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Office of Scientific and Technical Information
Measurement of Expected Nucleation Precursor Species and 3�500-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
Increase in background stratospheric aerosol observed with lidar at Mauna Loa Observatory and Boulder, Colorado - article no. L15808
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)
Atmospheric Concentrations of CO2 from Mauna Loa, Hawaii
NLE Websites -- All DOE Office Websites (Extended Search)
Atmospheric Concentrations of CO2 from Mauna Loa, Hawaii Atmospheric Concentrations of CO2 from Mauna Loa, Hawaii The graphs on this page are generated from data taken from "Trends in Carbon Dioxide" page on the Department of Commerce/National Oceanic and Atmospheric Administration (NOAA) website. The NOAA website presents monthly and weekly atmospheric CO2 concentrations measured at the Mauna Loa Observatory in Hawaii. It offers weekly and monthly data, additional graphs, analysis, descriptions of how the data are collected, and an animation of historical changes in atmospheric CO2. Mauna Loa constitutes the longest record of direct measurements of CO2 in the atmosphere. The measurents were started by C. David Keeling of the Scripps Institution of Oceanography in March of 1958. Recent Monthly Average CO2
Living in the shadow of Mauna Loa
E-Print Network (OSTI)
One of Hawaii's most dangerous natural hazards is sitting in plain sight: Mauna Loa volcano. The mighty mountain makes up more than fifty percent of the island and is the largest volcano on Earth. Since 1843, when people ...
Hirji, Zahra R. (Zahra Rafik)
Atmospheric Carbon Dioxide Record from Mauna Loa
SIO Air Sampling Network » Mauna Loa SIO Air Sampling Network » Mauna Loa Atmospheric Carbon Dioxide Record from Mauna Loa DOI: 10.3334/CDIAC/atg.035 graphics Graphics data Data Investigators R.F. Keeling, S.C. Piper, A.F. Bollenbacher and J.S. Walker Carbon Dioxide Research Group Scripps Institution of Oceanography University of California La Jolla, California 92093-0444, U.S.A. Period of Record 1958-2008 Methods Air samples at Mauna Loa are collected continuously from air intakes at the top of four 7-m towers and one 27-m tower. Four air samples are collected each hour for the purpose of determining the CO2 concentration. Determinations of CO2 are made by using a Siemens Ultramat 3 nondispersive infrared gas analyzer with a water vapor freeze trap. This analyzer registers the concentration of CO2 in a stream of air flowing at ~0.5
Direct-Current Resistivity Survey At Mauna Loa Northeast Rift...
Open Energy Info (EERE)
Details Location Mauna Loa Northeast Rift Area Exploration Technique Direct-Current Resistivity Survey Activity Date Usefulness useful DOE-funding Unknown Notes The vertical...
Mauna Loa Northeast Rift Geothermal Area | Open Energy Information
Mauna Loa Northeast Rift Geothermal Area Mauna Loa Northeast Rift Geothermal Area (Redirected from Mauna Loa Northeast Rift Area) Jump to: navigation, search GEOTHERMAL ENERGYGeothermal Home Geothermal Resource Area: Mauna Loa Northeast Rift Geothermal Area Contents 1 Area Overview 2 History and Infrastructure 3 Regulatory and Environmental Issues 4 Exploration History 5 Well Field Description 6 Geology of the Area 7 Geofluid Geochemistry 8 NEPA-Related Analyses (0) 9 Exploration Activities (6) 10 References Area Overview Geothermal Area Profile Location: Hawaii Exploration Region: Hawaii Geothermal Region GEA Development Phase: 2008 USGS Resource Estimate Mean Reservoir Temp: Estimated Reservoir Volume: Mean Capacity: Click "Edit With Form" above to add content History and Infrastructure Operating Power Plants: 0
Geothermometry At Mauna Loa Northeast Rift Area (Thomas, 1986) | Open
Geothermometry At Mauna Loa Northeast Rift Area (Thomas, 1986) Geothermometry At Mauna Loa Northeast Rift Area (Thomas, 1986) Jump to: navigation, search GEOTHERMAL ENERGYGeothermal Home Exploration Activity: Geothermometry At Mauna Loa Northeast Rift Area (Thomas, 1986) Exploration Activity Details Location Mauna Loa Northeast Rift Area Exploration Technique Geothermometry Activity Date Usefulness useful DOE-funding Unknown Notes A reexamination of all groundwater sources in the Keaau area was undertaken in an effort to confirm the chemical and temperature anomalies that formed the primary basis on which the Keaau area was identified during the preliminary assessment survey. The data generated by this survey (Table 9) determined that all of the anomalous data present in the earlier data base were spurious and that the groundwater chemistry and temperatures in this
Orographic Cloud over the Eastern Slopes of Mauna Loa Volcano, Hawaii, Related to Insolation and Wind
During the period 1�11 June 1978, solar radiation and other meteorological data were gathered at eight stations arranged in a nearly linear transaction extending from the coast at Hilo, Hawaii to Mauna Loa Observatory, 60 km inland and 3400 m ...
Alfred J. Garrett
Mauna Loa Southwest Rift Geothermal Area | Open Energy Information
Mauna Loa Southwest Rift Geothermal Area Mauna Loa Southwest Rift Geothermal Area Jump to: navigation, search GEOTHERMAL ENERGYGeothermal Home Geothermal Resource Area: Mauna Loa Southwest Rift Geothermal Area Contents 1 Area Overview 2 History and Infrastructure 3 Regulatory and Environmental Issues 4 Exploration History 5 Well Field Description 6 Geology of the Area 7 Geofluid Geochemistry 8 NEPA-Related Analyses (0) 9 Exploration Activities (2) 10 References Area Overview Geothermal Area Profile Location: Hawaii Exploration Region: Hawaii Geothermal Region GEA Development Phase: 2008 USGS Resource Estimate Mean Reservoir Temp: Estimated Reservoir Volume: Mean Capacity: Click "Edit With Form" above to add content History and Infrastructure Operating Power Plants: 0 No geothermal plants listed. Add a new Operating Power Plant
Mauna Loa Northeast Rift Geothermal Area Mauna Loa Northeast Rift Geothermal Area Jump to: navigation, search GEOTHERMAL ENERGYGeothermal Home Geothermal Resource Area: Mauna Loa Northeast Rift Geothermal Area Contents 1 Area Overview 2 History and Infrastructure 3 Regulatory and Environmental Issues 4 Exploration History 5 Well Field Description 6 Geology of the Area 7 Geofluid Geochemistry 8 NEPA-Related Analyses (0) 9 Exploration Activities (6) 10 References Area Overview Geothermal Area Profile Location: Hawaii Exploration Region: Hawaii Geothermal Region GEA Development Phase: 2008 USGS Resource Estimate Mean Reservoir Temp: Estimated Reservoir Volume: Mean Capacity: Click "Edit With Form" above to add content History and Infrastructure Operating Power Plants: 0 No geothermal plants listed. Add a new Operating Power Plant
Mercury Vapor At Mauna Loa Northeast Rift Area (Thomas, 1986) | Open Energy
Mauna Loa Northeast Rift Area (Thomas, 1986) Mauna Loa Northeast Rift Area (Thomas, 1986) Jump to: navigation, search GEOTHERMAL ENERGYGeothermal Home Exploration Activity: Mercury Vapor At Mauna Loa Northeast Rift Area (Thomas, 1986) Exploration Activity Details Location Mauna Loa Northeast Rift Area Exploration Technique Mercury Vapor Activity Date Usefulness not indicated DOE-funding Unknown Notes Soil mercury and radon emanometry sampling conducted in the Keaau prospect were similarly unable to define any anomalies that could reasonably be interpreted to be due to subsurface thermal effects. References Donald M. Thomas (1 January 1986) Geothermal Resources Assessment In Hawaii Retrieved from "http://en.openei.org/w/index.php?title=Mercury_Vapor_At_Mauna_Loa_Northeast_Rift_Area_(Thomas,_1986)&oldid=390060
Gas Flux Sampling At Mauna Loa Northeast Rift Area (Thomas, 1986) | Open
Gas Flux Sampling At Mauna Loa Northeast Rift Area (Thomas, 1986) Gas Flux Sampling At Mauna Loa Northeast Rift Area (Thomas, 1986) Jump to: navigation, search GEOTHERMAL ENERGYGeothermal Home Exploration Activity: Gas Flux Sampling At Mauna Loa Northeast Rift Area (Thomas, 1986) Exploration Activity Details Location Mauna Loa Northeast Rift Area Exploration Technique Gas Flux Sampling Activity Date Usefulness not indicated DOE-funding Unknown Notes Soil mercury and radon emanometry sampling conducted in the Keaau prospect were similarly unable to define any anomalies that could reasonably be interpreted to be due to subsurface thermal effects. References Donald M. Thomas (1 January 1986) Geothermal Resources Assessment In Hawaii Retrieved from "http://en.openei.org/w/index.php?title=Gas_Flux_Sampling_At_Mauna_Loa_Northeast_Rift_Area_(Thomas,_1986)&oldid=389039"
Aeromagnetic Survey At Mauna Loa Northeast Rift Area (Thomas, 1986) | Open
Rift Area (Thomas, 1986) Rift Area (Thomas, 1986) Jump to: navigation, search GEOTHERMAL ENERGYGeothermal Home Exploration Activity: Aeromagnetic Survey At Mauna Loa Northeast Rift Area (Thomas, 1986) Exploration Activity Details Location Mauna Loa Northeast Rift Area Exploration Technique Aeromagnetic Survey Activity Date Usefulness useful DOE-funding Unknown Notes Aeromagnetic data (Godson et al., 1981) for the lower northeast rift of Mauna Loa tend to substantiate this conclusion as well. The lower extension of the rift zone does not exhibit any significant magnetic features that would correspond to a thermal source within the inferred trace of the rift zone. References Donald M. Thomas (1 January 1986) Geothermal Resources Assessment In Hawaii Retrieved from "http://en.openei.org/w/index.php?title=Aeromagnetic_Survey_At_Mauna_Loa_Northeast_Rift_Area_(Thomas,_1986)&oldid=40242
Direct-Current Resistivity Survey At Mauna Loa Southwest Rift Area (Thomas,
Area (Thomas, Area (Thomas, 1986) Jump to: navigation, search GEOTHERMAL ENERGYGeothermal Home Exploration Activity: Direct-Current Resistivity Survey At Mauna Loa Southwest Rift Area (Thomas, 1986) Exploration Activity Details Location Mauna Loa Southwest Rift Area Exploration Technique Direct-Current Resistivity Survey Activity Date Usefulness not indicated DOE-funding Unknown Notes Field surveys in the South Point area were limited to a series of Schlumberger soundings and a self-potential traverse across the rift zone. The absence of groundwater wells and time and funding constraints precluded any geochemical field surveys. References Donald M. Thomas (1 January 1986) Geothermal Resources Assessment In Hawaii Retrieved from "http://en.openei.org/w/index.php?title=Direct-Current_Resistivity_Survey_At_Mauna_Loa_Southwest_Rift_Area_(Thomas,_1986)&oldid=510541"
Self Potential At Mauna Loa Southwest Rift Area (Thomas, 1986) | Open
Southwest Rift Area (Thomas, 1986) Southwest Rift Area (Thomas, 1986) Jump to: navigation, search GEOTHERMAL ENERGYGeothermal Home Exploration Activity: Self Potential At Mauna Loa Southwest Rift Area (Thomas, 1986) Exploration Activity Details Location Mauna Loa Southwest Rift Area Exploration Technique Self Potential Activity Date Usefulness not indicated DOE-funding Unknown Notes Field surveys in the South Point area were limited to a series of Schlumberger soundings and a self-potential traverse across the rift zone. The absence of groundwater wells and time and funding constraints precluded any geochemical field surveys. References Donald M. Thomas (1 January 1986) Geothermal Resources Assessment In Hawaii Retrieved from "http://en.openei.org/w/index.php?title=Self_Potential_At_Mauna_Loa_Southwest_Rift_Area_(Thomas,_1986)&oldid=389751
Direct-Current Resistivity Survey At Mauna Loa Northeast Rift Area (Thomas,
Direct-Current Resistivity Survey At Mauna Loa Direct-Current Resistivity Survey At Mauna Loa Northeast Rift Area (Thomas, 1986) Exploration Activity Details Location Mauna Loa Northeast Rift Area Exploration Technique Direct-Current Resistivity Survey Activity Date Usefulness useful DOE-funding Unknown Notes The vertical electrical sounding surveys encountered few difficulties and were able to resolve basement resistivities in all locations. The resistivity sections derived indicated a 3000- 20,000 ohm.m surface layer underlain by a 500- 900 ohm-m cold freshwatersaturated layer and a basement layer of less than 100 ohm.m (Kauahikaua and Mattice, 1981). The depth of penetration of these soundings was estimated to be about 800 m to 900 m b.s.1. and thus the basement resistivities probably correspond to basalts
Scale-free Universal Spectrum for Atmospheric Aerosol Size Distribution for Davos, Mauna Loa and Izana
Atmospheric flows exhibit fractal fluctuations and inverse power law form for power spectra indicating an eddy continuum structure for the selfsimilar fluctuations. A general systems theory for fractal fluctuations developed by the author is based on the simple visualisation that large eddies form by space-time integration of enclosed turbulent eddies, a concept analogous to Kinetic Theory of Gases in Classical Statistical Physics. The ordered growth of atmospheric eddy continuum is in dynamical equilibrium and is associated with Maximum Entropy Production. The model predicts universal (scale-free) inverse power law form for fractal fluctuations expressed in terms of the golden mean. Atmospheric particulates are held in suspension in the fractal fluctuations of vertical wind velocity. The mass or radius (size) distribution for homogeneous suspended atmospheric particulates is expressed as a universal scale-independent function of the golden mean, the total number concentration and the mean volume radius. Model predicted spectrum is in agreement (within two standard deviations on either side of the mean) with total averaged radius size spectra for the AERONET (aerosol inversions) stations Davos and Mauna Loa for the year 2010 and Izana for the year 2009 daily averages. The general systems theory model for aerosol size distribution is scale free and is derived directly from atmospheric eddy dynamical concepts. At present empirical models such as the log normal distribution with arbitrary constants for the size distribution of atmospheric suspended particulates are used for quantitative estimation of earth-atmosphere radiation budget related to climate warming/cooling trends. The universal aerosol size spectrum will have applications in computations of radiation balance of earth-atmosphere system in climate models.
A. M. Selvam
Mapnottoscale. Mauna Kea, HI
LIGO Hanford, WA W. M. KECK OBSERVATORY Mauna Kea, HI #12;19Su m m E r 2012 ENGINEERING & SCIENCE of observatories are giving astronomers, physicists, and engineers from across the globe an unparalleled view in Millimeter- Wave Astronomy (CArMA), which consists of 23 radio telescopes working together to produce high
Well Field Information Development Area: Number of Production Wells: Number of Injection Wells: Number of Replacement Wells: Average Temperature of Geofluid: Sanyal...
Loa, Utah: Energy Resources | Open Energy Information
Login | Sign Up Search Page Edit with form History Facebook icon Twitter icon Loa, Utah: Energy Resources Jump to: navigation, search Equivalent URI DBpedia Coordinates...
Results from the 1995 Stratospheric Ozone Profile Intercomparison at Mauna Loa
. PHAST--A program for simulating ground-water flow, solute transport, and multicomponent geochemical.L., and Charlton, S.R., 2010. PHAST version 2 --A program for simulating groundwater flow, solute transport
Solar Irradiance Anomalies Caused by Clear-Sky Transmission Variations above Mauna Loa: 1958�99
The clear-sky transmission of the atmosphere contributes to determining the amount of solar irradiance that reaches various levels in the atmosphere, which in turn is fundamental to defining the climate of the earth. As of the end of 1999, ...
Ellsworth G. Dutton; Barry A. Bodhaine
T.LoaDS abbreviated systems architecture
The Tactical Logistics Distribution System (T.LoaDS or TLoaDS) is a powerful and flexible simulation application for assessing current or future tactical or sea-based distribution systems. In its current state of development, it is an analytical model ...
Bob Hamber
Subtropical Climatology of Direct Beam Solar Radiation
A climatology of direct beam irradiance has been compiled for Mauna Loa Observatory. A broadband transmittance, calculated from the direct-beam data, has been stratified into clear sky and optically thin and thick cloud regimes; statistics of ...
T. M. Thompson; S. K. Cox
Calibrating Broadband UV Instruments: Ozone and Solar Zenith Angle Dependence
A UV spectroradiometer was installed at Mauna Loa Observatory (MLO), Hawaii, in July 1995. This instrument has been employed to characterize several broadband UV instruments of a type commonly used to estimate erythemal irradiance at many sites ...
Barry A. Bodhaine; Ellsworth G. Dutton; Richard L. McKenzie; Paul V. Johnston
Carbon Dioxide Variability and Atmospheric Circulation
Hourly values of the concentration of atmospheric carbon dioxide at Mauna Loa Observatory (MLO) formed the basis for an investigation of concentration fluctuations on daily to monthly time scales. In agreement with earlier studies we found no ...
James C. Sadler; Colin S. Ramage; Arnold M. Hori
Wind Velocities at the Chajnantor and Mauna Kea Sites and the Effect on MMA Pointing
Wind Velocities at the Chajnantor and Mauna Kea Sites and the Effect on MMA Pointing M.A. Holdaway email: (mholdawa, sfoster, demerson, jcheng, fschwab)@nrao.edu August 9, 1996 Abstract We analyze wind April 1996 for the purposes of understanding the effects of the winds on pointing errors. Both
Groppi, Christopher
The Boulder Atmospheric Observatory
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
The Mount Bachelor Observatory
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.
HAWC Observatory captures first image
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
Black Carbon�s Properties and Role in the Environment: A Comprehensive Review
NOAA/ESRL. Mauna Loa Carbon Dioxide Annual Mean Data.H. Can reducing black carbon emissions counteract globalanalysis of black carbon in soils. Global Biogeochem. Cycle.
Shrestha, Gyami
A New Model to Construct Ice Stream Surface Elevation Profiles and Calculate Contributions to Sea-Level Rise
the injection of carbon dioxide and other greenhouse gasesdirect measurements of carbon dioxide atop Mauna Loa on theof fossil fuel-derived carbon dioxide in the atmosphere from
Adachi, Yosuke
Mobile Climate Observatory on the Pacific
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...
National Astronomical Observatory, Japan
Abstract. At the altitude of 3,370 m on the Peruvian Andes, a 32m antenna owned by the telecommunications company Telef�nica 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
The Lick Observatory Supernova Search
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
MBO: The Mount Bachelor Observatory
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...
The Large Aperture GRB Observatory
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; Gonz�lez, J; Berisso, M Gomez; Grajales, J; Guada, C; Day, W R Guevara; Ishitsuka, J; L�pez, J A; Mart�nez, O; Melfo, A; Meza, E; Loza, P Miranda; Barbosa, E Moreno; Murrugarra, C; N��ez, L A; Ormachea, L J Otiniano; P�rez, 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; Villase�or, L; Wahl, D; Zamalloa, M A
The Mount Washington Observatory�50 Years Old
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
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)
Worldwide R&D of Virtual Observatory
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
Upgrade To The Pierre Auger Cosmic Ray Observatory's Lidar System.
??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
The Astrophysical Multimessenger Observatory Network (AMON)
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. M�sz�ros; G. Te�i?; 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. M�rka; B. J. Owen; I. Taboada
Signals, backgrounds and calibrations in the Sudbury Neutrino Observatory
The Sudbury Neutrino Observatory is a large underground neutrino detector which is presently under construction
Bhaskar Sur; The SNO Collaboration
Hanohano:A Deep Ocean Antineutrino Observatory
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
M. Batygov; S. T. Dye; J. G. Learned; S. Matsuno; S. Pakvasa; G. Varner
Hybrid Performance of the Pierre Auger Observatory
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
Status of the Milagro $\\gamma$ Ray Observatory
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; N�methy, P; Ryan, J M; Schneider, M; Shen, B; Shoup, A L; Sinnis, G; Smith, A J; Sullivan, G W; Thompson, T N; T�mer, T O; Wang, K; Wascko, M O; Westerhoff, S; Williams, D A; Yang, T; Yodh, G B
A Climate Transect through Tropical Montane Rain Forest in Hawaii
Two years of climate data from a transect of three surface meteorological stations on the windward slopes of Mauna Loa, Hawaii, are analyzed. The stations constitute a transect between 700 and 1640 m through the wet, montane rain forest zone ...
James O. Juvik; Dennis Nullet
The Power of Monitoring Stations and a CO2 Fertilization Effect: Evidence from Causal Relationships between NDVI and Carbon Dioxide
Two hypotheses are tested: 1) monitoring stations (e.g., Mauna Loa) are not able to measure changes in atmospheric concentrations of CO2 that are generated by changes in terrestrial vegetation at distant locations; 2) changes in the atmospheric ...
R. K. Kaufmann; L. F. Paletta; H. Q. Tian; R. B. Myneni; R. D. D�Arrigo
Implementing an Observatory Control System-I. A Generic Approach
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
The endless mantra : innovation at the Keck Observatory
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
Operations of and Future Plans for the Pierre Auger Observatory
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.
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
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
The High Altitude Water Cherenkov Observatory
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...
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
Solar Neutrino Observations at the Sudbury Neutrino Observatory
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
A. W. P. Poon
Science Potential of a Deep Ocean Antineutrino Observatory
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
The Fan Observatory Bench Optical Spectrograph (FOBOS)
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
Anisotropy studies with the Pierre Auger Observatory
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
Latitudinal variation of the solar photospheric intensity
We have examined images from the Precision Solar Photometric Telescope (PSPT) at the Mauna Loa Solar Observatory (MLSO) in search of latitudinal variation in the solar photospheric intensity. Along with the expected brightening of the solar activity belts, we have found a weak enhancement of the mean continuum intensity at polar latitudes (continuum intensity enhancement $\\sim0.1 - 0.2%$ corresponding to a brightness temperature enhancement of $\\sim2.5{\\rm K}$). This appears to be thermal in origin and not due to a polar accumulation of weak magnetic elements, with both the continuum and CaIIK intensity distributions shifted towards higher values with little change in shape from their mid-latitude distributions. Since the enhancement is of low spatial frequency and of very small amplitude it is difficult to separate from systematic instrumental and processing errors. We provide a thorough discussion of these and conclude that the measurement captures real solar latitudinal intensity variations.
Rast, Mark P; Meisner, Randle W
ORISE: Capabilities in Climate and Atmospheric Research
Capabilities Capabilities ORISE partners with NOAA to operate climate monitoring network U.S. Climate Reference Network (CRN) station in Hawaii The U.S. Climate Reference Network (CRN) consists of 121 stations throughout the continental U.S., Alaska, Hawaii and Canada. The stations use highly accurate and reliable sensors and gauges to measure temperature, wind speed and precipitation. The network allows scientists to study the climate of an area over sustained periods, from 50 to 100 years. Pictured here is a CRN station at the Mauna Loa Slope Observatory in Hawaii. The Oak Ridge Institute for Science and Education (ORISE) works closely with the National Oceanic and Atmospheric Administration's (NOAA) Atmospheric Turbulence and Diffusion Division (ATDD) to perform lower
Structured Query Language for Virtual Observatory
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
Low Energy Investigations at Kamioka Observatory
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
Neutrino observations from the Sudbury Neutrino Observatory
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.
The HAWC observatory as a GRB detector
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
Low-multiplicity Burst Search at the Sudbury Neutrino Observatory
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
The Solar Dynamics Observatory: Your eye on the Sun
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
The Lidar System of the Pierre Auger Observatory
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
Volcanology and volcanic activity with a primary focus on potential hazard impacts for the Hawaii geothermal project
DOE Green Energy (OSTI)
This annotated bibliography reviews published references about potential volcanic hazards on the Island of Hawaii that are pertinent to drilling and operating geothermal wells. The first two sections of this annotated bibliography list the most important publications that describe eruptions of Kilauea volcano, with special emphasis on activity in and near the designated geothermal subzones. References about historic eruptions from Mauna Loa`s northeast rift zone, as well as the most recent activity on the southern flank of dormant Mauna Kea, adjacent to the Humu`ula Saddle are described. The last section of this annotated bibliography lists the most important publications that describe and analyze deformations of the surface of Kilauea and Mauna Loa volcanoes.
Moore, R.B. [Federal Center, Denver, CO (United States); Delaney, P.T. [2255 North Gemini Drive, Flagstaff, AZ (United States); Kauahikaua, J.P. [Geological Survey, Hawaii National Park, HI (United States). Hawaiian Volcano Observatory
Results from the Milagro Gamma-Ray Observatory
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
Spectral Analysis via the Virtual Observatory: The Service Theossa
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
Installation package for Hyde Memorial Observatory, Lincoln, Nebraska
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
e-government procurement observatory model, design and pilot testing
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 Porr�a; Carlos Pimenta
Visualizing Spatial and Temporal Variability in Coastal Observatories
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
Future development of the PLATO observatory for Antarctic science
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.
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
Evaluation, design, and construction of the Wallace Astrophysical Observatory Camera for astronomical observations
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
A remote sensing observatory for hydrologic sciences: A genesis for scaling to continental hydrology
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
Measurement of Aerosols at the Pierre Auger Observatory
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. Garc�a; 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. Rodr�guez-Fr�as; 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
Technology development for a neutrino astrophysical observatory. Letter of intent
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
Technology Development for a Neutrino AstrophysicalObservatory
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.
Testing the surface detector simulation for the Pierre Auger Observatory
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
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
Calibrating laser test-beams for cosmic-ray observatories
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
Performance of the Pierre Auger Observatory Surface Detector
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
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)
Suomijarvi, Tiina
Trigger and data rates expected for the CTA Observatory
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
New gamma-ray observatory begins operations at Sierra Negra volcano in the
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
Observatory of Renewable Energy for Latin America and the Caribbean | Open
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
Airborne Laser Altimetry Digital Elevation Model, Barrow Environmental Observatory, 0.5m spatial resolution
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
The Pierre Auger Observatory II: Studies of Cosmic Ray Composition and Hadronic Interaction models
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-Mu�iz; 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. B�cker; M. Balzer; K. B. Barber; A. F. Barbosa; R. Bardenet; S. L. C. Barroso; B. Baughman; J. B�uml; J. J. Beatty; B. R. Becker; K. H. Becker; A. Bell�toile; J. A. Bellido; S. BenZvi; C. Berat; X. Bertou; P. L. Biermann; P. Billoir; F. Blanco; M. Blanco; C. Bleve; H. Bl�mer; 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. Concei��o; 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. D�az 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. Fr�hlich; B. Fuchs; R. Gaior; R. F. Gamarra; S. Gambetta; B. Garc�a; D. Garc�a G�mez; 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. G�mez Berisso; P. Gon�alves; D. Gonzalez; J. G. Gonzalez; B. Gookin; D. G�ra; 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. H�randel; 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. K�gl; 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. Kr�mer; D. Kruppke-Hansen; F. Kuehn; D. Kuempel; J. K. Kulbartz; N. Kunka; G. La Rosa; C. Lachaud; P. Lautridou; M. S. A. B. Le�o; D. Lebrun; P. Lebrun; M. A. Leigui de Oliveira; A. Lemiere; A. Letessier-Selvon; I. Lhenry-Yvon; K. Link; R. L�pez; A. Lopez Ag�era; 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. Mart�nez 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. M�ller; M. M�nchmeyer; 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. No�ka; M. Nyklicek; J. Oehlschl�ger; 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. Rodr�guez-Fr�as; G. Ros; J. Rosado
DOE Data Explorer (OSTI)
LAGOVirtual: A Collaborative Environment for the Large Aperture GRB Observatory
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
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
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
Heavy Rain Events over the South-Facing Slopes of Hawaii: Attendant Conditions
Heavy rain events (>100 mm day?1) over the southeast flank of Mauna Loa volcano on the island of Hawaii are examined using surface, rawinsonde, rain gauge, and satellite data. The events occur in the presence of four types of synoptic-scale ...
Kevin Kodama; Gary M. Barnes
Current technology development efforts on the international X-ray Observatory
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
Probing Dark Energy via Neutrino and Supernova Observatories
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
Searching for Double Beta Decay with the Enriched Xenon Observatory
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
Charge Management for Gravitational Wave Observatories using UV LEDs
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
Precision Solar Neutrino Measurements with the Sudbury Neutrino Observatory
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)
The SECIS instrument on the Lomnicky Peak Observatory
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
Fluorescence and Hybrid Detection Aperture of the Pierre Auger Observatory
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
Performance of the Keck Observatory adaptive optics system
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
The Offline Software Framework of the Pierre Auger Observatory
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; Gonz�lez, J; Nellen, L; Paul, T; Porter, T A; Prado, L; Roth, M; Ulrich, R; Veberic, D
Argiro, S; Gonz�lez, J; Nellen, L; Paul, T; Porter, T A; Roth, M; Ulrich, R; Veberic, D
Experiment Profile: COUPP NAME: Chicagoland Observatory for Underground Particle
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
Measurement of the nue and Total 8B Solar Neutrino Fluxes with the Sudbury Neutrino Observatory Phase I Data Set
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
Performance of the Pierre Auger Observatory Surface Array
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
Bertou, X
Performance of the Pierre Auger Observatory surface array
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
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
SNO Data: Results from Experiments at the Sudbury Neutrino Observatory
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.
The offline software framework of the Pierre Auger Observatory
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.
Preliminary systems engineering evaluations for the National Ecological Observatory Network.
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.
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
S. Argiro; S. L. C Barroso; J. Gonzalez; L. Nellen; T. Paul; T. A. Porter; L. Prado Jr.; M. Roth; R. Ulrich; D. Veberic
The Time-Dependent Hydraulic Flow and Dissipation over the Still of Observatory Inlet
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
Measurement of the cosmic ray and neutrino-induced muon flux at the Sudbury neutrino observatory
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 ...
Formaggio, Joseph A.
Great science observatories in the space station era and OWL efforts in Japan
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
A Decade of Ground�Air Temperature Tracking at Emigrant Pass Observatory, Utah
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
Clouds at Arctic Atmospheric Observatories. Part I: Occurrence and Macrophysical Properties
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
Geomagnetic observatory GAN Jakub Velimsky K. Chandra Shakar Rao Lars W. Pedersen Ahmed Muslim
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
Search for Ultra-High Energy Photons with the Pierre Auger Observatory
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
Optical Sky Brightness at Cerro Tololo Inter-American Observatory from 1992 to 2006
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
Bridging the Virtual Observatory and the GRID with the query element
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
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
Description of Atmospheric Conditions at the Pierre Auger Observatory using the Global Data Assimilation System (GDAS)
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.
We analyze the temperature and EUV line emission of a coronal cavity and surrounding streamer in terms of a morphological forward model. We use a series of iron line ratios observed with the Hinode Extreme-ultraviolet Imaging Spectrograph (EIS) on 2007 August 9 to constrain temperature as a function of altitude in a morphological forward model of the streamer and cavity. We also compare model predictions to the EIS EUV line intensities and polarized brightness (pB) data from the Mauna Loa Solar Observatory (MLSO) Mark 4 K-coronameter. This work builds on earlier analysis using the same model to determine geometry of and density in the same cavity and streamer. The fit to the data with altitude-dependent temperature profiles indicates that both the streamer and cavity have temperatures in the range 1.4-1.7 MK. However, the cavity exhibits substantial substructure such that the altitude-dependent temperature profile is not sufficient to completely model conditions in the cavity. Coronal prominence cavities are structured by magnetism so clues to this structure are to be found in their plasma properties. These temperature substructures are likely related to structures in the cavity magnetic field. Furthermore, we find that the model overestimates the EUV line intensities by a factor of 4-10, without overestimating pB. We discuss this difference in terms of filling factors and uncertainties in density diagnostics and elemental abundances.
Kucera, T. A. [NASA/GSFC, Code 671, Greenbelt, MD 20771 (United States); Gibson, S. E.; Schmit, D. J. [HAO/NCAR, P.O. Box 3000, Boulder, CO 80307-3000 (United States); Landi, E. [Department of Atmospheric, Oceanic and Space Science, Space Research Building, University of Michigan, 2455 Hayward St., Ann Arbor, MI 48109-2143 (United States); Tripathi, D. [Inter-University Centre for Astronomy and Astrophysics, Post Bag-4, Ganeshkhind, Pune University Campus, Pune 411 007 (India)
Signatures of storm sudden commencements in geomagnetic H, Y and Z elds at Indian observatories during 19581992
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
An intense SFE and SSC event in geomagnetic H, Y and Z elds at the Indian chain of observatories
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
Results from the Milagro Gamma-Ray Observatory E. Blaufuss a
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
Proceedings of ICRC 2001: 1 c Copernicus Gesellschaft 2001 Status of the Milagro Gamma Ray Observatory
, 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
Enhanced crustal geo-neutrino production near the Sudbury Neutrino Observatory, Ontario, Canada
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
The search for extended air showers at the Jicamarca Radio Observatory
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)
Albedo Influences on Surface UV Irradiance at the Sonnblick High-Mountain Observatory (3106-m Altitude)
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
Spectroscopy of low energy solar neutrinos by MOON -Mo Observatory Of Neutrinos-
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
Introduction SOHO, the Solar and Heliospheric Observatory, is a project of international cooperation between
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
The Science Vision for the Stratospheric Observatory for Infrared Astronomy (SOFIA)
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
Atmospheric CO2 From Flask Air Samples at 10 Sites in the SIO Air Sampling
Flask Air Samples, SIO Network Flask Air Samples, SIO Network Atmospheric CO2 From Flask Air Samples at 10 Sites in the SIO Air Sampling Network Scripps Institution of Oceanography Monitoring Sites Scripps Institution of Oceanography Monitoring Sites Mauna Loa, Hawaii Mauna Loa weekly average CO2 concentrations derived from continuous air samples Barrow, Alaska American Samoa South Pole Daily average CO2 concentrations derived from continuous air samples Alert, NWT, Canada Cape Kumukahi Christmas Island Baring Head Kermadec Island La Jolla Pier La Jolla Pier weekly average CO2 concentrations derived from continuous air samples PDF Documentation available as Atmospheric Carbon Dioxide Concentrations at 10 Locations Spanning Latitudes 82°N to 90°S, (NDP-001a) For information on calibration and some additional literature, go to
Piggyback Tectonics- Long-Term Growth Of Kilauea On The South Flank Of
Piggyback Tectonics- Long-Term Growth Of Kilauea On The South Flank Of Piggyback Tectonics- Long-Term Growth Of Kilauea On The South Flank Of Mauna Loa Jump to: navigation, search GEOTHERMAL ENERGYGeothermal Home Journal Article: Piggyback Tectonics- Long-Term Growth Of Kilauea On The South Flank Of Mauna Loa Details Activities (0) Areas (0) Regions (0) Abstract: Compositional and age data from offshore pillow lavas and volcaniclastic sediments, along with on-land geologic, seismic, and deformation data, provide broad perspectives on the early growth of Kilauea Volcano and the long-term geometric evolution of its rift zones. Sulfur-rich glass rinds on pillow lavas and volcaniclastic sediments derived from them document early underwater growth of a large compositionally diverse alkalic edifice. The alkalic rocks yield 40Ar / 39Ar ages as old as about 275 ka; transitional-composition lavas, which
Historic Sudbury Neutrino Observatory Data, Carried by ESnet, Lives on at
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, firstname.lastname@example.com, +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
Herschel Space Observatory - An ESA facility for far-infrared and submillimetre astronomy
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
Imaging simulations of selected science with the Magdalena Ridge Observatory Interferometer
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
A Search for Astrophysical Burst Signals at the Sudbury Neutrino Observatory
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
Radial Velocity Jitter in Stars from the California and Carnegie Planet Search at Keck Observatory
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
The Measurement of Tropospheric Trace Gases at Fritz Peak Observatory, Colorado, by Long-Path Absorption: OH and Ancillary Gases
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
A Climatology of Gravity Waves and Other Coherent Disturbances at the Boulder Atmospheric Observatory during March�April 1984
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
The Meteorological Model BOLAM at the National Observatory of Athens: Assessment of Two-Year Operational Use
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
The Chicagoland Observatory Underground for Particle Physics cosmic ray veto system
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
A multivariate study of mass composition for simulated showers at the Auger South Observatory
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
Proposal for a quantity based data model in the Virtual Observatory
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
Recent results from the Milagro TeV gamma-ray observatory
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
Radio detection of high-energy cosmic rays at the Pierre Auger Observatory
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
Some recent efforts in chemical hydrogen storage at Loa Alamos
Within the transportation sector, a necessity towards realizing the use of hydrogen (H{sub 2}) as an alternative fuel, is its storage for controlled delivery. The U.S. DOE's Centers of Excellence (CoE) in H{sub 2} storage have pursued different methodologies (metal hydrides, chemical hydrides, and sorbents), for the express purpose of supplanting gasoline's current > 300 mile driving range. Chemical H{sub 2} storage has been dominated by one material, ammonia borane (H3B-NH3, AB), due to its high gravimetric capacity of H{sub 2} (19.6 wt %) and low molecular weight (30.7 g mol{sup -1} ). As such, a number of publications have described H{sub 2} release from amine boranes, yielding various rates depending on the method applied. The viability of any storage system is also dependent on efficient recyclability. Within our CoE we have thus endeavored to find efficient base-metal catalyzed AB dehydrogenation pathways and regeneration schemes for the spent fuel from H{sub 2} depleted AB. We will present some recent results in these areas in this vein.
Gordon, John C [Los Alamos National Laboratory; Davis, Benjamin L [Los Alamos National Laboratory; Burrell, Anthony K [Los Alamos National Laboratory; Nakagawa, Tessui [Los Alamos National Laboratory; Ott, Kevin C [Los Alamos National Laboratory; Smythe, Nathan C [Los Alamos National Laboratory; Sutton, Andrew D [Los Alamos National Laboratory; Henson, Neil J [Los Alamos National Laboratory; Baker, R. Thomas [U. OTTAWA; Hamilton, Charles W [OD VISION, INC.; Dixon, David A [U. ALABAMA; Garner Ill, Edward B [U. ALABAMA; Vasiliu, Monica [U. ALABAMA
Atmospheric Calorimetry above 10$^{19}$ eV: Shooting Lasers at the Pierre Auger Cosmic-Ray Observatory
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
Modeling Optical Turbulence and Seeing over Mauna Kea
Atmospheric turbulence is a primary concern for astronomers. Turbulence causes amplitude and phase fluctuations in electromagnetic waves propagating through the atmosphere, constraining the maximum telescope resolution and resulting in telescope ...
T. Cherubini; S. Businger; R. Lyman; M. Chun
Using ACIS on the Chandra X-ray Observatory as a particle radiation monitor II
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
LISA-2020: An Intermediate Scale Space Gravitational Wave Observatory for This Decade
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
Searches for high frequency variations in the 8-B neutrino flux at the Sudbury neutrino observatory
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
Prospecting for Heavy Elements with Future Far-IR/Submillimeter Observatories
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
Solving the Solar Neutrino Problem 2 km Underground -- the Sudbury Neutrino Observatory
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
Back-to-Back Black Holes decay Signature at Neutrino Observatories
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
Development of the semi-arid climate and environment research observatory over Loess Plateau
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
Atmospheric Profiles at the Southern Pierre Auger Observatory and their Relevance to Air Shower Measurement
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
First results from the MACRO (Monopole, Astophysics, Cosmic Ray Observatory) detector at the Gran Sasso Laboratory
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
Operating Water Cherenkov Detectors in high altitude sites for the Large Aperture GRB Observatory
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.
Performance of the first prototype of the HAWC Gamma Ray Observatory
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; Carrami�ana, Alberto; Alvarez, Cesar
Selection of Image Parameters as the First Step towards Creating a CBIR System for the Solar Dynamics Observatory
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
Near-Neutral Surface Layer Turbulence at the Boulder Atmospheric Observatory Tower: Evidence of Increasing Vertical Turbulence with Height
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 3�5 km west of the tower. Results indicate ...
Brent M. Bowen
Methodology for Water Monitoring in the Upper Troposphere with Raman Lidar at the Haute-Provence Observatory
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
Climatology of aerosol optical depth in north?central Oklahoma: 1992�2008
Aerosol optical depth (AOD) has been measured at the Atmospheric Radiation Measurement Program central facility near Lamont, Oklahoma, since the fall of 1992. Most of the data presented are from the multifilter rotating shadowband radiometer, a narrow?band, interference?filter Sun radiometer with five aerosol bands in the visible and near infrared; however, AOD measurements have been made simultaneously and routinely at the site by as many as three different types of instruments, including two pointing Sun radiometers. Scatterplots indicate high correlations and small biases consistent with earlier comparisons. The early part of this 16 year record had a disturbed stratosphere with residual Mt. Pinatubo aerosols, followed by the cleanest stratosphere in decades. As such, the last 13 years of the record reflect changes that have occurred predominantly in the troposphere. The field calibration technique is briefly described and compared to Langley calibrations from Mauna Loa Observatory. A modified cloudscreening technique is introduced that increases the number of daily averaged AODs retrieved annually to about 250 days compared with 175 days when a more conservative method was employed in earlier studies. AODs are calculated when the air mass is less than six; that is, when the Sun�s elevation is greater than 9.25�. The more inclusive cloud screen and the use of most of the daylight hours yield a data set that can be used to more faithfully represent the true aerosol climate for this site. The diurnal aerosol cycle is examined month?by?month to assess the effects of an aerosol climatology on the basis of infrequent sampling such as that from satellites.
Michalsky, Joseph J.; Denn, Frederick; Flynn, Connor J.; Hodges, G. B.; Kiedron, Piotr; Koontz, Annette S.; Schlemmer, James; Schwartz, Stephen E.
Climatology of aerosol optical depth in North-Central Oklahoma: 1992-2008
Aerosol optical depth (AOD) has been measured at the Atmospheric Radiation Measurement Program central facility near Lamont, Oklahoma, since the fall of 1992. Most of the data presented are from the multifilter rotating shadowband radiometer, a narrow-band, interference-filter Sun radiometer with five aerosol bands in the visible and near infrared; however, AOD measurements have been made simultaneously and routinely at the site by as many as three different types of instruments, including two pointing Sun radiometers. Scatterplots indicate high correlations and small biases consistent with earlier comparisons. The early part of this 16 year record had a disturbed stratosphere with residual Mt. Pinatubo aerosols, followed by the cleanest stratosphere in decades. As such, the last 13 years of the record reflect changes that have occurred predominantly in the troposphere. The field calibration technique is briefly described and compared to Langley calibrations from Mauna Loa Observatory. A modified cloud-screening technique is introduced that increases the number of daily averaged AODs retrieved annually to about 250 days compared with 175 days when a more conservative method was employed in earlier studies. AODs are calculated when the air mass is less than six; that is, when the Sun's elevation is greater than 9.25{sup o}. The more inclusive cloud screen and the use of most of the daylight hours yield a data set that can be used to more faithfully represent the true aerosol climate for this site. The diurnal aerosol cycle is examined month-by-month to assess the effects of an aerosol climatology on the basis of infrequent sampling such as that from satellites.
Michalsky, J.; Schwartz, S.; Denn, F.; Flynn, C.; Hodges, G.; Kiedron, P.; Koontz, A.; Schlemmer, J., and Schwartz, S. E
Predictions for the Cosmogenic Neutrino Flux in Light of New Data from the Pierre Auger Observatory
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
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
Measurement of the Cosmic Ray and Neutrino-Induced Muon Flux at the Sudbury Neutrino Observatory
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.
The Apache Point Observatory Galactic Evolution Experiment: First Detection of High Velocity Milky Way Bar Stars
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
An array of low-background $^3$He proportional counters for the Sudbury Neutrino Observatory
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. Geissb�hler; 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
High-Energy Cosmic Ray Event Data from the Pierre Auger Cosmic Ray Observatory
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.
Effects of mode degeneracy in the LIGO Livingston Observatory recycling cavity
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
On the sensitivity of the HAWC observatory to gamma-ray bursts
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-Vel�zquez, J C; Badillo, C; Barber, A; Baughman, B M; Bautista-Elivar, N; Belmont, E; Ben�tez, E; BenZvi, S Y; Berley, D; Bernal, A; Bonamente, E; Braun, J; Caballero-Lopez, R; Cabrera, I; Carrami�ana, A; Carrasco, L; Castillo, M; Chambers, L; Conde, R; Condreay, P; Cotti, U; Cotzomi, J; D'Olivo, J C; de la Fuente, E; De Le�n, 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; Garc�a-Luna, J L; Garc�a-Torales, G; Garfias, F; Gonz�lez, L X; Gonz�lez, M M; Goodman, J A; Grabski, V; Gussert, M; Guzm�n-Ceron, C; Hampel-Arias, Z; Harris, T; Hays, E; Hernandez-Cervantes, L; H�ntemeyer, 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-Garc�a, R; Mart�nez, H; Mart�nez, J; Mart�nez, L A; Mart�nez, O; Mart�nez-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; P�rez, V; P�rez-P�rez, E G; Perkins, J S; Pretz, J; Ramirez, C; Ram�rez, I; Rebello, D; Renter�a, A; Reyes, J; Rosa-Gonz�lez, 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; Su�rez, 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; V�zquez, O; V�zquez, X; Villase�or, L; Wall, W; Walters, J S; Warner, D; Westerhoff, S; Wisher, I G; Wood, J; Yodh, G B; Zaborov, D; Zepeda, A
Gamma-ray astronomy: From Fermi up to the HAWC high-energy {gamma}-ray observatory in Sierra Negra
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
Selection and reconstruction of very inclined air showers with the Surface Detector of the Pierre Auger Observatory
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.
Weather induced effects on extensive air showers observed with the surface detector of the Pierre Auger Observatory
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
Measurement of the ?[subscript e] and total [superscript 8]B solar neutrino fluxes with the Sudbury Neutrino Observatory phase-III data set
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 ...
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.
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: email@example.com, E-mail: firstname.lastname@example.com, E-mail: firstname.lastname@example.com, E-mail: email@example.com [W. W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305-4085 (United States)
Measurement of the $?_e$ and Total $^{8}$B Solar Neutrino Fluxes with the Sudbury Neutrino Observatory Phase I Data Set
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
The Pierre Auger Observatory scaler mode for the study of solar activity modulation of galactic cosmic rays
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
Performance of MEMS-based visible-light adaptive optics at Lick Observatory: Closed- and open-loop control
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
The Lateral Trigger Probability function for the Ultra-High Energy Cosmic Ray Showers detected by the Pierre Auger Observatory
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-Mu�iz; 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. B�cker; M. Balzer; K. B. Barber; A. F. Barbosa; R. Bardenet; S. L. C. Barroso; B. Baughman; J. B�uml; J. J. Beatty; B. R. Becker; K. H. Becker; A. Bell�toile; J. A. Bellido; S. BenZvi; C. Berat; X. Bertou; P. L. Biermann; P. Billoir; F. Blanco; M. Blanco; C. Bleve; H. Bl�mer; 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. Concei��o; 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 R�o; O. Deligny; H. Dembinski; N. Dhital; C. Di Giulio; J. C. Diaz; M. L. D�az 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. Fr�hlich; B. Fuchs; R. Gaior; R. F. Gamarra; S. Gambetta; B. Garc�a; D. Garc�a G�mez; 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. G�mez Berisso; P. Gon�alves; D. Gonzalez; J. G. Gonzalez; B. Gookin; D. G�ra; 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. H�randel; 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. K�gl; 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. Kr�mer; D. Kruppke-Hansen; F. Kuehn; D. Kuempel; J. K. Kulbartz; N. Kunka; G. La Rosa; C. Lachaud; P. Lautridou; M. S. A. B. Le�o; D. Lebrun; P. Lebrun; M. A. Leigui de Oliveira; A. Lemiere; A. Letessier-Selvon; I. Lhenry-Yvon; K. Link; R. L�pez; A. Lopez Ag�era; 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. Mart�nez 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. M�ller; M. M�nchmeyer; 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. No�ka; M. Nyklicek; J. Oehlschl�ger; 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
Infrared Spectroscopic Data from the Apache Point Observatory Galactic Evolution Experiment (APOGEE), SDSS-III Data Release 10
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/
Ocean pC02 Data from the Lamont-Doherty Earth Observatory of Columbia University, 1994 - 2009
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.
Transport of Stratospheric Air Masses to the Nepal Climate Observatory�Pyramid (Himalaya; 5079 m MSL): A Synoptic-Scale Investigation
This work analyzes and classifies stratospheric airmass transport events (ST) detected at the Nepal Climate Observatory�Pyramid (NCO-P; 27�57?N, 86�48?E, 5079 m MSL) Global Atmospheric Watch�World 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
LIGO Hanford, WA W. M. KECK OBSERVATORY Mauna Kea, HI #12;19Su m m E r 2012 ENGINEERING & SCIENCE in Millimeter- Wave Astronomy (CArMA), which consists of 23 radio telescopes working together to produce high Meter telescope (tMt) is in the works there, too, with tentative plans for it to take its place among
Flury, Markus
Arnold Schwarzenegger Preserving California's
ReproducedfromSoilScienceSocietyofAmericaJournal.PublishedbySoilScienceSocietyofAmerica.Allcopyrightsreserved. DIVISION S-9--SOIL MINERALOGY
2 0 1 0 1 1 California Institute of Technology
Greer, Julia R.
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)
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: email@example.com [Instituto de Astrofisica de Canarias, E-38205 La Laguna, Tenerife (Spain); and others
Chandra X-ray Observatory Detection of Extended X-ray Emission from the Planetary Nebula BD+303639
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.
K�stner, J H; Vrtilek, S D; Dgani, R; Kastner, Joel H.; Soker, Noam; Vrtilek, Saeqa; Dgani, Ruth
Joel H. Kastner; Noam Soker; Saeqa Vrtilek; Ruth Dgani
Measurement of the proton-air cross-section at $\\sqrt{s}=57$ TeV with the Pierre Auger Observatory
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
A Study of the Effect of Molecular and Aerosol Conditions in the Atmosphere on Air Fluorescence Measurements at the Pierre Auger Observatory
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^...
The Catastrophic Flash-Flood Event of 8�9 September 2002 in the Gard Region, France: A First Case Study for the C�vennes�Vivarais Mediterranean Hydrometeorological Observatory
The C�vennes�Vivarais 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; V�ronique Ducrocq; Eric Gaume; Olivier Payrastre; Herv� Andrieu; Pierre-Alain Ayral; Christophe Bouvier; Luc Neppel; Marc Livet; Michel Lang; Jacques Parent du-Ch�telet; Andrea Walpersdorf; Wolfram Wobrock
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
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
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: firstname.lastname@example.com [Max-Plank-Institut fuer Sonnensystemforschung, Max-Planck-Str. 2, D-37191 Katlenburg-Lindau (Germany)
................................................................................................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.
Sommers-Bausch Observatory
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
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
Sudbury Neutrino Observatory
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...
Low energy threshold analysis of the phase I and phase II data sets of the Sudbury neutrino observatory
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
Reconstructing Past Solar Activity using Meridian Solar Observations: the Case of the Royal Observatory of the Spanish Navy (1833-1840)
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
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
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)
Time--Distance Helioseismology Data Analysis Pipeline for Helioseismic and Magnetic Imager onboard Solar Dynamics Observatory (SDO/HMI) and Its Initial Results
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
LARGE-SCALE DISTRIBUTION OF ARRIVAL DIRECTIONS OF COSMIC RAYS DETECTED ABOVE 10{sup 18} eV AT THE PIERRE AUGER OBSERVATORY
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
CONSTRAINTS ON THE ORIGIN OF COSMIC RAYS ABOVE 10{sup 18} eV FROM LARGE-SCALE ANISOTROPY SEARCHES IN DATA OF THE PIERRE AUGER OBSERVATORY
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
Day-night asymmetry of high and low energy solar neutrino events in Super-Kamiokande and in the Sudbury Neutrino Observatory
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
The effect of the geomagnetic field on cosmic ray energy estimates and large scale anisotropy searches on data from the Pierre Auger Observatory
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
High sensitivity measurement of 224Ra and 226Ra in water with an improved hydrous titanium oxide technique at the Sudbury Neutrino Observatory
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
A Search for Neutrinos from the Solar hep Reaction and the DiffuseSupernova Neutrino Background with the Sudbury Neutrino Observatory
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
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.
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: email@example.com [Dipartimento di Fisica, Universita di Palermo, Piazza del Parlamento 1, 90134 Palermo (Italy)
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
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)
Characteristics of geomagnetic cascading of ultra-high energy photons at the southern and northern sites of the Pierre Auger Observatory
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
The Ability of MM5 to Simulate Ice Clouds: Systematic Comparison between Simulated and Measured Fluxes and Lidar/Radar Profiles at SIRTA Atmospheric Observatory
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.
Measurement of the nue and Total 8B Solar Neutrino Fluxes with theSudbury Neutrino Observatory Phase I Data Set
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.
CSIRO GASLAB Network: Individual Flask Measurements of Atmospheric Trace
GASLAB Network GASLAB Network CSIRO GASLAB Network: Individual Flask Measurements of Atmospheric Trace Gases (April 2003) data Data Investigators L.P. Steele, P.R. Krummel, and R.L. Langenfelds Commonwealth Scientific and Industrial Research Organisation (CSIRO) DOI 10.3334/CDIAC/atg.db1021 Data are available for four atmospheric trace gases at nine stationary sites and one moving platform (aircraft over Cape Grim, Tasmania, and Bass Strait, between the Australian continent and Tasmania). The trace gases are carbon dioxide (CO2), methane (CH4), carbon monoxide (CO), and hydrogen (H2). Measurements of δ13C from CO2 are also included in this database. The nine stationary sites are, from north to south: Alert, Canada; Shetland Islands, Scotland; Estevan Point, Canada; Mauna Loa, Hawaii; Cape Ferguson,
Globally Averaged Atmospheric CFC-11 Concentrations: Monthly and Annual
Chlorofluorocarbons » Chlorofluorocarbons » Atmospheric CFC-11 Concentrations Globally Averaged Atmospheric CFC-11 Concentrations: Monthly and Annual Data for the Period 1975-1992 DOI: 10.3334/CDIAC/atg.db1010 data Data (DB1010) Investigator M. A. K. Khalil and R. A. Rasmussen Description This data set presents globally averaged atmospheric concentrations of chlorofluorocarbon 11, known also as CFC-11 or F-11 (chemical name: trichlorofluoromethane; formula: CCl3F). The monthly global average data are derived from flask air samples collected at eight sites in six locations over the period August 1980-July 1992. The sites are Barrow (Alaska), Cape Meares (Oregon), Cape Kumukahi and Mauna Loa (Hawaii), Cape Matatula (American Samoa), Cape Grim (Tasmania), Palmer Station, and the
Growth History Of Kilauea Inferred From Volatile Concentrations In
History Of Kilauea Inferred From Volatile Concentrations In History Of Kilauea Inferred From Volatile Concentrations In Submarine-Collected Basalts Jump to: navigation, search GEOTHERMAL ENERGYGeothermal Home Journal Article: Growth History Of Kilauea Inferred From Volatile Concentrations In Submarine-Collected Basalts Details Activities (4) Areas (2) Regions (0) Abstract: Major-element and volatile (H2O, CO2, S) compositions of glasses from the submarine flanks of Kilauea Volcano record its growth from pre-shield into tholeiite shield-stage. Pillow lavas of mildly alkalic basalt at 2600-1900 mbsl on the upper slope of the south flank are an intermediate link between deeper alkalic volcaniclastics and the modern tholeiite shield. Lava clast glasses from the west flank of Papau Seamount are subaerial Mauna Loa-like tholeiite and mark the contact between the two
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...
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: firstname.lastname@example.com [Department of Astronomy, University of Maryland, College Park, MD 20742-2421 (United States)
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
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
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
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.
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: firstname.lastname@example.com [Laboratory for Atmospheric and Space Physics, University of Colorado at Boulder, Boulder, CO 80301 (United States)
The summit of Mauna Kea is arguably the best site on Earth for astronomical observations and the capital investment in telescopes on Mauna Kea has exceeded $600 million. The success of astronomical observations on Mauna Kea isstrongly influenced ...
S. Businger; R. McLaren; R. Ogasawara; D. Simons; R. J. Wainscoat
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
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)
Solstice Observers and Observatories in Native California
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
Mary Lea Heger Shane: The Lick Observatory
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
Toward Observatory Cloud Computing | Argonne National Laboratory
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...
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
The Status of the STACEE Observatory
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; Sch�tte, D R; Theoret, C G; Williams, D A; M�ller, C
Toward a Resiliency and Vulnerability Observatory Network ...
... is already undertaking extensive investment in its ... vulnerability or more generally, equity, should permeate all ... etc.), parcel and/or tax portfolio data ...
Pierre Auger Observatory Surface Detector Cabling Plan
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
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: firstname.lastname@example.com, E-mail: email@example.com, E-mail: email@example.com, E-mail: email@example.com, E-mail: firstname.lastname@example.com [LESIA, Observatoire de Paris, CNRS, UPMC, Universite Paris Diderot, 5 Place Jules Janssen, 92190 Meudon (France)
Documentation of Probabilistic Fracture Mechanics Codes Used for Reactor Pressure Vessels Subjected to Pressurized Thermal Shock Loa ding: Parts 1 and 2
Pressurized thermal shock (PTS) can impact the safety and operability of PWR vessels with significant radiation embrittlement in the vessel walls. This report documents the results of probabilistic fracture mechanics analysis benchmark studies performed to validate the use of several codes for evaluating vessel PTS. Such benchmark studies provide the industry with a standard reference method for verifying probabilistic fracture mechanics codes used in PTS analyses.
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of transmISSIOn towers: (a) 500 kv; (b) 230-kV steel pole; (e) 69-kV wood tower; (d) 46-kV wood tower. HVDC. A simple one-line drawing of an HVDC link is shown in Fig. 3.36. HVDC lines offer the most economic form
Kammen, Daniel M.
Light management for landscape restoration| Suppression of a model weedy light-demanding pioneer shrub, Ulex europaeus on Mauna Kea Hawai`i.
?? The use of planted forests as a restoration tool has been shown to improve landscape health and may control invasive plant species by canopy� (more)
Perry, Cheyenne Hiapo
Study of the Role of Terrestrial Processes in the Carbon Cycle Based on Measurements of the Abundance and Isotopic Composition of Atmospheric CO2
The main objective of this project was to continue research to develop carbon cycle relationships related to the land biosphere based on remote measurements of atmospheric CO2 concentration and its isotopic ratios 13C/12C, 18O/16O, and 14C/12C. The project continued time-series observations of atmospheric carbon dioxide and isotopic composition begun by Charles D. Keeling at remote sites, including Mauna Loa, the South Pole, and eight other sites. Using models of varying complexity, the concentration and isotopic measurements were used to study long-term change in the interhemispheric gradients in CO2 and 13C/12C to assess the magnitude and evolution of the northern terrestrial carbon sink, to study the increase in amplitude of the seasonal cycle of CO2, to use isotopic data to refine constraints on large scale changes in isotopic fractionation which may be related to changes in stomatal conductance, and to motivate improvements in terrestrial carbon cycle models. The original proposal called for a continuation of the new time series of 14C measurements but subsequent descoping to meet budgetary constraints required termination of measurements in 2007.
Stephen C. Piper; Ralph F. Keeling
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: email@example.com, E-mail: email@example.com [Canada Research Chair. (Canada)
We announce the discovery of a {approx}2 Jupiter-mass planet in an eccentric 11 yr orbit around the K7/M0 dwarf GJ 328. Our result is based on 10 years of radial velocity (RV) data from the Hobby-Eberly and Harlan J. Smith telescopes at McDonald Observatory, and from the Keck Telescope at Mauna Kea. Our analysis of GJ 328's magnetic activity via the Na I D features reveals a long-period stellar activity cycle, which creates an additional signal in the star's RV curve with amplitude 6-10 m s{sup -1}. After correcting for this stellar RV contribution, we see that the orbit of the planet is more eccentric than suggested by the raw RV data. GJ 328b is currently the most massive, longest-period planet discovered around a low-mass dwarf.
Robertson, Paul; Endl, Michael; Cochran, William D.; MacQueen, Phillip J. [Department of Astronomy and McDonald Observatory, University of Texas at Austin, Austin, TX 78712 (United States); Boss, Alan P., E-mail: firstname.lastname@example.com [Department of Terrestrial Magnetism, Carnegie Institution, 5241 Broad Branch Road, NW, Washington DC 20015-1305 (United States)
Atmospheric Trace Gases, Carbon Isotopes, Radionuclides, and Aerosols: Atmospheric Carbon Dioxide Data from the Carbon Dioxide Information Analysis Center (CDIAC)
CDIAC products include numeric data packages, publications, trend data, atlases, models, etc. and can be searched for by subject area, keywords, authors, product numbers, time periods, collection sites, spatial references, etc. Some of the collections may also be included in the CDIAC publication titled Trends Online: A Compendium of Global Change Data. Most datasets, many with numerous data files, are free to download from CDIAC's ftp area. Information related to atmospheric carbon dioxide data includes: Atmospheric Carbon Dioxide and Carbon Isotopes � Atmospheric carbon dioxide records from Mauna Loa, Hawaii � Monthly atmospheric CO2 mixing ratios and other data from the NOAA/CMDL continuous monitoring network � Data from the CSIRO GASLAB Flask Sampling Network � Atmospheric CO2 records from continuous measurements at Jubany Station, Antarctica and from 10 sites in the SIO air sampling network � Historical data from the extended Vostok ice core (2003) and the Siple Station ice core (1997) � Historical records from the Law Dome DE08, DE08-2, and DSS ice cores (1998) � AmeriFlux Carbon Dioxide, Water Vapor, and Energy Balance Measurements � Data from the Canadian Background Air Pollution Monitoring Network � Flask Samples from at U.S.S.R.-Operated Sites (1991) � The CISIRO (Australia) Monitoring Program from Aircraft for 1972-1981 � CO2 Concentrations in Surface Water and the Atmosphere during 1986-1989 NOAA/PMEL Cruises in the Pacific and Indian Oceans � Surface Water and Atmospheric CO2 and Nitrous Oxide Observations by Shipboard Automated Gas Chromatography: Results from Expeditions Between 1977 and 1990 (1992) � IPCC Working Group 1, 1994: Modeling Results Relating Future Atmospheric CO2 Concentrations to Industrial Emissions (1995). New datasets are added when available to the category of atmospheric carbon dioxide.
Mobile Climate Observatory for Atmospheric Aerosols in India
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
GOPAL NARAYANAN's Curriculum Vitae Five College Radio Astronomy Observatory
Languages: FORTRAN, C, Perl, Pascal, BASIC, DCL, C shell, Tcl/Tk. Operating Systems: Linux, Solaris, Sun
Narayanan, Gopal
Evidence for neutrino oscillations in the Sudbury Neutrino Observatory
ux in the Standard Solar Model of the Sun. The long-standingwithin the solar core (inner ?20% of the Sun�s radius). Thesolar neutrino ?ux probe the nuclear fusion reactions fueling the Sun.
Marino, Alysia Diane
Lab scientist receives NASA award for the Solar Dynamics Observatory...
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...
Electron antineutrino search Sudbury Neutrino Observatory 9 Bellerive,
, 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
The Southern Great Plains Site: A Climate Observatory in Oklahoma
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...
NIST Spectral Data for the Chandra X-Ray Observatory
... 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 ...
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
, 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.
Extrasolar planet transit photometry at Wallace Astrophysical Observatory
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
NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia
can be driven. The difference between rise-times is less than 15 usec. Each multivibrator has its own
Clouds at Arctic Atmospheric Observatories. Part II: Thermodynamic Phase Characteristics
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
Formation flying for a Fresnel lens observatory mission
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
John Krizmanic; Gerry Skinner; Neil Gehrels
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
, 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
.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
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-
Los Alamos observatory fingers cosmic ray 'hot spots'
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...
Sensitivity Studies for Third-Generation Gravitational Wave Observatories
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. Gr�f; 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. L�ck; E. Majorana; I. Mandel; V. Mandic; M. Mantovani; I. Martin; C. Michel; Y. Minenkov; N. Morgado; S. Mosca; B Mours; H. M�ller-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. R�diger; L. Santamar�a; 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. Th�ring; 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
Design of light concentrators for Cherenkov telescope observatories
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...
H�nault, F; jocou, L; Kh�lifi, B; Manigot, P; Hormigos, S; Knodlseder, J; Olive, J F; Jean, P; Punch, M
Scottish Observatory for Work and Health University of Glasgow
, 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
Green Bank, West Virginia National Radio Astronomy Observatory
, 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
Historic Sudbury Neutrino Observatory Data, Carried by ESnet...
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...
An Integral Field Spectroscopic Study of Galactic Winds in (U)LIRGs
I propose to carry out a multi-wavelength integral field study of galactic winds to determine the relationship between properties of winds and their hosts. The study of galactic scale winds is a new and growing field. Detailed studies of individual galaxies and their outflows are showing that galactic winds can have a profound effect on their host galaxies and may be part of the solution to several unsolved problems in galaxy evolution. My work will provide new insight into how galactic winds are formed and how they affect galaxy evolution by providing the first statistical study of several galactic wind and host galaxy properties. I will utilize the new WiFeS Integral field unit (IFU) at the Siding Spring Observatory as well as the integral field units on Mauna Kea. This will allow me to cover a wide wavelength range (from 300-24000 nm) and provide access to the entire sky. WiFeS will provide excellent wide-field optical spectra of nearby (U)LIRGS which I will use to determine the relationship between wind structure and spatially resolved host properties using optical emission lines resulting from wind-ISM interaction. My local sample will
Jeffrey Rich
We present parallax and proper motion measurements, near-infrared spectra, and Wide-field Infrared Survey Explorer photometry for the low surface gravity L5{gamma} dwarf 2MASS J035523.37+113343.7 (2M0355). We use these data to evaluate photometric, spectral, and kinematic signatures of youth as 2M0355 is the reddest isolated L dwarf yet classified. We confirm its low-gravity spectral morphology and find a strong resemblance to the sharp triangular shaped H-band spectrum of the {approx}10 Myr planetary-mass object 2M1207b. We find that 2M0355 is underluminous compared to a normal field L5 dwarf in the optical and Mauna Kea Observatory J, H, and K bands and transitions to being overluminous from 3 to 12 {mu}m, indicating that enhanced photospheric dust shifts flux to longer wavelengths for young, low-gravity objects, creating a red spectral energy distribution. Investigating the near-infrared color-magnitude diagram for brown dwarfs confirms that 2M0355 is redder and underluminous compared to the known brown dwarf population, similar to the peculiarities of directly imaged exoplanets 2M1207b and HR8799bcd. We calculate UVW space velocities and find that the motion of 2M0355 is consistent with young disk objects (<2-3 Gyr) and it shows a high likelihood of membership in the AB Doradus association.
Faherty, Jacqueline K. [Department of Astronomy, Universidad de Chile Cerro Calan, Las Condes (Chile); Rice, Emily L.; Cruz, Kelle L.; Nunez, Alejandro [Department of Astrophysics , American Museum of Natural History, Central Park West at 79th Street, New York, NY 10034 (United States); Mamajek, Eric E., E-mail: firstname.lastname@example.com, E-mail: email@example.com [Cerro Tololo Inter-American Observatory, Casilla 603, La Serena (Chile)
Fast reactor safety program. Progress report, January-March 1980
The goal of the DOE LMFBR Safety Program is to provide a technology base fully responsive to safety considerations in the design, evaluation, licensing, and economic optimization of LMFBRs for electrical power generation. A strategy is presented that divides safety technology development into seven program elements, which have been used as the basis for the Work Breakdown Structure (WBS) for the Program. These elements include four lines of assurance (LOAs) involving core-related safety considerations, an element supporting non-core-related plant safety considerations, a safety R and D integration element, and an element for the development of test facilities and equipment to be used in Program experiments: LOA-1 (prevent accidents); LOA-2 (limit core damage); LOA-3 (maintain containment integrity); LOA-4 (attenuate radiological consequences); plant considerations; R and D integration; and facility development.
The Taiwanese-American Occultation Survey: The Multi-Telescope Robotic Observatory
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
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
Brownian force noise from molecular collisions and the sensitivity of advanced gravitational wave observatories
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.
Robert M. La Follette School of Public Affairs 1225 Observatory Drive, Madison, Wisconsin 53706
), and Polillo and Guillen (2005) for the remaining years.11 Finally, since we are interested in the behavior
Sheridan, Jennifer
Multilayer Scintillator Responses for Mo Observatory of Neutrino Experiment Studied Using a Prototype Detector MOON-1
, Toyonaka, Osaka 560-0043 10 Hiroshima University, Higashi Hiroshima, Hiroshima 739-8527 11 VNIIEF, 607188
Engel, Jonathan
NATIONAL Puano ASTRONOMY OBSERVATORY PosT OFFICE Box 2 REPORT
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
Abstract An Investigation of Matter Enhanced Neutrino Oscillation with the Sudbury Neutrino Observatory
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
. 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
Electron antineutrino search at the Sudbury Neutrino Observatory B. Aharmim,5
,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
Direct Evidence for Neutrino Flavor Transformation from Neutral-Current Interactions in the Sudbury Neutrino Observatory
, 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
A Search for TeV Gamma-Ray Burst Emission with the Milagro Observatory
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
Design and Deployment of the Bonne Bay Observatory (B2O) B. de Young
and one underwater connecting the sensors, joined by an armored 1.4 km electro-optic cable. The cable
deYoung, Brad
Development of a Coupled Land Surface Hydrologic Model and Evaluation at a Critical Zone Observatory
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
Regional Weather Patterns during Anomalous Air�Sea Fluxes at the Kuroshio Extension Observatory (KEO)
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
. 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
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
1225 Observatory Drive, Madison, Wisconsin 53706 608-262-3581 / www.lafollette.wisc.edu
natural gas power plants; ad- vances in ball bearings and tires for bicycles enabled development of auto
Prospects for Localization of Gravitational Wave Transients by the Advanced LIGO and Advanced Virgo Observatories
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; D�az, 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; Endr�czi, 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; G�sp�r, 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; Gonz�lez, G; Gordon, N; Gorodetsky, M L; Gossan, S; Go�ler, 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
Investigations of the cascade of Langmuir wave turbulence over HAARP Observatory in Gakona, Alaska
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
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
What NEON Is The National Ecological Observatory Network (NEON) is a continental-scale
at the Harvard Forest, Petersham, MA 2. Mid-Atlantic site (to be determined) 3. Southeast site based
Patterson, Bruce D.
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.
at the federal level. By and large, these attempts such as Project XCEL have had very limited success
MilagroA TeV Observatory for Gamma Ray Bursts
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
A Search for TeV Emission from Active Galaxies using the Milagro Observatory
: 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
Laboratory, Field, and Modeling Analysis of Solute Transport Behavior at the Shale Hills Critical Zone Observatory.
??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
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
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
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. D�az; 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. Endr�czi; 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. G�sp�r; 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. Gonz�lez; N. Gordon; M. L. Gorodetsky; S. Gossan; S. Go�ler; 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
Nuclear Stellar Populations in the Infrared Space Observatory Atlas of Bright Spiral Galaxies
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
.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
32ND INTERNATIONAL COSMIC RAY CONFERENCE, BEIJING 2011 The HEAT Telescopes of the Pierre Auger Observatory
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.
LABORATORY FOR ATMOSPHERIC ACOUSTICS SCRIPPS INSTITUTION OF OCEANOGRAPHY INSTITUTE OF GEOPHYSICS & PLANETARY PHYSICS Pion Flat Observatory
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
Application of Lidar Data to Assist Airmass Discrimination at the Whistler Mountaintop Observatory
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
EUV multilayer coatings for the Atmospheric Imaging Assembly instrument aboard the Solar Dynamics Observatory
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
Lunar landing : dynamic operator interaction with multi-modal automation systems
The ability of operators to "gracefully transition" (maintaining control and awareness of the system without excessive workload or decrements in flight performance) between levels of automation (LOA) in several case studies ...
Hainley, Christopher James, Jr
Statistical models for analyzing human genetic variation
G. J. McDonald, A. Tandon, A. Waliszewska, K. Penney, R. G.Alicja Waliszewska, Arti Tandon, Robin R. Lincoln, CariA. Wal- iszewska, A. Tandon, R. R. Lincoln, C. DeLoa, S. A.
Sankararaman, Sriram
Elements heavier than the iron group are found in nearly all halo stars. A substantial number of these elements, key to understanding neutron-capture nucleosynthesis mechanisms, can only be detected in the near-ultraviolet. We report the results of an observing campaign using the Space Telescope Imaging Spectrograph on board the Hubble Space Telescope to study the detailed heavy-element abundance patterns in four metal-poor stars. We derive abundances or upper limits from 27 absorption lines of 15 elements produced by neutron-capture reactions, including seven elements (germanium, cadmium, tellurium, lutetium, osmium, platinum, and gold) that can only be detected in the near-ultraviolet. We also examine 202 heavy-element absorption lines in ground-based optical spectra obtained with the Magellan Inamori Kyocera Echelle Spectrograph on the Magellan-Clay Telescope at Las Campanas Observatory and the High Resolution Echelle Spectrometer on the Keck I Telescope on Mauna Kea. We have detected up to 34 elements heavier than zinc. The bulk of the heavy elements in these four stars are produced by r-process nucleosynthesis. These observations affirm earlier results suggesting that the tellurium found in metal-poor halo stars with moderate amounts of r-process material scales with the rare earth and third r-process peak elements. Cadmium often follows the abundances of the neighboring elements palladium and silver. We identify several sources of systematic uncertainty that must be considered when comparing these abundances with theoretical predictions. We also present new isotope shift and hyperfine structure component patterns for Lu II and Pb I lines of astrophysical interest.
Roederer, Ian U.; Thompson, Ian B. [Carnegie Observatories, Pasadena, CA 91101 (United States); Lawler, James E. [Department of Physics, University of Wisconsin, Madison, WI 53706 (United States); Sobeck, Jennifer S. [Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637 (United States); Beers, Timothy C. [National Optical Astronomy Observatory, Tucson, AZ 85719 (United States); Cowan, John J. [Homer L. Dodge Department of Physics and Astronomy, University of Oklahoma, Norman, OK 73019 (United States); Frebel, Anna [Massachusetts Institute of Technology, Kavli Institute for Astrophysics and Space Research, Cambridge, MA 02139 (United States); Ivans, Inese I. [Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112 (United States); Schatz, Hendrik [Department of Physics and Astronomy, Michigan State University, E. Lansing, MI 48824 (United States); Sneden, Christopher [Department of Astronomy, University of Texas at Austin, Austin, TX 78712 (United States)
Astronomical Site Ranking Based on Tropospheric Wind Statistics
We present comprehensive and reliable statistics of high altitude wind speeds and the tropospheric flows at the location of five important astronomical observatories. Statistical analysis exclusively of high altitude winds point to La Palma as the most suitable site for adaptive optics, with a mean value of 22.13 m/s at the 200 mbar pressure level. La Silla is at the bottom of the ranking, with the largest average value 200 mbar wind speed(33.35 m/s). We have found a clear annual periodicity of high altitude winds for the five sites in study. We have also explored the connection of high to low altitude atmospheric winds as a first approach of the linear relationship between the average velocity of the turbulence and high altitude winds (Sarazin & Tokovinin 2001). We may conclude that high and low altitude winds show good linear relationships at the five selected sites. The highest correlation coefficients correspond to Paranal and San Pedro Martir, while La Palma and La Silla show similar high to low altitude wind connection. Mauna Kea shows the smallest degree of correlation, which suggests a weaker linear relationship. Our results support the idea of high altitude winds as a parameter for rank astronomical sites in terms of their suitability for adaptive optics, although we have no evidence for adopting the same linear coefficient at different sites. The final value of this linear coefficient at a particular site could drastically change the interpretation of high altitude wind speeds as a direct parameter for site characterization.
B. Garcia-Lorenzo; J. J. Fuensalida; C. Munoz-Tunon; E. Mendizabal
First results from the MIT optical rapid imaging system (MORIS) on the IRTF: A stellar occultation by Pluto and a transit by exoplanet XO-2b
We present a high-speed, visible-wavelength imaging instrument: MORIS (the MIT Optical Rapid Imaging System). MORIS is mounted on the 3 m Infrared Telescope Facility (IRTF) on Mauna Kea, Hawaii. Its primary component is ...
Gulbis, Amanda A. S.
L. S. , and Chin, J. S. , Carbon dioxide variations at MaunaX Stratospheric air X Carbon dioxide X Ozone X Human race Xas these. The mass of carbon dioxide is 7 thousand times
Johnston, Harold S.
quantifier les principaux processus de solidification magmatiques à l'oeuvre dans la genèse des basaltes de type "pipe" sous le rift du Mauna Ulu. Le mag
Analysis of 2-axis pencil beam sonar microbathymetric measurements of mine burial at the Martha's Vineyard Coastal Observatory
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
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)
Probing the origin of cosmic-rays with extremely high energy neutrinos using the IceCube Observatory
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. B�ser; 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. D�az-V�lez; 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. Gl�senkamp; A. Goldschmidt; G. Golup; J. G. Gonzalez; J. A. Goodman; D. G�ra; 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. Kl�s; S. R. Klein; J. -H. K�hne; G. Kohnen; H. Kolanoski; L. K�pke; 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. L�nemann; O. Mac�as; 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. P�rez de los Heros; C. Pfendner; D. Pieloth; D. Pieloth; E. Pinat; J. Posselt; P. B. Price; G. T. Przybylski; L. R�del; 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. Sch�neberg; A. Sch�nwald; 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. St��l; E. A. Strahler; R. Str�m; G. W. Sullivan; H. Taavola; I. Taboada; A. Tamburro; A. Tepe; S. Ter-Antonyan; G. Te�i?; 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
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
Smithsonian Astrophysical Observatory To: M. Cappi, Strong Gravity SDT/YB Team, XMS team mrg-2010-02v2
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
Classification of Ice Crystal Shapes in Midlatitude Ice Clouds from Three Years of Lidar Observations over the SIRTA Observatory
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
79Fermi Observatory Measures the Lumps in Space An artistic impression of two gamma-ray photons
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
Evaluation of the Parameter Sensitivities of a Coupled Land Surface Hydrologic Model at a Critical Zone Observatory
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
Class.Quantum Grav. 10 (1993) S1854185. Printed in the UK The Laser InterferometerGravitationalWave Observatory
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
The Great Observatories Origins Deep Survey - VLT/FORS2 Spectroscopy in the GOODS-South Field
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
The Great Observatories Origins Deep Survey. VLT/FORS2 Spectroscopy in the GOODS-South Field: Part III
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
Development and characterization of an observatory-class, broadband, non-fedback, leaf-spring interferometric seismometer
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.
Building ISOC Status Displays for the Large AreaTelescope aboard the Gamma Ray Large Area Space Telescope (GLAST) Observatory
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
NIST: Freq. Observ. Interstellar Molec. Micro. Trans. - Table 3
... Experiment Max-Planck-Institut f�r Radioastronomie European Southern Observatory Onsala Space Observatory Llano de Chanjnantor, Chile. ...
Observations of the Hubble Deep Field with the Infrared Space Observatory. V. Spectral Energy Distributions, Starburst Models and Star Formation History
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
arXiv:nuclex/0309004 Measurement of the Total Active 8 B Solar Neutrino Flux at the Sudbury Neutrino Observatory with
. 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
PHYSICAL REVIEW C 75, 045502 (2007) Determination of the # e and total 8 B solar neutrino fluxes using the Sudbury Neutrino Observatory
. 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
Measurement of the rate of e + d ! p + p + e interactions produced by 8 B solar neutrinos at the Sudbury Neutrino Observatory
. 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
Critical-angle transmission grating spectrometer for high-resolution soft x-ray spectroscopy on the International X-ray Observatory
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.
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)
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
The Ability of MM5 to Simulate Ice Clouds: Systematic Comparison between Simulated and Measured Fluxes and Lidar/Radar Profiles at the SIRTA Atmospheric Observatory
The ability of the fifth-generation Pennsylvania State University�NCAR 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
Dept. of Sol Science, UW-Madison/UW-Extension, 1525 Observatory Dr., Madison, WI 53706/608-262-0485 November 2010 Issue #2 2010
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.
Assessment of impact of degree of automation on human roles: the experts' analysis using gaming
This paper describes the results of the two assessments performed to evaluate the impact of increasing levels of automation (LoA) on Human Factors aspects and the impact on their responsibilities and interactions. This activity has been developed within ... Keywords: ATM, assessment, automation, gaming, human factors
R. Casar, A. Arranz, B. Escribano, A. Grosskreutz, R. Garcia, R. Suikat, M. Jipp, G. D. R. Zon, M. Joosse
CENTER FOR ENVIRONMENTAL RADIATION STUDIES Texas Tech University
of decommissioning old nuclear power plants, building and commissioning new plants and waste disposal. The panel also Executive and the Nuclear Decommissioning Authority. The LoA group work together in areas of common interestEPSRC/STFC Review of Nuclear Physics and Nuclear Engineering A report prepared for EPSRC and STFC
Rock, Chris
comparable, or nearly so, to energy supplied from the utility power grid. The geographic region is important contacted 143 major electric utilities, account- ing for more than 80% of the U.S. installed electric-2-3 APPROACH #12;Spotlighting Hawaii's Mauna Lani Bay Hotel This sprawling hotel had acres of roof space
Perez, Richard R.
Mountain Breathing Revisited�the Hyperventilation of a Volcano Cinder Cone
During 23 hours of fresh to strong winds in December 1975, air flowed rapidly and continuously out of a drill hole in the top of the summit cone of Mauna Kea volcano, Hawaii. Measurements made during this outflow indicate that the air entered the ...
Alfred H. Woodcock
Extended Commissioning and Calibration of the Dual-Beam Imaging Polarimeter
In our previous paper (Masiero et al. 2007) we presented the design and initial calibrations of the Dual-Beam Imaging Polarimeter (DBIP), a new optical instrument for the University of Hawaii's 2.2 m telescope on the summit of Mauna Kea, Hawaii. In this followup work we discuss our full-Stokes mode commissioning including crosstalk determination and our typical observing methodology.
Joseph Masiero; Klaus Hodapp; David Harrington; Haosheng Lin
Design criteria for a self-actuated shutdown system to ensure limitation of core damage. [LMFBR
Safety-based functional requirements and design criteria for a self-actuated shutdown system (SASS) are derived in accordance with LOA-2 success criteria and reliability goals. The design basis transients have been defined and evaluated for the CDS Phase II design, which is a 2550 MWt mixed oxide heterogeneous core reactor. A partial set of reactor responses for selected transients is provided as a function of SASS characteristics such as reactivity worth, trip points, and insertion times.
Deane, N.A.; Atcheson, D.B.
, Abastumani Astrophysical Observatory, Al. Kazbegi ave. 2a, Tbilisi 380060, Georgia Received 24 March 2003
DOI: 10.1002/adma.200802222 Materials Science in the Developing
Observatory located in the Karoo, Sutherland, etc.). For a South African academic institution intending
Rosei, Federico
drilling team from Dalhousie University and Lamont-Doherty Geo- logical Observatory, which encoun- tered fluid
Bresee, J. C.
UNIVERSITE TOULOUSE III -PAUL SABATIER En vue de l'obtention du
-RQMT-000804 JWST Project Science Objectives and Requirements JWST-HDBK-002046 JWST Observatory Constraints
astro-ph/001152728Nov2000 submitted to ApJ Letters 2000 Oct 21, revised 2000 Nov 28
Observatories, 813 Santa Barbara St., Pasadena CA 91101 8 Universidad de Zaragoza, Grupo de Mecanica Espacial
Coppi, Paolo
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
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: email@example.com, E-mail: firstname.lastname@example.com [Steward Observatory, University of Arizona, Tucson, AZ 85721 (United States)
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.
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
Spectral Characteristics of the Convective Boundary Layer Over Uneven Terrain
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
Atmospheric Radiation Measurement Program
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...
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
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.
The Design and Development of an Irish Sea Passenger-Ferry-Based Oceanographic Measurement System
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
An Update on the Status of the Pulsar?ALFA Survey
The Pulsar?ALFA (PALFA) survey is designed to search the Galactic plane for pulsars at 1.4 GHz using the Arecibo Observatory�s 7?beam ALFA receiver. The 64??s sampling time
P. Lazarus; The PALFA Consortium
Fermilab Today
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...
SciTech Connect: "smart grid"
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...
EUV beam line moves to PML
... Explorer (ACE), and the new twin Solar Terrestrial Relations Observatory (STEREO) spacecraft, America's space-weather early-warning systems ...
Synchrotron Programs and Projects
... Synchrotron Radiation-Based Calibrations for Space Weather Prediction Last ... NASA launched the Solar Dynamics Observatory ( SDO ) satellite on ...
A Unique Institution: The National Bureau of Standards, 1950 ...
... in 1964. Two years later, Raymond Davis, Jr., opened a "neutrino observatory" deep in South Dakota's Homestake gold mine. ...
The APO 3.5-meter remote observing program--2002 and beyond Bruce Gillespie*
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.
G. K. Shenoy P. J. Viccaro
at the Brookhaven National Laboratory in New Yo the Stanford hrotron Radiation Laboratory (SSRL). which uses of 1013 ph/sec/O.l%BW/mrad 8. SSRL 3.0 100 12.7 0.79 4.7 0.48 2.0 0.28 CHESS 5.5 L.,Oa 32.0 0.57 11.5 0 --- _.-------- , --=------~~--- ,, -- \\", """', ., \\-'-. \\ \\ ", NSLS (2.5 GeV, 500 rnA) \\ \\ '.... 6-GeV (1 rnA) \\ '.. SSRL (3.0 GeV, 100 rnA) \\ \\ " \\ CHESS (5.5 Ge
Kemner, Ken
Sixth International Conference on Precipitation: Predictability of Rainfall at the Various Scales. Abstracts
This volume contains abstracts of the papers presented at the Sixth International Conference on Precipitation: Predictability of Rainfall at the various scales, held at the Mauna Lani Bay and Bungalows, Hawaii, June 29 - July 1, 1998. The main goal of the conference was to bring together meteorologists, hydrologists, mathematicians, physicists, statisticians, and all others who are interested in fundamental principles governing the physical processes of precipitation. The results of the previous conferences have been published in issues of the Journal of Geophysical Research and Journal of Applied Meteorology. A similar format is planned for papers of this conference.
On acoustic wave generation in uniform shear flow G. Gogoberidze
, Abastumani Astrophysical Observatory, Tbilisi 0160, Georgia P. J. Morrison Department of Physics Department, Tbilisi State University, Tbilisi 0179, Georgia (Dated: October 2004) Abstract The linear
Morrison, Philip J.,
Three-dimensional magnetotelluric characterization of the Coso...
has been acquired over the east flank of the Coso geothermal system, CA, USA. Due to production related electromagnetic (EM) noise the permanent observatory at Parkfield, CA was...
Single-Column Modeling R. D. Cess Marine Sciences Research Center
measured by the upward facing pyranometer at the Boulder Atmospheric Observatory (BAO) tower located approximately 25 km north of Denver. The tower is surrounded by dry-plains...
Section 73
at the Boulder Atmospheric Observatory (BAO). The BAO has an instrumented 300-m tower with 5-min measurements of temperature and relative humidity available at the surface...
User Facilities in the Environmental Assessment Division (EVS...
The ARM Climate Research Facility, a Department of Energy (DOE) Office of Science user facility, provides data from strategically located climate observatories around the...
Acronyms and Abbreviations
Observatories Programme GOS Global Observing System (WMO and WWW) GOS &09:Geomagnetic Observing System GPC Global Processing Center GPCC Global Precipitation Climatology...
Properties of Powder Metallurgy Beryllium
Table 19 Some production applications of wrought hot pressed beryllium...Type of material Special characteristics Solar cell boards�??Orbiting Geophysical Observatory
Towards a Neutron Microscope
Towards a Neutron Microscope. Summary: ... The novel lens is a Wolter Optic similar in design to the telescope of the CHANDRA x-ray observatory. ...
--No Title--
UAO Urban Atmospheric Observatory Instrumentation Network Verification Facility - New York City A Center for the Development and Evaluation of Response Software and Instrumentation...
NETL: Methane Hydrates - DOE/NETL Projects
Horizon spill approximately 10 miles from the observatory showed increased levels of methane at two depths where detectable levels had not been seen in the past. The evidence...
Fermilab | Science at Fermilab | Questions for the Universe ...
someday shed light on dark matter: Large Hadron Collider, CERN, Geneva, Switzerland Sloan Digital Sky Survey, Fermilab, Batavia, IL VERITAS, Fred Lawrence Whipple Observatory,...
Nuclear Science Division Annual Report 1995-1996
Observatory Cosmic Gamma-Ray Bursts and Soft Gamma RepeatersAxions Theories of Gamma-Ray Bursts Origin Extracting Power
Authors, Various
Speeds and Arrival Times of Solar Transients Approximated by Self ...
Abstract The NASA Solar TErrestrial RElations Observatory (STEREO) mission offered the possibility to forecast the arrival times, speeds, and directions of solar �...
Earth Observatory of Columbia University, and the U.S. Department of Energy's National Energy Technology Lab. The science team was led by Dr. Timothy Collett (USGS) and...
Optical observations of afterglows of gamma ray bursts localized by the high energy transient explorer.
??In this thesis, I discuss observations of the optical afterglows of seven HETE GRBs, carried out mainly with the Magellan Telescopes at Las Campanas Observatory� (more)
Dullighan, Allyn, 1978-
Massachusetts | Department of Energy
July 25, 2012 This observatory is part of an air particles research initiative at Cape Cod National Seashore in Massachusetts, and includes dozens of sophisticated instruments...
Bluer Skies and Brighter Days: The U.S. and India Collaborate...
Articles This observatory is part of an air particles research initiative at Cape Cod National Seashore in Massachusetts, and includes dozens of sophisticated instruments...
Department of Energy Announces $7 Million in Funding for Climate...
Collaboration This observatory is part of an air particles research initiative at Cape Cod National Seashore in Massachusetts, and includes dozens of sophisticated instruments...
Celebrates Progress on Detector Array and Presents First Science Results MALARGE, Argentina -- Scientists of the Pierre Auger Observatory, a project to discover the origins of...
Inquiring Minds
particles. The observatory, currently being built on a vast plain in western Argentina, will use a collection of particle detectors spread over an area the size of Rhode...
About Fermilab - History
Michael Witherell named Fermilab's fourth director. March 17, 1999: Groundbreaking in Argentina for the southern hemisphere site of the Pierre Auger Observatory June 1, 1999:...
Energy Crossroads: Weather Data Resources | Environmental Energy...
the United States, three counting stations in Canada, and two counting stations in Argentina. Astronomical Applications Department of the U.S. Naval Observatory The Astronomical...
construction and commissioning of XMASS 800kg detector Jing Liu IPMU, Kamioka Observatory Abstract: The XMASS 800kg detector, aiming primarily at the dark matter search, is...
Tech Beat July 9, 2008
... With the aim of improving forecasts of space weather, NASA's Solar Dynamics Observatory will peer deep inside the sun, to where the solar ...
NIST Image Gallery: Image Details
... Description: With the aim of improving forecasts of space weather NASA's Solar Dynamics Observatory will peer deep inside the sun, to where the ...
National Nuclear Security Administration (NNSA)
1 1 II.CONTRACT ID CODE ~AGE 1 of AMENDMENT OF SOLICITATIONIMODIFICATION OF CONTRACT PAGES AC 5. PROJECT NO. (If applicable) 3. EFFECTNE DATE 2. AMENDMENTfMODIFICA TION NO. 4. REQUISITIONIPURCHASE REQ. NO. See Block 16c. NOPR 7. ADMINISTERED BY (If other than Item 6) CODE 05008 6. ISSUED BY CODE 05008 U.S. Department of Energy National Nuclear Security Administration U.S. Department of Energy National Nuclear Security Administration P.O. Box 2050 Oak Ridge, TN 37831 P.O. Box 2050 Oak Ridge, TN 37831 9A. AMENDMENT OF SOLICITATION NO. 8. NAME AND ADDRESS OF CONTRACTOR (No., street, county, state, ZIP Code) Babcock & Wilcox Technical Services Y-12, LLC P.O. Box 2009 MS 8014 9B. DATED (SEE ITEM 11) Oak Ridge, TN 37831-8014 lOA. MODIFICATION OF CONTRACT/ORDER NO.
Microsoft Word - DE-NR0000031-FY11.doc
.~._-_._.-_._.._----------------------- .~._-_._.-_._.._----------------------- AMENDMENT OF SOLICITATlON/MOOlFICATlON OF CONTRACT II. CONTRACT 10 CODE IPAGE~S 1 I 192 2. AMENDMENTIMODlFICATIONNO. 3. EFFECTIVE DATE 4. REQUISInONlPtJRCHASE REQ. NO. r PROJECT NO. (If~") 032 See Block 16C 6. ISSUED BY CODE 01111 7. ADMINISTEREDBY (lfotllerlMnltem 6) CODE T01111 NRLFO - PGH NRLFO - PGH US DEPARTMENT OF ENERGY US DEPARTMENT OF ENERGY NAVAL REACTORS LABORATORY FIELD OFFICE - PGH NAVAL REACTORS LABORATORY FIELD OFF POBOX 109 POBOX 109 WEST MIFFLIN PA 15122-0109 WEST MIFFLIN PA 15122-0109 6. NAMEAND "'DDRESS OF CONTRACTOR /NO *. _, ** _. _ rtd ZIPCodo} ~ 9***.AMENDMENTOF SOLICIT"'TION NO. BECHTEL MARINE PROPULSION CORPORATION ATTN JOHN E POTTS 98. O"'TED (SEE ITEM 11) 50 BEALE ST SAN FRANCISCO CA 941051813 lOA. MODIFICATIONOF CONTR"'CTIORDER NO. X DE-NROOOO031 lOB. D"'TED (SEE ITEM 13)
Auger Finance Board Meeting 16 November 2008 P. Mantsch
. Mantsch Observatory Maintenance Responsibilities Operations Readiness Reviews The project management Maintenance Responsibilities ï The overall responsibility for the operation of a detector or support system remains with the Task Group. ï The routine maintenance of a system is assumed by the Observatory staff
Creation and Detection of Cerenkov Light
Creation and Detection of Ÿ Cerenkov Light in the Sudbury Neutrino Observatory Michael David Lay Cerenkov Light in the Sudbury Neutrino Observatory Michael David Lay Wolfson College, Oxford Thesis on the detection of Ÿ Cerenkov photons to determine the location of an interaction in the detector and to deduce
LIGO-G000306-00-M Einstein's Theory of Gravitation
Hanford Observatory #12;LIGO-G000306-00-M LIGO Hanford Observatory #12;LIGO-G000306-00-M LIGO Plans schedule 1996 Construction Underway (mostly civil) 1997 Facility Construction (vacuum system) 1998 Interferometer Construction (complete facilities) 1999 Construction Complete (interferometers in vacuum) 2000
Frey, Raymond E.
Data challenges of time domain astronomy
Astronomy has been at the forefront of the development of the techniques and methodologies of data intensive science for over a decade with large sky surveys and distributed efforts such as the Virtual Observatory. However, it faces a new data deluge ... Keywords: Astronomy, Classification, Time domain, Virtual observatory
Matthew J. Graham; S. G. Djorgovski; Ashish Mahabal; Ciro Donalek; Andrew Drake; Giuseppe Longo
Observing Cold Dust with Herschel / SPIRE
A major component of the emission of many galaxies is in the Far Infrared and the Sub?mmillimeter. UV photons from stars are absorbed by dust and re?emitted at longer wavelengths. Fairly cold dust was found in large spirals by the Infrared Space Observatory and the Spitzer Observatory but their longest wavelength filters were centered at 200 and 160 microns respectively
Bernhard Schulz; The SPIRE Consortium
The 1998 November 14 Occultation of GSC 0622-00345 by Saturn. I. Techniques for Ground-Based Stellar Occultations
On 1998 November 14, Saturn and its rings occulted the star GSC 0622-00345. We observed atmospheric immersion with NSFCAM at the National Aeronautics and Space Administration's Infrared Telescope Facility on Mauna Kea, Hawaii. Immersion occurred at 55.5\\circ S planetocentric latitude. A 2.3 {\\mu}m, methane-band filter suppressed reflected sunlight. Atmospheric emersion and ring data were not successfully obtained. We describe our observation, light-curve production, and timing techniques, including improvements in aperture positioning, removal of telluric scintillation effects, and timing. Many of these techniques are known within the occultation community, but have not been described in the reviewed literature. We present a light curve whose signal-to-noise ratio per scale height is 267, among the best ground-based signals yet achieved, despite a disadvantage of up to 8 mag in the stellar flux compared to prior work.
Harrington, Joseph; 10.1088/0004-637X/716/1/398
Direct-Current Resistivity At Kawaihae Area (Thomas, 1986) | Open Energy
Kawaihae Area (Thomas, 1986) Kawaihae Area (Thomas, 1986) Jump to: navigation, search GEOTHERMAL ENERGYGeothermal Home Exploration Activity: Direct-Current Resistivity At Kawaihae Area (Thomas, 1986) Exploration Activity Details Location Kawaihae Area Exploration Technique Direct-Current Resistivity Survey Activity Date Usefulness not indicated DOE-funding Unknown Notes In addition to the aeromagnetic data, the field survey program in Kawaihae included six Schlumberger resistivity soundings between Kawaihae and Waimea (Kauahikaua and Mattice, 1981). The results of these sounding (Fig. 35) detected apparent resistivity differences in the surface rock depending on whether the soundings were done on Kohala or Mauna Kea lavas (Figs 36, 37), whereas uniform resistivities of 650- 850 ohm.m were found at depths of
Column Integrated Aerosol Properties During the May Column Integrated Aerosol Properties During the May 2003 Aerosol IOP P. Ricchiazzi and C. Gautier Institute for Computational Earth System Science (ICESS) University of California Santa Barbara, California Background Some recent studies of clear-sky radiation indicate that current radiative transfer (RT) models tend to underestimate atmospheric absorption when the aerosol optical depth is small and standard aerosol properties are assumed. This so-called clear-sky anomaly is manifested in predicted levels of diffuse radiation significantly above those observed at Southern Great Plains (SGP) and other sites in the continental U.S. (e.g., Halthore et al. 1998 GRL). In general, observations made at pristine sites do not show a discrepancy (Barnard and Powell 2001: [North Slope Alaska] 2001; Kato et al. 1999: [Mauna
Research Highlight
Characterizing Clouds at Arctic Atmospheric Observatories Characterizing Clouds at Arctic Atmospheric Observatories Download a printable PDF Submitter: Shupe, M., University of Colorado Area of Research: Cloud Distributions/Characterizations Working Group(s): Cloud Life Cycle Journal Reference: Shupe MD, VP Walden, E Eloranta, T Uttal, JR Campbell, SM Starkweather, and M Shiobara. 2011. "Clouds at Arctic atmospheric observatories, part I: occurrence and macrophysical properties." Journal of Applied Meteorology and Climatology, 50(3), 626-644. Shupe MD. 2011. "Clouds at Arctic atmospheric observatories, part II: thermodynamic phase characteristics." Journal of Applied Meteorology and Climatology, 50(3), 645-661. Figure 1: (a) Annual cycles of monthly mean cloud occurrence fraction at six Arctic atmospheric observatories. The average cloud fraction for all
HAWC Observatory captures first image HAWC Observatory captures first image April 30, 2013 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 construction inside the Parque Nacional Pico de Orizaba, a Mexican national park. Although only 10 percent of the observatory is constructed, the team has made its first astrophysical image-a shadow in the detected directions of cosmic rays caused by the Moon. Full-time operations at HAWC will begin this summer with one third of the observatory, making HAWC the most sensitive, wide field of view, continuously operating gamma-
LOS ALAMOS, N.M., Aug. 21, 2013-The High-Altitude Water Cherenkov (HAWC)
gamma-ray observatory begins gamma-ray observatory begins operations at Sierra Negra volcano in the state of Puebla, Mexico August 21, 2013 New site to observe supernovas and supermassive black holes LOS ALAMOS, N.M., Aug. 21, 2013-The High-Altitude Water Cherenkov (HAWC) Gamma Ray Observatory has begun formal operations at its site in Mexico. HAWC is designed to study the origin of very high-energy cosmic rays and observe the most energetic objects in the known universe. This extraordinary observatory, using a unique detection technique that differs from the classical astronomical design of mirrors, - 2 - lenses, and antennae, is a significant boost to international scientific and technical knowledge. "The HAWC observatory will search for signals from dark matter and to study some
Gulf of Mexico Gas Hydrates Sea-floor Observatory Project Last Reviewed 12/18/2013 Gulf of Mexico Gas Hydrates Sea-floor Observatory Project Last Reviewed 12/18/2013 DE-FE26-06NT42877, DE-FC26-02NT41628, and DE-FC26-00NT40920 Goal The goal of this project is to conduct activities leading to the development, implementation, and operation of a remote, multi-sensor seafloor observatory focused on behavior of the marine hydrocarbon system within the gas hydrate stability zone of the deepwater Gulf of Mexico and analysis of data resultant from that observatory over time. Attaining this goal will lead to an enhanced understanding of the role the hydrocarbon system plays in the environment surrounding the site. Investigations include physical, chemical, and microbiological studies. Models developed from these studies are designed to provide a better understanding of gas
Natural Hazards and Earth System Sciences (2003) 3: 165170 c European Geosciences Union 2003 Natural Hazards
. Kukhianidze2, and G. Ramishvili2 1Tbilisi State University, Chavchavadze st. 2, Tbilisi 380028, Georgia 2Abastumani Astrophysical Observatory, Kazbegi av. 2a, Tbilisi 380060, Georgia Received: 21 June 2002
Nonlin. Processes Geophys., 13, 231235, 2006 www.nonlin-processes-geophys.net/13/231/2006/
Institute of Physics, 6 Tamarashvili str.,Tbilisi 0171, Georgia 2Abastumani Astrophysical Observatory, 2a Kazbegi ave., Tbilisi 0161, Georgia 3Obninsk State Technical University of Atomic Energy (IATE), 1
Natural Hazards and Earth System Sciences (2004) 4: 5358 SRef-ID: 1684-9981/nhess/2004-4-53
Tbilisi State University, Chavchavadze st. 2, Tbilisi 380028, Georgia 2Abastumani Astrophysical Observatory, Kazbegi av. 2a, Tbilisi 380060, Georgia Received: 30 June 2003 Revised: 24 November 2003
Analysis of light curves from the 2003 Nov 14 occultation by Titan of TYC 1343-1855-1
We observed a stellar occultation by Titan on 2003 November 14 from La Palma Observatory using ULTRACAM with three Sloan filters: u', g', and i' (358, 487, and 758 nm, respectively). The occultation probed latitudes 2�S ...
Zalucha, Angela M. (Angela Marie)
Analysis of spatial mode sensitivity of gravitational wave interferometer and targeted search for gravitational radiation from the Crab pulsar
Over the last several years the Laser Interferometer Gravitational Wave Observatory (LIGO) has been making steady progress in improving the sensitivities of its three interferometers, two in Hanford, Washington, and one ...
Betzwieser, Joseph (Joseph Charles)
In Situ CO2 and O2 Measurements on a Profiling Float
In recent years, profiling floats, which form the basis of the successful international Argo observatory, are also being considered as platforms for marine biogeochemical research. This study showcases the utility of floats as a novel tool for ...
Bj�rn Fiedler; Peer Fietzek; Nuno Vieira; P�ricles Silva; Henry C. Bittig; Arne K�rtzinger
Variations of the North Pacific Subtropical Mode Water from Direct Observations
Mooring measurements from the Kuroshio Extension System Study (June 2004 to June 2006) and from the ongoing Kuroshio Extension Observatory (June 2004 to present) are combined with float measurements of the Argo network to study the variability of ...
Luc Rainville; Steven R. Jayne; Meghan F. Cronin
Intrinsic Absorption in the Spectrum of NGC 7469: Simultaneous Chandra, FUSE, and STIS Observations
We present simultaneous X-ray, far-ultraviolet, and near-ultraviolet spectra of the Seyfert 1 galaxy NGC 7469 obtained with the Chandra X-Ray Observatory, the Far Ultraviolet Spectroscopic Explorer, and the Space Telescope ...
Scott, Jennifer E.
Meteorological Tower Measurements of a Surface Cold Front
measurements from the Boulder Atmospheric Observatory meteorological research tower are used to describe the structure and physical processes of a strong surface cold front. Analysis reveals that the horizontal gradients in temperature and wind ...
M. A. Shapiro
The Frontal Hydraulic Head: A Micro-? Scale (1 km) Triggering Mechanism for Mesoconvective Weather Systems
Measurements from the NOAA Boulder Atmospheric Observatory (BAO) 300 m tower, the National Center for Atmospheric Research (NCAR) Sabreliner aircraft, and the NOAA GOES-5 satellite, give evidence for the cross-front scale collapse of ...
M. A. Shapiro; Tamara Hampel; Doris Rotzoll; F. Mosher
An Atmospheric Soliton Observed with Doppler Radar, Differential Absorption Lidar, and a Molecular Doppler Lidar
Airborne Leandre II differential absorption lidar (DIAL), S-band dual-polarization Doppler radar (S-Pol), and Goddard Lidar Observatory for Winds (GLOW) Doppler lidar data are used, in conjunction with surface mesonet and special sounding data, ...
Steven E. Koch; Cyrille Flamant; James W. Wilson; Bruce M. Gentry; Brian D. Jamison
Wave-Turbulence Dynamics in the Stably Stratified Boundary Layer
New data obtained at the Boulder Atmospheric Observatory (BAO) has been compared with a linear stability analysis of the background atmospheric state as measured by rawinsonde ascents. Good agreement was obtained between measured wave parameters ...
F. Einaudi; J. J. Finnigan
The role of oxygen in hydrogen sensing by a platinum-gate silicon carbide gas sensor: An ultrahigh vacuum study
demon- strated for monitoring automotive exhaust,7,8 flue gases from power plants,911 and selective steering for advanced laser interferometer gravitational wave observatory sensing and control signals Rev
Ghosh, Ruby N.
Element and system design for active and passive vibration isolation
This thesis focusses on broadband vibration isolation, with an emphasis on control of absolute payload motion for ultra-precision instruments such as the MIT/Caltech Laser-Interferometric Gravitational Wave Observatory ...
Zuo, Lei, 1974-
Establishing the Moon as a Spectral Radiance Standard
A new automated observatory dedicated to the radiometry of the moon has been constructed to provide new radiance information for calibration of earth-orbiting imaging instruments, particularly Earth Observing System instruments. Instrumentation ...
Hugh H. Kieffer; Robert L. Wildey
Surface Heat Flux Variations across the Kuroshio Extension as Observed by Surface Flux Buoys
Wintertime sea surface heat flux variability across the Kuroshio Extension (KE) front is analyzed using data from the Kuroshio Extension Observatory (KEO) buoy in the Kuroshio recirculation gyre south of the KE front and from the Japan Agency for ...
Masanori Konda; Hiroshi Ichikawa; Hiroyuki Tomita; Meghan F. Cronin
Characterization of an advanced LIGO quadruple pendulum system
The Laser Interferometer Gravitational-wave Observatory (LIGO) measures relative displacements of the interferometer mirrors induced by passing gravitational waves (GWs). At low frequencies, typically below 30 Hz, seismic ...
Thomas, Andrew C. (Andrew Christopher), 1981-
Project Title
Tracer for Tracking Permanent CO 2 Storage in Basaltic Rock DE-FE0004847 Juerg M. Matter The Earth Institute, Lamont-Doherty Earth Observatory, Columbia University U.S. Department...
Solar Neutrinos
Solar Neutrinos at the Conclusion of the Sudbury Neutrino Observatory Noah Oblath April 22, 2008 The study of solar neutrinos began with the idea that one could use the neutrinos...
Meso- and Microscale Features of a Colorado Cold Front
Data from the NOAA BAO (Boulder Atmospheric Observatory) tower and the PROFS (Program for Regional Observing and Forecasting Services) surface mesonetwork have been used to detect the meso- and microscale flow patterns associated with the passage ...
George S. Young; Richard H. Johnson
Sun or Moon Rise/Set Table for One Year
NEW YORK Astronomical Applications Dept. Location: W072 59, N40 50 Rise and Set for the Sun for 2013 U. S. Naval Observatory Washington, DC 20392-5420 Eastern Standard Time Jan....
The Accretion of Ice Particles by Rime during Dry Growth
Freezing nuclei were used as tracers in experiments to determine whether ice particles are accreted by rime during dry growth. Experiments were conducted in a wind tunnel and in natural clouds at a mountaintop observatory. The results in both ...
Terry Deshler
Rates from the Lick Observatory Supernova Search (LOSS) Weidong Li UC Berkeley Abstract: In this talk I will present new measurements of the observed rates of supernovae (SNe) in...
Seasonal and Diurnal Variations in Aerosol Concentration on Whistler Mountain: Boundary Layer Influence and Synoptic-Scale Controls
A mountain air chemistry observatory has been operational on the summit of Whistler Mountain in British Columbia, Canada, since 2002. A 1-yr dataset of condensation nuclei (CN) concentration from this site has been analyzed along with ...
John P. Gallagher; Ian G. McKendry; Anne Marie Macdonald; W. Richard Leaitch
Ground-Based Solar Absorption FTIR Spectroscopy: Characterization of Retrievals and First Results from a Novel Optical Design Instrument at a New NDACC Complementary Station
The authors describe the optical design of a high-resolution Fourier Transform Spectrometer (FTS), which serves as the primary instrument at the University of Toronto Atmospheric Observatory (TAO). The FTS is dedicated to ground-based infrared ...
A. Wiacek; J. R. Taylor; K. Strong; R. Saari; T. E. Kerzenmacher; N. B. Jones; D. W. T. Griffith
Jesuits' Contribution to Meteorology
Starting in the middle of the nineteenth century, as part of their scientific tradition, Jesuits founded a considerable number of meteorological observatories throughout the world. In many countries, Jesuits established and maintained the first ...
Agust�n Ud�as
Lori Garver, NASA Deputy Administrator SOFIA Joining Forces Event
airborne observatory a highly modified Boeing 747sp fitted with a 100 inch diameter infrared telescope selected the design for a new heavy-lift space exploration system to take American astronauts farther
Remote Real-Time Video-Enabled Docking for Underwater Autonomous Platforms
One of the key challenges in the development and implementation of ocean observatories is sustained observations over relevant temporal and spatial scales. Autonomous underwater vehicles (AUVs) have demonstrated their potential for synoptic ...
Mark A. Moline; Oscar Schofield
The Interaction of Tides with the Sill of a Tidally Energetic Inlet
The interaction of the tides with the sill of a tidally energetic inlet, Observatory Inlet, British Columbia, is studied. Because of temporal variations in the stratification of the inlet, a substantial seasonal variation is observed in the power ...
Michael W. Stacey
Atmospheric Transmission and Climate: Results from Smithsonian Measurements
A combination of published and archival observations from the Smithsonian Institution's Astrophysical Observatory (APO) is presented and analyzed. This paper concentrates on the data from the two primary sites�Mount Montezuma, Chile, and Table ...
Robert G. Roosen; Ronald J. Angione
Sorting in Patrick Geddes' Outlook Tower
i n g in P a t r i c k Outlook Tower Geddes' J� Joyce Barleythree months at the Outlook 'lower in Edinburgh, sorting theand services. � The Outlook Tower was a disused observatory
Earley, Joyce
NuSTAR helps solve riddle of black hole spin
for the first time. The findings, made by the two X-ray space observatories, NASA's Nuclear Spectroscopic Telescope Array (NuSTAR) and the European Space Agency's XMM-Newton,...
The Hidden Role of Women in Monitoring Nineteenth-Century African Weather: Instrumental Observations in Equatorial Guinea
Some of the first systematic meteorological observations in Africa were made by two women in Equatorial Guinea in 1875. Sisters Isabel and Juliana Urquiola, together with Manuel Iradier, Isabel's husband, built a meteorological observatory on ...
M. Cruz Gallego; Fernando Dom�nguez-Castro; Jos� M. Vaquero; Ricardo Garc�a-Herrera
Intense spreading of radar echoes from ionospheric plasmas
On December 25, 2004, a large-scale ionospheric plasma bubble was observed over Arecibo Observatory in Puerto Rico, inducing significant range spreading on ionograms. This phenomena may be explained by means of the E x B ...
Dorfman, Seth E
Incoherent scatter radar detection of enhanced plasma line in ionospheric E-region over Arecibo
A series of incoherent scatter radar (ISR) observation were conducted at the Arecibo Observatory from December 27, 2005 until January 3, 2006. From plasma line measurements that were taken during this radar campaign, we ...
Pradipta, Rezy
Moorings and Drifters for Real-Time Interdisciplinary Oceanography
A telemetering electronics/control unit (OASIS) has been developed for use on moorings and free-floating drifters. The OASIS controllers are part of a long-term �coastal ocean observatory,� consisting of an infrastructure of ships, submersibles, ...
Francisco P. Chavez; J. Timothy Pennington; Robert Herlien; Hans Jannasch; Gary Thurmond; Gernot E. Friederich
95-GHz Polarimetric Radar Measurements of Orographic Cap Clouds
The use of millimeter-wavelength radars for cloud microphysical research was investigated in experiments at the Elk Mountain Observatory near Laramie, Wyoming, between April 1990 and March 1992. The 95-GHz polarimetric radar used in these ...
Andrew Pazmany; James Mead; Robert McIntosh; Mark Hervig; Robert Kelly; Gabor Vali
October 2013 by B.D. Fields, (Univ. of Illinois) P. Molaro (Trieste Observatory) and S. Sarkar (Univ. of Oxford & Niels Bohr Institute, Copenhagen). Big-Bang nucleosynthesis (BBN)...
The Pulsar Search Collaboratory
The Pulsar Search Collaboratory (PSC) (NSF #0737641) is a joint project between the National Radio Astronomy Observatory and West Virginia University designed to interest high school students in science
R. Rosen; S. Heatherly; M. A. McLaughlin; R. Lynch; V. I. Kondratiev; J. R. Boyles; M. Wilson; D. R. Lorimer; S. Ransom
The search for gravitational wave bursts in data from the second LIGO science run
The network of detectors comprising the Laser Interferometer Gravitational-wave Observatory (LIGO) are among a new generation of detectors that seek to make the first direct observation of gravitational waves. While providing ...
Chatterji, Shourov Keith
Laboratory evaluation of laser-induced breakdown spectroscopy (LIBS) as a new in situ chemical sensing technique for the deep ocean
Present-day expeditionary oceanography is beginning to shift from a focus on short-term ship and submersible deployments to an ocean observatory mode where long-term temporally-focused studies are feasible. As a result, a ...
Michel, Anna Pauline Miranda, 1976-
Physics Letters A 305 (2002) 239244 www.elsevier.com/locate/pla
of Physics, University of Florida, PO Box 118440, Gainesville, FL 32611, USA b LIGO Hanford Observatory, PO motions impedes constructive interference of * Corresponding author. E-mail address: email@example.com (M
Florida, University of
Center at Fermilab Pierre Auger Cosmic-Ray Observatory Cyrogenic Dark Matter Search R&D for SRF acceleration technology Dark Energy Survey simulator COUPP dark-matter experiment...
A Study of the Remote Control for the East China Sea Seafloor Observation System
Seafloor observatories enable long-term, continuous, real-time, weather-independent, and multidisciplinary scientific observation and research that will promise major breakthroughs in ocean sciences. China has started to establish a seafloor ...
Yang Yu; Huiping Xu; Changwei Xu; Rufu Qin
Inversion of long-lived trace gas emissions using combined Eulerian and Lagrangian chemical transport models
We present a method for estimating emissions of long-lived trace gases from a sparse global network of high-frequency observatories, using both a global Eulerian chemical transport model and Lagrangian particle dispersion ...
Manning, A. J.
A high-frequency gravitational-wave burst search with LIGO's Hanford site
The Laser Interferometer Gravitational-Wave Observatory (LIGO) is a network of long-arm interferometers designed to directly measure gravitational-wave strain. Direct observation of gravitational waves would provide a test ...
Villadsen, Jacqueline Rose
A high-frequency gravitational-wave burst search with LIGO's Hanford site.
??The Laser Interferometer Gravitational-Wave Observatory (LIGO) is a network of long-arm interferometers designed to directly measure gravitational-wave strain. Direct observation of gravitational waves would provide� (more)
Novel approaches to Newtonian noise suppression in interferometric gravitational wave detection
The Laser Interferometer Gravitational-wave Observatory (LIGO) attempts to detect ripples in the curvature of spacetime using two large scale interferometers. These detectors are several kilometer long Michelson interferometers ...
Hunter-Jones, Nicholas R
ARM - Data Announcements Article
Aerosol Data From Pico Observatory Now Part of Value-Added Product Bookmark and Share Day with moderate aerosol loading (22 June 2010): AOD at five wavelengths (top) and...
Low-Frequency Atmospheric Acoustic Energy Associated with Vortices Produced by Thunderstorms
An infrasonic observatory collocated with the Colorado State University CHILL radar during the summer of 1995 permitted unique comparisons between severe storm kinematics and detected acoustic energy at subaudible frequencies near 1 Hz. Radar ...
A. J. Bedard
Graduate Course Catalog Table of Contents
of Intellectual Property Administration Nuclear Radiation Center Radiation Safety Office Research Compliance Environmental Research Center Jewett Observatory University Planetarium Nuclear Magnetic Resonance, Center WSU Spokane WSU Tri-Cities WSU Vancouver Graduate Certificate Programs Regional Programs Program
Underway and Moored Methods for Improving Accuracy in Measurement of Spectral Particulate Absorption and Attenuation
Optical sensors have distinct advantages when used in ocean observatories, autonomous platforms, and on vessels of opportunity, because of their high-frequency measurements, low power consumption, and the numerous established relationships ...
Wayne H. Slade; Emmanuel Boss; Giorgio Dall�Olmo; M. Rois Langner; James Loftin; Michael J. Behrenfeld; Collin Roesler; Toby K. Westberry
Achieving Climate Change Absolute Accuracy in Orbit
The Climate Absolute Radiance and Refractivity Observatory (CLARREO) mission will provide a calibration laboratory in orbit for the purpose of accurately measuring and attributing climate change. CLARREO measurements establish new climate change ...
Bruce A. Wielicki; D. F. Young; M. G. Mlynczak; K. J. Thome; S. Leroy; J. Corliss; J. G. Anderson; C.O. Ao; R. Bantges; F. Best; K. Bowman; H. Brindley; J. J. Butler; W. Collins; J. A. Dykema; D. R. Doelling; D. R. Feldman; N. Fox; X. Huang; R. Holz; Y. Huang; Z. Jin; D. Jennings; D. G. Johnson; K. Jucks; S. Kato; D. B. Kirk-Davidoff; R. Knuteson; G. Kopp; D. P. Kratz; X. Liu; C. Lukashin; A. J. Mannucci; N. Phojanamongkolkij; P. Pilewskie; V. Ramaswamy; H. Revercomb; J. Rice; Y. Roberts; C. M. Roithmayr; F. Rose; S. Sandford; E. L. Shirley; W.L. Smith; Sr.; B. Soden; P. W. Speth; W. Sun; P.C. Taylor; D. Tobin; X. Xiong
ARM - Instrument - mpl
ARIES Observatory, Nainital, Uttarkhand, India PVC M1 Browse Data Highland Center, Cape Cod MA; AMF 1 PYE M1 Browse Data Point Reyes, CA SBS S1 Browse Data Steamboat Springs CO,...
ARM - Instrument - tsi
ARIES Observatory, Nainital, Uttarkhand, India PVC M1 Browse Data Highland Center, Cape Cod MA; AMF 1 PYE M1 Browse Data Point Reyes, CA SBS M1 Browse Data Steamboat Springs CO,...
ARM - VAP Process - aerinf
Data ARIES Observatory, Nainital, Uttarkhand, India PVC M1 Browse Data Highland Center, Cape Cod MA; AMF 1 Contact(s) Timothy Shippert Developer (509) 375-5997 timothy.shippert...
ARM - Instrument - cpc
ARIES Observatory, Nainital, Uttarkhand, India PVC M1 Browse Data Highland Center, Cape Cod MA; AMF 1 PVC S1 Browse Data Highland Center, Cape Cod MA; MAOS See Also Contact(s)...
ARM - Datastreams - aosccn100
PGH M1 Browse Data ARIES Observatory, Nainital, Uttarkhand, India PVC M1 Browse Data Highland Center, Cape Cod MA; AMF 1 SBS S2 Browse Data Steamboat Springs CO, Christie Peak...
ARM - VAP Product - qcrad1long
ARM - Instrument - psap
ARIES Observatory, Nainital, Uttarkhand, India PVC M1 Browse Data Highland Center, Cape Cod MA; AMF 1 PVC S1 Browse Data Highland Center, Cape Cod MA; MAOS SBS S2 Browse Data...
ARM - Instrument - gndrad
ARM - Instrument - skyrad
ARM - Datastreams - nfov2ch
Shouxian, Anhui, China PGH M1 Browse Data ARIES Observatory, Nainital, Uttarkhand, India PVC M1 Browse Data Highland Center, Cape Cod MA; AMF 1 PYE M1 Browse Data Point Reyes, CA...
ARM - Datastreams - aosclap3w
ARIES Observatory, Nainital, Uttarkhand, India PVC M1 Browse Data Highland Center, Cape Cod MA; AMF 1 Contact(s) Yin-Nan Lee (631) 344-3294 email@example.com Gunnar Senum (631)...
ARM - Datastreams - mplpolfs
PGH M1 Browse Data ARIES Observatory, Nainital, Uttarkhand, India PVC M1 Browse Data Highland Center, Cape Cod MA; AMF 1 SBS S1 Browse Data Steamboat Springs CO, Thunderhead Lodge...
ARM - Instrument - met
ARM - Instrument - nfov
ARIES Observatory, Nainital, Uttarkhand, India PVC M1 Browse Data Highland Center, Cape Cod MA; AMF 1 PYE M1 Browse Data Point Reyes, CA Contact(s) Gary Hodges (303) 497-6460...
ARM - Instrument - dl
PGH M1 Browse Data ARIES Observatory, Nainital, Uttarkhand, India PVC M1 Browse Data Highland Center, Cape Cod MA; AMF 1 Contact(s) Rob Newsom (509) 372-6020 rob.newsom@pnnl...
ARM - Instrument - nephelometer
ARM - Datastreams - vceil25k
ARM - Instrument - mwrp
Data Niamey, Niger PGH M1 Browse Data ARIES Observatory, Nainital, Uttarkhand, India PVC M1 Browse Data Highland Center, Cape Cod MA; AMF 1 PYE M1 Browse Data Point Reyes, CA...
ARM - Instrument - sasze
Spirit PGH M1 Browse Data ARIES Observatory, Nainital, Uttarkhand, India PVC M1 Browse Data Highland Center, Cape Cod MA; AMF 1 Contact(s) Connor Flynn (509) 375-2041 connor.flynn...
ARM - Instrument - aeri
ARIES Observatory, Nainital, Uttarkhand, India PVC M1 Browse Data Highland Center, Cape Cod MA; AMF 1 PYE M1 Browse Data Point Reyes, CA Contact(s) Jonathan Gero 608-265-2335...
-----------------------REVIEW 1 ---------------------TITLE: Analyzing the most important part of the World Wide Web
statement of purpose in comparison to non-porn sites there is no comparison in the rating and sentiment acceptance as a short paper on the condition that: 1) The authors clearly set out why the porn observatory
Kuzmanovic, Aleksandar
10p Fermi 3/16/01
Center and the Pierre Auger Cosmic ray observatory currently under construction in Argentina. The CSU group has worked on the BABAR drift chamber and the DIRC, and is presently...
Fermi 3/29/02
Europe and Asia to northern Minnesota for the MINOS neutrino project, to southern Argentina for the Pierre Auger Observatory, to every part of the site, the reach of Material...
All News Releases
are colored white and located in the upper right quadrant of the array. New gamma-ray observatory begins operations at Sierra Negra volcano in the state of Puebla, Mexico...
Speaker: D. Vanden Berk, University of Pittsburg Title: Seeing the Sky Swiftly: Gamma-Ray Bursts and Beyond with the Swift Observatory 3:30 p.m. DIRECTOR'S COFFEE BREAK - 2nd...
Optical observations of afterglows of gamma ray bursts localized by the high energy transient explorer
In this thesis, I discuss observations of the optical afterglows of seven HETE GRBs, carried out mainly with the Magellan Telescopes at Las Campanas Observatory in Chile. Five of the bursts, GRBs 020331, 030115, 030418, ...
CO2 Retrieval over Clouds from the OCO Mission: Model Simulations and Error Analysis
Spectral characteristics of the future Orbiting Carbon Observatory (OCO) sensor, which will be launched in January 2009, were used to infer the carbon dioxide column-averaged mixing ratio over liquid water clouds over ocean by means of radiative ...
J�r�me Vidot; Ralf Bennartz; Christopher W. O�Dell; Ren� Preusker; Rasmus Lindstrot; Andrew K. Heidinger
KINGDOM BY DTlE ATOMIC UNITED ESERG Y,AljTHORK'Y
Office of Legacy Management (LM)
Energy Authority and operated with the-co-operation of the Dominion Observatory, Canada, the Bhabha Institute f o r Atomic Research, Trombay, and t h e Australian National...
Surface Meteorological Observations in Severe Thunderstorms. Part I: Design Details of TOTO
The TOTO (Totable Tornado Observatory) device was designed as a prototype meteorological measuring instrument for use by severe storm intercept teams. Portions of the instrument evolved from our work in producing �hardened� sensors for use in ...
A. J. Bedard Jr.; C. Ramzy
Fusion Energy Sciences Advisory Committee Meeting Marriott Hotel (301-590-0044)
/Registration - Sheraton Hotel 12:00pm 10:00pm Students arrive throughout the day 11:00am Box lunches Sheraton Hotel ·Hill Top ·SSRL 5:15pm Shuttle Bus from hotels to SLAC Top of the Hill 6:00pm 6:30pm Opening General Transportation to Hotels and/or to Stanford Student Observatory 8:15pm 9:30pm Stanford Student Observatory Tour
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I~' I~' CONTRACT ID CODE IPAGE OF PAGES DE-NR0000031 . 1 I 1 2. AMENDMENT/MODIFICATION NO. 3. EFFECTIVE DATE 4. REQUISITION/PURCHASE REQ. NO. I 5. PROJECT NO. (If applicable) 003 Same as Block 16G . N~ 6. ISSUED BV CODE 7. ADMINISTERED BV (If other than Item 6) Code I U.S. Department of Energy Pittsburgh Naval Reactors Office P.O. Box 109 West Mifflin, PA 15122-0109 8. NAME AND ADDRESS OF CONTRACTOR (No. street, county, State and ZIP Code) (*...) 9.A. AMENDMENT OF SOLICITATION NO. Bechtel Marine Propulsion Corporation 9.6. DATED (SEE ITEM 11) 50 Beale Street San Francisco, CA 94105-1895 lOA MODIFICATION OF Contract/Order NO. *... DE-NROOOOO31 10.B. DATED (SEE ITEM 13) CODE N/A I FACILlTV CODE N/A Seotember 18, 2008 11. THIS ITEM ONLV APPLIES TO AMENDMENTS OF SOLICITATIONS D The above numbered solicitation is amended as set forth in Item 14. The hour and date specified for receipt of Offers Dis
Detection of Small Kuiper Belt Objects by Stellar Occultations
Knowledge of the Kuiper Belt is currently limited to those objects that can be detected directly. Objects with diameters less than $\\sim$10km reflect too little light to be detected. These smaller bodies could contain most of the mass in the Kuiper Belt while the abundance of these bodies may constrain the distribution of mass. The overall size distribution of bodies within the Kuiper Belt can also be inferred from the relative abundances of sub-km and larger bodies. Stellar occultations are already used to study dark objects in the Solar System, such as asteroids or planetary rings. Occultation by a KBO of a size comparable to, or larger than, that of the Fresnel Scale will result in Fresnel diffraction. Detection of diffraction effects requires fast multiple-star photometry, which will be conducted in July 2007 using the Orthogonal Parallel Transfer Imaging Camera (OPTIC) mounted on the University of Hawaii 2.2m telescope on Mauna Kea. This paper details how knowledge of the mass and structure of the outer Solar System may be obtained through the detection of serendipitous stellar occultations.
R. Stevenson