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1

Endstates Initiative | Department of Energy  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

Endstates Initiative Endstates Initiative Endstates Initiative Endstates Initiative Scientific and technical, institutional and regulatory, and closure management challenges are currently hindering cleanup and closure of remaining environmental legacy waste sites across the Department of Energy (DOE) complex. There are no simple solu¬tions for these integrated challenges and they demand innovative scientific and technical solutions and approaches, developed with the regulatory community. DOE Office of Environmental Management (EM), Office of Groundwater and Soil Remediation is developing and implement¬ing a systems-based, risk-informed framework to help site owners meet these challenges. Contacts Skip Chamberlain DOE-EM Office of Soil & Groundwater Remediation (301) 903-7248

2

NSLS Endstations | Center for Functional Nanomaterials  

NLE Websites -- All DOE Office Websites (Extended Search)

UV and X-ray Probes UV and X-ray Probes The CFN operates three end-stations at the National Synchrotron Light Source (NSLS) for nanomaterials characterization. The station located at the X9 beamline performs simultaneous small- and wide-angle X-ray scattering experiments for nano-scale structural characterization of a variety of materials. The Ambient Pressure X-ray Photoelectron Spectroscopy (AP-XPS) station located at beamline X1A1 is capable of soft X-ray photoelectron spectroscopy for quantitative surface chemical analysis of a range of materials at gas pressures up to about 1 Torr. The undulator beamline U5UA hosts a station operating in ultra-high vacuum with a low-energy electron microscope (LEEM) and X-ray photo-emission electron microscope (XPEEM). The LEEM-XPEEM system can be used to study static and

3

The Nanofocus Endstation of the MINAXS Beamline of PETRA III  

SciTech Connect

The Micro- and Nanofocus X-ray Scattering Beamline (MINAXS) of the new 3rd generation source PETRA III is equipped with two endstations, out of which the farthest from the high beta undulator source is designed to provide a high flux, monochromatic X-ray beam focused to a size in the order of 100 nmx100 nm routinely used for microdiffraction experiments (nanofocus endstation). This contribution presents an overview on the current status of the nanofocus endstation and outlines the to-be-used experimental setup.

Krywka, C. A. [IEAP, Christian-Albrechts-Universitaet zu Kiel, Leibnizstrasse 19, D-24098 Kiel (Germany); Doehrmann, R.; Roth, S. V. [DESY, Notkestrasse 85, D-22063 Hamburg (Germany); Mueller, M. [GKSS Forschungszentrum Geesthacht, Max-Planck-Strasse 1, D-21502 Geesthacht (Germany)

2010-06-23T23:59:59.000Z

4

The holography endstation of beamline P10 at PETRA III  

SciTech Connect

We present the design and instrumentation of a novel holography endstation for the P10 coherence beamline at PETRA III at DESY. The experimental imaging scheme is based on a highly coherent and divergent (cone) beam illumination, achieved by fixed curvature focusing mirrors with additional spatial and coherence filtering by x-ray waveguides. The optical elements along the beam path and the instrument under construction are described. Preliminary results obtained in a similar setting under comparable parameters are given as a benchmark, and first simulations of one of the two mirrors are presented to study the effect of imperfections on the field distribution in the focal plane.

Kalbfleisch, S.; Osterhoff, M.; Giewekemeyer, K.; Neubauer, H.; Krueger, S. P.; Hartmann, B.; Bartels, M.; Salditt, T. [Institut fuer Roentgenphysik, Universitaet Goettingen, Friedrich-Hund-Platz 1, 37077 Goettingen (Germany); Sprung, M.; Leupold, O. [HASYLAB at DESY, Notkestr. 85, 22607 Hamburg (Germany); Siewert, F. [Helmholtz Zentrum Berlin, BESSY-II, Albert-Einstein-Str. 15, 12489 Berlin (Germany)

2010-06-23T23:59:59.000Z

5

Thin Cloud Length Scales Using CALIPSO and CloudSat Data  

E-Print Network (OSTI)

Thin clouds are the most difficult cloud type to observe. The recent availability of joint cloud products from the active remote sensing instruments aboard CloudSat and the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite (CALIPSO) facilitates...

Solbrig, Jeremy E.

2010-10-12T23:59:59.000Z

6

Macrophysical Properties of Tropical Cirrus Clouds from the CALIPSO Satellite and from Ground-based Micropulse and Raman Lidars  

SciTech Connect

Lidar observations of cirrus cloud macrophysical properties over the U.S. Department of Energy Atmospheric Radiation Measurement (ARM) program Darwin, Australia site are compared from the Cloud-Aerosol Lidar and In- frared Pathfinder Satellite Observation (CALIPSO) satellite, the ground-based ARM micropulse lidar (MPL), and the ARM Raman lidar (RL). Comparisons are made using the subset of profiles where the lidar beam is not fully attenuated. Daytime measurements using the RL are shown to be relatively unaffected by the solar background and are therefore suited for checking the validity of diurnal cycles. RL and CALIPSO cloud fraction profiles show good agreement while the MPL detects significantly less cirrus, particularly during the daytime. Both MPL and CALIPSO observations show that cirrus clouds occur less frequently during the day than at night at all altitudes. In contrast, the RL diurnal cy- cle is significantly different than zero only below about 11 km; where it is the opposite sign (i.e. more clouds during the daytime). For cirrus geomet- rical thickness, the MPL and CALIPSO observations agree well and both datasets have signficantly thinner clouds during the daytime than the RL. From the examination of hourly MPL and RL cirrus cloud thickness and through the application of daytime detection limits to all CALIPSO data we find that the decreased MPL and CALIPSO cloud thickness during the daytime is very likely a result of increased daytime noise. This study highlights the vast im- provement the RL provides (compared to the MPL) in the ARM program's ability to observe tropical cirrus clouds as well as a valuable ground-based lidar dataset for the validation of CALIPSO observations and to help im- prove our understanding of tropical cirrus clouds.

Thorsen, Tyler J.; Fu, Qiang; Comstock, Jennifer M.; Sivaraman, Chitra; Vaughan, Mark A.; Winker, D.; Turner, David D.

2013-08-27T23:59:59.000Z

7

Sensors for Environmental Observatories  

E-Print Network (OSTI)

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 sensor technology and the networks that collect data from them. Present work clearly demonstrates

Hamilton, Michael P.

8

HAWC ?-Ray Observatory  

NLE Websites -- All DOE Office Websites (Extended Search)

(HAWC) Gamma Ray Observatory formally began operations. HAWC is designed to study the origin of very high-energy cosmic rays and observe the most energetic objects in the known...

9

The Boulder Atmospheric Observatory  

Science Journals Connector (OSTI)

The Boulder Atmospheric Observatory (BAO) is a unique research facility for studying the planetary boundary layer and for testing and calibrating atmospheric sensors. The facility includes a 300 m tower instrumented with fast- and slow-response ...

J. C. Kaimal; J. E. Gaynor

1983-05-01T23:59:59.000Z

10

Comparison of the CALIPSO satellite and ground-based observations of cirrus clouds at the ARM TWP sites  

SciTech Connect

Statistics of ice cloud macrophysical and optical properties from the Cloud-Aerosol LIdar with Orthogonal Polarization (CALIOP) instrument on board the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) satellite are compared with those from ground-based lidar observations over a 31 month period. Ground-based lidar observations are taken from the micropulse lidars (MPL) at the three Department of Energy Atmospheric Radiation Measurement (ARM) tropical western pacific (TWP) sites: Manus, Nauru and Darwin. CALIPSO observations show a larger cloud fraction at high altitudes while the ground-based MPLs show a larger cloud fraction at low altitudes. The difference in mean ice cloud top and base heights at the Manus and Nauru sites are all within 0.51 km, although differences are statistically significant. Mean ice cloud geometrical thickness agree to within 0.05 km at the Manus and Nauru sites. Larger differences exist at Darwin due to excessive degradation of the MPL output power during our sampling period. Both sets of observations show thicker clouds during the nighttime which may be real but could also be partially an artifact of the decreased signal-to-noise ratio during the daytime. The number of ice cloud layers per profile are also shown to be consistent after accounting for the difference in spatial resolution. For cloud optical depths, four different retrieval methods are compared, two for each set of observations. All products show that the majority of ice cloud optical depths ({approx}60%) fall below an optical depth of 0.2. For most comparisons all four retrievals agree to within the uncertainty intervals. We find that both CALIPSO retrievals agree best to ground-based optical depths when the lidar ratio in the latter is retrieved instead of set to a fixed value. Also thoroughly compared is the cloud properties for the subset of ice clouds which reside in the tropical tropopause layer (TTL).

Thorsen, Tyler J.; Fu, Q.; Comstock, Jennifer M.

2011-11-10T23:59:59.000Z

11

Alexey Kuznetsov Armagh Observatory  

E-Print Network (OSTI)

Solar radio emission · History · Instruments and methods · Results of observations Radio emission) 1933-1934: John Kraus & Arthur Adel (University of Michigan) 1890-1940: first attempts to detect radio performed during solar minima. #12;21 September 2012 Armagh Observatory 4 1942: discovery of solar radio

12

Armagh Observatory Annual Report  

E-Print Network (OSTI)

Media Mentions, 1998 21 F Public Queries, 1998 24 G Astropark Display Panels 27 #12; 1 Introduction, many of whom are engaged on fixed­term research contracts for periods ranging from one to three years Astrophysics, the Sun, Solar System astronomy, and the Earth's climate. Facilities at Armagh Observatory

13

The Green Computing Observatory: from  

E-Print Network (OSTI)

The Green Computing Observatory: from instrumentation to ontology Cécile Germain-Renaud1, Fredéric a gateway Files in XML format Available from the Grid Observatory portal GreenDays@LyonThe Green Computing) n GreenDays@LyonThe Green Computing Observatory #12;The GRIF-LAL computing room Green

Lefèvre, Laurent

14

HAWC Observatory captures first image  

NLE Websites -- All DOE Office Websites (Extended Search)

April » April » HAWC Observatory captures first image HAWC Observatory captures first image The facility is designed to detect cosmic rays and the highest energy gamma rays ever observed from astrophysical sources. April 30, 2013 The High-Altitude Water Cherenkov (HAWC) Observatory is under construction. The High-Altitude Water Cherenkov (HAWC) Observatory is under construction. HAWC is under construction inside the Parque Nacional Pico de Orizaba, a Mexican national park. An international team of researchers, including scientists from Los Alamos, has taken the first image of the High-Altitude Water Cherenkov Observatory, or HAWC. The facility is designed to detect cosmic rays and the highest energy gamma rays ever observed from astrophysical sources. HAWC is under

15

Beamline 12.2.2  

NLE Websites -- All DOE Office Websites (Extended Search)

2.2 2.2 Beamline 12.2.2 Print Tuesday, 20 October 2009 09:31 High-Pressure (California High-Pressure Science Observatory: Calipso) Endstations: Medium pressure High pressure laser heating GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Superbend magnet, 1.9GeV, 5.29Tesla, 500mA Monochromator Si(111) or Multilayer Energy range 6-40 keV for Si(111), 14-28 keV for Multilayer Resolving power (E/ΔE) Si(111) = 7000, Multilayer =100 Beam size (HxV) Focused: 10 x 10 micron Unfocused: 90 x 100 micron Scientific applications High-pressure science Scientific disciplines Earth sciences, materials science, construction materials, chemistry, energy. Endstations Medium pressure High pressure laser heating

16

Beamline 12.2.2  

NLE Websites -- All DOE Office Websites (Extended Search)

2.2 Print 2.2 Print High-Pressure (California High-Pressure Science Observatory: Calipso) Endstations: Medium pressure High pressure laser heating GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Superbend magnet, 1.9GeV, 5.29Tesla, 500mA Monochromator Si(111) or Multilayer Energy range 6-40 keV for Si(111), 14-28 keV for Multilayer Resolving power (E/ΔE) Si(111) = 7000, Multilayer =100 Beam size (HxV) Focused: 10 x 10 micron Unfocused: 90 x 100 micron Scientific applications High-pressure science Scientific disciplines Earth sciences, materials science, construction materials, chemistry, energy. Endstations Medium pressure High pressure laser heating Experimental techniques High pressure, diffraction, x-ray imaging, XAS, laser heating

17

Beamline 12.2.2  

NLE Websites -- All DOE Office Websites (Extended Search)

2.2 Print 2.2 Print High-Pressure (California High-Pressure Science Observatory: Calipso) Endstations: Medium pressure High pressure laser heating GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Superbend magnet, 1.9GeV, 5.29Tesla, 500mA Monochromator Si(111) or Multilayer Energy range 6-40 keV for Si(111), 14-28 keV for Multilayer Resolving power (E/ΔE) Si(111) = 7000, Multilayer =100 Beam size (HxV) Focused: 10 x 10 micron Unfocused: 90 x 100 micron Scientific applications High-pressure science Scientific disciplines Earth sciences, materials science, construction materials, chemistry, energy. Endstations Medium pressure High pressure laser heating Experimental techniques High pressure, diffraction, x-ray imaging, XAS, laser heating

18

Beamline 12.2.2  

NLE Websites -- All DOE Office Websites (Extended Search)

2.2 Print 2.2 Print High-Pressure (California High-Pressure Science Observatory: Calipso) Endstations: Medium pressure High pressure laser heating GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Superbend magnet, 1.9GeV, 5.29Tesla, 500mA Monochromator Si(111) or Multilayer Energy range 6-40 keV for Si(111), 14-28 keV for Multilayer Resolving power (E/ΔE) Si(111) = 7000, Multilayer =100 Beam size (HxV) Focused: 10 x 10 micron Unfocused: 90 x 100 micron Scientific applications High-pressure science Scientific disciplines Earth sciences, materials science, construction materials, chemistry, energy. Endstations Medium pressure High pressure laser heating Experimental techniques High pressure, diffraction, x-ray imaging, XAS, laser heating

19

Beamline 12.2.2  

NLE Websites -- All DOE Office Websites (Extended Search)

2.2 Print 2.2 Print High-Pressure (California High-Pressure Science Observatory: Calipso) Endstations: Medium pressure High pressure laser heating GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Superbend magnet, 1.9GeV, 5.29Tesla, 500mA Monochromator Si(111) or Multilayer Energy range 6-40 keV for Si(111), 14-28 keV for Multilayer Resolving power (E/ΔE) Si(111) = 7000, Multilayer =100 Beam size (HxV) Focused: 10 x 10 micron Unfocused: 90 x 100 micron Scientific applications High-pressure science Scientific disciplines Earth sciences, materials science, construction materials, chemistry, energy. Endstations Medium pressure High pressure laser heating Experimental techniques High pressure, diffraction, x-ray imaging, XAS, laser heating

20

Beamline 12.2.2  

NLE Websites -- All DOE Office Websites (Extended Search)

2.2 Print 2.2 Print High-Pressure (California High-Pressure Science Observatory: Calipso) Endstations: Medium pressure High pressure laser heating GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Superbend magnet, 1.9GeV, 5.29Tesla, 500mA Monochromator Si(111) or Multilayer Energy range 6-40 keV for Si(111), 14-28 keV for Multilayer Resolving power (E/ΔE) Si(111) = 7000, Multilayer =100 Beam size (HxV) Focused: 10 x 10 micron Unfocused: 90 x 100 micron Scientific applications High-pressure science Scientific disciplines Earth sciences, materials science, construction materials, chemistry, energy. Endstations Medium pressure High pressure laser heating Experimental techniques High pressure, diffraction, x-ray imaging, XAS, laser heating

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


21

Beamline 12.2.2  

NLE Websites -- All DOE Office Websites (Extended Search)

2.2 Print 2.2 Print High-Pressure (California High-Pressure Science Observatory: Calipso) Endstations: Medium pressure High pressure laser heating GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Superbend magnet, 1.9GeV, 5.29Tesla, 500mA Monochromator Si(111) or Multilayer Energy range 6-40 keV for Si(111), 14-28 keV for Multilayer Resolving power (E/ΔE) Si(111) = 7000, Multilayer =100 Beam size (HxV) Focused: 10 x 10 micron Unfocused: 90 x 100 micron Scientific applications High-pressure science Scientific disciplines Earth sciences, materials science, construction materials, chemistry, energy. Endstations Medium pressure High pressure laser heating Experimental techniques High pressure, diffraction, x-ray imaging, XAS, laser heating

22

Beamline 12.2.2  

NLE Websites -- All DOE Office Websites (Extended Search)

Beamline 12.2.2 Beamline 12.2.2 Beamline 12.2.2 Print Tuesday, 20 October 2009 09:31 High-Pressure (California High-Pressure Science Observatory: Calipso) Endstations: Medium pressure High pressure laser heating GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Superbend magnet, 1.9GeV, 5.29Tesla, 500mA Monochromator Si(111) or Multilayer Energy range 6-40 keV for Si(111), 14-28 keV for Multilayer Resolving power (E/ΔE) Si(111) = 7000, Multilayer =100 Beam size (HxV) Focused: 10 x 10 micron Unfocused: 90 x 100 micron Scientific applications High-pressure science Scientific disciplines Earth sciences, materials science, construction materials, chemistry, energy. Endstations Medium pressure

23

Beamline 12.2.2  

NLE Websites -- All DOE Office Websites (Extended Search)

2.2 Print 2.2 Print High-Pressure (California High-Pressure Science Observatory: Calipso) Endstations: Medium pressure High pressure laser heating GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Superbend magnet, 1.9GeV, 5.29Tesla, 500mA Monochromator Si(111) or Multilayer Energy range 6-40 keV for Si(111), 14-28 keV for Multilayer Resolving power (E/ΔE) Si(111) = 7000, Multilayer =100 Beam size (HxV) Focused: 10 x 10 micron Unfocused: 90 x 100 micron Scientific applications High-pressure science Scientific disciplines Earth sciences, materials science, construction materials, chemistry, energy. Endstations Medium pressure High pressure laser heating Experimental techniques High pressure, diffraction, x-ray imaging, XAS, laser heating

24

Beamline 12.2.2  

NLE Websites -- All DOE Office Websites (Extended Search)

2.2 Print 2.2 Print High-Pressure (California High-Pressure Science Observatory: Calipso) Endstations: Medium pressure High pressure laser heating GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Superbend magnet, 1.9GeV, 5.29Tesla, 500mA Monochromator Si(111) or Multilayer Energy range 6-40 keV for Si(111), 14-28 keV for Multilayer Resolving power (E/ΔE) Si(111) = 7000, Multilayer =100 Beam size (HxV) Focused: 10 x 10 micron Unfocused: 90 x 100 micron Scientific applications High-pressure science Scientific disciplines Earth sciences, materials science, construction materials, chemistry, energy. Endstations Medium pressure High pressure laser heating Experimental techniques High pressure, diffraction, x-ray imaging, XAS, laser heating

25

Evaluation of tropical cloud and precipitation statistics of CAM3 using CloudSat and CALIPSO data  

SciTech Connect

The combined CloudSat and CALIPSO satellite observations provide the first simultaneous measurements of cloud and precipitation vertical structure, and are used to examine the representation of tropical clouds and precipitation in the Community Atmosphere Model Version 3 (CAM3). A simulator package utilizing a model-to-satellite approach facilitates comparison of model simulations to observations, and a revised clustering method is used to sort the subgrid-scale patterns of clouds and precipitation into principal cloud regimes. Results from weather forecasts performed with CAM3 suggest that the model underestimates the horizontal extent of low and mid-level clouds in subsidence regions, but overestimates that of high clouds in ascending regions. CAM3 strongly overestimates the frequency of occurrence of the deep convection with heavy precipitation regime, but underestimates the horizontal extent of clouds and precipitation at low and middle levels when this regime occurs. This suggests that the model overestimates convective precipitation and underestimates stratiform precipitation consistent with a previous study that used only precipitation observations. Tropical cloud regimes are also evaluated in a different version of the model, CAM3.5, which uses a highly entraining plume in the parameterization of deep convection. While the frequency of occurrence of the deep convection with heavy precipitation regime from CAM3.5 forecasts decreases, the incidence of the low clouds with precipitation and congestus regimes increases. As a result, the parameterization change does not reduce the frequency of precipitating convection that is far too high relative to observations. For both versions of CAM, clouds and precipitation are overly reflective at the frequency of the CloudSat radar and thin clouds that could be detected by the lidar only are underestimated.

Zhang, Y; Klein, S; Boyle, J; Mace, G G

2008-11-20T23:59:59.000Z

26

Space Telescope Programs Hubble Observatory  

E-Print Network (OSTI)

Assurance/Configuration Management Mr. Christopher Scholz EAG QA Manager #12;Space Telescope Programs Hubble · COS-UCB-002 QA Implementation Plan Released December 1, 1999 · COS-UCB-003 CM Plan released DecemberSpace Telescope Programs Hubble Observatory HST-COS FUV PER 11/8/00 FUV Detector System Quality

Colorado at Boulder, University of

27

Virtual Observatories A New Era for Astronomy  

E-Print Network (OSTI)

Virtual Observatories A New Era for Astronomy Reinaldo R. de Carvalho DAS-INPE/MCT 2010 Wednesday, April 7, 2010 #12;Virtual Observatories A New Era for Astronomy Reinaldo R. de Carvalho DAS!;#--&$G !!!$ ! ' !"#$%&'&#()*! !!!$#%& !( $ ' !%&$ $ ! (% +#&,&'- .'/0&#,& Wednesday, April 7, 2010 #12;Virtual Observatories A New Era for Astronomy Reinaldo R. de

28

Chandra X-ray Observatory Center  

E-Print Network (OSTI)

Chandra X-ray Observatory Center Harvard-Smithsonian Center for Astrophysics 60 Garden St. Cambridge, MA 02138 USA http://chandra.harvard.edu Four Supernova Remnants: NASA's Chandra X-ray Observatory's Chandra X-ray Observatory, four newly processed images of supernova remnants dramatically illustrate

29

Data Center Observatory General Schematic  

E-Print Network (OSTI)

Data Center Observatory General Schematic Rack 12 critical infrastr. Rack 10 1U Rack 11 1U Rack 9 Blades Battery Battery UPS UPS PDU PDU Rack 8 mix Rack 7 1U Rack 6 1U Rack 5 1U Rack 4 3U Rack 3 1U Rack 2 1U Rack 1 3U Air FM40 Air FM40 Campuschilledwaterloop PUMP ROOM (FMS BUILDING) CICBUILDING ZONE 1

30

Worldwide R&D of Virtual Observatory  

E-Print Network (OSTI)

Virtual Observatory (VO) is a data intensive online astronomical research and education environment, taking advantages of advanced information technologies to achieve seamless and uniform access to astronomical information. The concept of VO was introduced in late of 1990s to meet challenges brought up with data avalanche in astronomy. This paper reviews current status of International Virtual Observatory Alliance, technical highlights from world wide VO projects, and a brief introduction of Chinese Virtual Observatory.

Chenzhou Cui; Yongheng Zhao

2007-11-27T23:59:59.000Z

31

Governors of the Armagh Observatory and Planetarium: Armagh Observatory Safeguarding Children and Vulnerable  

E-Print Network (OSTI)

40 Governors of the Armagh Observatory and Planetarium: Armagh Observatory Safeguarding Children the procedures in place at the Observatory in order to achieve this aim. For the purposes of this Safeguarding on the legislative context and best practice for the protection of children: "Guidance on Safeguarding Children

32

Governors of the Armagh Observatory and Planetarium: Armagh Observatory Safeguarding Children and Vulnerable  

E-Print Network (OSTI)

35 Governors of the Armagh Observatory and Planetarium: Armagh Observatory Safeguarding Children the procedures in place at the Observatory in order to achieve this aim. For the purposes of this Safeguarding on the legislative context and best practice for the protection of children: "Guidance on Safeguarding Children

33

Chandra X-ray Observatory Center  

E-Print Network (OSTI)

Chandra X-ray Observatory Center Harvard-Smithsonian Center for Astrophysics 60 Garden St 200 million light years from Earth. (Credit: X-ray: NASA/CXC/UAH/M.Sun et al; Optical: NASA, ESA, & the Hubble Heritage Team (STScI/AURA) Caption: This composite image from the Chandra X-ray Observatory (blue

34

The Pierre Auger Cosmic Ray Observatory  

E-Print Network (OSTI)

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.

,

2015-01-01T23:59:59.000Z

35

The Mars Atmospheric Constellation Observatory (MACO) Concept  

Science Journals Connector (OSTI)

The Mars Atmospheric Constellation Observatory (MACO) represents an innovative approach...2, and dust cycles together with the energy and momentum budgets. The mission concept is based on a constellation of satel...

E. R. Kursinski; W. Folkner; C. Zuffada

2004-01-01T23:59:59.000Z

36

3D Spectroscopy and the Virtual Observatory  

E-Print Network (OSTI)

Integral field, or 3D, spectroscopy is the technique of obtaining spectral information over a two-dimensional, hopefully contiguous, field of view. While there is some form of astronomical 3D spectroscopy at all wavelengths, there has been a rapid increase in interest in optical and near-infrared 3D spectroscopy. This has resulted in the deployment of a large variety of integral-field spectrographs on most of the large optical/infrared telescopes. The amount of IFU data available in observatory archives is large and growing rapidly. The complications of treating IFU data as both imaging and spectroscopy make it a special challenge for the virtual observatory. This article describes the various techniques of optical and near-infrared spectroscopy and some of the general needs and issues related to the handling of 3D data by the virtual observatory.

Bryan W. Miller

2007-08-15T23:59:59.000Z

37

Hybrid Performance of the Pierre Auger Observatory  

E-Print Network (OSTI)

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.

B. R. Dawson; for the Pierre Auger Collaboration

2007-06-08T23:59:59.000Z

38

Recent Progress at the Pierre Auger Observatory  

Science Journals Connector (OSTI)

......the shape of the cosmic ray energy spectrum, the nature of the...of light. For the highest energy cosmic rays this cascade...observatory in Men- doza Province, Argentina, is funded and is under construction...growing to 16 detectors at an energy of 1020eV. This sampling of......

Bruce R. Dawson

2003-05-01T23:59:59.000Z

39

Solar Dynamics Observatory/ Extreme Ultraviolet Variability Experiment  

E-Print Network (OSTI)

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

Mojzsis, Stephen J.

40

UK observatories look to private sector  

Science Journals Connector (OSTI)

... London. The British government has announced that private-sector organizations will be invited to bid for the services provided by its 'Royal ... a negotiator with the Institute of Professionals, Managers and Specialists (IPMS), says that private-sector management of the observatories is not the solution to what he describes as " ...

Ehsan Masood

1996-05-02T23:59:59.000Z

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


41

Carnegie Mellon Opens Data Center Observatory  

E-Print Network (OSTI)

of up to 774 kW â " more than the rate of consumption of 750 average-sized homes. In addition Home > Media Center > In the News > Carnegie Mellon Opens Data Center Observatory Carnegie Mellon Opens,000-square-foot DCO has the ability to support 40 racks of computers, which would consume energy at a rate

42

Bishop's University Astronomical Observatory October 2009  

E-Print Network (OSTI)

of our visitors. The solar panel and battery system provide sufficient energy to easily light the deck that was built on the roof of Nicolls adjacent to the Observatory and the other is Bishop's first-ever solar panel mounted next to it. The deck was built late last summer and completes the final phase

43

Chandra X-ray Observatory Center  

E-Print Network (OSTI)

Chandra X-ray Observatory Center Harvard-Smithsonian Center for Astrophysics 60 Garden St in hot gas about 250 million light years from Earth. (Credit: X-ray: NASA/CXC/SAO/E.Bulbul, et al-Newton has revealed a mysterious X-ray signal in the data. This signal is represented in the circled data

44

Chandra X-ray Observatory Center  

E-Print Network (OSTI)

Chandra X-ray Observatory Center Harvard-Smithsonian Center for Astrophysics 60 Garden St million light years from Earth. (Credit: X-ray: NASA/CXC/Wesleyan Univ./R.Kilgard, et al; Optical: NASA with optical data from the Hubble Space Telescope (red, green, and blue). The X-ray data reveal hundreds

45

The endless mantra : innovation at the Keck Observatory  

E-Print Network (OSTI)

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 ...

Bobra, Monica Godha

2005-01-01T23:59:59.000Z

46

The Pierre Auger Observatory: Perspectives on Ultra-High Energy  

E-Print Network (OSTI)

¨ue, Argentina Abstract The Pierre Auger Observatory for ultra-high energy cosmic rays is under constructionThe Pierre Auger Observatory: Perspectives on Ultra-High Energy Cosmic Rays Tiina Suomij¨arvi1 in Argentina. The Observatory will consist when completed of 1600 water Cerenkov tanks and 24 fluorescence

Paris-Sud XI, Université de

47

Science Potential of a Deep Ocean Antineutrino Observatory  

E-Print Network (OSTI)

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.

Steve Dye

2006-12-15T23:59:59.000Z

48

National Radio Astronomy Observatory Electronics Division Technical Note No. 219  

E-Print Network (OSTI)

1 National Radio Astronomy Observatory Electronics Division Technical Note No. 219 Measurements of Automotive Radar Emissions received by a Radio Astronomy Observatory Darrel Emerson (National Radio Astronomy (Continental Corporation, A.D.C. Automotive Distance Control Systems GmbH, Germany), Juergen

Groppi, Christopher

49

THE CAMPUS OBSERVATORY at the University of Saskatchewan  

E-Print Network (OSTI)

THE CAMPUS OBSERVATORY at the University of Saskatchewan ABOUT: The campus observatory provides facilities at the University of Saskatchewan are available for use by both uni- versity students and visitors-deductible contribution payable to the University of Saskatchewan. Adoption rates de- pend upon the star's apparent

Peak, Derek

50

AstroGrid and the Astrophysical Virtual Observatory: first capabilities  

Science Journals Connector (OSTI)

......Astrophysical Virtual Observatory initiative. Its "first light" event was held at Jodrell Bank Observatory on 20 January...lan- der will plunge into the thin mart- ian atmosphere on Christmas Day, using a parachute and airbags dur- ing its descent to......

Nicholas Walton

2003-08-01T23:59:59.000Z

51

The Aosta Valley Astronomical Observatory Carbognani, A.1,2  

E-Print Network (OSTI)

The Aosta Valley Astronomical Observatory Carbognani, A.1,2 1 B.P. 4229 F-06304 NICE Cedex 4 Observatory of the Autonomous Region of the Aosta Valley (Italy). The centre is located in the northwestern Italian Alps, near the border with France and Switzerland (Lat: 45° 47 22 N, Long: 7° 28 42 E), at 1675 m

Paris-Sud XI, Université de

52

Ocean Observatories Initiative: Pacific Northwest The Endurance Array  

E-Print Network (OSTI)

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

Kurapov, Alexander

53

Science with the constellation-X observatory  

SciTech Connect

The Constellation X-ray Mission is a high throughput X-ray facility emphasizing observations at high spectral resolution (E/{delta}E{approx}300-3000), and broad energy bandpass (0.25-40 keV). Constellation-X will provide a factor of nearly 100 increase in sensitivity over current high resolution X-ray spectroscopy missions. It is the X-ray astronomy equivalent of large ground-based optical telescopes such as the Keck Observatory and the ESO Very Large Telescope. When observations commence toward the end of next decade, Constellation-X will address many fundamental astrophysics questions such as: the formation and evolution of clusters of galaxies; constraining the baryon content of the Universe; determining the spin and mass of supermassive black holes in AGN; and probing strong gravity in the vicinity of black holes.

Valinia, Azita [NASA's Goddard Space Flight Center, Code 662, Greenbelt, Maryland 20771 (United States); Department of Astronomy, University of Maryland, College Park, Maryland 20742 (United States); White, Nicholas [NASA's Goddard Space Flight Center, Code 662, Greenbelt, Maryland 20771 (United States); Tananbaum, Harvey [Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, Massachusetts 02138 (United States)

1999-04-27T23:59:59.000Z

54

Science with the constellation-X observatory  

Science Journals Connector (OSTI)

The Constellation X-ray Mission is a high throughput X-ray facility emphasizing observations at high spectral resolution ( E /? E ?3003000) and broad energy bandpass (0.2540 keV). Constellation-X will provide a factor of nearly 100 increase in sensitivity over current high resolution X-ray spectroscopy missions. It is the X-ray astronomy equivalent of large ground-based optical telescopes such as the Keck Observatory and the ESO Very Large Telescope. When observations commence toward the end of next decade Constellation-X will address many fundamental astrophysics questions such as: the formation and evolution of clusters of galaxies; constraining the baryon content of the Universe; determining the spin and mass of supermassive black holes in AGN; and probing strong gravity in the vicinity of black holes.

Azita Valinia; Nicholas White; Harvey Tananbaum

1999-01-01T23:59:59.000Z

55

EChO - Exoplanet Characterisation Observatory  

E-Print Network (OSTI)

A dedicated mission to investigate exoplanetary atmospheres represents a major milestone in our quest to understand our place in the universe by placing our Solar System in context and by addressing the suitability of planets for the presence of life. EChO -the Exoplanet Characterisation Observatory- is a mission concept specifically geared for this purpose. EChO will provide simultaneous, multi-wavelength spectroscopic observations on a stable platform that will allow very long exposures. EChO will build on observations by Hubble, Spitzer and groundbased telescopes, which discovered the first molecules and atoms in exoplanetary atmospheres. EChO will simultaneously observe a broad enough spectral region -from the visible to the mid-IR- to constrain from one single spectrum the temperature structure of the atmosphere and the abundances of the major molecular species. The spectral range and resolution are tailored to separate bands belonging to up to 30 molecules to retrieve the composition and temperature str...

Tinetti, G; Henning, T; Meyer, M; Micela, G; Ribas, I; Stam, D; Swain, M; Krause, O; Ollivier, M; Pace, E; Swinyard, B; Aylward, A; van Boekel, R; Coradini, A; Encrenaz, T; Snellen, I; Zapatero-Osorio, M R; Bouwman, J; Cho, J Y-K; Foresto, V Coud du; Guillot, T; Lopez-Morales, M; Mueller-Wodarg, I; Palle, E; Selsis, F; Sozzetti, A; Ade, P A R; Achilleos, N; Adriani, A; Agnor, C B; Afonso, C; Prieto, C Allende; Bakos, G; Barber, R J; Barlow, M; Bernath, P; Bezard, B; Bord, P; Brown, L R; Cassan, A; Cavarroc, C; Ciaravella, A; Cockell, C O U; Coustenis, A; Danielski, C; Decin, L; De Kok, R; Demangeon, O; Deroo, P; Doel, P; Drossart, P; Fletcher, L N; Focardi, M; Forget, F; Fossey, S; Fouqu, P; Frith, J; Galand, M; Gaulme, P; Hernndez, J I Gonzlez; Grasset, O; Grassi, D; Grenfell, J L; Griffin, M J; Griffith, C A; Grzinger, U; Guedel, M; Guio, P; Hainaut, O; Hargreaves, R; Hauschildt, P H; Heng, K; Heyrovsky, D; Hueso, R; Irwin, P; Kaltenegger, L; Kervella, P; Kipping, D; Koskinen, T T; Kovcs, G; La Barbera, A; Lammer, H; Lellouch, E; Leto, G; Morales, M Lopez; Valverde, M A Lopez; Lopez-Puertas, M; Lovis, C; Maggio, A; Maillard, J P; Prado, J Maldonado; Marquette, J B; Martin-Torres, F J; Maxted, P; Miller, S; Molinari, S; Montes, D; Moro-Martin, A; Moses, J I; Mousis, O; Tuong, N Nguyen; Nelson, R; Orton, G S; Pantin, E; Pascale, E; Pezzuto, S; Pinfield, D; Poretti, E; Prinja, R; Prisinzano, L; Rees, J M; Reiners, A; Samuel, B; Sanchez-Lavega, A; Forcada, J Sanz; Sasselov, D; Savini, G; Sicardy, B; Smith, A; Stixrude, L; Strazzulla, G; Tennyson, J; Tessenyi, M; Vasisht, G; Vinatier, S; Viti, S; Waldmann, I; White, G J; Widemann, T; Wordsworth, R; Yelle, R; Yung, Y; Yurchenko, S N

2011-01-01T23:59:59.000Z

56

Radio Wavelength Observatories within the Exploration Architecture  

E-Print Network (OSTI)

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.

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

2007-01-26T23:59:59.000Z

57

E-Print Network 3.0 - astrophysical observatory letter Sample...  

NLE Websites -- All DOE Office Websites (Extended Search)

restore and widen access... ; 15; strengthen the Observatory's research capacity in solar system and stellar astrophysics; 15... interests of Observatory sta11; currently...

58

Low Energy Investigations at Kamioka Observatory  

E-Print Network (OSTI)

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...

Sekiya, Hiroyuki

2013-01-01T23:59:59.000Z

59

The Green Computing Observatory: status of acquisition and analysis  

E-Print Network (OSTI)

The Green Computing Observatory: status of acquisition and analysis Cécile Germain-Renaud1, Julien, CNRS, INRIA 2: Laboratoire de l'Accélérateur Linéaire, CNRS-IN2P3 #12; Previous GreenDays talks o GreenDays@Paris The Green Computing Observatory: plans and scientific challenges o GreenDays@Lyon The Green Computing

Lefèvre, Laurent

60

Low Energy Investigations at Kamioka Observatory  

E-Print Network (OSTI)

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.

Hiroyuki Sekiya

2013-01-30T23:59:59.000Z

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


61

Atmospheric aerosol monitoring at the Pierre Auger Observatory  

SciTech Connect

For a ground based cosmic-ray observatory the atmosphere is an integral part of the detector. Air fluorescence detectors (FDs) are particularly sensitive to the presence of aerosols in the atmosphere. These aerosols, consisting mainly of clouds and dust, can strongly affect the propagation of fluorescence and Cherenkov light from cosmic-ray induced extensive air showers. The Pierre Auger Observatory has a comprehensive program to monitor the aerosols within the atmospheric volume of the detector. In this paper the aerosol parameters that affect FD reconstruction will be discussed. The aerosol monitoring systems that have been deployed at the Pierre Auger Observatory will be briefly described along with some measurements from these systems.

Cester, R.; Chiosso, M.; Chirin, J.; Clay, R.; Dawson, B.; Fick, B.; Filipcic, A.; Garcia, B.; Grillo, A.; Horvat, M.; Iarlori, M.; Malek, M.; Matthews, J.; Matthews,; Melo, D.; Meyhandan, R.; Mostafa, M.; Mussa, R.; Prouza, M.; Raefert, B.; Rizi, V.

2005-07-01T23:59:59.000Z

62

The GAMMA-400 space observatory: status and perspectives  

E-Print Network (OSTI)

The present design of the new space observatory GAMMA-400 is presented in this paper. The instrument has been designed for the optimal detection of gamma rays in a broad energy range (from ~100 MeV up to 3 TeV), with excellent angular and energy resolution. The observatory will also allow precise and high statistic studies of the electron component in the cosmic rays up to the multi TeV region, as well as protons and nuclei spectra up to the knee region. The GAMMA-400 observatory will allow to address a broad range of science topics, like search for signatures of dark matter, studies of Galactic and extragalactic gamma-ray sources, Galactic and extragalactic diffuse emission, gamma-ray bursts and charged cosmic rays acceleration and diffusion mechanism up to the knee.

Galper, A M; Topchiev, N P; Adriani, O; Aptekar, R L; Arkhangelskaja, I V; Arkhangelskiy, A I; Bergstrom, L; Berti, E; Bigongiari, G; Bobkov, S G; Boezio, M; Bogomolov, E A; Bonechi, S; Bongi, M; Bottai, S; Boyarchuk, K A; Castellini, G; Cattaneo, P W; Cumani, P; Dedenko, G L; De Donato, C; Dogiel, V A; 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; Mikhailov, V V; Mocchiutti, E; Moiseev, A A; Mori, N; Moskalenko, I V; Naumov, P Yu; Papini, P; Pearce, M; Picozza, P; Popov, A V; Rappoldi, A; Ricciarini, S; Runtso, M F; Ryde, F; Serdin, O V; Sparvoli, R; Spillantini, P; Suchkov, S I; Tavani, M; Taraskin, A A; Tiberio, A; Tyurin, E M; Ulanov, M V; Vacchi, A; Vannuccini, E; Vasilyev, G I; Yurkin, Yu T; Zampa, N; Zirakashvili, V N; Zverev, V G

2014-01-01T23:59:59.000Z

63

European Information Technology Observatory EITO 2002 2. What is sustainable  

E-Print Network (OSTI)

250 European Information Technology Observatory · EITO 2002 2. What is sustainable development the Brundtland Commis- sion's 1987 report, "Our Common Future". Here, sustainable development is defined their own needs".1 This chapter defines sustainable develop- ment as: A dynamic process which enables all

Loke, Seng W. - Loke, Seng W.

64

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

65

Neutral Current Detectors for the Sudbury Neutrino Observatory  

E-Print Network (OSTI)

3 Neutral Current Detectors for the Sudbury Neutrino Observatory Peter Michael Thornewell Lincoln), a 1,000 tonne heavy water Cerenkov detector presently under construction. This detector will measure the 8B e flux and energy spectrum via a pure charge current reaction, and independently the 8B total

Waltham, Chris

66

India-Based Neutrino Observatory (INO) Mar 28, 2014  

E-Print Network (OSTI)

India-Based Neutrino Observatory (INO) Mar 28, 2014 PRESS RELEASE Sub: Misreporting on Media of INO project strongly condemn the recent media mis-information campaign and vilification in reports that have. Such rumour-mongering is at best poor reporting, and at worst deliberate and malicious. It is reprehensible

Udgaonkar, Jayant B.

67

Wayne State Solar Observatory located at Lake St. Clair Metropark  

E-Print Network (OSTI)

Wayne State Solar Observatory located at Lake St. Clair Metropark Dustin Scriven working under resources, we aim to open the doors of exploration to those in the region who may not otherwise have into the STEM fields. This year we planned to start by emphasizing solar observations as opposed to night sky

Cinabro, David

68

NOAA Satellite and Information Service Deep Space Climate Observatory (DSCOVR)  

E-Print Network (OSTI)

such as the commercial airline, electric power and GPS industries. Our national security and economic well-being, whichNOAA Satellite and Information Service Deep Space Climate Observatory (DSCOVR) Background: DSCOVR will maintain the Nation's solar wind observations, which are critical to maintaining the accuracy and lead time

69

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

DOE Data Explorer (OSTI)

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.

Bob Busey; Larry Hinzman

70

E-Print Network 3.0 - apache point observatory Sample Search...  

NLE Websites -- All DOE Office Websites (Extended Search)

Public Education Apache Point Observatory www.apo.nmsu.edu 505... -437-6822 2001 Apache Point Road P.O. Box 59 Sunspot, NM 88349-0059 Fred Lawrence Whipple Observatory cfa... ......

71

The Local Seeing Environment at Big Bear Solar Observatory Angelo Verdoni and Carsten Denker1  

E-Print Network (OSTI)

­ Big Bear Solar Observatory (BBSO) in California, Mees Solar Observatory (MSO) on Haleakal¯a, MauiThe Local Seeing Environment at Big Bear Solar Observatory Angelo Verdoni and Carsten Denker1 New Jersey Institute of Technology, Center for Solar-Terrestrial Research, 323 Martin Luther King Blvd

72

Effort on Developing Cabled Ocean Observatories Research Assitant, Institute of Mechatronics Control Engineering, Zhejiang University  

E-Print Network (OSTI)

Effort on Developing Cabled Ocean Observatories in China Yanhu Chen Research Assitant, Institute and Resources Engineering, University of Hawaii Abstract Cabled ocean observatory that enables abundant power cabled ocean observatories to support ocean scientific research in China, Zhejiang University has been

Frandsen, Jannette B.

73

Identifying clouds over the Pierre Auger Observatory using infrared satellite data  

SciTech Connect

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.

Abreu, Pedro; et al.,

2013-12-01T23:59:59.000Z

74

Hybrid Detection of UHECR with the Pierre Auger Observatory  

E-Print Network (OSTI)

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.

Miguel Mostafa; for the Pierre Auger Collaboration

2006-07-31T23:59:59.000Z

75

The Hybrid Activities of the Pierre Auger Observatory  

E-Print Network (OSTI)

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 I describe the hybrid reconstruction approach and the latest hybrid measurements.

Miguel Mostafa

2006-08-30T23:59:59.000Z

76

Technology Development for a Neutrino AstrophysicalObservatory  

SciTech Connect

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.

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.

1996-02-01T23:59:59.000Z

77

Technology development for a neutrino astrophysical observatory. Letter of intent  

SciTech Connect

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.

Chaloupka, V.; Cole, T.; Crawford, H.J. [and others

1996-02-01T23:59:59.000Z

78

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

SciTech Connect

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.

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

2009-06-01T23:59:59.000Z

79

EARLY SCIENCE WITH SOFIA, THE STRATOSPHERIC OBSERVATORY FOR INFRARED ASTRONOMY  

SciTech Connect

The Stratospheric Observatory For Infrared Astronomy (SOFIA) is an airborne observatory consisting of a specially modified Boeing 747SP with a 2.7 m telescope, flying at altitudes as high as 13.7 km (45,000 ft). Designed to observe at wavelengths from 0.3 {mu}m to 1.6 mm, SOFIA operates above 99.8% of the water vapor that obscures much of the infrared and submillimeter. SOFIA has seven science instruments under development, including an occultation photometer, near-, mid-, and far-infrared cameras, infrared spectrometers, and heterodyne receivers. SOFIA, a joint project between NASA and the German Aerospace Center Deutsches Zentrum fuer Luft und-Raumfahrt, began initial science flights in 2010 December, and has conducted 30 science flights in the subsequent year. During this early science period three instruments have flown: the mid-infrared camera FORCAST, the heterodyne spectrometer GREAT, and the occultation photometer HIPO. This Letter provides an overview of the observatory and its early performance.

Young, E. T.; Becklin, E. E.; De Buizer, J. M.; Andersson, B.-G.; Casey, S. C.; Helton, L. A. [SOFIA Science Center, Universities Space Research Association, NASA Ames Research Center, MS 232, Moffett Field, CA 94035 (United States); Marcum, P. M.; Roellig, T. L.; Temi, P. [NASA Ames Research Center, MS 232, Moffett Field, CA 94035 (United States); Herter, T. L. [Astronomy Department, 202 Space Sciences Building, Cornell University, Ithaca, NY 14853-6801 (United States); Guesten, R. [Max-Planck Institut fuer Radioastronomie, Auf dem Huegel 69, Bonn (Germany); Dunham, E. W. [Lowell Observatory, 1400 W. Mars Hill Rd., Flagstaff AZ 86001 (United States); Backman, D.; Burgdorf, M. [SOFIA Science Center, NASA Ames Research Center, MS 211-1, Moffett Field, CA 94035 (United States); Caroff, L. J.; Erickson, E. F. [NASA Ames Research Center, Moffett Field, CA 94035 (United States); Davidson, J. A. [School of Physics, The University of Western Australia (M013), 35 Stirling Highway, Crawley WA 6009 (Australia); Gehrz, R. D. [Minnesota Institute for Astrophysics, School of Physics and Astronomy, 116 Church Street, S. E., University of Minnesota, Minneapolis, MN 55455 (United States); Harper, D. A. [Yerkes Observatory, University of Chicago, 373 W. Geneva St., Williams Bay, WI (United States); Harvey, P. M. [Astronomy Department, University of Texas at Austin, 1 University Station C1400, Austin, TX 78712-0259 (United States); and others

2012-04-20T23:59:59.000Z

80

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

SciTech Connect

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.

Mason, Brian D.; Hartkopf, William I.; Wycoff, Gary L., E-mail: bdm@usno.navy.mil, E-mail: wih@usno.navy.mil [U.S. Naval Observatory, 3450 Massachusetts Avenue, NW, Washington, DC 20392-5420 (United States)

2011-08-15T23:59:59.000Z

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


81

SPECKLE INTERFEROMETRY AT THE U.S. NAVAL OBSERVATORY. XV  

SciTech Connect

Results of 2433 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 1013 mean relative positions and range in separation from 0.''96 to 58.''05, with a mean separation of 13.''50. This paper is the 15th in the series of papers and covers the period 2008 January 3 through 2008 December 21.

Mason, Brian D.; Hartkopf, William I.; Wycoff, Gary L., E-mail: bdm@usno.navy.mi, E-mail: wih@usno.navy.mi, E-mail: glw@usno.navy.mi [U.S. Naval Observatory, 3450 Massachusetts Avenue, NW, Washington, DC 20392-5420 (United States)

2010-08-15T23:59:59.000Z

82

Photometric stability analysis of the Exoplanet Characterisation Observatory  

E-Print Network (OSTI)

Photometric stability is a key requirement for time-resolved spectroscopic observations of transiting extrasolar planets. In the context of the Exoplanet Characterisation Observatory (EChO) mission design, we here present and investigate means of translating spacecraft pointing instabilities as well as temperature fluctuation of its optical chain into an overall error budget of the exoplanetary spectrum to be retrieved. Given the instrument specifications as of date, we investigate the magnitudes of these photometric instabilities in the context of simulated observations of the exoplanet HD189733b secondary eclipse.

Waldmann, I P; Swinyard, B; Tinetti, G; Amaral-Rogers, A; Spencer, L; Tessenyi, M; Ollivier, M; Foresto, V Coud du

2013-01-01T23:59:59.000Z

83

SCALER MODE OF THE AUGER OBSERVATORY AND SUNSPOTS  

SciTech Connect

Recent data from the Auger Observatory on low-energy secondary cosmic ray particles are analyzed to study temporal correlations together with data on the daily sunspot numbers and neutron monitor data. Standard spectral analysis demonstrates that the available data show 1/f {sup {beta}} fluctuations with {beta} Almost-Equal-To 1 in the low-frequency range. All data behave like Brownian fluctuations in the high-frequency range. The existence of long-range correlations in the data was confirmed by detrended fluctuation analysis. The real data confirmed the correlation between the scaling exponent of the detrended analysis and the exponent of the spectral analysis.

Canal, Carlos A. Garcia; Tarutina, Tatiana [Instituto de Fisica La Plata, CCT La Plata, CONICET and Departamento de Fisica, Facultad de Ciencias Exactas, Universidad Nacional de La Plata CC 67, 1900 La Plata (Argentina); Hojvat, Carlos [Fermilab, P.O. Box 500, Batavia, IL 60510-0500 (United States)

2012-10-15T23:59:59.000Z

84

The Central Laser Facility at the Pierre Auger Observatory  

E-Print Network (OSTI)

The Central Laser Facility is located near the middle of the Pierre Auger Observatory in Argentina. It features a UV laser and optics that direct a beam of calibrated pulsed light into the sky. Light scattered from this beam produces tracks in the Auger optical detectors which normally record nitrogen fluorescence tracks from cosmic ray air showers. The Central Laser Facility provides a "test beam" to investigate properties of the atmosphere and the fluorescence detectors. The laser can send light via optical fiber simultaneously to the nearest surface detector tank for hybrid timing analyses. We describe the facility and show some examples of its many uses.

F. Arqueros; J. Bellido; C. Covault; D. D'Urso; C. Di Giulio; P. Facal; B. Fick; F. Guarino; M. Malek; J. A. J. Matthews; J. Matthews; R. Meyhandan; M. Monasor; M. Mostafa; P. Petrinca; M. Roberts; P. Sommers; P. Travnicek; L. Valore; V. Verzi; L. Wiencke

2005-07-13T23:59:59.000Z

85

New gamma-ray observatory begins operations at Sierra Negra volcano in the  

NLE Websites -- All DOE Office Websites (Extended Search)

New gamma-ray observatory begins operations New gamma-ray observatory begins operations New gamma-ray observatory begins operations at Sierra Negra volcano in the state of Puebla, Mexico The High-Altitude Water Cherenkov Gamma Ray Observatory has begun formal operations at its site in Mexico. August 21, 2013 The HAWC Observatory taken in August 2013 from the summit of Sierra Negra. The image has been digitally altered to show HAWC as it will appear when construction is complete in 2014. The 111 Cherenkov detectors currently installed (100 Cherenkov detectors in operation) are colored white and located in the upper right quadrant of the array. The HAWC Observatory taken in August 2013 from the summit of Sierra Negra. The image has been digitally altered to show HAWC as it will appear when construction is complete in 2014. The 111 Cherenkov detectors currently

86

HSRL mass estimate based on CALIPSO  

NLE Websites -- All DOE Office Websites (Extended Search)

NASA B-200 King Air ARCTAS/ISDAC NASA B-200 King Air ARCTAS/ISDAC Operations and Science Richard Ferrare, Chris Hostetler, John Hair, Anthony Cook, David Harper, Mike Obland, Ray Rogers, Sharon Burton, Matt Shupe, Dave Turner, Connor Flynn B200/HSRL Deployment During ARCTAS (Spring)  Independently measures aerosol/cloud extinction and backscatter profiles at 532 nm  Includes - Backscatter channels at 1064 nm - Polarization sensitivity at 532 and 1064 nm  Profile Measurement capabilities - Extensive measurements * Backscatter at 532 and 1064 nm * Extinction at 532 nm - Intensive measurements * Color ratio (or Angstrom coeff.) for backscatter (β 1064 / β 532 ) * Extinction-to-backscatter ratio at 532 nm * Depolarization at 532 and 1064 nm High Spectral Resolution Lidar (HSRL) *B200 based in Barrow, Alaska

87

HSRL mass estimate based on CALIPSO  

NLE Websites -- All DOE Office Websites (Extended Search)

NASA B-200 King Air ARCTASISDAC Operations and Science Richard Ferrare, Chris Hostetler, John Hair, Anthony Cook, David Harper, Mike Obland, Ray Rogers, Sharon Burton, Matt Shupe,...

88

HSRL mass estimate based on CALIPSO  

NLE Websites -- All DOE Office Websites (Extended Search)

OBSERVATIONS FROM THE NASA LANGLEY AIRBORNE HIGH SPECTRAL RESOLUTION LIDAR AND PLANS FOR ACTIVE-PASSIVE AEROSOL-CLOUD RETRIEVALS Chris A. Hostetler, Richard A. Ferrare, John W....

89

Observatory of Renewable Energy for Latin America and the Caribbean | Open  

Open Energy Info (EERE)

Observatory of Renewable Energy for Latin America and the Caribbean Observatory of Renewable Energy for Latin America and the Caribbean Jump to: navigation, search Logo: Observatory of Renewable Energy for Latin America and the Caribbean Name Observatory of Renewable Energy for Latin America and the Caribbean Agency/Company /Organization Latin America Energy Organization Partner UNIDO Sector Energy Focus Area Renewable Energy, Agriculture, Biomass, Energy Efficiency, Industry, Solar Topics Background analysis, Technology characterizations Resource Type Dataset, Software/modeling tools Website http://www.renenergyobservator Program Start 2009 Country Brazil, Chile, Costa Rica, Colombia, Cuba, Dominican Republic, Ecuador, Mexico, Nicaragua, Paraguay, Peru, Uruguay UN Region Caribbean, Central America, South America

90

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

SciTech Connect

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.

Gangodagamage, Chandana; Wilson, Cathy; Rowland, Joel

2013-12-08T23:59:59.000Z

91

E-Print Network 3.0 - auger observatory surface Sample Search...  

NLE Websites -- All DOE Office Websites (Extended Search)

MOU Outreach 12;Auger Finance... sch Surface Array Maintenance Activities Solar panels ... Source: Pierre Auger Observatory Collection: Physics 14 F t Pl t...

92

Informational Webinar: Frontier Observatory for Research in Geothermal Energy (FORGE) Funding Opportunity Announcement  

Energy.gov (U.S. Department of Energy (DOE))

The Energy Department will present a live webinar titled Frontier Observatory for Research in Geothermal Energy (FORGE) Funding Opportunity Announcement Informational Webinar," focusing on the...

93

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

E-Print Network (OSTI)

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.

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-Muiz; 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. Bcker; M. Balzer; K. B. Barber; A. F. Barbosa; R. Bardenet; S. L. C. Barroso; B. Baughman; J. Buml; J. J. Beatty; B. R. Becker; K. H. Becker; A. Belltoile; J. A. Bellido; S. BenZvi; C. Berat; X. Bertou; P. L. Biermann; P. Billoir; F. Blanco; M. Blanco; C. Bleve; H. Blmer; M. Boh?ov; 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. Conceio; 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. Daz 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. Frhlich; B. Fuchs; R. Gaior; R. F. Gamarra; S. Gambetta; B. Garca; D. Garca Gmez; 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. Gmez Berisso; P. Gonalves; D. Gonzalez; J. G. Gonzalez; B. Gookin; D. Gra; 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. Hrandel; A. Horneffer; M. Hrabovsk; T. Huege; A. Insolia; F. Ionita; A. Italiano; C. Jarne; S. Jiraskova; M. Josebachuili; K. Kadija; K. -H. Kampert; P. Karhan; P. Kasper; B. Kgl; 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. Krmer; D. Kruppke-Hansen; F. Kuehn; D. Kuempel; J. K. Kulbartz; N. Kunka; G. La Rosa; C. Lachaud; P. Lautridou; M. S. A. B. Leo; D. Lebrun; P. Lebrun; M. A. Leigui de Oliveira; A. Lemiere; A. Letessier-Selvon; I. Lhenry-Yvon; K. Link; R. Lpez; A. Lopez Agera; 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. Martnez 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. Mostaf; C. A. Moura; S. Mueller; M. A. Muller; G. Mller; M. Mnchmeyer; 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. Noka; M. Nyklicek; J. Oehlschlger; 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. Rodrguez-Fras; G. Ros; J. Rosado

2011-07-24T23:59:59.000Z

94

E-Print Network 3.0 - astrophysical observatory cambridge Sample...  

NLE Websites -- All DOE Office Websites (Extended Search)

Rt. Hon. John Denham MP Summary: physics University of Cambridge Particle physics phenomenology Royal Observatory Edinburgh Astrophysics... physics University of Cambridge High...

95

Hydrogen: An End-State Solution for Transportation?  

Science Journals Connector (OSTI)

There is presently no global consensus on how our human society might ultimately transform from a hydrocarbon, fossil fuel-based energy economy to an alternative low-carbon, or zero-carbon economy. The same is tr...

Asel Sartbaeva; Stephen A. Wells

2012-01-01T23:59:59.000Z

96

James Cronin, CP Violation, and the Pierre Auger Observatory  

Office of Scientific and Technical Information (OSTI)

James Cronin, CP Violation and the Pierre Auger Observatory James Cronin, CP Violation and the Pierre Auger Observatory Resources with Additional Information James Cronin Courtesy Brookhaven National Laboratory James Watson Cronin "received his B.S. degree from Southern Methodist University in 1951. He then attended the University of Chicago for graduate school, earning his M.S. in 1953 and his Ph.D. in 1955. He began his scientific career at Brookhaven National Laboratory, where he served as an assistant physicist from 1955 to 1958. Cronin joined the faculty at Princeton University in 1958, where he remained until 1971, when he was appointed the University Professor of Physics at the University of Chicago. He became University Professor Emeritus of physics in 1997."1 "While working at Brookhaven National Laboratory in 1964, Cronin and [Val L.] Fitch, both then at Princeton, observed the first example of nature's preference for matter over antimatter."1 "The experiment uncovered the CP [charge-parity] violation, or a break in particle-antiparticle symmetry, and earned Cronin and Fitch the 1980 Nobel Prize in Physics ."2

97

HEAT - a low energy enhancement of the Pierre Auger Observatory  

E-Print Network (OSTI)

The High Elevation Auger Telescopes (HEAT) are three tiltable fluorescence telescopes which represent a low energy enhancement of the fluorescence telescope system of the southern site of the Pierre Auger Observatory in Argentina. The Pierre Auger Observatory is a hybrid cosmic ray detector consisting of 24 fluorescence telescopes to measure the fluorescence light of extensive air showers complemented by 1600 water Cherenkov detectors to determine the particle densities at ground. In this configuration air showers with a primary energy of 10^18 eV and above are investigated. By lowering the energy threshold by approximately one order of magnitude down to a primary energy of 10^17 eV, HEAT provides the possibility to study the cosmic ray energy spectrum and mass composition in a very interesting energy range, where the transition from galactic to extragalactic cosmic rays is expected to happen. The installation of HEAT was finished in 2009 and data have been taken continuously since September 2009. Within thes...

Meurer, C

2011-01-01T23:59:59.000Z

98

DOI 10.1007/s11207-009-9485-8 THE SOLAR DYNAMICS OBSERVATORY  

E-Print Network (OSTI)

) since December 1995. ESP is designed to measure solar Extreme UltraViolet (EUV) irradiance in four first · Spectrophotometer · Radiometric calibration 1. Introduction The Solar Dynamics Observatory (SDO) is the first NASASolar Phys DOI 10.1007/s11207-009-9485-8 THE SOLAR DYNAMICS OBSERVATORY EUV SpectroPhotometer (ESP

Didkovsky, Leonid

99

Proceedings of ICRC 2001: 752 c Copernicus Gesellschaft 2001 Surface detector calibration for the Auger Observatory  

E-Print Network (OSTI)

Observatorio Pierre Auger, Av. San Martin Norte 304, (5613) Malarg¨ue, Argentina Abstract. The ground array Observatory in Malarg¨ue, Argentina. 1 Introduction The purpose of the Pierre Auger Observatory is the study of the origin and the nature of the highest energy cosmic rays, with energies above 1019 eV (Auger collaboration

100

2012 International Conference on Lightning Protection (ICLP), Vienna, Austria Lightning Observatory in Gainesville (LOG), Florida  

E-Print Network (OSTI)

) and 1(b), respectively. The LOG was originally designed to respond to both natural lightning flashes2012 International Conference on Lightning Protection (ICLP), Vienna, Austria Lightning Observatory, Inc., Tucson, Arizona, USA E-mail: (rakov@ece.ufl.edu) Abstract--The Lightning Observatory

Florida, University of

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


101

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

E-Print Network (OSTI)

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

Joseph, Robert D.

102

Parallel air temperature measurements at the KNMI observatory in De Bilt (the  

E-Print Network (OSTI)

in De Bilt (the Netherlands) May 2003 - June 2005 | March 14, 2011 Page 6 of 56 #12;nal | Parallel air at the KNMI observatory in De Bilt (the Netherlands) May 2003 - June 2005 | March 14, 2011 Page 8 of 56 #12Parallel air temperature measurements at the KNMI observatory in De Bilt (the Netherlands) May 2003

Brandsma, Theo

103

Observatory/data centre partnerships and the VO-centric archive: The JCMT Science Archive experience  

E-Print Network (OSTI)

We present, as a case study, a description of the partnership between an observatory (JCMT) and a data centre (CADC) that led to the development of the JCMT Science Archive (JSA). The JSA is a successful example of a service designed to use Virtual Observatory (VO) technologies from the start. We describe the motivation, process and lessons learned from this approach.

Economou, Frossie; Jenness, Tim; Redman, Russell O; Goliath, Sharon; Dowler, Patrick; Currie, Malcolm J; Bell, Graham S; Graves, Sarah F; Ouellette, John; Johnstone, Doug; Schade, David; Chrysostomou, Antonio

2014-01-01T23:59:59.000Z

104

Experiment Profile: COUPP NAME: Chicagoland Observatory for Underground Particle  

NLE Websites -- All DOE Office Websites (Extended Search)

COUPP COUPP NAME: Chicagoland Observatory for Underground Particle Physics, or COUPP WHAT WILL THIS TELL US ABOUT THE WORLD? Everything you see, visible matter, makes up 4 percent of the universe. Dark matter and dark energy makes up the rest of the universe. Physicists understand that dark matter acts as an invisible source of gravity, but little more. COUPP seeks to pinpoint what particles make up dark matter, which will help explain how the universe came to exist. Without the added gravitational attraction of dark matter, stars and galaxies would never have formed. The expansion of the universe after the Big Bang would have dispersed visible matter too quickly. WHY IS THIS EXPERIMENT NEEDED NOW? Physicists have narrowed the hunt for what particles constitute dark

105

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

SciTech Connect

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.

Mason, Brian D.; Hartkopf, William I.; Hurowitz, Haley M., E-mail: bdm@usno.navy.mil, E-mail: wih@usno.navy.mil, E-mail: hurowitz@mit.edu [U.S. Naval Observatory, 3450 Massachusetts Avenue, NW, Washington, DC 20392-5420 (United States)

2013-09-15T23:59:59.000Z

106

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

SciTech Connect

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.

Mason, Brian D.; Hartkopf, William I.; Friedman, Elizabeth A., E-mail: bdm@usno.navy.mil, E-mail: wih@usno.navy.mil, E-mail: efriedman09@ucla.edu [U.S. Naval Observatory, 3450 Massachusetts Avenue, NW, Washington, DC 20392-5420 (United States)

2012-05-15T23:59:59.000Z

107

Results from the Sudbury Neutrino Observatory Phase III  

SciTech Connect

The third and last phase of the Sudbury Neutrino Observatory (SNO) used a technique independent of previous methods, to measure the rate of neutral-current interactions in heavy water and determine precisely the total active {sup 8}B solar neutrino flux. The total flux obtained is 5.54{sub -0.31}{sup +0.33}(stat){sub -0.34}{sup +0.36}(syst) x 10{sup 6} cm{sup -2}s{sup -1}, in agreement with previous measurements and standard solar models. Results from a global analysis of solar and reactor neutrino give {Delta}m{sup 2} = 7.59{sub -0.21}{sup +0.19} x 10{sup -5} eV{sup 2} and {theta} = 34.4{sub -1.2}{sup +1.3} degrees with a reduced uncertainty on the mixing angle compared to previous phases.

SNO Collaboration; Prior, G.

2008-11-03T23:59:59.000Z

108

The Large Observatory For X-ray Timing: LOFT  

E-Print Network (OSTI)

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.

Bozzo, E

2013-01-01T23:59:59.000Z

109

Single Ion Trapping For The Enriched Xenon Observatory  

E-Print Network (OSTI)

In the last decade, a variety of neutrino oscillation experiments have established that there is a mass difference between neutrino flavors, without determining the absolute neutrino mass scale. The Enriched Xenon Observatory for neutrinoless double beta decay (EXO) will search for the rare decays of xenon to determine the absolute value of the neutrino mass. The experiment uses a novel technique to minimize backgrounds, identifying the decay daughter product in real time using single ion spectroscopy. Here, we describe single ion trapping and spectroscopy compatible with the EXO detector. We extend the technique of single ion trapping in ultrahigh vacuum to trapping in xenon gas. With this technique, EXO will achieve a neutrino mass sensitivity of ? m?? ≃ .010 eV.

Waldman, S J

2005-01-01T23:59:59.000Z

110

LIGO: the Laser Interferometer Gravitational-Wave Observatory  

Science Journals Connector (OSTI)

The goal of the Laser Interferometric Gravitational-Wave Observatory (LIGO) is to detect and study gravitational waves (GWs) of astrophysical origin. Direct detection of GWs holds the promise of testing general relativity in the strong-field regime, of providing a new probe of exotic objects such as black holes and neutron stars and of uncovering unanticipated new astrophysics. LIGO, a joint CaltechMIT project supported by the National Science Foundation, operates three multi-kilometer interferometers at two widely separated sites in the United States. These detectors are the result of decades of worldwide technology development, design, construction and commissioning. They are now operating at their design sensitivity, and are sensitive to gravitational wave strains smaller than one part in 1021. With this unprecedented sensitivity, the data are being analyzed to detect or place limits on GWs from a variety of potential astrophysical sources.

B P Abbott; R Abbott; R Adhikari; P Ajith; B Allen; G Allen; R S Amin; S B Anderson; W G Anderson; M A Arain; M Araya; H Armandula; P Armor; Y Aso; S Aston; P Aufmuth; C Aulbert; S Babak; P Baker; S Ballmer; C Barker; D Barker; B Barr; P Barriga; L Barsotti; M A Barton; I Bartos; R Bassiri; M Bastarrika; B Behnke; M Benacquista; J Betzwieser; P T Beyersdorf; I A Bilenko; G Billingsley; R Biswas; E Black; J K Blackburn; L Blackburn; D Blair; B Bland; T P Bodiya; L Bogue; R Bork; V Boschi; S Bose; P R Brady; V B Braginsky; J E Brau; D O Bridges; M Brinkmann; A F Brooks; D A Brown; A Brummit; G Brunet; A Bullington; A Buonanno; O Burmeister; R L Byer; L Cadonati; J B Camp; J Cannizzo; K C Cannon; J Cao; L Cardenas; S Caride; G Castaldi; S Caudill; M Cavagli; C Cepeda; T Chalermsongsak; E Chalkley; P Charlton; S Chatterji; S Chelkowski; Y Chen; N Christensen; C T Y Chung; D Clark; J Clark; J H Clayton; T Cokelaer; C N Colacino; R Conte; D Cook; T R C Corbitt; N Cornish; D Coward; D C Coyne; J D E Creighton; T D Creighton; A M Cruise; R M Culter; A Cumming; L Cunningham; S L Danilishin; K Danzmann; B Daudert; G Davies; E J Daw; D DeBra; J Degallaix; V Dergachev; S Desai; R DeSalvo; S Dhurandhar; M Daz; A Dietz; F Donovan; K L Dooley; E E Doomes; R W P Drever; J Dueck; I Duke; J-C Dumas; J G Dwyer; C Echols; M Edgar; A Effler; P Ehrens; E Espinoza; T Etzel; M Evans; T Evans; S Fairhurst; Y Faltas; Y Fan; D Fazi; H Fehrmenn; L S Finn; K Flasch; S Foley; C Forrest; N Fotopoulos; A Franzen; M Frede; M Frei; Z Frei; A Freise; R Frey; T Fricke; P Fritschel; V V Frolov; M Fyffe; V Galdi; J A Garofoli; I Gholami; J A Giaime; S Giampanis; K D Giardina; K Goda; E Goetz; L M Goggin; G Gonzlez; M L Gorodetsky; S Goler; R Gouaty; A Grant; S Gras; C Gray; M Gray; R J S Greenhalgh; A M Gretarsson; F Grimaldi; R Grosso; H Grote; S Grunewald; M Guenther; E K Gustafson; R Gustafson; B Hage; J M Hallam; D Hammer; G D Hammond; C Hanna; J Hanson; J Harms; G M Harry; I W Harry; E D Harstad; K Haughian; K Hayama; J Heefner; I S Heng; A Heptonstall; M Hewitson; S Hild; E Hirose; D Hoak; K A Hodge; K Holt; D J Hosken; J Hough; D Hoyland; B Hughey; S H Huttner; D R Ingram; T Isogai; M Ito; A Ivanov; B Johnson; W W Johnson; D I Jones; G Jones; R Jones; L Ju; P Kalmus; V Kalogera; S Kandhasamy; J Kanner; D Kasprzyk; E Katsavounidis; K Kawabe; S Kawamura; F Kawazoe; W Kells; D G Keppel; A Khalaidovski; F Y Khalili; R Khan; E Khazanov; P King; J S Kissel; S Klimenko; K Kokeyama; V Kondrashov; R Kopparapu; S Koranda; D Kozak; B Krishnan; R Kumar; P Kwee; P K Lam; M Landry; B Lantz; A Lazzarini; H Lei; M Lei; N Leindecker; I Leonor; C Li; H Lin; P E Lindquist; T B Littenberg; N A Lockerbie; D Lodhia; M Longo; M Lormand; P Lu; M Lubinski; A Lucianetti; H Lck; B Machenschalk; M MacInnis; M Mageswaran; K Mailand; I Mandel; V Mandic; S Mrka; Z Mrka; A Markosyan; J Markowitz; E Maros; I W Martin; R M Martin; J N Marx; K Mason; F Matichard; L Matone; R A Matzner; N Mavalvala; R McCarthy; D E McClelland; S C McGuire; M McHugh; G McIntyre; D J A McKechan; K McKenzie; M Mehmet; A Melatos; A C Melissinos; D F Menndez; G Mendell; R A Mercer; S Meshkov; C Messenger; M S Meyer; J Miller; J Minelli; Y Mino; V P Mitrofanov; G Mitselmakher; R Mittleman; O Miyakawa; B Moe; S D Mohanty; S R P Mohapatra; G Moreno; T Morioka; K Mors; K Mossavi; C MowLowry; G Mueller; H Mller-Ebhardt; D Muhammad; S Mukherjee; H Mukhopadhyay; A Mullavey; J Munch; P G Murray; E Myers; J Myers; T Nash; J Nelson; G Newton; A Nishizawa; K Numata; J O'Dell; B O'Reilly; R O'Shaughnessy; E Ochsner; G H Ogin; D J Ottaway; R S Ottens; H Overmier; B J Owen; Y Pan; C Pankow; M A Papa; V Parameshwaraiah; P Patel; M Pedraza; S Penn; A Perraca; V Pierro; I M Pinto; M Pitkin; H J Pletsch; M V Plissi; F Postiglione; M Principe; R Prix; L Prokhorov; O Punken; V Quetschke; F J Raab; D S Rabeling; H Radkins; P Raffai; Z Raics; N Rainer; M Rakhmanov; V Raymond; C M Reed; T Reed; H Rehbein; S Reid; D H Reitze; R Riesen; K Riles; B Rivera; P Roberts; N A Robertson; C Robinson; E L Robinson; S Roddy; C Rver; J Rollins; J D Romano; J H Romie; S Rowan; A Rdiger; P Russell; K Ryan; S Sakata; L Sancho de la Jordana; V Sandberg; V Sannibale; L Santamara; S Saraf; P Sarin; B S Sathyaprakash; S Sato; M Satterthwaite; P R Saulson; R Savage; P Savov; M Scanlan; R Schilling; R Schnabel; R Schofield; B Schulz; B F Schutz; P Schwinberg; J Scott; S M Scott; A C Searle; B Sears; F Seifert; D Sellers; A S Sengupta; A Sergeev; B Shapiro; P Shawhan; D H Shoemaker; A Sibley; X Siemens; D Sigg; S Sinha; A M Sintes; B J J Slagmolen; J Slutsky; J R Smith; M R Smith; N D Smith; K Somiya; B Sorazu; A Stein; L C Stein; S Steplewski; A Stochino; R Stone; K A Strain; S Strigin; A Stroeer; A L Stuver; T Z Summerscales; K-X Sun; M Sung; P J Sutton; G P Szokoly; D Talukder; L Tang; D B Tanner; S P Tarabrin; J R Taylor; R Taylor; J Thacker; K A Thorne; A Thring; K V Tokmakov; C Torres

2009-01-01T23:59:59.000Z

111

Optical calibration hardware for the Sudbury Neutrino Observatory  

E-Print Network (OSTI)

The optical properties of the Sudbury Neutrino Observatory (SNO) heavy water Cherenkov neutrino detector are measured in situ using a light diffusing sphere ("laserball"). This diffuser is connected to a pulsed nitrogen/dye laser via specially developed underwater optical fibre umbilical cables. The umbilical cables are designed to have a small bending radius, and can be easily adapted for a variety of calibration sources in SNO. The laserball is remotely manipulated to many positions in the D2O and H2O volumes, where data at six different wavelengths are acquired. These data are analysed to determine the absorption and scattering of light in the heavy water and light water, and the angular dependence of the response of the detector's photomultiplier tubes. This paper gives details of the physical properties, construction, and optical characteristics of the laserball and its associated hardware.

B. A. Moffat; R. J. Ford; F. A. Duncan; K. Graham; A. L. Hallin; C. A. W. Hearns; J. Maneira; P. Skensved; D. R. Grant

2005-07-19T23:59:59.000Z

112

The SOFIA Observatory at the Start of Routine Science Operations : Mission capabilities and performance  

E-Print Network (OSTI)

The Stratospheric Observatory for Infrared Astronomy (SOFIA) has recently concluded a set of engineering flights for Observatory performance evaluation. These in-flight opportunities are viewed as a first comprehensive assessment of the Observatory's performance and are used to guide future development activities, as well as to identify additional Observatory upgrades. Pointing stability was evaluated, including the image motion due to rigid-body and flexible-body telescope modes as well as possible aero-optical image motion. We report on recent improvements in pointing stability by using an active mass damper system installed on the telescope. Measurements and characterization of the shear layer and cavity seeing, as well as image quality evaluation as a function of wavelength have also been performed. Additional tests targeted basic Observatory capabilities and requirements, including pointing accuracy, chopper evaluation and imager sensitivity. This paper reports on the data collected during these flights ...

Temi, Pasquale; Young, Erick; Adams, Joseph D; Adams, Sybil; Andersson, B -G; Becklin, Eric E; Boogert, Adwin; Brewster, Rick; Burgh, Eric; Cobleigh, Brent R; Culp, Steven; De Buizer, Jim; Dunham, Edward W; Engfer, Christian; Ediss, Geoffrey; Fujieh, Maura; Grashuis, Randy; Gross, Michael; Harmon, Edward; Helton, Andrew; Hoffman, Douglas; Homan, Jeff; Hutwohl, Michael; Jakob, Holger; Jensen, Stephen C; Kaminski, Charles; Kozarsky, Daniel; Krabbe, Alfred; Klein, Randolf; Lammen, Yannick; Lampater, Ulrich; Latter, William B; Le, Jeanette; McKown, Nancy; Melchiorri, Riccardo; Meyer, Allan W; Miles, John; Miller, Walter E; Miller, Scott; Moore, Elizabeth; Nickison, Donald J; Opshaug, Kortney; Pfueller, Enrico; Radomski, James; Rasmussen, John; Reach, William; Reinacher, Andreas; Roellig, Thomas L; Sandell, Goran; Sankrit, Ravi; Savage, Maureen L; Shenoy, Sachindev; Schonfeld, Julie E; Shuping, Ralph Y; Smith, Erin C; Talebi, Ehsan; Teufel, Stefan; Tseng, Ting C; Vacca, William D; Vaillancourt, John; Van Cleve, Jeffrey E; Wiedemann, Manuel; Wolf, Jurgen; Zavala, Eddie; Zeile, Oliver; Zell, Peter T; Zinnecker, Hans

2014-01-01T23:59:59.000Z

113

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

E-Print Network (OSTI)

The Mauna Kea Observatories Near-Infrared Filter Set. I: Defining Optima 1-5µm Bandpasses D. A #12;The Mauna Kea Observatories Near-Infrared Filter Set. I: Defining Optimal 1­5 µm Bandpasses D. A. This was discussed in detail by Young et al. (1994). The Mauna Kea Observatories Near-Infrared (MKO-NIR) filters

114

The Large Observatory For x-ray Timing  

E-Print Network (OSTI)

The Large Observatory For x-ray Timing (LOFT) was studied within ESA M3 Cosmic Vision framework and participated in the final down-selection for a launch slot in 2022-2024. Thanks to the unprecedented combination of effective area and spectral resolution of its main instrument, LOFT will study the behaviour of matter under extreme conditions, such as the strong gravitational field in the innermost regions of accretion flows close to black holes and neutron stars, and the supra-nuclear densities in the interior of neutron stars. The science payload is based on a Large Area Detector (LAD, 10 m 2 effective area, 2-30 keV, 240 eV spectral resolution, 1 deg collimated field of view) and a WideField Monitor (WFM, 2-50 keV, 4 steradian field of view, 1 arcmin source location accuracy, 300 eV spectral resolution). The WFM is equipped with an on-board system for bright events (e.g. GRB) localization. The trigger time and position of these events are broadcast to the ground within 30 s from discovery. In this paper we ...

Feroci, M; Bozzo, E; Barret, D; Brandt, S; Hernanz, M; van der Klis, M; Pohl, M; Santangelo, A; Stella, L; Watts, A; Wilms, J; Zane, S; Ahangarianabhari, M; Albertus, C; Alford, M; Alpar, A; Altamirano, D; Alvarez, L; Amati, L; Amoros, C; Andersson, N; Antonelli, A; Argan, A; Artigue, R; Artigues, B; Atteia, J -L; Azzarello, P; Bakala, P; Baldazzi, G; Balman, S; Barbera, M; van Baren, C; Bhattacharyya, S; Baykal, A; Belloni, T; Bernardini, F; Bertuccio, G; Bianchi, S; Bianchini, A; Binko, P; Blay, P; Bocchino, F; Bodin, P; Bombaci, I; Bidaud, J -M Bonnet; Boutloukos, S; Bradley, L; Braga, J; Brown, E; Bucciantini, N; Burderi, L; Burgay, M; Bursa, M; Budtz-Jrgensen, C; Cackett, E; Cadoux, F R; Cais, P; Caliandro, G A; Campana, R; Campana, S; Capitanio, F; Casares, J; Casella, P; Castro-Tirado, A J; Cavazzuti, E; Cerda-Duran, P; Chakrabarty, D; Chteau, F; Chenevez, J; Coker, J; Cole, R; Collura, A; Cornelisse, R; Courvoisier, T; Cros, A; Cumming, A; Cusumano, G; D'A, A; D'Elia, V; Del Monte, E; De Luca, A; De Martino, D; Dercksen, J P C; De Pasquale, M; De Rosa, A; Del Santo, M; Di Cosimo, S; Diebold, S; Di Salvo, T; 1), I Donnarumma; (32), A Drago; (33), M Durant; (107), D Emmanoulopoulos; (135), M H Erkut; (85), P Esposito; (1, Y Evangelista; 1b),; (24), A Fabian; (34), M Falanga; (25), Y Favre; (35), C Feldman; (128), V Ferrari; (3), C Ferrigno; (133), M Finger; (36), M H Finger; (35, G W Fraser; +),; (2), M Frericks; (7), F Fuschino; (125), M Gabler; (37), D K Galloway; (6), J L Galvez Sanchez; (6), E Garcia-Berro; (10), B Gendre; (62), S Gezari; (39), A B Giles; (40), M Gilfanov; (10), P Giommi; (102), G Giovannini; (102), M Giroletti; (4), E Gogus; (105), A Goldwurm; (86), K Goluchov; (16), D Gtz; (16), C Gouiffes; (56), M Grassi; (42), P Groot; (17), M Gschwender; (128), L Gualtieri; (32), C Guidorzi; (3), L Guy; (2), D Haas; (50), P Haensel; (29), M Hailey; (19), F Hansen; (42), D H Hartmann; (43), C A Haswell; (88), K Hebeler; (37), A Heger; (2), W Hermsen; (28), J Homan; (19), A Hornstrup; (23, R Hudec; 72),; (45), J Huovelin; (5), A Ingram; (2), J J M in't Zand; (27), G Israel; (20), K Iwasawa; (47), L Izzo; (2), H M Jacobs; (17), F Jetter; (118, T Johannsen; 127),; (2), H M Jacobs; (2), P Jonker; (126), J Jos; (49), P Kaaret; (123), G Kanbach; (23), V Karas; (6), D Karelin; (29), D Kataria; (49), L Keek; (29), T Kennedy; (17), D Klochkov; (50), W Kluzniak; (17), K Kokkotas; (45), S Korpela; (51), C Kouveliotou; (87), I Kreykenbohm; (2), L M Kuiper; (19), I Kuvvetli; (7), C Labanti; (52), D Lai; (53), F K Lamb; (2), P P Laubert; (105), F Lebrun; (8), D Lin; (29), D Linder; (54), G Lodato; (55), F Longo; (19), N Lund; (131), T J Maccarone; (14), D Macera; (8), S Maestre; (62), S Mahmoodifar; (17), D Maier; (56), P Malcovati; (120), I Mandel; (144), V Mangano; (50), A Manousakis; (7), M Marisaldi; (109), A Markowitz; (35), A Martindale; (59), G Matt; (107), I M McHardy; (60), A Melatos; (61), M Mendez; (85), S Mereghetti; (68), M Michalska; (20), S Migliari; (85, R Mignani; 108),; (62), M C Miller; (49), J M Miller; (57), T Mineo; (112), G Miniutti; (64), S Morsink; (65), C Motch; (13), S Motta; (66), M Mouchet; (8), G Mouret; (19), J Mula?ov; (1, F Muleri; 1b),; (140), T Muoz-Darias; (95), I Negueruela; (28), J Neilsen; (43), A J Norton; (28), M Nowak; (35), P O'Brien; (19), P E H Olsen; (102), M Orienti; (99, M Orio; 110),; (7), M Orlandini; (68), P Orleanski; (35), J P Osborne; (69), R Osten; (70), F Ozel; (1, L Pacciani; 1b),; (119), M Paolillo; (6), A Papitto; (20), J M Paredes; (83, A Patruno; 141),; (71), B Paul; (17), E Perinati; (115), A Pellizzoni; (47), A V Penacchioni; (136), M A Perez; (72), V Petracek; (10), C Pittori; (95), J Pons; (6), J Portell; (115), A Possenti; (73), J Poutanen; (122), M Prakash; (16), P Le Provost; (70), D Psaltis; (8), D Rambaud; (8), P Ramon; (76), G Ramsay; (1, M Rapisarda; 1b),; (77), A Rachevski; (77), I Rashevskaya; (78), P S Ray; (6), N Rea; (80), S Reddy; (113, P Reig; 81),; (63), M Reina Aranda; (28), R Remillard; (62), C Reynolds; (124), L Rezzolla; (20), M Ribo; (2), R de la Rie; (115), A Riggio; (138), A Rios; (82, P Rodrguez- Gil; 104),; (16), J Rodriguez; (3), R Rohlfs; (57), P Romano; (83), E M R Rossi; (50), A Rozanska; (29), A Rousseau; (84), F Ryde; (63), L Sabau-Graziati; (6), G Sala; (85), R Salvaterra; (61), A Sanna; (134), J Sandberg; (130), S Scaringi; (16), S Schanne; (86), J Schee; (87), C Schmid; (117), S Shore; (27), R Schneider; (88), A Schwenk; (89), A D Schwope; (114), J -Y Seyler; (90), A Shearer; (29), A Smith; (58), D M Smith; (29), P J Smith; (23), V Sochora; (1), P Soffitta; (61), P Soleri; (29), A Spencer

2014-01-01T23:59:59.000Z

115

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

SciTech Connect

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.

Mason, Brian D.; Hartkopf, William I.; Wycoff, Gary L., E-mail: bdm@usno.navy.mil, E-mail: wih@usno.navy.mil [U.S. Naval Observatory, 3450 Massachusetts Avenue, NW, Washington, DC 20392-5420 (United States)

2011-05-15T23:59:59.000Z

116

EChOSim: The Exoplanet Characterisation Observatory software simulator  

E-Print Network (OSTI)

EChOSim is the end-to-end time-domain simulator of the Exoplanet Characterisation Observatory (EChO) space mission. EChOSim has been developed to assess the capability EChO has to detect and characterize the atmospheres of transiting exoplanets, and through this revolutionize the knowledge we have of the Milky Way and of our place in the Galaxy. Here we discuss the details of the EChOSim implementation and describe the models used to represent the instrument and to simulate the detection. Software simulators have assumed a central role in the design of new instrumentation and in assessing the level of systematics affecting the measurements of existing experiments. Thanks to its high modularity, EChOSim can simulate basic aspects of several existing and proposed spectrometers for exoplanet transits, including instruments on the Hubble Space Telescope and Spitzer, or ground-based and balloon borne experiments. A discussion of different uses of EChOSim is given, including examples of simulations performed to ass...

Pascale, E; MacTavish, C J; Papageorgiou, A; Amaral-Rogers, A; Varley, R; de Foresto, V Coud; Griffin, M J; Ollivier, M; Sarkar, S; Spencer, L; Swinyard, B M; Tessenyi, M; Tinetti, G

2014-01-01T23:59:59.000Z

117

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

E-Print Network (OSTI)

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.

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

2006-04-28T23:59:59.000Z

118

The next generation Cherenkov Telescope Array observatory: CTA  

E-Print Network (OSTI)

The Cherenkov Telescope Array (CTA) is a large collaborative effort aimed at the design and operation of an observatory dedicated to the VHE gamma-ray astrophysics in the energy range 30 GeV-100 TeV, which will improve by about one order of magnitude the sensitivity with respect to the current major arrays (H.E.S.S., MAGIC, and VERITAS). In order to achieve such improved performance, for both the northern and southern CTA sites, four units of 23m diameter Large Size Telescopes (LSTs) will be deployed close to the centre of the array with telescopes separated by about 100m. A larger number (about 25 units) of 12m Medium Size Telescopes (MSTs, separated by about 150m), will cover a larger area. The southern site will also include up to 24 Schwarzschild-Couder dual-mirror medium-size Telescopes (SCTs) with the primary mirror diameter of 9.5m. Above a few TeV, the Cherenkov light intensity is such that showers can be detected even well outside the light pool by telescopes significantly smaller than the MSTs. To a...

Vercellone, Stefano

2014-01-01T23:59:59.000Z

119

3D Spectroscopy in the Virtual Observatory: Current Status  

E-Print Network (OSTI)

Three cornerstones for the 3D data support in the Virtual Observatory are: (1) data model to describe them, (2) data access services providing access to fully-reduced datasets, and (3) client applications which can deal with 3D data. Presently all these components became available in the VO. We demonstrate an application of the IVOA Characterisation data model to description of IFU and Fabry-Perot datasets. Two services providing SSA-like access to 3D-spectral data and Characterisation metadata have been implemented by us: ASPID-SR at SAO RAS for accessing IFU and Fabry-Perot data from the Russian 6-m telescope, and the Giraffe Archive at the VO Paris portal for the VLT FLAMES-Giraffe datasets. We have implemented VO Paris Euro3D Client, handling Euro3D FITS format, that interacts with CDS Aladin and ESA VOSpec using PLASTIC to display spatial and spectral cutouts of 3D datasets. Though the prototype we are presenting is yet rather simple, it demonstrates how 3D spectroscopic data can be fully integrated into the VO infrastructure.

Igor Chilingarian; Francois Bonnarel; Mireille Louys; Ivan Zolotukhin; Frederic Royer; Isabelle Jegouzo; Pierre Le Sidaner; Pierre Fernique; Thomas Boch

2007-11-02T23:59:59.000Z

120

The Offline Software Framework of the Pierre Auger Observatory  

E-Print Network (OSTI)

The Pierre Auger Observatory is designed to unveil the nature and the origins of the highest energy cosmic rays. The large and geographically dispersed collaboration of physicists and the wide-ranging collection of simulation and reconstruction tasks pose some special challenges for the offline analysis software. We have designed and implemented a general purpose framework which allows collaborators to contribute algorithms and sequencing instructions to build up the variety of applications they require. The framework includes machinery to manage these user codes, to organize the abundance of user-contributed configuration files, to facilitate multi-format file handling, and to provide access to event and time-dependent detector information which can reside in various data sources. A number of utilities are also provided, including a novel geometry package which allows manipulation of abstract geometrical objects independent of coordinate system choice. The framework is implemented in C++, and takes advantage of object oriented design and common open source tools, while keeping the user side simple enough for C++ novices to learn in a reasonable time. The distribution system incorporates unit and acceptance testing in order to support rapid development of both the core framework and contributed user code.

S. Argiro; S. L. C. Barroso; J. Gonzalez; L. Nellen; T. Paul; T. A. Porter; L. Prado Jr.; M. Roth; R. Ulrich; D. Veberic

2007-07-11T23:59:59.000Z

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121

The Offline Software Framework of the Pierre Auger Observatory  

E-Print Network (OSTI)

The Pierre Auger Observatory is designed to unveil the nature and the origins of the highest energy cosmic rays. The large and geographically dispersed collaboration of physicists and the wide-ranging collection of simulation and reconstruction tasks pose some special challenges for the offline analysis software. We have designed and implemented a general purpose framework which allows collaborators to contribute algorithms and sequencing instructions to build up the variety of applications they require. The framework includes machinery to manage these user codes, to organize the abundance of user-contributed configuration files, to facilitate multi-format file handling, and to provide access to event and time-dependent detector information which can reside in various data sources. A number of utilities are also provided, including a novel geometry package which allows manipulation of abstract geometrical objects independent of coordinate system choice. The framework is implemented in C++, and takes advantage of object oriented design and common open source tools, while keeping the user side simple enough for C++ novices to learn in a reasonable time. The distribution system incorporates unit and acceptance testing in order to support rapid development of both the core framework and contributed user code.

S. Argiro; S. L. C Barroso; J. Gonzalez; L. Nellen; T. Paul; T. A. Porter; L. Prado Jr.; M. Roth; R. Ulrich; D. Veberic

2006-01-01T23:59:59.000Z

122

The Final Results from the Sudbury Neutrino Observatory  

ScienceCinema (OSTI)

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.

None

2011-04-25T23:59:59.000Z

123

Enhanced crustal geo-neutrino production near the Sudbury Neutrino Observatory, Ontario, Canada  

E-Print Network (OSTI)

records average crustal radio-activity over the whole crustal column and is unaffected by small-scale Observatory (SNO) has been in operation since November 1999. The upgrade of the facility to SNO+ in the coming

Long, Bernard

124

Photographic observations of comet Hale-Bopp at the Pulkovo Observatory: The detection of dust envelopes  

Science Journals Connector (OSTI)

The photographic observations of comet Hale-Bopp with the 26-inch Pulkovo Observatory ... in MarchApril, 1998, revealed three hemispherical gas-dust envelopes and one spiral jet in...

Yu. N. Gnedin; A. A. Kiselev; T. P. Kiseleva; K. L. Maslennikov

2001-04-01T23:59:59.000Z

125

The Instrumentation and Observing Program at Grinnell Colleges Grant O. Gale Observatory  

Science Journals Connector (OSTI)

Many small observatories are associated with undergraduate colleges at which research programs must be integrated with a broad spectrum of educational programs. The instrumentation and observing programs of Grinn...

R. R. Cadmus Jr.; F. M. Melsheimer

1986-01-01T23:59:59.000Z

126

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

E-Print Network (OSTI)

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) ...

Sonley, Thomas John

2009-01-01T23:59:59.000Z

127

Using ACIS on the Chandra X-ray Observatory as a particle radiation monitor  

E-Print Network (OSTI)

The Advanced CCD Imaging Spectrometer (ACIS) is one of two focal-plane instruments on the Chandra X-ray Observatory. During initial radiation-belt passes, the exposed ACIS suffered significant radiation damage from trapped ...

Grant, Catherine E.

128

Study on 10 kVDC powered junction box for a cabled ocean observatory system  

Science Journals Connector (OSTI)

A cabled ocean observatory system that can provide abundant power and broad bandwidth communication for undersea instruments ... current (kVDC) with up to 10 kW power, along with 1 Gigabit/sec Ethernet communicat...

Yan-hu Chen ???; Can-jun Yang ???; De-jun Li ???; Bo Jin ? ?

2013-04-01T23:59:59.000Z

129

Evidence for neutrino oscillations in the Sudbury Neutrino Observatory  

SciTech Connect

The Sudbury Neutrino Observatory (SNO) is a large-volume heavy water Cerenkov detector designed to resolve the solar neutrino problem. SNO observes charged-current interactions with electron neutrinos, neutral-current interactions with all active neutrinos, and elastic-scattering interactions primarily with electron neutrinos with some sensitivity to other flavors. This dissertation presents an analysis of the solar neutrino flux observed in SNO in the second phase of operation, while {approx}2 tonnes of salt (NaCl) were dissolved in the heavy water. The dataset here represents 391 live days of data. Only the events above a visible energy threshold of 5.5 MeV and inside a fiducial volume within 550 cm of the center of the detector are studied. The neutrino flux observed via the charged-current interaction is [1.71 {+-} 0.065(stat.){+-}{sub 0.068}{sup 0.065}(sys.){+-}0.02(theor.)] x 10{sup 6}cm{sup -2}s{sup -1}, via the elastic-scattering interaction is [2.21{+-}0.22(stat.){+-}{sub 0.12}{sup 0.11}(sys.){+-}0.01(theor.)] x 10{sup 6}cm{sup -2}s{sup -1}, and via the neutral-current interaction is [5.05{+-}0.23(stat.){+-}{sub 0.37}{sup 0.31}(sys.){+-}0.06(theor.)] x 10{sup 6}cm{sup -2}s{sup -1}. The electron-only flux seen via the charged-current interaction is more than 7{sigma} below the total active flux seen via the neutral-current interaction, providing strong evidence that neutrinos are undergoing flavor transformation as they travel from the core of the Sun to the Earth. The most likely origin of the flavor transformation is matter-induced flavor oscillation.

Marino, Alysia Diane

2004-08-10T23:59:59.000Z

130

The next generation Cherenkov Telescope Array observatory: CTA  

Science Journals Connector (OSTI)

Abstract The Cherenkov Telescope Array (CTA) is a large collaborative effort aimed at the design and operation of an observatory dedicated to the very high-energy gamma-ray astrophysics in the energy range 30GeV100TeV, which will improve by about one order of magnitude the sensitivity with respect to the current major arrays (H.E.S.S., MAGIC, and VERITAS). In order to achieve such improved performance, for both the northern and southern CTA sites, four units of 23m diameter Large Size Telescopes (LSTs) will be deployed close to the centre of the array with telescopes separated by about 100m. A larger number (about 25 units) of 12m Medium Size Telescopes (MSTs, separated by about 150m), will cover a larger area. The southern site will also include up to 24 SchwarzschildCouder dual-mirror medium-size Telescopes (SCTs) with the primary mirror diameter of 9.5m. Above a few TeV, the Cherenkov light intensity is such that showers can be detected even well outside the light pool by telescopes significantly smaller than the MSTs. To achieve the required sensitivity at high energies, a huge area on the ground needs to be covered by Small Size Telescopes (SSTs) with a field of view of about 10 and an angular resolution of about 0.2, making the dual-mirror configuration very effective. The SST sub-array will be composed of 5070 telescopes with a mirror area of about 510m2 and about 300m spacing, distributed across an area of about 10km2. In this presentation we will focus on the innovative solution for the optical design of the medium and small size telescopes based on a dual-mirror configuration. This layout will allow us to reduce the dimension and the weight of the camera at the focal plane of the telescope, to adopt Silicon-based photo-multipliers as light detectors thanks to the reduced plate-scale, and to have an optimal imaging resolution on a wide field of view.

S. Vercellone

2014-01-01T23:59:59.000Z

131

GLAST Observatory Renamed for Fermi, Reveals Entire Gamma-Ray Sky |  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

GLAST Observatory Renamed for Fermi, Reveals Entire Gamma-Ray Sky GLAST Observatory Renamed for Fermi, Reveals Entire Gamma-Ray Sky GLAST Observatory Renamed for Fermi, Reveals Entire Gamma-Ray Sky August 26, 2008 - 3:20pm Addthis WASHINGTON, D.C. - The U.S. Department of Energy (DOE) and NASA announced today that the Gamma-Ray Large Area Space Telescope (GLAST) has revealed its first all-sky map in gamma rays. The onboard Large Area Telescope's (LAT) all-sky image-which shows the glowing gas of the Milky Way, blinking pulsars and a flaring galaxy billions of light-years away-was created using only 95 hours of "first light" observations, compared with past missions which took years to produce a similar image. Scientists expect the telescope will discover many new pulsars in our own galaxy, reveal powerful

132

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

SciTech Connect

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.

Abreu, P.; /Lisbon, IST; Aglietta, M.; /Turin U. /INFN, Turin; Ahlers, M.; /Wisconsin U., Madison; Ahn, E.J.; /Fermilab; Albuquerque, I.F.M.; /Sao Paulo U.; Allard, D.; /APC, Paris; Allekotte, I.; /Buenos Aires, CONICET; Allen, J.; /New York U.; Allison, P.; /Ohio State U.; Almela, A.; /Natl. Tech. U., San Nicolas /Buenos Aires, CONICET; Alvarez Castillo, J.; /Mexico U., ICN /Santiago de Compostela U.

2012-01-01T23:59:59.000Z

133

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

E-Print Network (OSTI)

, California, U.S.A.; bNew Jersey Institute of Technology, Newark, New Jersey, U.S.A. ABSTRACT The New SolarDesign 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

134

Introduction: Observatory Techniques in Nineteenth-Century Science and Society David Aubin, Charlotte Bigg, and H. Otto Sibum  

E-Print Network (OSTI)

1 Introduction: Observatory Techniques in Nineteenth-Century Science and Society monument surrounded by delightful gardens, a makeshift camp on a desolate beach, a wooden shack the observatory's multiple roles in nineteenth-century scientific, economic, and cultural life. #12;2 Without

Aubin, David

135

29th International Cosmic Ray Conference Pune (2005) 00, 101106 The Central Laser Facility at the Pierre Auger Observatory  

E-Print Network (OSTI)

is located near the middle of the Pierre Auger Observatory in Argentina. It features a UV laser and optics. 1. Introduction The southern Pierre Auger Observatory in Mendoza Province, Argentina measures measurement of shower energy because the amount of fluorescence light emitted is proportional to the energy

136

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

137

ARC Scientist (5-year non-tenure-track Associate Professor or Assistant Professor), NAOJ Chile Observatory, stationed at Mitaka  

E-Print Network (OSTI)

astronomer and a) conduct the tasks needed for ALMA Science Operations and b) do scientific research using ALMA. The Science Operations tasks conducted by the team include: - Support of preparation of ALMA Observatory, stationed at Mitaka The National Astronomical Observatory of Japan (NAOJ) has been conducting

Ito, Atsushi

138

ARC Scientist (5-year non-tenure-track Associate Professor or Assistant Professor), NAOJ Chile Observatory, stationed at Mitaka)  

E-Print Network (OSTI)

astronomer and a) conduct the tasks needed for ALMA Science Operations and b) do scientific research using ALMA. The Science Operations tasks conducted by the team include: - Support of preparation of ALMA Observatory, stationed at Mitaka) The National Astronomical Observatory of Japan (NAOJ) has been conducting

Ito, Atsushi

139

Robert M. La Follette School of Public Affairs 1225 Observatory Drive, Madison, Wisconsin 53706  

E-Print Network (OSTI)

tax as a way of maintaining the level of public services in light of large cuts in state in which real per capita tax revenue grew during this period were Arkansas, New Hampshire, Louisiana, SouthRobert M. La Follette School of Public Affairs 1225 Observatory Drive, Madison, Wisconsin 53706

Wisconsin at Madison, University of

140

MilagroA TeV Observatory for Gamma Ray Bursts  

E-Print Network (OSTI)

Milagro­A TeV Observatory for Gamma Ray Bursts B.L. Dingus and the Milagro Collaboration Los energy gamma-rays from gamma-ray bursts. The highest energy gamma rays supply very strong constraints on the nature of gamma-ray burst sources as well as fundamental physics. Because the highest energy gamma-rays

California at Santa Cruz, University of

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


141

The Cosmic Web Imager : An integral field spectrograph for the Hale Telescope at Palomar Observatory. Instrument  

E-Print Network (OSTI)

The Cosmic Web Imager : An integral field spectrograph for the Hale Telescope at Palomar for the Hale 200" telescope at the Palomar Observatory. CWI has been built specifically for the observation), and oxygen (OVI 1036°A) to detect and map diffuse gas around and between galaxies and quasars at redshifts 2

Martin, Chris

142

Governors of the Armagh Observatory and Planetarium: Safeguarding Children and Vulnerable Adults Policy and  

E-Print Network (OSTI)

15 Governors of the Armagh Observatory and Planetarium: Safeguarding Children and Vulnerable Adults been drafted by considering law and government policies and procedures on safeguarding. A list has been as being safe and protected from harm. For the purposes of this Safeguarding policy the terms `child

143

Governors of the Armagh Observatory and Planetarium: Safeguarding Children and Vulnerable Adults Policy and  

E-Print Network (OSTI)

15 Governors of the Armagh Observatory and Planetarium: Safeguarding Children and Vulnerable Adults drafted by considering law and government policies and procedures on safeguarding. A list has been as being safe and protected from harm. For the purposes of this Safeguarding policy the terms `child

144

Comment on Hunting long-lived gluinos at the Pierre Auger Observatory  

Science Journals Connector (OSTI)

A Comment on the article by Anchordoqui etal. Hunting long-lived gluinos at the Pierre Auger Observatory [L.?A. Anchordoqui, A. Delgado, C.?A. Garca Canal, and S.?J. Sciutto, Phys. Rev. D 77, 023009 (2008)].

V. Kopenkin; Y. Fujimoto; T. Sinzi

2008-06-17T23:59:59.000Z

145

Tropospheric ozone trends at Mauna Loa Observatory tied to decadal climate variability  

E-Print Network (OSTI)

measurements at Mauna Loa Observatory in Hawaii reveal little change in tropospheric ozone levels during spring a suite of chemistry­climate model simulations. We show that the flow of ozone-rich air from Eurasia towards Hawaii during spring weakened in the 2000s as a result of La-Niña-like decadal cooling

146

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

E-Print Network (OSTI)

The 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 Luther King Blvd, Newark, NJ 07102, US ABSTRACT We present the basic design of the THermal Control System

147

Adaptive Optics at the Big Bear Solar Observatory: Instrument Description and First Observations  

E-Print Network (OSTI)

to the AO system operated at the NSO Dunn Solar Tower (DST) incorporating a 97 actuator deformable mirrorAdaptive Optics at the Big Bear Solar Observatory: Instrument Description and First Observations Carsten Denker New Jersey Institute of Technology, Center for Solar-Terrestrial Research, 323 Martin

148

The Mauna Kea Observatories Near-Infrared Filter Set. III. Isophotal Wavelengths and Absolute Calibration  

E-Print Network (OSTI)

The isophotal wavelengths, flux densities, and AB magnitudes for Vega (alpha Lyr) are presented for the Mauna Kea Observatories near-infrared filter set. We show that the near-infrared absolute calibration for Vega determined by Cohen et al. and Megessier are consistent within the uncertainties, so that either absolute calibration may be used.

A. T. Tokunaga; W. D. Vacca

2005-02-05T23:59:59.000Z

149

Components of an environmental observatory information system Jeffery S. Horsburgh a,n  

E-Print Network (OSTI)

of cyberinfrastructure. In this paper, we describe the architecture and functional requirements for an environmentalComponents of an environmental observatory information system Jeffery S. Horsburgh a,n , David G and Environmental Engineering, Utah State University, Logan, UT, USA b Center for Research in Water Resources

Tarboton, David

150

Historic Sudbury Neutrino Observatory Data, Carried by ESnet, Lives on at  

NLE Websites -- All DOE Office Websites (Extended Search)

Historic Sudbury Historic Sudbury Neutrino Observatory Data, Carried by ESnet, Lives on at NERSC Historic Sudbury Neutrino Observatory Data, Carried by ESnet, Lives on at NERSC January 26, 2010 | Tags: Astrophysics Contact: Linda Vu, lvu@lbl.gov, +1 510 486 2402 SNO.jpg SNO onsists of an 18-meters-in-diameter stainless steel geodesic sphere inside of which is an acrylic vessel filled with 1000 tons of heavy water (deuterium oxide or D2O). Attached to the sphere are 9,522 ultra-sensitive light-sensors called photomultiplier tubes. When neutrinos passing through the heavy water interact with deuterium nuclei, flashes of light are emitted. The photomultiplier tubes detect these light flashes and convert them into electronic signals that scientists can analyze for the presence

151

CCD and photon-counting photometric observations of asteroids carried out at Padova and Catania observatories  

E-Print Network (OSTI)

We present the results of observational campaigns of asteroids performed at Asiago Station of Padova Astronomical Observatory and at M.G. Fracastoro Station of Catania Astrophysical Observatory, as part of the large research programme on Solar System minor bodies undertaken since 1979 at the Physics and Astronomy Department of Catania University. Photometric observations of six Main-Belt asteroids (27 Euterpe, 173 Ino, 182 Elsa, 539 Pamina, 849 Ara, and 984 Gretia), one Hungaria (1727 Mette), and two Near-Earth Objects (3199 Nefertiti and 2004 UE) are reported. The first determination of the synodic rotational period of 2004 UE was obtained. For 182 Elsa and 1727 Mette the derived synodic period of 80.23+/-0.08 h and 2.981+/-0.001 h, respectively, represents a significant improvement on the previously published values. For 182 Elsa the first determination of the H-G magnitude relation is also presented.

Davide Gandolfi; Massimo Cigna; Daniele Fulvio; Carlo Blanco

2008-10-09T23:59:59.000Z

152

An Advanced Analysis Technique for Transient Searches in Wide-Field Gamma-Ray Observatories  

E-Print Network (OSTI)

Wide-field gamma-ray telescopes typically have highly variable event-by-event resolution which leads to a number of unique and challenging analysis requirements -- particularly when conducting transient searches over multiple time scales. By generalizing the ideas of the Gaussian weighting analysis to point-spread functions of arbitrary shape and the regime of Poisson statistics, an efficient analysis which uses the event-by-event resolution is developed with a sensitivity similar to that of a well-implemented maximum likelihood analysis. In this development, the effect of a number of different approximations on the sensitivity and speed of the final analysis can be easily determined and tuned to the particular application. The analysis method is particularly well suited to transient detection in wide field-of-view gamma-ray observatories, and is currently used for the 40 s -- 3 hour transient search in the Milagro observatory.

M. F. Morales; D. A. Williams; T. DeYoung

2003-07-15T23:59:59.000Z

153

Low-energy-threshold analysis of the Phase I and Phase II data sets of the Sudbury Neutrino Observatory  

E-Print Network (OSTI)

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 Teff=3.5 MeV, the lowest analysis threshold yet achieved ...

Monroe, Jocelyn

154

Grand Observatories and multiple-OWL for high energy neutrino astrophysics  

Science Journals Connector (OSTI)

A possible Space Factory on the International Space Station (ISS) for Grand Observatories would permit a large astrophysical observatory in space. Grand-Observatories could revolutionize the great observatories that were hitherto pre-assembled and deployed by the Space Transportation System (STS). The concept of the ISS-Space-Factory envisages a plan of orbital construction fine-tuning and deployment of large-scale astrophysical instruments into the desired free-flying orbit. It incorporates physical aids of the robotics arms and Extra-Vehicular Activities (EVA) of astronauts. This concept study also examines the necessary infrastructure on ISS for manufacturing a large spaceship for future deployment to the Moon Mars and other interplanetary destinations. We envision a step-by-step advancement of the Space Factory with the most frontier astrophysical programs. Less demanding experiments could precede the construction of the most demanding optical telescopes. Multiple-OWL (Orbiting-array of Wide-angle Light collector) has very forgiving optical resolution (?0.1 degrees) and would be suitable for the first generation payload to be built on and deployed from the ISS. This system is an earths night-sky-watcher for observing the highest energy cosmic rays and other atmospheric phenomena and is currently in the SEU Explorer Concept. Using the Space Factory this collector can drastically advance its capacity to cover a 120 Field-of-View (FOV) in which the entire horizon of the earth (?6000 km diameter) can be viewed from a low-earth orbit (?1000 km). We have already developed a revolutionary wide-angle Fresnel-lens optic in the OWL program and the Multiple-OWL can use several units of them. As one of the Grand Observatories the proposed Multiple-OWL satellite can open a new window for observational universe in terms of high energy neutrino astrophysics. The OWL may also be used for monitoring earth-threatening meteorites if flipped on orbit at daytime for deep space observation.

Yoshiyuki Takahashi; John O. Dimmock; Lloyd W. Hillman; James B. Hadaway; David J. Lamb; Mamoru Mohri; Toshikazu Ebisuzaki

1999-01-01T23:59:59.000Z

155

OBSERVATORY OPPORTUNITIES  

E-Print Network (OSTI)

solar system objects, as well as distant stars, black holes, galaxies, quasars, and other mysterious observations are recorded at each 25 m antenna and combined electronically at a central processing facility at a meeting of the American Astronomical Society. Besides their research, students take part in other

Groppi, Christopher

156

The Chicagoland Observatory Underground for Particle Physics cosmic ray veto system  

SciTech Connect

A photomultiplier (PMT) readout system has been designed for use by the cosmic ray veto systems of two warm liquid bubble chambers built at Fermilab by the Chicagoland Observatory Underground for Particle Physics (COUPP) collaboration. The systems are designed to minimize the infrastructure necessary for installation. Up to five PMTs can be daisy-chained on a single data link using standard Category 5 network cable. The cables is also serve distribute to low voltage power. High voltage is generated locally on each PMT base. Analog and digital signal processing is also performed locally. The PMT base and system controller design and performance measurements are presented.

Crisler, M.; Hall, J.; Ramberg, E.; Kiper, T.; /Fermilab

2010-11-01T23:59:59.000Z

157

The gamma?ray burst capabilities of BATSE and the Gamma Ray Observatory  

Science Journals Connector (OSTI)

The Gamma Ray Observatory (GRO) scheduled for launch in 1990 will provide new and enhanced capabilities for the study of gamma?ray bursts. These include higher sensitivity increased time resolution broader energy coverage rapid burst data dissemination and burst location by a single spacecraft. All four of the GRO instruments have burst capabilities however the Burst and Transient Source Experiment (BATSE) is designed primarily for the study of gamma?ray bursts. The capabilities of BATSE and the GRO for gamma?ray burst studies are described.

G. J. Fishman

1988-01-01T23:59:59.000Z

158

Constraints and measurements of hadronic interactions in extensive air showers with the Pierre Auger Observatory  

E-Print Network (OSTI)

The characteristics of extensive air showers are sensitive to the details of hadronic interactions at energies and in kinematic regions beyond those tested by human-made accelerators. Uncertainties on extrapolations of the hadronic interaction models in these regions hamper the interpretation of the ultra high energy cosmic ray data in terms of primary mass composition. We report on how the Pierre Auger Observatory is able to constrain the hadronic interaction models by measuring the muon content and muon production depth of air showers and also by measuring the proton-air cross section for particle production at a center-of-mass energy per nucleon of 57 TeV.

L. Cazon

2014-05-20T23:59:59.000Z

159

Inverse diffraction for the Atmospheric Imaging Assembly in the Solar Dynamics Observatory  

E-Print Network (OSTI)

The Atmospheric Imaging Assembly in the Solar Dynamics Observatory provides full Sun images every 1 seconds in each of 7 Extreme Ultraviolet passbands. However, for a significant amount of these images, saturation affects their most intense core, preventing scientists from a full exploitation of their physical meaning. In this paper we describe a mathematical and automatic procedure for the recovery of information in the primary saturation region based on a correlation/inversion analysis of the diffraction pattern associated to the telescope observations. Further, we suggest an interpolation-based method for determining the image background that allows the recovery of information also in the region of secondary saturation (blooming).

Torre, Gabriele; Benvenuto, Federico; Massone, Anna Maria; Piana, Michele

2015-01-01T23:59:59.000Z

160

Calibration of Muon Reconstruction Algorithms Using an External Muon Tracking System at the Sudbury Neutrino Observatory  

E-Print Network (OSTI)

To help constrain the algorithms used in reconstructing high-energy muon events incident on the Sudbury Neutrino Observatory (SNO), a muon tracking system was installed. The system consisted of four planes of wire chambers, which were triggered by scintillator panels. The system was integrated with SNO's main data acquisition system and took data for a total of 95 live days. Using cosmic-ray events reconstructed in both the wire chambers and in SNO's water Cherenkov detector, the external muon tracking system was able to constrain the uncertainty on the muon direction to better than 0.6 degrees.

SNO Collaboration

2011-05-06T23:59:59.000Z

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


161

Constraints and measurements of hadronic interactions in extensive air showers with the Pierre Auger Observatory  

E-Print Network (OSTI)

The characteristics of extensive air showers are sensitive to the details of hadronic interactions at energies and in kinematic regions beyond those tested by human-made accelerators. Uncertainties on extrapolations of the hadronic interaction models in these regions hamper the interpretation of the ultra high energy cosmic ray data in terms of primary mass composition. We report on how the Pierre Auger Observatory is able to constrain the hadronic interaction models by measuring the muon content and muon production depth of air showers and also by measuring the proton-air cross section for particle production at a center-of-mass energy per nucleon of 57 TeV.

,

2014-01-01T23:59:59.000Z

162

Constraints on Nucleon Decay via Invisible Modes from the Sudbury Neutrino Observatory  

Science Journals Connector (OSTI)

Data from the Sudbury Neutrino Observatory have been used to constrain the lifetime for nucleon decay to invisible modes, such as n?3?. The analysis was based on a search for ?rays from the deexcitation of the residual nucleus that would result from the disappearance of either a proton or neutron from O16. A limit of ?inv>21029??yr is obtained at 90% confidence for either neutron- or proton-decay modes. This is about an order of magnitude more stringent than previous constraints on invisible proton-decay modes and 400times more stringent than similar neutron modes.

S. N. Ahmed et al. (SNO Collaboration)

2004-03-10T23:59:59.000Z

163

Proposal for a quantity based data model in the Virtual Observatory  

E-Print Network (OSTI)

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.

Brian Thomas; Edward Shaya

2003-12-23T23:59:59.000Z

164

Optimization of the design of OMNIS, the observatory of multiflavor neutrinos from supernovae  

E-Print Network (OSTI)

A Monte Carlo code has been developed to simulate the operation of the planned detectors in OMNIS, a supernova neutrino observatory. OMNIS will detect neutrinos originating from a core collapse supernova by the detection of spalled neutrons from Pb- or Fe-nuclei. This might be accomplished using Gd-loaded liquid scintillator. Results for the optimum configuration for such modules with respect to both neutron detection efficiency and cost efficiency are presented. Careful consideration has been given to the expected levels of radioactive backgrounds and their effects. The results show that the amount of data to be processed by a software trigger can be reduced to the 30%.

J. J. Zach; A. StJ. Murphy; D. Marriott; R. N. Boyd

2002-05-17T23:59:59.000Z

165

Interpretation of the depths of maximum of extensive air showers measured by the Pierre Auger Observatory  

SciTech Connect

To interpret the mean depth of cosmic ray air shower maximum and its dispersion, we parametrize those two observables as functions of the first two moments of the ln A distribution. We examine the goodness of this simple method through simulations of test mass distributions. The application of the parameterization to Pierre Auger Observatory data allows one to study the energy dependence of the mean ln A and of its variance under the assumption of selected hadronic interaction models. We discuss possible implications of these dependences in term of interaction models and astrophysical cosmic ray sources.

Collaboration: Pierre Auger Collaboration

2013-02-01T23:59:59.000Z

166

Radio detection of high-energy cosmic rays at the Pierre Auger Observatory  

E-Print Network (OSTI)

The southern Auger Observatory provides an excellent test bed to study the radio detection of extensive air showers as an alternative, cost-effective, and accurate tool for cosmic-ray physics. The data from the radio setup can be correlated with those from the well-calibrated baseline detectors of the Pierre Auger Observatory. Furthermore, human-induced radio noise levels at the southern Auger site are relatively low. We have started an R&D program to test various radio-detection concepts. Our studies will reveal Radio Frequency Interferences (RFI) caused by natural effects such as day-night variations, thunderstorms, and by human-made disturbances. These RFI studies are conducted to optimise detection parameters such as antenna design, frequency interval, antenna spacing and signal processing. The data from our initial setups, which presently consist of typically 3 - 4 antennas, will be used to characterise the shower from radio signals and to optimise the initial concepts. Furthermore, the operation of a large detection array requires autonomous detector stations. The current design is aiming at stations with antennas for two polarisations, solar power, wireless communication, and local trigger logic. The results of this initial phase will provide an important stepping stone for the design of a few tens kilometers square engineering array

A. M. van den Berg; for the Pierre Auger Collaboration

2007-08-13T23:59:59.000Z

167

Atmospheric Calorimetry above 10$^{19}$ eV: Shooting Lasers at the Pierre Auger Cosmic-Ray Observatory  

E-Print Network (OSTI)

The Pierre Auger Cosmic-Ray Observatory uses the earth's atmosphere as a calorimeter to measure extensive air-showers created by particles of astrophysical origin. Some of these particles carry joules of energy. At these extreme energies, test beams are not available in the conventional sense. Yet understanding the energy response of the observatory is important. For example, the propagation distance of the highest energy cosmic-rays through the cosmic microwave background radiation (CMBR) is predicted to be strong function of energy. This paper will discuss recently reported results from the observatory and the use of calibrated pulsed UV laser "test-beams" that simulate the optical signatures of ultra-high energy cosmic rays. The status of the much larger 200,000 km$^3$ companion detector planned for the northern hemisphere will also be outlined.

L. Wiencke; for the Pierre Auger Collaboration

2008-07-17T23:59:59.000Z

168

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)

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 #12;The National Radio Astronomy Observatory is a facility of the National Science Foundation

Groppi, Christopher

169

The Natural satellite database of the Main Astronomical Observa-tory of the National Academy of Sciences of Ukraine. An overview  

E-Print Network (OSTI)

of Sciences of Ukraine. An overview Irina Kulyk, Yelena Yizhakevych, Lyudmila Pakuliak Main Astronomical Observatory NASU, Kyiv, Ukraine, irinakulyk@yahoo.com Introduction The dynamical studies and development-1990) at the Main Astronomical Observatory of the National Academy of Sciences of Ukraine (Golosiiv) led

Paris-Sud XI, Université de

170

Muons in air showers at the Pierre Auger Observatory: Measurement of atmospheric production depth  

E-Print Network (OSTI)

The surface detector array of the Pierre Auger Observatory provides information about the longitudinal development of the muonic component of extensive air showers. Using the timing information from the flash analog-to-digital converter traces of surface detectors far from the shower core, it is possible to reconstruct a muon production depth distribution. We characterize the goodness of this reconstruction for zenith angles around 60 deg. and different energies of the primary particle. From these distributions we define X(mu)max as the depth along the shower axis where the production of muons reaches maximum. We explore the potentiality of X(mu)max as a useful observable to infer the mass composition of ultrahigh-energy cosmic rays. Likewise, we assess its ability to constrain hadronic interaction models.

Pierre Auger Collaboration

2014-07-22T23:59:59.000Z

171

Telescope Array Radar (TARA) observatory for Ultra-High Energy Cosmic Rays  

Science Journals Connector (OSTI)

Abstract 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 8MW Effective Radiated Power (ERP) VHF transmitter and smart receiver system based on a 250MS/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.

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

2014-01-01T23:59:59.000Z

172

Search for periodicities in the B8 solar neutrino flux measured by the Sudbury Neutrino Observatory  

Science Journals Connector (OSTI)

A search has been made for sinusoidal periodic variations in the B8 solar neutrino flux using data collected by the Sudbury Neutrino Observatory over a 4-year time interval. The variation at a period of 1yr is consistent with modulation of the B8 neutrino flux by the Earths orbital eccentricity. No significant sinusoidal periodicities are found with periods between 1d and 10 years with either an unbinned maximum likelihood analysis or a Lomb-Scargle periodogram analysis. The data are inconsistent with the hypothesis that the results of the recent analysis by Sturrock et al., based on elastic scattering events in Super-Kamiokande, can be attributed to a 7% sinusoidal modulation of the total B8 neutrino flux.

B. Aharmim et al. (SNO Collaboration)

2005-09-30T23:59:59.000Z

173

Using ACIS on the Chandra X-ray Observatory as a particle radiation monitor  

E-Print Network (OSTI)

The Advanced CCD Imaging Spectrometer (ACIS) is one of two focal-plane instruments on the Chandra X-ray Observatory. During initial radiation-belt passes, the exposed ACIS suffered significant radiation damage from trapped soft protons scattering off the x-ray telescope's mirrors. The primary effect of this damage was to increase the charge-transfer inefficiency (CTI) of the ACIS 8 front-illuminated CCDs. Subsequently, the Chandra team implemented procedures to remove the ACIS from the telescope's focus during high-radiation events: planned protection during radiation-belt transits; autonomous protection triggered by an on-board radiation monitor; and manual intervention based upon assessment of space-weather conditions. However, as Chandra's multilayer insulation ages, elevated temperatures have reduced the effectiveness of the on-board radiation monitor for autonomous protection. Here we investigate using the ACIS CCDs themselves as a radiation monitor. We explore the 10-year database to evaluate the CCDs' ...

Grant, C E; Bautz, M W; O'Dell, S L

2010-01-01T23:59:59.000Z

174

Energy Department Announces Up to $31 Million for Initial Phases of Enhanced Geothermal Systems Field Observatory  

Office of Energy Efficiency and Renewable Energy (EERE)

As part of the Administrations all-of-the-above energy strategy, the Energy Department today announced up to $31 million to establish the initial phases of the Frontier Observatory for Research in Geothermal Energy (FORGE), a field laboratory dedicated to cutting-edge research on enhanced geothermal systems (EGS). EGS are engineered reservoirs, created beneath the surface of the Earth, where there is hot rock but limited pathways through which fluid can flow. During EGS development, underground fluid pathways are safely created and their size and connectivity increased. These enhanced pathways allow fluid to circulate throughout the hot rock and carry heat to the surface to generate electricity. In the long term, EGS may enable domestic access to a geographically diverse baseload, and carbon-free energy resource on the order of 100 gigawatts, or enough to power about 100 million homes.

175

The X-Ray Microcalorimeter Spectrometer for the International X-Ray Observatory  

SciTech Connect

The International X-Ray Observatory (IXO) is under formulation by NASA, ESA and JAXA for deployment in 2022. IXO emerged over the last 18 months as the NASA Constellation-X and ESA/JAXA X-Ray Evolving Universe Spectrometer (XEUS) missions were combined. The driving performance requirements for the X-Ray Microcalorimeter Spectrometer (XMS) are a spectral resolution of 2.5 eV over the central 2'x2' in the 0.3-7.0 keV band, and 10 eV to the edge of the 5'x5' field of view (FOV). The XMS is now based on a microcalorimeter array of Transition-Edge Sensor (TES) thermometers with Au/Bi absorbers and a SQUID MUX readout. One of the concepts studied as part of the mission formulation has a core 40x40 array corresponding to a 2'x2' FOV with 3'' pixels surrounded by an outer, annular 52x52 array of 6'' pixels that extends the field of view to 5.4'x5.4' with better than 10 eV resolution. There are several options for implementing the readout and cooling system of the XMS under study in the US, Europe and Japan. The ADR system will have from two to five stages depending on the performance of the cryocooler. Mechanical coolers with sufficient cooling power at 4K are available now, and {approx}2K coolers are under development. In this paper we give an overview of the XMS instrument, and some of the tradeoffs to be addressed for this observatory instrument.

Kelley, R. L.; Bandler, S. R.; Kilbourne, C. A.; Porter, F. S.; Shirron, P.; Smith, S. J.; Whitehouse, P. [NASA/Goddard Space Flight Center, Greenbelt, MD (United States); Doriese, W. B.; Irwin, K. [National Institute of Standards and Technology, Boulder, CO (United States); Ezoe, Y.; Ishisaki, Y.; Ohashi, T. [Tokyo Metropolitan University, Hachioji, Tokyo (Japan); Fujimoto, R.; Sato, K. [Faculty of Mathematics and Physics, Kanazawa University, Kanazawa (Japan); Gottardi, L.; Hartog, R. den; Herder, J.-W. den; Hoevers, H.; Korte, P. de; Kuur, J. van der [SRON Netherlands Institute for Space Research, Utrecht (Netherlands)] (and others)

2009-12-16T23:59:59.000Z

176

Institute for Astronomy The Royal Observatory Edinburgh comprises the UK Astronomy Technology Centre of the Science and Technology  

E-Print Network (OSTI)

Institute for Astronomy The Royal Observatory Edinburgh comprises the UK Astronomy Technology Centre of the Science and Technology Facilities Council, the Institute for Astronomy of the University of Edinburgh and the ROE Visitor Centre. Undergraduate study at the IfA The Institute for Astronomy (If

Tittley, Eric

177

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

E-Print Network (OSTI)

Observatorio Pierre Auger, Av. San Martin Norte 304, 5613 Malarg¨ue, Argentina 3 Karlsruhe Institute and as a function of height in the atmosphere where high energy air showers develop. The data have been recorded Observatory location in Argentina to effect a major upgrade of the central laser facility. Keywords

178

CONTROL ID: 974053 TITLE: A Virtual Ocean Observatory for Climate and Ocean Science: Synergistic Applications for SWOT  

E-Print Network (OSTI)

measurements, that are important to the modeling of ocean currents, eddies and mixing. INDEX TERMS: [1910Proof CONTROL ID: 974053 TITLE: A Virtual Ocean Observatory for Climate and Ocean Science: Synergistic Applications for SWOT and XOVWM PRESENTATION TYPE: Assigned by Committee (Oral or Poster) CURRENT

Arabshahi, Payman

179

First Light of the 1.6 meter off-axis New Solar Telescope at Big Bear Solar Observatory  

E-Print Network (OSTI)

First Light of the 1.6 meter off-axis New Solar Telescope at Big Bear Solar Observatory Wenda Caoab, Nicolas Gorceixb, Roy Coulterb, Aaron Coulterb, Philip R. Goodeab aCenter for Solar-Terrestrial Research, New Jersey Institute of Technology, 323 Martin Luther King Blvd., Newark, NJ 07102; bBig Bear Solar

180

TARGET SELECTION FOR THE APACHE POINT OBSERVATORY GALACTIC EVOLUTION EXPERIMENT (APOGEE)  

SciTech Connect

The Apache Point Observatory Galactic Evolution Experiment (APOGEE) is a high-resolution infrared spectroscopic survey spanning all Galactic environments (i.e., bulge, disk, and halo), with the principal goal of constraining dynamical and chemical evolution models of the Milky Way. APOGEE takes advantage of the reduced effects of extinction at infrared wavelengths to observe the inner Galaxy and bulge at an unprecedented level of detail. The survey's broad spatial and wavelength coverage enables users of APOGEE data to address numerous Galactic structure and stellar populations issues. In this paper we describe the APOGEE targeting scheme and document its various target classes to provide the necessary background and reference information to analyze samples of APOGEE data with awareness of the imposed selection criteria and resulting sample properties. APOGEE's primary sample consists of {approx}10{sup 5} red giant stars, selected to minimize observational biases in age and metallicity. We present the methodology and considerations that drive the selection of this sample and evaluate the accuracy, efficiency, and caveats of the selection and sampling algorithms. We also describe additional target classes that contribute to the APOGEE sample, including numerous ancillary science programs, and we outline the targeting data that will be included in the public data releases.

Zasowski, G.; Johnson, Jennifer A.; Andrews, B.; Epstein, C. [Department of Astronomy, Ohio State University, Columbus, OH 43210 (United States); Frinchaboy, P. M.; Jackson, K. [Department of Physics and Astronomy, Texas Christian University, Fort Worth, TX 76129 (United States); Majewski, S. R.; Chojnowski, S. D.; Skrutskie, M. F.; Beaton, R. L. [Department of Astronomy, University of Virginia, Charlottesville, VA 22904 (United States); Nidever, D. L. [Department of Astronomy, University of Michigan, Ann Arbor, MI 48109 (United States); Pinto, H. J. Rocha; Girardi, L. [Laboratorio Interinstitucional de e-Astronomia-LIneA, Rio de Janeiro, RJ 20921-400 (Brazil); Cudworth, K. M. [Yerkes Observatory, University of Chicago, Williams Bay, WI 53191 (United States); Munn, J. [US Naval Observatory, Flagstaff Station, Flagstaff, AZ 86001 (United States); Blake, C. H. [Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544 (United States); Covey, K. [Lowell Observatory, Flagstaff, AZ 86001 (United States); Deshpande, R.; Fleming, S. W. [Department of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802 (United States); Fabbian, D., E-mail: gail.zasowski@gmail.com [Instituto de Astrofisica de Canarias, Calle Via Lactea s/n, E-38205 La Laguna, Tenerife (Spain); and others

2013-10-01T23:59:59.000Z

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181

LIMITS ON THE STOCHASTIC GRAVITATIONAL WAVE BACKGROUND FROM THE NORTH AMERICAN NANOHERTZ OBSERVATORY FOR GRAVITATIONAL WAVES  

SciTech Connect

We present an analysis of high-precision pulsar timing data taken as part of the North American Nanohertz Observatory for Gravitational Waves (NANOGrav) project. We have observed 17 pulsars for a span of roughly five years using the Green Bank and Arecibo radio telescopes. We analyze these data using standard pulsar timing models, with the addition of time-variable dispersion measure and frequency-variable pulse shape terms. Sub-microsecond timing residuals are obtained in nearly all cases, and the best rms timing residuals in this set are {approx}30-50 ns. We present methods for analyzing post-fit timing residuals for the presence of a gravitational wave signal with a specified spectral shape. These optimally take into account the timing fluctuation power removed by the model fit, and can be applied to either data from a single pulsar, or to a set of pulsars to detect a correlated signal. We apply these methods to our data set to set an upper limit on the strength of the nHz-frequency stochastic supermassive black hole gravitational wave background of h{sub c} (1 yr{sup -1}) < 7 Multiplication-Sign 10{sup -15} (95%). This result is dominated by the timing of the two best pulsars in the set, PSRs J1713+0747 and J1909-3744.

Demorest, P. B.; Ransom, S. [National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903 (United States)] [National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903 (United States); Ferdman, R. D.; Kaspi, V. M. [Department of Physics, McGill University, 3600 rue Universite, Montreal, QC H3A 2T8 (Canada)] [Department of Physics, McGill University, 3600 rue Universite, Montreal, QC H3A 2T8 (Canada); Gonzalez, M. E.; Stairs, I. H. [Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1 (Canada)] [Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1 (Canada); Nice, D. [Department of Physics, Lafayette College, Easton, PA 18042 (United States)] [Department of Physics, Lafayette College, Easton, PA 18042 (United States); Arzoumanian, Z. [Center for Research and Exploration in Space Science and Technology and X-Ray Astrophysics Laboratory, NASA Goddard Space Flight Center, Code 662, Greenbelt, MD 20771 (United States)] [Center for Research and Exploration in Space Science and Technology and X-Ray Astrophysics Laboratory, NASA Goddard Space Flight Center, Code 662, Greenbelt, MD 20771 (United States); Brazier, A.; Cordes, J. M. [Department of Astronomy, Cornell University, Ithaca, NY 14853 (United States)] [Department of Astronomy, Cornell University, Ithaca, NY 14853 (United States); Burke-Spolaor, S.; Lazio, J. [Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91106 (United States)] [Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91106 (United States); Chamberlin, S. J.; Ellis, J.; Giampanis, S. [Center for Gravitation, Cosmology and Astrophysics, Department of Physics, University of Wisconsin-Milwaukee, P.O. Box 413, Milwaukee, WI 53201 (United States)] [Center for Gravitation, Cosmology and Astrophysics, Department of Physics, University of Wisconsin-Milwaukee, P.O. Box 413, Milwaukee, WI 53201 (United States); Finn, L. S. [Department of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802 (United States)] [Department of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802 (United States); Freire, P. [Max-Planck-Institut fur Radioastronomie, D-53121 Bonn (Germany)] [Max-Planck-Institut fur Radioastronomie, D-53121 Bonn (Germany); Jenet, F. [Center for Gravitational Wave Astronomy, University of Texas at Brownsville, Brownsville, TX 78520 (United States)] [Center for Gravitational Wave Astronomy, University of Texas at Brownsville, Brownsville, TX 78520 (United States); Lommen, A. N. [Department of Physics and Astronomy, Franklin and Marshall College, P.O. Box 3003, Lancaster, PA 17604 (United States)] [Department of Physics and Astronomy, Franklin and Marshall College, P.O. Box 3003, Lancaster, PA 17604 (United States); McLaughlin, M. [Department of Physics, West Virginia University, P.O. Box 6315, Morgantown, WV 26505 (United States)] [Department of Physics, West Virginia University, P.O. Box 6315, Morgantown, WV 26505 (United States); and others

2013-01-10T23:59:59.000Z

182

Coronal Magnetic Field Measurement from EUV Images made by the Solar Dynamics Observatory  

E-Print Network (OSTI)

By measuring the geometrical properties of the coronal mass ejection (CME) flux rope and the leading shock observed on 2010 June 13 by the Solar Dynamics Observatory (SDO) mission's Atmospheric Imaging Assembly (AIA) we determine the Alfv\\'en speed and the magnetic field strength in the inner corona at a heliocentric distance of ~ 1.4 Rs. The basic measurements are the shock standoff distance (deltaR) ahead of the CME flux rope, the radius of curvature of the flux rope (Rc), and the shock speed. We first derive the Alfv\\'enic Mach number (M) using the relationship, deltaR/Rc = 0.81[(gamma-1) M^2 + 2]/[(gamma+1)(M^2-1)], where gamma is the only parameter that needed to be assumed. For gamma =4/3, the Mach number declined from 3.7 to 1.5 indicating shock weakening within the field of view of the imager. The shock formation coincided with the appearance of a type II radio burst at a frequency of ~300 MHz (harmonic component), providing an independent confirmation of the shock. The shock compression ratio derived...

Gopalswamy, Nat; Akiyama, Sachiko; Mkel, Pertti; Yashiro, Seiji

2011-01-01T23:59:59.000Z

183

New superconducting toroidal magnet system for IAXO, the international AXion observatory  

SciTech Connect

Axions are hypothetical particles that were postulated to solve one of the puzzles arising in the standard model of particle physics, namely the strong CP (Charge conjugation and Parity) problem. The new International AXion Observatory (IAXO) will incorporate the most promising solar axions detector to date, which is designed to enhance the sensitivity to the axion-photon coupling by one order of magnitude beyond the limits of the current state-of-the-art detector, the CERN Axion Solar Telescope (CAST). The IAXO detector relies on a high-magnetic field distributed over a very large volume to convert solar axions into X-ray photons. Inspired by the successful realization of the ATLAS barrel and end-cap toroids, a very large superconducting toroid is currently designed at CERN to provide the required magnetic field. This toroid will comprise eight, one meter wide and twenty one meter long, racetrack coils. The system is sized 5.2 m in diameter and 25 m in length. Its peak magnetic field is 5.4 T with a stored energy of 500 MJ. The magnetic field optimization process to arrive at maximum detector yield is described. In addition, materials selection and their structure and sizing has been determined by force and stress calculations. Thermal loads are estimated to size the necessary cryogenic power and the concept of a forced flow supercritical helium based cryogenic system is given. A quench simulation confirmed the quench protection scheme.

Shilon, I.; Dudarev, A.; Silva, H.; Wagner, U.; Kate, H. H. J. ten [European Organization for Nuclear Research (CERN), CH-1211, Genve 23 (Switzerland)

2014-01-29T23:59:59.000Z

184

An array of low-background 3He proportional counters for theSudbury Neutrino Observatory  

SciTech Connect

An array of Neutral-Current Detectors (NCDs) has been builtin order to make a unique measurement of the total active ux of solarneutrinos in the Sudbury Neutrino Observatory (SNO). Data in the thirdphase of the SNO experiment were collected between November 2004 andNovember 2006, after the NCD array was added to improve theneutral-current sensitivity of the SNO detector. This array consisted of36 strings of proportional counters lled with a mixture of 3He and CF4gas capable of detecting the neutrons liberated by the neutrino-deuteronneutral current reaction in the D2O, and four strings lled with a mixtureof 4He and CF4 gas for background measurements. The proportional counterdiameter is 5 cm. The total deployed array length was 398 m. The SNO NCDarray is the lowest-radioactivity large array of proportional countersever produced. This article describes the design, construction,deployment, and characterization of the NCD array, discusses theelectronics and data acquisition system, and considers event signaturesand backgrounds.

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

2007-02-01T23:59:59.000Z

185

A Coronal Hole Jet Observed with Hinode and the Solar Dynamics Observatory  

E-Print Network (OSTI)

A small blowout jet was observed at the boundary of the south coronal hole on 2011 February 8 at around 21:00 UT. Images from the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO) revealed an expanding loop rising from one footpoint of a compact, bipolar bright point. Magnetograms from the Helioseismic Magnetic Imager (HMI) on board SDO showed that the jet was triggered by the cancelation of a parasitic positive polarity feature near the negative pole of the bright point. The jet emission was present for 25 mins and it extended 30 Mm from the bright point. Spectra from the EUV Imaging Spectrometer on board Hinode yielded a temperature and density of 1.6 MK and 0.9-1.7 x 10^8 cm^-3 for the ejected plasma. Line-of-sight velocities reached up to 250 km/s. The density of the bright point was 7.6 x 10^8 cm^-3, and the peak of the bright point's emission measure occurred at 1.3 MK, with no plasma above 3 MK.

Young, Peter R

2014-01-01T23:59:59.000Z

186

Midlatitude Cirrus Clouds and Multiple Tropopauses from a 2002-2006 Climatology over the SIRTA Observatory  

E-Print Network (OSTI)

This study present a comparison of lidar observations of midlatitude cirrus clouds over the SIRTA observatory between 2002 and 2006 with multiple tropopauses (MT) retrieved from radiosounding temperature profiles. The temporal variability of MT properties (frequency, thickness) are discussed. Results show a marked annual cycle, with MT frequency reaching its lowest point in May (~18% occurrence of MT) and slowly rising to more than 40% in DJF. The average thickness of the MT also follows an annual cycle, going from less than 1 km in spring to 1.5 km in late autumn. Comparison with lidar observations show that cirrus clouds show a preference for being located close below the 1st tropopause. When the cloud top is above the 1st tropopause (7% of observations), in 20% of cases the cloud base is above it as well, resulting in a cirrus cloud "sandwiched" between the two tropopauses. Compared to the general distribution of cirrus, cross-tropopause cirrus show a higher frequency of large optical depths, while inter-t...

Noel, Vincent

2007-01-01T23:59:59.000Z

187

OH/IR stars and their superwinds as observed by the Herschel Space Observatory  

E-Print Network (OSTI)

Aim : In order to study the history of mass loss in extreme OH/IR stars, we observed a number of these objects using CO as a tracer of the density and temperature structure of their circumstellar envelopes. Method : Combining CO observations from the Herschel Space Observatory with those from the ground, we trace mass loss rates as a function of radius in five extreme OH/IR stars. Using radiative transfer modelling, we modelled the dusty envelope as well as the CO emission. The high-rotational transitions of CO indicate that they originate in a dense superwind region close to the star while the lower transitions tend to come from a more tenuous outer wind which is a result of the mass loss since the early AGB phase. Result : The models of the circumstellar envelopes around these stars suggest that they have entered a superwind phase in the past 200 - 500 years. The low 18O/17O (~ 0.1 compared to the solar abundance ratio of ~ 5) and 12C/13C (3-30 cf. the solar value of 89) ratios derived from our study suppor...

Justtanont, K; Barlow, M J; Matsuura, M; Swinyard, B; Waters, L B F M; Yates, J

2013-01-01T23:59:59.000Z

188

Depth of Maximum of Air-Shower Profiles at the Pierre Auger Observatory: Composition Implications  

E-Print Network (OSTI)

Using the data taken at the Pierre Auger Observatory between December 2004 and December 2012, we have examined the implications of the distributions of depths of atmospheric shower maximum (Xmax), using a hybrid technique, for composition and hadronic interaction models. We do this by fitting the distributions with predictions from a variety of hadronic interaction models for variations in the composition of the primary cosmic rays and examining the quality of the fit. Regardless of what interaction model is assumed, we find that our data are not well described by a mix of protons and iron nuclei over most of the energy range. Acceptable fits can be obtained when intermediate masses are included, and when this is done consistent results for the proton and iron-nuclei contributions can be found using the available models. We observe a strong energy dependence of the resulting proton fractions, and find no support from any of the models for a significant contribution from iron nuclei. However, we also observe a...

,

2014-01-01T23:59:59.000Z

189

Effects of mode degeneracy in the LIGO Livingston Observatory recycling cavity  

E-Print Network (OSTI)

We analyze the electromagnetic fields in a Pound-Drever-Hall locked, marginally unstable, Fabry-Perot cavity as a function of small changes in the cavity length during resonance. More specifically, we compare the results of a detailed numerical model with the behavior of the recycling cavity of the Laser Interferometer Gravitational-wave Observatory (LIGO) detector that is located in Livingston, Louisiana. In the interferometer's normal mode of operation, the recycling cavity is stabilized by inducing a thermal lens in the cavity mirrors with an external CO2 laser. During the study described here, this thermal compensation system was not operating, causing the cavity to be marginally optically unstable and cavity modes to become degenerate. In contrast to stable optical cavities, the modal content of the resonating beam in the uncompensated recycling cavity is significantly altered by very small cavity length changes. This modifies the error signals used to control the cavity length in such a way that the zero crossing point is no longer the point of maximum power in the cavity nor is it the point where the input beam mode in the cavity is maximized.

Andri M. Gretarsson; Erika D'Ambrosio; Valery Frolov; Brian O'Reilly; Peter K. Fritschel

2007-08-26T23:59:59.000Z

190

HOMOLOGOUS EXTREME ULTRAVIOLET WAVES IN THE EMERGING FLUX REGION OBSERVED BY THE SOLAR DYNAMICS OBSERVATORY  

SciTech Connect

Taking advantage of the high temporal and spatial resolution of the Solar Dynamics Observatory (SDO) observations, we present four homologous extreme ultraviolet (EUV) waves within 3 hr on 2010 November 11. All EUV waves emanated from the same emerging flux region (EFR), propagated in the same direction, and were accompanied by surges, weak flares, and faint coronal mass ejections (CMEs). The waves had the basically same appearance in all EUV wavebands of the Atmospheric Imaging Assembly on SDO. The waves propagated at constant velocities in the range of 280-500 km s{sup -1}, with little angular dependence, which indicated that the homologous waves could be likely interpreted as fast-mode waves. The waves are supposed to likely involve more than one driving mechanism, and it was most probable that the waves were driven by the surges, due to their close timing and location relations. We also propose that the homologous waves were intimately associated with the continuous emergence and cancellation of magnetic flux in the EFR, which could supply sufficient energy and trigger the onsets of the waves.

Zheng Ruisheng; Jiang Yunchun; Yang Jiayan; Bi Yi; Hong Junchao; Yang, B.; Yang Dan, E-mail: zhrsh@ynao.ac.cn [National Astronomical Observatories/Yunnan Observatory, Chinese Academy of Sciences, Kunming 650011 (China)

2012-03-01T23:59:59.000Z

191

Combined analysis of all three phases of solar neutrino data from the Sudbury Neutrino Observatory  

Science Journals Connector (OSTI)

We report results from a combined analysis of solar neutrino data from all phases of the Sudbury Neutrino Observatory (SNO). By exploiting particle identification information obtained from the proportional counters installed during the third phase, this analysis improved background rejection in that phase of the experiment. The combined analysis of the SNO data resulted in a total flux of active neutrino flavors from 8B decays in the Sun of (5.250.16(stat.)?0.13+0.11(syst.))106cm?2s?1, while a two-flavor neutrino oscillation analysis yielded ?m212=(5.6?1.4+1.9)10?5eV2 and tan2?12=0.427?0.029+0.033. A three-flavor neutrino oscillation analysis combining the SNO result with results of all other solar neutrino experiments and reactor neutrino experiments yielded ?m212=(7.46?0.19+0.20)10?5eV2, tan2?12=0.443?0.025+0.030, and sin2?13=(2.49?0.32+0.20)10?2.

B. Aharmim et al. (SNO Collaboration)

2013-08-01T23:59:59.000Z

192

Measurement of the cosmic ray and neutrino-induced muon flux at the Sudbury neutrino observatory  

Science Journals Connector (OSTI)

Results are reported on the measurement of the atmospheric neutrino-induced muon flux at a depth of 2 kilometers below the Earths surface from 1229 days of operation of the Sudbury Neutrino Observatory (SNO). By measuring the flux of through-going muons as a function of zenith angle, the SNO experiment can distinguish between the oscillated and unoscillated portion of the neutrino flux. A total of 514 muonlike events are measured between -1?cos??zenith?0.4 in a total exposure of 2.301014??cm2?s. The measured flux normalization is 1.220.09 times the Bartol three-dimensional flux prediction. This is the first measurement of the neutrino-induced flux where neutrino oscillations are minimized. The zenith distribution is consistent with previously measured atmospheric neutrino oscillation parameters. The cosmic ray muon flux at SNO with zenith angle cos??zenith>0.4 is measured to be (3.310.01(stat)0.09(sys))10-10???/s/cm2.

B. Aharmim et al. (SNO Collaboration)

2009-07-10T23:59:59.000Z

193

SEARCHES FOR HIGH-FREQUENCY VARIATIONS IN THE {sup 8}B SOLAR NEUTRINO FLUX AT THE SUDBURY NEUTRINO OBSERVATORY  

SciTech Connect

We have performed three searches for high-frequency signals in the solar neutrino flux measured by the Sudbury Neutrino Observatory, motivated by the possibility that solar g-mode oscillations could affect the production or propagation of solar {sup 8}B neutrinos. The first search looked for any significant peak in the frequency range 1-144 day{sup -1}, 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 Solar and Heliospheric Observatory 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.

Aharmim, B.; Chauhan, D. [Department of Physics and Astronomy, Laurentian University, Sudbury, ON P3E 2C6 (Canada); Ahmed, S. N.; Boulay, M. G.; Cai, B.; Chen, M.; Dai, X. [Department of Physics, Queen's University, Kingston, ON K7L 3N6 (Canada); Anthony, A. E. [Department of Physics, University of Texas at Austin, Austin, TX 78712-0264 (United States); Barros, N. [Laboratorio de Instrumentacao e Fisica Experimental de PartIculas, Av. Elias Garcia 14, 1, 1000-149 Lisboa (Portugal); Beier, E. W.; Deng, H. [Department of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104-6396 (United States); Bellerive, A.; Boudjemline, K. [Ottawa-Carleton Institute for Physics, Department of Physics, Carleton University, Ottawa, ON K1S 5B6 (Canada); Beltran, B. [Department of Physics, University of Alberta, Edmonton, Alberta, T6G 2R3 (Canada); Bergevin, M.; Chan, Y. D. [Institute for Nuclear and Particle Astrophysics and Nuclear Science Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720 (United States); Biller, S. D.; Cleveland, B. T. [Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH (United Kingdom); Burritt, T. H.; Cox, G. A. [Center for Experimental Nuclear Physics and Astrophysics, and Department of Physics, University of Washington, Seattle, WA 98195 (United States)

2010-02-10T23:59:59.000Z

194

The magnetic sun from different views: A comparison of the mean and background magnetic field observations made in different observatories and in different spectral lines  

Science Journals Connector (OSTI)

A comparison is made of observational data on the mean magnetic field of the Sun from several observatories (a ... correlation and regression analyses of observations of background magnetic fields at the STOP tel...

M. L. Demidov

195

EMERGING DIMMINGS OF ACTIVE REGIONS OBSERVED BY THE SOLAR DYNAMICS OBSERVATORY  

SciTech Connect

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.

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)

2012-12-01T23:59:59.000Z

196

CORONAL MAGNETIC FIELD MEASUREMENT FROM EUV IMAGES MADE BY THE SOLAR DYNAMICS OBSERVATORY  

SciTech Connect

By measuring the geometrical properties of the coronal mass ejection (CME) flux rope and the leading shock observed on 2010 June 13 by the Solar Dynamics Observatory (SDO) mission's Atmospheric Imaging Assembly we determine the Alfven speed and the magnetic field strength in the inner corona at a heliocentric distance of {approx}1.4 Rs. The basic measurements are the shock standoff distance ({Delta}R) ahead of the CME flux rope, the radius of curvature of the flux rope (R{sub c}), and the shock speed. We first derive the Alfvenic Mach number (M) using the relationship, {Delta}R/R{sub c} = 0.81[({gamma}-1) M{sup 2} + 2]/[({gamma}+1)(M{sup 2} - 1)], where {gamma} is the only parameter that needed to be assumed. For {gamma} = 4/3, the Mach number declined from 3.7 to 1.5 indicating shock weakening within the field of view of the imager. The shock formation coincided with the appearance of a type II radio burst at a frequency of {approx}300 MHz (harmonic component), providing an independent confirmation of the shock. The shock compression ratio derived from the radio dynamic spectrum was found to be consistent with that derived from the theory of fast-mode MHD shocks. From the measured shock speed and the derived Mach number, we found the Alfven speed to increase from {approx}140 km s{sup -1} to 460 km s{sup -1} over the distance range 1.2-1.5 Rs. By deriving the upstream plasma density from the emission frequency of the associated type II radio burst, we determined the coronal magnetic field to be in the range 1.3-1.5 G. The derived magnetic field values are consistent with other estimates in a similar distance range. This work demonstrates that the EUV imagers, in the presence of radio dynamic spectra, can be used as coronal magnetometers.

Gopalswamy, Nat; Akiyama, Sachiko; Maekelae, Pertti; Yashiro, Seiji [NASA Goddard Space Flight Center, Greenbelt, MD 20771-0001 (United States); Nitta, Nariaki [Lockheed-Martin Solar and Astrophysics Laboratory, Palo Alto, CA 94304 (United States)

2012-01-01T23:59:59.000Z

197

Quartz tube extensometer for observation of Earth tides and local tectonic deformations at the Sopronbanfalva Geodynamic Observatory, Hungary  

SciTech Connect

In May 1990, a quartz tube extensometer was installed in the Sopronbanfalva Geodynamic Observatory of the Geodetic and Geophysical Research Institute (GGRI) of the Hungarian Academy of Sciences for recording Earth tides and recent tectonic movements. The paper describes the construction of the extensometer and a portable calibrator used for the in situ calibration of the instrument. The extensometer is very sensitive. Its scale factor is 2.093{+-}0.032 nm/mV according to the highly precise calibration method developed at the GGRI. Since the stability of extensometers is strongly influenced by the geological structure and properties of the rocks in the vicinity of the recording site, the observatory instrument system was tested by coherence analysis between theoretical (as the input signal) and measured tidal data series (as the output signal). In the semidiurnal tidal frequency band the coherence is better than 0.95, while in the diurnal band it is about 0.8. Probably this is due to the fact that the noise is higher in the diurnal band (0.4-0.5 nstr) than in the semidiurnal band (0.19-0.22 nstr). Coherence analysis between theoretical and measured data corrected for barometric changes yielded a small improvement of coherence in both frequency bands, while using temperature data correction, no observable improvement was obtained. Results of the tidal analysis also show that the observatory instrument system is suitable for recording very small tectonic movements. The 18 years of continuous data series measured by the extensometer prove the high quality of the extensometer. On the basis of investigations, it was pointed out that further efforts should be done to improve the barometric correction method and that correction for ocean load, as well as considering topographic and cavity effects are necessary to increase the accuracy of determining tidal parameters.

Mentes, Gy. [Geodetic and Geophysical Research Institute of the Hungarian Academy of Sciences, Csatkai Endre u. 6-8, H-9400 Sopron (Hungary)

2010-07-15T23:59:59.000Z

198

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

SciTech Connect

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.

Abreu, P.; /Lisbon, LIFEP /Lisbon, IST; Aglietta, M.; /Turin Observ. /Turin U. /INFN, Turin; Ahn, E.J.; /Fermilab; Allard, D.; /APC, Paris; Allekotte, I.; /Centro Atomico Bariloche /Balseiro Inst., San Carlos de Bariloche; Allen, J.; /New York U.; Alvarez Castillo, J.; /Mexico U.; Alvarez-Muniz, J.; /Santiago de Compostela U.; Ambrosio, M.; /Naples U. /INFN, Naples; Aminaei, A.; /Nijmegen U., IMAPP; Anchordoqui, L.; /Wisconsin U., Milwaukee /Lisbon, LIFEP /Lisbon, IST

2011-01-01T23:59:59.000Z

199

Bounds on the density of sources of ultra-high energy cosmic rays from the Pierre Auger Observatory  

SciTech Connect

We derive lower bounds on the density of sources of ultra-high energy cosmic rays from the lack of significant clustering in the arrival directions of the highest energy events detected at the Pierre Auger Observatory. The density of uniformly distributed sources of equal intrinsic intensity was found to be larger than ? (0.06?5) 10{sup ?4} Mpc{sup ?3} at 95% CL, depending on the magnitude of the magnetic deflections. Similar bounds, in the range (0.2?7) 10{sup ?4} Mpc{sup ?3}, were obtained for sources following the local matter distribution.

Collaboration: Pierre Auger Collaboration

2013-05-01T23:59:59.000Z

200

Temporal Pointing Variations of The Solar Dynamics Observatory's HMI and AIA Instruments on Sub-Weekly Time Scales  

E-Print Network (OSTI)

Achieving sub-arcsecond co-registration across varying time-lines of multi-wavelength and instrument images is not trivial, and requires accurate characterization of instrument pointing jitter. In this work we have investigated internal pointing errors, on daily and yearly time-scales, occurring across the \\textit{Solar Dynamics Observatory}'s (SDO) {\\it Atmospheric Imaging Assembly} (AIA) and { \\it Helioseismic Magnetic Imager} (HMI). Using cross-correlation techniques on AIA 1700\\,{\\AA} passband and HMI line-of-sight (LOS) magnetograms, from three years of observational image pairs at approximately three day intervals, internal pointing errors are quantified. Pointing variations of $\\pm$\\,0.26$\\arcsec$ (jitter limited) and $\\pm$\\,0.50$\\arcsec$ in the solar East-West ($x$) and North-South ($y$) directions, respectively, are measured. AIA observations of the Venus June 2012 transit are used to measure existing coalignment offsets in all passbands. We find AIA passband pointing variations are $$\\,$=$\\, 1.10$\\a...

Orange, N Brice; Chesny, David L; Patel, Maulik; Champey, Patrick; Hesterly, Katie; Anthony, Dylan; Treen, Robert

2015-01-01T23:59:59.000Z

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


201

Observations and modeling of the emerging EUV loops in the quiet Sun as seen with the Solar Dynamics Observatory  

E-Print Network (OSTI)

We used data from the Helioseismic and Magnetic Imager (HMI), and Atmospheric Imaging Assembly (AIA) on the \\textit{Solar Dynamics Observatory} (SDO) to study coronal loops at small scales, emerging in the quiet Sun. With HMI line-of-sight magnetograms, we derive the integrated and unsigned photospheric magnetic flux at the loop footpoints in the photosphere. These loops are bright in the EUV channels of AIA. Using the six AIA EUV filters, we construct the differential emission measure (DEM) in the temperature range $5.7 - 6.5$ in log $T$ (K) for several hours of observations. The observed DEMs have a peak distribution around log $T \\approx$ 6.3, falling rapidly at higher temperatures. For log $T temperature is calculated, and its time variations are compared with those of magnetic flux. We present two possibilities for explaining the observed DEMs and temperatures variations. (a) Assuming the observed loop...

Chitta, LP; van Ballegooijen, A A; DeLuca, E E; Hasan, S S; Hanslmeier, A

2013-01-01T23:59:59.000Z

202

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

DOE Data Explorer (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/

203

Design and Initial Performance of SHARP, a Polarimeter for the SHARC-II Camera at the Caltech Submillimeter Observatory  

E-Print Network (OSTI)

We have developed a fore-optics module that converts the SHARC-II camera at the Caltech Submillimeter Observatory into a sensitive imaging polarimeter at wavelengths of 350 and 450 microns. We refer to this module as "SHARP". SHARP splits the incident radiation into two orthogonally polarized beams that are then re-imaged onto opposite ends of the 32 x 12 pixel detector array in SHARC-II. A rotating half-wave plate is used just upstream from the polarization-splitting optics. The effect of SHARP is to convert SHARC-II into a dual-beam 12 x 12 pixel polarimeter. A novel feature of SHARP's design is the use of a crossed grid in a submillimeter polarimeter. Here we describe the detailed optical design of SHARP and present results of tests carried out during our first few observing runs. At 350 microns, the beam size (9 arcseconds), throughput (75%), and instrumental polarization (design goals.

H. Li; C. D. Dowell; L. Kirby; G. Novak; J. E. Vaillancourt

2007-07-01T23:59:59.000Z

204

Constraints on neutrino-nucleon interactions at energies of 1EeV with the IceCube Neutrino Observatory  

Science Journals Connector (OSTI)

A search for extremely high energy cosmic neutrinos has been carried out with the IceCube Neutrino Observatory. The main signals in the search are neutrino-induced energetic charged leptons and their rate depends on the neutrino-nucleon cross section. The upper limit on the neutrino flux has implications for possible new physics beyond the standard model such as the extra space-time dimension scenarios which lead to a cross section much higher than the standard particle physics prediction. In this study we constrain the neutrino-nucleon cross section at energies beyond 109??GeV with the IceCube observation. The constraints are obtained as a function of the extraterrestrial neutrino flux in the relevant energy range, which accounts for the astrophysical uncertainty of neutrino production models.

Shigeru Yoshida

2010-11-22T23:59:59.000Z

205

SOHO, the Solar and Heliospheric Observatory, is a project of international cooperation between ESA and NASA to study the Sun, from its deep core to the outer  

E-Print Network (OSTI)

Fact sheet SOHO SOHO, the Solar and Heliospheric Observatory, is a project of international cooperation between ESA and NASA to study the Sun, from its deep core to the outer corona, and the solar wind, will be extended to other stars by ESA's forthcoming Eddington mission. Science highlights to date SOHO has

206

13Moving Magnetic Filaments Near Sunspots These two images were taken by the Hinode (Solar-B) solar observatory on October 30, 2006.  

E-Print Network (OSTI)

13Moving Magnetic Filaments Near Sunspots These two images were taken by the Hinode (Solar-B) solar://spacemath.gsfc.nasa.gov These two images were taken by the Hinode (Solar-B) solar observatory on October 30, 2006. The size of each also use transparent paper or film, overlay the paper on each image, and mark the locations carefully

207

Real-time flare detection in ground-based H$\\alpha$ imaging at Kanzelh\\"ohe Observatory  

E-Print Network (OSTI)

Kanzelh\\"ohe Observatory (KSO) regularly performs high-cadence full-disk imaging of the solar chromosphere in the H$\\alpha$ and CaIIK spectrallines as well as the solar photosphere in white-light. In the frame of ESA's Space Situational Awareness (SSA) programme, a new system for real-time H$\\alpha$ data provision and automatic flare detection was developed at KSO. The data and events detected are published in near real-time at ESA's SSA Space Weather portal (http://swe.ssa.esa.int/web/guest/kso-federated). In this paper, we describe the H$\\alpha$ instrument, the image recognition algorithms developed, the implementation into the KSO H$\\alpha$ observing system and present the evaluation results of the real-time data provision and flare detection for a period of five months. The H$\\alpha$ data provision worked in $99.96$% of the images, with a mean time lag between image recording and online provision of 4s. Within the given criteria for the automatic image recognition system (at least three H$\\alpha$ images a...

Ptzi, Werner; Riegler, Gernot; Amerstorfer, Ulrike; Pock, Thomas; Temmer, Manuela; Polanec, Wolfgang; Baumgartner, Dietmar J

2014-01-01T23:59:59.000Z

208

Operations and Performance of the PACS Instrument 3He Sorption Cooler on board of the Herschel Space Observatory  

E-Print Network (OSTI)

A 3He sorption cooler produced the operational temperature of 285mK for the bolometer arrays of the Photodetector Array Camera and Spectrometer (PACS) instrument of the Herschel Space Observatory. This cooler provided a stable hold time between 60 and 73h, depending on the operational conditions of the instrument. The respective hold time could be determined by a simple functional relation established early on in the mission and reliably applied by the scientific mission planning for the entire mission. After exhaustion of the liquid 3He due to the heat input by the detector arrays, the cooler was recycled for the next operational period following a well established automatic procedure. We give an overview of the cooler operations and performance over the entire mission and distinguishing in-between the start conditions for the cooler recycling and the two main modes of PACS photometer operations. As a spin-off, the cooler recycling temperature effects on the Herschel cryostat 4He bath were utilized as an alt...

Sauvage, Marc; Klaas, Ulrich; Muller, Thomas; Moor, Andras; Poglitsch, Albrecht; Feuchtgruber, Helmut; Duband, Lionel

2014-01-01T23:59:59.000Z

209

The Upgraded Arecibo Observatory  

Science Journals Connector (OSTI)

...illuminated target back to the laser. This permits a total...4. Schematic of the laser survey meth-od. The laser and its steering mirror...This con-sists of two turbine-driven generators...carriage house. Primary control of the transmitter is...

L. M. LaLonde

1974-10-18T23:59:59.000Z

210

OBSERVATORY SNO INSTITUTE MEMBERS  

E-Print Network (OSTI)

from Canada, the United States and the United Kingdom. Through its use of heavy water, the SNO detector and regular water. The construction of the SNO Laboratory began in 1990 and was completed in 1998 at a capital, the National Research Council of Canada, the Northern Ontario Heritage Foundation, Industry, Science

Abolmaesumi, Purang

211

The Upper Atmosphere Observatory  

Science Journals Connector (OSTI)

...with *the plasma frethe progress...explorcreated an even larger number of...the upper atmosphere and ionosphere...the upper atmosphere. For this...ionospheric plasma motion simul-taneously...field is large, the horizontal...resolved. The atmospheric gravity waves...simul-taneously at a large number of...two regions plasma drifts separated...

J. V. Evans

1972-05-05T23:59:59.000Z

212

NATIONAL RADIO ASTRONOMY OBSERVATORY  

E-Print Network (OSTI)

a window in which a thin plastic film vacuum barrier is supported by a thick slab of low density dielectric REPORT NO. 292 A STUDY OF MATERIALS FOR A BROADBAND MILLIMETER-WAVE QUASI-OPTICAL VACUUM WINDOW A. R WINDOW A. R. Kerr, N. J. Bailey, D. E. Boyd and N. Horner August 21, 1992 Introduction Cryogenic

Groppi, Christopher

213

The Upper Atmosphere Observatory  

Science Journals Connector (OSTI)

...DATA, JOURNAL OF ATMOSPHERIC AND TERRESTRIAL...IN NEAR-EARTH PLASMA, SPACE SCIENCE...INVESTIGATION OF WHISTLING ATMOSPHERICS, PHILOSOPHICAL...TRANSPOLAR EXOSPHERIC PLASMA .1. PLASMASPHERE...dynamics of the upper atmosphere. For this purpose...the ionospheric plasma motion simul-taneously...

J. V. Evans

1972-05-05T23:59:59.000Z

214

National Radio Astronomy Observatory  

Science Journals Connector (OSTI)

...Fabrication in the Bliss plant of part of the yoke for the...central ridge. The electric power distribution sys-tem found...short as 3 centimeters. The specifications for the instrument have gone...absence of strong winds or thermal effects, the user should be...

Richard M. Emberson

1959-11-13T23:59:59.000Z

215

National Radio Astronomy Observatory  

Science Journals Connector (OSTI)

...possibility of making thermal emission studies...committee listed eight specifications for the site...of electrical insulation. 7) Size. The...automobile. A ninth specification was added by the...strong winds or thermal effects, the...

Richard M. Emberson

1959-11-13T23:59:59.000Z

216

Armagh Observatory Annual Report  

E-Print Network (OSTI)

. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 1 1.3 Organizational Structure . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 20 4 Education and Lifelong Learning 20 4.1 e

217

European Southern Observatory  

E-Print Network (OSTI)

extreme environmental conditions like survival wind load, rain or snow Keep the inner air volume equilibrium with the external environment without active air conditioning Minimize dome seeing Do not create t Material: Structure Mild steel Cladding Aluminium sandwich Pneumatic seal Polyester Inspired by Cargo

Liske, Jochen

218

The Herschel Space Observatory  

E-Print Network (OSTI)

Passively cooled front end with 2 fixed tuned Schottky diode 2nd harmonic mixers Observed O2, CI, H2O, H2 18 Paul Goldsmith Sunshield and Solar Array Cryostat Focal Plane Instruments Herschel Planck 3.5m diameter Sylda housing around Planck Herschel Overview Paul Goldsmith Ariane V164 launch Herschel Web Sites

Shumway, John

219

Analysis of the Tropical Tropopause Layer Cirrus in CALIPSO and MLS Data - A Water Perspective  

E-Print Network (OSTI)

in order to screen for noise (see the data quality and description document at http://mls.jpl.nasa.gov/data/v2- 2_data_quality_document.pdf). Single IWC measurements from MLS have a vertical resolution of around 3 km and horizontal along-track and cross... in order to screen for noise (see the data quality and description document at http://mls.jpl.nasa.gov/data/v2- 2_data_quality_document.pdf). Single IWC measurements from MLS have a vertical resolution of around 3 km and horizontal along-track and cross...

Wang, Tao

2012-07-16T23:59:59.000Z

220

LARGE-SCALE CORONAL PROPAGATING FRONTS IN SOLAR ERUPTIONS AS OBSERVED BY THE ATMOSPHERIC IMAGING ASSEMBLY ON BOARD THE SOLAR DYNAMICS OBSERVATORYAN ENSEMBLE STUDY  

SciTech Connect

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 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.

Nitta, Nariaki V.; Schrijver, Carolus J.; Title, Alan M.; Liu, Wei [Lockheed Martin Advanced Technology Center, Dept/A021S, B/252, 3251 Hanover Street, Palo Alto, CA 94304 (United States)

2013-10-10T23:59:59.000Z

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


221

Observatory -New Materials, Called MOFs, May Aid in Capture of Carbon -NYTimes.com http://www.nytimes.com/2009/12/08/science/08obgas.html?_r=2&ref=science[12/8/2009 9:38:13 AM  

E-Print Network (OSTI)

Observatory - New Materials, Called MOFs, May Aid in Capture of Carbon - NYTimes.com http The New York Times » OBSERVATORY New Materials May Aid in Capturing Carbon By HENRY FOUNTAIN Published, or MOFs, hold promise for carbon capture. In a paper in The Proceedings of the National Academy

Yaghi, Omar M.

222

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

E-Print Network (OSTI)

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.

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

2000-08-01T23:59:59.000Z

223

LARGE-SCALE DISTRIBUTION OF ARRIVAL DIRECTIONS OF COSMIC RAYS DETECTED ABOVE 10{sup 18} eV AT THE PIERRE AUGER OBSERVATORY  

SciTech Connect

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.

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. [Instituto de Fisica, Universidade de Sao Paulo, 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. [Facultad Regional Buenos Aires, Universidad Tecnologica Nacional, 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. [IFGW, Universidade Estadual de Campinas, 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); Arganda, E. [IFLP, Universidad Nacional de La Plata and CONICET, La Plata (Argentina); Collaboration: Pierre Auger Collaboration; and others

2012-12-15T23:59:59.000Z

224

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

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.

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); Castillo, J. Alvarez [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); Arganda, E. [IFLP, Universidad Nacional de La Plata and CONICET, La Plata (Argentina); Collaboration: Pierre Auger Collaboration; and others

2013-01-01T23:59:59.000Z

225

Using Realistic MHD Simulations for Modeling and Interpretation of Quiet-Sun Observations with the Solar Dynamics Observatory Helioseismic and Magnetic Imager  

E-Print Network (OSTI)

The solar atmosphere is extremely dynamic, and many important phenomena develop on small scales that are unresolved in observations with the Helioseismic and Magnetic Imager (HMI) instrument on the Solar Dynamics Observatory (SDO). For correct calibration and interpretation, it is very important to investigate the effects of small-scale structures and dynamics on the HMI observables, such as Doppler shift, continuum intensity, spectral line depth, and width. We use 3D radiative hydrodynamics simulations of the upper turbulent convective layer and the atmosphere of the Sun, and a spectro-polarimetric radiative transfer code to study observational characteristics of the Fe I 6173A line observed by HMI in quiet-Sun regions. We use the modeling results to investigate the sensitivity of the line Doppler shift to plasma velocity, and also sensitivities of the line parameters to plasma temperature and density, and determine effective line formation heights for observations of solar regions located at different dista...

Kitiashvili, Irina N; Lagg, Andreas

2014-01-01T23:59:59.000Z

226

On the possibility to discriminate the mass of the primary cosmic ray using the muon arrival times from extensive air showers: Application for Pierre Auger Observatory  

SciTech Connect

In this paper we study the possibility to discriminate the mass of the primary cosmic ray by observing the muon arrival times in ground detectors. We analyzed extensive air showers (EAS) induced by proton and iron nuclei with the same energy 8 Multiplication-Sign 10{sup 17} eV simulated with CORSIKA, and analyzed the muon arrival times at ground measured by the infill array detectors of the Pierre Auger Observatory (PAO). From the arrival times of the core and of the muons the atmospheric depth of muon generation locus is evaluated. The results suggest a potential mass discrimination on the basis of muon arrival times and of the reconstructed atmospheric depth of muon production. An analysis of a larger set of CORSIKA simulations carried out for primary energies above 10{sup 18} eV is in progress.

Arsene, N.; Rebel, H.; Sima, O. [Institute of Space Science (ISS), Bucharest-Magurele, P.O. Box MG-23 (Romania) and Physics Department, University of Bucharest, Bucharest-Magurele (Romania); Karlsruhe Institute of Technology, Karlsruhe (Germany); Physics Department, University of Bucharest, Bucharest-Magurele (Romania)

2012-11-20T23:59:59.000Z

227

Measurement of the ?e and total 8B solar neutrino fluxes with the Sudbury Neutrino Observatory phase-III data set  

Science Journals Connector (OSTI)

This paper details the solar neutrino analysis of the 385.17-day phase-III data set acquired by the Sudbury Neutrino Observatory (SNO). An array of 3He proportional counters was installed in the heavy-water target to measure precisely the rate of neutrino-deuteron neutral-current interactions. This technique to determine the total active 8B solar neutrino flux was largely independent of the methods employed in previous phases. The total flux of active neutrinos was measured to be 5.54?0.31+0.33(stat.)?0.34+0.36(syst.)106cm?2s?1, consistent with previous measurements and standard solar models. A global analysis of solar and reactor neutrino mixing parameters yielded the best-fit values of ?m2=7.59?0.21+0.1910?5eV2 and ?=34.4?1.2+1.3degrees.

B. Aharmim et al. (SNO Collaboration)

2013-01-18T23:59:59.000Z

228

Independent Measurement of the Total Active B8 Solar Neutrino Flux Using an Array of He3 Proportional Counters at the Sudbury Neutrino Observatory  

Science Journals Connector (OSTI)

The Sudbury Neutrino Observatory (SNO) used an array of He3 proportional counters to measure the rate of neutral-current interactions in heavy water and precisely determined the total active (?x) B8 solar neutrino flux. This technique is independent of previous methods employed by SNO. The total flux is found to be 5.54-0.31+0.33(stat)-0.34+0.36(syst)106??cm-2?s-1, in agreement with previous measurements and standard solar models. A global analysis of solar and reactor neutrino results yields ?m2=7.59-0.21+0.1910-5??eV2 and ?=34.4-1.2+1.3 degrees. The uncertainty on the mixing angle has been reduced from SNOs previous results.

B. Aharmim et al. (SNO Collaboration)

2008-09-09T23:59:59.000Z

229

Studies of a three-stage dark matter and neutrino observatory based on multi-ton combinations of liquid xenon and liquid argon detectors  

E-Print Network (OSTI)

We study a three stage dark matter and neutrino observatory based on multi-ton two-phase liquid Xe and Ar detectors with sufficiently low backgrounds to be sensitive to WIMP dark matter interaction cross sections down to 10E-47 cm^2, and to provide both identification and two independent measurements of the WIMP mass through the use of the two target elements in a 5:1 mass ratio, giving an expected similarity of event numbers. The same detection systems will also allow measurement of the pp solar neutrino spectrum, the neutrino flux and temperature from a Galactic supernova, and neutrinoless double beta decay of 136Xe to the lifetime level of 10E27 - 10E28 y corresponding to the Majorana mass predicted from current neutrino oscillation data. The proposed scheme would be operated in three stages G2, G3, G4, beginning with fiducial masses 1-ton Xe + 5-ton Ar (G2), progressing to 10-ton Xe + 50-ton Ar (G3) then, dependent on results and performance of the latter, expandable to 100-ton Xe + 500-ton Ar (G4). This ...

Arisaka, K; Smith, P F; Beltrame, P; Ghag, C; Lung, K; Teymourian, A; Wang, H; Cline, D B

2011-01-01T23:59:59.000Z

230

Early-type stars observed in the ESO UVES Paranal Observatory Project: I -- Interstellar Na I UV, Ti II and Ca II K observations  

E-Print Network (OSTI)

We present an analysis of interstellar Na I (lambda=3302.37\\AA, 3302.98\\AA), Ti II (lambda=3383.76\\AA) and Ca II K (lambda=3933.66\\AA) absorption features for 74 sightlines towards O- and B-type stars in the Galactic disc. The data were obtained from the UVES Paranal Observatory Project, at a spectral resolution of 3.75km/s and with mean signal to noise ratios per pixel of 260, 300 and 430 for the Na I, Ti II and Ca II observations, respectively. Interstellar features were detected in all but one of the Ti II sightlines and all of the Ca II sightlines. The dependence of the column density of these three species with distance, height relative to the Galactic plane, H I column density, reddening and depletion relative to the solar abundance has been investigated. We also examine the accuracy of using the Na I column density as an indicator of that for H I. In general we find similar strong correlations for both Ti and Ca, and weaker correlations for Na. Our results confirm the general belief that Ti and Ca occur in the same regions of the interstellar medium and also that the Ti II/Ca II ratio is constant over all parameters. We hence conclude that the absorption properties of Ti and Ca are essentially constant under the general interstellar medium conditions of the Galactic disc.

I. Hunter; J. V. Smoker; F. P. Keenan; C. Ledoux; E. Jehin; R. Cabanac; C. Melo; S. Bagnulo

2006-01-17T23:59:59.000Z

231

Measurement of the nue and Total 8B Solar Neutrino Fluxes with theSudbury Neutrino Observatory Phase I Data Set  

SciTech Connect

This article provides the complete description of resultsfrom the Phase I data set of the Sudbury Neutrino Observatory (SNO). ThePhase I data set is based on a 0.65 kt-year exposure of heavy water tothe solar 8B neutrino flux. Included here are details of the SNO physicsand detector model, evaluations of systematic uncertainties, andestimates of backgrounds. Also discussed are SNO's approach tostatistical extraction of the signals from the three neutrino reactions(charged current, neutral current, and elastic scattering) and theresults of a search for a day-night asymmetry in the ?e flux. Under theassumption that the 8B spectrum is undistorted, the measurements fromthis phase yield a solar ?e flux of ?(?e) =1.76+0.05?0.05(stat.)+0.09?0.09 (syst.) x 106 cm?2 s?1, and a non-?ecomponent ?(? mu) = 3.41+0.45?0.45(stat.)+0.48?0.45 (syst.) x 106 cm?2s?1. The sum of these components provides a total flux in excellentagreement with the predictions of Standard Solar Models. The day-nightasymmetry in the ?e flux is found to be Ae = 7.0 +- 4.9 (stat.)+1.3?1.2percent (sys.), when the asymmetry in the total flux is constrained to bezero.

Aharmim, B.; Ahmad, Q.R.; Ahmed, S.N.; Allen, R.C.; Andersen,T.C.; Anglin, J.D.; Buehler, G.; Barton, J.C.; Beier, E.W.; Bercovitch,M.; Bergevin, M.; Bigu, J.; Biller, S.D.; Black, R.A.; Blevis, I.; Boardman, R.J.; Boger, J.; Bonvin, E.; Boulay, M.G.; Bowler, M.G.; Bowles, T.J.; Brice, S.J.; Browne, M.C.; Bullard, T.V.; Burritt, T.H.; Cameron, J.; Chan, Y.D.; Chen, H.H.; Chen, M.; Chen, X.; Cleveland, B.T.; Cowan, J.H.M.; Cowen, D.F.; Cox, G.A.; Currat, C.A.; Dai, X.; Dalnoki-Veress, F.; Davidson, W.F.; Deng, H.; DiMarco, M.; Doe, P.J.; Doucas, G.; Dragowsky, M.R.; Duba, C.A.; Duncan, F.A.; Dunford, M.; Dunmore, J.A.; Earle, E.D.; Elliott, S.R.; Evans, H.C.; Ewan, G.T.; Farine, J.; Fergani, H.; Ferraris, A.P.; Fleurot, F.; Ford, R.J.; Formaggio, J.A.; Fowler, M.M.; Frame, K.; Frank, E.D.; Frati, W.; Gagnon,N.; Germani, J.V.; Gil, S.; Goldschmidt, A.; Goon, J.T.M.; Graham, K.; Grant, D.R.; Guillian, E.; Hahn, R.L.; Hallin, A.L.; Hallman, E.D.; Hamer, A.S.; Hamian, A.A.; Handler, W.B.; Haq, R.U.; Hargrove, C.K.; Harvey, P.J.; Hazama, R.; Heeger, K.M.; Heintzelman, W.J.; Heise, J.; Helmer, R.L.; Henning, R.; Hepburn, J.D.; Heron, H.; Hewett, J.; Hime,A.; Howard, C.; Howe, M.A.; Huang, M.; Hykawy, J.G.; Isaac, M.C.P.; Jagam, P.; Jamieson, B.; Jelley, N.A.; Jillings, C.; Jonkmans, G.; Kazkaz, K.; Keener, P.T.; Kirch, K.; Klein, J.R.; Knox, A.B.; Komar,R.J.; Kormos, L.L.; Kos, M.; Kouzes, R.; Krueger, A.; Kraus, C.; Krauss,C.B.; Kutter, T.; Kyba, C.C.M.; Labranche, H.; Lange, R.; Law, J.; Lawson, I.T.; Lay, M.; Lee, H.W.; Lesko, K.T.; Leslie, J.R.; Levine, I.; Loach, J.C.; Locke, W.; Luoma, S.; Lyon, J.; MacLellan, R.; Majerus, S.; Mak, H.B.; Maneira, J.; Marino, A.D.; Martin, R.; McCauley, N.; McDonald,A.B.; McDonald, D.S.; McFarlane, K.; McGee, S.; McGregor, G.; MeijerDrees, R.; Mes, H.; Mifflin, C.; Miknaitis, K.K.S.; Miller, M.L.; Milton,G.; Moffat, B.A.; Monreal, B.; Moorhead, M.; Morrissette, B.; Nally,C.W.; Neubauer, M.S.; et al.

2007-02-01T23:59:59.000Z

232

OBSERVATIONS AND MODELING OF THE EMERGING EXTREME-ULTRAVIOLET LOOPS IN THE QUIET SUN AS SEEN WITH THE SOLAR DYNAMICS OBSERVATORY  

SciTech Connect

We used data from the Helioseismic and Magnetic Imager (HMI) and the Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory (SDO) to study coronal loops at small scales, emerging in the quiet Sun. With HMI line-of-sight magnetograms, we derive the integrated and unsigned photospheric magnetic flux at the loop footpoints in the photosphere. These loops are bright in the EUV channels of AIA. Using the six AIA EUV filters, we construct the differential emission measure (DEM) in the temperature range 5.7-6.5 in log T (K) for several hours of observations. The observed DEMs have a peak distribution around log T Almost-Equal-To 6.3, falling rapidly at higher temperatures. For log T < 6.3, DEMs are comparable to their peak values within an order of magnitude. The emission-weighted temperature is calculated, and its time variations are compared with those of magnetic flux. We present two possibilities for explaining the observed DEMs and temperatures variations. (1) Assuming that the observed loops are composed of a hundred thin strands with certain radius and length, we tested three time-dependent heating models and compared the resulting DEMs and temperatures with the observed quantities. This modeling used enthalpy-based thermal evolution of loops (EBTEL), a zero-dimensional (0D) hydrodynamic code. The comparisons suggest that a medium-frequency heating model with a population of different heating amplitudes can roughly reproduce the observations. (2) We also consider a loop model with steady heating and non-uniform cross-section of the loop along its length, and find that this model can also reproduce the observed DEMs, provided the loop expansion factor {gamma} {approx} 5-10. More observational constraints are required to better understand the nature of coronal heating in the short emerging loops on the quiet Sun.

Chitta, L. P.; Van Ballegooijen, A. A.; DeLuca, E. E. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS-15, Cambridge, MA 02138 (United States); Kariyappa, R.; Hasan, S. S. [Indian Institute of Astrophysics, Bangalore 560 034 (India); Hanslmeier, A. [Institut fuer Physik, IGAM, Universitaet Graz, Universitaetsplatz 5, A-8010 Graz (Austria)

2013-05-01T23:59:59.000Z

233

Integrated High-Level Waste System Planning - Utilizing an Integrated Systems Planning Approach to Ensure End-State Definitions are Met and Executed - 13244  

SciTech Connect

The Savannah River Site (SRS) is a Department of Energy site which has produced nuclear materials for national defense, research, space, and medical programs since the 1950's. As a by-product of this activity, approximately 37 million gallons of high-level liquid waste containing approximately 292 million curies of radioactivity is stored on an interim basis in 45 underground storage tanks. Originally, 51 tanks were constructed and utilized to support the mission. Four tanks have been closed and taken out of service and two are currently undergoing the closure process. The Liquid Waste System is a highly integrated operation involving safely storing liquid waste in underground storage tanks; removing, treating, and dispositioning the low-level waste fraction in grout; vitrifying the higher activity waste at the Defense Waste Processing Facility; and storing the vitrified waste in stainless steel canisters until permanent disposition. After waste removal and processing, the storage and processing facilities are decontaminated and closed. A Liquid Waste System Plan (hereinafter referred to as the Plan) was developed to integrate and document the activities required to disposition legacy and future High-Level Waste and to remove from service radioactive liquid waste tanks and facilities. It establishes and records a planning basis for waste processing in the liquid waste system through the end of the program mission. The integrated Plan which recognizes the challenges of constrained funding provides a path forward to complete the liquid waste mission within all regulatory and legal requirements. The overarching objective of the Plan is to meet all Federal Facility Agreement and Site Treatment Plan regulatory commitments on or ahead of schedule while preserving as much life cycle acceleration as possible through incorporation of numerous cost savings initiatives, elimination of non-essential scope, and deferral of other scope not on the critical path to compliance. There is currently a premium on processing and storage space in the radioactive liquid waste tank system. To enable continuation of risk reduction initiatives, the Plan establishes a processing strategy that provides tank space required to meet, or minimizes the impacts to meeting, programmatic objectives. The Plan also addresses perturbations in funding and schedule impacts. (authors)

Ling, Lawrence T. [URS-Savannah River Remediation, Savannah River Site, Building 766-H Room 2205, Aiken, SC 29808 (United States)] [URS-Savannah River Remediation, Savannah River Site, Building 766-H Room 2205, Aiken, SC 29808 (United States); Chew, David P. [URS-Savannah River Remediation, Savannah River Site, Building 766-H Room 2426, Aiken, SC 29808 (United States)] [URS-Savannah River Remediation, Savannah River Site, Building 766-H Room 2426, Aiken, SC 29808 (United States)

2013-07-01T23:59:59.000Z

234

Evapotranspiration And Geochemical Controls On Groundwater Plumes At Arid Sites: Toward Innovative Alternate End-States For Uranium Processing And Tailings Facilities  

SciTech Connect

Management of legacy tailings/waste and groundwater contamination are ongoing at the former uranium milling site in Tuba City AZ. The tailings have been consolidated and effectively isolated using an engineered cover system. For the existing groundwater plume, a system of recovery wells extracts contaminated groundwater for treatment using an advanced distillation process. The ten years of pump and treat (P&T) operations have had minimal impact on the contaminant plume primarily due to geochemical and hydrological limits. A flow net analysis demonstrates that groundwater contamination beneath the former processing site flows in the uppermost portion of the aquifer and exits the groundwater as the plume transits into and beneath a lower terrace in the landscape. The evaluation indicates that contaminated water will not reach Moenkopi Wash, a locally important stream. Instead, shallow groundwater in arid settings such as Tuba City is transferred into the vadose zone and atmosphere via evaporation, transpiration and diffuse seepage. The dissolved constituents are projected to precipitate and accumulate as minerals such as calcite and gypsum in the deep vadose zone (near the capillary fringe), around the roots of phreatophyte plants, and near seeps. The natural hydrologic and geochemical controls common in arid environments such as Tuba City work together to limit the size of the groundwater plume, to naturally attenuate and detoxify groundwater contaminants, and to reduce risks to humans, livestock and the environment. The technical evaluation supports an alternative beneficial reuse (brownfield) scenario for Tuba City. This alternative approach would have low risks, similar to the current P&T scenario, but would eliminate the energy and expense associated with the active treatment and convert the former uranium processing site into a resource for future employment of local citizens and ongoing benefit to the Native American Nations.

Looney, Brian B.; Denham, Miles E.; Eddy-Dilek, Carol A.; Millings, Margaret R.; Kautsky, Mark

2014-01-08T23:59:59.000Z

235

HAWC Observatory captures first image  

NLE Websites -- All DOE Office Websites (Extended Search)

in the known universe: supernova explosions, active galactic nuclei, and gamma-ray bursts. The gamma rays are signatures of the acceleration sites of charged cosmic...

236

Golf Courses ObservatoriesPlaying  

E-Print Network (OSTI)

Edgecliffe Cathedral Hospital St Marys College Gatty Marine Laboratory Albany Park Bute Building Post Office. However, we would strongly recommend wearing a helmet and ensuring that you have lights on your bike

Brierley, Andrew

237

WORK OF THE LICK OBSERVATORY  

Science Journals Connector (OSTI)

...at least as satisfactorily as they did when new. The original design of the great tele-scope did not provide for power to wind the driving clock; it was wound by hand. A Pelton water-wheel was installed for this purpose in 1890, but it never...

W. W. Campbell

1903-04-17T23:59:59.000Z

238

Physical Properties of High-Level Cloud over Land and Ocean from CloudSatCALIPSO Data  

Science Journals Connector (OSTI)

Unlike other cloud types, high-level clouds play an important role, often imposing a warming effect, in the earthatmosphere radiative energy budget. In this paper, macro- and microphysical characteristics of cirrus clouds, such as their ...

Juan Huo; Daren Lu

2014-12-01T23:59:59.000Z

239

Identifying the top of the tropical tropopause layer from vertical mass flux analysis and CALIPSO lidar cloud observations  

E-Print Network (OSTI)

defined as the level of zero net radiative heating, which occurs near 14.5­15 km [e.g., Folkins et al layer (TTL) by analyzing the vertical mass flux profile based on radiative transfer calculations will rise into the stratosphere. Thus convection has to transport air at least to the zero radiative heating

Hochberg, Michael

240

Beamline 9.3.1  

NLE Websites -- All DOE Office Websites (Extended Search)

1 Print Atomic, molecular, and materials science Endstations: X-ray absorption endstation Polarized-x-ray emission spectrometer GENERAL BEAMLINE INFORMATION Operational Yes Source...

Note: This page contains sample records for the topic "observatory calipso endstations" from the National Library of EnergyBeta (NLEBeta).
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they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


241

Searches for Large-Scale Anisotropy in the Arrival Directions of Cosmic Rays Detected above Energy of $10^{19}$ eV at the Pierre Auger Observatory and the Telescope Array  

SciTech Connect

Spherical harmonic moments are well-suited for capturing anisotropy at any scale in the flux of cosmic rays. An unambiguous measurement of the full set of spherical harmonic coefficients requires full-sky coverage. This can be achieved by combining data from observatories located in both the northern and southern hemispheres. To this end, a joint analysis using data recorded at the Telescope Array and the Pierre Auger Observatory above 1019 eV is presented in this work. The resulting multipolar expansion of the flux of cosmic rays allows us to perform a series of anisotropy searches, and in particular to report on the angular power spectrum of cosmic rays above 1019 eV. No significant deviation from isotropic expectations is found throughout the analyses performed. Upper limits on the amplitudes of the dipole and quadrupole moments are derived as a function of the direction in the sky, varying between 7% and 13% for the dipole and between 7% and 10% for a symmetric quadrupole.

Aab, Alexander; et al,

2014-10-07T23:59:59.000Z

242

X6.9-CLASS FLARE-INDUCED VERTICAL KINK OSCILLATIONS IN A LARGE-SCALE PLASMA CURTAIN AS OBSERVED BY THE SOLAR DYNAMICS OBSERVATORY/ATMOSPHERIC IMAGING ASSEMBLY  

SciTech Connect

We present rare observational evidence of vertical kink oscillations in a laminar and diffused large-scale plasma curtain as observed by the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory. The X6.9-class flare in active region 11263 on 2011 August 9 induces a global large-scale disturbance that propagates in a narrow lane above the plasma curtain and creates a low density region that appears as a dimming in the observational image data. This large-scale propagating disturbance acts as a non-periodic driver that interacts asymmetrically and obliquely with the top of the plasma curtain and triggers the observed oscillations. In the deeper layers of the curtain, we find evidence of vertical kink oscillations with two periods (795 s and 530 s). On the magnetic surface of the curtain where the density is inhomogeneous due to coronal dimming, non-decaying vertical oscillations are also observed (period ? 763-896 s). We infer that the global large-scale disturbance triggers vertical kink oscillations in the deeper layers as well as on the surface of the large-scale plasma curtain. The properties of the excited waves strongly depend on the local plasma and magnetic field conditions.

Srivastava, A. K. [Aryabhatta Research Institute of Observational Sciences (ARIES), Manora Peak, Nainital 263 002 (India); Goossens, M. [Centre for Mathematical Plasma Astrophysics, Department of Mathematics, KU Leuven, Celestijnenlaan 200B, B-3001 Leuven (Belgium)

2013-11-01T23:59:59.000Z

243

Electron energy spectra, fluxes, and day-night asymmetries of 8B solar neutrinos from measurements with NaCl dissolved in the heavy-water detector at the Sudbury Neutrino Observatory  

Science Journals Connector (OSTI)

Results are reported from the complete salt phase of the Sudbury Neutrino Observatory experiment in which NaCl was dissolved in the H22O (D2O) target. The addition of salt enhanced the signal from neutron capture as compared to the pure D2O detector. By making a statistical separation of charged-current events from other types based on event-isotropy criteria, the effective electron recoil energy spectrum has been extracted. In units of 106cm-2s-1, the total flux of active-flavor neutrinos from B8 decay in the Sun is found to be 4.94-0.21+0.21(stat)-0.34+0.38(syst) and the integral flux of electron neutrinos for an undistorted B8 spectrum is 1.68-0.06+0.06(stat)-0.09+0.08(syst); the signal from (?x,e) elastic scattering is equivalent to an electron-neutrino flux of 2.35-0.22+0.22(stat)-0.15+0.15(syst). These results are consistent with those expected for neutrino oscillations with the so-called large mixing angle parameters and also with an undistorted spectrum. A search for matter-enhancement effects in the Earth through a possible day-night asymmetry in the charged-current integral rate is consistent with no asymmetry. Including results from other experiments, the best-fit values for two-neutrino mixing parameters are ?m2=(8.0-0.4+0.6)10-5 eV2 and ?=33.9-2.2+2.4 degrees.

B. Aharmim et al. (SNO Collaboration)

2005-11-30T23:59:59.000Z

244

NATIONAL RADIO ASTRONOMY OBSERVATORY Charlottesville, Virginia 22901  

E-Print Network (OSTI)

Report No. 127 THE 45-FOOT ANTENNA DRIVE SYSTEM John M. Payne MARCH 1973 NUMBER OF COPIES: 150 #12;THE 45-FOOT ANTENNA DRIVE SYSTEM John M. Payne TABLE OF CONTENTS Page 1. 0 Introduction .............................................. .........9 6. 1 Power Amplifiers

Groppi, Christopher

245

IATP | Trade Observatory | Headlines q What's new  

E-Print Network (OSTI)

in developing countries that are increasingly important producers and exporters of forest products," said Mining q Midwest, Plains Flooding Deaths Reach 22 q Climate change called security issue like Cold War q

246

The Annual Visitation of the Royal Observatory  

Science Journals Connector (OSTI)

... were not then favourable for insulation. Subsequently the wires were damaged in the snowstorm of December 26-27 last> ani were temporarily^epaired on January 25. It is believed that they ... the wind prevented the raising of the ball. For fourteen days after the snowstorm of December 26-27, no signals were sent to or received from the Deal time-ball tower, ...

1887-06-09T23:59:59.000Z

247

DEBRA S. SHEPHERD National Radio Astronomy Observatory  

E-Print Network (OSTI)

, NM 87801 REFEREED PUBLICATIONS Shepherd, D. S., Povich, M. S., Whitney, B. A., Robitaille, T. P., N.A., Walter, F., Shepherd, D.S., Halpern, J., Peck, A.B., Menten, K.M., Yost, S.A., Fox, D.W. 2002, ApJ, 565., Piro, L., Pooley, G. G., Price, P. A., Reichart, D., Ricker, G. R., Shepherd, D., Schmidt, B., Walter

Shepherd, Debra

248

Mixed fortunes for X-ray observatories  

Science Journals Connector (OSTI)

......are also on track for future comet exploration. The Stardust...towards its 2004 rendezvous with Comet Wild-2, where it should collect samples of comet dust from Wild-2 for return...observations of the Mars Polar Lander landing site in the hope of imaging......

Peter Bond

2000-04-01T23:59:59.000Z

249

NATIONAL RADIO ASTRONOMY OBSERVATORY Charlottesville, Virginia  

E-Print Network (OSTI)

: December 20, 1989 DISTRIBUTION: GB CV TU LLA GB Library ER Library Library Downtown VIA Library R. Lacasse IR Library Library Mountain P. Napier D. Schiebel M. Balister R. Freund J. Campbell E. Childers C-write-protected disk with sufficient space to store the data must be placed in current "Mass Storage Is" device Upon

Groppi, Christopher

250

The Gemini Observatory Fast Turnaround Program  

E-Print Network (OSTI)

Gemini's Fast Turnaround program is intended to greatly decrease the time from having an idea to acquiring the supporting data. The scheme will offer monthly proposal submission opportunities, and proposals will be reviewed by the principal investigators or co-investigators of other proposals submitted during the same round. Here, we set out the design of the system and outline the plan for its implementation, leading to the launch of a pilot program at Gemini North in January 2015.

Mason, R E; Kissler-Patig, M; Levenson, N A; Adamson, A; Emmanuel, C; Crabtree, D

2014-01-01T23:59:59.000Z

251

State Lands Management Plan Rosemary Hill Observatory  

E-Print Network (OSTI)

resources . . . . . . . . . 21. Plans for Non-renewable Natural and Cultural Resources . . . . 22 and Improvements . . . . . . . . . 4. Proximity to Significant Public Resources . . . . . . . . . . . 5 RESOURCES . . . . . . . . . . . . . . 8. Resources Listed in the Florida Natural Areas Inventory . . . . 9

Slatton, Clint

252

VLA Technical Memo Smithsonian Astrophysical Observatory  

E-Print Network (OSTI)

. The expansion should result in a significant improvement, that is to say order of magnitude improvement the expansion. The memo also shows how eye chart style images and familiar terrestrial scenes can be used this gap, the new antennas should expand the VLA outward beyond the A array in order to improve the highest

Groppi, Christopher

253

A Christmas Visit to Ben Nevis Observatory  

Science Journals Connector (OSTI)

... the mist into the brightest of daylight. Overhead the sky was blue, a fresh light breeze was blowing, and the reflected sunlight was shining in silvery masses on the ... watching the observers at work, in dining (which we did very comfortably off the Christmas cheer, viz. roast turkey and plum pudding, provided for the inhabitants of Ben ...

G. CHRYSTAL

1884-01-03T23:59:59.000Z

254

NATIONAL RADIO ASTRONOMY OBSERVATORY CHARLOTTESVILLE, VIRGINIA  

E-Print Network (OSTI)

No. 186 A PROGRESS REPORT ON JOSEPHSON JUNCTION MIXERS FOR MILLIMETER WAVE RADIO ASTRONOMY D. R. DECKER FEBRUARY 1978 NUMBER OF COPIES: 150 #12;A PROGRESS REPORT ON JOSEPHSON JUNCTION MIXERS FOR MILLIMETER WAVE RADIO ASTRONOMY D. R. Decker ABSTRACT Interest in use of Josephson junction devices

Groppi, Christopher

255

Andrew Wiles Building Radcliffe Observatory Quarter  

E-Print Network (OSTI)

- Orange or Apple £3.20 per litre Soft drinks ­ Coke, Diet Coke, Sprite, Fanta £1.95 each Cake & Pastry

256

The Status of the STACEE Observatory  

E-Print Network (OSTI)

The Solar Tower Atmospheric Cherenkov Effect Experiment (STACEE) is a ground-based instrument designed to study astrophysical sources of gamma radiation in the energy range of 50 to 500 GeV. STACEE uses an array of large heliostat mirrors at the National Solar Thermal Test Facility in Albuquerque, New Mexico, USA. The heliostats are used to collect Cherenkov light produced in gamma-ray air showers. The light is concentrated onto an array of photomultiplier tubes located near the top of a tower. The construction of STACEE started in 1997 and has been completed in 2001. During the 1998-99 observing season, we used a portion of the experiment, STACEE-32, to detect gamma-rays from the Crab Nebula. The completed version of STACEE uses 64 heliostat mirrors, having a total collection area of 2300 m^2. During the last year, we have also installed custom electronics for pulse delay and triggering, and 1 GHz Flash ADCs to read out the photomultiplier tubes. The commissioning of the full STACEE instrument is underway. Preliminary observations and simulation work indicate that STACEE will have an energy threshold below 70 GeV and a reach for extragalactic gamma-ray sources out to redshift of ~1.0. In this paper we describe the design and performance of STACEE.

C. E. Covault; L. M. Boone; D. Bramel; E. Chae; P. Fortin; D. M Gingrich; J. A. Hinton; D. S. Hanna; R. Mukherjee; C. Mueller R. A. Ong; K. Ragan; R. A. Scalzo; D. R. Schuette; C. G. Theoret; D. A. Williams

2001-07-21T23:59:59.000Z

257

The Status of the STACEE Observatory  

E-Print Network (OSTI)

The Solar Tower Atmospheric Cherenkov Effect Experiment (STACEE) is a ground-based instrument designed to study astrophysical sources of gamma radiation in the energy range of 50 to 500 GeV. STACEE uses an array of large heliostat mirrors at the National Solar Thermal Test Facility in Albuquerque, New Mexico, USA. The heliostats are used to collect Cherenkov light produced in gamma-ray air showers. The light is concentrated onto an array of photomultiplier tubes located near the top of a tower. The construction of STACEE started in 1997 and has been completed in 2001. During the 1998-99 observing season, we used a portion of the experiment, STACEE-32, to detect gamma-rays from the Crab Nebula. The completed version of STACEE uses 64 heliostat mirrors, having a total collection area of 2300 m^2. During the last year, we have also installed custom electronics for pulse delay and triggering, and 1 GHz Flash ADCs to read out the photomultiplier tubes. The commissioning of the full STACEE instrument is underway. P...

Covault, C E; Bramel, D A; Chae, E; Fortin, P; Gingrich, D M; Hinton, J A; Hanna, D S; Mukherjee, R; Ong, R A; Ragan, K; Scalzo, R A; Schtte, D R; Theoret, C G; Williams, D A; Mller, C

2001-01-01T23:59:59.000Z

258

ASTRONOMICAL AND PHYSICAL Mr. WILSON'S OBSERVATORY,  

E-Print Network (OSTI)

111 115 ILLUSTRATIONS. Daramoxa ............. frontispiece. Heliostat Facing page 88 The Sun ,, ,, 94. The experiments on the radiation of heat from sun spots were made by means of a large polar heliostat, having

Dworetsky, Mike

259

Recent Progress at the Pierre Auger Observatory  

Science Journals Connector (OSTI)

......design and schedule for the completion of the Auger detector. As...org/admin/DesignReport/index.html . 10) Sommers P. Astropart...design and schedule for the completion of the Auger detector. As...org/admin/DesignReport/index.html) 10) P. Sommers......

Bruce R. Dawson

2003-05-01T23:59:59.000Z

260

Rothney Astrological Observatory (Priddis) Emergency Instructions  

E-Print Network (OSTI)

Security at 403-220-5333 from a safe location Hazardous Materials Spill Only attempt to clean up a spill to an armed assailant, run away from the subject Hide - if you cannot flee, or do not know the location of the shooter, hide in a locked or barricaded room and turn out the lights Fight ­ if confronted by the shooter

de Leon, Alex R.

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


261

The frequency of tropopause-level thick and thin cirrus clouds as observed by CALIPSO and the relationship to relative humidity and outgoing longwave radiation  

E-Print Network (OSTI)

Thick cloud frequencies, in percent, for SON............................................ 52 15 DJF thin cirrus frequencies in colored contours at a) 121-hPa, b) 100-hPa, and c) 82-hPa with OLR values of 230 W-m-2 in black... contours......................................................................................... 53 16 MAM thin cirrus frequencies in colored contours at a) 121-hPa, b) 100-hPa, and c) 82-hPa with OLR values of 230 W-m-2...

Cardona, Allison Leanne

2008-10-10T23:59:59.000Z

262

Présentation PowerPoint  

NLE Websites -- All DOE Office Websites (Extended Search)

Cirrus cloud Cirrus cloud radiative radiative forcing forcing Cirrus cloud Cirrus cloud radiative radiative forcing forcing on surface on surface - - level shortwave and level shortwave and longwave longwave irradiances irradiances at regional and global scale at regional and global scale M. Haeffelin 1 , J-C. Dupont 1 , C. Long 2 1 Institut Pierre et Simon Laplace, Ecole Polytechnique/CNRS, France 2 Pacific Northwest National Laboratory, Richland WA, USA The authors acknowledge the US ARM program, the IPSL observatories and the NASA/CNES CALIPSO and NASA/AIRS programs for providing the data used in this study. We thank the Centre National d'Etudes Spatiales (CNES) and Centre National de la Recherche Scientifique (CNRS) for their support in this study. 19th ARM Science Team Meeting 1 Apr 2009 0 25 50 75 (%) Stubenrauch et al. (2006)

263

Mobile Climate Observatory for Atmospheric Aerosols in India  

NLE Websites -- All DOE Office Websites (Extended Search)

Atmospheric Aerosols in India Atmospheric Aerosols in India Nainital, India, was the site chosen for deployment of a portable climate research laboratory to study how aerosols impact clouds and energy transfer in the atmosphere. The well-being of hundreds of millions of residents in northeastern India depends on the fertile land around the Ganges River, which is fed by monsoon rains and runoff from the nearby Himalayan Mountains. Any disturbance to the monsoon rains could threaten the population. In the same region, increased industrial activities due to economic growth are releasing small aerosol particles, such as soot and dust, that absorb and scatter sunlight and thus can change cloud formation processes and the heat distribution in the atmosphere. Such changes could greatly increase or

264

NATIONAL RADIO ASTRONOMY OBSERVATORY GREEN BANK, W ES  

E-Print Network (OSTI)

. For the material to emit a minimal amount of radiation to the cold station it should be at a low temperature, which implies that the thermal conductivity should be high so that the center of the filter is not significantly is an important issue. This note describes the selection procedures for materials, the thermal design

Groppi, Christopher

265

NATIONAL RADIO ASTRONOMY OBSERVATORY GREEN BANK, WEST VIRGINIA  

E-Print Network (OSTI)

with the 9862A plotter. Some typical results for the 140-foot and 300-foot telescope are given at the end100 G(0) sin 0 de 0 #12;3 where 0 = feed look angle from antenna axis. G(0) = power pattern of feed

Groppi, Christopher

266

. CondonAuthor(s NATIONAL RADIO ASTRONOMY OBSERVATORY  

E-Print Network (OSTI)

for the 300-foot telescope A simple geometrical/physical model for the 300-foot telescope declination pointing suggests that the declination pointing correction is well represented by the power series AO = C1 + C2-S cross section of the 300-foot telescope. The (x, y) coordinate origin is at its vertex, and the focal

Groppi, Christopher

267

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network (OSTI)

-foot and 140-foot computers. The address that was selected for the A/C input is '0065. To input from into the existing interface wherever it was possible. The address is decoded in slot 14, then power amplified

Groppi, Christopher

268

NATIONAL RADIO ASTRONOMY OBSERVATORY GREEN BANK, WEST VIRGINIA  

E-Print Network (OSTI)

located at the 140 Foot Antenna. The Mark III VLBI station at the 140-foot is being used to process to transmit the IF signals to the 140 Foot Antenna control room, the local oscillator reference signals from the total power for monitoring receiver performance. The X-R and S-R IF signals along with the 500 MHz Local

Groppi, Christopher

269

NATIONAL RADIO ASTRONOMY OBSERVATORY GREEN BANK) WEST VIRGINIA  

E-Print Network (OSTI)

provide monitoring facilities of the 15 V DC and +5 V DC power supplies. #12;45 FOOT TELESCOPE DIGITAL No. 149 NRAO 45-FOOT TELESCOPE DIGITAL POSITION CONTROL AND READOUT SYSTEM J. RAY HALLMAN NOVERMBER 1974 NUMBER OF COPIES: 150 #12;NRAO 45-FOOT TELESCOPE DIGITAL POSITION CONTROL AND READOUT SYSTEM J

Groppi, Christopher

270

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network (OSTI)

.75 and a 30-minute (hail-power width) sidelobe at -22. 5 dia for a 50-foot dish at A = 11 cm, The equations Hoerner [2] to total power reception with parametric amplifiers, we find that the number of detectable sources for 60 fifty-foot paraboloids is .4/ 4 x 10 5 per steradian; assuming 20 arc seconds of resolution

Groppi, Christopher

271

NATIONAL RADIO ASTRONOMY OBSERVATORY GREEN BANK, WEST VIRGINIA  

E-Print Network (OSTI)

range of the 300-foot antenna and minimize the scan loss when compared with a single feed receiver Power and Phase Patterns The computed 2 x 8 array power and phase patterns for 0.0 feet offset from) in a plane thru the long dimension of the array. The power pattern shows a null at about 62 degrees which

Groppi, Christopher

272

NATIONAL RADIO ASTRONOMY OBSERVATORY ELECTRONICS DIVISION INTERNAL REPORT NO. 321  

E-Print Network (OSTI)

in the 5-10 GHz range. The materials tested were: aluminum alloys 1100-T6 and 6061-O, C101 copper used in microwave devices: aluminum alloys 1100-T6 and 6061-O, C101 copper, benzotriazole treated C101, aluminum, benzotriazole. 1 Introduction Input circuit loss is an important factor limiting the sensitivity

Groppi, Christopher

273

A Networked Telerobotic Observatory for Collaborative Remote Observation of Avian  

E-Print Network (OSTI)

, Berkeley, California Welder Wildlife Foundation, Sinton, Texas Smithsonian National Zoological Park. Sinton, Texas (28E6'51.1" N, 97E25'2.2" W). The region in which the refuge is located has the highest

Goldberg, Ken

274

The Magdalena Ridge Observatory interferometer: 2014 status update  

E-Print Network (OSTI)

the full complement of 10 telescope beams of the MROI. The design enables ICoNN to detect and track the interferometer fringe phase at either the H or Ks infrared bandpasses for any distribution of neighboring telescopes. It is a dedicated fringe... -mechanical stability even when tested in a university laboratory environment with no temperature or vibration control. Previous proceedings (Jurgenson et al. 2008 and McCracken et al. 2012, Santoro et al. 2012) have detailed the design and plans for laboratory...

Creech-Eakman, M. J.; Romero, V.; Payne, I.; Haniff, C. A.; Buscher, D. F.; Dahl, C.; Farris, A.; Fisher, M.; Jurgenson, C.; Klinglesmith, D.; McCracken, T.; Napolitano, M.; Olivares, A.; Riker, J.; Rochelle, S.; Salcido, C.; Santoro, F.; Schmidt, L.; Selina, R.; Seneta, E. B.; Shtromberg, A.; Sun, X.; Wilson, D. M. A.; Young, J. S.

2014-07-24T23:59:59.000Z

275

Los Alamos observatory fingers cosmic ray 'hot spots'  

NLE Websites -- All DOE Office Websites (Extended Search)

as a backdrop to research and innovation covering multi-disciplines from bioscience, sustainable energy sources, to plasma physics and new materials. Los Alamos National Laboratory...

276

Operations of and Future Plans Pierre Auger Observatory  

E-Print Network (OSTI)

. B¨acker42 , D. Badagnani6 , K.B. Barber11 , A.F. Barbosa14 , S.L.C. Barroso20 , B. Baughman92 , P

277

The Anglo-Australian Observatory 2dF facility  

Science Journals Connector (OSTI)

......corrector design. The prism material is a high refractive...the observations. 7 Diagram showing design of fibre...button handles. The handling of the fibre probes...a sheet of magnetic material which was then mounted...Hertzsprung-Russell diagram. This can be compared......

I. J. Lewis; R. D. Cannon; K. Taylor; K. Glazebrook; J. A. Bailey; I. K. Baldry; J. R. Barton; T. J. Bridges; G. B. Dalton; T. J. Farrell; P. M. Gray; A. Lankshear; C. McCowage; I. R. Parry; R. M. Sharples; K. Shortridge; G. A. Smith; J. Stevenson; J. O. Straede; L. G. Waller; J. D. Whittard; J. K. Wilcox; K. C. Willis

2002-06-21T23:59:59.000Z

278

Future development of the PLATO observatory for Antarctic science  

E-Print Network (OSTI)

.5­1 kW of continuous electrical power for a year from diesel engines running on Jet-A1, supplemented during the summertime with solar panels. One of the 10-foot shipping containers houses the power system, include a more modular design, using lithium iron-phosphate batteries, higher power output, and a light

Ashley, Michael C. B.

279

CUORE: A Cryogenic Underground Observatory for Rare Events  

E-Print Network (OSTI)

Recently, neutrino oscillation experiments have unequivocally demonstrated that neutrinos have mass and mix. These experiments have yielded valuable information on the mixing angles and on the mass differences of the three eigenstates but cannot determine the scale of the neutrino mass, which is fixed by the lightest neutrino mass eigenvalue. This can only be directly determined by kinematic measurementsor by the observation and measurement of the neutrinoless double-beta decay (NDBD) half-life. The CUORE experiment is designed with a sensitivity capable of probing the range indicated by oscillation experiments. It consists of an array of 988, 750 g, TeO2 bolometers operating at 8 to 10 mK and arranged in a cylindrical geometry of 19 towers hanging on the bottom of the mixing chamber of a dilution refrigerator. Each tower consists of 13 4-detector modules for a total of 52 bolometers. One such tower has been successfully constructed and is now operated in the Gran Sasso Laboratory as a test experiment, and also as an independent NDBD experiment called CUORICINO. In fact, the 3 year half-life sensitivity of CUORICINO for NDBD decay of 130Te is 6.1E24 years. Thus far the CUORICINO data demonstrate the technical feasibility of the expanded CUORE array while showing what and where the sources of background are and how to reduce them. A background reduction to 0.01 counts/keV/kg/y in the NDBD energy region is therefore possible. This would allow the full CUORE array to achieve a 5-year sensitivity of the order of 30 meV on the effective neutrino mass. Another order of magnitude reduction (corresponding to a sensitivity of about 15 meV) will present a real challenge, but is also possible. The CUORE experiment will be installed in the Laboratori Nazionali del Gran Sasso (LNGS) in Assergi, Italy.

R. Ardito

2005-01-06T23:59:59.000Z

280

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network (OSTI)

No 101 THE 108-CHANNEL MULTIPLEXER FOR USE WITH THE HONEYWELL 316 SPECTRAL LINE PROCESSOR John M. Payne WITH THE HONEYWELL 316 SPECTRAL LINE PROCESSOR John M. Payne TABLE OF CONTENTS Page 1 2. 0 Mode of Operation O 0 0 to the Honeywell 316 11 Reference Generator Block Diagram 12 Reference Generator Circuit Diagram #12;THE 108

Groppi, Christopher

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


281

New Approaches in Embedded Networked Sensing for Terrestrial Ecological Observatories  

E-Print Network (OSTI)

within a montane mixed- conifer forests, we ask the questionmontane mixed conifer and oak forest, mon- tane chaparral,

2007-01-01T23:59:59.000Z

282

Building Virtual Earth Observatories using Ontologies, Linked Geospatial Data and  

E-Print Network (OSTI)

and Kapodistrian University of Athens, Greece koubarak@di.uoa.gr 2 German Aerospace Center (DLR), Germany Abstract. Advances in remote sensing technologies have allowed us to send an ever-increasing number of satellites science and application do- mains (environment, oceanography, geology, archaeology, security, etc

Koubarakis, Manolis

283

NATIONAL RADIO ASTRONOMY OBSERVATORY GREEN BANK, WEST VIRGINIA  

E-Print Network (OSTI)

was then built using Ferroxcube 387 material that measured 0.22 ps/°C, an order of magnitude better than the best for chart recorder scale factor. The coarse phase offset switch permits full phase rotation in 10 ns (18

Groppi, Christopher

284

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network (OSTI)

level is reliable with power levels accurate to approximately an order of magnitude. The case .............................................................................................. 1 2, Frequency Spectrum Charts

Groppi, Christopher

285

GOVERNORS OF ARMAGH OBSERVATORY AND PLANETARIUM Employment Application Form  

E-Print Network (OSTI)

Assistant -- Solar Physics Please complete all sections of the form in full and return it by the specified: 5. References. Give the name, title and address of each referee, and the capacity in which you: . . . . . . . . . . . . . . . . . . . . . . . . FAX: . . . . . . . . . . . . . . . . . . . . . . . . Capacity

286

GOVERNORS OF ARMAGH OBSERVATORY AND PLANETARIUM Employment Application Form  

E-Print Network (OSTI)

-- Solar Physics Please complete all sections of the form in full and return it by the specified closing, and the capacity in which you are known to them. It is your responsibility to ensure that at least two and no more: . . . . . . . . . . . . . . . . . . . . . . . . FAX: . . . . . . . . . . . . . . . . . . . . . . . . Capacity: . . . . . . . . . . . . . . . . . .

287

LOFT: the Large Observatory For X-ray Timing  

E-Print Network (OSTI)

The LOFT mission concept is one of four candidates selected by ESA for the M3 launch opportunity as Medium Size missions of the Cosmic Vision programme. The launch window is currently planned for between 2022 and 2024. ...

Chakrabarty, Deepto

288

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network (OSTI)

of RF signals over the 10 MHz to 1000 MHz band. The units used are General Optronics Corporation model the noise from the transmitters the reflections in the fiber transmission must be low. General Optronics had

Groppi, Christopher

289

NATIONAL RADIO ASTRONOMY OBSERVATORY ELECTRONICS DIVISION TECHNICAL NOTE NO. 97  

E-Print Network (OSTI)

Load Temperature (Kelvins) A is the Receiver Power Out Hot Load On (watts) B is the Receiver Power Out Cold Load On (watts) and D is the Receiver Power Out Cold Load + Cal On (watts). #12;The calibration prints a list of the file numbers and the associated alpha-numeric identification; (2) LOAD DATA FILE

Groppi, Christopher

290

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network (OSTI)

as shown in Figure L The feed is constructed with the 307 cm horn centered in the 11 cm horn. Di- electric-band and S-band sweep signal generators are provided to measure paramp gain, The model numbers, manufacturers. The local oscillator system minimizes the phase changes due to cable temperature variations and maintains

Groppi, Christopher

291

NATIONAL RADIO ASTRONOMY OBSERVATORY GREEN BANK, WEST VIRGINIA  

E-Print Network (OSTI)

NO. 147 Title: EVALUATION OF EDM FOR SMALL WAVEGUIDE FABRICATION Author(s): A. R. Kerr, J. W. Lamb, N. Srikanth M. Crawford N. Horner VLA VLA Library P. Napier J. Campbell W. Brundage #12;EVALUATION OF EDM Discharge Machining has a number of attractive features as a procedure for fabricating short sections

Groppi, Christopher

292

National Radio Astronomy Observatory Green Bank Science Center  

E-Print Network (OSTI)

:Thanksgiving Day, Friday after Thanksgiving, Christmas Eve, Christmas Day, New Years Eve, New Years Day, and Easter that makes it difficult to do radio astronomy. Find out more! Find out how bad light pollution is in your

Groppi, Christopher

293

Last of NASA's Great Observatories flies the nest  

Science Journals Connector (OSTI)

... SIRTF should blast off on a Boeing Delta 2 rocket from Cape Canaveral, Florida, at 05:35 GMT on 25 August ...

Joanne Baker

2003-08-23T23:59:59.000Z

294

The observatory : designing data-driven decision making tools  

E-Print Network (OSTI)

Creative usages of graphics to encode information date back to at least the beginnings of the industrial revolution. It is also around that same time that a gap between the wealthiest of nations and least begins to develop. ...

Simoes, Alexander James Gaspar

2012-01-01T23:59:59.000Z

295

Education and public outreach of the Pierre Auger Observatory  

SciTech Connect

The Auger collaboration's broad mission in education, outreach and public relations is coordinated in a separate task. Its goals are to encourage and support a wide range of outreach efforts that link schools and the public with the Auger scientists and the science of cosmic rays, particle physics, and associated technologies. This report focuses on recent activities and future initiatives.

Garcia, B.; /Natl. Tech. U., San Rafael; Snow, G.

2005-08-01T23:59:59.000Z

296

New Approaches in Embedded Networked Sensing for Terrestrial Ecological Observatories  

E-Print Network (OSTI)

and solar radiation are detected, or as soil sensors andsensors; and (3) untethered fixed nodes are battery-powered, solar-solar and thermal radiation values at the soil surface. Currently, the number and types of sensors and

2007-01-01T23:59:59.000Z

297

NATIONAL RADIO ASTRONOMY OBSERVATORY GREEN BANK, WEST VIRGINIA  

E-Print Network (OSTI)

information on the cooled ortho-mode transition, and Section IV contains drawings, schematics, and wiring, designed for mounting in the prime focus Sterling mount. The FEB is equipped with eight thermoelectric- tor/control chassis, four RF modules, and six printed circuit card slots. The feeds are dual mode

Groppi, Christopher

298

A realtime observatory for laboratory simulation of planetary flows  

E-Print Network (OSTI)

Motivated by the large-scale circulation of the atmosphere and ocean, we develop a system that uses

Ravela, Srinivas (Sai)

299

Lamont Doherty Earth Observatory General Administration Human Resources  

E-Print Network (OSTI)

Manager, Purchasing Karen Hoffer Manager, Safety, Security, Communications & Property Howard Matza Leonard Sullivan Support Staff - 10 Officers - 3Asst. Manager, Safety & Security Cathy Troutman Night Supervisor Stephen Weinstein Support Staff - 1 Analyst/Buyer Bonnie Deutsch Support Staff - 1 Officer - 1

Khatiwala, Samar

300

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network (OSTI)

of the unit. The time word is in BCD, and contains tens and units of hours, tens and units of minutes storage unit is shown in Figure III. Time is taken from the BCD outputs of the NRAO sidereal clock or code, date, time, telescope position and frequency. Other required parameters may be recorded by using

Groppi, Christopher

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


301

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia,  

E-Print Network (OSTI)

the projection display on the console. The 10 line decimal code is converted to BCD 1-2-4-8 code for recording for the operator and electrical Binary Coded Decimal position data is available for recordi.ng. Auto- matic gray) code. See Digital Drawing DL-750 The excess codes are converted to 10 line decimal code to drive

Groppi, Christopher

302

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network (OSTI)

to provide binary-coded-decimal (BCD) time signals at each telescope. 1. Use a standard oscillator at each telescope to provide the BCD signals. This syt m has the advantage that only a few signals at the central location. The counter provides BCD signals. The counter (clock) BCD outputs are transmitted to all

Groppi, Christopher

303

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network (OSTI)

was chosen and thus noise on the BCD data lines causes only a temporary error. General Binary Coded Decimal Standard Identification Data is recorded as Binary Coded Decimal numbers. A standard frequency could location and the Binary-Coded Deci- mal Time Signals transmitted to the scopes. The second system

Groppi, Christopher

304

The Anglo-Australian Observatory's 2dF Facility  

E-Print Network (OSTI)

The 2dF (Two-degree Field) facility at the prime focus of the Anglo-Australian Telescope provides multiple object spectroscopy over a 2 degree field of view. Up to 400 target fibres can be independently positioned by a complex robot. Two spectrographs provide spectra with resolutions of between 500 and 2000, over wavelength ranges of 440nm and 110nm respectively. The 2dF facility began routine observations in 1997. 2dF was designed primarily for galaxy redshift surveys and has a number of innovative features. The large corrector lens incorporates an atmospheric dispersion compensator, essential for wide wavelength coverage with small diameter fibres. The instrument has two full sets of fibres on separate field plates, so that re-configuring can be done in parallel with observing. The robot positioner places one fibre every 6 seconds, to a precision of 0.3 arcsec (20micron) over the full field. All components of 2dF, including the spectrographs, are mounted on a 5-m diameter telescope top-end ring for ease of handling and to keep the optical fibres short in order to maximise UV throughput . There is a pipeline data reduction system which allows each data set to be fully analysed while the next field is being observed. In this paper we provide the historical background to the 2dF facility, the design philosophy, a full technical description and a summary of the performance of the instrument. We also briefly review its scientific applications and possible future developments.

I. J. Lewis; R. D. Cannon; K. Taylor; K. Glazebrook; J. A. Bailey; I. K. Baldry; J. R. Barton; T. J. Bridges; G. B. Dalton; T. J. Farrell; P. M. Gray; A. Lankshear; C. McCowage; I. R. Parry; R. M. Sharples; K. Shortridge; G. A. Smith; J. Stevenson; J. O. Straede; L. G. Waller; J. D. Whittard; J. K. Wilcox; K. C. Willis

2002-02-08T23:59:59.000Z

305

NATIONAL RADIO ASTRONOMY OBSERVATORY GREEN BANK, WEST VIRGINIA  

E-Print Network (OSTI)

- - - - - - - - - - - - - - 3 Memory (RAM) Detail - - - - - - - - - - - - - - - - - - - - - 6 3 ROM Memory Map in ROM 10A - - - - - - - - - 61 6 Default Digital Output Locations in ROM 10A - - - - - - - - - 63 TEST initializes FEDAL analog outputs to 0 V and digital outputs to default values specified in ROM. It then tests

Groppi, Christopher

306

NATIONAL RADIO ASTRONOMY OBSERVATORY GREEN BANK/ WEST VIRGINIA  

E-Print Network (OSTI)

Instrumentation Chassis Constant Current FET Supply for 10A Control Room Monitor and Control Chassis Front 10B H. BEHRENS) FEBRUARY 1981 NUMBER OF COPIES: 150 #12;C-Band Noise Temperature Measur L -Band Noise Temperature Measurements Operating Voltages for GaAs FET Amplifiers Measured Noise Temperatures and Noise

Groppi, Christopher

307

NATIONAL RADIO ASTRONOMY OBSERVATORY GREEN BANK WEST VIRGINIA  

E-Print Network (OSTI)

sockets for the op amp and detector diode, provide a new input amplifier and to eliminate ground and power This report covers the new 256-channel, 2 MHz per channel, filter system, an updated version of the systems in the back panel. This sig- nal also changes the digital card to accommodate the inverted channel counting

Groppi, Christopher

308

Historic Sudbury Neutrino Observatory Data, Carried by ESnet...  

NLE Websites -- All DOE Office Websites (Extended Search)

Sun) to muon or tau neutrinos. In 2001, Science Magazine identified SNO's solution to the solar neutrino mystery as one of their 10 science breakthroughs of the year. "SNO data...

309

Radiosonde campaign in Paranal Observatory 2011: PWV measurement.  

E-Print Network (OSTI)

Aeronautica Civil) worked without problems. The launching zone was on the satellite communication antenna the warning zone and the two cases aborted were affected by these, because the wind directions

310

Milagro all-sky TeV gamma ray observatory.  

SciTech Connect

Milagro is a water Cherenkov telescope sensitive to gamma rays with energies above 100 GeV. Unlike air-Cherenkov telescopes, Milagro continuously views the entire overhead sky. This capability makes it well suited to search for transient phenomena such as gamma-ray bursts and to discover new phenomena. I will review the design and construction of Milagro, detail the sensitivity of the instrument, including a discussion of background rejection with Milagro. Recent and ongoing upgrades to the instrument are discussed. The paper concludes with a summary of some recent physics results with Milagro.

Sinnis, C. (Constantine)

2002-01-01T23:59:59.000Z

311

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network (OSTI)

capacity, which should make for less expensive operating costs. #12;1. Introduction The National Radio to the conduction through the hydrogen heat switch, conduction in the JT structure, and radiative loading. #12;H =7 .,_. valve .53 / I \\\\., low p IP, L___. valve \\ compressor gas volumes It is clear that if an initial

Groppi, Christopher

312

Beamline 9.3.1  

NLE Websites -- All DOE Office Websites (Extended Search)

1 Print 1 Print Atomic, molecular, and materials science Endstations: X-ray absorption endstation Polarized-x-ray emission spectrometer Magnetic mass spectrometer Liquid cell endstation GENERAL BEAMLINE INFORMATION Operational Yes, but not open to users Source characteristics Bend magnet Energy range 2320eV-5600eV Monochromator Double Si(111) crystal Measured flux (1.9 GeV, 300 mA) 1011 photons/s Resolving power (E/ΔE) 3000-8000 Beam size Adjustable with 2nd mirror Focused: 1.0 mm x 0.7 mm (~0.5 mm square at 2800 eV) Unfocused: 10 mm x 10 mm or larger Endstations X-ray absorption endstation Polarized-x-ray emission spectrometer Magnetic mass spectrometer Liquid cell endstation Local contact Wayne Stolte Advanced Light Source, Berkeley Lab Phone: (510) 486-5804 Fax: (510) 495-2111

313

Beamline 9.3.1  

NLE Websites -- All DOE Office Websites (Extended Search)

1 Print 1 Print Atomic, molecular, and materials science Endstations: X-ray absorption endstation Polarized-x-ray emission spectrometer Magnetic mass spectrometer Liquid cell endstation GENERAL BEAMLINE INFORMATION Operational Yes, but not open to users Source characteristics Bend magnet Energy range 2320eV-5600eV Monochromator Double Si(111) crystal Measured flux (1.9 GeV, 300 mA) 1011 photons/s Resolving power (E/ΔE) 3000-8000 Beam size Adjustable with 2nd mirror Focused: 1.0 mm x 0.7 mm (~0.5 mm square at 2800 eV) Unfocused: 10 mm x 10 mm or larger Endstations X-ray absorption endstation Polarized-x-ray emission spectrometer Magnetic mass spectrometer Liquid cell endstation Local contact Wayne Stolte Advanced Light Source, Berkeley Lab Phone: (510) 486-5804 Fax: (510) 495-2111

314

Beamline 9.3.1  

NLE Websites -- All DOE Office Websites (Extended Search)

1 Print 1 Print Atomic, molecular, and materials science Endstations: X-ray absorption endstation Polarized-x-ray emission spectrometer Magnetic mass spectrometer Liquid cell endstation GENERAL BEAMLINE INFORMATION Operational Yes, but not open to users Source characteristics Bend magnet Energy range 2320eV-5600eV Monochromator Double Si(111) crystal Measured flux (1.9 GeV, 300 mA) 1011 photons/s Resolving power (E/ΔE) 3000-8000 Beam size Adjustable with 2nd mirror Focused: 1.0 mm x 0.7 mm (~0.5 mm square at 2800 eV) Unfocused: 10 mm x 10 mm or larger Endstations X-ray absorption endstation Polarized-x-ray emission spectrometer Magnetic mass spectrometer Liquid cell endstation Local contact Wayne Stolte Advanced Light Source, Berkeley Lab Phone: (510) 486-5804 Fax: (510) 495-2111

315

Beamline 9.3.1  

NLE Websites -- All DOE Office Websites (Extended Search)

1 Print 1 Print Atomic, molecular, and materials science Endstations: X-ray absorption endstation Polarized-x-ray emission spectrometer Magnetic mass spectrometer Liquid cell endstation GENERAL BEAMLINE INFORMATION Operational Yes, but not open to users Source characteristics Bend magnet Energy range 2320eV-5600eV Monochromator Double Si(111) crystal Measured flux (1.9 GeV, 300 mA) 1011 photons/s Resolving power (E/ΔE) 3000-8000 Beam size Adjustable with 2nd mirror Focused: 1.0 mm x 0.7 mm (~0.5 mm square at 2800 eV) Unfocused: 10 mm x 10 mm or larger Endstations X-ray absorption endstation Polarized-x-ray emission spectrometer Magnetic mass spectrometer Liquid cell endstation Local contact Wayne Stolte Advanced Light Source, Berkeley Lab Phone: (510) 486-5804 Fax: (510) 495-2111

316

Y.Takeuchi (Y.Takeuchi (KamiokaKamioka Observatory, ICRR)Observatory, ICRR) Radon workshop @ NEUTRINO 2000  

E-Print Network (OSTI)

for water950L for water ·· RnRn--lessless--airair supply systemsupply system ·· Water purification systemWater·Covered with MINEGUARD ·supply fresh air from outside mine (10m3/h) Water purificationWater purification systemsystem Rn (stainless steel) water (+50mmAq) 60cm SK dome air #12;Water purification systemWater purification system

Takeuchi, Yasuo

317

Center for Nanophase Materials Sciences (CNMS) - CNMS Research  

NLE Websites -- All DOE Office Websites (Extended Search)

Emerges From Ongoing Computational Nanoscience Endstation Effort Achievement: A team led by Thomas Schulthess, including Gonzalo Alvarez, Mike Summers, Thomas Maier, and Paul...

318

Microsoft Word - NERSCplan-final7a.docx  

NLE Websites -- All DOE Office Websites (Extended Search)

Endstation computationalists 3 Tactical data planning in situ with small teams Boots on the ground at DOE facilities (BES beamlines, benchtops, and detector labs). NERSC...

319

General User Proposals  

NLE Websites -- All DOE Office Websites (Extended Search)

Proposals Print General Users are granted beam time through a peer review proposal process. They may use beamlines and endstations provided by the ALS or the Participating Research...

320

General User Proposals  

NLE Websites -- All DOE Office Websites (Extended Search)

General User Proposals Print General Users are granted beam time through a peer review proposal process. They may use beamlines and endstations provided by the ALS or the...

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


321

General User Proposals  

NLE Websites -- All DOE Office Websites (Extended Search)

Office General User Proposals Print General Users are granted beam time through a peer review proposal process. They may use beamlines and endstations provided by the ALS...

322

Microsoft PowerPoint - Mace_Poster_ARM-ATrain_Comparison [Compatibilit...  

NLE Websites -- All DOE Office Websites (Extended Search)

p Jay Mace Sally Benson Jay Mace, Sally Benson y , y Contributions from: Roger Marchand (Cloudsat mask) Mark Vaughn (CALIPSO Mask) Eugene Clothiaux (MMCR mask) Contributions...

323

Beamline 7.0.1  

NLE Websites -- All DOE Office Websites (Extended Search)

0.1 Print 0.1 Print Surface and Materials Science, Spectromicroscopy Scientific disciplines: Correlated electron system, materials science Endstations: nanoARPES (nARPES) Electronic Structure Factory (ESF) Advanced x-ray inelastic scattering (AXIS) GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics 5-cm period undulator (U5) (first, third, and fifth harmonics) Energy range See endstation tables Monochromator See endstation tables Scientific disciplines Correlated electron system, materials science Website Beamline 7: http://www-bl7.lbl.gov/ ENDSTATION INFORMATION Endstation name nanoARPES Operational This instrument is currently under development. Expected user operation in 2012. For consideration, speak to the beamline scientist before applying for beamtime.

324

Beamline 7.0.1  

NLE Websites -- All DOE Office Websites (Extended Search)

0.1 Print 0.1 Print Surface and Materials Science, Spectromicroscopy Scientific disciplines: Correlated electron system, materials science Endstations: nanoARPES (nARPES) Electronic Structure Factory (ESF) Advanced x-ray inelastic scattering (AXIS) GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics 5-cm period undulator (U5) (first, third, and fifth harmonics) Energy range See endstation tables Monochromator See endstation tables Scientific disciplines Correlated electron system, materials science Website Beamline 7: http://www-bl7.lbl.gov/ ENDSTATION INFORMATION Endstation name nanoARPES Operational This instrument is currently under development. Expected user operation in 2012. For consideration, speak to the beamline scientist before applying for beamtime.

325

Beamline 7.0.1  

NLE Websites -- All DOE Office Websites (Extended Search)

0.1 Print 0.1 Print Surface and Materials Science, Spectromicroscopy Scientific disciplines: Correlated electron system, materials science Endstations: nanoARPES (nARPES) Electronic Structure Factory (ESF) Advanced x-ray inelastic scattering (AXIS) GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics 5-cm period undulator (U5) (first, third, and fifth harmonics) Energy range See endstation tables Monochromator See endstation tables Scientific disciplines Correlated electron system, materials science Website Beamline 7: http://www-bl7.lbl.gov/ ENDSTATION INFORMATION Endstation name nanoARPES Operational This instrument is currently under development. Expected user operation in 2012. For consideration, speak to the beamline scientist before applying for beamtime.

326

Beamline 7.0.1  

NLE Websites -- All DOE Office Websites (Extended Search)

0.1 Print 0.1 Print Surface and Materials Science, Spectromicroscopy Scientific disciplines: Correlated electron system, materials science Endstations: nanoARPES (nARPES) Electronic Structure Factory (ESF) Advanced x-ray inelastic scattering (AXIS) GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics 5-cm period undulator (U5) (first, third, and fifth harmonics) Energy range See endstation tables Monochromator See endstation tables Scientific disciplines Correlated electron system, materials science Website Beamline 7: http://www-bl7.lbl.gov/ ENDSTATION INFORMATION Endstation name nanoARPES Operational This instrument is currently under development. Expected user operation in 2012. For consideration, speak to the beamline scientist before applying for beamtime.

327

Beamline 7.0.1  

NLE Websites -- All DOE Office Websites (Extended Search)

7.0.1 Print 7.0.1 Print Surface and Materials Science, Spectromicroscopy Scientific disciplines: Correlated electron system, materials science Endstations: nanoARPES (nARPES) Electronic Structure Factory (ESF) Advanced x-ray inelastic scattering (AXIS) GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics 5-cm period undulator (U5) (first, third, and fifth harmonics) Energy range See endstation tables Monochromator See endstation tables Scientific disciplines Correlated electron system, materials science Website Beamline 7: http://www-bl7.lbl.gov/ ENDSTATION INFORMATION Endstation name nanoARPES Operational This instrument is currently under development. Expected user operation in 2012. For consideration, speak to the beamline scientist before applying for beamtime.

328

Beamline 7.0.1  

NLE Websites -- All DOE Office Websites (Extended Search)

0.1 Print 0.1 Print Surface and Materials Science, Spectromicroscopy Scientific disciplines: Correlated electron system, materials science Endstations: nanoARPES (nARPES) Electronic Structure Factory (ESF) Advanced x-ray inelastic scattering (AXIS) GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics 5-cm period undulator (U5) (first, third, and fifth harmonics) Energy range See endstation tables Monochromator See endstation tables Scientific disciplines Correlated electron system, materials science Website Beamline 7: http://www-bl7.lbl.gov/ ENDSTATION INFORMATION Endstation name nanoARPES Operational This instrument is currently under development. Expected user operation in 2012. For consideration, speak to the beamline scientist before applying for beamtime.

329

Beamline 7.0.1  

NLE Websites -- All DOE Office Websites (Extended Search)

0.1 Print 0.1 Print Surface and Materials Science, Spectromicroscopy Scientific disciplines: Correlated electron system, materials science Endstations: nanoARPES (nARPES) Electronic Structure Factory (ESF) Advanced x-ray inelastic scattering (AXIS) GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics 5-cm period undulator (U5) (first, third, and fifth harmonics) Energy range See endstation tables Monochromator See endstation tables Scientific disciplines Correlated electron system, materials science Website Beamline 7: http://www-bl7.lbl.gov/ ENDSTATION INFORMATION Endstation name nanoARPES Operational This instrument is currently under development. Expected user operation in 2012. For consideration, speak to the beamline scientist before applying for beamtime.

330

Hanford tanks initiative alternatives generation and analysis plan for AX tank farm closure basis  

SciTech Connect

The purpose of this document is: (1) to review the HTI Mission Analysis and related documents to determine their suitability for use in developing performance measures for AX Tank Farm closure, (2) to determine the completeness and representativeness of selected alternative closure scenarios, (3) to determine the completeness of current plans for development of tank end-state criteria, and (4) to analyze the activities that are necessary and sufficient to recommend the end-state criteria and performance measures for the AX Tank Farm and recommend activities not currently planned to support establishment of its end-state criteria.

Schaus, P.S., Westinghouse Hanford, Richland, WA

1997-10-22T23:59:59.000Z

331

Beamline 12.0.1  

NLE Websites -- All DOE Office Websites (Extended Search)

2.0.1 Print 2.0.1 Print EUV optics testing and interferometry, angle- and spin-resolved photoemission Scientific discipline: Applied science, correlated electron systems Endstations: Angle- and spin-resolved photoemission (12.0.1.1) Berkeley Dose Calibration Tool (DCT)(12.0.1.2) SEMATECH Berkeley Microfield Exposure Tool (MET) (12.0.1.3) GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics 8-cm-period undulator (U8) Energy range See endstation tables Monochromator See endstation tables Endstations Angle- and spin-resolved photoemission (12.0.1.1) SEMATECH Berkeley Microfield Exposure Tool (MET) (12.0.1.2) Berkeley Dose Calibration Tool (DCT)(12.0.1.3) Beamline phone numbers (510) 495-2121 (12.0.1.1)

332

Beamline 12.0.1  

NLE Websites -- All DOE Office Websites (Extended Search)

2.0.1 Print 2.0.1 Print EUV optics testing and interferometry, angle- and spin-resolved photoemission Scientific discipline: Applied science, correlated electron systems Endstations: Angle- and spin-resolved photoemission (12.0.1.1) Berkeley Dose Calibration Tool (DCT)(12.0.1.2) SEMATECH Berkeley Microfield Exposure Tool (MET) (12.0.1.3) GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics 8-cm-period undulator (U8) Energy range See endstation tables Monochromator See endstation tables Endstations Angle- and spin-resolved photoemission (12.0.1.1) SEMATECH Berkeley Microfield Exposure Tool (MET) (12.0.1.2) Berkeley Dose Calibration Tool (DCT)(12.0.1.3) Beamline phone numbers (510) 495-2121 (12.0.1.1)

333

Beamline 12.0.1  

NLE Websites -- All DOE Office Websites (Extended Search)

2.0.1 Print 2.0.1 Print EUV optics testing and interferometry, angle- and spin-resolved photoemission Scientific discipline: Applied science, correlated electron systems Endstations: Angle- and spin-resolved photoemission (12.0.1.1) Berkeley Dose Calibration Tool (DCT)(12.0.1.2) SEMATECH Berkeley Microfield Exposure Tool (MET) (12.0.1.3) GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics 8-cm-period undulator (U8) Energy range See endstation tables Monochromator See endstation tables Endstations Angle- and spin-resolved photoemission (12.0.1.1) SEMATECH Berkeley Microfield Exposure Tool (MET) (12.0.1.2) Berkeley Dose Calibration Tool (DCT)(12.0.1.3) Beamline phone numbers (510) 495-2121 (12.0.1.1)

334

Beamline 12.0.1  

NLE Websites -- All DOE Office Websites (Extended Search)

2.0.1 Print 2.0.1 Print EUV optics testing and interferometry, angle- and spin-resolved photoemission Scientific discipline: Applied science, correlated electron systems Endstations: Angle- and spin-resolved photoemission (12.0.1.1) Berkeley Dose Calibration Tool (DCT)(12.0.1.2) SEMATECH Berkeley Microfield Exposure Tool (MET) (12.0.1.3) GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics 8-cm-period undulator (U8) Energy range See endstation tables Monochromator See endstation tables Endstations Angle- and spin-resolved photoemission (12.0.1.1) SEMATECH Berkeley Microfield Exposure Tool (MET) (12.0.1.2) Berkeley Dose Calibration Tool (DCT)(12.0.1.3) Beamline phone numbers (510) 495-2121 (12.0.1.1)

335

Beamline 12.0.1  

NLE Websites -- All DOE Office Websites (Extended Search)

2.0.1 Print 2.0.1 Print EUV optics testing and interferometry, angle- and spin-resolved photoemission Scientific discipline: Applied science, correlated electron systems Endstations: Angle- and spin-resolved photoemission (12.0.1.1) Berkeley Dose Calibration Tool (DCT)(12.0.1.2) SEMATECH Berkeley Microfield Exposure Tool (MET) (12.0.1.3) GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics 8-cm-period undulator (U8) Energy range See endstation tables Monochromator See endstation tables Endstations Angle- and spin-resolved photoemission (12.0.1.1) SEMATECH Berkeley Microfield Exposure Tool (MET) (12.0.1.2) Berkeley Dose Calibration Tool (DCT)(12.0.1.3) Beamline phone numbers (510) 495-2121 (12.0.1.1)

336

General User Proposals  

NLE Websites -- All DOE Office Websites (Extended Search)

Proposals Print Tuesday, 01 June 2010 09:36 General Users are granted beam time through a peer review proposal process. They may use beamlines and endstations provided by the ALS...

337

Comparative risk analysis for the Rocky Flats Plant integrated project planning  

SciTech Connect

The Rocky Flats Plant is developing, with active stakeholder a comprehensive planning strategy that will support transition of the Rocky Flats Plant from a nuclear weapons production facility to site cleanup and final disposition. Final disposition of the Rocky Flats Plant materials and contaminants requires consideration of the interrelated nature of sitewide problems, such as material movement and disposition, facility and land use endstates, costs relative risks to workers and the public, and waste disposition. Comparative Risk Analysis employs both incremental risk and cumulative risk evaluations to compare risks from postulated options or endstates. These postulated options or endstates can be various remedial alternatives, or future endstate uses of federal agency land. Currently, there does not exist any approved methodology that aggregates various incremental risk estimates. Comparative Risk Analysis has been developed to aggregate various incremental risk estimates to develop a site cumulative risk estimate. This paper discusses development of the Comparative Risk Analysis methodology, stakeholder participation and lessons learned from these challenges.

Jones, M.E.; Shain, D.I.

1994-05-01T23:59:59.000Z

338

National Radio Astronomy Observatory Measurements of Copper Heat Straps Near 4 K  

E-Print Network (OSTI)

as OFHC. When annealed, these materials have very high thermal conductivity, with a maximum measurements of the thermal resistance of heat straps used in the ALMA Band 6 cartridges. The results suggest the contact area is large (~ 10 cm2 ) but that grease actually increases the thermal resistance when

Groppi, Christopher

339

Magnetic Shear in Two-ribbon Solar Flares M.S., Purple Mountain Observatory (2004)  

E-Print Network (OSTI)

Caughey for his contributions to the research. I also want to thank the other SSXG group members: Dr. Loraine

Su, Yingna

340

Remote sensing-based characterization of plant functional type distributions at the Barrow Environmental Observatory  

SciTech Connect

Arctic ecosystems have been observed to be warming faster than the global average and are predicted to experience accelerated changes in climate due to global warming. Arctic vegetation is particularly sensitive to warming conditions and likely to exhibit shifts in species composition, phenology and productivity under changing climate. Mapping and monitoring of changes in vegetation is essential to understand the effect of climate change on the ecosystem functions. Vegetation exhibits unique spectral characteristics which can be harnessed to discriminate plant types and develop quantitative vegetation indices. We have combined high resolution multi-spectral remote sensing from the WorldView 2 satellite with LIDAR-derived digital elevation models to characterize the tundra landscape on the North Slope of Alaska. Classification of landscape using spectral and topographic characteristics yields spatial regions with expectedly similar vegetation characteristics. A field campaign was conducted during peak growing season to collect vegetation harvests from a number of 1m x 1m plots in the study region, which were then analyzed for distribution of vegetation types in the plots. Statistical relationships were developed between spectral and topographic characteristics and vegetation type distributions at the vegetation plots. These derived relationships were employed to statistically upscale the vegetation distributions for the landscape based on spectral characteristics. Vegetation distributions developed are being used to provide Plant Functional Type (PFT) maps for use in the Community Land Model (CLM).

Kumar, Jitendra; Hoffman, Forrest M.

2014-03-18T23:59:59.000Z

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


341

1225 Observatory Drive, Madison, Wisconsin 53706 608-262-3581 / www.lafollette.wisc.edu  

E-Print Network (OSTI)

://www.lafollette.wisc.edu/publications/workingpapers Credibility, ambition, and discretion in long-term U.S. energy policy targets from 1973 to 2011 Gregory F;Credibility, ambition, and discretion in long-term U.S. energy policy targets from 1973 to 2011 Gregory F, and assimilation of new information. This paper reviews the effectiveness, duration, and ambition of 63 energy

Wisconsin at Madison, University of

342

FIRST MEASUREMENT OF THE FLUX OF SOLAR NEUTRINOS FROM THE SUN AT THE SUDBURY NEUTRINO OBSERVATORY  

E-Print Network (OSTI)

Energy Physics Engineering Group taught me how to work in a lab and how to think critically about making signal relative to the theoretical predictions. Such a con#12;rmation is the #12;rst step in SNO's ambit

Waltham, Chris

343

Position angle of the VSOP antenna feed. National Radio Astronomy Observatory, Socorro, New Mexico, USA  

E-Print Network (OSTI)

, including antenna and solar panels, is shown in Fig. 1. We define a right hand coordinate system fixed about which the solar panels can be rotated. The solar panels are pointed at the Sun by rotation the source and the Sun, there are two possible orientations of the satellite and the solar panels

Groppi, Christopher

344

Operations with the new FUSE observatory: three-axis control with one reaction wheel  

E-Print Network (OSTI)

control system, particularly those of gyroscopes and reaction wheels, have made science operations in all three axes. Jitter values of no more than ±1 arcsecond in pitch, ±10 arcsecond in yaw, and ±1-516-8503; fax 410-516-5494; http://fuse.pha.jhu.edu #12;The FUSE Attitude Control System (ACS) contains two sets

345

Bibliography and citation count of the Lowell Observatory 21 inch telescope,  

E-Print Network (OSTI)

- Johnson, H. L. 1959. On the luminosities of early-type stars. Lowell Obs. Bull., 4, 87 (no. 94) 1- Sinton

Lockwood, Wes

346

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

E-Print Network (OSTI)

studies of the Moon's surface were of much use to the American astronauts who landed on our natural watched Comet Hale-Bopp with it. Calver Telescope The Calver telescope was originally made for an English research interests lie in solar system astronomy and the dynamics of bodies such as comets and asteroids

347

EUROPEAN SOUTHERN OBSERVATORY Organisation Europeene pour des Recherches Astronomiques dans l'Hemisph`ere Austral  

E-Print Network (OSTI)

.2 Bad Pixel Mask ,Master Dark and Master Flat . . . . . . . . . . . . . . . . . . 6 3.2.1 Linearity frames . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 6 3.2.2 Dark frames://www.eso.org/projects/dfs/dfs-shared/web/vlt/vlt-instru

Liske, Jochen

348

E-Print Network 3.0 - aperture grb observatory Sample Search...  

NLE Websites -- All DOE Office Websites (Extended Search)

Collection: Mathematics 8 arXiv:astro-ph9711245v120Nov1997 To be published in "Gamma-Ray Bursts, 4th Huntsville Symposium", 1998, ed. Summary: aperture to the APT, but has a...

349

Undergraduate Honors Research Projects Assessing Flat Field Quality at the University of Maryland Observatory, David Blankenship,  

E-Print Network (OSTI)

Tully-Fisher Relation Using Gas Dominated Galaxies, David V. Stark, (Stacy McGaugh) 2008. Dynamics of Comet Hale-Bopp, Nathaniel Doane (M

Gruner, Daniel S.

350

Physical Models of Sunspots Warsaw University Observatory, Al. Ujazdowskie 4, 00478 Warsaw  

E-Print Network (OSTI)

''. The discovery of the Zeeman splitting of spectral lines in spots by Hale (1908) revealed a new agent which the convective motion of an ionized gas, and this effect has to be taken into account in any explanation

Jahn, Krzysztof

351

Potential solar axion signatures in X-ray observations with the XMMNewton observatory  

Science Journals Connector (OSTI)

......temporally and in terms of the accepted...forward-directed, and enter the field of view...are given of a search for axion-conversion...axions - using the term indiscriminately...magnitude greater, in terms of their product...extensively used to search for the spectral...conversion photons can enter the FOV of XMM-Newton......

G.W. Fraser; A.M. Read; S. Sembay; J.A. Carter; E. Schyns

2014-01-01T23:59:59.000Z

352

Observatory, 125, 2324, 2005 NEGATIVE REPORT OF OCCULTATION BY THE D-TYPE ASTEROID  

E-Print Network (OSTI)

unfavourable weather (heavy rain and wind), the clouds dispersed shortly before the predicted time was caused by exceptionally poor atmospheric `seeing' in the wake of the passing active weather system significant contributions to knowledge in this rapidly advancing field. The Armagh Occultation Team's report

353

The Pointing System of the Herschel Space Observatory. Description, Calibration, Performance and Improvements  

E-Print Network (OSTI)

We present the activities carried out to calibrate and characterise the performance of the elements of attitude control and measurement on board the Herschel spacecraft. The main calibration parameters and the evolution of the indicators of the pointing performance are described, from the initial values derived from the observations carried out in the performance verification phase to those attained in the last year and half of mission, an absolute pointing error around or even below 1 arcsec, a spatial relative pointing error of some 1 arcsec and a pointing stability below 0.2 arsec. The actions carried out at the ground segment to improve the spacecraft pointing measurements are outlined. On-going and future developments towards a final refinement of the Herschel astrometry are also summarised. A brief description of the different components of the attitude control and measurement system (both in the space and in the ground segments) is also given for reference. We stress the importance of the cooperation b...

Snchez-Portal, Miguel; Altieri, Bruno; Aussel, Herv; Feuchtgruber, Helmut; Klaas, Ulrich; Linz, Hendrik; Lutz, Dieter; Mern, Bruno; Mller, Thomas; Nielbock, Markus; Oort, Marc; Pilbratt, Gran; Schmidt, Micha; Stephenson, Craig; Tuttlebee, Mark

2014-01-01T23:59:59.000Z

354

A Bayesian analysis of the 27 highest energy cosmic rays detected by the Pierre Auger Observatory  

Science Journals Connector (OSTI)

......analysis of the 27 highest energy cosmic rays detected by the...is possible that ultrahigh energy cosmic rays (UHECRs) are...is located near Malargue in Argentina, at a longitude of 69.4...UHECRs with reliable detected energies of E obsE min = 5.7 1019......

Laura J. Watson; Daniel J. Mortlock; Andrew H. Jaffe

2011-11-21T23:59:59.000Z

355

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

E-Print Network (OSTI)

Energy Cosmic Rays Using Two Large Air Shower Detectors Mendoza, Argentina (construction underway - 1932 Jakarta Genoa Auger and LePrince-Ringuet sailed between Le Havre and Argentina in 1933 Cosmic Rays are charged particles, the nuclei of atoms. Like the drunken man's walk! BUT the highest energy particles

356

Proceedings of ICRC 2001: 703 c Copernicus Gesellschaft 2001 Layout of the Pierre Auger Observatory  

E-Print Network (OSTI)

. del Libertador 8250, (1429) Buenos Aires, Argentina 2 Observatorio Pierre Auger, Av. San Mart´in Norte 304, (5613) Malarg¨ue, Argentina Abstract. The Pierre Auger Collaboration was formed to study the highest energy cosmic ray showers, focusing the attention on energies above 5·1019 eV. The strong flux sup

357

29th International Cosmic Ray Conference Pune (2005) 00, 101-104 The Pierre Auger Observatory  

E-Print Network (OSTI)

Auger, Av. San Martin Norte 304, 5613 Malarge, Argentina (b) Pierre Auger Collaboration: http was designed for a high statistics, full sky study of cosmic rays at the highest energies. Energy, direction, now under construction in the Province of Mendoza, Argentina, is well over half finished. Active

358

30TH INTERNATIONAL COSMIC RAY CONFERENCE Astrophysics Motivation behind the Pierre Auger Southern Observatory Enhance-  

E-Print Network (OSTI)

Collaboration intends to extend the energy range of its southern observa- tory in Argentina for high quality. San Martn Norte 304, (5613) Malargue, Argentina gmtanco@nucleares.unam.mx Abstract: The Pierre Auger to the highest energies observed. The evolution of the spectrum through the second knee and ankle

359

Fiber scrambling for high-resolution spectrographs. II. A double fiber scrambler for Keck Observatory  

E-Print Network (OSTI)

We have designed a fiber scrambler as a prototype for the Keck HIRES spectrograph, using double scrambling to stabilize illumination of the spectrometer and a pupil slicer to increase spectral resolution to R = 70,000 with minimal slit losses. We find that the spectral line spread function (SLSF) for the double scrambler observations is 18 times more stable than the SLSF for comparable slit observations and 9 times more stable than the SLSF for a single fiber scrambler that we tested in 2010. For the double scrambler test data, we further reduced the radial velocity scatter from an average of 2.1 m/s to 1.5 m/s after adopting a median description of the stabilized SLSF in our Doppler model. This demonstrates that inaccuracies in modeling the SLSF contribute to the velocity RMS. Imperfect knowledge of the SLSF, rather than stellar jitter, sets the precision floor for chromospherically quiet stars analyzed with the iodine technique using Keck HIRES and other slit-fed spectrometers. It is increasingly common pra...

Spronck, Julien F P; Kaplan, Zachary; Jurgenson, Colby; Valenti, Jeff; Moriarty, John; Szymkowiak, Andrew E

2015-01-01T23:59:59.000Z

360

Oceans. Europe2005 An Acoustically-Linked Deep-Ocean Observatory  

E-Print Network (OSTI)

), diesel generator for power, and fiber optic connections to a seafloorjunction box. These =e ideal to communications power efficiency and cost of the acoustic and satellite telemetry systems. The efficiency ship servicing. Solarcells on the buoy provide enough power for many hours of Iridium terminal

Massachusetts at Amherst, University of

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


361

Cryogenic far-infrared laser absorptivity measurements of the Herschel Space Observatory telescope mirror coatings  

Science Journals Connector (OSTI)

Far-infrared laser calorimetry was used to measure the absorptivity, and thus the emissivity, of aluminum-coated silicon carbide mirror samples produced during the coating...

Fischer, Jacqueline; Klaassen, Tjeerd; Hovenier, Niels; Jakob, Gerd; Poglitsch, Albrecht; Sternberg, Oren

2004-01-01T23:59:59.000Z

362

Third Level Trigger for the Fluorescence Telescopes of the Pierre Auger Observatory  

E-Print Network (OSTI)

The trigger system for the Auger fluorescence telescopes is implemented in hard- and software for an efficient selection of fluorescence light tracks induced by high-energy extensive air showers. The algorithm of the third stage uses the multiplicity signal of the hardware for fast rejection of lightning events with above 99% efficiency. In a second step direct muon hits in the camera and random triggers are rejected by analyzing the space-time correlation of the pixels. The trigger algorithm was tested with measured and simulated showers and implemented in the electronics of the fluorescence telescopes. A comparison to a prototype trigger without multiplicity shows the superiority of this approach, e.g. the false rejection rate is a factor 10 lower.

A. Schmidt; T. Asch; H. Gemmeke; M. Kleifges; H. -J. Mathes; A. Menshikov; F. Schssler; D. Tcherniakhovski

2008-08-01T23:59:59.000Z

363

Third Level Trigger for the Fluorescence Telescopes of the Pierre Auger Observatory  

E-Print Network (OSTI)

The trigger system for the Auger fluorescence telescopes is implemented in hard- and software for an efficient selection of fluorescence light tracks induced by high-energy extensive air showers. The algorithm of the third stage uses the multiplicity signal of the hardware for fast rejection of lightning events with above 99% efficiency. In a second step direct muon hits in the camera and random triggers are rejected by analyzing the space-time correlation of the pixels. The trigger algorithm was tested with measured and simulated showers and implemented in the electronics of the fluorescence telescopes. A comparison to a prototype trigger without multiplicity shows the superiority of this approach, e.g. the false rejection rate is a factor 10 lower.

Schmidt, A; Gemmeke, H; Kleifges, M; Mathes, H -J; Menchikov, A; Schssler, F; Tcherniakhovski, D

2008-01-01T23:59:59.000Z

364

.--,' , Meteorological Observatory 11 ,r . / r' . , ',~A.Iv' .',1 '" 7 , " "'(.)7()(} ES'T  

E-Print Network (OSTI)

)c 1.1 35 OF t-.JNvI/ R.H. '1'.:: '1c Ppn. Liq. 1900 24 hr, Mov. mi, Prevo DiL T 'y,. ~\\0'\\\\~p-p-n-.--c~:-4~---~--·~-~~--------~~-------7~~-------i-v~·~is-, ~) 0, in. in. mi. ~!; mi.~5 mi. Vis. tr in. I~M (~ mi. ,.;15 mi. j 0 mi. #12;t-:~~ T~:l'IY1S c1Q jq 1vJ: M TUNJ ,,;15 J [I II) '. q4

Thompson, Anne

365

High-altitude meteors and meteoroid fragmentation observed at the Jicamarca Radio Observatory  

Science Journals Connector (OSTI)

......both 36.6- and 69-MHz radars. These observations...used to help establish atmospheric density and scaleheights...using the JRO HPLA 50-MHz radar. The high-power JRO 50-MHz radar is ideal for seeing more extended plasmas, and it might well......

B. Gao; J. D. Mathews

2015-02-01T23:59:59.000Z

366

Abundance Inhomogeneity in the Northeastern Rim of the Cygnus Loop Revealed by Suzaku Observatory  

E-Print Network (OSTI)

We present the results of a spatially resolved spectral analysis from four Suzaku observations covering the northeastern rim of the Cygnus Loop. A two-kT_e non-ionization equilibrium (NEI) model fairly well represents our data, which confirms the NEI condition of the plasma there. The metal abundances are depleted relative to the solar values almost everywhere in our field of view. We find abundance inhomogeneities across the field: the northernmost region (Region A) has enhanced absolute abundances compared with other regions. In addition, the relative abundances of Mg/O and Fe/O in Region A are lower than the solar values, while those in the other regions are twice higher than the solar values. As far as we are concerned, neither a circumstellar medium, fragments of ejecta, nor abundance inhomogeneities of the local interstellar medium around the Cygnus Loop can explain the relatively enhanced abundance in Region A. This point is left as an open question for future work.

S. Katsuda; H. Tsunemi; H. Uchida; E. Miyata; N. Nemes; E. D. Miller; K. Mori; J. P. Hughes

2008-03-03T23:59:59.000Z

367

Development of Regional Coastal Ocean Observatories and the Potential Benefits to Marine Sanctuaries  

E-Print Network (OSTI)

. These observational assets are coupled to nowcast/forecast data assimilative models. These systems will allow the mean sanctuaries per se, the sanctuaries stand to gain an unprecedented opportunity to benefit from real-time data in three enabling observational technologies. These technologies include (1) data acquisition systems

Moline, Mark

368

Solar neutrino measurement in SK and larger detector a Kamioka observatory, ICRR, Univ. of Tokyo,  

E-Print Network (OSTI)

the solar neutrino ux but also its energy spectrum and time variations such as day-night and seasonal di#11). The advantages of the detector as a solar neutrino observation are the time variation measurements and very-I 2.1. Solar neutrino ux The observed solar neutrino ux in SK-I, whose energy threshold is 5.0Me

Tokyo, University of

369

Infrared Imaging Solar Spectrograph at Purple Mountain Observatory Hui Li , Zhongyu Fan and Jianqi You  

E-Print Network (OSTI)

of solar activity. Studies of solar flares have scored great success. However, some problems pertinent to solar flare, such as energy transportation and line broadening mechanisms, have puzzled solar physicists formed at different heights in the solar atmosphere to assure the energy transportation is via thermal

Li, Hui

370

Robert M. La Follette School of Public Affairs 1225 Observatory Drive, Madison, Wisconsin 53706  

E-Print Network (OSTI)

://www.lafollette.wisc.edu/publications/workingpapers A Critical Review of Property Tax Relief in Wisconsin: The School Levy Credit and the First Dollar Credit tax relief programs, the school levy credit and the first dollar credit. By statute, the money spent. The existence of the credits may actually encourage local school boards to increase gross property tax levies

Wisconsin at Madison, University of

371

The VLBI Space Observatory Programme and the Radio-Astronomical Satellite HALCA  

Science Journals Connector (OSTI)

......caused by cos- mic radiation. Two Ni-Cd batteries are used as back-up power supplies and...eclipse duration is required to recharge the batteries before observing can recommence. To date...only a small amount of hydrazine RCS fuel remains, and one reaction wheel has been......

Hisashi Hirabayashi; Haruto Hirosawa; Hideyuki Kobayashi; Yasuhiro Murata; Yoshiharu Asaki; Ian M. Avruch; Philip G. Edwards; Edward B. Fomalont; Tsutomu Ichikawa; Tsuneo Kii; Rikako Okayasu; Kiyoaki Wajima; Makoto Inoue; Noriyuki Kawaguchi; Yoshihiro Chikada; Takeshi Bushimata; Kenta Fujisawa; Shinji Horiuchi; Seiji Kameno; Takeshi Miyaji; Kazunori M. Shibata; Zhi-Qiang Shen; Tomofumi Umemoto; Takashi Kasuga; Jun'ichi Nakajima; Yukio Takahashi; Shinzou Enome; Masaki Morimoto; Jordan Ellis; David L. Meier; David W. Murphy; Robert A. Preston; Joel G. Smith; Rick D. Wietfeldt; John M. Benson; Mark J. Claussen; Chris Flatters; George A. Moellenbrock; Jonathan D. Romney; James S. Ulvestad; Glen I. Langston; Anthony H. Minter; Larry R. D'Addario; Peter E. Dewdney; Sean M. Dougherty; David L. Jauncey; James E. J. Lovell; Steven J. Tingay; Anastasios K. Tzioumis; A. Russell Taylor; Wayne H. Cannon; Leonid I. Gurvits; Richard T. Schilizzi; Roy S. Booth; Misha V. Popov

2000-12-01T23:59:59.000Z

372

AAACCOMPLISHMENTSCCOMPLISHMENTSCCOMPLISHMENTS 2012201220122012 FAU Harbor Branch Research Highlights INDIAN RIVER LAGOON OBSERVATORY PROGRAM ESTABLISHED  

E-Print Network (OSTI)

. Applications for the undersea imaging include naval mine detection and characterization, inspection of ship Scientists from the FAU Harbor Branch Marine Biomedical and Biotechnology Research (MBBR) program (supported use of manzamine A, a natural product isolated from a marine sponge, as a treatment in pancreatic

Fernandez, Eduardo

373

Summer Courses in Ocean Optics and Biogeochemistry: "Monitoring the Oceans with Coastal Observatories" and  

E-Print Network (OSTI)

Summer Courses in Ocean Optics and Biogeochemistry: "Monitoring the Oceans with Coastal integration of optical approaches into oceanographic research in general. OBJECTIVES These two courses created and optical oceanography and ocean color remote sensing to learn the fundamentals of optics in a coastal

Boss, Emmanuel S.

374

National Radio Astronomy Observatory Cryogenic (4K) Measurements of Some Resistors and Capacitors  

E-Print Network (OSTI)

measurements using a long cable between the bridge and the unknown, the electrical length of the cable can components. About 1980, we found that TaN resistors from one manufacturer changed substantially at ~ 4 K of stainless steel 50-ohm coaxial cable to a 1 kHz digital capacitance meter [6]. With the capacitor

Groppi, Christopher

375

The PIN1 and PIN2 GPS Sites at Pinon Flat Observatory  

E-Print Network (OSTI)

of the preamp antenna (BPA)which is equivalent to the topbe TAB-TLP (equivalent to TAB-BPA), since the antenna mightTable 2 Date Based on TAB-BPA TAB-BPA (N) TAB-BPA (S) MAB-

Wyatt, Frank K; Agnew, Duncan Carr

2005-01-01T23:59:59.000Z

376

Energy and Matter: The design of a nature centre, tunnel, and neutrino observatory.  

E-Print Network (OSTI)

??Neutrino physics proposes radical new conceptions of matter. Contemplating the extraordinary and mysterious nature of neutrinos in architectural terms, Energy and Matter considers the ideas (more)

Elsworthy, William

2015-01-01T23:59:59.000Z

377

Measurement of the UHECR energy spectrum from hybrid data of the Pierre Auger Observatory  

E-Print Network (OSTI)

More than two years of fluorescence detector data collected in coincidence with at least one station of the surface detector array (``hybrid data'') are used to measure the flux and energy spectrum of cosmic rays above about 10$^{18}$ eV. The hybrid measurement extends towards lower energies the spectrum measured with the surface detector data only, and provides a cross-check with an independent data set. The determination of the fluorescence detector aperture and of its live-time, which is the major aspect of this measurement, is illustrated in detail. Our current estimate of the corresponding systematic uncertainties are given.

Lorenzo Perrone; for the the Pierre Auger Collaboration

2007-06-18T23:59:59.000Z

378

Development of a direct current power system for a multi-node cabled ocean observatory system  

Science Journals Connector (OSTI)

Due to the shortage of suitable research methods for real-time and long-term observation of oceans, an innovative approach that can provide abundant power and wide bandwidth is being developed worldwide ... , we ...

Yan-hu Chen; Can-jun Yang; De-jun Li; Bo Jin

2012-08-01T23:59:59.000Z

379

Energy partition of seismic coda waves in layered media: Theory and application to Pinyon Flats Observatory  

Science Journals Connector (OSTI)

......varying half-space-a new representation of...Academic Press, New York. Ryzhik L.V...Pacheco J., 2000. The energy partitioning and the...Springer-Verlag, Berlin and New York. Wu R.L. , 1985...Multiple scattering and energy transfer of seismic......

L. Margerin; M. Campillo; B. A. Van Tiggelen; R. Hennino

2009-05-01T23:59:59.000Z

380

Spectral-Line Observing at Arecibo Observatory Karen O'Neil  

E-Print Network (OSTI)

run through running the AO-Control graphical users interface (gui) o#11;-line, and then saving your/questions/comments/suggestions on this document, please contact Karen O'Neil (koneil@naic.edu) #12; 2 Contents 1 Spectral-Line Observing at AO 4 1 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 13 1.5 INTEGRATION TIME (per Data Record) . . . . . . . . . . . . . . . . . . . . 14 1.6 NOISE DIODE

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


381

Instrument Science Report WFPC2 2002-06 Results of the Observatory  

E-Print Network (OSTI)

-voltage power supply (LVPS), the mechanical systems and the thermo-electric coolers (TECs), while power was kept) was carried out, which involved the addition of several new hardware items including the Nicmos Cryo-cooler

Sirianni, Marco

382

IODP Expedition 328: Cascadia Subduction Zone ACORK Observatory Site U1364 Summary  

E-Print Network (OSTI)

(VIT) was deployed to observe the bit contacting the seafloor at 1329.0 m below rig floor (mbrf to the rig floor. After jetting in the 16 inch casing and re-entry cone, our next objective was to drill a 14) mud. The drill string was recovered with the bit clearing the rotary table at 1435 hr on 14 September

383

Australian Astronomical Observatory: 2 degree field facility 2dFGRS Galaxy Redshift Survey  

E-Print Network (OSTI)

to Sobral, Brazil and Principe, W Africa Path of totality Solar Eclipse of 29 May 1919 Frank Dyson energy density #12;Progress in Cosmology: III - Distant Supernovae Supernovae act as`standard candles' so as the density of matter is reduced Dark energy � a more general explanation of unknown form which acts

Greer, Julia R.

384

Faculty Roles in Managing and Operating the University of California Observatories S. M. Faber, Interim Director  

E-Print Network (OSTI)

are organized. The third section lists and describes the ten separate functions management and relationships to UCO staff. Faculty carry out ten different. Introduction The first section of this document summarizes the current structure

385

The next-generation liquid-scintillator neutrino observatory LENA Michael Wurm a,b,  

E-Print Network (OSTI)

ae , Walter Potzel a , Tomi Räihä k , Georg G. Raffelt af , Gioacchino Ranucci g , Soebur Razzaque ag of Fundamental Research, Mumbai, India j Hawaii Pacific University, Kaneohe, HI, USA k Oulu Southern Institute of Bucharest, Romania s Department of Physics and Astronomy, University of Hawaii, Honolulu, HI, USA

Mcdonough, William F.

386

The PIN1 and PIN2 GPS Sites at Pinon Flat Observatory  

E-Print Network (OSTI)

skills of Harold Bolton. Hadley Johnson spent a great dealFrank Wyatt, Steve Bralla, Hadley Johnson, Stephen Dockter,is 0.0984 m according to Hadleys measurement. Note that as

Wyatt, Frank K; Agnew, Duncan Carr

2005-01-01T23:59:59.000Z

387

Progress Report on the Berkeley/Anglo-Australian Observatory High-redshift Supernova Search  

DOE R&D Accomplishments (OSTI)

There are two main efforts related to supernovae in progress at Berkeley. The first is an automated supernova search for nearby supernovae, which was already discussed by Carl Pennypacker at this conference. The second is a search for distant supernovae, in the z = 0.3 to 0.5 region, aimed at measuring {Omega}. It is the latter that I want to discuss in this paper.

Goldhaber, G.; Perlmutter, S.; Pennypacker, C.; Marvin, H.; Muller, R. A.; Couch, W.; Boyle, B.

1990-11-00T23:59:59.000Z

388

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

E-Print Network (OSTI)

Introduction The observation of high-energy gamma ray sources has helped us to gain a better understandingProceedings of ICRC 2001: 1 c Copernicus Gesellschaft 2001 ICRC 2001 Status of the Milagro Gamma ability to reject background and more accurately reconstruct the gamma-ray direction and energy

California at Santa Cruz, University of

389

GEODETIC AND ASTRONOI{ICAL COORDINATES OF TIIE CERRO TOLOLO INTER-ATI{ERTCAN OBSERVATORY  

E-Print Network (OSTI)

and solar panels for power sources, and has four strobe units which insure almost uniform apparent flash in Astronomy, Inc., under contract with the National Science Foundation. ** #12;-1- INTRODUCTION Cerro Tololo

Mamajek, Eric E.

390

EUROPEAN SOUTHERN OBSERVATORY ESO/UC-67 Draft Minutes of the 26th  

E-Print Network (OSTI)

--------------------------------------------------------------------------------------------------------------------------------------- Page 2 of 18 Present were the UC members Chairperson: L. Wisotzki (Germany) Vice-Chairperson: J.V. Clausen (Denmark) E. Cappellaro (Italy) L. Kaper (The Netherlands) P. North (Switzerland) G. ?stlin. Bremer (United Kingdom) Group of "Frequent Users": M. Nonino (Italy) T. Prusti (The Netherlands) M

Liske, Jochen

391

Robust Signal Extraction Methods and Monte Carlo Sensitivity Studies for the Sudbury Neutrino Observatory and  

E-Print Network (OSTI)

+. An important part of the SNO+ physics program will be a search for neutrinoless double beta decay, carried out a reasonable choice for the 150 Nd neutrinoless double beta decay matrix element, these half lives correspond are competitive with those expected from all other near-term neutrinoless double beta decay experiments. ii #12

Waltham, Chris

392

The Sudbury Neutrino Observatory # C.J. Virtue (for the SNO Collaboration + ) a  

E-Print Network (OSTI)

of Physics and Astronomy, Laurentian University, Sudbury, ON, Canada P3E 2C6. Designed and constructed to address the solar neutrino problem by measuring the charged and neutral current interactions of solar. In particular, SNO was designed to ad­ dress the problem of the apparent deficit of solar neutrinos observed

Waltham, Chris

393

Predicted X-ray backgrounds for the International X-ray Observatory  

E-Print Network (OSTI)

The background that will be observed by IXO's X-ray detectors naturally separates into two components: (1) a Cosmic X-ray Background (CXB), primarily due to unresolved point sources at high energies (E>2 keV), along with ...

Bautz, Marshall W.

394

E-Print Network 3.0 - amma-catch gourma observatory Sample Search...  

NLE Websites -- All DOE Office Websites (Extended Search)

Manuscript Draft Summary: : AMMA-CATCH studies in the Sahelian region of West-Africa: an overview. Article Type: Special Issue... will find herewith the manuscript of the...

395

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

E-Print Network (OSTI)

the concentrations of uranium and thorium in the crust must be determined precisely for the future geoneutrino with measure- ments on outcrop and core samples, and with heat flow data. The concentrations of uranium, thorium, and po- tassium from radiometric surveys are correlated with geology, but heat production

396

Search for Galactic PeV gamma rays with the IceCube Neutrino Observatory  

Science Journals Connector (OSTI)

Gamma-ray induced air showers are notable for their lack of muons, compared to hadronic showers. Hence, air shower arrays with large underground muon detectors can select a sample greatly enriched in photon showers by rejecting showers containing muons. IceCube is sensitive to muons with energies above ?500??GeV at the surface, which provides an efficient veto system for hadronic air showers with energies above 1PeV. One year of data from the 40-string IceCube configuration was used to perform a search for point sources and a Galactic diffuse signal. No sources were found, resulting in a 90%C.L. upper limit on the ratio of gamma rays to cosmic rays of 1.210-3 for the flux coming from the Galactic plane region (-80?l?-30; -10?b?5) in the energy range 1.26.0PeV. In the same energy range, point source fluxes with E-2 spectra have been excluded at a level of (E/TeV)2d?/dE?10-1210-11??cm-2?s-1?TeV-1 depending on source declination. The complete IceCube detector will have a better sensitivity (due to the larger detector size), improved reconstruction, and vetoing techniques. Preliminary data from the nearly final IceCube detector configuration have been used to estimate the 5-yr sensitivity of the full detector. It is found to be more than an order of magnitude better, allowing the search for PeV extensions of known TeV gamma-ray emitters.

M. G. Aartsen et al. (IceCube Collaboration)

2013-03-20T23:59:59.000Z

397

First search for extremely high energy cosmogenic neutrinos with the IceCube Neutrino Observatory  

Science Journals Connector (OSTI)

We report on the results of the search for extremely-high energy neutrinos with energies above 107??GeV obtained with the partially (?30%) constructed IceCube in 2007. From the absence of signal events in the sample of 242.1 days of effective live time, we derive a 90% C.L. model independent differential upper limit based on the number of signal events per energy decade at E2??e+??+???1.410-6??GeV?cm-2?sec?-1?sr-1 for neutrinos in the energy range from 3107 to 3109??GeV.

R. Abbasi et al. (IceCube Collaboration)

2010-10-07T23:59:59.000Z

398

Studying Clouds and Aerosols with Lidar Depolarization Ratio and Backscatter Relationships  

E-Print Network (OSTI)

comparison of mineral dust aerosol retrievals from two instruments, MODIS and CALIPSO lidar. And, we implement and evaluate a new mineral dust detection algorithm based on the analysis of thin dust radiative signature. In comparison, three commonly used...

Cho, Hyoun-Myoung

2012-02-14T23:59:59.000Z

399

Multi-year Satellite and Surface Observations of AOD in support of Two-Column Aerosol Project (TCAP) Field Campaign  

SciTech Connect

We use combined multi-year measurements from the surface and space for assessing the spatial and temporal distribution of aerosol properties within a large (~400x400 km) region centered on Cape Cod, Massachusetts, along the East Coast of the United States. The ground-based Aerosol Robotic Network (AERONET) measurements at Marthas Vineyard Coastal Observatory (MVCO) site and Moderate Resolution Imaging Spectrometer (MODIS) sensors on board the Terra and Aqua satellites provide horizontal and temporal variations of aerosol optical depth, while the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) offers the altitudes of aerosol-layers. The combined ground-based and satellite measurements indicated several interesting features among which were the large differences in the aerosol properties observed in July and February. We applied the climatology of aerosol properties for designing the Two-Column Aerosol Project (TCAP), which is supported by the U.S. Department of Energys (DOEs) Atmospheric Radiation Measurement (ARM) Program. The TCAP field campaign involves 12-month deployment (started July 1, 2012) of the ground-based ARM Mobile Facility (AMF) and Mobile Aerosol Observing System (MAOS) on Cape Cod and complimentary aerosol observations from two research aircraft: the DOE Gulfstream-1 (G-1) and the National Aeronautics and Space Administration (NASA) B200 King Air. Using results from the coordinated G-1 and B200 flights during the recent (July, 2012) Intensive Observation Period, we demonstrated that the G-1 in situ measurements and B200 active remote sensing can provide complementary information on the temporal and spatial changes of the aerosol properties off the coast of North America.

Kassianov, Evgueni I.; Chand, Duli; Berg, Larry K.; Fast, Jerome D.; Tomlinson, Jason M.; Ferrare, R.; Hostetler, Chris A.; Hair, John

2012-11-01T23:59:59.000Z

400

31Black Holes....IV Thanks to two orbiting X-ray observatories, astronomers have the first strong evidence  

E-Print Network (OSTI)

1242-11 located 700 million light years from the Milky Way, in the constellation Virgo. (News Report at phenomena in converting matter into energy. As matter falls inward in an orbiting disk of gas, friction heats the gas up, and the energy released can be as much as 7% of the rest mass energy of the infalling

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


401

Building ISOC Status Displays for the Large AreaTelescope aboard the Gamma Ray Large Area Space Telescope (GLAST) Observatory  

SciTech Connect

In September 2007 the Gamma Ray Large Area Space Telescope (GLAST) is scheduled to launch aboard a Delta II rocket in order to put two high-energy gamma-ray detectors, the Large Area Telescope (LAT) and the GLAST Burst Monitor (GBM) into low earth orbit. The Instrument Science Operations Center (ISOC) at SLAC is responsible for the LAT operations for the duration of the mission, and will therefore build an operations center including a monitoring station at SLAC to inform operations staff and visitors of the status of the LAT instrument and GLAST. This monitoring station is to include sky maps showing the location of GLAST in its orbit as well as the LAT's projected field of view on the sky containing known gamma-ray sources. The display also requires a world map showing the locations of GLAST and three Tracking and Data Relay Satellites (TDRS) relative to the ground, their trail lines, and ''footprint'' circles indicating the range of communications for each satellite. The final display will also include a space view showing the orbiting and pointing information of GLAST and the TDRS satellites. In order to build the displays the astronomy programs Xephem, DS9, SatTrack, and STK were employed to model the position of GLAST and pointing information of the LAT instrument, and the programming utilities Python and Cron were used in Unix to obtain updated information from database and load them into the programs at regular intervals. Through these methods the indicated displays were created and combined to produce a monitoring display for the LAT and GLAST.

Ketchum, Christina; /SLAC

2006-09-01T23:59:59.000Z

402

Anisotropy and chemical composition of ultra-high energy cosmic rays using arrival directions measured by the Pierre Auger Observatory  

SciTech Connect

The Pierre Auger Collaboration has reported evidence for anisotropy in the distribution of arrival directions of the cosmic rays with energies E > Eth = 5.5 x 1019 eV. These show a correlation with the distribution of nearby extragalactic objects, including an apparent excess around the direction of Centaurus A. If the particles responsible for these excesses at E > Eth are heavy nuclei with charge Z, the proton component of the sources should lead to excesses in the same regions at energies E/Z. We here report the lack of anisotropies in these directions at energies above Eth/Z (for illustrative values of Z = 6,13,26). If the anisotropies above Eth are due to nuclei with charge Z, and under reasonable assumptions about the acceleration process, these observations imply stringent constraints on the allowed proton fraction at the lower energies.

Abreu, P [Lisbon, IST; Aglietta, M [IFSI, Turin; Ahn, E J [Fermilab; Albuquerque, I F.M. [Sao Paulo U.; Allard, D [APC, Paris; Allekotte, I [Centro Atomico Bariloche; Allen, J [New York U.; Allison, P [Ohio State U.; Alvarez Castillo, J [Mexico U., ICN; Alvarez-Muniz, J [Santiago de Compostela U.; Ambrosio, M [Napoli Seconda U.; INFN, Naples; Nijmegen U., IMAPP

2011-06-17T23:59:59.000Z

403

Nearby supernova rates from the Lick Observatory Supernova Search IV. A recovery method for the delay-time distribution  

Science Journals Connector (OSTI)

......distribution (DTD) - the SN rate versus time that would...SN progenitors and physics, as well as on the...curve, normalized to pass through the psi3 rate, which is the most...again normalized to pass through our best-fitting psi3 rate. The DD-Close-3......

Dan Maoz; Filippo Mannucci; Weidong Li; Alexei V. Filippenko; Massimo Della Valle; Nino Panagia

2011-04-11T23:59:59.000Z

404

Abstract--The Cosmic Ray Observatory Project (CROP) at University of Nebraska/Lincoln and the Washington Area Large-  

E-Print Network (OSTI)

developed to collect and synchronize the data from each detector site. The cost for each card is under US October 29, 2003. This work was supported in part by the U.S. Department of Energy, Quarknet, and the U.S several outreach projects siting cosmic-ray detectors at local high schools in cities around North America

Berns, Hans-Gerd

405

Vol. 22, No. 3 The Elusive Placelessness of the Mont-Blanc Observatory (18931909): The Social Underpinnings of  

E-Print Network (OSTI)

Third Republic at the turn of the century. Following some of the ways the MBO was connected to other into the twentieth century (astrophysical aeronautical practices, spatial stations, polar exploration, etc increasing accessibility. Above all, it was quickly becoming the base camp for climbing the highest mountain

Aubin, David

406

OWL opto-mechanics, phase A. E. Brunetto, M. Dimmler, F.Koch, M Quattri (European Southern Observatory).  

E-Print Network (OSTI)

will perform and how much it will cost. The two diagrams below summarize the trend of these two key parameters maintenance and handling, localized air conditioning, thermal insulation, cable wraps and paint (50 tons). 0 STATUS The telescope design is based on existing technologies and materials. · Telescope trusses

Liske, Jochen

407

Coronal Response of Bi-directional Jets Armagh Observatory, College Hill, Armagh BT61 9DG, N. Ireland  

E-Print Network (OSTI)

, Bartoe & Brueckner 1989) and 3300 s 1 (Ryutova & Tarbell 2000). They are characterized by spatial scales with Doppler shifts up to 250 km s 1 (Dere, Bartoe & Brueckner 1989) and often appear in bursts lasting several

408

Anisotropy and chemical composition of ultra-high energy cosmic rays using arrival directions measured by the Pierre Auger Observatory  

The Pierre Auger Collaboration has reported evidence for anisotropy in the distribution of arrival directions of the cosmic rays with energies E > Eth = 5.5 x 1019 eV. These show a correlation with the distribution of nearby extragalactic objects, including an apparent excess around the direction of Centaurus A. If the particles responsible for these excesses at E > Eth are heavy nuclei with charge Z, the proton component of the sources should lead to excesses in the same regions at energies E/Z. We here report the lack of anisotropies in these directions at energies above Eth/Z (for illustrative values of Z = 6,13,26). If the anisotropies above Eth are due to nuclei with charge Z, and under reasonable assumptions about the acceleration process, these observations imply stringent constraints on the allowed proton fraction at the lower energies.

Abreu, P [Lisbon, IST; Aglietta, M [IFSI, Turin; Ahn, E J [Fermilab; Albuquerque, I F.M. [Sao Paulo U.; Allard, D [APC, Paris; Allekotte, I [Centro Atomico Bariloche; Allen, J [New York U.; Allison, P [Ohio State U.; Alvarez Castillo, J [Mexico U., ICN; Alvarez-Muniz, J [Santiago de Compostela U.; Ambrosio, M [Napoli Seconda U.; INFN, Naples; Nijmegen U., IMAPP

2011-06-17T23:59:59.000Z

409

Kenya International Radio Observatory Joseph Otieno Malo, University of Nairobi,Joseph Otieno Malo, University of Nairobi,  

E-Print Network (OSTI)

of the terrestrial magnetosphere, ionosphere and neutral atmosphere using traditional asionosphere and neutral (INISSE) and the constructionElectronics (INISSE) and the construction of Giant Equatorial Radio in the fields of energy generation, rapid communications and generalgeneration, rapid communications and general

410

EUROPEAN SOUTHERN OBSERVATORY Organisation Europ eenne pour des Recherches Astronomiques dans l'H emisph ere Austral  

E-Print Network (OSTI)

. Abstract We have obtained deep near infrared observations (J #24; 24) of 8 nearby white dwarfs to search to this project: b) still required to complete this project: 5. Special remarks 6. Principal Investigator: M. Burleigh (University of Leicester, UK, mbu@star.le.ac.uk) CoI(s): F. Clarke (ESO/Chile, ESO), S. Hodgkin

Burleigh, Matt

411

Control and Acquisition Software for the Visible-Light Fabry-Prot Interferometer at the Big Bear Solar Observatory  

E-Print Network (OSTI)

-Light Imaging Magnetograph (VIM). We describe the software libraries and methods that we use to develop (VIM) and the InfraRed Imaging Magnetograph (IRIM). A detailed description of IRIM is given elsewhere in these proceedings.[2] VIM has two advantages over the DVMG system: (1) it has been designed to work with adaptive

412

Development and characterization of an observatory-class, broadband, non-fedback, leaf-spring interferometric seismometer  

E-Print Network (OSTI)

of the cylinders is 7. Foam insulation for the northwestfoam (General Plastics, P/N: FR-6710). The new insulation

Otero, Jos D.

2009-01-01T23:59:59.000Z

413

The Thermal Environment of the Fiber Glass Dome for the New Solar Telescope at Big Bear Solar Observatory  

E-Print Network (OSTI)

The New Solar Telescope (NST) is a 1.6-meter off-axis Gregory-type telescope with an equatorial mount and an open optical support structure. To mitigate the temperature fluctuations along the exposed optical path, the effects of local/dome-related seeing have to be minimized. To accomplish this, NST will be housed in a 5/8-sphere fiberglass dome that is outfitted with 14 active vents evenly spaced around its perimeter. The 14 vents house louvers that open and close independently of one another to regulate and direct the passage of air through the dome. In January 2006, 16 thermal probes were installed throughout the dome and the temperature distribution was measured. The measurements confirmed the existence of a strong thermal gradient on the order of 5 degree Celsius inside the dome. In December 2006, a second set of temperature measurements were made using different louver configurations. In this study, we present the results of these measurements along with their integration into the thermal control system (ThCS) and the overall telescope control system (TCS).

A. P. Verdoni; C. Denker; J. R. Varsik; S. Shumko; J. Nenow; R. Coulter

2007-08-04T23:59:59.000Z

414

Proceedings of ICRC 2001: 756 c Copernicus Gesellschaft 2001 Surface detector electronics for the Pierre Auger Observatory  

E-Print Network (OSTI)

for trigger, data acquisition and monitoring. Moreover, the electronics is powered by solar energy limited system (CDAS). Each detector station has a two level trigger, memory for temporary data storage operating gain, 2 105 , is required. The EA is equipped with PMTs from three different companies: Hamamatsu

415

HOBBY-EBERLY TELESCOPE The Hobby-Eberly Telescope is operated by McDonald Observatory on behalf of the  

E-Print Network (OSTI)

(VIRUS) instrument is being built to support observations for the Hobby-Eberly Telescope Dark Energy The Hobby Eberly Telescope Dark Energy Experiment (HETDEX) is a project aimed at looking for Dark Energy (5000 square degrees) blind survey for Lyman alpha emitting galaxies at redshifts z

416

First Neutrino Observations from the Sudbury Neutrino Observatory A.B. McDonald, Queen's University, Kingston, Ontario, Canada  

E-Print Network (OSTI)

's University, Kingston, Ontario, Canada For the SNO Collaboration a The #12;rst neutrino observations from and location, the data in the region of interest appear to be dominated by 8 B solar neutrinos, detected's Creighton mine near Sudbury, Ontario, Canada. The SNO detector has been #12;lled with water since May, 1999

Waltham, Chris

417

Probing the origin of cosmic rays with extremely high energy neutrinos using the IceCube Observatory  

Science Journals Connector (OSTI)

We have searched for extremely high energy neutrinos using data taken with the IceCube detector between May 2010 and May 2012. Two neutrino-induced particle shower events with energies around 1PeV were observed, as reported previously. In this work, we investigate whether these events could originate from cosmogenic neutrinos produced in the interactions of ultrahigh energy cosmic rays with ambient photons while propagating through intergalactic space. Exploiting IceCubes large exposure for extremely high energy neutrinos and the lack of observed events above 100PeV, we can rule out the corresponding models at more than 90% confidence level. The model-independent quasidifferential 90%C.L. upper limit, which amounts to E2??e+??+??=1.210-7??GeV?cm-2?s-1?sr-1 at 1EeV, provides the most stringent constraint in the energy range from 10PeV to 10EeV. Our observation disfavors strong cosmological evolution of the highest energy cosmic-ray sources such as the Fanaroff-Riley type II class of radio galaxies.

M. G. Aartsen et al. (IceCube Collaboration)

2013-12-16T23:59:59.000Z

418

STATE OF CALIFORNIA --NATURAL RESOURCES AGENCY EDMUND G. BROWN JR., Governor CALIFORNIA ENERGY COMMISSION  

E-Print Network (OSTI)

of the California Solar Initiative, a comprehensive statewide solar program. The NSHP provides rebates to encourage of the NSHP is to install 400 MW of solar electric capacity on new homes and residential buildings by the endSTATE OF CALIFORNIA -- NATURAL RESOURCES AGENCY EDMUND G. BROWN JR., Governor CALIFORNIA ENERGY

419

www.ecocar.gatech.edu/newsite EcoCAR: The NeXt Challenge COME OUT and learn about the  

E-Print Network (OSTI)

, developing and implementing a vehicle propulsion system that minimizes fuel consumption and emissions university engineering students to re- engineer a GM donated vehicle to achieve improved fuel efficiency and will provide performance metrics such as fuel usage and end-state battery state of charge. Engine Tuning

Houston, Paul L.

420

Automation of the EMBL Hamburg protein crystallography beamline BW7B  

Science Journals Connector (OSTI)

The automation of the EMBL Hamburg wiggler beamline BW7B for protein crystallography is described. The beamline features an automated end-station, a robotic sample changer, semi-automated sample centering based on UV fluorescence and new control software including intuitive graphical user interfaces.

Pohl, E.

2004-08-17T23:59:59.000Z

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


421

Atmos. Chem. Phys., 12, 683691, 2012 www.atmos-chem-phys.net/12/683/2012/  

E-Print Network (OSTI)

is usually defined by the level of zero net radiative heat- ing. Above this level air tends to riseAtmos. Chem. Phys., 12, 683­691, 2012 www.atmos-chem-phys.net/12/683/2012/ doi:10.5194/acp-12 measure- ments of CALIPSO and Aura/MLS we calculated the cor- relation of water vapor, ice water content

Meskhidze, Nicholas

422

Light Scattering by Ice Crystals and Mineral Dust Aerosols in the Atmosphere  

E-Print Network (OSTI)

of cirrus clouds is demonstrated and explained theoretically, which provides guidance in the calibration algorithm for 1.064-m channel on the Calipso lidar. Dust aerosols have no particular morphology. To develop an approach to modeling the optical...

Bi, Lei

2012-07-16T23:59:59.000Z

423

Cloud Effects on Radiative Heating Rate Profiles over Darwin using ARM and A-train Radar/Lidar Observations  

SciTech Connect

Observations of clouds from the ground-based U.S. Department of Energy Atmospheric Radiation Measurement program (ARM) and satellite-based A-train are used to compute cloud radiative forcing profiles over the ARM Darwin, Australia site. Cloud properties are obtained from both radar (the ARM Millimeter Cloud Radar (MMCR) and the CloudSat satellite in the A-train) and lidar (the ARM Micropulse lidar (MPL) and the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation (CALIPSO) satellite in the A-train) observations. Cloud microphysical properties are taken from combined radar and lidar retrievals for ice clouds and radar only or lidar only retrievals for liquid clouds. Large, statistically significant differences of up to 1.43 K/day exist between the mean ARM and A-train net cloud radiative forcing profiles. The majority of the difference in cloud radiative forcing profiles is shown to be due to a large difference in the cloud fraction above 12 km. Above this altitude the A-train cloud fraction is significantly larger because more clouds are detected by CALIPSO than by the ground-based MPL. It is shown that the MPL is unable to observe as many high clouds as CALIPSO due to being more frequently attenuated and a poorer sensitivity even in otherwise clear-sky conditions. After accounting for cloud fraction differences and instrument sampling differences due to viewing platform we determined that differences in cloud radiative forcing due to the retrieved ice cloud properties is relatively small. This study demonstrates that A-train observations are better suited for the calculation cloud radiative forcing profiles. In addition, we find that it is necessary to supplement CloudSat with CALIPSO observations to obtain accurate cloud radiative forcing profiles since a large portion of clouds at Darwin are detected by CALIPSO only.

Thorsen, Tyler J.; Fu, Qiang; Comstock, Jennifer M.

2013-06-11T23:59:59.000Z

424

Dept. of Soil Science, UW-Madison/UW-Extension, 1525 Observatory Dr., Madison, WI 53706/608-262-0485 November 2008 Issue #3 2008  

E-Print Network (OSTI)

Resources Extension Specialist Biological Systems Engineering Univ. of Wisconsin-Madison Rural land drainage came from Europe in the 1970s with the introduction of plastic drain tubing, which is still or modifications to a drain

Balser, Teri C.

425

The Great Observatories Origins Deep Survey: Constraints on the Lyman Continuum Escape Fraction Distribution of Lyman--Break Galaxies at 3.4  

E-Print Network (OSTI)

We use ultra-deep ultraviolet VLT/VIMOS intermediate-band and VLT/FORS1 narrow-band imaging in the GOODS Southern field to derive limits on the distribution of the escape fraction (f_esc) of ionizing radiation for L >~ L*(z=3) Lyman Break Galaxies (LBGs) at redshift 3.4--4.5. Only one LBG, at redshift z=3.795, is detected in its Lyman continuum (LyC; S/N~5.5), the highest redshift galaxy currently known with a direct detection. Its ultraviolet morphology is quite compact (R_eff=0.8, kpc physical). Three out of seven AGN are also detected in their LyC, including one at redshift z=3.951 and z850 = 26.1. From stacked data (LBGs) we set an upper limit to the average f_esc in the range 5%--20%, depending on the how the data are selected (e.g., by magnitude and/or redshift). We undertake extensive Monte Carlo simulations that take into account intergalactic attenuation, stellar population synthesis models, dust extinction and photometric noise in order to explore the moments of the distribution of the escaping radi...

Vanzella, E; Inoue, A; Nonino, M; Fontanot, F; Cristiani, S; Grazian, A; Dickinson, M; Stern, D; Tozzi, P; Giallongo, E; Ferguson, H; Spinrad, H; Boutsia, K; Fontana, A; Rosati, P

2010-01-01T23:59:59.000Z

426

Dept. of Soil Science, UW-Madison/UW-Extension, 1525 Observatory Dr., Madison, WI 53706/608-262-0485 November 2010 Issue #3 2010  

E-Print Network (OSTI)

for Oneida County and 45 ppm increase in Portage County. Soil test P changes in counties that predominantly Wisconsin counties had either no increase or a decrease in soil test P after regular upward trends in soil P to the medium/fine-textured soils where the average was 50 ppm. The counties where soils are intensively managed

Balser, Teri C.

427

Dept. of Soil Science, UW-Madison/UW-Extension, 1525 Observatory Dr., Madison, WI 53706/608-262-0485 November 2008 Issue #4 2008  

E-Print Network (OSTI)

of producing ammonia, which results in higher prices for all nitrogen and ammoniated phosphate fertilizer

Balser, Teri C.

428

Observations of the Hubble Deep Field with the Infrared Space Observatory. V. Spectral Energy Distributions, Starburst Models and Star Formation History  

E-Print Network (OSTI)

We have modelled the spectral energy distributions of the 13 HDF galaxies reliably detected by ISO. For 2 galaxies the emission detected by ISO is consistent with being starlight or the infrared 'cirrus' in the galaxies. For the remaining 11 galaxies there is a clear mid-infrared excess, which we interpret as emission from dust associated with a strong starburst. 10 of these galaxies are spirals or interacting pairs, while the remaining one is an elliptical with a prominent nucleus and broad emission lines. We give a new discussion of how the star formation rate can be deduced from the far infrared luminosity and derive star formation rates for these galaxies of 8-1000 $\\phi M_{\\sun}$ per yr, where $\\phi$ takes account of the uncertainty in the initial mass function. The HDF galaxies detected by ISO are clearly forming stars at a prodigious rate compared with nearby normal galaxies. We discuss the implications of our detections for the history of star and heavy element formation in the universe. Although uncertainties in the calibration, reliability of source detection, associations, and starburst models remain, it is clear that dust plays an important role in star formation out to redshift 1 at least.

The ISO-HDF Consortium; :; Michael Rowan-Robinson

1997-07-02T23:59:59.000Z

429

Dept. of Soil Science, UW-Madison/UW-Extension, 1525 Observatory Dr., Madison, WI 53706/608-262-0485 November 2010 Issue #1 2010  

E-Print Network (OSTI)

Hegeman 1/ Introduction Municipal biosolids are the product of the treatment of domestic wastewater of wastewater and contain plant nutrients, organic matter, and other materials that reflect their origin considerations for the safe and effective recycling of biosolids by land application in Wisconsin. Rules

Balser, Teri C.

430

146 IEEE JOURNAL OF OCEANIC ENGINEERING, VOL 27, NO.2, APRIL2002 r! The Long-TermEcosystem Observatory:An  

E-Print Network (OSTI)

, observational data are collected from satellites, aircrafts, ships, fixed/relocatable moorings and autonomous underwater vehicles. The majority of the data are available in real-time allowing for adaptive sampling of episodic events and are assimilated into ocean forecast models. In this observationally rich environment

Moline, Mark

431

SOLAR MERIDIONAL CIRCULATION FROM DOPPLER SHIFTS OF THE Fe I LINE AT 5250 A AS MEASURED BY THE 150-FOOT SOLAR TOWER TELESCOPE AT THE MT. WILSON OBSERVATORY  

SciTech Connect

Doppler shifts of the Fe I spectral line at 5250 A from the full solar disk obtained over the period 1986 to 2009 are analyzed to determine the circulation velocity of the solar surface along meridional planes. Simultaneous measurements of the Zeeman splitting of this line are used to obtain measurements of the solar magnetic field that are used to select low field points and impose corrections for the magnetically induced Doppler shift. The data utilized is from a new reduction that preserves the full spatial resolution of the original observations so that the circulation flow can be followed to latitudes of 80{sup 0} N/S. The deduced meridional flow is shown to differ from the circulation velocities derived from magnetic pattern movements. A reversed circulation pattern is seen in polar regions for three successive solar minima. A surge in circulation velocity at low latitudes is seen during the rising phases of cycles 22 and 23.

Ulrich, Roger K. [Department of Physics and Astronomy, University of California, Los Angeles, CA 90095-1562 (United States)

2010-12-10T23:59:59.000Z

432

Water Ice, Silicate, and Polycyclic Aromatic Hydrocarbon Emission Features in the Infrared Space Observatory Spectrum of the Carbon-Rich Planetary Nebula CPD -56 degree 8032  

E-Print Network (OSTI)

Combined ISO SWS and LWS spectroscopy is presented of the late WC-type planetary nebula nucleus CPD-56 8032 and its carbon-rich nebula. The extremely broad coverage (2.4-197 microns) enables us to recognize the clear and simultaneous presence of emission features from both oxygen- and carbon- rich circumstellar materials. Removing a smooth continuum highlights bright emission bands characteristic of polycyclic aromatic hydrocarbons (hereafter PAHs) in the 3-14 micron region, bands from crystalline silicates longwards of 18 microns, and the 43- and 62-micron bands of crystalline water ice. We discuss the probable evolutionary state and history of this unusual object in terms of (a) a recent transition from an O-rich to a C-rich outflow following a helium shell flash; or (b) a carbon-rich nebular outflow encountering an O-rich comet cloud.

Cohen, M; Sylvester, R J; Liu, X W; Cox, P; Lim, T; Schmitt, B; Speck, A K; Cohen, Martin

1999-01-01T23:59:59.000Z

433

Beamline 4.0.3  

NLE Websites -- All DOE Office Websites (Extended Search)

3 Print 3 Print High-resolution spectroscopy of complex materials (MERLIN) Endstations: MERIXS: High-resolution inelastic scattering ARPES: Angle-resolved photoemission spectroscopy GENERAL BEAMLINE INFORMATION Operational 2011 Source characteristics 9.0-cm-period quasiperiodic elliptical polarization undulator (EPU9) Energy range 9eV-120eV with current gratings Monochromator Variable-included-angle spherical grating monochromator (SGM) Calculated flux (1.9 GeV, 400 mA) 1012 photons/s/0.01%BW at 100 eV Resolving power (E/ΔE) High flux 1200 lines/mm; ~1/25,000 Endstations High-resolution inelastic scattering (MERIXS) and ARPES Characteristics Milli-Electron-volt Resolution beamLINe (MERLIN): Ultrahigh-resolution inelastic scattering and angle-resolved photoemission

434

Beamline 12.0.2  

NLE Websites -- All DOE Office Websites (Extended Search)

2 Print 2 Print Coherent science Scientific disciplines: Applied science, magnetism, materials science Endstations: 12.0.2.1: Coherent optics 12.0.2.2: Coherent x-ray scattering GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Third harmonic of 8-cm-period undulator (U8) Energy range 300-1500 eV Monochromator VLS-PGM, with two gratings (600 and 1200 lines/mm) Calculated flux (1.9 GeV, 400 mA) 1013 photons/s/0.1%BW at 500 eV Resolving power (E/DE) 1,000 Beam size Focused: 70 x 10 µm Unfocused: 200 x 200 µm Endstations 12.0.2.1: Coherent optics 12.0.2.2: Coherent scattering Detectors DetectorsCCD, photodiode, scintillator Scientific applications Branchlines designed for spatially coherent soft x-ray experiments

435

Beamline 12.0.2  

NLE Websites -- All DOE Office Websites (Extended Search)

2 Print 2 Print Coherent science Scientific disciplines: Applied science, magnetism, materials science Endstations: 12.0.2.1: Coherent optics 12.0.2.2: Coherent x-ray scattering GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Third harmonic of 8-cm-period undulator (U8) Energy range 300-1500 eV Monochromator VLS-PGM, with two gratings (600 and 1200 lines/mm) Calculated flux (1.9 GeV, 400 mA) 1013 photons/s/0.1%BW at 500 eV Resolving power (E/DE) 1,000 Beam size Focused: 70 x 10 µm Unfocused: 200 x 200 µm Endstations 12.0.2.1: Coherent optics 12.0.2.2: Coherent scattering Detectors DetectorsCCD, photodiode, scintillator Scientific applications Branchlines designed for spatially coherent soft x-ray experiments

436

Beamline 11.0.1  

NLE Websites -- All DOE Office Websites (Extended Search)

1 Print 1 Print PEEM3, Soft X-Ray Scattering Scientific disciplines: Magnetism, materials, surface science, polymers Endstations: 11.0.1.1: Photoemission electron microscope (PEEM3) 11.0.1.2: Soft x-ray scattering GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics 5.0-cm period elliptical polarization undulator (EPU5) Energy range 150-2000 eV Monochromator VLS-PGM Calculated flux (1.9 GeV, 400 mA) 1013 photons/s/0.1%BW at 800 eV Resolving power (E/ΔE) 4,000 at 800 eV Endstations 11.0.1.1: Photoemission electron microscope (PEEM3) 11.0.1.2: Soft x-ray scattering Special notes Polarization is user selectable; linear polarization continuously variable from horizontal to vertical; left and right elliptical (or circular) polarization

437

Beamline 9.3.2  

NLE Websites -- All DOE Office Websites (Extended Search)

2 Print 2 Print Chemical and Materials Scientific disciplines: Surfaces, interfaces, catalysis, environmental science, material science, electrochemistry Endstations: Ambient pressure X-ray Photoelectron Spectroscopy (APXPS)* Ambient pressure photoemission GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Bend magnet Energy range 30-850 eV Monochromator SGM (gratings: 100, 600 lines/mm) Calculated flux (1.9 GeV, 400 mA) up to 1.5 x 1011 photons/sec, energy dependent Resolving power (E/ΔE) <10,000 Scientific disciplines Surfaces, interfaces, catalysis, environmental science, material science, electrochemistry. Endstations Ambient pressure X-ray Photoelectron Spectroscopy (APXPS)*

438

Beamline 9.3.2  

NLE Websites -- All DOE Office Websites (Extended Search)

2 Print 2 Print Chemical and Materials Scientific disciplines: Surfaces, interfaces, catalysis, environmental science, material science, electrochemistry Endstations: Ambient pressure X-ray Photoelectron Spectroscopy (APXPS)* Ambient pressure photoemission GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Bend magnet Energy range 30-850 eV Monochromator SGM (gratings: 100, 600 lines/mm) Calculated flux (1.9 GeV, 400 mA) up to 1.5 x 1011 photons/sec, energy dependent Resolving power (E/ΔE) <10,000 Scientific disciplines Surfaces, interfaces, catalysis, environmental science, material science, electrochemistry. Endstations Ambient pressure X-ray Photoelectron Spectroscopy (APXPS)*

439

Beamline 12.0.2  

NLE Websites -- All DOE Office Websites (Extended Search)

0.2 Print 0.2 Print Coherent science Scientific disciplines: Applied science, magnetism, materials science Endstations: 12.0.2.1: Coherent optics 12.0.2.2: Coherent x-ray scattering GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Third harmonic of 8-cm-period undulator (U8) Energy range 300-1500 eV Monochromator VLS-PGM, with two gratings (600 and 1200 lines/mm) Calculated flux (1.9 GeV, 400 mA) 1013 photons/s/0.1%BW at 500 eV Resolving power (E/DE) 1,000 Beam size Focused: 70 x 10 µm Unfocused: 200 x 200 µm Endstations 12.0.2.1: Coherent optics 12.0.2.2: Coherent scattering Detectors DetectorsCCD, photodiode, scintillator Scientific applications Branchlines designed for spatially coherent soft x-ray experiments

440

Beamline 4.0.3  

NLE Websites -- All DOE Office Websites (Extended Search)

3 Print 3 Print High-resolution spectroscopy of complex materials (MERLIN) Endstations: MERIXS: High-resolution inelastic scattering ARPES: Angle-resolved photoemission spectroscopy GENERAL BEAMLINE INFORMATION Operational 2011 Source characteristics 9.0-cm-period quasiperiodic elliptical polarization undulator (EPU9) Energy range 9eV-120eV with current gratings Monochromator Variable-included-angle spherical grating monochromator (SGM) Calculated flux (1.9 GeV, 400 mA) 1012 photons/s/0.01%BW at 100 eV Resolving power (E/ΔE) High flux 1200 lines/mm; ~1/25,000 Endstations High-resolution inelastic scattering (MERIXS) and ARPES Characteristics Milli-Electron-volt Resolution beamLINe (MERLIN): Ultrahigh-resolution inelastic scattering and angle-resolved photoemission

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


441

Beamline 9.3.2  

NLE Websites -- All DOE Office Websites (Extended Search)

2 Print 2 Print Chemical and Materials Scientific disciplines: Surfaces, interfaces, catalysis, environmental science, material science, electrochemistry Endstations: Ambient pressure X-ray Photoelectron Spectroscopy (APXPS)* Ambient pressure photoemission GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Bend magnet Energy range 30-850 eV Monochromator SGM (gratings: 100, 600 lines/mm) Calculated flux (1.9 GeV, 400 mA) up to 1.5 x 1011 photons/sec, energy dependent Resolving power (E/ΔE) <10,000 Scientific disciplines Surfaces, interfaces, catalysis, environmental science, material science, electrochemistry. Endstations Ambient pressure X-ray Photoelectron Spectroscopy (APXPS)*

442

Beamline 4.0.3  

NLE Websites -- All DOE Office Websites (Extended Search)

3 Print 3 Print High-resolution spectroscopy of complex materials (MERLIN) Endstations: MERIXS: High-resolution inelastic scattering ARPES: Angle-resolved photoemission spectroscopy GENERAL BEAMLINE INFORMATION Operational 2011 Source characteristics 9.0-cm-period quasiperiodic elliptical polarization undulator (EPU9) Energy range 9eV-120eV with current gratings Monochromator Variable-included-angle spherical grating monochromator (SGM) Calculated flux (1.9 GeV, 400 mA) 1012 photons/s/0.01%BW at 100 eV Resolving power (E/ΔE) High flux 1200 lines/mm; ~1/25,000 Endstations High-resolution inelastic scattering (MERIXS) and ARPES Characteristics Milli-Electron-volt Resolution beamLINe (MERLIN): Ultrahigh-resolution inelastic scattering and angle-resolved photoemission

443

Beamline 12.0.2  

NLE Websites -- All DOE Office Websites (Extended Search)

2 Print 2 Print Coherent science Scientific disciplines: Applied science, magnetism, materials science Endstations: 12.0.2.1: Coherent optics 12.0.2.2: Coherent x-ray scattering GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Third harmonic of 8-cm-period undulator (U8) Energy range 300-1500 eV Monochromator VLS-PGM, with two gratings (600 and 1200 lines/mm) Calculated flux (1.9 GeV, 400 mA) 1013 photons/s/0.1%BW at 500 eV Resolving power (E/DE) 1,000 Beam size Focused: 70 x 10 µm Unfocused: 200 x 200 µm Endstations 12.0.2.1: Coherent optics 12.0.2.2: Coherent scattering Detectors DetectorsCCD, photodiode, scintillator Scientific applications Branchlines designed for spatially coherent soft x-ray experiments

444

Beamline 11.0.1  

NLE Websites -- All DOE Office Websites (Extended Search)

1 Print 1 Print PEEM3, Soft X-Ray Scattering Scientific disciplines: Magnetism, materials, surface science, polymers Endstations: 11.0.1.1: Photoemission electron microscope (PEEM3) 11.0.1.2: Soft x-ray scattering GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics 5.0-cm period elliptical polarization undulator (EPU5) Energy range 150-2000 eV Monochromator VLS-PGM Calculated flux (1.9 GeV, 400 mA) 1013 photons/s/0.1%BW at 800 eV Resolving power (E/ΔE) 4,000 at 800 eV Endstations 11.0.1.1: Photoemission electron microscope (PEEM3) 11.0.1.2: Soft x-ray scattering Special notes Polarization is user selectable; linear polarization continuously variable from horizontal to vertical; left and right elliptical (or circular) polarization

445

Beamline 9.3.2  

NLE Websites -- All DOE Office Websites (Extended Search)

3.2 Print 3.2 Print Chemical and Materials Scientific disciplines: Surfaces, interfaces, catalysis, environmental science, material science, electrochemistry Endstations: Ambient pressure X-ray Photoelectron Spectroscopy (APXPS)* Ambient pressure photoemission GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Bend magnet Energy range 30-850 eV Monochromator SGM (gratings: 100, 600 lines/mm) Calculated flux (1.9 GeV, 400 mA) up to 1.5 x 1011 photons/sec, energy dependent Resolving power (E/ΔE) <10,000 Scientific disciplines Surfaces, interfaces, catalysis, environmental science, material science, electrochemistry. Endstations Ambient pressure X-ray Photoelectron Spectroscopy (APXPS)*

446

Beamline 4.0.3  

NLE Websites -- All DOE Office Websites (Extended Search)

3 Print 3 Print High-resolution spectroscopy of complex materials (MERLIN) Endstations: MERIXS: High-resolution inelastic scattering ARPES: Angle-resolved photoemission spectroscopy GENERAL BEAMLINE INFORMATION Operational 2011 Source characteristics 9.0-cm-period quasiperiodic elliptical polarization undulator (EPU9) Energy range 9eV-120eV with current gratings Monochromator Variable-included-angle spherical grating monochromator (SGM) Calculated flux (1.9 GeV, 400 mA) 1012 photons/s/0.01%BW at 100 eV Resolving power (E/ΔE) High flux 1200 lines/mm; ~1/25,000 Endstations High-resolution inelastic scattering (MERIXS) and ARPES Characteristics Milli-Electron-volt Resolution beamLINe (MERLIN): Ultrahigh-resolution inelastic scattering and angle-resolved photoemission

447

Beamline 11.0.1  

NLE Websites -- All DOE Office Websites (Extended Search)

1 Print 1 Print PEEM3, Soft X-Ray Scattering Scientific disciplines: Magnetism, materials, surface science, polymers Endstations: 11.0.1.1: Photoemission electron microscope (PEEM3) 11.0.1.2: Soft x-ray scattering GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics 5.0-cm period elliptical polarization undulator (EPU5) Energy range 150-2000 eV Monochromator VLS-PGM Calculated flux (1.9 GeV, 400 mA) 1013 photons/s/0.1%BW at 800 eV Resolving power (E/ΔE) 4,000 at 800 eV Endstations 11.0.1.1: Photoemission electron microscope (PEEM3) 11.0.1.2: Soft x-ray scattering Special notes Polarization is user selectable; linear polarization continuously variable from horizontal to vertical; left and right elliptical (or circular) polarization

448

Beamline 11.0.1  

NLE Websites -- All DOE Office Websites (Extended Search)

1 Print 1 Print PEEM3, Soft X-Ray Scattering Scientific disciplines: Magnetism, materials, surface science, polymers Endstations: 11.0.1.1: Photoemission electron microscope (PEEM3) 11.0.1.2: Soft x-ray scattering GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics 5.0-cm period elliptical polarization undulator (EPU5) Energy range 150-2000 eV Monochromator VLS-PGM Calculated flux (1.9 GeV, 400 mA) 1013 photons/s/0.1%BW at 800 eV Resolving power (E/ΔE) 4,000 at 800 eV Endstations 11.0.1.1: Photoemission electron microscope (PEEM3) 11.0.1.2: Soft x-ray scattering Special notes Polarization is user selectable; linear polarization continuously variable from horizontal to vertical; left and right elliptical (or circular) polarization

449

Beamline 12.0.2  

NLE Websites -- All DOE Office Websites (Extended Search)

2 Print 2 Print Coherent science Scientific disciplines: Applied science, magnetism, materials science Endstations: 12.0.2.1: Coherent optics 12.0.2.2: Coherent x-ray scattering GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Third harmonic of 8-cm-period undulator (U8) Energy range 300-1500 eV Monochromator VLS-PGM, with two gratings (600 and 1200 lines/mm) Calculated flux (1.9 GeV, 400 mA) 1013 photons/s/0.1%BW at 500 eV Resolving power (E/DE) 1,000 Beam size Focused: 70 x 10 µm Unfocused: 200 x 200 µm Endstations 12.0.2.1: Coherent optics 12.0.2.2: Coherent scattering Detectors DetectorsCCD, photodiode, scintillator Scientific applications Branchlines designed for spatially coherent soft x-ray experiments

450

Beamline 11.0.1  

NLE Websites -- All DOE Office Websites (Extended Search)

1 Print 1 Print PEEM3, Soft X-Ray Scattering Scientific disciplines: Magnetism, materials, surface science, polymers Endstations: 11.0.1.1: Photoemission electron microscope (PEEM3) 11.0.1.2: Soft x-ray scattering GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics 5.0-cm period elliptical polarization undulator (EPU5) Energy range 150-2000 eV Monochromator VLS-PGM Calculated flux (1.9 GeV, 400 mA) 1013 photons/s/0.1%BW at 800 eV Resolving power (E/ΔE) 4,000 at 800 eV Endstations 11.0.1.1: Photoemission electron microscope (PEEM3) 11.0.1.2: Soft x-ray scattering Special notes Polarization is user selectable; linear polarization continuously variable from horizontal to vertical; left and right elliptical (or circular) polarization

451

Beamline 9.3.2  

NLE Websites -- All DOE Office Websites (Extended Search)

3.2 Print 3.2 Print Chemical and Materials Scientific disciplines: Surfaces, interfaces, catalysis, environmental science, material science, electrochemistry Endstations: Ambient pressure X-ray Photoelectron Spectroscopy (APXPS)* Ambient pressure photoemission GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Bend magnet Energy range 30-850 eV Monochromator SGM (gratings: 100, 600 lines/mm) Calculated flux (1.9 GeV, 400 mA) up to 1.5 x 1011 photons/sec, energy dependent Resolving power (E/ΔE) <10,000 Scientific disciplines Surfaces, interfaces, catalysis, environmental science, material science, electrochemistry. Endstations Ambient pressure X-ray Photoelectron Spectroscopy (APXPS)*

452

Beamline 11.0.1  

NLE Websites -- All DOE Office Websites (Extended Search)

1 Print 1 Print PEEM3, Soft X-Ray Scattering Scientific disciplines: Magnetism, materials, surface science, polymers Endstations: 11.0.1.1: Photoemission electron microscope (PEEM3) 11.0.1.2: Soft x-ray scattering GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics 5.0-cm period elliptical polarization undulator (EPU5) Energy range 150-2000 eV Monochromator VLS-PGM Calculated flux (1.9 GeV, 400 mA) 1013 photons/s/0.1%BW at 800 eV Resolving power (E/ΔE) 4,000 at 800 eV Endstations 11.0.1.1: Photoemission electron microscope (PEEM3) 11.0.1.2: Soft x-ray scattering Special notes Polarization is user selectable; linear polarization continuously variable from horizontal to vertical; left and right elliptical (or circular) polarization

453

Beamline 11.0.1  

NLE Websites -- All DOE Office Websites (Extended Search)

1 Print 1 Print PEEM3, Soft X-Ray Scattering Scientific disciplines: Magnetism, materials, surface science, polymers Endstations: 11.0.1.1: Photoemission electron microscope (PEEM3) 11.0.1.2: Soft x-ray scattering GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics 5.0-cm period elliptical polarization undulator (EPU5) Energy range 150-2000 eV Monochromator VLS-PGM Calculated flux (1.9 GeV, 400 mA) 1013 photons/s/0.1%BW at 800 eV Resolving power (E/ΔE) 4,000 at 800 eV Endstations 11.0.1.1: Photoemission electron microscope (PEEM3) 11.0.1.2: Soft x-ray scattering Special notes Polarization is user selectable; linear polarization continuously variable from horizontal to vertical; left and right elliptical (or circular) polarization

454

Beamline 4.0.3  

NLE Websites -- All DOE Office Websites (Extended Search)

3 Print 3 Print High-resolution spectroscopy of complex materials (MERLIN) Endstations: MERIXS: High-resolution inelastic scattering ARPES: Angle-resolved photoemission spectroscopy GENERAL BEAMLINE INFORMATION Operational 2011 Source characteristics 9.0-cm-period quasiperiodic elliptical polarization undulator (EPU9) Energy range 9eV-120eV with current gratings Monochromator Variable-included-angle spherical grating monochromator (SGM) Calculated flux (1.9 GeV, 400 mA) 1012 photons/s/0.01%BW at 100 eV Resolving power (E/ΔE) High flux 1200 lines/mm; ~1/25,000 Endstations High-resolution inelastic scattering (MERIXS) and ARPES Characteristics Milli-Electron-volt Resolution beamLINe (MERLIN): Ultrahigh-resolution inelastic scattering and angle-resolved photoemission

455

Beamline 11.0.1  

NLE Websites -- All DOE Office Websites (Extended Search)

1 Print 1 Print PEEM3, Soft X-Ray Scattering Scientific disciplines: Magnetism, materials, surface science, polymers Endstations: 11.0.1.1: Photoemission electron microscope (PEEM3) 11.0.1.2: Soft x-ray scattering GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics 5.0-cm period elliptical polarization undulator (EPU5) Energy range 150-2000 eV Monochromator VLS-PGM Calculated flux (1.9 GeV, 400 mA) 1013 photons/s/0.1%BW at 800 eV Resolving power (E/ΔE) 4,000 at 800 eV Endstations 11.0.1.1: Photoemission electron microscope (PEEM3) 11.0.1.2: Soft x-ray scattering Special notes Polarization is user selectable; linear polarization continuously variable from horizontal to vertical; left and right elliptical (or circular) polarization

456

Beamline 4.0.3  

NLE Websites -- All DOE Office Websites (Extended Search)

3 Print 3 Print High-resolution spectroscopy of complex materials (MERLIN) Endstations: MERIXS: High-resolution inelastic scattering ARPES: Angle-resolved photoemission spectroscopy GENERAL BEAMLINE INFORMATION Operational 2011 Source characteristics 9.0-cm-period quasiperiodic elliptical polarization undulator (EPU9) Energy range 9eV-120eV with current gratings Monochromator Variable-included-angle spherical grating monochromator (SGM) Calculated flux (1.9 GeV, 400 mA) 1012 photons/s/0.01%BW at 100 eV Resolving power (E/ΔE) High flux 1200 lines/mm; ~1/25,000 Endstations High-resolution inelastic scattering (MERIXS) and ARPES Characteristics Milli-Electron-volt Resolution beamLINe (MERLIN): Ultrahigh-resolution inelastic scattering and angle-resolved photoemission

457

Beamline 9.3.2  

NLE Websites -- All DOE Office Websites (Extended Search)

3.2 Print 3.2 Print Chemical and Materials Scientific disciplines: Surfaces, interfaces, catalysis, environmental science, material science, electrochemistry Endstations: Ambient pressure X-ray Photoelectron Spectroscopy (APXPS)* Ambient pressure photoemission GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Bend magnet Energy range 30-850 eV Monochromator SGM (gratings: 100, 600 lines/mm) Calculated flux (1.9 GeV, 400 mA) up to 1.5 x 1011 photons/sec, energy dependent Resolving power (E/ΔE) <10,000 Scientific disciplines Surfaces, interfaces, catalysis, environmental science, material science, electrochemistry. Endstations Ambient pressure X-ray Photoelectron Spectroscopy (APXPS)*

458

Page not found | Department of Energy  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

891 - 21900 of 28,905 results. 891 - 21900 of 28,905 results. Page Endstates Initiative Scientific and technical, institutional and regulatory, and closure management challenges are currently hindering cleanup and closure of remaining environmental legacy waste sites across the... http://energy.gov/em/endstates-initiative Page Technical Assistance The Technical Assistance program is managed through the Center for Sustainable Soil and Groundwater Solutions at SRNL. The Technical Assistance program provides teams of nationally recognized... http://energy.gov/em/technical-assistance Article EM Collaborates on Best Practices for Reviews WASHINGTON, D.C. - EM is contributing its expertise to an award-winning federal interagency workgroup tasked with developing tools for federal facility site managers to streamline and communicate a five-year review

459

Beamline 4.0.3  

NLE Websites -- All DOE Office Websites (Extended Search)

3 Print 3 Print High-resolution spectroscopy of complex materials (MERLIN) Endstations: MERIXS: High-resolution inelastic scattering ARPES: Angle-resolved photoemission spectroscopy GENERAL BEAMLINE INFORMATION Operational 2011 Source characteristics 9.0-cm-period quasiperiodic elliptical polarization undulator (EPU9) Energy range 9eV-120eV with current gratings Monochromator Variable-included-angle spherical grating monochromator (SGM) Calculated flux (1.9 GeV, 400 mA) 1012 photons/s/0.01%BW at 100 eV Resolving power (E/ΔE) High flux 1200 lines/mm; ~1/25,000 Endstations High-resolution inelastic scattering (MERIXS) and ARPES Characteristics Milli-Electron-volt Resolution beamLINe (MERLIN): Ultrahigh-resolution inelastic scattering and angle-resolved photoemission

460

Beamline 9.3.2  

NLE Websites -- All DOE Office Websites (Extended Search)

3.2 Print 3.2 Print Chemical and Materials Scientific disciplines: Surfaces, interfaces, catalysis, environmental science, material science, electrochemistry Endstations: Ambient pressure X-ray Photoelectron Spectroscopy (APXPS)* Ambient pressure photoemission GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Bend magnet Energy range 30-850 eV Monochromator SGM (gratings: 100, 600 lines/mm) Calculated flux (1.9 GeV, 400 mA) up to 1.5 x 1011 photons/sec, energy dependent Resolving power (E/ΔE) <10,000 Scientific disciplines Surfaces, interfaces, catalysis, environmental science, material science, electrochemistry. Endstations Ambient pressure X-ray Photoelectron Spectroscopy (APXPS)*

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


461

Beamline 9.3.2  

NLE Websites -- All DOE Office Websites (Extended Search)

2 Print 2 Print Chemical and Materials Scientific disciplines: Surfaces, interfaces, catalysis, environmental science, material science, electrochemistry Endstations: Ambient pressure X-ray Photoelectron Spectroscopy (APXPS)* Ambient pressure photoemission GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Bend magnet Energy range 30-850 eV Monochromator SGM (gratings: 100, 600 lines/mm) Calculated flux (1.9 GeV, 400 mA) up to 1.5 x 1011 photons/sec, energy dependent Resolving power (E/ΔE) <10,000 Scientific disciplines Surfaces, interfaces, catalysis, environmental science, material science, electrochemistry. Endstations Ambient pressure X-ray Photoelectron Spectroscopy (APXPS)*

462

Beamline 11.0.1  

NLE Websites -- All DOE Office Websites (Extended Search)

0.1 Print 0.1 Print PEEM3, Soft X-Ray Scattering Scientific disciplines: Magnetism, materials, surface science, polymers Endstations: 11.0.1.1: Photoemission electron microscope (PEEM3) 11.0.1.2: Soft x-ray scattering GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics 5.0-cm period elliptical polarization undulator (EPU5) Energy range 150-2000 eV Monochromator VLS-PGM Calculated flux (1.9 GeV, 400 mA) 1013 photons/s/0.1%BW at 800 eV Resolving power (E/ΔE) 4,000 at 800 eV Endstations 11.0.1.1: Photoemission electron microscope (PEEM3) 11.0.1.2: Soft x-ray scattering Special notes Polarization is user selectable; linear polarization continuously variable from horizontal to vertical; left and right elliptical (or circular) polarization

463

Beamline 4.0.3  

NLE Websites -- All DOE Office Websites (Extended Search)

3 Print 3 Print High-resolution spectroscopy of complex materials (MERLIN) Endstations: MERIXS: High-resolution inelastic scattering ARPES: Angle-resolved photoemission spectroscopy GENERAL BEAMLINE INFORMATION Operational 2011 Source characteristics 9.0-cm-period quasiperiodic elliptical polarization undulator (EPU9) Energy range 9eV-120eV with current gratings Monochromator Variable-included-angle spherical grating monochromator (SGM) Calculated flux (1.9 GeV, 400 mA) 1012 photons/s/0.01%BW at 100 eV Resolving power (E/ΔE) High flux 1200 lines/mm; ~1/25,000 Endstations High-resolution inelastic scattering (MERIXS) and ARPES Characteristics Milli-Electron-volt Resolution beamLINe (MERLIN): Ultrahigh-resolution inelastic scattering and angle-resolved photoemission

464

Beamline 9.3.2  

NLE Websites -- All DOE Office Websites (Extended Search)

2 Print 2 Print Chemical and Materials Scientific disciplines: Surfaces, interfaces, catalysis, environmental science, material science, electrochemistry Endstations: Ambient pressure X-ray Photoelectron Spectroscopy (APXPS)* Ambient pressure photoemission GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Bend magnet Energy range 30-850 eV Monochromator SGM (gratings: 100, 600 lines/mm) Calculated flux (1.9 GeV, 400 mA) up to 1.5 x 1011 photons/sec, energy dependent Resolving power (E/ΔE) <10,000 Scientific disciplines Surfaces, interfaces, catalysis, environmental science, material science, electrochemistry. Endstations Ambient pressure X-ray Photoelectron Spectroscopy (APXPS)*

465

Beamline 11.0.1  

NLE Websites -- All DOE Office Websites (Extended Search)

1 Print 1 Print PEEM3, Soft X-Ray Scattering Scientific disciplines: Magnetism, materials, surface science, polymers Endstations: 11.0.1.1: Photoemission electron microscope (PEEM3) 11.0.1.2: Soft x-ray scattering GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics 5.0-cm period elliptical polarization undulator (EPU5) Energy range 150-2000 eV Monochromator VLS-PGM Calculated flux (1.9 GeV, 400 mA) 1013 photons/s/0.1%BW at 800 eV Resolving power (E/ΔE) 4,000 at 800 eV Endstations 11.0.1.1: Photoemission electron microscope (PEEM3) 11.0.1.2: Soft x-ray scattering Special notes Polarization is user selectable; linear polarization continuously variable from horizontal to vertical; left and right elliptical (or circular) polarization

466

Beamline 9.3.2  

NLE Websites -- All DOE Office Websites (Extended Search)

9.3.2 9.3.2 Beamline 9.3.2 Print Tuesday, 20 October 2009 09:06 Chemical and Materials Scientific disciplines: Surfaces, interfaces, catalysis, environmental science, material science, electrochemistry Endstations: Ambient pressure X-ray Photoelectron Spectroscopy (APXPS)* Ambient pressure photoemission GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Bend magnet Energy range 30-850 eV Monochromator SGM (gratings: 100, 600 lines/mm) Calculated flux (1.9 GeV, 400 mA) up to 1.5 x 1011 photons/sec, energy dependent Resolving power (E/ΔE) <10,000 Scientific disciplines Surfaces, interfaces, catalysis, environmental science, material science, electrochemistry. Endstations Ambient pressure X-ray Photoelectron Spectroscopy (APXPS)*

467

Comparative risk analysis for the Rocky Flats Plant integrated project planning  

SciTech Connect

The Rocky Flats Plant is developing, with active stakeholder participation, a comprehensive planning strategy that will support transition of the Rocky Flats Plant from a nuclear weapons production facility to site cleanup and final disposition. Final disposition of the Rocky Flats Plant materials and contaminants requires consideration of the interrelated nature of sitewide problems, such as material movement and disposition, facility and land use endstates, costs, relative risks to workers and the public, and waste disposition. Comparative risk analysis employs both incremental risk and cumulative risk evaluations to compare risks from postulated options or end states. These postulated options or end states can be various remedial alternatives, or future endstate uses of federal land.

Jones, M.E.; Shain, D.I.

1994-12-31T23:59:59.000Z

468

Achieving Vibration Stability of the NSLS-II Hard X-ray Nanoprobe Beamline  

SciTech Connect

The Hard X-ray Nanoprobe (HXN) Beamline of National Synchrotron Light Source II (NSLS-lI) requires high levels of stability in order to achieve the desired instrument resolution. To ensure that the design of the endstation helps meet the stringent criteria and that natural and cultural vibration is mitigated both passively and actively, a comprehensive study complimentary to the design process has been undertaken. Vibration sources that have the potential to disrupt sensitive experiments such as wind, traffic and NSLS II operating systems have been studied using state of the art simulations and an array of field data. Further, final stage vibration isolation principles have been explored in order to be utilized in supporting endstation instruments. This paper presents results of the various study aspects and their influence on the HXN design optimization.

Simos, N.; Chu, Y. N.; Broadbent, A.; Nazaretski, E.; Margulies, L.; Dyling, O.; Shen, Q.; Fallier, M.

2010-08-30T23:59:59.000Z

469

Beamline 12.0.2  

NLE Websites -- All DOE Office Websites (Extended Search)

2 Print 2 Print Coherent science Scientific disciplines: Applied science, magnetism, materials science Endstations: 12.0.2.1: Coherent optics 12.0.2.2: Coherent x-ray scattering GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Third harmonic of 8-cm-period undulator (U8) Energy range 300-1500 eV Monochromator VLS-PGM, with two gratings (600 and 1200 lines/mm) Calculated flux (1.9 GeV, 400 mA) 1013 photons/s/0.1%BW at 500 eV Resolving power (E/DE) 1,000 Beam size Focused: 70 x 10 µm Unfocused: 200 x 200 µm Endstations 12.0.2.1: Coherent optics 12.0.2.2: Coherent scattering Detectors DetectorsCCD, photodiode, scintillator Scientific applications Branchlines designed for spatially coherent soft x-ray experiments

470

Beamline 12.0.2  

NLE Websites -- All DOE Office Websites (Extended Search)

2 Print 2 Print Coherent science Scientific disciplines: Applied science, magnetism, materials science Endstations: 12.0.2.1: Coherent optics 12.0.2.2: Coherent x-ray scattering GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Third harmonic of 8-cm-period undulator (U8) Energy range 300-1500 eV Monochromator VLS-PGM, with two gratings (600 and 1200 lines/mm) Calculated flux (1.9 GeV, 400 mA) 1013 photons/s/0.1%BW at 500 eV Resolving power (E/DE) 1,000 Beam size Focused: 70 x 10 µm Unfocused: 200 x 200 µm Endstations 12.0.2.1: Coherent optics 12.0.2.2: Coherent scattering Detectors DetectorsCCD, photodiode, scintillator Scientific applications Branchlines designed for spatially coherent soft x-ray experiments

471

Beamline 11.0.1  

NLE Websites -- All DOE Office Websites (Extended Search)

1 Print 1 Print PEEM3, Soft X-Ray Scattering Scientific disciplines: Magnetism, materials, surface science, polymers Endstations: 11.0.1.1: Photoemission electron microscope (PEEM3) 11.0.1.2: Soft x-ray scattering GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics 5.0-cm period elliptical polarization undulator (EPU5) Energy range 150-2000 eV Monochromator VLS-PGM Calculated flux (1.9 GeV, 400 mA) 1013 photons/s/0.1%BW at 800 eV Resolving power (E/ΔE) 4,000 at 800 eV Endstations 11.0.1.1: Photoemission electron microscope (PEEM3) 11.0.1.2: Soft x-ray scattering Special notes Polarization is user selectable; linear polarization continuously variable from horizontal to vertical; left and right elliptical (or circular) polarization

472

Beamline 12.0.2  

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2.0.2 Print 2.0.2 Print Coherent science Scientific disciplines: Applied science, magnetism, materials science Endstations: 12.0.2.1: Coherent optics 12.0.2.2: Coherent x-ray scattering GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Third harmonic of 8-cm-period undulator (U8) Energy range 300-1500 eV Monochromator VLS-PGM, with two gratings (600 and 1200 lines/mm) Calculated flux (1.9 GeV, 400 mA) 1013 photons/s/0.1%BW at 500 eV Resolving power (E/DE) 1,000 Beam size Focused: 70 x 10 µm Unfocused: 200 x 200 µm Endstations 12.0.2.1: Coherent optics 12.0.2.2: Coherent scattering Detectors DetectorsCCD, photodiode, scintillator Scientific applications Branchlines designed for spatially coherent soft x-ray experiments

473

Development of in situ, at-wavelength metrology for soft x-ray nano-focusing  

SciTech Connect

At the Advanced Light Source (ALS), we are developing broadly applicable, high-accuracy, in situ, at-wavelength wavefront slope measurement techniques for Kirkpatrick-Baez (KB) mirror nano-focusing. We describe here details of the metrology beamline endstation, the at-wavelength tests, and an original alignment method that have already allowed us to precisely set a bendable KB mirror to achieve a FWHM focused spot size of ~;;120 nm, at 1-nm soft x-ray wavelength.

Yuan, Sheng Sam; Yashchuk, Valeriy V.; Goldberg, Kenneth A.; Celestre, Richard; McKinney, Wayne R.; Morrison, Gregory Y.; Warwick, Tony; Padmore, Howard A.

2010-09-19T23:59:59.000Z

474

Comparative risk analysis for the Rocky Flats Plant Integrated Project Planning  

SciTech Connect

The Rocky Flats Plant is developing a comprehensive planning strategy that will support transition of the Rocky Flats Plant from a nuclear weapons production facility to site cleanup and final disposition. Final disposition of the Rocky Flats Plant materials and contaminants requires consideration of the interrelated nature of sitewide problems, such as material movement and disposition, facility and land use endstates, costs, relative risks to workers and the public, and waste disposition. Comparative Risk Analysis employs both incremental risk and cumulative risk evaluations to compare risk from postulated options or endstates. Comparative Risk Analysis is an analytical tool for the Rocky Flats Plant Integrated Project Planning which can assist a decision-maker in evaluating relative risks among proposed remedial options or future endstates. It addresses the cumulative risks imposed by the Rocky Flats Plant and provides risk information, both human health and ecological, to aid in reducing unnecessary resource and monetary expenditures. Currently, there is no approved methodology that aggregates various risk estimates. Along with academic and field expert review, the Comparative Risk Analysis methodology is being reviewed and refined. A Rocky Flats Plant Risk Assessment Focus Group was established. Stakeholder involvement in the development provides an opportunity to influence the information delivered to a decision-maker. This paper discusses development of the methodology.

Jones, M.E. [EG& G Rocky Flats, Inc., Englewood, CO (United States); Shain, D.I. [EG& G Rocky Flats, Inc., Golden, CO (United States)

1994-12-31T23:59:59.000Z

475

On the Origin of Interstellar Radio Disturbances  

Science Journals Connector (OSTI)

...Observatory, Cambridge, Massachusetts On the Origin of Interstellar...Observatory, Cambridge, Massachusetts. | Journal Article VOL...OBSERVATORY, CAMBRIDGE, MASSACHUSETTS Communicated February 5...the non-appearance of a solar effect in the received intensities...

Fred L. Whipple; Jesse L. Greenstein

1937-01-01T23:59:59.000Z

476

On the Correction to Saha's Formula for Small Deviations from Thermodynamic Equilibrium  

Science Journals Connector (OSTI)

...Observatory, Cambridge, Massachusetts On the Correction to Saha's...Observatory, Cambridge, Massachusetts. | Journal Article ASTRONOMY...OBSERVATORY, CAMBRIDG}, MASSACHUSETTS Communicated March 4, 1927...the ionization theory to solar and stellar physics are based...

B. P. Gerasimovi?

1927-01-01T23:59:59.000Z

477

EVIDENCE FOR A COMET BELT BEYOND NEPTUNE  

Science Journals Connector (OSTI)

...OBSERVATORY, CAMBRIDGE, MASSACHUSETTS HARVARD COLLEGE OBSERVATORY, CAMBRIDGE, MASSACHUSETTS EVIDENCE FOR A COMET...OBSERVATORY, CAMBRIDGE, MASSACHUSETTS. | Journal Article Proceedings...the outskirts of the solar system." I concur with...

Fred L. Whipple

1964-01-01T23:59:59.000Z

478

E-Print Network Topics: N  

NLE Websites -- All DOE Office Websites (Extended Search)

base naval nuclear propulsion naval observatory ccd naval observatory vlbi naval oil shale reserves naval oil shale naval ordnance laboratory naval ordnance test naval petroleum...

479

E-Print Network 3.0 - atmospheric cerenkov telescopes Sample...  

NLE Websites -- All DOE Office Websites (Extended Search)

Group Collection: Physics 67 The Pierre Auger Observatory: Perspectives on Ultra-High Energy Summary: in Argentina. The Observatory will consist when completed of 1600 water...

480

Press Pass - Press Releases  

NLE Websites -- All DOE Office Websites (Extended Search)

observatory Scientists of the Pierre Auger Observatory, a project to study the highest-energy cosmic rays, will celebrate the inauguration of their 3000-square-kilometer...

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


481

E-Print Network 3.0 - astrographs Sample Search Results  

NLE Websites -- All DOE Office Websites (Extended Search)

of Solar System Bodies with Telescopes of Pulkovo Observatory Summary: ), and ZA-320M mirror astrograph of Pulkovo observatory. In the Laboratory, investigations are carried......

482

Hermann C. Vogel, 18421907  

Science Journals Connector (OSTI)

... director of the Potsdam Observatory since 1882, and at his death he was succeeded by Schwarzschild. ...

1942-03-28T23:59:59.000Z

483

Solar Phys (2013) 288:637650 DOI 10.1007/s11207-013-0317-5  

E-Print Network (OSTI)

Coronagraph (LASCO: Brueckner et al., 1995) onboard the Solar and Heliospheric Observatory (SOHO) have made

484

RESEARCH POSTER PRESENTATION DESIGN 2012 www.PosterPresentations.com  

E-Print Network (OSTI)

-based Neutrino Observatory (INO) [1] - a proposed underground facility to look for atmospheric neutrinos

Shyamasundar, R.K.

485

A SIMULATION STUDY ON THE HADRONIC RESPONSE OF THE INO-ICAL DETECTOR Moon Moon Devi  

E-Print Network (OSTI)

. INTRODUCTION · The India-based Neutrino Observatory (INO) is a proposed underground facility for hosting

Shyamasundar, R.K.

486

THE NEUTRINO ENERGY & DIRECTION RESOLUTIONS IN THE INO-ICAL DETECTOR Moon Moon Devi  

E-Print Network (OSTI)

-based Neutrino Observatory (INO) [1] is a proposed underground facility for hosting de- cisive neutrino

Shyamasundar, R.K.

487

RESEARCH POSTER PRESENTATION DESIGN 2012 www.PosterPresentations.com  

E-Print Network (OSTI)

-based Neutrino Observatory (INO) [1] is a proposed underground facility to look for atmospheric neutrinos

Shyamasundar, R.K.

488

Notes  

Science Journals Connector (OSTI)

... director of the astrophysical observatory at Potsdam, in succession to the late Prof. K. Schwarzschild.

1917-08-09T23:59:59.000Z

489

Computer code for double beta decay QRPA based calculations  

E-Print Network (OSTI)

. The Enriched Xenon Observatory for neutrinoless double beta decay (EXO) will search for the rare decays

Bertulani, Carlos A. - Department of Physics and Astronomy, Texas A&M University

490

The Journal of the European Association of Studies on Australia, Vol.3. No.2, 2012, ISSN 1988-5946 under the auspices of Coolabah Observatori: Centre d'Estudis  

E-Print Network (OSTI)

, Universitat de Barcelona 2 "Australia's Decision": Uranium Mining and Aboriginal Communities of direct economic rewards. A case in point is that of uranium mining which, well after the Second World War with uranium mining for peaceful purposes at Ranger (Northern Territory), and comparing it with the more recent

Paris-Sud XI, Université de

491

Solar Meridional Circulation from Doppler Shifts of the Fe I line at lambda 5250 Angstroms as Measured by the 150-foot Solar Tower Telescope at the Mt. Wilson Observatory  

E-Print Network (OSTI)

Doppler shifts of the Fe I spectral line at lambda5250 Angstroms from the full solar disk obtained over the period 1986 to 2009 are analyzed to determine the circulation velocity of the solar surface along meridional planes. Simultaneous measurements of the Zeeman splitting of this line are used to obtain measurements of the solar magnetic field that are used to select low field points and impose corrections for the magnetically induced Doppler shift. The data utilized is from a new reduction that preserves the full spatial resolution of the original observations so that the circulation flow can be followed to latitudes of 80 degrees N/S. The deduced meridional flow is shown to differ from the circulation velocities derived from magnetic pattern movements. A reversed circulation pattern is seen in polar regions for three successive solar minima. An surge in circulation velocity at low latitudes is seen during the rising phases of cycles 22 and 23.

Ulrich, Roger K

2010-01-01T23:59:59.000Z

492

MOSE: operational forecast of the optical turbulence and atmospheric parameters at European Southern Observatory ground-based sites II. Atmospheric parameters in the surface layer 030 m  

Science Journals Connector (OSTI)

......filtering of the weak winds) and is always inferior...to the threshold of the wind speed. The improvements...orography of both sites (local peaks surrounded by mountainous...difficulties in forecasting the wind direction in such conditions...another mesocale model, wrf. Indeed, using a nesting......

F. Lascaux; E. Masciadri; L. Fini

2013-01-01T23:59:59.000Z

493

New Ion Beam Materials Laboratory for Materials Modification and Irradiation Effects Research  

SciTech Connect

A new multifunctional ion beam materials laboratory (IBML) has been established at the University of Tennessee, in partnership with Oak Ridge National Laboratory. The IBML is currently equipped with two ion sources, a 3 MV tandem accelerator, three beamlines and three endstations. The IBML is primarily dedicated to fundamental research on ion-solid interaction, ion beam analysis, ion beam modification, and other basic and applied research on irradiation effects in a wide range of materials. An overview of the IBML facility is provided, and experimental results are reported to demonstrate the specific capabilities.

Zhang, Yanwen [ORNL; Crespillo, Miguel L [University of Tennessee (UT); Xue, Haizhou [University of Tennessee, Knoxville (UTK); Jin, Ke [University of Tennessee, Knoxville (UTK); Chen, Chien-Hung [University of Tennessee, Knoxville (UTK); Fontana, Cristiano L [ORNL; Graham, Dr. Joseph T. [The University of Tennessee; Weber, William J [ORNL

2014-01-01T23:59:59.000Z

494

Chemical Sciences Division annual report 1994  

SciTech Connect

The division is one of ten LBL research divisions. It is composed of individual research groups organized into 5 scientific areas: chemical physics, inorganic/organometallic chemistry, actinide chemistry, atomic physics, and chemical engineering. Studies include structure and reactivity of critical reaction intermediates, transients and dynamics of elementary chemical reactions, and heterogeneous and homogeneous catalysis. Work for others included studies of superconducting properties of high-{Tc} oxides. In FY 1994, the division neared completion of two end-stations and a beamline for the Advanced Light Source, which will be used for combustion and other studies. This document presents summaries of the studies.

NONE

1995-06-01T23:59:59.000Z

495

The Current Performance of the Wide Range (90-2500 eV) Soft X-ray Beamline at the Australian Synchrotron  

SciTech Connect

The Soft X-ray beamline at the Australian synchrotron has been constructed around a collimated light Plane Grating Monochromator taking light from an Elliptically Polarized Undulator (EPU). The beamline covers a wide photon energy range between 90 to 2500 eV, using two gratings of 250 l/mm and 1200 l/mm. At present the output from the monochromator is directed into one branchline with a dedicated UHV endstation. The measured performance of the beamline in flux and resolution is shown to be very close to that of theoretical calculations.

Cowie, B. C. C.; Tadich, A.; Thomsen, L. [Australian Synchrotron, 800 Blackburn Road, Clayton, Victoria (Australia)

2010-06-23T23:59:59.000Z

496

The New X-Ray Lithography Beamline BL1 At DELTA  

SciTech Connect

Lithography using synchrotron radiation in the x-ray regime provides a powerful method to produce mechanical components of sub-millimeter size with a very good quality for microtechnological applications. In recent years the demand for x-ray lithography beamtime for industrial production of microparts increased rapidly resulting in the development of new experimental endstations at synchrotron radiation sources dedicated for the production of micromechanical devices. We present in this work the layout of the new x-ray lithography beamline BL1 at the synchrotron radiation source DELTA in Dortmund and discuss first results of exposure tests.

Lietz, D.; Paulus, M.; Sternemann, C.; Berges, U.; Hippert, B.; Tolan, M. [Fakultaet Physik / DELTA, TU Dortmund, Maria-Goeppert-Mayer-Str. 2, 44227 Dortmund (Germany)

2010-06-23T23:59:59.000Z

497

Achieving Vibration Stability of the NSLS-II Hard X-ray Nanoprobe Beamline  

SciTech Connect

The hard x-ray nanoprobe (HXN) beamline of the National Synchrotron Light Source II (NSLS-II) requires high levels of stability in order to achieve the desired instrument resolution. To ensure that the design of the endstation helps meet the stringent criteria and that natural and cultural vibration is mitigated both passively and actively, a comprehensive study complimentary to the design process has been undertaken. Vibration sources that have the potential to disrupt sensitive experiments such as wind, traffic, and NSLS II operating systems have been studied using state-of-the-art simulations and an array of field data. Further, final stage vibration isolation principles have been explored.

Simos, N.; Chu, Y. S.; Broadbent, A.; Nazaretski, E.; Margulies, L.; Dyling, O.; Shen, Q.; Fallier, M. [National Synchrotron Light Source II, Brookhaven National Laboratory, Upton, NY 11973 (United States)

2011-09-09T23:59:59.000Z

498

ALSNews Vol. 308  

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8 Print 8 Print In This Issue Rotary Firing in Ring-Shaped Protein Explains Unidirectionality Biomimetic Dye Molecules for Solar Cells Photon Science for Renewable Energy: A News ALS Brochure Everything You Wanted To Know About ALS Proposals, Beam Time Allocations ALS Science Cafés Successful, Continue VUVX 2010 Conference Update Ring Leaders: Scientific Support Group Announcements: Vogue Shines Light on the ALS, ALS Facebook Flourishing, Guest House Special Extended Who's in the News Operations Update News Links RingLeaders Ring Leaders Scientific Support Division Deputy for Scientific Support Zahid Hussein introduces the Scientific Support Group's duties, goals, and achievements. Read the Article announcements Announcements Vogue Shines Light on the ALS The April issue of Vogue magazine features "Great American Women," including Facebook COO Sheryl Sandberg, whose photo was taken in front of the microARPES endstation of the MAESTRO beamline (Sector 7). The computers all show Facebook, but the high-tech background of the endstation stands out behind Sandberg. Read the Vogue story

499

Beamline 12.0.2  

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0.2 0.2 Beamline 12.0.2 Print Tuesday, 20 October 2009 09:30 Coherent science Scientific disciplines: Applied science, magnetism, materials science Endstations: 12.0.2.1: Coherent optics 12.0.2.2: Coherent x-ray scattering GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Third harmonic of 8-cm-period undulator (U8) Energy range 300-1500 eV Monochromator VLS-PGM, with two gratings (600 and 1200 lines/mm) Calculated flux (1.9 GeV, 400 mA) 1013 photons/s/0.1%BW at 500 eV Resolving power (E/DE) 1,000 Beam size Focused: 70 x 10 µm Unfocused: 200 x 200 µm Endstations 12.0.2.1: Coherent optics 12.0.2.2: Coherent scattering Detectors DetectorsCCD, photodiode, scintillator Scientific applications Branchlines designed for spatially coherent soft x-ray experiments

500

ALSNews Vol. 308  

NLE Websites -- All DOE Office Websites (Extended Search)

8 Print 8 Print In This Issue Rotary Firing in Ring-Shaped Protein Explains Unidirectionality Biomimetic Dye Molecules for Solar Cells Photon Science for Renewable Energy: A News ALS Brochure Everything You Wanted To Know About ALS Proposals, Beam Time Allocations ALS Science Cafés Successful, Continue VUVX 2010 Conference Update Ring Leaders: Scientific Support Group Announcements: Vogue Shines Light on the ALS, ALS Facebook Flourishing, Guest House Special Extended Who's in the News Operations Update News Links RingLeaders Ring Leaders Scientific Support Division Deputy for Scientific Support Zahid Hussein introduces the Scientific Support Group's duties, goals, and achievements. Read the Article announcements Announcements Vogue Shines Light on the ALS The April issue of Vogue magazine features "Great American Women," including Facebook COO Sheryl Sandberg, whose photo was taken in front of the microARPES endstation of the MAESTRO beamline (Sector 7). The computers all show Facebook, but the high-tech background of the endstation stands out behind Sandberg. Read the Vogue story