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1

Integration Observatory  

E-Print Network [OSTI]

Hill, Stephen Wampler National Solar Observatory Piet Martens, Alisdair Davey Montana State University Joseph B. Gurman, George Dimitoglou Solar Data Analysis Center #12; VSO Overview 1 Perspective + From documents. ê Independent of platform and programming language + Three major components â Data encapsulation

Bogart, Richard S.

2

Sensors for Environmental Observatories  

E-Print Network [OSTI]

Sensors for Environmental Observatories Report of the NSF-Sponsored Workshop December 2004 #12 States of America. 2005. #12;Sensors for Environmental Observatories Report of the NSF Sponsored Workshop sensor technology and the networks that collect data from them. Present work clearly demonstrates

Hamilton, Michael P.

3

Alexey Kuznetsov Armagh Observatory  

E-Print Network [OSTI]

by the high-energy electrons that are the key factor in development of the flares. Therefore, radio Observatory 8 Radiometers / radiopolarimeters Full-disk observations * + " + , ' - & . $ / $ 0 $ $ 0 $ $ 1 2 3

4

The Sudbury Neutrino Observatory  

SciTech Connect (OSTI)

A report is given on the status of the Sudbury Neutrino Observatory, presently under construction in the Creighton nickel mine near Sudbury, Ontario in Canada. Focus is upon the technical factors involving a measurement of the charged-current and neutral-current interactions of solar neutrinos on deuterium.

Hime, A.

1996-09-01T23:59:59.000Z

5

Armagh Observatory Annual Report  

E-Print Network [OSTI]

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

6

The Green Computing Observatory: from  

E-Print Network [OSTI]

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

Lefèvre, Laurent

7

The Enriched Xenon Observatory  

SciTech Connect (OSTI)

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

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

2009-12-17T23:59:59.000Z

8

Energy Blog | Department of Energy  

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

7, 2011 ARM Mobile Facility instrumentation is installed in June 2011 at the ARIES Observatory in Nainital, India, for the Ganges Valley Aerosol Experiment (GVAX). | Courtesy of...

9

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

10

Space Telescope Programs Hubble Observatory  

E-Print Network [OSTI]

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

Colorado at Boulder, University of

11

Virtual Observatories A New Era for Astronomy  

E-Print Network [OSTI]

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

12

Chandra X-ray Observatory Center  

E-Print Network [OSTI]

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

13

Science with Virtual Observatory Tools  

E-Print Network [OSTI]

The Virtual Observatory is now mature enough to produce cutting-edge science results. The exploitation of astronomical data beyond classical identification limits with interoperable tools for statistical identification of sources has become a reality. I present the discovery of 68 optically faint, obscured (i.e., type 2) active galactic nuclei (AGN) candidates in the two GOODS fields using the Astrophysical Virtual Observatory (AVO) prototype. Thirty-one of these sources have high estimated X-ray powers (>10^44 erg/s) and therefore qualify as optically obscured quasars, the so-called QSO 2. The number of these objects in the GOODS fields is now 40, an improvement of a factor > 4 when compared to the only 9 such sources previously known. By going ~ 3 magnitudes fainter than previously known type 2 AGN in the GOODS fields the AVO is sampling a region of redshift -- power space much harder to reach with classical methods. I also discuss the AVO move to our next phase, the EURO-VO, and our short-term plans to continue doing science with the Virtual Observatory.

P. Padovani

2004-11-12T23:59:59.000Z

14

HAWC Observatory captures first image  

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

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May JunDatastreamsmmcrcalgovInstrumentsruc DocumentationP-SeriesFlickr FlickrGuided Self-Assembly of GoldHAWC Observatory captures first

15

HAWC Observatory captures first image  

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

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr MayAtmospheric Optical Depth7-1D: Vegetation ProposedUsingFun with Big Sky9, 2010 The meeting was called to order byHAWC Observatory

16

HAWC γ-Ray Observatory  

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

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr MayAtmospheric Optical Depth7-1D: Vegetation ProposedUsingFun with Big Sky9, 2010 The meeting was called to order byHAWC ObservatoryHAWC

17

Chandra X-ray Observatory Center  

E-Print Network [OSTI]

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

18

The Pierre Auger Cosmic Ray Observatory  

E-Print Network [OSTI]

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

,

2015-01-01T23:59:59.000Z

19

NATIONAL RADIO ASTRONOMY OBSERVATORY GREEN BANK, WEST VIRGINIA  

E-Print Network [OSTI]

NATIONAL RADIO ASTRONOMY OBSERVATORY GREEN BANK, WEST VIRGINIA ELECTRONICS DIVISION TECHNICAL NOTE R. Lacasse #12;NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia 140-ft CASSEGRAIN BAa

Groppi, Christopher

20

THE SAAO ASTRONOMICAL MUSEUM OBSERVATORY, CAPE TOWN  

E-Print Network [OSTI]

power came from the battery house next door. The batteries were charged by a steam-powered generator Observatory 1 #12;THE BUILDING The building which houses the museum is usually called the McClean, after its

Glass, Ian S.

Note: This page contains sample records for the topic "observatory nainital uttarkhand" 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

CHAPTER 3.4 Observatory mathematics in the nineteenth  

E-Print Network [OSTI]

of science was in fact inaugurated by a debate about Tycho Brahe's observatory (Hannaway 1986; Shackelford

Aubin, David

22

Synoptic Observing Programs at Big Bear Solar Observatory  

E-Print Network [OSTI]

Solar Observatory in China, and will explore collaboration with observatories in Canary Island to extendSynoptic Observing Programs at Big Bear Solar Observatory Haimin Wang and Philip R. Goode Big Bear Solar Observatory, New Jersey Institute of Technology, Newark, NJ 07102, USA Abstract. New Jersey

23

3D Spectroscopy and the Virtual Observatory  

E-Print Network [OSTI]

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

Bryan W. Miller

2007-08-15T23:59:59.000Z

24

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

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.

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

1999-06-24T23:59:59.000Z

26

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

27

UNIVERSITY OF CALIFORNIA, SANTA CRUZ UC OBSERVATORIES  

E-Print Network [OSTI]

UNIVERSITY OF CALIFORNIA, SANTA CRUZ UC OBSERVATORIES POSTDOCTORAL SCHOLAR ­ EMPLOYEE The Inter Stellar+Galactic Medium Program of Studies (IMPS) at the University of California, Santa Cruz invites of funding. START DATE: October 2013 TO APPLY: Applicants should send curriculum vitae with list

California at Santa Cruz, University of

28

Solar Dynamics Observatory/ Extreme Ultraviolet Variability Experiment  

E-Print Network [OSTI]

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

Mojzsis, Stephen J.

29

NATIONAL RADIO ASTRONOMY OBSERVATORY CHARLOTTESVILLE) VA  

E-Print Network [OSTI]

NATIONAL RADIO ASTRONOMY OBSERVATORY CHARLOTTESVILLE) VA ELECTRONICS DIVISION INTERNAL REPORT No ' : : lg Measurement Programs DETECTO R1 . · · · · .· · · . · · · · · · · NOISEL3.B. . 9· · . · · · · · · · · . . . Automated ' : : lg Measurement Programs DETECTO R1

Groppi, Christopher

30

Chandra X-ray Observatory Center  

E-Print Network [OSTI]

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

31

Chandra X-ray Observatory Center  

E-Print Network [OSTI]

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

32

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

33

Updated Multichannel Infrared Solar Spectrograph at Purple Mountain Observatory  

E-Print Network [OSTI]

Updated Multichannel Infrared Solar Spectrograph at Purple Mountain Observatory LI Hui( û), YOU Jianqi( ? ), WU Qindi( ¸Ð) and YU Xingfeng(åÐ ) Purple Mountain Observatory, CAS, Nanjing 210008, China National Astronomical Observatories, CAS, Beijing 100012, China Email: lihui@mail.pmo.ac.cn Tel: 025

Li, Hui

34

The Virtual Observatory and Grid in Spain  

E-Print Network [OSTI]

The Virtual Observatory (VO) is nearing maturity, and in Spain the Spanish VO (SVO) exists since June 2004. There have also been numerous attempts at providing more or less encompassing grid initiatives at the national level, and finally Spain has an official National Grid Initiative (NGI). In this article we will show the VO and Grid development status of nationally funded initiatives in Spain, and we will hint at potential joint VO-Grid use-cases to be developed in Spain in the near future.

J. D. Santander-Vela

2008-07-08T23:59:59.000Z

35

Science Potential of a Deep Ocean Antineutrino Observatory  

E-Print Network [OSTI]

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

Steve Dye

2006-12-15T23:59:59.000Z

36

auger observatory status: Topics by E-print Network  

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

Pierre Auger Observatory is presently under construction in Malargue, Mendoza, Argentina. It combines two complementary air shower observation techniques; the detection of...

37

auger observatory closes: Topics by E-print Network  

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

Pierre Auger Observatory (PAO), currently under construction in Province of Mendoza, Argentina, and with another site planned in the Northern hemisphere, is a major international...

38

auger observatory celebrates: Topics by E-print Network  

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

Pierre Auger Observatory (PAO), currently under construction in Province of Mendoza, Argentina, and with another site planned in the Northern hemisphere, is a major international...

39

auger observatory estudo: Topics by E-print Network  

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

Pierre Auger Observatory (PAO), currently under construction in Province of Mendoza, Argentina, and with another site planned in the Northern hemisphere, is a major international...

40

auger observatory progress: Topics by E-print Network  

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

part of the Auger Observatory, now under construction in the Province of Mendoza, Argentina, is well over half finished. Active detectors have been recording events for one and...

Note: This page contains sample records for the topic "observatory nainital uttarkhand" 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

auger observatory project: Topics by E-print Network  

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

Pierre Auger Observatory (PAO), currently under construction in Province of Mendoza, Argentina, and with another site planned in the Northern hemisphere, is a major international...

42

Ocean Observatories Initiative: Pacific Northwest The Endurance Array  

E-Print Network [OSTI]

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

Kurapov, Alexander

43

National Radio Astronomy Observatory Electronics Division Technical Note No. 219  

E-Print Network [OSTI]

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

Groppi, Christopher

44

THE CAMPUS OBSERVATORY at the University of Saskatchewan  

E-Print Network [OSTI]

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

Peak, Derek

45

Updated Multichannel Infrared Solar Spectrograph at Purple Mountain Observatory #  

E-Print Network [OSTI]

in solar flare [12] , which is # Supported by the National Natural Science Foundation of China (NSFC, NoUpdated Multichannel Infrared Solar Spectrograph at Purple Mountain Observatory # LI Hui(©¿), YOU Jianqi(?OŠ), WU Qindi(?,l) and YU Xingfeng(?lb) Purple Mountain Observatory, CAS, Nanjing 210008, China

Li, Hui

46

Towards a Taxonomy for Web Observatories Web Science Institute  

E-Print Network [OSTI]

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

47

NATIONAL RADIO ASTRONOMY OBSERVATORY GREEN BANK, WEST VIRGINIA  

E-Print Network [OSTI]

NATIONAL RADIO ASTRONOMY OBSERVATORY GREEN BANK, WEST VIRGINIA ELECTRONICS DIVISION INTERNAL REPORT and Ionospheric Center, Arecibo, Puerto Rico by the National Radio Astronomy Observatory at Green Bank, West Virginia. The general design concept was taken from previous receivers assembled at NRAO. S. Weinreb and N

Groppi, Christopher

48

NATIONAL RADIO ASTRONOMY OBSERVATORY Green, Bank, West Virginia  

E-Print Network [OSTI]

NATIONAL RADIO ASTRONOMY OBSERVATORY Green, Bank, West Virginia Electronics Division Internal Rep preformed by the Standard Receiver Section of the National Radio Astronomy Observatory at Green Bank, West Virginia. The following breakdown was used to divide the costs into various categories: (1) Emckajs.c1 . 1

Groppi, Christopher

49

EChO - Exoplanet Characterisation Observatory  

E-Print Network [OSTI]

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

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

2011-01-01T23:59:59.000Z

50

Client Interfaces to the Virtual Observatory Registry  

E-Print Network [OSTI]

The Virtual Observatory Registry is a distributed directory of information systems and other resources relevant to astronomy. To make it useful, facilities to query that directory must be provided to humans and machines alike. This article reviews the development and status of such facilities, also considering the lessons learnt from about a decade of experience with Registry interfaces. After a brief outline of the history of the standards development, it describes the use of Registry interfaces in some popular clients as well as dedicated UIs for interrogating the Registry. It continues with a thorough discussion of the design of the two most recent Registry interface standards, RegTAP on the one hand and a full-text-based interface on the other hand. The article finally lays out some of the less obvious conventions that emerged in the interaction between providers of registry records and Registry users as well as remaining challenges and current developments.

Demleitner, Markus; Taylor, Mark; Normand, Jonathan

2015-01-01T23:59:59.000Z

51

Radio Wavelength Observatories within the Exploration Architecture  

E-Print Network [OSTI]

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

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

2007-01-26T23:59:59.000Z

52

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

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

y Tcnica 12;Pierre Auger ... Source: Pierre Auger Observatory Collection: Physics 50 CERN Courier CERN COURIER Summary: -ray observatory bearing Auger's name is studying...

53

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

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

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

54

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

55

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network [OSTI]

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia Elec-xonics Division Internal Report 140 MV The battery voltage as a function of temperature was also measured. The voltage was extremely

Groppi, Christopher

56

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network [OSTI]

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia Electronics Division Internal Report with the calculator. It is constructed from CMOS logic for lowest power consumption and has a NiCad battery back

Groppi, Christopher

57

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network [OSTI]

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia Electronics Division Internal Report an opposition battery, a DC Null Voltmeter and a recorder. With this set-up a variation in temperature of .02 C

Groppi, Christopher

58

auger southern observatory: Topics by E-print Network  

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

Auger Collaboration intends to extend the energy range of its southern observatory in Argentina for high quality data from 0.1 to 3 EeV. The extensions, described in accompanying...

59

apache point observatory: Topics by E-print Network  

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

sky observatory's largest telescope is the versatile ARC 3.5-m, which Telescope, Dan LongAPO APOLLO and 3.5-m Observations One synoptic study is the APOLLO (Apache PointApache...

60

The Green Computing Observatory: status of acquisition and analysis  

E-Print Network [OSTI]

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

Lefèvre, Laurent

Note: This page contains sample records for the topic "observatory nainital uttarkhand" 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

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network [OSTI]

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia Electronics Division Internal Report line. A 12 V stor- e battery may be attached to the battery connector with pin 1 ground and pin 2 +12 V DC nominal. When the primary power fails, the battery will supply power to the clock. About 1 1/2 amp

Groppi, Christopher

62

NATIONAL RADIO ASTRONOMY OBSERVATORY GREEN BANK, WEST VIRGINIA  

E-Print Network [OSTI]

NATIONAL RADIO ASTRONOMY OBSERVATORY GREEN BANK, WEST VIRGINIA ELECTRONICS DIVISION TECHNICAL NOTE .:41; CLOCK INFORMATION FOR AST 286 COMPUTERS Ronald B. Weimer The battery backed clock is only read (which does not set the battery clock) the AST keeps time from a second crystal oscillator. A rough block

Groppi, Christopher

63

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network [OSTI]

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia Electronics Division Internal Report No. 109 BATTERY PACK FOR HEWLETT-PACKARD 5065A RUBIDIUM FREQUENCY STANDARD Michael Balister OCTOBER 1971 NUMBER OF COPIES: 150 #12;BATTERY PACK FOR HEWLETT-PACKARD 5065A RUBIDIUM FREQUENCY STANDARD

Groppi, Christopher

64

Neutral Current Detectors for the Sudbury Neutrino Observatory  

E-Print Network [OSTI]

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

Waltham, Chris

65

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

66

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

E-Print Network [OSTI]

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

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

2013-01-01T23:59:59.000Z

67

11Chandra 'Sees' a Distant Planet Evaporating NASA's Chandra Observatory  

E-Print Network [OSTI]

energy. A simple model of this planet's interior suggests that its atmosphere might account for as much11Chandra 'Sees' a Distant Planet Evaporating NASA's Chandra Observatory has discovered that the star CoRot-2a is a powerful X-ray source. This is unfortunate because it is also known that a planet

68

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

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

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

Bob Busey; Larry Hinzman

69

Early Science Results from SOFIA, the World's Largest Airborne Observatory  

E-Print Network [OSTI]

The Stratospheric Observatory For Infrared Astronomy, or SOFIA, is the largest flying observatory ever built,consisting of a 2.7-meter diameter telescope embedded in a modified Boeing 747-SP aircraft. SOFIA is a joint project between NASA and the German Aerospace Center Deutsches Zentrum fur Luft und-Raumfahrt (DLR). By flying at altitudes up to 45000 feet, the observatory gets above 99.9 percent of the infrared-absorbing water vapor in the Earth's atmosphere. This opens up an almost uninterrupted wavelength range from 0.3-1600 microns that is in large part obscured from ground based observatories. Since its 'Initial Science Flight' in December 2010, SOFIA has flown several dozen science flights, and has observed a wide array of objects from Solar System bodies, to stellar nurseries, to distant galaxies. This paper reviews a few of the exciting new science results from these first flights which were made by three instruments: the mid-infrared camera FORCAST, the far-infrared heterodyne spectrometer GREAT, and...

De Buizer, James M

2013-01-01T23:59:59.000Z

70

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

71

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network [OSTI]

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia ELECTRONICS DIVISION INTERNAL REPORT the earth's axis and perpendic- ular to the Greenwich Meridian, call it the east-west plane. A telescope's rectangular cordinate components (x,y,z) are X = 882880.0208m Distance from the east-west plane, Greenwich

Groppi, Christopher

72

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network [OSTI]

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia Electronics Division Internal Report which has been used on all systems mounted in the past at the 300-foot telescope. The East and West 14 are so made to allow the East and West 1410 MHz feeds to be positioned 2. 63, 5.24, 7.88 and 10. 52

Groppi, Christopher

73

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network [OSTI]

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia Electronics Division Internal Report (Polarization) Focus Declination Beam East on Sky (Feed West of Center) Beam North to West on Sky (Feed North to West on Sky) Feed moves down toward surface Beam South on Sky Position Read- out Sign 300-FOOT

Groppi, Christopher

74

NATIONAL RADIO ASTRONOMY OBSERVATORY GREEN BANK ) WEST VIRGINIA  

E-Print Network [OSTI]

NATIONAL RADIO ASTRONOMY OBSERVATORY GREEN BANK ) WEST VIRGINIA ELECTRONICS DIVISION INTERNAL REPORT No. 159 INTERFERENCE POTENTIAL FOR RADIO ASTRONOMY OBSERVATIONS AT GREEN BANK, WEST VIRGINIA CRAIG ASTRONOMY OBSERVATIONS AT GREEN BANK, WEST VIRGINIA Craig R. Moore and James L. Dolan Introduction

Groppi, Christopher

75

UNIVERSITY OF CALIFORNIA, SANTA CRUZ DEPARTMENT OF UC OBSERVATORIES  

E-Print Network [OSTI]

UNIVERSITY OF CALIFORNIA, SANTA CRUZ DEPARTMENT OF UC OBSERVATORIES Postdoctoral Scholar The Inter) and the University of California, Santa Cruz (UCSC) invites applications for the position of Postdoctoral Scholar: Postdoctoral Scholar - Employee SALARY: $51,776 ­ $55,128, commensurate with qualifications and experience

California at Santa Cruz, University of

76

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

E-Print Network [OSTI]

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

77

European Information Technology Observatory EITO 2002 2. What is sustainable  

E-Print Network [OSTI]

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

Loke, Seng W. - Loke, Seng W.

78

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

E-Print Network [OSTI]

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

79

Identifying clouds over the Pierre Auger Observatory using infrared satellite data  

SciTech Connect (OSTI)

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

Abreu, Pedro; et al.,

2013-12-01T23:59:59.000Z

80

Managing Distributed Software Development in the Virtual Astronomical Observatory  

E-Print Network [OSTI]

The U.S. Virtual Astronomical Observatory (VAO) is a product-driven organization that provides new scientific research capabilities to the astronomical community. Software development for the VAO follows a lightweight framework that guides development of science applications and infrastructure. Challenges to be overcome include distributed development teams, part-time efforts, and highly constrained schedules. We describe the process we followed to conquer these challenges while developing Iris, the VAO application for analysis of 1-D astronomical spectral energy distributions (SEDs). Iris was successfully built and released in less than a year with a team distributed across four institutions. The project followed existing International Virtual Observatory Alliance inter-operability standards for spectral data and contributed a SED library as a by-product of the project. We emphasize lessons learned that will be folded into future development efforts. In our experience, a well-defined process that provides gu...

Evans, Janet D; Bonaventura, Nina; Busko, Ivo; Cresitello-Dittmar, Mark; D'Abrusco, Raffaele; Doe, Stephen; Ebert, Rick; Laurino, Omar; Pevunova, Olga; Refsdal, Brian; Thomas, Brian

2012-01-01T23:59:59.000Z

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


81

A SURVEY OF EGRET SOURCES USING THE MILAGRO OBSERVATORY  

E-Print Network [OSTI]

V. The third EGRET catalog contained 271 new gamma-ray sources with energies above 100 MeV. The 271 sources OBSERVATORY By Chuan Chen Very high energy gamma-rays can be used to understand some of the most pow- erful detected gamma-ray emission from 30 keV to 30 GeV. EGRET covered an energy range between 20 MeV and 30 Ge

California at Santa Cruz, University of

82

The HAWC Gamma-Ray Observatory: Observations of Cosmic Rays  

E-Print Network [OSTI]

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

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

2013-01-01T23:59:59.000Z

83

High-energy Astrophysics and the Virtual Observatory  

E-Print Network [OSTI]

The Virtual Observatory (VO) will revolutionise the way we do Astronomy by allowing easy access to all astronomical data and by making the handling and analysis of datasets at various locations across the globe much simpler and faster. I report here on the need for the VO and its status in Europe, concentrating on the recently started EURO-VO project, and then give two specific applications of VO tools to high-energy astrophysics.

P. Padovani

2005-07-26T23:59:59.000Z

84

Technology Development for a Neutrino AstrophysicalObservatory  

SciTech Connect (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

85

Technology development for a neutrino astrophysical observatory. Letter of intent  

SciTech Connect (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

86

Hybrid Detection of UHECR with the Pierre Auger Observatory  

E-Print Network [OSTI]

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

Miguel Mostafa; for the Pierre Auger Collaboration

2006-07-31T23:59:59.000Z

87

The Hybrid Activities of the Pierre Auger Observatory  

E-Print Network [OSTI]

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

Miguel Mostafa

2006-08-30T23:59:59.000Z

88

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

SciTech Connect (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) Measurement of the average depth of shower maximum and its fluctuations with the Pierre Auger Observatory; (2) Study of the nuclear mass composition of UHECR with the surface detectors of the Pierre Auger Observatory; (3) Comparison of data from the Pierre Auger Observatory with predictions from air shower simulations: testing models of hadronic interactions; (4) A Monte Carlo exploration of methods to determine the UHECR composition with the Pierre Auger Observatory; (5) The delay of the start-time measured with the Pierre Auger Observatory for inclined showers and a comparison of its variance with models; (6) UHE neutrino signatures in the surface detector of the Pierre Auger Observatory; and (7) The electromagnetic component of inclined air showers at the Pierre Auger Observatory.

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

2009-06-01T23:59:59.000Z

89

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.

Tiina Suomijarvi for the Pierre Auger Collaboration

2007-09-12T23:59:59.000Z

90

Solar Simulations for the Atacama Large Millimeter Observatory Network  

E-Print Network [OSTI]

The Atacama Large Millimeter/submillimeter Array (ALMA) will be a valuable tool for observing the chromosphere of our Sun at (sub-)millimeter wavelengths at high spatial, temporal and spectral resolution and as such has great potential to address long-standing scientific questions in solar physics. In order to make the best use of this scientific opportunity, the Solar Simulations for the Atacama Large Millimeter Observatory Network has been initiated. A key goal of this international collaboration is to support the preparation and interpretation of future observations of the Sun with ALMA.

Wedemeyer, Sven; Brajsa, Roman; Barta, Miroslav; Shimojo, Masumi

2015-01-01T23:59:59.000Z

91

Photometric stability analysis of the Exoplanet Characterisation Observatory  

E-Print Network [OSTI]

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

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

2013-01-01T23:59:59.000Z

92

The Astrophysical Virtual Observatory to EURO-VO Transition  

E-Print Network [OSTI]

The Astrophysical Virtual Observatory (AVO) initiative, jointly funded by the European Commission and six European organisations, had the task of creating the foundations of a regional scale infrastructure by conducting a research and demonstration programme on the VO scientific requirements and necessary technologies. The AVO project is now formally concluded. I highlight AVO's main achievements and then describe its successor, the EURO-VO project. With its three new interlinked structures, the Data Centre Alliance, the Facility Centre, and the Technology Centre, the EURO-VO is the logical next step for the deployment of an operational VO in Europe.

P. Padovani

2005-11-09T23:59:59.000Z

93

The Central Laser Facility at the Pierre Auger Observatory  

E-Print Network [OSTI]

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

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

2005-07-13T23:59:59.000Z

94

HAWC Observatory to study universe's most energetic phenomena  

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

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May JunDatastreamsmmcrcalgovInstrumentsruc DocumentationP-SeriesFlickr FlickrGuided Self-Assembly of GoldHAWC Observatory captures

95

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

Broader source: Energy.gov [DOE]

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

96

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

DOE Data Explorer [Office of Scientific and Technical Information (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.

Gangodagamage, Chandana; Wilson, Cathy; Rowland, Joel

97

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

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

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

98

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

SciTech Connect (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.

Gangodagamage, Chandana; Wilson, Cathy; Rowland, Joel

2013-12-08T23:59:59.000Z

99

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

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

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

100

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

Note: This page contains sample records for the topic "observatory nainital uttarkhand" 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

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

SciTech Connect (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) Measurement of the cosmic ray energy spectrum above 10{sup 18} eV with the Pierre Auger Observatory; (2) The cosmic ray flux observed at zenith angles larger than 60 degrees with the Pierre Auger Observatory; (3) Energy calibration of data recorded with the surface detectors of the Pierre Auger Observatory; (4) Exposure of the Hybrid Detector of The Pierre Auger Observatory; and (5) Energy scale derived from Fluorescence Telescopes using Cherenkov Light and Shower Universality.

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

102

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

103

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

104

Engineering in the service of science; construction of a cabled ocean observatory  

E-Print Network [OSTI]

Engineering in the service of science; construction of a cabled ocean observatory Mr. Peter Phibbs for maintenance can quickly make a system uneconomic. Peter Phibbs was project manager for the $75M construction ocean observatory, and went into operation fifteen months ago. The infrastructure demonstrates not only

Frandsen, Jannette B.

105

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

E-Print Network [OSTI]

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

Didkovsky, Leonid

106

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

E-Print Network [OSTI]

mirror (M1) and its alignment with the secondary mirror (M2) will be actively controlled. HighThe Telescope Control System of the New Solar Telescope at Big Bear Solar Observatory G. Yang*a, J of Technology, 323 Martin Luther King Blvd., Newark, NJ 07104; bBig Bear Solar Observatory, 40386 North Shore

107

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

E-Print Network [OSTI]

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

Joseph, Robert D.

108

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

E-Print Network [OSTI]

of Mechatronics Control Engineering, Zhejiang University Post-doctoral Research Fellow, Department of Ocean and Resources Engineering, University of Hawaii Abstract Cabled ocean observatory that enables abundant powerEffort on Developing Cabled Ocean Observatories in China Yanhu Chen Research Assitant, Institute

Frandsen, Jannette B.

109

Observations and New Astronomical Facilities in Lijiang Observatory , X.L. Zhang12  

E-Print Network [OSTI]

solar system objects (SSO) and Gaia itself (Thuillot 2011)[1]. Lijiang Observatory has joined the GAIA) as the main instrument. Other insturments like the Lijiang Exoplanet Tracker (LiJET, see Figure 1), PI the observatory and sit behind his own laptop. 87 #12;Fig. 1: Layout of Lijiang Exoplanet Tracker (Erskine & Ge

Paris-Sud XI, Université de

110

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

E-Print Network [OSTI]

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

Brandsma, Theo

111

Sophia E. Brumer Lamont-Doherty Earth Observatory of Columbia University  

E-Print Network [OSTI]

Sophia E. Brumer Lamont-Doherty Earth Observatory of Columbia University Ocean and Climate Physics Graduate Research Fellow, Columbia University Department of Earth and Environmental Science (DEES. Gordon, A. Sobel Columbia University, Lamont-Doherty Earth Observatory 2010--2011 J. Hirshi, A. Megann

112

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

E-Print Network [OSTI]

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

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

2014-01-01T23:59:59.000Z

113

The Large Observatory For X-ray Timing: LOFT  

E-Print Network [OSTI]

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

Bozzo, E

2013-01-01T23:59:59.000Z

114

VAMOS: a Pathfinder for the HAWC Gamma-Ray Observatory  

E-Print Network [OSTI]

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

Abeysekara, A U; Alvarez, C; lvarez, J D; ngeles, F; Arceo, R; Arteaga-Velzquez, J C; Avila-Aroche, A; Solares, H A Ayala; Badillo, C; Barber, A S; Baughman, B M; Bautista-Elivar, N; Gonzalez, J Becerra; Belmont, E; Bentez, E; BenZvi, S Y; Berley, D; Bernal, A; Rosales, M Bonilla; Braun, J; Caballero-Lopez, R A; Caballero-Mora, K S; Cabrera, I; Carramiana, A; Castaeda-Martnez, L; Castillo, M; Cotti, U; Cotzomi, J; de la Fuente, E; De Len, C; DeYoung, T; Diaz-Azuara, A; Diaz-Cruz, L; Hernandez, R Diaz; Daz-Vlez, J C; Dingus, B L; Dultzin, D; DuVernois, M A; Ellsworth, R W; Fernandez, A; Fiorino, D W; Fraija, N; Galindo, A; Garca-Torales, G; Garfias, F; Gonzlez, A; Gonzlez, L X; Gonzlez, M M; Goodman, J A; Grabski, V; Gussert, M; Guzmn-Cern, C; Hampel-Arias, Z; Harding, J P; Hernndez-Cervantes, L; Hui, C M; Hntemeyer, P; Imran, A; Iriarte, A; Karn, P; Kieda, D; Kunde, G J; Langarica, R; Lara, A; Lara, G; Lauer, R J; Lee, W H; Lennarz, D; Vargas, H Len; Linares, E C; Linnemann, J T; Longo, M; Luna-Garcia, R; Marinelli, A; Martnez, L A; Martnez, H; Martnez, O; Martnez-Castro, J; Martos, M; Matthews, J A J; McEnery, J; Torres, E Mendoza; Miranda-Romagnoli, P; Moreno, E; Mostaf, M; Nava, J; Nellen, L; Newbold, M; Noriega-Papaqui, R; Oceguera-Becerra, T; Page, D P; Patricelli, B; Pelayo, R; Prez-Prez, E G; Pretz, J; Ramrez, I; Renter, A; Rivire, C; Rosa-Gonzlez, D; Ruiz-Sala, F; Ruiz-Velasco, E L; Ryan, J; Sacahui, J R; Salazar, H; Salesa, F; Sandoval, A; Santos, E; Schneider, M; Silich, S; Sinnis, G; Smith, A J; Woodle, K Sparks; Springer, R W; Suarez, F; Taboada, I; Tepe, A; Toale, P A; Tollefson, K; Torres, I; Tinoco, S; Ukwatta, T N; Galicia, J F Valds; Vanegas, P; Vzquez, A; Villaseor, L; Wall, W; Weisgarber, T; Westerhoff, S; Wisher, I G; Wood, J; Yodh, G B; Younk, P W; Zaborov, D; Zepeda, A; Zhou, H

2014-01-01T23:59:59.000Z

115

Single Ion Trapping for the Enriched Xenon Observatory  

SciTech Connect (OSTI)

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

Waldman, Samuel J.; /Stanford U., Phys. Dept. /SLAC; ,

2006-03-28T23:59:59.000Z

116

The Theoretical Astrophysical Observatory: Cloud-Based Mock Galaxy Catalogues  

E-Print Network [OSTI]

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

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

2014-01-01T23:59:59.000Z

117

Optical calibration hardware for the Sudbury Neutrino Observatory  

E-Print Network [OSTI]

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

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

2005-07-19T23:59:59.000Z

118

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

E-Print Network [OSTI]

>David Aubin, Charlotte Bigg, and H. Otto Sibum Observatories--Temples of the most sublime of the sciences

Aubin, David

119

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

E-Print Network [OSTI]

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

120

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

Note: This page contains sample records for the topic "observatory nainital uttarkhand" 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

Milagro - A TeV Observatory for Gamma Ray Bursts  

SciTech Connect (OSTI)

Milagro is a large field of view ({approx} 2 sr), high duty cycle ({approx}90%), ground-based observatory sensitive to gamma-rays above {approx}100 GeV. This unique detector is ideal for observing the highest energy gamma-rays from gamma-ray bursts. The highest energy gamma rays supply very strong constraints on the nature of gamma-ray burst sources as well as fundamental physics. Because the highest energy gamma-rays are attenuated by pair production with the extragalactic infrared background light, Milagro's sensitivity decreases rapidly for bursts with redshift > 0.5. While only 10 % of bursts have been measured to be within z=0.5, these bursts are very well studied at all wavelengths resulting in the most complete understanding of GRB phenomena. Milagro has sufficient sensitivity in units of E2 dN/dE to detect VHE luminosities lower than the observed luminosities at {approx} 100 keV for these nearby bursts. Therefore, the launch of SWIFT and its ability to localize and measure redshifts of many bursts points to great future possibilities.

Dingus, B.L. [Los Alamos National Laboratory (United States)

2004-09-28T23:59:59.000Z

122

EChOSim: The Exoplanet Characterisation Observatory software simulator  

E-Print Network [OSTI]

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

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

2014-01-01T23:59:59.000Z

123

Preliminary systems engineering evaluations for the National Ecological Observatory Network.  

SciTech Connect (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

124

Conceptual Design of the International Axion Observatory (IAXO)  

E-Print Network [OSTI]

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

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

2014-01-01T23:59:59.000Z

125

The Final Results from the Sudbury Neutrino Observatory  

ScienceCinema (OSTI)

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

None

2011-04-25T23:59:59.000Z

126

3D Spectroscopy in the Virtual Observatory: Current Status  

E-Print Network [OSTI]

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

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

2007-11-02T23:59:59.000Z

127

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

128

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

129

Was Lepenski Vir an ancient Sun or Pleiades observatory?  

E-Print Network [OSTI]

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

Pankovic, Vladan; Krmar, Miodrag

2015-01-01T23:59:59.000Z

130

SNO Data: Results from Experiments at the Sudbury Neutrino Observatory  

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

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

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

131

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

E-Print Network [OSTI]

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

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

2006-04-28T23:59:59.000Z

132

The Large Observatory For x-ray Timing  

E-Print Network [OSTI]

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

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

2014-01-01T23:59:59.000Z

133

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

E-Print Network [OSTI]

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

Grant, Catherine E.

134

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

E-Print Network [OSTI]

-static SeaSonde surface current radars; and (3) a growing fleet of autonomous underwater vehicles and nowcasting/forecasting models. The construction of the observatories is being fueled by the rapid development

Moline, Mark

135

The role of project science in the Chandra X-ray Observatory  

E-Print Network [OSTI]

The Chandra X-ray Observatory, one of NASA's Great Observatories, has an outstanding record of scientific and technical success. This success results from the efforts of a team comprising NASA, its contractors, the Smithsonian Astrophysical Observatory, the instrument groups, and other elements of the scientific community -- including the thousands of scientists who utilize this powerful facility for astrophysical research. We discuss the role of NASA Project Science in the formulation, development, calibration, and operation of the Chandra X-ray Observatory. In addition to serving as an interface between the scientific community and the Project, Project Science performed what we term "science systems engineering". This activity encompasses translation of science requirements into technical requirements and assessment of the scientific impact of programmatic and technical trades. We briefly describe several examples of science systems engineering conducted by Chandra Project Science.

Stephen L. O'Dell; Martin C. Weisskopf

2006-06-16T23:59:59.000Z

136

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

E-Print Network [OSTI]

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

Long, Bernard

137

A Reusable Process Control System Framework for the Orbiting Carbon Observatory and NPP Sounder PEATE missions  

E-Print Network [OSTI]

PEATE missions Chris A. Mattmann, Dana Freeborn, Dan Crichton, Brian Foster, Andrew Hart, David Woollard missions: the Orbiting Carbon Observatory (OCO), and NPP Sounder PEATE projects. 1 Introduction Data volume

Mattmann, Chris

138

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

E-Print Network [OSTI]

We report results from a combined analysis of solar neutrino data from all phases of the Sudbury Neutrino Observatory (SNO). By exploiting particle identification information obtained from the proportional counters installed ...

Formaggio, Joseph A.

139

MEASUREMENT OF THE 8 B SOLAR NEUTRINO ENERGY SPECTRUM AT THE SUDBURY NEUTRINO OBSERVATORY  

E-Print Network [OSTI]

MEASUREMENT OF THE 8 B SOLAR NEUTRINO ENERGY SPECTRUM AT THE SUDBURY NEUTRINO OBSERVATORY Monica me everything from the fine details of signal extraction, iii #12; Fortran and C++ to bird watching

Waltham, Chris

140

WEST VIRGINIA UNIVERSITY and NATIONAL RADIO ASTRONOMY OBSERVATORY APPLICATION FOR RARECATS PROGRAM Deadline for postmark of this application and supporting  

E-Print Network [OSTI]

WEST VIRGINIA UNIVERSITY and NATIONAL RADIO ASTRONOMY OBSERVATORY APPLICATION FOR RARECATS PROGRAM 604 Allen Hall, PO Box 6122 West Virginia University Morgantown, WV 26506-6122 #12;

Groppi, Christopher

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141

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

SciTech Connect (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

142

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

E-Print Network [OSTI]

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

143

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

E-Print Network [OSTI]

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

Ito, Atsushi

144

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

E-Print Network [OSTI]

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

Ito, Atsushi

145

AN INFRARED SPACE OBSERVATORY ATLAS OF BRIGHT SPIRAL GALAXIES1 George J. Bendo,2,3,4  

E-Print Network [OSTI]

AN INFRARED SPACE OBSERVATORY ATLAS OF BRIGHT SPIRAL GALAXIES1 George J. Bendo,2,3,4 Robert D in a series we present an atlas of infrared images and photometry from 1.2 to 180 lm for a sample of bright galaxies. Using the Infrared Space Observatory (ISO), we have obtained 12 lm images and photometry at 60

Joseph, Robert D.

146

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

E-Print Network [OSTI]

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

147

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

E-Print Network [OSTI]

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

148

NATIONAL RADIO ASTRONOMY OBSERVATORY TITLE: A REVISED VAX FARANT SPLOT ROUTINE AND RELATED APPLE  

E-Print Network [OSTI]

NATIONAL RADIO ASTRONOMY OBSERVATORY TITLE: A REVISED VAX FARANT SPLOT ROUTINE AND RELATED APPLE #12;A REVISED VAX FARANT SPLOT ROUTINE AND RELATED APPLE II PLOTTING PROGRAM. The purpose of this report is to describe some upgrades made to the VAX 1 SPLOT" routine and the related Apple plotting

Groppi, Christopher

149

Tycho Brahe made observations of the motions of the planets from his great observatory on  

E-Print Network [OSTI]

Tycho Brahe made observations of the motions of the planets from his great observatory,and understood the importance of random and systematic errors in his observations. In 1600Tycho Brahe employed such a diligent observer inTycho Brahe that his observations convicted this Ptolemaic calculation of an error of 8

150

Production and counting of uncontained sources in the Sudbury Neutrino Observatory  

SciTech Connect (OSTI)

I describe production and distribution of uncontained sources of {sup 24}Na and {sup 222}Rn inside the Sudbury Neutrino Observatory (SNO). These unique sources provided a uniquely accurate calibration of the SNO detector of its response to neutrons, produced through photodisintegration of the deuterons in the heavy water target, and to low energy {beta}-{gamma} decays.

Peeters, Simon J. M. [Pevensey II, Falmer, Brighton, BN1 9QH (United Kingdom)

2011-04-27T23:59:59.000Z

151

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

E-Print Network [OSTI]

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

152

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

E-Print Network [OSTI]

The Thermal Control of the New Solar Telescope at Big Bear Observatory Angelo P. Verdonia and Carsten Denkera aNew Jersey Institute of Technology, Center for Solar-Terrestrial Research, 323 Martin Luther King Blvd, Newark, NJ 07102, US ABSTRACT We present the basic design of the THermal Control System

153

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 hydrology Witold F. Krajewski,1 Martha C. Anderson,2 William E. Eichinger,1 Dara Entekhabi,3 Brian K arise primarily from an inadequate understanding of the hydrological cycle: on land, in oceans

Katul, Gabriel

154

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

155

Nasmyth focus instrumentation of the New Solar Telescope at Big Bear Solar Observatory  

E-Print Network [OSTI]

field stop and heat reflector (heat-stop), elliptical secondary mirror (SM) and diagonal flats. Figure 1Nasmyth focus instrumentation of the New Solar Telescope at Big Bear Solar Observatory Wenda Caoab Coulterb, and Philip R. Goodeab aCenter for Solar-Terrestrial Research, New Jersey Institute of Technology

156

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

157

Directions to the National Radio Astronomy Observatory Green Bank, West Virginia  

E-Print Network [OSTI]

Directions to the National Radio Astronomy Observatory Green Bank, West Virginia From Charleston Roanoke, VA: Via I-64 West, exit at White Sulphur Springs (Exit 181) and take Rt. 92 North to Green Bank, then take Rt. 92 South to Green Bank. From Washington DC: Via I-66 West to I-81 South. Option 1: Take I-81

Groppi, Christopher

158

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

E-Print Network [OSTI]

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

159

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

SciTech Connect (OSTI)

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

Norman, E B

2009-07-07T23:59:59.000Z

160

SEARCH FOR NEUTRON ANTI-NEUTRON OSCILLATION AT THE SUDBURY NEUTRINO OBSERVATORY  

E-Print Network [OSTI]

SEARCH FOR NEUTRON ANTI-NEUTRON OSCILLATION AT THE SUDBURY NEUTRINO OBSERVATORY A Thesis Presented to explain the baryon asymmetry of the universe. In this thesis, a limit on the neutron anti-neutron (nnbar is sampled from the three phases of the SNO experiment to construct a three-phase blind analysis. The profile

Waltham, Chris

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


161

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

E-Print Network [OSTI]

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

A. T. Tokunaga; W. D. Vacca

2005-02-05T23:59:59.000Z

162

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

E-Print Network [OSTI]

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

Tarboton, David

163

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

E-Print Network [OSTI]

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

Babu, G. Jogesh

164

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

E-Print Network [OSTI]

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

Wisconsin at Madison, University of

165

Beyond the Second Generation of Laser-Interferometric Gravitational Wave Observatories  

E-Print Network [OSTI]

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

Stefan Hild

2011-11-27T23:59:59.000Z

166

MilagroA TeV Observatory for Gamma Ray Bursts  

E-Print Network [OSTI]

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

California at Santa Cruz, University of

167

PROFESSOR WILLIAM MENKE, F-AGU LAMONT-DOHERTY EARTH OBSERVATORY OF COLUMBIA UNIVERSITY  

E-Print Network [OSTI]

PROFESSOR WILLIAM MENKE, F-AGU LAMONT-DOHERTY EARTH OBSERVATORY OF COLUMBIA UNIVERSITY CONTACT Prof PREPARATION Ph.D. 1982, Department of Geological Sciences, Columbia University, Geological Sciences, Thesis of Geological Sciences, Columbia University. MS, BS 1976, Department of Earth and Planetary Sciences

Menke, William

168

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

E-Print Network [OSTI]

FIRST MEASUREMENT OF THE FLUX OF SOLAR NEUTRINOS FROM THE SUN AT THE SUDBURY NEUTRINO OBSERVATORY for approaching problems that I found to be more generally useful. Godwin Mayers, Chuck Alexander, Jim Cook and with me. v #12; ABSTRACT FIRST MEASUREMENT OF THE FLUX OF SOLAR NEUTRINOS FROM THE SUN AT THE SUDBURY

Waltham, Chris

169

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

E-Print Network [OSTI]

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

Davide Gandolfi; Massimo Cigna; Daniele Fulvio; Carlo Blanco

2008-10-09T23:59:59.000Z

170

Reconstruction of inclined air showers detected with the Pierre Auger Observatory  

E-Print Network [OSTI]

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

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

2014-07-11T23:59:59.000Z

171

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

E-Print Network [OSTI]

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

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

2003-07-15T23:59:59.000Z

172

The Canadian Automated Meteor Observatory (CAMO): System overview R.J. Weryk a,  

E-Print Network [OSTI]

The Canadian Automated Meteor Observatory (CAMO): System overview R.J. Weryk a, , M.D. Campbell-Brown a,b , P.A. Wiegert a,b , P.G. Brown a,b , Z. Krzeminski a , R. Musci a a Dept. of Physics and Brown, 2012, 2013) using the Canadian Meteor Orbit Radar (CMOR) and a number of Gen-III image

Wiegert, Paul

173

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

E-Print Network [OSTI]

Neutrino Observatory Heavy Water, Earth Sciences Di- vision,17 O Measurement in Bruce Heavy Water Samples with 17 O NMR,O Analysis of Ontario Hydro Heavy Water, Center for Isotope

2007-01-01T23:59:59.000Z

174

Proceedings of ICRC 2001: 773 c Copernicus Gesellschaft 2001 Implementation of the first level trigger for the auger observatory  

E-Print Network [OSTI]

(Suomijarvi, 2001) powered by solar panels. The station electronics communicates with the observatory delivery schedule, power consump- tion, functionality, and cost goals. This paper discusses the trigger

175

Atlantis 11-32 Report Page 1 Update on Experiments Associated with CORK Subseafloor Observatories installed during IODP  

E-Print Network [OSTI]

) replacement of data loggers at Holes 1026B, 1301A, and 1301B and installation of a supplemental battery associated with other CORK observatories, microbiological sampling, and in-situ analysis

Fisher, Andrew

176

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

E-Print Network [OSTI]

Results are reported from a joint analysis of Phase I and Phase II data from the Sudbury Neutrino Observatory. The effective electron kinetic energy threshold used is Teff=3.5 MeV, the lowest analysis threshold yet achieved ...

Monroe, Jocelyn

177

Looking for matter enhanced neutrino oscillations via day v. night asymmetries in the NCD phase of the Sudbury Neutrino Observatory  

E-Print Network [OSTI]

To measure the regeneration of electron neutrinos during passage through the Earth via the MSW effect, the difference in electron neutrino flux between day and night is measured at the Sudbury Neutrino Observatory (SNO). ...

Ott, Richard Anthony, III

2011-01-01T23:59:59.000Z

178

Observatory Collaboration  

E-Print Network [OSTI]

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

Waltham, Chris

179

OBSERVATORY OPPORTUNITIES  

E-Print Network [OSTI]

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

Groppi, Christopher

180

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

E-Print Network [OSTI]

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

L. Cazon

2014-05-20T23:59:59.000Z

Note: This page contains sample records for the topic "observatory nainital uttarkhand" 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.


181

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

E-Print Network [OSTI]

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

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

2015-01-01T23:59:59.000Z

182

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

E-Print Network [OSTI]

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

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

2013-01-01T23:59:59.000Z

183

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

E-Print Network [OSTI]

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

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

2013-01-01T23:59:59.000Z

184

The Chicagoland Observatory Underground for Particle Physics cosmic ray veto system  

SciTech Connect (OSTI)

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

185

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

186

HAWC (High Altitude Water Cherenkov) Observatory for Surveying the TeV Sky  

SciTech Connect (OSTI)

The HAWC observatory is a proposed, large field of view ({approx}2 sr), high duty cycle (>95%) TeV gamma-ray detector which uses a large pond of water (150 m x 150 m) located at 4300 m elevation. The pond contains 900 photomultiplier tubes (PMTs) to observe the relativistic particles and secondary gamma lays in extensive air showers. This technique has been used successfully by the Milagro observatory to detect known, as well as new, TeV sources. The PMTs and much of the data acquisition system of Milagro will be reused for HAWC, resulting in a cost effective detector ({approx}6M$) that can be built quickly in 2-3 years. The improvements of HAWC will result in {approx}15 times the sensitivity of Milagro. HAWC will survey 2{pi} sr of the sky every day with a sensitivity of the Crab flux at a median energy of 1 TeV. After five years of operation half of the sky will be surveyed to 20 mCrab. This sensitivity will likely result in the discovery of new sources as well as allow the identification of which GLAST sources extend to higher energies.

Dingus, Brenda L. [Los Alamos National Lab, Los Alamos, NM 87545 (United States)

2007-07-12T23:59:59.000Z

187

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

188

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

E-Print Network [OSTI]

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

Groppi, Christopher

189

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

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

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

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

2014-12-01T23:59:59.000Z

190

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

E-Print Network [OSTI]

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

Pierre Auger Collaboration

2014-07-22T23:59:59.000Z

191

Anisotropy studies around the Galactic Centre at EeV energies with the Auger Observatory  

SciTech Connect (OSTI)

Data from the Pierre Auger Observatory are analyzed to search for anisotropies near the direction of the Galactic Centre at EeV energies. The exposure of the surface array in this part of the sky is already significantly larger than that of the fore-runner experiments. Our results do not support previous findings of localized excesses in the AGASA and SUGAR data. We set an upper bound on a point-like flux of cosmic rays arriving from the Galactic Centre which excludes several scenarios predicting sources of EeV neutrons from Sagittarius A. Also the events detected simultaneously by the surface and fluorescence detectors (the ''hybrid'' data set), which have better pointing accuracy but are less numerous than those of the surface array alone, do not show any significant localized excess from this direction.

Aglietta, M.; Aguirre, C.; Allard, D.; Allekotte, I.; Allison, P.; Alvarez, C.; Alvarez-Muniz, J.; Ambrosio, M.; Anchordoqui, L.; Anjos, J.C.; Aramo, C.; /Centro Atomico Bariloche /Buenos Aires, IAFE /Buenos Aires, CONICET /Pierre Auger Observ. /La Plata U. /Natl. Tech. U., San Rafael /Adelaide U. /Catholic U. of Bolivia, La Paz /Bolivia U. /Rio de Janeiro, CBPF /Sao Paulo U.; ,

2006-07-01T23:59:59.000Z

192

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

E-Print Network [OSTI]

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

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

2005-01-01T23:59:59.000Z

193

Probing low-x QCD with cosmic neutrinos at the Pierre Auger Observatory  

SciTech Connect (OSTI)

The sources of the observed ultra-high energy cosmic rays must also generate ultra-high energy neutrinos. Deep inelastic scattering of these neutrinos with nucleons on Earth probe center-of-mass energies {radical}s {approx} 100 TeV, well beyond those attainable at terrestrial colliders. By comparing the rates for two classes of observable events, any departure from the benchmark (unscreened perturbative QCD) neutrino-nucleon cross-section can be constrained. Using the projected sensitivity of the Pierre Auger Observatory to quasi-horizontal showers and Earth-skimming tau neutrinos, we show that a ''Super-Auger'' detector can thus provide an unique probe of strong interaction dynamics.

Anchordoqui, Luis A.; /Northeastern U. /Wisconsin U., Milwaukee; Cooper-Sarkar, Amanda M.; /Oxford U.; Hooper, Dan; /Fermilab; Sarkar, Subir; /Oxford U.

2006-05-01T23:59:59.000Z

194

SSALMON - The Solar Simulations for the Atacama Large Millimeter Observatory Network  

E-Print Network [OSTI]

The Solar Simulations for the Atacama Large Millimeter Observatory Network (SSALMON) was initiated in 2014 in connection with two ALMA development studies. The Atacama Large Millimeter/submillimeter Array (ALMA) is a powerful new tool, which can also observe the Sun at high spatial, temporal, and spectral resolution. The international SSALMONetwork aims at coordinating the further development of solar observing modes for ALMA and at promoting scientific opportunities for solar physics with particular focus on numerical simulations, which can provide important constraints for the observing modes and can aid the interpretation of future observations. The radiation detected by ALMA originates mostly in the solar chromosphere - a complex and dynamic layer between the photosphere and corona, which plays an important role in the transport of energy and matter and the heating of the outer layers of the solar atmosphere. Potential targets include active regions, prominences, quiet Sun regions, flares. Here, we give a...

Wedemeyera, S; Brajsa, R; Barta, M; Hudson, H; Fleishman, G; Loukitcheva, M; Fleck, B; Kontar, E; De Pontieu, B; Tiwari, S; Kato, Y; Soler, R; Yagoubov, P; Black, J H; Antolin, P; Gunar, S; Labrosse, N; Benz, A O; Nindos, A; Steffen, M; Scullion, E; Doyle, J G; Zaqarashvili, T; Hanslmeier, A; Nakariakov, V M; Heinzel, P; Ayres, T; Karlicky, M

2015-01-01T23:59:59.000Z

195

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

196

NATIONAL RADIO ASTRONOMY OBSERVATORY TITLE: USE OF THE VAX-11 FARANT MICROWAVE DESIGN PROGRAM FROM GREEN BANK  

E-Print Network [OSTI]

NATIONAL RADIO ASTRONOMY OBSERVATORY TITLE: USE OF THE VAX-11 FARANT MICROWAVE DESIGN PROGRAM FROM #12;USE OF THE VAX-il FARANT MICROWAVE DESIGN PROGRAM FROM GREEN BANK R. Norrod Recently, I have learned to use the FARANT microwave analysis and optimization program which resides on the VAX-11 in CV

Groppi, Christopher

197

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

E-Print Network [OSTI]

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

Tittley, Eric

198

53Estimating the Diameter of the SN1979C Black Hole The Chandra X-Ray Observatory  

E-Print Network [OSTI]

with a mass of 120 solar masses. Can it escape or remain where it is? Space Math http, as well as NASA's Swift, the European Space Agency's XMM-Newton and the German ROSAT observatory revealed been observed. This behavior and the X-ray spectrum, or distribution of X-rays with energy, support

199

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

E-Print Network [OSTI]

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

200

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

E-Print Network [OSTI]

Generation region of pulsating aurora obtained simultaneously by the FAST satellite and a Syowa 2004; published 7 October 2004. [1] We have carried out a direct comparison of pulsating auroras), with reference to simultaneous data obtained by a Syowa-Iceland conjugate pair of observatories. The aurora

California at Berkeley, University of

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201

INTELLIGENCE PLANNING AND TOURISM. PERSPECTIVE AND THE OBSERVATORIES OIDTE EIDT, TAG TEAM TERRITORIOS POSIBLES. CASES IN ARGENTINA AND  

E-Print Network [OSTI]

1 INTELLIGENCE PLANNING AND TOURISM. PERSPECTIVE AND THE OBSERVATORIES OIDTE EIDT, TAG TEAM_fabricio@hotmail.com Summary: Territorial intelligence applied to tourism seeks to resolve tensions, build projects and subjects compatible between tourism and other logics of territorial occupation and appropriation

Paris-Sud XI, Université de

202

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

E-Print Network [OSTI]

Kenya International Radio Observatory (KIRO) Joseph Otieno Malo, University of Nairobi,Joseph Otieno Malo, University of Nairobi, KenyaKenya Bo Thide, Uppsala University, SwedenBo Thide, Uppsala.environmental, and communications research. Located in northern Kenya, on the geomagnetic equator,Located in northern Kenya

203

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

E-Print Network [OSTI]

. NIHOUS Associate Professor, PhD 1983, UC Berkeley. Ocean Thermal Energy Conversion (OTEC), marineFaculty BRUCE HOWE Chair and Professor , PhD 1986, UC San Diego. Ocean observatories, ocean in the ocean, atmospheric and ionospheric tomography. KWOK FAI CHEUNG Professor , PhD 1991, British Columbia

Frandsen, Jannette B.

204

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

E-Print Network [OSTI]

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

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

2015-01-01T23:59:59.000Z

205

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

SciTech Connect (OSTI)

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

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

2014-01-29T23:59:59.000Z

206

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

SciTech Connect (OSTI)

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

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

2013-10-01T23:59:59.000Z

207

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

E-Print Network [OSTI]

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

Noel, Vincent

2007-01-01T23:59:59.000Z

208

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

209

The Data Reduction Pipeline for the Apache Point Observatory Galactic Evolution Experiment  

E-Print Network [OSTI]

The Apache Point Observatory Galactic Evolution Experiment (APOGEE), part of the Sloan Digital Sky Survey III, explores the stellar populations of the Milky Way using the Sloan 2.5-m telescope linked to a high resolution (R~22,500), near-infrared (1.51-1.70 microns) spectrograph with 300 optical fibers. For over 100,000 predominantly red giant branch stars that APOGEE targeted across the Galactic bulge, disks and halo, the collected high S/N (>100 per half-resolution element) spectra provide accurate (~0.1 km/s) radial velocities, stellar atmospheric parameters, and precise (~0.1 dex) chemical abundances for about 15 chemical species. Here we describe the basic APOGEE data reduction software that reduces multiple 3D raw data cubes into calibrated, well-sampled, combined 1D spectra, as implemented for the SDSS-III/APOGEE data releases (DR10 and DR12). The processing of the near-IR spectral data of APOGEE presents some challenges for reduction, including automated sky subtraction and telluric correction over a ...

Nidever, David L; Prieto, Carlos Allende; Beland, Stephane; Bender, Chad; Bizyaev, Dmitry; Burton, Adam; Desphande, Rohit; Fleming, Scott W; Perez, Ana Elia Garcia; Hearty, Fred R; Majewski, Steven R; Meszaros, Szabolcs; Muna, Demitri; Nguyen, Duy; Schiavon, Ricardo P; Shetrone, Matthew; Skrutskie, Michael F; Wilson, John C

2015-01-01T23:59:59.000Z

210

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

SciTech Connect (OSTI)

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

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

2012-03-01T23:59:59.000Z

211

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

SciTech Connect (OSTI)

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

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

2013-01-10T23:59:59.000Z

212

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

SciTech Connect (OSTI)

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

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

2007-02-01T23:59:59.000Z

213

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

214

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

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

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 [50522(stat)-36+28(syst)]??mb is found.

Abrue, P

2012-08-01T23:59:59.000Z

215

54X-rays from Hot Gases Near the SN1979C Black Hole The Chandra X-Ray Observatory  

E-Print Network [OSTI]

is in solar mass units, and R is in kilometers. Problem 1 - Combining these equations using the method-Newton and the German ROSAT observatory revealed a bright source of X-rays that has remained steady for the 12 years, or distribution of X-rays with energy, support the idea that the object in SN 1979C is a black hole being fed

216

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.

217

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

SciTech Connect (OSTI)

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

218

EMERGING DIMMINGS OF ACTIVE REGIONS OBSERVED BY THE SOLAR DYNAMICS OBSERVATORY  

SciTech Connect (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

219

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

E-Print Network [OSTI]

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

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

2015-01-01T23:59:59.000Z

220

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

Note: This page contains sample records for the topic "observatory nainital uttarkhand" 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

Origin of atmospheric aerosols at the Pierre Auger Observatory using studies of air mass trajectories in South America  

E-Print Network [OSTI]

The Pierre Auger Observatory is making significant contributions towards understanding the nature and origin of ultra-high energy cosmic rays. One of its main challenges is the monitoring of the atmosphere, both in terms of its state variables and its optical properties. The aim of this work is to analyze aerosol optical depth $\\tau_{\\rm a}(z)$ values measured from 2004 to 2012 at the observatory, which is located in a remote and relatively unstudied area of the Pampa Amarilla, Argentina. The aerosol optical depth is in average quite low - annual mean $\\tau_{\\rm a}(3.5~{\\rm km})\\sim 0.04$ - and shows a seasonal trend with a winter minimum - $\\tau_{\\rm a}(3.5~{\\rm km})\\sim 0.03$ -, and a summer maximum - $\\tau_{\\rm a}(3.5~{\\rm km})\\sim 0.06$ -, and an unexpected increase from August to September - $\\tau_{\\rm a}(3.5~{\\rm km})\\sim 0.055$). We computed backward trajectories for the years 2005 to 2012 to interpret the air mass origin. Winter nights with low aerosol concentrations show air masses originating from t...

Curci, Gabriele

2014-01-01T23:59:59.000Z

222

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

E-Print Network [OSTI]

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

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

2007-07-01T23:59:59.000Z

223

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

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

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

224

Re-evaluation of total and Umkehr ozone data from NOAA-CMDL Dobson spectrophotometer observatories. Final report  

SciTech Connect (OSTI)

This report describes work to improve the quality of total ozone and Umkehr data obtained in the past at the NOAA Climate Monitoring and Diagnostics Laboratory and the Dobson spectrophotometer ozone observatories. The authors present results of total ozone data re-evaluations for ten stations: Byrd, Antarctica; Fairbanks, Alaska; Hallett, Antarctica; Huancayo, Peru; Haute Provence, France; Lauder, New Zealand; Perth, Australia; Poker Flat, Alaska; Puerto Montt, Chile; and South Pole, Antarctica. The improved data will be submitted in early 1996 to the World Meteorological Organization (WMO) World Ozone Data Center (WODC), and the Atmospheric Environment Service for archiving. Considerable work has been accomplished, also, in reevaluating Umkehr data from seven of the stations, viz., Huancayo, Haute Provence, Lauder, Perth, Poker Flat, Boulder, Colorado; and Mauna Loa, Hawaii.

Komhyr, W.D.; Quincy, D.M.; Grass, R.D.; Koenig, G.L. [Univ. of Colorado, Boulder, CO (United States)] [Univ. of Colorado, Boulder, CO (United States); [National Oceanic and Atmospheric Administration, Boulder, CO (United States). Climate Monitoring and Diagnostics Lab.

1995-12-01T23:59:59.000Z

225

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

SciTech Connect (OSTI)

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

Abreu, P.; /Lisbon, IST; Aglietta, M.; /Turin U. /INFN, Turin; 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.; 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

226

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

E-Print Network [OSTI]

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

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

2013-01-01T23:59:59.000Z

227

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

DOE Data Explorer [Office of Scientific and Technical Information (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.

228

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

E-Print Network [OSTI]

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

229

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

E-Print Network [OSTI]

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

230

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

E-Print Network [OSTI]

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

California at Santa Cruz, University of

231

Smallholder farmer welfare in a time of changing climate: the role of cropping decisions in local food security in the Nainital District of Uttarakhand, India  

E-Print Network [OSTI]

polarized perspectives 2.6 Amartya Sen and the mechanisms ofPenguin, New York, 2005. Amartya Sen. Poverty and Famines:Press, Oxford, 1981. Amartya Sen. The Political Economy of

Lin, Marena

2013-01-01T23:59:59.000Z

232

Smallholder farmer welfare in a time of changing climate: the role of cropping decisions in local food security in the Nainital District of Uttarakhand, India  

E-Print Network [OSTI]

trees ?12. Do more water harvesting ?13. Do more off-farmtrees 4.1 Do more water harvesting 4.1 Do more off-farma lesser degree, doing more water harvesting and livelihood

Lin, Marena

2013-01-01T23:59:59.000Z

233

Smallholder farmer welfare in a time of changing climate: the role of cropping decisions in local food security in the Nainital District of Uttarakhand, India  

E-Print Network [OSTI]

Climate change and Indian agriculture . . . . . . . . . . . . . . . . . .of climate change on Chinas agriculture. Agricultural1 Introduction Climate change and Indian agriculture Recent

Lin, Marena

2013-01-01T23:59:59.000Z

234

THREE-MINUTE OSCILLATIONS ABOVE SUNSPOT UMBRA OBSERVED WITH THE SOLAR DYNAMICS OBSERVATORY/ATMOSPHERIC IMAGING ASSEMBLY AND NOBEYAMA RADIOHELIOGRAPH  

SciTech Connect (OSTI)

Three-minute oscillations over a sunspot's umbra in AR 11131 were observed simultaneously in UV/EUV emission by the Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) and in radio emission by the Nobeyama Radioheliograph (NoRH). We use 24 hr series of SDO and 8 hr series of NoRH observations to study spectral, spatial, and temporal variations of pulsations in the 5-9 mHz frequency range at different layers of the solar atmosphere. High spatial and temporal resolution of SDO/AIA in combination with long-duration observations allowed us to trace the variations of the cutoff frequency and spectrum of oscillations across the umbra. We found that higher frequency oscillations are more pronounced closer to the umbra's center, while the lower frequencies concentrate on the peripheral parts. We interpreted this discovery as a manifestation of variation of the magnetic field inclination across the umbra at the level of temperature minimum. Possible implications of this interpretation for the diagnostics of sunspot atmospheres are discussed.

Reznikova, V. E.; Shibasaki, K. [Nobeyama Solar Radio Observatory/NAOJ, Nagano 384-1305 (Japan); Sych, R. A. [Key Laboratory of Solar Activity, NAOC, Beijing 100012 (China); Nakariakov, V. M., E-mail: reznik@nro.nao.ac.jp [Physics Department, University of Warwick, Coventry CV4 7AL (United Kingdom)

2012-02-20T23:59:59.000Z

235

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

SciTech Connect (OSTI)

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

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

2011-12-30T23:59:59.000Z

236

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

E-Print Network [OSTI]

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

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

2014-01-01T23:59:59.000Z

237

RESULTS OF THE LICK OBSERVATORY SUPERNOVA SEARCH FOLLOW-UP PHOTOMETRY PROGRAM: BVRI LIGHT CURVES OF 165 TYPE Ia SUPERNOVAE  

SciTech Connect (OSTI)

We present BVRI light curves of 165 Type Ia supernovae (SNe Ia) from the Lick Observatory Supernova Search follow-up photometry program from 1998 through 2008. Our light curves are typically well sampled (cadence of 3-4 days) with an average of 21 photometry epochs. We describe our monitoring campaign and the photometry reduction pipeline that we have developed. Comparing our data set to that of Hicken et al., with which we have 69 overlapping supernovae (SNe), we find that as an ensemble the photometry is consistent, with only small overall systematic differences, although individual SNe may differ by as much as 0.1 mag, and occasionally even more. Such disagreement in specific cases can have significant implications for combining future large data sets. We present an analysis of our light curves which includes template fits of light-curve shape parameters useful for calibrating SNe Ia as distance indicators. Assuming the B - V color of SNe Ia at 35 days past maximum light can be presented as the convolution of an intrinsic Gaussian component and a decaying exponential attributed to host-galaxy reddening, we derive an intrinsic scatter of {sigma} = 0.076 {+-} 0.019 mag, consistent with the Lira-Phillips law. This is the first of two papers, the second of which will present a cosmological analysis of the data presented herein.

Ganeshalingam, Mohan; Li Weidong; Filippenko, Alexei V.; Anderson, Carmen; Foster, Griffin; Griffith, Christopher V.; Joubert, Niels; Leja, Joel; Macomber, Brent; Pritchard, Tyler; Thrasher, Patrick; Winslow, Dustin [Department of Astronomy, University of California, Berkeley, CA 94720-3411 (United States); Gates, Elinor L.; Grigsby, Bryant J.; Lowe, Thomas B. [Lick Observatory, P.O. Box 85, Mount Hamilton, CA 95140 (United States)

2010-10-15T23:59:59.000Z

238

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

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

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

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

2011-12-30T23:59:59.000Z

239

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

SciTech Connect (OSTI)

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

240

HAWC ?-Ray Observatory  

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

These phenomena include the collisions of two neutron stars, the explosions of supernovae, binary systems of stars with stellar accretion, and active galactic nuclei which...

Note: This page contains sample records for the topic "observatory nainital uttarkhand" 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

European Southern Observatory  

E-Print Network [OSTI]

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

Liske, Jochen

242

European Southern Observatory  

E-Print Network [OSTI]

. Maintenance-friendly, high redundancy. Highly reliable Optimal load distribution (connected hydraulic "whiffle thermal inertia. Wind disturbance. Maintenance. Segment re-coating Access to sub-systems. #12;4 European and M2 6- mirror, spherical M1, flat M2 Highest cost Feasibility M2? No mass-produced optics Centering

Liske, Jochen

243

OBSERVATORY SNO INSTITUTE MEMBERS  

E-Print Network [OSTI]

and Astronomy Research Council of the U.K. The heavy water is on loan from Canada's federal agency AECL

Abolmaesumi, Purang

244

NATIONAL RADIO ASTRONOMY OBSERVATORY  

E-Print Network [OSTI]

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

Groppi, Christopher

245

Armagh Observatory Annual Report  

E-Print Network [OSTI]

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

246

The Herschel Space Observatory  

E-Print Network [OSTI]

Teflon Aperture Cover Star Tracker Herschel Overview Paul Goldsmith 2nd Submm Spectroscopic Pathfinder Paul Goldsmith Sunshield and Solar Array Cryostat Focal Plane Instruments Herschel Planck 3.5m diameter

Shumway, John

247

European Southern Observatory  

E-Print Network [OSTI]

, materials and processes, from design to operations Max. reliance on serial production or standard parts Max

Liske, Jochen

248

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

SciTech Connect (OSTI)

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

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

2013-11-01T23:59:59.000Z

249

HYDRATE RESEARCH ACTIVITIES THAT BOTH SUPPORT AND DERIVE FROM THE MONITORING STATION/SEA-FLOOR OBSERVATORY, MISSISSIPPI CANYON 118, NORTHERN GULF OF MEXICO  

SciTech Connect (OSTI)

A permanent observatory has been installed on the seafloor at Federal Lease Block, Mississippi Canyon 118 (MC118), northern Gulf of Mexico. Researched and designed by the Gulf of Mexico Hydrates Research Consortium (GOM-HRC) with the geological, geophysical, geochemical and biological characterization of in situ gas hydrates systems as the research goal, the site has been designated by the Bureau of Ocean Energy Management as a permanent Research Reserve where studies of hydrates and related ocean systems may take place continuously and cooperatively into the foreseeable future. The predominant seafloor feature at MC118 is a carbonate-hydrate complex, officially named Woolsey Mound for the founder of both the GOM-HRC and the concept of the permanent seafloor hydrates research facility, the late James Robert Bob Woolsey. As primary investigator of the overall project until his death in mid-2008, Woolsey provided key scientific input and served as chief administrator for the Monitoring Station/ Seafloor Observatory (MS-SFO). This final technical report presents highlights of research and accomplishments to date. Although not all projects reached the status originally envisioned, they are all either complete or positioned for completion at the earliest opportunity. All Department of Energy funds have been exhausted in this effort but, in addition, leveraged to great advantage with additional federal input to the project and matched efforts and resources. This report contains final reports on all subcontracts issued by the University of Mississippi, Administrators of the project, Hydrate research activities that both support and derive from the monitoring station/sea-floor Observatory, Mississippi Canyon 118, northern Gulf of Mexico, as well as status reports on the major components of the project. All subcontractors have fulfilled their primary obligations. Without continued funds designated for further project development, the Monitoring Station/Seafloor Observatory is in danger of lapsing into disuse. However, for the present, interest in the site on the continental slope is healthy and The Center for Marine Resources and Environmental Technology continues to coordinate all activity at the MS/SFO as arranged through the BOEM in 2005. Field and laboratory research projects and findings are reviewed, new technologies and tests described. Many new sensors, systems and two custom ROVs have been developed specifically for this project. Characteristics of marine gas hydrates are dramatically more refined than when the project was initiated and include appear in sections entitled Accomplishments, Products and Publications.

Lutken, Carol

2013-07-31T23:59:59.000Z

250

An upper limit to the photon fraction in cosmic rays above 10**19-eV from the Pierre Auger Observatory  

SciTech Connect (OSTI)

An upper limit of 16% (at 95% c.l.) is derived for the photon fraction in cosmic rays with energies above 10{sup 19} eV, based on observations of the depth of shower maximum performed with the hybrid detector of the Pierre Auger Observatory. This is the first such limit on photons obtained by observing the fluorescence light profile of air showers. This upper limit confirms and improves on previous results from the Haverah Park and AGASA surface arrays. Additional data recorded with the Auger surface detectors for a subset of the event sample, support the conclusion that a photon origin of the observed events is not favored.

Abraham, J.; Aglietta, M.; Aguirre, C.; Allard, D.; Allekotte, I.; Allison, P.; Alvarez, C.; Alvarez-Muniz, J.; Ambrosio, M.; Anchordoqui, L.; Anjos, J.C.; /Centro Atomico Bariloche /Buenos Aires, CONICET /La Plata U. /Pierre Auger Observ. /CNEA, San Martin /Adelaide U. /Catholic U. of Bolivia, La Paz /Bolivia U. /Sao Paulo U. /Campinas State U. /UEFS, Feira de Santana; ,

2006-06-01T23:59:59.000Z

251

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

SciTech Connect (OSTI)

This paper presents a study of a large sample of global disturbances in the solar corona with characteristic propagating fronts as intensity enhancement, similar to the phenomena that have often been referred to as Extreme Ultraviolet Imaging Telescope (EIT) waves or extreme-ultraviolet (EUV) waves. Now EUV images obtained by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory provide a significantly improved view of these large-scale coronal propagating fronts (LCPFs). Between 2010 April and 2013 January, a total of 171 LCPFs have been identified through visual inspection of AIA images in the 193 channel. Here we focus on the 138 LCPFs that are seen to propagate across the solar disk, first studying how they are associated with flares, coronal mass ejections (CMEs), and type II radio bursts. We measure the speed of the LCPF in various directions until it is clearly altered by active regions or coronal holes. The highest speed is extracted for each LCPF. It is often considerably higher than EIT waves. We do not find a pattern where faster LCPFs decelerate and slow LCPFs accelerate. Furthermore, the speeds are not strongly correlated with the flare intensity or CME magnitude, nor do they show an association with type II bursts. We do not find a good correlation either between the speeds of LCPFs and CMEs in a subset of 86 LCPFs observed by one or both of the Solar and Terrestrial Relations Observatory spacecraft as limb events.

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

2013-10-10T23:59:59.000Z

252

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

E-Print Network [OSTI]

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

Yaghi, Omar M.

253

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 (OSTI)

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

254

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

SciTech Connect (OSTI)

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

255

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

SciTech Connect (OSTI)

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

256

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

2000-09-19T23:59:59.000Z

257

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

SciTech Connect (OSTI)

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

Shen Yuandeng; Liu Yu, E-mail: ydshen@ynao.ac.cn [Yunnan Astronomical Observatory, Chinese Academy of Sciences, Kunming 650011 (China)

2012-07-20T23:59:59.000Z

258

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

SciTech Connect (OSTI)

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

259

Making an Energy Histogram Using Pierre Auger Observatory Surface Detector Data A histogram is essentially a graphical representation of the frequency or distribution of a variable over specific intervals  

E-Print Network [OSTI]

Making an Energy Histogram Using Pierre Auger Observatory Surface Detector Data Histogram A histogram is essentially a graphical representation of the frequency or distribution of a variable over energies. Before you start you should know that: o This set of instructions only assumes a very minimal

260

The Study of TeV Variability and Duty Cycle of Mrk 421 from 3 Years of Observations with the Milagro Observatory  

E-Print Network [OSTI]

TeV flaring activity with time scales as short as tens of minutes and an orphan TeV flare have been observed from the blazar Markarian 421 (Mrk 421). The TeV emission from Mrk 421 is believed to be produced by leptonic synchrotron self-Compton (SSC) emission. In this scenario, correlations between the X-ray and the TeV fluxes are expected, TeV orphan flares are hardly explained and the activity (measured as duty cycle) of the source at TeV energies is expected to be equal or less than that observed in X-rays if only SSC is considered. To estimate the TeV duty cycle of Mrk 421 and to establish limits on its variability at different time scales, we continuously observed Mrk 421 with the Milagro observatory. Mrk 421 was detected by Milagro with a statistical significance of 7.1 standard deviations between 2005 September 21 and 2008 March 15. The observed spectrum is consistent with previous observations by VERITAS. We estimate the duty cycle of Mrk 421 for energies above 1 TeV for different hypothesis of the bas...

Abdo, A A; Allen, B T; Aune, T; Barber, A S; Berley, D; Braun, J; Chen, C; Christopher, G E; Delay, R S; DeYoung, T; Dingus, B L; Ellsworth, R W; Fraija, N; Gonzlez, M M; Goodman, J A; Hays, E; Hoffman, C M; Hntemeyer, P H; Imran, A; Kolterman, B E; Linnemann, J T; Marinelli, A; McEnery, J E; Morgan, T; Mincer, A I; Nemethy, P; Patricelli, B; Pretz, J; Ryan, J M; Parkinson, P M Saz; Schneider, M; Shoup, A; Sinnis, G; Smith, A J; Vasileiou, V; Walker, G P; Williams, D A; Yodh, G B

2014-01-01T23:59:59.000Z

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261

Measurement of the cosmic ray spectrum above $4{\\times}10^{18}$ eV using inclined events detected with the Pierre Auger Observatory  

E-Print Network [OSTI]

A measurement of the cosmic-ray spectrum for energies exceeding $4{\\times}10^{18}$ eV is presented, which is based on the analysis of showers with zenith angles greater than $60^{\\circ}$ detected with the Pierre Auger Observatory between 1 January 2004 and 31 December 2013. The measured spectrum confirms a flux suppression at the highest energies. Above $5.3{\\times}10^{18}$ eV, the "ankle", the flux can be described by a power law $E^{-\\gamma}$ with index $\\gamma=2.70 \\pm 0.02 \\,\\text{(stat)} \\pm 0.1\\,\\text{(sys)}$ followed by a smooth suppression region. For the energy ($E_\\text{s}$) at which the spectral flux has fallen to one-half of its extrapolated value in the absence of suppression, we find $E_\\text{s}=(5.12\\pm0.25\\,\\text{(stat)}^{+1.0}_{-1.2}\\,\\text{(sys)}){\\times}10^{19}$ eV.

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

2015-03-26T23:59:59.000Z

262

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

E-Print Network [OSTI]

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

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

2006-01-17T23:59:59.000Z

263

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 (OSTI)

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

264

Searches for HCl and HF in comets 103P/Hartley 2 and C/2009 P1 (Garradd) with the Herschel space observatory  

E-Print Network [OSTI]

HCl and HF are expected to be the main reservoirs of fluorine and chlorine wherever hydrogen is predominantly molecular. They are found to be strongly depleted in dense molecular clouds, suggesting freeze-out onto grains in such cold environments. We can then expect that HCl and HF were also the major carriers of Cl and F in the gas and icy phases of the outer solar nebula, and were incorporated into comets. We aimed to measure the HCl and HF abundances in cometary ices as they can provide insights on the halogen chemistry in the early solar nebula. We searched for the J(1-0) lines of HCl and HF at 626 and 1232 GHz, respectively, using the HIFI instrument on board the Herschel Space Observatory. HCl was searched for in comets 103P/Hartley 2 and C/2009 P1 (Garradd), whereas observations of HF were conducted in comet C/2009 P1. In addition, observations of H$_2$O and H$_2^{18}$O lines were performed in C/2009 P1 to measure the H$_2$O production rate. Three lines of CH$_3$OH were serendipitously observed in the ...

Bockele-Morvan, D; Crovisier, J; Lis, D C; Hartogh, P; Moreno, R; de Val-Borro, M; Blake, G A; Szutowicz, S; Boissier, J; Cernicharo, J; Charnley, S B; Combi, M; Cordiner, M A; de Graauw, T; Encrenaz, P; Kidger, M; Kppers, M; Milam, S N; Mller, H S P; Phillips, T G; Rengel, M

2014-01-01T23:59:59.000Z

265

Measurement of the cosmic ray spectrum above $4{\\times}10^{18}$ eV using inclined events detected with the Pierre Auger Observatory  

E-Print Network [OSTI]

A measurement of the cosmic-ray spectrum for energies exceeding $4{\\times}10^{18}$ eV is presented, which is based on the analysis of showers with zenith angles greater than $60^{\\circ}$ detected with the Pierre Auger Observatory between 1 January 2004 and 31 December 2013. The measured spectrum confirms a flux suppression at the highest energies. Above $5.3{\\times}10^{18}$ eV, the "ankle", the flux can be described by a power law $E^{-\\gamma}$ with index $\\gamma=2.70 \\pm 0.02 \\,\\text{(stat)} \\pm 0.1\\,\\text{(sys)}$ followed by a smooth suppression region. For the energy ($E_\\text{s}$) at which the spectral flux has fallen to one-half of its extrapolated value in the absence of suppression, we find $E_\\text{s}=(5.12\\pm0.25\\,\\text{(stat)}^{+1.0}_{-1.2}\\,\\text{(sys)}){\\times}10^{19}$ eV.

,

2015-01-01T23:59:59.000Z

266

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

SciTech Connect (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

267

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  

SciTech Connect (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

268

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

SciTech Connect (OSTI)

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

269

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

SciTech Connect (OSTI)

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

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

2013-05-01T23:59:59.000Z

270

Okayama Astrophysical Observatory, National Astronomical Observatory of Japan,  

E-Print Network [OSTI]

Abstract. The development of large ground-based telescopes and sensitive large format detectors, as well as the develepment of various techniques for the selection of high-z galaxies enabled us to construct large samples of galaxies in the early universe, as reported in the many contributions in this proceedings. The next major step for the comprehensive understanding of the galaxy evolution would be to explore the relationship of galaxies selected with different criteria at different epochs and find links between them. In this contribution we present the properties of Lyman break galaxies (LBGs) at z ? 5 obtained by deep and wide blank field surveys, and through the comparison with samples at lower redshift ranges we discuss the evolution of star-forming galaxies in the early universe.

F. Combes; J. Palous; Kiuchi G; Sawicki M

2006-01-01T23:59:59.000Z

271

Solar & Heliospheric Observatory The SOLAR AND HELIOSPHERIC OBSERVATORY  

E-Print Network [OSTI]

of international cooperation be­ tween ESA (the EUROPEAN SPACE AGENCY) and NASA to study the Sun, from its deep core to the outer corona, and the solar wind. SOHO was launched on De­ cember 2, 1995, on top of an Atlas/Centaur combina­ tion, from Cape Canaveral Air­Force Base in Florida. It reached its operating

Martens, Petrus C.

272

Data Center Observatory General Schematic  

E-Print Network [OSTI]

2 1U Rack 1 3U Air FM40 Air FM40 Campuschilledwaterloop PUMP ROOM (FMS BUILDING) CICBUILDING ZONE 1 · High density enclosure (HDE) · 12 racks · Heat contained within HDE · Exterior room air is 72 degrees system · Distance-read sub-floor leak detection system PUMP ROOM · Redundant heat exchangers and pumps

273

Data Center Observatory General Schematic  

E-Print Network [OSTI]

2 1U Rack 1 3U Air FM40 Air FM40 Campuschilledwaterloop PUMP ROOM (FMS BUILDING) CICBUILDING · High-action sprinkler system · Distance-read sub-floor leak detection system PUMP ROOM · Redundant heat exchangers Density Enclosures (HDE) · Zone1: 12 Racks · Zone2: 11 Racks · Heat contained within HDE · Exterior room

274

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

SciTech Connect (OSTI)

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

Aab, Alexander; et al,

2014-10-07T23:59:59.000Z

275

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  

SciTech Connect (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

276

NATIONAL RADIO ASTRONOMY OBSERVATORY CHARLOTTESVILLE VIRGINIA  

E-Print Network [OSTI]

. It is programed in BASIC and has been implemented on the VAX -11 as well as the HP 9845A desktop computer. Using Optimization to Solve Constrained-Variable and III. FARANT on the VAX-11 and the HP 9845A . · · · . · * . 37 1. Using the Apple Computer as a VAX Terminal · . · · · . 37 2. Peculiarities of VAX BASIC

Groppi, Christopher

277

NATIONAL RADIO ASTRONOMY OBSERVATORY CHARLOTTESVILLE, VIRGINIA  

E-Print Network [OSTI]

.2.13.4 Miscellaneous Routines · · · · · 0 0 0 0 0 . 36 2.3 Setup and Environment in VAX · . · · . · · · · . 36 2.3.1 Pieces of FARANT in VAX · ·· · · 0 · 0 0 0 · 37 2.3.2 Running of FARANT in VAX . · 38· · .· · · · · · 2 . · · · · 66 3.4.3 Miscellaneous · · · · · 0 · · · · ·0 0 0 . 0 67 3.5 HP 9845 BASIC And VAX FORTRAN

Groppi, Christopher

278

IATP | Trade Observatory | Headlines q What's new  

E-Print Network [OSTI]

towards the elimination of tariffs, non-tariff barriers, and putting in place more effective trade rules

279

Neutrino observations from the Sudbury Neutrino Observatory  

E-Print Network [OSTI]

Energy of Canada Limited (AECL), Agra-Monenco, Canatom,The heavy water was loaned by AECL with the cooperation of

2001-01-01T23:59:59.000Z

280

nuclex/9910016 The Sudbury Neutrino Observatory  

E-Print Network [OSTI]

.T.H. Clifford, R. Deal, E.D. Earle, E. Gaudette, G. Milton, B.Sur Chalk River Laboratories, AECL Research, Chalk

Waltham, Chris

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281

Crossing the Transition Region High Altitude Observatory,  

E-Print Network [OSTI]

: enhanced emission at TR temperatures Much lower density in umbra and plume: (log(Ne/cm 3)=10 Lyman line profiles not reversed in umbra and plume TR above sunspots is higher and probably more extended than in the surrounding plage region ------plage -.-.-.penumbra ......umbra ____plume #12;Outline Recent observations

282

VLA Technical Memo Smithsonian Astrophysical Observatory  

E-Print Network [OSTI]

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

Groppi, Christopher

283

State Lands Management Plan Rosemary Hill Observatory  

E-Print Network [OSTI]

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

Slatton, Clint

284

NATIONAL RADIO ASTRONOMY OBSERVATORY CHARLOTTESVILLE, VIRGINIA  

E-Print Network [OSTI]

is engaged it supplies the various power supplies, cooling fans, and output receptacles with power DISTRIBUTION A master circuit breaker is supplied on the bottom front panel of the cabinet. The circuit breaker conductor cable supplies the necessary 110 volts single phase alternating current. When the circuit breaker

Groppi, Christopher

285

ORIGINAL ARTICLE Colonization of subsurface microbial observatories  

E-Print Network [OSTI]

Toner5 , C Geoffrey Wheat6 and Katrina J Edwards1 1 University of Southern California, Los Angeles, CA and the lithosphere (Fisher and Wheat, 2010). Circulation of fluid within oceanic crust and redox reactions are known-moderate temperatures (0­40 1C) on ridge flanks (Wheat et al., 2003). Considerin

Fisher, Andrew

286

NATIONAL RADIO ASTRONOMY OBSERVATORY CHARLOTTESVILLE, VIRGINIA  

E-Print Network [OSTI]

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

Groppi, Christopher

287

Bishop's University Astronomical Observatory October 2009  

E-Print Network [OSTI]

a smaller carbon footprint. This is part of the multi-million dollar Energy Services Contract initiative

288

The Sudbury Neutrino Observatory The SNO Collaboration  

E-Print Network [OSTI]

, University of Guelph, Guelph, Ontario N1G 2W1 CANADA2 C. Alexander, E.W. Beier, J.C. Cook, D.F. Cowen, E designed to determine whether the currently observed solar neutri

Waltham, Chris

289

Rothney Astrological Observatory (Priddis) Emergency Instructions  

E-Print Network [OSTI]

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

de Leon, Alex R.

290

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 (OSTI)

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

291

The Anglo-Australian Observatorys 2dF facility  

E-Print Network [OSTI]

The 2dF (Two-degree Field) facility at the prime focus of the Anglo-Australian Telescope provides multiple object spectroscopy over a 2 ? field of view. Up to 400 target fibres can be independently positioned by a complex robot. Two spectrographs provide spectra with resolutions of between 500 and 2000, over wavelength ranges of 440nm and 110nm respectively. The 2dF facility began routine observations in 1997. 2dF was designed primarily for galaxy redshift surveys and has a number of innovative features. The large corrector lens incorporates an atmospheric dispersion compensator, essential for wide wavelength coverage with small diameter fibres. The instrument has two full sets of fibres on separate field plates, so that re-configuring can be done in parallel with observing. The robot positioner places one fibre every 6 seconds, to a precision of 0.3 arcsec (20 m) over the full field. All components of 2dF, including the spectrographs, are mounted on a 5-m diameter telescope top-end ring for ease of handling and to keep the optical fibres short in order to maximise UV throughput.

I. J. Lewis; R. D. Cannon; K. Taylor; K. Glazebrook; J. A. Bailey; J. D. Whittard; J. K. Wilcox; K. C. Willis

292

Operations of and Future Plans Pierre Auger Observatory  

E-Print Network [OSTI]

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

293

Future development of the PLATO observatory for Antarctic science  

E-Print Network [OSTI]

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

Ashley, Michael C. B.

294

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network [OSTI]

square law for low voltage and current. At high current the resistance of the diode and the load re function. The curve for Rx 1. 5 K ohm follows the square law curve for outputs from 10 millivolts to 150 millivolts. The Rx = 1. 5 K ohm curve starts near the one-diode curve and ap- proaches the two-diode curve

Groppi, Christopher

295

NATIONAL RADIO ASTRONOMY OBSERVATORY GREEN BANK, WEST VIRGINIA  

E-Print Network [OSTI]

diodes and provides a fairly wide square law range. The curve is adjusted by varying the DC load that the load changed the shape of the error curve as well as the tilt. It appeared to be an indirect method of curve control. In the process of experimenting with the circuit it was discovered that source impedance

Groppi, Christopher

296

NATIONAL RADIO ASTRONOMY OBSERVATORY ELECTRONICS DIVISION TECHNICAL NOTE NO 113  

E-Print Network [OSTI]

the Apple II for Graphics Output from VAX FA AUTHOR(S): Stowe Keller DATE: August 3, 1982 Distribution: J;USING THE APPLE II FOR GRAPHICS OUTPUT FROM VAX FARANT Stowe Keller I. Introduction FARANT, a program design. It has been implemented on the HP-9845A desktop computer and the VAX 11. The HP-9845A offers

Groppi, Christopher

297

Results from the Sudbury Neutrino Observatory Phase III  

E-Print Network [OSTI]

current interactions in heavy water and determine preciselySNO) is a 1 kton heavy water Cherenkov detector, located atNaCl) were added to the heavy water to enhance the neutron

Prior, G.; SNO Collaboration

2009-01-01T23:59:59.000Z

298

NATIONAL RADIO ASTRONOMY OBSERVATORY GREEN BANK, WEST VIRGINIA  

E-Print Network [OSTI]

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

Groppi, Christopher

299

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network [OSTI]

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

Groppi, Christopher

300

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network [OSTI]

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

Groppi, Christopher

Note: This page contains sample records for the topic "observatory nainital uttarkhand" 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

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

302

atmospheric observatory uao: Topics by E-print Network  

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

of a 1 kiloton heavy water Cherenkov detector able to detect and reconstruct high-energy muons created from cosmic ray showers and atmospheric neutrino interactions. By...

303

A Networked Telerobotic Observatory for Collaborative Remote Observation of Avian  

E-Print Network [OSTI]

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

Goldberg, Ken

304

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network [OSTI]

Power Supply Schematic - - - - - Fig. 21 Isolation Transformer Module Schematic Fig. 1 Interferometer OF CONTENTS 2.0 IF PROCESSING COMPONENTS Fig. 7 - Interferometer System Time Delays 2.1 IF Cable Equalizers Module - - - - - - - - - - - - - - 2.6 HP 460AR IF Amplifier 2.7 Total Power Module 2.8 TP/AGC DC

Groppi, Christopher

305

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network [OSTI]

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

Groppi, Christopher

306

The observatory : designing data-driven decision making tools  

E-Print Network [OSTI]

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

Simoes, Alexander James Gaspar

2012-01-01T23:59:59.000Z

307

Education and public outreach of the Pierre Auger Observatory  

SciTech Connect (OSTI)

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

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

2005-08-01T23:59:59.000Z

308

New Approaches in Embedded Networked Sensing for Terrestrial Ecological Observatories  

E-Print Network [OSTI]

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

2007-01-01T23:59:59.000Z

309

Electron antineutrino search Sudbury Neutrino Observatory 9 Bellerive,  

E-Print Network [OSTI]

, Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA Alamos National Laboratory, Alamos Accelerator Center, Menlo Park, California, d Present address: Max­Planck­Institut Nuclear Physics, Heidelberg

310

NATIONAL RADIO ASTRONOMY OBSERVATORY GREEN BANK, WEST VIRGINIA  

E-Print Network [OSTI]

radiation from the room temperature dewar walls to the internal surfaces is typically the largest heat load with equation 6 allows calculation of the net heat flow from the simplified gray body equation when T INTERNAL REPORT NO. 323 On Radiation Loading in Cryogenic Dewars and Emissivity Measurements

Groppi, Christopher

311

NATIONAL RADIO ASTRONOMY OBSERVATORY GREEN BANK, WEST VIRGINIA  

E-Print Network [OSTI]

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

Groppi, Christopher

312

A realtime observatory for laboratory simulation of planetary flows  

E-Print Network [OSTI]

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

Ravela, Srinivas (Sai)

313

Lamont Doherty Earth Observatory General Administration Human Resources  

E-Print Network [OSTI]

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

Khatiwala, Samar

314

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia,  

E-Print Network [OSTI]

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

Groppi, Christopher

315

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network [OSTI]

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

Groppi, Christopher

316

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network [OSTI]

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

Groppi, Christopher

317

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

E-Print Network [OSTI]

University, Chelyabinsk, 454080, Russia 3Cardiff Centre for Astrobiology, Cardiff University, Cardiff CF10 3

318

The Anglo-Australian Observatory's 2dF Facility  

E-Print Network [OSTI]

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

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

2002-02-08T23:59:59.000Z

319

NATIONAL RADIO ASTRONOMY OBSERVATORY GREEN BANK WEST VIRGINIA  

E-Print Network [OSTI]

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

Groppi, Christopher

320

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network [OSTI]

. At a later date, the data may be derived from the NRAO solar clock. SID information contains record name No. 31 DIGITAL OUTPUT UNIT FOR THE LUNAR OCCULTATION RECEIVERS Nigel J. Keen JUNE 1964 NUMBER OF COPIES: 75 #12;DIGITAL OUTPUT UNIT F It THE LUNAR OCCULTATION RECEIVERS Nigel J. Keen General The outputs

Groppi, Christopher

Note: This page contains sample records for the topic "observatory nainital uttarkhand" 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

NATIONAL RADIO ASTRONOMY OBSERVATORY GREEN BANK, W ES  

E-Print Network [OSTI]

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

Groppi, Christopher

322

HAWC Observatory to study universe's most energetic phenomena  

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

of supermassive black holes at the center of some galaxies-as well as tracking gamma ray bursts and other large explosions. The researchers will also work to determine the...

323

NATIONAL RADIO ASTRONOMY OBSERVATORY GREEN BANK, WEST VIRGINIA  

E-Print Network [OSTI]

an Ellis and Watts Company Model LCAH-23 chilled water system and a proportion- ally controlled heater OOOOOOOOOOOOOOOOOOOOOOO ·········· 7 Temperature Control Circuit OOOOOOOOOOOOOOOOOOOOO ·· ......... .... 7 Heater Current) CABIN CONTROL SIGNAL · TEMP CONTROLLER 208V, 30 HEATER TEMP MONITOR [-- RETURN LIQUID CHILLER

Groppi, Christopher

324

NATIONAL RADIO ASTRONOMY OBSERVATORY ELECTRONICS DIVISION INTERNAL REPORT NO. 321  

E-Print Network [OSTI]

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

Groppi, Christopher

325

SCIENTIFIC HIGHLIGHTS FROM THE SOLAR AND HELIOSPHERIC OBSERVATORY  

E-Print Network [OSTI]

scientific results from the ESA/NASA SOHO mission, with a special emphasis on remote sensing observations are \\Gamma to study the solar interior, using the techniques of helioseismology, \\Gamma to study the heating to investigate the solar wind and its acceleration processes, again by remote sensing, and by in situ particle

Martens, Petrus C.

326

The Magdalena Ridge Observatory interferometer: 2014 status update  

E-Print Network [OSTI]

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

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

2014-07-24T23:59:59.000Z

327

James Cronin, CP Violation, and the Pierre Auger Observatory  

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

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May JunDatastreamsmmcrcalgovInstrumentsruc DocumentationP-SeriesFlickrinformation for andFuel-EfficientJeffersonAna Moore

328

Experiment Profile: COUPP NAME: Chicagoland Observatory for Underground Particle  

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

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr MayAtmospheric Optical Depth7-1D: Vegetation ProposedUsing ZirconiaPolicy and Assistance100 tonusingdeposition.EnergyExpedited6 DES

329

Los Alamos observatory fingers cosmic ray 'hot spots'  

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

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May JunDatastreamsmmcrcalgovInstrumentsrucLas Conchas recovery challenge fund Las Conchas recoveryNuclear energyInstrumentLos

330

Radiosonde campaign in Paranal Observatory 2011: PWV measurement.  

E-Print Network [OSTI]

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

331

Milagro all-sky TeV gamma ray observatory.  

SciTech Connect (OSTI)

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

Sinnis, C. (Constantine)

2002-01-01T23:59:59.000Z

332

NATIONAL RADIO ASTRONOMY OBSERVATORY Green Bank, West Virginia  

E-Print Network [OSTI]

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

Groppi, Christopher

333

ICRC 2007: Mrida, Mexico Highlights from the Pierre Auger Observatory  

E-Print Network [OSTI]

and side-by- side." V.H.Hess, Nobel Lecture, December 1936 #12;2 Argentina Australia Brasil Bolivia* Mexico (stereo low N) ~ 0.2 ~ 1 - 2 ~ 3 - 5 Flat with energy AND E, A, spectral mass and model (M) free slope and M dependent A and M free A and M A and M free dependent Angular Resolution Aperture Energy #12

334

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

E-Print Network [OSTI]

for water950L for water ·· RnRn--lessless--airair supply systemsupply system ·· Water purification systemWater (stainless steel) water (+50mmAq) 60cm SK dome air #12;Water purification systemWater purification system purification system ·· Membrane degassing module testMembrane degassing module test ·· SummarySummary #12

Takeuchi, Yasuo

335

The National Astronomical Observatory of Japan (NAOJ) invites application for the following Mitaka-based staff of the NAOJ Chile Observatory  

E-Print Network [OSTI]

astronomy 4. Duties and responsibilities: The East Asian Project Scientist (EA-PS) mainly has the following to collect and summarize science demand in the East Asian community of researchers. For new enhancement communication skills to build and maintain good collaborative relationship are of critical importance. The EA

Ito, Atsushi

336

Oceans. Europe2005 An Acoustically-Linked Deep-Ocean Observatory  

E-Print Network [OSTI]

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

Massachusetts at Amherst, University of

337

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

E-Print Network [OSTI]

photometry curve for type Ia supernovae and the redshift vsdistributions for observed supernovae. Figure 5 from Millermain efforts related to supernovae in progress at Berkeley.

Goldhaber, G.

2008-01-01T23:59:59.000Z

338

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

E-Print Network [OSTI]

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

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

2008-08-01T23:59:59.000Z

339

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

E-Print Network [OSTI]

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

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

2008-01-01T23:59:59.000Z

340

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

E-Print Network [OSTI]

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

Thompson, Anne

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


341

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

342

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

E-Print Network [OSTI]

://www.lafollette.wisc.edu/publications/workingpapers Choose Your Weapon: International Trade Agreements and Exchange Rate Policy Choice Mark S. Copelovitch La@uchicago.edu #12;CHOOSE YOUR WEAPON: INTERNATIONAL TRADE AGREEMENTS AND EXCHANGE RATE POLICY CHOICE Mark S in their nominal effective exchange rates during this period and this relationship is also conditional

Wisconsin at Madison, University of

343

``STUDIES OF THE SUDBURY NEUTRINO OBSERVATORY DETECTOR AND SONOLUMINESCENCE USING A SONOLUMINESCENT SOURCE''  

E-Print Network [OSTI]

heavy water Cerenkov solar neutrino detector. 1000 metric tonnes of heavy water is used as a neutrino electron neutrinos via charged current interactions of electron neutrinos with deuterons in the heavy water Water, have taught me the most. It is incredible how willing they were to help at any time they were

344

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

E-Print Network [OSTI]

tonnes of ultrapure heavy water (D 2 O) contained in aninteractions within SNOs heavy water. It is essential thatabsorbing gas in the heavy water. It was decided to ?ll the

2008-01-01T23:59:59.000Z

345

Investigating gamma-ray lines from dark matter with future observatories  

SciTech Connect (OSTI)

We study the prospects for studying line features in gamma-ray spectra with upcoming gamma-ray experiments, such as HESS-II, the Cherenkov Telescope Array (CTA), and the GAMMA-400 satellite. As an example we use the narrow feature at 130 GeV seen in public data from the Fermi-LAT satellite. We found that all three experiments should be able to confidently confirm or rule out the presence of this 130 GeV feature. If it is real, it should be confirmed with a confidence level higher than 5?. Assuming it to be a spectral signature of dark matter origin, GAMMA-400, thanks to a projected energy resolution of about 1.5 % at 100 GeV, should also be able to resolve both the ?? line and a corresponding Z? or H? feature, if the corresponding branching ratio is comparable to that into two photons. It will also allow to distinguish between a gamma-ray line and the similar feature resulting from internal bremsstrahlung photons.

Bergstrm, Lars; Conrad, Jan; Farnier, Christian [The Oskar Klein Centre for Cosmoparticle Physics, Department of Physics, Stockholm University, AlbaNova, SE-106 91 Stockholm (Sweden); Bertone, Gianfranco [GRAPPA Institute, University of Amsterdam, Science Park 904, 1090 GL Amsterdam (Netherlands); Weniger, Christoph, E-mail: lbe@fysik.su.se, E-mail: gf.bertone@gmail.com, E-mail: conrad@fysik.su.se, E-mail: Christian.Farnier@fysik.su.se, E-mail: weniger@mpp.mpg.de [Max-Planck-Institut fr Physik, Fhringer Ring 6, 80805 Mnchen (Germany)

2012-11-01T23:59:59.000Z

346

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

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

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

Kumar, Jitendra; Hoffman, Forrest M.

347

Remote sensing-based characterization, 2-m, Plant Functional Type Distributions, Barrow Environmental Observatory, 2010  

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

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

Zachary Langford; Forrest Hoffman; Jitendra Kumar

348

Coronal Oscillations above Sunspots? Armagh Observatory, College Hill, Armagh BT61 9DG, N. Ireland  

E-Print Network [OSTI]

that the sunspot oscillations are prominent in transition region lines above the umbra (Maltby et al. 2001 that the oscillation amplitude above the umbra increases with increasing temperature, reaches a maximum

349

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

E-Print Network [OSTI]

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

Tokyo, University of

350

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

E-Print Network [OSTI]

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

Li, Hui

351

NATIONAL RADIO ASTRONOMY OBSERVATORY POST OFFICE BOX 2 GREEN BANK, WEST VIRGINIA 24944-0002  

E-Print Network [OSTI]

telescope collapsed, we eliminated that loop by looping back at the control building. Most of this cable to FEDAL 4 CB to 140-ft PC to PC for carbon copy We used ST type connectors on all of our multimode cables

Groppi, Christopher

352

Limits on Very High Energy Emission from Gamma-Ray Bursts with the Milagro Observatory  

E-Print Network [OSTI]

The Milagro telescope monitors the northern sky for 100 GeV to 100 TeV transient emission through continuous very high energy wide-field observations. The large effective area and ~100 GeV energy threshold of Milagro allow it to detect very high energy (VHE) gamma-ray burst emission with much higher sensitivity than previous instruments and a fluence sensitivity at VHE energies comparable to that of dedicated gamma-ray burst satellites at keV to MeV energies. Even in the absence of a positive detection, VHE observations can place important constraints on gamma-ray burst (GRB) progenitor and emission models. We present limits on the VHE flux of 40 s -- 3 h duration transients nearby to earth, as well as sensitivity distributions which have been corrected for gamma-ray absorption by extragalactic background light and cosmological effects. The sensitivity distributions suggest that the typical intrinsic VHE fluence of GRBs is similar or weaker than the keV -- MeV emission, and we demonstrate how these sensitivit...

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

2004-01-01T23:59:59.000Z

353

Observations of GRB 990123 by the Compton $\\gamma$-Ray Observatory  

E-Print Network [OSTI]

GRB 990123 was the first burst from which simultaneous optical, X-ray and gamma-ray emission was detected; its afterglow has been followed by an extensive set of radio, optical and X-ray observations. We have studied the gamma-ray burst itself as observed by the CGRO detectors. We find that gamma-ray fluxes are not correlated with the simultaneous optical observations, and the gamma-ray spectra cannot be extrapolated simply to the optical fluxes. The burst is well fit by the standard four-parameter GRB function, with the exception that excess emission compared to this function is observed below ~15 keV during some time intervals. The burst is characterized by the typical hard-to-soft and hardness-intensity correlation spectral evolution patterns. The energy of the peak of the nu f_nu spectrum, E_p, reaches an unusually high value during the first intensity spike, 1470 +/- 110 keV, and then falls to consistent with a power law with a photon index of about -3. By fluence, GRB 990123 is brighter than all but 0.4...

Briggs, M S; Kippen, R M; Preece, R D; Kouveliotou, C; Van Paradijs, J; Share, G H; Murphy, R J; Matz, S M; Connors, A; Winkler, C; McConnell, M L; Ryan, J M; Williams, O R; Young, C A; Dingus, B L; Catelli, J R; Wijers, R A M J

1999-01-01T23:59:59.000Z

354

Abstract B44A02: A Strategy for Global Phenological Observatories  

E-Print Network [OSTI]

developed clusters based on a wavelet-filtered subset of the 1982­1999 global Pathfinder Advanced Very High Resolution Radiometer (AVHRR) Land (PAL) Normalized Difference Vegetation Index (NDVI) dataset, a global 10. Oak Ridge National Laboratory is managed by UT-Battelle, LLC, for the U.S. Department of Energy under

Hoffman, Forrest M.

355

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

E-Print Network [OSTI]

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

Groppi, Christopher

356

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

E-Print Network [OSTI]

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

357

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

E-Print Network [OSTI]

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

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

2015-01-01T23:59:59.000Z

358

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

E-Print Network [OSTI]

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

359

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

E-Print Network [OSTI]

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

Lockwood, Wes

360

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

E-Print Network [OSTI]

://www.lafollette.wisc.edu/publications/workingpapers U.S. Health Care Reform: A Primer and an Assessment Robert Haveman La Follette School of Public at the University of Wisconsin-Madison August 19, 2010 #12;1 US Health Care Reform: A Primer and an Assessment presidents and numerous Senators and Congressional Representatives, a comprehensive health care reform bill

Wisconsin at Madison, University of

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


361

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

E-Print Network [OSTI]

.S. health care system does not effectively promote and utilize evidence- based research. Despite the failings of current governance arrangements in the health care system, few researchers have focused of the current health reform proposals will depend critically on the governance arrangements they employ, we have

Wisconsin at Madison, University of

362

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

E-Print Network [OSTI]

that observes very high energy gamma rays (100 GeV to 100 TeV) using the water-Cerenkov technique Mexico, Milagro observes most of the Northern Hemisphere over the course of a day. The high duty cycleV candidates. Active galaxies have been observed to be highly variable at TeV energies. To test for episodic

California at Santa Cruz, University of

363

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

E-Print Network [OSTI]

). The market model relies on financial incentives and performance measures to control behavior, and has been extrinsic incentives crowd out intrinsic incentives such as public service motivation. The limitations, the market model adds a behavioral framework from economic theory explicitly based on assumptions of self

Wisconsin at Madison, University of

364

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

E-Print Network [OSTI]

dwarfs are expected to be brown dwarfs, e.g. do not reach the hydrogen burning phase. Brown dwarf are carried out via the standard LT pipeline. These z band images suffer from strong fringing. We do among 56 frames of the 2M1807+5015 field in Figure 1. 3.Parallax and proper motions Pipeline used: We

Joergens, Viki

365

The Wave-Front Correction System for the Sunrise Balloon-Borne Solar Observatory  

E-Print Network [OSTI]

This paper describes the wave-front correction system developed for the Sunrise balloon telescope, and provides information about its in-flight performance. For the correction of low-order aberrations, a Correlating Wave-Front Sensor (CWS) was used. It consisted of a six-element Shack-Hartmann wave-front sensor (WFS), a fast tip-tilt mirror for the compensation of image motion, and an active telescope secondary mirror for focus correction. The CWS delivered a stabilized image with a precision of 0.04 arcsec (rms), whenever the coarse pointing was better than 90 arcsec peak-to-peak. The automatic focus adjustment maintained a focus stability of 0.01 waves in the focal plane of the CWS. During the 5.5 day flight, good image quality and stability was achieved during 33 hours, containing 45 sequences that lasted between 10 and 45 minutes.

Berkefeld, T; Soltau, D; Bell, A; Doerr, H P; Feger, B; Friedlein, R; Gerber, K; Heidecke, F; Kentischer, T; Lhe, O v d; Sigwarth, M; Wlde, E; Barthol, P; Deutsch, W; Gandorfer, A; Germerott, D; Grauf, B; Meller, R; Alvarez-Herrero, A; Knlker, M; Pillet, V Martinez; Solanki, S K; Title, A M

2010-01-01T23:59:59.000Z

366

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

SciTech Connect (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

367

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

E-Print Network [OSTI]

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

Boss, Emmanuel S.

368

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

E-Print Network [OSTI]

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

Groppi, Christopher

369

Accepted Manuscript The AMMA-CATCH Gourma observatory site in Mali: Relating climatic var  

E-Print Network [OSTI]

-la-Vallée, France20 e Centro de Estudios Avanzados en Zonas Aridas, Casilla 599, colina El Pino s/n La Serena, Chile

Boyer, Edmond

370

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

E-Print Network [OSTI]

topological defects, evaporating primordial black holes, and dark matter particle annihilation and decay could, is the world's first large-area water Cherenkov de- tector capable of continuously monitoring the entire sky stage of construction is under way. We are deploying 170 aux- iliary "outrigger" water Cherenkov

California at Santa Cruz, University of

371

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

E-Print Network [OSTI]

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

Elsworthy, William

2015-01-01T23:59:59.000Z

372

amma-catch gourma observatory: Topics by E-print Network  

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

2.8Angpix and 3.6Angpix. Our spectra include all the important Sodium and Mercury light pollution lines and span a wide interval of azimuth and observing conditions, essential to...

373

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

E-Print Network [OSTI]

(Blank, 2000; Dixit, 2002; Heinrich and Marschke, 2010). In light of the additional noise and special

Wisconsin at Madison, University of

374

Spectral-Line Observing at Arecibo Observatory Karen O'Neil  

E-Print Network [OSTI]

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

375

Instrument Science Report WFPC2 2002-06 Results of the Observatory  

E-Print Network [OSTI]

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

Sirianni, Marco

376

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

E-Print Network [OSTI]

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

377

Observations of GRB 990123 by the Compton Gamma-Ray Observatory  

E-Print Network [OSTI]

GRB 990123 was the first burst from which simultaneous optical, X-ray and gamma-ray emission was detected; its afterglow has been followed by an extensive set of radio, optical and X-ray observations. We have studied the gamma-ray burst itself as observed by the CGRO detectors. We find that gamma-ray fluxes are not correlated with the simultaneous optical observations, and the gamma-ray spectra cannot be extrapolated simply to the optical fluxes. The burst is well fit by the standard four-parameter GRB function, with the exception that excess emission compared to this function is observed below ~15 keV during some time intervals. The burst is characterized by the typical hard-to-soft and hardness-intensity correlation spectral evolution patterns. The energy of the peak of the nu f_nu spectrum, E_p, reaches an unusually high value during the first intensity spike, 1470 +/- 110 keV, and then falls to \\~300 keV during the tail of the burst. The high-energy spectrum above ~MeV is consistent with a power law with a photon index of about -3. By fluence, GRB 990123 is brighter than all but 0.4% of the GRBs observed with BATSE, clearly placing it on the -3/2 power-law portion of the intensity distribution. However, the redshift measured for the afterglow is inconsistent with the Euclidean interpretation of the -3/2 power-law. Using the redshift value of >= 1.61 and assuming isotropic emission, the gamma-ray fluence exceeds 10E54 ergs.

M. S. Briggs; D. L. Band; R. M. Kippen; R. D. Preece; C. Kouveliotou; J. van Paradijs; G. H. Share; R. J. Murphy; S. M. Matz; A. Connors; C. Winkler; M. L. McConnell; J. M. Ryan; O. R. Williams; C. A. Young; B. Dingus; J. R. Catelli; R. A. M. J. Wijers

1999-03-16T23:59:59.000Z

378

Limits on Very High Energy Emission from Gamma-Ray Bursts with the Milagro Observatory  

E-Print Network [OSTI]

The Milagro telescope monitors the northern sky for 100 GeV to 100 TeV transient emission through continuous very high energy wide-field observations. The large effective area and ~100 GeV energy threshold of Milagro allow it to detect very high energy (VHE) gamma-ray burst emission with much higher sensitivity than previous instruments and a fluence sensitivity at VHE energies comparable to that of dedicated gamma-ray burst satellites at keV to MeV energies. Even in the absence of a positive detection, VHE observations can place important constraints on gamma-ray burst (GRB) progenitor and emission models. We present limits on the VHE flux of 40 s -- 3 h duration transients nearby to earth, as well as sensitivity distributions which have been corrected for gamma-ray absorption by extragalactic background light and cosmological effects. The sensitivity distributions suggest that the typical intrinsic VHE fluence of GRBs is similar or weaker than the keV -- MeV emission, and we demonstrate how these sensitivity distributions may be used to place observational constraints on the absolute VHE luminosity of gamma-ray bursts for any GRB emission and progenitor model.

The Milagro Collaboration; R. Atkins; W. Benbow; D. Berley; E. Blaufuss; J. Bussons; D. G. Coyne; T. DeYoung; B. L. Dingus; D. E. Dorfan; R. W. Ellsworth; L. Fleysher; R. Fleysher; G. Gisler; M. M. Gonzalez; J. A. Goodman; T. J. Haines; E. Hays; C. M. Hoffman; L. A. Kelley; J. E. McEnery; R. S. Miller; A. I. Mincer; M. F. Morales; P. Nemethy; D. Noyes; J. M. Ryan; F. W. Samuelson; A. Shoup; G. Sinnis; A. J. Smith; G. W. Sullivan; D. A. Williams; S. Westerhoff; M. E. Wilson; X. Xu; G. B. Yodh

2004-02-06T23:59:59.000Z

379

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

E-Print Network [OSTI]

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

Waltham, Chris

380

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

E-Print Network [OSTI]

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

Note: This page contains sample records for the topic "observatory nainital uttarkhand" 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

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

E-Print Network [OSTI]

, Brett M. Morris, (Derek Richardson) 2012. Neutron Star Radii: Theoretical Tests of Frequency Scattering using HNBody, James Keane, (Douglas P. Hamilton) 2011 Measurements of the Mass and Radius of the Neutron Star 4U 1636-53 Using Millisecond Brightness Oscillations during Thermonuclear X-ray Bursts, Ryan

Gruner, Daniel S.

382

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

E-Print Network [OSTI]

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

Mcdonough, William F.

383

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

E-Print Network [OSTI]

.................................................................................................9 Key Features of TAD Programs........................................................................................................................................11 TAD Eligibility ...............................................................................................................................................................11 TAD Program Components

Wisconsin at Madison, University of

384

Arecibo Observatory Technical Memo AOTM 200001 THE LBW FEED: THE MUELLER MATRIX IN 1999 AND 2000  

E-Print Network [OSTI]

of MA+F ; there are only six independent elements. We present five below; the sixth element m QUANTITIES: TWO YEARS, TWO FREQUENCIES Quantity Mar99, 1420.4 Mar00, 1420.4 Mar00, 1665.3 mQI 0 \\Sigma 0:0004 0 \\Sigma 0:0007 0 \\Sigma 0:0005 mUI 0:0112 \\Sigma 0:0002 0:0065 \\Sigma 0:0007 0:0044 \\Sigma 0:0006 m

385

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

E-Print Network [OSTI]

constructed by Deep Ocean Engineering, Inc. 9 to operate in1 cm diameter Deep Ocean Engineering, San Leandro, CA, URL:

2008-01-01T23:59:59.000Z

386

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

E-Print Network [OSTI]

once poor countries such as South Korea to rise rapidly into the ranks of developed nations. This paper networks and communities. Discussing this topic requires a degree of terminological clarification before that result from the greatly increased levels of international interaction B most obviously but not limited

Wisconsin at Madison, University of

387

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

E-Print Network [OSTI]

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

Mamajek, Eric E.

388

White Papers submitted in advance of Keck Observatory Strategic Planning meeting, Sept. 2014  

E-Print Network [OSTI]

into the giant planets of our solar system, Tom Stallard et al. (4) The Keck is sufficiently high that the AO system itself will act as the fringe tracker, as already demonstrated at even

Abu-Mostafa, Yaser S.

389

Remote sensing-based characterization, 2-m, Plant Functional Type Distributions, Barrow Environmental Observatory, 2010  

SciTech Connect (OSTI)

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

Zachary Langford; Forrest Hoffman; Jitendra Kumar

2014-01-01T23:59:59.000Z

390

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

SciTech Connect (OSTI)

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

Kumar, Jitendra; Hoffman, Forrest M.

2014-03-18T23:59:59.000Z

391

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

E-Print Network [OSTI]

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

Liske, Jochen

392

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

E-Print Network [OSTI]

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

Groppi, Christopher

393

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

E-Print Network [OSTI]

is that carbon prices generate large benefits for conventional oil producers--making a climate backstop unappealing for them. Unilateral investment does become more likely under: stringent carbon policy, social stage investment is inexpensive and could provide a hedge against such developments, particularly

Wisconsin at Madison, University of

394

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

E-Print Network [OSTI]

the period after 1997 are discussed, including the saving-investment approach, the intertemporal approach Classification Nos.: F32, F41 Keywords: Current account; net foreign assets; saving glut; investment drought States ran enormous current account deficits. China, the rest of East Asia, and the oil exporting

Wisconsin at Madison, University of

395

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

E-Print Network [OSTI]

problems that cross national boundaries and demand a multi-actor response. At the same time, traditional performance regimes work best. Instead, they must work in the context of a disarticulated state, with policy and the complexity of modern governance, identifying implications and questions for research and practice

Wisconsin at Madison, University of

396

SciTech Connect: Cosmic-ray physics with the milagro gamma-ray observatory  

Office of Scientific and Technical Information (OSTI)

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May Jun Jul(Summary)morphinan antagonist Journal Article:Biasi, A.long baseline neutrino experiment" Find + AdvancedsourcesName

397

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

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

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr MayAtmosphericNuclear Security Administration the Contributions andDataNational Libraryornl.gov RonStaffReturningNewNew

398

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

Office of Environmental Management (EM)

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May Jun Jul(Summary) "of Energy Power.pdf11-161-LNG | Department of Energy Freeport LNGEnergy

399

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

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

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr May JunDatastreamsmmcrcalgovInstrumentsrucLas Conchas recoveryLaboratory | NationalJohn CyberNeutrons usedDOENewNew exhibitAlternativestate

400

More about SOHO --SOHO (The Solar and Heliospheric Observatory) is a joint international space mission carried  

E-Print Network [OSTI]

the internal structure of the Sun, the heating of its extensive outer atmosphere, and the origin of the solar Flap Flap Flap Flap Fold Fold #12;B EAFD G Glue this to solar panel, Side A with black boxes lined up of communications dish and the "x" at bottom of blue solar panels. Extend it if inserting in something like a clay

Note: This page contains sample records for the topic "observatory nainital uttarkhand" 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

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

E-Print Network [OSTI]

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

Liske, Jochen

402

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

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

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

403

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

Open Energy Info (EERE)

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Office of InspectorConcentrating Solar Powerstories onFocus AreaDataBusPFAN)Change Assessment Model (GCAM) |

404

High-Resolution Spectroscopy with the Chandra X-ray Observatory  

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

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE:1 First Use of Energy for All Purposes (Fuel and Nonfuel),Feet) Year Jan Feb Mar Apr MayAtmospheric Optical Depth7-1D: Vegetation ProposedUsingFun withconfinement plasmas in thein theSurfactant-AssistedWater-

405

DOE Announces Notice of Intent for EGS Observatory | Department of Energy  

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

AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Delicious Rank EERE:Year in Review: Top FiveDepartmentfor06/2015) CIO, DCIO,Developmentof Energy

406

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

E-Print Network [OSTI]

Energy had won an award. In interpreting what follows, we note that the readership and/or market niche groups or questionnaires, we use a market-based empirical measure to indicate important issues conclusions here and provide additional details below. Figure 1 provides a visual summary of our findings

Wisconsin at Madison, University of

407

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

E-Print Network [OSTI]

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

Bautz, Marshall W.

408

The Environmental Data Acquisition System (EDAS) developed at the Royal Observatory of Belgium  

E-Print Network [OSTI]

conditions due to thermal waves were met. Similar equipment (EDAS) was also experimented on during the solar in this paper. The transducer's qualification is carried out in a laboratory where the admittance of various

Beauducel, Franois

409

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

E-Print Network [OSTI]

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

410

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

E-Print Network [OSTI]

-carbon energy technology Gregory F. Nemet La Follette School of Public Affairs and the Nelson Institute-commercial low-carbon energy technology Gregory F. Nemet1 and Erin Baker2 April 9, 2008 Abstract We combined subsidies. We modeled their effects on the future costs of a low-carbon energy technology

Wisconsin at Madison, University of

411

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

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

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

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

2011-06-17T23:59:59.000Z

412

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

E-Print Network [OSTI]

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

Burleigh, Matt

413

Nuclear Instruments and Methods in Physics Research A 518 (2004) 775798 CUORE: a cryogenic underground observatory for rare events  

E-Print Network [OSTI]

-67010 Assergi (L'Aquila), Italy f Laboratorio de Fisica Nuclear y Altas Energias, Universid"ad de of 130 Te (33.8% abundance), cold dark matter, solar axions, and rare nuclear decays. A preliminary

414

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

E-Print Network [OSTI]

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

415

Status of the Milagro Gamma Ray Observatory J.F. McCullough 1 for the Milagro Collaboration  

E-Print Network [OSTI]

monitoring the sky at TeV energies. Located in the mountains of northern New Mexico, Milagro will perform an all sky survey of the Northern Hemisphere at energies between #24; 250 GeV and 50 TeV. With a high), Milagro is uniquely capable of searching for transient and DC sources of high­energy ­ray emission

California at Santa Cruz, University of

416

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

E-Print Network [OSTI]

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

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

2007-08-04T23:59:59.000Z

417

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

SciTech Connect (OSTI)

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

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

2011-06-17T23:59:59.000Z

418

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

E-Print Network [OSTI]

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

Berns, Hans-Gerd

419

29th International Cosmic Ray Conference Pune (2005) 00, 101106 Performance of the Pierre Auger Observatory Surface Array  

E-Print Network [OSTI]

-alone solar panel system. With large ambient temperature variations, that can reach over 20 degrees in 24 via a custom built wireless communication system. Two solar panels charging two 12 V batteries provide is obtained by a GPS Motorola unit, and communication to the Central Data Acquisition System (CDAS) is done

420

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

E-Print Network [OSTI]

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

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


421

A Collaborative Portal for Ocean Observatories Michael A Godin*, James G Bellingham*, Kanna Rajan*, Naomi Leonard, Yi Chao  

E-Print Network [OSTI]

*, Naomi Leonard, Yi Chao *Monterey Bay Aquarium Research Institute (MBARI) 7700 Sandholdt Rd, Moss Landing

Leonard, Naomi

422

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

E-Print Network [OSTI]

of phenomena charac- terizing the solar transition region. Using simultaneously obtained SUMER obser- vations the wider frame-work of the upper solar atmosphere is still uncertain. These dynamic events were #12;rst counterparts to bi-directional jets were presented by Dere (1994), Moses & Cook (1994) and Teriaca, Madjarska

423

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

E-Print Network [OSTI]

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

Balser, Teri C.

424

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

425

NASA Marshall Space Flight Center (MSFC) -Automated Lunar and Meteor Observatory (ALaMO) -Candidate lunar impact observation database NASA Meteoroid Environment Office (MEO)  

E-Print Network [OSTI]

.4 Newtonian T 119 StellaCam EX Sony GV-D800 MSFC 4487 Suggs and Swift http://science.nasa.gov/headlines/y2005.4 Newtonian T 119 StellaCam EX Sony GV-D800 MSFC ALAMO Moser and McNamara http 19.1 25.4 Newtonian T 119 StellaCam EX Sony GV-D800 MSFC ALAMO Swift, Hollon, & Altstatt 105 21-Jun

Waliser, Duane E.

426

An Independent Measurement of the Total Active 8B Solar Neutrino Flux Using an Array of 3He Proportional Counters at the Sudbury Neutrino Observatory  

E-Print Network [OSTI]

current interactions in heavy water and precisely determinedNaCl to the ?1000 Mg of heavy water (D 2 O). This enhancedvated NaCl, into the heavy water in October 2005 and October

Aharmim,, B.; SNO Collaboration

2008-01-01T23:59:59.000Z

427

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

E-Print Network [OSTI]

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

Moline, Mark

428

NICMOS Imaging of Candidate ExtraSolar Planetary Systems Glenn Schneider (Steward Observatory, U. of Arizona) and the NICMOS IDT/EONS* Teams  

E-Print Network [OSTI]

of HD 98800 (7232). Here we present a sampling of results from our NICMOS coronagraphic imaging surveys

Schneider, Glenn

429

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

E-Print Network [OSTI]

over the Internet. We report on progress in the design and construction of a high resolution, large digitizing the catalog of plates, constructing an automatic pipeline to make the scanned images useful

430

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

E-Print Network [OSTI]

. Formerly called sewage sludge, they reflect the current best technology for the biological treatment. There are three methods for handling biosolids, which include land-filling, incineration, and land application considerations for the safe and effective recycling of biosolids by land application in Wisconsin. Rules

Balser, Teri C.

431

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

E-Print Network [OSTI]

des Géomatériaux, Université Marne-la-Vallée, France e Centro de Estudios Avanzados en Zonas Aridas

Guichard, Francoise

432

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

E-Print Network [OSTI]

The GONG++ DATA Processing Pipeline F. Hill,, J. Bolding, C. Toner, T. Corbard, S. Wampler, B pipeline is currently under construction. This system will produce the GONG++ science data products data, we have adopted an automated pipeline approach to the system. Here we describe the software

Corbard, Thierry

433

The Tenth Data Release of the Sloan Digital Sky Survey: First Spectroscopic Data from the SDSS-III Apache Point Observatory Galactic Evolution Experiment  

E-Print Network [OSTI]

,327 stellar spectra, selected over 6373.2 deg2. Keywords: AtlasesCatalogsSurveys 1. INTRODUCTION 1 Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA. 2 Center for Astrophysical Sciences, Department of Physics... and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA. 3 Instituto de Astrof?sica de Canarias (IAC), C/V?a Lactea, s/n, E-38200, La Laguna, Tenerife, Spain. 4 Departamento de Astrof?sica, Universidad de La Laguna, E...

Ahn, Christopher P.; Alexandroff, Rachael; Allende Prieto, Carlos; Anders, Friedrich; Anderson, Scott F.; Anderton, Timothy; Andrews, Brett H.; Aubourg, ric; Bailey, Stephen; Bastien, Fabienne A.; Bautista, Julian E.; Beers, Timothy C.; Beifiori, Alessandra; Bender, Chad F.; Berlind, Andreas A.; Beutler, Florian; Bhardwaj, Vaishali; Bird, Jonathan C.; Bizyaev, Dmitry; Blake, Cullen H.; Blanton, Michael R.; Blomqvist, Michael; Bochanski, John J.; Bolton, Adam S.; Borde, Arnaud; Bovy, Jo; Bradley, Alaina Shelden; Brandt, W. N.; Brauer, Dorothe; Brinkmann, J.; Brownstein, Joel R.; Busca, Nicols G.; Carithers, William; Carlberg, Joleen K.; Carnero, Aurelio R.; Carr, Michael A.; Chiappini, Cristina; Chojnowski, S. Drew; Chuang, Chia-Hsun; Comparat, Johan; Crepp, Justin R.; Cristiani, Stefano; Croft, Rupert A. C.; Cuesta, Antonio J.; Cunha, Katia; da Costa, Luiz N.; Dawson, Kyle S.; De Lee, Nathan; Dean, Janice D. R.; Delubac, Timothe; Deshpande, Rohit; Dhital, Saurav; Ealet, Anne; Ebelke, Garrett L.; Edmondson, Edward M.; Eisenstein, Daniel J.; Epstein, Courtney R.; Escoffier, Stephanie; Esposito, Massimiliano; Evans, Michael L.; Fabbian, D.; Fan, Xiaohui; Favole, Ginevra; Femena Castell, Bruno; Fernndez Alvar, Emma; Feuillet, Diane; Filiz Ak, Nurten; Finley, Hayley; Fleming, Scott W.; Font-Ribera, Andreu; Frinchaboy, Peter M.; Galbraith-Frew, J. G.; Garca-Hernndez, D. A.; Garca Prez, Ana E.; Ge, Jian; Gnova-Santos, R.; Gillespie, Bruce A.; Girardi, Lo; Gonzlez Hernndez, Jonay I.; Gott, J. RIchard III; Gunn, James E.; Guo, Hong; Halverson, Samuel; Harding, Paul; Harris, David W.; Hasselquist, Sten; Hawley, Suzanne L.; Hayden, Michael; Hearty, Frederick R.; Herrero Dav, Artemio; Ho, Shirley; Hogg, David W.; Holtzman, Jon A.; Honscheid, Klaus; Huehnerhoff, Joseph; Ivans, Inese I.; Jackson, Kelly M.; Jiang, Peng; Johnson, Jennifer A.; Kinemuchi, K.; Kirkby, David; Klaene, Mark A.; Kneib, Jean-Paul; Koesterke, Lars; Lan, Ting-Wen; Lang, Dustin; Le Goff, Jean-Marc; Leauthaud, Alexie; Lee, Khee-Gan; Lee, Young Sun; Long, Daniel C.; Loomis, Craig P.; Lucatello, Sara; Lupton, Robert H.; Ma, Bo; Mack, Claude E. III; Mahadevan, Suvrath; Maia, Marcio A. G.; Majewski, Steven R.; Malanushenko, Elena; Malanushenko, Viktor; Manchado, A.; Manera, Marc; Maraston, Claudia; Margala, Daniel; Martell, Sarah L.; Masters, Karen L.; McBride, Cameron K.; McGreer, Ian D.; McMahon, Richard G.; Mnard, Brice; Mszros, Sz.; Miralda-Escud, Jordi; Miyatake, Hironao; Montero-Dorta, Antonio D.; Montesano, Francesco; More, Surhud; Morrison, Heather L.; Muna, Demitri; Munn, Jeffrey A.; Myers, Adam D.; Nguyen, Duy Cuong; Nichol, Robert C.; Nidever, David L.; Noterdaeme, Pasquier; Nuza, Sebastin E.; O'Connell, Julia E.; O'Connell, Robert W.; O'Connell, Ross; Olmstead, Matthew D.; Oravetz, Daniel J.; Owen, Russell; Padmanabhan, Nikhil; Palanque-Delabrouille, Nathalie; Pan, Kaike; Parejko, John K.; Parihar, Prachi; Pris, Isabelle; Pepper, Joshua; Percival, Will J.; Prez-Rfols, Ignasi; Perottoni, Hlio Dotto; Petitjean, Patrick; Pieri, Matthew M.; Pinsonneault, M. H.; Prada, Francisco; Price-Whelan, Adrain M.; Raddick, M. Jordan; Rahman, Mubdi; Rebolo, Rafael; Reid, Beth A.; Richards, Jonathan C.; Riffel, Rogrio; Robin, Annie C.; Rocha-Pinto, H. J.; Rockosi, Constance M.; Roe, Natalie A.; Ross, Ashley J.; Ross, Nicholas P.; Rossi, Graziano; Roy, Arpita; Rubio-Martin, J. A.; Sabiu, Cristiano G.; Snchez, Ariel G.; Santiago, Baslio; Sayres, Conor; Schiavon, Ricardo P.; Schlegel, David J.; Schlesinger, Katharine J.; Schmidt, Sarah J.; Schneider, Donald P.; Schultheis, Mathias; Sellgren, Kris; Seo, Hee-Jong; Shen, Yue; Shetrone, Matthew; Shu, Yiping; Simmons, Audrey E.; Skrutskie, M. F.; Slosar, Ane; Smith, Verne V.; Snedden, Stephanie A.; Sobeck, Jennifer S.; Sobreira, Flavia; Stassun, Keivan G.; Steinmetz, Matthias; Strauss, Michael A.; Streblyanska, Alina; Suzuki, Nao; Swanson, Molly E. C.; Terrien, Ryan C.; Thakar, Aniruddha R.; Thomas, Daniel; Thompson, Benjamin A.; Tinker, Jeremy L.; Tojeiro, Rita; Troup, Nicholas W.; Vandenberg, Jan; Vargas Magaa, Mariana; Viel, Matteo; Vogt, Nicole P.; Wake, David A.; Weaver, Benjamin A.; Weinberg, David H.; Weiner, Benjamin J.; White, Martin; White, Simon D. M.; Wilson, John C.; Wisniewski, John P.; Wood-Vasey, W. M.; Yche, Christophe; York, Donald G.; Zamora, O.; Zasowski, Gail; Zehavi, Idit; Zhao, Gong-Bo; Zheng, Zheng; Zhu, Guangtun

2014-03-18T23:59:59.000Z

434

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

E-Print Network [OSTI]

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

Balser, Teri C.

435

X-ray Properties of Young Stellar Objects in OMC-2 and OMC-3 from the Chandra X-ray Observatory  

E-Print Network [OSTI]

We report X-ray results of the Chandra observation of Orion Molecular Cloud 2 and 3. A deep exposure of \\sim 100 ksec detects \\sim 400 X-ray sources in the field of view of the ACIS array, providing one of the largest X-ray catalogs in a star forming region. Coherent studies of the source detection, time variability, and energy spectra are performed. We classify the X-ray sources into class I, class II, and class III+MS based on the J, H, and K-band colors of their near infrared counterparts and discuss the X-ray properties (temperature, absorption, and time variability) along these evolutionary phases.

M. Tsujimoto; K. Koyama; Y. Tsuboi; M. Goto; N. Kobayashi

2001-10-12T23:59:59.000Z

436

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

E-Print Network [OSTI]

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

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

2010-01-01T23:59:59.000Z

437

Global and regional emissions of HFC-125 (CHF[subscript 2]CF[subscript 3]) from in situ and air archive atmospheric observations at AGAGE and SOGE observatories  

E-Print Network [OSTI]

High-frequency, in situ observations from the Advanced Global Atmospheric Gases Experiment (AGAGE) and System for Observation of halogenated Greenhouse gases in Europe (SOGE) networks for the period 1998 to 2008, combined ...

O'Doherty, S.

438

E-Print Network 3.0 - auger decay study Sample Search Results  

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

Sarkar 4.0 Auger South (Angela Source: Pierre Auger Observatory Collection: Physics 91 CERN Courier CERN COURIER Summary: -ray observatory bearing Auger's name is studying...

439

Curriculum vitae Amaya Moro-Martn  

E-Print Network [OSTI]

/05/2001 Research Experience for Undergraduates (REU) Intern Maria Mitchel Observatory (Nantucket, MA, USA) Start Perkins Scholarship, Maria Mitchell Observatory (REU), Nantucket, MA (USA). 1994 ISEP (International

Moro-Martin, Amaya

440

THE NEAR-INFRARED CAMERA AND MULTI-OBJECT SPECTROMETER ULTRA DEEP FIELD: OBSERVATIONS, DATA REDUCTION, AND GALAXY PHOTOMETRY  

E-Print Network [OSTI]

Stobie Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721 and Sune

Schneider, Glenn

Note: This page contains sample records for the topic "observatory nainital uttarkhand" 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

THE NEW GLOBAL HIGHRESOLUTION H NETWORK: FIRST OBSERVATIONS AND FIRST RESULTS M. Steinegger1  

E-Print Network [OSTI]

¨ohe Solar Observatory (KSO) in Aus- tria, and Yunnan Astronomical Observatory (YNAO) in China. 2. NETWORK , A. Hanslmeier3 , G. Luo4 , D. Chen4 , and Q. Zhang4 1 Big Bear Solar Observatory, NJIT, 40386 North Shore Lane, Big Bear City, CA 92314, U.S.A. 2 Kanzelh¨ohe Solar Observatory, A­9521 Treffen, Austria 3

442

Computer code for double beta decay QRPA based calculations  

E-Print Network [OSTI]

. The Enriched Xenon Observatory for neutrinoless double beta decay (EXO) will search for the rare decays

Bertulani, Carlos A. - Department of Physics and Astronomy, Texas A&M University

443

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]

for designing and building the spectrometer pre-optics sub-system, which includes a set of four image slicers a hexagonal primary mirror with a collecting area of 25 square metres, passively cooled to 40K and placed, ranging from the first luminous glows after the Big Bang, to the formation of solar systems capable

Tittley, Eric

444

The Journal of the European Association of Studies on Australia, Vol.3. No.2, 2012, ISSN 1988-5946 under the auspices of Coolabah Observatori: Centre d'Estudis  

E-Print Network [OSTI]

, Universitat de Barcelona 2 "Australia's Decision": Uranium Mining and Aboriginal Communities of direct economic rewards. A case in point is that of uranium mining which, well after the Second World War with uranium mining for peaceful purposes at Ranger (Northern Territory), and comparing it with the more recent

Paris-Sud XI, Université de

445

Solar Meridional Circulation from Doppler Shifts of the Fe I line at lambda 5250 Angstroms as Measured by the 150-foot Solar Tower Telescope at the Mt. Wilson Observatory  

E-Print Network [OSTI]

Doppler shifts of the Fe I spectral line at lambda5250 Angstroms from the full solar disk obtained over the period 1986 to 2009 are analyzed to determine the circulation velocity of the solar surface along meridional planes. Simultaneous measurements of the Zeeman splitting of this line are used to obtain measurements of the solar magnetic field that are used to select low field points and impose corrections for the magnetically induced Doppler shift. The data utilized is from a new reduction that preserves the full spatial resolution of the original observations so that the circulation flow can be followed to latitudes of 80 degrees N/S. The deduced meridional flow is shown to differ from the circulation velocities derived from magnetic pattern movements. A reversed circulation pattern is seen in polar regions for three successive solar minima. An surge in circulation velocity at low latitudes is seen during the rising phases of cycles 22 and 23.

Ulrich, Roger K

2010-01-01T23:59:59.000Z

446

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 (OSTI)

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

447

Imaging polarimetry of Comet C/2013 V1 (Boattini) and Comet 290P/Jager before and after perihelion  

E-Print Network [OSTI]

We report the results obtained from the optical polarimetric study of the light scattered by Comet C/2013 V1 (Boattini) and Comet 290P/Jager at lower phase angles. The polarimetric observations of two comets have been performed with the 1.04-metre Sampurnanand telescope of ARIES near Nainital in India on 4th \\& 5th of December, 2013 and on 24th April, 2014 using R photometric band ($\\lambda$ = 630 nm, $\\Delta$$\\lambda$ =120nm). We covered observations in both the pre and post perihelion passage of Comet C/2013 V1 (Boattini) and Comet 290P/Jager at two phase angles $\\sim$ 13$^\\circ$ and 27$^\\circ$. The degree of polarization changes from ($-1.4$$\\pm 0.3$)\\% to (+2.8$\\pm 0.5$)\\% for Comet C/2013 V1 (Boattini) and ($-1.6$$\\pm 0.5$)\\% to (+2.5$\\pm 0.5$)\\% for Comet 290P/Jager at phase angles $\\sim$ 13$^\\circ$ and 27$^\\circ$ respectively. The change in the physical properties of cometary dust is being well studied from the polarization maps obtained for both the period of observations. It is found that the ape...

Roy, P Deb; Das, H S; Medhi, B J

2015-01-01T23:59:59.000Z

448

A ring system detected around the minor planet (10199) F. Braga-Ribas1  

E-Print Network [OSTI]

, Montevideo, Uruguay. 20. Dpto. Astronomia, Facultad Ciencias, Uruguay. 21. Observatorio El Catalejo, Santa´on, Uruguay. 25. National Astronomical Observatories/Yunnan Observatory. 26. Key Laboratory for the Structure

Demoulin, Pascal

449

Planar feasibility study for primary mirror control of large imaging space systems using binary actuators  

E-Print Network [OSTI]

The greatest discoveries in astronomy have come with advancements in ground-based observatories and space telescopes. Latest trends in ground-based observatories have been ever increasing size of the primary mirror, providing ...

Lee, Seung Jae, S.M. Massachusetts Institute of Technology

2010-01-01T23:59:59.000Z

450

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.

451

E-Print Network 3.0 - anhydrobiotic tardigrade milnesium Sample...  

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

of - Alpine Microbial Observatory Collection: Environmental Sciences and Ecology 6 BIOL 332: Invertebrate Zoology PANARTHROPODA Summary: in freshwater ecosystem: tardigrades...

452

PROCEEDINGS OF 1976 SUMMER WORKSHOP ON AN ENERGY EXTENSION SERVICE  

E-Print Network [OSTI]

energy audits of individual homes, as has the Urban Observatory in San Diego. A number of colleges and universities,

Authors, Various

2010-01-01T23:59:59.000Z

455

THE NEW GLOBAL HIGHRESOLUTION H NETWORK: PRELIMINARY RESULTS ON THE CHROMOSPHERIC DIFFERENTIAL ROTATION  

E-Print Network [OSTI]

, H. Freislich2 , A. Hanslmeier3 , G. Luo4 , D. Chen4 , and Q. Zhang4 1 Big Bear Solar Observatory, NJIT, 40386 North Shore Lane, Big Bear City, CA 92314, U. S. A. 2 Kanzelh¨ohe Solar Observatory, A­9521 Graz, Austria 4 Yunnan Astronomical Observatory, P. O. Box 110, Kunming 650011, P. R. China ABSTRACT

456

De Bilt, 2011 | Scientific report; WR 2011-01 Parallel air temperature measurements  

E-Print Network [OSTI]

at the KNMI observatory in De Bilt (the Netherlands) May 2003 - June 2005 | March 14, 2011 Page 6 of 56 #12 observatory in De Bilt (the Netherlands) May 2003 - June 2005 Theo Brandsma #12;#12;Parallel air temperature measurements at the KNMI observatory in De Bilt (the Netherlands) May 2003 - June 2005 Version 1.0 Date March

Haak, Hein

457

E-Print Network 3.0 - absorbents Sample Search Results  

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

Astronomy Observatory Collection: Physics 13 Potential for High Efficiency in CIGS Thin Film Solar Cells: A Laboratory Perspective Summary: a summary of our work with the...

458

E-Print Network 3.0 - absorbance Sample Search Results  

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

Astronomy Observatory Collection: Physics 13 Potential for High Efficiency in CIGS Thin Film Solar Cells: A Laboratory Perspective Summary: a summary of our work with the...

459

Geothermal Technologies Office Director Doug Hollett Keynotes...  

Energy Savers [EERE]

portfolio for the coming years - the Frontier Observatory for Research in Geothermal Energy (FORGE). Click below for the full presentation. To see a listing of all GTO...

460

E-Print Network 3.0 - automatic exposure control Sample Search...  

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

Laboratory, Data Quality Objectives Program, Visual Sample Plan Collection: Environmental Management and Restoration Technologies 46 Operating the Serin Observatory Direct CCD...

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


461

auf dem boden: Topics by E-print Network  

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

by spicules. We use spectral data from the Solar Ultraviolet Measurements of Emitted Radiation (SUMER) spectrometer on-board the Solar Heliospheric Observatory (SoHO) covering the...

462

auf dem weg: Topics by E-print Network  

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

by spicules. We use spectral data from the Solar Ultraviolet Measurements of Emitted Radiation (SUMER) spectrometer on-board the Solar Heliospheric Observatory (SoHO) covering the...

463

auf dem gitter: Topics by E-print Network  

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

by spicules. We use spectral data from the Solar Ultraviolet Measurements of Emitted Radiation (SUMER) spectrometer on-board the Solar Heliospheric Observatory (SoHO) covering the...

464

auf dem gebiet: Topics by E-print Network  

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

by spicules. We use spectral data from the Solar Ultraviolet Measurements of Emitted Radiation (SUMER) spectrometer on-board the Solar Heliospheric Observatory (SoHO) covering the...

465

abfallbehandlungszentrum auf dem: Topics by E-print Network  

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

by spicules. We use spectral data from the Solar Ultraviolet Measurements of Emitted Radiation (SUMER) spectrometer on-board the Solar Heliospheric Observatory (SoHO) covering the...

466

auf dem pruefstand: Topics by E-print Network  

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

by spicules. We use spectral data from the Solar Ultraviolet Measurements of Emitted Radiation (SUMER) spectrometer on-board the Solar Heliospheric Observatory (SoHO) covering the...

467

auf dem bergwerk: Topics by E-print Network  

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

by spicules. We use spectral data from the Solar Ultraviolet Measurements of Emitted Radiation (SUMER) spectrometer on-board the Solar Heliospheric Observatory (SoHO) covering the...

468

auf dem wege: Topics by E-print Network  

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

by spicules. We use spectral data from the Solar Ultraviolet Measurements of Emitted Radiation (SUMER) spectrometer on-board the Solar Heliospheric Observatory (SoHO) covering the...

469

auf dem gelaende: Topics by E-print Network  

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

by spicules. We use spectral data from the Solar Ultraviolet Measurements of Emitted Radiation (SUMER) spectrometer on-board the Solar Heliospheric Observatory (SoHO) covering the...

470

E-Print Network 3.0 - automated natural language Sample Search...  

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

of Language Communities and its Implication for Language-specific Crawling Rizza... Camus Caminero Language Observatory Nagaoka University of Technology Nagaoka, Niigata, Japan...

471

NOAA AND ENERGY NOAA's involvement with the energy sector is wide-ranging. NOAA has an interest or is actively engaged in  

E-Print Network [OSTI]

power; biomass and biofuel. NOAA provides data, scientific research, technical products, management, ocean buoys, ships and aircraft, and seafloor observatories. NOAA can help advance the renewable energy

472

NETL F 451.1/1-1, Categorical Exclusion Designation Form  

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

Lamont-Doherty Earth Observatory SCNGO FY14-17 1012013 - 09302017 John Terneus Palisades, NY Mechanisms for Methane Transport and Hydrate Accumulation in Coarse-Grained...

473

E-Print Network 3.0 - africa optimum scale Sample Search Results  

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

>> 1 For more information contact: Dr. Andrew Nyblade Summary: of geologic time and many spatial scales using data from the AfricaArray scientific observatories, plus......

474

E-Print Network 3.0 - analog sum trigger Sample Search Results  

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

for the ... Source: Pierre Auger Observatory Collection: Physics 7 An Approach to Active Spatial Data Mining Based on Statistical Information Summary: that extends the current...

475

E-Print Network 3.0 - active galaxy unification Sample Search...  

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

than, e.g., low Source: Lick Observatory, University of California at Santa Cruz, DEEP Project Collection: Physics 63 The Astrophysical Journal, 714:17791788, 2010 May 10...

476

E-Print Network 3.0 - all-wavelength extended groth Sample Search...  

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

allows ... Source: Lick Observatory, University of California at Santa Cruz, DEEP Project Collection: Physics 6 Bibliography of Marc Davis Marc Davis, R. Ruffini, William H....

477

E-Print Network 3.0 - anchored flux tubes Sample Search Results  

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

Solar Physics, held from Dec. 1022, 2006 at Kodaikanal Solar Observatory, India, S.S. Hasan and D. Banerjee (eds.), 2007 American Institute of Summary: . 919 Photospheric...

478

E-Print Network 3.0 - ain jrvalt tiina Sample Search Results  

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

94 Pierre Auger Observatory Bi-monthly Report Summary: 2008. WBS 2.2 Surface Detector Electronics (Tiina Suomijarvi - IPN Orsay) Maintenance Photonis has Source: Pierre Auger...

479

E-Print Network 3.0 - adaptive optical systems Sample Search...  

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

- European Southern Observatory Collection: Physics 22 CONCEPTS FOR TEACHING OPTOELECTRONIC CIRCUITS AND SYSTEMS Summary: .Lastname@esisar.inpg.fr Keywords : Optoelectronic...

480

E-Print Network 3.0 - alcohol fuels provisions Sample Search...  

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

CA, USA,3 Alcohol and Drug Research, National Institute for Health and Welfare, Helsinki, Finland Source: Stockholm Observatory Collection: Physics 75 DistributorProducer...

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


481

E-Print Network 3.0 - ain kallis viivi Sample Search Results  

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

Germany Ain Kull, University... Ruosteenoja, Finnish Meteorological Institute, Helsinki, Finland Viivi Russak, Tartu Observatory, Estonia Ralf Source: von Storch, Hans - Institute...

482

NP Scientific User Facilities | U.S. DOE Office of Science (SC...  

Office of Science (SC) Website

Sudbury Neutrino Observatory in Canada, the KATRIN direct neutrino mass measurement in Germany, and the Majorana project searching for double beta decay at Pacific Northwest...

483

Intersections: SOURCE Symposium & Poster Session 2008 Winners  

E-Print Network [OSTI]

Aureoles." Mentor: Professor Mark Bulmer, Department of Geophysical Flow Observatory Honorable Mention (tie): Carolyn Richmonds: "A Combined Plasma-Electrochemical Method to Produce Colloidal Metal

Rollins, Andrew M.

484

E-Print Network 3.0 - abundance ratio determinations Sample Search...  

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

Dworetsky, Mike - University of London Observatory & Department of Physics and Astronomy, University College London Collection: Physics 2 Towards a coronal unification with...

485

E-Print Network 3.0 - astrophysics asymptotic normalization Sample...  

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

Bubbles 3 Source: Bicknell, Geoff - Mt. Stromlo Observatory & Research School of Astronomy and Astrophysics, Australian National University Collection: Physics 2 High Energy...

486

E-Print Network 3.0 - apparent vlba jet Sample Search Results  

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

Flare in September 2001 Summary: , Michael P. Rupen & Vivek Dhawan National Radio Astronomy Observatory VLBA images of Cygnus X-3 from... after a February 1997 flare show a...

487

E-Print Network 3.0 - antennae galaxies ngc Sample Search Results  

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

Physics 2 John E. Hibbard National Radio Summary: John E. Hibbard National Radio Astronomy Observatory The Antennae Galaxies: Archetype for Colliding... Galaxies 12;The...

488

E-Print Network 3.0 - ancient star forming Sample Search Results  

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

relatively young stars formed from ... Source: Sjouwerman, Lornt - National Radio Astronomy Observatory Collection: Physics 2 The Evening Sky in June 2011 Sirius, the brightest...

489

E-Print Network 3.0 - absorbing galaxies mrk Sample Search Results  

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

Mrk 817... , but also, for the first time, ... Source: Hibbard, John - National Radio Astronomy Observatory Collection: Physics 2 www.mpifrbonn.mpg.de August 2000 Cont peak flux...

490

auger electron-emitting estrogens: Topics by E-print Network  

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

and results Astrophysics (arXiv) Summary: The Pierre Auger Observatory, a hybrid detector for the study of ultra-high energy cosmic rays (UHECRs), is now approaching...

491

E-Print Network 3.0 - assessing meiofaunal variation Sample Search...  

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

C, Heller L, Peak KK, Wingfield, DOn "Assessment of the Utility of Automated Source: Colorado at Boulder, University of - Alpine Microbial Observatory Collection:...

492

E-Print Network 3.0 - animal mediante pcr Sample Search Results  

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

task. In recent years, quantitative PCR (qPCR, also referred to as real-time ... Source: Colorado at Boulder, University of - Alpine Microbial Observatory; Jackson, Robert B. -...

493

E-Print Network 3.0 - argentina secado solar Sample Search Results  

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

Argentina's Mendoza Province, near the town of Malarge, the observatory... with photo sensors and sprouting solar panels and communications antennae, these Auger particle...

494

Improving the detectability of gravitational wave counterparts of short hard gamma ray bursts .  

E-Print Network [OSTI]

??With multiple observatories and missions being planned for detecting orphaned afterglows associated with gamma-ray bursts (GRBs) we emphasize the importance of developing data analysis strategies (more)

[No author

2013-01-01T23:59:59.000Z

495

E-Print Network 3.0 - austrian research center Sample Search...  

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

Universitt Wien Collection: Physics ; Materials Science 2 Manuela TEMMER Curriculum Vitae Kanzelhhe ObservatoryIGAM, Institute of Physics, University of Graz Summary:...

496

E-Print Network 3.0 - austrian physical society Sample Search...  

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

results for: austrian physical society Page: << < 1 2 3 4 5 > >> 1 Manuela TEMMER Curriculum Vitae Kanzelhhe ObservatoryIGAM, Institute of Physics, University of Graz Summary:...

497

Code for Largest Cosmological Simulations Ever on GPUs Is Gordon...  

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

Advancements to instruments in observatories and satellites can stretch the eye of the observer billions of light-years away to the fringes of the observable universe....

498

auger emitter sb-119: Topics by E-print Network  

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

Pierre Auger Observatory (PAO), currently under construction in Province of Mendoza, Argentina, and with another site planned in the Northern hemisphere, is a major international...

499

anamalous npp auger: Topics by E-print Network  

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

Pierre Auger Observatory (PAO), currently under construction in Province of Mendoza, Argentina, and with another site planned in the Northern hemisphere, is a major international...

500

auger snails terebridae: Topics by E-print Network  

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

Pierre Auger Observatory (PAO), currently under construction in Province of Mendoza, Argentina, and with another site planned in the Northern hemisphere, is a major international...