; T. J. Haines; C. M. Hoffman; S. Hugenberger; L. A. Kelley; I. Leonor; J. Macri; M. McConnell; J. F. McCullough; J. E. McEnery; R. S. Miller; A. I. Mincer; M. F. Morales; P. Nemethy; J. M. Ryan; M. Schneider; B. Shen; A. Shoup; G. Sinnis; A. J. Smith; G. W. Sullivan; T. N. Thompson; O. T. Tumer; K. Wang; M. O. Wascko; S. Westerhoff; D. A. Williams; T. Yang; G. B. Yodh

    1999-06-24

    The Milagro Gamma Ray Observatory is the world's first large-area water Cherenkov detector capable of continuously monitoring the sky at TeV energies. Located in northern New Mexico, Milagro will perform an all sky survey of the Northern Hemisphere at energies between ~250 GeV and 50 TeV. With a high duty cycle, large detector area (~5000 square meters), and a wide field-of-view (~1 sr), Milagro is uniquely capable of searching for transient and DC sources of high-energy gamma-ray emission. Milagro has been operating since February, 1999. The current status of the Milagro Observatory and initial results will be discussed.

  9. The origin of the Hawaiian Volcano Observatory

    SciTech Connect (OSTI)

    Dvorak, John [University of Hawaii's Institute for Astronomy (United States)

    2011-05-15

    I first stepped through the doorway of the Hawaiian Volcano Observatory in 1976, and I was impressed by what I saw: A dozen people working out of a stone-and-metal building perched at the edge of a high cliff with a spectacular view of a vast volcanic plain. Their primary purpose was to monitor the island's two active volcanoes, Kilauea and Mauna Loa. I joined them, working for six weeks as a volunteer and then, years later, as a staff scientist. That gave me several chances to ask how the observatory had started.

  10. Axions at the International Axion Observatory

    E-Print Network [OSTI]

    Redondo, Javier

    2016-01-01

    QCD axions with meV mass can be behind some stellar cooling anomalies and form all or part of the cold dark matter of the universe. We discuss on a proposed experiment to discover the solar flux of meV mass axions: the International AXion Observatory: IAXO.

  11. Solar Dynamics Observatory/ Extreme Ultraviolet Variability Experiment

    E-Print Network [OSTI]

    Mojzsis, Stephen J.

    Solar Dynamics Observatory/ EVE Extreme Ultraviolet Variability Experiment Frequently Asked and model solar extreme ultraviolet irradiance variations due to solar flares, solar rotation, and solar and structure of the Sun. What is solar variability? Solar radiation varies on all time scales ranging from

  12. Observatory Conversion of Pixels to Coordinates

    E-Print Network [OSTI]

    Greisen, Eric

    Eric W. Greisen Mark Calabretta National Radio Astronomy Observatory Australia Telescope National 300 330 60 30 0 ­30 ­60 Hammer­Aitoff projection 0 30 60 90 120 150 180 180 210 240 270 300 330 60 30, pole (0, 30) 0 30 60 90 120 150 180 180 210 240 270 300 330 60 30 0 ­30 ­60 Hammer­Aitoff projection

  13. Bishop's University Astronomical Observatory October 2009

    E-Print Network [OSTI]

    that was built on the roof of Nicolls adjacent to the Observatory and the other is Bishop's first-ever solar of our visitors. The solar panel and battery system provide sufficient energy to easily light the deck that reduce the level of light pollution. The installation of the solar energy system and the replacement

  14. Operations of and Future Plans for the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Abraham, : J.; Abreu, P.; Aglietta, M.; Aguirre, C.; Ahn, E.J.; Allard, D.; Allekotte, I.; Allen, J.; Alvarez-Muniz, J.; Ambrosio, M.; Anchordoqui, L.

    2009-06-01

    These are presentations to be presented at the 31st International Cosmic Ray Conference, in Lodz, Poland during July 2009. It consists of the following presentations: (1) Performance and operation of the Surface Detectors of the Pierre Auger Observatory; (2) Extension of the Pierre Auger Observatory using high-elevation fluorescence telescopes (HEAT); (3) AMIGA - Auger Muons and Infill for the Ground Array of the Pierre Auger Observatory; (4) Radio detection of Cosmic Rays at the southern Auger Observatory; (5) Hardware Developments for the AMIGA enhancement at the Pierre Auger Observatory; (6) A simulation of the fluorescence detectors of the Pierre Auger Observatory using GEANT 4; (7) Education and Public Outreach at the Pierre Auger Observatory; (8) BATATA: A device to characterize the punch-through observed in underground muon detectors and to operate as a prototype for AMIGA; and (9) Progress with the Northern Part of the Pierre Auger Observatory.

  15. "Towards Optics-Based Measurements in Ocean Observatories"

    E-Print Network [OSTI]

    Boss, Emmanuel S.

    /JPSS ­ UAV ­ Ocean optics, Biological ­ Laser penetration New opportunity · Insitu Sensors ­ (Gliders"Towards Optics-Based Measurements in Ocean Observatories" "Ocean Observatories Contributions to Ocean Models and Data Assimilation For Ecosystems" Ocean Optics 2012 Glasgow Scotland Robert Arnone

  16. The endless mantra : innovation at the Keck Observatory

    E-Print Network [OSTI]

    Bobra, Monica Godha

    2005-01-01

    A study of historical, current, and future developments at the Keck Observatory revealed a thriving philosophy of innovation. Intended to defy obsoletion and keep the observatory competitive over long time scales, this ...

  17. The Antarctic Submillimeter Telescope and Remote Observatory (AST/RO)

    E-Print Network [OSTI]

    Antony A. Stark; John Bally; Simon P. Balm; T. M. Bania; Alberto D. Bolatto; Richard A. Chamberlin; Gregory Engargiola; Maohai Huang; James G. Ingalls; Karl Jacobs; James M. Jackson; Jacob W. Kooi; Adair P. Lane; K. -Y. Lo; Rodney D. Marks; Christopher L. Martin; Dennis Mumma; Roopesh Ojha; Rudolf Schieder; Johannes Staguhn; Juergen Stutzki; Christopher K. Walker; Robert W. Wilson; Gregory A. Wright; Xiaolei Zhang; Peter Zimmermann; Ruediger Zimmermann

    2000-12-15

    AST/RO, a 1.7 m diameter telescope for astronomy and aeronomy studies at wavelengths between 200 and 2000 microns, was installed at the South Pole during the 1994-1995 Austral summer. The telescope operates continuously through the Austral winter, and is being used primarily for spectroscopic studies of neutral atomic carbon and carbon monoxide in the interstellar medium of the Milky Way and the Magellanic Clouds. The South Pole environment is unique among observatory sites for unusually low wind speeds, low absolute humidity, and the consistent clarity of the submillimeter sky. Four heterodyne receivers, an array receiver, three acousto-optical spectrometers, and an array spectrometer are installed. A Fabry-Perot spectrometer using a bolometric array and a Terahertz receiver are in development. Telescope pointing, focus, and calibration methods as well as the unique working environment and logistical requirements of the South Pole are described.

  18. Science Potential of a Deep Ocean Antineutrino Observatory

    E-Print Network [OSTI]

    Steve Dye

    2006-12-15

    This paper presents science potential of a deep ocean antineutrino observatory under development at Hawaii. The observatory design allows for relocation from one site to another. Positioning the observatory some 60 km distant from a nuclear reactor complex enables precision measurement of neutrino mixing parameters, leading to a determination of neutrino mass hierarchy. At a mid-Pacific location the observatory measures the flux and ratio of uranium and thorium decay neutrinos from earth's mantle and performs a sensitive search for a hypothetical natural fission reactor in earth's core. A subsequent deployment at another mid-ocean location would test lateral heterogeneity of uranium and thorium in earth's mantle.

  19. Radio Wavelength Observatories within the Exploration Architecture

    E-Print Network [OSTI]

    J. Lazio; R. J. Macdowall; J. Burns; L. Demaio; D. L. Jones; K. W. Weiler

    2007-01-26

    Observations at radio wavelengths address key problems in astrophysics, astrobiology, and lunar structure including the first light in the Universe (the Epoch of Reionization), the presence of magnetic fields around extrasolar planets, particle acceleration mechanisms, and the structure of the lunar ionosphere. Moreover, achieving the performance needed to address these scientific questions demands observations at wavelengths longer than those that penetrate the Earth's ionosphere, observations in extremely "radio quiet" locations such as the Moon's far side, or both. We describe a series of lunar-based radio wavelength interferometers of increasing capability. The Radio Observatory for Lunar Sortie Science (ROLSS) is an array designed to be deployed during the first lunar sorties (or even before via robotic rovers) and addressing particle acceleration and the lunar ionosphere. Future arrays would be larger, more capable, and deployed as experience is gained in working on the lunar surface.

  20. PARKER LIBRARY STEWARD OBSERVATORY PLSO Guide to the Library

    E-Print Network [OSTI]

    Ziurys, Lucy M.

    PARKER LIBRARY STEWARD OBSERVATORY PLSO Guide to the Library I. Circulation Guidelines A. Borrowers and Planetary Lab, and Kitt Peak National Observatory. b. Undergraduate astronomy majors, whose names and campus PLSO materials only in the library. b. Other persons who wish to borrow material from the library must

  1. Ocean Observatories Initiative: Pacific Northwest The Endurance Array

    E-Print Network [OSTI]

    Kurapov, Alexander

    Ocean Observatories Initiative: Pacific Northwest The Endurance Array The processes that shape. The Ocean Observatories Initiative (OOI) will build a 25­30 year laboratory on the seafloor, in the water column, and at the ocean surface. It will make available novel platforms for oceanographic discovery

  2. 7 March 2013 Armagh Observatory Forthcoming Public Events

    E-Print Network [OSTI]

    for approximately half an hour. 2. St. Patrick's Day Event The Armagh Observatory and the Armagh Public Library Evensong from 3.15pm to 4.00pm. (www.stpatricks-cathedral.org) b. The Armagh Public Library and No. 57 March 2013 Armagh Observatory Forthcoming Public Events 1. "Comet PANSTARRS IS COMING" Students

  3. Towards a Taxonomy for Web Observatories Web Science Institute

    E-Print Network [OSTI]

    Towards a Taxonomy for Web Observatories Ian Brown Web Science Institute University of Southampton University of Southampton Southampton, SO17 1BJ, UK +44 (0)23 8059 5000 wh@soton.ac.uk Lisa Harris Web.j.harris@soton.ac.uk ABSTRACT In this paper, we propose an initial structure to support a taxonomy for Web Observatories (WO

  4. Field Operations Manager-Domain 3 The National Ecological Observatory Network (NEON) is a $430 million dollar observatory project dedicated to

    E-Print Network [OSTI]

    Ma, Lena

    ) is a $430 million dollar observatory project dedicated to understanding how changes in climate, land use

  5. The Gemini Observatory Science Operations Plan Phil Puxley, Fred Gillett, Matt Mountain and Doug Simons

    E-Print Network [OSTI]

    The Gemini Observatory Science Operations Plan Phil Puxley, Fred Gillett, Matt Mountain and Doug Gemini Observatory Science Operations Plan Phil Puxley, Fred Gillett, Matt Mountain and Doug Simons

  6. GAMMA-400 gamma-ray observatory

    E-Print Network [OSTI]

    Topchiev, N P; Bonvicini, V; Adriani, O; Aptekar, R L; Arkhangelskaja, I V; Arkhangelskiy, A I; Bakaldin, A V; Bergstrom, L; Berti, E; Bigongiari, G; Bobkov, S G; Boezio, M; Bogomolov, E A; Bonechi, L; Bongi, M; Bottai, S; Castellini, G; Cattaneo, P W; Cumani, P; Dalkarov, O D; Dedenko, G L; De Donato, C; Dogiel, V A; Finetti, N; Gascon, D; Gorbunov, M S; Gusakov, Yu V; Hnatyk, B I; Kadilin, V V; Kaplin, V A; Kaplun, A A; Kheymits, M D; Korepanov, V E; Larsson, J; Leonov, A A; Loginov, V A; Longo, F; Maestro, P; Marrocchesi, P S; Martinez, M; Menshenin, A L; Mikhailov, V V; Mocchiutti, E; Moiseev, A A; Mori, N; Moskalenko, I V; Naumov, P Yu; Papini, P; Paredes, J M; Pearce, M; Picozza, P; Rappoldi, A; Ricciarini, S; Runtso, M F; Ryde, F; Serdin, O V; Sparvoli, R; Spillantini, P; Stozhkov, Yu I; Suchkov, S I; Taraskin, A A; Tavani, M; Tiberio, A; Tyurin, E M; Ulanov, M V; Vacchi, A; Vannuccini, E; Vasilyev, G I; Ward, J E; Yurkin, Yu T; Zampa, N; Zirakashvili, V N; Zverev, V G

    2015-01-01

    The GAMMA-400 gamma-ray telescope with excellent angular and energy resolutions is designed to search for signatures of dark matter in the fluxes of gamma-ray emission and electrons + positrons. Precision investigations of gamma-ray emission from Galactic Center, Crab, Vela, Cygnus, Geminga, and other regions will be performed, as well as diffuse gamma-ray emission, along with measurements of high-energy electron + positron and nuclei fluxes. Furthermore, it will study gamma-ray bursts and gamma-ray emission from the Sun during periods of solar activity. The energy range of GAMMA-400 is expected to be from ~20 MeV up to TeV energies for gamma rays, up to 20 TeV for electrons + positrons, and up to 10E15 eV for cosmic-ray nuclei. For high-energy gamma rays with energy from 10 to 100 GeV, the GAMMA-400 angular resolution improves from 0.1{\\deg} to ~0.01{\\deg} and energy resolution from 3% to ~1%; the proton rejection factor is ~5x10E5. GAMMA-400 will be installed onboard the Russian space observatory.

  7. Observatory, 125, 319322, 2005 EARTH IN THE COSMIC SHOOTING GALLERY

    E-Print Network [OSTI]

    , Vacheslav Emel'yanenko2 and Bill Napier3 1Armagh Observatory, College Hill, Armagh, BT61 9DG 2South Ural University, Chelyabinsk, 454080, Russia 3Cardiff Centre for Astrobiology, Cardiff University, Cardiff CF10 3

  8. Low-multiplicity Burst Search at the Sudbury Neutrino Observatory

    E-Print Network [OSTI]

    Chen, Min

    Results are reported from a search for low-multiplicity neutrino bursts in the Sudbury Neutrino Observatory. Such bursts could indicate the detection of a nearby core-collapse supernova explosion. The data were taken from ...

  9. Low Energy Investigations at Kamioka Observatory

    E-Print Network [OSTI]

    Hiroyuki Sekiya

    2013-01-30

    At Kamioka Observatory many activities for low energy rare event search are ongoing. Super-Kamiokande(SK), the largest water Cherenkov neutrino detector, currently continues data taking as the fourth phase of the experiment (SK-IV). In SK-IV, we have upgraded the water purification system and tuned water flow in the SK tank. Consequently the background level was lowered significantly. This allowed SK-IV to derive solar neutrino results down to 3.5MeV energy region. With these data, neutrino oscillation parameters are updated from global fit; $\\Delta m^2_{12}=7.44^{+0.2}_{-0.19}\\times10^{-5} {\\rm eV}^2$, $\\sin^2\\theta_{12}=0.304\\pm0.013$, $\\sin^2\\theta_{13}=0.030^{+0.017}_{-0.015}$. NEWAGE, the directional sensitive dark matter search experiment, is currently operated as "NEWAGE-0.3a" which is a $0.20\\times0.25\\times0.31$ m$^3$ micro-TPC filled with CF4 gas at 152 Torr. Recently we have developed "NEWAGE-0.3b". It was succeeded to lower the operation pressure down to 76 Torr and the threshold down to 50 keV (F recoils). XMASS experiment is looking for scintillation signals from dark matter interaction in 1 ton of liquid xenon. It was designed utilizing its self-shielding capability with fiducial volume confinement. However, we could lower the analysis threshold down to 0.3 keVee using whole volume of the detector. In February 2012, low threshold and very large exposure data (5591 kg$\\cdot$days) were collected. With these data, we have excluded some part of the parameter spaces claimed by DAMA/LIBRA and CoGeNT experiments.

  10. TeV GAMMA-RAY SURVEY OF THE NORTHERN HEMISPHERE SKY USING THE MILAGRO OBSERVATORY R. Atkins,1,2

    E-Print Network [OSTI]

    California at Santa Cruz, University of

    to search the entire northern hemisphere for such objects. The search for short bursts of TeV gamma rays hasTeV GAMMA-RAY SURVEY OF THE NORTHERN HEMISPHERE SKY USING THE MILAGRO OBSERVATORY R. Atkins,1,2 W) are presented. The data have been searched for steady point sources of TeV gamma rays between declinations of 1

  11. Design and Deployment of the Bonne Bay Observatory (B2O) B. de Young

    E-Print Network [OSTI]

    deYoung, Brad

    and data acquisition for the subsea node. Shore based computers collect the data from the observatory

  12. 8. Hokuriku Earthquake Prediction Observatory, Fukui (D.P.R.I.)

    E-Print Network [OSTI]

    Takada, Shoji

    11 34 8. Hokuriku Earthquake Prediction Observatory, Fukui (D.P.R.I.) 9. Primate Research Institute Quality Control (Eng.) 12. Shigaraki MU Observatory (R.I.S.H) 13. Osakayama Earthquake Prediction Observatory, Otsu, Shiga (D.P.R.I.) 14. Abuyama Earthquake Prediction Observatory, Takatsuki, Osaka (D

  13. LONG EXPOSURE POINT SPREAD FUNCTION ESTIMATION FROM SOLAR ADAPTIVE OPTICS LOOP DATA

    E-Print Network [OSTI]

    Astronomer, National Solar Observatory, New Mexico, USA Dr. Haimin Wang, Dissertation Co-Advisor DateABSTRACT LONG EXPOSURE POINT SPREAD FUNCTION ESTIMATION FROM SOLAR ADAPTIVE OPTICS LOOP DATA during solar observations due to the lack of point sources in the field-of-view. Moreover, the highly

  14. Supporting a Social Media Observatory with Customizable Index Structures --Architecture

    E-Print Network [OSTI]

    research activity in analysis of social media and micro- blogging data in recent years suggests media data. To support these "social media observatories" effectively, a storage platform must satisfy special requirements for loading and storage of multi-terabyte datasets, as well as efficient evaluation

  15. Wide-field stellar photometry in Piwnice Observatory

    E-Print Network [OSTI]

    Gracjan Maciejewski

    2007-12-17

    In this paper research projects based on the wide-field CCD photometry performed in Piwnice Observatory are discussed. The used telescopes, as well as dedicated software pipeline for data reduction are presented. The prospects for collaboration between Polish and Bulgarian institutes in the field of wide-field photometry are also discussed.

  16. NASA/TP--2006214434 Examination of the Armagh Observatory

    E-Print Network [OSTI]

    NASA/TP--2006­214434 Examination of the Armagh Observatory Annual Mean Temperature Record, 1844, Alabama July 2006 #12;The NASA STI Program Office...in Profile Since its founding, NASA has been dedicated to the advancement of aeronautics and space science. The NASA Scientific and Technical Information (STI) Program

  17. Results from the Milagro Gamma-Ray Observatory

    E-Print Network [OSTI]

    California at Santa Cruz, University of

    V energies, and a search for transient emission above 100 GeV from gamma-ray bursts. 1 Introduction remnants and gamma-ray bursts (GRB). Gamma rays are also produced when high-energy cosmic rays interactResults from the Milagro Gamma-Ray Observatory E. Blaufuss for the Milagro Collaboration a,1 , a

  18. NGEE Arctic Webcam Photographs, Barrow Environmental Observatory, Barrow, Alaska

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

    Bob Busey; Larry Hinzman

    The NGEE Arctic Webcam (PTZ Camera) captures two views of seasonal transitions from its generally south-facing position on a tower located at the Barrow Environmental Observatory near Barrow, Alaska. Images are captured every 30 minutes. Historical images are available for download. The camera is operated by the U.S. DOE sponsored Next Generation Ecosystem Experiments - Arctic (NGEE Arctic) project.

  19. The Royal Observatory Edinburgh: Astronomy past, present, and future

    E-Print Network [OSTI]

    Peacock, John

    on James Clerk Maxwell Telescope in Hawaii World's first CCD-like sub-millimetre camera SCUBA2 survey led, VISTA) ­ Next generation CCD surveys ­ Virtual Observatory and e-science tools #12;Scientific outlook Aims: ·Probing the nature of dark matter and dark energy ·Understanding the format

  20. The HAWC Gamma-Ray Observatory: Design, Calibration, and Operation

    E-Print Network [OSTI]

    Abeysekara, A U; Alvarez, C; Álvarez, J D; Arceo, R; Arteaga-Velázquez, J C; Solares, H A Ayala; Barber, A S; Baughman, B M; Bautista-Elivar, N; Belmont, E; BenZvi, S Y; Berley, D; Rosales, M Bonilla; Braun, J; Caballero-Lopez, R A; Caballero-Mora, K S; Carramiñana, A; Castillo, M; Cotti, U; Cotzomi, J; de la Fuente, E; De León, C; DeYoung, T; Hernandez, R Diaz; Díaz-Vélez, J C; Dingus, B L; DuVernois, M A; Ellsworth, R W; Fernandez, A; Fiorino, D W; Fraija, N; Galindo, A; Garfias, F; González, L X; González, M M; Goodman, J A; Grabski, V; Gussert, M; Hampel-Arias, Z; Hui, C M; Hüntemeyer, P; Imran, A; Iriarte, A; Karn, P; Kieda, D; Kunde, G J; Lara, A; Lauer, R J; Lee, W H; Lennarz, D; Vargas, H León; Linares, E C; Linnemann, J T; Longo, M; Luna-GarcIa, R; Marinelli, A; Martinez, H; Martinez, O; Martínez-Castro, J; Matthews, J A J; Miranda-Romagnoli, P; Moreno, E; Mostafá, M; Nava, J; Nellen, L; Newbold, M; Noriega-Papaqui, R; Oceguera-Becerra, T; Patricelli, B; Pelayo, R; Pérez-Pérez, E G; Pretz, J; Rivière, C; Rosa-González, D; Salazar, H; Salesa, F; Sanchez, F E; Sandoval, A; Santos, E; Schneider, M; Silich, S; Sinnis, G; Smith, A J; Sparks, K; Springer, R W; Taboada, I; Toale, P A; Tollefson, K; Torres, I; Ukwatta, T N; Villaseñor, L; Weisgarber, T; Westerhoff, S; Wisher, I G; Wood, J; Yodh, G B; Younk, P W; Zaborov, D; Zepeda, A; Zhou, H

    2013-01-01

    The High-Altitude Water Cherenkov Gamma Ray Observatory (HAWC) is under construction 4100 meters above sea level at Sierra Negra, Mexico. We describe the design and cabling of the detector, the characterization of the photomultipliers, and the timing calibration system. We also outline a next-generation detector based on the water Cherenkov technique.

  1. Instruments and Science Programs at Fresno State's Campus Observatory

    E-Print Network [OSTI]

    Ringwald, Frederick A.

    an Orion Ultrablock Light-Pollution Filter, also called a nebular filter since it passes only hydrogen betaGlow Broadband light pollution filter, which also passes the hydrogen alpha line. The observatory's 1.25-inch Hutech IDAS light-pollution suppression (LPS) filter deserves special mention. It has five narrow bands

  2. BIG BEAR SOLAR OBSERVATORY CENTER FOR SOLAR-TERRESTRIAL RESEARCH

    E-Print Network [OSTI]

    BIG BEAR SOLAR OBSERVATORY CENTER FOR SOLAR-TERRESTRIAL RESEARCH Faculty Position in Solar Physics, New Jersey Institute of Technology A tenure track faculty position in solar physics is available of NJIT's program in solar physics, visit http://solar.njit.edu. Applicants are required to have a Ph

  3. The World Space Observatory (WSO-UV) - Current status

    E-Print Network [OSTI]

    Michela Uslenghi; Isabella Pagano; Cristian Pontoni; Salvatore Scuderi; Boris Shustov

    2008-01-14

    This paper reports on the current status of the World Space Observatory WSO-UV, a space mission for UV astronomy, planned for launch at the beginning of next decade. It is based on a 1.7 m telescope, with focal plane instruments including high resolution spectrographs, long slit low resolution spectrographs and imaging cameras.

  4. A SURVEY OF EGRET SOURCES USING THE MILAGRO OBSERVATORY

    E-Print Network [OSTI]

    California at Santa Cruz, University of

    V. The third EGRET catalog contained 271 new gamma-ray sources with energies above 100 MeV. The 271 sources in this catalog include the single 1991 solar flare, the Large Magellanic Cloud, five pulsars, one radio galaxy objects. Located in northern New Mexico, the Milagro gamma-ray observatory employs a water

  5. SUN-EARTH CONNECTION Solar TErrestrial RElations Observatory

    E-Print Network [OSTI]

    MISSIONS SUN-EARTH CONNECTION STEREO Solar TErrestrial RElations Observatory Hinode CORONAL MASS. Twin spacecraft, placed in different orbits, take images to produce 3-D pictures of the Sun and Solar Japanese/US/UK mission to study interactions between the Sun's magnetic field and its outer atmosphere

  6. Radiosonde campaign in Paranal Observatory 2011: PWV measurement.

    E-Print Network [OSTI]

    to SOW document this report is a deliverable to ESO as part of the contract. 1Avenida Gran Bretaña 1111, Valparaíso, Chile. Contact: omar.cuevas@uv.cl - michel.cure@uv.cl 2European Southern Observatory 3http://www

  7. NGEE Arctic Webcam Photographs, Barrow Environmental Observatory, Barrow, Alaska

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

    Bob Busey; Larry Hinzman

    2012-04-01

    The NGEE Arctic Webcam (PTZ Camera) captures two views of seasonal transitions from its generally south-facing position on a tower located at the Barrow Environmental Observatory near Barrow, Alaska. Images are captured every 30 minutes. Historical images are available for download. The camera is operated by the U.S. DOE sponsored Next Generation Ecosystem Experiments - Arctic (NGEE Arctic) project.

  8. Synoptic Observing Programs at Big Bear Solar Observatory

    E-Print Network [OSTI]

    Synoptic Observing Programs at Big Bear Solar Observatory Haimin Wang and Philip R. Goode Big Bear and en- hance the comprehensive synoptic observing programs at BBSO, which include the following ve studies. Statistical studies on sunspot areas and magnetic shear are among the highlights of this research

  9. The Gemini Observatory Science Operations Plan Phil Puxley, Fred Gillett, Matt Mountain and Doug Simons

    E-Print Network [OSTI]

    The Gemini Observatory Science Operations Plan Phil Puxley, Fred Gillett, Matt Mountain and Doug; The Gemini Observatory Science Operations Plan Phil Puxley, Fred Gillett, Matt Mountain and Doug Simons

  10. Great Salt Lake Basin Hydrologic Observatory Prospectus Submitted to CUAHSI for consideration as a CUAHSI Hydrologic Observatory

    E-Print Network [OSTI]

    Tarboton, David

    1 Great Salt Lake Basin Hydrologic Observatory Prospectus Submitted to CUAHSI for consideration.S., the Great Salt Lake Basin provides the opportunity to observe climate and human-induced land-surface changes relationship between people and water across the globe and make the Great Salt Lake Basin a microcosm

  11. Geomagnetic observatory GAN Jakub Velimsky K. Chandra Shakar Rao Lars W. Pedersen Ahmed Muslim

    E-Print Network [OSTI]

    Cerveny, Vlastislav

    ´imsk´y et al. (ETH,UK,DTU,NGRI,GMO) Geomagnetic observatory GAN 27.4.2011/KG MFF UK 1 / 16 #12;Participating, Univ. Stuttgart) John Riddick (BGS, retired) Vel´imsk´y et al. (ETH,UK,DTU,NGRI,GMO) Geomagnetic Measurements and Observatory Practice, 1996) Vel´imsk´y et al. (ETH,UK,DTU,NGRI,GMO) Geomagnetic observatory

  12. US earthquake observatories: recommendations for a new national network

    SciTech Connect (OSTI)

    Not Available

    1980-01-01

    This report is the first attempt by the seismological community to rationalize and optimize the distribution of earthquake observatories across the United States. The main aim is to increase significantly our knowledge of earthquakes and the earth's dynamics by providing access to scientifically more valuable data. Other objectives are to provide a more efficient and cost-effective system of recording and distributing earthquake data and to make as uniform as possible the recording of earthquakes in all states. The central recommendation of the Panel is that the guiding concept be established of a rationalized and integrated seismograph system consisting of regional seismograph networks run for crucial regional research and monitoring purposes in tandem with a carefully designed, but sparser, nationwide network of technologically advanced observatories. Such a national system must be thought of not only in terms of instrumentation but equally in terms of data storage, computer processing, and record availability.

  13. Identifying clouds over the Pierre Auger Observatory using infrared satellite data

    SciTech Connect (OSTI)

    Abreu, Pedro; et al.,

    2013-12-01

    We describe a new method of identifying night-time clouds over the Pierre Auger Observatory using infrared data from the Imager instruments on the GOES-12 and GOES-13 satellites. We compare cloud identifications resulting from our method to those obtained by the Central Laser Facility of the Auger Observatory. Using our new method we can now develop cloud probability maps for the 3000 km^2 of the Pierre Auger Observatory twice per hour with a spatial resolution of ~2.4 km by ~5.5 km. Our method could also be applied to monitor cloud cover for other ground-based observatories and for space-based observatories.

  14. Hybrid Detection of UHECR with the Pierre Auger Observatory

    E-Print Network [OSTI]

    Miguel Mostafa; for the Pierre Auger Collaboration

    2006-07-31

    The Pierre Auger Observatory detects ultra-high energy cosmic rays by implementing two complementary air-shower techniques. The combination of a large ground array and fluorescence detectors, known as the "hybrid" concept, means that a rich variety of measurements can be made on a single shower, providing much improved information over what is possible with either detector alone. In this paper the hybrid reconstruction approach and its performance are described.

  15. The HAWC Gamma-Ray Observatory: Observations of Cosmic Rays

    E-Print Network [OSTI]

    Abeysekara, A U; Alvarez, C; Álvarez, J D; Arceo, R; Arteaga-Velázquez, J C; Solares, H A Ayala; Barber, A S; Baughman, B M; Bautista-Elivar, N; Belmont, E; BenZvi, S Y; Berley, D; Rosales, M Bonilla; Braun, J; Caballero-Lopez, R A; Caballero-Mora, K S; Carramiñana, A; Castillo, M; Cotti, U; Cotzomi, J; de la Fuente, E; De León, C; DeYoung, T; Hernandez, R Diaz; Díaz-Vélez, J C; Dingus, B L; DuVernois, M A; Ellsworth, R W; Fernandez, A; Fiorino, D W; Fraija, N; Galindo, A; Garfias, F; González, L X; González, M M; Goodman, J A; Grabski, V; Gussert, M; Hampel-Arias, Z; Hui, C M; Hüntemeyer, P; Imran, A; Iriarte, A; Karn, P; Kieda, D; Kunde, G J; Lara, A; Lauer, R J; Lee, W H; Lennarz, D; Vargas, H León; Linares, E C; Linnemann, J T; Longo, M; Luna-GarcIa, R; Marinelli, A; Martinez, H; Martinez, O; Martínez-Castro, J; Matthews, J A J; Miranda-Romagnoli, P; Moreno, E; Mostafá, M; Nava, J; Nellen, L; Newbold, M; Noriega-Papaqui, R; Oceguera-Becerra, T; Patricelli, B; Pelayo, R; Pérez-Pérez, E G; Pretz, J; Rivière, C; Rosa-González, D; Salazar, H; Salesa, F; Sanchez, F E; Sandoval, A; Santos, E; Schneider, M; Silich, S; Sinnis, G; Smith, A J; Sparks, K; Springer, R W; Taboada, I; Toale, P A; Tollefson, K; Torres, I; Ukwatta, T N; Villaseñor, L; Weisgarber, T; Westerhoff, S; Wisher, I G; Wood, J; Yodh, G B; Younk, P W; Zaborov, D; Zepeda, A; Zhou, H

    2013-01-01

    We describe measurements of GeV and TeV cosmic rays with the High-Altitude Water Cherenkov Gamma-Ray Observatory, or HAWC. The measurements include the observation of the shadow of the moon; the observation of small-scale and large-scale angular clustering of the TeV cosmic rays; the prospects for measurement of transient solar events with HAWC; and the observation of Forbush decreases with the HAWC engineering array and HAWC-30.

  16. Technology Development for a Neutrino AstrophysicalObservatory

    SciTech Connect (OSTI)

    Chaloupka, V.; Cole, T.; Crawford, H.J.; He, Y.D.; Jackson, S.; Kleinfelder, S.; Lai, K.W.; Learned, J.; Ling, J.; Liu, D.; Lowder, D.; Moorhead, M.; Morookian, J.M.; Nygren, D.R.; Price, P.B.; Richards, A.; Shapiro, G.; Shen, B.; Smoot, George F.; Stokstad, R.G.; VanDalen, G.; Wilkes, J.; Wright, F.; Young, K.

    1996-02-01

    We propose a set of technology developments relevant to the design of an optimized Cerenkov detector for the study of neutrino interactions of astrophysical interest. Emphasis is placed on signal processing innovations that enhance significantly the quality of primary data. These technical advances, combined with field experience from a follow-on test deployment, are intended to provide a basis for the engineering design for a kilometer-scale Neutrino Astrophysical Observatory.

  17. Technology development for a neutrino astrophysical observatory. Letter of intent

    SciTech Connect (OSTI)

    Chaloupka, V.; Cole, T.; Crawford, H.J.

    1996-02-01

    The authors propose a set of technology developments relevant to the design of an optimized Cerenkov detector for the study of neutrino interactions of astrophysical interest. Emphasis is placed on signal processing innovations that enhance significantly the quality of primary data. These technical advances, combined with field experience from a follow-on test deployment, are intended to provide a basis for the engineering design for a kilometer-scale Neutrino Astrophysical Observatory.

  18. Studies of Cosmic Ray Composition and Air Shower Structure with the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Abraham, : J.; Abreu, P.; Aglietta, M.; Aguirre, C.; Ahn, E.J.; Allard, D.; Allekotte, I.; Allen, J.; Alvarez-Muniz, J.; Ambrosio, M.; Anchordoqui, L.

    2009-06-01

    These are presentations to be presented at the 31st International Cosmic Ray Conference, in Lodz, Poland during July 2009. It consists of the following presentations: (1) Measurement of the average depth of shower maximum and its fluctuations with the Pierre Auger Observatory; (2) Study of the nuclear mass composition of UHECR with the surface detectors of the Pierre Auger Observatory; (3) Comparison of data from the Pierre Auger Observatory with predictions from air shower simulations: testing models of hadronic interactions; (4) A Monte Carlo exploration of methods to determine the UHECR composition with the Pierre Auger Observatory; (5) The delay of the start-time measured with the Pierre Auger Observatory for inclined showers and a comparison of its variance with models; (6) UHE neutrino signatures in the surface detector of the Pierre Auger Observatory; and (7) The electromagnetic component of inclined air showers at the Pierre Auger Observatory.

  19. SPECKLE INTERFEROMETRY AT THE U.S. NAVAL OBSERVATORY. XVII

    SciTech Connect (OSTI)

    Mason, Brian D.; Hartkopf, William I.; Wycoff, Gary L. E-mail: wih@usno.navy.mil

    2011-08-15

    The results of 3362 intensified CCD observations of double stars, made with the 26 inch refractor of the U.S. Naval Observatory, are presented. Each observation of a system represents a combination of over 2000 short-exposure images. These observations are averaged into 1970 mean relative positions and range in separation from 0.''78 to 72.''17, with a mean separation of 14.''76. This is the 17th in this series of papers and covers the period 2010 January 6 through December 20. Also presented are 10 pairs that are resolved for the first time.

  20. The "PISCO" speckle camera at Pic du Midi Observatory

    E-Print Network [OSTI]

    Jean-Louis Prieur; Laurent Koechlin; Christine André; Gérard Gallou; Christian Lucuix

    2006-09-29

    We present a new speckle camera designed and built at Observatoire Midi-Pyr\\'{e}n\\'{e}es. This focal instrument has been used for four years with the 2-meter Bernard Lyot Telescope of Pic du Midi observatory. It can be set in various operating modes: full pupil imaging, masked-pupil imaging, spectroscopy, wave-front sensor and stellar coronagraphy, hence its name "PISCO" ("Pupil Interferometry Speckle COronagraph"). Restored images of double and triple stars have demonstrated its capabilities in providing close to diffraction limited images (0.06 arcsec in V). PISCO has been fully tested and is now ready to be used by the whole astronomical community.

  1. Ultrahigh Energy Neutrinos at the Pierre Auger Observatory

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

    Abreu, P.; Aglietta, M.; Ahlers, M.; Ahn, E. J.; Albuquerque, I. F. M.; Allard, D.; Allekotte, I.; Allen, J.; Allison, P.; Almela, A.; et al

    2013-01-01

    The observation of ultrahigh energy neutrinos (UHE?s) has become a priority in experimental astroparticle physics. UHE?s can be detected with a variety of techniques. In particular, neutrinos can interact in the atmosphere (downward-going?) or in the Earth crust (Earth-skimming?), producing air showers that can be observed with arrays of detectors at the ground. With the surface detector array of the Pierre Auger Observatory we can detect these types of cascades. The distinguishing signature for neutrino events is the presence of very inclined showers produced close to the ground (i.e., after having traversed a large amount of atmosphere). In this workmore »we review the procedure and criteria established to search for UHE?s in the data collected with the ground array of the Pierre Auger Observatory. This includes Earth-skimming as well as downward-going neutrinos. No neutrino candidates have been found, which allows us to place competitive limits to the diffuse flux of UHE?s in the EeV range and above.« less

  2. The UFFO (Ultra-Fast Flash Observatory) Pathfinder

    E-Print Network [OSTI]

    Park, I H; Lim, H; Nam, J W; Chen, Pisin; Khrenov, B A; Kim, Y -K; Lee, C -H; Lee, J; Linder, E V; Panasyuk, M; Park, J H; Smoot, G F; Uhm, Z L

    2009-01-01

    Hundreds of gamma-ray burst (GRB) UV-optical light curves have been measured since the discovery of optical afterglows, however, even after nearly 5 years of operation of the SWIFT observatory, only a handful of measurements have been made soon (within a minute) after the gamma ray signal. This lack of early observations fails to address burst physics at the short time scales associated with burst events and progenitors. Because of this lack of sub-minute data, the characteristics of the UV-optical light curve of short-hard type GRB and rapid-rising GRB, which may account for ~30% of all GRB, remain practically unknown. We have developed methods for reaching the sub-minute and the sub-second timescales in a small spacecraft observatory appropriate for launch on a microsatellite. Rather than slewing the entire spacecraft to aim the UV-optical instrument at the GRB position, we use rapidly moving mirrors to redirect our optical beam. Our collaboration has produced a unique MEMS (microelectromechanical systems) ...

  3. Euro-VO - Coordination of Virtual Observatory activities in Europe

    E-Print Network [OSTI]

    Genova, Francoise; Arviset, Christophe; Lawrence, Andy; Pasian, Fabio; Solano, Enrique; Wambsganss, Joachim

    2015-01-01

    The European Virtual Observatory Euro-VO has been coordinating European VO activities through a series of projects co-funded by the European Commission over the last 15 years. The bulk of VO work in Europe is ensured by the national VO initiatives and those of intergovernmental agencies. VO activities at the European level coordinate the work in support of the three "pillars" of the Virtual Observatory: support to the scientific community, take-up by the data providers, and technological activities. Several Euro-VO projects have also provided direct support to selected developments and prototyping. This paper explains the methodology used by Euro-VO over the years. It summarizes the activities which were performed and their evolutions at different stages of the development of the VO, explains the Euro-VO role with respect to the international and national levels of VO activities, details the lessons learnt for best practices for the coordination of the VO building blocks, and the liaison with other European i...

  4. The Pierre Auger Observatory II: Studies of Cosmic Ray Composition and Hadronic Interaction models

    E-Print Network [OSTI]

    The Pierre Auger Collaboration; P. Abreu; M. Aglietta; E. J. Ahn; I. F. M. Albuquerque; D. Allard; I. Allekotte; J. Allen; P. Allison; J. Alvarez Castillo; J. Alvarez-Muñiz; M. Ambrosio; A. Aminaei; L. Anchordoqui; S. Andringa; T. Anti?i?; A. Anzalone; C. Aramo; E. Arganda; F. Arqueros; H. Asorey; P. Assis; J. Aublin; M. Ave; M. Avenier; G. Avila; T. Bäcker; M. Balzer; K. B. Barber; A. F. Barbosa; R. Bardenet; S. L. C. Barroso; B. Baughman; J. Bäuml; J. J. Beatty; B. R. Becker; K. H. Becker; A. Bellétoile; J. A. Bellido; S. BenZvi; C. Berat; X. Bertou; P. L. Biermann; P. Billoir; F. Blanco; M. Blanco; C. Bleve; H. Blümer; M. Bohá?ová; D. Boncioli; C. Bonifazi; R. Bonino; N. Borodai; J. Brack; P. Brogueira; W. C. Brown; R. Bruijn; P. Buchholz; A. Bueno; R. E. Burton; K. S. Caballero-Mora; L. Caramete; R. Caruso; A. Castellina; O. Catalano; G. Cataldi; L. Cazon; R. Cester; J. Chauvin; S. H. Cheng; A. Chiavassa; J. A. Chinellato; A. Chou; J. Chudoba; R. W. Clay; M. R. Coluccia; R. Conceição; F. Contreras; H. Cook; M. J. Cooper; J. Coppens; A. Cordier; U. Cotti; S. Coutu; C. E. Covault; A. Creusot; A. Criss; J. Cronin; A. Curutiu; S. Dagoret-Campagne; R. Dallier; S. Dasso; K. Daumiller; B. R. Dawson; R. M. de Almeida; M. De Domenico; C. De Donato; S. J. de Jong; G. De La Vega; W. J. M. de Mello Junior; J. R. T. de Mello Neto; I. De Mitri; V. de Souza; K. D. de Vries; G. Decerprit; L. del Peral; O. Deligny; H. Dembinski; N. Dhital; C. Di Giulio; J. C. Diaz; M. L. Díaz Castro; P. N. Diep; C. Dobrigkeit; W. Docters; J. C. D'Olivo; P. N. Dong; A. Dorofeev; J. C. dos Anjos; M. T. Dova; D. D'Urso; I. Dutan; J. Ebr; R. Engel; M. Erdmann; C. O. Escobar; A. Etchegoyen; P. Facal San Luis; I. Fajardo Tapia; H. Falcke; G. Farrar; A. C. Fauth; N. Fazzini; A. P. Ferguson; A. Ferrero; B. Fick; A. Filevich; A. Filip?i?; S. Fliescher; C. E. Fracchiolla; E. D. Fraenkel; U. Fröhlich; B. Fuchs; R. Gaior; R. F. Gamarra; S. Gambetta; B. García; D. García Gámez; D. Garcia-Pinto; A. Gascon; H. Gemmeke; K. Gesterling; P. L. Ghia; U. Giaccari; M. Giller; H. Glass; M. S. Gold; G. Golup; F. Gomez Albarracin; M. Gómez Berisso; P. Gonçalves; D. Gonzalez; J. G. Gonzalez; B. Gookin; D. Góra; A. Gorgi; P. Gouffon; S. R. Gozzini; E. Grashorn; S. Grebe; N. Griffith; M. Grigat; A. F. Grillo; Y. Guardincerri; F. Guarino; G. P. Guedes; A. Guzman; J. D. Hague; P. Hansen; D. Harari; S. Harmsma; J. L. Harton; A. Haungs; T. Hebbeker; D. Heck; A. E. Herve; C. Hojvat; N. Hollon; V. C. Holmes; P. Homola; J. R. Hörandel; A. Horneffer; M. Hrabovský; T. Huege; A. Insolia; F. Ionita; A. Italiano; C. Jarne; S. Jiraskova; M. Josebachuili; K. Kadija; K. -H. Kampert; P. Karhan; P. Kasper; B. Kégl; B. Keilhauer; A. Keivani; J. L. Kelley; E. Kemp; R. M. Kieckhafer; H. O. Klages; M. Kleifges; J. Kleinfeller; J. Knapp; D. -H. Koang; K. Kotera; N. Krohm; O. Krömer; D. Kruppke-Hansen; F. Kuehn; D. Kuempel; J. K. Kulbartz; N. Kunka; G. La Rosa; C. Lachaud; P. Lautridou; M. S. A. B. Leão; D. Lebrun; P. Lebrun; M. A. Leigui de Oliveira; A. Lemiere; A. Letessier-Selvon; I. Lhenry-Yvon; K. Link; R. López; A. Lopez Agüera; K. Louedec; J. Lozano Bahilo; A. Lucero; M. Ludwig; H. Lyberis; M. C. Maccarone; C. Macolino; S. Maldera; D. Mandat; P. Mantsch; A. G. Mariazzi; J. Marin; V. Marin; I. C. Maris; H. R. Marquez Falcon; G. Marsella; D. Martello; L. Martin; H. Martinez; O. Martínez Bravo; H. J. Mathes; J. Matthews; J. A. J. Matthews; G. Matthiae; D. Maurizio; P. O. Mazur; G. Medina-Tanco; M. Melissas; D. Melo; E. Menichetti; A. Menshikov; P. Mertsch; C. Meurer; S. Mi?anovi?; M. I. Micheletti; W. Miller; L. Miramonti; S. Mollerach; M. Monasor; D. Monnier Ragaigne; F. Montanet; B. Morales; C. Morello; E. Moreno; J. C. Moreno; C. Morris; M. Mostafá; C. A. Moura; S. Mueller; M. A. Muller; G. Müller; M. Münchmeyer; R. Mussa; G. Navarra; J. L. Navarro; S. Navas; P. Necesal; L. Nellen; A. Nelles; J. Neuser; P. T. Nhung; L. Niemietz; N. Nierstenhoefer; D. Nitz; D. Nosek; L. Nožka; M. Nyklicek; J. Oehlschläger; A. Olinto; V. M. Olmos-Gilbaja; M. Ortiz; N. Pacheco; D. Pakk Selmi-Dei; M. Palatka; J. Pallotta; N. Palmieri; G. Parente; E. Parizot; A. Parra; R. D. Parsons; S. Pastor; T. Paul; M. Pech; J. P?kala; R. Pelayo; I. M. Pepe; L. Perrone; R. Pesce; E. Petermann; S. Petrera; P. Petrinca; A. Petrolini; Y. Petrov; J. Petrovic; C. Pfendner; N. Phan; R. Piegaia; T. Pierog; P. Pieroni; M. Pimenta; V. Pirronello; M. Platino; V. H. Ponce; M. Pontz; P. Privitera; M. Prouza; E. J. Quel; S. Querchfeld; J. Rautenberg; O. Ravel; D. Ravignani; B. Revenu; J. Ridky; S. Riggi; M. Risse; P. Ristori; H. Rivera; V. Rizi; J. Roberts; C. Robledo; W. Rodrigues de Carvalho; G. Rodriguez; J. Rodriguez Martino; J. Rodriguez Rojo; I. Rodriguez-Cabo; M. D. Rodríguez-Frías; G. Ros; J. Rosado

    2011-07-24

    Studies of the composition of the highest energy cosmic rays with the Pierre Auger Observatory, including examination of hadronic physics effects on the structure of extensive air showers.

  5. Digital Elevation Model, 0.5-m, Barrow Environmental Observatory, Alaska, 2012

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

    Gangodagamage, Chandana; Wilson, Cathy; Rowland, Joel

    The dataset is a digital elevation model, DEM, of a 2km by 7km region in the vicinity of the Barrow Environmental Observatory near Barrow, Ak.

  6. Proceedings of ICRC 2001: 1 c Copernicus Gesellschaft 2001 Status of the Milagro Gamma Ray Observatory

    E-Print Network [OSTI]

    California at Santa Cruz, University of

    Gamma Ray Observatory, located at an altitude of 8,600 feet in the Jemez Mountains of New Mexico of the solar mag

  7. The Cosmic Ray Energy Spectrum and Related Measurements with the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Abraham, : J.; Abreu, P.; Aglietta, M.; Aguirre, C.; Ahn, E.J.; Allard, D.; Allekotte, I.; Allen, J.; Alvarez-Muniz, J.; Ambrosio, M.; Anchordoqui, L.

    2009-06-01

    These are presentations to be presented at the 31st International Cosmic Ray Conference, in Lodz, Poland during July 2009. It consists of the following presentations: (1) Measurement of the cosmic ray energy spectrum above 10{sup 18} eV with the Pierre Auger Observatory; (2) The cosmic ray flux observed at zenith angles larger than 60 degrees with the Pierre Auger Observatory; (3) Energy calibration of data recorded with the surface detectors of the Pierre Auger Observatory; (4) Exposure of the Hybrid Detector of The Pierre Auger Observatory; and (5) Energy scale derived from Fluorescence Telescopes using Cherenkov Light and Shower Universality.

  8. Astrophysical Sources of Cosmic Rays and Related Measurements with the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Abraham, : J.; Abreu, P.; Aglietta, M.; Aguirre, C.; Ahn, E.J.; Allard, D.; Allekotte, I.; Allen, J.; Alvarez-Muniz, J.; Ambrosio, M.; Anchordoqui, L.

    2009-06-01

    These are presentations to be presented at the 31st International Cosmic Ray Conference, in Lodz, Poland during July 2009. It consists of the following presentations: (1) Correlation of the highest energy cosmic rays with nearby extragalactic objects in Pierre Auger Observatory data; (2) Discriminating potential astrophysical sources of the highest energy cosmic rays with the Pierre Auger Observatory; (3) Intrinsic anisotropy of the UHECR from the Pierre Auger Observatory; (4) Ultra-high energy photon studies with the Pierre Auger Observatory; (5) Limits on the flux of diffuse ultra high energy neutrinos set using the Pierre Auger Observatory; (6) Search for sidereal modulation of the arrival directions of events recorded at the Pierre Auger Observatory; (7) Cosmic Ray Solar Modulation Studies in the Pierre Auger Observatory; (8) Investigation of the Displacement Angle of the Highest Energy Cosmic Rays Caused by the Galactic Magnetic Field; (9) Search for coincidences with astrophysical transients in Pierre Auger Observatory data; and (10) An alternative method for determining the energy of hybrid events at the Pierre Auger Observatory.

  9. Digital Elevation Model, 0.5-m, Barrow Environmental Observatory, Alaska, 2012

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

    Wilson,Cathy; Rowland,Joel; Gangodagamage,Chandana

    2013-12-08

    The dataset is a digital elevation model, DEM, of a 2km by 7km region in the vicinity of the Barrow Environmental Observatory near Barrow, Ak.

  10. PowerPoint Presentation

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

    for medical point of care diagnostics and drug delivery Ronen Polsky Department of Biosensors and Nanomaterials February 25, 2015 Sandia MedTech Showcase Sandia National...

  11. PowerPoint Presentation

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

    System (RapiDx) * Portable microfluidic in vitro diagnostic instrument for cancer and infectious disease biomarkers in human biological samples * Point-of-Care...

  12. PowerPoint Presentation

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

    optic links will replace many hardwire connections - Remotely programmable set-points and monitoring for each klystron cart - Klystron collector over-temperature protection will...

  13. Web points of interest

    E-Print Network [OSTI]

    Web points of interest ... JUGGLING CLUB; The Lafayette Citizens Band Home Page; Harold Boas' incredible list of math and life resources on the WEB.

  14. The Large Observatory For X-ray Timing: LOFT

    E-Print Network [OSTI]

    Bozzo, E

    2013-01-01

    LOFT, the Large Observatory for X-ray Timing, is a new space mission concept devoted to observations of Galactic and extra-Galactic sources in the X-ray domain with the main goals of probing gravity theory in the very strong field environment of black holes and other compact objects, and investigating the state of matter at supra-nuclear densities in neutron stars. The instruments on-board LOFT, the Large area detector and the Wide Field Monitor combine for the first time an unprecedented large effective area (~10 m2 at 8 keV) sensitive to X-ray photons mainly in the 2-30 keV energy range and a spectral resolution approaching that of CCD-based telescopes (down to 200 eV at 6 keV). LOFT is currently competing for a launch of opportunity in 2022 together with the other M3 mission candidates of the ESA Cosmic Vision Program.

  15. Low Multiplicity Burst Search at the Sudbury Neutrino Observatory

    E-Print Network [OSTI]

    SNO Collaboration

    2010-11-24

    Results are reported from a search for low-multiplicity neutrino bursts in the Sudbury Neutrino Observatory (SNO). Such bursts could indicate detection of a nearby core-collapse supernova explosion. The data were taken from Phase I (November 1999 - May 2001), when the detector was filled with heavy water, and Phase II (July 2001 - August 2003), when NaCl was added to the target. The search was a blind analysis in which the potential backgrounds were estimated and analysis cuts were developed to eliminate such backgrounds with 90% confidence before the data were examined. The search maintained a greater than 50% detection probability for standard supernovae occurring at a distance of up to 60 kpc for Phase I and up to 70 kpc for Phase II. No low-multiplicity bursts were observed during the data-taking period.

  16. Searching for Double Beta Decay with the Enriched Xenon Observatory

    SciTech Connect (OSTI)

    Hall, C.; /SLAC

    2007-03-16

    The Enriched Xenon Observatory (EXO) Collaboration is building a series of experiments to search for the neutrinoless double beta decay of {sup 136}Xe. The first experiment, known as EXO-200, will utilize 200 kg of xenon enriched to 80% in the isotope of interest, making it the largest double beta decay experiment to date by one order of magnitude. This experiment is rapidly being constructed, and will begin data taking in 2007. The EXO collaboration is also developing a technique to identify on an event-by-event basis the daughter barium ion of the double beta decay. If successful, this method would eliminate all conventional radioactive backgrounds to the decay, resulting in an ideal experiment. We summarize here the current status of EXO-200 construction and the barium tag R&D program.

  17. VAMOS: a Pathfinder for the HAWC Gamma-Ray Observatory

    E-Print Network [OSTI]

    Abeysekara, A U; Alvarez, C; Álvarez, J D; Ángeles, F; Arceo, R; Arteaga-Velázquez, J C; Avila-Aroche, A; Solares, H A Ayala; Badillo, C; Barber, A S; Baughman, B M; Bautista-Elivar, N; Gonzalez, J Becerra; Belmont, E; Benítez, E; BenZvi, S Y; Berley, D; Bernal, A; Rosales, M Bonilla; Braun, J; Caballero-Lopez, R A; Caballero-Mora, K S; Cabrera, I; Carramiñana, A; Castañeda-Martínez, L; Castillo, M; Cotti, U; Cotzomi, J; de la Fuente, E; De León, C; DeYoung, T; Diaz-Azuara, A; Diaz-Cruz, L; Hernandez, R Diaz; Díaz-Vélez, J C; Dingus, B L; Dultzin, D; DuVernois, M A; Ellsworth, R W; Fernandez, A; Fiorino, D W; Fraija, N; Galindo, A; García-Torales, G; Garfias, F; González, A; González, L X; González, M M; Goodman, J A; Grabski, V; Gussert, M; Guzmán-Cerón, C; Hampel-Arias, Z; Harding, J P; Hernández-Cervantes, L; Hui, C M; Hüntemeyer, P; Imran, A; Iriarte, A; Karn, P; Kieda, D; Kunde, G J; Langarica, R; Lara, A; Lara, G; Lauer, R J; Lee, W H; Lennarz, D; Vargas, H León; Linares, E C; Linnemann, J T; Longo, M; Luna-Garcia, R; Marinelli, A; Martínez, L A; Martínez, H; Martínez, O; Martínez-Castro, J; Martos, M; Matthews, J A J; McEnery, J; Torres, E Mendoza; Miranda-Romagnoli, P; Moreno, E; Mostafá, M; Nava, J; Nellen, L; Newbold, M; Noriega-Papaqui, R; Oceguera-Becerra, T; Page, D P; Patricelli, B; Pelayo, R; Pérez-Pérez, E G; Pretz, J; Ramírez, I; Renter, A; Rivière, C; Rosa-González, D; Ruiz-Sala, F; Ruiz-Velasco, E L; Ryan, J; Sacahui, J R; Salazar, H; Salesa, F; Sandoval, A; Santos, E; Schneider, M; Silich, S; Sinnis, G; Smith, A J; Woodle, K Sparks; Springer, R W; Suarez, F; Taboada, I; Tepe, A; Toale, P A; Tollefson, K; Torres, I; Tinoco, S; Ukwatta, T N; Galicia, J F Valdés; Vanegas, P; Vázquez, A; Villaseñor, L; Wall, W; Weisgarber, T; Westerhoff, S; Wisher, I G; Wood, J; Yodh, G B; Younk, P W; Zaborov, D; Zepeda, A; Zhou, H

    2014-01-01

    VAMOS was a prototype detector built in 2011 at an altitude of 4100m a.s.l. in the state of Puebla, Mexico. The aim of VAMOS was to finalize the design, construction techniques and data acquisition system of the HAWC observatory. HAWC is an air-shower array currently under construction at the same site of VAMOS with the purpose to study the TeV sky. The VAMOS setup included six water Cherenkov detectors and two different data acquisition systems. It was in operation between October 2011 and May 2012 with an average live time of 30%. Besides the scientific verification purposes, the eight months of data were used to obtain the results presented in this paper: the detector response to the Forbush decrease of March 2012, and the analysis of possible emission, at energies above 30 GeV, for long gamma-ray bursts GRB111016B and GRB120328B.

  18. SPECKLE INTERFEROMETRY AT THE U.S. NAVAL OBSERVATORY. XVIII

    SciTech Connect (OSTI)

    Mason, Brian D.; Hartkopf, William I.; Friedman, Elizabeth A. E-mail: wih@usno.navy.mil

    2012-05-15

    The results of 2490 intensified CCD observations of double stars, made with the 26 inch refractor of the U.S. Naval Observatory, are presented. Each observation of a system represents a combination of over 2000 short-exposure images. These observations are averaged into 1462 mean relative positions and range in separation from 0.''56 to 71.''80, with a mean separation of 14.''81. This is the 18th in this series of papers and covers the period 2011 January 3 through 2011 December 18. Also presented are four pairs which are resolved for the first time, thirteen other pairs which appear to be lost, and linear elements for four additional pairs.

  19. SPECKLE INTERFEROMETRY AT THE U.S. NAVAL OBSERVATORY. XIX

    SciTech Connect (OSTI)

    Mason, Brian D.; Hartkopf, William I.; Hurowitz, Haley M. E-mail: wih@usno.navy.mil

    2013-09-15

    The results of 2916 intensified CCD observations of double stars, made with the 26 inch refractor of the U.S. Naval Observatory, are presented. Each observation of a system represents a combination of over two thousand short-exposure images. These observations are averaged into 1584 mean relative positions and range in separation from 0.''54 to 98.''09, with a median separation of 11.''73. This is the 19th in this series of papers and covers the period 2012 January 5 through 2012 December 18. Also presented are 10 pairs that are reported for the first time, 17 pairs that appear to be lost, linear elements for 18 pairs, and orbital elements for 2 additional pairs.

  20. The Theoretical Astrophysical Observatory: Cloud-Based Mock Galaxy Catalogues

    E-Print Network [OSTI]

    Bernyk, Maksym; Tonini, Chiara; Hodkinson, Luke; Hassan, Amr H; Garel, Thibault; Duffy, Alan R; Mutch, Simon J; Poole, Gregory B

    2014-01-01

    We introduce the Theoretical Astrophysical Observatory (TAO), an online virtual laboratory that houses mock observations of galaxy survey data. Such mocks have become an integral part of the modern analysis pipeline. However, building them requires an expert knowledge of galaxy modelling and simulation techniques, significant investment in software development, and access to high performance computing. These requirements make it difficult for a small research team or individual to quickly build a mock catalogue suited to their needs. To address this TAO offers access to multiple cosmological simulations and semi-analytic galaxy formation models from an intuitive and clean web interface. Results can be funnelled through science modules and sent to a dedicated supercomputer for further processing and manipulation. These modules include the ability to (1) construct custom observer light-cones from the simulation data cubes; (2) generate the stellar emission from star formation histories, apply dust extinction, a...

  1. Thompson March 2003 -1STEREO -Solar Terrestrial Relations Observatory Mission STEREO GS PR

    E-Print Network [OSTI]

    -www.nrl.navy.mil] ­ S/WAVES Heritage: WIND WAVES [www-lep.gsfc.nasa.gov/waves/waves.html] ­ IMPACT Heritage: WIND 3Dp.sr.unh.edu/data.html] and at UCLA with IMPACT #12;Thompson ­ March 2003 - 7STEREO - Solar Terrestrial Relations Observatory MissionThompson ­ March 2003 - 1STEREO - Solar Terrestrial Relations Observatory Mission STEREO GS PR

  2. Adaptive optics system for the IRSOL solar observatory Renzo Ramelli a

    E-Print Network [OSTI]

    , Switzerland Abstract We present a low cost adaptive optics system developed for the solar observatoryAdaptive optics system for the IRSOL solar observatory by Renzo Ramelli a , Roberto Bucher b filter system REFERENCES [1] Bianda, M., Ramelli, R., and Gisler, D., Observing the Second Solar Spectrum

  3. A Search for TeV Emission from Active Galaxies using the Milagro Observatory

    E-Print Network [OSTI]

    California at Santa Cruz, University of

    A Search for TeV Emission from Active Galaxies using the Milagro Observatory by Elizabeth A. HaysV Emission from Active Galaxies using the Milagro Observatory Elizabeth A. Hays, Doctor of Philosophy, 2004 the results of two separate searches of the Milagro data for TeV emission. A real-time search of the entire

  4. A New High Contrast Imaging Program at Palomar Observatory SASHA HINKLEY,1,2

    E-Print Network [OSTI]

    A New High Contrast Imaging Program at Palomar Observatory SASHA HINKLEY,1,2 BEN R. OPPENHEIMER,3-term high contrast imaging program at the 200 inch (5 m) Hale Telescope at Palomar Observatory. The primary. The entire combination is mounted behind the Palomar adaptive optics (AO) system. The spectrograph obtains

  5. Big Bear Solar Observatory -New Jersey Institute of Technology 2005 Greetings

    E-Print Network [OSTI]

    Big Bear Solar Observatory - New Jersey Institute of Technology 2005 Greetings The Center for Solar-Terrestrial Reasearch (CSTR) at New Jersey Institute of Technology operates Big Bear Solar Observatory (BBSO), which provides a unique and precise measure of the Earth's reflectance (a critical climate parameter since

  6. A Large Area Detector proposed for the Large Observatory for X-ray Timing (LOFT)

    E-Print Network [OSTI]

    Zane, S; Kennedy, T; Feroci, M; Herder, J -W Den; Ahangarianabhari, M; Argan, A; Azzarello, P; Baldazzi, G; Barret, D; Bertuccio, G; Bodini, P; Bozzo, E; Cadoux, F; Cais, P; Campana, R; Coker, J; Cros, A; Del Monte, E; De Rosa, A; Di Cosimo, S; Donnarumma, I; Evangelista, Y; Favre, Y; Feldman, C; Fraser, G; Fuschino, F; Grassi, M; Hailey, M R; Hudec, R; Labanti, C; Macera, D; Malcovati, P; Marisaldi, M; Martindale, A; Mineo, T; Muleri, F; Nowak, M; Orlandini, M; Pacciani, L; Perinati, E; Petracek, V; Pohl, M; Rachevski, A; Smith, P; Santangelo, A; Seyler, J -Y; Schmid, C; Soffitta, P; Suchy, S; Tenzer, C; Uttley, P; Vacchi, A; Zampa, G; Zampa, N; Wilms, J; Winter, B

    2012-01-01

    The Large Observatory for X-ray Timing (LOFT) is one of the four candidate ESA M3 missions considered for launch in the 2022 time-frame. It is specifically designed to perform fast X-ray timing and probe the status of the matter near black holes and neutron stars. The LOFT scientific payload is composed of a Large Area Detector (LAD) and a Wide Field Monitor (WFM). The LAD is a 10 m2-class pointed instrument with 20 times the collecting area of the best past timing missions (such as RXTE) over the 2-30 keV range, which holds the capability to revolutionize studies of X-ray variability down to the millisecond time scales. Its ground-breaking characteristic is a low mass per unit surface, enabling an effective area of ~10 m^2 (@10 keV) at a reasonable weight. The development of such large but light experiment, with low mass and power per unit area, is now made possible by the recent advancements in the field of large-area silicon detectors - able to time tag an X-ray photon with an accuracy <10 {\\mu}s and an...

  7. Design, Environmental and Sustainability Constraints of new African Observatories: The example of the Mozambique Radio Astronomy Observatory

    E-Print Network [OSTI]

    Barbosa, Domingos; Ribeiro, Valerio A R M; Loots, Anita; Thondikulam, Venkatasubramani L; Gaylard, Michael; van Ardenne, Arnold; Colafrancesco, Sergio; Bergano, Miguel; Amador, Jose Carlos; Maia, Rodrigo; Melo, Rui

    2013-01-01

    The Mozambique Radio Astronomy Observatory (MRAO) will be a first milestone towards development of radioastronomy in Mozambique. Development of MRAO will constitute a preparation step towards participation in the upcoming Africa VLBI Network and the Square Kilometer Array project. The MRAO first antenna is planned to serve as a capacitation and training facility and will be installed after the conversion of a 7-meter telecom dish in South Africa. Therefore, this first radiotelescope design has to comply with local spectral and environmental constraints. Furthermore, power availability and long term sustainability with potential inclusion of solar power and control of Radio Frequency Interference are analyzed. Here we outline some of the design, environmental and power sustainability constraints.

  8. Search for patterns by combining cosmic-ray energy and arrival directions at the Pierre Auger Observatory

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

    Aab, A.; Abreu, P.; Aglietta, M.; Ahn, E. J.; Samarai, I. Al; Albuquerque, I. F. M.; Allekotte, I.; Allen, J.; Allison, P.; Almela, A.; et al

    2015-06-20

    Energy-dependent patterns in the arrival directions of cosmic rays are searched for using data of the Pierre Auger Observatory. We investigate local regions around the highest-energy cosmic rays with $E \\ge 6 \\times 10^{19}$ eV by analyzing cosmic rays with energies above $E \\ge 5 \\times 10^{18}$ eV arriving within an angular separation of approximately 15$^{\\circ }$ . We characterize the energy distributions inside these regions by two independent methods, one searching for angular dependence of energy-energy correlations and one searching for collimation of energy along the local system of principal axes of the energy distribution. No significant patterns aremore »found with this analysis. As a result, the comparison of these measurements with astrophysical scenarios can therefore be used to obtain constraints on related model parameters such as strength of cosmic-ray deflection and density of point sources.« less

  9. SNO Data: Results from Experiments at the Sudbury Neutrino Observatory

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

    The Sudbury Neutrino Observatory (SNO) was built 6800 feet under ground, in INCO's Creighton mine near Sudbury, Ontario. SNO is a heavy-water Cherenkov detector that is designed to detect neutrinos produced by fusion reactions in the sun. It uses 1000 tonnes of heavy water, on loan from Atomic Energy of Canada Limited (AECL), contained in a 12 meter diameter acrylic vessel. Neutrinos react with the heavy water (D2O) to produce flashes of light called Cherenkov radiation. This light is then detected by an array of 9600 photomultiplier tubes mounted on a geodesic support structure surrounding the heavy water vessel. The detector is immersed in light (normal) water within a 30 meter barrel-shaped cavity (the size of a 10 story building!) excavated from Norite rock. Located in the deepest part of the mine, the overburden of rock shields the detector from cosmic rays. The detector laboratory is extremely clean to reduce background signals from radioactive elements present in the mine dust which would otherwise hide the very weak signal from neutrinos. (From http://www.sno.phy.queensu.ca/]

    The SNO website provides access to various datasets. See also the SNO Image Catalog at http://www.sno.phy.queensu.ca/sno/images/ and computer-generated images of SNO events at http://www.sno.phy.queensu.ca/sno/events/ and the list of published papers.

  10. Astrophysics Motivation behind the Pierre Auger Southern Observatory Enhancements

    E-Print Network [OSTI]

    Gustavo Medina-Tanco; for the Pierre Auger Collaboration

    2007-09-06

    The Pierre Auger Collaboration intends to extend the energy range of its southern observatory in Argentina for high quality data from 0.1 to 3 EeV. The extensions, described in accompanying papers, include three additional fluorescence telescopes with a more elevated field of view (HEAT) and a nested surface array with 750 and 433 m spacing respectively and additional muon detection capabilities (AMIGA). The enhancement of the detector will allow measurement of cosmic rays, using the same techniques, from below the second knee up to the highest energies observed. The evolution of the spectrum through the second knee and ankle, and corresponding predicted changes in composition, are crucial to the understanding of the end of Galactic confinement and the effects of propagation on the lower energy portion of the extragalactic flux. The latter is strongly related to the cosmological distribution of sources and to the composition of the injected spectrum. We discuss the science motivation behind these enhancements as well as the impact of combined HEAT and AMIGA information on the assessment of shower simulations and reconstruction techniques.

  11. LOFT: the Large Observatory For X-ray Timing

    E-Print Network [OSTI]

    Belloni, Tomaso M

    2012-01-01

    LOFT, the large observatory for X-ray timing, is a new mission concept competing with other four candidates for a launch opportunity in 2022-2024. LOFT will be performing high-time resolution X-ray observations of compact objects, combining for the first time an unprecedented large collecting area for X-ray photons and a spectral resolution approaching that of CCD-based X-ray instruments (down to 200 eV FWHM at 6 keV). The operating energy range is 2-80 keV. The main science goals of LOFT are the measurement of the neutron stars equation of states and the test of General Relativity in the strong field regime. The breakthrough capabilities of the instruments on-board LOFT will permit to open also new discovery windows for a wide range of Galactic and extragalactic X-ray sources. In this contribution, we provide a general description of the mission concept and summarize its main scientific capabilities.

  12. Conceptual Design of the International Axion Observatory (IAXO)

    E-Print Network [OSTI]

    Armengaud, E; Betz, M; Brax, P; Brun, P; Cantatore, G; Carmona, J M; Carosi, G P; Caspers, F; Caspi, S; Cetin, S A; Chelouche, D; Christensen, F E; Dael, A; Dafni, T; Davenport, M; Derbin, A V; Desch, K; Diago, A; Döbrich, B; Dratchnev, I; Dudarev, A; Eleftheriadis, C; Fanourakis, G; Ferrer-Ribas, E; Galán, J; García, J A; Garza, J G; Geralis, T; Gimeno, B; Giomataris, I; Gninenko, S; Gómez, H; González-Díaz, D; Guendelman, E; Hailey, C J; Hiramatsu, T; Hoffmann, D H H; Horns, D; Iguaz, F J; Irastorza, I G; Isern, J; Imai, K; Jakobsen, A C; Jaeckel, J; Jakov?i?, K; Kaminski, J; Kawasaki, M; Karuza, M; Kr?mar, M; Kousouris, K; Krieger, C; Laki?, B; Limousin, O; Lindner, A; Liolios, A; Luzón, G; Matsuki, S; Muratova, V N; Nones, C; Ortega, I; Papaevangelou, T; Pivovaroff, M J; Raffelt, G; Redondo, J; Ringwald, A; Russenschuck, S; Ruz, J; Saikawa, K; Savvidis, I; Sekiguchi, T; Semertzidis, Y K; Shilon, I; Sikivie, P; Silva, H; Kate, H ten; Tomas, A; Troitsky, S; Vafeiadis, T; Bibber, K van; Vedrine, P; Villar, J A; Vogel, J K; Walckiers, L; Weltman, A; Wester, W; Yildiz, S C; Zioutas, K

    2014-01-01

    The International Axion Observatory (IAXO) will be a forth generation axion helioscope. As its primary physics goal, IAXO will look for axions or axion-like particles (ALPs) originating in the Sun via the Primakoff conversion of the solar plasma photons. In terms of signal-to-noise ratio, IAXO will be about 4-5 orders of magnitude more sensitive than CAST, currently the most powerful axion helioscope, reaching sensitivity to axion-photon couplings down to a few $\\times 10^{-12}$ GeV$^{-1}$ and thus probing a large fraction of the currently unexplored axion and ALP parameter space. IAXO will also be sensitive to solar axions produced by mechanisms mediated by the axion-electron coupling $g_{ae}$ with sensitivity $-$for the first time$-$ to values of $g_{ae}$ not previously excluded by astrophysics. With several other possible physics cases, IAXO has the potential to serve as a multi-purpose facility for generic axion and ALP research in the next decade. In this paper we present the conceptual design of IAXO, w...

  13. The Fourth US Naval Observatory CCD Astrograph Catalog (UCAC4)

    E-Print Network [OSTI]

    Zacharias, Norbert; Girard, Terry; Henden, Arne; Bartlett, Jennifer; Monet, Dave; Zacharias, Marion

    2012-01-01

    The fourth United States Naval Observatory (USNO) CCD Astrograph Catalog, UCAC4 was released in August 2012 (double-sided DVD and CDS data center Vizier catalog I/322). It is the final release in this series and contains over 113 million objects; over 105 million of them with proper motions. UCAC4 is an updated version of UCAC3 with about the same number of stars also covering all-sky. Bugs were fixed, Schmidt plate survey data were avoided, and precise 5-band photometry were added. Astrograph observations have been supplemented for bright stars by FK6, Hipparcos and Tycho-2 data to compile a UCAC4 star catalog complete to about magnitude R = 16. Epoch 1998 to 2004 positions are obtained from observations with the 20 cm aperture USNO Astrograph's red lens, equipped with a 4k by 4k CCD. Mean positions and proper motions are derived by combining these observations with over 140 ground- and space-based catalogs, including Hipparcos/Tycho and the AC2000.2, as well as unpublished measures of over 5000 plates from ...

  14. Japanese Virtual Observatory (JVO) as an advanced astronomical research enviroment

    E-Print Network [OSTI]

    Y. Shirasaki; M. Tanaka; S. Kawanomoto; S. Honda; M. Ohishi; Y. Mizumoto; N. Yasuda; Y. Masunaga; Y. Ishihara; J. Tsutsumi; H. Nakamoto; Y. Kobayashi; M. Sakamoto

    2006-04-28

    We present the design and implementation of the Japanese Virtual Observatory (JVO) system. JVO is a portal site to various kinds of astronomical resources distributed all over the world. We have developed five components for constructing the portal: (1) registry, (2) data service, (3) workflow system, (4) data analysis service (5) portal GUI. Registry services are used for publishing and searching data services in the VO, and they are constructed using an OAI-PMH metadata harvesting protocol and a SOAP web service protocol so that VO standard architecture is applied. Data services are developed based on the Astronomical Data Query Language (ADQL) which is an international VO standard and an extension of the standard SQL. The toolkit for building the ADQL-based service is released to the public on the JVO web site. The toolkit also provides the protocol translation from a Simple Image Access Protocol (SIAP) to ADQL protocol, so that both the VO standard service can be constructed using our toolkit. In order to federate the distributed databases and analysis services, we have designed a workflow language which is described in XML and developed execution system of the workflow. We have succeeded to connect to a hundred of data resources of the world as of April 2006. We have applied this system to the study of QSO environment by federating a QSO database, a Subaru Suprim-Cam database, and some analysis services such a SExtractor and HyperZ web services. These experiences are described is this paper.

  15. Was Lepenski Vir an ancient Sun or Pleiades observatory?

    E-Print Network [OSTI]

    Pankovic, Vladan; Krmar, Miodrag

    2015-01-01

    In this work we consider some old hypotheses according to which remarkable mesolithic village Lepenski Vir (9500 -- 5500 BC) at the right (nearly west) Danube riverside in the Iron gate in Serbia was an ancient (one of the oldest) Sun observatory. We use method recently suggested by A. C. Sparavigna, concretely we use "freely available software" or local Sun radiation direction simulation computer programs. In this way we obtain and discuss pictures of the sunrise in the Lepenski Vir during winter and summer solstice and spring and autumn equinox in relation to position of the mountains, especially Treskavac (Trescovat) and Kukuvija at left (nearly east) Danube riverside (in Romania). While mountain Kukuvija represents really the marker for the Sun in date of the winter solstice, mountain Treskavac, in despite to usual opinions, does not represent a real marker for the Sun in date of the summer solstice. Sun rises behind Treskavac, roughly speaking, between 22.April and 1. May. It corresponds to year period w...

  16. SPECKLE INTERFEROMETRY AT THE U.S. NAVAL OBSERVATORY. XVI

    SciTech Connect (OSTI)

    Mason, Brian D.; Hartkopf, William I.; Wycoff, Gary L. E-mail: wih@usno.navy.mil

    2011-05-15

    The results of 1031 speckle-interferometric observations of double stars, made with the 26 inch refractor of the U.S. Naval Observatory, are presented. Each speckle-interferometric observation of a system represents a combination of over two thousand short-exposure images. These observations are averaged into 457 mean relative positions and range in separation from 0.''15 to 16.''94, with a median separation of 3.''03. The range in V-band magnitudes for the primary (secondary) of observed targets is 3.1-12.9 (3.2-13.3). This is the sixteenth in a series of papers presenting measurements obtained with this system and covers the period 2009 January 12 through 2009 December 17. Included in these data are 12 older measurements whose positions were previously deemed possibly aberrant, but are no longer classified this way following a confirming observation. Also, 10 pairs with a single observation are herein confirmed. This paper also includes the first data obtained using a new ICCD with fiber optic cables.

  17. The Final Results from the Sudbury Neutrino Observatory

    ScienceCinema (OSTI)

    None

    2011-04-25

    The Sudbury Neutrino Observatory (SNO) was a water Cherenkov detector dedicated to investigate elementary particles called neutrinos. It successfully took data between 1999 and 2006. The detector was unique in its use of heavy water as a detection medium, permitting it to make a solar model-independent test of solar neutrino mixing. In fact, SNO conclusively showed that solar neutrinos oscillate on their way from the core of the Sun to the Earth. This groundbreaking observation was made during three independent phases of the experiment. Even if data taking ended, SNO is still in a mode of precise determination of the solar neutrino oscillation parameters because all along SNO had developed several methods to tell charged-current events apart from neutral-current events. This ability is crucial for the final and ultimate data analysis of all the phases. The physics reach of a combined three-phase solar analysis will be reviewed together with results and subtleties about solar neutrino physics.

  18. Preliminary systems engineering evaluations for the National Ecological Observatory Network.

    SciTech Connect (OSTI)

    Robertson, Perry J.; Kottenstette, Richard Joseph; Crouch, Shannon M.; Brocato, Robert Wesley; Zak, Bernard Daniel; Osborn, Thor D.; Ivey, Mark D.; Gass, Karl Leslie; Heller, Edwin J.; Dishman, James Larry; Schubert, William Kent; Zirzow, Jeffrey A.

    2008-11-01

    The National Ecological Observatory Network (NEON) is an ambitious National Science Foundation sponsored project intended to accumulate and disseminate ecologically informative sensor data from sites among 20 distinct biomes found within the United States and Puerto Rico over a period of at least 30 years. These data are expected to provide valuable insights into the ecological impacts of climate change, land-use change, and invasive species in these various biomes, and thereby provide a scientific foundation for the decisions of future national, regional, and local policy makers. NEON's objectives are of substantial national and international importance, yet they must be achieved with limited resources. Sandia National Laboratories was therefore contracted to examine four areas of significant systems engineering concern; specifically, alternatives to commercial electrical utility power for remote operations, approaches to data acquisition and local data handling, protocols for secure long-distance data transmission, and processes and procedures for the introduction of new instruments and continuous improvement of the sensor network. The results of these preliminary systems engineering evaluations are presented, with a series of recommendations intended to optimize the efficiency and probability of long-term success for the NEON enterprise.

  19. Highlights from the High Altitude Water Cherenkov Observatory

    E-Print Network [OSTI]

    Pretz, John

    2015-01-01

    The High Altitude Water Cherenkov (HAWC) Gamma-Ray Observatory was completed this year at a 4100-meter site on the flank of the Sierra Negra volcano in Mexico. HAWC is a water Cherenkov ground array with the capability to distinguish 100 GeV - 100 TeV gamma rays from the hadronic cosmic-ray background. HAWC is uniquely suited to study extremely high energy cosmic-ray sources, search for regions of extended gamma-ray emission, and to identify transient gamma-ray phenomena. HAWC will play a key role in triggering multi-wavelength and multi-messenger studies of active galaxies, gamma-ray bursts, supernova remnants and pulsar wind nebulae. Observation of TeV photons also provide unique tests for a number of fundamental physics phenomena including dark matter annihilation and primordial black hole evaporation. Operation began mid-2013 with the partially-completed detector. Multi-TeV emission from the Galactic Plane is clearly seen in the first year of operation, confirming a number of known TeV sources, and a numb...

  20. Relative Photometry with data from the Peter van de Kamp Observatory D. Cohen and E. Jensen

    E-Print Network [OSTI]

    Cohen, David

    Relative Photometry with data from the Peter van de Kamp Observatory D with those reduced images. While in principle, we could "do photometry on" some can download the data: http://astro.swarthmore.edu/~cohen/telescope/sample_photometry

  1. A measurement of the atmospheric neutrino flux and oscillation parameters at the Sudbury Neutrino Observatory

    E-Print Network [OSTI]

    Sonley, Thomas John

    2009-01-01

    Through-going muon events are analyzed as a function of their direction of travel through the Sudbury Neutrino Observatory. Based on simulations and previous measurements, muons with a zenith angle of 1 < cos([theta]zenith) ...

  2. Impact of the Geo-synchronous Orbit Radiation Environment on the Design of Astronomical Observatories

    E-Print Network [OSTI]

    Kruk, Jeffrey W; Armani, Nerses; Stauffer, Craig; Hirata, Christopher M

    2015-01-01

    Geo-Synchronous orbits are appealing for Solar or astrophysical observatories because they permit continuous data downlink at high rates. The radiation environment in these orbits presents unique challenges, however. This paper describes the characteristics of the radiation environment in Geo-Synchronous orbit and the implications for instrument design. Radiation-induced background event rates are given for some simplified shielding models, and for a detailed model of the proposed Wide-Field InfraRed Survey Telescope observatory.

  3. Search for Ultra-High Energy Photons with the Pierre Auger Observatory

    E-Print Network [OSTI]

    M. D. Healy; for the Pierre Auger Collaboration

    2007-09-28

    Data taken at the Pierre Auger Observatory are used to search for air showers initiated by ultra-high energy (UHE) photons. Results of searches are reported from hybrid observations where events are measured with both fluorescence and array detectors. Additionally, a more stringent test of the photon fluxes predicted with energies above 10^19 eV is made using a larger data set measured using only the surface detectors of the observatory.

  4. Light pollution at the Roque de los Muchachos Observatory

    E-Print Network [OSTI]

    M. Pedani

    2004-07-06

    Sky spectra were obtained from archival science frames taken with DoLoRes at the 3.58m Telescopio Nazionale Galileo with a wavelength range ~3800 - 8000Ang and resolution of 2.8Ang/pix and 3.6Ang/pix. Our spectra include all the important Sodium and Mercury light pollution lines and span a wide interval of azimuth and observing conditions, essential to disentangle environmental and seasonal effects. New sodium and mercury lines were also detected for the first time at the observatory. Light pollution from NaD_{5892-8} emitted by the LPS lamps increased by a factor of 1.5 - 2 with respect to the average values of 1998. At the same time, light pollution from Hg lines decreased by ~40% and reaches the 1998 levels only when observing toward the towns. The contribution of NaD_{5892-8} from LPS lamps to sky background is 0.05-0.10mag at V-band and 0.07-0.12mag at R-band. Synthetic sky brightness measures calculated from our spectra at V, B and R bands are in good agreement with those of Benn & Ellison(1998) if we take into account that our observations were done during 2003, seven years after the last sunspot minimum. The effects of the application of the Canary Sky Law are directly visible in the spectra as a 50% dimming of the Hg light-polluting lines in the spectra taken after local midnight.

  5. INSIGHTS INTO FILAMENT ERUPTION ONSET FROM SOLAR DYNAMICS OBSERVATORY OBSERVATIONS

    SciTech Connect (OSTI)

    Sterling, Alphonse C.; Moore, Ronald L.; Freeland, Samuel L. E-mail: ron.moore@nasa.gov

    2011-04-10

    We examine the buildup to and onset of an active region filament confined eruption of 2010 May 12, using EUV imaging data from the Solar Dynamics Observatory (SDO) Atmospheric Imaging Array and line-of-sight magnetic data from the SDO Helioseismic and Magnetic Imager. Over the hour preceding eruption the filament undergoes a slow rise averaging {approx}3 km s{sup -1}, with a step-like trajectory. Accompanying a final rise step {approx}20 minutes prior to eruption is a transient preflare brightening, occurring on loops rooted near the site where magnetic field had canceled over the previous 20 hr. Flow-type motions of the filament are relatively smooth with speeds {approx}50 km s{sup -1} prior to the preflare brightening and appear more helical, with speeds {approx}50-100 km s{sup -1}, after that brightening. After a final plateau in the filament's rise, its rapid eruption begins, and concurrently an outer shell 'cocoon' of the filament material increases in emission in hot EUV lines, consistent with heating in a newly formed magnetic flux rope. The main flare brightenings start {approx}5 minutes after eruption onset. The main flare arcade begins between the legs of an envelope-arcade loop that is nearly orthogonal to the filament, suggesting that the flare results from reconnection among the legs of that loop. This progress of events is broadly consistent with flux cancellation leading to formation of a helical flux rope that subsequently erupts due to onset of a magnetic instability and/or runaway tether cutting.

  6. NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia

    E-Print Network [OSTI]

    Groppi, Christopher

    and tested in the lab. Measurements on Tunnel Diode Amplifier, Novrnt?,er_14, 1962 The noise temperature was also measured. A minimum occurred at 105 my (measured at the test point), the voltage recommended be disconnected at the relay chassis and a cable clamp mounted behind the chassis must be re- moved also) Switch

  7. ARM - Point Reyes News

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

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity ofkandz-cm11 Comments?govInstrumentsnoaacrnBarrow, Alaska OutreachCalendar NSAProductsMergedProductsVaisala CL51CaliforniaPoint

  8. THE FOURTH US NAVAL OBSERVATORY CCD ASTROGRAPH CATALOG (UCAC4)

    SciTech Connect (OSTI)

    Zacharias, N.; Finch, C. T.; Bartlett, J. L.; Girard, T. M.; Henden, A.; Monet, D. G.; Zacharias, M. I.

    2013-02-01

    The fourth United States Naval Observatory (USNO) CCD Astrograph Catalog, UCAC4, was released in 2012 August (double-sided DVD and CDS data center Vizier catalog I/322). It is the final release in this series and contains over 113 million objects; over 105 million of them with proper motions (PMs). UCAC4 is an updated version of UCAC3 with about the same number of stars also covering all-sky. Bugs were fixed, Schmidt plate survey data were avoided, and precise five-band photometry was added for about half the stars. Astrograph observations have been supplemented for bright stars by FK6, Hipparcos, and Tycho-2 data to compile a UCAC4 star catalog complete from the brightest stars to about magnitude R = 16. Epoch 1998-2004 positions are obtained from observations with the 20 cm aperture USNO Astrograph's 'red lens', equipped with a 4k by 4k CCD. Mean positions and PMs are derived by combining these observations with over 140 ground- and space-based catalogs, including Hipparcos/Tycho and the AC2000.2, as well as unpublished measures of over 5000 plates from other astrographs. For most of the faint stars in the southern hemisphere, the first epoch plates from the Southern Proper Motion program form the basis for PMs, while the Northern Proper Motion first epoch plates serve the same purpose for the rest of the sky. These data are supplemented by 2MASS near-IR photometry for about 110 million stars and five-band (B, V, g, r, i) APASS data for over 51 million stars. Thus the published UCAC4, as were UCAC3 and UCAC2, is a compiled catalog with the UCAC observational program being a major component. The positional accuracy of stars in UCAC4 at mean epoch is about 15-100 mas per coordinate, depending on magnitude, while the formal errors in PMs range from about 1 to 10 mas yr{sup -1} depending on magnitude and observing history. Systematic errors in PMs are estimated to be about 1-4 mas yr{sup -1}.

  9. Description of Atmospheric Conditions at the Pierre Auger Observatory using the Global Data Assimilation System (GDAS)

    SciTech Connect (OSTI)

    Abreu, P.; Aglietta, M.; Ahlers, M.; Ahn, E.J.; Albuquerque, I.F.M.; Allard, D.; Allekotte, I.; Allen, J.; Allison, P.; Almela, A.; Alvarez Castillo, J.; /Mexico U., ICN /Santiago de Compostela U.

    2012-01-01

    Atmospheric conditions at the site of a cosmic ray observatory must be known for reconstructing observed extensive air showers. The Global Data Assimilation System (GDAS) is a global atmospheric model predicated on meteorological measurements and numerical weather predictions. GDAS provides altitude-dependent profiles of the main state variables of the atmosphere like temperature, pressure, and humidity. The original data and their application to the air shower reconstruction of the Pierre Auger Observatory are described. By comparisons with radiosonde and weather station measurements obtained on-site in Malargue and averaged monthly models, the utility of the GDAS data is shown.

  10. LamontDoherty Earth Observatory The Earth Institute at Columbia UniversityThe Earth Institute at Columbia Univ

    E-Print Network [OSTI]

    12 12 Lamont­Doherty Earth Observatory The Earth Institute at Columbia UniversityThe Earth-DOHERTYEARTHOBSERVATORYTHEEARTHINSTITUTEATCOLUMBIAUNIVERSITYBIENNIALREPORT2000­2002 #12;Lamont-Doherty Earth Observatory is renowned in the internationLamont-Doherty Earth suc- cess and innovation in advancing understanding of Earth, for itcess and innovation in advancing

  11. Generation region of pulsating aurora obtained simultaneously by the FAST satellite and a Syowa-Iceland conjugate pair of observatories

    E-Print Network [OSTI]

    California at Berkeley, University of

    Generation region of pulsating aurora obtained simultaneously by the FAST satellite and a Syowa-Iceland), with reference to simultaneous data obtained by a Syowa-Iceland conjugate pair of observatories. The aurora simultaneously by the FAST satellite and a Syowa-Iceland conjugate pair of observatories, J. Geophys. Res., 109

  12. Progress on the 1.6-meter New Solar Telescope at Big Bear Solar Observatory

    E-Print Network [OSTI]

    of the drivers for building solar telescopes with large apertures. Recent advances in adaptive optics (AO) make it possible to build solar telescopes in an open configuration and thus go beyond the conventional meterProgress on the 1.6-meter New Solar Telescope at Big Bear Solar Observatory C. Denkera, P. R

  13. Shanghai Astronomical Observatory, China email: youfenwang@shao.ac.cn University Of Hertfordshire, UK

    E-Print Network [OSTI]

    Joergens, Viki

    Youfen Wang , Hugh Jones, Ricky Smart, Federico Marocco, Zhengyi Shao et al. 1. Introduction Most L is a useful bridge between studies of stars and planets. Parallaxes are a model independent parameter that can use the methods adopted in the Torino Observatory Parallax Program (Smart et al. 2003, 2007

  14. The Armagh Observatory was founded and endowed by Archbishop Richard Robinson, who wished to establish

    E-Print Network [OSTI]

    . Richard Robinson was born in 1708 into a high society Yorkshire family. He was educated at Westminster of Armagh Observatory. This was to be his last completed building in Armagh. Architecture and Grounds of Culture, Arts and Leisure, while the Science and Technology Facilities Council supports individual

  15. The Thermal Control of the New Solar Telescope at Big Bear Observatory

    E-Print Network [OSTI]

    For large-diameter solar telescopes operating at the theoretical diffraction limit, one of the main designThe Thermal Control of the New Solar Telescope at Big Bear Observatory Angelo P. Verdonia and Carsten Denkera aNew Jersey Institute of Technology, Center for Solar-Terrestrial Research, 323 Martin

  16. PRELIMINARY PARALLAXES OF 40 L AND T DWARFS FROM THE US NAVAL OBSERVATORY INFRARED ASTROMETRY PROGRAM

    E-Print Network [OSTI]

    Golimowski, David A.

    Observatory, Flagstaff Station, P.O. Box 1149, Flagstaff, AZ 86002; fjv@nofs.navy.mil, aah@nofs.navy.mil, cbl@nofs.navy.mil, guetter@nofs.navy.mil, jam@nofs.navy.mil, blaise@nofs.navy.mil A. J. Burgasser2 Division of Astronomy

  17. Results from the Milagro Gamma-Ray Observatory E. Blaufuss a

    E-Print Network [OSTI]

    California at Santa Cruz, University of

    V emission from the galactic plane, and a search for transient emission above 100 GeV from gamma ray bursts- clei (AGN), supernova remnants and gamma-ray bursts (GRB). Gamma rays are also produced when high1 Results from the Milagro Gamma-Ray Observatory E. Blaufuss a for the Milagro Collaboration

  18. The Armagh Observatory was founded and endowed by Archbishop Richard Robinson, who wished to establish

    E-Print Network [OSTI]

    interests lie in solar system astronomy and the dynamics of bodies such as comets and asteroids, the Sun, the solar system, and solar-system -- terrestrial relationships. The Observatory is one of the UK and Ireland's leading astronomical research institutes. Basic operational costs are borne by the Department

  19. The Astrophysical Multimessenger Observatory Network (AMON) M.W.E. Smith a,b,

    E-Print Network [OSTI]

    Babu, G. Jogesh

    Gravitational radiation Neutrinos Cosmic rays Gamma-ray bursts Supernovae a b s t r a c t We summarize including the Swift [6] and Fermi [7] satellites, the HESS [8], VERITAS [9], and MAGIC [10] TeV gamma-ray telescopes, and the HAWC [11] TeV gamma-ray observatory. Collectively, these facilities promise the first

  20. Estimating concentrations of heat producing elements in the crust near the Sudbury Neutrino Observatory, Ontario, Canada

    E-Print Network [OSTI]

    Observatory, Ontario, Canada Catherine Phaneuf, Jean-Claude Mareschal GEOTOP, University of Quebec at Montreal, Montreal, QC, Canada a b s t r a c ta r t i c l e i n f o Article history: Received 1 August 2013 in the Creighton Mine, near Sudbury, Ontario. The facility has been upgraded and a new kiloton scale liquid

  1. Beyond the Second Generation of Laser-Interferometric Gravitational Wave Observatories

    E-Print Network [OSTI]

    Stefan Hild

    2011-11-27

    This article gives an overview of potential upgrades of second generation gravitational wave detectors and the required key technologies to improve the limiting noise sources. In addition the baseline design of the Einstein Telescope, a European third generation gravitational wave observatory, is briefly discussed.

  2. Soil CO2 production and surface flux at four climate observatories in eastern Canada

    E-Print Network [OSTI]

    Beltrami, Hugo

    Soil CO2 production and surface flux at four climate observatories in eastern Canada David Risk December 2002. [1] Soils constitute the largest terrestrial source of carbon dioxide to the atmosphere the climatic controls on soil respiration. We use subsurface CO2 concentrations, surface CO2 flux and detailed

  3. The Observer April 2003 page 3 Adaptive Optics Available at CSU Fresno Observatory

    E-Print Network [OSTI]

    Ringwald, Frederick A.

    The Observer April 2003 page 3 Adaptive Optics Available at CSU Fresno Observatory By Greg Morgan-tilt mirror continually adjusts the telescopes light cone to hold a guide star on a designated pixel an AO-7 adaptive optics device. It is just one of the many state-of-the-art instruments available

  4. Why are we still studying cosmic rays? Pierre Auger Observatory: past, present, future

    E-Print Network [OSTI]

    higher than the Calculated Chance Rate ­ even when the counters were as far as 300 m apart. #12;Large GM;photomultiplier Steel tank Cherenkov Light emission in water 41° When a particle travels faster than the velocity Auger Project A new cosmic ray observatory designed for a high statistics study of the The Highest

  5. A Wireless Internet-Based Observatory: The Real-time Coastal Observation Network

    E-Print Network [OSTI]

    A Wireless Internet-Based Observatory: The Real-time Coastal Observation Network (ReCON) S. A community and educational institutions through the internet. A real-time database management system provides to the success of regional coastal ocean observing systems. The pervasiveness of wireless internet technology

  6. High-energy Atmospheric Muon Flux Expected at India-Based Neutrino Observatory

    E-Print Network [OSTI]

    Sukanta Panda; Sergei I. Sinegovsky

    2008-02-04

    We calculate the zenith-angle dependence of conventional and prompt high-energy muon fluxes at India-Based Neutrino Observatory (INO) depth. This study demonstrates a possibility to discriminate models of the charm hadroproduction including the low-x QCD behaviour of hadronic cross-sections relevant at very high energies.

  7. Building a new space weather facility at the National Observatory Ioannis Kontogiannis

    E-Print Network [OSTI]

    Anastasiadis, Anastasios

    Building a new space weather facility at the National Observatory of Athens Ioannis Kontogiannis) the operation of a small full-disk solar telescope to conduct regular observations of the Sun in the H of solar wind, and affecting the near- Earth space environment in numerous ways. Both flares and CMEs

  8. Spectroscopy of low energy solar neutrinos by MOON -Mo Observatory Of Neutrinos-

    E-Print Network [OSTI]

    Washington at Seattle, University of

    Spectroscopy of low energy solar neutrinos by MOON -Mo Observatory Of Neutrinos- R. Hazamaa , P Be solar 's. The present status of MOON for the low energy solar experiment is briefly discussed the pp solar flux with good accuracy. 1. INTRODUCTION Realtime studies of the high-energy component of 8

  9. Prospects for and Status of CUORE ? The Cryogenic Underground Observatory for Rare Events

    SciTech Connect (OSTI)

    Norman, E B

    2009-07-07

    CUORE (Cryogenic Underground Observatory for Rare Events) is a next generation experiment designed to search for the neutrinoless DBD of {sup 130}Te using a bolometric technique. The present status of the CUORE is presented along with the latest results from its prototype, CUORICINO.

  10. Ground-based observations of Kepler asteroseismic targets

    E-Print Network [OSTI]

    Uytterhoeven, K; Southworth, J; Randall, S; Ostensen, R; Molenda-Zakowicz, J; Marconi, M; Kurtz, D W; Kiss, L; Gutierrez-Soto, J; Frandsen, S; De Cat, P; Bruntt, H; Briquet, M; Zhang, X B; Telting, J H; Steslicki, M; Ripepi, V; Pigulski, A; Paparo, M; Oreiro, R; Choong, Ngeow Chow; Niemczura, E; Nemec, J; Narwid, A; Mathias, P; Martin-Ruiz, S; Lehman, H; Kopacki, G; Karoff, C; Jackiewicz, J; Henden, A A; Handler, G; Grigachene, A; Green, E M; Garrido, R; Machado, L Fox; Debosscher, J; Creevey, O L; Catanzaro, G; Bognar, Z; Biazzo, K; Bernabei, S

    2010-01-01

    We present the ground-based activities within the different working groups of the Kepler Asteroseismic Science Consortium (KASC). The activities aim at the systematic characterization of the 5000+ KASC targets, and at the collection of ground-based follow-up time-series data of selected promising Kepler pulsators. So far, 35 different instruments at 30 telescopes on 22 different observatories in 12 countries are in use, and a total of more than 530 observing nights has been awarded. (Based on observations made with the Isaac Newton Telescope, William Herschel Telescope, Nordic Optical Telescope, Telescopio Nazionale Galileo, Mercator Telescope (La Palma, Spain), and IAC-80 (Tenerife, Spain). Also based on observations taken at the observatories of Sierra Nevada, San Pedro Martir, Vienna, Xinglong, Apache Point, Lulin, Tautenburg, Loiano, Serra la Nave, Asiago, McDonald, Skinakas, Pic du Midi, Mauna Kea, Steward Observatory, Bialkow Observatory of the Wroclaw University, Piszkesteto Mountain Station, Observato...

  11. Florida Nuclear Profile - Turkey Point

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

    Turkey Point" "Unit","Summer capacity (mw)","Net generation (thousand mwh)","Summer capacity factor (percent)","Type","Commercial operation date","License expiration date"...

  12. Day-night asymmetry of high and low energy solar neutrino events in Super-Kamiokande and in the Sudbury Neutrino Observatory

    E-Print Network [OSTI]

    G. L. Fogli; E. Lisi; D. Montanino; A. Palazzo

    2000-09-19

    In the context of solar neutrino oscillations among active states, we briefly discuss the current likelihood of Mikheyev-Smirnov-Wolfenstein (MSW) solutions to the solar neutrino problem, which appear to be currently favored at large mixing, where small Earth regeneration effects might still be observable in Super-Kamiokande (SK) and in the Sudbury Neutrino Observatory (SNO). We point out that, since such effects are larger at high (low) solar neutrino energies for high (low) values of the mass square difference \\delta m^2, it may be useful to split the night-day rate asymmetry in two separate energy ranges. We show that the difference \\Delta of the night-day asymmetry at high and low energy may help to discriminate the two large-mixing solutions at low and high \\delta m^2 through a sign test, both in SK and in SNO, provided that the sensitivity to \\Delta can reach the (sub)percent level.

  13. 3rd International Workshop on Scientific Use of Submarine Cables and Related Technologies, 25-27 June 2003, Tokyo, Japan Physical Oceanography from Deep Ocean Submarine Cable Observatories

    E-Print Network [OSTI]

    Luther, Douglas S.

    -27 June 2003, Tokyo, Japan Physical Oceanography from Deep Ocean Submarine Cable Observatories Douglas S. LUTHER Department of Oceanography, University of Hawaii KEYWORDS: Physical Oceanography, Observatories" are reviewed. Perhaps the more important role for observatories in physical oceanography may be the provision

  14. Adaptive optics system for the IRSOL solar observatory Renzo Ramellia, Roberto Bucherb, Leopoldo Rossinia,b,c, Michele Biandaa, Silvano Balemib

    E-Print Network [OSTI]

    a low cost adaptive optics system developed for the solar observatory at Istituto Ricerche SolariAdaptive optics system for the IRSOL solar observatory Renzo Ramellia, Roberto Bucherb, Leopoldo The solar observatory at Istituto Ricerche Solari Locarno (IRSOL) focuses its activity on precise

  15. A search for point sources of EeV photons

    SciTech Connect (OSTI)

    Aab, A.; Abreu, P.; Andringa, S.; Aglietta, M.; Ahlers, M.; Ahn, E. J.; Al Samarai, I.; Albuquerque, I. F. M.; Allekotte, I.; Allen, J.; Allison, P.; Almela, A.; Castillo, J. Alvarez; Alvarez-Muñiz, J.; Batista, R. Alves; Ambrosio, M.; Aramo, C.; Aminaei, A.; Anchordoqui, L.; Arqueros, F.; Collaboration: Pierre Auger Collaboration102; and others

    2014-07-10

    Measurements of air showers made using the hybrid technique developed with the fluorescence and surface detectors of the Pierre Auger Observatory allow a sensitive search for point sources of EeV photons anywhere in the exposed sky. A multivariate analysis reduces the background of hadronic cosmic rays. The search is sensitive to a declination band from –85° to +20°, in an energy range from 10{sup 17.3} eV to 10{sup 18.5} eV. No photon point source has been detected. An upper limit on the photon flux has been derived for every direction. The mean value of the energy flux limit that results from this, assuming a photon spectral index of –2, is 0.06 eV cm{sup –2} s{sup –1}, and no celestial direction exceeds 0.25 eV cm{sup –2} s{sup –1}. These upper limits constrain scenarios in which EeV cosmic ray protons are emitted by non-transient sources in the Galaxy.

  16. Reconstruction of inclined air showers detected with the Pierre Auger Observatory

    E-Print Network [OSTI]

    The Pierre Auger Collaboration; A. Aab; P. Abreu; M. Aglietta; M. Ahlers; E. J. Ahn; I. Al Samarai; I. F. M. Albuquerque; I. Allekotte; J. Allen; P. Allison; A. Almela; J. Alvarez Castillo; J. Alvarez-Muñiz; R. Alves Batista; M. Ambrosio; A. Aminaei; L. Anchordoqui; S. Andringa; C. Aramo; F. Arqueros; H. Asorey; P. Assis; J. Aublin; M. Ave; M. Avenier; G. Avila; A. M. Badescu; K. B. Barber; J. Bäuml; C. Baus; J. J. Beatty; K. H. Becker; J. A. Bellido; C. Berat; X. Bertou; P. L. Biermann; P. Billoir; F. Blanco; M. Blanco; C. Bleve; H. Blümer; M. Bohá?ová; D. Boncioli; C. Bonifazi; R. Bonino; N. Borodai; J. Brack; I. Brancus; P. Brogueira; W. C. Brown; P. Buchholz; A. Bueno; M. Buscemi; K. S. Caballero-Mora; B. Caccianiga; L. Caccianiga; M. Candusso; L. Caramete; R. Caruso; A. Castellina; G. Cataldi; L. Cazon; R. Cester; A. G. Chavez; S. H. Cheng; A. Chiavassa; J. A. Chinellato; J. Chudoba; M. Cilmo; R. W. Clay; G. Cocciolo; R. Colalillo; L. Collica; M. R. Coluccia; R. Conceição; F. Contreras; M. J. Cooper; S. Coutu; C. E. Covault; A. Criss; J. Cronin; A. Curutiu; R. Dallier; B. Daniel; S. Dasso; K. Daumiller; B. R. Dawson; R. M. de Almeida; M. De Domenico; S. J. de Jong; J. R. T. de Mello Neto; I. De Mitri; J. de Oliveira; V. de Souza; L. del Peral; O. Deligny; H. Dembinski; N. Dhital; C. Di Giulio; A. Di Matteo; J. C. Diaz; M. L. D\\'\\iaz Castro; P. N. Diep; F. Diogo; C. Dobrigkeit; W. Docters; J. C. D'Olivo; P. N. Dong; A. Dorofeev; Q. Dorosti Hasankiadeh; M. T. Dova; J. Ebr; R. Engel; M. Erdmann; M. Erfani; C. O. Escobar; J. Espadanal; A. Etchegoyen; P. Facal San Luis; H. Falcke; K. Fang; G. Farrar; A. C. Fauth; N. Fazzini; A. P. Ferguson; M. Fernandes; B. Fick; J. M. Figueira; A. Filevich; A. Filip?i?; B. D. Fox; O. Fratu; U. Fröhlich; B. Fuchs; T. Fuji; R. Gaior; B. Garc\\'\\ia; S. T. Garcia Roca; D. Garcia-Gamez; D. Garcia-Pinto; G. Garilli; A. Gascon Bravo; F. Gate; H. Gemmeke; P. L. Ghia; U. Giaccari; M. Giammarchi; M. Giller; C. Glaser; H. Glass; F. Gomez Albarracin; M. Gómez Berisso; P. F. Gómez Vitale; P. Gonçalves; J. G. Gonzalez; B. Gookin; A. Gorgi; P. Gorham; P. Gouffon; S. Grebe; N. Griffith; A. F. Grillo; T. D. Grubb; Y. Guardincerri; F. Guarino; G. P. Guedes; P. Hansen; D. Harari; T. A. Harrison; J. L. Harton; A. Haungs; T. Hebbeker; D. Heck; P. Heimann; A. E. Herve; G. C. Hill; C. Hojvat; N. Hollon; E. Holt; P. Homola; J. R. Hörandel; P. Horvath; M. Hrabovský; D. Huber; T. Huege; A. Insolia; P. G. Isar; K. Islo; I. Jandt; S. Jansen; C. Jarne; M. Josebachuili; A. Kääpä; O. Kambeitz; K. H. Kampert; P. Kasper; I. Katkov; B. Kégl; B. Keilhauer; A. Keivani; E. Kemp; R. M. Kieckhafer; H. O. Klages; M. Kleifges; J. Kleinfeller; R. Krause; N. Krohm; O. Krömer; D. Kruppke-Hansen; D. Kuempel; N. Kunka; G. La Rosa; D. LaHurd; L. Latronico; R. Lauer; M. Lauscher; P. Lautridou; S. Le Coz; M. S. A. B. Leão; D. Lebrun; P. Lebrun; M. A. Leigui de Oliveira; A. Letessier-Selvon; I. Lhenry-Yvon; K. Link; R. López; A. Lopez Agëra; K. Louedec; J. Lozano Bahilo; L. Lu; A. Lucero; M. Ludwig; H. Lyberis; M. C. Maccarone; M. Malacari; S. Maldera; J. Maller; D. Mandat; P. Mantsch; A. G. Mariazzi; V. Marin; I. C. Mari?; G. Marsella; D. Martello; L. Martin; H. Martinez; O. Mart\\'\\inez Bravo; D. Martraire; J. J. Mas\\'\\ias Meza; H. J. Mathes; S. Mathys; A. J. Matthews; J. Matthews; G. Matthiae; D. Maurel; D. Maurizio; E. Mayotte; P. O. Mazur; C. Medina; G. Medina-Tanco; M. Melissas; D. Melo; E. Menichetti; A. Menshikov; S. Messina; R. Meyhandan; S. Mi?anovi?; M. I. Micheletti; L. Middendorf; I. A. Minaya; L. Miramonti; B. Mitrica; L. Molina-Bueno; S. Mollerach; M. Monasor; D. Monnier Ragaigne; F. Montanet; C. Morello; J. C. Moreno; M. Mostafá; C. A. Moura; M. A. Muller; G. Müller; M. Münchmeyer; R. Mussa; G. Navarra; S. Navas; P. Necesal; L. Nellen; A. Nelles; J. Neuser; D. Newton; M. Niechciol; L. Niemietz; T. Niggemann; D. Nitz; D. Nosek; V. Novotny; L. Nožka; L. Ochilo; A. Olinto; M. Oliveira; V. M. Olmos-Gilbaja; M. Ortiz; N. Pacheco; D. Pakk Selmi-Dei; M. Palatka; J. Pallotta; N. Palmieri; P. Papenbreer; G. Parente; A. Parra; S. Pastor; T. Paul; M. Pech; J. P?kala; R. Pelayo; I. M. Pepe; L. Perrone; R. Pesce; E. Petermann; C. Peters; S. Petrera; A. Petrolini; Y. Petrov; R. Piegaia; T. Pierog; P. Pieroni; M. Pimenta; V. Pirronello; M. Platino; M. Plum; A. Porcelli; C. Porowski; P. Privitera; M. Prouza; V. Purrello; E. J. Quel; S. Querchfeld; S. Quinn; J. Rautenberg; O. Ravel; D. Ravignani; B. Revenu; J. Ridky; S. Riggi; M. Risse; P. Ristori; V. Rizi; J. Roberts; W. Rodrigues de Carvalho; I. Rodriguez Cabo; G. Rodriguez Fernandez; J. Rodriguez Rojo; M. D. Rodr\\'\\iguez-Fr\\'\\ias; G. Ros; J. Rosado; T. Rossler; M. Roth; E. Roulet; A. C. Rovero; C. Rühle; S. J. Saffi; A. Saftoiu; F. Salamida; H. Salazar; F. Salesa Greus

    2014-07-11

    We describe the method devised to reconstruct inclined cosmic-ray air showers with zenith angles greater than $60^\\circ$ detected with the surface array of the Pierre Auger Observatory. The measured signals at the ground level are fitted to muon density distributions predicted with atmospheric cascade models to obtain the relative shower size as an overall normalization parameter. The method is evaluated using simulated showers to test its performance. The energy of the cosmic rays is calibrated using a sub-sample of events reconstructed with both the fluorescence and surface array techniques. The reconstruction method described here provides the basis of complementary analyses including an independent measurement of the energy spectrum of ultra-high energy cosmic rays using very inclined events collected by the Pierre Auger Observatory.

  17. Herschel Space Observatory - An ESA facility for far-infrared and submillimetre astronomy

    E-Print Network [OSTI]

    Pilbratt, G L; Passvogel, T; Crone, G; Doyle, D; Gageur, U; Heras, A M; Jewell, C; Metcalfe, L; Ott, S; Schmidt, M

    2010-01-01

    Herschel was launched on 14 May 2009, and is now an operational ESA space observatory offering unprecedented observational capabilities in the far-infrared and submillimetre spectral range 55-671 {\\mu}m. Herschel carries a 3.5 metre diameter passively cooled Cassegrain telescope, which is the largest of its kind and utilises a novel silicon carbide technology. The science payload comprises three instruments: two direct detection cameras/medium resolution spectrometers, PACS and SPIRE, and a very high-resolution heterodyne spectrometer, HIFI, whose focal plane units are housed inside a superfluid helium cryostat. Herschel is an observatory facility operated in partnership among ESA, the instrument consortia, and NASA. The mission lifetime is determined by the cryostat hold time. Nominally approximately 20,000 hours will be available for astronomy, 32% is guaranteed time and the remainder is open to the worldwide general astronomical community through a standard competitive proposal procedure.

  18. Astrometrical Observations of Pluto - Charon System with the Automated Telescopes of Pulkovo Observatory

    E-Print Network [OSTI]

    Devyatkin, Alexander V; Slesarenko, Vyacheslav Yu

    2015-01-01

    The space probe 'New Horizon' was launched on 19th of January 2006 in order to study Pluto and its moons. Spacecraft will fly by Pluto as close as 12500 km in the middle of July 2015 and will get the most detailed images of Pluto and its moon until this moment. At the same time, observation obtained by the ground-based telescopes may also be helpful for the research of such distant system. Thereby, the Laboratory of observational astrometry of Pulkovo Observatory of RAS made a decision to reprocess observations obtained during last decade. More than 350 positional observations of Pluto - Charon system were carried out with the mirror astrograph ZA-320M at Pulkovo and Maksutov telescope MTM-500M near Kislovodsk. These observations were processed by means of software system APEX-II developed in Pulkovo observatory and numerical simulation was performed to calculate the differences between positions of photocenter and barycenter of Pluto - Charon system.

  19. Points

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

    (Fluidic Energy, Inc.) 5,133,150 Tempe, AZ Energy Storage A new class of metal-air batteries using ionic liquids, with many times the energy density of today's lithium-ion...

  20. Light pollution at high zenith angles, as measured at Cerro Tololo Inter-American Observatory

    E-Print Network [OSTI]

    Krisciunas, Kevin; Sanhueza, Pedro; Smith, Malcolm G

    2010-01-01

    On the basis of measurements of the V-band sky brightness obtained at Cerro Tololo Inter-American Observatory in December 2006 and December 2008 we confirm the functional form of the basic model of Garstang (1989, 1991). At high zenith angles we measure an enhancement of a factor of two over Garstang's later model when there is no marine cloud layer over La Serena/Coquimbo. No corresponding enhancement is found in the B-band.

  1. Take Home Points Horticultural Prospective

    E-Print Network [OSTI]

    Ma, Lena

    HLB Take Home Points Horticultural Prospective Stephen H. Futch Extension Agent, Multi County Co plants, ACP adults preferentially light on infected within first 48 hour but on uninfected after 7 days

  2. Join Point Encapsulation David Larochelle

    E-Print Network [OSTI]

    Huang, Wei

    , behavior observation and modification are possible. We believe that it is undesirable to make all join points nec- essarily subject to behavioral observation and modification by aspects. To do so

  3. OBSERVATORY OPPORTUNITIES

    E-Print Network [OSTI]

    Groppi, Christopher

    solar system objects, as well as distant stars, black holes, galaxies, quasars, and other mysterious on the plains of San Augustin fifty miles west of Socorro, New Mexico. Each antenna is 25 m in diameter located at the Array Operations Center in Socorro, New Mexico. Acting like a giant eye 8,600 km wide

  4. Heliophysics Observatory

    E-Print Network [OSTI]

    Aulanier, Guillaume

    ........................................................................................................9 4.2 SQL query.................................................................................................................................14 SQL basics

  5. Observatory Collaboration

    E-Print Network [OSTI]

    Waltham, Chris

    . Gaudette, G. Milton, B.Sur Chalk River Laboratories, AECL Research, Chalk River, Ontario K0J 1J0 CANADA 2 J

  6. ASTRONOMICAL OBSERVATORY

    E-Print Network [OSTI]

    Hill, Wendell T.

    HOUSE 164 COLLEGE PARK FIRE STATION 802 110 ANNE ARUNDEL 060 SHOEMAKER 037 BIOMOLECULAR SCIENCES 296 GOLF COURSE CLUB HOUSE 166 CENTER FOR YOUNG CHILDREN 381 201 158 SHUTTLE BUS FACILITY 424 010 237 999 FIELD CAMBRIDGE COMMUNITY CENTER 097 382 109 103 119 CAMPUS FARM ANIMAL SCIENCES/ AGRICULTURE

  7. EVIDENCE FOR THE WAVE NATURE OF AN EXTREME ULTRAVIOLET WAVE OBSERVED BY THE ATMOSPHERIC IMAGING ASSEMBLY ON BOARD THE SOLAR DYNAMICS OBSERVATORY

    SciTech Connect (OSTI)

    Shen Yuandeng; Liu Yu

    2012-07-20

    Extreme-ultraviolet (EUV) waves have been found for about 15 years. However, significant controversy remains over their physical natures and origins. In this paper, we report an EUV wave that was accompanied by an X1.9 flare and a partial halo coronal mass ejection (CME). Using high temporal and spatial resolution observations taken by the Solar Dynamics Observatory and the Solar-TErrestrial RElations Observatory, we are able to investigate the detailed kinematics of the EUV wave. We find several arguments that support the fast-mode wave scenario. (1) The speed of the EUV wave (570 km s{sup -1}) is higher than the sound speed of the quiet-Sun corona. (2) Significant deceleration of the EUV wave (-130 m s{sup -2}) is found during its propagation. (3) The EUV wave resulted in the oscillations of a loop and a filament along its propagation path, and a reflected wave from the polar coronal hole is also detected. (4) Refraction or reflection effect is observed when the EUV wave was passing through two coronal bright points. (5) The dimming region behind the wavefront stopped to expand when the wavefront started to become diffuse. (6) The profiles of the wavefront exhibited a dispersive nature, and the magnetosonic Mach number of the EUV wave derived from the highest intensity jump is about 1.4. In addition, triangulation indicates that the EUV wave propagated within a height range of about 60-100 Mm above the photosphere. We propose that the EUV wave observed should be a nonlinear fast-mode magnetosonic wave that propagated freely in the corona after it was driven by the CME expanding flanks during the initial period.

  8. Proposal for a quantity based data model in the Virtual Observatory

    E-Print Network [OSTI]

    Brian Thomas; Edward Shaya

    2003-12-23

    We propose the beginnings of a data model for the Virtual Observatory (VO) built up from simple ``quantity'' objects. In this paper we present how an object-oriented, domain (or namespace)-scoped simple quantity may be used to describe astronomical data. Our model is designed around the requirements that it be searchable and serve as a transport mechanism for all types of VO data and meta-data. In this paper we describe this model in terms of an OWL ontology and UML diagrams. An XML schema is available online.

  9. The HAWC Gamma-Ray Observatory: Sensitivity to Steady and Transient Sources of Gamma Rays

    E-Print Network [OSTI]

    Abeysekara, A U; Alvarez, C; Álvarez, J D; Arceo, R; Arteaga-Velázquez, J C; Solares, H A Ayala; Barber, A S; Baughman, B M; Bautista-Elivar, N; Belmont, E; BenZvi, S Y; Berley, D; Rosales, M Bonilla; Braun, J; Caballero-Lopez, R A; Caballero-Mora, K S; Carramiñana, A; Castillo, M; Cotti, U; Cotzomi, J; de la Fuente, E; De León, C; DeYoung, T; Hernandez, R Diaz; Díaz-Vélez, J C; Dingus, B L; DuVernois, M A; Ellsworth, R W; Fernandez, A; Fiorino, D W; Fraija, N; Galindo, A; Garfias, F; González, L X; González, M M; Goodman, J A; Grabski, V; Gussert, M; Hampel-Arias, Z; Hui, C M; Hüntemeyer, P; Imran, A; Iriarte, A; Karn, P; Kieda, D; Kunde, G J; Lara, A; Lauer, R J; Lee, W H; Lennarz, D; Vargas, H León; Linares, E C; Linnemann, J T; Longo, M; Luna-GarcIa, R; Marinelli, A; Martinez, H; Martinez, O; Martínez-Castro, J; Matthews, J A J; Miranda-Romagnoli, P; Moreno, E; Mostafá, M; Nava, J; Nellen, L; Newbold, M; Noriega-Papaqui, R; Oceguera-Becerra, T; Patricelli, B; Pelayo, R; Pérez-Pérez, E G; Pretz, J; Rivière, C; Rosa-González, D; Salazar, H; Salesa, F; Sanchez, F E; Sandoval, A; Santos, E; Schneider, M; Silich, S; Sinnis, G; Smith, A J; Sparks, K; Springer, R W; Taboada, I; Toale, P A; Tollefson, K; Torres, I; Ukwatta, T N; Villaseñor, L; Weisgarber, T; Westerhoff, S; Wisher, I G; Wood, J; Yodh, G B; Younk, P W; Zaborov, D; Zepeda, A; Zhou, H

    2013-01-01

    The High-Altitude Water Cherenkov (HAWC) Gamma-Ray Observatory is designed to record air showers produced by cosmic rays and gamma rays between 100 GeV and 100 TeV. Because of its large field of view and high livetime, HAWC is well-suited to measure gamma rays from extended sources, diffuse emission, and transient sources. We describe the sensitivity of HAWC to emission from the extended Cygnus region as well as other types of galactic diffuse emission; searches for flares from gamma-ray bursts and active galactic nuclei; and the first measurement of the Crab Nebula with HAWC-30.

  10. The HAWC Gamma-Ray Observatory: Dark Matter, Cosmology, and Fundamental Physics

    E-Print Network [OSTI]

    Abeysekara, A U; Alvarez, C; Álvarez, J D; Arceo, R; Arteaga-Velázquez, J C; Solares, H A Ayala; Barber, A S; Baughman, B M; Bautista-Elivar, N; Belmont, E; BenZvi, S Y; Berley, D; Rosales, M Bonilla; Braun, J; Caballero-Lopez, R A; Caballero-Mora, K S; Carramiñana, A; Castillo, M; Cotti, U; Cotzomi, J; de la Fuente, E; De León, C; DeYoung, T; Hernandez, R Diaz; Díaz-Vélez, J C; Dingus, B L; DuVernois, M A; Ellsworth, R W; Fernandez, A; Fiorino, D W; Fraija, N; Galindo, A; Garfias, F; González, L X; González, M M; Goodman, J A; Grabski, V; Gussert, M; Hampel-Arias, Z; Hui, C M; Hüntemeyer, P; Imran, A; Iriarte, A; Karn, P; Kieda, D; Kunde, G J; Lara, A; Lauer, R J; Lee, W H; Lennarz, D; Vargas, H León; Linares, E C; Linnemann, J T; Longo, M; Luna-GarcIa, R; Marinelli, A; Martinez, H; Martinez, O; Martínez-Castro, J; Matthews, J A J; Miranda-Romagnoli, P; Moreno, E; Mostafá, M; Nava, J; Nellen, L; Newbold, M; Noriega-Papaqui, R; Oceguera-Becerra, T; Patricelli, B; Pelayo, R; Pérez-Pérez, E G; Pretz, J; Rivière, C; Rosa-González, D; Salazar, H; Salesa, F; Sanchez, F E; Sandoval, A; Santos, E; Schneider, M; Silich, S; Sinnis, G; Smith, A J; Sparks, K; Springer, R W; Taboada, I; Toale, P A; Tollefson, K; Torres, I; Ukwatta, T N; Villaseñor, L; Weisgarber, T; Westerhoff, S; Wisher, I G; Wood, J; Yodh, G B; Younk, P W; Zaborov, D; Zepeda, A; Zhou, H

    2013-01-01

    The High-Altitude Water Cherenkov Gamma Ray Observatory (HAWC) is designed to perform a synoptic survey of the TeV sky. The high energy coverage of the experiment will enable studies of fundamental physics beyond the Standard Model, and the large field of view of the detector will enable detailed studies of cosmologically significant backgrounds and magnetic fields. We describe the sensitivity of the full HAWC array to these phenomena in five contributions shown at the 33rd International Cosmic Ray Conference in Rio de Janeiro, Brazil (July 2013).

  11. Defocused Observations of Selected Exoplanet Transits with T100 in TUBITAK National Observatory of Turkey (TUG)

    E-Print Network [OSTI]

    Basturk, Ozgur; Ozavci, Ibrahim; Yorukoglu, Onur; Selam, Selim O

    2015-01-01

    It is crucial to determine masses and radii of extrasolar planets with high precision to have constraints on their chemical composition, internal structure and thereby their formation and evolution. In order to achieve this goal, we apply the defocus technique in the observations of selected planetary systems with the 1 m Turkish telescope T100 in TUBITAK National Observatory (TUG). With this contribution, we aim to present preliminary analyses of transit light curves of the selected exoplanets KELT-3b, HAT-P-10b/WASP-11b, HAT-P-20b, and HAT-P-22b, observed with this technique using T100.

  12. An upper limit to photons from first data taken by the Pierre Auger Observatory

    E-Print Network [OSTI]

    Markus Risse

    2007-01-03

    Many models for ultra-high energy cosmic rays postulate exotic scenarios to explain the sources or the nature of these particles. A characteristic feature of these models is the prediction of a significant flux of photons at ultra-high energy. The Pierre Auger Observatory offers a great potential to search for such photons. We present shower observables with sensitivity to photons and the search strategy employed. An upper limit to photon primaries is derived from first Auger data. Prospects for constraining theoretical source models are discussed.

  13. High-Resolution Spectroscopy with the Chandra X-ray Observatory

    ScienceCinema (OSTI)

    Canizares, Claude R. [MIT, Cambridge, Massachusetts, United States

    2010-01-08

    The capabilities of the Chandra X-ray Observatory and XMM-Newton for high-resolution spectroscopy have brought tradition plasma diagnostic techniques to the study of cosmic plasma. Observations have probed nearly every class of astronomical object, from young proto-starts through massive O starts and black hole binaries, supernova remnants, active galactic nuclei, and the intergalactic medium. Many of these sources show remarkable rich spectra that reveal new physical information, such as emission measure distributions, elemental abundances, accretion disk and wind signatures, and time variability. This talk will present an overview of the Chandra instrumentaton and selected examples of spectral observations of astrophysical and cosmological importance.

  14. Coverage and large scale anisotropies estimation methods for the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Hamilton, Jean-Christophe; /Paris, IN2P3

    2005-07-01

    When searching for anisotropies in the arrival directions of Ultra High Energy Cosmic Rays, one must estimate the number of events expected in each direction of the sky in the case of a perfect isotropy. We present in this article a new method, developed for the Auger Observatory, based on a smooth estimate of the zenith angle distribution obtained from the data itself (which is essentially unchanged in the case of the presence of a large scale anisotropy pattern). We also study the sensitivity of several methods to detect large-scale anisotropies in the cosmic ray arrival direction distribution : Rayleigh analysis, dipole fitting and angular power spectrum estimation.

  15. Femtosecond photoelectron point projection microscope

    SciTech Connect (OSTI)

    Quinonez, Erik; Handali, Jonathan; Barwick, Brett

    2013-10-15

    By utilizing a nanometer ultrafast electron source in a point projection microscope we demonstrate that images of nanoparticles with spatial resolutions of the order of 100 nanometers can be obtained. The duration of the emission process of the photoemitted electrons used to make images is shown to be of the order of 100 fs using an autocorrelation technique. The compact geometry of this photoelectron point projection microscope does not preclude its use as a simple ultrafast electron microscope, and we use simple analytic models to estimate temporal resolutions that can be expected when using it as a pump-probe ultrafast electron microscope. These models show a significant increase in temporal resolution when comparing to ultrafast electron microscopes based on conventional designs. We also model the microscopes spectroscopic abilities to capture ultrafast phenomena such as the photon induced near field effect.

  16. Starting Points | National Nuclear Security Administration

    National Nuclear Security Administration (NNSA)

    (M&O) Contract Competition Starting Points Starting Points Kansas City Plant Related Web Pages Summary Kansas City Plant Home Page Kansas City Plant Contracts DOE Directives...

  17. Energy Estimation of Cosmic Rays with the Engineering Radio Array of the Pierre Auger Observatory

    E-Print Network [OSTI]

    Aab, Alexander; Aglietta, Marco; Ahn, Eun-Joo; Samarai, Imen Al; Albuquerque, Ivone; Allekotte, Ingomar; Allison, Patrick; Almela, Alejandro; Castillo, Jesus Alvarez; Alvarez-Muñiz, Jaime; Batista, Rafael Alves; Ambrosio, Michelangelo; Aminaei, Amin; Anastasi, Gioacchino Alex; Anchordoqui, Luis; Andringa, Sofia; Aramo, Carla; Arqueros, Fernando; Arsene, Nicusor; Asorey, Hernán Gonzalo; Assis, Pedro; Aublin, Julien; Avila, Gualberto; Awal, Nafiun; Badescu, Alina Mihaela; Baus, Colin; Beatty, Jim; Becker, Karl Heinz; Bellido, Jose A; Berat, Corinne; Bertaina, Mario Edoardo; Bertou, Xavier; Biermann, Peter; Billoir, Pierre; Blaess, Simon G; Blanco, Alberto; Blanco, Miguel; Blazek, Jiri; Bleve, Carla; Blümer, Hans; Bohá?ová, Martina; Boncioli, Denise; Bonifazi, Carla; Borodai, Nataliia; Brack, Jeffrey; Brancus, Iliana; Bretz, Thomas; Bridgeman, Ariel; Brogueira, Pedro; Buchholz, Peter; Bueno, Antonio; Buitink, Stijn; Buscemi, Mario; Caballero-Mora, Karen S; Caccianiga, Barbara; Caccianiga, Lorenzo; Candusso, Marina; Caramete, Laurentiu; Caruso, Rossella; Castellina, Antonella; Cataldi, Gabriella; Cazon, Lorenzo; Cester, Rosanna; Chavez, Alan G; Chiavassa, Andrea; Chinellato, Jose Augusto; Chudoba, Jiri; Cilmo, Marco; Clay, Roger W; Cocciolo, Giuseppe; Colalillo, Roberta; Coleman, Alan; Collica, Laura; Coluccia, Maria Rita; Conceição, Ruben; Contreras, Fernando; Cooper, Mathew J; Cordier, Alain; Coutu, Stephane; Covault, Corbin; Cronin, James; Dallier, Richard; Daniel, Bruno; Dasso, Sergio; Daumiller, Kai; Dawson, Bruce R; de Almeida, Rogerio M; de Jong, Sijbrand J; De Mauro, Giuseppe; Neto, Joao de Mello; De Mitri, Ivan; de Oliveira, Jaime; de Souza, Vitor; del Peral, Luis; Deligny, Olivier; Dhital, Niraj; Di Giulio, Claudio; Di Matteo, Armando; Diaz, Johana Chirinos; Castro, Mary Lucia Díaz; Diogo, Francisco; Dobrigkeit, Carola; Docters, Wendy; D'Olivo, Juan Carlos; Dorofeev, Alexei; Hasankiadeh, Qader Dorosti; Anjos, Rita dos; Dova, Maria Teresa; Ebr, Jan; Engel, Ralph; Erdmann, Martin; Erfani, Mona; Escobar, Carlos O; Espadanal, Joao; Etchegoyen, Alberto; Falcke, Heino; Fang, Ke; Farrar, Glennys; Fauth, Anderson; Fazzini, Norberto; Ferguson, Andrew P; Fick, Brian; Figueira, Juan Manuel; Filevich, Alberto; Filip?i?, Andrej; Fratu, Octavian; Freire, Martín Miguel; Fujii, Toshihiro; García, Beatriz; Garcia-Gamez, Diego; Garcia-Pinto, Diego; Gate, Florian; Gemmeke, Hartmut; Gherghel-Lascu, Alexandru; Ghia, Piera Luisa; Giaccari, Ugo; Giammarchi, Marco; Giller, Maria; G?as, Dariusz; Glaser, Christian; Glass, Henry; Golup, Geraldina; Berisso, Mariano Gómez; Vitale, Primo F Gómez; González, Nicolás; Gookin, Ben; Gordon, Jacob; Gorgi, Alessio; Gorham, Peter; Gouffon, Philippe; Griffith, Nathan; Grillo, Aurelio; Grubb, Trent D; Guarino, Fausto; Guedes, Germano; Hampel, Matías Rolf; Hansen, Patricia; Harari, Diego; Harrison, Thomas A; Hartmann, Sebastian; Harton, John; Haungs, Andreas; Hebbeker, Thomas; Heck, Dieter; Heimann, Philipp; Herve, Alexander E; Hill, Gary C; Hojvat, Carlos; Hollon, Nicholas; Holt, Ewa; Homola, Piotr; Hörandel, Jörg; Horvath, Pavel; Hrabovský, Miroslav; Huber, Daniel; Huege, Tim; Insolia, Antonio; Isar, Paula Gina; Jandt, Ingolf; Jansen, Stefan; Jarne, Cecilia; Johnsen, Jeffrey A; Josebachuili, Mariela; Kääpä, Alex; Kambeitz, Olga; Kampert, Karl Heinz; Kasper, Peter; Katkov, Igor; Keilhauer, Bianca; Kemp, Ernesto; Kieckhafer, Roger; Klages, Hans; Kleifges, Matthias; Kleinfeller, Jonny; Krause, Raphael; Krohm, Nicole; Kuempel, Daniel; Mezek, Gasper Kukec; Kunka, Norbert; Awad, Alaa Metwaly Kuotb; LaHurd, Danielle; Latronico, Luca; Lauer, Robert; Lauscher, Markus; Lautridou, Pascal; Coz, Sandra Le; Lebrun, Didier; Lebrun, Paul; de Oliveira, Marcelo Augusto Leigui; Letessier-Selvon, Antoine; Lhenry-Yvon, Isabelle; Link, Katrin; Lopes, Luis; López, Rebeca; Casado, Aida López; Louedec, Karim; Lucero, Agustin; Malacari, Max; Mallamaci, Manuela; Maller, Jennifer; Mandat, Dusan; Mantsch, Paul; Mariazzi, Analisa; Marin, Vincent; Mari?, Ioana; Marsella, Giovanni; Martello, Daniele; Martinez, Humberto; Bravo, Oscar Martínez; Martraire, Diane; Meza, Jimmy Masías; Mathes, Hermann-Josef; Mathys, Sebastian; Matthews, James; Matthews, John; Matthiae, Giorgio; Maurizio, Daniela; Mayotte, Eric; Mazur, Peter; Medina, Carlos; Medina-Tanco, Gustavo; Meissner, Rebecca; Mello, Victor; Melo, Diego; Menshikov, Alexander; Messina, Stefano; Micheletti, Maria Isabel; Middendorf, Lukas; Minaya, Ignacio A; Miramonti, Lino; Mitrica, Bogdan; Molina-Bueno, Laura; Mollerach, Silvia; Montanet, François

    2015-01-01

    The Auger Engineering Radio Array (AERA) is part of the Pierre Auger Observatory and is used to detect the radio emission of cosmic-ray air showers. These observations are compared to the data of the surface detector stations of the Observatory, which provide well-calibrated information on the cosmic-ray energies and arrival directions. The response of the radio stations in the 30 to 80 MHz regime has been thoroughly calibrated to enable the reconstruction of the incoming electric field. For the latter, the energy density is determined from the radio pulses at each observer position and is interpolated using a two dimensional function that takes into account signal asymmetries due to interference between the geomagnetic and charge excess emission components. The spatial integral over the signal distribution gives a direct measurement of the energy transferred from the primary cosmic ray into radio emission in the AERA frequency range. We measure 15.8 MeV of radiation energy for a 1 EeV air shower arriving per...

  18. The Jay Baum Rich telescope: a Centurion 28 at the Wise Observatory

    E-Print Network [OSTI]

    Brosch, Noah; Niv, Saar; Manulis, Ilan

    2015-01-01

    We describe the third telescope of the Wise Observatory, a 0.70-m Centurion 28 (C28IL) installed in 2013 and named the Jay Baum Rich telescope to enhance significantly the wide-field imaging possibilities of the observatory. The telescope operates from a 5.5-m diameter dome and is equipped with a large-format red-sensitive CCD camera, offering a ~one square degree imaged field sampled at 0".83/pixel. The telescope was acquired to provide an alternative to the existing 1-m telescope for studies such as microlensing, photometry of transiting exo-planets, the follow-up of supernovae and other optical transients, and the detection of very low surface brightness extended features around galaxies. The operation of the C28IL is robotic, requiring only the creation of a night observing plan that is loaded in the afternoon prior to the observations. The entire facility was erected for a component and infrastructure cost of well under 300k$ and a labor investment of about two person-year. The successful implementation ...

  19. Breaking Points in Quartic Maps

    E-Print Network [OSTI]

    M. Romera; G. Pastor; M. -F. Danca; A. Martin; A. B. Orue; F. Montoya

    2014-12-18

    Dynamical systems, whether continuous or discrete, are used by physicists in order to study non-linear phenomena. In the case of discrete dynamical systems, one of the most used is the quadratic map depending on a parameter. However, some phenomena can depend alternatively of two values of the same parameter. We use the quadratic map $x_{n+1} =1-ax_{n}^{2} $ when the parameter alternates between two values during the iteration process. In this case, the orbit of the alternate system is the sum of the orbits of two quartic maps. The bifurcation diagrams of these maps present breaking points where abruptly change their evolution.

  20. Capital Point | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION JEnvironmentalBowerbank,Cammack Village, Arkansas: EnergyCounty,NewHatteras ElecPoint Jump to:

  1. Points of Contact - Hanford Site

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

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity ofkandz-cm11 Outreach Home Room NewsInformationJesseworkSURVEYI/OPerformancePi Day Pi Day Pi DayPlasmaandAbout UsPoints of

  2. Telescope Array Radar (TARA) Observatory for Ultra-High Energy Cosmic Rays

    SciTech Connect (OSTI)

    Abbasi, R.; Takai, H.; Allen, C.; Beard, L.; Belz, J.; Besson, D.; Byrne, M.; Abou Bakr Othman, M.; Farhang-Boroujeny, B.; Gardner, A.; Gillman, W.H.; Hanlon, W.; Hanson, J.; Jayanthmurthy, C.; Kunwar, S.; Larson, S. L.; Myers, I.; Prohira, S.; Ratzlaff, K.; Sokolsky, P.; Thomson, G. B.; Von Maluski, D.

    2014-08-19

    Construction was completed during summer 2013 on the Telescope Array RAdar (TARA) bi-static radar observatory for Ultra-High Energy Cosmic Rays (UHECR). TARA is co-located with the Telescope Array, the largest “conventional” cosmic ray detector in the Northern Hemisphere, in radio-quiet Western Utah. TARA employs an 8 MW Effective Radiated Power (ERP) VHF transmitter and smart receiver system based on a 250 MS/s data acquisition system in an effort to detect the scatter of sounding radiation by UHECR-induced atmospheric ionization. TARA seeks to demonstrate bi-static radar as a useful new remote sensing technique for UHECRs. In this report, we describe the design and performance of the TARA transmitter and receiver systems.

  3. Telescope Array Radar (TARA) Observatory for Ultra-High Energy Cosmic Rays

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

    Abbasi, R.; Takai, H.; Allen, C.; Beard, L.; Belz, J.; Besson, D.; Byrne, M.; Abou Bakr Othman, M.; Farhang-Boroujeny, B.; Gardner, A.; et al

    2014-08-19

    Construction was completed during summer 2013 on the Telescope Array RAdar (TARA) bi-static radar observatory for Ultra-High Energy Cosmic Rays (UHECR). TARA is co-located with the Telescope Array, the largest “conventional” cosmic ray detector in the Northern Hemisphere, in radio-quiet Western Utah. TARA employs an 8 MW Effective Radiated Power (ERP) VHF transmitter and smart receiver system based on a 250 MS/s data acquisition system in an effort to detect the scatter of sounding radiation by UHECR-induced atmospheric ionization. TARA seeks to demonstrate bi-static radar as a useful new remote sensing technique for UHECRs. In this report, we describe themore »design and performance of the TARA transmitter and receiver systems.« less

  4. Telescope Array Radar (TARA) Observatory for Ultra-High Energy Cosmic Rays

    SciTech Connect (OSTI)

    Abbasi, R. [Univ. of Utah, Salt Lake City, UT (United States); Takai, H. [Brookhaven National Laboratory (BNL), Upton, NY (United States); Allen, C. [Univ. of Kansas, Lawrence, KS (United States); Beard, L. [Purdue Univ., West Lafayette, IN (United States); Belz, J. [Univ. of Utah, Salt Lake City, UT (United States); Besson, D. [Univ. of Kansas, Lawrence, KS (United States). Moscow Engineering and Physics Inst. (Russian Federation); Byrne, M. [Univ. of Utah, Salt Lake City, UT (United States); Abou Bakr Othman, M. [Univ. of Utah, Salt Lake City, UT (United States); Farhang-Boroujeny, B. [Univ. of Utah, Salt Lake City, UT (United States); Gardner, A. [Univ. of Utah, Salt Lake City, UT (United States); Gillman, W.H. [Gillman and Associates, Salt Lake City, UT (United States); Hanlon, W. [Univ. of Utah, Salt Lake City, UT (United States); Hanson, J. [Univ. of Kansas, Lawrence, KS (United States); Jayanthmurthy, C. [Univ. of Utah, Salt Lake City, UT (United States); Kunwar, S. [Univ. of Kansas, Lawrence, KS (United States); Larson, S. L. [Utah State Univ., Logan, UT (United States); Myers, I. [Univ. of Utah, Salt Lake City, UT (United States); Prohira, S. [Univ. of Kansas, Lawrence, KS (United States); Ratzlaff, K. [Univ. of Kansas, Lawrence, KS (United States); Sokolsky, P. [Univ. of Utah, Salt Lake City, UT (United States); Thomson, G. B. [Univ. of Utah, Salt Lake City, UT (United States); Von Maluski, D. [Univ. of Utah, Salt Lake City, UT (United States)

    2014-12-01

    Construction was completed during summer 2013 on the Telescope Array RAdar (TARA) bi-static radar observatory for Ultra-High Energy Cosmic Rays (UHECR). TARA is co-located with the Telescope Array, the largest “conventional” cosmic ray detector in the Northern Hemisphere, in radio-quiet Western Utah. TARA employs an 8 MW Effective Radiated Power (ERP) VHF transmitter and smart receiver system based on a 250 MS/s data acquisition system in an effort to detect the scatter of sounding radiation by UHECR-induced atmospheric ionization. TARA seeks to demonstrate bi-static radar as a useful new remote sensing technique for UHECRs. In this report, we describe the design and performance of the TARA transmitter and receiver systems.

  5. Detecting particles with cell phones: the Distributed Electronic Cosmic-ray Observatory

    E-Print Network [OSTI]

    Vandenbroucke, Justin; Karn, Peter; Meehan, Matthew; Plewa, Matthew; Ruggles, Tyler; Schultz, David; Peacock, Jeffrey; Simons, Ariel Levi

    2015-01-01

    In 2014 the number of active cell phones worldwide for the first time surpassed the number of humans. Cell phone camera quality and onboard processing power (both CPU and GPU) continue to improve rapidly. In addition to their primary purpose of detecting photons, camera image sensors on cell phones and other ubiquitous devices such as tablets, laptops and digital cameras can detect ionizing radiation produced by cosmic rays and radioactive decays. While cosmic rays have long been understood and characterized as a nuisance in astronomical cameras, they can also be identified as a signal in idle camera image sensors. We present the Distributed Electronic Cosmic-ray Observatory (DECO), a platform for outreach and education as well as for citizen science. Consisting of an app and associated database and web site, DECO harnesses the power of distributed camera image sensors for cosmic-ray detection.

  6. Detecting particles with cell phones: the Distributed Electronic Cosmic-ray Observatory

    E-Print Network [OSTI]

    Justin Vandenbroucke; Silvia Bravo; Peter Karn; Matthew Meehan; Matthew Plewa; Tyler Ruggles; David Schultz; Jeffrey Peacock; Ariel Levi Simons

    2015-10-26

    In 2014 the number of active cell phones worldwide for the first time surpassed the number of humans. Cell phone camera quality and onboard processing power (both CPU and GPU) continue to improve rapidly. In addition to their primary purpose of detecting photons, camera image sensors on cell phones and other ubiquitous devices such as tablets, laptops and digital cameras can detect ionizing radiation produced by cosmic rays and radioactive decays. While cosmic rays have long been understood and characterized as a nuisance in astronomical cameras, they can also be identified as a signal in idle camera image sensors. We present the Distributed Electronic Cosmic-ray Observatory (DECO), a platform for outreach and education as well as for citizen science. Consisting of an app and associated database and web site, DECO harnesses the power of distributed camera image sensors for cosmic-ray detection.

  7. The History of the Mysterious Eclipses of KH 15D: Asiago Observatory, 1967-1982

    E-Print Network [OSTI]

    John A. Johnson; Joshua N. Winn

    2003-12-23

    We are gathering archival observations to determine the photometric history of the unique and unexplained eclipses of the pre-main-sequence star KH 15D. Here we present a light curve from 1967-1982, based on photographic plates from Asiago Observatory. During this time, the system alternated periodically between bright and faint states, as observed today. However, the bright state was 0.9 mag brighter than the modern value, and the fractional variation between bright and faint states (Delta I = 0.7 mag) was smaller than observed today (3.5 mag). A possible explanation for these findings is that the system contains a second star that was previously blended with the eclipsing star, but is now completely obscured.

  8. The exposure of the hybrid detector of the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Not Available

    2010-06-01

    The Pierre Auger Observatory is a detector for ultra-high energy cosmic rays. It consists of a surface array to measure secondary particles at ground level and a fluorescence detector to measure the development of air showers in the atmosphere above the array. The 'hybrid' detection mode combines the information from the two subsystems. We describe the determination of the hybrid exposure for events observed by the fluorescence telescopes in coincidence with at least one water-Cherenkov detector of the surface array. A detailed knowledge of the time dependence of the detection operations is crucial for an accurate evaluation of the exposure. We discuss the relevance of monitoring data collected during operations, such as the status of the fluorescence detector, background light and atmospheric conditions, that are used in both simulation and reconstruction.

  9. Search for Very High Energy Emission from Satellite-triggered GRBs with the Milagro Observatory

    E-Print Network [OSTI]

    Parkinson, P M S; Atkins, R; Benbow, W; Berley, D; Blaufuss, E; Coyne, D G; De Young, T R; Dingus, B L; Dorfan, D E; Ellsworth, R W; Fleysher, L; Gisler, G; González, M M; Goodman, J A; Haines, T J; Hays, E; Hoffman, C M; Kelley, L A; Lansdell, C P; Linnemann, J T; McEnery, J E; Miller, R S; Mincer, A I; Morales, M F; Némethy, P; Noyes, D; Ryan, J M; Samuelson, F W; Saz-Parkinson, P M; Shoup, A; Sinnis, G; Smith, A J; Sullivan, G W; Williams, D A; Wilson, M E; Xu, X W; Yodh, G B

    2005-01-01

    The Milagro gamma-ray observatory employs a water Cherenkov detector to observe extensive air showers produced by high energy particles interacting in the Earth's atmosphere. Milagro has a wide field of view (2 sr) and high duty cycle (> 90%) making it an ideal all-sky monitor of the northern hemisphere in the 100 GeV to 100 TeV energy range. More than 45 satellite-triggered gamma-ray bursts (GRBs) have occurred in the field of view of Milagro since January 2000, with the rate of bursts increasing significantly with the launch of Swift. We discuss the most recent results of a search for very high energy (VHE) emission from these GRBs.

  10. New method for atmospheric calibration at the Pierre Auger Observatory using FRAM, a robotic astronomical telescope

    E-Print Network [OSTI]

    Segev BenZvi; Martina Bohacova; Brian Connolly; Jiri Grygar; Miroslav Hrabovsky; Tatiana Karova; Dusan Mandat; Petr Necesal; Dalibor Nosek; Libor Nozka; Miroslav Palatka; Miroslav Pech; Michael Prouza; Jan Ridky; Petr Schovanek; Radomir Smida; Petr Travnicek; Primo Vitale; Stefan Westerhoff; for the Pierre Auger Collaboration

    2007-06-12

    FRAM - F/(Ph)otometric Robotic Atmospheric Monitor is the latest addition to the atmospheric monitoring instruments of the Pierre Auger Observatory. An optical telescope equipped with CCD camera and photometer, it automatically observes a set of selected standard stars and a calibrated terrestrial source. Primarily, the wavelength dependence of the attenuation is derived and the comparison between its vertical values (for stars) and horizontal values (for the terrestrial source) is made. Further, the integral vertical aerosol optical depth can be obtained. A secondary program of the instrument, the detection of optical counterparts of gamma-ray bursts, has already proven successful. The hardware setup, software system, data taking procedures, and first analysis results are described in this paper.

  11. 8Li electron spectrum versus 8B neutrino spectrum: implications for the Sudbury Neutrino Observatory

    E-Print Network [OSTI]

    G. Jonkmans; I. S. Towner; B. Sur

    1998-02-25

    The sensitivity of the Sudbury Neutrino Observatory (SNO) to measure the shape of the recoil electron spectrum in the charged-current reaction of $^{8}$B solar neutrinos interacting with deuterium can be improved if the results of a $^{8}$Li beta-decay calibration experiment are included in the test. We calculate an improvement in sensitivity, under certain idealistic assumptions, of about a factor of 2, sufficient to resolve different neutrino-oscillation solutions to the solar-neutrino problem. We further examine the role of recoil and radiative corrections on both the $^{8}$B neutrino spectrum and the $^{8}$Li electron spectrum and conclude that the influence of these effects on the ratio of the two spectra as measured by SNO is very small.

  12. Physics Potential of the ICAL detector at the India-based Neutrino Observatory (INO)

    E-Print Network [OSTI]

    Ahmed, Shakeel; Hasan, Rashid; Salim, Mohammad; Singh, S K; Inbanathan, S S R; Singh, Venktesh; Subrahmanyam, V S; Behera, Shiba Prasad; Chandratre, Vinay B; Dash, Nitali; Datar, Vivek M; Kashyap, V K S; Mohanty, Ajit K; Pant, Lalit M; Chatterjee, Animesh; Choubey, Sandhya; Gandhi, Raj; Ghosh, Anushree; Tiwari, Deepak; Ajmi, Ali; Sankar, S Uma; Behera, Prafulla; Chacko, Aleena; Jafer, Sadiq; Libby, James; Raveendrababu, K; Rebin, K R; Indumathi, D; Meghna, K; Lakshmi, S M; Murthy, M V N; Pal, Sumanta; Rajasekaran, G; Sinha, Nita; Agarwalla, Sanjib Kumar; Khatun, Amina; Mehta, Poonam; Bhatnagar, Vipin; Kanishka, R; Kumar, A; Shahi, J S; Singh, J B; Ghosh, Monojit; Ghoshal, Pomita; Goswami, Srubabati; Gupta, Chandan; Raut, Sushant; Bhattacharya, Sudeb; Bose, Suvendu; Ghosal, Ambar; Jash, Abhik; Kar, Kamalesh; Majumdar, Debasish; Majumdar, Nayana; Mukhopadhyay, Supratik; Saha, Satyajit; Acharya, B S; Banerjee, Sudeshna; Bhattacharya, Kolahal; Dasgupta, Sudeshna; Devi, Moon Moon; Dighe, Amol; Majumder, Gobinda; Mondal, Naba K; Redij, Asmita; Samuel, Deepak; Satyanarayana, B; Thakore, Tarak; Ravikumar, C D; Vinodkumar, A M; Gangopadhyay, Gautam; Raychaudhuri, Amitava; Choudhary, Brajesh C; Gaur, Ankit; Kaur, Daljeet; Kumar, Ashok; Kumar, Sanjeev; Naimuddin, Md; Bari, Waseem; Malik, Manzoor A; Singh, Jyotsna; Krishnaveni, S; Ravikumar, H B; Ranganathaiah, C; Mahapatra, Swapna; Biswas, Saikat; Chattopadhyay, Subhasis; Ganai, Rajesh; Ghosh, Tapasi; Viyogi, Y P

    2015-01-01

    The upcoming 50 kt magnetized iron calorimeter (ICAL) detector at the India-based Neutrino Observatory (INO) is designed to study the atmospheric neutrinos and antineutrinos separately over a wide range of energies and path lengths. The primary focus of this experiment is to explore the Earth matter effects by observing the energy and zenith angle dependence of the atmospheric neutrinos in the multi-GeV range. This study will be crucial to address some of the outstanding issues in neutrino oscillation physics, including the fundamental issue of neutrino mass hierarchy. In this document, we present the physics potential of the detector as obtained from realistic detector simulations. We describe the simulation framework, the neutrino interactions in the detector, and the expected response of the detector to particles traversing it. The ICAL detector can determine the energy and direction of the muons to a high precision, and in addition, its sensitivity to multi-GeV hadrons increases its physics reach substant...

  13. Software Holography: Interferometric Data Analysis for the Challenges of Next Generation Observatories

    E-Print Network [OSTI]

    Miguel F. Morales; Michael Matejek

    2008-10-28

    Next generation radio observatories such as the MWA, LWA, LOFAR, CARMA and SKA provide a number of challenges for interferometric data analysis. These challenges include heterogeneous arrays, direction-dependent instrumental gain, and refractive and scintillating atmospheric conditions. From the analysis perspective, this means that calibration solutions can not be described using a single complex gain per antenna. In this paper we use the optimal map-making formalism developed for CMB analyses to extend traditional interferometric radio analysis techniques--removing the assumption of a single complex gain per antenna and allowing more complete descriptions of the instrumental and atmospheric conditions. Due to the similarity with holographic mapping of radio antenna surfaces, we call this extended analysis approach software holography. The resulting analysis algorithms are computationally efficient, unbiased, and optimally sensitive. We show how software holography can be used to solve some of the challenges of next generation observations, and how more familiar analysis techniques can be derived as limiting cases.

  14. Development of Atmospheric Monitoring System at Akeno Observatory for the Telescope Array Project

    E-Print Network [OSTI]

    T. Yamamoto; M. Teshima; M. Chikawa; N. Hayashida; S. Kawakami; N. Minagawa; Y. Morizane; M. Sasano; K. Yasui

    2002-08-09

    We have developed an atmospheric monitoring system for the Telescope Array experiment at Akeno Observatory. It consists of a Nd:YAG laser with an alt-azimuth shooting system and a small light receiver. This system is installed inside an air conditioned weather-proof dome. All parts, including the dome, laser, shooter, receiver, and optical devices are fully controlled by a personal computer utilizing the Linux operating system. It is now operated as a back-scattering LIDAR System. For the Telescope Array experiment, to estimate energy reliably and to obtain the correct shower development profile, the light transmittance in the atmosphere needs to be calibrated with high accuracy. Based on observational results using this monitoring system, we consider this LIDAR to be a very powerful technique for Telescope Array experiments. The details of this system and its atmospheric monitoring technique will be discussed.

  15. The Solar TErrestrial RElations Observatory (STEREO) mission is the third in a coordinated sequence of science missions within the Solar Terrestrial

    E-Print Network [OSTI]

    Christian, Eric

    generated by the solar dynamo. CORONAL MASS EJECTIONS One of the most important scientific advances the determination of the structure of the ambient solar wind. Two space based observatories, one drifting aheadThe Solar TErrestrial RElations Observatory (STEREO) mission is the third in a coordinated sequence

  16. 32ND INTERNATIONAL COSMIC RAY CONFERENCE, BEIJING 2011 Atmospheric "Super Test Beam" for the Pierre Auger Observatory

    E-Print Network [OSTI]

    _spokespersons@fnal.gov Abstract: We present results from 200 hours of operation of an atmospheric super test beam system developed system combines a Raman backscatter LIDAR receiver with a calibrated pulsed UV laser system to generate Facilities (CLF [1] & XLF) generate tracks that are recorded by the Auger Observatory fluorescence detector

  17. The Mauna Kea Observatories Near-Infrared Filter Set. I: Defining Optima 1-5m Bandpasses

    E-Print Network [OSTI]

    with obtaining precision photometry with the relatively wide infrared filters in use to date. Water vapor plays to be relatively immune to water vapor contamination, thereby driving filter bandwidths to be fairly narrowThe Mauna Kea Observatories Near-Infrared Filter Set. I: Defining Optima 1-5µm Bandpasses D. A

  18. Time at the Royal Observatory The rotation of the Earth gives us two kinds of time (1) ordinary

    E-Print Network [OSTI]

    Glass, Ian S.

    Time at the Royal Observatory ISG STAR TIME The rotation of the Earth gives us two kinds of time (1) ordinary Sun-related time of 24 hours and (2) Sidereal time relating to the stars. This means that a star's position in the sky is always the same at the same sidereal time. A sidereal day is shorter by about four

  19. BRUCE HOWE Chair and Professor , PhD 1986, UC San Diego. Ocean observatories, ocean acoustic tomography, sensor webs

    E-Print Network [OSTI]

    Frandsen, Jannette B.

    Faculty BRUCE HOWE Chair and Professor , PhD 1986, UC San Diego. Ocean observatories, ocean in the ocean, atmospheric and ionospheric tomography. KWOK FAI CHEUNG Professor , PhD 1991, British Columbia transport. R. CENGIZ ERTEKIN Professor, PhD 1984, UC Berkeley. Hydrodynamics/elasticity, computational

  20. Intercomparison of Biogeochemical Properties at Atlantic and Pacific Observatory Sites Using Ocean Data and a PARADIGM Model

    E-Print Network [OSTI]

    Yoder, James S.

    Intercomparison of Biogeochemical Properties at Atlantic and Pacific Observatory Sites Using Ocean compare 34 locations in the Atlantic and Pacific Oceans with respect to key upper ocean ecological by SeaWiFS mean chlorophyll: low chlorophyll ocean gyres, comparatively high chlorophyll ocean margin

  1. Dithering Strategies and Point-Source Photometry

    E-Print Network [OSTI]

    Samsing, Johan

    2011-01-01

    Strategies and Point-Source Photometry Johan Samsing DARK-The accuracy in the photometry of a point source depends onobjects in a single source photometry (Lauer 1999a) and the

  2. VOLUMETRIC SNAPPING: WATERTIGHT TRIANGULATION OF POINT CLOUDS

    E-Print Network [OSTI]

    Floater, Michael S.

    VOLUMETRIC SNAPPING: WATERTIGHT TRIANGULATION OF POINT CLOUDS Tim Volodine KULeuven, Department: meshing, surface reconstruction, volumetric grid, contouring, point clouds. Abstract: We propose, a volumetric method that does not rely on a signed distance function was proposed recently by Hornung

  3. Other Purdue Web points of Interest

    E-Print Network [OSTI]

    Other Purdue Web points of interest. Purdue University Home Page --- Schedule of Classes · Graduate School · Agronomy · Computer Science --- CS & E ...

  4. CenterPoint Energy New Homes Program

    Broader source: Energy.gov [DOE]

    Note: This program is only available to electric Customers in CenterPoint Energy's service territory (greater Houston area, Texas).

  5. SCIENCE WITH THE STELLA ROBOTIC OBSERVATORY M. Weber 1 , K. G. Strassmeier 1 , J. Bartus 1 , H. Korhonen 1 , Zs. Kovari 2 , K. Olah 2 , A. Schwope 1 , A.

    E-Print Network [OSTI]

    1 SCIENCE WITH THE STELLA ROBOTIC OBSERVATORY M. Weber 1 , K. G. Strassmeier 1 , J. Bartus 1 , H The STELLA robotic observatory is made up of two telescopes (1.2m & 0.8m), one equipped with a high res. The observatory is fully robotic, and its strengths are in long­term monitoring and survey programs on one side

  6. Critical point analysis of phase envelope diagram

    SciTech Connect (OSTI)

    Soetikno, Darmadi; Siagian, Ucok W. R.; Kusdiantara, Rudy Puspita, Dila Sidarto, Kuntjoro A. Soewono, Edy; Gunawan, Agus Y.

    2014-03-24

    Phase diagram or phase envelope is a relation between temperature and pressure that shows the condition of equilibria between the different phases of chemical compounds, mixture of compounds, and solutions. Phase diagram is an important issue in chemical thermodynamics and hydrocarbon reservoir. It is very useful for process simulation, hydrocarbon reactor design, and petroleum engineering studies. It is constructed from the bubble line, dew line, and critical point. Bubble line and dew line are composed of bubble points and dew points, respectively. Bubble point is the first point at which the gas is formed when a liquid is heated. Meanwhile, dew point is the first point where the liquid is formed when the gas is cooled. Critical point is the point where all of the properties of gases and liquids are equal, such as temperature, pressure, amount of substance, and others. Critical point is very useful in fuel processing and dissolution of certain chemicals. Here in this paper, we will show the critical point analytically. Then, it will be compared with numerical calculations of Peng-Robinson equation by using Newton-Raphson method. As case studies, several hydrocarbon mixtures are simulated using by Matlab.

  7. High-Energy Cosmic Ray Event Data from the Pierre Auger Cosmic Ray Observatory

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

    The Pierre Auger Cosmic Ray Observatory in Mendoza, Argentina is the result of an international collaboration funded by 15 countries and many different organizations. Its mission is to capture high-energy cosmic ray events or air showers for research into their origin and nature. The Pierre Auger Collaboration agreed to make 1% of its data available to the public. The Public Event Explorer is a search tool that allows users to browse or search for and display figures and data plots of events collected since 2004. The repository is updated daily, and, as of June, 2014, makes more than 35,000 events publicly available. The energy of a cosmic ray is measured in Exa electron volts or EeV. These event displays can be browsed in order of their energy level from 0.1 to 41.1 EeV. Each event has an individual identification number.

    The event displays provide station data, cosmic ray incoming direction, various energy measurements, plots, vector-based images, and an ASCII data file.

  8. Constraints on Type IIn Supernova Progenitor Outbursts from the Lick Observatory Supernova Search

    E-Print Network [OSTI]

    Bilinski, Christopher; Li, Weidong; Williams, G Grant; Zheng, WeiKang; Filippenko, Alexei V

    2015-01-01

    We searched through roughly 12 years of archival survey data acquired by the Katzman Automatic Imaging Telescope (KAIT) as part of the Lick Observatory Supernova Search (LOSS) in order to detect or place limits on possible progenitor outbursts of Type IIn supernovae (SNe~IIn). The KAIT database contains multiple pre-SN images for 5 SNe~IIn (plus one ambiguous case of a SN IIn/imposter) within 50 Mpc. No progenitor outbursts are found using the false discovery rate (FDR) statistical method in any of our targets. Instead, we derive limiting magnitudes (LMs) at the locations of the SNe. These limiting magnitudes (typically reaching $m_R \\approx 19.5\\,\\mathrm{mag}$) are compared to outbursts of SN 2009ip and $\\eta$ Car, plus additional simulated outbursts. We find that the data for SN 1999el and SN 2003dv are of sufficient quality to rule out events $\\sim40$ days before the main peak caused by initially faint SNe from blue supergiant (BSG) precursor stars, as in the cases of SN 2009ip and SN 2010mc. These SNe~IIn...

  9. The search for TeV-scale dark matter with the HAWC observatory

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

    Harding, J. Patrick

    2015-01-01

    The High Altitude Water Cherenkov (HAWC) observatory is a wide field-of-view detector sensitive to 100 GeV - 100 TeV gamma rays and cosmic rays. Located at an elevation of 4100 m on the Sierra Negra mountain in Mexico, HAWC observes extensive air showers from gamma and cosmic rays with an array of water tanks which produce Cherenkov light in the presence of air showers. With a field-of-view capable of observing 2/3 of the sky each day, and a sensitivity of 1 Crab/day, HAWC will be able to map out the sky in gamma and cosmic rays in detail. In thismore »paper, we discuss the capabilities of HAWC to map out the directions and spectra of TeV gamma rays and cosmic rays coming from sources of dark matter annihilation. We discuss the HAWC sensitivity to multiple extended sources of dark matter annihilation and the possibility of HAWC observations of annihilations in nearby dark matter subhalos.« less

  10. On the sensitivity of the HAWC observatory to gamma-ray bursts

    E-Print Network [OSTI]

    Abeysekara, A U; Aguilar, S; Alfaro, R; Almaraz, E; Álvarez, C; Álvarez-Romero, J de D; Álvarez, M; Arceo, R; Arteaga-Velázquez, J C; Badillo, C; Barber, A; Baughman, B M; Bautista-Elivar, N; Belmont, E; Benítez, E; BenZvi, S Y; Berley, D; Bernal, A; Bonamente, E; Braun, J; Caballero-Lopez, R; Cabrera, I; Carramiñana, A; Carrasco, L; Castillo, M; Chambers, L; Conde, R; Condreay, P; Cotti, U; Cotzomi, J; D'Olivo, J C; de la Fuente, E; De León, C; Delay, S; Delepine, D; DeYoung, T; Diaz, L; Diaz-Cruz, L; Dingus, B L; Duvernois, M A; Edmunds, D; Ellsworth, R W; Fick, B; Fiorino, D W; Flandes, A; Fraija, N I; Galindo, A; García-Luna, J L; García-Torales, G; Garfias, F; González, L X; González, M M; Goodman, J A; Grabski, V; Gussert, M; Guzmán-Ceron, C; Hampel-Arias, Z; Harris, T; Hays, E; Hernandez-Cervantes, L; Hüntemeyer, P H; Imran, A; Iriarte, A; Jimenez, J J; Karn, P; Kelley-Hoskins, N; Kieda, D; Langarica, R; Lara, A; Lauer, R; Lee, W H; Linares, E C; Linnemann, J T; Longo, M; Luna-García, R; Martínez, H; Martínez, J; Martínez, L A; Martínez, O; Martínez-Castro, J; Martos, M; Matthews, J; McEnery, J E; Medina-Tanco, G; Mendoza-Torres, J E; Miranda-Romagnoli, P A; Montaruli, T; Moreno, E; Mostafa, M; Napsuciale, M; Nava, J; Nellen, L; Newbold, M; Noriega-Papaqui, R; Oceguera-Becerra, T; Tapia, A Olmos; Orozco, V; Pérez, V; Pérez-Pérez, E G; Perkins, J S; Pretz, J; Ramirez, C; Ramírez, I; Rebello, D; Rentería, A; Reyes, J; Rosa-González, D; Rosado, A; Ryan, J M; Sacahui, J R; Salazar, H; Salesa, F; Sandoval, A; Santos, E; Schneider, M; Shoup, A; Silich, S; Sinnis, G; Smith, A J; Sparks, K; Springer, W; Suárez, F; Suarez, N; Taboada, I; Tellez, A F; Tenorio-Tagle, G; Tepe, A; Toale, P A; Tollefson, K; Torres, I; Ukwatta, T N; Valdes-Galicia, J; Vanegas, P; Vasileiou, V; Vázquez, O; Vázquez, X; Villaseñor, L; Wall, W; Walters, J S; Warner, D; Westerhoff, S; Wisher, I G; Wood, J; Yodh, G B; Zaborov, D; Zepeda, A

    2011-01-01

    We present the sensitivity of HAWC to Gamma Ray Bursts (GRBs). HAWC is a very high-energy gamma-ray observatory currently under construction in Mexico at an altitude of 4100 m. It will observe atmospheric air showers via the water Cherenkov method. HAWC will consist of 300 large water tanks instrumented with 4 photomultipliers each. HAWC has two data acquisition (DAQ) systems. The main DAQ system reads out coincident signals in the tanks and reconstructs the direction and energy of individual atmospheric showers. The scaler DAQ counts the hits in each photomultiplier tube (PMT) in the detector and searches for a statistical excess over the noise of all PMTs. We show that HAWC has a realistic opportunity to observe the high-energy power law components of GRBs that extend at least up to 30 GeV, as it has been observed by Fermi LAT. The two DAQ systems have an energy threshold that is low enough to observe events similar to GRB 090510 and GRB 090902b with the characteristics observed by Fermi LAT. HAWC will prov...

  11. Massive Structures of Galaxies at High Redshifts in the Great Observatories Origins Deep Survey Fields

    E-Print Network [OSTI]

    Kang, Eugene

    2016-01-01

    If the Universe is dominated by cold dark matter and dark energy as in the currently popular LCDM cosmology, it is expected that large scale structures form gradually, with galaxy clusters of mass M > ~10^14 Msun appearing at around 6 Gyrs after the Big Bang (z ~ 1). Here, we report the discovery of 59 massive structures of galaxies with masses greater than a few x 10^13 Msun at redshifts between z=0.6 and 4.5 in the Great Observatories Origins Deep Survey fields. The massive structures are identified by running top-hat filters on the two dimensional spatial distribution of magnitude-limited samples of galaxies using a combination of spectroscopic and photometric redshifts. We analyze the Millennium simulation data in a similar way to the analysis of the observational data in order to test the LCDM cosmology. We find that there are too many massive structures (M > 7 x 10^13 Msun) observed at z > 2 in comparison with the simulation predictions by a factor of a few, giving a probability of < 1/2500 of the ob...

  12. The potential of the HAWC Observatory to observe violations of Lorentz Invariance

    E-Print Network [OSTI]

    Nellen, Lukas

    2015-01-01

    The framework of relativistic quantum-field theories requires Lorentz Invariance. Many theories of quantum gravity, on the other hand, include violations of Lorentz Invariance at small scales and high energies. This generates a lot of interest in establishing limits on such effects, and, if possible, observing them directly. Gamma-ray observatories provide a tool to probe parts of the parameter space of models of Lorentz Invariance Violation that is not accessible in terrestrial laboratories and man-made accelerators. Transients, especially gamma-ray bursts, are a particularly promising class of events to search for such phenomena. By combining cosmological distances with high energy emission and short duration, emitting photons up to 30 GeV in less than a second, one can measure the energy dependence of the speed of photons to one part in $10^{16}$. We will discuss the potential of HAWC to detect effects of the violation of Lorentz Invariance and place its sensitivity in the context of existing limits.

  13. The next generation of axion helioscopes: The international axion observatory (IAXO)

    SciTech Connect (OSTI)

    Vogel, J. K. [Lawrence Livermore National Laboratory (LLNL), Livermore, CA (United States); Armengaud, E. [CEA Irfu, Centre de Saclay, Gif-sur-yvette (France); Avignone, F. T. [Univ. of South Carolina, Columbia, SC (United States); Betz, M. [European Organization for Nuclear Research (CERN), Geneve (Switzerland); Brax, P. [eIPHT, Centre d’E´tudes de Saclay (CEA-Saclay), Gif-sur-Yvette (France); Brun, P. [CEA Irfu, Centre de Saclay, Gif-sur-yvette (France); Cantatore, G. [Sezione di Trieste and Univ. di Trieste, Trieste (Italy); Carmona, J. M. [Univ. de Zaragoza, Zaragoza (Spain); Carosi, G. P. [Lawrence Livermore National Laboratory (LLNL), Livermore, CA (United States); Caspers, F. [European Organization for Nuclear Research (CERN), Geneve (Switzerland); Caspi, S. [Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States); Cetin, S. A. [Dogus Univ., Istanbul (Turkey); Chelouche, D. [Univ. of Haifa, Haifa (Israel); Christensen, F. E. [Technical Univ. of Denmark, Lyngby (Denmark); Dael, A. [CEA Irfu, Centre de Saclay, Gif-sur-yvette (France); Dafni, T. [Univ. de Zaragoza, Zaragoza (Spain); Davenport, M. [European Organization for Nuclear Research (CERN), Geneve (Switzerland); Derbin, A. V. [St. Petersburg Nuclear Physics Institute, St. Petersburg (Russia); Desch, K. [Physikalisches Institut der Univ. Bonn, Bonn (Germany); Diago, A. [Univ. de Zaragoza, Zaragoza (Spain); Döbrich, B. [Deutsches Elektronen-Synchrotron (DESY), Hamburg (Germany); Dratchnev, I. [St. Petersburg Nuclear Physics Institute, St. Petersburg (Russia); Dudarev, A. [European Organization for Nuclear Research (CERN), Geneva (Switzerland); Eleftheriadis, C. [Aristotle Univ., Thessaloniki (Greece); Fanourakis, G. [National Center for Scientific Research Demokritos, Athens (Greece); Ferrer-Ribas, E. [CEA Irfu, Centre de Saclay, Gif-sur-yvette (France); Galán, J. [CEA Irfu, Centre de Saclay, Gif-sur-yvette (France); García, J. A. [Univ. de Zaragoza, Zaragoza (Spain); Garza, J. G. [Univ. de Zaragoza, Zaragoza (Spain); Geralis, T. [National Center for Scientific Research Demokritos, Athens (Greece); Gimeno, B. [Univ. de Valencia, Valencia (Spain); Giomataris, I. [CEA Irfu, Centre de Saclay, Gif-sur-yvette (France); Gninenko, S. [Russian Academy of Sciences (RAS), Moscow (Russian Federation); Gómez, H. [Univ. de Zaragoza, Zaragoza (Spain); González-Díaz, D. [Univ. de Zaragoza, Zaragoza (Spain); Guendelman, E. [Ben Gurion Univ. Beer Sheva (Israel); Hailey, C. J. [Columbia Univ., New York, NY (United States); Hiramatsu, T. [Kyoto Univ. (Japan); Hoffmann, D. H.H. [Technische Univ. Darmstadt, Darmstadt (Germany); Horns, D. [Univ. Hamburg, Hamburg (Germany); Iguaz, F. J. [Univ. de Zaragoza, Zaragoza (Spain); Irastorza, I. G. [Univ. de Zaragoza, Zaragoza (Spain); Isern, J. [Institut de Ciencies de l'Espai, Bellaterra (Spain); Imai, K. [Univ. Heidelberg, Heidelberg (Germany); Jakobsen, A. C. [Technical Univ. of Denmark, Lyngby (Denmark); Jaeckel, J. [Univ. Heidelberg, Heidelberg (Germany); Jakov?i?, K. [Rudjer Boskovic Institute, Zagreb (Croatia); Kaminski, J. [Physikalisches Institut der Univ. Bonn, Bonn (Germany); Kawasaki, M. [Univ. of Tokyo, Tokyo (Japan); Karuza, M. [Univ. of Rijeka (Croatia); Kr?mar, M. [Rudjer Boskovic Institute, Zagreb (Croatia); Kousouris, K. [European Organization for Nuclear Research (CERN), Geneve (Switzerland); Krieger, C. [Physikalisches Institut der Univ. Bonn, Bonn (Germany); Laki?, B. [Rudjer Boskovic Institute, Zagreb (Croatia); Limousin, O. [CEA Irfu, Gif-sur-Yvette (France); Lindner, A. [Deutsches Elektronen-Synchrotron (DESY), Hamburg (Germany); Liolios, A. [Aristotle Univ., Thessaloniki (Greece); Luzón, G. [Univ. de Zaragoza, Zaragoza (Spain); Matsuki, S. [Kyoto Univ., Kyoto (Japan); Muratova, V. N. [St. Petersburg Nuclear Physics Institute, St. Petersburg (Russia); Nones, C. [CEA Irfu, Gif-sur-Yvette (France); Ortega, I. [Univ. de Zaragoza, Zaragoza (Spain); Papaevangelou, T. [CEA Irfu, Centre de Saclay, Gif-sur-yvette (France); Pivovaroff, M. J. [Lawrence Livermore National Laboratory (LLNL), Livermore, CA (United States)

    2015-01-01

    The International Axion Observatory (IAXO) is a proposed 4th-generation axion helioscope with the primary physics research goal to search for solar axions via their Primakoff conversion into photons of 1 – 10 keV energies in a strong magnetic field. IAXO will achieve a sensitivity to the axion-photon coupling ga? down to a few ×10?¹² GeV?¹ for a wide range of axion masses up to ~ 0.25 eV. This is an improvement over the currently best (3rd generation) axion helioscope, the CERN Axion Solar Telescope (CAST), of about 5 orders of magnitude in signal strength, corresponding to a factor ~ 20 in the axion photon coupling. IAXO’s sensitivity relies on the construction of a large superconducting 8-coil toroidal magnet of 20 m length optimized for axion research. Each of the eight 60 cm diameter magnet bores is equipped with x-ray optics focusing the signal photons into ~ 0.2 cm² spots that are imaged by very low background x-ray detectors. The magnet will be built into a structure with elevation and azimuth drives that will allow solar tracking for 12 hours each day. This contribution is a summary of our papers [1, 2, 3] and we refer to these for further details.

  14. The next generation of axion helioscopes: The international axion observatory (IAXO)

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

    Vogel, J. K.; Armengaud, E.; Avignone, F. T.; Betz, M.; Brax, P.; Brun, P.; Cantatore, G.; Carmona, J. M.; Carosi, G. P.; Caspers, F.; et al

    2015-03-24

    The International Axion Observatory (IAXO) is a proposed 4th-generation axion helioscope with the primary physics research goal to search for solar axions via their Primakoff conversion into photons of 1 – 10 keV energies in a strong magnetic field. IAXO will achieve a sensitivity to the axion-photon coupling ga? down to a few ×10?¹² GeV?¹ for a wide range of axion masses up to ~ 0.25 eV. This is an improvement over the currently best (3rd generation) axion helioscope, the CERN Axion Solar Telescope (CAST), of about 5 orders of magnitude in signal strength, corresponding to a factor ~ 20more »in the axion photon coupling. IAXO’s sensitivity relies on the construction of a large superconducting 8-coil toroidal magnet of 20 m length optimized for axion research. Each of the eight 60 cm diameter magnet bores is equipped with x-ray optics focusing the signal photons into ~ 0.2 cm² spots that are imaged by very low background x-ray detectors. The magnet will be built into a structure with elevation and azimuth drives that will allow solar tracking for 12 hours each day. This contribution is a summary of our papers [1, 2, 3] and we refer to these for further details.« less

  15. Measurement of radium concentration in water with Mn-coated beads at the Sudbury Neutrino Observatory

    E-Print Network [OSTI]

    T. C. Andersen

    2003-04-01

    We describe a method to measure the concentration of 224Ra and 226Ra in the heavy water target used to detect solar neutrinos at the Sudbury Neutrino Observatory and in the surrounding light water shielding. A water volume of (50-400) m^3 from the detector is passed through columns which contain beads coated with a compound of manganese oxide onto which the Ra dissolved in the water is adsorbed. The columns are removed, dried, and mounted below an electrostatic chamber into which the Rn from the decay of trapped Ra is continuously flowed by a stream of nitrogen gas. The subsequent decay of Rn gives charged Po ions which are swept by the electric field onto a solid-state alpha counter. The content of Ra in the water is inferred from the measured decay rates of 212Po, 214Po, 216Po, and 218Po. The Ra extraction efficiency is >95%, the counting efficiency is 24% for 214Po and 6% for 216Po, and the method can detect a few atoms of 224Ra per m^3 and a few tens of thousands of atoms of 226Ra per m^3. Converted to equivalent equilibrium values of the topmost elements of the natural radioactive chains, the detection limit in a single assay is a few times 10^(-16) g Th or U/cm^3. The results of some typical assays are presented and the contributions to the systematic error are discussed.

  16. HOMOLOGOUS FLUX ROPES OBSERVED BY THE SOLAR DYNAMICS OBSERVATORY ATMOSPHERIC IMAGING ASSEMBLY

    SciTech Connect (OSTI)

    Li, Ting; Zhang, Jun E-mail: zjun@nao.cas.cn

    2013-12-01

    We present the first Solar Dynamics Observatory observations of four homologous flux ropes in the active region (AR) 11745 on 2013 May 20-22. The four flux ropes are all above the neutral line of the AR, with endpoints anchoring at the same region, and have a generally similar morphology. The first three flux ropes rose with a velocity of less than 30 km s{sup –1} after their appearance, and subsequently their intensities at 131 Å decreased and the flux ropes became obscure. The fourth flux rope erupted last, with a speed of about 130 km s{sup –1} and formed a coronal mass ejection (CME). The associated filament showed an obvious anti-clockwise twist motion at the initial stage, and the twist was estimated at 4?. This indicates that kink instability possibly triggers the early rise of the fourth flux rope. The activated filament material was spatially within the flux rope and showed consistent evolution in the early stages. Our findings provide new clues for understanding the characteristics of flux ropes. Firstly, multiple flux ropes are successively formed at the same location during an AR evolution process. Secondly, a slow-rise flux rope does not necessarily result in a CME, and a fast-eruption flux rope does result in a CME.

  17. THREE-DIMENSIONAL RECONSTRUCTION OF AN ERUPTING FILAMENT WITH SOLAR DYNAMICS OBSERVATORY AND STEREO OBSERVATIONS

    SciTech Connect (OSTI)

    Li Ting; Zhang Jun; Zhang Yuzong; Yang Shuhong E-mail: zjun@nao.cas.cn

    2011-09-20

    On 2010 August 1, a global solar event was launched involving almost the entire Earth-facing side of the Sun. This event mainly consisted of a C3.2 flare, a polar crown filament eruption, and two Earth-directed coronal mass ejections. The observations from the Solar Dynamics Observatory (SDO) and STEREO showed that all the activities were coupled together, suggesting a global character of the magnetic eruption. We reconstruct the three-dimensional geometry of the polar crown filament using observations from three different viewpoints (STEREO A, STEREO B, and SDO) for the first time. The filament undergoes two eruption processes. First, the main body of the filament rises up, while it also moves toward the low-latitude region with a change in inclination by {approx}48{sup 0} and expands only in the altitudinal and latitudinal direction in the field of view of the Atmospheric Imaging Assembly. We investigate the true velocities and accelerations of different locations along the filament and find that the highest location always has the largest acceleration during this eruption process. During the late phase of the first eruption, part of the filament material separates from the eastern leg. This material displays a projectile motion and moves toward the west at a constant velocity of 141.8 km s{sup -1}. This may imply that the polar crown filament consists of at least two groups of magnetic systems.

  18. An array of low-background $^3$He proportional counters for the Sudbury Neutrino Observatory

    E-Print Network [OSTI]

    J. F. Amsbaugh; J. M. Anaya; J. Banar; T. J. Bowles; M. C. Browne; T. V. Bullard; T. H. Burritt; G. A. Cox-Mobrand; X. Dai; H. Deng; M. Di Marco; P. J. Doe; M. R. Dragowsky; C. A. Duba; F. A. Duncan; E. D. Earle; S. R. Elliott; E. -I. Esch; H. Fergani; J. A. Formaggio; M. M. Fowler; J. E. Franklin; P. Geissbühler; J. V. Germani; A. Goldschmidt; E. Guillian; A. L. Hallin; G. Harper; P. J. Harvey; R. Hazama; K. M. Heeger; J. Heise; A. Hime; M. A. Howe; M. Huang; L. L. Kormos; C. Kraus; C. B. Krauss; J. Law; I. T. Lawson; K. T. Lesko; J. C. Loach; S. Majerus; J. Manor; S. McGee; K. K. S. Miknaitis; G. G. Miller; B. Morissette; A. Myers; N. S. Oblath; H. M. O'Keeffe; R. W. Ollerhead; S. J. M. Peeters; A. W. P. Poon; G. Prior; S. D. Reitzner; K. Rielage; R. G. H. Robertson; P. Skensved; A. R. Smith; M. W. E. Smith; T. D. Steiger; L. C. Stonehill; P. M. Thornewell; N. Tolich; B. A. VanDevender; T. D. Van Wechel; B. L. Wall; H. Wan Chan Tseung; J. Wendland; N. West; J. B. Wilhelmy; J. F. Wilkerson; J. M. Wouters

    2007-05-23

    An array of Neutral-Current Detectors (NCDs) has been built in order to make a unique measurement of the total active flux of solar neutrinos in the Sudbury Neutrino Observatory (SNO). Data in the third phase of the SNO experiment were collected between November 2004 and November 2006, after the NCD array was added to improve the neutral-current sensitivity of the SNO detector. This array consisted of 36 strings of proportional counters filled with a mixture of $^3$He and CF$_4$ gas capable of detecting the neutrons liberated by the neutrino-deuteron neutral current reaction in the D$_2$O, and four strings filled with a mixture of $^4$He and CF$_4$ gas for background measurements. The proportional counter diameter is 5 cm. The total deployed array length was 398 m. The SNO NCD array is the lowest-radioactivity large array of proportional counters ever produced. This article describes the design, construction, deployment, and characterization of the NCD array, discusses the electronics and data acquisition system, and considers event signatures and backgrounds.

  19. Physics Potential of the ICAL detector at the India-based Neutrino Observatory (INO)

    E-Print Network [OSTI]

    The ICAL Collaboration; Shakeel Ahmed; M. Sajjad Athar; Rashid Hasan; Mohammad Salim; S. K. Singh; S. S. R. Inbanathan; Venktesh Singh; V. S. Subrahmanyam; Shiba Prasad Behera; Vinay B. Chandratre; Nitali Dash; Vivek M. Datar; V. K. S. Kashyap; Ajit K. Mohanty; Lalit M. Pant; Animesh Chatterjee; Sandhya Choubey; Raj Gandhi; Anushree Ghosh; Deepak Tiwari; Ali Ajmi; S. Uma Sankar; Prafulla Behera; Aleena Chacko; Sadiq Jafer; James Libby; K. Raveendrababu; K. R. Rebin; D. Indumathi; K. Meghna; S. M. Lakshmi; M. V. N. Murthy; Sumanta Pal; G. Rajasekaran; Nita Sinha; Sanjib Kumar Agarwalla; Amina Khatun; Poonam Mehta; Vipin Bhatnagar; R. Kanishka; A. Kumar; J. S. Shahi; J. B. Singh; Monojit Ghosh; Pomita Ghoshal; Srubabati Goswami; Chandan Gupta; Sushant Raut; Sudeb Bhattacharya; Suvendu Bose; Ambar Ghosal; Abhik Jash; Kamalesh Kar; Debasish Majumdar; Nayana Majumdar; Supratik Mukhopadhyay; Satyajit Saha; B. S. Acharya; Sudeshna Banerjee; Kolahal Bhattacharya; Sudeshna Dasgupta; Moon Moon Devi; Amol Dighe; Gobinda Majumder; Naba K. Mondal; Asmita Redij; Deepak Samuel; B. Satyanarayana; Tarak Thakore; C. D. Ravikumar; A. M. Vinodkumar; Gautam Gangopadhyay; Amitava Raychaudhuri; Brajesh C. Choudhary; Ankit Gaur; Daljeet Kaur; Ashok Kumar; Sanjeev Kumar; Md. Naimuddin; Waseem Bari; Manzoor A. Malik; Jyotsna Singh; S. Krishnaveni; H. B. Ravikumar; C. Ranganathaiah; Swapna Mahapatra; Saikat Biswas; Subhasis Chattopadhyay; Rajesh Ganai; Tapasi Ghosh; Y. P. Viyogi

    2015-05-27

    The upcoming 50 kt magnetized iron calorimeter (ICAL) detector at the India-based Neutrino Observatory (INO) is designed to study the atmospheric neutrinos and antineutrinos separately over a wide range of energies and path lengths. The primary focus of this experiment is to explore the Earth matter effects by observing the energy and zenith angle dependence of the atmospheric neutrinos in the multi-GeV range. This study will be crucial to address some of the outstanding issues in neutrino oscillation physics, including the fundamental issue of neutrino mass hierarchy. In this document, we present the physics potential of the detector as obtained from realistic detector simulations. We describe the simulation framework, the neutrino interactions in the detector, and the expected response of the detector to particles traversing it. The ICAL detector can determine the energy and direction of the muons to a high precision, and in addition, its sensitivity to multi-GeV hadrons increases its physics reach substantially. Its charge identification capability, and hence its ability to distinguish neutrinos from antineutrinos, makes it an efficient detector for determining the neutrino mass hierarchy. In this report, we outline the analyses carried out for the determination of neutrino mass hierarchy and precision measurements of atmospheric neutrino mixing parameters at ICAL, and give the expected physics reach of the detector with 10 years of runtime. We also explore the potential of ICAL for probing new physics scenarios like CPT violation and the presence of magnetic monopoles.

  20. Hadron energy response of the Iron Calorimeter detector at the India-based Neutrino Observatory

    E-Print Network [OSTI]

    Moon Moon Devi; Anushree Ghosh; Daljeet Kaur; Lakshmi S. Mohan; Sandhya Choubey; Amol Dighe; D. Indumathi; Sanjeev Kumar; M. V. N. Murthy; Md. Naimuddin

    2013-10-30

    The results of a Monte Carlo simulation study of the hadron energy response for the magnetized Iron CALorimeter detector, ICAL, proposed to be located at the India-based Neutrino Observatory (INO) is presented. Using a GEANT4 modeling of the detector ICAL, interactions of atmospheric neutrinos with target nuclei are simulated. The detector response to hadrons propagating through it is investigated using the hadron hit multiplicity in the active detector elements. The detector response to charged pions of fixed energy is studied first, followed by the average response to the hadrons produced in atmospheric neutrino interactions using events simulated with the NUANCE event generator. The shape of the hit distribution is observed to fit the Vavilov distribution, which reduces to a Gaussian at high energies. In terms of the parameters of this distribution, we present the hadron energy resolution as a function of hadron energy, and the calibration of hadron energy as a function of the hit multiplicity. The energy resolution for hadrons is found to be in the range 85% (for 1GeV) -- 36% (for 15 GeV).

  1. The search for TeV-scale dark matter with the HAWC observatory

    SciTech Connect (OSTI)

    Harding, J. Patrick [Los Alamos National Lab. (LANL), Los Alamos, NM (United States)

    2015-01-01

    The High Altitude Water Cherenkov (HAWC) observatory is a wide field-of-view detector sensitive to 100 GeV - 100 TeV gamma rays and cosmic rays. Located at an elevation of 4100 m on the Sierra Negra mountain in Mexico, HAWC observes extensive air showers from gamma and cosmic rays with an array of water tanks which produce Cherenkov light in the presence of air showers. With a field-of-view capable of observing 2/3 of the sky each day, and a sensitivity of 1 Crab/day, HAWC will be able to map out the sky in gamma and cosmic rays in detail. In this paper, we discuss the capabilities of HAWC to map out the directions and spectra of TeV gamma rays and cosmic rays coming from sources of dark matter annihilation. We discuss the HAWC sensitivity to multiple extended sources of dark matter annihilation and the possibility of HAWC observations of annihilations in nearby dark matter subhalos.

  2. Evaluation of expected solar flare neutrino events in the IceCube observatory

    E-Print Network [OSTI]

    de Wasseige, G; Hanson, K; van Eijndhoven, N; Klein, K -L

    2015-01-01

    Since the end of the eighties and in response to a reported increase in the total neutrino flux in the Homestake experiment in coincidence with a solar flare, solar neutrino detectors have searched for solar flare signals. Neutrinos from the decay of mesons, which are themselves produced in collisions of accelerated protons with the solar atmosphere, would provide a novel window on the underlying physics of the acceleration process. For our studies we focus on the IceCube Neutrino Observatory, a cubic kilometer neutrino detector located at the geographical South Pole. Due to its Supernova data acquisition system and its DeepCore component, dedicated to low energy neutrinos, IceCube may be sensitive to solar flare neutrinos and thus permit either a measurement of the signal or the establishment of more stringent upper limits on the solar flare neutrino flux. We present an approach for a time profile analysis based on a stacking method and an evaluation of a possible solar flare signal in IceCube using the Gean...

  3. PURE STRATEGY NASH EQUILIBRIUM POINTS AND THE LEFSCHETZ FIXED POINT THEOREM

    E-Print Network [OSTI]

    Tesfatsion, Leigh

    PURE STRATEGY NASH EQUILIBRIUM POINTS AND THE LEFSCHETZ FIXED POINT THEOREM by Leigh Tesfatsion of Minnesota Minneapolis, Minnesota 55455 #12;ABSTRAcr A pure strategy Nash equilibrium point existence theorem cases of the existence theorem are also discussed. #12;PURE STRATEGY NASH EQUILIBRIUM POINTS

  4. Weather induced effects on extensive air showers observed with the surface detector of the Pierre Auger Observatory

    E-Print Network [OSTI]

    Carla Bleve; for the Pierre Auger Collaboration

    2007-06-11

    The rate of events measured with the surface detector of the Pierre Auger Observatory is found to be modulated by the weather conditions. This effect is due to the increasing amount of matter traversed by the shower as the ground pressure increases and to the inverse proportionality of the Moliere radius to the air density near ground. Air-shower simulations with different realistic profiles of the atmosphere support this interpretation of the observed effects.

  5. Measurement of the Proton-Air Cross Section at ?s=57 TeV with the Pierre Auger Observatory

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

    Abreu, P.; Aglietta, M.; Ahn, E. J.; Albuquerque, I. F. M.; Allard, D.; Allekotte, I.; Allen, J.; Allison, P.; Almeda, A.; Alvarez Castillo, J.; et al

    2012-08-10

    We report a measurement of the proton-air cross section for particle production at the center-of-mass energy per nucleon of 57 TeV. This is derived from the distribution of the depths of shower maxima observed with the Pierre Auger Observatory: systematic uncertainties are studied in detail. Analyzing the tail of the distribution of the shower maxima, a proton-air cross section of [505±22(stat)+28-36(syst)] mb is found.

  6. Building Green in Greensburg: Prairie Pointe Townhomes

    Office of Energy Efficiency and Renewable Energy (EERE)

    This poster highlights energy efficiency, renewable energy, and sustainable features of the high-performing Prairie Pointe Townhomes in Greensburg, Kansas.

  7. VPP Points of Contact web version 07092015

    Office of Environmental Management (EM)

    Updated 792015 VPP POINTS OF CONTACT Organization DOE POC Contractor DOE Federal POC Advanced Technologies and Laboratories International, Inc. (ATL)222-S Laboratory Analytical...

  8. SIMPLE EXPLICIT FORMULA FOR COUNTING LATTICE POINTS ...

    E-Print Network [OSTI]

    2007-02-14

    by a simple formula involving the evaluation of ? zx over the integral points of those ... different) formula from a decomposition of the generating function into.

  9. HOLOMORPHIC ONE FORMS, INTEGRAL AND RATIONAL POINTS ...

    E-Print Network [OSTI]

    2014-09-23

    Abstract The first goal of this paper is to study the question of finiteness of integral points on a cofinite non-compact complex two dimensional ball quotient ...

  10. Wisconsin Nuclear Profile - Point Beach Nuclear Plant

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

    Point Beach Nuclear Plant" "Unit","Summer capacity (mw)","Net generation (thousand mwh)","Summer capacity factor (percent)","Type","Commercial operation date","License expiration...

  11. New York Nuclear Profile - Indian Point

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

    Indian Point" "Unit","Summer capacity (mw)","Net generation (thousand mwh)","Summer capacity factor (percent)","Type","Commercial operation date","License expiration date"...

  12. Wolf Point Substation, Roosevelt County, Montana

    SciTech Connect (OSTI)

    Not Available

    1991-05-01

    The Western Area Power Administration (Western), an agency of the United States Department of Energy, is proposing to construct the 115-kV Wolf Point Substation near Wolf Point in Roosevelt County, Montana (Figure 1). As part of the construction project, Western's existing Wolf Point Substation would be taken out of service. The existing 115-kV Wolf Point Substation is located approximately 3 miles west of Wolf Point, Montana (Figure 2). The substation was constructed in 1949. The existing Wolf Point Substation serves as a Switching Station'' for the 115-kV transmission in the region. The need for substation improvements is based on operational and reliability issues. For this environmental assessment (EA), the environmental review of the proposed project took into account the removal of the old Wolf Point Substation, rerouting of the five Western lines and four lines from the Cooperatives and Montana-Dakota Utilities Company, and the new road into the proposed substation. Reference to the new proposed Wolf Point Substation in the EA includes these facilities as well as the old substation site. The environmental review looked at the impacts to all resource areas in the Wolf Point area. 7 refs., 6 figs.

  13. EMERGING DIMMINGS OF ACTIVE REGIONS OBSERVED BY THE SOLAR DYNAMICS OBSERVATORY

    SciTech Connect (OSTI)

    Zhang Jun; Yang Shuhong [Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012 (China); Liu Yang; Sun Xudong, E-mail: zjun@nao.cas.cn, E-mail: shuhongyang@nao.cas.cn, E-mail: yliu@sun.stanford.edu, E-mail: xudong@sun.stanford.edu [W. W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305-4085 (United States)

    2012-12-01

    Using the observations from the Atmospheric Imaging Assembly and the Helioseismic and Magnetic Imager on board the Solar Dynamics Observatory, we statistically investigate the emerging dimmings (EDs) of 24 isolated active regions (IARs) from 2010 June to 2011 May. All the IARs show EDs in lower-temperature lines (e.g., 171 A) at their early emerging stages. Meanwhile, in higher temperature lines (e.g., 211 A), the ED regions brighten continuously. There are two types of EDs: fan-shaped and halo-shaped. There are 19 fan-shaped EDs and 5 halo-shaped ones. The EDs appear to be delayed by several to more than ten hours relative to the first emergence of the IARs. The shortest delay is 3.6 hr and the longest is 19.0 hr. The EDs last from 3.3 hr to 14.2 hr, with a mean duration of 8.3 hr. Before the appearance of the EDs, the emergence rate of the magnetic flux of the IARs is between 1.2 Multiplication-Sign 10{sup 19} Mx hr{sup -1} to 1.4 Multiplication-Sign 10{sup 20} Mx hr{sup -1}. The larger the emergence rate is, the shorter the delay time is. While the dimmings appear, the magnetic flux of the IARs ranges from 8.8 Multiplication-Sign 10{sup 19} Mx to 1.3 Multiplication-Sign 10{sup 21} Mx. These observations imply that the reconfiguration of the coronal magnetic fields due to reconnection between the newly emerging flux and the surrounding existing fields results in a new thermal distribution which leads to a dimming for the cooler channel (171 A) and brightening in the warmer channels.

  14. URBAN ATMOSPHERIC OBSERVATORY (UAO) FIRST PLANNING WORKSHOP, JANUARY 27-28-2003. WORKSHOP SUMMARY.

    SciTech Connect (OSTI)

    REYNOLDS,R.M.; LEE,H.N.

    2003-03-27

    The Urban Atmospheric Observatory (UAO) First Planning Workshop was held on 27-28 January 2003 at the Environmental Measurements Laboratory (EML) in downtown Manhattan, New York City. The meeting was well attended by local, state, and national administrators, as well as scientists and engineers from the national laboratories and academia. The real-time intensive UAO is a necessary step toward the development and validation of new technologies in support of the New York City emergency management and anti-terrorism effort. The real-time intensive UAO will be a dense array of meteorological instrumentation, remote sensing and satellite products and model output, as well as radiation detection, gamma spectrometer and aerosol measurements focused onto a small area in the heart of Manhattan. Such a test-bed, developed in a somewhat homogeneous urban area, and with a well-developed communication and data collection backbone, will be of immense utility for understanding how models of all scales can be improved and how they can best be integrated into the city's emergency program. The goal of the First Planning Workshop was to bring together a small group of experts in the fields of urban meteorology, modeling from mesoscale to fine-mesh computational fluid dynamics, instrumentation, communications and visualization, in order to (1) establish the importance of the observational program, (2) define the most efficient and cost-effective design for the program, (3) define needed intensive observational efforts and establish a schedule, and (4) define the importance of the UAO in emergency operations. The workshop achieved its goals with the enthusiastic participation of over forty persons. There was a synthesis of ideas towards a world-class facility that would benefit both immediate emergency management activities and, over an extended time, the entire field of urban meteorology and contaminant dispersion modeling.

  15. On Robust Regression in Photogrammetric Point Clouds

    E-Print Network [OSTI]

    Schindler, Konrad

    On Robust Regression in Photogrammetric Point Clouds Konrad Schindler and Horst Bischof Institute,bischof}@icg.tu-graz.ac.at Abstract. Many applications in computer vision require robust linear regression on photogrammetrically for robust regression are based on distance measures from the regression surface to the points

  16. Traveling water waves with point vortices

    E-Print Network [OSTI]

    Kristoffer Varholm

    2015-03-20

    We construct small-amplitude solitary traveling gravity-capillary water waves with a finite number of point vortices along a vertical line, on finite depth. This is done using a local bifurcation argument. The properties of the resulting waves are also examined: We find that they depend significantly on the position of the point vortices in the water column.

  17. Three-point spherical mirror mount

    DOE Patents [OSTI]

    Cutburth, R.W.

    1984-01-23

    A three-point spherical mirror mount for use with lasers is disclosed. The improved mirror mount is adapted to provide a pivot ring having an outer surface with at least three spaced apart mating points to engage an inner spherical surface of a support housing.

  18. Interaction between Injection Points during Hydraulic Fracturing

    E-Print Network [OSTI]

    Hals, Kjetil M D

    2012-01-01

    We present a model of the hydraulic fracturing of heterogeneous poroelastic media. The formalism is an effective continuum model that captures the coupled dynamics of the fluid pressure and the fractured rock matrix and models both the tensile and shear failure of the rock. As an application of the formalism, we study the geomechanical stress interaction between two injection points during hydraulic fracturing (hydrofracking) and how this interaction influences the fracturing process. For injection points that are separated by less than a critical correlation length, we find that the fracturing process around each point is strongly correlated with the position of the neighboring point. The magnitude of the correlation length depends on the degree of heterogeneity of the rock and is on the order of 30-45 m for rocks with low permeabilities. In the strongly correlated regime, we predict a novel effective fracture-force that attracts the fractures toward the neighboring injection point.

  19. Soil Temperatures at Armagh Observatory, N. Ireland, from 1904 to 2002

    E-Print Network [OSTI]

    sites have positive slopes in all seasons which vary from 0.04 to 0.25 o C/decade, depending on the season, depth and location. There appear to be some geographical di#11;erences, with relatively shallow. (2002) have pointed out that the amplitude of the annual variation in heat storage of the top 5m of soil

  20. Observations of comet ISON (C/2012 S1) from Lowell observatory

    SciTech Connect (OSTI)

    Knight, Matthew M.; Schleicher, David G.

    2015-01-01

    We observed the dynamically new sungrazing comet ISON (C/2012 S1) extensively at Lowell Observatory throughout 2013 in order to characterize its behavior prior to perihelion. ISON had “typical” abundances for an Oort Cloud comet. Its dust production, as measured by Af?, remained nearly constant during the apparition but its CN gas production increased by ?50 ×. The minimum active area necessary to support observed water production rates exceeded the likely surface area of the nucleus and suggests a population of icy grains in the coma. Together with the flattening of the dust radial profile over time, this is consistant with ejection of a large quantity of slow moving dust and icy grains in the coma at large heliocentric distance. The dust morphology was dominated by the tail, but a faint sunward dust fan was detected in March, April, May, and September. We imaged multiple gas species in September, October, and November. All gas species were more extended than the dust coma, although only CN had sufficient signal-to-noise for detailed morphological study. Excess CN signal was observed in the sunward hemisphere in September and early October. In November the excess CN signal was in the tailward hemisphere and two faint CN features appeared approximately orthogonal to the tail with position angles varying by about ±20° from night to night. Using numerical modeling, we best reproduced the orientation and shape of these features as well as the bulk brightness with a pole oriented approximately toward the Sun and a single source located within ?35° of the equator. Variations in position angle and relative brightness of the CN features from night to night suggest a rotation period shorter than 24 hr. The production rates and coma morphology suggest a nucleus that was active over nearly its entire sunward facing hemisphere in September and October but which underwent a significant mass loss event, potentially including fragmentation, shortly before November 1. Significant subsequent mass loss likely continued at the same site over subsequent days/weeks and may have catastrophically weakened the nucleus prior to perihelion.

  1. POLYNOMIAL PARTITIONING ON VARIETIES AND POINT ...

    E-Print Network [OSTI]

    2014-06-09

    Jun 9, 2014 ... breakthrough in a long-standing problem of Erd?os on the number of distinct dis- tances between a n points in the plane, by nearly proving the ...

  2. CenterPoint Energy Sustainable Schools Program

    Broader source: Energy.gov [DOE]

    The Sustainable Schools Program focuses on energy savings through behavioral and operational improvements, and may be used along with CenterPoint Energy’s SCORES and Load Management programs. It...

  3. Critical-Point Structure in Finite Nuclei

    E-Print Network [OSTI]

    A. Leviatan

    2006-12-04

    Properties of quantum shape-phase transitions in finite nuclei are considered in the framework of the interacting boson model. Special emphasis is paid to the dynamics at the critical-point of a general first-order phase transition.

  4. CenterPoint Energy's Energy Wise Program

    Broader source: Energy.gov [DOE]

    CenterPoint Energy's Energy Wise program provides take-home kits containing efficiency devices with classroom and in-home education techniques with the aim to inspire families to adopt new resource...

  5. Measurement of the Proton-Air Cross Section at ?s=57 TeV with the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Abreu, P.; Aglietta, M.; Ahn, E. J.; Albuquerque, I. F. M.; Allard, D.; Allekotte, I.; Allen, J.; Allison, P.; Almeda, A.; Alvarez Castillo, J.; Alvarez-Muñiz, J.; Ambrosio, M.; Aminaei, A.; Anchordoqui, L.; Andringa, S.; Anti?i?, T.; Aramo, C.; Arganda, E.; Arqueros, F.; Asorey, H.; Assis, P.; Aublin, J.; Ave, M.; Avenier, M.; Avila, G.; Bäcker, T.; Balzer, M.; Barber, K. B.; Barbosa, A. F.; Bardenet, R.; Barroso, S. L. C.; Baughman, B.; Bäuml, J.; Beatty, J. J.; Becker, B. R.; Becker, K. H.; Bellétoile, A.; Bellido, J. A.; BenZvi, S.; Berat, C.; Bertou, X.; Biermann, P. L.; Billoir, P.; Blanco, F.; Blanco, M.; Bleve, C.; Blümer, H.; Bohá?ová, M.; Boncioli, D.; Bonifazi, C.; Bonino, R.; Borodai, N.; Brack, J.; Brogueira, P.; Brown, W. C.; Bruijn, R.; Buchholz, P.; Bueno, A.; Burton, R. E.; Caballero-Mora, K. S.; Caramete, L.; Caruso, R.; Castellina, A.; Catalano, O.; Cataldi, G.; Cazon, L.; Cester, R.; Chauvin, J.; Cheng, S. H.; Chiavassa, A.; Chinellato, J. A.; Chirinos Diaz, J.; Chudoba, J.; Clay, R. W.; Coluccia, M. R.; Conceição, R.; Contreras, F.; Cook, H.; Cooper, M. J.; Coppens, J.; Cordier, A.; Coutu, S.; Covault, C. E.; Creusot, A.; Criss, A.; Cronin, J.; Curutiu, A.; Dagoret-Campagne, S.; Dallier, R.; Dasso, S.; Daumiller, K.; Dawson, B. R.; de Almeida, R. M.; De Domenico, M.; De Donato, C.; de Jong, S. J.; De La Vega, G.; de Mello Junior, W. J. M.; de Mello Neto, J. R. T.; De Mitri, I.; de Souza, V.; de Vries, K. D.; Decerprit, G.; del Peral, L.; del Río, M.; Deligny, O.; Dembinski, H.; Dhital, N.; Di Giulio, C.; Díaz Castro, M. L.; Diep, P. N.; Dobrigkeit, C.; Docters, W.; D’Olivo, J. C.; Dong, P. N.; Dorofeev, A.; dos Anjos, J. C.; Dova, M. T.; D’Urso, D.; Dutan, I.; Ebr, J.; Engel, R.; Erdmann, M.; Escobar, C. O.; Espadanal, J.; Etchegoyen, A.; Facal San Luis, P.; Fajardo Tapia, I.; Falcke, H.; Farrar, G.; Fauth, A. C.; Fazzini, N.; Ferguson, A. P.; Ferrero, A.; Fick, B.; Filevich, A.; Filip?i?, A.; Fliescher, S.; Fracchiolla, C. E.; Fraenkel, E. D.; Fröhlich, U.; Fuchs, B.; Gaior, R.; Gamarra, R. F.; Gambetta, S.; García, B.; Garcia-Gamez, D.; Garcia-Pinto, D.; Gascon, A.; Gemmeke, H.; Gesterling, K.; Ghia, P. L.; Giaccari, U.; Giller, M.; Glass, H.; Gold, M. S.; Golup, G.; Gomez Albarracin, F.; Gómez Berisso, M.; Gonçalves, P.; Gonzalez, D.; Gonzalez, J. G.; Gookin, B.; Góra, D.; Gorgi, A.; Gouffon, P.; Gozzini, S. R.; Grashorn, E.; Grebe, S.; Griffith, N.; Grigat, M.; Grillo, A. F.; Guardincerri, Y.; Guarino, F.; Guedes, G. P.; Guzman, A.; Hague, J. D.; Hansen, P.; Harari, D.; Harmsma, S.; Harrison, T. A.; Harton, J. L.; Haungs, A.; Hebbeker, T.; Heck, D.; Herve, A. E.; Hojvat, C.; Hollon, N.; Holmes, V. C.; Homola, P.; Hörandel, J. R.; Horneffer, A.; Horvath, P.; Hrabovský, M.; Huege, T.; Insolia, A.; Ionita, F.; Italiano, A.; Jarne, C.; Jiraskova, S.; Josebachuili, M.; Kadija, K.; Kampert, K. H.; Karhan, P.; Kasper, P.; Kégl, B.; Keilhauer, B.; Keivani, A.; Kelley, J. L.; Kemp, E.; Kieckhafer, R. M.; Klages, H. O.; Kleifges, M.; Kleinfeller, J.; Knapp, J.; Koang, D.-H.; Kotera, K.; Krohm, N.; Krömer, O.; Kruppke-Hansen, D.; Kuehn, F.; Kuempel, D.; Kulbartz, J. K.; Kunka, N.; La Rosa, G.; Lachaud, C.; Lauer, R.; Lautridou, P.; Le Coz, S.; Leão, M. S. A. B.; Lebrun, D.; Lebrun, P.; Leigui de Oliveira, M. A.; Lemiere, A.; Letessier-Selvon, A.; Lhenry-Yvon, I.; Link, K.; López, R.; Lopez Agüera, A.; Louedec, K.; Lozano Bahilo, J.; Lu, L.; Lucero, A.; Ludwig, M.; Lyberis, H.; Macolino, C.; Maldera, S.; Mandat, D.; Mantsch, P.; Mariazzi, A. G.; Marin, J.; Marin, V.; Maris, I. C.; Marquez Falcon, H. R.; Marsella, G.; Martello, D.; Martin, L.; Martinez, H.; Martínez Bravo, O.; Mathes, H. J.; Matthews, J.; Matthews, J. A. J.; Matthiae, G.; Maurizio, D.; Mazur, P. O.; Medina-Tanco, G.; Melissas, M.; Melo, D.; Menichetti, E.; Menshikov, A.; Mertsch, P.; Meurer, C.; Mi?anovi?, S.; Micheletti, M. I.; Miller, W.; Miramonti, L.; Molina-Bueno, L.; Mollerach, S.; Monasor, M.; Monnier Ragaigne, D.; Montanet, F.; Morales, B.; Morello, C.; Moreno, E.; Moreno, J. C.; Morris, C.; Mostafá, M.; Moura, C. A.; Mueller, S.; Muller, M. A.; Müller, G.; Münchmeyer, M.; Mussa, R.; Navarra, G.; Navarro, J. L.; Navas, S.; Necesal, P.; Nellen, L.; Nelles, A.; Neuser, J.; Nhung, P. T.; Niemietz, L.; Nierstenhoefer, N.; Nitz, D.; Nosek, D.; Nožka, L.; Nyklicek, M.; Oehlschläger, J.; Olinto, A.; Olmos-Gilbaja, V. M.; Ortiz, M.; Pacheco, N.; Pakk Selmi-Dei, D.; Palatka, M.; Pallotta, J.; Palmieri, N.; Parente, G.; Parizot, E.; Parra, A.; Parsons, R. D.; Pastor, S.; Paul, T.; Pech, M.; P?kala, J.; Pelayo, R.; Pepe, I. M.; Perrone, L.; Pesce, R.; Petermann, E.; Petrera, S.; Petrinca, P.; Petrolini, A.; Petrov, Y.; Petrovic, J.; Pfendner, C.; Phan, N.

    2012-08-01

    We report a measurement of the proton-air cross section for particle production at the center-of-mass energy per nucleon of 57 TeV. This is derived from the distribution of the depths of shower maxima observed with the Pierre Auger Observatory: systematic uncertainties are studied in detail. Analyzing the tail of the distribution of the shower maxima, a proton-air cross section of [505±22(stat)+28-36(syst)] mb is found.

  6. The Pierre Auger Observatory scaler mode for the study of solar activity modulation of galactic cosmic rays

    SciTech Connect (OSTI)

    Abreu, P.; Aglietta, M.; Ahn, E.J.; Allard, D.; Allekotte, I.; Allen, J.; Alvarez Castillo, J.; Alvarez-Muniz, J.; Ambrosio, M.; Aminaei, A.; Anchordoqui, L.; /Wisconsin U., Milwaukee /Lisbon, LIFEP /Lisbon, IST

    2011-01-01

    Since data-taking began in January 2004, the Pierre Auger Observatory has been recording the count rates of low energy secondary cosmic ray particles for the self-calibration of the ground detectors of its surface detector array. After correcting for atmospheric effects, modulations of galactic cosmic rays due to solar activity and transient events are observed. Temporal variations related with the activity of the heliosphere can be determined with high accuracy due to the high total count rates. In this study, the available data are presented together with an analysis focused on the observation of Forbush decreases, where a strong correlation with neutron monitor data is found.

  7. THE FERNALD DOSIMETRY RECONSTRUCTION Task 1: Identification of Release Points

    E-Print Network [OSTI]

    fires, spills, and UF6 leaks and releases. The Stack Release Points and Other Release Points are located

  8. Hot Springs Point Geothermal Project | Open Energy Information

    Open Energy Info (EERE)

    Point Geothermal Project Jump to: navigation, search GEOTHERMAL ENERGYGeothermal Home Development Project: Hot Springs Point Geothermal Project Project Location Information...

  9. Superconductivity, superfluidity and zero-point oscillations

    E-Print Network [OSTI]

    B. V. Vasiliev

    2013-06-29

    Currently it is thought that in order to explain the phenomenon of superconductivity is necessary to understand the mechanism of formation of electron pairs. However, the paired electrons cannot form a superconducting condensate. They perform disorderly zero-point oscillations and there are no attractive forces in their ensemble. To create a unified ensemble of particles, the pairs must order their zero-point fluctuations so that an attraction between the particles appears. For this reason, the ordering of zero-point oscillations in the electron gas is the cause of superconductivity and the parameters characterizing this order determine the properties of superconductors. The model of condensation of zero-point oscillations creates the possibility to obtain estimates for the critical parameters of elementary superconductors, which are also in the satisfactory agreement with measured data. On the another hand, the phenomenon of superfluidity in He-4 and He-3 can be similarly explained due to the ordering of zero-point fluctuations. Thus it is established that the both related phenomena are based on the same physical mechanism.

  10. The Lateral Trigger Probability function for the Ultra-High Energy Cosmic Ray Showers detected by the Pierre Auger Observatory

    E-Print Network [OSTI]

    The Pierre Auger Collaboration; P. Abreu; M. Aglietta; E. J. Ahn; I. F. M. Albuquerque; D. Allard; I. Allekotte; J. Allen; P. Allison; J. Alvarez Castillo; J. Alvarez-Muñiz; M. Ambrosio; A. Aminaei; L. Anchordoqui; S. Andringa; T. Anti?i?; A. Anzalone; C. Aramo; E. Arganda; F. Arqueros; H. Asorey; P. Assis; J. Aublin; M. Ave; M. Avenier; G. Avila; T. Bäcker; M. Balzer; K. B. Barber; A. F. Barbosa; R. Bardenet; S. L. C. Barroso; B. Baughman; J. Bäuml; J. J. Beatty; B. R. Becker; K. H. Becker; A. Bellétoile; J. A. Bellido; S. BenZvi; C. Berat; X. Bertou; P. L. Biermann; P. Billoir; F. Blanco; M. Blanco; C. Bleve; H. Blümer; M. Bohá?ová; D. Boncioli; C. Bonifazi; R. Bonino; N. Borodai; J. Brack; P. Brogueira; W. C. Brown; R. Bruijn; P. Buchholz; A. Bueno; R. E. Burton; K. S. Caballero-Mora; L. Caramete; R. Caruso; A. Castellina; O. Catalano; G. Cataldi; L. Cazon; R. Cester; J. Chauvin; S. H. Cheng; A. Chiavassa; J. A. Chinellato; A. Chou; J. Chudoba; R. W. Clay; M. R. Coluccia; R. Conceição; F. Contreras; H. Cook; M. J. Cooper; J. Coppens; A. Cordier; S. Coutu; C. E. Covault; A. Creusot; A. Criss; J. Cronin; A. Curutiu; S. Dagoret-Campagne; R. Dallier; S. Dasso; K. Daumiller; B. R. Dawson; R. M. de Almeida; M. De Domenico; C. De Donato; S. J. de Jong; G. De La Vega; W. J. M. de Mello Junior; J. R. T. de Mello Neto; I. De Mitri; V. de Souza; K. D. de Vries; G. Decerprit; L. del Peral; M. del Río; O. Deligny; H. Dembinski; N. Dhital; C. Di Giulio; J. C. Diaz; M. L. Díaz Castro; P. N. Diep; C. Dobrigkeit; W. Docters; J. C. D'Olivo; P. N. Dong; A. Dorofeev; J. C. dos Anjos; M. T. Dova; D. D'Urso; I. Dutan; J. Ebr; R. Engel; M. Erdmann; C. O. Escobar; J. Espadanal; A. Etchegoyen; P. Facal San Luis; I. Fajardo Tapia; H. Falcke; G. Farrar; A. C. Fauth; N. Fazzini; A. P. Ferguson; A. Ferrero; B. Fick; A. Filevich; A. Filip?i?; S. Fliescher; C. E. Fracchiolla; E. D. Fraenkel; U. Fröhlich; B. Fuchs; R. Gaior; R. F. Gamarra; S. Gambetta; B. García; D. García Gámez; D. Garcia-Pinto; A. Gascon; H. Gemmeke; K. Gesterling; P. L. Ghia; U. Giaccari; M. Giller; H. Glass; M. S. Gold; G. Golup; F. Gomez Albarracin; M. Gómez Berisso; P. Gonçalves; D. Gonzalez; J. G. Gonzalez; B. Gookin; D. Góra; A. Gorgi; P. Gouffon; S. R. Gozzini; E. Grashorn; S. Grebe; N. Griffith; M. Grigat; A. F. Grillo; Y. Guardincerri; F. Guarino; G. P. Guedes; A. Guzman; J. D. Hague; P. Hansen; D. Harari; S. Harmsma; J. L. Harton; A. Haungs; T. Hebbeker; D. Heck; A. E. Herve; C. Hojvat; N. Hollon; V. C. Holmes; P. Homola; J. R. Hörandel; A. Horneffer; M. Hrabovský; T. Huege; A. Insolia; F. Ionita; A. Italiano; C. Jarne; S. Jiraskova; M. Josebachuili; K. Kadija; K. H. Kampert; P. Karhan; P. Kasper; B. Kégl; B. Keilhauer; A. Keivani; J. L. Kelley; E. Kemp; R. M. Kieckhafer; H. O. Klages; M. Kleifges; J. Kleinfeller; J. Knapp; D. -H. Koang; K. Kotera; N. Krohm; O. Krömer; D. Kruppke-Hansen; F. Kuehn; D. Kuempel; J. K. Kulbartz; N. Kunka; G. La Rosa; C. Lachaud; P. Lautridou; M. S. A. B. Leão; D. Lebrun; P. Lebrun; M. A. Leigui de Oliveira; A. Lemiere; A. Letessier-Selvon; I. Lhenry-Yvon; K. Link; R. López; A. Lopez Agüera; K. Louedec; J. Lozano Bahilo; L. Lu; A. Lucero; M. Ludwig; H. Lyberis; M. C. Maccarone; C. Macolino; S. Maldera; D. Mandat; P. Mantsch; A. G. Mariazzi; J. Marin; V. Marin; I. C. Maris; H. R. Marquez Falcon; G. Marsella; D. Martello; L. Martin; H. Martinez; O. Martínez Bravo; H. J. Mathes; J. Matthews; J. A. J. Matthews; G. Matthiae; D. Maurizio; P. O. Mazur; G. Medina-Tanco; M. Melissas; D. Melo; E. Menichetti; A. Menshikov; P. Mertsch; C. Meurer; S. Mi?anovi?; M. I. Micheletti; W. Miller; L. Miramonti; L. Molina-Bueno; S. Mollerach; M. Monasor; D. Monnier Ragaigne; F. Montanet; B. Morales; C. Morello; E. Moreno; J. C. Moreno; C. Morris; M. Mostafá; C. A. Moura; S. Mueller; M. A. Muller; G. Müller; M. Münchmeyer; R. Mussa; G. Navarra ‡; J. L. Navarro; S. Navas; P. Necesal; L. Nellen; A. Nelles; J. Neuser; P. T. Nhung; L. Niemietz; N. Nierstenhoefer; D. Nitz; D. Nosek; L. Nožka; M. Nyklicek; J. Oehlschläger; A. Olinto; P. Oliva; V. M. Olmos-Gilbaja; M. Ortiz; N. Pacheco; D. Pakk Selmi-Dei; M. Palatka; J. Pallotta; N. Palmieri; G. Parente; E. Parizot; A. Parra; R. D. Parsons; S. Pastor; T. Paul; M. Pech; J. P?kala; R. Pelayo; I. M. Pepe; L. Perrone; R. Pesce; E. Petermann; S. Petrera; P. Petrinca; A. Petrolini; Y. Petrov; J. Petrovic; C. Pfendner; N. Phan; R. Piegaia; T. Pierog; P. Pieroni; M. Pimenta; V. Pirronello; M. Platino; V. H. Ponce; M. Pontz; P. Privitera; M. Prouza; E. J. Quel; S. Querchfeld; J. Rautenberg; O. Ravel; D. Ravignani; B. Revenu; J. Ridky; S. Riggi; M. Risse; P. Ristori; H. Rivera; V. Rizi; J. Roberts; C. Robledo; W. Rodrigues de Carvalho; G. Rodriguez; J. Rodriguez Martino; J. Rodriguez Rojo

    2011-11-28

    In this paper we introduce the concept of Lateral Trigger Probability (LTP) function, i.e., the probability for an extensive air shower (EAS) to trigger an individual detector of a ground based array as a function of distance to the shower axis, taking into account energy, mass and direction of the primary cosmic ray. We apply this concept to the surface array of the Pierre Auger Observatory consisting of a 1.5 km spaced grid of about 1600 water Cherenkov stations. Using Monte Carlo simulations of ultra-high energy showers the LTP functions are derived for energies in the range between 10^{17} and 10^{19} eV and zenith angles up to 65 degs. A parametrization combining a step function with an exponential is found to reproduce them very well in the considered range of energies and zenith angles. The LTP functions can also be obtained from data using events simultaneously observed by the fluorescence and the surface detector of the Pierre Auger Observatory (hybrid events). We validate the Monte-Carlo results showing how LTP functions from data are in good agreement with simulations.

  11. Project Reports for San Carlos Apache Tribe- 2011 Project

    Office of Energy Efficiency and Renewable Energy (EERE)

    The core purpose of this project is to provide for the analysis and implementation of a Tribal Energy Organization that can effectively provide for coordination, leadership, and energy expertise to the rest of the tribal government in understanding and pursuing energy programs and plans.

  12. V-162: Apache Struts "ParameterInterceptor" Security Bypass Vulnerabil...

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

    to enable method execution and execute arbitrary methods, bypassing Struts and OGNL library protections. 2. Any unsanitized String variable exposed by an action and have it...

  13. Apache County, Arizona: Energy Resources | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIX ECoop IncIowaWisconsin: EnergyYork Jump| Open EnergyNew Jersey:AntiguaAnyang

  14. Apache Junction, Arizona: Energy Resources | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIX ECoop IncIowaWisconsin: EnergyYork Jump| Open EnergyNew Jersey:AntiguaAnyangJunction,

  15. V-170: Apache Subversion Hook Scripts Arbitrary Command Injection

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

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of Natural GasAdjustmentsShirleyEnergyThe U.S.Lacledeutilities. The Economics of

  16. V-188: Apache XML Security XPointer Expressions Processing Buffer Overflow

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

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of Natural GasAdjustmentsShirleyEnergyThe U.S.Lacledeutilities. The Economics ofConductMultiple vulnerabilities have

  17. Mescalero Apache Strategic Energy Plan | Department of Energy

    Energy Savers [EERE]

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on DeliciousMathematicsEnergyInterested Parties - WAPAEnergy May 28 WebinarProtect MigratoryRegulators,and

  18. U-058: Apache Struts Conversion Error OGNL Expression Injection

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

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Delicious RankADVANCEDInstallers/ContractorsPhotovoltaicsStateof Energy TwoEvent at the Pu2:ServersVulnerability |

  19. Relative localization of point particle interactions

    E-Print Network [OSTI]

    José Ricardo Oliveira

    2011-10-25

    We review the main concepts of the recently introduced principle of relative locality and investigate some aspects of classical interactions between point particles from this new perspective. We start with a physical motivation and basic mathematical description of relative locality and review the treatment of a system of classical point particles in this framework. We then examine one of the unsolved problems of this picture, the apparent ambiguities in the definition of momentum constraints caused by a non-commutative and/or non-associative momentum addition rule. The gamma ray burst experiment is used as an illustration. Finally, we use the formalism of relative locality to reinterpret the well-known multiple point particle system coupled to 2+1 Einstein gravity, analyzing the geometry of its phase space and once again referring to the gamma ray burst problem as an example.

  20. Phase-shifting point diffraction interferometer

    DOE Patents [OSTI]

    Medecki, H.

    1998-11-10

    Disclosed is a point diffraction interferometer for evaluating the quality of a test optic. In operation, the point diffraction interferometer includes a source of radiation, the test optic, a beam divider, a reference wave pinhole located at an image plane downstream from the test optic, and a detector for detecting an interference pattern produced between a reference wave emitted by the pinhole and a test wave emitted from the test optic. The beam divider produces separate reference and test beams which focus at different laterally separated positions on the image plane. The reference wave pinhole is placed at a region of high intensity (e.g., the focal point) for the reference beam. This allows reference wave to be produced at a relatively high intensity. Also, the beam divider may include elements for phase shifting one or both of the reference and test beams. 8 figs.

  1. Phase-shifting point diffraction interferometer

    DOE Patents [OSTI]

    Medecki, Hector (Berkeley, CA)

    1998-01-01

    Disclosed is a point diffraction interferometer for evaluating the quality of a test optic. In operation, the point diffraction interferometer includes a source of radiation, the test optic, a beam divider, a reference wave pinhole located at an image plane downstream from the test optic, and a detector for detecting an interference pattern produced between a reference wave emitted by the pinhole and a test wave emitted from the test optic. The beam divider produces separate reference and test beams which focus at different laterally separated positions on the image plane. The reference wave pinhole is placed at a region of high intensity (e.g., the focal point) for the reference beam. This allows reference wave to be produced at a relatively high intensity. Also, the beam divider may include elements for phase shifting one or both of the reference and test beams.

  2. Multiple Critical Points in Effective Quark Models

    E-Print Network [OSTI]

    Ferroni, Lorenzo; Pinto, Marcus B

    2010-01-01

    We consider the two flavor version of the Linear Sigma Model as well as of the Nambu Jona-Lasinio model, at finite temperature and quark chemical potential, beyond the Mean Field Approximation. Using parameter values for the pion and quark current masses which weakly break chiral symmetry we show that both models can present more than one critical end point. In particular, we explicitly show that the appearance of a new critical point associated with a first order line at high temperature and low densities could help to conciliate some lattice results with model predictions. Using different techniques, we perform an extensive thermodynamical analysis to understand the physical nature of the different critical points. For both models, our results suggest that the new first order line which starts at vanishing chemical potential has a more chiral character than the usual line which displays a character more reminiscent of a liquid-gas phase transition.

  3. The ROSAT HRI Point Spread Function

    E-Print Network [OSTI]

    Peter Predehl; Almudena Prieto

    2001-09-28

    A sample of the brightest point-like sources observed with the ROSAT-HRI were analysed to asses on the intrinsic shape of the ROSAT-HRI Point Spread Function (PSF). Almost all of the HRI observations collected during the ROSAT lifetime are found to be artificially broadened by factors up two ~2 due to residual errors in the ROSAT aspect solution. After correction by departing pointing positions, the width of the core of the PSF is found to be less than 5 arcsec (half energy width, HEW). On the basis of these results, an improved analytical representation of the ROSAT-HRI PSF is provided. However, for most of the new observations the source countrate is too weak to allow reliable recovering pf the ROSAT-HRI resolution. Therefore, a series of examples (data, correction, and theoretical PSF) are given in order to help the ROSAT user in determining whether "his/her source" is extended or not.

  4. Nanotexturing of surfaces to reduce melting point.

    SciTech Connect (OSTI)

    Garcia, Ernest J.; Zubia, David; Mireles, Jose; Marquez, Noel; Quinones, Stella

    2011-11-01

    This investigation examined the use of nano-patterned structures on Silicon-on-Insulator (SOI) material to reduce the bulk material melting point (1414 C). It has been found that sharp-tipped and other similar structures have a propensity to move to the lower energy states of spherical structures and as a result exhibit lower melting points than the bulk material. Such a reduction of the melting point would offer a number of interesting opportunities for bonding in microsystems packaging applications. Nano patterning process capabilities were developed to create the required structures for the investigation. One of the technical challenges of the project was understanding and creating the specialized conditions required to observe the melting and reshaping phenomena. Through systematic experimentation and review of the literature these conditions were determined and used to conduct phase change experiments. Melting temperatures as low as 1030 C were observed.

  5. Symmetry and Dirac points in graphene spectrum

    E-Print Network [OSTI]

    Gregory Berkolaiko; Andrew Comech

    2015-04-23

    Existence and stability of Dirac points in the dispersion relation of operators periodic with respect to the hexagonal lattice is investigated for different sets of additional symmetries. The following symmetries are considered: rotation by $2\\pi/3$ and inversion, rotation by $2\\pi/3$ and horizontal reflection, inversion or reflection with weakly broken rotation symmetry, and the case where no Dirac points arise: rotation by $2\\pi/3$ and vertical reflection. All proofs are based on symmetry considerations and are elementary in nature. In particular, existence of degeneracies in the spectrum is proved by a transplantation argument (which is deduced from the (co)representation of the relevant symmetry group). The conical shape of the dispersion relation is obtained from its invariance under rotation by $2\\pi/3$. Persistence of conical points when the rotation symmetry is weakly broken is proved using a geometric phase in one case and parity of the eigenfunctions in the other.

  6. Non-lead hollow point bullet

    DOE Patents [OSTI]

    Vaughn, Norman L. (Knoxville, TN); Lowden, Richard A. (Clinton, TN)

    2003-04-15

    The non-lead hollow point bullet of the instant invention comprises a mixed construction slug further comprising, a monolithic metal insert having a tapered (preferred conical) hollow point tip and a tapered (preferred conical) tail protrusion, and an unsintered powdered metal composite core in tandem alignment with the insert. The core has a hollow tapered (preferred conical) cavity tip portion coupled with the tapered (preferred conical) tail protrusion on the insert. An open tip jacket envelops at least a portion of the insert and the core. The jacket is swaged at the open tip.

  7. Sequential conditions for fixed and periodic points 

    E-Print Network [OSTI]

    Peters, Burnis Charles

    1970-01-01

    ) (Member) ~A (Month) 1970 (Year) ~04SQQ ABSTRACT Sec, uential Conditions fo. Fixed and Periodic Points (August 1970) Burnis C. Peter, Jr. , B. A. , Texas ASM University; M. S. , Texas A&M University Directed by: Jack Bryant and L. F. Guseman, Jr.... Let (X, d) be a metric space and f a selfmap of X. It is shown that a number of known theorems on the existence of fixed and periodic points are related through simple properties of the n sequence (f ) of iterates . ACMOVI. EDGEMENTS I wish...

  8. QCD Critical Point: The Race is On

    E-Print Network [OSTI]

    Gavai, Rajiv V

    2014-01-01

    A critical point in the phase diagram of Quantum Chromodynamics (QCD), if established either theoretically or experimentally, would be as profound a discovery as the good-old gas-liquid critical point. Unlike the latter, however, first-principles based approaches are being employed to locate it theoretically. Due to the short lived nature of the concerned phases, novel experimental techniques are needed to search for it. The Relativistic Heavy Ion Collider (RHIC) in USA has an experimental program to do so. This short review is an attempt to provide a glimpse of the race between the theorists and the experimentalists as well as that of the synergy between them.

  9. Points of Pride | The Ames Laboratory

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

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity ofkandz-cm11 Outreach Home Room NewsInformationJesseworkSURVEYI/OPerformancePi Day Pi Day Pi DayPlasmaandAbout UsPointsPoints

  10. EXCEPTIONAL COVERS AND BIJECTIONS ON RATIONAL POINTS

    E-Print Network [OSTI]

    Fried, Michael

    EXCEPTIONAL COVERS AND BIJECTIONS ON RATIONAL POINTS ROBERT M. GURALNICK, THOMAS J. TUCKER proved by Davenport and Lewis [DL], Mac- Cluer [Mac], Williams [Wi], Cohen [Co], and Fried [Fr, Fr3, FGS was partially supported by NSF grant DMS-0140578. 1 #12;2 ROBERT M. GURALNICK, THOMAS J. TUCKER, AND MICHAEL E

  11. EXCEPTIONAL COVERS AND BIJECTIONS ON RATIONAL POINTS

    E-Print Network [OSTI]

    Zieve, Michael E.

    EXCEPTIONAL COVERS AND BIJECTIONS ON RATIONAL POINTS ROBERT M. GURALNICK, THOMAS J. TUCKER cases and weaker versions were previously proved by Davenport and Lewis [DL], Mac- Cluer [Mac], Williams was partially supported by NSF grant DMS-0140578. 1 #12;2 ROBERT M. GURALNICK, THOMAS J. TUCKER, AND MICHAEL E

  12. Killam Library Service Point August 20, 2013

    E-Print Network [OSTI]

    Lotze, Heike K.

    , the Library will make special provisions insofar as feasible to permit the patrons to examine sources impression of the Library. Individual assistance to patrons who come to the Library is the primary5 Killam Library Service Point Policy 2013-02-18 August 20, 2013 Head, Killam Memorial Library

  13. Discovering Point Sources in Unknown Environments

    E-Print Network [OSTI]

    Ferguson, Thomas S.

    - ted from the yet-to-be-located source. We will refer to the information from the range sensorDiscovering Point Sources in Unknown Environments Yanina Landa1 , Nicolay M. Tanushev2 , Richard of Texas at Austin, {nicktan,ytsai}@math.utexas.edu 3 Institute for Computational and Appplied Mathematics

  14. Form drag at Three Tree Point

    E-Print Network [OSTI]

    for this study Seattle Tacoma Edwards et al., 2004 Puget Sound, WA Point Three Tree Previous work McCabe et al 24 ­ drag due to tilt = residual drag total form drag #12;Cruise at TTP in Dec. 2009 Seattle Tacoma

  15. Multilinear generalized Radon transforms and point configurations

    E-Print Network [OSTI]

    Grafakos, Loukas; Iosevich, Alex; Palsson, Eyvindur

    2012-01-01

    We study multilinear generalized Radon transforms using a graph-theoretic paradigm that includes the widely studied linear case. These provide a general mechanism to study Falconer-type problems involving $(k+1)$-point configurations in geometric measure theory, with $k \\ge 2$, including the distribution of simplices, volumes and angles determined by the points of fractal subsets $E \\subset {\\Bbb R}^d$, $d \\ge 2$. If $T_k(E)$ denotes the set of noncongruent $(k+1)$-point configurations determined by $E$, we show that if the Hausdorff dimension of $E$ is greater than $d-\\frac{d-1}{2k}$, then the ${k+1 \\choose 2}$-dimensional Lebesgue measure of $T_k(E)$ is positive. This compliments previous work on the Falconer conjecture (\\cite{Erd05} and the references there), as well as work on finite point configurations \\cite{EHI11,GI10}. We also give applications to Erd\\"os-type problems in discrete geometry and a fractal regular value theorem, providing a multilinear framework for the results in \\cite{EIT11}.

  16. Multilinear generalized Radon transforms and point configurations

    E-Print Network [OSTI]

    Grafakos, Loukas

    Multilinear generalized Radon transforms and point configurations Loukas Grafakos, Allan Greenleaf, Alex Iosevich and Eyvindur Palsson Abstract. We study multilinear generalized Radon transforms using for the results in [7]. 1. Introduction Linear generalized Radon transforms are operators of the form (1.1) Rf

  17. Ground Vibration Measurements at LHC Point 4

    SciTech Connect (OSTI)

    Bertsche, Kirk; /SLAC; Gaddi, Andrea; /CERN

    2012-09-17

    Ground vibration was measured at Large Hadron Collider (LHC) Point 4 during the winter shutdown in February 2012. This report contains the results, including power and coherence spectra. We plan to collect and analyze vibration data from representative collider halls to inform specifications for future linear colliders, such as ILC and CLIC. We are especially interested in vibration correlations between final focus lens locations.

  18. Surveying points in the complex projective plane

    E-Print Network [OSTI]

    Lane Hughston; Simon Salamon

    2014-10-21

    We classify SIC-POVMs of rank one in CP^2, or equivalently sets of nine equally-spaced points in CP^2, without the assumption of group covariance. If two points are fixed, the remaining seven must lie on a pinched torus that a standard moment mapping projects to a circle in R^3. We use this approach to prove that any SIC set in CP^2 is isometric to a known solution, given by nine points lying in triples on the equators of the three 2-spheres each defined by the vanishing of one homogeneous coordinate. We set up a system of equations to describe hexagons in CP^2 with the property that any two vertices are related by a cross ratio (transition probability) of 1/4. We then symmetrize the equations, factor out by the known solutions, and compute a Groebner basis to show that no SIC sets remain. We do find new configurations of nine points in which 27 of the 36 pairs of vertices of the configuration are equally spaced.

  19. A Formula for Inserting Point Masses

    E-Print Network [OSTI]

    Manwah Lilian Wong

    2010-09-08

    Let mu be a probability measure on the unit circle and nu be the measure formed by adding a pure point to mu. We give a formula for the Verblunsky coefficients of the perturbed measure, based on a result of Simon.

  20. ON LYAPUNOV FAMILIES AROUND COLLINEAR LIBRATION POINTS

    SciTech Connect (OSTI)

    Hou, X. Y.; Liu, L. [Astronomy Department, Nanjing University, Nanjing 210093 (China)], E-mail: lliu@nju.edu.cn

    2009-06-15

    Evolution details of the planar and vertical Lyapunov families around the three collinear libration points in the restricted three-body problem were studied. Researches before were generally restricted to be within the colliding orbits with the primaries and for fixed mass parameters {mu}. In this paper, members after colliding orbits were computed. With increasing {mu}, how these families evolve was studied.

  1. Emergency Preparedness Plan Horn Point Laboratory

    E-Print Network [OSTI]

    Boynton, Walter R.

    Emergency Preparedness Plan Horn Point Laboratory March 2015 Introduction This plan summarizes the actions which will be taken in preparation for and in response to emergencies impacting the regular technology security and infrastructure, business functions, and academic and research continuity. Emergencies

  2. Language Production General Points about Speech Production

    E-Print Network [OSTI]

    Coulson, Seana

    Language Production #12;General Points about Speech Production 15 speech sounds per second => 2, shall I say `t' or `d'' (Levelt) Production side has gotten less attention in Psycholinguistics than the comprehension side. Evidence for speech production behaviour has until recently relied heavily on speech errors

  3. Point-to-Point Car Racing: an Initial Study of Evolution Versus Temporal Difference Learning

    E-Print Network [OSTI]

    Togelius, Julian

    Point-to-Point Car Racing: an Initial Study of Evolution Versus Temporal Difference Learning Simon, jtogel}@essex.ac.uk Abstract-- This paper considers variations on an extremely simple form of car racing-evaluation neural networks, and these were greatly superior to human drivers. Keywords: Car racing, reinforcement

  4. The Efficiency of Point-to-Point Financial Transmission Rights is Limited by the Network Topology

    E-Print Network [OSTI]

    Blumsack, Seth

    of the restructured electric power industry envisioned replacing the transmission business of a regulated utility of electric-sector restructuring would place transmission under a market regime similar to generationThe Efficiency of Point-to-Point Financial Transmission Rights is Limited by the Network Topology

  5. Integral points on hyperbolas: A special case

    E-Print Network [OSTI]

    Konstantine Zelator

    2009-07-21

    The subject matter of this work is integral points on conics described by the general equation, ax^2+bxy+cy^2+dx+ey+f=0 (1) where the six coefficients are integers satisfying the conditions, b^2-4ac=k^2, with a and c being nonzero and k a positive integer. It is well known the when b^2-4ac>0, equation (1) describes either a hyperbola on the plane or a pair of two straight lines(the degenerate case). The key integer is the number, I=k^2(d^2-4af)-(2ae-bd)^2. In Section 2, we show via a straightforward algebraic method that equation (1) can be put in the form, g(x,y)h(x,y)=I, where g(x,y) and h(x,y) are linear polynomials in x and y with integer coefficients. Thus, when I is not zero, equation (1) has only finitely many integer solutions (x,y). The process of finding these solutions is outlined in Section 3. In Section 4,we give a detailed numerical example. In Section 5, we offer some observations and remarks. In Section 6, we discuss the case b=d=e=0. In Section 7 we discuss the case a=1=k, and we show that when I=2^n, n>or=2, the above hyperbola has exactly 2(n-1) integral points, all explicitly given. In Section 10, we prove that these points are distinct. In Section 8 we discuss the case I=0, the hyperbola in (1) has either infinitely many integral points: or no integral points. Finally in Section 9, we discuss the special case d=e=f=0.

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

    E-Print Network [OSTI]

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

    2015-01-01

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

  7. The First U.S. Naval Observatory Robotic Astrometric Telescope Catalog (URAT1)

    E-Print Network [OSTI]

    Zacharias, Norbert; Subasavage, John; Bredthauer, Greg; Crockett, Chris; DiVittorio, Mike; Ferguson, Erik; Harris, Fred; Harris, Hugh; Henden, Arne; Kilian, Chris; Munn, Jeff; Rafferty, Ted; Rhodes, Al; Schultheiss, Mike; Tilleman, Trudy; Wieder, Gary

    2015-01-01

    URAT1 is an observational, astrometric catalog covering most of the Dec >= -15 deg area and a magnitude range of about R = 3 to 18.5. Accurate positions (typically 10 to 30 mas standard error) are given for over 228 million objects at a mean epoch around 2013.5. For the over 188 million objects matched with the 2MASS point source catalog proper motions (typically 5 to 7 mas/yr std. errors) are provided. These data are supplemented by 2MASS and APASS photometry. Observations, reductions and catalog construction are described together with results from external data verifications. The catalog data are served by CDS, Starsbourg (I/329). There is no DVD release.

  8. Search for signatures of magnetically-induced alignment in the arrival directions measured by the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Abreu, P.; Aglietta, M.; Ahn, E.J.; Albuquerque, I.F.M.; Allard, D.; Allekotte, I.; Allen, J.; Allison, P.; Alvarez Castillo, J.; Alvarez-Muniz, J.; Ambrosio, M.; /Naples U. /INFN, Naples /Nijmegen U., IMAPP

    2011-11-01

    We present the results of an analysis of data recorded at the Pierre Auger Observatory in which we search for groups of directionally-aligned events (or ''multiplets'') which exhibit a correlation between arrival direction and the inverse of the energy. These signatures are expected from sets of events coming from the same source after having been deflected by intervening coherent magnetic fields. The observation of several events from the same source would open the possibility to accurately reconstruct the position of the source and also measure the integral of the component of the magnetic field orthogonal to the trajectory of the cosmic rays. We describe the largest multiplets found and compute the probability that they appeared by chance from an isotropic distribution. We find no statistically significant evidence for the presence of multiplets arising from magnetic deflections in the present data.

  9. Ocean pC02 Data from the Lamont-Doherty Earth Observatory of Columbia University, 1994 - 2009

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

    Takahashi, T.

    The Earth Institute of Columbia University has, as an overarching goal, to help achieve sustainable development primarily by expanding the world's understanding of Earth as one integrated system. The Earth Institute encompasses centers of excellence with an established reputation for groundbreaking research, including the renowned Lamont-Doherty Earth Observatory (LDEO), home to more than 200 researchers who study Earth and its systems. The Carbon Dioxide Research Group, led by Dr. Taro Takahashi, studies pCO2 in seawater, carbon sequestration models related to deep aquifers, and air-sea CO2 flux. Datasets from ocean cruises in the years 1994 to the present are made available from this website, along with a list of publications, and cruise maps.

  10. Searches for High Frequency Variations in the $^8$B Solar Neutrino Flux at the Sudbury Neutrino Observatory

    E-Print Network [OSTI]

    SNO Collaboration

    2009-10-13

    We have performed three searches for high-frequency signals in the solar neutrino flux measured by the Sudbury Neutrino Observatory (SNO), motivated by the possibility that solar $g$-mode oscillations could affect the production or propagation of solar $^8$B neutrinos. The first search looked for any significant peak in the frequency range 1/day to 144/day, with a sensitivity to sinusoidal signals with amplitudes of 12% or greater. The second search focused on regions in which $g$-mode signals have been claimed by experiments aboard the SoHO satellite, and was sensitive to signals with amplitudes of 10% or greater. The third search looked for extra power across the entire frequency band. No statistically significant signal was detected in any of the three searches.

  11. Planck Intermediate Results. XXXVI. Optical identification and redshifts of Planck SZ sources with telescopes in the Canary Islands Observatories

    E-Print Network [OSTI]

    Ade, P A R; Arnaud, M; Ashdown, M; Aumont, J; Baccigalupi, C; Banday, A J; Barreiro, R B; Barrena, R; Bartolo, N; Battaner, E; Benabed, K; Benoit-Lévy, A; Bernard, J -P; Bersanelli, M; Bielewicz, P; Bikmaev, I; Böhringer, H; Bonaldi, A; Bonavera, L; Bond, J R; Borrill, J; Bouchet, F R; Burenin, R; Burigana, C; Calabrese, E; Cardoso, J -F; Catalano, A; Chamballu, A; Chary, R -R; Chiang, H C; Chon, G; Christensen, P R; Clements, D L; Colombo, L P L; Combet, C; Comis, B; Crill, B P; Curto, A; Cuttaia, F; Dahle, H; Danese, L; Davies, R D; Davis, R J; de Bernardis, P; de Rosa, A; de Zotti, G; Delabrouille, J; Diego, J M; Dole, H; Donzelli, S; Doré, O; Douspis, M; Dupac, X; Efstathiou, G; Elsner, F; Enßlin, T A; Eriksen, H K; Ferragamo, A; Finelli, F; Forni, O; Frailis, M; Fraisse, A A; Franceschi, E; Fromenteau, S; Galeotta, S; Galli, S; Ganga, K; Génova-Santos, R T; Giard, M; Gjerløw, E; González-Nuevo, J; Górski, K M; Gruppuso, A; Hansen, F K; Harrison, D L; Hempel, A; Hernández-Monteagudo, C; Herranz, D; Hildebrandt, S R; Hivon, E; Hornstrup, A; Hovest, W; Huffenberger, K M; Hurier, G; Jaffe, T R; Keihänen, E; Keskitalo, R; Khamitov, I; Kisner, T S; Knoche, J; Kunz, M; Kurki-Suonio, H; Lamarre, J -M; Lasenby, A; Lattanzi, M; Lawrence, C R; Leonardi, R; León-Tavares, J; Levrier, F; Lietzen, H; Liguori, M; Lilje, P B; Linden-Vørnle, M; López-Caniego, M; Lubin, P M; Macías-Pérez, J F; Maffei, B; Maino, D; Mandolesi, N; Maris, M; Martin, P G; Martínez-González, E; Masi, S; Matarrese, S; McGehee, P; Melchiorri, A; Mennella, A; Migliaccio, M; Miville-Deschênes, M -A; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Munshi, D; Murphy, J A; Naselsky, P; Nati, F; Natoli, P; Novikov, D; Novikov, I; Oxborrow, C A; Pagano, L; Pajot, F; Paoletti, D; Pasian, F; Perdereau, O; Pettorino, V; Piacentini, F; Piat, M; Pierpaoli, E; Plaszczynski, S; Pointecouteau, E; Polenta, G; Pratt, G W; Prunet, S; Puget, J -L; Rachen, J P; Rebolo, R; Reinecke, M; Remazeilles, M; Renault, C; Renzi, A; Ristorcelli, I; Rocha, G; Rosset, C; Rossetti, M; Roudier, G; Rubiño-Martín, J A; Rusholme, B; Sandri, M; Santos, D; Savelainen, M; Savini, G; Scott, D; Stolyarov, V; Streblyanska, A; Sudiwala, R; Sunyaev, R; Suur-Uski, A -S; Sygnet, J -F; Terenzi, L; Toffolatti, L; Tomasi, M; Tramonte, D; Tristram, M; Tucci, M; Valenziano, L; Valiviita, J; Van Tent, B; Vielva, P; Villa, F; Wade, L A; Wandelt, B D; Wehus, I K; Yvon, D; Zacchei, A; Zonca, A

    2015-01-01

    We present the results of approximately three years of observations of Planck Sunyaev-Zeldovich (SZ) sources with telescopes at the Canary Islands observatories, as part of the general optical follow-up programme undertaken by the Planck collaboration. In total, 78 SZ sources are discussed. Deep imaging observations were obtained for most of those sources; spectroscopic observations in either in long-slit or multi-object modes were obtained for many. We found optical counterparts for 73 of the 78 candidates. This sample includes 53 spectroscopic redshifts determinations, 20 of them obtained with a multi-object spectroscopic mode. The sample contains new redshifts for 27 Planck clusters that were not included in the first Planck SZ source catalogue (PSZ1).

  12. Redeveloping or preserving public housing : the future of Columbia Point

    E-Print Network [OSTI]

    Lee, Sharon Hsueh-Jen

    1981-01-01

    Columbia Point, Boston's largest and most stigmatized public housing project, has been a focal point for public and private. investment strategies to create a new mixed-income residential community. Columbia Point provided ...

  13. From Point to Pixel: A Genealogy of Digital Aesthetics

    E-Print Network [OSTI]

    Hoy, Meredith Anne

    2010-01-01

    From Point to Pixel: A Genealogy of Digital Aesthetics byFrom Point to Pixel: A Genealogy of Digital Aesthetics byFrom Point to Pixel: A Genealogy of Digital Aesthetics, I

  14. Quasi-Symmetries of Determinantal Point Processes

    E-Print Network [OSTI]

    Alexander I. Bufetov

    2014-09-06

    The main result of this paper is that determinantal point processes on the real line corresponding to projection operators with integrable kernels are quasi-invariant, in the continuous case, under the group of diffeomorphisms with compact support (Theorem 1.5); in the discrete case, under the group of all finite permutations of the phase space (Theorem 1.7). The Radon-Nikodym derivative is computed explicitly and is given by a regularized multiplicative functional. Theorem 1.5 applies, in particular, to the sine-process and the Bessel point process; Theorem 1.7 to the discrete sine process and the Gamma kernel process. The paper answers a question of Grigori Olshanski.

  15. Big Rock Point severe accident management strategies

    SciTech Connect (OSTI)

    Brogan, B.A. [Consumers Power Co., Charlevoix, MI (United States); Gabor, J.R. [Dames and Moore, Westmont, IL (United States)

    1996-07-01

    December 1994, the Nuclear Energy Institute (NEI) issued guidance relative to the formal industry position on Severe Accident Management (SAM) approved by the NEI Strategic Issues Advisory Committee on November 4, 1994. This paper summarizes how Big Rock Point (BRP) has and continues to address SAM strategies. The historical accounting portion of this presentation includes a description of how the following projects identified and defined the current Big Rock Point SAM strategies: the 1981 Level 3 Probabilistic Risk Assessment performance; the development of the Plant Specific Technical Guidelines from which the symptom oriented Emergency Operating Procedures (EOPs) were developed; the Control Room Design Review; and, the recent completion of the Individual Plant Evaluation (IPE). In addition to the historical presentation deliberation, this paper the present activities that continue to stress SAM strategies.

  16. Remote temperature-set-point controller

    DOE Patents [OSTI]

    Burke, W.F.; Winiecki, A.L.

    1984-10-17

    An instrument is described for carrying out mechanical strain tests on metallic samples with the addition of means for varying the temperature with strain. The instrument includes opposing arms and associated equipment for holding a sample and varying the mechanical strain on the sample through a plurality of cycles of increasing and decreasing strain within predetermined limits, circuitry for producing an output signal representative of the strain during the tests, apparatus including a a set point and a coil about the sample for providing a controlled temperature in the sample, and circuitry interconnected between the strain output signal and set point for varying the temperature of the sample linearly with strain during the tests.

  17. Dynamic trapping near a quantum critical point

    E-Print Network [OSTI]

    Michael Kolodrubetz; Emanuel Katz; Anatoli Polkovnikov

    2015-03-02

    The study of dynamics in closed quantum systems has recently been revitalized by the emergence of experimental systems that are well-isolated from their environment. In this paper, we consider the closed-system dynamics of an archetypal model: spins near a second order quantum critical point, which are traditionally described by the Kibble-Zurek mechanism. Imbuing the driving field with Newtonian dynamics, we find that the full closed system exhibits a robust new phenomenon -- dynamic critical trapping -- in which the system is self-trapped near the critical point due to efficient absorption of field kinetic energy by heating the quantum spins. We quantify limits in which this phenomenon can be observed and generalize these results by developing a Kibble-Zurek scaling theory that incorporates the dynamic field. Our findings can potentially be interesting in the context of early universe physics, where the role of the driving field is played by the inflaton or a modulus.

  18. Perforation of domain wall by point mass

    E-Print Network [OSTI]

    D. V. Gal'tsov; E. Yu. Melkumova; P. A. Spirin

    2013-12-30

    We investigate collision of a point particle and an infinitely thin planar domain wall interacting gravitationally within the linearized gravity in Minkowski space-time of arbitrary dimension. In this setting we are able to describe analytically the perforation of the wall by an impinging particle, showing that it is accompanied by excitation of the spherical shock branon wave propagating outwards with the speed of light. Formally, the shock wave is a free solution of the branon wave equation which has to be added to ensure the validity of the retarded solution at the perforation point. Physically, the domain wall gets excited due to the shake caused by an instantaneous change of sign of the repulsive gravitational force. This effect is shown to hold, in particular, in four space-time dimensions, being applicable to the problem of cosmological domain walls.

  19. Perforation of domain wall by point mass

    E-Print Network [OSTI]

    Gal'tsov, D V; Spirin, P A

    2013-01-01

    We investigate collision of a point particle and an infinitely thin planar domain wall interacting gravitationally within the linearized gravity in Minkowski space-time of arbitrary dimension. In this setting we are able to describe analytically the perforation of the wall by an impinging particle, showing that it is accompanied by excitation of the spherical shock branon wave propagating outwards with the speed of light. Formally, the shock wave is a free solution of the branon wave equation which has to be added to ensure the validity of the retarded solution at the perforation point. Physically, the domain wall gets excited due to the shake caused by an instantaneous change of sign of the repulsive gravitational force. This effect is shown to hold, in particular, in four space-time dimensions, being applicable to the problem of cosmological domain walls.

  20. EIS-0153: Niagara Import Point Project

    Broader source: Energy.gov [DOE]

    The Federal Energy Regulatory Commission prepared this statement to assess the environmental impacts of the proposed Niagara Import Point project that would construct an interstate natural gas pipeline to transport gas from Canada and domestic sources to the Northeastern United States market. The U.S. Department of Energy's Office of Fossil Energy was a cooperating agency during statement development and adopted this statement on 6/15/1990.

  1. Focusing: coming to the point in metamaterials

    E-Print Network [OSTI]

    Sebastien Guenneau; Andre Diatta; Ross McPhedran

    2010-09-02

    The point of the paper is to show some limitations of geometrical optics in the analysis of subwavelength focusing. We analyze the resolution of the image of a line source radiating in the Maxwell fisheye and the Veselago-Pendry slab lens. The former optical medium is deduced from the stereographic projection of a virtual sphere and displays a heterogeneous refractive index n(r) which is proportional to the inverse of 1+r^2. The latter is described by a homogeneous, but negative, refractive index. It has been suggested that the fisheye makes a perfect lens without negative refraction [Leonhardt, Philbin arxiv:0805.4778v2]. However, we point out that the definition of super-resolution in such a heterogeneous medium should be computed with respect to the wavelength in a homogenized medium, and it is perhaps more adequate to talk about a conjugate image rather than a perfect image (the former does not necessarily contains the evanescent components of the source). We numerically find that both the Maxwell fisheye and a thick silver slab lens lead to a resolution close to lambda/3 in transverse magnetic polarization (electric field pointing orthogonal to the plane). We note a shift of the image plane in the latter lens. We also observe that two sources lead to multiple secondary images in the former lens, as confirmed from light rays travelling along geodesics of the virtual sphere. We further observe resolutions ranging from lambda/2 to nearly lambda/4 for magnetic dipoles of varying orientations of dipole moments within the fisheye in transverse electric polarization (magnetic field pointing orthogonal to the plane). Finally, we analyse the Eaton lens for which the source and its image are either located within a unit disc of air, or within a corona 1

  2. Low-melting point heat transfer fluid

    DOE Patents [OSTI]

    Cordaro, Joseph Gabriel (Oakland, CA); Bradshaw, Robert W. (Livermore, CA)

    2010-11-09

    A low-melting point, heat transfer fluid made of a mixture of five inorganic salts including about 29.1-33.5 mol % LiNO.sub.3, 0-3.9 mol % NaNO.sub.3, 2.4-8.2 mol % KNO.sub.3, 18.6-19.9 mol % NaNO.sub.2, and 40-45.6 mol % KNO.sub.2. These compositions can have liquidus temperatures below 80.degree. C. for some compositions.

  3. High speed point derivative microseismic detector

    DOE Patents [OSTI]

    Uhl, J.E.; Warpinski, N.R.; Whetten, E.B.

    1998-06-30

    A high speed microseismic event detector constructed in accordance with the present invention uses a point derivative comb to quickly and accurately detect microseismic events. Compressional and shear waves impinging upon microseismic receiver stations disposed to collect waves are converted into digital data and analyzed using a point derivative comb including assurance of quiet periods prior to declaration of microseismic events. If a sufficient number of quiet periods have passed, the square of a two point derivative of the incoming digital signal is compared to a trip level threshold exceeding the determined noise level to declare a valid trial event. The squaring of the derivative emphasizes the differences between noise and signal, and the valid event is preferably declared when the trip threshold has been exceeded over a temporal comb width to realize a comb over a given time period. Once a trial event has been declared, the event is verified through a spatial comb, which applies the temporal event comb to additional stations. The detector according to the present invention quickly and accurately detects initial compressional waves indicative of a microseismic event which typically exceed the ambient cultural noise level by a small amount, and distinguishes the waves from subsequent larger amplitude shear waves. 9 figs.

  4. High speed point derivative microseismic detector

    DOE Patents [OSTI]

    Uhl, James Eugene (Albuquerque, NM); Warpinski, Norman Raymond (Albuquerque, NM); Whetten, Ernest Blayne (Albuquerque, NM)

    1998-01-01

    A high speed microseismic event detector constructed in accordance with the present invention uses a point derivative comb to quickly and accurately detect microseismic events. Compressional and shear waves impinging upon microseismic receiver stations disposed to collect waves are converted into digital data and analyzed using a point derivative comb including assurance of quiet periods prior to declaration of microseismic events. If a sufficient number of quiet periods have passed, the square of a two point derivative of the incoming digital signal is compared to a trip level threshold exceeding the determined noise level to declare a valid trial event. The squaring of the derivative emphasizes the differences between noise and signal, and the valid event is preferably declared when the trip threshold has been exceeded over a temporal comb width to realize a comb over a given time period. Once a trial event has been declared, the event is verified through a spatial comb, which applies the temporal event comb to additional stations. The detector according to the present invention quickly and accurately detects initial compressional waves indicative of a microseismic event which typically exceed the ambient cultural noise level by a small amount, and distinguishes the waves from subsequent larger amplitude shear waves.

  5. Energy Department Authorizes Dominion Cove Point LNG to Export...

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

    Energy Department Authorizes Dominion Cove Point LNG to Export Liquefied Natural Gas Energy Department Authorizes Dominion Cove Point LNG to Export Liquefied Natural Gas May 7,...

  6. Fast Change Point Detection for Electricity Market Analysis

    E-Print Network [OSTI]

    Gu, William

    2014-01-01

    The trouble with electricity markets: understandingPoint Detection for Electricity Market Analysis William Gu ?Point Detection for Electricity Market Analysis William Gu,

  7. The GONG++ DATA Processing Pipeline F. Hill,, J. Bolding, C. Toner, T. Corbard, S. Wampler, B. Goodrich, J. Goodrich, P. Eliason National Solar Observatory

    E-Print Network [OSTI]

    Corbard, Thierry

    The GONG++ DATA Processing Pipeline F. Hill,, J. Bolding, C. Toner, T. Corbard, S. Wampler, B. Goodrich, J. Goodrich, P. Eliason­ National Solar Observatory Introduction The GONG++ data processing pipeline is currently under construction. This system will produce the GONG++ science data products

  8. The AMMA-CATCH Gourma observatory site in Mali: Relating climatic variations to changes in vegetation, surface hydrology, fluxes and natural resources

    E-Print Network [OSTI]

    Guichard, Francoise

    The AMMA-CATCH Gourma observatory site in Mali: Relating climatic variations to changes, 38041 Grenoble Cedex 9, France c Centre IRD, Quartier Hippodrome, BP 2528, Bamako, Mali d Laboratoire, LMTG, F-31400 Toulouse, France l Institut d'Economie Rurale, BP 258 ­ rue Mohamed V, Bamako, Mali m

  9. VIRTUAL OBSERVATORY: Plate Content Digitization, Archive Mining & Image Sequence Processing edited by M. Tsvetkov, V. Golev, F. Murtagh, and R. Molina, Heron Press, Soa, 2005

    E-Print Network [OSTI]

    Project D. Mink1 , A. Doane2 R. Simcoe2 E. Los2 J. Grindlay3 1 Smithsonian Astrophysical Observatory digitizing the catalog of plates, constructing an automatic pipeline to make the scanned images useful. Telescopes in the United States, South America, New Zealand, and South Africa gave complete sky coverage over

  10. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under a cooperative agreement by Associated Universities, Inc. Astronomy: The Visible and Invisible Universe

    E-Print Network [OSTI]

    Groppi, Christopher

    under a cooperative agreement by Associated Universities, Inc. Astronomy: The Visible and Invisible Universe #12;The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under a cooperative agreement by Associated Universities, Inc. A light wave is a light wave

  11. Wax Point Determinations Using Acoustic Resonance Spectroscopy

    SciTech Connect (OSTI)

    Bostick, D.T.; Jubin, R.T.; Schmidt, T.W.

    2001-06-01

    The thermodynamic characterization of the wax point of a given crude is essential in order to maintain flow conditions that prevent plugging of undersea pipelines. This report summarizes the efforts made towards applying an Acoustic Cavity Resonance Spectrometer (ACRS) to the determination of pressures and temperatures at which wax precipitates from crude. Phillips Petroleum Company, Inc., the CRADA participant, supplied the ACRS. The instrumentation was shipped to Dr. Thomas Schmidt of ORNL, the CRADA contractor, in May 2000 after preliminary software development performed under the guidance of Dr. Samuel Colgate and Dr. Evan House of the University of Florida, Gainesville, Fl. Upon receipt it became apparent that a number of modifications still needed to be made before the ACRS could be precisely and safely used for wax point measurements. This report reviews the sequence of alterations made to the ACRS, as well as defines the possible applications of the instrumentation once the modifications have been completed. The purpose of this Cooperative Research and Development Agreement (CRADA) between Phillips Petroleum Company, Inc. (Participant) and Lockheed Martin Energy Research Corporation (Contractor) was the measurement of the formation of solids in crude oils and petroleum products that are commonly transported through pipelines. This information is essential in the proper design, operation and maintenance of the petroleum pipeline system in the United States. Recently, new petroleum discoveries in the Gulf of Mexico have shown that there is a potential for plugging of undersea pipeline because of the precipitation of wax. It is important that the wax points of the expected crude oils be well characterized so that the production facilities for these new wells are capable of properly transporting the expected production. The goal of this work is to perform measurements of solids formation in crude oils and petroleum products supplied by the Participant. It is anticipated that these data will be used in the design of new production facilities and in the development of thermodynamic models that describe the behavior of wax-saturated petroleum.

  12. Tipping Point Renewable Energy | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page| Open Energy Information Serbia-EnhancingEt Al., 2013)Open EnergyTinox Jump to: navigation, searchTipping Point

  13. Global integrators based on equispaced points 

    E-Print Network [OSTI]

    Kirker, Martha Jane

    1966-01-01

    . Sims for the patient and understanding guidance I received during the preparation of this thesis. TABLE OF CONTENTS Chapter Page I. INTRODUCTION . . . . . . . . . . . . . 1 II. GLOBAL INTEGRATORS . ~ . ~ ~ ~ ~ ~ ~ ~ ~ e ~ 3 III. PROGRAM... DESCRIPTION . . . ~ 13 IVo RESULTS a e a a ~ o ~ a ~ ~ ~ ~ e ~ e ~ 18 BIBLIOGRAPHY 20 APPENDIX 21 C HAP TER I INTRODUCTION A set of functions wl(x) wg(x) w +1(x) and n+1 a set of points xl, x2, --- x +1 can be found such that n&1 f(n)du = S wi...

  14. FortyPoint Seven | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QAsource History View New PagesSustainable Urban TransportFortistar LLC Jump to: navigation, search Name:FortyPoint

  15. Point Bio Energy LLC | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QAsource History ViewMayo, Maryland:NPIProtectio1975) |Texas: Energy Resources JumpOhio:Pod GeneratingPoint Bio

  16. Beryllium Program Points of Contact - Hanford Site

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

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity ofkandz-cm11 Outreach Home Room News PublicationsAudits & InspectionsBeryllium and Chronic BerylliumProgramProgram Points

  17. Star Point Wind Farm | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION JEnvironmental Jump to:EA EIS ReportEurope GmbHSoloPage EditStamford,Energy Center Wind FarmPoint

  18. Starting Points | National Nuclear Security Administration

    National Nuclear Security Administration (NNSA)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of NaturalDukeWakefield Municipal GasAdministration Medal01 Sandia4) August 20123/%2A en Signature ofSebStarting Points |

  19. power point | OpenEI Community

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIX ECoop IncIowa (UtilityMichigan)data book Homefuelleasingoutages Homeplanningpower point

  20. Microsoft PowerPoint - BSQ-300.pptx

    Energy Savers [EERE]

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on DeliciousMathematicsEnergyInterested Parties - WAPAEnergy May 28MarEnergy Microsoft PowerPoint -BSQ-300

  1. Points of Contact and Privacy Act Advisory

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

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity ofkandz-cm11 Outreach Home Room NewsInformationJesseworkSURVEYI/OPerformancePi Day Pi Day Pi DayPlasmaandAbout UsPoints

  2. Event Year Requirements Induction 1 mandatory; 10 training points

    E-Print Network [OSTI]

    Obbard, Darren

    /masterclass 30 training points (module I); 50 training points (module I and II) 20 hours Training strand 3Event Year Requirements Induction 1 mandatory; 10 training points Symposium All mandatory; 20 training points in Y1 only Training strand 1: Research skills Thematic group meetings (4) Advanced

  3. Input Observer: Measuring Text Entry and Pointing Performance from

    E-Print Network [OSTI]

    Wobbrock, Jacob O.

    Input Observer: Measuring Text Entry and Pointing Performance from Naturalistic Everyday Computer that will be capable of measuring a user's text entry and pointing abilities from everyday computer use "in the wild for both text entry and mouse pointing. Keywords Text entry, mouse pointing, field studies, naturalistic

  4. Low-melting point heat transfer fluid

    DOE Patents [OSTI]

    Cordaro, Joseph G. (Oakland, CA); Bradshaw, Robert W. (Livermore, CA)

    2011-04-12

    A low-melting point, heat transfer fluid comprising a mixture of LiNO.sub.3, NaNO.sub.3, KNO.sub.3, NaNO.sub.2 and KNO.sub.2 salts where the Li, Na and K cations are present in amounts of about 20-33.5 mol % Li, about 18.6-40 mol % Na, and about 40-50.3 mol % K and where the nitrate and nitrite anions are present in amounts of about 36-50 mol % NO.sub.3, and about 50-62.5 mol % NO.sub.2. These compositions can have liquidus temperatures between 70.degree. C. and 80.degree. C. for some compositions.

  5. A Search for Ultra-High Energy Neutrinos in Highly Inclined Events at the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Abreu, P [LIP, Coimbra; Lisbon, IST; Aglietta, M; Ahlers, M; Ahn, E J; Albuquerque, I F.M.; Allard, D

    2011-12-30

    The Surface Detector of the Pierre Auger Observatory is sensitive to neutrinos of all flavors above 0.1 EeV. These interact through charged and neutral currents in the atmosphere giving rise to extensive air showers. When interacting deeply in the atmosphere at nearly horizontal incidence, neutrinos can be distinguished from regular hadronic cosmic rays by the broad time structure of their shower signals in the water-Cherenkov detectors. In this paper we present for the first time an analysis based on down-going neutrinos. We describe the search procedure, the possible sources of background, the method to compute the exposure and the associated systematic uncertainties. No candidate neutrinos have been found in data collected from 1 January 2004 to 31 May 2010. Assuming an E-2 differential energy spectrum the limit on the single-flavor neutrino is E2dN/dE < 1.74 x 10-7 GeV cm-2s-1sr-1 at 90% C.L. in the energy range 1 x 1017eV < E < 1 x 1020 eV.

  6. An improved limit to the diffuse flux of ultra-high energy neutrinos from the Pierre Auger Observatory

    E-Print Network [OSTI]

    Aab, Alexander; Aglietta, Marco; Ahn, Eun-Joo; Samarai, Imen Al; Albuquerque, Ivone; Allekotte, Ingomar; Allison, Patrick; Almela, Alejandro; Castillo, Jesus Alvarez; Alvarez-Muñiz, Jaime; Batista, Rafael Alves; Ambrosio, Michelangelo; Aminaei, Amin; Anchordoqui, Luis; Andringa, Sofia; Aramo, Carla; Aranda, Victor Manuel; Arqueros, Fernando; Arsene, Nicusor; Asorey, Hernán Gonzalo; Assis, Pedro; Aublin, Julien; Ave, Maximo; Avenier, Michel; Avila, Gualberto; Awal, Nafiun; Badescu, Alina Mihaela; Barber, Kerri B; Bäuml, Julia; Baus, Colin; Beatty, Jim; Becker, Karl Heinz; Bellido, Jose A; Berat, Corinne; Bertaina, Mario Edoardo; Bertou, Xavier; Biermann, Peter; Billoir, Pierre; Blaess, Simon G; Blanco, Alberto; Blanco, Miguel; Bleve, Carla; Blümer, Hans; Bohá?ová, Martina; Boncioli, Denise; Bonifazi, Carla; Borodai, Nataliia; Brack, Jeffrey; Brancus, Iliana; Bridgeman, Ariel; Brogueira, Pedro; Brown, William C; Buchholz, Peter; Bueno, Antonio; Buitink, Stijn; Buscemi, Mario; Caballero-Mora, Karen S; Caccianiga, Barbara; Caccianiga, Lorenzo; Candusso, Marina; Caramete, Laurentiu; Caruso, Rossella; Castellina, Antonella; Cataldi, Gabriella; Cazon, Lorenzo; Cester, Rosanna; Chavez, Alan G; Chiavassa, Andrea; Chinellato, Jose Augusto; Chudoba, Jiri; Cilmo, Marco; Clay, Roger W; Cocciolo, Giuseppe; Colalillo, Roberta; Coleman, Alan; Collica, Laura; Coluccia, Maria Rita; Conceição, Ruben; Contreras, Fernando; Cooper, Mathew J; Cordier, Alain; Coutu, Stephane; Covault, Corbin; Cronin, James; Dallier, Richard; Daniel, Bruno; Dasso, Sergio; Daumiller, Kai; Dawson, Bruce R; de Almeida, Rogerio M; de Jong, Sijbrand J; De Mauro, Giuseppe; Neto, Joao de Mello; De Mitri, Ivan; de Oliveira, Jaime; de Souza, Vitor; del Peral, Luis; Deligny, Olivier; Dembinski, Hans; Dhital, Niraj; Di Giulio, Claudio; Di Matteo, Armando; Diaz, Johana Chirinos; Castro, Mary Lucia Díaz; Diogo, Francisco; Dobrigkeit, Carola; Docters, Wendy; D'Olivo, Juan Carlos; Dorofeev, Alexei; Hasankiadeh, Qader Dorosti; Dova, Maria Teresa; Ebr, Jan; Engel, Ralph; Erdmann, Martin; Erfani, Mona; Escobar, Carlos O; Espadanal, Joao; Etchegoyen, Alberto; Falcke, Heino; Fang, Ke; Farrar, Glennys; Fauth, Anderson; Fazzini, Norberto; Ferguson, Andrew P; Fernandes, Mateus; Fick, Brian; Figueira, Juan Manuel; Filevich, Alberto; Filip?i?, Andrej; Fox, Brendan; Fratu, Octavian; Freire, Martín Miguel; Fuchs, Benjamin; Fujii, Toshihiro; García, Beatriz; Garcia-Pinto, Diego; Gate, Florian; Gemmeke, Hartmut; Gherghel-Lascu, Alexandru; Ghia, Piera Luisa; Giaccari, Ugo; Giammarchi, Marco; Giller, Maria; G?as, Dariusz; Glaser, Christian; Glass, Henry; Golup, Geraldina; Berisso, Mariano Gómez; Vitale, Primo F Gómez; González, Nicolás; Gookin, Ben; Gordon, Jacob; Gorgi, Alessio; Gorham, Peter; Gouffon, Philippe; Griffith, Nathan; Grillo, Aurelio; Grubb, Trent D; Guardincerri, Yann; Guarino, Fausto; Guedes, Germano; Hampel, Matías Rolf; Hansen, Patricia; Harari, Diego; Harrison, Thomas A; Hartmann, Sebastian; Harton, John; Haungs, Andreas; Hebbeker, Thomas; Heck, Dieter; Heimann, Philipp; Herve, Alexander E; Hill, Gary C; Hojvat, Carlos; Hollon, Nicholas; Holt, Ewa; Homola, Piotr; Hörandel, Jörg; Horvath, Pavel; Hrabovský, Miroslav; Huber, Daniel; Huege, Tim; Insolia, Antonio; Isar, Paula Gina; Jandt, Ingolf; Jansen, Stefan; Jarne, Cecilia; Johnsen, Jeffrey A; Josebachuili, Mariela; Kääpä, Alex; Kambeitz, Olga; Kampert, Karl Heinz; Kasper, Peter; Katkov, Igor; Kégl, Balazs; Keilhauer, Bianca; Keivani, Azadeh; Kemp, Ernesto; Kieckhafer, Roger; Klages, Hans; Kleifges, Matthias; Kleinfeller, Jonny; Krause, Raphael; Krohm, Nicole; Krömer, Oliver; Kuempel, Daniel; Kunka, Norbert; LaHurd, Danielle; Latronico, Luca; Lauer, Robert; Lauscher, Markus; Lautridou, Pascal; Coz, Sandra Le; Lebrun, Didier; Lebrun, Paul; de Oliveira, Marcelo Augusto Leigui; Letessier-Selvon, Antoine; Lhenry-Yvon, Isabelle; Link, Katrin; Lopes, Luis; López, Rebeca; Casado, Aida López; Louedec, Karim; Lu, Lu; Lucero, Agustin; Malacari, Max; Maldera, Simone; Mallamaci, Manuela; Maller, Jennifer; Mandat, Dusan; Mantsch, Paul; Mariazzi, Analisa; Marin, Vincent; Mari?, Ioana; Marsella, Giovanni; Martello, Daniele; Martin, Lilian; Martinez, Humberto; Bravo, Oscar Martínez; Martraire, Diane; Meza, Jimmy Masías; Mathes, Hermann-Josef; Mathys, Sebastian; Matthews, James; Matthews, John; Matthiae, Giorgio; Maurel, Detlef; Maurizio, Daniela; Mayotte, Eric; Mazur, Peter; Medina, Carlos; Medina-Tanco, Gustavo; Meissner, Rebecca; Mello, Victor; Melo, Diego; Menshikov, Alexander; Messina, Stefano

    2015-01-01

    Neutrinos in the cosmic ray flux with energies near 1 EeV and above are detectable with the Surface Detector array of the Pierre Auger Observatory. We report here on searches through Auger data from 1 January 2004 until 20 June 2013. No neutrino candidates were found, yielding a limit to the diffuse flux of ultra-high energy neutrinos that challenges the Waxman-Bahcall bound predictions. Neutrino identification is attempted using the broad time-structure of the signals expected in the SD stations, and is efficiently done for neutrinos of all flavors interacting in the atmosphere at large zenith angles, as well as for "Earth-skimming" neutrino interactions in the case of tau neutrinos. In this paper the searches for downward-going neutrinos in the zenith angle bins $60^\\circ-75^\\circ$ and $75^\\circ-90^\\circ$ as well as for upward-going neutrinos, are combined to give a single limit. The $90\\%$ C.L. single-flavor limit to the diffuse flux of ultra-high energy neutrinos with an $E^{-2}$ spectrum in the energy ra...

  7. Characterizing the Habitable Zones of Exoplanetary Systems with a Large Ultraviolet/Visible/Near-IR Space Observatory

    E-Print Network [OSTI]

    France, Kevin; Linsky, Jeffrey; Roberge, Aki; Ayres, Thomas; Barman, Travis; Brown, Alexander; Davenport, James; Desert, Jean-Michel; Domagal-Goldman, Shawn; Fleming, Brian; Fontenla, Juan; Fossati, Luca; Froning, Cynthia; Hallinan, Gregg; Hawley, Suzanne; Hu, Renyu; Kaltenegger, Lisa; Kasting, James; Kowlaski, Adam; Loyd, Parke; Mauas, Pablo; Miguel, Yamila; Osten, Rachel; Redfield, Seth; Rugheimer, Sarah; Schneider, Christian; Segura, Antigona; Stocke, John; Tian, Feng; Tumlinson, Jason; Vieytes, Mariela; Walkowicz, Lucianne; Wood, Brian; Youngblood, Allison

    2015-01-01

    Understanding the surface and atmospheric conditions of Earth-size, rocky planets in the habitable zones (HZs) of low-mass stars is currently one of the greatest astronomical endeavors. Knowledge of the planetary effective surface temperature alone is insufficient to accurately interpret biosignature gases when they are observed in the coming decades. The UV stellar spectrum drives and regulates the upper atmospheric heating and chemistry on Earth-like planets, is critical to the definition and interpretation of biosignature gases, and may even produce false-positives in our search for biologic activity. This white paper briefly describes the scientific motivation for panchromatic observations of exoplanetary systems as a whole (star and planet), argues that a future NASA UV/Vis/near-IR space observatory is well-suited to carry out this work, and describes technology development goals that can be achieved in the next decade to support the development of a UV/Vis/near-IR flagship mission in the 2020s.

  8. Early-type stars observed in the ESO UVES Paranal Observatory Project - V. Time-variable interstellar absorption

    E-Print Network [OSTI]

    McEvoy, Catherine M; Dufton, Philip L; Smith, Keith T; Kennedy, Michael B; Keenan, Francis P; Lambert, David L; Welty, Daniel E; Lauroesch, James T

    2015-01-01

    The structure and properties of the diffuse interstellar medium (ISM) on small scales, sub-au to 1 pc, are poorly understood. We compare interstellar absorption-lines, observed towards a selection of O- and B-type stars at two or more epochs, to search for variations over time caused by the transverse motion of each star combined with changes in the structure in the foreground ISM. Two sets of data were used: 83 VLT- UVES spectra with approximately 6 yr between epochs and 21 McDonald observatory 2.7m telescope echelle spectra with 6 - 20 yr between epochs, over a range of scales from 0 - 360 au. The interstellar absorption-lines observed at the two epochs were subtracted and searched for any residuals due to changes in the foreground ISM. Of the 104 sightlines investigated with typically five or more components in Na I D, possible temporal variation was identified in five UVES spectra (six components), in Ca II, Ca I and/or Na I absorption-lines. The variations detected range from 7\\% to a factor of 3.6 in co...

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

    E-Print Network [OSTI]

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

    2014-01-01

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

  10. A Search for Ultra-High Energy Neutrinos in Highly Inclined Events at the Pierre Auger Observatory

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

    Abreu, P [LIP, Coimbra; Lisbon, IST; Aglietta, M; Ahlers, M; Ahn, E J; Albuquerque, I F.M.; Allard, D

    2011-12-30

    The Surface Detector of the Pierre Auger Observatory is sensitive to neutrinos of all flavors above 0.1 EeV. These interact through charged and neutral currents in the atmosphere giving rise to extensive air showers. When interacting deeply in the atmosphere at nearly horizontal incidence, neutrinos can be distinguished from regular hadronic cosmic rays by the broad time structure of their shower signals in the water-Cherenkov detectors. In this paper we present for the first time an analysis based on down-going neutrinos. We describe the search procedure, the possible sources of background, the method to compute the exposure and the associated systematic uncertainties. No candidate neutrinos have been found in data collected from 1 January 2004 to 31 May 2010. Assuming an E-2 differential energy spectrum the limit on the single-flavor neutrino is E2dN/dE -7 GeV cm-2s-1sr-1 at 90% C.L. in the energy range 1 x 1017eV 20 eV.

  11. A Search for Ultra-High Energy Neutrinos in Highly Inclined Events at the Pierre Auger Observatory

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

    Abreu, P

    2011-12-30

    The Surface Detector of the Pierre Auger Observatory is sensitive to neutrinos of all flavors above 0.1 EeV. These interact through charged and neutral currents in the atmosphere giving rise to extensive air showers. When interacting deeply in the atmosphere at nearly horizontal incidence, neutrinos can be distinguished from regular hadronic cosmic rays by the broad time structure of their shower signals in the water-Cherenkov detectors. In this paper we present for the first time an analysis based on down-going neutrinos. We describe the search procedure, the possible sources of background, the method to compute the exposure and the associatedmore »systematic uncertainties. No candidate neutrinos have been found in data collected from 1 January 2004 to 31 May 2010. Assuming an E-2 differential energy spectrum the limit on the single-flavor neutrino is E2dN/dE -7 GeV cm-2s-1sr-1 at 90% C.L. in the energy range 1 x 1017eV 20 eV.« less

  12. Precovery of near-Earth asteroids by a citizen-science project of the Spanish Virtual Observatory

    E-Print Network [OSTI]

    Solano, E; Pulido, R; Carry, B

    2013-01-01

    This article describes a citizen-science project conducted by the Spanish Virtual Observatory (SVO) to improve the orbits of near-Earth asteroids (NEAs) using data from astronomical archives. The list of NEAs maintained at the Minor Planet Center (MPC) is checked daily to identify new objects or changes in the orbital parameters of already catalogued objects. Using NEODyS we compute the position and magnitude of these objects at the observing epochs of the 938 046 images comprising the Eigth Data Release of the Sloan Digitised Sky Survey (SDSS). If the object lies within the image boundaries and the magnitude is brighter than the limiting magnitude, then the associated image is visually inspected by the project's collaborators (the citizens) to confirm or discard the presence of the NEA. If confirmed, accurate coordinates and, sometimes, magnitudes are submitted to the MPC. Using this methodology, 3,226 registered users have made during the first fifteen months of the project more than 167,000 measurements wh...

  13. Measurement of the proton-air cross-section at $\\sqrt{s}=57$ TeV with the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Collaboration, Auger

    2012-08-01

    We report a measurement of the proton-air cross section for particle production at the center-of-mass energy per nucleon of 57 TeV. This is derived from the distribution of the depths of shower maxima observed with the Pierre Auger Observatory: systematic uncertainties are studied in detail. Analyzing the tail of the distribution of the shower maxima, a proton-air cross section of [505 {+-} 22(stat){sub -36}{sup +28}(syst)] mb is found.

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

    SciTech Connect (OSTI)

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

    2011-12-20

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

  15. Two-point derivative dispersion relations

    E-Print Network [OSTI]

    Erasmo Ferreira; Javier Sesma

    2014-03-24

    A new derivation is given for the representation, under certain conditions, of the integral dispersion relations of scattering theory through local forms. The resulting expressions have been obtained through an independent procedure to construct the real part, and consist of new mathematical structures of double infinite summations of derivatives. In this new form the derivatives are calculated at the generic value of the energy $E$ and separately at the reference point $E=m$ that is the lower limit of the integration. This new form may be more interesting in certain circumstances and directly shows the origin of the difficulties in convergence that were present in the old truncated forms called standard-DDR. For all cases in which the reductions of the double to single sums were obtained in our previous work, leading to explicit demonstration of convergence, these new expressions are seen to be identical to the previous ones. We present, as a glossary, the most simplified explicit results for the DDR's in the cases of imaginary amplitudes of forms $(E/m)^\\lambda[\\ln (E/m)]^n$, that cover the cases of practical interest in particle physics phenomenology at high energies. We explicitly study the expressions for the cases with $\\lambda$ negative odd integers, that require identification of cancelation of singularities, and provide the corresponding final results.

  16. on equilibrium points of logarithmic and newtonian potentials

    E-Print Network [OSTI]

    2006-07-18

    Thus the question is whether such a field must always have an equilibrium point, that is a point upon which a free electron (or wire) once placed would remain.

  17. Scott Runnels of Computational Physics to teach at West Point

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

    at West Point Runnels has been selected for a two-year faculty post in the Department of Physics and Nuclear Engineering at West Point. March 19, 2013 Scott Runnels Scott Runnels...

  18. Improvements in floating point addition/subtraction operations

    DOE Patents [OSTI]

    Farmwald, P.M.

    1984-02-24

    Apparatus is described for decreasing the latency time associated with floating point addition and subtraction in a computer, using a novel bifurcated, pre-normalization/post-normalization approach that distinguishes between differences of floating point exponents.

  19. A Martingale Approach to Point Processes in the Plane

    E-Print Network [OSTI]

    Merzbach, Ely; Nualart, David

    1988-02-05

    A rigorous definition of two-parameter point processes is given as a distribution of a denumerable number of random points in the plane. A characterization with stopping lines and relation with predictability are obtained. Using the one...

  20. Period tripling accumulation point for complexified Henon map

    E-Print Network [OSTI]

    O. B. Isaeva; S. P. Kuznetsov

    2005-09-06

    Accumulation point of period-tripling bifurcations for complexified Henon map is found. Universal scaling properties of parameter space and Fourier spectrum intrinsic to this critical point is demonstrated.

  1. Indirect L to T point optical transition in bismuth nanowires

    E-Print Network [OSTI]

    Levin, A. J.

    An indirect electronic transition from the L point valence band to the T point valence band has been previously observed in Bi nanowires oriented along the [011? 2] crystalline direction (used by Black et al. and by Reppert ...

  2. CenterPoint Energy Low-Rise Multi Family Program

    Broader source: Energy.gov [DOE]

    Note: This Incentive is only available to customers in the CenterPoint Energy Houston electric territory.

  3. CenterPoint Energy Healthcare Energy Efficiency Program

    Broader source: Energy.gov [DOE]

    Note: Program is only available to electric customers in CenterPoint Energy's service territory (greater Houston, Texas area)

  4. LARGE DUST PARTICLES FROM COMETS. K. J. Meech, Institute for Astronomy, University of Hawaii, Honolulu HI, 96822, USA, meech@ifa.hawaii.edu, T. L. Farnham, Lowell Observatory, Flagstaff, AZ 86001, farnham@lowell.edu.

    E-Print Network [OSTI]

    Meech, Karen Jean

    LARGE DUST PARTICLES FROM COMETS. K. J. Meech, Institute for Astronomy, University of Hawaii, Honolulu HI, 96822, USA, meech@ifa.hawaii.edu, T. L. Farnham, Lowell Observatory, Flagstaff, AZ 86001

  5. Sur les surfaces lorentziennes compactes sans points conjugus

    E-Print Network [OSTI]

    Mounoud, Pierre

    Sur les surfaces lorentziennes compactes sans points conjugués CHRISTOPHE BAVARD PIERRE MOUNOUD Nous prouvons l'existence de métriques sans points conjugués dans toute com- posante connexe de l lorentziens sans points conjugués non plats contraste avec la situation riemannienne (théorème de E. Hopf). We

  6. SPATIAL POINT PROCESSES AND GRAPH BASED STATISTICAL FEATURES

    E-Print Network [OSTI]

    Jyväskylä, University of

    2010 2000 Mathematics Subject Classification. 60G55, 62-07, 62M30. ISSN 1457-9235 #12;SPATIAL POINT Classification. 60G55, 62-07, 62M30. 1 #12;Spatial point processes and graph based statistical features Tuomas library has been developed for the computation of the graph-based summaries. Keywords: Spatial point

  7. Coarser connected topologies and non-normality points

    E-Print Network [OSTI]

    Yengulalp, Lynne Christine

    2009-01-01

    point of the Stone-Cech remainder of a space a non-normality point of the remainder? We will discuss the question in the case that X is a discrete space and then when X is a metric space without isolated points. We show that under certain set...

  8. COE March 4, 2009 Fractal Point Events in Physics, Biology,

    E-Print Network [OSTI]

    Teich, Malvin C.

    -CONVERSION: ENTANGLED PHOTONS Laser c(2) Crystal Signal Idler Pump kr wr r ks ws s ki wi i wr = ws + wi RANDOM POINT EVENTS IN NEUROPHYSIOLOGY WHAT ARE THE COUNTING STATISTICS OF THESE POINT EVENTS? #12;COE ­ March 4, 2009 COUNTING STATISTICS FOR POINT EVENTS IN THE MAMMALIAN AUDITORY SYSTEM Eighth

  9. Seven points in P2 and the universal Kummer threefold

    E-Print Network [OSTI]

    California at Berkeley, University of

    Sturmfels (Seven points in P2 and the universal Kummer threefoldSep 27, 2012 6 / 17 #12;Weyl group on P6Seven points in P2 and the universal Kummer threefold Qingchun Ren UC Berkeley Joint work Sam, Gus Schrader and Bernd Sturmfels (Seven points in P2 and the universal Kummer threefoldSep 27

  10. Access Point Selection for Improving Throughput Fairness in Wireless LANs

    E-Print Network [OSTI]

    Siris, Vasilios A.

    Access Point Selection for Improving Throughput Fairness in Wireless LANs Vasilios A. Siris investigate the problem of access point selection in wireless LANs based on the IEEE 802.11 standard, when solely at the wireless stations, which passively monitor the activity of each access point's channel

  11. Best Entry Points for Structured Document Retrieval Part I: Characteristics

    E-Print Network [OSTI]

    Lalmas, Mounia

    Best Entry Points for Structured Document Retrieval ­ Part I: Characteristics Jane Reida , Mounia documents. This paper examines the concept of best entry points, which are document components from which investigates the basic characteristics of best entry points. Keywords: Structured document retrieval, focussed

  12. An Evaluation of Volumetric Interest Points University of Cambridge

    E-Print Network [OSTI]

    Martin, Ralph R.

    An Evaluation of Volumetric Interest Points Tsz-Ho Yu University of Cambridge Cambridge, UK thy23 the first performance eval- uation of interest points on scalar volumetric data. Such data encodes 3D shape detectors of interest points in volumetric data, in terms of repeatability, number and nature of interest

  13. Redevelopment and the Politics of Place in Bayview-Hunters Point

    E-Print Network [OSTI]

    Dillon, Lindsey

    2011-01-01

    2011. 2011. Hunters Point Shipyard: A Shifting Landscape.Point/Hunters Point Shipyard Phase II: Urban Design1973. Hunters Point Naval Shipyard Economic Re-Use Study.

  14. ASPCAP: The Apogee Stellar Parameter and Chemical Abundances Pipeline

    E-Print Network [OSTI]

    Pérez, Ana E García; Holtzman, Jon A; Shetrone, Matthew; Mészáros, Szabolcs; Bizyaev, Dmitry; Carrera, Ricardo; Cunha, Katia; García-Hernández, D A; Johnson, Jennifer A; Majewski, Steven R; Nidever, David L; Schiavon, Ricardo P; Shane, Neville; Smith, Verne V; Sobeck, Jennifer; Troup, Nicholas; Zamora, Olga; Bovy, Jo; Eisenstein, Daniel J; Feuillet, Diane; Frinchaboy, Peter M; Hayden, Michael R; Hearty, Fred R; Nguyen, Duy C; O'Connell, Robert W; Pinsonneault, Marc H; Weinberg, David H; Wilson, John C; Zasowski, Gail

    2015-01-01

    The Apache Point Observatory Galactic Evolution Experiment (APOGEE) has built the largest moderately high-resolution (R=22, 500) spectroscopic map of the stars across the Milky Way, and including dust-obscured areas. The APOGEE Stellar Parameter and Chemical Abundances Pipeline (ASPCAP) is the software developed for the automated analysis of these spectra. ASPCAP determines atmospheric parameters and chemical abundances from observed spectra by comparing observed spectra to libraries of theoretical spectra, using chi-2 minimization in a multidimensional parameter space. The package consists of a fortran90 code that does the actual minimization, and a wrapper IDL code for book-keeping and data handling. This paper explains in detail the ASPCAP components and functionality, and presents results from a number of tests designed to check its performance. ASPCAP provides stellar effective temperatures, surface gravities, and metallicities precise to 2%, 0.1 dex, and 0.05 dex, respectively, for most APOGEE stars, wh...

  15. A Kiloparsec-Scale Nuclear Stellar Disk in the Milky Way

    E-Print Network [OSTI]

    Debattista, Victor P; Earp, Samuel W F; Cole, David R

    2015-01-01

    Gas in the Milky Way is driven inwards by its bar, some of it settling into a disk extending to Galactocentric radius $\\sim 1.4 \\kpc$. The stellar distribution in this region has not been well understood because of stellar crowding and high extinction. Here we use a high resolution simulation of a barred galaxy, which crucially includes gas and star formation, to guide our interpretation of the Apache Point Observatory Galactic Evolution Experiment (APOGEE) stellar velocity data for the inner Milky Way. We show that the data favor the presence of a thin, rapidly-rotating, nuclear disk extending to $\\sim 1 \\kpc$. This is the first detection of a nuclear stellar disk in the Milky Way.

  16. Compound nucleus decay: Comparison between saddle point and scission point barriers

    SciTech Connect (OSTI)

    Santos, T. J.; Carlson, B. V.

    2014-11-11

    One of the principal characteristics of nuclear multifragmentation is the emission of complex fragments of intermediate mass. An extension of the statistical multifragmentation model has been developed, in which the process can be interpreted as the near simultaneous limit of a series of sequential binary decays. In this extension, intermediate mass fragment emissions are described by expressions almost identical to those of light particle emission. At lower temperatures, similar expressions have been shown to furnish a good description of very light intermediate mass fragment emission but not of the emission of heavier fragments, which seems to be determined by the transition density at the saddle-point rather than at the scission point. Here, we wish to compare these different formulations of intermediate fragmment emission and analyze the extent to which they remain distinguishable at high excitation energy.

  17. Dual-domain point diffraction interferometer

    DOE Patents [OSTI]

    Naulleau, Patrick P. (5239 Miles Ave., Apt. A, Oakland, CA 94618); Goldberg, Kenneth Alan (1195 Keeler Ave., Berkeley, CA 94708)

    2000-01-01

    A hybrid spatial/temporal-domain point diffraction interferometer (referred to as the dual-domain PS/PDI) that is capable of suppressing the scattered-reference-light noise that hinders the conventional PS/PDI is provided. The dual-domain PS/PDI combines the separate noise-suppression capabilities of the widely-used phase-shifting and Fourier-transform fringe pattern analysis methods. The dual-domain PS/PDI relies on both a more restrictive implementation of the image plane PS/PDI mask and a new analysis method to be applied to the interferograms generated and recorded by the modified PS/PDI. The more restrictive PS/PDI mask guarantees the elimination of spatial-frequency crosstalk between the signal and the scattered-light noise arising from scattered-reference-light interfering with the test beam. The new dual-domain analysis method is then used to eliminate scattered-light noise arising from both the scattered-reference-light interfering with the test beam and the scattered-reference-light interfering with the "true" pinhole-diffracted reference light. The dual-domain analysis method has also been demonstrated to provide performance enhancement when using the non-optimized standard PS/PDI design. The dual-domain PS/PDI is essentially a three-tiered filtering system composed of lowpass spatial-filtering the test-beam electric field using the more restrictive PS/PDI mask, bandpass spatial-filtering the individual interferogram irradiance frames making up the phase-shifting series, and bandpass temporal-filtering the phase-shifting series as a whole.

  18. Searches for anisotropies in the arrival directions of the highest energy cosmic rays detected by the Pierre Auger Observatory

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

    Aab, A.; Abreu, P.; Aglietta, M.; Ahn, E. J.; Samarai, I. Al; Albuquerque, I. F. M.; Allekotte, I.; Allen, J.; Allison, P.; Almela, A.; et al

    2015-04-24

    In this study, we analyze the distribution of arrival directions of ultra-high-energy cosmic rays recorded at the Pierre Auger Observatory in 10 years of operation. The data set, about three times larger than that used in earlier studies, includes arrival directions with zenith angles up to 80°, thus covering from $-90{}^\\circ $ to $+45{}^\\circ $ in declination. After updating the fraction of events correlating with the active galactic nuclei (AGNs) in the Véron-Cetty and Véron catalog, we subject the arrival directions of the data with energies in excess of 40 EeV to different tests for anisotropy. We search for localizedmore »excess fluxes, self-clustering of event directions at angular scales up to 30°, and different threshold energies between 40 and 80 EeV. We then look for correlations of cosmic rays with celestial structures both in the Galaxy (the Galactic Center and Galactic Plane) and in the local universe (the Super-Galactic Plane). We also examine their correlation with different populations of nearby extragalactic objects: galaxies in the 2MRS catalog, AGNs detected by Swift-BAT, radio galaxies with jets, and the Centaurus A (Cen A) galaxy. None of the tests show statistically significant evidence of anisotropy. The strongest departures from isotropy (post-trial probability $\\sim 1.4$%) are obtained for cosmic rays with $E\\gt 58$ EeV in rather large windows around Swift AGNs closer than 130 Mpc and brighter than 1044 erg/s (18° radius), and around the direction of Centaurus A (15° radius).« less

  19. A search for anisotropy in the arrival directions of ultra high energy cosmic rays recorded at the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Abreu, P.; ,

    2012-01-01

    Observations of cosmic ray arrival directions made with the Pierre Auger Observatory have previously provided evidence of anisotropy at the 99% CL using the correlation of ultra high energy cosmic rays (UHECRs) with objects drawn from the Veron-Cetty Veron catalog. In this paper we report on the use of three catalog independent methods to search for anisotropy. The 2pt-L, 2pt+ and 3pt methods, each giving a different measure of self-clustering in arrival directions, were tested on mock cosmic ray data sets to study the impacts of sample size and magnetic smearing on their results, accounting for both angular and energy resolutions. If the sources of UHECRs follow the same large scale structure as ordinary galaxies in the local Universe and if UHECRs are deflected no more than a few degrees, a study of mock maps suggests that these three methods can efficiently respond to the resulting anisotropy with a P-value = 1.0% or smaller with data sets as few as 100 events. Using data taken from January 1, 2004 to July 31, 2010 we examined the 20, 30, ..., 110 highest energy events with a corresponding minimum energy threshold of about 51 EeV. The minimum P-values found were 13.5% using the 2pt-L method, 1.0% using the 2pt+ method and 1.1% using the 3pt method for the highest 100 energy events. In view of the multiple (correlated) scans performed on the data set, these catalog-independent methods do not yield strong evidence of anisotropy in the highest energy cosmic rays.

  20. 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.

  1. A digital seismogram archive of nuclear explosion signals, recorded at the Borovoye Geophysical Observatory, Kazakhstan, from 1966 to 1996

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

    An, Vadim A.; Ovtchinnikov, Vladimir M.; Kaazik, Pyotr B.; Adushkin, Vitaly V.; Sokolova, Inna N.; Aleschenko, Iraida B.; Mikhailova, Natalya N.; Kim, Won -Young; Richards, Paul G.; Patton, Howard J.; et al

    2015-03-27

    Seismologists from Kazakhstan, Russia, and the United States have rescued the Soviet-era archive of nuclear explosion seismograms recorded at Borovoye in northern Kazakhstan during the period 1966–1996. The signals had been stored on about 8000 magnetic tapes, which were held at the recording observatory. After hundreds of man-years of work, these digital waveforms together with significant metadata are now available via the project URL, namely http://www.ldeo.columbia.edu/res/pi/Monitoring/Data/ as a modern open database, of use to diverse communities. Three different sets of recording systems were operated at Borovoye, each using several different seismometers and different gain levels. For some explosions, more thanmore »twenty different channels of data are available. A first data release, in 2001, contained numerous glitches and lacked many instrument responses, but could still be used for measuring accurate arrival times and for comparison of the strengths of different types of seismic waves. The project URL also links to our second major data release, for nuclear explosions in Eurasia recorded in Borovoye, in which the data have been deglitched, all instrument responses have been included, and recording systems are described in detail. This second dataset consists of more than 3700 waveforms (digital seismograms) from almost 500 nuclear explosions in Eurasia, many of them recorded at regional distances. It is important as a training set for the development and evaluation of seismological methods of discriminating between earthquakes and underground explosions, and can be used for assessment of three-dimensional models of the Earth’s interior structure.« less

  2. Searches for anisotropies in the arrival directions of the highest energy cosmic rays detected by the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Aab, A.; Abreu, P.; Aglietta, M.; Ahn, E. J.; Samarai, I. Al; Albuquerque, I. F. M.; Allekotte, I.; Allen, J.; Allison, P.; Almela, A.; Castillo, J. Alvarez; Alvarez-Muñiz, J.; Batista, R. Alves; Ambrosio, M.; Aminaei, A.; Anchordoqui, L.; Andringa, S.; Aramo, C.; Aranda, V. M.; Arqueros, F.; Asorey, H.; Assis, P.; Aublin, J.; Ave, M.; Avenier, M.; Avila, G.; Awal, N.; Badescu, A. M.; Barber, K. B.; Bäuml, J.; Baus, C.; Beatty, J. J.; Becker, K. H.; Bellido, J. A.; Berat, C.; Bertaina, M. E.; Bertou, X.; Biermann, P. L.; Billoir, P.; Blaess, S. G.; Blanco, M.; Bleve, C.; Blümer, H.; Bohá?ová, M.; Boncioli, D.; Bonifazi, C.; Bonino, R.; Borodai, N.; Brack, J.; Brancus, I.; Bridgeman, A.; Brogueira, P.; Brown, W. C.; Buchholz, P.; Bueno, A.; Buitink, S.; Buscemi, M.; Caballero-Mora, K. S.; Caccianiga, B.; Caccianiga, L.; Candusso, M.; Caramete, L.; Caruso, R.; Castellina, A.; Cataldi, G.; Cazon, L.; Cester, R.; Chavez, A. G.; Chiavassa, A.; Chinellato, J. A.; Chudoba, J.; Cilmo, M.; Clay, R. W.; Cocciolo, G.; Colalillo, R.; Coleman, A.; Collica, L.; Coluccia, M. R.; Conceição, R.; Contreras, F.; Cooper, M. J.; Cordier, A.; Coutu, S.; Covault, C. E.; Cronin, J.; Curutiu, A.; Dallier, R.; Daniel, B.; Dasso, S.; Daumiller, K.; Dawson, B. R.; Almeida, R. M. de; Domenico, M. De; Jong, S. J. de; Neto, J. R. T. de Mello; Mitri, I. De; Oliveira, J. de; Souza, V. de; Peral, L. del; Deligny, O.; Dembinski, H.; Dhital, N.; Giulio, C. Di; Matteo, A. Di; Diaz, J. C.; Castro, M. L. Díaz; Diogo, F.; Dobrigkeit, C.; Docters, W.; D’Olivo, J. C.; Dorofeev, A.; Hasankiadeh, Q. Dorosti; Dova, M. T.; Ebr, J.; Engel, R.; Erdmann, M.; Erfani, M.; Escobar, C. O.; Espadanal, J.; Etchegoyen, A.; Luis, P. Facal San; Falcke, H.; Fang, K.; Farrar, G.; Fauth, A. C.; Fazzini, N.; Ferguson, A. P.; Fernandes, M.; Fick, B.; Figueira, J. M.; Filevich, A.; Filip?i?, A.; Fox, B. D.; Fratu, O.; Freire, M. M.; Fröhlich, U.; Fuchs, B.; Fujii, T.; Gaior, R.; García, B.; Gamez, D. Garcia-; Pinto, D. Garcia-; Garilli, G.; Bravo, A. Gascon; Gate, F.; Gemmeke, H.; Ghia, P. L.; Giaccari, U.; Giammarchi, M.; Giller, M.; Glaser, C.; Glass, H.; Berisso, M. Gómez; Vitale, P. F. Gómez; Gonçalves, P.; Gonzalez, J. G.; González, N.; Gookin, B.; Gordon, J.; Gorgi, A.; Gorham, P.; Gouffon, P.; Grebe, S.; Griffith, N.; Grillo, A. F.; Grubb, T. D.; Guarino, F.; Guedes, G. P.; Hampel, M. R.; Hansen, P.; Harari, D.; Harrison, T. A.; Hartmann, S.; Harton, J. L.; Haungs, A.; Hebbeker, T.; Heck, D.; Heimann, P.; Herve, A. E.; Hill, G. C.; Hojvat, C.; Hollon, N.; Holt, E.; Homola, P.; Hörandel, J. R.; Horvath, P.; Hrabovský, M.; Huber, D.; Huege, T.; Insolia, A.; Isar, P. G.; Jandt, I.; Jansen, S.; Jarne, C.; Josebachuili, M.; Kääpä, A.; Kambeitz, O.; Kampert, K. H.; Kasper, P.; Katkov, I.; Kégl, B.; Keilhauer, B.; Keivani, A.; Kemp, E.; Kieckhafer, R. M.; Klages, H. O.; Kleifges, M.; Kleinfeller, J.; Krause, R.; Krohm, N.; Krömer, O.; Hansen, D. Kruppke-; Kuempel, D.; Kunka, N.; LaHurd, D.; Latronico, L.; Lauer, R.; Lauscher, M.; Lautridou, P.; Coz, S. Le; Leão, M. S. A. B.; Lebrun, D.; Lebrun, P.; Leigui de Oliveira, M. A.; Letessier-Selvon, A.; Lhenry-Yvon, I.; Link, K.; López, R.; Louedec, K.; Bahilo, J. Lozano; Lu, L.; Lucero, A.; Ludwig, M.; Malacari, M.; Maldera, S.; Mallamaci, M.; Maller, J.; Mandat, D.; Mantsch, P.; Mariazzi, A. G.; Marin, V.; Mari?, I. C.; Marsella, G.; Martello, D.; Martin, L.; Martinez, H.; Bravo, O. Martínez; Martraire, D.; Meza, J. J. Masías; Mathes, H. J.; Mathys, S.; Matthews, J.; Matthews, J. A. J.; Matthiae, G.; Maurel, D.; Maurizio, D.; Mayotte, E.; Mazur, P. O.; Medina, C.; Tanco, G. Medina-; Meissner, R.; Melissas, M.; Melo, D.; Menshikov, A.; Messina, S.; Meyhandan, R.; Mi?anovi?, S.; Micheletti, M. I.; Middendorf, L.; Minaya, I. A.; Miramonti, L.; Mitrica, B.; Bueno, L. Molina-; Mollerach, S.; Monasor, M.; Ragaigne, D. Monnier; Montanet, F.; Morello, C.; Mostafá, M.; Moura, C. A.; Muller, M. A.; Müller, G.; Müller, S.; Münchmeyer, M.; Mussa, R.; Navarra, G.; Navas, S.; Necesal, P.; Nellen, L.; Nelles, A.; Neuser, J.; Nguyen, P. H.; Niechciol, M.; Niemietz, L.; Niggemann, T.; Nitz, D.; Nosek, D.; Novotny, V.; Nožka, L.; Ochilo, L.; Oikonomou, F.; Olinto, A.; Oliveira, M.; Pacheco, N.; Dei, D. Pakk Selmi-; Palatka, M.; Pallotta, J.; Palmieri, N.; Papenbreer, P.; Parente, G.; Parra, A.; Paul, T.; Pech, M.; P?kala, J.; Pelayo, R.; Pepe, I. M.; Perrone, L.; Petermann, E.; Peters, C.; Petrera, S.; Petrov, Y.; Phuntsok, J.; Piegaia, R.; Pierog, T.; Pieroni, P.; Pimenta, M.; Pirronello, V.; Platino, M.; Plum, M.; Porcelli, A.; Porowski, C.; Prado, R. R.; Privitera, P.; Prouza, M.; Purrello, V.; Quel, E. J.; Querchfeld, S.; Quinn, S.; Rautenberg, J.; Ravel, O.; Ravignani, D.

    2015-04-24

    In this study, we analyze the distribution of arrival directions of ultra-high-energy cosmic rays recorded at the Pierre Auger Observatory in 10 years of operation. The data set, about three times larger than that used in earlier studies, includes arrival directions with zenith angles up to 80°, thus covering from $-90{}^\\circ $ to $+45{}^\\circ $ in declination. After updating the fraction of events correlating with the active galactic nuclei (AGNs) in the Véron-Cetty and Véron catalog, we subject the arrival directions of the data with energies in excess of 40 EeV to different tests for anisotropy. We search for localized excess fluxes, self-clustering of event directions at angular scales up to 30°, and different threshold energies between 40 and 80 EeV. We then look for correlations of cosmic rays with celestial structures both in the Galaxy (the Galactic Center and Galactic Plane) and in the local universe (the Super-Galactic Plane). We also examine their correlation with different populations of nearby extragalactic objects: galaxies in the 2MRS catalog, AGNs detected by Swift-BAT, radio galaxies with jets, and the Centaurus A (Cen A) galaxy. None of the tests show statistically significant evidence of anisotropy. The strongest departures from isotropy (post-trial probability $\\sim 1.4$%) are obtained for cosmic rays with $E\\gt 58$ EeV in rather large windows around Swift AGNs closer than 130 Mpc and brighter than 1044 erg/s (18° radius), and around the direction of Centaurus A (15° radius).

  3. Overview of the Manitou Experimental Forest Observatory: site description and selected science results from 2008 to 2013

    SciTech Connect (OSTI)

    Ortega, John; Turnipseed, A.; Guenther, Alex B.; Karl, Thomas G.; Day, D. A.; Gochis, David; Huffman, J. A.; Prenni, Anthony J.; Levin, E. J.; Kreidenweis, Sonia M.; DeMott, Paul J.; Tobo, Y.; Patton, E. G.; Hodzic, Alma; Cui, Y. Y.; Harley, P.; Hornbrook, R. S.; Apel, E. C.; Monson, Russell K.; Eller, A. S.; Greenberg, J. P.; Barth, Mary; Campuzano-Jost, Pedro; Palm, B. B.; Jiminez, J. L.; Aiken, A. C.; Dubey, Manvendra K.; Geron, Chris; Offenberg, J.; Ryan, M. G.; Fornwalt, Paula J.; Pryor, S. C.; Keutsch, Frank N.; DiGangi, J. P.; Chan, A. W.; Goldstein, Allen H.; Wolfe, G. M.; Kim, S.; Kaser, L.; Schnitzhofer, R.; Hansel, A.; Cantrell, Chris; Mauldin, R. L.; Smith, James N.

    2014-01-01

    The Bio-hydro-atmosphere interactions of Energy, Aerosols, Carbon, H2O, Organics & Nitrogen (BEACHON) project seeks to understand the feedbacks and interrelationships between hydrology, biogenic emissions, carbon assimilation, aerosol properties, clouds and associated feedbacks within water-limited ecosystems. The Manitou Experimental Forest Observatory (MEFO) was established in 2008 by the National Center for Atmospheric Research to address many of the BEACHON research objectives, and it now provides a fixed field site with significant infrastructure. MEFO is a mountainous, semi-arid ponderosa pine-dominated forest site that is normally dominated by clean continental air but is periodically influenced by anthropogenic sources from Colorado Front Range cities. This article summarizes the past and ongoing research activities at the site, and highlights some of the significant findings that have resulted from these measurements. These activities include – soil property measurements; – hydrological studies; – measurements of high-frequency turbulence parameters; – eddy covariance flux measurements of water, energy, aerosols and carbon dioxide through the canopy; – determination of biogenic and anthropogenic volatile organic compound emissions and their influence on regional atmospheric chemistry; – aerosol number and mass distributions; – chemical speciation of aerosol particles; – characterization of ice and cloud condensation nuclei; – trace gas measurements; and – model simulations using coupled chemistry and meteorology. In addition to various long-term continuous measurements, three focused measurement campaigns with state-of-the-art instrumentation have taken place since the site was established, and two of these studies are the subjects of this special issue: BEACHON-ROCS (Rocky Mountain Organic Carbon Study, 2010) and BEACHON-RoMBAS (Rocky Mountain Biogenic Aerosol Study, 2011).

  4. Science in Context, Vol. 22, No. 3 The Hotel that Became an Observatory: Mount Faulhorn as Singularity, Microcosm, and

    E-Print Network [OSTI]

    Aubin, David

    . In this paper, I take this mountain as my entry point into the examination of the special attraction managed, at advantageous cost, as [I did with respect to] my stay here. The climb up took from 6 at such altitude, new telescopic stars and new comets might perhaps be discovered whose weak rays would never break

  5. HAWC ?-Ray Observatory

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

    States. Personnel from the Institutes of Astronomy, Nuclear Sciences, Physics, and Geophysics at UNAM and INAOE have played a very prominent role in the construction of HAWC and...

  6. European Southern Observatory

    E-Print Network [OSTI]

    Liske, Jochen

    ? These objects may be visible through their supernovae/hypernovae or their surrounding ionization zones. How many

  7. Armagh Observatory Annual Report

    E-Print Network [OSTI]

    . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 24 4.2 Light Pollution

  8. Glenn Schneider Steward Observatory

    E-Print Network [OSTI]

    Schneider, Glenn

    , the recent solar eclipse can fairly lay claim to be the first astronomical event to be observed from an airplane. Although the flight and observation made at Fort Sill, Okla., were not undertaken with any: ECLIPSE OBSERVATIONS FROM AIRPLANES 1st Flight: TSE 08 June 1918, Fort Sill, Oklahoma, USA #12;Scientific

  9. Observatory Joachim Puls

    E-Print Network [OSTI]

    Crowther, Paul

    for expanding atmospheres with the isothermal sound, speed a v 2 v v 1 d GM a da a dr r r dr g esc can be neglected, sinc 2 v a v v 1 v e GM a R d GM g g g g GM dr r r 2 1 ( ) GM r r luminosity in wind at infinity is vv v 2 with maximum m v ass loss, if 2 2 2 GM GM L M M R R L L

  10. A SEARCH FOR POINT SOURCES OF EeV NEUTRONS

    SciTech Connect (OSTI)

    Abreu, P.; Andringa, S.; Aglietta, M.; Ahlers, M.; Ahn, E. J.; Albuquerque, I. F. M.; Allard, D.; Allekotte, I.; Allen, J.; Allison, P.; Almela, A.; Alvarez Castillo, J.; Alvarez-Muniz, J.; Alves Batista, R.; Ambrosio, M.; Aramo, C.; Aminaei, A.; Anchordoqui, L.; Antici'c, T.; Arganda, E.; Collaboration: Pierre Auger Collaboration; and others

    2012-12-01

    A thorough search of the sky exposed at the Pierre Auger Cosmic Ray Observatory reveals no statistically significant excess of events in any small solid angle that would be indicative of a flux of neutral particles from a discrete source. The search covers from -90 Degree-Sign to +15 Degree-Sign in declination using four different energy ranges above 1 EeV (10{sup 18} eV). The method used in this search is more sensitive to neutrons than to photons. The upper limit on a neutron flux is derived for a dense grid of directions for each of the four energy ranges. These results constrain scenarios for the production of ultrahigh energy cosmic rays in the Galaxy.

  11. Low Energy Threshold Analysis of the Phase I and Phase II Data Sets of the Sudbury Neutrino Observatory

    E-Print Network [OSTI]

    The SNO Collaboration

    2010-06-09

    Results are reported from a joint analysis of Phase I and Phase II data from the Sudbury Neutrino Observatory. The effective electron kinetic energy threshold used is T_eff=3.5 MeV, the lowest analysis threshold yet achieved with water Cherenkov detector data. In units of 10^6 cm^{-2} s^{-1}, the total flux of active-flavor neutrinos from 8B decay in the Sun measured using the neutral current (NC) reaction of neutrinos on deuterons, with no constraint on the 8B neutrino energy spectrum, is found to be Phi_NC = 5.140 ^{+0.160}_{-0.158} (stat) ^{+0.132}_{-0.117} (syst). These uncertainties are more than a factor of two smaller than previously published results. Also presented are the spectra of recoil electrons from the charged current reaction of neutrinos on deuterons and the elastic scattering of electrons. A fit to the SNO data in which the free parameters directly describe the total 8B neutrino flux and the energy-dependent nu_e survival probability provides a measure of the total 8B neutrino flux Phi_8B = 5.046 ^{+0.159}_{-0.152} (stat) ^{+0.107}_{-0.123} (syst). Combining these new results with results of all other solar experiments and the KamLAND reactor experiment yields best-fit values of the mixing parameters of theta_{12}=34.06 ^{+1.16}_{-0.84} degrees and Delta m^2_{21}=7.59 ^{+0.20}_{-0.21} x 10^{-5} eV^2. The global value of Phi_8B is extracted to a precision of ^{+2.38}_{-2.95} %. In a three-flavor analysis the best fit value of sin^2\\theta_{13} is 2.00 ^{+2.09}_{-1.63} x 10^{-2}. Interpreting this as a limit implies an upper bound of sin^2\\theta_{13} < 0.057 (95% C. L.).

  12. MEASURING THE COOLING OF THE NEUTRON STAR IN CASSIOPEIA A WITH ALL CHANDRA X-RAY OBSERVATORY DETECTORS

    SciTech Connect (OSTI)

    Elshamouty, K. G.; Heinke, C. O.; Sivakoff, G. R. [Department of Physics, University of Alberta, CCIS 4-181, Edmonton AB T6G 2E1 (Canada); Ho, W. C. G. [School of Mathematics, University of Southampton, Southampton SO17 1BJ (United Kingdom); Shternin, P. S.; Yakovlev, D. G. [Ioffe Physical Technical Institute, Politekhnicheskaya 26, 194021 St Petersburg (Russian Federation); Patnaude, D. J.; David, L., E-mail: alshamou@ualberta.ca [Harvard-Smithsonian Centre for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States)

    2013-11-01

    The thermal evolution of young neutron stars (NSs) reflects the neutrino emission properties of their cores. Heinke and Ho measured a 3.6% ± 0.6% decay in the surface temperature of the Cassiopeia A (Cas A) NS between 2000 and 2009, using archival data from the Chandra X-ray Observatory ACIS-S detector in Graded mode. Page et al. and Shternin et al. attributed this decay to enhanced neutrino emission from a superfluid neutron transition in the core. Here we test this decline, combining analysis of the Cas A NS using all Chandra X-ray detectors and modes (HRC-S, HRC-I, ACIS-I, ACIS-S in Faint mode, and ACIS-S in Graded mode) and adding a 2012 May ACIS-S Graded mode observation, using the most current calibrations (CALDB 4.5.5.1). We measure the temperature changes from each detector separately and test for systematic effects due to the nearby filaments of the supernova remnant. We find a 0.92%-2.0% decay over 10 yr in the effective temperature, inferred from HRC-S data, depending on the choice of source and background extraction regions, with a best-fit decay of 1.0% ± 0.7%. In comparison, the ACIS-S Graded data indicate a temperature decay of 3.1%-5.0% over 10 yr, with a best-fit decay of 3.5% ± 0.4%. Shallower observations using the other detectors yield temperature decays of 2.6% ± 1.9% (ACIS-I), 2.1% ± 1.0% (HRC-I), and 2.1% ± 1.9% (ACIS-S Faint mode) over 10 yr. Our best estimate indicates a decline of 2.9% ± 0.5%{sub stat} ± 1.0{sub sys}% over 10 yr. The complexity of the bright and varying supernova remnant background makes a definitive interpretation of archival Cas A Chandra observations difficult. A temperature decline of 1%-3.5% over 10 yr would indicate extraordinarily fast cooling of the NS that can be regulated by superfluidity of nucleons in the stellar core.

  13. Jacobi fields, conjugate points and cut points on timelike geodesics in special spacetimes

    E-Print Network [OSTI]

    Leszek M. Soko?owski; Zdzis?aw A. Golda

    2015-07-09

    Several physical problems such as the `twin paradox' in curved spacetimes have purely geometrical nature and may be reduced to studying properties of bundles of timelike geodesics. The paper is a general introduction to systematic investigations of the geodesic structure of physically relevant spacetimes. The investigations are focussed on the search of locally and globally maximal timelike geodesics. The method of dealing with the local problem is in a sense algorithmic and is based on the geodesic deviation equation. Yet the search for globally maximal geodesics is non-algorithmic and cannot be treated analytically by solving a differential equation. Here one must apply a mixture of methods: spacetime symmetries (we have effectively employed the spherical symmetry), the use of the comoving coordinates adapted to the given congruence of timelike geodesics and the conjugate points on these geodesics. All these methods have been effectively applied in both the local and global problems in a number of simple and important spacetimes and their outcomes have already been published in three papers. Our approach shows that even in Schwarzschild spacetime (as well as in other static spherically symetric ones) one can find a new unexpected geometrical feature: instead of one there are three different infinite sets of conjugate points on each stable circular timelike geodesic curve. Due to problems with solving differential equations we are dealing solely with radial and circular geodesics.

  14. Lunar distances observed by Cook's expedition at Point Venus in ...

    E-Print Network [OSTI]

    In the modern navigator's language this is called GHA Aries (Greenwich hour angle of the point of the spring equinox). One of the two astronomers who made ...

  15. Electrochemical Surface Potential due to Classical Point Charge...

    Office of Scientific and Technical Information (OSTI)

    Potential due to Classical Point Charge Models Drives Anion Adsorption to the Air-Water Interface Citation Details In-Document Search Title: Electrochemical Surface Potential...

  16. Update Invalid Reservation Points for Transmission Service Requests...

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

    Teams Customer Training Interconnection Notices Rates Standards of Conduct Tariff TF Web Based Training Update: Invalid Reservation Points for Transmission Service Requests on...

  17. Topological phase diagram and saddle point singularity in a tunable...

    Office of Scientific and Technical Information (OSTI)

    Topological phase diagram and saddle point singularity in a tunable topological crystalline insulator Citation Details In-Document Search This content will become publicly...

  18. FIXED POINT INDICES AND MANIFOLDS WITH COLLARS Chen ...

    E-Print Network [OSTI]

    2005-05-05

    Brasiliero de Topologia 53 (1988), 59–67, Universidade de Sao Paulo, Sao Carlos S. P., Brasil. [8]. , A de Moivre like formula for fixed point theory, Proceedings ...

  19. ChargePoint is Helping Electrify America's Transportation | Department...

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

    of plug-in electric vehicles (PEVs), the Energy Department supported the ChargePoint America project in 2009 under the American Recovery and Reinvestment Act. At the...

  20. Generating and executing programs for a floating point single...

    Office of Scientific and Technical Information (OSTI)

    Generating and executing programs for a floating point single instruction multiple data instruction set architecture Citation Details In-Document Search Title: Generating and...

  1. New York Nuclear Profile - Nine Mile Point Nuclear Station

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

    Nine Mile Point Nuclear Station" "Unit","Summer capacity (mw)","Net generation (thousand mwh)","Summer capacity factor (percent)","Type","Commercial operation date","License...

  2. singularities, swallowtails and dirac points. an analysis for families

    E-Print Network [OSTI]

    2012-07-05

    Jul 5, 2012 ... in graphene). Of particular interest are Dirac points in triply periodic materials, such as the Gyroid network: they can be viewed as mag-.

  3. Energy Department Authorizes Dominion's Proposed Cove Point Facility...

    Office of Environmental Management (EM)

    Department announced today that it has conditionally authorized Dominion Cove Point LNG, LP to export domestically produced liquefied natural gas (LNG) to countries that do...

  4. Point-Wise Quantification of Craniofacial Stephanie Lanche

    E-Print Network [OSTI]

    -splines) transformations. Qualitative and quantitative validations of the presented methods were carried out This thesis presents a methodology of point-wise quantification of craniofacial asymmetry. The asymmetry

  5. CenterPoint Energy A/C Distributor Program

    Broader source: Energy.gov [DOE]

    Note:  This incentive is only available to customers within CenterPoint Energy’s electric service territory (greater Houston area, Texas)

  6. Optimizing minimum free-energy crossing points in solution: Linear...

    Office of Scientific and Technical Information (OSTI)

    Optimizing minimum free-energy crossing points in solution: Linear-response free energyspin-flip density functional theory approach Citation Details In-Document Search Title:...

  7. HYDRATE RESEARCH ACTIVITIES THAT BOTH SUPPORT AND DERIVE FROM THE MONITORING STATION/SEA-FLOOR OBSERVATORY, MISSISSIPPI CANYON 118, NORTHERN GULF OF MEXICO

    SciTech Connect (OSTI)

    Lutken, Carol

    2013-07-31

    A permanent observatory has been installed on the seafloor at Federal Lease Block, Mississippi Canyon 118 (MC118), northern Gulf of Mexico. Researched and designed by the Gulf of Mexico Hydrates Research Consortium (GOM-HRC) with the geological, geophysical, geochemical and biological characterization of in situ gas hydrates systems as the research goal, the site has been designated by the Bureau of Ocean Energy Management as a permanent Research Reserve where studies of hydrates and related ocean systems may take place continuously and cooperatively into the foreseeable future. The predominant seafloor feature at MC118 is a carbonate-hydrate complex, officially named Woolsey Mound for the founder of both the GOM-HRC and the concept of the permanent seafloor hydrates research facility, the late James Robert “Bob” Woolsey. As primary investigator of the overall project until his death in mid-2008, Woolsey provided key scientific input and served as chief administrator for the Monitoring Station/ Seafloor Observatory (MS-SFO). This final technical report presents highlights of research and accomplishments to date. Although not all projects reached the status originally envisioned, they are all either complete or positioned for completion at the earliest opportunity. All Department of Energy funds have been exhausted in this effort but, in addition, leveraged to great advantage with additional federal input to the project and matched efforts and resources. This report contains final reports on all subcontracts issued by the University of Mississippi, Administrators of the project, Hydrate research activities that both support and derive from the monitoring station/sea-floor Observatory, Mississippi Canyon 118, northern Gulf of Mexico, as well as status reports on the major components of the project. All subcontractors have fulfilled their primary obligations. Without continued funds designated for further project development, the Monitoring Station/Seafloor Observatory is in danger of lapsing into disuse. However, for the present, interest in the site on the continental slope is healthy and The Center for Marine Resources and Environmental Technology continues to coordinate all activity at the MS/SFO as arranged through the BOEM in 2005. Field and laboratory research projects and findings are reviewed, new technologies and tests described. Many new sensors, systems and two custom ROVs have been developed specifically for this project. Characteristics of marine gas hydrates are dramatically more refined than when the project was initiated and include appear in sections entitled Accomplishments, Products and Publications.

  8. Simultaneous Observation of Solar Neutrons from the ISS and High Mountain Observatories in association with a flare on July 8, 2014

    E-Print Network [OSTI]

    Muraki, Y; Koga, K; Kakimoto, F; Goka, T; Gonzalez, L X; Masuda, S; Matsubara, Y; Matsumoto, H; Miranda, P; Okudaira, O; Obara, T; Salinas, J; Sako, T; Shibata, S; Ticona, R; Tsunesada, Y; Valdes-Galicia, J F; Watanabe, K; Yamamoto, T

    2015-01-01

    An M6.5-class flare was observed at N12E56 of the solar surface at 16:06 UT on July 8, 2014. In association with this flare, solar neutron detectors located on two high mountains, Mt. Sierra Negra and Chacaltaya and at the space station observed enhancements in the neutral channel. The authors analysed these data and a possible scenario of enhancements produced by high-energy protons and neutrons is proposed, using the data from continuous observation of a solar surface by the ultraviolet telescope onboard the Solar Dynamical Observatory (SDO).

  9. NASH-STAMPACCHIA EQUILIBRIUM POINTS ON MANIFOLDS ALEXANDRU KRISTALY

    E-Print Network [OSTI]

    NASH-STAMPACCHIA EQUILIBRIUM POINTS ON MANIFOLDS ALEXANDRU KRIST´ALY Abstract. Motivated by Nash equilibrium problems on 'curved' strategy sets, the concept of Nash-Stampacchia equilibrium points Riemannian manifolds. Characterization, existence, and stability of Nash- Stampacchia equilibria are studied

  10. Tetrahedral Mesh Generation with Good Dihedral Angles Using Point Lattices

    E-Print Network [OSTI]

    O'Brien, James F.

    be of good quality; in partic- ular there should be no plane or dihedral angle close to 0 or 180 degreesTetrahedral Mesh Generation with Good Dihedral Angles Using Point Lattices by Franc¸ois Labelle B Tetrahedral Mesh Generation with Good Dihedral Angles Using Point Lattices by Franc¸ois Labelle Doctor

  11. An Empirical Comparison of "Wiimote" Gun Attachments for Pointing Tasks

    E-Print Network [OSTI]

    MacKenzie, Scott

    An Empirical Comparison of "Wiimote" Gun Attachments for Pointing Tasks Victoria McArthur, Steven J, a plastic gun-shaped shell designed for shooter games, the Wii Wheel, designed for driving games is to investigate whether gun- shaped peripherals help or hinder pointing performance with the Wiimote

  12. (sketches 102) Interactive Ray Tracing of Point-based Models

    E-Print Network [OSTI]

    Wald, Ingo

    " head, each point represented by a disc. b) The splats blendet to an implicit function and intersected(x) are the weighted averages of the positions resp. normals of all points (pi,ni,ri) overlapping x. Part II: Choosing optimal "Splat" Radii. Instead of having the user decide on the "optimal" splat radius, we used the method

  13. Evaluating Energy Efficiency of Floating Point Matrix Multiplication on FPGAs

    E-Print Network [OSTI]

    Prasanna, Viktor K.

    Evaluating Energy Efficiency of Floating Point Matrix Multiplication on FPGAs Kiran Kumar Matam, prasanna}@usc.edu Abstract--Energy efficiency has emerged as one of the key performance metrics in scientific computing. In this work, we evaluate the energy efficiency of floating point matrix multipli

  14. PAYLOAD POINTING AND ACTIVE VIBRATION ISOLATION USING HEXAPOD PLATFORMS

    E-Print Network [OSTI]

    PAYLOAD POINTING AND ACTIVE VIBRATION ISOLATION USING HEXAPOD PLATFORMS Hong-Jen Chen* , Ronald M isolation techniques on hexapods at the Spacecraft Research and Design Center (SRDC) of Naval Postgraduate School (NPS). The center has two hexapod platforms: Ultra Quiet Platform (UQP) and Precision Pointing

  15. Jet schemes of rational double point singularities Hussein Mourtada

    E-Print Network [OSTI]

    Bodin, Arnaud

    Jet schemes of rational double point singularities Hussein Mourtada Abstract. We prove that for m N, m big enough, the number of irreducible compo- nents of the schemes of m-jets centered at a point on the minimal reso- lution of the singularity. We also relate some irreducible components of the jet schemes

  16. MATRIX RATIONAL INTERPOLATION WITH POLES AS INTERPOLATION POINTS

    E-Print Network [OSTI]

    Labahn, George

    MATRIX RATIONAL INTERPOLATION WITH POLES AS INTERPOLATION POINTS M. VAN BAREL Department, we show the equivalence between matrix rational interpolation problems with poles as interpolation points and no-pole problems. This equivalence provides an effective method for computing matrix rational

  17. Mathematical features of Whitehead's point-free geometry

    E-Print Network [OSTI]

    Gerla, Giangiacomo

    1 Mathematical features of Whitehead's point- free geometry In HANDBOOK OF WHITEHEADIAN PROCESS quote computability theory, lat- tice theory, computer science. Now, the basic ideas of point over' and is the symbol for the fundamental relation of extension." Moreover, Whitehead in PNK lists

  18. Spawning rings of exceptional points out of Dirac cones

    E-Print Network [OSTI]

    Zhen, Bo; Igarashi, Yuichi; Lu, Ling; Kaminer, Ido; Pick, Adi; Chua, Song-Liang; Joannopoulos, John D; Solja?i?, Marin

    2015-01-01

    The Dirac cone underlies many unique electronic properties of graphene and topological insulators, and its band structure--two conical bands touching at a single point--has also been realized for photons in waveguide arrays, atoms in optical lattices, and through accidental degeneracy. Deformations of the Dirac cone often reveal intriguing properties; an example is the quantum Hall effect, where a constant magnetic field breaks the Dirac cone into isolated Landau levels. A seemingly unrelated phenomenon is the exceptional point, also known as the parity-time symmetry breaking point, where two resonances coincide in both their positions and widths. Exceptional points lead to counter-intuitive phenomena such as loss-induced transparency, unidirectional transmission or reflection, and lasers with reversed pump dependence or single-mode operation. These two fields of research are in fact connected: here we discover the ability of a Dirac cone to evolve into a ring of exceptional points, which we call an "exceptio...

  19. Distributing many points on spheres: minimal energy and designs

    E-Print Network [OSTI]

    Johann S. Brauchart; Peter J. Grabner

    2014-11-07

    This survey discusses recent developments in the context of spherical designs and minimal energy point configurations on spheres. The recent solution of the long standing problem of the existence of spherical $t$-designs on $\\mathbb{S}^d$ with $\\mathcal{O}(t^d)$ number of points by A. Bondarenko, D. Radchenko, and M. Viazovska attracted new interest to this subject. Secondly, D. P. Hardin and E. B. Saff proved that point sets minimising the discrete Riesz energy on $\\mathbb{S}^d$ in the hypersingular case are asymptotically uniformly distributed. Both results are of great relevance to the problem of describing the quality of point distributions on $\\mathbb{S}^d$, as well as finding point sets, which exhibit good distribution behaviour with respect to various quality measures.

  20. NELIOTA: ESA's new NEO lunar impact monitoring project with the 1.2m telescope at the National Observatory of Athens

    E-Print Network [OSTI]

    Bonanos, A Z; Boumis, P; Bellas-Velidis, I; Maroussis, A; Dapergolas, A; Fytsilis, A; Charmandaris, V; Tsiganis, K; Tsinganos, K

    2015-01-01

    NELIOTA is a new ESA activity launched at the National Observatory of Athens in February 2015 aiming to determine the distribution and frequency of small near-earth objects (NEOs) via lunar monitoring. The project involves upgrading the 1.2m Kryoneri telescope at the National Observatory of Athens, procuring two fast-frame cameras, and developing a software system, which will control the telescope and the cameras, process the images and automatically detect NEO impacts. NELIOTA will provide a web-based user interface, where the impact events will be reported and made available to the scientific community and the general public. The objective of this 3.5 year activity is to design, develop and implement a highly automated lunar monitoring system, which will conduct an observing campaign for 2 years in search of NEO impact flashes on the Moon. The impact events will be verified, characterised and reported. The 1.2m telescope will be capable of detecting flashes much fainter than current, small-aperture, lunar m...

  1. LARGE-SCALE CORONAL PROPAGATING FRONTS IN SOLAR ERUPTIONS AS OBSERVED BY THE ATMOSPHERIC IMAGING ASSEMBLY ON BOARD THE SOLAR DYNAMICS OBSERVATORY—AN ENSEMBLE STUDY

    SciTech Connect (OSTI)

    Nitta, Nariaki V.; Schrijver, Carolus J.; Title, Alan M.; Liu, Wei

    2013-10-10

    This paper presents a study of a large sample of global disturbances in the solar corona with characteristic propagating fronts as intensity enhancement, similar to the phenomena that have often been referred to as Extreme Ultraviolet Imaging Telescope (EIT) waves or extreme-ultraviolet (EUV) waves. Now EUV images obtained by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory provide a significantly improved view of these large-scale coronal propagating fronts (LCPFs). Between 2010 April and 2013 January, a total of 171 LCPFs have been identified through visual inspection of AIA images in the 193 Å channel. Here we focus on the 138 LCPFs that are seen to propagate across the solar disk, first studying how they are associated with flares, coronal mass ejections (CMEs), and type II radio bursts. We measure the speed of the LCPF in various directions until it is clearly altered by active regions or coronal holes. The highest speed is extracted for each LCPF. It is often considerably higher than EIT waves. We do not find a pattern where faster LCPFs decelerate and slow LCPFs accelerate. Furthermore, the speeds are not strongly correlated with the flare intensity or CME magnitude, nor do they show an association with type II bursts. We do not find a good correlation either between the speeds of LCPFs and CMEs in a subset of 86 LCPFs observed by one or both of the Solar and Terrestrial Relations Observatory spacecraft as limb events.

  2. Non-rigid point set registration: Coherent Point Drift Andriy Myronenko Xubo Song Miguel A. Carreira-Perpi~nan

    E-Print Network [OSTI]

    Carreira-Perpiñán, Miguel Á.

    for many computer vision applications such as ro- bot navigation, image guided surgery, motion tracking, point set correspondence, image segmentation and shape/pattern matching. The registration problem, the point locations is the most general of all features. Registration techniques can be rigid or non

  3. Unifying Bit-width Optimisation for Fixed-point and Floating-point Designs Altaf Abdul Gaffar1

    E-Print Network [OSTI]

    Mencer, Oskar

    Unifying Bit-width Optimisation for Fixed-point and Floating-point Designs Altaf Abdul Gaffar1 , Oskar Mencer1 , Wayne Luk1 and Peter Y.K. Cheung2 1 Department of Computing, Imperial College, London SW7 2BZ, UK. 2 Department of EEE, Imperial College, London SW7 2BT, UK. Abstract This paper presents

  4. On the nature of unstable equilibrium points in power systems

    SciTech Connect (OSTI)

    Berggren, B.; Andersson, G. . Dept. of Electric Power Systems)

    1993-05-01

    This paper concerns the application of direct methods for transient stability analysis of stressed power systems. One of the most important issues in this area is to find the controlling unstable equilibrium point for the disturbance under consideration. This paper provides a conceptual framework for discussing stable and unstable equilibrium points in power systems based on simple topological arguments. It is for instance shown that every conceivable case of system separation can be related to a specific unstable equilibrium point (u.e.p) in an unloaded system. This result can be seen as a verification of the soundness of the often used corrected corner point approximation and ray point approximation, since these two approximations would give the same unstable equilibrium points in an unloaded system. Moreover, it is shown, by an example, that some of these unstable equilibrium points can disappear when the loading of the system increases. The implications of the findings of this paper are discussed for the so-called MOD method of finding the controlling u.e.p., which is used in some software packages. Finally, a method based on a combination of MOD method and the BCU method is outlined and proposed as the subject of future investigation.

  5. The slopes determined by n points in the plane

    E-Print Network [OSTI]

    Martin, Jeremy L.

    2006-01-01

    field k,andletG be a graph with vertices V and edges E.Apicture P of G consists of a point P(v)for each vertex and a line P(e) for each edge, subject to the condition that P(v) ? P(e) whenever v is an endpoint of e.Thusthedataofn points and parenleftbig... n 2 parenrightbig lines described earlier is a picture of the complete graph K n on n vertices. The set of all pictures of G is called the picture space X(G). A picture is generic if the points P(v) are all different; the closure of the locus...

  6. Unsteady Reversed Stagnation-Point Flow over a Flat Plate

    E-Print Network [OSTI]

    Sin, Vai Kuong

    2013-01-01

    This paper investigates the nature of the development of two-dimensional laminar flow of an incompressible fluid at the reversed stagnation-point. ". In this study, we revisit the problem of reversed stagnation-point flow over a flat plate. Proudman and Johnson (1962) first studied the flow and obtained an asymptotic solution by neglecting the viscous terms. This is no true in neglecting the viscous terms within the total flow field. In particular it is pointed out that for a plate impulsively accelerated from rest to a constant velocity V0 that a similarity solution to the self-similar ODE is obtained which is noteworthy completely analytical.

  7. X(5) Critical-Point Structure in a Finite System

    E-Print Network [OSTI]

    A. Leviatan

    2005-09-01

    X(5) is a paradigm for the structure at the critical point of a particular first-order phase transition for which the intrinsic energy surface has two degenerate minima separated by a low barrier. For a finite system, we show that the dynamics at such a critical point can be described by an effective deformation determined by minimizing the energy surface after projection onto angular momentum zero, and combined with two-level mixing. Wave functions of a particular analytic form are used to derive estimates for energies and quadrupole rates at the critical point.

  8. Advances in Plasmonic Technologies for Point of Care Applications

    E-Print Network [OSTI]

    Tokel, Onur

    Demand for accessible and affordable healthcare for infectious and chronic diseases present significant challenges for providing high-value and effective healthcare. Traditional approaches are expanding to include point-of-care ...

  9. Shot noise in systems with semi-Dirac points

    SciTech Connect (OSTI)

    Zhai, Feng; Wang, Juan

    2014-08-14

    We calculate the ballistic conductance and shot noise of electrons through a two-dimensional stripe system (width W ? length L) with semi-Dirac band-touching points. We find that the ratio between zero-temperature noise power and mean current (the Fano factor) is highly anisotropic. When the transport is along the linear-dispersion direction and the Fermi energy is fixed at the semi-Dirac point, the Fano factor has a universal value F?=?0.179 while a minimum conductivity exists and scales with L{sup 1?2}. Along the parabolic dispersion direction, the Fano factor at the semi-Dirac point has a contact-independent limit exceeding 0.9, which varies weakly with L due to the common-path interference of evanescent waves. Our findings suggest a way to discern the type of band-touching points.

  10. TIPPING POINT (Synopsis) (Roy Thompson, Open Studies Summer Course, 2010)

    E-Print Network [OSTI]

    stations; followed by factory chimneys; yellow blotches on her brilliantly white skin; coal-burning; her tipping point from which recovery will be impossible. A worried look crosses Tabbris' face. Act III

  11. Quantifying the Impact of Single Bit Flips on Floating Point...

    Office of Scientific and Technical Information (OSTI)

    specific bits in the most widely used IEEE floating-point representation in an architecture-agnostic manner, i.e., without requiring proprietary information such as bit flip...

  12. A Naturally Arising Self-Correcting Point Process

    E-Print Network [OSTI]

    Frederic Schoenberg

    2011-01-01

    stationary Poisson and renewal models (Johnson and Gutsell,f (t) = 0 for t Renewal models embody the notion thatDespite the popularity of renewal models for temporal point

  13. Point Cloud Context Analysis for Rehabilitation Grasping Assistance

    E-Print Network [OSTI]

    point clouds. This paper presents a low-cost, real- time system for semantic image labeling of household, and structuring movements in task-specific ways, such as passive assistance by relieving the weight of the arm

  14. Polynomial partitioning on varieties of codimension two and point ...

    E-Print Network [OSTI]

    2014-09-03

    Sep 3, 2014 ... [ES11], they made a breakthrough in a long-standing problem of Erd?os on the number of distinct distances between points in the plane, ...

  15. SeptemberOctober 2008 | PCI Journal54 Editor's quick points

    E-Print Network [OSTI]

    September­October 2008 | PCI Journal54 Editor's quick points n This paper proposes provisions, NCHRP project 12-64, was to expand the use of the AASHTO LRFD specifications to reinforced 54 #12;55PCI

  16. Characterization of a Dipole Flow System Using Point Velocity Probes

    E-Print Network [OSTI]

    Bowen, Ian Reed

    2010-11-23

    A direct groundwater velocity measurement tool, the Point Velocity Probe, was developed to measure velocities in the vertical and horizontal directions. The tool was designed and tested in a low-cost laboratory flow-through tank. Following testing...

  17. EIS-0349: Cherry Point Co-generation Project

    Broader source: Energy.gov [DOE]

    This EIS analyzes DOE's decision to support BP West Coast Products, LLC proposal to construct and operate a 720-megawatt, natural-gas-fired, combined-cycle cogeneration facility on land adjacent to its BP Cherry Point Refinery.

  18. Energy Department Authorizes Dominion Cove Point LNG to Export...

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

    Dominion Cove Point LNG, LP to export domestically produced liquefied natural gas (LNG) to countries that do not have a Free Trade Agreement (FTA) with the United States. The Cove...

  19. Mixed Abstractions for Floating-Point Arithmetic Angelo Brillout

    E-Print Network [OSTI]

    Kröning, Daniel

    --Floating-point arithmetic is essential for many em- bedded and safety-critical systems, such as in the avionics industry by the the Toyota Motor Corporation, by the Semiconductor Research Corporation (SRC) under contract no. 2006-TJ-1539

  20. 2011 Radioactive Materials Usage Survey for Unmonitored Point Sources

    SciTech Connect (OSTI)

    Sturgeon, Richard W.

    2012-06-27

    This report provides the results of the 2011 Radioactive Materials Usage Survey for Unmonitored Point Sources (RMUS), which was updated by the Environmental Protection (ENV) Division's Environmental Stewardship (ES) at Los Alamos National Laboratory (LANL). ES classifies LANL emission sources into one of four Tiers, based on the potential effective dose equivalent (PEDE) calculated for each point source. Detailed descriptions of these tiers are provided in Section 3. The usage survey is conducted annually; in odd-numbered years the survey addresses all monitored and unmonitored point sources and in even-numbered years it addresses all Tier III and various selected other sources. This graded approach was designed to ensure that the appropriate emphasis is placed on point sources that have higher potential emissions to the environment. For calendar year (CY) 2011, ES has divided the usage survey into two distinct reports, one covering the monitored point sources (to be completed later this year) and this report covering all unmonitored point sources. This usage survey includes the following release points: (1) all unmonitored sources identified in the 2010 usage survey, (2) any new release points identified through the new project review (NPR) process, and (3) other release points as designated by the Rad-NESHAP Team Leader. Data for all unmonitored point sources at LANL is stored in the survey files at ES. LANL uses this survey data to help demonstrate compliance with Clean Air Act radioactive air emissions regulations (40 CFR 61, Subpart H). The remainder of this introduction provides a brief description of the information contained in each section. Section 2 of this report describes the methods that were employed for gathering usage survey data and for calculating usage, emissions, and dose for these point sources. It also references the appropriate ES procedures for further information. Section 3 describes the RMUS and explains how the survey results are organized. The RMUS Interview Form with the attached RMUS Process Form(s) provides the radioactive materials survey data by technical area (TA) and building number. The survey data for each release point includes information such as: exhaust stack identification number, room number, radioactive material source type (i.e., potential source or future potential source of air emissions), radionuclide, usage (in curies) and usage basis, physical state (gas, liquid, particulate, solid, or custom), release fraction (from Appendix D to 40 CFR 61, Subpart H), and process descriptions. In addition, the interview form also calculates emissions (in curies), lists mrem/Ci factors, calculates PEDEs, and states the location of the critical receptor for that release point. [The critical receptor is the maximum exposed off-site member of the public, specific to each individual facility.] Each of these data fields is described in this section. The Tier classification of release points, which was first introduced with the 1999 usage survey, is also described in detail in this section. Section 4 includes a brief discussion of the dose estimate methodology, and includes a discussion of several release points of particular interest in the CY 2011 usage survey report. It also includes a table of the calculated PEDEs for each release point at its critical receptor. Section 5 describes ES's approach to Quality Assurance (QA) for the usage survey. Satisfactory completion of the survey requires that team members responsible for Rad-NESHAP (National Emissions Standard for Hazardous Air Pollutants) compliance accurately collect and process several types of information, including radioactive materials usage data, process information, and supporting information. They must also perform and document the QA reviews outlined in Section 5.2.6 (Process Verification and Peer Review) of ES-RN, 'Quality Assurance Project Plan for the Rad-NESHAP Compliance Project' to verify that all information is complete and correct.

  1. Fast Change Point Detection for Electricity Market Analysis

    SciTech Connect (OSTI)

    UC Berkeley; Gu, William; Choi, Jaesik; Gu, Ming; Simon, Horst; Wu, Kesheng

    2013-08-25

    Electricity is a vital part of our daily life; therefore it is important to avoid irregularities such as the California Electricity Crisis of 2000 and 2001. In this work, we seek to predict anomalies using advanced machine learning algorithms. These algorithms are effective, but computationally expensive, especially if we plan to apply them on hourly electricity market data covering a number of years. To address this challenge, we significantly accelerate the computation of the Gaussian Process (GP) for time series data. In the context of a Change Point Detection (CPD) algorithm, we reduce its computational complexity from O($n^{5}$) to O($n^{2}$). Our efficient algorithm makes it possible to compute the Change Points using the hourly price data from the California Electricity Crisis. By comparing the detected Change Points with known events, we show that the Change Point Detection algorithm is indeed effective in detecting signals preceding major events.

  2. City of High Point Electric- Residential Energy Efficiency Rebate Program

    Broader source: Energy.gov [DOE]

    The City of High Point offers the Hometown Green Program to help customers reduce energy use. Under this program, rebates are available for newly constructed energy efficient homes, heat pumps, and...

  3. Change-Point Detection for High-Dimensional Data

    E-Print Network [OSTI]

    Xie, Yao

    November 5, 2013 #12;Power network monitoring a change-point Northeast blackout, 2003 Northeast blackout-time might prevent large-scale blackout 2 / 29 #12;Solar flare detection June, 2012. solar storm: a large

  4. A Behavioral Analysis of Clovis Point Morphology Using Geometric Morphometrics 

    E-Print Network [OSTI]

    Smith, Heather Lynn

    2012-02-14

    then be used to address research questions concerning Clovis point variability, and ultimately, the spread of this tool-form across North America. This paper addresses obstacles to behavioral investigations of stone tool morphology such as the effects...

  5. Laser Radar Point-Target Localization at High Photon Efficiency

    E-Print Network [OSTI]

    Shapiro, Jeffrey H.

    2013-01-01

    Minimum error-probability laser radar point-target localization is analyzed, including the effects of dark counts, background counts, and target speckle. Results from preliminary table-top experiments are reported.

  6. Advances in interior point methods and column generation 

    E-Print Network [OSTI]

    González Brevis, Pablo; Brevis, Pablo

    2013-11-28

    In this thesis we study how to efficiently combine the column generation technique (CG) and interior point methods (IPMs) for solving the relaxation of a selection of integer programming problems. In order to obtain an ...

  7. Method of making a non-lead hollow point bullet

    DOE Patents [OSTI]

    Vaughn, Norman L.; Lowden, Richard A.

    2003-10-07

    The method of making a non-lead hollow point bullet has the steps of a) compressing an unsintered powdered metal composite core into a jacket, b) punching a hollow cavity tip portion into the core, c) seating an insert, the insert having a hollow point tip and a tail protrusion, on top of the core such that the tail protrusion couples with the hollow cavity tip portion, and d) swaging the open tip of the jacket.

  8. Radar antenna pointing for optimized signal to noise ratio.

    SciTech Connect (OSTI)

    Doerry, Armin Walter; Marquette, Brandeis

    2013-01-01

    The Signal-to-Noise Ratio (SNR) of a radar echo signal will vary across a range swath, due to spherical wavefront spreading, atmospheric attenuation, and antenna beam illumination. The antenna beam illumination will depend on antenna pointing. Calculations of geometry are complicated by the curved earth, and atmospheric refraction. This report investigates optimizing antenna pointing to maximize the minimum SNR across the range swath.

  9. Tone and point of view in Thackeray's Henry Esmond 

    E-Print Network [OSTI]

    Ellison, Gerald Vance

    1966-01-01

    attitudes with those of Henry Esmond can be made. Second, ~Henr Esmond, like many of Thackeray's other works, contains some autobiographical material. Ray points out that Esmond is the most melancholy of Thackeray's novels, a point of which he was quite... aware while he wrote his book and which filled him with the gloomiest forebodings con- cerning its chances of popular success. The atmosphere of melancholy that pervades Esmond is explained if we examine its "secret history, " if we note down...

  10. 3 Linear Point Distribution Models 3.1 Introduction

    E-Print Network [OSTI]

    Bowden, Richard

    . Figure 3.2.2 - Hyper-elipsoid in n Dimensional Space x v1 v3 v2 z y v = eigenvectors Hyper a point in a 2n dimensional space (xi n2 ) and each vector is similar in shape, each example will produce a similar point in this 2n dimensional shape space. In fact, it would be expected that the training set

  11. On simple modules for certain pointed Hopf algebras 

    E-Print Network [OSTI]

    Pereira Lopez, Mariana

    2007-04-25

    -1 ON SIMPLE MODULES FOR CERTAIN POINTED HOPF ALGEBRAS A Dissertation by MARIANA PEREIRA LOPEZ Submitted to the Office of Graduate Studies of Texas A&M University in partial fulfifllment of the requirements for the degree of DOCTOR OF PHILOSOPHY December 2006... Major Subject: Mathematics ON SIMPLE MODULES FOR CERTAIN POINTED HOPF ALGEBRAS A Dissertation by MARIANA PEREIRA LOPEZ Submitted to the Office of Graduate Studies of Texas A&M University in partial fulfifllment of the requirements for the degree...

  12. Point kinetics calculations with fully coupled thermal fluids reactivity feedback

    SciTech Connect (OSTI)

    Zhang, H.; Zou, L.; Andrs, D.; Zhao, H.; Martineau, R.

    2013-07-01

    The point kinetics model has been widely used in the analysis of the transient behavior of a nuclear reactor. In the traditional nuclear reactor system safety analysis codes such as RELAP5, the reactivity feedback effects are calculated in a loosely coupled fashion through operator splitting approach. This paper discusses the point kinetics calculations with the fully coupled thermal fluids and fuel temperature feedback implemented into the RELAP-7 code currently being developed with the MOOSE framework. (authors)

  13. Cove Point: A step back into the LNG business

    SciTech Connect (OSTI)

    Katz, M.G.

    1995-12-31

    In 1978, ships began unloading LNG from Algeria at Cove Point`s berthing facilities 1.25 miles offshore. An underwater pipeline transported the LNG to land, where it was stored in the terminal`s four 140-foot-high cryogenic storage tanks. When the LNG was needed, the terminals 10 vaporizers converted it back to gas for send out via an 87-mile-long, 36-inch-diameter pipeline linking the terminal with interstate pipelines of CNG Transmission Corp. and Columbia Gas Transmission Corp. in Loudon County, Va. But Cove Point handled only about 80 shiploads of LNG before shutting down in December 1980, after a dispute about gas prices between US customers and Algeria. The plant sat dormant until the natural gas industry`s deregulation under Order 636. Deregulation resulted in major pipelines abandoning their sales service, and gas distributors and large customers found it was now their obligation to ensure that they had adequate gas supplies during winter peak-demand periods. Enter Cove Point`s peaking capabilities. They had to add the liquefaction unit and recommission other parts of the plant, but the timing was right. Cove Point`s new liquefaction unit is liquefying about 15 million cubic feet (MMcf) of LNG per day of domestic gas. It chills the gas to {minus}260 degrees Fahrenheit to turn it into a liquid for injection and storage in one of the facility`s double-walled insulated tanks. During its initial injection season, which ends Dec. 15, Cove Point is expected to produce enough LNG to almost fill one tank, which can store up to 1.25 billion cubic feet (Bcf). Were the gas not intended for peak-shaving purposes, it would be enough to supply 14,000 homes for a year. As it is, most of the gas will be returned as pipeline gas, during next January and February`s expected cold snaps, to the utilities and users who supplied it. Cove Point`s initial daily sendout capacity is about 400 MMcf.

  14. LARGE-SCALE DISTRIBUTION OF ARRIVAL DIRECTIONS OF COSMIC RAYS DETECTED ABOVE 10{sup 18} eV AT THE PIERRE AUGER OBSERVATORY

    SciTech Connect (OSTI)

    Abreu, P.; Andringa, S.; Aglietta, M.; Ahlers, M.; Ahn, E. J.; Albuquerque, I. F. M.; Allard, D.; Allekotte, I.; Allen, J.; Allison, P.; Almela, A.; Alvarez Castillo, J.; Alvarez-Muniz, J.; Alves Batista, R.; Ambrosio, M.; Aramo, C.; Aminaei, A.; Anchordoqui, L.; Antici'c, T.; Arganda, E.; Collaboration: Pierre Auger Collaboration; and others

    2012-12-15

    A thorough search for large-scale anisotropies in the distribution of arrival directions of cosmic rays detected above 10{sup 18} eV at the Pierre Auger Observatory is presented. This search is performed as a function of both declination and right ascension in several energy ranges above 10{sup 18} eV, and reported in terms of dipolar and quadrupolar coefficients. Within the systematic uncertainties, no significant deviation from isotropy is revealed. Assuming that any cosmic-ray anisotropy is dominated by dipole and quadrupole moments in this energy range, upper limits on their amplitudes are derived. These upper limits allow us to test the origin of cosmic rays above 10{sup 18} eV from stationary Galactic sources densely distributed in the Galactic disk and predominantly emitting light particles in all directions.

  15. CONSTRAINTS ON THE ORIGIN OF COSMIC RAYS ABOVE 10{sup 18} eV FROM LARGE-SCALE ANISOTROPY SEARCHES IN DATA OF THE PIERRE AUGER OBSERVATORY

    SciTech Connect (OSTI)

    Abreu, P.; Andringa, S.; Aglietta, M.; Ahlers, M.; Ahn, E. J.; Albuquerque, I. F. M.; Allard, D.; Allekotte, I.; Allen, J.; Allison, P.; Almela, A.; Castillo, J. Alvarez; Alvarez-Muniz, J.; Alves Batista, R.; Ambrosio, M.; Aramo, C.; Aminaei, A.; Anchordoqui, L.; Antici'c, T.; Arganda, E.; Collaboration: Pierre Auger Collaboration; and others

    2013-01-01

    A thorough search for large-scale anisotropies in the distribution of arrival directions of cosmic rays detected above 10{sup 18} eV at the Pierre Auger Observatory is reported. For the first time, these large-scale anisotropy searches are performed as a function of both the right ascension and the declination and expressed in terms of dipole and quadrupole moments. Within the systematic uncertainties, no significant deviation from isotropy is revealed. Upper limits on dipole and quadrupole amplitudes are derived under the hypothesis that any cosmic ray anisotropy is dominated by such moments in this energy range. These upper limits provide constraints on the production of cosmic rays above 10{sup 18} eV, since they allow us to challenge an origin from stationary galactic sources densely distributed in the galactic disk and emitting predominantly light particles in all directions.

  16. Reconstructing Past Solar Activity using Meridian Solar Observations: the Case of the Royal Observatory of the Spanish Navy (1833-1840)

    E-Print Network [OSTI]

    Vaquero, J M

    2014-01-01

    Solar meridian observations have been used to evaluate the solar activity of the past. Some important examples are the solar meridian observations made at the Basilica of San Petronio in Bologna by several astronomers and the observations made by Hevelius published in his book Machina Coelestis. However, we do not know whether these observations, which were not aimed to estimate the solar activity, are reliable for evaluating solar activity. In this paper, we present the marginal notes about sunspots that are included in the manuscripts of the meridian solar observations made at the Royal Observatory of the Spanish Navy during the period 1833-1840. We compare these observations with other solar activity indices such as sunspot area and number. Our conclusion is that solar meridian observations should be used with extreme caution to evaluate past solar activity.

  17. Estimation of low energy neutron flux ($E_n\\leq15$ MeV) in India-based Neutrino Observatory cavern using Monte Carlo techniques

    E-Print Network [OSTI]

    Dokania, N; Mathimalar, S; Garai, A; Nanal, V; Pillay, R G; Bhushan, K G

    2015-01-01

    The neutron flux at low energy ($E_n\\leq15$ MeV) resulting from the radioactivity of the rock in the underground cavern of the India-based Neutrino Observatory is estimated using Geant4-based Monte Carlo simulations. The neutron production rate due to the spontaneous fission of U, Th and ($\\alpha, n$) interactions in the rock is determined employing the actual rock composition. It has been demonstrated that the total flux is equivalent to a finite size cylindrical rock ($D=L=140$ cm) element. The energy integrated neutron flux thus obtained at the center of the underground tunnel is 2.76 (0.47) $\\times 10^{-6}\\rm~n ~cm^{-2}~s^{-1}$. The estimated neutron flux is of the same order ($\\sim10^{-6}\\rm~n ~cm^{-2}~s^{-1}$)~as measured in other underground laboratories.

  18. Estimation of low energy neutron flux ($E_n\\leq15$ MeV) in India-based Neutrino Observatory cavern using Monte Carlo techniques

    E-Print Network [OSTI]

    N. Dokania; V. Singh; S. Mathimalar; A. Garai; V. Nanal; R. G. Pillay; K. G. Bhushan

    2015-09-23

    The neutron flux at low energy ($E_n\\leq15$ MeV) resulting from the radioactivity of the rock in the underground cavern of the India-based Neutrino Observatory is estimated using Geant4-based Monte Carlo simulations. The neutron production rate due to the spontaneous fission of U, Th and ($\\alpha, n$) interactions in the rock is determined employing the actual rock composition. It has been demonstrated that the total flux is equivalent to a finite size cylindrical rock ($D=L=140$ cm) element. The energy integrated neutron flux thus obtained at the center of the underground tunnel is 2.76 (0.47) $\\times 10^{-6}\\rm~n ~cm^{-2}~s^{-1}$. The estimated neutron flux is of the same order ($\\sim10^{-6}\\rm~n ~cm^{-2}~s^{-1}$)~as measured in other underground laboratories.

  19. Simulations Study of Muon Response in the Peripheral Regions of the Iron Calorimeter Detector at the India-based Neutrino Observatory

    E-Print Network [OSTI]

    Kanishka, R; Bhatnagar, Vipin; Indumathi, D; Sinha, Nita

    2015-01-01

    The magnetized Iron CALorimeter detector (ICAL) which is proposed to be built in the India-based Neutrino Observatory (INO) laboratory, aims to study atmospheric neutrino oscillations primarily through charged current interactions of muon neutrinos and anti-neutrinos with the detector. The response of muons and charge identification efficiency, angle and energy resolution as a function of muon momentum and direction are studied from GEANT4-based simulations in the peripheral regions of the detector. This completes the characterisation of ICAL with respect to muons over the entire detector and has implications for the sensitivity of ICAL to the oscillation parameters and mass hierarchy compared to the studies where only the resolutions and efficiencies of the central region of ICAL were assumed for the entire detector. Selection criteria for track reconstruction in the peripheral region of the detector were determined from the detector response. On applying these, for the 1--20 GeV energy region of interest fo...

  20. The effect of the geomagnetic field on cosmic ray energy estimates and large scale anisotropy searches on data from the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Abreu, P.; Aglietta, M.; Ahn, E.J.; Albuquerque, I.F.M.; Allard, D.; Allekotte, I.; Allen, J.; Allison, P.; Alvarez Castillo, J.; Alvarez-Muniz, J.; Ambrosio, M.; ,

    2011-11-01

    We present a comprehensive study of the influence of the geomagnetic field on the energy estimation of extensive air showers with a zenith angle smaller than 60{sup o}, detected at the Pierre Auger Observatory. The geomagnetic field induces an azimuthal modulation of the estimated energy of cosmic rays up to the {approx} 2% level at large zenith angles. We present a method to account for this modulation of the reconstructed energy. We analyse the effect of the modulation on large scale anisotropy searches in the arrival direction distributions of cosmic rays. At a given energy, the geomagnetic effect is shown to induce a pseudo-dipolar pattern at the percent level in the declination distribution that needs to be accounted for. In this work, we have identified and quantified a systematic uncertainty affecting the energy determination of cosmic rays detected by the surface detector array of the Pierre Auger Observatory. This systematic uncertainty, induced by the influence of the geomagnetic field on the shower development, has a strength which depends on both the zenith and the azimuthal angles. Consequently, we have shown that it induces distortions of the estimated cosmic ray event rate at a given energy at the percent level in both the azimuthal and the declination distributions, the latter of which mimics an almost dipolar pattern. We have also shown that the induced distortions are already at the level of the statistical uncertainties for a number of events N {approx_equal} 32 000 (we note that the full Auger surface detector array collects about 6500 events per year with energies above 3 EeV). Accounting for these effects is thus essential with regard to the correct interpretation of large scale anisotropy measurements taking explicitly profit from the declination distribution.

  1. The motion of point particles in curved spacetime

    E-Print Network [OSTI]

    Eric Poisson; Adam Pound; Ian Vega

    2011-09-26

    This review is concerned with the motion of a point scalar charge, a point electric charge, and a point mass in a specified background spacetime. In each of the three cases the particle produces a field that behaves as outgoing radiation in the wave zone, and therefore removes energy from the particle. In the near zone the field acts on the particle and gives rise to a self-force that prevents the particle from moving on a geodesic of the background spacetime. The field's action on the particle is difficult to calculate because of its singular nature: the field diverges at the position of the particle. But it is possible to isolate the field's singular part and show that it exerts no force on the particle. What remains after subtraction is a smooth field that is fully responsible for the self-force. The mathematical tools required to derive the equations of motion of a point scalar charge, a point electric charge, and a point mass in a specified background spacetime are developed here from scratch. The review begins with a discussion of the basic theory of bitensors. It then applies the theory to the construction of convenient coordinate systems to chart a neighbourhood of the particle's word line. It continues with a thorough discussion of Green's functions in curved spacetime. The review presents a detailed derivation of each of the three equations of motion. Because the notion of a point mass is problematic in general relativity, the review concludes with an alternative derivation of the equations of motion that applies to a small body of arbitrary internal structure.

  2. MHD Wave Propagation in the Neighbourhood of Two Null Points

    E-Print Network [OSTI]

    J. A. McLaughlin; A. W. Hood

    2007-12-11

    The nature of fast magnetoacoustic and Alfv\\'en waves is investigated in a zero $\\beta$ plasma in the neighbourhood of a pair of two-dimensional null points. This gives an indication of wave propagation in the low $\\beta$ solar corona, for a more complicated magnetic configuration than that looked at by McLaughlin & Hood (2004). It is found that the fast wave is attracted to the null points and that the front of the wave slows down as it approaches the null point pair, with the wave splitting and part of the wave accumulating at one null and the rest at the other. Current density will then accumulate at these points and ohmic dissipation will then extract the energy in the wave at these points. This suggests locations where wave heating will occur in the corona. The Alfv\\'en wave behaves in a different manner in that the wave accumulates along the separatrices. Hence, the current density will accumulate at this part of the topology and this is where wave heating will occur. However, the phenomenon of wave accumulation at a specific place is a feature of both wave types, and illustrates the importance of studying the topology of the corona when considering MHD wave propagation.

  3. Energy dissipation in magnetic null points at kinetic scales

    E-Print Network [OSTI]

    Olshevsky, Vyacheslav; Eriksson, Elin; Markidis, Stefano; Lapenta, Giovanni

    2015-01-01

    We use kinetic particle-in-cell and magnetohydrodynamic simulations supported by an observational dataset to investigate magnetic reconnection in clusters of null points in space plasma. The magnetic configuration under investigation is driven by fast adiabatic flux rope compression that dissipates almost half of the initial magnetic field energy. In this phase powerful currents are excited producing secondary instabilities, and the system is brought into a state of `intermittent turbulence' within a few ion gyro-periods. Reconnection events are distributed all over the simulation domain and energy dissipation is rather volume-filling. Numerous spiral null points interconnected via their spines form null lines embedded into magnetic flux ropes; null point pairs demonstrate the signatures of torsional spine reconnection. However, energy dissipation mainly happens in the shear layers formed by adjacent flux ropes with oppositely directed currents. In these regions radial null pairs are spontaneously emerging an...

  4. Thermal conductivity at a disordered quantum critical point

    E-Print Network [OSTI]

    Hartnoll, Sean A; Santos, Jorge E

    2015-01-01

    Strongly disordered and strongly interacting quantum critical points are difficult to access with conventional field theoretic methods. They are, however, both experimentally important and theoretically interesting. In particular, they are expected to realize universal incoherent transport. Such disordered quantum critical theories have recently been constructed holographically by deforming a CFT by marginally relevant disorder. In this paper we find additional disordered fixed points via relevant disordered deformations of a holographic CFT. Using recently developed methods in holographic transport, we characterize the thermal conductivity in both sets of theories in 1+1 dimensions. The thermal conductivity is found to tend to a constant at low temperatures in one class of fixed points, and to scale as $T^{0.3}$ in the other. Furthermore, in all cases the thermal conductivity exhibits discrete scale invariance, with logarithmic in temperature oscillations superimposed on the low temperature scaling behavior....

  5. Remarks on a fixed point theorem of Caristi 

    E-Print Network [OSTI]

    Egle, David Lee

    1977-01-01

    ) = u and f(v) = v. Then, d(u, v) = d(f(u), f(v)) & o(d(u, f(u) + d(v, f(v))) = 0. 13 Thus, u = v and the fixed point is unique. The convergence of any sequence of i terates follows from the observation following Theorem 1. 3. & The concept of a... of the fixed point follows directly from the uniqueness of the fixed point for fn(u) Let x c X. Let s(x) = max (d(f (x), u) : j = 0, 1, . . . , (n(u)-l)). For m sufficiently large, write m = p n(u) + q, where 0 & q & n(u), p & 0. Then d(f (x, u) = d(f...

  6. Physical Point Simulation in 2+1 Flavor Lattice QCD

    E-Print Network [OSTI]

    PACS-CS Collaboration; :; S. Aoki; K. -I. Ishikawa; N. Ishizuka; T. Izubuchi; D. Kadoh; K. Kanaya; Y. Kuramashi; Y. Namekawa; M. Okawa; Y. Taniguchi; A. Ukawa; N. Ukita; T. Yamazaki; T. Yoshie

    2010-04-04

    We present the results of the physical point simulation in 2+1 flavor lattice QCD with the nonperturbatively $O(a)$-improved Wilson quark action and the Iwasaki gauge action at $\\beta=1.9$ on a $32^3 \\times 64$ lattice. The physical quark masses together with the lattice spacing is determined with $m_\\pi$, $m_K$ and $m_\\Omega$ as physical inputs. There are two key algorithmic ingredients to make possible the direct simulation at the physical point: One is the mass-preconditioned domain-decomposed HMC algorithm to reduce the computational cost. The other is the reweighting technique to adjust the hopping parameters exactly to the physical point. The physics results include the hadron spectrum, the quark masses and the pseudoscalar meson decay constants. The renormalization factors are nonperturbatively evaluated with the Schr{\\"o}dinger functional method. The results are compared with the previous ones obtained by the chiral extrapolation method.

  7. Engineering to Control Noise, Loading, and Optimal Operating Points

    SciTech Connect (OSTI)

    Mitchell R. Swartz

    2000-11-12

    Successful engineering of low-energy nuclear systems requires control of noise, loading, and optimum operating point (OOP) manifolds. The latter result from the biphasic system response of low-energy nuclear reaction (LENR)/cold fusion systems, and their ash production rate, to input electrical power. Knowledge of the optimal operating point manifold can improve the reproducibility and efficacy of these systems in several ways. Improved control of noise, loading, and peak production rates is available through the study, and use, of OOP manifolds. Engineering of systems toward the OOP-manifold drive-point peak may, with inclusion of geometric factors, permit more accurate uniform determinations of the calibrated activity of these materials/systems.

  8. Methods for point source analysis in high energy neutrino telescopes

    E-Print Network [OSTI]

    Jim Braun; Jon Dumm; Francesco De Palma; Chad Finley; Albrecht Karle; Teresa Montaruli

    2008-01-10

    Neutrino telescopes are moving steadily toward the goal of detecting astrophysical neutrinos from the most powerful galactic and extragalactic sources. Here we describe analysis methods to search for high energy point-like neutrino sources using detectors deep in the ice or sea. We simulate an ideal cubic kilometer detector based on real world performance of existing detectors such as AMANDA, IceCube, and ANTARES. An unbinned likelihood ratio method is applied, making use of the point spread function and energy distribution of simulated neutrino signal events to separate them from the background of atmospheric neutrinos produced by cosmic ray showers. The unbinned point source analyses are shown to perform better than binned searches and, depending on the source spectral index, the use of energy information is shown to improve discovery potential by almost a factor of two.

  9. The motion of point particles in curved spacetime

    E-Print Network [OSTI]

    Eric Poisson

    2004-04-01

    This review is concerned with the motion of a point scalar charge, a point electric charge, and a point mass in a specified background spacetime. In each of the three cases the particle produces a field that behaves as outgoing radiation in the wave zone, and therefore removes energy from the particle. In the near zone the field acts on the particle and gives rise to a self-force that prevents the particle from moving on a geodesic of the background spacetime. The field's action on the particle is difficult to calculate because of its singular nature: the field diverges at the position of the particle. But it is possible to isolate the field's singular part and show that it exerts no force on the particle -- its only effect is to contribute to the particle's inertia. What remains after subtraction is a smooth field that is fully responsible for the self-force. Because this field satisfies a homogeneous wave equation, it can be thought of as a free (radiative) field that interacts with the particle; it is this interaction that gives rise to the self-force. The mathematical tools required to derive the equations of motion of a point scalar charge, a point electric charge, and a point mass in a specified background spacetime are developed here from scratch. The review begins with a discussion of the basic theory of bitensors (part I). It then applies the theory to the construction of convenient coordinate systems to chart a neighbourhood of the particle's word line (part II). It continues with a thorough discussion of Green's functions in curved spacetime (part III). The review concludes with a detailed derivation of each of the three equations of motion (part IV).

  10. New algorithms for adaptive optics point-spread function reconstruction

    E-Print Network [OSTI]

    Eric Gendron; Yann Clénet; Thierry Fusco; Gérard Rousset

    2006-06-28

    Context. The knowledge of the point-spread function compensated by adaptive optics is of prime importance in several image restoration techniques such as deconvolution and astrometric/photometric algorithms. Wavefront-related data from the adaptive optics real-time computer can be used to accurately estimate the point-spread function in adaptive optics observations. The only point-spread function reconstruction algorithm implemented on astronomical adaptive optics system makes use of particular functions, named $U\\_{ij}$. These $U\\_{ij}$ functions are derived from the mirror modes, and their number is proportional to the square number of these mirror modes. Aims. We present here two new algorithms for point-spread function reconstruction that aim at suppressing the use of these $U\\_{ij}$ functions to avoid the storage of a large amount of data and to shorten the computation time of this PSF reconstruction. Methods. Both algorithms take advantage of the eigen decomposition of the residual parallel phase covariance matrix. In the first algorithm, the use of a basis in which the latter matrix is diagonal reduces the number of $U\\_{ij}$ functions to the number of mirror modes. In the second algorithm, this eigen decomposition is used to compute phase screens that follow the same statistics as the residual parallel phase covariance matrix, and thus suppress the need for these $U\\_{ij}$ functions. Results. Our algorithms dramatically reduce the number of $U\\_{ij}$ functions to be computed for the point-spread function reconstruction. Adaptive optics simulations show the good accuracy of both algorithms to reconstruct the point-spread function.

  11. Chiral-Scale Perturbation Theory About an Infrared Fixed Point

    E-Print Network [OSTI]

    R. J. Crewther; Lewis C. Tunstall

    2014-01-31

    We review the failure of lowest order chiral $SU(3)_L \\times SU(3)_R$ perturbation theory $\\chi$PT$_3$ to account for amplitudes involving the $f_0(500)$ resonance and $O(m_K)$ extrapolations in momenta. We summarize our proposal to replace $\\chi$PT$_3$ with a new effective theory $\\chi$PT$_\\sigma$ based on a low-energy expansion about an infrared fixed point in 3-flavour QCD. At the fixed point, the quark condensate $\\langle\\bar{q}q\\rangle_\\mathrm{vac}\

  12. An order theoretic approach in fixed point theory

    E-Print Network [OSTI]

    Yaé Ulrich Gaba

    2014-11-07

    In the present article, we show the existence of a coupled fixed point for an order preserving mapping in a preordered left K-complete quasi-pseudometric space using a preorder induced by an appropriate function. We also define the concept of left-weakly related mappings on a preordered space and discuss common coupled fixed points for two and three left-weakly related mappings in the same space. Similar results are given for right-weakly related mappings, the dual notion of left-weakly related mappings.

  13. Measurement of thermodynamic temperature of high temperature fixed points

    SciTech Connect (OSTI)

    Gavrilov, V. R.; Khlevnoy, B. B.; Otryaskin, D. A.; Grigorieva, I. A.; Samoylov, M. L.; Sapritsky, V. I.

    2013-09-11

    The paper is devoted to VNIIOFI's measurements of thermodynamic temperature of the high temperature fixed points Co-C, Pt-C and Re-C within the scope of the international project coordinated by the Consultative Committee for Thermometry working group 5 'Radiation Thermometry'. The melting temperatures of the fixed points were measured by a radiance mode radiation thermometer calibrated against a filter radiometer with known irradiance spectral responsivity via a high temperature black body. This paper describes the facility used for the measurements, the results and estimated uncertainties.

  14. Point X-ray sources in the SNR G 315.4-2.30 (MSH 14-63, RCW 86)

    E-Print Network [OSTI]

    V. V. Gvaramadze; A. A. Vikhlinin

    2002-12-25

    We report the results of a search for a point X-ray source (stellar remnant) in the southwest protrusion of the supernova remnant G 315.4-2.30 (MSH 14-63, RCW 86) using the archival data of the Chandra X-ray Observatory. The search was motivated by a hypothesis that G 315.4-2.30 is the result of an off-centered cavity supernova explosion of a moving massive star, which ended its evolution just near the edge of the main-sequence wind-driven bubble. This hypothesis implies that the southwest protrusion in G 315.4-2.30 is the remainder of a pre-existing bow shock-like structure created by the interaction of the supernova progenitor's wind with the interstellar medium and that the actual location of the supernova blast center is near the center of this hemispherical structure. We have discovered two point X-ray sources in the "proper" place. One of the sources has an optical counterpart with the photographic magnitude $13.38\\pm0.40$, while the spectrum of the source can be fitted with an optically thin plasma model. We interpret this source as a foreground active star of late spectral type. The second source has no optical counterpart to a limiting magnitude $\\sim 21$. The spectrum of this source can be fitted almost equally well with several simple models (power law: photon index $=1.87$; two-temperature blackbody: $kT_1 =0.11$ keV, $R_1 =2.34 $ km and $kT_2 =0.71$ keV, $R_2 =0.06$ km; blackbody plus power law: $kT =0.07$ keV, photon index $=2.3$). We interpret this source as a candidate stellar remnant (neutron star), while the photon index and non-thermal luminosity of the source (almost the same as those of the Vela pulsar and the recently discovered pulsar PSR J 0205+6449 in the supernova remnant 3C 58) suggest that it can be a young "ordinary" pulsar.

  15. Global Warming 20 Years Later: Tipping Points Near

    E-Print Network [OSTI]

    Hansen, James E.

    Global Warming 20 Years Later: Tipping Points Near Jim Hansen 23 June 2008 National Press Club, and House Select Committee on Energy Independence & Global Warming Washington, DC #12;1988 Testimony Has Big Effects Did Not Emphasize That Global Warming Enhances Both Extremes of Water Cycle - More

  16. Stochastic Analog Circuit Behavior Modeling by Point Estimation Method

    E-Print Network [OSTI]

    He, Lei

    -based method such as APEX with the similar accuracy. ACM Classification Keywords: B.7.2: - Integrated Circuits- Design Aids General Terms: Algorithms, Performance Authors Keywords: Behavior Modeling, Point Estima and man- Permission to make digital or hard copies of all or part of this work for personal or classroom

  17. Material for Point Design (final summary of DIME material)

    SciTech Connect (OSTI)

    Bradley, Paul A.

    2014-02-25

    These slides summarize the motivation of the Defect Induced Mix Experiment (DIME) project, the “point design” of the Polar Direct Drive (PDD) version of the NIF separated reactant capsule, the experimental requirements, technical achievements, and some useful backup material. These slides are intended to provide much basic material in one convenient location and will hopefully be of some use for subsequent experimental projects.

  18. Climate Tipping Points* The Threat to the Planet

    E-Print Network [OSTI]

    Hansen, James E.

    Climate Tipping Points* The Threat to the Planet Jim Hansen 19 February 2008 Illinois Wesleyan/policymakers) 2. A Planetary Emergency - Climate Inertia Pipeline Effect - Positive Feedbacks Predominate 3. Good. Great Inertia of Systems - Climate: >½ Warming Still `in Pipeline' - Energy Infrastructure: Decades

  19. Markov Properties for Point Processes on the Plane

    E-Print Network [OSTI]

    Nualart, David; Merzbach, Ely

    1990-02-02

    It is proved that for a wide class of point processes indexed by the positive quadrant of the plane, and for a class of compact sets in this quadrant, the germ ?-field is equal to the ?-field generated by the values of the process on the set...

  20. Quantum Chaos for point scatterers on flat tori

    E-Print Network [OSTI]

    Henrik Ueberschaer

    2013-04-23

    This survey article deals with a delta potential - also known as a point scatterer - on flat 2D and 3D tori. We introduce the main conjectures regarding the spectral and wave function statistics of this model in the so- called weak and strong coupling regimes. We report on recent progress as well as a number of open problems in this field.

  1. Fermi point in graphene as a monopole in momentum space

    E-Print Network [OSTI]

    M . A. Zubkov

    2011-12-15

    We consider the effective field theory of graphene monolayer with the Coulomb interaction between fermions taken into account. The gauge field in momentum space is introduced. The position of the Fermi point coincides with the position of the corresponding monopole. The procedure of extracting such monopoles during lattice simulations is suggested.

  2. Comparing Genomes with Duplications: A Computational Complexity Point of View

    E-Print Network [OSTI]

    Chauve, Cedric

    Comparing Genomes with Duplications: A Computational Complexity Point of View Guillaume Blin are interested in the computational complexity of computing (dis)similarity measures between two genomes when they contain duplicated genes or genomic markers, a problem that happens frequently when comparing whole

  3. Fast Quadrupling of a Point on Elliptic Curves Cryptography

    E-Print Network [OSTI]

    International Association for Cryptologic Research (IACR)

    Fast Quadrupling of a Point on Elliptic Curves Cryptography Duc-Phong Le Temasek Laboratories of Weierstrass form. In this paper we extend their method and present a fast algorithm for computing 4P with only algorithm gains better results. Keywords: Elliptic curve cryptography, fast arithmetic, affine co- ordinates

  4. Fast Multipole Representation of Diffusion Curves and Points Timothy Sun

    E-Print Network [OSTI]

    Columbia University

    Fast Multipole Representation of Diffusion Curves and Points Timothy Sun Papoj Thamjaroenporn performed on the fast multipole representation. Abstract We propose a new algorithm for random-access evaluation of diffu- sion curve images (DCIs) using the fast multipole method. Unlike all previous methods

  5. An Extreme Point Tabu Search Method for Data Mining

    E-Print Network [OSTI]

    Mitchell, John E.

    An Extreme Point Tabu Search Method for Data Mining Kristin P. Bennett \\Lambda Jennifer A. Blue error of all the decisions in the tree concurrently. Decision trees are ideal for data­mining because optimize existing decision trees. This capability can be used in data mining for avoiding overfitting

  6. TWIN BUILDING LATTICES DO NOT HAVE ASYMPTOTIC CUT-POINTS

    E-Print Network [OSTI]

    Caprace, Pierre-Emmanuel

    TWIN BUILDING LATTICES DO NOT HAVE ASYMPTOTIC CUT-POINTS PIERRE-EMMANUEL CAPRACE*, FRANÇOIS DAHMANI**, AND VINCENT GUIRARDEL** Abstract. We show that twin building lattices have linear divergence, which implies of asymptotic cones of twin building lattices. Theorem 1. The asymptotic cones of a twin building lattice do

  7. SIAM Conference on Gemetric Design, 2003 Point Cloud Denoising

    E-Print Network [OSTI]

    de Figueiredo, Luiz Henrique

    1 SIAM Conference on Gemetric Design, 2003 Point Cloud Denoising Luiz Velho Boris Mederos Madrazo Luiz Henrique de Figueiredo IMPA ­ Instituto de Matemática Pura e Aplicada Luiz Velho © SIAM Conference · Smoothing Operator rr ntrrQ +=)( })(|{ xxQx = )(' xQx r n t Luiz Velho © SIAM Conference on Gemetric Design

  8. Spring 2011 | PCI Journal88 Editor's quick points

    E-Print Network [OSTI]

    Spring 2011 | PCI Journal88 Editor's quick points n This article is the first part of a two to provide bearing for the deck sections, so the L-shaped slen- #12;89PCI Journal | Spring 2011 to maintain is outlined in the sixth edition of the PCI Design Handbook: Precast and Prestressed Concrete.7 The PCI Design

  9. Fall 2011 | PCI Journal106 Editor's quick points

    E-Print Network [OSTI]

    Fall 2011 | PCI Journal106 Editor's quick points This paper summarizes the results in the sixth edition of the PCI Design Handbook: Precast and Prestressed Con- crete6 often results in conservative, heavy reinforcement #12;107PCI Journal | Fall 2011 results1 to study the various parameters

  10. Outline Overview Design Principles Key Points Design Principles

    E-Print Network [OSTI]

    Almulhem, Ahmad

    Engineering Department, KFUPM Spring 2008 Ahmad Almulhem - Network Security Engineering - 2008 1 / 12 #12-Safe Defaults Economy of Mechanism Complete Mediation Open Design Separation of Privilege Least Common Mechanism Psychological Acceptability 3 Key Points Ahmad Almulhem - Network Security Engineering - 2008 2 / 12 #12;Outline

  11. Schur Complements on Hilbert Spaces and Saddle Point Systems

    E-Print Network [OSTI]

    Bacuta, Constantin

    constants. In the light of the new spectral results for the Schur complements, we review the classical, multilevel methods, adaptive methods 1 Introduction In the present literature, the abstract formulation to adaptive algorithms for solving saddle point systems, see [3,4,12]. The main advantage of the new

  12. Dependency Calculus Reasoning in a General Point Relation Algebra

    E-Print Network [OSTI]

    Nebel, Bernhard

    of flowing water, we can draw conclusions about pollution at other points (cf. Fig. 1). If pollution is found- pects and complexity results from one algebra to another. If we observe pollution in an ecosystem at D, F is polluted as well. It B C E D F A Figure 1: A pipe network. Flow occurs along the "pipes

  13. Type-Based Termination, Inflationary Fixed-Points, and

    E-Print Network [OSTI]

    Abel, Andreas

    Type-Based Termination, Inflationary Fixed-Points, and Mixed Inductive-Coinductive Types Andreas Science (FICS 2012) ETAPS 2012, Tallinn, Estonia 24 March 2012 Andreas Abel (LMU) Type-Based Termination AIM XV 1 / 1 #12;Introduction Aspects of Termination What the talk is about: foundational approach

  14. Monochromatic and random wave breaking at blocking points

    E-Print Network [OSTI]

    Kirby, James T.

    ; published 4 July 2002. [1] In this paper we study the energy dissipation due to current-limited waveMonochromatic and random wave breaking at blocking points Arun Chawla Center for Coastal and Land and Technology, Portland, Oregon, USA James T. Kirby Center for Applied Coastal Research, University of Delaware

  15. Jet schemes of rational double point singularities Hussein MOURTADA

    E-Print Network [OSTI]

    Jet schemes of rational double point singularities Hussein MOURTADA September 30, 2012 Abstract We prove that for m N, m big enough, the number of irreducble components of the schemes of m-jets centered of the jet schemes of an E6 singularity to its "minimal" embedded resolutions of singularities. 1

  16. Non-crossing Matchings of Points with Geometric Objects1

    E-Print Network [OSTI]

    Demaine, Erik

    ´e Libre de Bruxelles, CP212, Bld. du Triomphe, 1050 Brussels, Belgium. b MIT Computer Science the algorithmic problem of deter- mining whether a non-crossing matching exists between a given point-object pairPoSe: Fonds National de la Recherche Scientifique (F.R.S.-FNRS) - EUROGIGA NR 13604, for Belgium, and MICINN

  17. The Point in Polygon Problem for Arbitrary Polygons

    E-Print Network [OSTI]

    Hormann, Kai

    and the winding number, the former lead- ing to ray-crossing, the latter to angle summation algorithms. First we version of an algorithm for determining the winding number. Then we examine how to accelerate in literature and discuss the results. Keywords: polygons, point containment, winding number, integer algorithms

  18. Ubiquitous Computing at Point of Care in Hospitals

    E-Print Network [OSTI]

    Ubiquitous Computing at Point of Care in Hospitals: A User-Centered Approach Thesis for the degree, the dissemination of ubiquitous computing has been slow. Research on this type of technology has in many ways been, there is little design guidance that can help technology developers apply ubiquitous computing designs

  19. Towards the physical point hadronic vacuum polarisation from Moebius DWF

    E-Print Network [OSTI]

    Marinkovic, Marina; Del Debbio, Luigi; Juettner, Andreas; Maltman, Kim; Portelli, Antonin

    2015-01-01

    We present steps towards the computation of the leading-order hadronic contribution to the muon anomalous magnetic moment on RBC/UKQCD physical point DWF ensembles. We discuss several methods for controlling and reducing uncertainties associated to the determination of the HVP form factor.

  20. Towards the physical point hadronic vacuum polarisation from Moebius DWF

    E-Print Network [OSTI]

    Marina Marinkovic; Peter Boyle; Luigi Del Debbio; Andreas Juettner; Kim Maltman; Antonin Portelli

    2015-02-18

    We present steps towards the computation of the leading-order hadronic contribution to the muon anomalous magnetic moment on RBC/UKQCD physical point DWF ensembles. We discuss several methods for controlling and reducing uncertainties associated to the determination of the HVP form factor.