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1

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

E-Print Network (OSTI)

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

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

2007-01-01T23:59:59.000Z

2

Inter-American Development Bank (IDB) | Open Energy Information  

Open Energy Info (EERE)

Inter-American Development Bank (IDB) Inter-American Development Bank (IDB) (Redirected from Inter-American Development Bank) Jump to: navigation, search Logo: Inter-American Development Bank Name Inter-American Development Bank Address 1300 New York Avenue, N.W. Place Washington, D.C. Zip 20577 Region Northeast - NY NJ CT PA Area Year founded 1959 Phone number (202) 623-1000 Website http://www.iadb.org/index.cfm? Coordinates 38.899316°, -77.031605° Loading map... {"minzoom":false,"mappingservice":"googlemaps3","type":"ROADMAP","zoom":14,"types":["ROADMAP","SATELLITE","HYBRID","TERRAIN"],"geoservice":"google","maxzoom":false,"width":"600px","height":"350px","centre":false,"title":"","label":"","icon":"","visitedicon":"","lines":[],"polygons":[],"circles":[],"rectangles":[],"copycoords":false,"static":false,"wmsoverlay":"","layers":[],"controls":["pan","zoom","type","scale","streetview"],"zoomstyle":"DEFAULT","typestyle":"DEFAULT","autoinfowindows":false,"kml":[],"gkml":[],"fusiontables":[],"resizable":false,"tilt":0,"kmlrezoom":false,"poi":true,"imageoverlays":[],"markercluster":false,"searchmarkers":"","locations":[{"text":"","title":"","link":null,"lat":38.899316,"lon":-77.031605,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

3

Inter-American Development Bank (IDB) | Open Energy Information  

Open Energy Info (EERE)

Inter-American Development Bank (IDB) Inter-American Development Bank (IDB) Jump to: navigation, search Logo: Inter-American Development Bank Name Inter-American Development Bank Address 1300 New York Avenue, N.W. Place Washington, D.C. Zip 20577 Region Northeast - NY NJ CT PA Area Year founded 1959 Phone number (202) 623-1000 Website http://www.iadb.org/index.cfm? Coordinates 38.899316°, -77.031605° Loading map... {"minzoom":false,"mappingservice":"googlemaps3","type":"ROADMAP","zoom":14,"types":["ROADMAP","SATELLITE","HYBRID","TERRAIN"],"geoservice":"google","maxzoom":false,"width":"600px","height":"350px","centre":false,"title":"","label":"","icon":"","visitedicon":"","lines":[],"polygons":[],"circles":[],"rectangles":[],"copycoords":false,"static":false,"wmsoverlay":"","layers":[],"controls":["pan","zoom","type","scale","streetview"],"zoomstyle":"DEFAULT","typestyle":"DEFAULT","autoinfowindows":false,"kml":[],"gkml":[],"fusiontables":[],"resizable":false,"tilt":0,"kmlrezoom":false,"poi":true,"imageoverlays":[],"markercluster":false,"searchmarkers":"","locations":[{"text":"","title":"","link":null,"lat":38.899316,"lon":-77.031605,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

4

The Inter-American Tropical Tuna Commission (IATTC) was established  

E-Print Network (OSTI)

49 The Inter-American Tropical Tuna Commission (IATTC) was established by an international convention in 1950 and is responsible for the conservation of tunas and management of fisheries for tunas and other species taken by tuna-fishing vessels in the eastern Pacific Ocean (EPO). Such conser- vation

5

INTER-AMERICAN TROPICAL TUNA COMMISSION COMISIN INTERAMERICANA DEL ATN TROPICAL  

E-Print Network (OSTI)

INTER-AMERICAN TROPICAL TUNA COMMISSION COMISI?N INTERAMERICANA DEL AT?N TROPICAL 73RD MEETING The Inter-American Tropical Tuna Commission (IATTC): Taking into account the FAO International Plan to evaluate the incidental mortality of seabirds during longline fishing operations for tunas and tuna

6

Kurt M. Schaefer Inter-American Tropical Tuna Commission. Scripps Institution of Oceanography  

E-Print Network (OSTI)

Kurt M. Schaefer Inter-American Tropical Tuna Commission. Scripps Institution of Oceanography 8604 of yellowfin tuna, Thunnus albacares, near Clipperton Atoll in the eastern Pacific Ocean 98 Abstract.-Spawning of yellowfin tuna, Thunnus albacares, around Clipperton Atoll, in the eastern Pacific Ocean, occurred between

7

Regulatory Impact Review Implementation of Inter-American Tropical Tuna Commission Resolutions Adopted in  

E-Print Network (OSTI)

Regulatory Impact Review Implementation of Inter-American Tropical Tuna Commission Resolutions to implement the decisions of the IATTC. The Tuna Conventions Act (16 U.S.C. 951-961) authorizes the Secretary the Resolution on Tuna Conservation 2011-2013 (C-11-01), the Resolution Prohibiting Fishing on Data Buoys (C-11

8

The Boulder Atmospheric Observatory  

Science Conference Proceedings (OSTI)

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

J. C. Kaimal; J. E. Gaynor

1983-05-01T23:59:59.000Z

9

The Mount Bachelor Observatory  

Science Conference Proceedings (OSTI)

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

2009-12-04T23:59:59.000Z

10

HAWC Observatory captures first image  

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

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

11

Mobile Climate Observatory on the Pacific  

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

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

12

National Astronomical Observatory, Japan  

E-Print Network (OSTI)

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

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

2005-01-01T23:59:59.000Z

13

The Lick Observatory Supernova Search  

Science Conference Proceedings (OSTI)

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

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

2000-01-01T23:59:59.000Z

14

MBO: The Mount Bachelor Observatory  

Science Conference Proceedings (OSTI)

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

2008-12-23T23:59:59.000Z

15

The Large Aperture GRB Observatory  

E-Print Network (OSTI)

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

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

2009-01-01T23:59:59.000Z

16

The Mount Washington Observatory50 Years Old  

Science Conference Proceedings (OSTI)

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

Alan A. Smith

1982-09-01T23:59:59.000Z

17

the Large Aperture GRB Observatory  

SciTech Connect

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

Bertou, Xavier [Centro Atomico Bariloche (Argentina)

2009-04-30T23:59:59.000Z

18

Worldwide R&D of Virtual Observatory  

E-Print Network (OSTI)

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

Chenzhou Cui; Yongheng Zhao

2007-11-27T23:59:59.000Z

19

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

E-Print Network (OSTI)

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

Petermann, Emily B

2010-01-01T23:59:59.000Z

20

The Astrophysical Multimessenger Observatory Network (AMON)  

E-Print Network (OSTI)

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

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

2012-11-23T23:59:59.000Z

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


21

Signals, backgrounds and calibrations in the Sudbury Neutrino Observatory  

Science Conference Proceedings (OSTI)

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

Bhaskar Sur; The SNO Collaboration

1995-01-01T23:59:59.000Z

22

Hanohano:A Deep Ocean Antineutrino Observatory  

E-Print Network (OSTI)

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

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

2008-01-01T23:59:59.000Z

23

Hanohano:A Deep Ocean Antineutrino Observatory  

E-Print Network (OSTI)

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

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

2008-10-03T23:59:59.000Z

24

Hybrid Performance of the Pierre Auger Observatory  

E-Print Network (OSTI)

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

B. R. Dawson; for the Pierre Auger Collaboration

2007-06-08T23:59:59.000Z

25

Status of the Milagro $\\gamma$ Ray Observatory  

E-Print Network (OSTI)

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

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

2001-01-01T23:59:59.000Z

26

Operations of and Future Plans for the Pierre Auger Observatory  

Science Conference Proceedings (OSTI)

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

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

2009-06-01T23:59:59.000Z

27

UNIVERSITY OF CALIFORNIA, SANTA CRUZ UNIVERSITY OF CALIFORNIA OBSERVATORIES  

E-Print Network (OSTI)

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

California at Santa Cruz, University of

28

UNIVERSITY OF CALIFORNIA, SANTA CRUZ UNIVERSITY OF CALIFORNIA OBSERVATORIES  

E-Print Network (OSTI)

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

California at Santa Cruz, University of

29

The endless mantra : innovation at the Keck Observatory  

E-Print Network (OSTI)

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

Bobra, Monica Godha

2005-01-01T23:59:59.000Z

30

Implementing an Observatory Control System-I. A Generic Approach  

E-Print Network (OSTI)

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

Sunu Engineer

2004-01-06T23:59:59.000Z

31

The High Altitude Water Cherenkov Observatory  

E-Print Network (OSTI)

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

,

2013-01-01T23:59:59.000Z

32

POSITION STATEMENT SAVING THE ARECIBO OBSERVATORY  

E-Print Network (OSTI)

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

unknown authors

2008-01-01T23:59:59.000Z

33

Science Potential of a Deep Ocean Antineutrino Observatory  

E-Print Network (OSTI)

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

Steve Dye

2006-11-22T23:59:59.000Z

34

Solar Neutrino Observations at the Sudbury Neutrino Observatory  

E-Print Network (OSTI)

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

Poon, A W P

2002-01-01T23:59:59.000Z

35

Solar Neutrino Observations at the Sudbury Neutrino Observatory  

E-Print Network (OSTI)

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

A. W. P. Poon

2002-11-06T23:59:59.000Z

36

Anisotropy studies with the Pierre Auger Observatory  

E-Print Network (OSTI)

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

Neto, J R T de Mello

2013-01-01T23:59:59.000Z

37

The Fan Observatory Bench Optical Spectrograph (FOBOS)  

E-Print Network (OSTI)

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

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

2005-02-23T23:59:59.000Z

38

Low Energy Investigations at Kamioka Observatory  

E-Print Network (OSTI)

At Kamioka Observatory many activities for low energy rare event search are ongoing. Super-Kamiokande(SK), the largest water Cherenkov neutrino detector, currently continues data taking as the fourth phase of the experiment (SK-IV). In SK-IV, we have upgraded the water purification system and tuned water flow in the SK tank. Consequently the background level was lowered significantly. This allowed SK-IV to derive solar neutrino results down to 3.5MeV energy region. With these data, neutrino oscillation parameters are updated from global fit; $\\Delta m^2_{12}=7.44^{+0.2}_{-0.19}\\times10^{-5} {\\rm eV}^2$, $\\sin^2\\theta_{12}=0.304\\pm0.013$, $\\sin^2\\theta_{13}=0.030^{+0.017}_{-0.015}$. NEWAGE, the directional sensitive dark matter search experiment, is currently operated as "NEWAGE-0.3a" which is a $0.20\\times0.25\\times0.31$ m$^3$ micro-TPC filled with CF4 gas at 152 Torr. Recently we have developed "NEWAGE-0.3b". It was succeeded to lower the operation pressure down to 76 Torr and the threshold down to 50 keV (F...

Sekiya, Hiroyuki

2013-01-01T23:59:59.000Z

39

Neutrino observations from the Sudbury Neutrino Observatory  

SciTech Connect

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

Ahmad, Q.R.; Allen, R.C.; Andersen, T.C.; Anglin, J.D.; Barton,J.C.; Beier, E.W.; Bercovitch, M.; Bigu, J.; Biller, S.D.; Black, R.A.; Blevis, I.; Boardman, R.J.; Boger, J.; Bonvin, E.; Boulay, M.G.; Bowler,M.G.; Bowles, T.J.; Brice, S.J.; Browne, M.C.; Bullard, T.V.; Buhler, G.; Cameron, J.; Chan, Y.D.; Chen, H.H.; Chen, M.; Chen, X.; Cleveland, B.T.; Clifford, E.T.H.; Cowan, J.H.M.; Cowen, D.F.; Cox, G.A.; Dai, X.; Dalnoki-Veress, F.; Davidson, W.F.; Doe, P.J.; Doucas, G.; Dragowsky,M.R.; Duba, C.A.; Duncan, F.A.; Dunford, M.; Dunmore, J.A.; Earle, E.D.; Elliott, S.R.; Evans, H.C.; Ewan, G.T.; Farine, J.; Fergani, H.; Ferraris, A.P.; Ford, R.J.; Formaggio, J.A.; Fowler, M.M.; Frame, K.; Frank, E.D.; Frati, W.; Gagnon, N.; Germani, J.V.; Gil, S.; Graham, K.; Grant, D.R.; Hahn, R.L.; Hallin, A.L.; Hallman, E.D.; Hamer, A.S.; Hamian, A.A.; Handler, W.B.; Haq, R.U.; Hargrove, C.K.; Harvey, P.J.; Hazama, R.; Heeger, K.M.; Heintzelman, W.J.; Heise, J.; Helmer, R.L.; Hepburn, J.D.; Heron, H.; Hewett, J.; Hime, A.; Hykawy, J.G.; Isaac,M.C.P.; Jagam, P.; Jelley, N.A.; Jillings, C.; Jonkmans, G.; Kazkaz, K.; Keener, P.T.; Klein, J.R.; Knox, A.B.; Komar, R.J.; Kouzes, R.; Kutter,T.; Kyba, C.C.M.; Law, J.; Lawson, I.T.; Lay, M.; Lee, H.W.; Lesko, K.T.; Leslie, J.R.; Levine, I.; Locke, W.; Luoma, S.; Lyon, J.; Majerus, S.; Mak, H.B.; Maneira, J.; Manor, J.; Marino, A.D.; McCauley, N.; McDonald,D.S.; McDonald, A.B.; McFarlane, K.; McGregor, G.; Meijer, R.; Mifflin,C.; Miller, G.G.; Milton, G.; Moffat, B.A.; Moorhead, M.; Nally, C.W.; Neubauer, M.S.; Newcomer, F.M.; Ng, H.S.; Noble, A.J.; Norman, E.B.; Novikov, V.M.; O' Neill, M.; Okada, C.E.; Ollerhead, R.W.; Omori, M.; Orrell, J.L.; Oser, S.M.; Poon, A.W.P.; Radcliffe, T.J.; Roberge, A.; Robertson, B.C.; Robertson, R.G.H.; Rosendahl, S.S.E.; Rowley, J.K.; Rusu, V.L.; Saettler, E.; Schaffer, K.K.; Schwendener,M.H.; Schulke, A.; Seifert, H.; Shatkay, M.; Simpson, J.J.; Sims, C.J.; et al.

2001-09-24T23:59:59.000Z

40

Structured Query Language for Virtual Observatory  

E-Print Network (OSTI)

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

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

2004-11-19T23:59:59.000Z

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


41

The HAWC observatory as a GRB detector  

E-Print Network (OSTI)

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

Zaborov, D

2013-01-01T23:59:59.000Z

42

The Solar Dynamics Observatory: Your eye on the Sun  

Science Conference Proceedings (OSTI)

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

W. Dean Pesnell

2011-03-01T23:59:59.000Z

43

Low-multiplicity Burst Search at the Sudbury Neutrino Observatory  

E-Print Network (OSTI)

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

Chen, Min

44

The Lidar System of the Pierre Auger Observatory  

E-Print Network (OSTI)

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

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

2006-09-03T23:59:59.000Z

45

Variable stars in the globular cluster M28 (NGC 6626)  

E-Print Network (OSTI)

We present a new search for variable stars in the Galactic globular cluster M28 (NGC 6626). The search is based on a series of BVI images obtained with the SMARTS Consortium's 1.3m telescope at Cerro Tololo Inter-American Observatory, Chile. The search was carried out using the ISIS v2.2 image subtraction package. We find a total of 25 variable stars in the field of the cluster, 9 being new discoveries. Of the newly found variables, 1 is an ab-type RR Lyrae star, 6 are c-type RR Lyrae, and 2 are long-period/semi-regular variables. V22, previously classified as a type II Cepheid, appears as a bona-fide RRc in our data. In turn, V20, previously classified as an ab-type RR Lyrae, could not be properly phased with any reasonable period. The properties of the ab-type RR Lyrae stars in M28 appear most consistent with an Oosterhoff-intermediate classification, which is unusual for bona-fide Galactic globulars clusters. However, the cluster's c-type variables do not clearly support such an Oosterhoff type, and a hybr...

Prieto, G; Ramos, R Contreras; Pritzl, B J; Smith, H A; Alonso-Garcia, J

2012-01-01T23:59:59.000Z

46

THE ULTIMATE LIGHT CURVE OF SN 1998bw/GRB 980425  

SciTech Connect

We present multicolor light curves of SN 1998bw which appeared in ESO184-G82 in close temporal and spatial association with GRB 980425. The light curves are based on observations conducted at Cerro Tololo Inter-American Observatory (CTIO) and data from the literature. The CTIO photometry reaches {approx}86 days after the gamma-ray burst (GRB) in U and {approx}160 days after the GRB in BV(RI){sub C}. The observations in U extend the previously known coverage by about 30 days and determine the slope of the early exponential tail. We calibrate a large set of local standards in common with those of previous studies and use them to transform published observations of the supernova (SN) to our realization of the standard photometric system. We show that the photometry from different sources merges smoothly and we provide a unified set of 300 observations of the SN in five bands. Using the extensive set of spectra in the public domain, we compute extinction and K-corrections and build quasi-bolometric unreddened rest-frame light curves. We provide low-degree piecewise spline fits to these light curves with daily sampling. They reach {approx}86 rest-frame days after the GRB with U-band coverage and {approx}498 rest-frame days after the GRB without U.

Clocchiatti, Alejandro [Departamento de Astronomia y Astrofisica, Pontificia Universidad Catolica de Chile, Casilla 306, Santiago 22 (Chile); Suntzeff, Nicholas B. [Department of Physics and Astronomy, Mitchell Institute for Fundamental Physics and Astronomy, Texas A and M University, College Station, TX 77843 (United States); Covarrubias, Ricardo [Australian Astronomical Observatory, P.O. Box 296, Epping, NSW 1710 (Australia); Candia, Pablo, E-mail: aclocchi@astro.puc.cl, E-mail: nsuntzeff@tamu.edu, E-mail: ricardo@aao.gov.au, E-mail: pcandia@gemini.edu [Gemini Observatory, Casilla 603, La Serena (Chile)

2011-05-15T23:59:59.000Z

47

The Dark Energy Spectrometer (DESpec): A Multi-Fiber Spectroscopic Upgrade of the Dark Energy Camera and Survey for the Blanco Telescope  

E-Print Network (OSTI)

We describe an initiative to build and use the Dark Energy Spectrometer (DESpec), a wide-field spectroscopic survey instrument for the Blanco 4 meter telescope at Cerro Tololo InterAmerican Observatory (CTIO) in Chile. A new system with about 4000 robotically positioned optical fibers will be interchangeable with the CCD imager of the existing Dark Energy Camera (DECam), accessing a field of view of 3.8 square degrees in a single exposure. The proposed instrument will be operated by CTIO and available for use by the astronomy community. Our collaboration proposes to use DESpec to conduct a wide, deep spectroscopic survey to study Dark Energy. In a survey of about 350 nights, the DESpec collaboration proposes to obtain spectroscopic redshifts for about 8 million galaxies over 5000 square degrees selected from the Dark Energy Survey (DES). This Dark Energy Spectroscopic Survey will advance our knowledge of cosmic expansion and structure growth significantly beyond that obtainable with imaging-only surveys. Sinc...

Abdalla, F; Bacon, D; Bridle, S; Castander, F; Colless, M; DePoy, D; Diehl, H T; Eriksen, M; Flaugher, B; Frieman, J; Gaztanaga, E; Hogan, C; Jouvel, S; Kent, S; Kirk, D; Kron, R; Kuhlmann, S; Lahav, O; Lawrence, J; Lin, H; Marriner, J; Marshall, J; Mohr, J; Nichol, R C; Sako, M; Saunders, W; Soares-Santos, M; Thomas, D; Wechsler, R; West, A; Wu, H

2012-01-01T23:59:59.000Z

48

Spectral Analysis via the Virtual Observatory: The Service Theossa  

E-Print Network (OSTI)

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

Ringat, Ellen; Werner, Klaus

2011-01-01T23:59:59.000Z

49

Installation package for Hyde Memorial Observatory, Lincoln, Nebraska  

DOE Green Energy (OSTI)

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

Not Available

1978-12-01T23:59:59.000Z

50

Results from the Milagro Gamma-Ray Observatory  

E-Print Network (OSTI)

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

California at Santa Cruz, University of

51

Future development of the PLATO observatory for Antarctic science  

E-Print Network (OSTI)

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

Ashley, Michael C. B.

52

e-government procurement observatory model, design and pilot testing  

Science Conference Proceedings (OSTI)

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

Gaston Concha; Miguel Porra; Carlos Pimenta

2010-10-01T23:59:59.000Z

53

Visualizing Spatial and Temporal Variability in Coastal Observatories  

Science Conference Proceedings (OSTI)

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

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

2003-10-01T23:59:59.000Z

54

BIG BEAR SOLAR OBSERVATORY CENTER FOR SOLAR-TERRESTRIAL RESEARCH  

E-Print Network (OSTI)

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

55

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

E-Print Network (OSTI)

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

Rojas, Folkers Eduardo

2009-01-01T23:59:59.000Z

56

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

E-Print Network (OSTI)

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

Katul, Gabriel

57

Measurement of Aerosols at the Pierre Auger Observatory  

E-Print Network (OSTI)

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

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

2007-06-21T23:59:59.000Z

58

Testing the surface detector simulation for the Pierre Auger Observatory  

E-Print Network (OSTI)

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

Ghia, Piera L

2007-01-01T23:59:59.000Z

59

Technology development for a neutrino astrophysical observatory. Letter of intent  

Science Conference Proceedings (OSTI)

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

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

1996-02-01T23:59:59.000Z

60

Technology Development for a Neutrino AstrophysicalObservatory  

Science Conference Proceedings (OSTI)

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

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

1996-02-01T23:59:59.000Z

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


61

Testing the surface detector simulation for the Pierre Auger Observatory  

E-Print Network (OSTI)

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

Piera L. Ghia; for the Pierre Auger Collaboration

2007-06-08T23:59:59.000Z

62

SCALER MODE OF THE AUGER OBSERVATORY AND SUNSPOTS  

Science Conference Proceedings (OSTI)

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

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

2012-10-15T23:59:59.000Z

63

Performance of the Pierre Auger Observatory Surface Detector  

E-Print Network (OSTI)

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

Suomijarvi, Tiina

2007-01-01T23:59:59.000Z

64

Performance of the Pierre Auger Observatory Surface Detector  

SciTech Connect

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

Collaboration, Tiina Suomijarvi for the Pierre Auger

2007-09-01T23:59:59.000Z

65

Calibrating laser test-beams for cosmic-ray observatories  

E-Print Network (OSTI)

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

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

2011-01-01T23:59:59.000Z

66

Trigger and data rates expected for the CTA Observatory  

E-Print Network (OSTI)

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

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

2012-11-13T23:59:59.000Z

67

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

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

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

68

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

69

LAGOVirtual: A Collaborative Environment for the Large Aperture GRB Observatory  

E-Print Network (OSTI)

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

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

2009-12-12T23:59:59.000Z

70

LAGOVirtual: A Collaborative Environment for the Large Aperture GRB Observatory  

E-Print Network (OSTI)

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

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

2009-01-01T23:59:59.000Z

71

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

Open Energy Info (EERE)

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

72

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

E-Print Network (OSTI)

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

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

2011-07-24T23:59:59.000Z

73

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

SciTech Connect

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

Cathy Wilson; Chandana Gangodagamage; Joel Rowland

2013-12-08T23:59:59.000Z

74

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

DOE Data Explorer (OSTI)

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

Cathy Wilson; Chandana Gangodagamage; Joel Rowland

75

Experiment Profile: COUPP NAME: Chicagoland Observatory for Underground Particle  

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

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

76

Charge Management for Gravitational Wave Observatories using UV LEDs  

E-Print Network (OSTI)

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

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

2009-01-01T23:59:59.000Z

77

Precision Solar Neutrino Measurements with the Sudbury Neutrino Observatory  

Science Conference Proceedings (OSTI)

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

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

2007-10-26T23:59:59.000Z

78

The SECIS instrument on the Lomnicky Peak Observatory  

E-Print Network (OSTI)

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

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

2010-01-01T23:59:59.000Z

79

The Offline Software Framework of the Pierre Auger Observatory  

E-Print Network (OSTI)

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

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

2007-01-01T23:59:59.000Z

80

The Offline Software Framework of the Pierre Auger Observatory  

E-Print Network (OSTI)

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

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

2005-01-01T23:59:59.000Z

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81

Probing Dark Energy via Neutrino and Supernova Observatories  

SciTech Connect

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

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

2006-07-10T23:59:59.000Z

82

Searching for Double Beta Decay with the Enriched Xenon Observatory  

Science Conference Proceedings (OSTI)

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

Hall, C.; /SLAC

2007-03-16T23:59:59.000Z

83

Performance of the Keck Observatory adaptive optics system  

SciTech Connect

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

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

2004-01-19T23:59:59.000Z

84

Fluorescence and Hybrid Detection Aperture of the Pierre Auger Observatory  

E-Print Network (OSTI)

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

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

2005-07-05T23:59:59.000Z

85

Current technology development efforts on the international X-ray Observatory  

Science Conference Proceedings (OSTI)

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

David Robinson

2011-03-01T23:59:59.000Z

86

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

E-Print Network (OSTI)

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

2007-01-01T23:59:59.000Z

87

Preliminary systems engineering evaluations for the National Ecological Observatory Network.  

Science Conference Proceedings (OSTI)

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

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

2008-11-01T23:59:59.000Z

88

The Offline Software Framework of the Pierre Auger Observatory  

E-Print Network (OSTI)

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

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

2007-07-11T23:59:59.000Z

89

The Offline Software Framework of the Pierre Auger Observatory  

E-Print Network (OSTI)

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

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

2006-01-01T23:59:59.000Z

90

The offline software framework of the Pierre Auger Observatory  

SciTech Connect

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

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

2005-08-01T23:59:59.000Z

91

Performance of the Pierre Auger Observatory Surface Array  

E-Print Network (OSTI)

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

The Pierre Auger Collaboration

2005-08-22T23:59:59.000Z

92

Performance of the Pierre Auger Observatory Surface Array  

E-Print Network (OSTI)

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

Bertou, X

2005-01-01T23:59:59.000Z

93

Performance of the Pierre Auger Observatory surface array  

SciTech Connect

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

Bertou, Xavier

2005-07-01T23:59:59.000Z

94

Charge Management for Gravitational Wave Observatories using UV LEDs  

E-Print Network (OSTI)

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

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

2009-12-09T23:59:59.000Z

95

SNO Data: Results from Experiments at the Sudbury Neutrino Observatory  

DOE Data Explorer (OSTI)

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

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

96

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

Science Conference Proceedings (OSTI)

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

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

2006-08-01T23:59:59.000Z

97

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

Science Conference Proceedings (OSTI)

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

Michael W. Stacey; Len J. Zedel

1986-06-01T23:59:59.000Z

98

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

Science Conference Proceedings (OSTI)

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

Yoshiyuki Takahashi

1998-01-01T23:59:59.000Z

99

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

E-Print Network (OSTI)

Results are reported on the measurement of the atmospheric neutrino-induced muon flux at a depth of 2 kilometers below the Earths surface from 1229 days of operation of the Sudbury Neutrino Observatory (SNO). By measuring ...

Formaggio, Joseph A.

100

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

Science Conference Proceedings (OSTI)

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

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

2011-03-01T23:59:59.000Z

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


101

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

E-Print Network (OSTI)

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

Cerveny, Vlastislav

102

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

E-Print Network (OSTI)

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

M. D. Healy; for the Pierre Auger Collaboration

2007-09-28T23:59:59.000Z

103

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

104

Bridging the Virtual Observatory and the GRID with the query element  

E-Print Network (OSTI)

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

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

2006-05-05T23:59:59.000Z

105

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

Science Conference Proceedings (OSTI)

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

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

2012-01-01T23:59:59.000Z

106

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

E-Print Network (OSTI)

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

Paris-Sud XI, Université de

107

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

E-Print Network (OSTI)

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

Paris-Sud XI, Université de

108

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

E-Print Network (OSTI)

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

California at Santa Cruz, University of

109

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

E-Print Network (OSTI)

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

California at Santa Cruz, University of

110

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

E-Print Network (OSTI)

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

Long, Bernard

111

The search for extended air showers at the Jicamarca Radio Observatory  

SciTech Connect

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

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

2009-04-30T23:59:59.000Z

112

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

E-Print Network (OSTI)

SOHO Introduction SOHO, the Solar and Heliospheric Observatory, is a project of international cooperation between ESA and NASA to study the Sun, from its deep core to the outer corona, and the solar wind of the solar interior? · Why does the solar corona exist and how is it heated to the extremely high temperature

Christian, Eric

113

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

Science Conference Proceedings (OSTI)

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

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

1999-11-01T23:59:59.000Z

114

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

E-Print Network (OSTI)

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

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

2009-01-01T23:59:59.000Z

115

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

E-Print Network (OSTI)

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

Washington at Seattle, University of

116

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

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

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

117

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

E-Print Network (OSTI)

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

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

2010-01-01T23:59:59.000Z

118

Imaging simulations of selected science with the Magdalena Ridge Observatory Interferometer  

E-Print Network (OSTI)

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

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

119

A Search for Astrophysical Burst Signals at the Sudbury Neutrino Observatory  

E-Print Network (OSTI)

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

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

2013-09-04T23:59:59.000Z

120

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

E-Print Network (OSTI)

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

J. T. Wright

2005-05-11T23:59:59.000Z

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


121

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

Science Conference Proceedings (OSTI)

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

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

1995-06-01T23:59:59.000Z

122

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

Science Conference Proceedings (OSTI)

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

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

1989-02-01T23:59:59.000Z

123

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

Science Conference Proceedings (OSTI)

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

George H. Mount; Jerald W. Harder

1995-10-01T23:59:59.000Z

124

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

Science Conference Proceedings (OSTI)

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

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

2003-11-01T23:59:59.000Z

125

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

E-Print Network (OSTI)

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

Gustavo A. Medina Tanco; Sergio J. Sciutto

2001-09-10T23:59:59.000Z

126

Proposal for a quantity based data model in the Virtual Observatory  

E-Print Network (OSTI)

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

Brian Thomas; Edward Shaya

2003-12-23T23:59:59.000Z

127

Recent results from the Milagro TeV gamma-ray observatory  

E-Print Network (OSTI)

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

Parkinson, P M S

2005-01-01T23:59:59.000Z

128

The Chicagoland Observatory Underground for Particle Physics cosmic ray veto system  

SciTech Connect

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

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

2010-11-01T23:59:59.000Z

129

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

E-Print Network (OSTI)

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

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

2007-08-13T23:59:59.000Z

130

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

E-Print Network (OSTI)

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

L. Wiencke; for the Pierre Auger Collaboration

2008-07-17T23:59:59.000Z

131

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

E-Print Network (OSTI)

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

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

2002-01-01T23:59:59.000Z

132

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

E-Print Network (OSTI)

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

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

2005-07-12T23:59:59.000Z

133

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

Science Conference Proceedings (OSTI)

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

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

1989-01-01T23:59:59.000Z

134

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

E-Print Network (OSTI)

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

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

2012-01-01T23:59:59.000Z

135

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

E-Print Network (OSTI)

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

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

2013-01-01T23:59:59.000Z

136

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

SciTech Connect

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

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

2009-01-01T23:59:59.000Z

137

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

E-Print Network (OSTI)

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

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

2013-03-19T23:59:59.000Z

138

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

E-Print Network (OSTI)

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

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

2007-01-01T23:59:59.000Z

139

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

E-Print Network (OSTI)

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

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

2003-11-30T23:59:59.000Z

140

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

E-Print Network (OSTI)

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

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

2009-01-01T23:59:59.000Z

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141

Performance of the first prototype of the HAWC Gamma Ray Observatory  

E-Print Network (OSTI)

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

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

2009-01-01T23:59:59.000Z

142

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

Science Conference Proceedings (OSTI)

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

Brent M. Bowen

2000-05-01T23:59:59.000Z

143

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

Science Conference Proceedings (OSTI)

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

Juan M. Banda; Rafal A. Angryk

2010-12-01T23:59:59.000Z

144

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

Science Conference Proceedings (OSTI)

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

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

2009-10-01T23:59:59.000Z

145

Terms of Reference First Joint Mission GOVERNMENT OF GRENADA TERMS OF REFERENCE FOR First Joint Mission of INTER-AMERICAN DEVELOPMENT BANK and the WORLD BANK  

E-Print Network (OSTI)

Martinique is located at 11 582 North latitude and 61 202 west longitude and lies between Trinidad and Tobago to the south and St. Vincent and the Grenadines to the north. It is the southernmost of the Windward Islands. Grenada is a Small Island Developing State (SIDS) comprising three islands with the largest being Grenada which is 34 km (21 miles) long and 18km (12 miles) wide and the three islands taken together have a land area of 345 sq. km (133 sq. miles). The country is characterized by humid tropical climate, with relatively constant temperatures throughout the year averaging 26 degrees centigrade. The mean maximum temperature is 31.4 degrees centigrade while the mean minimum is 24.0 degrees centigrade. The dry season typically runs from January to May and the rainy season from June to December. Carriacou and Petit Martinique generally receive lower levels of rainfall and during the dry season can experience severe drought conditions. 2. Economy The economy of Grenada has been hit hard by the global crisis. The economic downturn had stronger impact than was predicted in 2008 which is reflected in declining tourism receipts, Foreign

Pilot Project; On Climate Resilience

2010-01-01T23:59:59.000Z

146

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

SciTech Connect

Results are reported on the measurement of the atmospheric neutrino-induced muon flux at a depth of 2 kilometers below the Earth's surface from 1229 days of operation of the Sudbury Neutrino Observatory (SNO). By measuring the flux of through-going muons as a function of zenith angle, the SNO experiment can distinguish between the oscillated and un-oscillated portion of the neutrino flux. A total of 514 muon-like events are measured between -1 {le} cos {theta}{sub zenith} 0.4 in a total exposure of 2.30 x 10{sup 14} cm{sup 2} s. The measured flux normalization is 1.22 {+-} 0.09 times the Bartol three-dimensional flux prediction. This is the first measurement of the neutrino-induced flux where neutrino oscillations are minimized. The zenith distribution is consistent with previously measured atmospheric neutrino oscillation parameters. The cosmic ray muon flux at SNO with zenith angle cos {theta}{sub zenith} > 0.4 is measured to be (3.31 {+-} 0.01 (stat.) {+-} 0.09 (sys.)) x 10{sup -10} {micro}/s/cm{sup 2}.

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

2009-02-16T23:59:59.000Z

147

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

E-Print Network (OSTI)

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

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

2007-09-05T23:59:59.000Z

148

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

E-Print Network (OSTI)

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

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

2013-02-10T23:59:59.000Z

149

Effects of mode degeneracy in the LIGO Livingston Observatory recycling cavity  

E-Print Network (OSTI)

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

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

2007-08-26T23:59:59.000Z

150

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

SciTech Connect

Results are reported on the measurement of the atmospheric neutrino-induced muon flux at a depth of 2 kilometers below the Earth's surface from 1229 days of operation of the Sudbury Neutrino Observatory (SNO). By measuring the flux of through-going muons as a function of zenith angle, the SNO experiment can distinguish between the oscillated and un-oscillated portion of the neutrino flux. A total of 514 muon-like events are measured between -1 {le} cos {theta}{sub zenith} 0.4 in a total exposure of 2.30 x 10{sup 14} cm{sup 2} s. The measured flux normalization is 1.22 {+-} 0.09 times the Bartol three-dimensional flux prediction. This is the first measurement of the neutrino-induced flux where neutrino oscillations are minimized. The zenith distribution is consistent with previously measured atmospheric neutrino oscillation parameters. The cosmic ray muon flux at SNO with zenith angle cos {theta}{sub zenith} > 0.4 is measured to be (3.31 {+-} 0.01 (stat.) {+-} 0.09 (sys.)) x 10{sup -10} {micro}/s/cm{sup 2}.

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

2009-02-16T23:59:59.000Z

151

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

DOE Data Explorer (OSTI)

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

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

None

152

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

E-Print Network (OSTI)

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

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

2012-01-01T23:59:59.000Z

153

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

E-Print Network (OSTI)

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

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

2007-05-23T23:59:59.000Z

154

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

E-Print Network (OSTI)

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

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

2011-01-01T23:59:59.000Z

155

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

SciTech Connect

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

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

2013-06-12T23:59:59.000Z

156

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

E-Print Network (OSTI)

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

Carla Bleve; for the Pierre Auger Collaboration

2007-06-11T23:59:59.000Z

157

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

Science Conference Proceedings (OSTI)

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

Newton, D.; /Santiago de Compostela U.

2007-06-01T23:59:59.000Z

158

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

E-Print Network (OSTI)

This paper details the solar neutrino analysis of the 385.17-day phase-III data set acquired by the Sudbury Neutrino Observatory (SNO). An array of [superscript 3]He proportional counters was installed in the heavy-water ...

Formaggio, Joseph A.

159

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

SciTech Connect

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

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

2003-03-27T23:59:59.000Z

160

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

SciTech Connect

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

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

2003-03-27T23:59:59.000Z

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161

EMERGING DIMMINGS OF ACTIVE REGIONS OBSERVED BY THE SOLAR DYNAMICS OBSERVATORY  

Science Conference Proceedings (OSTI)

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

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

2012-12-01T23:59:59.000Z

162

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

E-Print Network (OSTI)

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

SNO Collaboration

2006-10-13T23:59:59.000Z

163

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

Science Conference Proceedings (OSTI)

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

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

2011-01-01T23:59:59.000Z

164

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

E-Print Network (OSTI)

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

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

2011-11-28T23:59:59.000Z

165

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

E-Print Network (OSTI)

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

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

2010-01-01T23:59:59.000Z

166

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

DOE Data Explorer (OSTI)

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

167

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

DOE Data Explorer (OSTI)

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

Takahashi, T.

168

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

Science Conference Proceedings (OSTI)

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

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

2012-08-01T23:59:59.000Z

169

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

Science Conference Proceedings (OSTI)

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

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

2011-09-01T23:59:59.000Z

170

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

Science Conference Proceedings (OSTI)

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

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

2009-08-15T23:59:59.000Z

171

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

E-Print Network (OSTI)

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

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

2000-01-01T23:59:59.000Z

172

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

E-Print Network (OSTI)

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

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

2000-10-09T23:59:59.000Z

173

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

Science Conference Proceedings (OSTI)

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

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

2012-08-20T23:59:59.000Z

174

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

SciTech Connect

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

Collaboration, Auger

2012-08-01T23:59:59.000Z

175

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

E-Print Network (OSTI)

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

,

2010-01-01T23:59:59.000Z

176

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

Science Conference Proceedings (OSTI)

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

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

2005-02-01T23:59:59.000Z

177

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

E-Print Network (OSTI)

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

Szadkowski, Z

2009-01-01T23:59:59.000Z

178

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

Science Conference Proceedings (OSTI)

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

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

2013-05-20T23:59:59.000Z

179

SOUTH AFRICAN ASTRONOMICAL OBSERVATORY  

E-Print Network (OSTI)

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

Glass, Ian S.

180

Sommers-Bausch Observatory  

E-Print Network (OSTI)

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

Stowell, Michael

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181

Sudbury Neutrino Observatory  

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

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

182

OBSERVATORY STUDENT CENTER  

E-Print Network (OSTI)

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

183

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

Science Conference Proceedings (OSTI)

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

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

2009-01-01T23:59:59.000Z

184

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

E-Print Network (OSTI)

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

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

2011-01-01T23:59:59.000Z

185

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

E-Print Network (OSTI)

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

Vaquero, J M

2014-01-01T23:59:59.000Z

186

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

SciTech Connect

A thorough search for large-scale anisotropies in the distribution of arrival directions of cosmic rays detected above 10{sup 18} eV at the Pierre Auger Observatory is presented. This search is performed as a function of both declination and right ascension in several energy ranges above 10{sup 18} eV, and reported in terms of dipolar and quadrupolar coefficients. Within the systematic uncertainties, no significant deviation from isotropy is revealed. Assuming that any cosmic-ray anisotropy is dominated by dipole and quadrupole moments in this energy range, upper limits on their amplitudes are derived. These upper limits allow us to test the origin of cosmic rays above 10{sup 18} eV from stationary Galactic sources densely distributed in the Galactic disk and predominantly emitting light particles in all directions.

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

2012-12-15T23:59:59.000Z

187

CONSTRAINTS ON THE ORIGIN OF COSMIC RAYS ABOVE 10{sup 18} eV FROM LARGE-SCALE ANISOTROPY SEARCHES IN DATA OF THE PIERRE AUGER OBSERVATORY  

SciTech Connect

A thorough search for large-scale anisotropies in the distribution of arrival directions of cosmic rays detected above 10{sup 18} eV at the Pierre Auger Observatory is reported. For the first time, these large-scale anisotropy searches are performed as a function of both the right ascension and the declination and expressed in terms of dipole and quadrupole moments. Within the systematic uncertainties, no significant deviation from isotropy is revealed. Upper limits on dipole and quadrupole amplitudes are derived under the hypothesis that any cosmic ray anisotropy is dominated by such moments in this energy range. These upper limits provide constraints on the production of cosmic rays above 10{sup 18} eV, since they allow us to challenge an origin from stationary galactic sources densely distributed in the galactic disk and emitting predominantly light particles in all directions.

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

2013-01-01T23:59:59.000Z

188

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

SciTech Connect

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

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

2012-11-20T23:59:59.000Z

189

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

E-Print Network (OSTI)

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

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

2000-08-01T23:59:59.000Z

190

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

Science Conference Proceedings (OSTI)

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

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

2011-11-01T23:59:59.000Z

191

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

SciTech Connect

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

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

2007-02-01T23:59:59.000Z

192

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

E-Print Network (OSTI)

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

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

2008-03-28T23:59:59.000Z

193

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

SciTech Connect

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

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

2006-08-01T23:59:59.000Z

194

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

Science Conference Proceedings (OSTI)

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

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

2012-05-01T23:59:59.000Z

195

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

Science Conference Proceedings (OSTI)

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

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

2009-12-20T23:59:59.000Z

196

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

E-Print Network (OSTI)

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

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

2006-08-04T23:59:59.000Z

197

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

SciTech Connect

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

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

2005-03-18T23:59:59.000Z

198

HAWC Observatory captures first image  

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

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

199

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

Science Conference Proceedings (OSTI)

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

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

2012-11-01T23:59:59.000Z

200

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

E-Print Network (OSTI)

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

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

2013-01-01T23:59:59.000Z

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


201

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

Science Conference Proceedings (OSTI)

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

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

2011-09-01T23:59:59.000Z

202

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

SciTech Connect

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

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

1994-02-01T23:59:59.000Z

203

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

Science Conference Proceedings (OSTI)

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

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

2011-07-20T23:59:59.000Z

204

Toward Observatory Cloud Computing | Argonne National Laboratory  

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

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

205

NATIONAL RADIO ASTRONOMY OBSERVATORY CHARLOTTESVILLE, VIRGINIA  

E-Print Network (OSTI)

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

Groppi, Christopher

206

Mary Lea Heger Shane: The Lick Observatory  

E-Print Network (OSTI)

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

Shane, Mary Lea; Calciano, Elizabeth Spedding

1969-01-01T23:59:59.000Z

207

Solstice Observers and Observatories in Native California  

E-Print Network (OSTI)

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

Hudson, Travis; Lee, Georgia; Hedges, Ken

1979-01-01T23:59:59.000Z

208

The Status of the STACEE Observatory  

E-Print Network (OSTI)

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

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

2001-01-01T23:59:59.000Z

209

Toward a Resiliency and Vulnerability Observatory Network ...  

Science Conference Proceedings (OSTI)

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

2009-02-05T23:59:59.000Z

210

Pierre Auger Observatory Surface Detector Cabling Plan  

E-Print Network (OSTI)

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

211

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

SciTech Connect

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

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

2011-09-10T23:59:59.000Z

212

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

Science Conference Proceedings (OSTI)

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

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

2010-11-20T23:59:59.000Z

213

DOE to Participate in Colombian Regional Energy Meeting Ahead...  

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

as well regional multilateral organizations, including the Inter-American Development Bank, the Organization of American States and the U.S.-Colombia Chamber of Commerce, to...

214

Nicaragua-San Jacinto-Tizate Geothermal Power Project | Open...  

Open Energy Info (EERE)

Geothermal Power Project AgencyCompany Organization Inter-American Development Bank Sector Energy Focus Area Renewable Energy, Geothermal Topics Background analysis...

215

Secretary Moniz Addresses Conference on the Caribbean's Energy...  

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

6, 2013 - 2:42pm Addthis Secretary Moniz Addresses Conference on the Caribbeans Energy Future Secretary Moniz joined Inter-American Development Bank President Luis...

216

LACRP List Serve | Open Energy Information  

Open Energy Info (EERE)

list on ledsgp.org. Name Organization Email Alpizar, William Costa Rica Ministry of Environment and Energy Alatorre Frenk, Claudio Inter-American Development Bank (IDB) Amin,...

217

Surface Finish Metrology  

Science Conference Proceedings (OSTI)

... NMI's in the Inter-American Metrology System (SIM) showed good agreement of NIST results with Mexico, Brazil, Canada, and Argentina, and was ...

2012-11-26T23:59:59.000Z

218

LEDSGP/about/Latin America and Caribbean Regional Platform |...  

Open Energy Info (EERE)

(EBRD) Inter-American Development Bank (IDB) World Bank Algeria Egypt Indonesia Jordan Kazakhstan Mexico Morocco Nigeria Philippines South Africa Thailand Tunisia Caribbean...

219

NIST Spectral Data for the Chandra X-Ray Observatory  

Science Conference Proceedings (OSTI)

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

2011-12-09T23:59:59.000Z

220

NATIONAL RADIO ASTRONMY OBSERVATORY GREEN BANK, WEST VIRGINIA  

E-Print Network (OSTI)

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

Groppi, Christopher

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


221

Mobile Climate Observatory for Atmospheric Aerosols in India  

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

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

222

Sensitivity Studies for Third-Generation Gravitational Wave Observatories  

E-Print Network (OSTI)

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

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

2010-12-04T23:59:59.000Z

223

Design of light concentrators for Cherenkov telescope observatories  

E-Print Network (OSTI)

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

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

2013-01-01T23:59:59.000Z

224

GOPAL NARAYANAN's Curriculum Vitae Five College Radio Astronomy Observatory  

E-Print Network (OSTI)

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

Narayanan, Gopal

225

Evidence for neutrino oscillations in the Sudbury Neutrino Observatory  

E-Print Network (OSTI)

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

Marino, Alysia Diane

2004-01-01T23:59:59.000Z

226

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

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

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

227

Scottish Observatory for Work and Health University of Glasgow  

E-Print Network (OSTI)

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

Glasgow, University of

228

Green Bank, West Virginia National Radio Astronomy Observatory  

E-Print Network (OSTI)

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

Groppi, Christopher

229

NATIONAL RADIO ASTRONOMY OBSERVATORY GREEN BANK, WEST VIRGINIA  

E-Print Network (OSTI)

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

Groppi, Christopher

230

Los Alamos observatory fingers cosmic ray 'hot spots'  

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

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

231

Electron antineutrino search Sudbury Neutrino Observatory 9 Bellerive,  

E-Print Network (OSTI)

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

232

The Southern Great Plains Site: A Climate Observatory in Oklahoma  

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

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

233

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

Science Conference Proceedings (OSTI)

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

Matthew D. Shupe

2011-03-01T23:59:59.000Z

234

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network (OSTI)

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

Groppi, Christopher

235

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network (OSTI)

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

Groppi, Christopher

236

Evidence for neutrino oscillations in the Sudbury Neutrino Observatory  

E-Print Network (OSTI)

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

Marino, Alysia Diane

2004-01-01T23:59:59.000Z

237

Formation flying for a Fresnel lens observatory mission  

E-Print Network (OSTI)

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

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

2006-01-01T23:59:59.000Z

238

Formation flying for a Fresnel lens observatory mission  

E-Print Network (OSTI)

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

John Krizmanic; Gerry Skinner; Neil Gehrels

2006-01-03T23:59:59.000Z

239

INDIA-BASED NEUTRINO OBSERVATORY INO/2005/01  

E-Print Network (OSTI)

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

Udgaonkar, Jayant B.

240

Extrasolar planet transit photometry at Wallace Astrophysical Observatory  

E-Print Network (OSTI)

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

Fong, Wen-fai

2008-01-01T23:59:59.000Z

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


241

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network (OSTI)

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

Groppi, Christopher

242

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

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

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

243

New SX Phoenicis Variables in the Globular Cluster NGC 4833  

E-Print Network (OSTI)

We report the discovery of 6 SX Phoenicis stars in the southern globular cluster NGC 4833. Images were obtained from January through June 2011 with the Southeastern Association for Research in Astronomy 0.6 meter telescope located at Cerro Tololo Interamerican Observatory. The image subtraction method of Alard & Lupton (1998)was used to search for variable stars in the cluster. We confirmed 17 previously cataloged variables by Demers & Wehlau(1977). In addition to the previously known variables we have identified 10 new variables. Of the total number of confirmed variables in our 10x10 arcmin^2 field, we classified 10 RRab variables, with a mean period of 0.69591 days, 7 RRc, with a mean period of 0.39555 days, 2 possible RRe variables with a mean period of 0.30950 days, a W Ursae Majoris contact binary, an Algol-type binary, and the 6 SX Phoenicis stars with a mean period of 0.05847 days. The periods, relative numbers of RRab and RRc variables, and Bailey diagram are indicative of the cluster being o...

Darragh, Andrew N

2012-01-01T23:59:59.000Z

244

The Dark Energy Survey instrument design  

SciTech Connect

We describe a new project, the Dark Energy Survey (DES), aimed at measuring the dark energy equation of state parameter, w, to a statistical precision of {approx}5%, with four complementary techniques. The survey will use a new 3 sq. deg. mosaic camera (DECam) mounted at the prime focus of the Blanco 4m telescope at the Cerro-Tololo International Observatory (CTIO). DECam includes a large mosaic camera, a five element optical corrector, four filters (g,r,i,z), and the associated infrastructure for operation in the prime focus cage. The focal plane consists of 62 2K x 4K CCD modules (0.27''/pixel) arranged in a hexagon inscribed within the 2.2 deg. diameter field of view. We plan to use the 250 micron thick fully-depleted CCDs that have been developed at the Lawrence Berkeley National Laboratory (LBNL). At Fermilab, we will establish a packaging factory to produce four-side buttable modules for the LBNL devices, as well as to test and grade the CCDs. R&D is underway and delivery of DECam to CTIO is scheduled for 2009.

Flaugher, B.; /Fermilab

2006-05-01T23:59:59.000Z

245

PHYSICAL, CHEMICAL, AND BIOLOGICAL OCEANOGRAPHIC OBSERVATIONS  

E-Print Network (OSTI)

by the University of California, Scripps Institution of Oceanography and the Inter- American Tropical Tuna, bacterial abundance, and zooplankton standing crop. A nearly continuous record of incident solar radiation

246

SCP2003hubsimpletrans.pdf  

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

0.25,0.75 0.25, 0 1, 0 redshift z Supernova Cosmology Project Knop et al. (2003) CalanTololo & CfA Supernova Cosmology Project effective m B...

247

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

E-Print Network (OSTI)

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

deYoung, Brad

248

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

Science Conference Proceedings (OSTI)

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

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

249

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

Science Conference Proceedings (OSTI)

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

Nicholas A. Bond; Meghan F. Cronin

2008-04-01T23:59:59.000Z

250

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

E-Print Network (OSTI)

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

California at Santa Cruz, University of

251

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

E-Print Network (OSTI)

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

Kuntz, Brad

2010-01-01T23:59:59.000Z

252

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

E-Print Network (OSTI)

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

Sheridan, Jennifer

253

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

E-Print Network (OSTI)

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

Wisconsin at Madison, University of

254

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

E-Print Network (OSTI)

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

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

2013-04-02T23:59:59.000Z

255

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

E-Print Network (OSTI)

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

George J. Bendo; Robert D. Joseph

2004-03-04T23:59:59.000Z

256

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

E-Print Network (OSTI)

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

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

2008-01-01T23:59:59.000Z

257

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

E-Print Network (OSTI)

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

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

2008-02-04T23:59:59.000Z

258

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

E-Print Network (OSTI)

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

Evans, Matthew J.

259

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

E-Print Network (OSTI)

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

Sheridan, Jennifer

260

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

E-Print Network (OSTI)

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

Engel, Jonathan

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


261

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

E-Print Network (OSTI)

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

Sheridan, Jennifer

262

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

E-Print Network (OSTI)

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

Hörandel, Jörg R.

263

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

E-Print Network (OSTI)

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

Burton, Laura M

2007-01-01T23:59:59.000Z

264

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

E-Print Network (OSTI)

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

Sheridan, Jennifer

265

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

E-Print Network (OSTI)

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

Sheridan, Jennifer

266

MilagroA TeV Observatory for Gamma Ray Bursts  

E-Print Network (OSTI)

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

California at Santa Cruz, University of

267

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

E-Print Network (OSTI)

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

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

2002-01-01T23:59:59.000Z

268

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

E-Print Network (OSTI)

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

269

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

E-Print Network (OSTI)

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

270

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

E-Print Network (OSTI)

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

271

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

E-Print Network (OSTI)

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

Miguel F. Morales

2003-08-06T23:59:59.000Z

272

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

E-Print Network (OSTI)

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

Patterson, Bruce D.

273

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

DOE R&D Accomplishments (OSTI)

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

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

1990-11-00T23:59:59.000Z

274

NATIONAL Puano ASTRONOMY OBSERVATORY PosT OFFICE Box 2 REPORT  

E-Print Network (OSTI)

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

Groppi, Christopher

275

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

E-Print Network (OSTI)

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

Sheridan, Jennifer

276

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

E-Print Network (OSTI)

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

Sheridan, Jennifer

277

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

E-Print Network (OSTI)

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

Sheridan, Jennifer

278

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

E-Print Network (OSTI)

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

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

2013-01-01T23:59:59.000Z

279

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

E-Print Network (OSTI)

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

Constable, Steve

280

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

Science Conference Proceedings (OSTI)

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

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

2012-10-01T23:59:59.000Z

Note: This page contains sample records for the topic "tololo inter-american observatory" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
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to obtain the most current and comprehensive results.


281

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

Science Conference Proceedings (OSTI)

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

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

2006-02-09T23:59:59.000Z

282

Time Brightness  

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

Perlmutter, et al., in Thermonuclear Supernovae, NATO ASI, v. 486 (1997) Perlmutter, et al., in Thermonuclear Supernovae, NATO ASI, v. 486 (1997) Cosmology from . . . Time Brightness ... . . . 50-100 Fields Lunar Calendar Scheduled Follow-Up Imaging at Hubble, Cerro Tololo, WIYN, Isaac Newton Scheduled Follow-Up Spectroscopy at Keck Almost 1000 Galaxies per Field RESULT: ~24 Type Ia supernovae discovered while still brightening, at new moon Berkeley Lab Keck WIYN Cerro Tololo Isaac Newton Hubble Strategy We developed a strategy to guarantee a group of supernova discoveries on a certain date. Just after a new moon, we observe some 50 to 100 high-galactic lattitute fields-each containing almost a thousand high-redshift galaxies-in two nights on the Cerro Tololo 4-meter telescope with Tyson & Bernstein's wide-field camera. We return three weeks later to observe the same

283

8g SUMMITS OF THE AMERICAS  

E-Print Network (OSTI)

with an analysis of key policy areas relevant to the inter-American agenda, and are intended to enrich the multilateral dialogue and consensus-building inherent to the Summits process in order to facilitate collective approaches to the Hemispheres challenges. Energy Security in the Americas

P Olicy; Brief S Eries

2009-01-01T23:59:59.000Z

284

Plant and Soil 247: 189198, 2002. 2002 Kluwer Academic Publishers. Printed in the Netherlands.  

E-Print Network (OSTI)

TIME SPEAKER UNIVERSITY TITLE LAB 1:30P José Osorio Universidad InterAmericana de Puerto RicoAmerican University, Puerto Rico 2:30P Halley Coplin Rensselaer Polytechnic Institute Direct Browser Integration of 3D UNIVERSITY TITLE LAB MODERATOR: Jose Rodriguez InterAmerican University, Puerto Rico 10:50A Errol Markland

Willig, Michael

285

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

E-Print Network (OSTI)

We have searched for extremely high energy neutrinos using data taken with the IceCube detector between May 2010 and May 2012. Two neutrino induced particle shower events with energies around 1 PeV were observed, as reported previously. In this work, we investigate whether these events could originate from cosmogenic neutrinos produced in the interactions of ultra-high energy cosmic-rays with ambient photons while propagating through intergalactic space. Exploiting IceCube's large exposure for extremely high energy neutrinos and the lack of observed events above 100 PeV, we can rule out the corresponding models at more than 90% confidence level. The model independent quasi-differential 90% CL upper limit, which amounts to $E^2 \\phi_{\

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

2013-10-21T23:59:59.000Z

286

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

E-Print Network (OSTI)

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

Otero, Jos D.

2009-01-01T23:59:59.000Z

287

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

E-Print Network (OSTI)

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

Gotowka, Brendan Reed

2005-01-01T23:59:59.000Z

288

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

DOE Green Energy (OSTI)

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

Ketchum, Christina; /SLAC

2006-09-01T23:59:59.000Z

289

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

E-Print Network (OSTI)

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

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

2004-06-25T23:59:59.000Z

290

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

E-Print Network (OSTI)

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

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

2007-11-06T23:59:59.000Z

291

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

Science Conference Proceedings (OSTI)

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

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

2012-10-01T23:59:59.000Z

292

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

Science Conference Proceedings (OSTI)

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

Vincent Noel; Helene Chepfer; Martial Haeffelin; Yohann Morille

2006-11-01T23:59:59.000Z

293

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

Science Conference Proceedings (OSTI)

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

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

294

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

E-Print Network (OSTI)

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

Adolphs, Ralph

295

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

E-Print Network (OSTI)

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

296

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

E-Print Network (OSTI)

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

2007-01-01T23:59:59.000Z

297

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

E-Print Network (OSTI)

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

Garcia, Michael

298

Mesoscale Wind Regimes in Chile at 30S  

Science Conference Proceedings (OSTI)

In November of 1999, four permanent surface stations were installed in the vicinity of the surface ozone monitoring station on the summit of the Cerro Tololo (2200 m MSL) in Chile at 30S. These stations were used to study the atmospheric flow ...

Norbert Kalthoff; Inge Bischoff-Gau; Melitta Fiebig-Wittmaack; Franz Fiedler; Jutta Thrauf; Enrique Novoa; Clotilde Pizarro; Rubn Castillo; Laura Gallardo; Roberto Rondanelli; Martin Kohler

2002-09-01T23:59:59.000Z

299

SCP2003hubbletrans.pdf  

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

1.0 0.5 0.0 0.5 1.0 mag. residual from empty cosmology 0.25,0.75 0.25, 0 1, 0 0.25,0.75 0.25, 0 1, 0 redshift z Supernova Cosmology Project Knop et al. (2003) CalanTololo & CfA...

300

Event:IDB Climate Change and Sustainability Day | Open Energy Information  

Open Energy Info (EERE)

IDB Climate Change and Sustainability Day IDB Climate Change and Sustainability Day Jump to: navigation, search Calendar.png IDB Climate Change and Sustainability Day: on 2012/06/20 The Inter-American Development Bank is organizing an event on Climate Change and Sustainability on the sidelines of the UN Conference on Sustainable Development (UNCSD, or Rio+20). The event is open to the private and public sectors as well as civil society. Discussions will address, among other topics: mitigation and adaptation to climate change, resilient low carbon development, biodiversity, sustainable energy and the challenges of a local level sustainability agenda. Event Details Name IDB Climate Change and Sustainability Day Date 2012/06/20 Location Rio de Janeiro, Brazil Organizer Inter-American Development Bank (IDB)

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


301

GEF-Colombia-Geothermal Energy Grant | Open Energy Information  

Open Energy Info (EERE)

Colombia-Geothermal Energy Grant Colombia-Geothermal Energy Grant Jump to: navigation, search Name GEF-Colombia-Geothermal Energy Grant Agency/Company /Organization Global Environment Facility (GEF), Inter-American Development Bank (IDB) Sector Energy Focus Area Geothermal Topics Finance, Implementation, Background analysis Website http://www.iadb.org/en/news/ne Program Start 2011 Country Colombia UN Region South America References Colombia promotes geothermal energy with IDB support[1] GEF-Colombia-Geothermal Energy Grant Screenshot "Colombia will promote investment in non-conventional renewable energy sources and lay the groundwork for its first geothermal project with a $2.7 million grant from the Global Environment Facility (GEF) administered by the Inter-American Development Bank (IDB). "

302

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

Science Conference Proceedings (OSTI)

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

303

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

E-Print Network (OSTI)

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

Delmotte, Nausicaa

304

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

E-Print Network (OSTI)

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

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

1997-07-02T23:59:59.000Z

305

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

Science Conference Proceedings (OSTI)

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

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

2006-03-01T23:59:59.000Z

306

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

E-Print Network (OSTI)

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

Balser, Teri C.

307

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

E-Print Network (OSTI)

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

Waltham, Chris

308

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

E-Print Network (OSTI)

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

309

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

E-Print Network (OSTI)

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

310

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

E-Print Network (OSTI)

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

Heilmann, Ralf K.

311

Ukraine-Clean Technology Fund (CTF) | Open Energy Information  

Open Energy Info (EERE)

Page Page Edit with form History Facebook icon Twitter icon » Ukraine-Clean Technology Fund (CTF) Jump to: navigation, search Name Ukraine-Climate Technology Fund (CTF) Agency/Company /Organization African Development Bank, Asian Development Bank, European Bank for Reconstruction and Development, Inter-American Development Bank, World Bank Sector Climate, Energy Focus Area Energy Efficiency, Geothermal, Transportation Topics Background analysis, Finance, Implementation, Low emission development planning, Market analysis Website http://www.climateinvestmentfu Country Ukraine Eastern Europe References Ukraine-CTF Investment Plan[1] Ukraine-Climate Technology Fund (CTF) Screenshot Overview "The Clean Technology Fund (CTF), one of two Climate Investment Funds,

312

Tunisia-Clean Technology Fund (CTF) | Open Energy Information  

Open Energy Info (EERE)

Page Page Edit with form History Facebook icon Twitter icon » Tunisia-Clean Technology Fund (CTF) Jump to: navigation, search Name Tunisia-Clean Technology Fund (CTF) Agency/Company /Organization African Development Bank, Asian Development Bank, European Bank for Reconstruction and Development, Inter-American Development Bank, World Bank Sector Climate, Energy Focus Area Energy Efficiency, Geothermal, Transportation Topics Background analysis, Finance, Implementation, Low emission development planning, Market analysis Website http://www.climateinvestmentfu Country Tunisia Northern Africa References Middle East and North Africa Regional Program (Algeria, Egypt, Jorban, Morroco, Tunisia)-Clean Technology Fund (CTF)[1] Tunisia-Clean Technology Fund (CTF) Screenshot

313

Chile-Clean Technology Fund (CTF) | Open Energy Information  

Open Energy Info (EERE)

Chile-Clean Technology Fund (CTF) Chile-Clean Technology Fund (CTF) Jump to: navigation, search Name Chile-Climate Technology Fund (CTF) Agency/Company /Organization African Development Bank, Asian Development Bank, European Bank for Reconstruction and Development, Inter-American Development Bank, World Bank Sector Climate, Energy Focus Area Energy Efficiency, Geothermal, Transportation Topics Background analysis, Finance, Implementation, Low emission development planning, Market analysis Website http://www.climateinvestmentfu Country Chile South America References Chile-CTF Investment Plan[1] Chile-Climate Technology Fund (CTF) Screenshot Overview "The Clean Technology Fund (CTF), one of two Climate Investment Funds, promotes scaled-up financing for demonstration, deployment and transfer of

314

India-Clean Technology Fund (CTF) | Open Energy Information  

Open Energy Info (EERE)

India-Clean Technology Fund (CTF) India-Clean Technology Fund (CTF) Jump to: navigation, search Name India-Clean Technology Fund (CTF) Agency/Company /Organization African Development Bank, Asian Development Bank, European Bank for Reconstruction and Development, Inter-American Development Bank, World Bank Sector Climate, Energy Focus Area Energy Efficiency, Geothermal, Transportation Topics Background analysis, Finance, Implementation, Low emission development planning, Market analysis Website http://www.climateinvestmentfu Country India Southern Asia References India-CTF Investment Plan[1] India-Clean Technology Fund (CTF) Screenshot Overview "The Clean Technology Fund (CTF), one of two Climate Investment Funds, promotes scaled-up financing for demonstration, deployment and transfer of

315

Program Program Organization Country Region Topic Sector Sector  

Open Energy Info (EERE)

Program Organization Country Region Topic Sector Sector Program Organization Country Region Topic Sector Sector Albania Enhancing Capacity for Low Emission Development Strategies EC LEDS Albania Enhancing Capacity for Low Emission Development Strategies EC LEDS United States Agency for International Development USAID United States Environmental Protection Agency United States Department of Energy United States Department of Agriculture United States Department of State Albania Southern Asia Low emission development planning LEDS Energy Land Climate Algeria Clean Technology Fund CTF Algeria Clean Technology Fund CTF African Development Bank Asian Development Bank European Bank for Reconstruction and Development EBRD Inter American Development Bank IDB World Bank Algeria South Eastern Asia Background analysis Finance Implementation

316

Climate Investment Funds | Open Energy Information  

Open Energy Info (EERE)

Climate Investment Funds Climate Investment Funds Jump to: navigation, search Tool Summary Name: Clean Technology Fund Agency/Company /Organization: African Development Bank, Asian Development Bank, European Bank for Reconstruction and Development, Inter-American Development Bank, World Bank Sector: Energy, Land Topics: Finance, Implementation, Low emission development planning, Market analysis, Background analysis Website: www.climateinvestmentfunds.org/cif/ References: Climate Investment Funds[1] Overview The Climate Investment Funds are a unique pair of financing instruments designed to support low-carbon and climate-resilient development through scaled-up financing channeled through the African Development Bank, Asian Development Bank, European Bank for Reconstruction and Development,

317

Bahamas-Caribbean Community (CARICOM) Sustainable Energy Roadmap and  

Open Energy Info (EERE)

Bahamas-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Bahamas-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Jump to: navigation, search Name Bahamas-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Agency/Company /Organization Inter-American Development Bank, World Watch Institute (WWI) Sector Climate, Energy Focus Area Renewable Energy, Economic Development, Energy Efficiency, Greenhouse Gas, Grid Assessment and Integration, Industry, People and Policy, Transportation Topics Background analysis, Baseline projection, Finance, GHG inventory, Implementation, Low emission development planning, -Roadmap, Market analysis, Policies/deployment programs, Resource assessment, Technology characterizations Program Start 2012 Program End 2012 Country Bahamas Caribbean

318

Algeria-Clean Technology Fund (CTF) | Open Energy Information  

Open Energy Info (EERE)

Algeria-Clean Technology Fund (CTF) Algeria-Clean Technology Fund (CTF) Jump to: navigation, search Name Algeria-Clean Technology Fund (CTF) Agency/Company /Organization African Development Bank, Asian Development Bank, European Bank for Reconstruction and Development, Inter-American Development Bank, World Bank Sector Climate, Energy Focus Area Renewable Energy, Solar, - Concentrating Solar Power Topics Background analysis, - Energy Security, Finance, Implementation, Low emission development planning, -LEDS, Market analysis, Policies/deployment programs, Technology characterizations Website https://www.climateinvestmentf Country Algeria UN Region South-Eastern Asia References Middle East and North Africa Regional Program (Algeria, Egypt, Jorban, Morroco, Tunisia)-Clean Technology Fund (CTF)[1]

319

St. Kitts and Nevis-Caribbean Community (CARICOM) Sustainable Energy  

Open Energy Info (EERE)

St. Kitts and Nevis-Caribbean Community (CARICOM) Sustainable Energy St. Kitts and Nevis-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Jump to: navigation, search Name St. Kitts and Nevis-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Agency/Company /Organization Inter-American Development Bank, World Watch Institute (WWI) Sector Climate, Energy Focus Area Renewable Energy, Economic Development, Energy Efficiency, Greenhouse Gas, Grid Assessment and Integration, Industry, People and Policy, Transportation Topics Background analysis, Baseline projection, Finance, GHG inventory, Implementation, Low emission development planning, -Roadmap, Market analysis, Policies/deployment programs, Resource assessment, Technology characterizations Program Start 2012 Program End 2012

320

Suriname-Caribbean Community (CARICOM) Sustainable Energy Roadmap and  

Open Energy Info (EERE)

Page Page Edit with form History Facebook icon Twitter icon » Suriname-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Jump to: navigation, search Name Suriname-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Agency/Company /Organization Inter-American Development Bank, World Watch Institute (WWI) Sector Climate, Energy Focus Area Renewable Energy, Economic Development, Energy Efficiency, Greenhouse Gas, Grid Assessment and Integration, Industry, People and Policy, Transportation Topics Background analysis, Baseline projection, Finance, GHG inventory, Implementation, Low emission development planning, -Roadmap, Market analysis, Policies/deployment programs, Resource assessment, Technology characterizations

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


321

South Africa-Clean Technology Fund (CTF) | Open Energy Information  

Open Energy Info (EERE)

South Africa-Clean Technology Fund (CTF) South Africa-Clean Technology Fund (CTF) Jump to: navigation, search Name South Africa-Clean Technology Fund (CTF) Agency/Company /Organization African Development Bank, Asian Development Bank, European Bank for Reconstruction and Development, Inter-American Development Bank, World Bank Sector Climate, Energy Focus Area Energy Efficiency, Geothermal, Transportation Topics Background analysis, Finance, Implementation, Low emission development planning, Market analysis Website http://www.climateinvestmentfu Country South Africa Southern Africa References Middle East and North Africa Regional Program (Algeria, Egypt, Jorban, Morroco, Tunisia)-Clean Technology Fund (CTF)[1] South Africa-CTF Investment Plan[2] South Africa-Clean Technology Fund (CTF) Screenshot

322

Trinidad and Tobago-Caribbean Community (CARICOM) Sustainable Energy  

Open Energy Info (EERE)

Trinidad and Tobago-Caribbean Community (CARICOM) Sustainable Energy Trinidad and Tobago-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Jump to: navigation, search Name Trinidad and Tobago-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Agency/Company /Organization Inter-American Development Bank, World Watch Institute (WWI) Sector Climate, Energy Focus Area Renewable Energy, Economic Development, Energy Efficiency, Greenhouse Gas, Grid Assessment and Integration, Industry, People and Policy, Transportation Topics Background analysis, Baseline projection, Finance, GHG inventory, Implementation, Low emission development planning, -Roadmap, Market analysis, Policies/deployment programs, Resource assessment, Technology characterizations Program Start 2012 Program End 2012

323

Belize-Caribbean Community (CARICOM) Sustainable Energy Roadmap and  

Open Energy Info (EERE)

Belize-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Belize-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Jump to: navigation, search Name Belize-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Agency/Company /Organization Inter-American Development Bank, World Watch Institute (WWI) Sector Climate, Energy Focus Area Renewable Energy, Economic Development, Energy Efficiency, Greenhouse Gas, Grid Assessment and Integration, Industry, People and Policy, Transportation Topics Background analysis, Baseline projection, Finance, GHG inventory, Implementation, Low emission development planning, -Roadmap, Market analysis, Policies/deployment programs, Resource assessment, Technology characterizations Program Start 2012 Program End 2012 Country Belize Central America

324

Clean Technology Fund (CTF) | Open Energy Information  

Open Energy Info (EERE)

Fund (CTF) Fund (CTF) (Redirected from Vietnam-Clean Technology Fund (CTF)) Jump to: navigation, search Name Clean Technology Fund (CTF) Agency/Company /Organization African Development Bank, Asian Development Bank, European Bank for Reconstruction and Development, Inter-American Development Bank, World Bank Sector Climate, Energy Focus Area Energy Efficiency, Geothermal, Transportation Topics Background analysis, Finance, Implementation, Low emission development planning, Market analysis Website http://www.climateinvestmentfu Country Algeria, Egypt, Indonesia, Jordan, Kazakhstan, Mexico, Morocco, Nigeria, Philippines, South Africa, Thailand, Tunisia UN Region South-Eastern Asia References Middle East and North Africa Regional Program (Algeria, Egypt, Jorban, Morroco, Tunisia)-Clean Technology Fund (CTF)[1]

325

Montserrat-Caribbean Community (CARICOM) Sustainable Energy Roadmap and  

Open Energy Info (EERE)

Montserrat-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Montserrat-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Jump to: navigation, search Name Montserrat-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Agency/Company /Organization Inter-American Development Bank, World Watch Institute (WWI) Sector Climate, Energy Focus Area Renewable Energy, Economic Development, Energy Efficiency, Greenhouse Gas, Grid Assessment and Integration, Industry, People and Policy, Transportation Topics Background analysis, Baseline projection, Finance, GHG inventory, Implementation, Low emission development planning, -Roadmap, Market analysis, Policies/deployment programs, Resource assessment, Technology characterizations Program Start 2012 Program End 2012 Country Montserrat

326

Nigeria-Clean Technology Fund (CTF) | Open Energy Information  

Open Energy Info (EERE)

Nigeria-Clean Technology Fund (CTF) Nigeria-Clean Technology Fund (CTF) Jump to: navigation, search Name Nigeria-Climate Technology Fund (CTF) Agency/Company /Organization African Development Bank, Asian Development Bank, European Bank for Reconstruction and Development, Inter-American Development Bank, World Bank Sector Climate, Energy Focus Area Energy Efficiency, Geothermal, Transportation Topics Background analysis, Finance, Implementation, Low emission development planning, Market analysis Website http://www.climateinvestmentfu Country Nigeria Western Africa References Nigeria-CTF Investment Plan[1] Nigeria-Climate Technology Fund (CTF) Screenshot Overview "The Clean Technology Fund (CTF), one of two Climate Investment Funds, promotes scaled-up financing for demonstration, deployment and transfer of

327

Guyana-Caribbean Community (CARICOM) Sustainable Energy Roadmap and  

Open Energy Info (EERE)

Guyana-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Guyana-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Jump to: navigation, search Name Guyana-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Agency/Company /Organization Inter-American Development Bank, World Watch Institute (WWI) Sector Climate, Energy Focus Area Renewable Energy, Economic Development, Energy Efficiency, Greenhouse Gas, Grid Assessment and Integration, Industry, People and Policy, Transportation Topics Background analysis, Baseline projection, Finance, GHG inventory, Implementation, Low emission development planning, -Roadmap, Market analysis, Policies/deployment programs, Resource assessment, Technology characterizations Program Start 2012 Program End 2012 Country Guyana South America

328

Haiti-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy  

Open Energy Info (EERE)

Haiti-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Haiti-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Jump to: navigation, search Name Haiti-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Agency/Company /Organization Inter-American Development Bank, World Watch Institute (WWI) Sector Climate, Energy Focus Area Renewable Energy, Economic Development, Energy Efficiency, Greenhouse Gas, Grid Assessment and Integration, Industry, People and Policy, Transportation Topics Background analysis, Baseline projection, Finance, GHG inventory, Implementation, Low emission development planning, -Roadmap, Market analysis, Policies/deployment programs, Resource assessment, Technology characterizations Program Start 2012 Program End 2012 Country Haiti Caribbean References CARICOM Sustainable Energy Roadmap and Strategy [1]

329

Grenada-Caribbean Community (CARICOM) Sustainable Energy Roadmap and  

Open Energy Info (EERE)

Grenada-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Grenada-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Jump to: navigation, search Name Grenada-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Agency/Company /Organization Inter-American Development Bank, World Watch Institute (WWI) Sector Climate, Energy Focus Area Renewable Energy, Economic Development, Energy Efficiency, Greenhouse Gas, Grid Assessment and Integration, Industry, People and Policy, Transportation Topics Background analysis, Baseline projection, Finance, GHG inventory, Implementation, Low emission development planning, -Roadmap, Market analysis, Policies/deployment programs, Resource assessment, Technology characterizations Program Start 2012 Program End 2012 Country Grenada Caribbean

330

Finanzas Carbono | Open Energy Information  

Open Energy Info (EERE)

Finanzas Carbono Finanzas Carbono Jump to: navigation, search Tool Summary LAUNCH TOOL Name: Finanzas Carbono Agency/Company /Organization: Inter-American Development Bank Partner: United Nations Environment Programme, World Bank Sector: Energy, Climate Focus Area: Offsets and Certificates Topics: Finance Resource Type: Dataset Website: finanzascarbono.org/ UN Region: Caribbean, Central America, South America Finanzas Carbono Screenshot References: Carbon Finance Portal[1] Logo: Finanzas Carbono "The knowledge platform Carbon Finance is a vehicle for exchanging information, capabilities and online services, serving as a meeting point for the various stakeholders in the carbon market in Latin America." "The knowledge platform Carbon Finance 's main objective is to become a

331

Turkey-Clean Technology Fund (CTF) | Open Energy Information  

Open Energy Info (EERE)

Turkey-Clean Technology Fund (CTF) Turkey-Clean Technology Fund (CTF) Jump to: navigation, search Name Turkey-Climate Technology Fund (CTF) Agency/Company /Organization African Development Bank, Asian Development Bank, European Bank for Reconstruction and Development, Inter-American Development Bank, World Bank Sector Climate, Energy Focus Area Energy Efficiency, Geothermal, Transportation Topics Background analysis, Finance, Implementation, Low emission development planning, Market analysis Website http://www.climateinvestmentfu Country Turkey Western Asia References Turkey-CTF Investment Plan[1] Turkey-Climate Technology Fund (CTF) Screenshot Overview "The Clean Technology Fund (CTF), one of two Climate Investment Funds, promotes scaled-up financing for demonstration, deployment and transfer of

332

Kazakhstan-Clean Technology Fund (CTF) | Open Energy Information  

Open Energy Info (EERE)

Kazakhstan-Clean Technology Fund (CTF) Kazakhstan-Clean Technology Fund (CTF) Jump to: navigation, search Name Climate Technology Fund (CTF) Agency/Company /Organization African Development Bank, Asian Development Bank, European Bank for Reconstruction and Development, Inter-American Development Bank, World Bank Sector Climate, Energy Focus Area Energy Efficiency, Geothermal, Transportation Topics Background analysis, Finance, Implementation, Low emission development planning, Market analysis Website http://www.climateinvestmentfu Country Kazakhstan Central Asia References Kazakhstan-CTF Investment Plan[1] Climate Technology Fund (CTF) Screenshot Overview "The Clean Technology Fund (CTF), one of two Climate Investment Funds, promotes scaled-up financing for demonstration, deployment and transfer of

333

Dominica-Caribbean Community (CARICOM) Sustainable Energy Roadmap and  

Open Energy Info (EERE)

Dominica-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Dominica-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Jump to: navigation, search Name Dominica-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Agency/Company /Organization Inter-American Development Bank, World Watch Institute (WWI) Sector Climate, Energy Focus Area Renewable Energy, Economic Development, Energy Efficiency, Greenhouse Gas, Grid Assessment and Integration, Industry, People and Policy, Transportation Topics Background analysis, Baseline projection, Finance, GHG inventory, Implementation, Low emission development planning, -Roadmap, Market analysis, Policies/deployment programs, Resource assessment, Technology characterizations Program Start 2012 Program End 2012 Country Dominica Caribbean

334

Colombia-Clean Technology Fund (CTF) | Open Energy Information  

Open Energy Info (EERE)

Colombia-Clean Technology Fund (CTF) Colombia-Clean Technology Fund (CTF) Jump to: navigation, search Name Colombia-Climate Technology Fund (CTF) Agency/Company /Organization African Development Bank, Asian Development Bank, European Bank for Reconstruction and Development, Inter-American Development Bank, World Bank Sector Climate, Energy Focus Area Energy Efficiency, Geothermal, Transportation Topics Background analysis, Finance, Implementation, Low emission development planning, Market analysis Website http://www.climateinvestmentfu Country Colombia South America References Colombia-CTF Investment Plan[1] Colombia-Climate Technology Fund (CTF) Screenshot Overview "The Clean Technology Fund (CTF), one of two Climate Investment Funds, promotes scaled-up financing for demonstration, deployment and transfer of

335

Saint Lucia-Caribbean Community (CARICOM) Sustainable Energy Roadmap and  

Open Energy Info (EERE)

Saint Lucia-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Saint Lucia-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Jump to: navigation, search Name Saint-LuciaCaribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Agency/Company /Organization Inter-American Development Bank, World Watch Institute (WWI) Sector Climate, Energy Focus Area Renewable Energy, Economic Development, Energy Efficiency, Greenhouse Gas, Grid Assessment and Integration, Industry, People and Policy, Transportation Topics Background analysis, Baseline projection, Finance, GHG inventory, Implementation, Low emission development planning, -Roadmap, Market analysis, Policies/deployment programs, Resource assessment, Technology characterizations Program Start 2012 Program End 2012 Country Saint Lucia

336

Clean Technology Fund (CTF) | Open Energy Information  

Open Energy Info (EERE)

Clean Technology Fund (CTF) Clean Technology Fund (CTF) Jump to: navigation, search Name Clean Technology Fund (CTF) Agency/Company /Organization African Development Bank, Asian Development Bank, European Bank for Reconstruction and Development, Inter-American Development Bank, World Bank Sector Climate, Energy Focus Area Energy Efficiency, Geothermal, Transportation Topics Background analysis, Finance, Implementation, Low emission development planning, Market analysis Website http://www.climateinvestmentfu Country Algeria, Egypt, Indonesia, Jordan, Kazakhstan, Mexico, Morocco, Nigeria, Philippines, South Africa, Thailand, Tunisia UN Region South-Eastern Asia References Middle East and North Africa Regional Program (Algeria, Egypt, Jorban, Morroco, Tunisia)-Clean Technology Fund (CTF)[1]

337

Saint Vincent and the Grenadines-Caribbean Community (CARICOM) Sustainable  

Open Energy Info (EERE)

Saint Vincent and the Grenadines-Caribbean Community (CARICOM) Sustainable Saint Vincent and the Grenadines-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Jump to: navigation, search Name Saint Vincent and the Grenadines-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Agency/Company /Organization Inter-American Development Bank, World Watch Institute (WWI) Sector Climate, Energy Focus Area Renewable Energy, Economic Development, Energy Efficiency, Greenhouse Gas, Grid Assessment and Integration, Industry, People and Policy, Transportation Topics Background analysis, Baseline projection, Finance, GHG inventory, Implementation, Low emission development planning, -Roadmap, Market analysis, Policies/deployment programs, Resource assessment, Technology characterizations Program Start 2012

338

Barbados-Caribbean Community (CARICOM) Sustainable Energy Roadmap and  

Open Energy Info (EERE)

Barbados-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Barbados-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Jump to: navigation, search Name Barbados-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Agency/Company /Organization Inter-American Development Bank, World Watch Institute (WWI) Sector Climate, Energy Focus Area Renewable Energy, Economic Development, Energy Efficiency, Greenhouse Gas, Grid Assessment and Integration, Industry, People and Policy, Transportation Topics Background analysis, Baseline projection, Finance, GHG inventory, Implementation, Low emission development planning, -Roadmap, Market analysis, Policies/deployment programs, Resource assessment, Technology characterizations Program Start 2012 Program End 2012 Country Barbados Caribbean

339

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

SciTech Connect

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

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

2011-10-01T23:59:59.000Z

340

The Royal Observatory Edinburgh comprises the UK Astronomy Technology Centre of the Science and Technology Facilities Council, the Institute for Astronomy of the University of Edinburgh and the ROE Visitor Centre.  

E-Print Network (OSTI)

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

Tittley, Eric

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341

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

E-Print Network (OSTI)

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

Paris-Sud XI, Université de

342

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

E-Print Network (OSTI)

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

343

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

E-Print Network (OSTI)

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

Rosei, Federico

344

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

E-Print Network (OSTI)

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

Coppi, Paolo

345

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

E-Print Network (OSTI)

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

Bresee, J. C.

2011-01-01T23:59:59.000Z

346

Uruguay-Climate Change Mitigation and Agriculture in Latin America and the  

Open Energy Info (EERE)

Uruguay-Climate Change Mitigation and Agriculture in Latin America and the Uruguay-Climate Change Mitigation and Agriculture in Latin America and the Caribbean Jump to: navigation, search Logo: Uruguay-Climate Change Mitigation and Agriculture in Latin America and the Caribbean Name Uruguay-Climate Change Mitigation and Agriculture in Latin America and the Caribbean Agency/Company /Organization Inter-American Development Bank, The Regional Fund for Agricultural Technology, Government of New Zealand Sector Climate, Land Focus Area Agriculture Topics Background analysis, GHG inventory, Low emission development planning Website http://www.iadb.org/en/news/ne Program Start 2011 Country Uruguay South America References IDB, FONTAGRO, Government of New Zealand sign agreement on climate change mitigation and agriculture in Latin America and the Caribbean[1]

347

Thailand-Clean Technology Fund (CTF) | Open Energy Information  

Open Energy Info (EERE)

Thailand-Clean Technology Fund (CTF) Thailand-Clean Technology Fund (CTF) Jump to: navigation, search Name Thailand-Climate Technology Fund (CTF) Agency/Company /Organization African Development Bank, Asian Development Bank, European Bank for Reconstruction and Development, Inter-American Development Bank, World Bank Sector Climate, Energy Focus Area Energy Efficiency, Geothermal, Transportation Topics Background analysis, Finance, Implementation, Low emission development planning, Market analysis Website http://www.climateinvestmentfu Country Thailand South-Eastern Asia References Thailand-CTF Investment Plan[1] Thailand-Climate Technology Fund (CTF) Screenshot Overview "The Clean Technology Fund (CTF), one of two Climate Investment Funds, promotes scaled-up financing for demonstration, deployment and transfer of

348

Jamaica-Caribbean Community (CARICOM) Sustainable Energy Roadmap and  

Open Energy Info (EERE)

form form View source History View New Pages Recent Changes All Special Pages Semantic Search/Querying Get Involved Help Apps Datasets Community Login | Sign Up Search Page Edit with form History Facebook icon Twitter icon » Jamaica-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Jump to: navigation, search Name Jamaica-Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Agency/Company /Organization Inter-American Development Bank, World Watch Institute (WWI) Sector Climate, Energy Focus Area Renewable Energy, Economic Development, Energy Efficiency, Greenhouse Gas, Grid Assessment and Integration, Industry, People and Policy, Transportation Topics Background analysis, Baseline projection, Finance, GHG inventory, Implementation, Low emission development planning, -Roadmap, Market analysis, Policies/deployment programs, Resource assessment, Technology characterizations

349

Deputy Secretary Poneman's Remarks at the FIESP Energy Conference - As  

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

FIESP Energy Conference - FIESP Energy Conference - As Prepared for Delivery Deputy Secretary Poneman's Remarks at the FIESP Energy Conference - As Prepared for Delivery August 15, 2011 - 6:21pm Addthis Deputy Secretary Daniel Poneman FIESP Energy Conference Keynote Remarks Monday, August 15, 2011 Sao Paulo, Brazil Introduction Bom dia. Thank you, Mr. Xavier, for the kind introduction. And thank you, FIESP, for the opportunity to speak here today at this important conference. Before I begin, I'd like to take a moment to recognize my colleagues joining me on stage: Carlos Henrique de Abreu e Silva, the Director of U.S., Canada and Inter-American Affairs for Brazil's Ministry of Foreign Affairs; Steven Bipes, the Executive Director of the U.S. Section of the Brazil-U.S. Business Council; and Luiz Gabriel Rico, the CEO of the

350

IADB/UNDP LEDS Community of Practice | Open Energy Information  

Open Energy Info (EERE)

IADB/UNDP LEDS Community of Practice IADB/UNDP LEDS Community of Practice Jump to: navigation, search Name IADB/UNDP LEDS Community of Practice Agency/Company /Organization Inter-American Development Bank, United Nations Development Programme (UNDP) Sector Climate, Energy Focus Area People and Policy Topics Low emission development planning, -LEDS, Policies/deployment programs Website http://finanzascarbono.org/com References LEDS Community of Practice-Carbon Finance Platform[1] "The objective of this Community of Practice is to provide the LAC region with information and facilitate technical discussions about the process of preparing national Low Emission Development Strategies. The workplan for 2012 includes the organization of discussion forums, seminars and webinars on LEDS preparation.

351

Chile-Climate Change Mitigation and Agriculture in Latin America and the  

Open Energy Info (EERE)

Chile-Climate Change Mitigation and Agriculture in Latin America and the Chile-Climate Change Mitigation and Agriculture in Latin America and the Caribbean Jump to: navigation, search Logo: Chile-Climate Change Mitigation and Agriculture in Latin America and the Caribbean Name Chile-Climate Change Mitigation and Agriculture in Latin America and the Caribbean Agency/Company /Organization Inter-American Development Bank, The Regional Fund for Agricultural Technology, Government of New Zealand Sector Climate, Land Focus Area Agriculture Topics Background analysis, GHG inventory, Low emission development planning Website http://www.iadb.org/en/news/ne Program Start 2011 Country Chile South America References IDB, FONTAGRO, Government of New Zealand sign agreement on climate change mitigation and agriculture in Latin America and the Caribbean[1]

352

Strategic Climate Fund (SCF) | Open Energy Information  

Open Energy Info (EERE)

SCF) SCF) Jump to: navigation, search Name Strategic Climate Fund (SCF) Agency/Company /Organization World Bank, African Development Bank, Asian Development Bank, European Development Bank, Inter-American Development Bank Sector Energy, Land Topics Finance, Market analysis Website http://www.climatefundsupdate. Program Start 2008 References Strategic Climate Fund (SCF)[1] "The Strategic Climate Fund (SCF) is one of the two funds of the Climate Investment Funds. It serves as an overarching framework to support three targeted programs with dedicated funding to pilot new approaches with potential for scaled-up, transformational action aimed at a specific climate change challenge or sectoral response. The SCF is an umbrella vehicle for the receipt of donor funds and

353

Secretary Moniz Addresses Conference on the Caribbean's Energy Future |  

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

Secretary Moniz Addresses Conference on the Caribbean's Energy Secretary Moniz Addresses Conference on the Caribbean's Energy Future Secretary Moniz Addresses Conference on the Caribbean's Energy Future December 6, 2013 - 2:42pm Addthis Secretary Moniz Addresses Conference on the Caribbean’s Energy Future Secretary Moniz joined Inter-American Development Bank President Luis Alberto Moreno in welcoming a group of Caribbean ministers who convened to discuss the region's energy future, climate change, and the roles of energy efficiency, renewable energy and natural gas. Addthis Related Articles Secretary Chu's Remarks at the 2012 IAEA General Conference -- As Prepared for Delivery Energy Department Invests Over $7 Million to Deploy Tribal Clean Energy Projects Deputy Secretary Daniel Poneman's Remarks to the Washington Institute for

354

Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy |  

Open Energy Info (EERE)

Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Jump to: navigation, search Name Caribbean Community (CARICOM) Sustainable Energy Roadmap and Strategy Agency/Company /Organization Inter-American Development Bank, World Watch Institute (WWI) Sector Climate, Energy Focus Area Renewable Energy, Economic Development, Energy Efficiency, Greenhouse Gas, Grid Assessment and Integration, Industry, People and Policy, Transportation Topics Background analysis, Baseline projection, Finance, GHG inventory, Implementation, Low emission development planning, -Roadmap, Market analysis, Policies/deployment programs, Resource assessment, Technology characterizations Program Start 2012 Program End 2012 Country Antigua and Barbuda, Bahamas, Barbados, Belize, Dominica, Grenada, Guyana, Haiti, Jamaica, Montserrat, St. Lucia, St. Vincent and the Grenadines, St. Kitts and Nevis, Suriname, Trinidad and Tobago

355

News & Blog | Department of Energy  

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

Blog Blog News & Blog News December 6, 2013 Secretary Moniz Addresses Conference on the Caribbean's Energy Future Secretary Moniz joined Inter-American Development Bank President Luis Alberto Moreno in welcoming a group of Caribbean ministers who convened to discuss the region's energy future, climate change, and the roles of energy efficiency, renewable ene December 5, 2013 Department of Energy signs Memorandum of Understanding with Colombia's Ministry of Mines and Energy to Strengthen Energy Cooperation On December 2, 2013, the Department of Energy signed a Memorandum of Understanding with Colombia's Ministry of Mines and Energy to strengthen cooperation in the energy sector and to promote regional leadership on energy and climate change. December 3, 2013 U.S.-South Africa Energy Meeting

356

Event:Latin American Carbon Forum 2013 | Open Energy Information  

Open Energy Info (EERE)

3 3 Jump to: navigation, search Calendar.png Latin American Carbon Forum 2013: on 2013/03/25 The Seventh Latin American and Caribbean Carbon Forum (LACF) will discuss prospects for carbon projects in Latin America. The Forum is co-organized by the Inter-American Development Bank (IDB), the Latin American Development Bank (CAF), the World Bank, the International Emissions Trading Association (IETA), the Latin American Energy Organization (OLADE), the UN Environment Programme (UNEP) Risø Centre and the UN Framework Convention on Climate Change (UNFCCC). Event Details Name Latin American Carbon Forum 2013 Date 2013/03/25 Location Rio de Janeiro, Brazil Tags LEDS, Training, CLEAN Website Event Website Ret LikeLike UnlikeLike You like this.Sign Up to see what your friends like.

357

Argentina-Climate Change Mitigation and Agriculture in Latin America and  

Open Energy Info (EERE)

Argentina-Climate Change Mitigation and Agriculture in Latin America and Argentina-Climate Change Mitigation and Agriculture in Latin America and the Caribbean Jump to: navigation, search Logo: Argentina-Climate Change Mitigation and Agriculture in Latin America and the Caribbean Name Argentina-Climate Change Mitigation and Agriculture in Latin America and the Caribbean Agency/Company /Organization Inter-American Development Bank, The Regional Fund for Agricultural Technology, Government of New Zealand Sector Climate, Land Focus Area Agriculture Topics Background analysis, GHG inventory, Low emission development planning, -LEDS, Policies/deployment programs Website http://www.iadb.org/en/news/ne Program Start 2011 Country Argentina UN Region South America References IDB, FONTAGRO, Government of New Zealand sign agreement on climate change mitigation and agriculture in Latin America and the Caribbean[1]

358

Indonesia-Clean Technology Fund (CTF) | Open Energy Information  

Open Energy Info (EERE)

Indonesia-Clean Technology Fund (CTF) Indonesia-Clean Technology Fund (CTF) Jump to: navigation, search Name Indonesia-Clean Technology Fund (CTF) Agency/Company /Organization African Development Bank, Asian Development Bank, European Bank for Reconstruction and Development, Inter-American Development Bank, World Bank Sector Climate, Energy Focus Area Energy Efficiency, Geothermal, Transportation Topics Background analysis, Finance, Implementation, Low emission development planning, Market analysis Website http://www.climateinvestmentfu Country Indonesia UN Region South-Eastern Asia References Indonesia-Clean Technology Fund (CTF)[1] Indonesia-Clean Technology Fund (CTF) Screenshot Contents 1 Overview 2 Activities 2.1 Indonesia 2.2 Other Countries 3 Outcomes, Lessons Learned and Good Practices

359

IDB-Colombia-Renwable Energy and Energy Efficiency Finance Facility | Open  

Open Energy Info (EERE)

Renwable Energy and Energy Efficiency Finance Facility Renwable Energy and Energy Efficiency Finance Facility Jump to: navigation, search Name IDB-Colombia-Renwable Energy and Energy Efficiency Finance Facility Agency/Company /Organization Inter-American Development Bank Partner International Finance Corporation (IFC), Clean Technology Funds (CFT) Sector Energy Focus Area Energy Efficiency Topics Finance Website http://www.iadb.org/en/news/ne Program Start 2011 Country Colombia UN Region South America References IDB approves innovative $90 million facility to support energy efficiency, cleaner production and renewable energy projects in Colombia[1] This article is a stub. You can help OpenEI by expanding it. References ↑ "IDB approves innovative $90 million facility to support energy efficiency, cleaner production and renewable energy projects in

360

PI News Archive | Department of Energy  

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

News Archive News Archive PI News Archive RSS December 6, 2013 Secretary Moniz Addresses Conference on the Caribbean's Energy Future Secretary Moniz joined Inter-American Development Bank President Luis Alberto Moreno in welcoming a group of Caribbean ministers who convened to discuss the region's energy future, climate change, and the roles of energy efficiency, renewable energy and natural gas. December 5, 2013 Department of Energy signs Memorandum of Understanding with Colombia's Ministry of Mines and Energy to Strengthen Energy Cooperation On December 2, 2013, the Department of Energy signed a Memorandum of Understanding with Colombia's Ministry of Mines and Energy to strengthen cooperation in the energy sector and to promote regional leadership on energy and climate change.

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361

Post-2012 Climate Instruments in the transport sector | Open Energy  

Open Energy Info (EERE)

Post-2012 Climate Instruments in the transport sector Post-2012 Climate Instruments in the transport sector Jump to: navigation, search Name Post-2012 Climate Instruments in the transport sector Agency/Company /Organization Energy Research Centre of the Netherlands Partner Asian Development Bank Sector Energy Focus Area Transportation Topics Finance Resource Type Presentation Website http://www.slocat.net Program Start 2009 Program End 2010 UN Region South-Eastern Asia References Post-2012 Climate Instruments in the transport sector (CITS)[1] The post 2012 Climate Instruments in the transport sector (CITS) project implemented by the Asian Development Bank (ADB), in cooperation with the Inter-American Development Bank (IDB), is a first step to help ensure that the transport sector can benefit from the revised/new climate change

362

DOE to Participate in Colombian Regional Energy Meeting Ahead of Energy and  

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

DOE to Participate in Colombian Regional Energy Meeting Ahead of DOE to Participate in Colombian Regional Energy Meeting Ahead of Energy and Climate Ministerial of the Americas DOE to Participate in Colombian Regional Energy Meeting Ahead of Energy and Climate Ministerial of the Americas February 26, 2010 - 12:00am Addthis WASHINGTON, D.C. - Secretary Chu announced today that senior representatives from the Department of Energy are attending a regional energy meeting hosted by the Colombian Ministry of Energy in Bogotá, Colombia. The meeting will bring together public and private representatives from the Andean region, as well regional multilateral organizations, including the Inter-American Development Bank, the Organization of American States and the U.S.-Colombia Chamber of Commerce, to discuss the Energy and Climate Partnership of the Americas (ECPA).

363

Colombia-Climate Change Mitigation and Agriculture in Latin America and the  

Open Energy Info (EERE)

Colombia-Climate Change Mitigation and Agriculture in Latin America and the Colombia-Climate Change Mitigation and Agriculture in Latin America and the Caribbean Jump to: navigation, search Logo: Colombia-Climate Change Mitigation and Agriculture in Latin America and the Caribbean Name Colombia-Climate Change Mitigation and Agriculture in Latin America and the Caribbean Agency/Company /Organization Inter-American Development Bank, The Regional Fund for Agricultural Technology, Government of New Zealand Sector Climate, Land Focus Area Agriculture Topics Background analysis, GHG inventory, Low emission development planning Website http://www.iadb.org/en/news/ne Program Start 2011 Country Colombia South America References IDB, FONTAGRO, Government of New Zealand sign agreement on climate change mitigation and agriculture in Latin America and the Caribbean[1]

364

Philippines-Clean Technology Fund (CTF) | Open Energy Information  

Open Energy Info (EERE)

Philippines-Clean Technology Fund (CTF) Philippines-Clean Technology Fund (CTF) Jump to: navigation, search Name Philippines-Climate Technology Fund (CTF) Agency/Company /Organization African Development Bank, Asian Development Bank, European Bank for Reconstruction and Development, Inter-American Development Bank, World Bank Sector Climate, Energy Focus Area Energy Efficiency, Geothermal, Transportation Topics Background analysis, Finance, Implementation, Low emission development planning, Market analysis Website http://www.climateinvestmentfu Country Philippines South-Eastern Asia References Philippines-CTF Investment Plan[1] Philippines-Climate Technology Fund (CTF) Screenshot Overview "The Clean Technology Fund (CTF), one of two Climate Investment Funds, promotes scaled-up financing for demonstration, deployment and transfer of

365

Dominican Republic-Climate Change Mitigation and Agriculture in Latin  

Open Energy Info (EERE)

Dominican Republic-Climate Change Mitigation and Agriculture in Latin Dominican Republic-Climate Change Mitigation and Agriculture in Latin America and the Caribbean Jump to: navigation, search Logo: Dominican Republic-Climate Change Mitigation and Agriculture in Latin America and the Caribbean Name Dominican Republic-Climate Change Mitigation and Agriculture in Latin America and the Caribbean Agency/Company /Organization Inter-American Development Bank, The Regional Fund for Agricultural Technology, Government of New Zealand Sector Climate, Land Focus Area Agriculture Topics Background analysis, GHG inventory, Low emission development planning Website http://www.iadb.org/en/news/ne Program Start 2011 Country Dominican Republic Caribbean References IDB, FONTAGRO, Government of New Zealand sign agreement on climate change mitigation and agriculture in Latin America and the Caribbean[1]

366

Egypt-Clean Technology Fund (CTF) | Open Energy Information  

Open Energy Info (EERE)

Egypt-Clean Technology Fund (CTF) Egypt-Clean Technology Fund (CTF) Jump to: navigation, search Name Egypt-Clean Technology Fund (CTF) Agency/Company /Organization African Development Bank, Asian Development Bank, European Bank for Reconstruction and Development, Inter-American Development Bank, World Bank Sector Climate, Energy Focus Area Energy Efficiency, Geothermal, Transportation Topics Background analysis, Finance, Implementation, Low emission development planning, Market analysis Website http://www.climateinvestmentfu Country Egypt Northern Africa References Middle East and North Africa Regional Program (Algeria, Egypt, Jorban, Morroco, Tunisia)-Clean Technology Fund (CTF)[1] Egypt-Clean Technology Fund (CTF) Screenshot Contents 1 Overview 2 Activities 2.1 Middle East and North Africa Regional Program (Algeria, Egypt, Jorban, Morroco, Tunisia)

367

Sustainable Transport and Air Quality Conference for Latin America and the  

Open Energy Info (EERE)

and Air Quality Conference for Latin America and the and Air Quality Conference for Latin America and the Caribbean 2011 Jump to: navigation, search Calendar.png Sustainable Transport and Air Quality Conference for Latin America and the Caribbean 2011: on 2011/05/09 "This Conference is co-sponsored by the Clean Air Institute (CAI), the Global Environment Facility (GEF), the Inter-American Development Bank (IDB), the World Bank, the World Mayors Council on Climate Change, GIZ and the Governments of Argentina, Mexico and Spain. Participants will discuss "How to Achieve Sustainable Urban Transport?" Among other things, the Conference will examine health and environmental benefits of improving urban transport, emissions inventories and monitoring, use of alternative fuels, carbon financing to improve urban transport, and regional

368

Jordan-Clean Technology Fund (CTF) | Open Energy Information  

Open Energy Info (EERE)

Jordan-Clean Technology Fund (CTF) Jordan-Clean Technology Fund (CTF) Jump to: navigation, search Name Jordan-Clean Technology Fund (CTF) Agency/Company /Organization African Development Bank, Asian Development Bank, European Bank for Reconstruction and Development, Inter-American Development Bank, World Bank Sector Climate, Energy Focus Area Energy Efficiency, Geothermal, Transportation Topics Background analysis, Finance, Implementation, Low emission development planning, Market analysis Website http://www.climateinvestmentfu Country Jordan Western Asia References Middle East and North Africa Regional Program (Algeria, Egypt, Jorban, Morroco, Tunisia)-Clean Technology Fund (CTF)[1] Jordan-Clean Technology Fund (CTF) Screenshot Contents 1 Overview 2 Activities 2.1 Middle East and North Africa Regional Program (Algeria, Egypt, Jorban, Morroco, Tunisia)

369

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

Science Conference Proceedings (OSTI)

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

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

2013-06-01T23:59:59.000Z

370

An Update on the Status of the Pulsar?ALFA Survey  

Science Conference Proceedings (OSTI)

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

P. Lazarus; The PALFA Consortium

2011-01-01T23:59:59.000Z

371

Fermilab Today  

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

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

372

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

E-Print Network (OSTI)

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

Collins, Gary S.

373

Atmospheric Radiation Measurement Program  

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

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

374

Spectral Characteristics of the Convective Boundary Layer Over Uneven Terrain  

Science Conference Proceedings (OSTI)

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

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

1982-05-01T23:59:59.000Z

375

SciTech Connect: "smart grid"  

Office of Scientific and Technical Information (OSTI)

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

376

EUV beam line moves to PML  

Science Conference Proceedings (OSTI)

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

2013-01-03T23:59:59.000Z

377

Synchrotron Programs and Projects  

Science Conference Proceedings (OSTI)

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

2010-05-24T23:59:59.000Z

378

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

Science Conference Proceedings (OSTI)

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

379

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

E-Print Network (OSTI)

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

Castillo, Steven P.

380

Properties of Powder Metallurgy Beryllium  

Science Conference Proceedings (OSTI)

Table 19   Some production applications of wrought hot pressed beryllium...Type of material Special characteristics Solar cell boards??Orbiting Geophysical Observatory

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


381

Nuclear Science Division Annual Report 1995-1996  

E-Print Network (OSTI)

Observatory Cosmic Gamma-Ray Bursts and Soft Gamma RepeatersAxions Theories of Gamma-Ray Bursts Origin Extracting Power

Authors, Various

2010-01-01T23:59:59.000Z

382

Speeds and Arrival Times of Solar Transients Approximated by Self ...  

Science Conference Proceedings (OSTI)

Abstract The NASA Solar TErrestrial RElations Observatory (STEREO) mission offered the possibility to forecast the arrival times, speeds, and directions of solar ...

383

HMNewsFall06  

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

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...

384

On acoustic wave generation in uniform shear flow G. Gogoberidze  

E-Print Network (OSTI)

, 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.,

385

Three-dimensional magnetotelluric characterization of the Coso...  

Open Energy Info (EERE)

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...

386

Single-Column Modeling R. D. Cess Marine Sciences Research Center  

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

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...

387

Section 73  

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

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...

388

Optical observations of afterglows of gamma ray bursts localized by the high energy transient explorer.  

E-Print Network (OSTI)

??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-

2004-01-01T23:59:59.000Z

389

Massachusetts | Department of Energy  

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

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...

390

Bluer Skies and Brighter Days: The U.S. and India Collaborate...  

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

Articles This observatory is part of an air particles research initiative at Cape Cod National Seashore in Massachusetts, and includes dozens of sophisticated instruments...

391

Department of Energy Announces $7 Million in Funding for Climate...  

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

Collaboration This observatory is part of an air particles research initiative at Cape Cod National Seashore in Massachusetts, and includes dozens of sophisticated instruments...

392

Fermilab Today  

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

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...

393

Inquiring Minds  

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

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...

394

About Fermilab - History  

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

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:...

395

Energy Crossroads: Weather Data Resources | Environmental Energy...  

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

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...

396

--No Title--  

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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...

397

--No Title--  

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

UAO Urban Atmospheric Observatory Instrumentation Network Verification Facility - New York City A Center for the Development and Evaluation of Response Software and Instrumentation...

398

NETL: Methane Hydrates - DOE/NETL Projects  

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

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...

399

Fermilab | Science at Fermilab | Questions for the Universe ...  

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

someday shed light on dark matter: Large Hadron Collider, CERN, Geneva, Switzerland Sloan Digital Sky Survey, Fermilab, Batavia, IL VERITAS, Fred Lawrence Whipple Observatory,...

400

Acronyms and Abbreviations  

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

Observatories Programme GOS Global Observing System (WMO and WWW) GOS &09:Geomagnetic Observing System GPC Global Processing Center GPCC Global Precipitation Climatology...

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


401

User Facilities in the Environmental Assessment Division (EVS...  

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

The ARM Climate Research Facility, a Department of Energy (DOE) Office of Science user facility, provides data from strategically located climate observatories around the...

402

Towards a Neutron Microscope  

Science Conference Proceedings (OSTI)

Towards a Neutron Microscope. Summary: ... The novel lens is a Wolter Optic similar in design to the telescope of the CHANDRA x-ray observatory. ...

2013-07-23T23:59:59.000Z

403

Tech Beat July 9, 2008  

Science Conference Proceedings (OSTI)

... With the aim of improving forecasts of space weather, NASA's Solar Dynamics Observatory will peer deep inside the sun, to where the solar ...

2011-05-03T23:59:59.000Z

404

NIST Image Gallery: Image Details  

Science Conference Proceedings (OSTI)

... Description: With the aim of improving forecasts of space weather NASA's Solar Dynamics Observatory will peer deep inside the sun, to where the ...

405

Mapnottoscale. Mauna Kea, HI  

E-Print Network (OSTI)

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

406

Observing Cold Dust with Herschel / SPIRE  

Science Conference Proceedings (OSTI)

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

2010-01-01T23:59:59.000Z

407

Auger Finance Board Meeting 16 November 2008 P. Mantsch  

E-Print Network (OSTI)

. 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

408

Data challenges of time domain astronomy  

Science Conference Proceedings (OSTI)

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

2012-10-01T23:59:59.000Z

409

Creation and Detection of Cerenkov Light  

E-Print Network (OSTI)

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

410

LIGO-G000306-00-M Einstein's Theory of Gravitation  

E-Print Network (OSTI)

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.

411

LOS ALAMOS, N.M., Aug. 21, 2013-The High-Altitude Water Cherenkov (HAWC)  

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

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

412

Research Highlight  

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

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

413

1  

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

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-

414

New Variable Stars in the Globular Cluster NGC 6584  

E-Print Network (OSTI)

Using the Southeastern Association for Research in Astronomy 0.6 meter telescope located at Cerro Tololo, we searched for variable stars in the southern globular cluster NGC 6584. We obtained images during 8 nights between 28 May and 6 July of 2011. After processing the images, we used the image subtraction package ISIS developed by Alard (2000)to search for the variable stars. We identified a total of 69 variable stars in our 10x10 arcmin^2 field, including 43 variables cataloged by Millis & Liller (1980) and 26 hereto unknown variables. In total, we classified 46 of the variables as type RRab, with a mean period of 0.56776 days, 15 as type RRc with a mean period of 0.30886 days, perhaps one lower amplitude type RRe, with a period of 0.26482 days, 4 eclipsing binaries, and 3 long period (P > 2 days) variable stars. As many as 15 of the RRab Lyrae stars exhibited the Blazhko Effect. Furthermore, the mean periods of the RR Lyrae types, the exhibited period/amplitude relationship, and the ratio of N_c/(N_ab...

Toddy, Joseph M; Darragh, Andrew N; Murphy, Brian W

2012-01-01T23:59:59.000Z

415

Surface Heat Flux Variations across the Kuroshio Extension as Observed by Surface Flux Buoys  

Science Conference Proceedings (OSTI)

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

2010-10-01T23:59:59.000Z

416

Characterization of an advanced LIGO quadruple pendulum system  

E-Print Network (OSTI)

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-

2004-01-01T23:59:59.000Z

417

Project Title  

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

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...

418

Solar Neutrinos  

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

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...

419

NETL: Methane Hydrates - DOE/NETL Projects  

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

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

420

Low-Frequency Atmospheric Acoustic Energy Associated with Vortices Produced by Thunderstorms  

Science Conference Proceedings (OSTI)

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

2005-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "tololo inter-american observatory" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
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421

Graduate Course Catalog Table of Contents  

E-Print Network (OSTI)

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

Collins, Gary S.

422

Carbon Dioxide Variability and Atmospheric Circulation  

Science Conference Proceedings (OSTI)

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

1982-06-01T23:59:59.000Z

423

Underway and Moored Methods for Improving Accuracy in Measurement of Spectral Particulate Absorption and Attenuation  

Science Conference Proceedings (OSTI)

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 DallOlmo; M. Rois Langner; James Loftin; Michael J. Behrenfeld; Collin Roesler; Toby K. Westberry

2010-10-01T23:59:59.000Z

424

Achieving Climate Change Absolute Accuracy in Orbit  

Science Conference Proceedings (OSTI)

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

425

Natural Hazards and Earth System Sciences (2003) 3: 165170 c European Geosciences Union 2003 Natural Hazards  

E-Print Network (OSTI)

. 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

Paris-Sud XI, Université de

426

Nonlin. Processes Geophys., 13, 231235, 2006 www.nonlin-processes-geophys.net/13/231/2006/  

E-Print Network (OSTI)

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

Paris-Sud XI, Université de

427

Natural Hazards and Earth System Sciences (2004) 4: 5358 SRef-ID: 1684-9981/nhess/2004-4-53  

E-Print Network (OSTI)

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

Paris-Sud XI, Université de

428

Analysis of light curves from the 2003 Nov 14 occultation by Titan of TYC 1343-1855-1  

E-Print Network (OSTI)

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 2S ...

Zalucha, Angela M. (Angela Marie)

2007-01-01T23:59:59.000Z

429

Analysis of spatial mode sensitivity of gravitational wave interferometer and targeted search for gravitational radiation from the Crab pulsar  

E-Print Network (OSTI)

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)

2008-01-01T23:59:59.000Z

430

Subtropical Climatology of Direct Beam Solar Radiation  

Science Conference Proceedings (OSTI)

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

1982-03-01T23:59:59.000Z

431

In Situ CO2 and O2 Measurements on a Profiling Float  

Science Conference Proceedings (OSTI)

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 ...

Bjrn Fiedler; Peer Fietzek; Nuno Vieira; Pricles Silva; Henry C. Bittig; Arne Krtzinger

2013-01-01T23:59:59.000Z

432

Variations of the North Pacific Subtropical Mode Water from Direct Observations  

Science Conference Proceedings (OSTI)

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

433

Intrinsic Absorption in the Spectrum of NGC 7469: Simultaneous Chandra, FUSE, and STIS Observations  

E-Print Network (OSTI)

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.

434

Meteorological Tower Measurements of a Surface Cold Front  

Science Conference Proceedings (OSTI)

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

1984-08-01T23:59:59.000Z

435

The Frontal Hydraulic Head: A Micro-? Scale (1 km) Triggering Mechanism for Mesoconvective Weather Systems  

Science Conference Proceedings (OSTI)

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

1985-07-01T23:59:59.000Z

436

ARM - Instrument - mpl  

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

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,...

437

ARM - Instrument - tsi  

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

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,...

438

ARM - VAP Process - aerinf  

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

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...

439

ARM - Instrument - cpc  

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

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)...

440

ARM - Datastreams - aosccn100  

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

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...

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


441

ARM - VAP Product - qcrad1long  

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

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,...

442

ARM - Instrument - psap  

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

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...

443

ARM - Instrument - gndrad  

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

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,...

444

ARM - Instrument - skyrad  

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

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,...

445

ARM - Datastreams - nfov2ch  

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

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...

446

ARM - Datastreams - aosclap3w  

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

ARIES Observatory, Nainital, Uttarkhand, India PVC M1 Browse Data Highland Center, Cape Cod MA; AMF 1 Contact(s) Yin-Nan Lee (631) 344-3294 ynlee@bnl.gov Gunnar Senum (631)...

447

ARM - Datastreams - mplpolfs  

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

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...

448

ARM - Instrument - met  

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

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,...

449

ARM - Instrument - nfov  

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

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...

450

ARM - Instrument - dl  

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

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...

451

ARM - Instrument - nephelometer  

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

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...

452

ARM - Datastreams - vceil25k  

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

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,...

453

ARM - Instrument - mwrp  

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

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...

454

ARM - Instrument - sasze  

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

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...

455

ARM - Instrument - aeri  

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

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...

456

-----------------------REVIEW 1 ---------------------TITLE: Analyzing the most important part of the World Wide Web  

E-Print Network (OSTI)

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

457

10p Fermi 3/16/01  

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

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...

458

Fermi 3/29/02  

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

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...

459

All News Releases  

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

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...

460

Fermilab Today  

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

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...

Note: This page contains sample records for the topic "tololo inter-american observatory" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
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to obtain the most current and comprehensive results.


461

Optical observations of afterglows of gamma ray bursts localized by the high energy transient explorer  

E-Print Network (OSTI)

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, ...

Dullighan, Allyn, 1978-

2004-01-01T23:59:59.000Z

462

Intense spreading of radar echoes from ionospheric plasmas  

E-Print Network (OSTI)

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

2005-01-01T23:59:59.000Z

463

Incoherent scatter radar detection of enhanced plasma line in ionospheric E-region over Arecibo  

E-Print Network (OSTI)

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

2006-01-01T23:59:59.000Z

464

Moorings and Drifters for Real-Time Interdisciplinary Oceanography  

Science Conference Proceedings (OSTI)

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

1997-10-01T23:59:59.000Z

465

95-GHz Polarimetric Radar Measurements of Orographic Cap Clouds  

Science Conference Proceedings (OSTI)

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

1994-02-01T23:59:59.000Z

466

bigbangnucrpp.dvi  

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

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)...

467

A Study of the Remote Control for the East China Sea Seafloor Observation System  

Science Conference Proceedings (OSTI)

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

2012-08-01T23:59:59.000Z

468

Inversion of long-lived trace gas emissions using combined Eulerian and Lagrangian chemical transport models  

E-Print Network (OSTI)

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.

469

A high-frequency gravitational-wave burst search with LIGO's Hanford site  

E-Print Network (OSTI)

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

2009-01-01T23:59:59.000Z

470

A high-frequency gravitational-wave burst search with LIGO's Hanford site.  

E-Print Network (OSTI)

??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)

Villadsen, Jacqueline Rose

2009-01-01T23:59:59.000Z

471

Novel approaches to Newtonian noise suppression in interferometric gravitational wave detection  

E-Print Network (OSTI)

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

2011-01-01T23:59:59.000Z

472

ARM - Data Announcements Article  

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

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...

473

The role of oxygen in hydrogen sensing by a platinum-gate silicon carbide gas sensor: An ultrahigh vacuum study  

E-Print Network (OSTI)

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.

474

Element and system design for active and passive vibration isolation  

E-Print Network (OSTI)

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-

2005-01-01T23:59:59.000Z

475

Establishing the Moon as a Spectral Radiance Standard  

Science Conference Proceedings (OSTI)

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

1996-04-01T23:59:59.000Z

476

The Pulsar Search Collaboratory  

Science Conference Proceedings (OSTI)

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

2010-01-01T23:59:59.000Z

477

The search for gravitational wave bursts in data from the second LIGO science run  

E-Print Network (OSTI)

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

2005-01-01T23:59:59.000Z

478

Laboratory evaluation of laser-induced breakdown spectroscopy (LIBS) as a new in situ chemical sensing technique for the deep ocean  

E-Print Network (OSTI)

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-

2007-01-01T23:59:59.000Z

479

Physics Letters A 305 (2002) 239244 www.elsevier.com/locate/pla  

E-Print Network (OSTI)

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: malik@phys.ufl.edu (M

Florida, University of

480

--No Title--  

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

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...

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


481

An Atmospheric Soliton Observed with Doppler Radar, Differential Absorption Lidar, and a Molecular Doppler Lidar  

Science Conference Proceedings (OSTI)

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

2008-08-01T23:59:59.000Z

482

Wave-Turbulence Dynamics in the Stably Stratified Boundary Layer  

Science Conference Proceedings (OSTI)

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

1993-07-01T23:59:59.000Z

483

The Interaction of Tides with the Sill of a Tidally Energetic Inlet  

Science Conference Proceedings (OSTI)

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

1984-06-01T23:59:59.000Z

484

Atmospheric Transmission and Climate: Results from Smithsonian Measurements  

Science Conference Proceedings (OSTI)

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 sitesMount Montezuma, Chile, and Table ...

Robert G. Roosen; Ronald J. Angione

1984-09-01T23:59:59.000Z

485

Sorting in Patrick Geddes' Outlook Tower  

E-Print Network (OSTI)

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

1991-01-01T23:59:59.000Z

486

NuSTAR helps solve riddle of black hole spin  

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

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,...

487

The Hidden Role of Women in Monitoring Nineteenth-Century African Weather: Instrumental Observations in Equatorial Guinea  

Science Conference Proceedings (OSTI)

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 Domnguez-Castro; Jos M. Vaquero; Ricardo Garca-Herrera

2011-03-01T23:59:59.000Z

488

Meso- and Microscale Features of a Colorado Cold Front  

Science Conference Proceedings (OSTI)

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

1984-09-01T23:59:59.000Z

489

Sun or Moon Rise/Set Table for One Year  

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

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....

490

The Accretion of Ice Particles by Rime during Dry Growth  

Science Conference Proceedings (OSTI)

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

1985-01-01T23:59:59.000Z

491

--No Title--  

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

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...

492

Seasonal and Diurnal Variations in Aerosol Concentration on Whistler Mountain: Boundary Layer Influence and Synoptic-Scale Controls  

Science Conference Proceedings (OSTI)

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

2011-11-01T23:59:59.000Z

493

Calibrating Broadband UV Instruments: Ozone and Solar Zenith Angle Dependence  

Science Conference Proceedings (OSTI)

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

1998-08-01T23:59:59.000Z

494

Ground-Based Solar Absorption FTIR Spectroscopy: Characterization of Retrievals and First Results from a Novel Optical Design Instrument at a New NDACC Complementary Station  

Science Conference Proceedings (OSTI)

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

2007-03-01T23:59:59.000Z

495

Jesuits' Contribution to Meteorology  

Science Conference Proceedings (OSTI)

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 ...

Agustn Udas

1996-10-01T23:59:59.000Z

496

Lori Garver, NASA Deputy Administrator SOFIA Joining Forces Event  

E-Print Network (OSTI)

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

497

Remote Real-Time Video-Enabled Docking for Underwater Autonomous Platforms  

Science Conference Proceedings (OSTI)

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

2009-12-01T23:59:59.000Z

498

CO2 Retrieval over Clouds from the OCO Mission: Model Simulations and Error Analysis  

Science Conference Proceedings (OSTI)

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 ...

Jrme Vidot; Ralf Bennartz; Christopher W. ODell; Ren Preusker; Rasmus Lindstrot; Andrew K. Heidinger

2009-06-01T23:59:59.000Z

499

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...

500

Surface Meteorological Observations in Severe Thunderstorms. Part I: Design Details of TOTO  

Science Conference Proceedings (OSTI)

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

1983-05-01T23:59:59.000Z