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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

FAMS DECOMMISSIONING END-STATE ALTERNATIVE EVALUATION  

SciTech Connect

Nuclear Material Management (NMM) completed a comprehensive study at the request of the Department of Energy Savannah River Operations Office (DOE-SR) in 2004 (Reference 11.1). The study evaluated the feasibility of removal and/or mitigation of the Pu-238 source term in the F-Area Material Storage (FAMS) facility during on-going material storage operations. The study recommended different options to remove and/or mitigate the Pu-238 source term depending on its location within the facility. During April 2005, the Department of Energy (DOE) sent a letter of direction (LOD) to Washington Savannah River Company (WSRC) directing WSRC to implement a new program direction that would enable an accelerated shutdown and decommissioning of FAMS (Reference 11.2). Further direction in the LOD stated that effective December 1, 2006 the facility will be transitioned to begin deactivation and decommissioning (D&D) activities. To implement the LOD, Site D&D (SDD) and DOE agreed the planning end-state would be demolition of the FAMS structure to the building slab. SDD developed the D&D strategy, preliminary cost and schedule, and issued the deactivation project plan in December 2005 (Reference 11.3). Due to concerns and questions regarding the FAMS planning end-state and in support of the project's Critical Decision 1, an alternative study was performed to evaluate the various decommissioning end-states and the methods by which those end-states are achieved. This report documents the results of the alternative evaluation which was performed in a structured decision-making process as outlined in the E7 Manual, Procedure 2.15, ''Alternative Studies'' (Reference 11.4).

Grimm, B; Stephen Chostner, S; Brenda Green, B

2006-05-25T23:59:59.000Z

3

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

4

Quantum Monte Carlo Endstation for Petascale Computing  

SciTech Connect

NCSU research group has been focused on accomplising the key goals of this initiative: establishing new generation of quantum Monte Carlo (QMC) computational tools as a part of Endstation petaflop initiative for use at the DOE ORNL computational facilities and for use by computational electronic structure community at large; carrying out high accuracy quantum Monte Carlo demonstration projects in application of these tools to the forefront electronic structure problems in molecular and solid systems; expanding the impact of QMC methods and approaches; explaining and enhancing the impact of these advanced computational approaches. In particular, we have developed quantum Monte Carlo code (QWalk, www.qwalk.org) which was significantly expanded and optimized using funds from this support and at present became an actively used tool in the petascale regime by ORNL researchers and beyond. These developments have been built upon efforts undertaken by the PI's group and collaborators over the period of the last decade. The code was optimized and tested extensively on a number of parallel architectures including petaflop ORNL Jaguar machine. We have developed and redesigned a number of code modules such as evaluation of wave functions and orbitals, calculations of pfaffians and introduction of backflow coordinates together with overall organization of the code and random walker distribution over multicore architectures. We have addressed several bottlenecks such as load balancing and verified efficiency and accuracy of the calculations with the other groups of the Endstation team. The QWalk package contains about 50,000 lines of high quality object-oriented C++ and includes also interfaces to data files from other conventional electronic structure codes such as Gamess, Gaussian, Crystal and others. This grant supported PI for one month during summers, a full-time postdoc and partially three graduate students over the period of the grant duration, it has resulted in 13 published papers, 15 invited talks and lectures nationally and internationally. My former graduate student and postdoc Dr. Michal Bajdich, who was supported byt this grant, is currently a postdoc with ORNL in the group of Dr. F. Reboredo and Dr. P. Kent and is using the developed tools in a number of DOE projects. The QWalk package has become a truly important research tool used by the electronic structure community and has attracted several new developers in other research groups. Our tools use several types of correlated wavefunction approaches, variational, diffusion and reptation methods, large-scale optimization methods for wavefunctions and enables to calculate energy differences such as cohesion, electronic gaps, but also densities and other properties, using multiple runs one can obtain equations of state for given structures and beyond. Our codes use efficient numerical and Monte Carlo strategies (high accuracy numerical orbitals, multi-reference wave functions, highly accurate correlation factors, pairing orbitals, force biased and correlated sampling Monte Carlo), are robustly parallelized and enable to run on tens of thousands cores very efficiently. Our demonstration applications were focused on the challenging research problems in several fields of materials science such as transition metal solids. We note that our study of FeO solid was the first QMC calculation of transition metal oxides at high pressures.

Lubos Mitas

2011-01-26T23:59:59.000Z

5

Quantum Monte Carlo Endstation for Petascale Computing  

Science Conference Proceedings (OSTI)

The major achievements enabled by QMC Endstation grant include * Performance improvement on clusters of x86 multi-core systems, especially on Cray XT systems * New and improved methods for the wavefunction optimizations * New forms of trial wavefunctions * Implementation of the full application on NVIDIA GPUs using CUDA The scaling studies of QMCPACK on large-scale systems show excellent parallel efficiency up to 216K cores on Jaguarpf (Cray XT5). The GPU implementation shows speedups of 10-15x over the CPU implementation on older generation of x86. We have implemented hybrid OpenMP/MPI scheme in QMC to take advantage of multi-core shared memory processors of petascale systems. Our hybrid scheme has several advantages over the standard MPI-only scheme. * Memory optimized: large read-only data to store one-body orbitals and other shared properties to represent the trial wave function and many-body Hamiltonian can be shared among threads, which reduces the memory footprint of a large-scale problem. * Cache optimized: the data associated with an active Walker are in cache during the compute-intensive drift-diffusion process and the operations on an Walker are optimized for cache reuse. Thread-local objects are used to ensure the data affinity to a thread. * Load balanced: Walkers in an ensemble are evenly distributed among threads and MPI tasks. The two-level parallelism reduces the population imbalance among MPI tasks and reduces the number of point-to-point communications of large messages (serialized objects) for the Walker exchange. * Communication optimized: the communication overhead, especially for the collective operations necessary to determine ET and measure the properties of an ensemble, is significantly lowered by using less MPI tasks. The multiple forms of parallelism afforded by QMC algorithms make them ideal candidates for acceleration in the many-core paradigm. We presented the results of our effort to port the QMCPACK simulation code to the NVIDIA CUDA GPU platform. We restructured the CPU algorithms to express additional parallelism, minimize GPU-CPU communication, and efficiently utilize the GPU memory hierarchy. Using mixed precision on GT200 GPUs and MPI for intercommunication and load balancing, we observe typical full-application speedups of approximately 10x to 15x relative to quad-core Xeon CPUs alone, while reproducing the double-precision CPU results within statistical error. We developed an all-electron quantum Monte Carlo (QMC) method for solids that does not rely on pseudopotentials, and used it to construct a primary ultra-high-pressure calibration based on the equation of state of cubic boron nitride. We computed the static contribution to the free energy with the QMC method and obtained the phonon contribution from density functional theory, yielding a high-accuracy calibration up to 900 GPa usable directly in experiment. We computed the anharmonic Raman frequency shift with QMC simulations as a function of pressure and temperature, allowing optical pressure calibration. In contrast to present experimental approaches, small systematic errors in the theoretical EOS do not increase with pressure, and no extrapolation is needed. This all-electron method is applicable to first-row solids, providing a new reference for ab initio calculations of solids and benchmarks for pseudopotential accuracy. We compared experimental and theoretical results on the momentum distribution and the quasiparticle renormalization factor in sodium. From an x-ray Compton-profile measurement of the valence-electron momentum density, we derived its discontinuity at the Fermi wavevector finding an accurate measure of the renormalization factor that we compared with quantum-Monte-Carlo and G0W0 calculations performed both on crystalline sodium and on the homogeneous electron gas. Our calculated results are in good agreement with the experiment. We have been studying the heat of formation for various Kubas complexes of molecular hydrogen on Ti(1,2)ethylene-nH2 using Diffusion Monte Carlo. This work has been started and is o

David Ceperley

2011-03-02T23:59:59.000Z

6

CALIPSO/CALIOP Cloud Phase Discrimination Algorithm  

Science Conference Proceedings (OSTI)

The current cloud thermodynamic phase discrimination by Cloud-Aerosol Lidar Pathfinder Satellite Observations (CALIPSO) is based on the depolarization of backscattered light measured by its lidar [Cloud-Aerosol Lidar with Orthogonal Polarization (...

Yongxiang Hu; David Winker; Mark Vaughan; Bing Lin; Ali Omar; Charles Trepte; David Flittner; Ping Yang; Shaima L. Nasiri; Bryan Baum; Robert Holz; Wenbo Sun; Zhaoyan Liu; Zhien Wang; Stuart Young; Knut Stamnes; Jianping Huang; Ralph Kuehn

2009-11-01T23:59:59.000Z

7

Evaluation of AIRS cloud thermodynamic phase determination with CALIPSO  

Science Conference Proceedings (OSTI)

The Atmospheric Infrared Sounder (AIRS) infrared-based cloud thermodynamic phase retrievals are evaluated using the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) cloud thermodynamic phase. The AIRS cloud phase is ...

Hongchun Jin; Shaima L. Nasiri

8

The CALIPSO Automated Aerosol Classification and Lidar Ratio Selection Algorithm  

Science Conference Proceedings (OSTI)

Descriptions are provided of the aerosol classification algorithms and the extinction-to-backscatter ratio (lidar ratio) selection schemes for the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) aerosol products. One ...

Ali H. Omar; David M. Winker; Mark A. Vaughan; Yongxiang Hu; Charles R. Trepte; Richard A. Ferrare; Kam-Pui Lee; Chris A. Hostetler; Chieko Kittaka; Raymond R. Rogers; Ralph E. Kuehn; Zhaoyan Liu

2009-10-01T23:59:59.000Z

9

CALIPSO-Derived Three-Dimensional Structure of Aerosol over the Atlantic Basin and Adjacent Continents  

Science Conference Proceedings (OSTI)

Accurate modeling of the impact of aerosols on climate requires a detailed understanding of the vertical distribution of aerosols. The CloudAerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) provides continuous high-resolution ...

Aaron M. Adams; Joseph M. Prospero; Chidong Zhang

2012-10-01T23:59:59.000Z

10

Remote sensing of atmospheric particles using LIDAR, Calipso satellite, & AERONET: algorithm development  

Science Conference Proceedings (OSTI)

Algorithms have been developed for the determination of essential parameters such as Aerosol Size Distribution, Angstrom coefficient, and Single Scattering Albedo necessary in the determination of regional climatological model and weather prediction ... Keywords: AERONET, Calipso, atmospheric parameters, lidar, remote sensing

Javier Mndez; Hamed Parsiani; Emmanuel Sanchez

2009-01-01T23:59:59.000Z

11

The CALIPSO Lidar Cloud and Aerosol Discrimination: Version 2 Algorithm and Initial Assessment of Performance  

Science Conference Proceedings (OSTI)

The CloudAerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) satellite was launched in April 2006 to provide global vertically resolved measurements of clouds and aerosols. Correct discrimination between clouds and aerosols ...

Zhaoyan Liu; Mark Vaughan; David Winker; Chieko Kittaka; Brian Getzewich; Ralph Kuehn; Ali Omar; Kathleen Powell; Charles Trepte; Chris Hostetler

2009-07-01T23:59:59.000Z

12

Tropical Tropopause Transition Layer Cirrus as Represented by CALIPSO Lidar Observations  

Science Conference Proceedings (OSTI)

The spatial and temporal variability of cirrus cloud fraction within the tropical tropopause transition layer (TTL) is investigated based on three years of data from the CloudAerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) ...

Katrina S. Virts; John M. Wallace; Qiang Fu; Thomas P. Ackerman

2010-10-01T23:59:59.000Z

13

Quantum Monte Carlo algorithms for electronic structure at the petascale; the endstation project.  

SciTech Connect

Over the past two decades, continuum quantum Monte Carlo (QMC) has proved to be an invaluable tool for predicting of the properties of matter from fundamental principles. By solving the Schrodinger equation through a stochastic projection, it achieves the greatest accuracy and reliability of methods available for physical systems containing more than a few quantum particles. QMC enjoys scaling favorable to quantum chemical methods, with a computational effort which grows with the second or third power of system size. This accuracy and scalability has enabled scientific discovery across a broad spectrum of disciplines. The current methods perform very efficiently at the terascale. The quantum Monte Carlo Endstation project is a collaborative effort among researchers in the field to develop a new generation of algorithms, and their efficient implementations, which will take advantage of the upcoming petaflop architectures. Some aspects of these developments are discussed here. These tools will expand the accuracy, efficiency and range of QMC applicability and enable us to tackle challenges which are currently out of reach. The methods will be applied to several important problems including electronic and structural properties of water, transition metal oxides, nanosystems and ultracold atoms.

Kim, J; Ceperley, D M; Purwanto, W; Walter, E J; Krakauer, H; Zhang, S W; Kent, P.R. C; Hennig, R G; Umrigar, C; Bajdich, M; Kolorenc, J; Mitas, L

2008-10-01T23:59:59.000Z

14

Retrieval of cloud properties using CALIPSO Imaging Infrared Radiometer. Part II: effective diameter and ice water path  

Science Conference Proceedings (OSTI)

The paper describes the version 3 Level 2 operational analysis of the Imaging Infrared Radiometer (IIR) data collected in the framework of the CALIPSO mission to retrieve cirrus cloud effective diameter and ice water path in synergy with the ...

Anne Garnier; Jacques Pelon; Philippe Dubuisson; Ping Yang; Michal Faivre; Olivier Chomette; Nicolas Pascal; Pat Lucker; Tim Murray

15

The Boulder Atmospheric Observatory  

Science Conference Proceedings (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

16

Study of Horizontally Oriented Ice Crystals with CALIPSO Observations and Comparison with Monte Carlo Radiative Transfer Simulations  

E-Print Network (OSTI)

Study of Horizontally Oriented Ice Crystals with CALIPSO Observations and Comparison with Monte oriented ice crystals (HOIC) occur frequently in both ice and mixed-phase clouds. When compared with the case for clouds consisting of randomly oriented ice crystals (ROIC), lidar measurements from clouds

Baum, Bryan A.

17

CALIPSO/CALIOP Cloud Phase Discrimination Algorithm YONGXIANG HU,* DAVID WINKER,* MARK VAUGHAN,* BING LIN,* ALI OMAR,* CHARLES TREPTE,*  

E-Print Network (OSTI)

In passive remote sensing, cloud thermodynamic phase (water or ice) information typically comes from the specCALIPSO/CALIOP Cloud Phase Discrimination Algorithm YONGXIANG HU,* DAVID WINKER,* MARK VAUGHAN The current cloud thermodynamic phase discrimination by Cloud-Aerosol Lidar Pathfinder Satellite Ob

Baum, Bryan A.

18

The Mount Bachelor Observatory  

Science Conference Proceedings (OSTI)

The Mount Bachelor Observatory, is an EPRI-sponsored high-elevation mountaintop air quality sampling station that provides an ideal location for assessing the origin and impact of long-range transport of critical contaminantssuch as mercury (Hg), ozone (O3), nitrogen oxides (NOx), and particulate matteron the atmospheric composition along North America's West Coast.

2009-12-04T23:59:59.000Z

19

Comparison of CALIPSO-Like, LaRC, and MODIS Retrievals of Ice-Cloud Properties over SIRTA in France and Florida during CRYSTAL-FACE  

Science Conference Proceedings (OSTI)

This study compares cirrus-cloud properties and, in particular, particle effective radius retrieved by a Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation (CALIPSO)-like method with two similar methods using Moderate-Resolution ...

M. Chiriaco; H. Chepfer; P. Minnis; M. Haeffelin; S. Platnick; D. Baumgardner; P. Dubuisson; M. McGill; V. Nol; J. Pelon; D. Spangenberg; S. Sun-Mack; G. Wind

2007-03-01T23:59:59.000Z

20

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

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

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 the study of these clouds. Using one of these joint cloud products, 2B-GEOPROF-Lidar, and a post-processing algorithm designed to find horizontally continuous thin clouds within the cloud product, the locations, length scales, and vertical distributions by length of thin clouds are determined. It is found that thin clouds vary in length from a few km to over 2900 km and tend to be longer in the tropical upper troposphere than lower in the atmosphere and at higher latitudes. In the upper troposphere between 0 and 40N, over 20% of all thin cloud measurements in the 2B-GEOPROF-Lidar product are contributed by thin clouds that are longer than 500 km. In fact, in this latitude range, over 65% of all thin cloud measurements are contributed by clouds longer than 100 km. Also, thin cloud length and frequency differ between the four seasons in the year of data used here.

Solbrig, Jeremy E.

2009-08-01T23:59:59.000Z

22

Mobile Climate Observatory on the Pacific  

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

Climate Observatory on the Pacific The AMF2 mobile climate observatory is traveling the Pacific ocean between Los Angeles and Honolulu to improve the way global climate models...

23

National Astronomical Observatory, Japan  

E-Print Network (OSTI)

Abstract. At the altitude of 3,370 m on the Peruvian Andes, a 32m antenna owned by the telecommunications company Telefnica del Per will be transformed to a Radio Telescope, it would be transferred to the Geophysical Institute of Peru (IGP). The parabolic antenna was constructed in 1984 by Nippon Electric Co. (NEC) and worked as an INTELSAT station until 2000. A team of the National Observatory of Japan (NAOJ) evaluated the antenna in 2003 and reported its availability to be used as a Radio Telescope. In collaboration of the NAOJ a 6.7 GHz receiver is under construction and will be installed within this year. Initially the telescope as a single dish will monitor and survey Methanol Maser of YSO, higher frequencies equipment and VLBI instruments will be considered. The antenna will be managed by the IGP and used by universities in Peru, becoming a VLBI station will be a grate contribution to astronomy and geodetic community. 1. The Antenna

R. Colomer; De Vicente; Kenta Fujisawa; Takashi Kasuga; Keisuke Miyazawa; Shinji Horiuchi

2005-01-01T23:59:59.000Z

24

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

25

The Lick Observatory Supernova Search  

Science Conference Proceedings (OSTI)

We report here the current status of the Lick Observatory Supernova Search (LOSS) with the Katzman Automatic Imaging Telescope (KAIT). The progress on both the hardware and the software of the system is described

W. D. Li; A. V. Filippenko; R. R. Treffers; A. Friedman; E. Halderson; R. A. Johnson; J. Y. King; M. Modjaz; M. Papenkova; Y. Sato; T. Shefler

2000-01-01T23:59:59.000Z

26

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

E-Print Network (OSTI)

Two mechanisms appear to be primarily responsible for the formation of cirrus clouds in Tropical Tropopause Layer (TTL): detrainment from deep convective anvils and in situ initiation. Here we propose to identify TTL cirrus clouds by analyzing water content measurements from the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) and Aura Microwave Limb Sounder (MLS). Using ice water content (IWC) and water vapor (H2O) abundances we identify TTL cirrus clouds that contain too much ice to have been formed in situ and therefore must be of convective origin. We use two methods to infer amounts of water vapor available for in situ formation. Clouds with IWC greater than this threshold are categorized as being of convective origin; clouds with IWC below the threshold are ambiguous they could either form from in situ or still be of convective origin. Applying the thresholds from December 2008 to November 2009, we found that at least 19.2% of tropical cirrus were definitively of convective origin at the tropopause (375 K) during boreal winter. At each level, we found three maxima in the occurrence of convective cirrus: western Pacific, equatorial Africa, and South America. Averaged over the entire tropics (30oS to 30oN), we found convective cirrus occurs more frequently in boreal winter and less frequently in boreal summer, basically following the a decreasing trend from DJF, MAM, SON, to JJA. During boreal summer, we found that only 4.6% of tropical cirrus come from convection. Sensitivity tests show that the thresholds derived at 390 K have the largest uncertainty. At lower levels, especially 375 K, our thresholds are robust.

Wang, Tao

2011-05-01T23:59:59.000Z

27

MBO: The Mount Bachelor Observatory  

Science Conference Proceedings (OSTI)

Intercontinental transport of pollutants from Asia has an impact on the atmospheric composition and air quality along the west coast of North America, which in turn has important implications for U.S. air quality. The Mount Bachelor Observatory (MBO) is a high-elevation mountaintop atmospheric observatory, located approximately 120 miles east of Eugene on Oregon's Mt. Bachelor. It provides an ideal location for sampling the global atmosphere in order to assess the impact of Asian long-range transport (AL...

2008-12-23T23:59:59.000Z

28

Validation of IIR/CALIPSO Level 1 Measurements by Comparison with Collocated Airborne Observations during CIRCLE-2 and Biscay 08 Campaigns  

Science Conference Proceedings (OSTI)

In the frame of validation of the spatial observations from the radiometer IIR on board CALIPSO, the two airborne campaigns Cirrus Cloud Experiment (CIRCLE)-2 and Biscay 08 took place in 2007 and 2008 in the western part of France, over the ...

Odran Sourdeval; Grard Brogniez; Jacques Pelon; Laurent C.-Labonnote; Philippe Dubuisson; Frdric Parol; Damien Josset; Anne Garnier; Michal Faivre; Andreas Minikin

2012-05-01T23:59:59.000Z

29

Intercomparison of Deep Convection over the Tibetan PlateauAsian Monsoon Region and Subtropical North America in Boreal Summer Using CloudSat/CALIPSO Data  

Science Conference Proceedings (OSTI)

Deep convection in the Tibetan Plateausouthern Asian monsoon region (TPSAMR) is analyzed using CloudSat and CloudAerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) data for the boreal summer season (JuneAugust) from 2006 to ...

Yali Luo; Renhe Zhang; Weimiao Qian; Zhengzhao Luo; Xin Hu

2011-04-01T23:59:59.000Z

30

The Large Aperture GRB Observatory  

E-Print Network (OSTI)

The Large Aperture GRB Observatory (LAGO) is aiming at the detection of the high energy (around 100 GeV) component of Gamma Ray Bursts, using the single particle technique in arrays of Water Cherenkov Detectors (WCD) in high mountain sites (Chacaltaya, Bolivia, 5300 m a.s.l., Pico Espejo, Venezuela, 4750 m a.s.l., Sierra Negra, Mexico, 4650 m a.s.l). WCD at high altitude offer a unique possibility of detecting low gamma fluxes in the 10 GeV - 1 TeV range. The status of the Observatory and data collected from 2007 to date will be presented.

Allard, D; Asorey, H; Barros, H; Bertou, X; Castillo, M; Chirinos, J M; De Castro, A; Flores, S; Gonzlez, J; Berisso, M Gomez; Grajales, J; Guada, C; Day, W R Guevara; Ishitsuka, J; Lpez, J A; Martnez, O; Melfo, A; Meza, E; Loza, P Miranda; Barbosa, E Moreno; Murrugarra, C; Nez, L A; Ormachea, L J Otiniano; Prez, G; Perez, Y; Ponce, E; Quispe, J; Quintero, C; Rivera, H; Rosales, M; Rovero, A C; Saavedra, O; Salazar, H; Tello, J C; Peralda, R Ticona; Varela, E; Velarde, A; Villaseor, L; Wahl, D; Zamalloa, M A

2009-01-01T23:59:59.000Z

31

The Mount Washington Observatory50 Years Old  

Science Conference Proceedings (OSTI)

The Mount Washington Observatory celebrates its 50th Anniversary this year. The history of the establishment and of the early days of the Observatory is summarized, and its research programs, instrumentation, and facilities from the early days to ...

Alan A. Smith

1982-09-01T23:59:59.000Z

32

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

33

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

34

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

35

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

36

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

37

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

38

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

39

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

40

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.


41

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

42

the Large Aperture GRB Observatory  

SciTech Connect

The Large Aperture GRB Observatory (LAGO) aims at the detection of high energy photons from Gamma Ray Bursts (GRB) using the single particle technique (SPT) in ground based water Cherenkov detectors (WCD). To reach a reasonable sensitivity, high altitude mountain sites have been selected in Mexico (Sierra Negra, 4550 m a.s.l.), Bolivia (Chacaltaya, 5300 m a.s.l.) and Venezuela (Merida, 4765 m a.s.l.). We report on the project progresses and the first operation at high altitude, search for bursts in 6 months of preliminary data, as well as search for signal at ground level when satellites report a burst.

Bertou, Xavier [Centro Atomico Bariloche (Argentina)

2009-04-30T23:59:59.000Z

43

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

44

Upgrade To The Pierre Auger Cosmic Ray Observatory's Lidar System.  

E-Print Network (OSTI)

??The Pierre Auger Cosmic Ray Observatory currently operates four elastic lidar systems in order to characterize the atmospheric aerosol content above the observatory. The atmospheric (more)

Petermann, Emily B

2010-01-01T23:59:59.000Z

45

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

46

The Astrophysical Multimessenger Observatory Network (AMON)  

E-Print Network (OSTI)

We summarize the science opportunity, design elements, current and projected partner observatories, and anticipated science returns of the Astrophysical Multimessenger Observatory Network (AMON). AMON will link multiple current and future high-energy, multimessenger, and follow-up observatories together into a single network, enabling near real-time coincidence searches for multimessenger astrophysical transients and their electromagnetic counterparts. Candidate and high-confidence multimessenger transient events will be identified, characterized, and distributed as AMON alerts within the network and to interested external observers, leading to follow-up observations across the electromagnetic spectrum. In this way, AMON aims to evoke the discovery of multimessenger transients from within observatory subthreshold data streams and facilitate the exploitation of these transients for purposes of astronomy and fundamental physics. As a central hub of global multimessenger science, AMON will also enable cross-collaboration analyses of archival datasets in search of rare or exotic astrophysical phenomena.

M. W. E. Smith; D. B. Fox; D. F. Cowen; P. Mszros; G. Tei?; J. Fixelle; I. Bartos; P. Sommers; Abhay Ashtekar; G. Jogesh Babu; S. D. Barthelmy; S. Coutu; T. DeYoung; A. D. Falcone; L. S. Finn; Shan Gao; B. Hashemi; A. Homeier; S. Mrka; B. J. Owen; I. Taboada

2012-11-23T23:59:59.000Z

47

Signals, backgrounds and calibrations in the Sudbury Neutrino Observatory  

Science Conference Proceedings (OSTI)

The Sudbury Neutrino Observatory is a large underground neutrino detector which is presently under construction

Bhaskar Sur; The SNO Collaboration

1995-01-01T23:59:59.000Z

48

Hanohano:A Deep Ocean Antineutrino Observatory  

E-Print Network (OSTI)

This paper presents the science potential of a deep ocean antineutrino observatory being developed at Hawaii and elsewhere. The observatory design allows for relocation from one site to another. Positioning the observaory some 60 km distant from a nuclear reactor complex enables preecision measurement of neutrino mixing parameters, leading to a determination of neutrino mass hierarchy and theta_13. At a mid-Pacific location, the observatory measures the flux of uranium and thorium decay series antineutrinos from earth's mantle and performs a sensitive search for a hypothetical natural fission reactor in earth's core. A subequent deployment at another mid-ocean location would test lateral homogeneity of uranium and thorium in earth's mantle. These measurements have significance for earth energy studies.

Batygov, M; Learned, J G; Matsuno, S; Pakvasa, S; Varner, G

2008-01-01T23:59:59.000Z

49

Hanohano:A Deep Ocean Antineutrino Observatory  

E-Print Network (OSTI)

This paper presents the science potential of a deep ocean antineutrino observatory being developed at Hawaii and elsewhere. The observatory design allows for relocation from one site to another. Positioning the observaory some 60 km distant from a nuclear reactor complex enables preecision measurement of neutrino mixing parameters, leading to a determination of neutrino mass hierarchy and theta_13. At a mid-Pacific location, the observatory measures the flux of uranium and thorium decay series antineutrinos from earth's mantle and performs a sensitive search for a hypothetical natural fission reactor in earth's core. A subequent deployment at another mid-ocean location would test lateral homogeneity of uranium and thorium in earth's mantle. These measurements have significance for earth energy studies.

M. Batygov; S. T. Dye; J. G. Learned; S. Matsuno; S. Pakvasa; G. Varner

2008-10-03T23:59:59.000Z

50

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

51

Status of the Milagro $\\gamma$ Ray Observatory  

E-Print Network (OSTI)

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

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

2001-01-01T23:59:59.000Z

52

Operations of and Future Plans for the Pierre Auger Observatory  

Science Conference Proceedings (OSTI)

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

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

53

UNIVERSITY OF CALIFORNIA, SANTA CRUZ UNIVERSITY OF CALIFORNIA OBSERVATORIES  

E-Print Network (OSTI)

UNIVERSITY OF CALIFORNIA, SANTA CRUZ UNIVERSITY OF CALIFORNIA OBSERVATORIES Postdoctoral Scholar - Employee The University of California Observatories invites applications for one Postdoctoral Scholar of funding. For appointments within the University of California, the total duration of an individual

California at Santa Cruz, University of

54

UNIVERSITY OF CALIFORNIA, SANTA CRUZ UNIVERSITY OF CALIFORNIA OBSERVATORIES  

E-Print Network (OSTI)

UNIVERSITY OF CALIFORNIA, SANTA CRUZ UNIVERSITY OF CALIFORNIA OBSERVATORIES POSTDOCTORAL SCHOLAR ­ EMPLOYEE The University of California Observatories invites applications for one Postdoctoral Scholar of California, the total duration of an individual's postdoctoral service may not exceed five years, including

California at Santa Cruz, University of

55

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

56

Implementing an Observatory Control System-I. A Generic Approach  

E-Print Network (OSTI)

An architectural framework for implementing a distributed observatory control system is presented here. It has been partially realized and tested in the 2m optical and infrared Observatory at Pune, India.

Sunu Engineer

2004-01-06T23:59:59.000Z

57

The High Altitude Water Cherenkov Observatory  

E-Print Network (OSTI)

The High Altitude Water Cherenkov (HAWC) observatory is a large field of view, continuously operated, TeV gamma-ray experiment under construction at 4,100 m a.s.l. in Mexico. The HAWC observatory will have an order of magnitude better sensitivity, angular resolution, and background rejection than its predecessor, the Milagro experiment. The improved performance will allow us to detect both transient and steady emissions, to study the Galactic diffuse emission at TeV energies, and to measure or constrain the TeV spectra of GeV gamma-ray sources. In addition, HAWC will be the only ground-based instrument capable of detecting prompt emission from gamma-ray bursts above 50 GeV. The HAWC observatory will consist of an array of 300 water Cherenkov detectors (WCDs), each with four photomultiplier tubes. This array is currently under construction on the flanks of the Sierra Negra volcano near the city of Puebla, Mexico. The first thirty WCDs (forming an array approximately the size of Milagro) were deployed in Summer...

,

2013-01-01T23:59:59.000Z

58

POSITION STATEMENT SAVING THE ARECIBO OBSERVATORY  

E-Print Network (OSTI)

A unique world resource, the Arecibo astronomical observatory in Puerto Rico is scheduled to be phased out over the next few years, due to withdrawal of funding by the National Science Foundation. With its 305-meter diameter antenna, the Arecibo Observatory is the world's largest and most sensitive radio-radar telescope. The IEEE recognized the observatory as an electrical engineering milestone in 2002. Arecibo is essential to support the recent congressionally-mandated NASA mission for highprecision tracking and characterizing potentially hazardous Near-Earth Objects (NEOs)--defined as objects 140 meters or greater in diameter, with orbits that may cross that of Earth. A NASA report released last year estimates that, among the many millions of asteroids and comets in the solar system, approximately 100,000 potentially hazardous NEOs are yet to be located. Some assess the likelihood of such an object hitting the earth in a typical human lifetime as about one in sixty. But we are doing little to reduce that likelihood. If a 140 meter NEO were to hit the earth, a huge amount of energy-- equivalent to 100 megatons of TNT-- would be released. As an actual historical reference, the Tunguska event in Siberia in 1908 was most likely caused by a meteor about 40 meters in diameter, exploding at about 10 kilometers altitude. The explosion toppled more than 80 million trees over 2,150 square kilometers, and was about 1,000 times as powerful as the bomb dropped on Hiroshima. IEEE-USA calls upon Congress and the administration to maintain the Arecibo, supporting the congressionally-mandated NASA NEO mission by: Provide funding for the continued operation and maintenance of the Arecibo facility at its present activity level. Directing the National Science Foundation to initiate and/or extend programs and activities to sustain the NASA mission and Encouraging NASA's continued use of Arecibo to carry out the mission

unknown authors

2008-01-01T23:59:59.000Z

59

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

2006-11-22T23:59:59.000Z

60

Solar Neutrino Observations at the Sudbury Neutrino Observatory  

E-Print Network (OSTI)

The Sudbury Neutrino Observatory (SNO) is a 1000-tonne heavy water Cherenkov detector. Its usage of \\dto as target allows the simultaneous measurements of the $\

Poon, A W P

2002-01-01T23:59:59.000Z

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.


61

Solar Neutrino Observations at the Sudbury Neutrino Observatory  

E-Print Network (OSTI)

The Sudbury Neutrino Observatory (SNO) is a 1000-tonne heavy water Cherenkov detector. Its usage of \\dto as target allows the simultaneous measurements of the $\

A. W. P. Poon

2002-11-06T23:59:59.000Z

62

Anisotropy studies with the Pierre Auger Observatory  

E-Print Network (OSTI)

We report recent results from the Pierre Auger Observatory about the study of the anisotropy in the arrival directions of ultra-high energy cosmic rays. We present the results of the search for a dipolar anisotropy at the EeV energy scale. Measurements of the phase and the amplitude of the first harmonic modulation in the right-ascension distribution are discussed. For cosmic rays with energies above 55 EeV, we present an update of the search for correlations between their arrival directions and the positions of active galactic nuclei from the Veron-Cetty and Veron catalog. We also discuss the results of correlation analyses applied to other populations of extragalactic objects. Finally we present the search for anisotropies in the data without the usage of astronomical catalogues.

Neto, J R T de Mello

2013-01-01T23:59:59.000Z

63

The Fan Observatory Bench Optical Spectrograph (FOBOS)  

E-Print Network (OSTI)

The Fan Observatory Bench Optical Spectrograph (FOBOS) is intended for single-object optical spectroscopy at moderate resolution (R~1500-3000) using a fiber-fed, bench-mounted design to maintain stability. Whenever possible, the instrument uses off-the-shelf components to maintain a modest cost. FOBOS supports Galactic astronomy projects that require consistently well-measured (~5 km/sec) radial velocities for large numbers of broadly distributed and relatively bright (Vdesign was optimized for use in the range 470-670 nm. Test data indicate that the instrument is stable and capable of measuring radial velocities with precision better than 3 km/sec at a resolution of R~1500 with minimal calibration overhead.

Jeffrey D. Crane; Steven R. Majewski; Richard J. Patterson; Michael F. Skrutskie; Elena Y. Adams; Peter M. Frinchaboy

2005-02-23T23:59:59.000Z

64

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

65

Neutrino observations from the Sudbury Neutrino Observatory  

SciTech Connect

The Sudbury Neutrino Observatory (SNO) is a water imaging Cherenkov detector. Its usage of 1000 metric tons of D{sub 2}O as target allows the SNO detector to make a solar-model independent test of the neutrino oscillation hypothesis by simultaneously measuring the solar {nu}{sub e} flux and the total flux of all active neutrino species. Solar neutrinos from the decay of {sup 8}B have been detected at SNO by the charged-current (CC) interaction on the deuteron and by the elastic scattering (ES) of electrons. While the CC reaction is sensitive exclusively to {nu}{sub e}, the ES reaction also has a small sensitivity to {nu}{sub {mu}} and {nu}{sub {tau}}. In this paper, recent solar neutrino results from the SNO experiment are presented. It is demonstrated that the solar flux from {sup 8}B decay as measured from the ES reaction rate under the no-oscillation assumption is consistent with the high precision ES measurement by the Super-Kamiokande experiment. The {nu}{sub e} flux deduced from the CC reaction rate in SNO differs from the Super-Kamiokande ES results by 3.3{sigma}. This is evidence for an active neutrino component, in additional to {nu}{sub e}, in the solar neutrino flux. These results also allow the first experimental determination of the total active {sup 8}B neutrino flux from the Sun, and is found to be in good agreement with solar model predictions.

Ahmad, Q.R.; Allen, R.C.; Andersen, T.C.; Anglin, J.D.; Barton,J.C.; Beier, E.W.; Bercovitch, 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.; Buhler, G.; Cameron, J.; Chan, Y.D.; Chen, H.H.; Chen, M.; Chen, X.; Cleveland, B.T.; Clifford, E.T.H.; Cowan, J.H.M.; Cowen, D.F.; Cox, G.A.; Dai, X.; Dalnoki-Veress, F.; Davidson, W.F.; 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.; Ford, R.J.; Formaggio, J.A.; Fowler, M.M.; Frame, K.; Frank, E.D.; Frati, W.; Gagnon, N.; Germani, J.V.; Gil, S.; Graham, K.; Grant, D.R.; 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.; Hepburn, J.D.; Heron, H.; Hewett, J.; Hime, A.; Hykawy, J.G.; Isaac,M.C.P.; Jagam, P.; Jelley, N.A.; Jillings, C.; Jonkmans, G.; Kazkaz, K.; Keener, P.T.; Klein, J.R.; Knox, A.B.; Komar, R.J.; Kouzes, R.; Kutter,T.; Kyba, C.C.M.; Law, J.; Lawson, I.T.; Lay, M.; Lee, H.W.; Lesko, K.T.; Leslie, J.R.; Levine, I.; Locke, W.; Luoma, S.; Lyon, J.; Majerus, S.; Mak, H.B.; Maneira, J.; Manor, J.; Marino, A.D.; McCauley, N.; McDonald,D.S.; McDonald, A.B.; McFarlane, K.; McGregor, G.; Meijer, R.; Mifflin,C.; Miller, G.G.; Milton, G.; Moffat, B.A.; Moorhead, M.; Nally, C.W.; Neubauer, M.S.; Newcomer, F.M.; Ng, H.S.; Noble, A.J.; Norman, E.B.; Novikov, V.M.; O' Neill, M.; Okada, C.E.; Ollerhead, R.W.; Omori, M.; Orrell, J.L.; Oser, S.M.; Poon, A.W.P.; Radcliffe, T.J.; Roberge, A.; Robertson, B.C.; Robertson, R.G.H.; Rosendahl, S.S.E.; Rowley, J.K.; Rusu, V.L.; Saettler, E.; Schaffer, K.K.; Schwendener,M.H.; Schulke, A.; Seifert, H.; Shatkay, M.; Simpson, J.J.; Sims, C.J.; et al.

2001-09-24T23:59:59.000Z

66

Structured Query Language for Virtual Observatory  

E-Print Network (OSTI)

Currently two query languages are defined as standards for the Virtual Observatory (VO). Astronomical Data Query Language (ADQL) is used for catalog data query and Simple Image Access Protocol (SIAP) is for image data query. As a result, when we query each data service, we need to know in advance which language is supported and then construct a query language accordingly. The construct of SIAP is simple, but they have a limited capability. For example, there is no way to specify multiple regions in one query, and it is difficult to specify complex query conditions. In this paper, we propose a unified query language for any kind of astronomical database on the basis of SQL99. SQL is a query language optimized for a table data, so to apply the SQL to the image and spectrum data set, the data structure need to be mapped to a table like structure. We present specification of this query language and an example of the architecture for the database system.

Yuji Shirasaki; Masatoshi Ohishi; Yoshihiko Mizumoto; Masahiro Tanaka; Satoshi Honda; Masafumi Oe; Naoki Yasuda; Yoshifumi Masunaga

2004-11-19T23:59:59.000Z

67

The HAWC observatory as a GRB detector  

E-Print Network (OSTI)

The High Altitude Water Cherenkov Observatory (HAWC) is an air shower array currently under construction in Mexico at an altitude of 4100 m. HAWC will consist of 300 large water tanks covering an area of about 22000 square meters and instrumented with 4 photomultipliers each. The experimental design allows for highly efficient detection of photon-induced air showers in the TeV and sub-TeV range and gamma-hadron separation. We show that HAWC has a reasonable chance to observe the high-energy power law components of GRBs that extend to 50 GeV. In particular, HAWC will be capable of observing events similar to GRB 090510 and GRB 090902B. The observations (or non-observations) of GRBs by HAWC will provide information on the high-energy spectra of GRBs. An engineering array consisting of 6 water tanks was operated at the HAWC site since September 2011, collecting 3 months of data. An upper limit on high energy emission from GRB 111016B is derived from these data.

Zaborov, D

2013-01-01T23:59:59.000Z

68

The Solar Dynamics Observatory: Your eye on the Sun  

Science Conference Proceedings (OSTI)

The Solar Dynamics Observatory (SDO) was launched on February 11, 2010. The instruments on SDO measure the changes in the Sun that cause Space Weather, from power outages, to navigation problems, and satellite drag. EVE measures the Heartbeat of Space ...

W. Dean Pesnell

2011-03-01T23:59:59.000Z

69

Low-multiplicity Burst Search at the Sudbury Neutrino Observatory  

E-Print Network (OSTI)

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

Chen, Min

70

The Lidar System of the Pierre Auger Observatory  

E-Print Network (OSTI)

The Pierre Auger Observatory in Malargue, Argentina, is designed to study the origin of ultrahigh energy cosmic rays with energies above 10^18 eV. The energy calibration of the detector is based on a system of four air fluorescence detectors. To obtain reliable calorimetric information from the fluorescence stations, the atmospheric conditions at the experiment's site need to be monitored continuously during operation. One of the components of the observatory's atmospheric monitoring system is a set of four elastic backscatter lidar stations, one station at each of the fluorescence detector sites. This paper describes the design, current status, standard operation procedure, and performance of the lidar system of the Pierre Auger Observatory.

S. Y. BenZvi; R. Cester; M. Chiosso; B. M. Connolly; A. Filipcic; B. Garcia; A. Grillo; F. Guarino; M. Horvat; M. Iarlori; C. Macolino; J. A. J. Matthews; D. Melo; R. Mussa; M. Mostafa; J. Pallota; S. Petrera; M. Prouza; V. Rizi; M. Roberts; J. R. Rodriguez Rojo; F. Salamida; M. Santander; G. Sequeiros; A. Tonachini; L. Valore; D. Veberic; S. Westerhoff; D. Zavrtanik; M. Zavrtanik

2006-09-03T23:59:59.000Z

71

Spectral Analysis via the Virtual Observatory: The Service Theossa  

E-Print Network (OSTI)

In the framework of the Virtual Observatory, the newly developed service TheoSSA provides access to theoretical stellar spectral-energy distributions. In a pilot phase, this service is based on the well established Tuebingen NLTE Model-Atmosphere Package for hot, compact stars. We demonstrate its present capabilities and future extensions.

Ringat, Ellen; Werner, Klaus

2011-01-01T23:59:59.000Z

72

Installation package for Hyde Memorial Observatory, Lincoln, Nebraska  

DOE Green Energy (OSTI)

This report contains installation information for a solar heating system installed in Hyde Memorial Observatory at Lincoln, Nebraska. This package includes a system operation and maintenance manual, hardware brochures, schematics, system operating modes and drawings. The Solar Engineering and Equipment Company (SEECO) developed this prototype solar heating system, which consists of the following subsystems: solar collector, control, and storage.

Not Available

1978-12-01T23:59:59.000Z

73

Results from the Milagro Gamma-Ray Observatory  

E-Print Network (OSTI)

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

California at Santa Cruz, University of

74

Future development of the PLATO observatory for Antarctic science  

E-Print Network (OSTI)

during the summertime with solar panels. One of the 10-foot shipping containers houses the power system is five months after the last possible human contact with the experiments, and when solar powerFuture development of the PLATO observatory for Antarctic science Michael C. B. Ashley*a, Colin S

Ashley, Michael C. B.

75

e-government procurement observatory model, design and pilot testing  

Science Conference Proceedings (OSTI)

Establishing the maturity level of public procurement portals is useful, as it allows the members of any government procurement network to identify those areas for joint action and it fosters knowledge-sharing among the governments in Latin American ... Keywords: e-procurement, maturity model, measurement, observatory

Gaston Concha; Miguel Porra; Carlos Pimenta

2010-10-01T23:59:59.000Z

76

Visualizing Spatial and Temporal Variability in Coastal Observatories  

Science Conference Proceedings (OSTI)

In this paper, we describe a set of 3D and 4D visualization tools and techniques for CORIE, a complex environmental observation and forecasting system (EOFS) for the Columbia River. The Columbia River, a complex and highly variable estuary, is the target ... Keywords: coastal observatories, environmental observation and forecasting systems, coasts, estuaries, Columbia River

Walter H. Jimenez; Wagner T. Correa; Claudio T. Silva; Baptista Baptista

2003-10-01T23:59:59.000Z

77

BIG BEAR SOLAR OBSERVATORY CENTER FOR SOLAR-TERRESTRIAL RESEARCH  

E-Print Network (OSTI)

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

78

Evaluation, design, and construction of the Wallace Astrophysical Observatory Camera for astronomical observations  

E-Print Network (OSTI)

The goal of this thesis is to upgrade the scientific capabilities of the 24" Cassegrain reflector telescope at the George R. Wallace, Jr. Astrophysical Observatory (Wallace Observatory), part of Massachusetts Institute of ...

Rojas, Folkers Eduardo

2009-01-01T23:59:59.000Z

79

A remote sensing observatory for hydrologic sciences: A genesis for scaling to continental hydrology  

E-Print Network (OSTI)

A remote sensing observatory for hydrologic sciences: A genesis for scaling to continental. It is in this spirit that we advocate establishing a hydrologic remote sensing observatory (RSO) to advance sensing al. (2006), A remote sensing observatory for hydrologic sciences: A genesis for scaling

Katul, Gabriel

80

Measurement of Aerosols at the Pierre Auger Observatory  

E-Print Network (OSTI)

The air fluorescence detectors (FDs) of the Pierre Auger Observatory are vital for the determination of the air shower energy scale. To compensate for variations in atmospheric conditions that affect the energy measurement, the Observatory operates an array of monitoring instruments to record hourly atmospheric conditions across the detector site, an area exceeding 3,000 square km. This paper presents results from four instruments used to characterize the aerosol component of the atmosphere: the Central Laser Facility (CLF), which provides the FDs with calibrated laser shots; the scanning backscatter lidars, which operate at three FD sites; the Aerosol Phase Function monitors (APFs), which measure the aerosol scattering cross section at two FD locations; and the Horizontal Attenuation Monitor (HAM), which measures the wavelength dependence of aerosol attenuation.

S. Y. BenZvi; F. Arqueros; R. Cester; M. Chiosso; B. M. Connolly; B. Fick; A. Filipcic; B. Garca; A. Grillo; F. Guarino; M. Horvat; M. Iarlori; C. Macolino; M. Malek; J. Matthews; J. A. J. Matthews; D. Melo; R. Meyhandan; M. Micheletti; M. Monasor; M. Mostaf; R. Mussa; J. Pallotta; S. Petrera; M. Prouza; V. Rizi; M. Roberts; J. R. Rodriguez Rojo; D. Rodrguez-Fras; F. Salamida; M. Santander; G. Sequeiros; P. Sommers; A. Tonachini; L. Valore; D. Verberic; E. Visbal; S. Westerhoff; L. Wiencke; D. Zavrtanik; M. Zavrtanik; for the Pierre Auger Collaboration

2007-06-21T23:59:59.000Z

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

Testing the surface detector simulation for the Pierre Auger Observatory  

E-Print Network (OSTI)

The building block of the surface detector of the Pierre Auger Observatory is a water Cherenkov tank. The response to shower particles is simulated using a dedi. program based on GEANT4. To check the simulation chain, we compare the simulated signals produced by cosmic muons at various zenith angles with experimental data from a special Cherenkov detector equipped with a muon hodoscope. The signals from muon-decay electrons and the evolution of the charge with water level are also studied.

Ghia, Piera L

2007-01-01T23:59:59.000Z

82

Technology development for a neutrino astrophysical observatory. Letter of intent  

Science Conference Proceedings (OSTI)

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

83

Technology Development for a Neutrino AstrophysicalObservatory  

Science Conference Proceedings (OSTI)

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

84

Testing the surface detector simulation for the Pierre Auger Observatory  

E-Print Network (OSTI)

The building block of the surface detector of the Pierre Auger Observatory is a water Cherenkov tank. The response to shower particles is simulated using a dedicated program based on GEANT4. To check the simulation chain, we compare the simulated signals produced by cosmic muons at various zenith angles with experimental data from a special Cherenkov detector equipped with a muon hodoscope. The signals from muon-decay electrons and the evolution of the charge with water level are also studied.

Piera L. Ghia; for the Pierre Auger Collaboration

2007-06-08T23:59:59.000Z

85

SCALER MODE OF THE AUGER OBSERVATORY AND SUNSPOTS  

Science Conference Proceedings (OSTI)

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

86

Performance of the Pierre Auger Observatory Surface Detector  

E-Print Network (OSTI)

The Surface Detector of the Pierre Auger Observatory will consist of 1600 water Cherenkov tanks sampling ground particles of air showers produced by energetic cosmic rays. The arrival times are obtained from GPS and power is provided by solar panels. The construction of the array is nearly completed and a large number of detectors has been operational for more than three years. In this paper the performance of different components of the detectors are discussed. The accuracy of the signal measurement and the trigger stability are presented. The performance of the solar power system and other hardware, as well as the water purity and its long-term stability are discussed.

Suomijarvi, Tiina

2007-01-01T23:59:59.000Z

87

Performance of the Pierre Auger Observatory Surface Detector  

SciTech Connect

The Surface Detector of the Pierre Auger Observatory will consist of 1600 water Cherenkov tanks sampling ground particles of air showers produced by energetic cosmic rays. The arrival times are obtained from GPS and power is provided by solar panels. The construction of the array is nearly completed and a large number of detectors has been operational for more than three years. In this paper the performance of different components of the detectors are discussed. The accuracy of the signal measurement and the trigger stability are presented. The performance of the solar power system and other hardware, as well as the water purity and its long-term stability are discussed.

Collaboration, Tiina Suomijarvi for the Pierre Auger

2007-09-01T23:59:59.000Z

88

Calibrating laser test-beams for cosmic-ray observatories  

E-Print Network (OSTI)

Pulsed UV lasers can provide useful "testbeams" for observatories that use optical detectors, especially fluorescence detectors, to measure high energy cosmic-rays. The light observed by the detector is proportional to the energy of the laser pulse. Since the absolute laser energy can be measured locally, a well-calibrated laser offers a practical way to test the photometric calibration of the cosmic-ray detector including atmospheric corrections. This poster will describe a robotic system for laser polarization and energy calibration. Laboratory measurements of laser energies and polarizations by energy probes from different manufactures will be presented

Wiencke, Lawrence; Compton, John; Monasor, Maria; Pilger, David; Rosado, Jaime

2011-01-01T23:59:59.000Z

89

Trigger and data rates expected for the CTA Observatory  

E-Print Network (OSTI)

The Cherenkov Telescope Array (CTA) is an initiative to build a next-generation observatory for very-high energy $\\gamma$-rays. Its expected large effective area ($\\mathcal{O}(10^{7} \\mathrm{m}^2)$) and energy threshold as low as 25 GeV imply a challenge for triggering and data acquisition systems. The analysis of the official CTA Monte Carlo production-1 simulations leads to array trigger rates of $\\mathcal{O}$(10 kHz) and data rates ranging from $\\mathcal{O}$(100 MB/s) to $\\mathcal{O}$(1000 MB/s), depending on the read-out scenario.

Manuel Paz Arribas; Ullrich Schwanke; Ralf Wischnewski; for the CTA Consortium

2012-11-13T23:59:59.000Z

90

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

91

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

92

LAGOVirtual: A Collaborative Environment for the Large Aperture GRB Observatory  

E-Print Network (OSTI)

We present the LAGOVirtual Project: an ongoing project to develop platform to collaborate in the Large Aperture GRB Observatory (LAGO). This continental-wide observatory is devised to detect high energy (around 100 GeV) component of Gamma Ray Bursts, by using the single particle technique in arrays of Water Cherenkov Detectors (WCD) at high mountain sites (Chacaltaya, Bolivia, 5300 m a.s.l., Pico Espejo, Venezuela, 4750 m a.s.l., Sierra Negra, Mexico, 4650 m a.s.l). This platform will allow LAGO collaboration to share data, and computer resources through its different sites. This environment has the possibility to generate synthetic data by simulating the showers through AIRES application and to store/preserve distributed data files collected by the WCD at the LAGO sites. The present article concerns the implementation of a prototype of LAGO-DR adapting DSpace, with a hierarchical structure (i.e. country, institution, followed by collections that contain the metadata and data files), for the captured/simulated data. This structure was generated by using the community, sub-community, collection, item model; available at the DSpace software. Each member institution-country of the project has the appropriate permissions on the system to publish information (descriptive metadata and associated data files). The platform can also associate multiple files to each item of data (data from the instruments, graphics, postprocessed-data, etc.).

R. Camacho; R. Chacon; G. Diaz; C. Guada; V. Hamar; H. Hoeger; A. Melfo; L. A. Nunez; Y. Perez; C. Quintero; M. Rosales; R. Torrens; the LAGO Collaboration

2009-12-12T23:59:59.000Z

93

LAGOVirtual: A Collaborative Environment for the Large Aperture GRB Observatory  

E-Print Network (OSTI)

We present the LAGOVirtual Project: an ongoing project to develop platform to collaborate in the Large Aperture GRB Observatory (LAGO). This continental-wide observatory is devised to detect high energy (around 100 GeV) component of Gamma Ray Bursts, by using the single particle technique in arrays of Water Cherenkov Detectors (WCD) at high mountain sites (Chacaltaya, Bolivia, 5300 m a.s.l., Pico Espejo, Venezuela, 4750 m a.s.l., Sierra Negra, Mexico, 4650 m a.s.l). This platform will allow LAGO collaboration to share data, and computer resources through its different sites. This environment has the possibility to generate synthetic data by simulating the showers through AIRES application and to store/preserve distributed data files collected by the WCD at the LAGO sites. The present article concerns the implementation of a prototype of LAGO-DR adapting DSpace, with a hierarchical structure (i.e. country, institution, followed by collections that contain the metadata and data files), for the captured/simulate...

Camacho, R; Diaz, G; Guada, C; Hamar, V; Hoeger, H; Melfo, A; Nunez, L A; Perez, Y; Quintero, C; Rosales, M; Torrens, R

2009-01-01T23:59:59.000Z

94

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

95

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

96

Airborne Laser Altimetry Digital Elevation Model, Barrow Environmental Observatory, 0.5m spatial resolution  

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.

Cathy Wilson; Chandana Gangodagamage; Joel Rowland

2013-12-08T23:59:59.000Z

97

Airborne Laser Altimetry Digital Elevation Model, Barrow Environmental Observatory, 0.5m spatial resolution  

DOE Data Explorer (OSTI)

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.

Cathy Wilson; Chandana Gangodagamage; Joel Rowland

98

XFEL Materials Imaging at the LCLS CXI Endstation  

Science Conference Proceedings (OSTI)

About this Abstract. Meeting, 2013 TMS Annual Meeting & Exhibition. Symposium , Characterization of Materials through High Resolution Coherent Imaging.

99

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

100

Charge Management for Gravitational Wave Observatories using UV LEDs  

E-Print Network (OSTI)

Accumulation of electrical charge on the end mirrors of gravitational wave observatories, such as the space-based LISA mission and ground-based LIGO detectors, can become a source of noise limiting the sensitivity of such detectors through electronic couplings to nearby surfaces. Torsion balances provide an ideal means for testing gravitational wave technologies due to their high sensitivity to small forces. Our torsion pendulum apparatus consists of a movable Au-coated Cu plate brought near a Au-coated Si plate pendulum suspended from a non-conducting quartz fiber. A UV LED located near the pendulum photoejects electrons from the surface, and a UV LED driven electron gun directs photoelectrons towards the pendulum surface. We have demonstrated both charging and discharging of the pendulum with equivalent charging rates of $\\sim

Pollack, S E; Schlamminger, S; Hagedorn, C A; Gundlach, J H

2009-01-01T23:59:59.000Z

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.


101

Precision Solar Neutrino Measurements with the Sudbury Neutrino Observatory  

Science Conference Proceedings (OSTI)

The Sudbury Neutrino Observatory (SNO) is the first experiment to measure the total flux of active, high-energy neutrinos from the sun. Results from SNO have solved the long-standing 'Solar Neutrino Problem' by demonstrating that neutrinos change flavor. SNO measured the total neutrino flux with the neutral-current interaction of solar neutrinos with 1000 tonnes of D{sub 2}O. In the first two phases of the experiment we detected the neutron from that interaction by capture on deuterium and capture on chlorine, respectively. In the third phase an array of {sup 3}He proportional counters was deployed in the detector. This allows a measurement of the neutral-current neutrons that is independent of the Cherenkov light detected by the PMT array. We are currently developing a unique, detailed simulation of the current pulses from the proportional-counter array that will be used to help distinguish signal and background pulses.

Oblath, Noah [Center for Experimental Nuclear Physics and Astrophysics University of Washington, Seattle, WA (United States)

2007-10-26T23:59:59.000Z

102

The SECIS instrument on the Lomnicky Peak Observatory  

E-Print Network (OSTI)

Heating mechanisms of the solar corona will be investigated at the high-altitude solar observatory Lomnicky Peak of the Astronomical Institute of SAS (Slovakia) using its mid-size Lyot coronagraph and post-focal instrument SECIS provided by Astronomical Institute of the University of Wroclaw (Poland). The data will be studied with respect to the energy transport and release responsible for heating the solar corona to temperatures of mega-Kelvins. In particular investigations will be focused on detection of possible high-frequency MHD waves in the solar corona. The scientific background of the project, technical details of the SECIS system modified specially for the Lomnicky Peak coronagraph, and inspection of the test data are described in the paper.

Ambroz, J; Rudawy, P; Rybak, J; Phillips, K J H

2010-01-01T23:59:59.000Z

103

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...

Argiro, S; Gonzlez, J; Nellen, L; Paul, T; Porter, T A; Prado, L; Roth, M; Ulrich, R; Veberic, D

2007-01-01T23:59:59.000Z

104

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...

Argiro, S; Gonzlez, J; Nellen, L; Paul, T; Porter, T A; Roth, M; Ulrich, R; Veberic, D

2005-01-01T23:59:59.000Z

105

Probing Dark Energy via Neutrino and Supernova Observatories  

SciTech Connect

A novel method for extracting cosmological evolution parameters is proposed, using a probe other than light: future observations of the diffuse anti-neutrino flux emitted from core-collapse supernovae (SNe), combined with the SN rate extracted from future SN surveys. The relic SN neutrino differential flux can be extracted by using future neutrino detectors such as Gadolinium-enriched, megaton, water detectors or 100-kiloton detectors of liquid Argon or liquid scintillator. The core-collapse SN rate can be reconstructed from direct observation of SN explosions using future precision observatories. Our method, by itself, cannot compete with the accuracy of the optical-based measurements but may serve as an important consistency check as well as a source of complementary information. The proposal does not require construction of a dedicated experiment, but rather relies on future experiments proposed for other purposes.

Hall, Lawrence; Hall, Lawrence J.; Murayama, Hitoshi; Papucci, Michele; Perez, Gilad

2006-07-10T23:59:59.000Z

106

Searching for Double Beta Decay with the Enriched Xenon Observatory  

Science Conference Proceedings (OSTI)

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

Hall, C.; /SLAC

2007-03-16T23:59:59.000Z

107

Performance of the Keck Observatory adaptive optics system  

SciTech Connect

In this paper, the adaptive optics (AO) system at the W.M. Keck Observatory is characterized. The authors calculate the error budget of the Keck AO system operating in natural guide star mode with a near infrared imaging camera. By modeling the control loops and recording residual centroids, the measurement noise and band-width errors are obtained. The error budget is consistent with the images obtained. Results of sky performance tests are presented: the AO system is shown to deliver images with average Strehl ratios of up to 0.37 at 1.58 {micro}m using a bright guide star and 0.19 for a magnitude 12 star.

van Dam, M A; Mignant, D L; Macintosh, B A

2004-01-19T23:59:59.000Z

108

Fluorescence and Hybrid Detection Aperture of the Pierre Auger Observatory  

E-Print Network (OSTI)

The aperture of the Fluorescence Detector (FD) of the Pierre Auger Observatory is evaluated from simulated events using different detector configurations: mono, stereo, 3-FD and 4-FD. The trigger efficiency has been modeled using shower profiles with ground impacts in the field of view of a single telescope and studying the trigger response (at the different levels) by that telescope and by its neighbours. In addition, analysis cuts imposed by event reconstruction have been applied. The hybrid aperture is then derived for the Auger final extension. Taking into account the actual Surface Detector (SD) array configuration and its trigger response, the aperture is also calculated for a typical configuration of the present phase.

J. A. Bellido; D. D'Urso; H. Geenen; F. Guarino; L. Perrone; S. Petrera; L. Prado Jr.; F. Salamida

2005-07-05T23:59:59.000Z

109

Current technology development efforts on the international X-ray Observatory  

Science Conference Proceedings (OSTI)

The International X-ray Observatory (IXO) is a collaboration between NASA, ESA, and JAXA which is under study for launch in 2021. IXO will be a large 6600 kilogram Great Observatory-class mission which will build upon the legacies of the Chandra and ...

David Robinson

2011-03-01T23:59:59.000Z

110

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

E-Print Network (OSTI)

Observatory Phase I Data Set B. Aharmim, 7 Q.R. Ahmad, 22of results from the Phase I data set of the Sudbury NeutrinoObservatory (SNO). The Phase I data set is based on a 0.65

2007-01-01T23:59:59.000Z

111

Preliminary systems engineering evaluations for the National Ecological Observatory Network.  

Science Conference Proceedings (OSTI)

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

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

2008-11-01T23:59:59.000Z

112

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

113

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

114

The offline software framework of the Pierre Auger Observatory  

SciTech Connect

The Pierre Auger Observatory is designed to unveil the nature and origin of the highest energy cosmic rays through the analysis of extensive air showers. 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. They have designed and implemented a general purpose framework which allows Auger collaborators to contribute algorithms and configuration 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 residing in many data sources. A number of utilities are also provided, including a novel geometry package allowing 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 the contributed user codes.

Argiro, S.; Barroso, S.L.C.; Dagoret-Campagne, S.; Gonzalez, Javier G.; Nellen, L.; Paul, T.; Porter, T.; Prado, L., Jr.; Roth, M.; Ulrich, R.; Veberic, D.

2005-08-01T23:59:59.000Z

115

Performance of the Pierre Auger Observatory Surface Array  

E-Print Network (OSTI)

The surface detector of the Pierre Auger Observatory is a 1600 water Cherenkov tank array on a triangular 1.5 km grid. The signals from each tank are read out using three 9'' photomultipliers and processed at a sampling frequency of 40 MHz, from which a local digital trigger efficiently selects shower candidates. GPS signals are used for time synchronization and a wireless communication system connects all tanks to the central data acquisition system. Power is provided by a stand-alone solar panel system. With large ambient temperature variations, that can reach over 20 degrees in 24 hours, high salinity, dusty air, high humidity inside the tank, and remoteness of access, the performance and reliability of the array is a challenge. Several key parameters are constantly monitored to ensure consistent operation. The Surface Array has currently over 750 detectors and has been in reliable operation since January 2004. Good uniformity in the response of different detectors and good long term stability is observed.

The Pierre Auger Collaboration

2005-08-22T23:59:59.000Z

116

Performance of the Pierre Auger Observatory Surface Array  

E-Print Network (OSTI)

The surface detector of the Pierre Auger Observatory is a 1600 water Cherenkov tank array on a triangular 1.5 km grid. The signals from each tank are read out using three 9'' photomultipliers and processed at a sampling frequency of 40 MHz, from which a local digital trigger efficiently selects shower candidates. GPS signals are used for time synchronization and a wireless communication system connects all tanks to the central data acquisition system. Power is provided by a stand-alone solar panel system. With large ambient temperature variations, that can reach over 20 degrees in 24 hours, high salinity, dusty air, high humidity inside the tank, and remoteness of access, the performance and reliability of the array is a challenge. Several key parameters are constantly monitored to ensure consistent operation. The Surface Array has currently over 750 detectors and has been in reliable operation since January 2004. Good uniformity in the response of different detectors and good long term stability is observed.

Bertou, X

2005-01-01T23:59:59.000Z

117

Performance of the Pierre Auger Observatory surface array  

SciTech Connect

The surface detector of the Pierre Auger Observatory is a 1600 water Cherenkov tank array on a triangular 1.5 km grid. The signals from each tank are read out using three 9'' photomultipliers and processed at a sampling frequency of 40MHz, from which a local digital trigger efficiently selects shower candidates. GPS signals are used for time synchronization and a wireless communication system connects all tanks to the central data acquisition system. Power is provided by a stand-alone solar panel system. With large ambient temperature variations, that can reach over 20 degrees in 24 hours, high salinity, dusty air, high humidity inside the tank, and remoteness of access, the performance and reliability of the array is a challenge. Several key parameters are constantly monitored to ensure consistent operation. The Surface Array has currently over 750 detectors and has been in reliable operation since January 2004. Good uniformity in the response of different detectors and good long term stability is observed.

Bertou, Xavier

2005-07-01T23:59:59.000Z

118

Charge Management for Gravitational Wave Observatories using UV LEDs  

E-Print Network (OSTI)

Accumulation of electrical charge on the end mirrors of gravitational wave observatories, such as the space-based LISA mission and ground-based LIGO detectors, can become a source of noise limiting the sensitivity of such detectors through electronic couplings to nearby surfaces. Torsion balances provide an ideal means for testing gravitational wave technologies due to their high sensitivity to small forces. Our torsion pendulum apparatus consists of a movable Au-coated Cu plate brought near a Au-coated Si plate pendulum suspended from a non-conducting quartz fiber. A UV LED located near the pendulum photoejects electrons from the surface, and a UV LED driven electron gun directs photoelectrons towards the pendulum surface. We have demonstrated both charging and discharging of the pendulum with equivalent charging rates of $\\sim$$10^5 e/\\mathrm{s}$, as well as spectral measurements of the pendulum charge resulting in a white noise level equivalent to $3\\times10^5 e/\\sqrt{Hz}$.

S. E. Pollack; M. D. Turner; S. Schlamminger; C. A. Hagedorn; J. H. Gundlach

2009-12-09T23:59:59.000Z

119

SNO Data: Results from Experiments at the Sudbury Neutrino Observatory  

DOE Data Explorer (OSTI)

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

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

120

A Decade of GroundAir Temperature Tracking at Emigrant Pass Observatory, Utah  

Science Conference Proceedings (OSTI)

Observations of air and ground temperatures collected between 1993 and 2004 from Emigrant Pass Geothermal Climate Observatory in northwestern Utah are analyzed to understand the relationship between these two quantities. The influence of surface ...

Marshall G. Bartlett; David S. Chapman; Robert N. Harris

2006-08-01T23:59:59.000Z

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.


121

The Time-Dependent Hydraulic Flow and Dissipation over the Still of Observatory Inlet  

Science Conference Proceedings (OSTI)

The time-dependent hydraulic flow over the sill of a tidally energetic fjord, Observatory Inlet, British Columbia, is studied. Acoustic observations of streamlines and velocity were made near the sill crest during the summer of 1982, a time when ...

Michael W. Stacey; Len J. Zedel

1986-06-01T23:59:59.000Z

122

Great science observatories in the space station era and OWL efforts in Japan  

Science Conference Proceedings (OSTI)

A concept of Space Factory on the International Space Station Alpha (ISSA) is described. By following the four great observatories that purposefully took advantage of the Space Transportation System (STS)

Yoshiyuki Takahashi

1998-01-01T23:59:59.000Z

123

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

E-Print Network (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 ...

Formaggio, Joseph A.

124

Clouds at Arctic Atmospheric Observatories. Part I: Occurrence and Macrophysical Properties  

Science Conference Proceedings (OSTI)

Cloud observations over the past decade from six Arctic atmospheric observatories are investigated to derive estimates of cloud occurrence fraction, vertical distribution, persistence in time, diurnal cycle, and boundary statistics. Each ...

Matthew D. Shupe; Von P. Walden; Edwin Eloranta; Taneil Uttal; James R. Campbell; Sandra M. Starkweather; Masataka Shiobara

2011-03-01T23:59:59.000Z

125

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

E-Print Network (OSTI)

Geomagnetic observatory GAN Jakub Vel´imsk´y K. Chandra Shakar Rao Lars W. Pedersen Ahmed Muslim´imsk´y et al. (ETH,UK,DTU,NGRI,GMO) Geomagnetic observatory GAN 27.4.2011/KG MFF UK 1 / 16 #12;Participating, Univ. Stuttgart) John Riddick (BGS, retired) Vel´imsk´y et al. (ETH,UK,DTU,NGRI,GMO) Geomagnetic

Cerveny, Vlastislav

126

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

E-Print Network (OSTI)

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

M. D. Healy; for the Pierre Auger Collaboration

2007-09-28T23:59:59.000Z

127

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

128

CALIPSO Lidar Description and Performance Assessment  

Science Conference Proceedings (OSTI)

This paper provides background material for a collection of CloudAerosol Lidar with Orthogonal Polarization (CALIOP) algorithm papers that are to be published in the Journal of Atmospheric and Oceanic Technology. It provides a brief description ...

William H. Hunt; David M. Winker; Mark A. Vaughan; Kathleen A. Powell; Patricia L. Lucker; Carl Weimer

2009-07-01T23:59:59.000Z

129

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....

130

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

131

Bridging the Virtual Observatory and the GRID with the query element  

E-Print Network (OSTI)

The current generation of Grid infrastructures designed for production activity is strongly computing oriented and tuned on the needs of applications that requires intensive computations. Problems arise when trying to use such Grids to satisfy the sharing of data-oriented and service-oriented resources as happens in the IVOA community. We have designed, developed and implemented a Grid query element to access data source from an existing production Grid environment. We also enhanced the Grid middleware model (collective resources and sites) to manage Data Sources extending the Grid semantic. The query element and the modified grid Information System are able to connect the Grid environment to Virtual Observatory resources. A specialized query element is designed to work as Virtual Observatory resource in the Grid so than an Astronomer can access Virtual Observatory data using the IVOA standards.

G. Taffoni; E. Ambrodsi; C. Vuerli; A. Barisani; R. Smareglia; A. Volpato; S. Pastore; A. Baruffolo; A. Ghiselli; F. Pasian; L. Benacchio

2006-05-05T23:59:59.000Z

132

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

Science Conference Proceedings (OSTI)

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

Signatures of storm sudden commencements in geomagnetic H, Y and Z elds at Indian observatories during 19581992  

E-Print Network (OSTI)

Signatures of storm sudden commencements in geomagnetic H, Y and Z ®elds at Indian observatories) impulses in hori- zontal (H), eastward (Y) and vertical (Z) ®elds at four Indian geomagnetic observatories 10±20°W of the geomagnetic meridian. The local time variation of the angle is more westerly during

Paris-Sud XI, Université de

134

An intense SFE and SSC event in geomagnetic H, Y and Z elds at the Indian chain of observatories  

E-Print Network (OSTI)

An intense SFE and SSC event in geomagnetic H, Y and Z ®elds at the Indian chain of observatories R, Gujarat University, Ahmedabad 380 009, India 2 Indian Institute of Geomagnetism, Mumbai 400 005, India 3 are reported at the chain of ten geomagnetic observatories in India during an intense solar crochet

Paris-Sud XI, Université de

135

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

E-Print Network (OSTI)

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

California at Santa Cruz, University of

136

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

E-Print Network (OSTI)

, active galactic nuclei (AGN), and gamma ray bursts (GRB). In addition, more exotic sources like Gamma Ray Observatory, located at an altitude of 8,600 feet in the Jemez Mountains of New Mexico for sources of TeV gamma rays. It is uniquely capable of search- ing for transient sources of VHE gamma rays

California at Santa Cruz, University of

137

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

E-Print Network (OSTI)

al. 2008). In principle, geo-neutrinos generated by the decay of Uranium, Thorium and Potassium). This observatory is installed at a depth of 2000 m in the Creighton mine, operated by Vale INCO at the edge of the Sudbury impact structure. The structure is known for its numerous mineral deposits and has been mined

Long, Bernard

138

The search for extended air showers at the Jicamarca Radio Observatory  

SciTech Connect

This paper presents the status of the project to detect extended air showers at the Jicamarca Radio Observatory. We report on detected anomalous signals and present a toy model to estimate at what altitudes we might expect to see air shower signals. According to this model, a significant number of high altitude horizontal air showers could be observed by radar techniques.

Wahl, D. [Radio Observatorio de Jicamarca, Instituto Geofisico del Peru (Peru); Instituto de Fisica, Universidad Nacional de Ingenieria, Lima (Peru); Chau, J.; Galindo, F.; Huaman, A. [Radio Observatorio de Jicamarca, Instituto Geofisico del Peru (Peru); Solano, C. J. [Instituto de Fisica, Universidad Nacional de Ingenieria, Lima (Peru); Instituto Nacional de Investigacion y Capacitacion de Telecomunicaciones, UNI, Lima (Peru)

2009-04-30T23:59:59.000Z

139

Introduction SOHO, the Solar and Heliospheric Observatory, is a project of international cooperation between  

E-Print Network (OSTI)

SOHO Introduction 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 of the solar interior? · Why does the solar corona exist and how is it heated to the extremely high temperature

Christian, Eric

140

Albedo Influences on Surface UV Irradiance at the Sonnblick High-Mountain Observatory (3106-m Altitude)  

Science Conference Proceedings (OSTI)

In this work the influences of ozone, aerosols, and albedo on the clear sky UVA and UVB irradiance at a high-mountain station are investigated by using both routine spectral UV measurements from the high-mountain Sonnblick observatory in Austria (...

Philipp Weihs; Stana Simic; Wolfgang Laube; Wieslaw Mikielewicz; Govindaraj Rengarajan; Michael Mandl

1999-11-01T23:59:59.000Z

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.


141

The Science Vision for the Stratospheric Observatory for Infrared Astronomy (SOFIA)  

E-Print Network (OSTI)

An updated Science Vision for the SOFIA project is presented, including an overview of the characteristics and capabilities of the observatory and first generation instruments. A primary focus is placed on four science themes: 'The Formation of Stars and Planets', 'The Interstellar Medium of the Milky Way', 'Galaxies and the Galactic Center' and 'Planetary Science'.

Roellig, T L; Evans, N J; De Buizer, J M; Meixner, M; Tielens, A G G M; Stacey, G J; Vacca, W D; Cuzzi, J N; Backman, D E

2009-01-01T23:59:59.000Z

142

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

E-Print Network (OSTI)

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

Washington at Seattle, University of

143

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

144

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

E-Print Network (OSTI)

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

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

2010-01-01T23:59:59.000Z

145

Imaging simulations of selected science with the Magdalena Ridge Observatory Interferometer  

E-Print Network (OSTI)

Cavendish Laboratory, J.J.Thomson Avenue, Cambridge, UK, CB3 0HE; cHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts, USA 02138 dMax Planck Institute for Astrophysics, Karl-Schwarzschild-Strass-1, Garching, Germany, 85741; e... resolution demonstrated here is likely to be a transformational step in contemporary astrophysics. REFERENCES [1] Creech-Eakman, M. et al., Magdalena Ridge Observatory Interferometer: advancing to first light and new science, Proceedings SPIE, 7734, 5...

Creech-Eakman, Michelle; Young, John; Haniff, Christopher; Buscher, David; Elvis, Martin; Chiavassa, Andrea; Schartmann, Marc

146

A Search for Astrophysical Burst Signals at the Sudbury Neutrino Observatory  

E-Print Network (OSTI)

The Sudbury Neutrino Observatory (SNO) has confirmed the standard solar model and neutrino oscillations through the observation of neutrinos from the solar core. In this paper we present a search for neutrinos associated with sources other than the solar core, such as gamma-ray bursters and solar flares. We present a new method for looking for temporal coincidences between neutrino events and astrophysical bursts of widely varying intensity. No correlations were found between neutrinos detected in SNO and such astrophysical sources.

B. Aharmim; S. N. Ahmed; A. E. Anthony; N. Barros; E. W. Beier; A. Bellerive; B. Beltran; M. Bergevin; S. D. Biller; K. Boudjemline; M. G. Boulay; B. Cai; Y. D. Chan; D. Chauhan; M. Chen; B. T. Cleveland; G. A. Cox; X. Dai; H. Deng; J. A. Detwiler; M. DiMarco; M. D. Diamond; P. J. Doe; G. Doucas; P. -L. Drouin; F. A. Duncan; M. Dunford; E. D. Earle; S. R. Elliott; H. C. Evans; G. T. Ewan; J. Farine; H. Fergani; F. Fleurot; R. J. Ford; J. A. Formaggio; N. Gagnon; J. TM. Goon; K. Graham; E. Guillian; S. Habib; R. L. Hahn; A. L. Hallin; E. D. Hallman; P. J. Harvey; R. Hazama; W. J. Heintzelman; J. Heise; R. L. Helmer; A. Hime; C. Howard; M. Huang; P. Jagam; B. Jamieson; N. A. Jelley; M. Jerkins; K. J. Keeter; J. R. Klein; L. L. Kormos; M. Kos; C. Kraus; C. B. Krauss; A. Krueger; T. Kutter; C. C. M. Kyba; R. Lange; J. Law; I. T. Lawson; K. T. Lesko; J. R. Leslie; I. Levine; J. C. Loach; R. MacLellan; S. Majerus; H. B. Mak; J. Maneira; R. Martin; N. McCauley; A. B. McDonald; S. R. McGee; M. L. Miller; B. Monreal; J. Monroe; B. G. Nickel; A. J. Noble; H. M. O'Keeffe; N. S. Oblath; R. W. Ollerhead; G. D. Orebi Gann; S. M. Oser; R. A. Ott; S. J. M. Peeters; A. W. P. Poon; G. Prior; S. D. Reitzner; K. Rielage; B. C. Robertson; R. G. H. Robertson; M. H. Schwendener; J. A. Secrest; S. R. Seibert; O. Simard; J. J. Simpson; D. Sinclair; P. Skensved; T. J. Sonley; L. C. Stonehill; G. Tesic; N. Tolich; T. Tsui; R. Van Berg; B. A. VanDevender; C. J. Virtue; B. L. Wall; D. Waller; H. Wan Chan Tseung; D. L. Wark; P. J. S. Watson; J. Wendland; N. West; J. F. Wilkerson; J. R. Wilson; J. M. Wouters; A. Wright; M. Yeh; F. Zhang; K. Zuber

2013-09-04T23:59:59.000Z

147

Radial Velocity Jitter in Stars from the California and Carnegie Planet Search at Keck Observatory  

E-Print Network (OSTI)

I present an empirical model for predicting a star's radial velocity jitter from its B-V color, activity level, and absolute magnitude. This model is based on observations of 450 well- observed stars from Keck Observatory for the California and Carnegie Planet Search Program. The model includes noise from both astrophysical sources and systematic errors, and describes jitter as generally increasing with a star's activity and height above the main sequence.

J. T. Wright

2005-05-11T23:59:59.000Z

148

Measurement of Expected Nucleation Precursor Species and 3500-nm Diameter Particles at Mauna Loa Observatory, Hawaii  

Science Conference Proceedings (OSTI)

Atmospheric measurements of expected homogeneous nucleation precursors and aerosols were made at the Mauna Loa Observatory, Hawaii, from 28 June to 27 July 1992. Large molecular clusters and gas phase species including sulfuric acid (H2SO4), ...

R. J. Weber; P. H. McMurry; F. L. Eisele; D. J. Tanner

1995-06-01T23:59:59.000Z

149

A Climatology of Gravity Waves and Other Coherent Disturbances at the Boulder Atmospheric Observatory during MarchApril 1984  

Science Conference Proceedings (OSTI)

We present a climatological study of gravity waves and other coherent disturbances at the Boulder Atmospheric Observatory, during the period mid-March-mid-April 1984. The data were collected by a network of microbarographs, and by sensors on the ...

F. Einaudi; A. J. Bedard Jr.; J. J. Finnigan

1989-02-01T23:59:59.000Z

150

The Measurement of Tropospheric Trace Gases at Fritz Peak Observatory, Colorado, by Long-Path Absorption: OH and Ancillary Gases  

Science Conference Proceedings (OSTI)

The determination of the concentration of the hydroxyl radical in the troposphere is of fundamental importance to an understanding of the chemistry of the lower atmosphere. Described here are experiments located at Fritz Peak Observatory, ...

George H. Mount; Jerald W. Harder

1995-10-01T23:59:59.000Z

151

The Meteorological Model BOLAM at the National Observatory of Athens: Assessment of Two-Year Operational Use  

Science Conference Proceedings (OSTI)

Since November 1999, the hydrostatic meteorological Bologna Limited-Area Model (BOLAM) has been running operationally at the National Observatory of Athens. The assessment of the model forecast skill during the 2-yr period included (a) ...

K. Lagouvardos; V. Kotroni; A. Koussis; H. Feidas; A. Buzzi; P. Malguzzi

2003-11-01T23:59:59.000Z

152

A multivariate study of mass composition for simulated showers at the Auger South Observatory  

E-Print Network (OSTI)

The output parameters from the ground array of the Auger South observatory, were simulated for the typical instrumental and environmental conditions at its Malarg\\"ue site using the code sample-sim. Extensive air showers started by photons, protons and iron nuclei at the top of the atmosphere were used as triggers. The study utilized the air shower simulation code Aires with both QGSJet and Sibyll hadronic interaction models. A total of 1850 showers were used to produce more than 35,000 different ground events. We report here on the results of a multivariate analysis approach, including principal component analysis and neural networks, to the development of new primary composition diagnostics.

Gustavo A. Medina Tanco; Sergio J. Sciutto

2001-09-10T23:59:59.000Z

153

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

154

Recent results from the Milagro TeV gamma-ray observatory  

E-Print Network (OSTI)

Milagro is a gamma-ray observatory employing a water Cherenkov detector to observe extensive air showers produced by high-energy particles impacting in the Earth's atmosphere. We discuss the first detection of TeV gamma-rays from the Galactic plane and report the detection of an extended TeV source coincident with the EGRET source 3EG J0520+2556, and the observation of TeV emission from the Cygnus region of our Galaxy. We also summarize the status of our search for Very High Energy (VHE) emission from satellite-triggered Gamma Ray Bursts (GRBs) and discuss plans for the next generation water Cherenkov detector.

Parkinson, P M S

2005-01-01T23:59:59.000Z

155

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

156

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

157

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

158

Prospecting for Heavy Elements with Future Far-IR/Submillimeter Observatories  

E-Print Network (OSTI)

To understand the cosmic history of element synthesis it will be important to obtain extinction-free measures of the heavy element contents of high-redshift objects and to chart two monumental events: the collapse of the first metal-free clouds to form stars, and the initial seeding of the universe with dust. The information needed to achieve these objectives is uniquely available in the far-infrared/submillimeter (FIR/SMM) spectral region. Following the Decadal Report and anticipating the development of the Single Aperture Far-IR (SAFIR) telescope and FIR/SMM interferometry, we estimate the measurement capabilities of a large-aperture, background-limited FIR/SMM observatory and an interferometer on a boom, and discuss how such instruments could be used to measure the element synthesis history of the universe.

Leisawitz, D T; Kashlinsky, A; Lawrence, C R; Mather, J C; Moseley, S H; Rinehart, S A; Silverberg, R F; Yorke, H W

2002-01-01T23:59:59.000Z

159

Atmospheric Profiles at the Southern Pierre Auger Observatory and their Relevance to Air Shower Measurement  

E-Print Network (OSTI)

The dependence of atmospheric conditions on altitude and time have to be known at the site of an air shower experiment for accurate reconstruction of extensive air showers and their simulations. The height-profile of atmospheric depth is of particular interest as it enters directly into the reconstruction of longitudinal shower development and of the primary energy and mass of cosmic rays. For the southern part of the Auger Observatory, the atmosphere has been investigated in a number of campaigns with meteorological radio soundings and with continuous measurements of ground-based weather stations. Focussing on atmospheric depth and temperature profiles, temporal variations are described and monthly profiles are developed. Uncertainties of the monthly atmospheres that are currently applied in the Auger reconstruction are discussed.

B. Keilhauer; J. Bluemer; R. Engel; D. Gora; P. Homola; H. Klages; J. Pekala; M. Risse; M. Unger; B. Wilczynska; H. Wilczynski; for the Pierre Auger Collaboration

2005-07-12T23:59:59.000Z

160

First results from the MACRO (Monopole, Astophysics, Cosmic Ray Observatory) detector at the Gran Sasso Laboratory  

Science Conference Proceedings (OSTI)

The MACRO (Monopole, Astrophysics, Cosmic Ray Observatory) detector which is being installed at the underground Gran Sasso Laboratory (LNGS) is described in detail. The performance of the detector's first supermodule ({approximately}800 m{sup 2}sr), which had its initial data run from February 27 to May 30, 1989, is reported. About 245,000 muon triggers were recorded during this first run. Preliminary results are presented on: the measured vertical muon flux; the detection features of MACRO as a high energy muon and muon neutrino telescope; the measured lateral spread and multiplicity distributions of muon bundles; a search for GUT magnetic monopoles; a search for electron anti-neutrinos from stellar collapses. In addition, there are results obtained in conjunction with the EAS-TOP detector located on top of the Gran Sasso mountain. 24 refs., 22 figs.

Calicchio, M.; De Cataldo, G.; De Marzo, C.; Erriquez, O.; Favuzzi, C.; Giglietto, N.; Nappi, E.; Spinelli, P.; Cecchini, S.; D'Antone, I.; Giacomelli, G.; Mandrioli, G.; Margiotta-Neri, A.; Matteuzzi, P.; Pal, B.; Patrizii, L.; Predieri, F.; Sanzani, G.L.; Serra, P.; Spurio, M.; Ahlen, S.P.; Ficenec, D.; Hazen, E.; Klein, S.; Levin, D.; Marin, A.; Stone, J.L.; Sulak, L.R.; Worstell, W.; Barish, B.; Coutu, S.; Hong, J.T.; Liu, G

1989-01-01T23:59:59.000Z

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161

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

E-Print Network (OSTI)

The Advanced CCD Imaging Spectrometer is an instrument on the Chandra X-ray Observatory. CCDs are vulnerable to radiation damage, particularly by soft protons in the radiation belts and solar storms. The Chandra team has implemented procedures to protect ACIS during high-radiation events including autonomous protection triggered by an on-board radiation monitor. Elevated temperatures have reduced the effectiveness of the on-board monitor. The ACIS team has developed an algorithm which uses data from the CCDs themselves to detect periods of high radiation and a flight software patch to apply this algorithm is currently active on-board the instrument. In this paper, we explore the ACIS response to particle radiation through comparisons to a number of external measures of the radiation environment. We hope to better understand the efficiency of the algorithm as a function of the flux and spectrum of the particles and the time-profile of the radiation event.

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

2012-01-01T23:59:59.000Z

162

LISA-2020: An Intermediate Scale Space Gravitational Wave Observatory for This Decade  

E-Print Network (OSTI)

Over the last three decades, an exceptionally good science case has been made for pursuing gravitational wave (GW) astronomy. This has engendered a worldwide effort to detect the extremely weak signals generated by expected sources. With the next round of upgrades the ground based instruments are likely to make the first detections of the sources, and a new era of astronomy will begin, possibly as early as 2017. Inconveniently, due to seismic noise and baseline length issues, the low frequency (2030 now seems very unlikely. This paper examines the case for a scaled down mission that is comparable in cost and duration to medium scale astrophysics missions such as the 1978 ($630M) Einstein (HEAO 2) x-ray Observatory...

Buchman, S; Byer, R L; DeBra, D; Balakrishnan, K; Cutler, G Dufresne; Al-Fauwaz, A; Hultgren, E; Al-Jadaan, A K; Saraf, S; Tan, S; Al-Thubiti, S; Zoellner, A

2013-01-01T23:59:59.000Z

163

Searches for high frequency variations in the 8-B neutrino flux at the Sudbury neutrino observatory  

SciTech Connect

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

Rielage, Keith [Los Alamos National Laboratory; Seibert, Stanley R [Los Alamos National Laboratory; Hime, Andrew [Los Alamos National Laboratory; Elliott, Steven R [Los Alamos National Laboratory; Stonehill, L C [Los Alamos National Laboratory; Wouters, J M [Los Alamos National Laboratory; Aharmim, B [LAURENTIAN UNIV; Ahmed, S N [QUEEN'S UNIV; Anthony, A E [UNIV OF TEXAS; Barros, N [PORTUGAL; Beier, E W [UNIV OF PA; Bellerive, A [CARLETON UNIV; Belttran, B [UNIV OF ALBERTA; Bergevin, M [LBNL; Biller, S D [UNIV OF OXFORD; Boudjemline, K [CARLETON UNIV; Burritt, T H [UNIV OF WASHINGTON; Cai, B [QUEEN'S UNIV; Chan, Y D [LBNL; Chauhan, D [LAURENTIAN UNIV; Chen, M [QUEEN'S UNIV; Cleveland, B T [UNIV OF OXFORD; Cox - Mobrand, G A [UNIV OF WASHINGTON; Dai, X [QUEEN'S UNIV; Deng, H [UNIV OF PA; Detwiler, J [LBNL; Dimarco, M [QUEEN'S UNIV; Doe, P J [UNIV OF WASHINGTON; Drouin, P - L [CARLTON UNIV; Duba, C A [UNIV OF WASHINGTON; Duncan, F A [SNOLAB, SUDBURY; Dunford, M [UNIV OF PA; Earle, E D [QUEEN'S UNIV; Evans, H C [QUEEN'S UNIV; Ewan, G T [QUEEN'S UNIV; Farine, J [LAURENTTIAN UNIV; Fergani, H [UNIV OF OXFORD; Fleurot, F [LAURENTIAN UNIV; Ford, R J [SNOLAB, SUDBURY; Formaggilo, J A [MASSACHUSETTS INST. OF TECH.; Gagnon, N [UNIV OF WASHINGTON; Goon, J Tm [LOUISIANA STATE UNIV; Guillian, E [QUEEN'S UNIV; Habib, S [UNIV OF ALBERTA; Hahn, R L [BNL; Hallin, A L [UNIV OF ALBERTA; Hallman, E D [LAURENTIAN UNIV; Harvey, P J [QUEEN'S UNIV; Hazama, R [UNIV OF WASHINGTON; Heintzelman, W J [UNIV OF PA; Heise, J [SNOLAB, SUDBURY; Helmer, R L [TRIUMF; Howard, C [UNIV OF ALBERTA; Howe, M A [UNIV OF WASHINGTON; Huang, M [UNIV OF TEXAS; Jamieson, B [UNIV OF BRITISH COLUMBIA; Jelley, N A [UNIV OF OXFORD; Keeter, K J [SNOLAB, SUDBURY; Klein, J R [UNIV OF TEXAS; Kos, M [QUEEN'S UNIV; Kraus, C [QUEEN'S UNIV; Krauss, C B [UNIV OF ALBERTA; Kutter, T [LOUISIANA STATE UNIV; Kyba, C C M [UNIV OF PA; Law, J [UNIV OF GUELPH; Lawson, I T [SNOLAB, SUDBURY; Lesko, K T [LBNL; Leslie, J R [QUEEN'S UNIV; Loach, J C [UNIV OF OXFORD; Maclellan, R [QUEEN'S UNIV; Majerus, S [UNIV OF OXFORD; Mak, H B [QUEEN'S UNIV; Maneira, J [PORTUGAL; Martin, R [QUEEN'S UNIV; Mccauley, N [UNIV OF PA; Mc Donald, A B [QUEEN'S UNIV; Mcgee, S [UNIV OF WASHINGTON; Miffin, C [CARLETON UNIV; Miller, M L [MASSACHUSETTS INST. OF TECH.; Monreal, B [MASSACHUSETTS INST. OF TECH.; Monroe, J [MASSACHUSETTS INST. OF TECH; Morissette, B [SNOLAB, SUDBURY; Nickel, B G [UNIV OF GUELPH; Noble, A J [QUEEN'S UNIV; O' Keeffe, H M [UNIV OF OXFORD; Oblath, N S [UNIV OF WASHINGTON; Orebi Gann, G D [UNIV OF OXFORD; Oser, S M [UNIV OF BRITISH COLUMBIA; Ott, R A [MASSACHUSETTS INST. OF TECH.; Peeters, S J M [UNIV OF OXFORD; Poon, A W P [LBNL; Prior, G [LBNL; Reitzner, S D [UNIV OF GUELPH; Robertson, B C [QUEEN'S UNIV; Robertson, R G H [UNIV OF WASHINGTON; Rollin, E [CARLETON UNIV; Schwendener, M H [LAURENTIAN UNIV; Secrest, J A [UNIV OF PA; Seibert, S R [UNIV OF TEXAS; Simard, O [CARLETON UNIV; Sinclair, D [CARLETON UNIV; Sinclair, L [CARLETON UNIV; Skensved, P [QUEEN'S UNIV; Sonley, T J [MASSACHUSETTS INST. OF TECH.; Tesic, G [CARLETON UNIV; Tolich, N [UNIV OF WASHINGTON; Tsui, T [UNIV OF BRITISH COLUMBIA; Tunnell, C D [UNIV OF TEXAS; Van Berg, R [UNIV OF PA; Van Devender, B A [UNIV OF WASHINGTON; Virtue, C J [LAURENTIAN UNIV; Wall, B L [UNIV OF WASHINGTON; Waller, D [CARLETON UNIV; Wan Chan Tseung, H [UNIV OF OXFORD; West, N [UNIV OF OXFORD; Wilkerson, J F [UNIV OF WASHINGTON; Wilson, J R [UNIV OF OXFORD; Wright, A [QUEEN'S UNIV; Yeh, M [BNL; Zhang, F [CARLETON UNIV; Zuber, K [UNIV OF OXFORD

2009-01-01T23:59:59.000Z

164

Back-to-Back Black Holes decay Signature at Neutrino Observatories  

E-Print Network (OSTI)

We propose a decay signature for non-thermal small black holes with masses in the TeV range which can be discovered by neutrino observatories. The black holes would result due to the impact between ultra high energy neutrinos with nuclei in water or ice and decay instantaneously. They could be produced if the Planck scale is in the few TeV region and the highly energetic fluxes are large enough. Having masses close to the Planck scale, the typical decay mode for these black holes is into two particles emitted back-to-back. For a certain range of angles between the emitted particles and the center of mass direction of motion, it is possible for the detectors to measure separate muons having specific energies and their trajectories oriented at a large enough angle to prove that they are the result of a back-to-back decay event.

Nicusor Arsene; Xavier Calmet; Lauretiu Ioan Caramete; Octavian Micu

2013-03-19T23:59:59.000Z

165

Development of the semi-arid climate and environment research observatory over Loess Plateau  

E-Print Network (OSTI)

Arid and semi-arid areas comprise about 30 % of earth surface. Changes in climate and climate variability will likely have a significant impact on these regions. Loess Plateau over Northwest China is a special semi-arid land surface and part of dust aerosol source. To improve understanding and observe the direct evident of the impact of human activity on semi-arid climate over Loess Plateau, the Semi-Arid Climate & Environment Observatory of Lanzhou University (SACOL) has been established since 2005. SACOL consists of a large set of instruments and focuses on: 1) monitoring of long term tendencies in semi-arid climate changes; 2) monitoring of the aerosol effect on water cycle; 3) studies of interaction between land surface and atmosphere; 4) improving the land surface and climate model; 5) validation of space-borne observations. This paper presents a description of SACOL objectives, measurements, and sampling strategies. Preliminary observation results are also reviewed in this paper. 2 1.

Jianping Huang; Wu Zhang; Jinqing Zuo; Congbin Fu; Jifan Chou; Jiuyi Yuan; Lei Zhang; Shigong Wang; Hongchao Zuo; Hua Fu; Zhoulin Chang; Jianrong Bi; Jinsen Shi

2007-01-01T23:59:59.000Z

166

Solving the Solar Neutrino Problem 2 km Underground -- the Sudbury Neutrino Observatory  

E-Print Network (OSTI)

The Sudbury Neutrino Observatory (SNO) is capable of measuring simultaneously the flux of electron-type neutrinos and the total flux of all active flavours of neutrinos originating from the Sun. A model-independent test of neutrino flavour transformation was performed by comparing these two measurements. Assuming an undistorted neutrino energy spectrum, this transformation has been definitively demonstrated in the pure D2O phase of the SNO experiment. In the second phase with dissolved NaCl in the D2O, the total active solar neutrino flux was measured without any assumption on the energy dependence of flavour transformation. In this talk, results from these measurements, their physics implications and the current status of the SNO experiment are presented.

A. W. P. Poon; for the SNO Collaboration

2003-11-30T23:59:59.000Z

167

Operating Water Cherenkov Detectors in high altitude sites for the Large Aperture GRB Observatory  

E-Print Network (OSTI)

Water Cherenkov Detectors (WCD) are efficient detectors for detecting GRBs in the 10 GeV - 1 TeV energy range using the single particle technique, given their sensitivity to low energy secondary photons produced by high energy photons when cascading in the atmosphere. The Large Aperture GRB Observatory (LAGO) operates arrays of WCD in high altitude sites (above 4500 m a.s.l.) in Bolivia, Mexico and Venezuela, with planned extension to Peru. Details on the operation and stability of these WCD in remote sites with high background rates of particles will be detailed, and compared to simulations. Specific issues due to operation at high altitude, atmospheric effects and solar activity, as well as possible hardware enhancements will also be presented.

Allard, D; Asorey, H; Barros, H; Bertou, X; Castillo, M; Chirinos, J M; De Castro, A; Flores, S; Gonzlez, J; Berisso, M Gomez; Grajales, J; Guada, C; Day, W R Guevara; Ishitsuka, J; Lpez, J A; Martnez, O; Melfo, A; Meza, E; Loza, P Miranda; Barbosa, E Moreno; Murrugarra, C; Nez, L A; Ormachea, L J Otiniano; Prez, G; Perez, Y; Ponce, E; Quispe, J; Quintero, C; Rivera, H; Rosales, M; Rovero, A C; Saavedra, O; Salazar, H; Tello, J C; Peralda, R Ticona; Varela, E; Velarde, A; Villaseor, L; Wahl, D; Zamalloa, M A

2009-01-01T23:59:59.000Z

168

Performance of the first prototype of the HAWC Gamma Ray Observatory  

E-Print Network (OSTI)

The HAWC gamma ray observatory, to be constructed at Sierra Negra, Puebla in Mexico, is a large array of water Cherenkov detectors sited at an elevation of 4100 m, which has been optimized for gamma/hadron discrimination of the primary cosmic rays in the TeV energy range. It is based on the Milagro experience, but the design has been changed from a water pond to individual water tanks. In order to validate the design with large water tanks a prototype array has been constructed near the HAWC site with 3 of the largest commercial rotomolded plastic tanks available in Mexico. They have been instrumented with 20 cm hemispherical photomultiplier tubes and read out with 2 Gsample/s flash ADCs. The performance of a single tank has been measured as well as the response of the array to cosmic ray showers. In this paper we present the first measurements of the performance of the HAWC prototype array.

Sandoval, Andres; Belmont, Ernesto; Grabski, Varlen; Renteria, Alejandro; Vasques, Alejandro R; Vazquez, Omar; Gonzalez, M Magdalena; Carramiana, Alberto; Alvarez, Cesar

2009-01-01T23:59:59.000Z

169

Near-Neutral Surface Layer Turbulence at the Boulder Atmospheric Observatory Tower: Evidence of Increasing Vertical Turbulence with Height  

Science Conference Proceedings (OSTI)

Wind and turbulence profiles were analyzed during breezy, near-neutral conditions at the Boulder Atmospheric Observatory tower to quantify the effects of an abrupt 20- to 30-m increase in terrain located 35 km west of the tower. Results indicate ...

Brent M. Bowen

2000-05-01T23:59:59.000Z

170

Selection of Image Parameters as the First Step towards Creating a CBIR System for the Solar Dynamics Observatory  

Science Conference Proceedings (OSTI)

This work describes the attribute evaluation sections of the ambitious goal of creating a large-scale content-based image retrieval (CBIR) system for solar phenomena in NASA images from the Solar Dynamics Observatory mission. This mission, with its Atmospheric ... Keywords: Attribute evaluation, content based image retrieval, correlation analysis, classification

Juan M. Banda; Rafal A. Angryk

2010-12-01T23:59:59.000Z

171

Methodology for Water Monitoring in the Upper Troposphere with Raman Lidar at the Haute-Provence Observatory  

Science Conference Proceedings (OSTI)

A Raman water vapor lidar has been developed at the Haute-Provence Observatory to study the distribution of water in the upper troposphere and its long-term evolution. Some investigations have been proposed and described to ensure a pertinent ...

Christophe Hoareau; Philippe Keckhut; Alain Sarkissian; Jean-Luc Baray; Georges Durry

2009-10-01T23:59:59.000Z

172

Measurement of the Cosmic Ray and Neutrino-Induced Muon Flux at the Sudbury Neutrino Observatory  

SciTech Connect

Results are reported on the measurement of the atmospheric neutrino-induced muon flux at a depth of 2 kilometers below the Earth's 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 un-oscillated portion of the neutrino flux. A total of 514 muon-like events are measured between -1 {le} cos {theta}{sub zenith} 0.4 in a total exposure of 2.30 x 10{sup 14} cm{sup 2} s. The measured flux normalization is 1.22 {+-} 0.09 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 {theta}{sub zenith} > 0.4 is measured to be (3.31 {+-} 0.01 (stat.) {+-} 0.09 (sys.)) x 10{sup -10} {micro}/s/cm{sup 2}.

SNO collaboration; Aharmim, B.; Ahmed, S.N.; Andersen, T.C.; Anthony, A.E.; Barros, N.; Beier, E.W.; Bellerive, A.; Beltran, B.; Bergevin, M.; Biller, S.D.; Boudjemline, K.; Boulay, M.G.; Burritt, T.H.; Cai, B.; Chan, Y.D.; Chen, M.; Chon, M.C.; Cleveland, B.T.; Cox-Mobrand, G.A.; Currat, C.A.; Dai, X.; Dalnoki-Veress, F.; Deng, H.; Detwiler, J.; Doe, P.J.; Dosanjh, R.S.; Doucas, G.; Drouin, P.-L.; Duncan, F.A.; Dunford, M.; Elliott, S.R.; Evans, H.C.; Ewan, G.T.; Farine, J.; Fergani, H.; Fleurot, F.; Ford, R.J.; Formaggio, J.A.; Gagnon, N.; Goon, J.TM.; Grant, D.R.; Guillian, E.; Habib, S.; Hahn, R.L.; Hallin, A.L.; Hallman, E.D.; Hargrove, C.K.; Harvey, P.J.; Harvey, P.J.; Heeger, K.M.; Heintzelman, W.J.; Heise, J.; Helmer, R.L.; Hemingway, R.J.; Henning, R.; Hime, A.; Howard, C.; Howe, M.A.; Huang, M.; Jamieson, B.; Jelley, N.A.; Klein, J.R.; Kos, M.; Kruger, A.; Kraus, C.; Krauss, C.B.; Kutter, T.; Kyba, C.C.M.; Lange, R.; Law, J.; Lawson, I.T.; Lesko, K.T.; Leslie, J.R.; Levine, I.; Loach, J.C.; Luoma, S.; MacLellan, R.; Majerus, S.; Mak, H.B.; Maneira, J.; Marino, A.D.; Martin, R.; McCauley, N.; McDonald, A.B.; McGee, S.; Mifflin, C.; Miller, M.L.; Monreal, B.; Monroe, J.; Noble, A.J.; Oblath, N.S.; Okada, C.E.; O?Keeffe, H.M.; Opachich, Y.; Orebi Gann, G.D.; Oser, S.M.; Ott, R.A.; Peeters, S.J.M.; Poon, A.W.P.; Prior, G.; Rielage, K.; Robertson, B.C.; Robertson, R.G.H.; Rollin, E.; Schwendener, M.H.; Secrest, J.A.; Seibert, S.R.; Simard, O.; Simpson, J.J.; Sinclair, D.; Skensved, P.; Smith, M.W.E.; Sonley, T.J.; Steiger, T.D.; Stonehill, L.C.; Tagg, N.; Tesic, G.; Tolich, N.; Tsui, T.; Van de Water, R.G.; VanDevender, B.A.; Virtue, C.J.; Waller, D.; Waltham, C.E.; Wan Chan Tseung, H.; Wark, D.L.; Watson, P.; Wendland, J.; West, N.; Wilkerson, J.F.; Wilson, J.R.; Wouters, J.M.; Wright, A.; Yeh, M.; Zhang, F.; Zuber, K.

2009-02-16T23:59:59.000Z

173

Predictions for the Cosmogenic Neutrino Flux in Light of New Data from the Pierre Auger Observatory  

E-Print Network (OSTI)

The Pierre Auger Observatory (PAO) has measured the spectrum and composition of the ultrahigh energy cosmic rays with unprecedented precision. We use these measurements to constrain their spectrum and composition as injected from their sources and, in turn, use these results to estimate the spectrum of cosmogenic neutrinos generated in their propagation through intergalactic space. We find that the PAO measurements can be well fit if the injected cosmic rays consist entirely of nuclei with masses in the intermediate (C, N, O) to heavy (Fe, Si) range. A mixture of protons and heavier species is also acceptable but (on the basis of existing hadronic interaction models) injection of pure light nuclei (p, He) results in unacceptable fits to the new elongation rate data. The expected spectrum of cosmogenic neutrinos can vary considerably, depending on the precise spectrum and chemical composition injected from the cosmic ray sources. In the models where heavy nuclei dominate the cosmic ray spectrum and few dissociated protons exceed GZK energies, the cosmogenic neutrino flux can be suppressed by up to two orders of magnitude relative to the all-proton prediction, making its detection beyond the reach of current and planned neutrino telescopes. Other models consistent with the data, however, are proton-dominated with only a small (1-10%) admixture of heavy nuclei and predict an associated cosmogenic flux within the reach of upcoming experiments. Thus a detection or non-detection of cosmogenic neutrinos can assist in discriminating between these possibilities.

Luis A. Anchordoqui; Haim Goldberg; Dan Hooper; Subir Sarkar; Andrew M. Taylor

2007-09-05T23:59:59.000Z

174

LISA-2020: An Intermediate Scale Space Gravitational Wave Observatory for This Decade  

E-Print Network (OSTI)

Over the last three decades, an exceptionally good science case has been made for pursuing gravitational wave (GW) astronomy. This has engendered a worldwide effort to detect the extremely weak signals generated by expected sources. With the next round of upgrades the ground based instruments are likely to make the first detections of the sources, and a new era of astronomy will begin, possibly as early as 2017. Inconveniently, due to seismic noise and baseline length issues, the low frequency (2030 now seems very unlikely. This paper examines the case for a scaled down mission that is comparable in cost and duration to medium scale astrophysics missions such as the 1978 ($630M) Einstein (HEAO 2) x-ray Observatory2, the 1989 ($680M) COBE Cosmic Background Explorer3, and the 1999 ($420M) FUSE Far Ultraviolet Spectroscopic Explorer4. We find that a mission of this class is possible if the measurement requirements are somewhat relaxed and a baseline smaller than LISA is used. It appears that such a mission could be launched by 2020 using a conventional program development plan, possibly including international collaboration. It would enable the timely development of this game-changing field of astrophysics, complementing the expected ground results with observations of massive black hole collisions. It would also serve as a stepping stone to LISA, greatly reducing the risk profile of that mission.

S. Buchman; J. A. Lipa; R. L. Byer; D. DeBra; K. Balakrishnan; G. Dufresne Cutler; A. Al-Fauwaz; E. Hultgren; A. K. Al-Jadaan; S. Saraf; S. Tan; S. Al-Thubiti; A. Zoellner

2013-02-10T23:59:59.000Z

175

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

176

Measurement of the Cosmic Ray and Neutrino-Induced Muon Flux at the Sudbury Neutrino Observatory  

SciTech Connect

Results are reported on the measurement of the atmospheric neutrino-induced muon flux at a depth of 2 kilometers below the Earth's 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 un-oscillated portion of the neutrino flux. A total of 514 muon-like events are measured between -1 {le} cos {theta}{sub zenith} 0.4 in a total exposure of 2.30 x 10{sup 14} cm{sup 2} s. The measured flux normalization is 1.22 {+-} 0.09 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 {theta}{sub zenith} > 0.4 is measured to be (3.31 {+-} 0.01 (stat.) {+-} 0.09 (sys.)) x 10{sup -10} {micro}/s/cm{sup 2}.

SNO collaboration; Aharmim, B.; Ahmed, S.N.; Andersen, T.C.; Anthony, A.E.; Barros, N.; Beier, E.W.; Bellerive, A.; Beltran, B.; Bergevin, M.; Biller, S.D.; Boudjemline, K.; Boulay, M.G.; Burritt, T.H.; Cai, B.; Chan, Y.D.; Chen, M.; Chon, M.C.; Cleveland, B.T.; Cox-Mobrand, G.A.; Currat, C.A.; Dai, X.; Dalnoki-Veress, F.; Deng, H.; Detwiler, J.; Doe, P.J.; Dosanjh, R.S.; Doucas, G.; Drouin, P.-L.; Duncan, F.A.; Dunford, M.; Elliott, S.R.; Evans, H.C.; Ewan, G.T.; Farine, J.; Fergani, H.; Fleurot, F.; Ford, R.J.; Formaggio, J.A.; Gagnon, N.; Goon, J.TM.; Grant, D.R.; Guillian, E.; Habib, S.; Hahn, R.L.; Hallin, A.L.; Hallman, E.D.; Hargrove, C.K.; Harvey, P.J.; Harvey, P.J.; Heeger, K.M.; Heintzelman, W.J.; Heise, J.; Helmer, R.L.; Hemingway, R.J.; Henning, R.; Hime, A.; Howard, C.; Howe, M.A.; Huang, M.; Jamieson, B.; Jelley, N.A.; Klein, J.R.; Kos, M.; Kruger, A.; Kraus, C.; Krauss, C.B.; Kutter, T.; Kyba, C.C.M.; Lange, R.; Law, J.; Lawson, I.T.; Lesko, K.T.; Leslie, J.R.; Levine, I.; Loach, J.C.; Luoma, S.; MacLellan, R.; Majerus, S.; Mak, H.B.; Maneira, J.; Marino, A.D.; Martin, R.; McCauley, N.; McDonald, A.B.; McGee, S.; Mifflin, C.; Miller, M.L.; Monreal, B.; Monroe, J.; Noble, A.J.; Oblath, N.S.; Okada, C.E.; O?Keeffe, H.M.; Opachich, Y.; Orebi Gann, G.D.; Oser, S.M.; Ott, R.A.; Peeters, S.J.M.; Poon, A.W.P.; Prior, G.; Rielage, K.; Robertson, B.C.; Robertson, R.G.H.; Rollin, E.; Schwendener, M.H.; Secrest, J.A.; Seibert, S.R.; Simard, O.; Simpson, J.J.; Sinclair, D.; Skensved, P.; Smith, M.W.E.; Sonley, T.J.; Steiger, T.D.; Stonehill, L.C.; Tagg, N.; Tesic, G.; Tolich, N.; Tsui, T.; Van de Water, R.G.; VanDevender, B.A.; Virtue, C.J.; Waller, D.; Waltham, C.E.; Wan Chan Tseung, H.; Wark, D.L.; Watson, P.; Wendland, J.; West, N.; Wilkerson, J.F.; Wilson, J.R.; Wouters, J.M.; Wright, A.; Yeh, M.; Zhang, F.; Zuber, K.

2009-02-16T23:59:59.000Z

177

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

DOE Data Explorer (OSTI)

The Pierre Auger Cosmic Ray Observatory in Mendoza, Argentina is the result of an international collaboration funded by 15 countries and many different organizations. Its mission is to capture high-energy cosmic ray events or air showers for research into their origin and nature. The Pierre Auger Collaboration agreed to make 1% of its data available to the public. The Public Event Explorer is a search tool that allows users to browse or search for and display figures and data plots of events collected since 2004. The repository is updated daily, and, as of July, 2009, makes 14,055 events publicly available. The energy of a cosmic ray is measured in Exa electron volts or EeV. These event displays can be browsed in order of their energy level from 0.1 to 41.1 EeV. Each event has an individual identification number.

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

None

178

The Apache Point Observatory Galactic Evolution Experiment: First Detection of High Velocity Milky Way Bar Stars  

E-Print Network (OSTI)

Commissioning observations with the Apache Point Observatory Galactic Evolution Experiment (APOGEE), part of the Sloan Digital Sky Survey III, have produced radial velocities (RVs) for ~4700 K/M-giant stars in the Milky Way bulge. These high-resolution (R \\sim 22,500), high-S/N (>100 per resolution element), near-infrared (1.51-1.70 um; NIR) spectra provide accurate RVs (epsilon_v~0.2 km/s) for the sample of stars in 18 Galactic bulge fields spanning -1-32 deg. This represents the largest NIR high-resolution spectroscopic sample of giant stars ever assembled in this region of the Galaxy. A cold (sigma_v~30 km/s), high-velocity peak (V_GSR \\sim +200 km/s) is found to comprise a significant fraction (~10%) of stars in many of these fields. These high RVs have not been detected in previous MW surveys and are not expected for a simple, circularly rotating disk. Preliminary distance estimates rule out an origin from the background Sagittarius tidal stream or a new stream in the MW disk. Comparison to various Galac...

Nidever, David L; Majewski, Steven R; Bird, Jonathan; Robin, Annie C; Martinez-Valpuesta, Inma; Beaton, Rachael L; Schoenrich, Ralph; Schultheis, Mathias; Wilson, John C; Skrutskie, Michael F; O'Connell, Robert W; Shetrone, Matthew; Schiavon, Ricardo P; Johnson, Jennifer A; Weiner, Benjamin; Gerhard, Ortwin; Schneider, Donald P; Prieto, Carlos Allende; Sellgren, Kris; Bizyaev, Dmitry; Brewington, Howard; Brinkmann, Jon; Eisenstein, Daniel J; Frinchaboy, Peter M; Perez, Ana Elia Garcia; Holtzman, Jon; Hearty, Fred R; Malanushenko, Elena; Malanushenko, Viktor; Muna, Demitri; Oravetz, Daniel; Pan, Kaike; Simmons, Audrey; Snedden, Stephanie; Weaver, Benjamin A

2012-01-01T23:59:59.000Z

179

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

E-Print Network (OSTI)

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

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

2007-05-23T23:59:59.000Z

180

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

E-Print Network (OSTI)

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

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

2011-01-01T23:59:59.000Z

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181

Gamma-ray astronomy: From Fermi up to the HAWC high-energy {gamma}-ray observatory in Sierra Negra  

SciTech Connect

Gamma-rays represent the most energetic electromagnetic window for the study of the Universe. They are studied both from space at MeV and GeV energies, with instruments like the Fermi{gamma}-ray Space Telescope, and at TeV energies with ground based instruments profiting of particle cascades in the atmosphere and of the Cerenkov radiation of charged particles in the air or in water. The Milagro gamma-ray observatory represented the first instrument to successfully implement the water Cerenkov technique for {gamma}-ray astronomy, opening the ground for the more sensitive HAWC {gamma}-ray observatory, currently under development in the Sierra Negra site and already providing early science results.

Carraminana, Alberto [Instituto Nacional de Astrofisica, Optica y Electronica Luis Enrique Erro 1, Tonantzintla, Puebla 72840 (Mexico); Collaboration: HAWC Collaboration

2013-06-12T23:59:59.000Z

182

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

E-Print Network (OSTI)

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

Carla Bleve; for the Pierre Auger Collaboration

2007-06-11T23:59:59.000Z

183

Selection and reconstruction of very inclined air showers with the Surface Detector of the Pierre Auger Observatory  

Science Conference Proceedings (OSTI)

The water-Cherenkov tanks of the Pierre Auger Observatory can detect particles at all zenith angles and are therefore well-suited for the study of inclined and horizontal air showers (60 degrees geomagnetic field. Dedicated algorithms for the selection and reconstruction of such events, as well as the corresponding acceptance calculation, have been set up on basis of muon maps obtained from shower simulations.

Newton, D.; /Santiago de Compostela U.

2007-06-01T23:59:59.000Z

184

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

E-Print Network (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 [superscript 3]He proportional counters was installed in the heavy-water ...

Formaggio, Joseph A.

185

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

SciTech Connect

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

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

2003-03-27T23:59:59.000Z

186

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

SciTech Connect

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

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

2003-03-27T23:59:59.000Z

187

EMERGING DIMMINGS OF ACTIVE REGIONS OBSERVED BY THE SOLAR DYNAMICS OBSERVATORY  

Science Conference Proceedings (OSTI)

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

188

Overview of the CALIPSO Mission and CALIOP Data Processing Algorithms  

Science Conference Proceedings (OSTI)

The Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) is a two-wavelength polarization lidar that performs global profiling of aerosols and clouds in the troposphere and lower stratosphere. CALIOP is the primary instrument on the Cloud-...

David M. Winker; Mark A. Vaughan; Ali Omar; Yongxiang Hu; Kathleen A. Powell; Zhaoyan Liu; William H. Hunt; Stuart A. Young

2009-11-01T23:59:59.000Z

189

Measurement of the $?_e$ and Total $^{8}$B Solar Neutrino Fluxes with the Sudbury Neutrino Observatory Phase I Data Set  

E-Print Network (OSTI)

This article provides the complete description of results from the Phase I data set of the Sudbury Neutrino Observatory (SNO). The Phase I data set is based on a 0.65 kt-year exposure of heavy water to the solar $^8$B neutrino flux. Included here are details of the SNO physics and detector model, evaluations of systematic uncertainties, and estimates of backgrounds. Also discussed are SNO's approach to statistical extraction of the signals from the three neutrino reactions (charged current, neutral current, and elastic scattering) and the results of a search for a day-night asymmetry in the $\

SNO Collaboration

2006-10-13T23:59:59.000Z

190

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

Science Conference Proceedings (OSTI)

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

191

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

E-Print Network (OSTI)

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

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; S. Coutu; C. E. Covault; A. Creusot; A. Criss; J. Cronin; A. Curutiu; S. Dagoret-Campagne; R. Dallier; S. Dasso; K. Daumiller; B. R. Dawson; R. M. de Almeida; M. De Domenico; C. De Donato; S. J. de Jong; G. De La Vega; W. J. M. de Mello Junior; J. R. T. de Mello Neto; I. De Mitri; V. de Souza; K. D. de Vries; G. Decerprit; L. del Peral; M. del Ro; 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; J. Espadanal; A. Etchegoyen; P. Facal San Luis; I. Fajardo Tapia; H. Falcke; G. Farrar; A. C. Fauth; N. Fazzini; A. P. Ferguson; A. Ferrero; B. Fick; A. Filevich; A. Filip?i?; S. Fliescher; C. E. Fracchiolla; E. D. Fraenkel; U. 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; L. Lu; A. Lucero; M. Ludwig; H. Lyberis; M. C. Maccarone; C. Macolino; S. Maldera; D. Mandat; P. Mantsch; A. G. Mariazzi; J. Marin; V. Marin; I. C. Maris; H. R. Marquez Falcon; G. Marsella; D. Martello; L. Martin; H. Martinez; O. 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; L. Molina-Bueno; 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; P. Oliva; V. M. Olmos-Gilbaja; M. Ortiz; N. Pacheco; D. Pakk Selmi-Dei; M. Palatka; J. Pallotta; N. Palmieri; G. Parente; E. Parizot; A. Parra; R. D. Parsons; S. Pastor; T. Paul; M. Pech; J. P?kala; R. Pelayo; I. M. Pepe; L. Perrone; R. Pesce; E. Petermann; S. Petrera; P. Petrinca; A. Petrolini; Y. Petrov; J. Petrovic; C. Pfendner; N. Phan; R. Piegaia; T. Pierog; P. Pieroni; M. Pimenta; V. Pirronello; M. Platino; V. H. Ponce; M. Pontz; P. Privitera; M. Prouza; E. J. Quel; S. Querchfeld; J. Rautenberg; O. Ravel; D. Ravignani; B. Revenu; J. Ridky; S. Riggi; M. Risse; P. Ristori; H. Rivera; V. Rizi; J. Roberts; C. Robledo; W. Rodrigues de Carvalho; G. Rodriguez; J. Rodriguez Martino; J. Rodriguez Rojo

2011-11-28T23:59:59.000Z

192

Performance of MEMS-based visible-light adaptive optics at Lick Observatory: Closed- and open-loop control  

E-Print Network (OSTI)

At the University of California's Lick Observatory, we have implemented an on-sky testbed for next-generation adaptive optics (AO) technologies. The Visible-Light Laser Guidestar Experiments instrument (ViLLaGEs) includes visible-light AO, a micro-electro-mechanical-systems (MEMS) deformable mirror, and open-loop control of said MEMS on the 1-meter Nickel telescope at Mt. Hamilton. In this paper we evaluate the performance of ViLLaGEs in open- and closed-loop control, finding that both control methods give equivalent Strehl ratios of up to ~ 7% in I-band and similar rejection of temporal power. Therefore, we find that open-loop control of MEMS on-sky is as effective as closed-loop control. Furthermore, after operating the system for three years, we find MEMS technology to function well in the observatory environment. We construct an error budget for the system, accounting for 130 nm of wavefront error out of 190 nm error in the science-camera PSFs. We find that the dominant known term is internal static error...

Morzinski, Katie; Gavel, Donald T; Grigsby, Bryant; Dillon, Daren; Reinig, Marc; Macintosh, Bruce A

2010-01-01T23:59:59.000Z

193

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/

194

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

DOE Data Explorer (OSTI)

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

Takahashi, T.

195

Transport of Stratospheric Air Masses to the Nepal Climate ObservatoryPyramid (Himalaya; 5079 m MSL): A Synoptic-Scale Investigation  

Science Conference Proceedings (OSTI)

This work analyzes and classifies stratospheric airmass transport events (ST) detected at the Nepal Climate ObservatoryPyramid (NCO-P; 2757?N, 8648?E, 5079 m MSL) Global Atmospheric WatchWorld Meteorological Organization station from March ...

A. Bracci; P. Cristofanelli; M. Sprenger; U. Bonaf; F. Calzolari; R. Duchi; P. Laj; A. Marinoni; F. Roccato; E. Vuillermoz; P. Bonasoni

2012-08-01T23:59:59.000Z

196

PATTERNS OF NANOFLARE STORM HEATING EXHIBITED BY AN ACTIVE REGION OBSERVED WITH SOLAR DYNAMICS OBSERVATORY/ATMOSPHERIC IMAGING ASSEMBLY  

Science Conference Proceedings (OSTI)

It is largely agreed that many coronal loops-those observed at a temperature of about 1 MK-are bundles of unresolved strands that are heated by storms of impulsive nanoflares. The nature of coronal heating in hotter loops and in the very important but largely ignored diffuse component of active regions is much less clear. Are these regions also heated impulsively, or is the heating quasi-steady? The spectacular new data from the Atmospheric Imaging Assembly (AIA) telescopes on the Solar Dynamics Observatory offer an excellent opportunity to address this question. We analyze the light curves of coronal loops and the diffuse corona in six different AIA channels and compare them with the predicted light curves from theoretical models. Light curves in the different AIA channels reach their peak intensities with predictable orderings as a function the nanoflare storm properties. We show that while some sets of light curves exhibit clear evidence of cooling after nanoflare storms, other cases are less straightforward to interpret. Complications arise because of line-of-sight integration through many different structures, the broadband nature of the AIA channels, and because physical properties can change substantially depending on the magnitude of the energy release. Nevertheless, the light curves exhibit predictable and understandable patterns consistent with impulsive nanoflare heating.

Viall, Nicholeen M.; Klimchuk, James A. [NASA Goddard Space Flight Center, Greenbelt, MD 20771 (United States)

2011-09-01T23:59:59.000Z

197

Increase in background stratospheric aerosol observed with lidar at Mauna Loa Observatory and Boulder, Colorado - article no. L15808  

Science Conference Proceedings (OSTI)

The stratospheric aerosol layer has been monitored with lidars at Mauna Loa Observatory in Hawaii and Boulder in Colorado since 1975 and 2000, respectively. Following the Pinatubo volcanic eruption in June 1991, the global stratosphere has not been perturbed by a major volcanic eruption providing an unprecedented opportunity to study the background aerosol. Since about 2000, an increase of 4-7% per year in the aerosol backscatter in the altitude range 20-30 km has been detected at both Mauna Loa and Boulder. This increase is superimposed on a seasonal cycle with a winter maximum that is modulated by the quasi-biennial oscillation (QBO) in tropical winds. Of the three major causes for a stratospheric aerosol increase: volcanic emissions to the stratosphere, increased tropical upwelling, and an increase in anthropogenic sulfur gas emissions in the troposphere, it appears that a large increase in coal burning since 2002, mainly in China, is the likely source of sulfur dioxide that ultimately ends up as the sulfate aerosol responsible for the increased backscatter from the stratospheric aerosol layer. The results are consistent with 0.6-0.8% of tropospheric sulfur entering the stratosphere.

Hofmann, D.; Barnes, J.; O'Neill, M.; Trudeau, M.; Neely, R. [NOAA, Boulder, CO (United States)

2009-08-15T23:59:59.000Z

198

Chandra X-ray Observatory Detection of Extended X-ray Emission from the Planetary Nebula BD+303639  

E-Print Network (OSTI)

We report the detection of well resolved, extended X-ray emission from the young planetary nebula BD+303639 using the Advanced CCD Imaging Spectrometer (ACIS) aboard the Chandra X-ray Observatory. The X-ray emission from BD+303639 appears to lie within, but is concentrated to one side of, the interior of the shell of ionized gas seen in high-resolution optical and IR images. The relatively low X-ray temperature (Tx ~ 3x10^6 K) and asymmetric morphology of the X-ray emission suggests that conduction fronts are present and/or mixing of shock-heated and photoionized gas has occurred and, furthermore, hints at the presence of magnetic fields. The ACIS spectrum suggests that the X-ray emitting region is enriched in the products of helium burning. Our detection of extended X-ray emission from BD+303639 demonstrates the power and utility of Chandra imaging as applied to the study of planetary nebulae.

Kstner, J H; Vrtilek, S D; Dgani, R; Kastner, Joel H.; Soker, Noam; Vrtilek, Saeqa; Dgani, Ruth

2000-01-01T23:59:59.000Z

199

Chandra X-ray Observatory Detection of Extended X-ray Emission from the Planetary Nebula BD+303639  

E-Print Network (OSTI)

We report the detection of well resolved, extended X-ray emission from the young planetary nebula BD+303639 using the Advanced CCD Imaging Spectrometer (ACIS) aboard the Chandra X-ray Observatory. The X-ray emission from BD+303639 appears to lie within, but is concentrated to one side of, the interior of the shell of ionized gas seen in high-resolution optical and IR images. The relatively low X-ray temperature (Tx ~ 3x10^6 K) and asymmetric morphology of the X-ray emission suggests that conduction fronts are present and/or mixing of shock-heated and photoionized gas has occurred and, furthermore, hints at the presence of magnetic fields. The ACIS spectrum suggests that the X-ray emitting region is enriched in the products of helium burning. Our detection of extended X-ray emission from BD+303639 demonstrates the power and utility of Chandra imaging as applied to the study of planetary nebulae.

Joel H. Kastner; Noam Soker; Saeqa Vrtilek; Ruth Dgani

2000-10-09T23:59:59.000Z

200

THE APACHE POINT OBSERVATORY GALACTIC EVOLUTION EXPERIMENT: FIRST DETECTION OF HIGH-VELOCITY MILKY WAY BAR STARS  

Science Conference Proceedings (OSTI)

Commissioning observations with the Apache Point Observatory Galactic Evolution Experiment (APOGEE), part of the Sloan Digital Sky Survey III, have produced radial velocities (RVs) for {approx}4700 K/M-giant stars in the Milky Way (MW) bulge. These high-resolution (R {approx} 22, 500), high-S/N (>100 per resolution element), near-infrared (NIR; 1.51-1.70 {mu}m) spectra provide accurate RVs ({epsilon}{sub V} {approx} 0.2 km s{sup -1}) for the sample of stars in 18 Galactic bulge fields spanning -1 Degree-Sign -32 Degree-Sign . This represents the largest NIR high-resolution spectroscopic sample of giant stars ever assembled in this region of the Galaxy. A cold ({sigma}{sub V} {approx} 30 km s{sup -1}), high-velocity peak (V{sub GSR} Almost-Equal-To +200 km s{sup -1}) is found to comprise a significant fraction ({approx}10%) of stars in many of these fields. These high RVs have not been detected in previous MW surveys and are not expected for a simple, circularly rotating disk. Preliminary distance estimates rule out an origin from the background Sagittarius tidal stream or a new stream in the MW disk. Comparison to various Galactic models suggests that these high RVs are best explained by stars in orbits of the Galactic bar potential, although some observational features remain unexplained.

Nidever, David L.; Zasowski, Gail; Majewski, Steven R.; Beaton, Rachael L.; Wilson, John C.; Skrutskie, Michael F.; O'Connell, Robert W. [Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325 (United States); Bird, Jonathan; Schoenrich, Ralph; Johnson, Jennifer A.; Sellgren, Kris [Department of Astronomy and the Center for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH 43210 (United States); Robin, Annie C.; Schultheis, Mathias [Institut Utinam, CNRS UMR 6213, OSU THETA, Universite de Franche-Comte, 41bis avenue de l'Observatoire, F-25000 Besancon (France); Martinez-Valpuesta, Inma; Gerhard, Ortwin [Max-Planck-Institut fuer Extraterrestrische Physik, Giessenbachstrasse, D-85748 Garching (Germany); Shetrone, Matthew [McDonald Observatory, University of Texas at Austin, Fort Davis, TX 79734 (United States); Schiavon, Ricardo P. [Gemini Observatory, 670 North A'Ohoku Place, Hilo, HI 96720 (United States); Weiner, Benjamin [Steward Observatory, 933 North Cherry Street, University of Arizona, Tucson, AZ 85721 (United States); Schneider, Donald P. [Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802 (United States); Allende Prieto, Carlos, E-mail: dln5q@virginia.edu [Instituto de Astrofisica de Canarias, E-38205 La Laguna, Tenerife (Spain); and others

2012-08-20T23:59:59.000Z

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.
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to obtain the most current and comprehensive results.


201

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

SciTech Connect

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

Collaboration, Auger

2012-08-01T23:59:59.000Z

202

A Study of the Effect of Molecular and Aerosol Conditions in the Atmosphere on Air Fluorescence Measurements at the Pierre Auger Observatory  

E-Print Network (OSTI)

The air fluorescence detector of the Pierre Auger Observatory is designed to perform calorimetric measurements of extensive air showers created by cosmic rays of above 10^18 eV. To correct these measurements for the effects introduced by atmospheric fluctuations, the Observatory contains a group of monitoring instruments to record atmospheric conditions across the detector site, an area exceeding 3,000 km^2. The atmospheric data are used extensively in the reconstruction of air showers, and are particularly important for the correct determination of shower energies and the depths of shower maxima. This paper contains a summary of the molecular and aerosol conditions measured at the Pierre Auger Observatory since the start of regular operations in 2004, and includes a discussion of the impact of these measurements on air shower reconstructions. Between 10^18 and 10^20 eV, the systematic uncertainties due to all atmospheric effects increase from 4% to 8% in measurements of shower energy, and 4 g/cm^2 to 8 g/cm^...

,

2010-01-01T23:59:59.000Z

203

The Catastrophic Flash-Flood Event of 89 September 2002 in the Gard Region, France: A First Case Study for the CvennesVivarais Mediterranean Hydrometeorological Observatory  

Science Conference Proceedings (OSTI)

The CvennesVivarais Mediterranean Hydrometeorological Observatory (OHM-CV) is a research initiative aimed at improving the understanding and modeling of the Mediterranean intense rain events that frequently result in devastating flash floods in ...

Guy Delrieu; John Nicol; Eddy Yates; Pierre-Emmanuel Kirstetter; Jean-Dominique Creutin; Sandrine Anquetin; Charles Obled; Georges-Marie Saulnier; Vronique Ducrocq; Eric Gaume; Olivier Payrastre; Herv Andrieu; Pierre-Alain Ayral; Christophe Bouvier; Luc Neppel; Marc Livet; Michel Lang; Jacques Parent du-Chtelet; Andrea Walpersdorf; Wolfram Wobrock

2005-02-01T23:59:59.000Z

204

Triggers for the Pierre Auger Observatory, the current status and plans for the future; EuCARD Editorial Series on Accelerator Science and Technology, (J-P.Koutchouk, R.S.Romaniuk, Editors), Vol.03  

E-Print Network (OSTI)

The Pierre Auger Observatory is a multi-national organization for research on ultra-high energy cosmic rays. The Southern Auger Observatory (Auger-South) in the province of Mendoza, Argentina, has been completed in 2008. First results on the energy spectrum, mass composition and distribution of arrival directions on the southern sky are really impressive. The planned Northern Auger Observatory in Colorado, USA, (Auger-North) will open a new window into the universe and establish charged particle astronomy to determine the origin and nature of ultra-high energy cosmic rays. These cosmic particles carry information complementary to neutrinos and photons and to gravitational waves. They also provide an extremely energetic beam for the study of particle interactions at energies that thirty times higher than those reached in terrestrial accelerators. The Auger Observatory is a hybrid detector consisting of a Surface Detector (SD) and an atmospheric Fluorescence Detector (FD). The hybrid data set obtained when both...

Szadkowski, Z

2009-01-01T23:59:59.000Z

205

COMPARISON OF FORCE-FREE CORONAL MAGNETIC FIELD MODELING USING VECTOR FIELDS FROM HINODE AND SOLAR DYNAMICS OBSERVATORY  

Science Conference Proceedings (OSTI)

Photospheric magnetic vector maps from two different instruments are used to model the nonlinear force-free coronal magnetic field above an active region. We use vector maps inferred from polarization measurements of the Solar Dynamics Observatory/Helioseismic and Magnetic Imager (HMI) and the Solar Optical Telescope's Spectropolarimeter (SP) on board Hinode. Besides basing our model calculations on HMI data, we use both SP data of original resolution and scaled down to the resolution of HMI. This allows us to compare the model results based on data from different instruments and to investigate how a binning of high-resolution data affects the model outcome. The resulting three-dimensional magnetic fields are compared in terms of magnetic energy content and magnetic topology. We find stronger magnetic fields in the SP data, translating into a higher total magnetic energy of the SP models. The net Lorentz forces of the HMI and SP lower boundaries verify their force-free compatibility. We find substantial differences in the absolute estimates of the magnetic field energy but similar relative estimates, e.g., the fraction of excess energy and of the flux shared by distinct areas. The location and extension of neighboring connectivity domains differ and the SP model fields tend to be higher and more vertical. Hence, conclusions about the magnetic connectivity based on force-free field models are to be drawn with caution. We find that the deviations of the model solution when based on the lower-resolution SP data are small compared to the differences of the solutions based on data from different instruments.

Thalmann, J. K.; Tiwari, S. K.; Wiegelmann, T., E-mail: thalmann@mps.mpg.de [Max-Plank-Institut fuer Sonnensystemforschung, Max-Planck-Str. 2, D-37191 Katlenburg-Lindau (Germany)

2013-05-20T23:59:59.000Z

206

SOUTH AFRICAN ASTRONOMICAL OBSERVATORY  

E-Print Network (OSTI)

................................................................................................62 8.3 Implementation Framework of the SALT­CBP .......................................63 8.4 Karoo in Southern Africa, with initiatives ranging from upliftment of the community in the Karoo-Hoogland area

Glass, Ian S.

207

Sommers-Bausch Observatory  

E-Print Network (OSTI)

the seminal HAO work in solar physics, space weather, and terrestrial climate effects) and the first graduate: Telescopes & Observing ......................................................... 37 Appendix III: Solar that was the optical heart of the solar telescope cracked from thermal stress. In the summer of 2007 we received a 10

Stowell, Michael

208

Sudbury Neutrino Observatory  

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

expertise in low-level radiation counting and both its local and Oroville counting facilities are essential for this. All materials used in the construction of the PSUP have...

209

OBSERVATORY STUDENT CENTER  

E-Print Network (OSTI)

RECEIVING CENTRAL GROUNDS FIELD HOUSE MORRIS GLENN PLANT #2 CHILL CENTER HEALTH HARTSHORN LORY B-WING GUGGEN- HEIM Theatre LSC GREENHOUSES QUONSETS N S HOLLEY PLANT ENVIRONMENTAL RESEARCH CENTER LAKE SUBSTATION

210

Low energy threshold analysis of the phase I and phase II data sets of the Sudbury neutrino observatory  

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

Seibert, S R [Los Alamos National Laboratory; Hime, A [Los Alamos National Laboratory; Elliott, S R [Los Alamos National Laboratory; Rielage, K [Los Alamos National Laboratory

2009-01-01T23:59:59.000Z

211

Time--Distance Helioseismology Data Analysis Pipeline for Helioseismic and Magnetic Imager onboard Solar Dynamics Observatory (SDO/HMI) and Its Initial Results  

E-Print Network (OSTI)

The Helioseismic and Magnetic Imager onboard the Solar Dynamics Observatory (SDO/HMI) provides continuous full-disk observations of solar oscillations. We develop a data-analysis pipeline based on the time-distance helioseismology method to measure acoustic travel times using HMI Doppler-shift observations, and infer solar interior properties by inverting these measurements. The pipeline is used for routine production of near-real-time full-disk maps of subsurface wave-speed perturbations and horizontal flow velocities for depths ranging from 0 to 20 Mm, every eight hours. In addition, Carrington synoptic maps for the subsurface properties are made from these full-disk maps. The pipeline can also be used for selected target areas and time periods. We explain details of the pipeline organization and procedures, including processing of the HMI Doppler observations, measurements of the travel times, inversions, and constructions of the full-disk and synoptic maps. Some initial results from the pipeline, includin...

Zhao, J; Bogart, R S; Parchevsky, K V; Birch, A C; Duvall, T L; Beck, J G; Kosovichev, A G; Scherrer, P H

2011-01-01T23:59:59.000Z

212

Reconstructing Past Solar Activity using Meridian Solar Observations: the Case of the Royal Observatory of the Spanish Navy (1833-1840)  

E-Print Network (OSTI)

Solar meridian observations have been used to evaluate the solar activity of the past. Some important examples are the solar meridian observations made at the Basilica of San Petronio in Bologna by several astronomers and the observations made by Hevelius published in his book Machina Coelestis. However, we do not know whether these observations, which were not aimed to estimate the solar activity, are reliable for evaluating solar activity. In this paper, we present the marginal notes about sunspots that are included in the manuscripts of the meridian solar observations made at the Royal Observatory of the Spanish Navy during the period 1833-1840. We compare these observations with other solar activity indices such as sunspot area and number. Our conclusion is that solar meridian observations should be used with extreme caution to evaluate past solar activity.

Vaquero, J M

2014-01-01T23:59:59.000Z

213

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

214

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

215

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

216

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

217

The effect of the geomagnetic field on cosmic ray energy estimates and large scale anisotropy searches on data from the Pierre Auger Observatory  

Science Conference Proceedings (OSTI)

We present a comprehensive study of the influence of the geomagnetic field on the energy estimation of extensive air showers with a zenith angle smaller than 60{sup o}, detected at the Pierre Auger Observatory. The geomagnetic field induces an azimuthal modulation of the estimated energy of cosmic rays up to the {approx} 2% level at large zenith angles. We present a method to account for this modulation of the reconstructed energy. We analyse the effect of the modulation on large scale anisotropy searches in the arrival direction distributions of cosmic rays. At a given energy, the geomagnetic effect is shown to induce a pseudo-dipolar pattern at the percent level in the declination distribution that needs to be accounted for. In this work, we have identified and quantified a systematic uncertainty affecting the energy determination of cosmic rays detected by the surface detector array of the Pierre Auger Observatory. This systematic uncertainty, induced by the influence of the geomagnetic field on the shower development, has a strength which depends on both the zenith and the azimuthal angles. Consequently, we have shown that it induces distortions of the estimated cosmic ray event rate at a given energy at the percent level in both the azimuthal and the declination distributions, the latter of which mimics an almost dipolar pattern. We have also shown that the induced distortions are already at the level of the statistical uncertainties for a number of events N {approx_equal} 32 000 (we note that the full Auger surface detector array collects about 6500 events per year with energies above 3 EeV). Accounting for these effects is thus essential with regard to the correct interpretation of large scale anisotropy measurements taking explicitly profit from the declination distribution.

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.; /Naples U. /INFN, Naples /Nijmegen U., IMAPP

2011-11-01T23:59:59.000Z

218

The CALIPSO Mission: A Global 3D View of Aerosols and Clouds  

Science Conference Proceedings (OSTI)

Aerosols and clouds have important effects on Earth's climate through their effects on the radiation budget and the cycling of water between the atmosphere and Earth's surface. Limitations in our understanding of the global distribution and ...

D. M. Winker; J. Pelon; J. A. Coakley Jr.; S. A. Ackerman; R. J. Charlson; P. R. Colarco; P. Flamant; Q. Fu; R. M. Hoff; C. Kittaka; T. L. Kubar; H. Le Treut; M. P. McCormick; G. Mgie; L. Poole; K. Powell; C. Trepte; M. A. Vaughan; B. A. Wielicki

2010-09-01T23:59:59.000Z

219

A Naive Bayesian Cloud-Detection Scheme Derived from CALIPSO and Applied within PATMOS-x  

Science Conference Proceedings (OSTI)

The naive Bayesian methodology has been applied to the challenging problem of cloud detection with NOAAs Advanced Very High Resolution Radiometer (AVHRR). An analysis of collocated NOAA-18/AVHRR and CloudAerosol Lidar and Infrared Pathfinder ...

Andrew K. Heidinger; Amato T. Evan; Michael J. Foster; Andi Walther

2012-06-01T23:59:59.000Z

220

Arctic Cloud Characteristics as Derived from MODIS, CALIPSO, and CloudSat  

Science Conference Proceedings (OSTI)

The Moderate Resolution Imaging Spectroradiometer (MODIS), CloudAerosol Lidar with Orthogonal Polarization (CALIOP), and CloudSat Cloud Profiling Radar (CPR) set of sensors, all in the Afternoon Constellation (A-Train), has been regarded as among ...

Mark Aaron Chan; Josefino C. Comiso

2013-05-01T23:59:59.000Z

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221

Fully Automated Detection of Cloud and Aerosol Layers in the CALIPSO Lidar Measurements  

Science Conference Proceedings (OSTI)

Accurate knowledge of the vertical and horizontal extent of clouds and aerosols in the earths atmosphere is critical in assessing the planets radiation budget and for advancing human understanding of climate change issues. To retrieve this ...

Mark A. Vaughan; Kathleen A. Powell; David M. Winker; Chris A. Hostetler; Ralph E. Kuehn; William H. Hunt; Brian J. Getzewich; Stuart A. Young; Zhaoyan Liu; Matthew J. McGill

2009-10-01T23:59:59.000Z

222

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

223

High sensitivity measurement of 224Ra and 226Ra in water with an improved hydrous titanium oxide technique at the Sudbury Neutrino Observatory  

E-Print Network (OSTI)

The existing hydrous titanium oxide (HTiO) technique for the measurement of 224Ra and 226Ra in the water at the Sudbury Neutrino Observatory (SNO) has been changed to make it faster and less sensitive to trace impurities in the HTiO eluate. Using HTiO-loaded filters followed by cation exchange adsorption and HTiO co-precipitation, Ra isotopes from 200-450 tonnes of heavy water can be extracted and concentrated into a single sample of a few millilitres with a total chemical efficiency of 50%. Combined with beta-alpha coincidence counting, this method is capable of measuring 2.0x10^3 uBq/kg of 224Ra and 3.7x10^3 uBq/kg of 226Ra from the 232Th and 238U decay chains, respectively, for a 275 tonne D2O assay, which are equivalent to 5x10^16 g Th/g and 3x10^16 g U/g in heavy water.

B. Aharmim; B. T. Cleveland; X. Dai; G. Doucas; J. Farine; H. Fergani; R. Ford; R. L. Hahn; E. D. Hallman; N. A. Jelley; R. Lange; S. Majerus; C. Mifflin; A. J. Noble; H. M. O'Keeffe; R. Rodriguez-Jimenez; D. Sinclair; M. Yeh

2008-03-28T23:59:59.000Z

224

A Search for Neutrinos from the Solar hep Reaction and the DiffuseSupernova Neutrino Background with the Sudbury Neutrino Observatory  

SciTech Connect

A search has been made for neutrinos from the hep reactionin the Sun and from the diffuse supernova neutrino background (DSNB)using data collected during the first operational phase of the SudburyNeutrino Observatory, with an exposure of 0.65 kilotonne-years. For thehep neutrino search, two events are observed in the effective electronenergy range of 14.3 MeV

Aharmim, B.; Ahmed, S.N.; Anthony, A.E.; Beier, E.W.; Bellerive,A.; Bergevin, M.; Biller, S.D.; Boulay, M.G.; Chan, Y.D.; Chen, M.; Chen,X.; Cleveland, B.T.; Cox, G.A.; Currat, C.A.; Dai, X.; Dalnoki-Veress,F.; Deng, H.; Detwiler, J.; DiMarco, M.; Doe, P.J.; Doucas, G.; Drouin,P.-L.; Duncan, F.A.; Dunford, M.; Dunmore, J.A.; Earle, E.D.; Evans,H.C.; Ewan, G.T.; Farine, J.; Fergani, H.; Fleurot, F.; Ford, R.J.; Formaggio, J.A.; Gagnon, N.; Goon, J.T.M.; Graham, K.; Guillian, E.; Hahn, R.L.; Hallin, A.L.; Hallman, E.D.; Harvey, P.J.; Hazama, R.; Heeger, K.M.; Heintzelman, W.J.; Heise, J.; Helmer, R.L.; Hemingway,R.J.; Henning, R.; Hime, A.; Howard, C.; Howe, M.A.; Huang, M.; Jagam,P.; Jelley, N.A.; Klein, J.R.; Kormos, L.L.; Kos, M.; Krueger, A.; Kraus,C.; Krauss, C.B.; Kutter, T.; Kyba, C.C.M.; Labranche, H.; Lange, R.; Law, J.Lawson.I.T.; Lesko, K.T.; Leslie, J.R.; Loach, J.C.; Luoma, S.; MacLellan, R.; Majerus, S.; Mak, H.B.; Maneira, J.; Marino, A.D.; Martin,R.; McCauley, N.; McDonald, A.B.; McGee, S.; Mifflin, C.; Miknaitis,K.K.S.; Miller, M.L.; Monreal, B.; Nickel, B.G.; Noble, A.J.; Norman,E.B.; Oblath, N.S.; Okada, C.E.; O'Keeffe, H.M.; Orebi Gann, G.D.; Oser,S.M.; Ott, R.; Peeters, S.J.M.; Poon, A.W.P.; Prior, G.; Rielage, K.; Robertson, B.C.; Robertson, R.G.H.; Rollin, E.; Schwendener, M.H.; Secrest, J.A.; Seibert, S.R.; Simard, O.; Sims, C.J.; Sinclair, D.; Skensved, P.; Stokstad, R.G.; Stonehill, L.C.; Tesic, G.; Tolich, N.; Tsui, T.; Van Berg, R.; Van de Water, R.G.; VanDevender, B.A.; Virtue,C.J.; Walker, T.J.; Wall, B.L.; Waller, D.; Wan Chan Tseung, H.; Wark,D.L.; Wendland, J.; West, N.; Wilkerson, J.F.; Wilson, J.R.; Wouters,J.M.; Wright, A.; Yeh, M.; Zhang, F.; Zuber, K.

2006-08-01T23:59:59.000Z

225

HINODE/EIS SPECTROSCOPIC VALIDATION OF VERY HOT PLASMA IMAGED WITH THE SOLAR DYNAMICS OBSERVATORY IN NON-FLARING ACTIVE REGION CORES  

Science Conference Proceedings (OSTI)

We use coronal imaging observations with the Solar Dynamics Observatory/Atmospheric Imaging Assembly (AIA), and Hinode/Extreme-ultraviolet Imaging Spectrometer (EIS) spectral data to explore the potential of narrowband EUV imaging data for diagnosing the presence of hot (T {approx}> 5 MK) coronal plasma in active regions. We analyze observations of two active regions (AR 11281, AR 11289) with simultaneous AIA imaging and EIS spectral data, including the Ca XVII line (at 192.8 A), which is one of the few lines in the EIS spectral bands sensitive to hot coronal plasma even outside flares. After careful co-alignment of the imaging and spectral data, we compare the morphology in a three-color image combining the 171, 335, and 94 A AIA spectral bands, with the image obtained for Ca XVII emission from the analysis of EIS spectra. We find that in the selected active regions the Ca XVII emission is strong only in very limited areas, showing striking similarities with the features bright in the 94 A (and 335 A) AIA channels and weak in the 171 A band. We conclude that AIA imaging observations of the solar corona can be used to track hot plasma (6-8 MK), and so to study its spatial variability and temporal evolution at high spatial and temporal resolution.

Testa, Paola [Smithsonian Astrophysical Observatory, 60 Garden street, MS 58, Cambridge, MA 02138 (United States); Reale, Fabio, E-mail: ptesta@cfa.harvard.edu [Dipartimento di Fisica, Universita di Palermo, Piazza del Parlamento 1, 90134 Palermo (Italy)

2012-05-01T23:59:59.000Z

226

NEW Fe IX LINE IDENTIFICATIONS USING SOLAR AND HELIOSPHERIC OBSERVATORY/SOLAR ULTRAVIOLET MEASUREMENT OF EMITTED RADIATION AND HINODE/EIS JOINT OBSERVATIONS OF THE QUIET SUN  

Science Conference Proceedings (OSTI)

In this work, we study joint observations of Hinode/EUV Imaging Spectrometer (EIS) and Solar and Heliospheric Observatory/Solar Ultraviolet Measurement of Emitted Radiation of Fe IX lines emitted by the same level of the high energy configuration 3s {sup 2}3p {sup 5}4p. The intensity ratios of these lines are dependent on atomic physics parameters only and not on the physical parameters of the emitting plasma, so that they are excellent tools to verify the relative intensity calibration of high-resolution spectrometers that work in the 170-200 A and 700-850 A wavelength ranges. We carry out extensive atomic physics calculations to improve the accuracy of the predicted intensity ratio, and compare the results with simultaneous EIS-SUMER observations of an off-disk quiet Sun region. We were able to identify two ultraviolet lines in the SUMER spectrum that are emitted by the same level that emits one bright line in the EIS wavelength range. Comparison between predicted and measured intensity ratios, wavelengths and energy separation of Fe IX levels confirms the identifications we make. Blending and calibration uncertainties are discussed. The results of this work are important for cross-calibrating EIS and SUMER, as well as future instrumentation.

Landi, E.; Young, P. R. [Naval Research Laboratory, Space Science Division, Washington, DC 20375 (United States)

2009-12-20T23:59:59.000Z

227

Characteristics of geomagnetic cascading of ultra-high energy photons at the southern and northern sites of the Pierre Auger Observatory  

E-Print Network (OSTI)

Cosmic-ray photons above 10^19 eV can convert in the geomagnetic field and initiate a preshower, i.e. a particle cascade before entering the atmosphere. We compare the preshower characteristics at the southern and northern sites of the Pierre Auger Observatory. In addition to a shift of the preshower patterns on the sky due to the different pointing of the local magnetic field vectors, the fact that the northern Auger site is closer to the geomagnetic pole results in a different energy dependence of the preshower effect: photon conversion can start at smaller energies, but large conversion probabilitites (>90%) are reached for the whole sky at higher energies compared to the southern Auger site. We show how the complementary preshower features at the two sites can be used to search for ultra-high energy photons among cosmic rays. In particular, the different preshower characteristics at the northern Auger site may provide an elegant and unambiguous confirmation if a photon signal is detected at the southern site.

P. Homola; M. Risse; R. Engel; D. Gora; J. Pekala; B. Wilczynska; H. Wilczynski

2006-08-04T23:59:59.000Z

228

The Ability of MM5 to Simulate Ice Clouds: Systematic Comparison between Simulated and Measured Fluxes and Lidar/Radar Profiles at SIRTA Atmospheric Observatory  

SciTech Connect

Ice clouds play a major role in the radiative energy budget of the Earth-atmosphere system (Liou 1986). Their radiative effect is governed primarily by the equilibrium between their albedo and greenhouse effects. Both macrophysical and microphysical properties of ice clouds regulate this equilibrium. For quantifying the effect of these clouds onto climate and weather systems, they must be properly characterized in atmospheric models. In this paper we use remote-sensing measurements from the SIRTA ground based atmospheric observatory (Site Instrumental de Recherche par Teledetection Atmospherique, http://sirta.lmd.polytechnique.fr). Lidar and radar observations taken over 18 months are used, in order to gain statistical confidence in the model evaluation. Along this period of time, 62 days are selected for study because they contain parts of ice clouds. We use the ''model to observations'' approach by simulating lidar and radar signals from MM5 outputs. Other more classical variables such as shortwave and longwave radiative fluxes are also used. Four microphysical schemes, among which that proposed by Reisner et al. (1998) with original or modified parameterizations of particle terminal fall velocities (Zurovac-Jevtic and Zhang 2003, Heymsfield and Donner 1990), and the simplified Dudhia (1989) scheme are evaluated in this study.

Chiriaco, M.; Vautard, R.; Chepfer, H.; Haeffelin, M.; Wanherdrick, Y.; Morille, Y.; Protat, A.; Dudhia, J.

2005-03-18T23:59:59.000Z

229

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...

230

A QUARTER-CENTURY OF OBSERVATIONS OF COMET 10P/TEMPEL 2 AT LOWELL OBSERVATORY: CONTINUED SPIN-DOWN, COMA MORPHOLOGY, PRODUCTION RATES, AND NUMERICAL MODELING  

Science Conference Proceedings (OSTI)

We report on photometry and imaging of Comet 10P/Tempel 2 obtained at Lowell Observatory from 1983 through 2011. We measured a nucleus rotation period of 8.950 {+-} 0.002 hr from 16 nights of imaging acquired between 2010 September and 2011 January. This rotation period is longer than the period we previously measured in 1999, which was itself longer than the period measured in 1988, and demonstrates that Tempel 2 is continuing to spin down, presumably due to torques caused by asymmetric outgassing. A nearly linear jet was observed which varied little during a rotation cycle in both R and CN images acquired during the 1999 and 2010 apparitions. We measured the projected direction of this jet throughout the two apparitions and, under the assumption that the source region of the jet was near the comet's pole, determined a rotational pole direction of R.A./decl. = 151 Degree-Sign /+59 Degree-Sign from CN measurements and R.A./decl. = 173 Degree-Sign /+57 Degree-Sign from dust measurements (we estimate a circular uncertainty of 3 Degree-Sign for CN and 4 Degree-Sign for dust). Different combinations of effects likely bias both gas and dust solutions and we elected to average these solutions for a final pole direction of R.A./decl. = 162 Degree-Sign {+-} 11 Degree-Sign /+58 Degree-Sign {+-} 1 Degree-Sign . Photoelectric photometry was acquired on 3 nights in 1983, 2 nights in 1988, 19 nights in 1999/2000, and 10 nights in 2010/2011. The activity exhibited a steep 'turn-on' {approx}3 months prior to perihelion (the exact timing of which varies) and a relatively smooth decline after perihelion. The activity during the 1999 and 2010 apparitions was similar; limited data in 1983 and 1988 (along with IUE data from the literature) were systematically higher and the difference cannot be explained entirely by the smaller perihelion distance. We measured a 'typical' composition, in agreement with previous investigators. Monte Carlo numerical modeling with our pole solution best replicated the observed coma morphology for a source region located near a comet latitude of +80 Degree-Sign and having a radius of {approx}10 Degree-Sign . Our model reproduced the seasonal changes in activity, suggesting that the majority of Tempel 2's activity originates from a small active region located near the pole. We also find that a cosine-squared solar angle function gives the best fit as compared to a standard cosine function.

Knight, Matthew M.; Schleicher, David G.; Schwieterman, Edward W.; Christensen, Samantha R. [Lowell Observatory, 1400 W. Mars Hill Road, Flagstaff, AZ 86001 (United States); Farnham, Tony L., E-mail: knight@lowell.edu [Department of Astronomy, University of Maryland, College Park, MD 20742-2421 (United States)

2012-11-01T23:59:59.000Z

231

The virtual observatory service TheoSSA: Establishing a database of synthetic stellar flux standards. I. NLTE spectral analysis of the DA-type white dwarf G 191-B2B  

E-Print Network (OSTI)

H-rich, DA-type white dwarfs are particularly suited as primary standard stars for flux calibration. State-of-the-art NLTE models consider opacities of species up to trans-iron elements and provide reliable synthetic stellar-atmosphere spectra to compare with observation. We establish a database of theoretical spectra of stellar flux standards that are easily accessible via a web interface. In the framework of the Virtual Observatory, the German Astrophysical Virtual Observatory developed the registered service TheoSSA. It provides easy access to stellar spectral energy distributions (SEDs) and is intended to ingest SEDs calculated by any model-atmosphere code. In case of the DA white dwarf G 191-B2B, we demonstrate that the model reproduces not only its overall continuum shape but also the numerous metal lines exhibited in its ultraviolet spectrum. TheoSSA is in operation and contains presently a variety of SEDs for DA white dwarfs. It will be extended in the near future and can host SEDs of all primary and ...

Rauch, T; Kruk, J W; Werner, K

2013-01-01T23:59:59.000Z

232

Center for Nanophase Materials Sciences (CNMS) - Nanomaterials...  

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

NANOMATERIALS THEORY INSTITUTE (NTI): Computational Nanoscience End-station (CNE) In analogy to experimental end-stations at large experimental facilities, the Computational...

233

The Retrieval of Profiles of Particulate Extinction from Cloud-Aerosol Lidar Infrared Pathfinder Satellite Observations (CALIPSO) Data: Algorithm Description  

Science Conference Proceedings (OSTI)

This work describes the algorithms used for the fully automated retrieval of profiles of particulate extinction coefficients from the attenuated backscatter data acquired by the lidar on board the Cloud-Aerosol Lidar Infrared Pathfinder Satellite ...

Stuart A. Young; Mark A. Vaughan

2009-06-01T23:59:59.000Z

234

OBSERVATIONS OF FIVE-MINUTE SOLAR OSCILLATIONS IN THE CORONA USING THE EXTREME ULTRAVIOLET SPECTROPHOTOMETER (ESP) ON BOARD THE SOLAR DYNAMICS OBSERVATORY EXTREME ULTRAVIOLET VARIABILITY EXPERIMENT (SDO/EVE)  

Science Conference Proceedings (OSTI)

We report on the detection of oscillations in the corona in the frequency range corresponding to five-minute acoustic modes of the Sun. The oscillations have been observed using soft X-ray measurements from the Extreme Ultraviolet Spectrophotometer (ESP) of the Extreme Ultraviolet Variability Experiment on board the Solar Dynamics Observatory. The ESP zeroth-order channel observes the Sun as a star without spatial resolution in the wavelength range of 0.1-7.0 nm (the energy range is 0.18-12.4 keV). The amplitude spectrum of the oscillations calculated from six-day time series shows a significant increase in the frequency range of 2-4 mHz. We interpret this increase as a response of the corona to solar acoustic (p) modes and attempt to identify p-mode frequencies among the strongest peaks. Due to strong variability of the amplitudes and frequencies of the five-minute oscillations in the corona, we study how the spectrum from two adjacent six-day time series combined together affects the number of peaks associated with the p-mode frequencies and their amplitudes. This study shows that five-minute oscillations of the Sun can be observed in the corona in variations of the soft X-ray emission. Further investigations of these oscillations may improve our understanding of the interaction of the oscillation modes with the solar atmosphere, and the interior-corona coupling, in general.

Didkovsky, L.; Judge, D.; Wieman, S. [Space Sciences Center, University of Southern California, Los Angeles, CA 90089 (United States); Kosovichev, A. G. [W. W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305 (United States); Woods, T., E-mail: leonid@usc.edu [Laboratory for Atmospheric and Space Physics, University of Colorado at Boulder, Boulder, CO 80301 (United States)

2011-09-01T23:59:59.000Z

235

Compton Gamma Ray Observatory/BATSE observations of energetic electrons scattered by cyclotron resonance with waves from powerful VLF transmitters. Final report, 13 October 1992-12 February 1994  

SciTech Connect

To obtain a better understanding of the wave-particle mechanisms responsible for the loss of electrons from the radiation belts, energetic electron data from the Burst and Transient Source Experiment (BATSE) on the NASA's Compton Gamma Ray Observatory (GRO) was studied. Powerful ground-based VLF transmitters resonantly scatter electrons from the inner radiation belt onto trajectories from which they precipitate into the atmosphere as they drift eastward. 563 instances in which the satellite traversed a cloud of energetic electrons which had been scattered into quasi-trapped trajectories were identified. From the longitude distribution, it was concluded that waves from the VLF transmitter NWC at 114 deg E are the origin of 257 of the events, and waves from UMSat 44 deg E related to 45 more. In another 177 cases the electrons had drifted from the longitude of these transmitters to a location in the western hemisphere. The previously reported seasonal variation in the frequency of occurrence of cyclotron resonance interaction is confirmed with the continuous coverage provided by GRO. The frequency of occurrence of the cyclotron resonance interactions is largest before sunrise, which the authors attribute to the diurnal variations in the transmission VLF waves through the ionosphere. For the first time, unique very narrow sheets of electrons occurring in the aftermath of a large geomagnetic storm are reported.

Datlowe, D.W.; Imhof, W.L.

1994-02-01T23:59:59.000Z

236

Felix-Klein-Kolloquium Heinrich-Heine-Universitt Dsseldorf  

E-Print Network (OSTI)

. Einstieg: Bahnhofsvorplatz, Bstg. 7 Ausstieg: Endstation Uni-Ost/Botanischer Garten Fahrtzeit: ca. 19

237

DIRECT IMAGING OF QUASI-PERIODIC FAST PROPAGATING WAVES OF {approx}2000 km s{sup -1} IN THE LOW SOLAR CORONA BY THE SOLAR DYNAMICS OBSERVATORY ATMOSPHERIC IMAGING ASSEMBLY  

Science Conference Proceedings (OSTI)

Quasi-periodic propagating fast mode magnetosonic waves in the solar corona were difficult to observe in the past due to relatively low instrument cadences. We report here evidence of such waves directly imaged in EUV by the new Atmospheric Imaging Assembly instrument on board the Solar Dynamics Observatory. In the 2010 August 1 C3.2 flare/coronal mass ejection event, we find arc-shaped wave trains of 1%-5% intensity variations (lifetime {approx}200 s) that emanate near the flare kernel and propagate outward up to {approx}400 Mm along a funnel of coronal loops. Sinusoidal fits to a typical wave train indicate a phase velocity of 2200 {+-} 130 km s{sup -1}. Similar waves propagating in opposite directions are observed in closed loops between two flare ribbons. In the k-{omega} diagram of the Fourier wave power, we find a bright ridge that represents the dispersion relation and can be well fitted with a straight line passing through the origin. This k-{omega} ridge shows a broad frequency distribution with power peaks at 5.5, 14.5, and 25.1 mHz. The strongest signal at 5.5 mHz (period 181 s) temporally coincides with quasi-periodic pulsations of the flare, suggesting a common origin. The instantaneous wave energy flux of (0.1-2.6) x 10{sup 7} erg cm{sup -2} s{sup -1} estimated at the coronal base is comparable to the steady-state heating requirement of active region loops.

Liu Wei; Title, Alan M.; Schrijver, Carolus J.; Aschwanden, Markus J.; De Pontieu, Bart; Tarbell, Theodore D. [Lockheed Martin Solar and Astrophysics Laboratory, Building 252, 3251 Hanover Street, Palo Alto, CA 94304 (United States); Zhao Junwei [W. W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305 (United States); Ofman, Leon [Catholic University of America and NASA Goddard Space Flight Center, Code 671, 8800 Greenbelt Road, Greenbelt, MD 20771 (United States)

2011-07-20T23:59:59.000Z

238

Toward Observatory Cloud Computing | Argonne National Laboratory  

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

August 27, 2013 Tweet EmailPrint New inexpensive and reliable sensing devices, such as weather cameras and floats, are allowing us to monitor in real-time a variety of phenomena on...

239

NATIONAL RADIO ASTRONOMY OBSERVATORY CHARLOTTESVILLE, VIRGINIA  

E-Print Network (OSTI)

and the photodetectors. The #12;light source is two miniature light bulbs which are mounted on the side of the chopper the light bulbs. The bracket in which they are mounted has a position adjustment for one as to see the hot load, and cold load in sequence. The inner radius is used to chop between the light source

Groppi, Christopher

240

Mary Lea Heger Shane: The Lick Observatory  

E-Print Network (OSTI)

to work with the people and learn as an apprentice.The old type of apprentice -- learning. from watching and

Shane, Mary Lea; Calciano, Elizabeth Spedding

1969-01-01T23:59:59.000Z

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.


241

Solstice Observers and Observatories in Native California  

E-Print Network (OSTI)

events in California rock art. Sources: a. Juniper Cave,events in California rock art. Sources: a, Hole- in-the-events in California rock art. Sources: Ker-17 (pictograph,

Hudson, Travis; Lee, Georgia; Hedges, Ken

1979-01-01T23:59:59.000Z

242

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

243

Toward a Resiliency and Vulnerability Observatory Network ...  

Science Conference Proceedings (OSTI)

... is already undertaking extensive investment in its ... vulnerability or more generally, equity, should permeate all ... etc.), parcel and/or tax portfolio data ...

2009-02-05T23:59:59.000Z

244

Pierre Auger Observatory Surface Detector Cabling Plan  

E-Print Network (OSTI)

ELECTRONICS METAL BOX Motherboard (PCC/CdF) MBB1 2 push-in terminals (tech name?) - 24V power in MBJ8 HE10 a comprehensive list of connectors on boards, terminals, feedthroughs, etc; that is, anything which constitutes used here. Pinouts for the sockets and terminals must also be collected. Connector part numbers, hole

245

THE 2011 FEBRUARY 15 X2 FLARE, RIBBONS, CORONAL FRONT, AND MASS EJECTION: INTERPRETING THE THREE-DIMENSIONAL VIEWS FROM THE SOLAR DYNAMICS OBSERVATORY AND STEREO GUIDED BY MAGNETOHYDRODYNAMIC FLUX-ROPE MODELING  

SciTech Connect

The 2011 February 15 X2.2 flare and associated Earth-directed halo coronal mass ejection were observed in unprecedented detail with high resolution in spatial, temporal, and thermal dimensions by the Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory, as well as by instruments on the two STEREO spacecraft, then at near-quadrature relative to the Sun-Earth line. These observations enable us to see expanding loops from a flux-rope-like structure over the shearing polarity-inversion line between the central {delta}-spot groups of AR 11158, developing a propagating coronal front ('EIT wave'), and eventually forming the coronal mass ejection moving into the inner heliosphere. The observations support the interpretation that all of these features, including the 'EIT wave', are signatures of an expanding volume traced by loops (much larger than the flux rope only), surrounded by a moving front rather than predominantly wave-like perturbations; this interpretation is supported by previously published MHD models for active-region and global scales. The lateral expansion of the eruption is limited to the local helmet-streamer structure and halts at the edges of a large-scale domain of connectivity (in the process exciting loop oscillations at the edge of the southern polar coronal hole). The AIA observations reveal that plasma warming occurs within the expansion front as it propagates over quiet Sun areas. This warming causes dimming in the 171 A (Fe IX and Fe X) channel and brightening in the 193 and 211 A (Fe XII-XIV) channels along the entire front, while there is weak 131 A (Fe VIII and Fe XXI) emission in some directions. An analysis of the AIA response functions shows that sections of the front running over the quiet Sun are consistent with adiabatic warming; other sections may require additional heating which MHD modeling suggests could be caused by Joule dissipation. Although for the events studied here the effects of volumetric expansion are much more obvious than true wave phenomena, we discuss how different magnetic environments within and around the erupting region can lead to the signatures of either or both of these aspects.

Schrijver, Carolus J.; Title, Alan M. [Lockheed Martin Advanced Technology Center, 3251 Hanover Street, Palo Alto, CA 94304 (United States); Aulanier, Guillaume; Pariat, Etienne; Delannee, Cecile, E-mail: schrijver@lmsal.com, E-mail: title@lmsal.com, E-mail: guillaume.aulanier@obspm.fr, E-mail: etienne.pariat@obspm.fr, E-mail: ceaulanier@voila.fr [LESIA, Observatoire de Paris, CNRS, UPMC, Universite Paris Diderot, 5 Place Jules Janssen, 92190 Meudon (France)

2011-09-10T23:59:59.000Z

246

Reply to Comments on ``Seasonal Variation of the Physical Properties of Marine Boundary Layer Clouds off the California Coast''  

E-Print Network (OSTI)

CloudSat and Cloud-Aerosol Lidar and Infrared Pathfinder Stellite Observations (CALIPSO). J. Geophys

247

THE PLERIONIC SUPERNOVA REMNANT G21.5-0.9 POWERED BY PSR J1833-1034: NEW SPECTROSCOPIC AND IMAGING RESULTS REVEALED WITH THE CHANDRA X-RAY OBSERVATORY  

Science Conference Proceedings (OSTI)

In 1999, the Chandra X-ray Observatory revealed a 150'' radius halo surrounding the 40'' radius pulsar wind nebula (PWN) G21.5-0.9. A 2005 imaging study of G21.5-0.9 showed that the halo is limb-brightened and suggested that this feature is a candidate for the long-sought supernova remnant (SNR) shell. We present a spectral analysis of SNR G21.5-0.9, using the longest effective observation to date (578.6 ks with the Advanced CCD Imaging Spectrometer (ACIS) and 278.4 ks with the High-Resolution Camera (HRC)) to study unresolved questions about the spectral nature of remnant features, such as the limb brightening of the X-ray halo and the bright knot in the northern part of the halo. The Chandra analysis favors the non-thermal interpretation of the limb. Its spectrum is fit well with a power-law model with a photon index {Gamma} = 2.13 (1.94-2.33) and a luminosity of L{sub x} (0.5-8 keV) = (2.3 {+-} 0.6) x 10{sup 33} erg s{sup -1} (at an assumed distance of 5.0 kpc). An srcut model was also used to fit the spectrum between the radio and X-ray energies. While the absence of a shell in the radio still prohibits constraining the spectrum at radio wavelengths, we assume a range of spectral indices to infer the 1 GHz flux density and the rolloff frequency of the synchrotron spectrum in X-rays and find that the maximum energy to which electrons are accelerated at the shock ranges from {approx}60 to 130 TeV (B/10 {mu}G){sup -1/2}, where B is the magnetic field in units of {mu}G. For the northern knot, we constrain previous models and find that a two-component power-law (or srcut) + pshock model provides an adequate fit, with the pshock model requiring a very low ionization timescale and solar abundances for Mg and Si. Our spectroscopic study of PSR J1833-1034, the highly energetic pulsar powering G21.5-0.9, shows that its spectrum is dominated by hard non-thermal X-ray emission with some evidence of a thermal component that represents {approx}9% of the observed non-thermal emission and that suggests non-standard rapid cooling of the neutron star. Finally, the ACIS and HRC-I images provide the first evidence for variability in the PWN, a property observed in other PWNe such as the Crab and Vela.

Matheson, Heather [Department of Physics and Astronomy, University of Manitoba, Winnipeg, Manitoba, R3T 2N2 (Canada); Safi-Harb, Samar, E-mail: matheson@physics.umanitoba.c, E-mail: samar@physics.umanitoba.c [Canada Research Chair. (Canada)

2010-11-20T23:59:59.000Z

248

The CM-SAF and FUB Cloud Detection Schemes for SEVIRI: Validation with Synoptic Data and Initial Comparison with MODIS and CALIPSO  

Science Conference Proceedings (OSTI)

The Satellite Application Facility on Climate Monitoring (CM-SAF) is aiming to retrieve satellite-derived geophysical parameters suitable for climate monitoring. CM-SAF started routine operations in early 2007 and provides a climatology of ...

M. Reuter; W. Thomas; P. Albert; M. Lockhoff; R. Weber; K-G. Karlsson; J. Fischer

2009-02-01T23:59:59.000Z

249

Evaluation of the Hydrometeor Layers in the East and West Pacific Within ISCCP Cloud Top Pressure-Optical Depth Bins Using Merged CloudSat and CALIPSO Data  

Science Conference Proceedings (OSTI)

ISCCP provides a multi-decadal and global description of cloud properties that are often grouped into joint histograms of column visible optical depth (?) and effective cloud top pressure (Ptop). It has not been possible until recently to know the ...

Gerald G. Mace; Forrest J. Wrenn

250

Comparing Occurrences and Vertical Structures of Hydrometeors between Eastern China and the Indian Monsoon Region Using CloudSat/CALIPSO Data  

Science Conference Proceedings (OSTI)

Seasonal variations in the occurrence frequency, vertical location, and radar reflectivity factor (dBZ) of hydrometeors covering eastern China and the Indian monsoon region are described using two CloudSat standard products [Geometrical Profiling ...

Yali Luo; Renhe Zhang; Hui Wang

2009-02-01T23:59:59.000Z

251

Characteristics of CALIPSO and CloudSat Backscatter at the Top Center Layers of Mesoscale Convective Systems and Relation to Cloud Microphysics  

Science Conference Proceedings (OSTI)

Following the discovery of anomalously high values of lidar integrated attenuated backscatter near the top center layers of mesoscale convective systems (MCSs) observed by the NASA Lidar In-Space Technology Experiment (LITE), a search of Cloud ...

C. M. R. Platt; M. A. Vaughan; R. T. Austin

2011-02-01T23:59:59.000Z

252

Study of MPLNET-Derived Aerosol Climatology over Kanpur, India, and Validation of CALIPSO Level 2 Version 3 Backscatter and Extinction Products  

Science Conference Proceedings (OSTI)

The level 2 aerosol backscatter and extinction profiles from the NASA Micropulse Lidar Network (MPLNET) at Kanpur, India, have been studied from May 2009 to September 2010. Monthly averaged extinction profiles from MPLNET shows high extinction ...

Amit Misra; S. N. Tripathi; D. S. Kaul; Ellsworth J. Welton

2012-09-01T23:59:59.000Z

253

Core-Shell Strain Structure of Zeolite Microcrystals  

Science Conference Proceedings (OSTI)

Study of Charge-Ordering in Manganites via Serial Femtosecond Crystallography XFEL Materials Imaging at the LCLS CXI Endstation...

254

Coherent Diffraction Imaging of Materials by Using an X-ray Free ...  

Science Conference Proceedings (OSTI)

Study of Charge-Ordering in Manganites via Serial Femtosecond Crystallography XFEL Materials Imaging at the LCLS CXI Endstation...

255

Nanoscale X-Ray Imaging - Programmaster.org  

Science Conference Proceedings (OSTI)

Study of Charge-Ordering in Manganites via Serial Femtosecond Crystallography XFEL Materials Imaging at the LCLS CXI Endstation...

256

On the Precipitation of ? Phase in Ni-Base Superalloy 718Plus  

Science Conference Proceedings (OSTI)

Study of Charge-Ordering in Manganites via Serial Femtosecond Crystallography XFEL Materials Imaging at the LCLS CXI Endstation...

257

Advanced Reconstruction Algorithms for Ptychography  

Science Conference Proceedings (OSTI)

Study of Charge-Ordering in Manganites via Serial Femtosecond Crystallography XFEL Materials Imaging at the LCLS CXI Endstation...

258

Diffractive Imaging at Large Fresnel Number and the Challenge of ...  

Science Conference Proceedings (OSTI)

Study of Charge-Ordering in Manganites via Serial Femtosecond Crystallography XFEL Materials Imaging at the LCLS CXI Endstation...

259

Applications of X-Ray Bragg Projections Ptychography  

Science Conference Proceedings (OSTI)

Study of Charge-Ordering in Manganites via Serial Femtosecond Crystallography XFEL Materials Imaging at the LCLS CXI Endstation...

260

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)

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

NIST Spectral Data for the Chandra X-Ray Observatory  

Science Conference Proceedings (OSTI)

... To search for the data previously contained in this database (multiply ionized spectra of Ne, Mg, Si, and S), please go to ASD by clicking on the link ...

2011-12-09T23:59:59.000Z

262

NATIONAL RADIO ASTRONMY OBSERVATORY GREEN BANK, WEST VIRGINIA  

E-Print Network (OSTI)

this context, our critical infrastructure and key resources (CIKR) may be directly exposed to the event themselves or indirectly exposed as a result of the dependencies and interde- pendencies among CIKR. Within the CIKR protection mission area, national priorities must include preventing catastrophic loss of life

Groppi, Christopher

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

Sensitivity Studies for Third-Generation Gravitational Wave Observatories  

E-Print Network (OSTI)

Advanced gravitational wave detectors, currently under construction, are expected to directly observe gravitational wave signals of astrophysical origin. The Einstein Telescope, a third-generation gravitational wave detector, has been proposed in order to fully open up the emerging field of gravitational wave astronomy. In this article we describe sensitivity models for the Einstein Telescope and investigate potential limits imposed by fundamental noise sources. A special focus is set on evaluating the frequency band below 10Hz where a complex mixture of seismic, gravity gradient, suspension thermal and radiation pressure noise dominates. We develop the most accurate sensitivity model, referred to as ET-D, for a third-generation detector so far, including the most relevant fundamental noise contributions.

S. Hild; M. Abernathy; F. Acernese; P. Amaro-Seoane; N. Andersson; K. Arun; F. Barone; B. Barr; M. Barsuglia; M. Beker; N. Beveridge; S. Birindelli; S. Bose; L. Bosi; S. Braccini; C. Bradaschia; T. Bulik; E. Calloni; G. Cella; E. Chassande Mottin; S. Chelkowski; A. Chincarini; J. Clark; E. Coccia; C. Colacino; J. Colas; A. Cumming; L. Cunningham; E. Cuoco; S. Danilishin; K. Danzmann; R. De Salvo; T. Dent; R. De Rosa; L. Di Fiore; A. Di Virgilio; M. Doets; V. Fafone; P. Falferi; R. Flaminio; J. Franc; F. Frasconi; A. Freise; D. Friedrich; P. Fulda; J. Gair; G. Gemme; E. Genin; A. Gennai; A. Giazotto; K. Glampedakis; C. Grf; M. Granata; H. Grote; G. Guidi; A. Gurkovsky; G. Hammond; M. Hannam; J. Harms; D. Heinert; M. Hendry; I. Heng; E. Hennes; J. Hough; S. Husa; S. Huttner; G. Jones; F. Khalili; K. Kokeyama; K. Kokkotas; B. Krishnan; T. G. F. Li; M. Lorenzini; H. Lck; E. Majorana; I. Mandel; V. Mandic; M. Mantovani; I. Martin; C. Michel; Y. Minenkov; N. Morgado; S. Mosca; B Mours; H. Mller-Ebhardt; P. Murray; R. Nawrodt; J. Nelson; R. Oshaughnessy; C. D. Ott; C. Palomba; A. Paoli; G. Parguez; A. Pasqualetti; R. Passaquieti; D. Passuello; L. Pinard; W. Plastino; R. Poggiani1; P. Popolizio; M. Prato; M. Punturo; P. Puppo; D. Rabeling; P. Rapagnani; J. Read; T. Regimbau; H. Rehbein; S. Reid; F. Ricci; F. Richard; A. Rocchi; S. Rowan; A. Rdiger; L. Santamara; B. Sassolas; B. Sathyaprakash; R. Schnabel; C. Schwarz; P. Seidel; A. Sintes; K. Somiya; F. Speirits; K. Strain; S Strigin; P. Sutton; S. Tarabrin; A. Thring; J. van den Brand; M. van Veggel; C. van den Broeck; A. Vecchio; J. Veitch; F. Vetrano; A. Vicere; S. Vyatchanin; B. Willke; G. Woan; K. Yamamoto

2010-12-04T23:59:59.000Z

265

Design of light concentrators for Cherenkov telescope observatories  

E-Print Network (OSTI)

The Cherenkov Telescope Array (CTA) will be the largest cosmic gamma ray detector ever built in the world. It will be installed at two different sites in the North and South hemispheres and should be operational for about 30 years. In order to cover the desired energy range, the CTA is composed of typically 50-100 collecting telescopes of various sizes (from 6 to 24-m diameters). Most of them are equipped with a focal plane camera consisting of 1500 to 2000 Photomultipliers (PM) equipped with light concentrating optics, whose double function is to maximize the amount of Cherenkov light detected by the photo-sensors, and to block any stray light originating from the terrestrial environment. Two different optical solutions have been designed, respectively based on a Compound Parabolic Concentrator (CPC), and on a purely dioptric concentrating lens. In this communication are described the technical specifications, optical designs and performance of the different solutions envisioned for all these light concentra...

Hnault, F; jocou, L; Khlifi, B; Manigot, P; Hormigos, S; Knodlseder, J; Olive, J F; Jean, P; Punch, M

2013-01-01T23:59:59.000Z

266

GOPAL NARAYANAN's Curriculum Vitae Five College Radio Astronomy Observatory  

E-Print Network (OSTI)

Languages: FORTRAN, C, Perl, Pascal, BASIC, DCL, C shell, Tcl/Tk. Operating Systems: Linux, Solaris, Sun

Narayanan, Gopal

267

Evidence for neutrino oscillations in the Sudbury Neutrino Observatory  

E-Print Network (OSTI)

ux in the Standard Solar Model of the Sun. The long-standingwithin the solar core (inner ?20% of the Suns radius). Thesolar neutrino ?ux probe the nuclear fusion reactions fueling the Sun.

Marino, Alysia Diane

2004-01-01T23:59:59.000Z

268

Lab scientist receives NASA award for the Solar Dynamics Observatory...  

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

movies are shown by news media outlets whenever there is intense solar activity such as solar flares and coronal mass ejections. By imaging the sun at specific EUV emission lines...

269

Scottish Observatory for Work and Health University of Glasgow  

E-Print Network (OSTI)

, Glasgow City, North Lanarkshire, South Lanarkshire) Item 1a & 1b will also be provided at CHCP level authorities (i.e. Glasgow City, North Lanarkshire, South Lanarkshire) and at CHCP level for CHCPs within

Glasgow, University of

270

Green Bank, West Virginia National Radio Astronomy Observatory  

E-Print Network (OSTI)

, 28.00 to repair the gear box for the site emergency generator which was damaged when the oil pump which indicates General Electric is the sole service. The jet engine oil system is common with the gear box oil system that failed. The oil sump had metal filing in it when the gear box was removed and sent

Groppi, Christopher

271

NATIONAL RADIO ASTRONOMY OBSERVATORY GREEN BANK, WEST VIRGINIA  

E-Print Network (OSTI)

Spray: Sprayed into the nose, nicotine enters the system very quickly. Non-Nicotine Medications­ Zyban (birth control pill) use -- African-American heritage UHS Health Promotion Office 110 Anderson Tower www

Groppi, Christopher

272

Los Alamos observatory fingers cosmic ray 'hot spots'  

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

magnetic fields near our solar system. November 24, 2008 Los Alamos National Laboratory sits on top of a once-remote mesa in northern New Mexico with the Jemez mountains as...

273

Electron antineutrino search Sudbury Neutrino Observatory 9 Bellerive,  

E-Print Network (OSTI)

, Tsui, 1 Berg, 9 Van Water, 7 Virtue, 5 Wall, Waller, Waltham, 1 Wan Chan Tseung, 8 L.Wark, 11 N.West, 8 B.Wilhelmy, 7 Wilkerson, R.Wilson, 8 Wittich, J. M.Wouters, M.Yeh, 2 and Zuber (SNO Collaboration

274

The Southern Great Plains Site: A Climate Observatory in Oklahoma  

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

other facilities throughout the SGP site. The 60-ft meteorological tower rises from a canola field at the SGP central facility in June 2011. The 60-ft meteorological tower rises...

275

Clouds at Arctic Atmospheric Observatories. Part II: Thermodynamic Phase Characteristics  

Science Conference Proceedings (OSTI)

Cloud phase defines many cloud properties and determines the ways in which clouds interact with other aspects of the climate system. The occurrence fraction and characteristics of clouds distinguished by their phase are examined at three Arctic ...

Matthew D. Shupe

2011-03-01T23:59:59.000Z

276

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network (OSTI)

, Mean Time Between Failures and Refrigeration Table 2, Design Chart for 0-ring Face Seal Glands . Table NO. 306 Guidelines for the Design of Cryogenic Systems George Behrens William Campbell Dave Williams Steven White March 1997 #12;3 Table of Contents 1.0 Introduction 2.0 Refrigeration .. 2.1 Refrigeration

Groppi, Christopher

277

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network (OSTI)

.0 Introduction ....................................................1 2.0 Dewar Package Design ................... ......................... 1 2.1 Vacuum Chamber ............................ ................ 2 2.2 Refrigeration ......... .............................. 8 2.5 Dewar Wiring ..... ................................... 9 3.0 Dewar Cardcage Design

Groppi, Christopher

278

Evidence for neutrino oscillations in the Sudbury Neutrino Observatory  

E-Print Network (OSTI)

the neutrinos from a nuclear reactor by the Cl 37 ( , e ? )the Savannah River nuclear reactor in 1956 [9]. Here Reinessources include nuclear reactors and the decays of cosmic-

Marino, Alysia Diane

2004-01-01T23:59:59.000Z

279

Formation flying for a Fresnel lens observatory mission  

E-Print Network (OSTI)

The employment of a large area Phase Fresnel Lens (PFL) in a gamma-ray telescope offers the potential to image astrophysical phenomena with micro-arcsecond angular resolution. In order to assess the feasibility of this concept, two detailed studies have been conducted of formation flying missions in which a Fresnel lens capable of focussing gamma-rays and the associated detector are carried on two spacecraft separated by up to 10$^6$ km. These studies were performed at the NASA Goddard Space Flight Center Integrated Mission Design Center (IMDC) which developed spacecraft, orbital dynamics, and mission profiles. The results of the studies indicated that the missions are challenging but could be accomplished with technologies available currently or in the near term. The findings of the original studies have been updated taking account of recent advances in ion thruster propulsion technology.

Krizmanic, J; Gehrels, N; Krizmanic, John; Skinner, Gerry; Gehrels, Neil

2006-01-01T23:59:59.000Z

280

Formation flying for a Fresnel lens observatory mission  

E-Print Network (OSTI)

The employment of a large area Phase Fresnel Lens (PFL) in a gamma-ray telescope offers the potential to image astrophysical phenomena with micro-arcsecond angular resolution. In order to assess the feasibility of this concept, two detailed studies have been conducted of formation flying missions in which a Fresnel lens capable of focussing gamma-rays and the associated detector are carried on two spacecraft separated by up to 10$^6$ km. These studies were performed at the NASA Goddard Space Flight Center Integrated Mission Design Center (IMDC) which developed spacecraft, orbital dynamics, and mission profiles. The results of the studies indicated that the missions are challenging but could be accomplished with technologies available currently or in the near term. The findings of the original studies have been updated taking account of recent advances in ion thruster propulsion technology.

John Krizmanic; Gerry Skinner; Neil Gehrels

2006-01-03T23:59:59.000Z

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.


281

INDIA-BASED NEUTRINO OBSERVATORY INO/2005/01  

E-Print Network (OSTI)

, Shobha K. Rao, A. K. Ray, L. V. Reddy, B. Satyanarayana, S. Upadhya, Piyush Verma · Variable Energy Institute of Nuclear Physics, Variable Energy Cyclotron Centre, Kolkata INO Spokesperson Naba K Mondal Tata.6.1 Ultra high energy neutrinos and muons . . . . . . . . . . . . . . . . . 46 3.6.2 Kolar Events

Udgaonkar, Jayant B.

282

Extrasolar planet transit photometry at Wallace Astrophysical Observatory  

E-Print Network (OSTI)

Extrasolar planet transit photometry is a relatively new astronomical technique developed over the past decade. Transit photometry is the measurement of a star's brightness as an orbiting planet passes in front of the star ...

Fong, Wen-fai

2008-01-01T23:59:59.000Z

283

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network (OSTI)

can be driven. The difference between rise-times is less than 15 usec. Each multivibrator has its own

Groppi, Christopher

284

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

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

at the Berkeley Lab who helped migrate data from disks at the SNO facility in Sudbury, Canada, to the NERSC facility in Oakland, Calif. "It is important to preserve this data for...

285

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

286

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

287

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

288

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

289

Participating Research Teams  

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

primary responsibility for experiment endstation equipment. They are entitled to a percentage of the beamline's operating time based on the resources the PRT contributes to the...

290

Risk-Based Radionuclide DCGLs for Concrete Slab End States  

Argonne National Laboratory (DOE, NRC, EPA) Adjustment of Relevant Parameters and Exposure Factors Concrete End-State vs. Soil (Preliminary Remediation Goals)

291

Ambient-Pressure X-ray Photoelectron Spectroscopy  

E-Print Network (OSTI)

and Lars-ke Nslund (both SSRL) who presented recent dataa dedicated APXPS endstation at SSRL. The second day of the

Bluhm, Hendrik

2008-01-01T23:59:59.000Z

292

Recent Major Improvements to the ALS Sector 5 Macromolecular Crystallography Beamlines  

E-Print Network (OSTI)

Source is a national user facility operated by Lawrencecontrol environment for users. This facility was immediatelyto our users. Detectors and endstation facilities The

2008-01-01T23:59:59.000Z

293

SLAC Linac Coherent Light Source User Site  

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

Policies and Guidelines Access | Installation of User-Supplied Endstations | Reporting and Acknowledgement | Publications and Press | Proposal Preparation | Proposal Review| Beam...

294

tude de l'effet d'inhibition du gel induit par les sulfates dans les nuages arctiques l'aide des mesures satellitaires de CloudSat et CALIPSO.  

E-Print Network (OSTI)

??Les sulfates issus de la pollution industrielle d'Eurasie et transports travers la basse troposphre arctique durant l'hiver sont souponns d'altrer les proprits des nuages (more)

Grenier, Patrick

2010-01-01T23:59:59.000Z

295

1  

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

Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) Quid Pro Quo Validation T. A. Kovacs, A. Omar, and M. P. McCormick Hampton University Center for Atmospheric...

296

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.

297

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.

298

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.

299

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.

300

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.

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301

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.

302

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.

303

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

E-Print Network (OSTI)

and one underwater connecting the sensors, joined by an armored 1.4 km electro-optic cable. The cable

deYoung, Brad

304

Development of a Coupled Land Surface Hydrologic Model and Evaluation at a Critical Zone Observatory  

Science Conference Proceedings (OSTI)

A fully-coupled land surface hydrologic model, Flux-PIHM, is developed by incorporating a land-surface scheme into the Penn State Integrated Hydrologic Model (PIHM). The land-surface scheme is adapted from the Noah LSM. Because PIHM is capable of ...

Yuning Shi; Kenneth J. Davis; Christopher J. Duffy; Xuan Yu

305

Regional Weather Patterns during Anomalous AirSea Fluxes at the Kuroshio Extension Observatory (KEO)  

Science Conference Proceedings (OSTI)

The weather patterns during periods of anomalous surface fluxes in the Kuroshio recirculation gyre of the western North Pacific are documented. Separate analyses are carried out for the cold season (October March) when the net surface heat flux ...

Nicholas A. Bond; Meghan F. Cronin

2008-04-01T23:59:59.000Z

306

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

E-Print Network (OSTI)

: Professor Gregory W. Sullivan, Chairman/Advisor Professor Jordan A. Goodman Professor Rabindra N. Mohapatra that observes very high energy gamma rays (100 GeV to 100 TeV) using the water-Cerenkov techniqueV candidates. Active galaxies have been observed to be highly variable at TeV energies. To test for episodic

California at Santa Cruz, University of

307

Laboratory, Field, and Modeling Analysis of Solute Transport Behavior at the Shale Hills Critical Zone Observatory.  

E-Print Network (OSTI)

??We collected and analyzed breakthrough curve (BTC) data to identify the parameters controlling transport from a series of undisturbed fully saturated soil cores and a (more)

Kuntz, Brad

2010-01-01T23:59:59.000Z

308

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

E-Print Network (OSTI)

physical units (tcf of natural gas) and further adjust for the fact that coal plants are typically less prices for natural gas for three geographies. Asian coal prices are also included to represent feet. Coal converted into tcf and adjusted for coal plants being 25% less efficient than natural gas

Sheridan, Jennifer

309

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

E-Print Network (OSTI)

a major Wisconsin city to offer a counter-force to the draw from Minneapolis. Commuters tend to have cities in other states whose metropolitan boundaries spread across state lines. Connecticut lies between nuclear submarines, jet engines and helicopters. Hartford was once the insurance capital of America

Wisconsin at Madison, University of

310

Prospects for Localization of Gravitational Wave Transients by the Advanced LIGO and Advanced Virgo Observatories  

E-Print Network (OSTI)

We present a possible observing scenario for the Advanced LIGO and Advanced Virgo gravitational wave detectors over the next decade, with the intention of providing information to the astronomy community to facilitate planning for multi-messenger astronomy with gravitational waves. We determine the expected sensitivity of the network to transient gravitational-wave signals, and study the capability of the network to determine the sky location of the source. For concreteness, we focus primarily on gravitational-wave signals from the inspiral of binary neutron star (BNS) systems, as the source considered likely to be the most common for detection and also promising for multimessenger astronomy. We find that confident detections will likely require at least 2 detectors operating with BNS sensitive ranges of at least 100 Mpc, while ranges approaching 200 Mpc should give at least ~1 BNS detection per year even under pessimistic predictions of signal rates. The ability to localize the source of the detected signals depends on the geographical distribution of the detectors and their relative sensitivity, and can be as large as thousands of square degrees with only 2 sensitive detectors operating. Determining the sky position of a significant fraction of detected signals to areas of 5 sq deg to 20 sq deg will require at least 3 detectors of sensitivity within a factor of ~2 of each other and with a broad frequency bandwidth. Should one of the LIGO detectors be relocated in India as expected, many gravitational-wave signals will be localized to a few square degrees by gravitational-wave observations alone.

LIGO Scientific Collaboration; Virgo Collaboration; J. Aasi; J. Abadie; B. P. Abbott; R. Abbott; T. D. Abbott; M. Abernathy; T. Accadia; F. Acernese; C. Adams; T. Adams; P. Addesso; R. X. Adhikari; C. Affeldt; M. Agathos; O. D. Aguiar; P. Ajith; B. Allen; A. Allocca; E. Amador Ceron; D. Amariutei; S. B. Anderson; W. G. Anderson; K. Arai; M. C. Araya; C. Arceneaux; S. Ast; S. M. Aston; P. Astone; D. Atkinson; P. Aufmuth; C. Aulbert; L. Austin; B. E. Aylott; S. Babak; P. Baker; G. Ballardin; S. Ballmer; Y. Bao; J. C. Barayoga; D. Barker; F. Barone; B. Barr; L. Barsotti; M. Barsuglia; M. A. Barton; I. Bartos; R. Bassiri; M. Bastarrika; A. Basti; J. Batch; J. Bauchrowitz; Th. S. Bauer; M. Bebronne; B. Behnke; M. Bejger; M. G. Beker; A. S. Bell; C. Bell; G. Bergmann; J. M. Berliner; A. Bertolini; J. Betzwieser; N. Beveridge; P. T. Beyersdorf; T. Bhadbade; I. A. Bilenko; G. Billingsley; J. Birch; S. Biscans; M. Bitossi; M. A. Bizouard; E. Black; J. K. Blackburn; L. Blackburn; D. Blair; B. Bland; M. Blom; O. Bock; T. P. Bodiya; C. Bogan; C. Bond; F. Bondu; L. Bonelli; R. Bonnand; R. Bork; M. Born; V. Boschi; S. Bose; L. Bosi; B. Bouhou; J. Bowers; C. Bradaschia; P. R. Brady; V. B. Braginsky; M. Branchesi; J. E. Brau; J. Breyer; T. Briant; D. O. Bridges; A. Brillet; M. Brinkmann; V. Brisson; M. Britzger; A. F. Brooks; D. A. Brown; D. D. Brown; F. Brueckner; K. Buckland; T. Bulik; H. J. Bulten; A. Buonanno; J. Burguet-Castell; D. Buskulic; C. Buy; R. L. Byer; L. Cadonati; G. Cagnoli; E. Calloni; J. B. Camp; P. Campsie; K. Cannon; B. Canuel; J. Cao; C. D. Capano; F. Carbognani; L. Carbone; S. Caride; A. D. Castiglia; S. Caudill; M. Cavagli; F. Cavalier; R. Cavalieri; G. Cella; C. Cepeda; E. Cesarini; T. Chalermsongsak; S. Chao; P. Charlton; E. Chassande-Mottin; X. Chen; Y. Chen; A. Chincarini; A. Chiummo; H. S. Cho; J. Chow; N. Christensen; Q. Chu; S. S. Y. Chua; C. T. Y. Chung; G. Ciani; F. Clara; D. E. Clark; J. A. Clark; F. Cleva; E. Coccia; P. -F. Cohadon; C. N. Colacino; A. Colla; M. Colombini; M. Constancio Jr; A. Conte; D. Cook; T. R. Corbitt; M. Cordier; N. Cornish; A. Corsi; C. A. Costa; M. Coughlin; J. -P. Coulon; S. Countryman; P. Couvares; D. M. Coward; M. Cowart; D. C. Coyne; K. Craig; J. D. E. Creighton; T. D. Creighton; A. Cumming; L. Cunningham; E. Cuoco; K. Dahl; M. Damjanic; S. L. Danilishin; S. D'Antonio; K. Danzmann; V. Dattilo; B. Daudert; H. Daveloza; M. Davier; G. S. Davies; E. J. Daw; T. Dayanga; R. De Rosa; G. Debreczeni; J. Degallaix; W. Del Pozzo; E. Deleeuw; T. Denker; T. Dent; V. Dergachev; R. DeRosa; R. DeSalvo; S. Dhurandhar; L. Di Fiore; A. Di Lieto; I. Di Palma; A. Di Virgilio; M. Daz; A. Dietz; F. Donovan; K. L. Dooley; S. Doravari; M. Drago; S. Drasco; R. W. P. Drever; J. C. Driggers; Z. Du; J. -C. Dumas; S. Dwyer; T. Eberle; M. Edwards; A. Effler; P. Ehrens; S. S. Eikenberry; G. Endrczi; R. Engel; R. Essick; T. Etzel; K. Evans; M. Evans; T. Evans; M. Factourovich; V. Fafone; S. Fairhurst; Q. Fang; B. F. Farr; W. Farr; M. Favata; D. Fazi; H. Fehrmann; D. Feldbaum; I. Ferrante; F. Ferrini; F. Fidecaro; L. S. Finn; I. Fiori; R. P. Fisher; R. Flaminio; S. Foley; E. Forsi; L. A. Forte; N. Fotopoulos; J. -D. Fournier; J. Franc; S. Franco; S. Frasca; F. Frasconi; M. Frede; M. A. Frei; Z. Frei; A. Freise; R. Frey; T. T. Fricke; D. Friedrich; P. Fritschel; V. V. Frolov; M. -K. Fujimoto; P. J. Fulda; M. Fyffe; J. Gair; M. Galimberti; L. Gammaitoni; J. Garcia; F. Garufi; M. E. Gspr; N. Gehrels; G. Gelencser; G. Gemme; E. Genin; A. Gennai; L. . Gergely; S. Ghosh; J. A. Giaime; S. Giampanis; K. D. Giardina; A. Giazotto; S. Gil-Casanova; C. Gill; J. Gleason; E. Goetz; G. Gonzlez; N. Gordon; M. L. Gorodetsky; S. Gossan; S. Goler; R. Gouaty; C. Graef; P. B. Graff; M. Granata; A. Grant; S. Gras; C. Gray; R. J. S. Greenhalgh; A. M. Gretarsson; C. Griffo; H. Grote; K. Grover; S. Grunewald; G. M. Guidi; C. Guido; E. K. Gustafson; R. Gustafson; D. Hammer; G. Hammond; J. Hanks; C. Hanna; J. Hanson; K. Haris; J. Harms; G. M. Harry; I. W. Harry; E. D. Harstad; M. T. Hartman; K. Haughian; K. Hayama; J. Heefner; A. Heidmann; M. C. Heintze; H. Heitmann; P. Hello; G. Hemming; M. A. Hendry; I. S. Heng; A. W. Heptonstall; M. Heurs; M. Hewitson; S. Hild; D. Hoak; K. A. Hodge; K. Holt; M. Holtrop; T. Hong; S. Hooper; J. Hough; E. J. Howell; V. Huang; E. A. Huerta; B. Hughey; S. H. Huttner; M. Huynh; T. Huynh-Dinh; D. R. Ingram; R. Inta; T. Isogai; A. Ivanov; B. R. Iyer; K. Izumi; M. Jacobson; E. James; H. Jang; Y. J. Jang; P. Jaranowski; E. Jesse; W. W. Johnson; D. Jones; D. I. Jones; R. Jones; R. J. G. Jonker; L. Ju; P. Kalmus; V. Kalogera; S. Kandhasamy; G. Kang; J. B. Kanner; M. Kasprzack; R. Kasturi; E. Katsavounidis; W. Katzman; H. Kaufer; K. Kawabe; S. Kawamura; F. Kawazoe; D. Keitel; D. Kelley; W. Kells; D. G. Keppel; A. Khalaidovski; F. Y. Khalili; E. A. Khazanov

2013-04-02T23:59:59.000Z

311

Nuclear Stellar Populations in the Infrared Space Observatory Atlas of Bright Spiral Galaxies  

E-Print Network (OSTI)

To understand the nuclear stellar populations and star formation histories of the nuclei of spiral galaxies, we have obtained K-band nuclear spectra for 41 galaxies and H-band spectra for 20 galaxies in the ISO Atlas of Bright Spiral Galaxies. In the vast majority of the subsample (80%), the near-infrared spectra suggest that evolved red stars completely dominate the nuclear stellar populations and that hot young stars are virtually non-existent. The signatures of recent star formation activity are only found in 20% of the subsample, even though older red stars still dominate the stellar populations in these galaxies. Given the dominance of evolved stars in most galaxy nuclei and the nature of the emission lines in the galaxies where they were detected, we suggest that nuclear star formation proceeds in the form of instantaneous bursts. The stars produced by these bursts comprise only ~2% of the total nuclear stellar mass in these galaxies, but we demonstrate how the nuclear stellar populations of normal spiral galaxies can be built up through a series of these bursts. The bursts were detected only in Sbc galaxies and later, and both bars and interactions appeared to be sufficient but not necessary triggers for the nuclear star formation activity. The vast majority of galaxies with nuclear star formation were classified as HII galaxies. With one exception, LINERs and transition objects were dominated by older red stars, which suggested that star formation was not responsible for generating these galaxies' optical line emission.

George J. Bendo; Robert D. Joseph

2004-03-04T23:59:59.000Z

312

The Taiwanese-American Occultation Survey: The Multi-Telescope Robotic Observatory  

E-Print Network (OSTI)

The Taiwanese-American Occultation Survey (TAOS) operates four telescopes to search for occultations of stars by Kuiper Belt Objects. This paper provides a detailed description of the TAOS multi-telescope system.

Lehner, M J; Wang, J -H; Marshall, S L; Schwamb, M E; Zhang, Z -W; Bianco, F B; Giammarco, J; Porrata, R; Alcock, C; Axelrod, T; Byun, Y -I; Chen, W P; Cook, K H; Dav, R; King, S -K; Lee, T; Lin, H -C; Wang, S -Y

2008-01-01T23:59:59.000Z

313

The Taiwanese-American Occultation Survey: The Multi-Telescope Robotic Observatory  

E-Print Network (OSTI)

The Taiwanese-American Occultation Survey (TAOS) operates four fully automatic telescopes to search for occultations of stars by Kuiper Belt Objects. It is a versatile facility that is also useful for the study of initial optical GRB afterglows. This paper provides a detailed description of the TAOS multi-telescope system, control software, and high-speed imaging.

M. J. Lehner; C. -Y. Wen; J. -H. Wang; S. L. Marshall; M. E. Schwamb; Z. -W. Zhang; F. B. Bianco; J. Giammarco; R. Porrata; C. Alcock; T. Axelrod; Y. -I. Byun; W. P. Chen; K. H. Cook; R. Dave; S. -K. King; T. Lee; H. -C. Lin; S. -Y. Wang

2008-02-04T23:59:59.000Z

314

Brownian force noise from molecular collisions and the sensitivity of advanced gravitational wave observatories  

E-Print Network (OSTI)

We present an analysis of Brownian force noise from residual gas damping of reference test masses as a fundamental sensitivity limit in small force experiments. The resulting acceleration noise increases significantly when ...

Evans, Matthew J.

315

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

E-Print Network (OSTI)

), and Polillo and Guillen (2005) for the remaining years.11 Finally, since we are interested in the behavior

Sheridan, Jennifer

316

Multilayer Scintillator Responses for Mo Observatory of Neutrino Experiment Studied Using a Prototype Detector MOON-1  

E-Print Network (OSTI)

, Toyonaka, Osaka 560-0043 10 Hiroshima University, Higashi Hiroshima, Hiroshima 739-8527 11 VNIIEF, 607188

Engel, Jonathan

317

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

E-Print Network (OSTI)

.Bystatisticalanalysis,weidentifiedseveralpotential sources of differences between EIA and eGRID estimates for individual plants. Estimates that are based partly or entirely on monitoring of stack gases (reported by eGRID only) differed of coal, oil, gas, geothermal, and municipal solid waste). The EPA data set, eGRID2006 version 2

Sheridan, Jennifer

318

32ND INTERNATIONAL COSMIC RAY CONFERENCE, BEIJING 2011 The HEAT Telescopes of the Pierre Auger Observatory  

E-Print Network (OSTI)

tanks on a 750 m grid close to the HEAT site the energy range of high quality hybrid air shower32ND INTERNATIONAL COSMIC RAY CONFERENCE, BEIJING 2011 The HEAT Telescopes of the Pierre Auger. A surface array of 1660 water Cherenkov detectors on a 1500 m triangular grid covers an area of 3000 km2

Hörandel, Jörg R.

319

Investigations of the cascade of Langmuir wave turbulence over HAARP Observatory in Gakona, Alaska  

E-Print Network (OSTI)

This thesis investigates the cascade lines from Langmuir wave turbulence as a result of Parametric Decay Instability (PDI) in the ionosphere. This effect is studied using a high-frequency (HF) heater located at the NSF/DoD ...

Burton, Laura M

2007-01-01T23:59:59.000Z

320

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

E-Print Network (OSTI)

is quantified using macro estimates and is then related to the decisions that potential innovators face. 5 to build new coal plants, e.g. with gasification, which are amenable to sequestration later, never mind macro-economic estimates are used to estimate the extent to which these incentives are lacking. 5

Sheridan, Jennifer

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

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

E-Print Network (OSTI)

at the federal level. By and large, these attempts such as Project XCEL have had very limited success

Sheridan, Jennifer

322

MilagroA TeV Observatory for Gamma Ray Bursts  

E-Print Network (OSTI)

The Biggest Bangs The Mystery of Gamma-Ray Bursts, The Most Violent Explosions in The Universe J. I. Did a Gamma-Ray Burst Kill the Dinosaurs? Will a Burst Kill Us? #15; Glossary #15; Sources #15; Index. On January 23, 1999, one of these four cameras recorded visible light from a gamma-ray burst

California at Santa Cruz, University of

323

Abstract An Investigation of Matter Enhanced Neutrino Oscillation with the Sudbury Neutrino Observatory  

E-Print Network (OSTI)

and have found that it is complete and satisfactory in all respects, and that any and all revisions required by the final examining committee have been made.

Miles Walter; Eldon Smith; Miles Walter; Eldon Smith; Steve Elliott; Peter Doe; Steve Elliott; Hamish Robertson; Miles Walter Eldon Smith

2002-01-01T23:59:59.000Z

324

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

E-Print Network (OSTI)

. G. Van de Water,9,13 B. A. VanDevender,19 C. J. Virtue,6 D. Waller,4 C. E. Waltham,2 H. Wan Chan. Wouters,9 A. Wright,14 M. Yeh,3 F. Zhang,4 and K. Zuber12,s (SNO Collaboration) 1 Department of Physics

325

Electron antineutrino search at the Sudbury Neutrino Observatory B. Aharmim,5  

E-Print Network (OSTI)

,10 G. Tesic´,3 M. Thomson,10 T. Tsui,1 R. Van Berg,9 R. G. Van de Water,7 C. J. Virtue,5 B. L. Wall.Wilkerson,13 J. R.Wilson,8 P.Wittich,9 J. M.Wouters,7 M.Yeh,2 and K. Zuber8 (SNO Collaboration) 1 Department

326

Direct Evidence for Neutrino Flavor Transformation from Neutral-Current Interactions in the Sudbury Neutrino Observatory  

E-Print Network (OSTI)

, 11 P.M. Thornewell, 11 P.T. Trent, 11 Y.I. Tserkovnyak, 2 R. Van Berg, 12 R.G. Van de Water, 9, 12 C, 17, 9 J.R. Wilson, 11 P. Wittich, 12 J.M. Wouters, 9 and M. Yeh 3 (SNO Collaboration) 1 Atomic Energy

327

A Search for TeV Gamma-Ray Burst Emission with the Milagro Observatory  

E-Print Network (OSTI)

The Milagro telescope monitors the northern sky for 100 GeV - 100 TeV transient emission through continuous very high energy wide-field observations. The large effective area and low energy threshold of Milagro allow it to detect very high energy gamma-ray burst emission with much higher sensitivity than previous instruments, and a fluence sensitivity at TeV energies comparable to dedicated gamma-ray burst satellites at keV-MeV energies. Observation of gamma-ray burst emission at TeV energies could place important constraints on gamma-ray burst progenitor and emission models. This study details the development of a weighted analysis technique; the implementation of this technique to perform a real time search for TeV transients of 40 seconds to 3 hours duration in the Milagro data; and the results from more than one year of observation. Between May 2nd, 2001, and May 22nd, 2002, no TeV transients of 40 seconds to 3 hours duration were observed. Upper limits on both observed and emitted high energy gamma-ray burst emission are presented.

Miguel F. Morales

2003-08-06T23:59:59.000Z

328

Optical Sky Brightness at Cerro Tololo Inter-American Observatory from 1992 to 2006  

E-Print Network (OSTI)

We present optical UBVRI sky brightness measures from 1992 through 2006. The data are based on CCD imagery obtained with the CTIO 0.9-m, 1.3-m, and 1.5-m telescopes. The B- and V-band data are in reasonable agreement with measurements previously made at Mauna Kea, though on the basis of a small number of images per year there are discrepancies for the years 1992 through 1994. Our CCD-based data are not significantly different than values obtained at Cerro Paranal. We find that the yearly averages of V-band sky brightness are best correlated with the 10.7-cm solar flux taken 5 days prior to the sky brightness measures. This implies an average speed of 350 km/sec for the solar wind. While we can measure an enhancement of the night sky levels over La Serena 10 degrees above the horizon, at elevation angles above 45 degrees we find no evidence that the night sky brightness at Cerro Tololo is affected by artificial light of nearby towns and cities.

Krisciunas, Kevin; Sanhueza, Pedro; Schwarz, Hugo E; Semler, Dylan R; Suntzeff, Nicholas B; Vera, Sergio

2007-01-01T23:59:59.000Z

329

What NEON Is The National Ecological Observatory Network (NEON) is a continental-scale  

E-Print Network (OSTI)

at the Harvard Forest, Petersham, MA 2. Mid-Atlantic site (to be determined) 3. Southeast site based

Patterson, Bruce D.

330

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

331

NATIONAL Puano ASTRONOMY OBSERVATORY PosT OFFICE Box 2 REPORT  

E-Print Network (OSTI)

of large steerable antennas") I suggested an off- axis part of a parabolic mirror, sitting flat not need any additional structure between feed package and feed tracks, but then the cylindrical trough becomes very high. If we take a large value for H, as shown in Fig.4, the trough becomes much o

Groppi, Christopher

332

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

E-Print Network (OSTI)

. Report NUREG/CR-5988, PNL-8480, U.S. Nuclear Regulatory Commission, Washington, DC, USA; 141 pp. 29. Van of the U.S. Salinity Laboratory at Riverside, California, which is a Microsoft Windows based modeling for the determination of windows of opportunities for mine detection. The simulations presented here dealt

Sheridan, Jennifer

333

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

E-Print Network (OSTI)

possible regimes. In the base case, which we call "backup generation", we assume that natural gas power plants are required as backup generation to ensure grid reliability. As PV's share of electricity

Sheridan, Jennifer

334

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

E-Print Network (OSTI)

natural gas power plants; ad- vances in ball bearings and tires for bicycles enabled development of auto

Sheridan, Jennifer

335

Prospects for Localization of Gravitational Wave Transients by the Advanced LIGO and Advanced Virgo Observatories  

E-Print Network (OSTI)

We present a possible observing scenario for the Advanced LIGO and Advanced Virgo gravitational wave detectors over the next decade, with the intention of providing information to the astronomy community to facilitate planning for multi-messenger astronomy with gravitational waves. We determine the expected sensitivity of the network to transient gravitational-wave signals, and study the capability of the network to determine the sky location of the source. For concreteness, we focus primarily on gravitational-wave signals from the inspiral of binary neutron star (BNS) systems, as the source considered likely to be the most common for detection and also promising for multimessenger astronomy. We find that confident detections will likely require at least 2 detectors operating with BNS sensitive ranges of at least 100 Mpc, while ranges approaching 200 Mpc should give at least ~1 BNS detection per year even under pessimistic predictions of signal rates. The ability to localize the source of the detected signals...

Aasi, J; Abbott, B P; Abbott, R; Abbott, T D; Abernathy, M; Accadia, T; Acernese, F; Adams, C; Adams, T; Addesso, P; Adhikari, R X; Affeldt, C; Agathos, M; Aguiar, O D; Ajith, P; Allen, B; Allocca, A; Ceron, E Amador; Amariutei, D; Anderson, S B; Anderson, W G; Arai, K; Araya, M C; Arceneaux, C; Ast, S; Aston, S M; Astone, P; Atkinson, D; Aufmuth, P; Aulbert, C; Austin, L; Aylott, B E; Babak, S; Baker, P; Ballardin, G; Ballmer, S; Bao, Y; Barayoga, J C; Barker, D; Barone, F; Barr, B; Barsotti, L; Barsuglia, M; Barton, M A; Bartos, I; Bassiri, R; Bastarrika, M; Basti, A; Batch, J; Bauchrowitz, J; Bauer, Th S; Bebronne, M; Behnke, B; Bejger, M; Beker, M G; Bell, A S; Bell, C; Bergmann, G; Berliner, J M; Bertolini, A; Betzwieser, J; Beveridge, N; Beyersdorf, P T; Bhadbade, T; Bilenko, I A; Billingsley, G; Birch, J; Biscans, S; Bitossi, M; Bizouard, M A; Black, E; Blackburn, J K; Blackburn, L; Blair, D; Bland, B; Blom, M; Bock, O; Bodiya, T P; Bogan, C; Bond, C; Bondu, F; Bonelli, L; Bonnand, R; Bork, R; Born, M; Boschi, V; Bose, S; Bosi, L; Bouhou, B; Bowers, J; Bradaschia, C; Brady, P R; Braginsky, V B; Branchesi, M; Brau, J E; Breyer, J; Briant, T; Bridges, D O; Brillet, A; Brinkmann, M; Brisson, V; Britzger, M; Brooks, A F; Brown, D A; Brown, D D; Brueckner, F; Buckland, K; Bulik, T; Bulten, H J; Buonanno, A; Burguet-Castell, J; Buskulic, D; Buy, C; Byer, R L; Cadonati, L; Cagnoli, G; Calloni, E; Camp, J B; Campsie, P; Cannon, K; Canuel, B; Cao, J; Capano, C D; Carbognani, F; Carbone, L; Caride, S; Castiglia, A D; Caudill, S; Cavagli, M; Cavalier, F; Cavalieri, R; Cella, G; Cepeda, C; Cesarini, E; Chalermsongsak, T; Chao, S; Charlton, P; Chassande-Mottin, E; Chen, X; Chen, Y; Chincarini, A; Chiummo, A; Cho, H S; Chow, J; Christensen, N; Chu, Q; Chua, S S Y; Chung, C T Y; Ciani, G; Clara, F; Clark, D E; Clark, J A; Cleva, F; Coccia, E; Cohadon, P -F; Colacino, C N; Colla, A; Colombini, M; Constancio, M; Conte, A; Cook, D; Corbitt, T R; Cordier, M; Cornish, N; Corsi, A; Costa, C A; Coughlin, M; Coulon, J -P; Countryman, S; Couvares, P; Coward, D M; Cowart, M; Coyne, D C; Craig, K; Creighton, J D E; Creighton, T D; Cumming, A; Cunningham, L; Cuoco, E; Dahl, K; Damjanic, M; Danilishin, S L; D'Antonio, S; Danzmann, K; Dattilo, V; Daudert, B; Daveloza, H; Davier, M; Davies, G S; Daw, E J; Dayanga, T; De Rosa, R; Debreczeni, G; Degallaix, J; Del Pozzo, W; Deleeuw, E; Denker, T; Dent, T; Dergachev, V; DeRosa, R; DeSalvo, R; Dhurandhar, S; Di Fiore, L; Di Lieto, A; Di Palma, I; Di Virgilio, A; Daz, M; Dietz, A; Donovan, F; Dooley, K L; Doravari, S; Drago, M; Drasco, S; Drever, R W P; Driggers, J C; Du, Z; Dumas, J -C; Dwyer, S; Eberle, T; Edwards, M; Effler, A; Ehrens, P; Eikenberry, S S; Endrczi, G; Engel, R; Essick, R; Etzel, T; Evans, K; Evans, M; Evans, T; Factourovich, M; Fafone, V; Fairhurst, S; Fang, Q; Farr, B F; Farr, W; Favata, M; Fazi, D; Fehrmann, H; Feldbaum, D; Ferrante, I; Ferrini, F; Fidecaro, F; Finn, L S; Fiori, I; Fisher, R P; Flaminio, R; Foley, S; Forsi, E; Forte, L A; Fotopoulos, N; Fournier, J -D; Franc, J; Franco, S; Frasca, S; Frasconi, F; Frede, M; Frei, M A; Frei, Z; Freise, A; Frey, R; Fricke, T T; Friedrich, D; Fritschel, P; Frolov, V V; Fujimoto, M -K; Fulda, P J; Fyffe, M; Gair, J; Galimberti, M; Gammaitoni, L; Garcia, J; Garufi, F; Gspr, M E; Gehrels, N; Gelencser, G; Gemme, G; Genin, E; Gennai, A; Gergely, L ; Ghosh, S; Giaime, J A; Giampanis, S; Giardina, K D; Giazotto, A; Gil-Casanova, S; Gill, C; Gleason, J; Goetz, E; Gonzlez, G; Gordon, N; Gorodetsky, M L; Gossan, S; Goler, S; Gouaty, R; Graef, C; Graff, P B; Granata, M; Grant, A; Gras, S; Gray, C; Greenhalgh, R J S; Gretarsson, A M; Griffo, C; Grote, H; Grover, K; Grunewald, S; Guidi, G M; Guido, C; Gustafson, E K; Gustafson, R; Hammer, D; Hammond, G; Hanks, J; Hanna, C; Hanson, J; Haris, K; Harms, J; Harry, G M; Harry, I W; Harstad, E D; Hartman, M T; Haughian, K; Hayama, K; Heefner, J; Heidmann, A; Heintze, M C; Heitmann, H; Hello, P; Hemming, G; Hendry, M A; Heng, I S; Heptonstall, A W; Heurs, M; Hewitson, M; Hild, S; Hoak, D; Hodge, K A; Holt, K; Holtrop, M; Hong, T; Hooper, S; Hough, J; Howell, E J; Huang, V; Huerta, E A; Hughey, B; Huttner, S H; Huynh, M; Huynh-Dinh, T; Ingram, D R; Inta, R; Isogai, T; Ivanov, A; Iyer, B R; Izumi, K; Jacobson, M; James, E; Jang, H; Jang, Y J; Jaranowski, P; Jesse, E; Johnson, W W; Jones, D; Jones, D I; Jones, R; Jonker, R J G; Ju, L; Kalmus, P; Kalogera, V; Kandhasamy, S; Kang, G; Kanner, J B; Kasprzack, M; Kasturi, R; Katsavounidis, E; Katzman, W; Kaufer, H; Kawabe, K; Kawamura, S; Kawazoe, F; Keitel, D; Kelley, D; Kells, W; Keppel, D G; Khalaidovski, A; Khalili, F Y; Khazanov, E A; Kim, B K; Kim, C; Kim, K; Kim, N; Kim, Y M; King, P J; Kinzel, D L; Kissel, J S; Klimenko, S; Kline, J; Kokeyama, K; Kondrashov, V; Koranda, S; Korth, W Z; Kowalska, I; Kozak, D; Kozameh, C; Kremin, A

2013-01-01T23:59:59.000Z

336

LABORATORY FOR ATMOSPHERIC ACOUSTICS SCRIPPS INSTITUTION OF OCEANOGRAPHY INSTITUTE OF GEOPHYSICS & PLANETARY PHYSICS Pion Flat Observatory  

E-Print Network (OSTI)

original scientific research and engineering design at the forefront of their particular area. Expertise in problem-solving methodologies, including engineering design and structured decision

Constable, Steve

337

Application of Lidar Data to Assist Airmass Discrimination at the Whistler Mountaintop Observatory  

Science Conference Proceedings (OSTI)

A ground-based lidar system that has been deployed in Whistler, British Columbia, Canada, since the spring of 2010 provides a means of evaluating vertical aerosol structure in a mountainous environment. This information is used to help to ...

John P. Gallagher; Ian G. McKendry; Paul W. Cottle; Anne Marie Macdonald; W. Richard Leaitch; Kevin Strawbridge

2012-10-01T23:59:59.000Z

338

EUV multilayer coatings for the Atmospheric Imaging Assembly instrument aboard the Solar Dynamics Observatory  

Science Conference Proceedings (OSTI)

Multilayer coatings for the 7 EUV channels of the AIA have been developed and completed successfully on all AIA flight mirrors. Mo/Si coatings (131, 171, 193.5, 211 {angstrom}) were deposited at Lawrence Livermore National Laboratory (LLNL). Mg/SiC (304, 335 {angstrom}) and Mo/Y (94 {angstrom}) coatings were deposited at Columbia University. EUV reflectance of the 131/335 {angstrom}, 171 {angstrom}, 193.5/211 {angstrom} primary and secondary flight mirrors and the 94/304 {angstrom} secondary flight mirror was measured at beamline 6.3.2. of the Advanced Light Source (ALS) at LBNL. EUV reflectance of the 94/304 {angstrom} primary and secondary flight mirrors was measured at beamline X24C of the National Synchrotron Light Source (NSLS) at Brookhaven National Lab. Preliminary EUV reflectance measurements of the 94, 304 and 335 {angstrom} coatings were performed with a laser plasma source reflectometer located at Columbia University. Prior to multilayer coating, Atomic Force Microscopy (AFM) characterization and cleaning of all flight substrates was performed at LLNL.

Soufli, R; Windt, D L; Robinson, J C; Baker, S L; Spiller, E; Dollar, F J; Aquila, A L; Gullikson, E M; Kjonrattanawanich, B; Seely, J F; Golub, L

2006-02-09T23:59:59.000Z

339

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)

340

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)

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

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)

342

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)

343

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)

344

Comparative risk analysis for the Rocky Flats Plant integrated project planning  

Science Conference Proceedings (OSTI)

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

345

A Cumulus Parameterization Based on the Generalized Convective Available Potential Energy  

Science Conference Proceedings (OSTI)

This paper reports tests of a cumulus parameterization in which the reference state associated with the generalized convective available potential energy (GCAPE) is chosen as the end-state of the convective adjustment. The GCAPE is defined as the ...

Junyi Wang; David A. Randall

1996-03-01T23:59:59.000Z

346

Beamline 12.0.2  

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

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...

347

Beamline 12.0.2  

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

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...

348

--No Title--  

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

The proposed decommissioning end-state for this project is to remove and demolish portions of the switchgear, (cubicles 1&2), from the 183-2C substation and relocate cubicle 3....

349

--No Title--  

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

fuel oil tank to the west of Building 710-B with concretegrout. The proposed decommissioning end-state for the building is demolition down to the slab, the storage container...

350

Beamline 11.0.1  

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

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...

351

High Performance Abrasion-Resistant Materials: Lessons from Nature  

E-Print Network (OSTI)

endstation X13B. The NSLS is supported under USDOE ContractSynchrotron Light Source (NSLS) in Brookhaven NationalX13B, Dr. Vesna Stanic of the NSLS in BNL for her help in

Wang, Qianqian

2012-01-01T23:59:59.000Z

352

Assessment of the Quality of MODIS Cloud Products from Radiance Simulations  

Science Conference Proceedings (OSTI)

Observations made by the Moderate Resolution Imaging Spectroradiometer (MODIS), the Atmospheric Infrared Sounder (AIRS), the CloudAerosol Lidar and Infrared Pathfinder Satellite Observation (CALIPSO), and CloudSat are synergistically used to ...

Seung-Hee Ham; Byung-Ju Sohn; Ping Yang; Bryan A. Baum

2009-08-01T23:59:59.000Z

353

Incorporating Ice Crystal Scattering Databases in the Simulation of Millimeter-Wavelength Radar Reflectivity  

Science Conference Proceedings (OSTI)

The Canadian CloudSat/CloudAerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) Validation Project (C3VP) was designed to acquire aircraft, surface, and satellite observations of particle size distributions during cold season ...

Andrew L. Molthan; Walter A. Petersen

2011-03-01T23:59:59.000Z

354

Annual, Interannual, and Intraseasonal Variability of Tropical Tropopause Transition Layer Cirrus  

Science Conference Proceedings (OSTI)

Cloud fields based on the first three years of data from the CloudAerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) mission are used to investigate the relationship between cirrus within the tropical tropopause transition ...

Katrina S. Virts; John M. Wallace

2010-10-01T23:59:59.000Z

355

Phenomenological Description of Tropical Clouds Using CloudSat Cloud Classification  

Science Conference Proceedings (OSTI)

Two years of tropical oceanic cloud observations are analyzed using the operational CloudSat cloud classification product and CloudAerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) lidar. Relationships are examined between ...

Ali Behrangi; Terry Kubar; Bjorn Lambrigtsen

2012-10-01T23:59:59.000Z

356

Boundary Layer and Cloud Structure Controls on Tropical Low Cloud Cover Using A-Train Satellite Data and ECMWF Analyses  

Science Conference Proceedings (OSTI)

The CloudAerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO), CloudSat radar, and the Moderate Resolution Imaging Spectroradiometer (MODIS) cloud data on the A-Train constellation complemented with the European Centre for ...

Terence L. Kubar; Duane E. Waliser; J-L. Li

2011-01-01T23:59:59.000Z

357

Testing IWC Retrieval Methods Using Radar and Ancillary Measurements with In Situ Data  

Science Conference Proceedings (OSTI)

Vertical profiles of ice water content (IWC) can now be derived globally from spaceborne cloud satellite radar (CloudSat) data. Integrating these data with Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation (CALIPSO) data may ...

Andrew J. Heymsfield; Alain Protat; Dominique Bouniol; Richard T. Austin; Robin J. Hogan; Julien Delano; Hajime Okamoto; Kaori Sato; Gerd-Jan van Zadelhoff; David P. Donovan; Zhien Wang

2008-01-01T23:59:59.000Z

358

Comparisons of Single- and Double-Moment Microphysics Schemes in the Simulation of a Synoptic-Scale Snowfall Event  

Science Conference Proceedings (OSTI)

The Canadian CloudSat/CloudAerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) Validation Project (C3VP) provided aircraft, surface, and remotely sensed observations of cloud and precipitation characteristics to support ...

Andrew L. Molthan; Brian A. Colle

2012-09-01T23:59:59.000Z

359

Meteorological Education and Training Using A-Train Profilers  

Science Conference Proceedings (OSTI)

NASA A-Train vertical profilers provide detailed observations of atmospheric features not seen in traditional imagery from other weather satellite data. CloudSat and CloudAerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) profiles ...

Thomas F. Lee; Richard L. Bankert; Cristian Mitrescu

2012-05-01T23:59:59.000Z

360

A Multisensor Perspective on the Radiative Impacts of Clouds and Aerosols  

Science Conference Proceedings (OSTI)

The launch of CloudSat and CloudAerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) in 2006 provided the first opportunity to incorporate information about the vertical distribution of cloud and aerosols directly into global ...

David S. Henderson; Tristan LEcuyer; Graeme Stephens; Phil Partain; Miho Sekiguchi

2013-04-01T23:59:59.000Z

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.


361

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

362

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

E-Print Network (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 1 PeV were observed, as reported previously. In this work, we investigate whether these events could originate from cosmogenic neutrinos produced in the interactions of ultra-high energy cosmic-rays with ambient photons while propagating through intergalactic space. Exploiting IceCube's large exposure for extremely high energy neutrinos and the lack of observed events above 100 PeV, we can rule out the corresponding models at more than 90% confidence level. The model independent quasi-differential 90% CL upper limit, which amounts to $E^2 \\phi_{\

IceCube Collaboration; M. G. Aartsen; R. Abbasi; M. Ackermann; J. Adams; J. A. Aguilar; M. Ahlers; D. Altmann; C. Arguelles; J. Auffenberg; X. Bai; M. Baker; S. W. Barwick; V. Baum; R. Bay; J. J. Beatty; J. Becker Tjus; K. -H. Becker; S. BenZvi; P. Berghaus; D. Berley; E. Bernardini; A. Bernhard; D. Z. Besson; G. Binder; D. Bindig; M. Bissok; E. Blaufuss; J. Blumenthal; D. J. Boersma; C. Bohm; D. Bose; S. Bser; O. Botner; L. Brayeur; H. -P. Bretz; A. M. Brown; R. Bruijn; J. Casey; M. Casier; D. Chirkin; A. Christov; B. Christy; K. Clark; F. Clevermann; S. Coenders; S. Cohen; D. F. Cowen; A. H. Cruz Silva; M. Danninger; J. Daughhetee; J. C. Davis; M. Day; C. De Clercq; S. De Ridder; P. Desiati; K. D. de Vries; M. de With; T. DeYoung; J. C. Daz-Vlez; M. Dunkman; R. Eagan; B. Eberhardt; J. Eisch; S. Euler; P. A. Evenson; O. Fadiran; A. R. Fazely; A. Fedynitch; J. Feintzeig; T. Feusels; K. Filimonov; C. Finley; T. Fischer-Wasels; S. Flis; A. Franckowiak; K. Frantzen; T. Fuchs; T. K. Gaisser; J. Gallagher; L. Gerhardt; L. Gladstone; T. Glsenkamp; A. Goldschmidt; G. Golup; J. G. Gonzalez; J. A. Goodman; D. Gra; D. T. Grandmont; D. Grant; P. Gretskov; J. C. Groh; A. Gro; C. Ha; A. Haj Ismail; P. Hallen; A. Hallgren; F. Halzen; K. Hanson; D. Heereman; D. Heinen; K. Helbing; R. Hellauer; S. Hickford; G. C. Hill; K. D. Hoffman; R. Hoffmann; A. Homeier; K. Hoshina; W. Huelsnitz; P. O. Hulth; K. Hultqvist; S. Hussain; A. Ishihara; E. Jacobi; J. Jacobsen; K. Jagielski; G. S. Japaridze; K. Jero; O. Jlelati; B. Kaminsky; A. Kappes; T. Karg; A. Karle; M. Kauer; J. L. Kelley; J. Kiryluk; J. Kls; S. R. Klein; J. -H. Khne; G. Kohnen; H. Kolanoski; L. Kpke; C. Kopper; S. Kopper; D. J. Koskinen; M. Kowalski; M. Krasberg; A. Kriesten; K. Krings; G. Kroll; J. Kunnen; N. Kurahashi; T. Kuwabara; M. Labare; H. Landsman; M. J. Larson; M. Lesiak-Bzdak; M. Leuermann; J. Leute; J. Lnemann; O. Macas; J. Madsen; G. Maggi; R. Maruyama; K. Mase; H. S. Matis; F. McNally; K. Meagher; M. Merck; T. Meures; S. Miarecki; E. Middell; N. Milke; J. Miller; L. Mohrmann; T. Montaruli; R. Morse; R. Nahnhauer; U. Naumann; H. Niederhausen; S. C. Nowicki; D. R. Nygren; A. Obertacke; S. Odrowski; A. Olivas; A. Omairat; A. O'Murchadha; L. Paul; J. A. Pepper; C. Prez de los Heros; C. Pfendner; D. Pieloth; D. Pieloth; E. Pinat; J. Posselt; P. B. Price; G. T. Przybylski; L. Rdel; M. Rameez; K. Rawlins; P. Redl; R. Reimann; E. Resconi; W. Rhode; M. Ribordy; M. Richman; B. Riedel; J. P. Rodrigues; C. Rott; T. Ruhe; B. Ruzybayev; D. Ryckbosch; S. M. Saba; H. -G. Sander; M. Santander; S. Sarkar; K. Schatto; F. Scheriau; T. Schmidt; M. Schmitz; S. Schoenen; S. Schneberg; A. Schnwald; A. Schukraft; L. Schulte; O. Schulz; D. Seckel; Y. Sestayo; S. Seunarine; R. Shanidze; C. Sheremata; M. W. E. Smith; D. Soldin; G. M. Spiczak; C. Spiering; M. Stamatikos; T. Stanev; N. A. Stanisha; A. Stasik; T. Stezelberger; R. G. Stokstad; A. Stl; E. A. Strahler; R. Strm; G. W. Sullivan; H. Taavola; I. Taboada; A. Tamburro; A. Tepe; S. Ter-Antonyan; G. Tei?; S. Tilav; P. A. Toale; M. N. Tobin; S. Toscano; E. Unger; M. Usner; S. Vallecorsa; N. van Eijndhoven; A. Van Overloop; J. van Santen; M. Vehring; M. Voge; M. Vraeghe; C. Walck; T. Waldenmaier; M. Wallraff; Ch. Weaver; M. Wellons; C. Wendt; S. Westerhoff; N. Whitehorn; K. Wiebe; C. H. Wiebusch; D. R. Williams; H. Wissing; M. Wolf; T. R. Wood; K. Woschnagg; D. L. Xu; X. W. Xu; J. P. Yanez; G. Yodh; S. Yoshida; P. Zarzhitsky; J. Ziemann; S. Zierke; M. Zoll

2013-10-21T23:59:59.000Z

363

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

E-Print Network (OSTI)

We then remove the brass STS1 mass from the seismometercorner-cube is epoxyed to a brass shim. The corner-cube andmass (Figure 3.2, note the brass shim directly below the

Otero, Jos D.

2009-01-01T23:59:59.000Z

364

Analysis of 2-axis pencil beam sonar microbathymetric measurements of mine burial at the Martha's Vineyard Coastal Observatory  

E-Print Network (OSTI)

The changing state of warfare has driven the US Navy's area of operations closer to shore into littoral coastal waters. Mine Warfare has been proven as an extremely effective means of battlespace control in these waters. ...

Gotowka, Brendan Reed

2005-01-01T23:59:59.000Z

365

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

DOE Green Energy (OSTI)

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

366

The Great Observatories Origins Deep Survey - VLT/FORS2 Spectroscopy in the GOODS-South Field  

E-Print Network (OSTI)

We present the first results of the ESO/GOODS program of spectroscopy of faint galaxies in the Chandra Deep Field South (CDF-S). 399 spectra of 303 unique targets have been obtained in service mode with the FORS2 spectrograph at the ESO/VLT, providing 234 redshift determinations (the median of the redshift distribution is at 1.04). The typical redshift uncertainty is estimated to be sig(z) ~ 0.001. Galaxies have been color selected in a way that the resulting redshift distribution typically spans from z=0.5 to 2. The reduced spectra and the derived redshifts are released to the community through the ESO web page http://www.eso.org/science/goods/ Large scale structure is clearly detected at z ~ 0.67, 0.73, 1.10 and 1.61. Three Lyman-break galaxies have also been included as targets and are confirmed to have redshifts z=4.800, 4.882 and 5.828. In a few cases, we observe clear [OII]3727 rotation curves, even at the relatively low resolution (R = 860) of the present observations. Assuming that the observed velocity structure is due to dynamically-relaxed rotation, this is an indication of large galactic masses (few times 10^(11) solar masses) at z ~ 1.

E. Vanzella; S. Cristiani; M. Dickinson; H. Kuntschner; L. A. Moustakas; M. Nonino; P. Rosati; D. Stern; C. Cesarsky; S. Ettori; H. C. Ferguson; R. A. E. Fosbury; M. Giavalisco; J. Haase; A. Renzini; A. Rettura; P. Serra

2004-06-25T23:59:59.000Z

367

The Great Observatories Origins Deep Survey. VLT/FORS2 Spectroscopy in the GOODS-South Field: Part III  

E-Print Network (OSTI)

Aims. We present the full data set of the spectroscopic campaign of the ESO/GOODS program in the GOODS-South field, obtained with the FORS2 spectrograph at the ESO/VLT. Method. Objects were selected as candidates for VLT/FORS2 observations primarily based on the expectation that the detection and measurement of their spectral features would benefit from the high throughput and spectral resolution of FORS2. The reliability of the redshift estimates is assessed using the redshift-magnitude and color-redshift diagrams, and comparing the results with public data. Results. Including the third part of the spectroscopic campaign (12 masks) to the previous work (26 masks, Vanzella et al. 2005, 2006), 1715 spectra of 1225 individual targets have been analyzed. The actual spectroscopic catalog provides 887 redshift determinations. The typical redshift uncertainty is estimated to be sigma(z) ~ 0.001. Galaxies have been selected adopting different color criteria and using photometric redshifts. The resulting redshift distribution typically spans two domains: from z=0.5 to 2 and z=3.5 to 6.3. The reduced spectra and the derived redshifts are released to the community through the ESO web page http://www.eso.org/science/goods/

E. Vanzella; S. Cristiani; M. Dickinson; M. Giavalisco; H. Kuntschner; J. Haase; M. Nonino; P. Rosati; C. Cesarsky; H. C. Ferguson; R. A. E. Fosbury; A. Grazian; L. A. Moustakas; A. Rettura; P. Popesso; A. Renzini; D. Stern; the GOODS Team

2007-11-06T23:59:59.000Z

368

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

Science Conference Proceedings (OSTI)

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

Meszaros, Sz.; Allende Prieto, C.; De Vicente, A. [Instituto de Astrofisica de Canarias (IAC), E-38200 La Laguna, Tenerife (Spain); Edvardsson, B.; Gustafsson, B. [Department of Physics and Astronomy, Division of Astronomy and Space Physics, Box 515, SE-751 20 Uppsala (Sweden); Castelli, F. [Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Trieste, via Tiepolo 11, I-34143 Trieste (Italy); Garcia Perez, A. E.; Majewski, S. R. [Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904-4325 (United States); Plez, B. [Laboratoire Univers et Particules de Montpellier, Universite Montpellier 2, CNRS, F-34095 Montpellier (France); Schiavon, R. [Gemini Observatory, 670 North A'ohoku Place, Hilo, HI 96720 (United States); Shetrone, M. [McDonald Observatory, University of Texas, Austin, TX 78712 (United States)

2012-10-01T23:59:59.000Z

369

Classification of Ice Crystal Shapes in Midlatitude Ice Clouds from Three Years of Lidar Observations over the SIRTA Observatory  

Science Conference Proceedings (OSTI)

This paper presents a study of ice crystal shapes in midlatitude ice clouds inferred from a technique based on the comparison of ray-tracing simulations with lidar depolarization ratio measured at 532 nm. This technique is applied to three years ...

Vincent Noel; Helene Chepfer; Martial Haeffelin; Yohann Morille

2006-11-01T23:59:59.000Z

370

Evaluation of the Parameter Sensitivities of a Coupled Land Surface Hydrologic Model at a Critical Zone Observatory  

Science Conference Proceedings (OSTI)

Land surface models (LSMs) and hydrologic models are parameterized models. The number of involved parameters is often large. Sensitivity analysis (SA) is a key step to understand the complex relationship between state variables and parameters, and ...

Yuning Shi; Kenneth J. Davis; Fuqing Zhang; Christopher J. Duffy

371

Class.Quantum Grav. 10 (1993) S1854185. Printed in the UK The Laser InterferometerGravitationalWave Observatory  

E-Print Network (OSTI)

systems. The project received funding in 1992 to begin design and construction. Sites for the two facilities (Hanford, Washington and Ljvingstob Lousiana) have been selected. Under the present schedule

Adolphs, Ralph

372

79Fermi Observatory Measures the Lumps in Space An artistic impression of two gamma-ray photons  

E-Print Network (OSTI)

explored to date. As the gamma-rays travel through space, the shortest-wavelength gamma-rays take? Problem 3 ­ The Fermi Telescope measured a gamma-ray pulse from a distant object located 10 billion light from a distant object located 10 billion light years from Earth. The time delay was no more than 0

373

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

E-Print Network (OSTI)

Events Remaining Total event triggers Neutrino triggers (hitMHz+50 MHz clocks Pulsed trigger events Section 9.1 Fiducialtags to remove pulsed trigger events, software- triggered

2007-01-01T23:59:59.000Z

374

Smithsonian Astrophysical Observatory To: M. Cappi, Strong Gravity SDT/YB Team, XMS team mrg-2010-02v2  

E-Print Network (OSTI)

decay time constant is increased beyond the current baseline of 300usec. We used the event simulator time constant of 150 usec, and high and mid intervals of 10 and 40 time constants. If the relevant time constant is instead 300 usec the intervals are likely 3.0 msec and 12 msec and the high counting rate

Garcia, Michael

375

NIST: Freq. Observ. Interstellar Molec. Micro. Trans. - Table 3  

Science Conference Proceedings (OSTI)

... Experiment Max-Planck-Institut fr Radioastronomie European Southern Observatory Onsala Space Observatory Llano de Chanjnantor, Chile. ...

376

No. 114 --December 2003 Spectrum of the star HD 37495 observed in the framework of the UVES Paranal Observatory Project (see S. Bagnulo et al., page 10)  

E-Print Network (OSTI)

the cities of Toconao and San Pedro de Ata- cama, and within relatively easy reach of the array itself formed by nuclear reactions in heavy stars that live for a very short while and blow them- selves up be formed. We are stardust. Astronomy, astrophysics and nuclear physics have made it possible for us

Delmotte, Nausicaa

377

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

378

The Ability of MM5 to Simulate Ice Clouds: Systematic Comparison between Simulated and Measured Fluxes and Lidar/Radar Profiles at the SIRTA Atmospheric Observatory  

Science Conference Proceedings (OSTI)

The ability of the fifth-generation Pennsylvania State UniversityNCAR Mesoscale Model (MM5) to simulate midlatitude ice clouds is evaluated. Model outputs are compared to long-term meteorological measurements by active (radar and lidar) and ...

M. Chiriaco; R. Vautard; H. Chepfer; M. Haeffelin; J. Dudhia; Y. Wanherdrick; Y. Morille; A. Protat

2006-03-01T23:59:59.000Z

379

Dept. of Sol Science, UW-Madison/UW-Extension, 1525 Observatory Dr., Madison, WI 53706/608-262-0485 November 2010 Issue #2 2010  

E-Print Network (OSTI)

plants burn low S coal and some have installed flue gas scrubbers to reduce sulfur emissions. Use is generated from burning coal. As a consequence of the 1990 Clean Air Act Amendment many coal-burning power power plants in the south- eastern part of the state producing FGD gypsum, with a third to come on

Balser, Teri C.

380

arXiv:nuclex/0309004 Measurement of the Total Active 8 B Solar Neutrino Flux at the Sudbury Neutrino Observatory with  

E-Print Network (OSTI)

. Van Berg, 9 R.G. Van de Water, 7 C.J. Virtue, 5 B.L. Wall, 13 D. Waller, 3 C.E. Waltham, 1 H. Wan Chan. Yeh, 2 and K. Zuber 8 (SNO Collaboration) 1 Department of Physics and Astronomy, University of BritishCl in the heavy water to enhance the sensitivity and signature for neutral­current interactions. The flux is found

Waltham, Chris

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

PHYSICAL REVIEW C 75, 045502 (2007) Determination of the # e and total 8 B solar neutrino fluxes using the Sudbury Neutrino Observatory  

E-Print Network (OSTI)

. Van Berg, 15 R. G. Van de Water, 10,15 C. J. Virtue, 7 T. J. Walker, 12 B. L. Wall, 22 C. E. Waltham, 17 M. Yeh, 3 and K. Zuber 14,¶¶¶¶¶ (SNO Collaboration) 1 Atomic Energy of Canada, Limited, Chalk

382

Measurement of the rate of e + d ! p + p + e interactions produced by 8 B solar neutrinos at the Sudbury Neutrino Observatory  

E-Print Network (OSTI)

. Thornewell 6;13;15 P.T. Trent 13z , Y.I. Tserkovnyak 10 , R. Van Berg 14 , R.G. Van de Water 14;6 , C.F. Wilkerson 15;6 , J. Wilson 13 , P. Wittich 14 , J.M. Wouters 6 , M. Yeh 2 (The SNO Collaboration) 1 Atomic

383

Critical-angle transmission grating spectrometer for high-resolution soft x-ray spectroscopy on the International X-ray Observatory  

E-Print Network (OSTI)

High-resolution spectroscopy at energies below 1 keV covers the lines of C, N, O, Ne and Fe ions, and is central to studies of the Interstellar Medium, the Warm Hot Intergalactic Medium, warm absorption and outflows in ...

Heilmann, Ralf K.

384

JOURNAL OF GEOPHYSICAL RESEARCH, VOL. ???, XXXX, DOI:10.1029/, The vertical cloud structure of the West African monsoon  

E-Print Network (OSTI)

of the West African monsoon: A four-year climatology using CloudSat and CALIPSO T. H. M. Stein,1 D. J. Parker Abstract. The West African summer monsoon (WAM) is an important driver of the global climate and locally. Introduction The West African summer monsoon (WAM) controls the climate of the countries of sub-Saharan West

Hogan, Robin

385

Colorado State University Center for Geosciences/Atmospheric Research (CG/AR)  

E-Print Network (OSTI)

forecasts. CloudSat Radar Reflectivity CALIPSO 1064 nm Backscatter BA Saudi Arabia Iran Iraq Persian Gulf 11 on solar CG/AR Quarterly Report No. 4 -5- January 1 ­ March 31, 2007 #12;radiation flux, an extension scientist. Operations ran smoothly, though the weather did not cooperate very well. We had one good CLEX

386

Relationships between Ice Water Content and Volume Extinction Coefficient from In Situ Observations for Temperatures from 0 C to ?86 C: Implications for Spaceborne Lidar Retrievals  

Science Conference Proceedings (OSTI)

An examination of two years of CALIPSO lidar observations and CloudSat cloud radar observations shows that ice clouds at temperatures below about ?45 C frequently fall below the CloudSat radars detection threshold, yet are readily detectable by ...

Andrew Heymsfield; Dave Winker; Melody Avery; Mark Vaughan; Glenn Diskin; Min Deng; Valentin Mitev

387

CESM Atmosphere Model Working Group Meeting 1 3 February 2012  

E-Print Network (OSTI)

aerosol" CAM5 configuration 9:25 Xiaohong Liu ­ Evaluating and constraining ice cloud parameterizations ­ Measurements for Guiding Ice Nucleation, PSD and Morphology Parameterizations in CAM5 11:15 Chris Bretherton Thermodynamic Phase Parameterization Based on CALIPSO Observations on Climate Simulation #12;CAM, high

388

Studying Clouds and Aerosols with Lidar Depolarization Ratio and Backscatter Relationships  

E-Print Network (OSTI)

This dissertation consists of three parts, each devoted to a particular issue of significant importance for CALIPSO lidar observation of depolarization ratio (delta) and backscatter (gamma?) to improve current understanding of the microphysical properties of clouds and aerosols. The relationships between depolarization ratio and backscatter allow us to retrieve particle thermodynamic phase and shape and/or orientation of aerosols and clouds. The first part is devoted to the investigation of the relationships between lidar backscatter and the corresponding depolarization ratio for different cloud classifications and aerosol types. For each cloud and aerosol types, layer-averaged backscatter and backscattering depolarization ratio from the CALIPSO measurements are discussed. The present results demonstrate the unique capabilities of the CALIPSO lidar instrument for determining cloud phase and aerosols subtypes. In the second part, we evaluate the MODIS IR cloud phase with the CALIPSO cloud products. The three possible misclassifications of MODIS IR cloud phasealgorithm, which are studied by Nasiri and Kahn (2008) with radiative transfer modeling, are tested by comparing between MODIS IR phase and CALIOP observations. The current results support their hypotheses, which is that the MODIS phase algorithm may tend to classify thin cirrus clouds as water clouds or mixed phase clouds or unknown, and classify midlevel and/or mid-temperature clouds as mixed or unknown phase. In the third part, we present a 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 visible and IR mineral dust detection algorithms, including BTD procedure, D parameter method, and multi-channel image algorithm, are evaluated with CALIPSO aerosol classification. The comparison reveals that those dust detection algorithms are not effective for optically thin dust layers, but for thick dust storm. The new algorithm using discriminant analysis with CALIPSO observation is much better in detecting thin dust layer of optical thickness between 0.1 and 2.

Cho, Hyoun-Myoung

2011-12-01T23:59:59.000Z

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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

390

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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)*

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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

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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)*

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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)*

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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

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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

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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)*

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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

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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)*

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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

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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

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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

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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

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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)*

405

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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)*

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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

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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

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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)*

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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

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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

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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

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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)*

413

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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

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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

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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

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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

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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

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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)*

419

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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

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Beamline 11.0.1  

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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

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

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

422

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

423

Assignment #1: Developing Algorithms  

E-Print Network (OSTI)

The purpose of this assignment is to give you some experience developing algorithms. According to Wikipedia, an algorithm is a finite list of well-defined instructions for accomplishing some task that, given an initial state, will terminate in a defined end-state [1]. 1. Consider the following initial state: A bag containing sliced bread A jar containing peanut butter A jar containing jelly A plastic knife Develop an algorithm for producing, as an end-state, a peanut butter and jelly sandwich. Be as precise as possible when developing your list of instructions. 2 Hand-In Instructions The assignment is due at the start of class on August 27 th. You are required to turn in a typed document. The document should include your name, your username, the date, the course number, and the assignment number. For example:

Andrew R. Dalton; Andy Dalton (adalton

2007-01-01T23:59:59.000Z

424

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

425

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

426

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

427

Beamline 12.0.2  

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

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

428

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

429

AREA COMPLETION STRATEGIES AT SAVANNAH RIVER SITE: CHARACTERIZATION FOR CLOSURE AND BEYOND  

SciTech Connect

During the first four decades of its 56 year existence, the Savannah River Site (SRS) was a key supplier of nuclear material for national defense. During the 1990s, the site's primary missions became waste site closure, environmental restoration, and deactivation and decommissioning (D&D) of remnant cold war apparatus. Since 1989, with the approval of State and Federal regulatory agencies and with the participation of interested stakeholders, SRS has implemented a final remedy for a majority of the more than 500 individual waste sites at the former nuclear materials complex. These waste sites range from small, inert rubble pits to large, heavy industrial areas and radioactive waste disposal grounds. The closure and final remediation of these waste sites mark significant progress toward achieving SRS's overarching goal of reducing or eliminating future environmental damage and human health threats. However, larger challenges remain. For example, what are appropriate and achievable end-states for decommissioned nuclear facilities? What environmental and human health risks are associated with these end-states? To answer these questions within the strictures of smaller budgets and accelerated schedules, SRS is implementing an ''area completion'' strategy that: (1) unites several discrete waste units into one conceptual model, (2) integrates historically disparate environmental characterization and D&D activities, (3) reduces the number of required regulatory documents, and (4) in some cases, compresses schedules for achieving a stakeholder-approved end-state.

Bagwell, L; Mark Amidon, M; Sadika Baladi, S

2007-06-11T23:59:59.000Z

430

L1B test results Jos de Kloe,  

E-Print Network (OSTI)

ADM-Aeolus L1B test results Jos de Kloe, L1B PM16 10-Mar-2009 #12;L2B-PM15, J. de Kloe, 11-Mar-2009 2 Test cases: Base Reference RMS (1) Academic Tests [with/without noise] (27) Sanity Tests (2) Realistic Tests [LITE data] (9) Mispointing Tests [CALIPSO data] (9) #12;L2B-PM15, J. de Kloe, 11-Mar-2009 3

Stoffelen, Ad

431

L2B test results Jos de Kloe,  

E-Print Network (OSTI)

ADM-Aeolus L2B test results Jos de Kloe, L2B PM15 11-Mar-2009 #12;L2B-PM15, J. de Kloe, 11-Mar-2009 2 Test cases: Base Reference RMS (1) Academic Tests [with/without noise] (27) Sanity Tests (2) Realistic Tests [LITE data] (9) Mispointing Tests [CALIPSO data] (9) #12;L2B-PM15, J. de Kloe, 11-Mar-2009 3

Stoffelen, Ad

432

THE ARIZONA RADIO OBSERVATORY CO MAPPING SURVEY OF GALACTIC MOLECULAR CLOUDS. II. THE W3 REGION IN CO J = 2-1, {sup 13}CO J = 2-1, AND CO J = 3-2 EMISSION  

SciTech Connect

We present fully sampled 38'' resolution maps of the CO and {sup 13}CO J = 2-1 lines in the molecular clouds toward the H II region complex W3. The maps cover a 2.{sup 0}0 x 1.{sup 0}67 section of the galactic plane and span -70 to -20 km s{sup -1} (LSR) in velocity with a resolution of {approx}1.3 km s{sup -1}. The velocity range of the images includes all the gas in the Perseus spiral arm. We also present maps of CO J = 3-2 emission for a 0.{sup 0}5 x 0.{sup 0}33 area containing the H II regions W3 Main and W3(OH). The J = 3-2 maps have velocity resolution of 0.87 km s{sup -1} and 24'' angular resolution. Color figures display the peak line brightness temperature, the velocity-integrated intensity, and velocity channel maps for all three lines, and also the (CO/{sup 13}CO) J = 2-1 line intensity ratios as a function of velocity. The line intensity image cubes are made available in standard FITS format as electronically readable files. We compare our molecular line maps with the 1.1 mm continuum image from the BOLOCAM Galactic Plane Survey (BGPS). From our {sup 13}CO image cube, we derive kinematic information for the 65 BGPS sources in the mapped field, in the form of Gaussian component fits.

Bieging, John H.; Peters, William L., E-mail: jbieging@as.arizona.edu, E-mail: wpeters@as.arizona.edu [Steward Observatory, University of Arizona, Tucson, AZ 85721 (United States)

2011-10-01T23:59:59.000Z

433

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.  

E-Print Network (OSTI)

targets so that we can explore the most distant galaxies formed just after The E-ELT will study nearby. the Big Bang, study individual stars in distant galaxies for the first time, and directly observe planets

Tittley, Eric

434

UNIVERSITE TOULOUSE III -PAUL SABATIER En vue de l'obtention du  

E-Print Network (OSTI)

-RQMT-000804 JWST Project Science Objectives and Requirements JWST-HDBK-002046 JWST Observatory Constraints

Paris-Sud XI, Université de

435

A&A 407, 315324 (2003) DOI: 10.1051/0004-6361:20030854  

E-Print Network (OSTI)

, Abastumani Astrophysical Observatory, Al. Kazbegi ave. 2a, Tbilisi 380060, Georgia Received 24 March 2003

436

DOI: 10.1002/adma.200802222 Materials Science in the Developing  

E-Print Network (OSTI)

Observatory located in the Karoo, Sutherland, etc.). For a South African academic institution intending

Rosei, Federico

437

astro-ph/001152728Nov2000 submitted to ApJ Letters 2000 Oct 21, revised 2000 Nov 28  

E-Print Network (OSTI)

Observatories, 813 Santa Barbara St., Pasadena CA 91101 8 Universidad de Zaragoza, Grupo de Mecanica Espacial

Coppi, Paolo

438

GEOTHERMAL PILOT STUDY FINAL REPORT: CREATING AN INTERNATIONAL GEOTHERMAL ENERGY COMMUNITY  

E-Print Network (OSTI)

drilling team from Dalhousie University and Lamont-Doherty Geo- logical Observatory, which encoun- tered fluid

Bresee, J. C.

2011-01-01T23:59:59.000Z

439

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

440

Regulatory Reform and License Termination Planning in Decommissioning  

SciTech Connect

Decommissioning of commercial nuclear power plants (NPPs) must be safe and cost-effective and consider the needs of a wide range of stakeholders. The creative tension among these objectives has provided opportunities to reform the way these plants are regulated and managed in decommissioning. Enlightened and visionary leaders from the U.S. Nuclear Regulatory Commission (NRC) and industry are seizing these opportunities to create new paradigms for risk-informed regulation; creative stakeholder involvement; and effective, end-state focused, license termination planning.

Michael J. Meisner

2000-06-04T23:59:59.000Z

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.


441

Idaho National Laboratory 2013-2022 Ten-Year Site Plan  

SciTech Connect

The Idaho National Laboratory (INL) Ten-Year Site Plan (TYSP) describes the strategy for accomplishing the long-term objective of transforming the laboratory to meet Department of Energy (DOE) national nuclear research and development (R&D) goals, as outlined in DOE strategic plans. The plan links R&D mission goals and INL core capabilities with infrastructure requirements (single- and multi-program), establishs the 10-year end-state vision for INL complexes, and identifies and prioritizes infrastructure needs and capability gaps. The TYSP serves as the basis for documenting and justifying infrastructure investments proposed as part of the FY 2013 budget formulation process.

Calvin Ozaki; Sheryl L. Morton; Elizabeth A. Connell; William T. Buyers; Craig L. Jacobson; Charles T. Mullen; Christopher P. Ischay; Ernest L. Fossum; Robert D. Logan

2011-06-01T23:59:59.000Z

442

The Design and Development of an Irish Sea Passenger-Ferry-Based Oceanographic Measurement System  

Science Conference Proceedings (OSTI)

An evolving coastal observatory has been hosted by the National Oceanography Centre at Liverpool, United Kingdom, for more than nine years. Within this observatory an instrumented ferry system has been developed and operated to provide near-...

C. A. Balfour; M. J. Howarth; D. S. Jones; T. Doyle

2013-06-01T23:59:59.000Z

443

An Update on the Status of the Pulsar?ALFA Survey  

Science Conference Proceedings (OSTI)

The Pulsar?ALFA (PALFA) survey is designed to search the Galactic plane for pulsars at 1.4 GHz using the Arecibo Observatorys 7?beam ALFA receiver. The 64??s sampling time

P. Lazarus; The PALFA Consortium

2011-01-01T23:59:59.000Z

444

Fermilab Today  

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

Pierre Auger Observatory Celebration, to be held November 9-12, 2005 in Malarge, Argentina BATAVIA, Illinois-Scientists of the Pierre Auger Observatory, a project to study the...

445

A WASHINGTON STATE UNIVERSITY POSTDOCTORAL POSITION FOR WORK AT LIGO HANFORD, WA Applications are invited for a postdoctoral position in the Gravity Group at the Department of Physics  

E-Print Network (OSTI)

A WASHINGTON STATE UNIVERSITY POSTDOCTORAL POSITION FOR WORK AT LIGO HANFORD, WA Applications characterization for the Advanced Laser Interferometer Gravitational wave Observatory (LIGO) at the Hanford site characterization at the LIGO Hanford observatory. Familiarity with data analysis pipelines for searching

Collins, Gary S.

446

Atmospheric Radiation Measurement Program  

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

Atmospheric Observatory (UAO) Pilot Experiment at NYC" - Michael Reynolds, BNL 17:30 "EML Pilot Studies for the Urban Atmospheric Observatory" - Hsi-Na (Sam) Lee, EML 17:40 "A...

447

Spectral Characteristics of the Convective Boundary Layer Over Uneven Terrain  

Science Conference Proceedings (OSTI)

The paper describes a convective boundary layer experiment conducted in April 1978 at the Boulder Atmospheric Observatory, and examines the spectral behavior of wind velocity and temperature from the Observatory's 300 m tower, from aircraft ...

J. C. Kaimal; R. A. Eversole; D. H. Lenschow; B. B. Stankov; P. H. Kahn; J. A. Businger

1982-05-01T23:59:59.000Z

448

SciTech Connect: "smart grid"  

Office of Scientific and Technical Information (OSTI)

Journal Article: Cosmic-ray physics with the milagro gamma-ray observatory Citation Details In-Document Search Title: Cosmic-ray physics with the milagro gamma-ray observatory...

449

ALSNews Vol. 308  

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

08 Print 08 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

450

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

451

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

452

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

453

Beamline 12.0.2  

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

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

454

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

455

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

456

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

457

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

458

Optima MDxt: A high throughput 335 keV mid-dose implanter  

SciTech Connect

The continuing demand for both energy purity and implant angle control along with high wafer throughput drove the development of the Axcelis Optima MDxt mid-dose ion implanter. The system utilizes electrostatic scanning, an electrostatic parallelizing lens and an electrostatic energy filter to produce energetically pure beams with high angular integrity. Based on field proven components, the Optima MDxt beamline architecture offers the high beam currents possible with singly charged species including arsenic at energies up to 335 keV as well as large currents from multiply charged species at energies extending over 1 MeV. Conversely, the excellent energy filtering capability allows high currents at low beam energies, since it is safe to utilize large deceleration ratios. This beamline is coupled with the >500 WPH capable endstation technology used on the Axcelis Optima XEx high energy ion implanter. The endstation includes in-situ angle measurements of the beam in order to maintain excellent beam-to-wafer implant angle control in both the horizontal and vertical directions. The Optima platform control system provides new generation dose control system that assures excellent dosimetry and charge control. This paper will describe the features and technologies that allow the Optima MDxt to provide superior process performance at the highest wafer throughput, and will provide examples of the process performance achievable.

Eisner, Edward; David, Jonathan; Justesen, Perry; Kamenitsa, Dennis; McIntyre, Edward; Rathmell, Robert; Ray, Andrew; Rzeszut, Richard [Axcelis Technologies, Inc., 108 Cherry Hill Drive, Beverly, MA 01915 (United States)

2012-11-06T23:59:59.000Z

459

Gravitational Collapse In Husain Space-time For Brans-Dicke Gravity Theory  

E-Print Network (OSTI)

The motive of this work is to study gravitational collapse in Husain space-time, in Brans-Dicke gravity theory. Among many scalar-tensor theories of gravity, Brans-Dicke is the simplest and the impact of it can be regulated by two parameters, coupling constant $\\omega$, and the assumed field dependency parameter $n$. V. Husain's work on exact solution for null fluid collapse in 1996 has influenced many authors to follow his way to find the end-state of the homogeneous/inhomogeneous dust cloud collapse using Vaidya's metric. Detecting whether the cosmological singularity is naked or wrapped by an event horizon, by the existence of future directed radial null geodesic emitted in past from the singularity is the basic objective. To point out the existence of positive trajectory tangent solution, both particular parametric cases (through tabular forms) and wide range contouring process have been applied. Precisely, perfect fluid's EoS ($p=k\\rho$) satisfies a wide range of phenomena: from dust to exotic fluid like dark energy. We have used this EoS parameter $k$ to determine the end state of collapse in different cosmological era. Our main target is to check low $\\omega$ (more Brans-Dicke effect) and negative $k$ zones. This particularly characterizes the nature of collapse end-state in accelerated expansion in Brans-Dicke gravity. It is noted that "low $\\omega$ $-$ low EoS parameter" increases the probability of getting naked singularities.

Prabir Rudra; Ritabrata Biswas; Ujjal Debnath

2013-07-23T23:59:59.000Z

460

Beamline 11.0.1  

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1 1 Beamline 11.0.1 Print Tuesday, 20 October 2009 09:16 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

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461

EUV beam line moves to PML  

Science Conference Proceedings (OSTI)

... Explorer (ACE), and the new twin Solar Terrestrial Relations Observatory (STEREO) spacecraft, America's space-weather early-warning systems ...

2013-01-03T23:59:59.000Z

462

Synchrotron Programs and Projects  

Science Conference Proceedings (OSTI)

... Synchrotron Radiation-Based Calibrations for Space Weather Prediction Last ... NASA launched the Solar Dynamics Observatory ( SDO ) satellite on ...

2010-05-24T23:59:59.000Z

463

A Unique Institution: The National Bureau of Standards, 1950 ...  

Science Conference Proceedings (OSTI)

... in 1964. Two years later, Raymond Davis, Jr., opened a "neutrino observatory" deep in South Dakota's Homestake gold mine. ...

464

The APO 3.5-meter remote observing program--2002 and beyond Bruce Gillespie*  

E-Print Network (OSTI)

The APO 3.5-meter remote observing program--2002 and beyond Bruce Gillespie* Site Operations Manager, Apache Point Observatory ABSTRACT The Apache Point Observatory 3.5-meter telescope is a working operational models. Keywords: Astrophysical Research Consortium, Apache Point Observatory, 3.5-meter telescope

Castillo, Steven P.

465

U2B Beamline | Photon Sciences | Brookhaven National Laboratory  

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BNL People BNL People Photon SciencesInfrared Programs PS Home Infrared Home Beamlines U2A U2B U4IR U10A U10B U12IR Publications User Info Useful Sites Beamline U2B Home Publications Equipment Schedule Beamtime Instrument Spectrometer endstation: Thermo Nicolet Magna 860 Step-Scan FTIR and Continuum IR microscope Frequency Range (cm-1): 500 - 4000 Spectral resolution (cm-1): 4.0 Spatial resolution: diffraction-limit (i.e. ~ 3 to 10 microns) Brightness (compared to a black body): 100x to 1000x Smallest practical targeting aperture size: 3 microns square Beamline angular acceptance: (milliradians): 40H x 40V (100% vertical collection down to 240 cm-1) Optical Configuration A two-mirror system (M1 and M2) collects and re-images the synchrotron infrared source at a point just outside of the storage ring's UHV. M1 is a

466

Beamline 9.0.2  

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2 Print 2 Print Chemical Dynamics Scientific disciplines: Chemical dynamics, aerosol chemistry, imaging mass spectrometry, chemical kinetics, laser ablation and clusters, combustion and flames. Endstations: Molecular-beam photoelectron/photoion imaging and spectroscopy Flame chamber Ablation chamber Aerosol chamber Kinetics chamber GENERAL BEAMLINE INFORMATION Operational Yes Source characteristics 10-cm period undulator (U10) (fundamental) Energy range 7.4-30 eV Undulator beam White beam (straight undulator beam) Calculated flux (1.9 GeV, 400 mA) 1016 photons/s, 2.5%BW Spot size at sample 170 (h) x 50 (v) µm Monochromator #1 3-m Off-plane Eagle Calculated flux (1.9 GeV, 400 mA) 1014 photons/s, 0.1%BW Spot size at sample 400 (h) x 350 (v) µm Monochromator #2 3-m Off-plane Eagle

467

Beamline 8.2.2  

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2 Print 2 Print Berkeley Center for Structural Biology (BCSB) Multiple-Wavelength Anomalous Diffraction (MAD) and Macromolecular Crystallography (MX) GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for Structural Biology Beamlines (2-month cycle) Source characteristics Superbend (5.0 T, single pole) Energy range 5-16 keV Monochromator Double crystal, Si(111) Measured flux (1.9 GeV, 400 mA) 3.0 x 1011 photons/sec Resolving power (E/ΔE) 7,000 Divergence (max at sample) 3.0(h) x 0.5(v) mrad Measured spot size at sample (FWHM) 100 µm Endstations Minihutch Detectors 3x3 CCD array (ADSC Q315) Sample format Single crystals of biological molecules Sample preparation Support labs available Sample environment Ambient or ~100 K Special notes Computers for data processing and analysis are available

468

Beamline 5.0.1  

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1 Print 1 Print Berkeley Center for Structural Biology (BCSB) Monochromatic protein crystallography Scientific discipline: Structural biology GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for Structural Biology Beamlines (2-month cycle) Source characteristics 11.4-cm-period wiggler (W11) Energy range 12.7 keV (fixed) Monochromator Si(220) Asymmetric cut single crystal Measured flux 1.50 x 1011 photons/s at 400-mA ring current, with 1.5-mrad divergence and 100-µm pinhole collimator Resolving power (E/ΔE) ~10,000 Divergence at sample 3.0 (h) x 0.4 (v) mrad (user selectable) Spot size 100 µm Endstations Standard hutch Detectors 3 x 3 CCD array (ADSC Q315R) Sample format Single crystals of biological molecules Sample preparation Support labs available

469

Beamline 10.0.1  

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

0.1 Print 0.1 Print Photoemission of Highly Correlated Materials; High-Resolution Atomic, Molecular, and Optical Physics Scientific disciplines: AMO, correlated electron systems Endstations: High energy resolution spectrometer (HERS) High-resolution atomic and molecular electron spectrometer (HiRAMES) HRAMO-Ion-photon beamline (IPB) Velocity map imaging spectrometer Electron spin polarization (ESP) GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics 10-cm period undulator (U10) (first and third harmonics) Energy range 17-350 eV Monochromator SGM (gratings: 380, 925, 2100 lines/mm) Calculated and measured flux (1.9 GeV, 400 mA) Up to 1013 photons/s/0.01% BW at 30 eV Resolving power (E/ΔE)

470

Instrumentation upgrades for the Macromolecular Crystallography beamlines  

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

Instrumentation upgrades for the Macromolecular Crystallography beamlines Instrumentation upgrades for the Macromolecular Crystallography beamlines of the Swiss Light Source Monday, October 29, 2012 - 2:00am SSRL, Bldg. 137, Rm. 322 Martin Fuchs, MX Group, Swiss Light Source; Paul Scherrer Institute (Villigen, Switzerland) A new unified diffractometer - the D3 - has been developed for the three MX beamlines. The first of the instruments is in general user operation at beamline X10SA since April 2012. The varied demands from both challenging academic research projects as well as high throughput industrial applications on today's macromolecular crystallography beamlines drive developments to both endstations and beamline optics. Recent instrumentation upgrades to the macromolecular crystallography (MX) beamlines of the Swiss Light Source therefore aimed to

471

Title Goes Here  

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

Diagnostics at SPEAR3 Diagnostics at SPEAR3 Jeff Corbett a , Weixing Cheng b , Alan S. Fisher a , Walter Mok a & Stuart Westerman a a SLAC National Accelerator Laboratory, Menlo Park, CA 94306, USA b Brookhaven National Laboratory, Upton, NY 11973, USA Abstract. The visible light diagnostic beam line at SPEAR3 utilizes dipole radiation extracted through an ID exit port to evaluate electron beam properties at a variety of diagnostic end-stations. The unfocused SR light is collected 17m from the source point by a 150mm diameter, f=2m lens and optically relayed to the appropriate station. For transverse imaging, an image-intensified PiMax camera with 2ns gate allows measurement of fast beam dynamics for either the stored beam or the injected beam. For these applications the visible light is switched into either a

472

Beamline 1.4.3  

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3 Print 3 Print FTIR spectromicroscopy Scientific disciplines: Biology, correlated electron systems, environmental science, geology, chemistry, polymers, soft materials GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Bend magnet Energy range 0.05-1.2 eV Frequency range 650 - 10,000 cm-1 Interferometer resolution Up to 0.125 cm-1 Endstations Nicolet Magna 760 FTIR, Nic-Plan IR Microscope (N2 purged) Characteristics Motorized sample stage, 0.1-micron resolution, reflection, transmission, and grazing-incidence reflection modes Spatial resolution Diffraction-limited (~wavelength); x-y stage with 0.1 micron accuracy Detectors MCT-A (mercury cadmium telluride) Spot size at sample 2-10 µm (diffraction-limited)

473

Beamline 5.0.3  

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

3 3 Beamline 5.0.3 Print Tuesday, 20 October 2009 08:36 Berkeley Center for Structural Biology (BCSB) Monochromatic protein crystallography Scientific discipline: Structural biology GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for Structural Biology Beamlines (2-month cycle) Source characteristics 11.4-cm-period wiggler (W11) Energy range 12,700 eV(fixed) Monochromator Asymmetric cut single crystal Si(220) Measured flux 2.4 x 1011 photons/s at 400-mA ring current, with 1.5-mrad divergence and 100-µm pinhole collimator Divergence at sample 3.0 (h) x 0.4 (v) mrad (user selectable) Spot size 100 µm Endstations Standard hutch Detectors 3 x 3 CCD array (ADSC Q315R) Sample format Single crystals of biological molecules Sample preparation Support labs available; automated sample mounting system

474

Beamline 10.0.1  

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

0.1 0.1 Beamline 10.0.1 Print Tuesday, 20 October 2009 09:08 Photoemission of Highly Correlated Materials; High-Resolution Atomic, Molecular, and Optical Physics Scientific disciplines: AMO, correlated electron systems Endstations: High energy resolution spectrometer (HERS) High-resolution atomic and molecular electron spectrometer (HiRAMES) HRAMO-Ion-photon beamline (IPB) Velocity map imaging spectrometer Electron spin polarization (ESP) GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics 10-cm period undulator (U10) (first and third harmonics) Energy range 17-350 eV Monochromator SGM (gratings: 380, 925, 2100 lines/mm) Calculated and measured flux (1.9 GeV, 400 mA) Up to 1013 photons/s/0.01% BW at 30 eV

475

Beamline 1.4.3  

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

3 Print 3 Print FTIR spectromicroscopy Scientific disciplines: Biology, correlated electron systems, environmental science, geology, chemistry, polymers, soft materials GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Bend magnet Energy range 0.05-1.2 eV Frequency range 650 - 10,000 cm-1 Interferometer resolution Up to 0.125 cm-1 Endstations Nicolet Magna 760 FTIR, Nic-Plan IR Microscope (N2 purged) Characteristics Motorized sample stage, 0.1-micron resolution, reflection, transmission, and grazing-incidence reflection modes Spatial resolution Diffraction-limited (~wavelength); x-y stage with 0.1 micron accuracy Detectors MCT-A (mercury cadmium telluride) Spot size at sample 2-10 µm (diffraction-limited)

476

Beamline 10.3.1  

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

1 Print 1 Print X-ray fluorescence microprobe Scientific disciplines: Environmental science, detector development, low-dose radiation effects in cells GENERAL BEAMLINE INFORMATION Operational Yes, but not open to users Source characteristics Bend magnet Energy range 3-20 keV Monochromator White light, multilayer mirrors in Kirkpatrick-Baez configuration Calculated flux (1.9 GeV, 400 mA) 3 x 1010 photons/s at 12.5 keV Resolving power (E/ΔE) White light to 30 at 12 keV Endstations Large hutch with optical table Characteristics X-ray fluorescence analysis of samples with high elemental sensitivity and high spatial resolution Spatial resolution 10 x 10 µm Detectors Silicon drift detector Spot size at sample 1.0 x 1.2 µm Sample format Sample size flexible up to 30 cm x 1 meter depending on configuration.

477

Beamline 1.4.3  

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

3 Print 3 Print FTIR spectromicroscopy Scientific disciplines: Biology, correlated electron systems, environmental science, geology, chemistry, polymers, soft materials GENERAL BEAMLINE INFORMATION Operational Yes Proposal cycle Proposals for General Sciences Beamlines (6-month cycle) Source characteristics Bend magnet Energy range 0.05-1.2 eV Frequency range 650 - 10,000 cm-1 Interferometer resolution Up to 0.125 cm-1 Endstations Nicolet Magna 760 FTIR, Nic-Plan IR Microscope (N2 purged) Characteristics Motorized sample stage, 0.1-micron resolution, reflection, transmission, and grazing-incidence reflection modes Spatial resolution Diffraction-limited (~wavelength); x-y stage with 0.1 micron accuracy Detectors MCT-A (mercury cadmium telluride) Spot size at sample 2-10 µm (diffraction-limited)

478

APS Beamline 6-ID-B,C  

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

B,C Home B,C Home Recent Publications Beamline Info Optics Instrumentation Software User Info Beamline 6-ID-B,C Beamline 6-ID-B,C is operated by the Magnetic Materials Group in the X-ray Science Division (XSD) of the Advanced Photon Source. Research on this beamline centers on general x-ray scattering studies of materials. The beamline has 2 end-stations: 6-ID-B: Psi -Diffractomter & In-Field Studies 6-ID-C: UHV in-situ growth Recent Research Highlights LSMO pictures Searching for Next-Generation Electronic Materials December 14, 2009 A new class of layered oxide materials discovered thanks to research at the beamline 6-ID-B offers scientists unprecedented opportunities for creating the next generation of electronic devices. Local Contact: Phil Ryan Local Contacts: Philip Ryan (Surface Diffraction) 630.252.0252 ryan@aps.anl.gov

479

Beamline 3.2.1  

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

2.1 Print 2.1 Print Commercial deep-etch x-ray lithography (LIGA) GENERAL BEAMLINE INFORMATION Operational Yes, but not open to users Source characteristics Bend magnet Energy range 3-12 keV Monochromator None Endstations Hutch with automated scanner Calculated spot size at sample 100 x 10 mm Sample format 3- and 4-in. wafer format; x-ray mask and LIGA substrate Sample environment Ambient, air Scientific disciplines Applied science Scientific applications Deep-etch x-ray lithography (LIGA) Spokesperson This e-mail address is being protected from spambots. You need JavaScript enabled to view it Advanced Light Source, Berkeley Lab Phone: (510) 486-5527 Fax: (510) 486-4102 This e-mail address is being protected from spambots. You need JavaScript enabled to view it AXSUN Technology

480

Beamline 5.4.1  

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

1 Print 1 Print Infrared spectromicroscopy GENERAL BEAMLINE INFORMATION Operational 2011 Source characteristics Bend magnet Energy range 0.07-1.25 eV Frequency range 600 - 10,000 cm-1 Interferometer resolution 0.125 cm-1 Endstations FTIR bench and IR microscope (N2 purged) Characteristics Computerized sample stage, 0.1-micron resolution; reflection, transmission, and attenuated total reflectance (ATR) modes; polarizing and UV fluorescence optics Spatial resolution Diffraction limited (~wavelength) Detectors Probably MCT-A*, MCT-B (mercury cadmium telluride) Spot size at sample 2-10 µm (diffraction-limited) Sample preparation Biological preparation equipment available including incubator, biohoods, prep table, and more TBD. Sample environment N2 purged, minimal clean area (no particle specification), microcryostat/heater stages available for 4.2-730 K