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We encourage you to perform a real-time search of NLEBeta
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1

Charles Knuffke  

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

Knuffke Knuffke WattStopper Charles.Knuffke@wattstopper.com This speaker was a visiting speaker who delivered a talk or talks on the date(s) shown at the links below. This speaker is not otherwise associated with Lawrence Berkeley National Laboratory, unless specifically identified as a Berkeley Lab staff member. Charles Knuffke had his first brush with Lighting Controls in 1983 when he was given the task of programming one of the earliest centralized Lighting Control systems during a co-op at GE, Schenectady. He's been involved with Lighting Controls ever since. For the past 21 years, Charles has worked with engineers, contractors and owners to design, specify, and commission Lighting Control Systems for wide-ranging projects. These systems have run the gamut from standalone relay panels with a timeclock to

2

Charles Rousseaux | Department of Energy  

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

Charles Rousseaux Charles Rousseaux About Us Charles Rousseaux - Senior Writer, Office of Science Charles Rousseaux A scientist by training and a blogger by accident, Charles Rousseaux writes about the discoveries and innovations of the Department of Energy's Office of Science. Before joining the Energy Department in October of 2010, Charles served as a speechwriter for several senior governmental officials, and also worked as an editorial writer for The Washington Times. A student of science and politics, and an ardent advocate of American exceptionalism, Charles spends his free time reading, taking even more graduate classes (groan!), and persevering through ultramarathons. Most Recent Energetic Science and Piranha-Proof Armor December 16 Complementary Chemistry and Matched Materials

3

The Message CHARLES J. KREBS  

E-Print Network [OSTI]

#12;The Message Q[Ecology CHARLES J. KREBS University of British Columbia 1817 L.IADDCD Jt. DnW;the first draft of this book. Alice Kenney helped me survey the literature and prepare the text. Many

Krebs, Charles J.

4

Charles Worthington | Department of Energy  

Energy Savers [EERE]

Data Initiatives at the Department of Energy. Previously, he founded Gray Duck Labs, a webmobile product design firm. In his spare time, Charles works on Preamp.fm, a live music...

5

Charles McConnell | Department of Energy  

Office of Environmental Management (EM)

for Fossil Energy Charles McConnell Charles McConnell is the former Assistant Secretary for Fossil Energy. Most Recent Adding "Utilization" to Carbon Capture and Storage May 1...

6

Lake Charles Urbanized Area MTP 2034  

E-Print Network [OSTI]

................................................................................................................................ 2-9 National Highway System ........................................................................................................................... 2-10 City of Lake Charles Transit System Routes... transportation. The Lake Charles Urbanized Area is located wholly within Calcasieu Parish and includes the cities of Lake Charles, Sulphur, and Westlake, as well as the unincorporated areas known as Moss Bluff, and Carlyss (see map on following page...

Lake Charles Urbanized Area Metropolitan Planning Organization

2009-08-04T23:59:59.000Z

7

Dave Kaminsky Charles L. Black  

E-Print Network [OSTI]

Edwin D. McKay Thomas L. McNeely Jean C. Persons Neysa P. Pickens Armant C. Touchy Jack S. Zoller 19511935 $50.00 Dave Kaminsky 1938 $200.00 Charles L. Black 1940 $50.00 Harold S. Miropol 1941 $67. Tennison Ben Thompson 1945 $250.00 Paul Finkelstein Harold J. Jacobs Lawrence Kahn 1946 $2,250.00 David W

8

Saint Charles International | Open Energy Information  

Open Energy Info (EERE)

France Product: A European fruit and vegetable distribution, transportation and logistics platform References: Saint Charles International1 This article is a stub. You can...

9

Lake Charles, LA Natural Gas LNG Imports from Equatorial Guinea...  

Gasoline and Diesel Fuel Update (EIA)

Lake Charles, LA Natural Gas LNG Imports from Equatorial Guinea (Dollars per Thousand Cubic Feet) Lake Charles, LA Natural Gas LNG Imports from Equatorial Guinea (Dollars per...

10

The Lake Charles CCS Project  

SciTech Connect (OSTI)

The Lake Charles CCS Project is a large-scale industrial carbon capture and sequestration (CCS) project which will demonstrate advanced technologies that capture and sequester carbon dioxide (CO{sub 2}) emissions from industrial sources into underground formations. Specifically the Lake Charles CCS Project will accelerate commercialization of large-scale CO{sub 2} storage from industrial sources by leveraging synergy between a proposed petroleum coke to chemicals plant (the LCC Gasification Project) and the largest integrated anthropogenic CO{sub 2} capture, transport, and monitored sequestration program in the U.S. Gulf Coast Region. The Lake Charles CCS Project will promote the expansion of EOR in Texas and Louisiana and supply greater energy security by expanding domestic energy supplies. The capture, compression, pipeline, injection, and monitoring infrastructure will continue to sequester CO{sub 2} for many years after the completion of the term of the DOE agreement. The objectives of this project are expected to be fulfilled by working through two distinct phases. The overall objective of Phase 1 was to develop a fully definitive project basis for a competitive Renewal Application process to proceed into Phase 2 - Design, Construction and Operations. Phase 1 includes the studies attached hereto that will establish: the engineering design basis for the capture, compression and transportation of CO{sub 2} from the LCC Gasification Project, and the criteria and specifications for a monitoring, verification and accounting (MVA) plan at the Hastings oil field in Texas. The overall objective of Phase 2, provided a successful competitive down-selection, is to execute design, construction and operations of three capital projects: (1) the CO{sub 2} capture and compression equipment, (2) a Connector Pipeline from the LLC Gasification Project to the Green Pipeline owned by Denbury and an affiliate of Denbury, and (3) a comprehensive MVA system at the Hastings oil field.

Doug Cathro

2010-06-30T23:59:59.000Z

11

Mon. Not. R. Astron. Soc. 317, 535544 (2000) New challenges for adaptive optics: extremely large telescopes  

E-Print Network [OSTI]

, Karl Schwarzschild Str. 2, D-85748 Garching, Germany 2 CRAL, Observatoire de Lyon, 9, Av. Charles Andre sources and up to three deformable mirrors, which increase up to 8-fold the corrected field size (up to 60 NTRO DUC TION The current generation of large ground-based optical telescopes has primary mirrors

Tokovinin, Andrei A.

12

Charles University Prague Faculty of Mathematics and Physics  

E-Print Network [OSTI]

Charles University Prague Faculty of Mathematics and Physics an abstract of the thesis submittedD. Department of Geophysics Faculty of Mathematics and Physics Charles University Prague V Holesovick´ach 2 180

Cerveny, Vlastislav

13

hello, poindexter! THE (UN)REMARKABLE DR. CHARLES LIU  

E-Print Network [OSTI]

hello, poindexter! THE (UN)REMARKABLE DR. CHARLES LIU October 8, 2008 at 12:35 pm · Filed under talk about whatever he thought hello, poindexter! » THE (UN)REMARKABLE DR. CHARLE... http

Liu, Charles

14

Charles L Neumeyer | Princeton Plasma Physics Lab  

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

Charles L Neumeyer Charles L Neumeyer ITER Steady State Electrical Systems WBS Manager, NSTX Project Engineer Charles Neumeyer Jr. is a registered professional engineer with more than 30 years experience in advanced technology research and project management. His experience covers functions ranging from design to procurement and conditioning. Neumeyer has managerial roles in activities associated with ITER and the National Spherical Torus Experiment Upgrade (NSTX-U). He is responsible for U.S. equipment contributions for the ITER Steady State Electrical Network, which will supply AC power to all ITER plant systems. As systems engineer for the NSTX-U, he is responsible for systems integration of the upgrade project. Interests Electromagnetic and high voltage engineering AC/DC power conditioning systems

15

Charles Townes, the Maser, and the Laser  

Office of Scientific and Technical Information (OSTI)

Charles Townes - the Maser and the Laser Resources with Additional Information · Awards and Honors Charles Townes Photo Courtesy of Lawrence Berkeley National Laboratory Charles Hard Townes was educated at Furman University (B.A. in Modern Languages and B.S. in Physics in 1935), at Duke University (M.A. in Physics in 1937), and at the California Institute of Technology (Ph.D. in Physics in 1939). ' Townes was a member of the technical staff of the Bell Telephone Laboratories from 1939 to 1947. He worked extensively during World War II on the design of radar bombing systems. From this he turned to the field of the microwave spectroscope which he foresaw both as a powerful new tool for the study of the structure of atoms and molecules and as a potential new basis for controlling electromagnetic waves. ...

16

The Severe Gout of Emperor Charles V  

Science Journals Connector (OSTI)

The Severe Gout of Emperor Charles V Correspondence, N Engl J Med 2006:355;1935-1936. In the authors' reply, Jaume Ordi, M.D. of the Hospital Clnic d'Investigacions Biomdiques August Pi i Sunyer, 08036 Barcelona, Spain, should have been included as an author. We regret the error. The Severe Gout of Emperor Charles V Correspondence, N Engl J Med 2006:355;1935-1936.. In the authors' reply, Jaume Ordi, M.D., of the Hospital Clnic d'Investigacions Biomdiques August Pi i Sunyer, 08036 Barcelona, Spain, should have been included as an ...

2006-12-21T23:59:59.000Z

17

The Severe Gout of Emperor Charles V  

Science Journals Connector (OSTI)

...Holy Roman Emperor Charles V suffered from what physicians had long suspected was severe tophaceous gout. Lead poisoning may also have contributed to the decline and fall of this emperor. Saturnine gout results from exposure to lead through the addition of lead sugar (acetate) to wine to sweeten it and... To the Editor: Ordi et al. (Aug. 3 issue)1 confirm that the Holy Roman Emperor Charles V suffered from what physicians had long suspected was severe tophaceous gout.2 Lead poisoning may also have contributed to the decline and fall of this emperor.3 ...

2006-11-02T23:59:59.000Z

18

The Cherenkov Telescope Array Large Size Telescope  

E-Print Network [OSTI]

The two arrays of the Very High Energy gamma-ray observatory Cherenkov Telescope Array (CTA) will include four Large Size Telescopes (LSTs) each with a 23 m diameter dish and 28 m focal distance. These telescopes will enable CTA to achieve a low-energy threshold of 20 GeV, which is critical for important studies in astrophysics, astroparticle physics and cosmology. This work presents the key specifications and performance of the current LST design in the light of the CTA scientific objectives.

Ambrosi, G; Baba, H; Bamba, A; Barcel, M; de Almeida, U Barres; Barrio, J A; Bigas, O Blanch; Boix, J; Brunetti, L; Carmona, E; Chabanne, E; Chikawa, M; Colin, P; Conteras, J L; Cortina, J; Dazzi, F; Deangelis, A; Deleglise, G; Delgado, C; Daz, C; Dubois, F; Fiasson, A; Fink, D; Fouque, N; Freixas, L; Fruck, C; Gadola, A; Garca, R; Gascon, D; Geffroy, N; Giglietto, N; Giordano, F; Graena, F; Gunji, S; Hagiwara, R; Hamer, N; Hanabata, Y; Hassan, T; Hatanaka, K; Haubold, T; Hayashida, M; Hermel, R; Herranz, D; Hirotani, K; Inoue, S; Inoue, Y; Ioka, K; Jablonski, C; Kagaya, M; Katagiri, H; Kishimoto, T; Kodani, K; Kohri, K; Konno, Y; Koyama, S; Kubo, H; Kushida, J; Lamanna, G; Flour, T Le; Lpez-Moya, M; Lpez, R; Lorenz, E; Majumdar, P; Manalaysay, A; Mariotti, M; Martnez, G; Martnez, M; Mazin, D; Miranda, J M; Mirzoyan, R; Monteiro, I; Moralejo, A; Murase, K; Nagataki, S; Nakajima, D; Nakamori, T; Nishijima, K; Noda, K; Nozato, A; Ohira, Y; Ohishi, M; Ohoka, H; Okumura, A; Orito, R; Panazol, J L; Paneque, D; Paoletti, R; Paredes, J M; Pauletta, G; Podkladkin, S; Prast, J; Rando, R; Reimann, O; Rib, M; Rosier-Lees, S; Saito, K; Saito, T; Saito, Y; Sakaki, N; Sakonaka, R; Sanuy, A; Sasaki, H; Sawada, M; Scalzotto, V; Schultz, S; Schweizer, T; Shibata, T; Shu, S; Sieiro, J; Stamatescu, V; Steiner, S; Straumann, U; Sugawara, R; Tajima, H; Takami, H; Tanaka, S; Tanaka, M; Tejedor, L A; Terada, Y; Teshima, M; Totani, T; Ueno, H; Umehara, K; Vollhardt, A; Wagner, R; Wetteskind, H; Yamamoto, T; Yamazaki, R; Yoshida, A; Yoshida, T; Yoshikoshi, T

2013-01-01T23:59:59.000Z

19

CHARLES STURT UNIVERSITY POSTGRADUATE DIPLOMA OF PSYCHOLOGY  

E-Print Network [OSTI]

CHARLES STURT UNIVERSITY POSTGRADUATE DIPLOMA OF PSYCHOLOGY Additional information to supplement criteria Applicants: should hold a degree which includes a three-year major in psychology accredited by the Australian Psychology Accreditation Council (APAC) completed within the last ten years must have completed

Thomas, Richard C.

20

CURRICULUM VITAE Name: John Charles Priscu  

E-Print Network [OSTI]

and Oceanography winter meeting, Salt Lake City. February 2003. Participant and discussion leader, National ScienceCURRICULUM VITAE Name: John Charles Priscu Birthdate: September 20, 1952 Citizenship: U-present. Chair, SCAR-SALE (Subglacial Antarctic Lake Environments) International Scientific Planning Group

Lawrence, Rick L.

Note: This page contains sample records for the topic "telescope baltay charles" 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

John Charles Grant Ledingham. 1875-1944  

Science Journals Connector (OSTI)

1 February 1947 research-article John Charles Grant Ledingham. 1875-1944 S. P. Bedson The Royal Society is collaborating with JSTOR to digitize, preserve, and extend access to Obituary Notices of Fellows of the Royal Society. www.jstor.org

1947-01-01T23:59:59.000Z

22

HISTORY OF HOMOLOGICAL ALGEBRA Charles A. Weibel  

E-Print Network [OSTI]

) and Betti (1871) on "homology numbers," and the rigorous development of the notion of homology numbers;2 CHARLES A. WEIBEL Betti numbers, Torsion Coefficients and the rise of Homology Homological algebra in the 19th century largely consisted of a gradual effor* *t to define the "Betti numbers

23

HISTORY OF HOMOLOGICAL ALGEBRA Charles A. Weibel  

E-Print Network [OSTI]

century, via the work of Riemann (1857) and Betti (1871) on ``homology numbers,'' and the rigorous CHARLES A. WEIBEL Betti numbers, Torsion Coefficients and the rise of Homology Homological algebra in the 19th century largely consisted of a gradual e#ort to define the ``Betti numbers'' of a (piecewise

24

EIS-0491: Lake Charles Liquefaction Project, Calcasieu Parish, Louisiana |  

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

91: Lake Charles Liquefaction Project, Calcasieu Parish, 91: Lake Charles Liquefaction Project, Calcasieu Parish, Louisiana EIS-0491: Lake Charles Liquefaction Project, Calcasieu Parish, Louisiana SUMMARY The Federal Energy Regulatory Commission (FERC) is preparing, with DOE as a cooperating agency, an EIS to analyze the potential environmental impacts of a proposal to expand an existing liquefied natural gas (LNG) import terminal in Calcasieu Parish, Louisiana, by constructing and operating natural gas liquefaction and exportation capabilities. PUBLIC COMMENT OPPORTUNITIES None available at this time. DOCUMENTS AVAILABLE FOR DOWNLOAD March 28, 2013 EIS-0491: Supplemental Notice of Intent to Prepare an Environmental Impact Statement Lake Charles Liquefaction Project, Calcasieu Parish, Louisiana September 25, 2012

25

The City of Lake Charles Bicycle and Pedestrian Master Plan.  

E-Print Network [OSTI]

?? This thesis was done in the professional project format. It was completed as a deliverable to the City of Lake Charles, Louisiana. It was (more)

Adams, Anthony

2011-01-01T23:59:59.000Z

26

Price of Lake Charles, LA Liquefied Natural Gas Total Imports...  

Gasoline and Diesel Fuel Update (EIA)

Liquefied Natural Gas Total Imports (Dollars per Thousand Cubic Feet) Price of Lake Charles, LA Liquefied Natural Gas Total Imports (Dollars per Thousand Cubic Feet) Decade Year-0...

27

LECTURE NOTES (WEEK 9), MATH 526 (SPRING 2011) CHARLES REZK  

E-Print Network [OSTI]

] = s (UVU ), [U, U - p] = s (UV ), [M, M - p] . Date: March 17, 2011. 1 #12;2 CHARLES REZK Proposition 1

Rezk, Charles

28

Dynamic View Dependent Isosurface Extraction Yarden Livnat, Charles Hansen  

E-Print Network [OSTI]

-004 Scientific Computing and Imaging Institute University of Utah Salt Lake City, UT 84112 USA Enter date here1 Dynamic View Dependent Isosurface Extraction Yarden Livnat, Charles Hansen UUSCI-2003 Extraction Yarden Livnat Charles Hansen Scientific Computing and Imaging Institute School of Computing

Livnat, Yarden

29

Alignment telescope for Antares  

SciTech Connect (OSTI)

The Antares Automatic Alignment System employs a specially designed telescope for alignment of its laser beamlines. There are two telescopes in the system, and since each telescope is a primary alignment reference, stringent boresight accuracy and stability over the focus range were required. Optical and mechanical designs, which meet this requirement as well as that of image quality over a wide wavelength band, are described. Special test techniques for initial assembly and alignment of the telescope are also presented. The telescope, which has a 180-mm aperture FK51-KZF2 type glass doublet objective, requires a boresight accuracy of 2.8 ..mu..rad at two focal lengths, and object distances between 11 meters and infinity. Travel of a smaller secondary doublet provides focus from 11 m to infinity with approximately 7.8 m effective focal length. By flipping in a third doublet, the effective focal length is reduced to 2.5 m. Telescope alignment was accomplished by using a rotary air bearing to establish an axis in front of the system and placing the focus of a Laser Unequal Path Interferometer (LUPI) at the image plane.

Appert, Q.D.; Swann, T.A.; Ward, J.H.; Hardesty, C.; Wright, L.

1983-01-01T23:59:59.000Z

30

Giant Molecules: Essential Materials for Everyday Living and Problem Solving (Seymour, Raymond B.; Caraher, Charles E.)  

Science Journals Connector (OSTI)

Giant Molecules: Essential Materials for Everyday Living and Problem Solving (Seymour, Raymond B.; Caraher, Charles E.) ...

George B. Kauffman

1990-01-01T23:59:59.000Z

31

SNAP 2008 Collaboration  

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

Attendees Name Affiliation Agarwal, Deb LBNL Arnouts, Stephane Canada France Hawaii Telescope Baltay, Charles Yale Univ Baptista, Brian Indiana Univ Bartlett, James G. APC - Universite Paris Diderot Bebek, Chris LBNL Bernstein, Gary Univ of Pennsylvania Besuner, Robert LBNL Biesiadzinski, Tomasz Univ of Michigan Bly, Vince NASA/GSFC Boehm, Nick GSFC/SGT Bohlin, Ralph C. STScI Bonfield, David GSFC/ORAU Bonissent, Alain CPPM Boucarut, Ray NASA/GSFC Bower, Chuck Indiana Univ Cahn, Robert LBNL Carithers, William Lawrence Berkeley Lab Castera, Alain CNRS Cerna, Cedric CPPM / CNRS Chiao, Meng GSFC/MUNIZ Chow, Ken LBNL Cominsky, Lynn Sonoma State Univ Connolly, Brian Univ of Pennsylvania Correll, Randall Ball Aerospace Counil, Jean-Louis CNES Craig, William UC Berkeley

32

Professor Akhlesh Lakhtakia The Charles G. Binder (Endowed) Professor  

E-Print Network [OSTI]

in Electrical Engineering from the University of Utah, Salt Lake City in 1981 and 1983. Thereafter, he joinedProfessor Akhlesh Lakhtakia The Charles G. Binder (Endowed) Professor Dept. of Engineering Science

Lakhtakia, Akhlesh

33

Transfer Function Combinations Liang Zhou, Mathias Schott, Charles Hansen  

E-Print Network [OSTI]

and Imaging Institute, University of Utah, 72 S Central Campus Drive, Salt Lake City, UT 84112, United StatesTransfer Function Combinations Liang Zhou, Mathias Schott, Charles Hansen Scientific Computing

Utah, University of

34

TBU-0026- In the Matter of Charles L. Evans  

Broader source: Energy.gov [DOE]

Charles Evans, a former employee of Fluor Hanford Inc. (Fluor), a Department of Energy (DOE) contractor, appeals the DOE Richland Operations Office=s (Richland) dismissal of the whistleblower...

35

D r . Charles F. Brooks, of Clark University,  

E-Print Network [OSTI]

NO* 301 April 29 D r . Charles F. Brooks, of Clark University, discusses: VARIATIONS IN TH?C SUN between sunspots and the solar constant. seem t o be received from the Dun, and the circulation

36

Interactive Isosurface Ray Tracing of Large Octree Aaron Knoll, Ingo Wald, Steven Parker, and Charles Hansen  

E-Print Network [OSTI]

, and Charles Hansen UUSCI-2006-026 Scientific Computing and Imaging Institute University of Utah Salt Lake City-026 Interactive Isosurface Ray Tracing of Large Octree Volumes Aaron Knoll Ingo Wald Steven Parker Charles Hansen

Utah, University of

37

SEMI-ANNUAL REPORTS FOR LAKE CHARLES EXPORTS, LLC - FE DKT. NO...  

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

LAKE CHARLES EXPORTS, LLC - FE DKT. NO. 11-59-LNG - ORDER 3324 SEMI-ANNUAL REPORTS FOR LAKE CHARLES EXPORTS, LLC - FE DKT. NO. 11-59-LNG - ORDER 3324 October 2013 April 2014...

38

h"p://per.colorado.edu/Electrodynamics Charles Baily, Michael Dubson & Steven Pollock  

E-Print Network [OSTI]

7/27/12 1 h"p://per.colorado.edu/Electrodynamics Charles Baily, Michael Dubson & Steven Pollock Department of Physics University of Colorado Boulder Contact: Charles.Baily@Colorado.EDU 2nd semester upper-division physics course

Colorado at Boulder, University of

39

Population Cycles in Small Mammals CHARLES J. KREBS and JUDITH H. MYERS  

E-Print Network [OSTI]

Population Cycles in Small Mammals CHARLES J. KREBS and JUDITH H. MYERS Institute of Animal;268 CHARLES J. KREBS AND JUDITH H. MYERS VII. Evolution of Microtine Cycles . . 384 VIII. Summary . . 386 be almost anything: golden mice, holy water fr

Krebs, Charles J.

40

MagLab - Pioneers in Electricity and Magnetism: Jean-Charles...  

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

Jean-Charles-Athanase Peltier (1785-1845) Jean-Charles-Athanase Peltier Although he didn't start studying physics until he retired from the clock-making business at age 30, French...

Note: This page contains sample records for the topic "telescope baltay charles" 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

Upgrade of the MAGIC telescopes  

E-Print Network [OSTI]

The MAGIC telescopes are two Imaging Atmospheric Cherenkov Telescopes (IACTs) located on the Canary island of La Palma. With 17m diameter mirror dishes and ultra-fast electronics, they provide an energy threshold as low as 50 GeV for observations at low zenith angles. The first MAGIC telescope was taken in operation in 2004 whereas the second one joined in 2009. In 2011 we started a major upgrade program to improve and to unify the stereoscopic system of the two similar but at that time different telescopes. Here we report on the upgrade of the readout electronics and digital trigger of the two telescopes, the upgrade of the camera of the MAGIC I telescope as well as the commissioning of the system after this major upgrade.

Mazin, Daniel; Garczarczyk, Markus; Giavitto, Gianluca; Sitarek, Julian

2014-01-01T23:59:59.000Z

42

A review of "Charles II and the Politics of Access" by Brian Weiser.  

E-Print Network [OSTI]

REVIEWS 257 Brian Weiser. Charles II and the Politics of Access. Suffolk: The Boydell Press, 2003. xii + 208 pp. Review by TY M. REESE, UNIVERSITY OF NORTH DAKOTA. The English Civil War and subsequent restoration of Charles II to the English... Charles II and the Politics of Access, Brian Weiser successfully challenges this idea of continual access by arguing that Charles II skillfully con- trolled access for political reasons. The book?s main argument, that access was one of the ?most...

Ty M. Reese

2004-01-01T23:59:59.000Z

43

Issues Related to HCI Application of Fitts's Law Charles E. Wright  

E-Print Network [OSTI]

Issues Related to HCI Application of Fitts's Law Charles E. Wright University of California, Irvine's Contact Information: Charles E. Wright Email: cewright@uci.edu Phone: 949-824-7589 Fax: 949-824-2307 Brief Authors' Biographies: Charles Wright is a cognitive psychologist with an interest in motor control

California at Irvine, University of

44

The Severe Gout of Holy Roman Emperor Charles V  

Science Journals Connector (OSTI)

...His physical suffering influenced decisions that affected the future of many countries. His physicians diagnosed his arthritic disease clinically as gout. However, to our knowledge, there has never been objective biologic confirmation of this diagnosis. Charles V was buried, in accordance with his wishes... Holy Roman Emperor Charles V was known to have had attacks of gout from early adulthood. This study provides objective confirmation of the clinical diagnosis on the basis of an examination of the mummified terminal phalanx of one of his fingers. The analysis demonstrated typical gouty tophi, eroding bone and extending into the soft tissues.

Ordi J.; Alonso P.L.; de Zulueta J.

2006-08-03T23:59:59.000Z

45

High Energy Neutrino Telescopes  

E-Print Network [OSTI]

This paper presents a review of the history, motivation and current status of high energy neutrino telescopes. Many years after these detectors were first conceived, the operation of kilometer-cubed scale detectors is finally on the horizon at both the South Pole and in the Mediterranean Sea. These new detectors will perhaps provide us the first view of high energy astrophysical objects with a new messenger particle and provide us with our first real glimpse of the distant universe at energies above those accessible by gamma-ray instruments. Some of the topics that can be addressed by these new instruments include the origin of cosmic rays, the nature of dark matter, and the mechanisms at work in high energy astrophysical objects such as gamma-ray bursts, active galactic nuclei, pulsar wind nebula and supernova remnants.

Hoffman, K D

2008-01-01T23:59:59.000Z

46

High Energy Neutrino Telescopes  

E-Print Network [OSTI]

This paper presents a review of the history, motivation and current status of high energy neutrino telescopes. Many years after these detectors were first conceived, the operation of kilometer-cubed scale detectors is finally on the horizon at both the South Pole and in the Mediterranean Sea. These new detectors will perhaps provide us the first view of high energy astrophysical objects with a new messenger particle and provide us with our first real glimpse of the distant universe at energies above those accessible by gamma-ray instruments. Some of the topics that can be addressed by these new instruments include the origin of cosmic rays, the nature of dark matter, and the mechanisms at work in high energy astrophysical objects such as gamma-ray bursts, active galactic nuclei, pulsar wind nebula and supernova remnants.

K. D. Hoffman

2008-12-18T23:59:59.000Z

47

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

48

Charles City (1Q08) Wind Farm | Open Energy Information  

Open Energy Info (EERE)

Charles City (1Q08) Wind Farm Charles City (1Q08) Wind Farm Facility Charles City (1Q08) Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner MidAmerican Energy Developer MidAmerican Energy Energy Purchaser MidAmerican Energy Location Charles City IA Coordinates 43.049152°, -92.734151° Loading map... {"minzoom":false,"mappingservice":"googlemaps3","type":"ROADMAP","zoom":14,"types":["ROADMAP","SATELLITE","HYBRID","TERRAIN"],"geoservice":"google","maxzoom":false,"width":"600px","height":"350px","centre":false,"title":"","label":"","icon":"","visitedicon":"","lines":[],"polygons":[],"circles":[],"rectangles":[],"copycoords":false,"static":false,"wmsoverlay":"","layers":[],"controls":["pan","zoom","type","scale","streetview"],"zoomstyle":"DEFAULT","typestyle":"DEFAULT","autoinfowindows":false,"kml":[],"gkml":[],"fusiontables":[],"resizable":false,"tilt":0,"kmlrezoom":false,"poi":true,"imageoverlays":[],"markercluster":false,"searchmarkers":"","locations":[{"text":"","title":"","link":null,"lat":43.049152,"lon":-92.734151,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

49

CHARLES STURT UNIVERSITY BACHELOR OF ARTS (HONOURS) -PSYCHOLOGY  

E-Print Network [OSTI]

CHARLES STURT UNIVERSITY BACHELOR OF ARTS (HONOURS) - PSYCHOLOGY Additional information criteria Applicants must hold a degree which includes a three-year major in psychology accredited by the Australian Psychology Accreditation Council (APAC) completed within the last five years must have completed

Thomas, Richard C.

50

FISH SCHOOLS AS OPERATIONAL STRUCTURES CHARLES M. BREDER, JR.!  

E-Print Network [OSTI]

FISH SCHOOLS AS OPERATIONAL STRUCTURES CHARLES M. BREDER, JR.! ABSTRACf The interaction of a space lattice, vortex trails, and the lubricity of fish surface mucus is shown to he important to the operation and structure of fish schools and significant in terms of locomotor efficiency. This is independent

51

Heating the Outer Heliosphere by Pickup Charles W. Smith  

E-Print Network [OSTI]

Heating the Outer Heliosphere by Pickup Protons Charles W. Smith£ , Philip A. Isenberg£ , William H the ability of a turbulent cascade within the solar wind to heat the thermal protons. Several sources of energy are required to accom- plish the observed heating. Wind shear and shocks originating

Richardson, John

52

Britiske Charles Edward Hatchwell forsker i brndselsceller p Ris.  

E-Print Network [OSTI]

Oxide Fuel Cells, eller fast- oxid-brændselsceller. Charles Edward Hatchwells projekt ligger ved siden/S gennem- fører Afdelingen for Materialeforskning et omfattende program for udvikling af SOFC'er - Solid af hovedretningen i programmet. "Jeg udfører grundforskning inden for grup- pen af metal-oxider med

53

Managing Florida Ponds for Fishing 1 Charles E. Cichra2  

E-Print Network [OSTI]

CIR802 Managing Florida Ponds for Fishing 1 Charles E. Cichra2 1. This document is CIR802, one-out and impounded waters, limerock pits, and sand or gravel pits, commonly called borrow pits. Fishing pressure in fishing as a source of recreation and food. Competition for public fishery resources, coupled

Watson, Craig A.

54

Curriculum Vitae Charles H. Michler, Ph.D.  

E-Print Network [OSTI]

Charles H. Michler, Ph.D. Director, Hardwood Tree Improvement and Regeneration Center National Science Foundation I/UCRC Center for Tree Genetics USDA Forest Service Phone: 765-496-6016 Northern Research Station Fax: 765-494-9461 Hardwood Tree Improvement & Email: michler@purdue.edu Regeneration Center 715 West

55

Voles and M ice RUDY BOONSTRA, CHARLES). KREBS, SCOTT GILBERT,  

E-Print Network [OSTI]

Voles and M ice RUDY BOONSTRA, CHARLES). KREBS, SCOTT GILBERT, & SABINE SCHWEIGER 10 #12;S mall sizes of five or six. Clethrionomys females can produce 28 young per season, while Microtus females can produce 19-23 young per season. However, more realistic rates of increase are half or less than this (i

Krebs, Charles J.

56

Charles City (2Q08) Wind Farm | Open Energy Information  

Open Energy Info (EERE)

2Q08) Wind Farm 2Q08) Wind Farm Facility Charles City (2Q08) Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner MidAmerican Energy Developer MidAmerican Energy Energy Purchaser MidAmerican Energy Location Charles City IA Coordinates 43.004101°, -92.722392° Loading map... {"minzoom":false,"mappingservice":"googlemaps3","type":"ROADMAP","zoom":14,"types":["ROADMAP","SATELLITE","HYBRID","TERRAIN"],"geoservice":"google","maxzoom":false,"width":"600px","height":"350px","centre":false,"title":"","label":"","icon":"","visitedicon":"","lines":[],"polygons":[],"circles":[],"rectangles":[],"copycoords":false,"static":false,"wmsoverlay":"","layers":[],"controls":["pan","zoom","type","scale","streetview"],"zoomstyle":"DEFAULT","typestyle":"DEFAULT","autoinfowindows":false,"kml":[],"gkml":[],"fusiontables":[],"resizable":false,"tilt":0,"kmlrezoom":false,"poi":true,"imageoverlays":[],"markercluster":false,"searchmarkers":"","locations":[{"text":"","title":"","link":null,"lat":43.004101,"lon":-92.722392,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

57

St. Charles County, Missouri: Energy Resources | Open Energy Information  

Open Energy Info (EERE)

St. Charles County, Missouri: Energy Resources St. Charles County, Missouri: Energy Resources Jump to: navigation, search Equivalent URI DBpedia Coordinates 38.7338885°, -90.8294002° Loading map... {"minzoom":false,"mappingservice":"googlemaps3","type":"ROADMAP","zoom":14,"types":["ROADMAP","SATELLITE","HYBRID","TERRAIN"],"geoservice":"google","maxzoom":false,"width":"600px","height":"350px","centre":false,"title":"","label":"","icon":"","visitedicon":"","lines":[],"polygons":[],"circles":[],"rectangles":[],"copycoords":false,"static":false,"wmsoverlay":"","layers":[],"controls":["pan","zoom","type","scale","streetview"],"zoomstyle":"DEFAULT","typestyle":"DEFAULT","autoinfowindows":false,"kml":[],"gkml":[],"fusiontables":[],"resizable":false,"tilt":0,"kmlrezoom":false,"poi":true,"imageoverlays":[],"markercluster":false,"searchmarkers":"","locations":[{"text":"","title":"","link":null,"lat":38.7338885,"lon":-90.8294002,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

58

Charles Mix County, South Dakota: Energy Resources | Open Energy  

Open Energy Info (EERE)

Charles Mix County, South Dakota: Energy Resources Charles Mix County, South Dakota: Energy Resources Jump to: navigation, search Equivalent URI DBpedia Coordinates 43.0985109°, -98.3964938° Loading map... {"minzoom":false,"mappingservice":"googlemaps3","type":"ROADMAP","zoom":14,"types":["ROADMAP","SATELLITE","HYBRID","TERRAIN"],"geoservice":"google","maxzoom":false,"width":"600px","height":"350px","centre":false,"title":"","label":"","icon":"","visitedicon":"","lines":[],"polygons":[],"circles":[],"rectangles":[],"copycoords":false,"static":false,"wmsoverlay":"","layers":[],"controls":["pan","zoom","type","scale","streetview"],"zoomstyle":"DEFAULT","typestyle":"DEFAULT","autoinfowindows":false,"kml":[],"gkml":[],"fusiontables":[],"resizable":false,"tilt":0,"kmlrezoom":false,"poi":true,"imageoverlays":[],"markercluster":false,"searchmarkers":"","locations":[{"text":"","title":"","link":null,"lat":43.0985109,"lon":-98.3964938,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

59

A review of "English Warfare." by Mark Charles Fissel  

E-Print Network [OSTI]

290 SEVENTEENTH-CENTURY NEWS important a contribution to seventeenth-century studies as was The Paradise of Women. Mark Charles Fissel. English Warfare 1511-1642. London and New York: Routledge, 2001. xviii + 382 pp. + 38 illus. $25.95 [library... edition $85]. Review by IAN GENTLES, GLENDON COL- LEGE, YORK UNIVERSITY, TORONTO. Mark Fissel advances a strong and ably-supported thesis? that the English accumulated a great deal of military experience in the sixteenth and early seventeenth centuries...

Ian Gentles

2002-01-01T23:59:59.000Z

60

Power operations in Morava E-theory Charles Rezk  

E-Print Network [OSTI]

Power operations in Morava E-theory a survey Charles Rezk University of Illinois at Urbana-Champaign May 2, 2009 http://www.math.uiuc.edu/~rezk/midwest-2009-power-ops.pdf #12;What are power operations? h = multiplicative cohomology theory: hp(X) hq(X) hp+q(X). m-th power map: x xm : hq (X) hmq (X). If h comes from

Rezk, Charles

Note: This page contains sample records for the topic "telescope baltay charles" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
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We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


61

Coherent Multiresolution Isosurface Ray Tracing Aaron Knoll, Charles Hansen, and Ingo Wald  

E-Print Network [OSTI]

Scientific Computing and Imaging Institute University of Utah Salt Lake City, Utah 84112 Email: {knolla1 Coherent Multiresolution Isosurface Ray Tracing Aaron Knoll, Charles Hansen, and Ingo Wald

Wald, Ingo

62

Price of Lake Charles, LA Natural Gas LNG Imports from United...  

Annual Energy Outlook 2013 [U.S. Energy Information Administration (EIA)]

Arab Emirates (Dollars per Thousand Cubic Feet) Price of Lake Charles, LA Natural Gas LNG Imports from United Arab Emirates (Dollars per Thousand Cubic Feet) Decade Year-0...

63

Price of Lake Charles, LA Natural Gas LNG Imports from Other...  

Annual Energy Outlook 2013 [U.S. Energy Information Administration (EIA)]

(Nominal Dollars per Thousand Cubic Feet) Price of Lake Charles, LA Natural Gas LNG Imports from Other Countries (Nominal Dollars per Thousand Cubic Feet) Decade Year-0...

64

Wide field of view telescope  

DOE Patents [OSTI]

A wide field of view telescope having two concave and two convex reflective surfaces, each with an aspheric surface contour, has a flat focal plane array. Each of the primary, secondary, tertiary, and quaternary reflective surfaces are rotationally symmetric about the optical axis. The combination of the reflective surfaces results in a wide field of view in the range of approximately 3.8.degree. to approximately 6.5.degree.. The length of the telescope along the optical axis is approximately equal to or less than the diameter of the largest of the reflective surfaces.

Ackermann, Mark R. (Albuquerque, NM); McGraw, John T. (Placitas, NM); Zimmer, Peter C. (Albuquerque, NM)

2008-01-15T23:59:59.000Z

65

Neutrino telescopes in the World  

SciTech Connect (OSTI)

Neutrino astronomy has rapidly developed these last years, being the only way to get specific and reliable information about astrophysical objects still poorly understood.Currently two neutrino telescopes are operational in the World: BAIKAL, in the lake of the same name in Siberia, and AMANDA, in the ices of the South Pole. Two telescopes of the same type are under construction in the Mediterranean Sea: ANTARES and NESTOR. All these telescopes belong to a first generation, with an instrumented volume smaller or equal to 0.02 km3. Also in the Mediterranean Sea, the NEMO project is just in its stag phase, within the framework of a cubic kilometer size neutrino telescope study. Lastly, the ICECUBE detector, with a volume reaching about 1 km3, is under construction on the site of AMANDA experiment, while an extension of the BAIKAL detector toward km3 is under study. We will present here the characteristics of these experiments, as well as the results of their observations.

Ernenwein, J.-P. [GRPHE, Universite de Haute Alsace, 61 rue Albert Camus, 68093 Mulhouse cedex (France)

2007-01-12T23:59:59.000Z

66

Charles A. Stock Research Oceanographer, NOAA/Geophysical Fluid Dynamics Laboratory  

E-Print Network [OSTI]

Change Impacts on Living Marine Resources", 2012 Ocean Sciences Meeting, Salt Lake City 2012-13 MemberCharles A. Stock Research Oceanographer, NOAA/Geophysical Fluid Dynamics Laboratory Princeton-mail: Charles.Stock@noaa.gov Education 2005 Ph.D., Woods Hole Oceanographic Institution/MIT Joint Program Civil

67

Coherent Multiresolution Isosurface Ray Tracing Aaron Knoll, Charles Hansen and Ingo Wald  

E-Print Network [OSTI]

-2007-001 Scientific Computing and Imaging Institute University of Utah Salt Lake City, UT 84112 USA1 Coherent Multiresolution Isosurface Ray Tracing Aaron Knoll, Charles Hansen and Ingo Wald UUSCI. Technical Report No UUSCI-2007-001 Coherent Multiresolution Isosurface Ray Tracing Aaron Knoll Charles

Utah, University of

68

Image-Based Volume Rendering with Opacity Light Miriah Meyer, Hanspeter Pfister, Charles Hansen, Chris Johnson  

E-Print Network [OSTI]

Lake City, UT 84112 USA March 24, 2005 Abstract: While low cost PC graphics hardware has proven1 Image-Based Volume Rendering with Opacity Light Fields Miriah Meyer, Hanspeter Pfister, Charles;Image-Based Volume Rendering with Opacity Light Fields Miriah Meyer1 Hanspeter Pfister2 Charles Hansen1

Utah, University of

69

Byron Price, Director of the Charles Russell Center and the OU Press to Receive Prestigious  

E-Print Network [OSTI]

Byron Price, Director of the Charles Russell Center and the OU Press to Receive Prestigious Chester -- Byron Price, director of the Charles M. Russell Center for the Study of Art of the National Cowboy & Western Heritage Museum. Price will be formally honored during

Oklahoma, University of

70

Department of Industrial & Manufacturing Engineering Fall 2009 Central Scheduling System for Charles Cole Memorial Hospital  

E-Print Network [OSTI]

for Charles Cole Memorial Hospital Overview There is little unity between facilities in the Charles Cole Memorial Hospital network. Each location acts as its own office instead of being part of a clinic hospital procedures. Analyzed the LSS system and different appointment techniques performed by schedulers

Demirel, Melik C.

71

On Quaternary MacDonald Codes Charles J. Colbourn and Manish K. Gupta  

E-Print Network [OSTI]

On Quaternary MacDonald Codes Charles J. Colbourn and Manish K. Gupta Department of Computer:{charles.colbourn,manish.gupta}@asu.edu December 11, 2002 Abstract This paper studies two families of codes over Z4, MacDonald codes of type map. Keywords: Codes over rings, Gray image, simplex codes, torsion code, weight distribu- tion, MacDonald

Gupta, Manish K.

72

Water balance in rats exposed to chronic centrifugation RUDY M. ORTIZ AND CHARLES E. WADE  

E-Print Network [OSTI]

Water balance in rats exposed to chronic centrifugation RUDY M. ORTIZ AND CHARLES E. WADE Life; accepted in final form 22 February 2000 Ortiz, Rudy M., and Charles E. Wade. Water balance in rats exposed was conducted to determine the effects of chronic centrifugation on water bal- ance. Eight Sprague-Dawley rats

Ortiz, Rudy M.

73

EIS-0464: Lake Charles Carbon Capture and Storage (CCS) Project in  

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

4: Lake Charles Carbon Capture and Storage (CCS) Project in 4: Lake Charles Carbon Capture and Storage (CCS) Project in Calcasieu Parish, Louisiana EIS-0464: Lake Charles Carbon Capture and Storage (CCS) Project in Calcasieu Parish, Louisiana Summary This EIS will evaluate the environmental impacts of a proposal to provide financial assistance for the construction and operation of a project proposed by Leucadia Energy, LLC. DOE selected this project for an award of financial assistance through a competitive process under the Industrial Carbon Capture and Sequestration Program. Public Comment Opportunities None available at this time. Documents Available for Download November 22, 2013 EIS-0464: EPA Notice of Availability of Final Environmental Impact Statement Lake Charles Carbon Capture and Sequestration Project, Lake Charles,

74

THE OPTIMAL GRAVITATIONAL LENS TELESCOPE  

SciTech Connect (OSTI)

Given an observed gravitational lens mirage produced by a foreground deflector (cf. galaxy, quasar, cluster, ...), it is possible via numerical lens inversion to retrieve the real source image, taking full advantage of the magnifying power of the cosmic lens. This has been achieved in the past for several remarkable gravitational lens systems. Instead, we propose here to invert an observed multiply imaged source directly at the telescope using an ad hoc optical instrument which is described in the present paper. Compared to the previous method, this should allow one to detect fainter source features as well as to use such an optimal gravitational lens telescope to explore even fainter objects located behind and near the lens. Laboratory and numerical experiments illustrate this new approach.

Surdej, J.; Hanot, C.; Sadibekova, T. [Department of Astrophysics, Geophysics and Oceanography (AGO), AEOS Group, Liege University, Allee du 6 Aout 17, 4000 Liege (Belgium); Delacroix, C.; Habraken, S. [Department of Physics (DEPHY), Hololab Group, Liege University, Allee du 6 Aout 17, 4000 Liege (Belgium); Coleman, P. [Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822 (United States); Dominik, M. [SUPA, University of St Andrews, School of Physics and Astronomy, North Haugh, St Andrews, KY16 9SS (United Kingdom); Le Coroller, H. [Observatoire de Haute Provence, F-04870 Saint Michel l'Observatoire (France); Mawet, D. [Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109 (United States); Quintana, H. [Departmento de Astronomia y Astrofisica, Pontificia Universidad Catolica de Chile, Casilla 306, CL 22 Santiago (Chile); Sluse, D., E-mail: surdej@astro.ulg.ac.b [Astronomisches Rechen-Institut am Zentrum fuer Astronomie der Universitaet Heidelberg, Moenchhofstrasse 12-14, 69120 Heidelberg (Germany)

2010-05-15T23:59:59.000Z

75

Ligand Rearrangement Reactions of Cr(CO)6 in Alcohol Solutions: Experiment and Theory Jennifer E. Shanoski, Elizabeth A. Glascoe, and Charles B. Harris*  

E-Print Network [OSTI]

. Shanoski, Elizabeth A. Glascoe, and Charles B. Harris* Department of Chemistry, UniVersity of California

Harris, Charles B.

76

Dynamics of an Excess Electron at Metal/Polar Interfaces Preston T. Snee, Sean Garrett-Roe, and Charles B. Harris*  

E-Print Network [OSTI]

-Roe, and Charles B. Harris* Department of Chemistry, UniVersity of California, Berkeley, California 94720

Harris, Charles B.

77

City of St Charles, Illinois (Utility Company) | Open Energy Information  

Open Energy Info (EERE)

Illinois (Utility Company) Illinois (Utility Company) Jump to: navigation, search Name City of St Charles Place Illinois Utility Id 17860 Utility Location Yes Ownership M NERC Location RFC NERC RFC Yes Activity Distribution Yes References EIA Form EIA-861 Final Data File for 2010 - File1_a[1] LinkedIn Connections CrunchBase Profile No CrunchBase profile. Create one now! This article is a stub. You can help OpenEI by expanding it. Utility Rate Schedules Grid-background.png General service Commercial Governmental Outdoor Sports Lighting Lighting Large General Service Industrial Municipal Owned Street Lighting and Traffic Signals Lighting Residential Residential Small General Service Commercial Average Rates Residential: $0.1010/kWh Commercial: $0.0839/kWh Industrial: $0.0679/kWh References

78

City of St Charles, Minnesota (Utility Company) | Open Energy Information  

Open Energy Info (EERE)

Minnesota (Utility Company) Minnesota (Utility Company) Jump to: navigation, search Name City of St Charles Place Minnesota Utility Id 17862 Utility Location Yes Ownership M NERC Location MRO NERC MRO Yes Operates Generating Plant Yes Activity Generation Yes Activity Buying Transmission Yes Activity Distribution Yes Activity Bundled Services Yes References EIA Form EIA-861 Final Data File for 2010 - File1_a[1] LinkedIn Connections CrunchBase Profile No CrunchBase profile. Create one now! This article is a stub. You can help OpenEI by expanding it. Utility Rate Schedules Grid-background.png Commercial- Single Phase Commercial Commercial- Three Phase Commercial Large Industrial Industrial Large Power Commercial Residential Residential Security Lighting Lighting Average Rates Residential: $0.1300/kWh

79

Charles D. Young Project Engineer Government Support Directorate  

Office of Legacy Management (LM)

Please call if you have questions regarding the attached recommendation. i?&,o-o; Please call if you have questions regarding the attached recommendation. i?&,o-o; ~~~pApv $l$I Charles D. Young Project Engineer Government Support Directorate Architecture Planning and Technology Division CDY/smb Attachment cc: J. Fiore ;;,ewis (w/o) TH' E AEROSPACE CORPORATION i ' 0 A Suite 7900, 955 L' Enfam Plaza. S. W., Woshingron. D.C. 20024-2174. Tekphonc (202) 488-6000 7117-03.87.cdy.43 23 September 1987 CA Mr. Andrew Wallo, III, NE-23 Division of Facility & Site Decosunissioning Projects U.S. Department of Energy Germantown, Maryland 20545 Dear Mr. Wallo: ELIMINATION RECOMMENDATION -- COLLEGES AND UNIVERSITIES The attached elimination reconnnendation was prepared in accordance PC.o= with your suggestion during our meeting on 22 September. The recommendation flD.o-02

80

Charles Mix Electric Assn, Inc | Open Energy Information  

Open Energy Info (EERE)

Electric Assn, Inc Electric Assn, Inc Jump to: navigation, search Name Charles Mix Electric Assn, Inc Place South Dakota Utility Id 3315 Utility Location Yes Ownership C NERC Location MRO Activity Distribution Yes References EIA Form EIA-861 Final Data File for 2010 - File1_a[1] LinkedIn Connections CrunchBase Profile No CrunchBase profile. Create one now! This article is a stub. You can help OpenEI by expanding it. Utility Rate Schedules Grid-background.png Rate Schedule A Residential Rate Schedule A - All Electric Heat Residential Rate Schedule A - Small Commercial Commercial Rate Schedule A - Small Commercial - All Electric Heat Commercial Rate Schedule B Commercial Rate Schedule B - All Electric Heat Commercial Rate Schedule B - Residential Residential Rate Schedule B - Residential - All Electric Heat Residential

Note: This page contains sample records for the topic "telescope baltay charles" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
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81

BNL | Large Synoptic Survey Telescope (LSST)  

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

Large Synoptic Survey Telescope Large Synoptic Survey Telescope About LSST Digital Sensor Array Brookhaven & Physics of the Universe LSST Project Website LSST: Providing an Unprecedented View of the Cosmos rendering of the LSST site in Chile A revolutionary 3.2 gigapixel camera mounted in a massive ground-based telescope will produce unprecedented views of the cosmos, driving discoveries with the widest, densest, and most complete images of our universe ever captured. New Visions The Large Synoptic Survey Telescope (LSST) will peer into space as no other telescope can. This new facility will create an unparalleled wide-field astronomical survey of our universe - wider and deeper in volume than all previous telescopes combined. The combination of a 3200 megapixel camera sensor array, a powerful supercomputer, a cutting-edge data processing and

82

Large aperture diffractive space telescope  

DOE Patents [OSTI]

A large (10's of meters) aperture space telescope including two separate spacecraft--an optical primary objective lens functioning as a magnifying glass and an optical secondary functioning as an eyepiece. The spacecraft are spaced up to several kilometers apart with the eyepiece directly behind the magnifying glass "aiming" at an intended target with their relative orientation determining the optical axis of the telescope and hence the targets being observed. The objective lens includes a very large-aperture, very-thin-membrane, diffractive lens, e.g., a Fresnel lens, which intercepts incoming light over its full aperture and focuses it towards the eyepiece. The eyepiece has a much smaller, meter-scale aperture and is designed to move along the focal surface of the objective lens, gathering up the incoming light and converting it to high quality images. The positions of the two space craft are controlled both to maintain a good optical focus and to point at desired targets which may be either earth bound or celestial.

Hyde, Roderick A. (Livermore, CA)

2001-01-01T23:59:59.000Z

83

Charles Byers, Summary Remarks | U.S. DOE Office of Science (SC)  

Office of Science (SC) Website

Charles Byers, Charles Byers, Summary Remarks Chemical Sciences, Geosciences, & Biosciences (CSGB) Division CSGB Home About Research Areas Scientific Highlights Reports & Activities Principal Investigators' Meetings BES Home Third DOE BES Separations Research Workshop Charles Byers, Summary Remarks Print Text Size: A A A RSS Feeds FeedbackShare Page Third DOE/Basic Energy Sciences Separations Research Workshop Savannah DeSoto Hilton, Savannah, Georgia May 12-14, 1999 Summary Remarks Charles H. Byers IsoPro International This presentation was prepared before the final sessions on Friday May 14 and represents a condensation of remarks made by participants during their primarily technical talks. A good deal of off-line conversational material is included in this document. Themes: There were many themes and crosscurrents that flowed through the

84

The Visual Haptic Workbench J. Dean Brederson Milan Ikits Christopher R. Johnson Charles D. Hansen  

E-Print Network [OSTI]

3490 Salt Lake City, UT 84112-9205, USA {jdb, ikits, crj, hansen}@cs.utah.edu Abstract MultimodalThe Visual Haptic Workbench J. Dean Brederson Milan Ikits Christopher R. Johnson Charles D. Hansen

Utah, University of

85

The Visual Haptic Workbench J. Dean Brederson Milan Ikits Christopher R. Johnson Charles D. Hansen  

E-Print Network [OSTI]

3490 Salt Lake City, UT 84112­9205, USA {jdb, ikits, crj, hansen}@cs.utah.edu Abstract MultimodalThe Visual Haptic Workbench J. Dean Brederson Milan Ikits Christopher R. Johnson Charles D. Hansen

Utah, University of

86

Interactive Caustics Using Local Precomputed Irradiance Chris Wyman Charles Hansen Peter Shirley  

E-Print Network [OSTI]

School of Computing, The University of Utah Salt Lake City, Utah, USA Abstract Bright patterns of lightInteractive Caustics Using Local Precomputed Irradiance Chris Wyman Charles Hansen Peter Shirley

Wyman, Chris

87

Parallel Methods for Isosurface Visualization Charles D. Hansen, Tushar Udeshi, Steven Parker, and Peter Shirley  

E-Print Network [OSTI]

Lake City, Utah 84112­9205 fhansen j tudeshi j sparker j shirleyg@cs.utah.edu Extended Abstract ManyParallel Methods for Isosurface Visualization Charles D. Hansen, Tushar Udeshi, Steven Parker

Utah, University of

88

Adaptive Temporal Tone Mapping Shaun David Ramsey, J. Thomas Johnson III, Charles Hansen  

E-Print Network [OSTI]

University of Utah, Salt Lake City, Utah, USA Abstract Monitor intensity ranges are much lower than the rangeAdaptive Temporal Tone Mapping Shaun David Ramsey, J. Thomas Johnson III, Charles Hansen

Utah, University of

89

FOLIATIONS INVARIANT BY RATIONAL MAPS CHARLES FAVRE AND JORGE VITORIO PEREIRA  

E-Print Network [OSTI]

FOLIATIONS INVARIANT BY RATIONAL MAPS CHARLES FAVRE AND JORGE VIT´ORIO PEREIRA Abstract. We give VIT ´ORIO PEREIRA Let us comment briefly on which surfaces U may appear. When is a subgroup of (C2

Pereira, Jorge Vitório

90

Price of Lake Charles, LA Natural Gas LNG Imports from Egypt...  

Gasoline and Diesel Fuel Update (EIA)

Egypt (Nominal Dollars per Thousand Cubic Feet) Price of Lake Charles, LA Natural Gas LNG Imports from Egypt (Nominal Dollars per Thousand Cubic Feet) Decade Year-0 Year-1 Year-2...

91

Price of Lake Charles, LA Natural Gas LNG Imports from Oman ...  

Annual Energy Outlook 2013 [U.S. Energy Information Administration (EIA)]

Oman (Dollars per Thousand Cubic Feet) Price of Lake Charles, LA Natural Gas LNG Imports from Oman (Dollars per Thousand Cubic Feet) Decade Year-0 Year-1 Year-2 Year-3 Year-4...

92

Price of Lake Charles, LA Natural Gas LNG Imports from Indonesia...  

U.S. Energy Information Administration (EIA) Indexed Site

Indonesia (Dollars per Thousand Cubic Feet) Price of Lake Charles, LA Natural Gas LNG Imports from Indonesia (Dollars per Thousand Cubic Feet) Decade Year-0 Year-1 Year-2 Year-3...

93

Price of Lake Charles, LA Natural Gas LNG Imports from Algeria...  

Annual Energy Outlook 2013 [U.S. Energy Information Administration (EIA)]

Algeria (Dollars per Thousand Cubic Feet) Price of Lake Charles, LA Natural Gas LNG Imports from Algeria (Dollars per Thousand Cubic Feet) Decade Year-0 Year-1 Year-2 Year-3 Year-4...

94

Price of Lake Charles, LA Natural Gas LNG Imports from Malaysia...  

Gasoline and Diesel Fuel Update (EIA)

Malaysia (Dollars per Thousand Cubic Feet) Price of Lake Charles, LA Natural Gas LNG Imports from Malaysia (Dollars per Thousand Cubic Feet) Decade Year-0 Year-1 Year-2 Year-3...

95

Price of Lake Charles, LA Natural Gas LNG Imports from Nigeria...  

Annual Energy Outlook 2013 [U.S. Energy Information Administration (EIA)]

Nigeria (Dollars per Thousand Cubic Feet) Price of Lake Charles, LA Natural Gas LNG Imports from Nigeria (Dollars per Thousand Cubic Feet) Decade Year-0 Year-1 Year-2 Year-3 Year-4...

96

Price of Lake Charles, LA Natural Gas LNG Imports from Brunei...  

Gasoline and Diesel Fuel Update (EIA)

Brunei (Dollars per Thousand Cubic Feet) Price of Lake Charles, LA Natural Gas LNG Imports from Brunei (Dollars per Thousand Cubic Feet) Decade Year-0 Year-1 Year-2 Year-3 Year-4...

97

Charles McMillan to lead Los Alamos National Laboratory's Weapons...  

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

McMillan to Lead Weapons Program Charles McMillan to lead Los Alamos National Laboratory's Weapons Program He will provide oversight and direction for the nuclear weapons program...

98

Community, individual, and world in the later works of Josiah Royce and Charles Taylor  

E-Print Network [OSTI]

are those of Josiah Royce and Charles Taylor. I wish to show the similarities and dissimilarities between their respective social philosophies, their social ontologies, and the ameliorative practices they advocate. Although I find Taylor's account...

Hilde, Thomas Christian

2012-06-07T23:59:59.000Z

99

Inventing the Charles River Basin : urban images and civic discourse in Boston, 1844-1994  

E-Print Network [OSTI]

The Charles River Basin, extending from the foot of Beacon Hill upstream past Harvard's Soldiers Field, has been called Boston's "Central Park." The river looks to all appearances tranquil and unchanging, one of the most ...

Haglund, Karl T

1997-01-01T23:59:59.000Z

100

Merguerian, Charles, 1979, Dismembered ophiolite along Cameron's Line, West Torrington, Connecticut.  

E-Print Network [OSTI]

Merguerian, Charles, 1979, Dismembered ophiolite along Cameron's Line, West Torrington, Connecticut. Cameron's Line is a zone of ductile deformation in northwestern Connecticut that's separates highly Torrington, Connecticut (abs.): Geological Society of America Abstracts with Programs, v. 11, p. 45. Filename

Merguerian, Charles

Note: This page contains sample records for the topic "telescope baltay charles" 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

VWA-0014- In the Matter of Charles Barry DeLoach  

Broader source: Energy.gov [DOE]

This Decision involves a whistleblower complaint filed by Charles Barry DeLoach (DeLoach) under the Department of Energy's (DOE) Contractor Employee Protection Program, 10 C.F.R. Part 708. For a...

102

A Fundamental Issue of Naive Bayes Harry Zhang 1 and Charles X. Ling 2  

E-Print Network [OSTI]

A Fundamental Issue of Naive Bayes Harry Zhang 1 and Charles X. Ling 2 1 Faculty of Computer#12;er, or simply naive Bayes (NB). g(E) = p(C = +) p(C = ) n Y i=1 p(a i jC = +) p(a i jC = ) : (1) #12; 2 Harry Zhang and Charles X. Ling. It is obvious that the conditional independence assumption

Ling, Charles X.

103

Intel / Charles E. Young Endowed Chair in Nanotechnology Director of the Nanoscience Institute for Medical and Engineering Technology  

E-Print Network [OSTI]

Intel / Charles E. Young Endowed Chair in Nanotechnology Director of the Nanoscience Institute of the Nanoscience Institute for Medical and Engineering Technology. The Intel Foundation established this endowment

Slatton, Clint

104

James Webb Space Telescope: PM Lessons Applied - Eric Smith,...  

Energy Savers [EERE]

James Webb Space Telescope: PM Lessons Applied - Eric Smith, Deputy Program Director, NASA James Webb Space Telescope: PM Lessons Applied - Eric Smith, Deputy Program Director,...

105

General surface equations for glancing incidence telescopes  

Science Journals Connector (OSTI)

A generalized set of equations are derived for two mirror glancing incidence telescopes using Fermats principle, a differential form of the law of reflection, the generalized sine...

Saha, Timo T

1987-01-01T23:59:59.000Z

106

Charles E. Elderkin, 1975 | U.S. DOE Office of Science (SC)  

Office of Science (SC) Website

Charles E. Elderkin, 1975 Charles E. Elderkin, 1975 The Ernest Orlando Lawrence Award Lawrence Award Home Nomination & Selection Guidelines Award Laureates 2000's 1990's 1980's 1970's 1960's Ceremony The Life of Ernest Orlando Lawrence Contact Information The Ernest Orlando Lawrence Award U.S. Department of Energy SC-2/Germantown Building 1000 Independence Ave., SW Washington, DC 20585 P: (301) 903-9395 E: lawrence.award@science.doe.gov 1970's Charles E. Elderkin, 1975 Print Text Size: A A A RSS Feeds FeedbackShare Page Reactors: For his innovative research on atmospheric turbulence, diffusion, and deposition of pollutants over land and over the sea; for contributions to the understanding of the impact on the environment of energy generation including nuclear energy generations; and for his outstanding management of

107

Charles D. Scott, 1980 | U.S. DOE Office of Science (SC)  

Office of Science (SC) Website

Charles D. Scott, 1980 Charles D. Scott, 1980 The Ernest Orlando Lawrence Award Lawrence Award Home Nomination & Selection Guidelines Award Laureates 2000's 1990's 1980's 1970's 1960's Ceremony The Life of Ernest Orlando Lawrence Contact Information The Ernest Orlando Lawrence Award U.S. Department of Energy SC-2/Germantown Building 1000 Independence Ave., SW Washington, DC 20585 P: (301) 903-9395 E: lawrence.award@science.doe.gov 1980's Charles D. Scott, 1980 Print Text Size: A A A RSS Feeds FeedbackShare Page Chemistry & Metallurgy: For the innovation and application of chemical engineering principles to the development and deployment of chromatographic separations systems, and advanced analytical and bio-analytical instrumentation, and for his significant contributions to nuclear fuel

108

Absolute calibration of imaging atmospheric Cherenkov telescopes  

E-Print Network [OSTI]

A calibrated laser pulse propagating through the atmosphere produces a flash of Rayleigh scattered light with an intensity that can be calculated very accurately when atmospheric conditions are good. This is used in a technique developed for the absolute calibration of ultra high energy cosmic ray fluorescence telescopes, and it can also be applied to imaging atmospheric Cherenkov telescopes (IACTs). In this paper we present the absolute calibration system being constructed and tested for the VERITAS project.

N. Shepherd; J. H. Buckley; O. Celik; J. Holder; S. LeBohec; H. Manseri; F. Pizlo; M. Roberts

2005-07-04T23:59:59.000Z

109

Schwarzschild-Couder telescope for the Cherenkov Telescope Array: Development of the Optical System  

E-Print Network [OSTI]

The CTA (Cherenkov Telescope Array) is the next generation ground-based experiment for very high-energy (VHE) gamma-ray observations. It will integrate several tens of imaging atmospheric Cherenkov telescopes (IACTs) with different apertures into a single astronomical instrument. The US part of the CTA collaboration has proposed and is developing a novel IACT design with a Schwarzschild-Couder (SC) aplanatic two mirror optical system. In comparison with the traditional single mirror Davies-Cotton IACT the SC telescope, by design, can accommodate a wide field-of-view, with significantly improved imaging resolution. In addition, the reduced plate scale of an SC telescope makes it compatible with highly integrated cameras assembled from silicon photo multipliers. In this submission we report on the status of the development of the SC optical system, which is part of the effort to construct a full-scale prototype telescope of this type at the Fred Lawrence Whipple Observatory in southern Arizona.

Rousselle, Julien; Errando, Manel; Humensky, Brian; Mukherjee, Reshmi; Nieto, Daniel; Okumura, Akira; Vassiliev, Vladimir

2013-01-01T23:59:59.000Z

110

Cost-Sensitive Test Strategies Victor S. Sheng, Charles X. Ling  

E-Print Network [OSTI]

Cost-Sensitive Test Strategies Victor S. Sheng, Charles X. Ling Department of Computer Science cost of medical tests and misdiagnosis. In this paper, we design cost-sensitive machine learning learning whose values may be obtained at cost (attribute cost), and misdiagnoses are like

Ling, Charles X.

111

On the security of UOV Jean-Charles Faug`ere, Ludovic Perret  

E-Print Network [OSTI]

investigate the security of the Unbalanced Oil and Vinegar Scheme [15]. To do so, we use a hybrid approachOn the security of UOV Jean-Charles Faug`ere, Ludovic Perret Abstract. In this short note, we cryptanalysis of this scheme. In this paper, we investigate the security of another multivariate signature

112

Efficient Multi-Ported Memories for FPGAs Charles Eric LaForest and J. Gregory Steffan  

E-Print Network [OSTI]

Efficient Multi-Ported Memories for FPGAs Charles Eric LaForest and J. Gregory Steffan Department of Electrical and Computer Engineering University of Toronto {laforest,steffan}@eecg.toronto.edu ABSTRACT Multi-ported ports. We present a thorough exploration of the design space of FPGA-based soft multi-ported memories

Toronto, University of

113

Review: Continuous hydrolysis and fermentation for cellulosic ethanol production Simone Brethauer, Charles E. Wyman *  

E-Print Network [OSTI]

, Charles E. Wyman * Center for Environmental Research and Technology and Chemical and Environmental costs, and reduced vessel down time for cleaning and filling. On the other hand, these systems are more the world uses, far more than derived from coal, natural gas, hydroelectric power, nuclear energy

California at Riverside, University of

114

Techniques for the removal of marker genes from transgenic plants Charles P. Scutt a,  

E-Print Network [OSTI]

reason to warrant their removal. In addition to environmental and health concerns, there are alsoReview Techniques for the removal of marker genes from transgenic plants Charles P. Scutt a of problems. Various techniques are under development for the removal of unwanted marker genes, while leaving

Meyer, Peter

115

Joule heating and nitric oxide in the thermosphere, 2 Charles A. Barth1  

E-Print Network [OSTI]

Joule heating and nitric oxide in the thermosphere, 2 Charles A. Barth1 Received 14 April 2010, gravity waves propagate from the polar regions toward the equator heating the thermosphere at 140 km and higher. These gravity waves are produced by Joule heating that occurs at latitudes of 60° and higher

Bailey, Scott

116

Fuzzy Rule-Based Networks for Control Charles M. Higgins and Rodney M. Goodman  

E-Print Network [OSTI]

Fuzzy Rule-Based Networks for Control Charles M. Higgins and Rodney M. Goodman Abstract| We present a method for the learning of fuzzy logic membership functions and rules to approximate a nu- merical- struct a fuzzy control system from examples of an existing control system's actions. This can be useful

117

Geothermal energy market study on the Atlantic Coastal Plain: geothermal community heating for Cape Charles, Virginia  

SciTech Connect (OSTI)

An economic feasibility study for a geothermal community heating system has been made for the residential heat load of Cape Charles, Virginia using the JHU/APL GRITS Computer Program. The effects of inflation, interest rates, wellhead temperatures, and the addition of reinjection wells are investigated.

Leffel, C.S. Jr.

1981-10-01T23:59:59.000Z

118

Simple and General Statistical Profiling with PCT Charles Blake Steve Bauer  

E-Print Network [OSTI]

Simple and General Statistical Profiling with PCT Charles Blake Steve Bauer Laboratory for Computer Science Laboratory for Computer Science Massachusettes Institute of Technology Massachusettes Institute of Technology cb@mit.edu bauer@mit.edu Abstract The Profile Collection Toolkit (PCT) provides a novel

119

ECS 122B: Algorithm Design and Analysis Handout ?? UC Davis --Charles Martel Jan. 4, 2010  

E-Print Network [OSTI]

ECS 122B: Algorithm Design and Analysis Handout ?? UC Davis -- Charles Martel Jan. 4, 2010 Problem for some future topics of program verification and testing. Real assignments will come soon. Problem 1), and a target integer t. Your function should return "-1" if t is is not in A, and the position

California at Davis, University of

120

Hybrid Cost-sensitive Decision Tree Shengli Sheng, Charles X. Ling  

E-Print Network [OSTI]

Hybrid Cost-sensitive Decision Tree Shengli Sheng, Charles X. Ling Department of Computer Science, The University of Western Ontario London, Ontario N6A 5B7, Canada {cling, ssheng}@ csd.uwo.ca Abstract. Cost-sensitive decision tree and cost-sensitive naïve Bayes are both new cost-sensitive learning models proposed recently

Ling, Charles X.

Note: This page contains sample records for the topic "telescope baltay charles" 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

STANDARD COMPONENTS OF A KRULL-SCHMIDT CATEGORY SHIPING LIU AND CHARLES PAQUETTE  

E-Print Network [OSTI]

STANDARD COMPONENTS OF A KRULL-SCHMIDT CATEGORY SHIPING LIU AND CHARLES PAQUETTE Abstract. First to be standard. Speciali- zing to the category of finitely presented representations of a strongly locally finite quiver and its bounded derived category, we obtain many new types of standard Auslander-Reiten components

Liu, Shiping

122

Contracting inside an organization: an experimental study Paul J. Healy, John O. Ledyard, Charles Noussair,  

E-Print Network [OSTI]

Contracting inside an organization: an experimental study Paul J. Healy, John O. Ledyard, Charles propose and test a contracting mechanism, Multi-Contract Cost Sharing (MCCS), for use in the management the true costs of various projects than does the contracting agency (adverse selection,) and (2

123

Fertilization of Fresh Water Fish Ponds 1 Craig Watson and Charles E. Cichra2  

E-Print Network [OSTI]

FA17 Fertilization of Fresh Water Fish Ponds 1 Craig Watson and Charles E. Cichra2 1. This document. If a fish species which consumes small natural foods is grown, such as the bluegill or golden shiner, then pond fertilization can increase the production of these fish. Fertilizers provide nutrients

Watson, Craig A.

124

Building Design Services in a Distributed Service Architecture Charles S. Han1  

E-Print Network [OSTI]

Building Design Services in a Distributed Service Architecture Charles S. Han1 , John C. Kunz2 design services over the Internet. The benefits of the framework for distributed design services are at least twofold. First, the framework provides a means to distribute design services in a modular

Stanford University

125

Making Automated Building Code Checking A Reality1 Charles S. Han, John Kunz, Kincho H. Law  

E-Print Network [OSTI]

in the September/October 1997 issue of Facility Management Journal 1 #12;2. A Building Model Standard In orderMaking Automated Building Code Checking A Reality1 Charles S. Han, John Kunz, Kincho H. Law Center set of building codes. The complexity and changing nature of codes leads to delays in both the design

Stanford University

126

The Economic Impact of the Charles Town Thoroughbred Horse Racing Industry on  

E-Print Network [OSTI]

The Economic Impact of the Charles Town Thoroughbred Horse Racing Industry on the Jefferson County Research Assistant Tom S Witt, Director and Associate Dean Bureau of Business and Economic Research College of Business and Economics West Virginia University November 2011 Funding for this research was provided

Mohaghegh, Shahab

127

TO: University of Connecticut Faculty and Staff FROM: Charles H. Eaton, CPA, Controller  

E-Print Network [OSTI]

TO: University of Connecticut Faculty and Staff FROM: Charles H. Eaton, CPA, Controller Michael for equipment at the University of Connecticut. Therefore, the University will be increasing the equipment,000 will be categorized as non-capital equipment and expensed in the period purchased. Per Connecticut State Statute 4

Holsinger, Kent

128

AUTONOMOUS ROVER TECHNOLOGY FOR MARS SAMPLE RETURN Charles R. Weisbin, Guillermo Rodriguez, Paul S. Schenker,  

E-Print Network [OSTI]

AUTONOMOUS ROVER TECHNOLOGY FOR MARS SAMPLE RETURN Charles R. Weisbin, Guillermo Rodriguez, Paul S An autonomous system is defined here as one that can execute multiple-command sequences robustly at the remote. The longer and more complex the task that a given rover can reliably execute by itself, the more autonomous

Volpe, Richard

129

The Potato Radius: a Lower Minimum Size for Dwarf Planets Charles H. Lineweaver & Marc Norman  

E-Print Network [OSTI]

The Potato Radius: a Lower Minimum Size for Dwarf Planets Charles H. Lineweaver & Marc Norman a rounded potato shape to a sphere. We derive this potato-to-sphere transition radius -- or "potato radius" -- from first principles. Using the empirical potato radii of asteroids and icy moons, we derive

Lineweaver, Charles H.

130

Solar Absorption by Mie Resonances in Cloud Droplets Charles S. Zender  

E-Print Network [OSTI]

Solar Absorption by Mie Resonances in Cloud Droplets Charles S. Zender Department of Earth System March 2005; accepted 31 March 2005 Abstract Recent studies suggest that resonant absorption of sunlight. We spectrally resolve, for the first time, all solar absorption, including sharp resonances

Zender, Charles

131

PATCH SIMILARITY UNDER NON GAUSSIAN NOISE Charles-Alban Deledalle, Florence Tupin  

E-Print Network [OSTI]

PATCH SIMILARITY UNDER NON GAUSSIAN NOISE Charles-Alban Deledalle, Florence Tupin Institut Telecom compare groups of pixels (patches) and provide dense match- ing. Patch similarity is a key ingredient difficulty when comparing two patches from "real" data is to decide whether the differences should

Paris-Sud XI, Université de

132

LuaAV: Extensibility and Heterogeneity for Audiovisual Graham WAKEFIELD and Wesley SMITH and Charles ROBERTS  

E-Print Network [OSTI]

LuaAV: Extensibility and Heterogeneity for Audiovisual Computing Graham WAKEFIELD and Wesley SMITH and Charles ROBERTS Media Arts and Technology, University of California Santa Barbara Santa Barbara, CA 93110 providing the flexibility and temporal accuracy demanded by interactive audio-visual media. Code generation

California at Santa Barbara, University of

133

ECS 122B: Algorithm Design and Analysis Handout ?? UC Davis ---Charles Martel May. 2001  

E-Print Network [OSTI]

ECS 122B: Algorithm Design and Analysis Handout ?? UC Davis --- Charles Martel May. 2001 SampleL layers in GL . (20) 2. After students graduate from Medical school they are assigned to hospitals. Each, but it illustrates a kind of question I might ask). (20) 3. In the select program for assignment 1 the main

California at Davis, University of

134

Gerard Charles Dismukes Tel:848-445-1489; dismukes@rci.rutgers.edu  

E-Print Network [OSTI]

Meeting, San Francisco August 10-14. 2014 invited speaker, BASF Chemical Company, Ludwigschafen, GermanyJune 2014 1 Gerard Charles Dismukes Tel:848-445-1489; dismukes@rci.rutgers.edu Web: http Academy of Sciences; 2008 Chinese Bioenergy Association Award, Chinese Academy of Sciences 2010

Lawson, Catherine L.

135

Simulation of the Simbol-X Telescope  

SciTech Connect (OSTI)

We have developed a simulation tool for a Wolter I telescope operating in formation flight. The aim is to understand and predict the behavior of the Simbol-X instrument. As the geometry is variable, formation flight introduces new challenges and complex implications. Our code, based on Monte Carlo ray tracing, computes the full photon trajectories up to the detector plane, along with the relative drifts of the two spacecrafts. It takes into account angle and energy dependent interactions of the photons with the mirrors and applies to any grazing incidence telescope. The resulting images of simulated sources from 0.1 keV to 100 keV allow us to optimize the configuration of the instrument and to assess the performance of the Simbol-X telescope.

Chauvin, M.; Roques, J. P. [Universite de Toulouse, UPS, CESR, 9 ave colonel Roche, F-31028 Toulouse cedex 9 (France); CNRS, UMR5187, F-31028 Toulouse (France)

2009-05-11T23:59:59.000Z

136

Telescopic nanotube device for hot nanolithography  

DOE Patents [OSTI]

A device for maintaining a constant tip-surface distance for producing nanolithography patterns on a surface using a telescopic nanotube for hot nanolithography. An outer nanotube is attached to an AFM cantilever opposite a support end. An inner nanotube is telescopically disposed within the outer nanotube. The tip of the inner nanotube is heated to a sufficiently high temperature and brought in the vicinity of the surface. Heat is transmitted to the surface for thermal imprinting. Because the inner tube moves telescopically along the outer nanotube axis, a tip-surface distance is maintained constant due to the vdW force interaction, which in turn eliminates the need of an active feedback loop.

Popescu, Adrian; Woods, Lilia M

2014-12-30T23:59:59.000Z

137

Multimessenger astronomy with the Einstein Telescope  

E-Print Network [OSTI]

Gravitational waves (GWs) are expected to play a crucial role in the development of multimessenger astrophysics. The combination of GW observations with other astrophysical triggers, such as from gamma-ray and X-ray satellites, optical/radio telescopes, and neutrino detectors allows us to decipher science that would otherwise be inaccessible. In this paper, we provide a broad review from the multimessenger perspective of the science reach offered by the third generation interferometric GW detectors and by the Einstein Telescope (ET) in particular. We focus on cosmic transients, and base our estimates on the results obtained by ET's predecessors GEO, LIGO, and Virgo.

Eric Chassande-Mottin; Martin Hendry; Patrick J. Sutton; Szabolcs Mrka

2010-04-12T23:59:59.000Z

138

4 m Davies-Cotton telescope for the Cherenkov Telescope Array  

E-Print Network [OSTI]

The Cherenkov Telescope Array (CTA) is the next generation very high energy gamma-ray observatory. It will consist of three classes of telescopes, of large, medium and small sizes. The small telescopes, of 4 m diameter, will be dedicated to the observations of the highest energy gamma-rays, above several TeV. We present the technical characteristics of a single mirror, 4 m diameter, Davies-Cotton telescope for the CTA and the performance of the sub-array consisting of the telescopes of this type. The telescope will be equipped with a fully digital camera based on custom made, hexagonal Geiger-mode avalanche photodiodes. The development of cameras based on such devices is an RnD since traditionally photomultipliers are used. The photodiodes are now being characterized at various institutions of the CTA Consortium. Glass mirrors will be used, although an alternative is being considered: composite mirrors that could be adopted if they meet the project requirements. We present a design of the telescope structure,...

Moderski, R; Barnacka, A; Basili, A; Boccone, V; Bogacz, L; Cadoux, F; Christov, A; Della Volpe, M; Dyrda, M; Frankowski, A; Grudzi?ska, M; Janiak, M; Karczewski, M; Kasperek, J; Kocha?ski, W; Korohoda, P; Kozio?, J; Lubi?ski, P; Ludwin, J; Lyard, E; Marsza?ek, A; Micha?owski, J; Montaruli, T; Nicolau-Kukli?ski, J; Niemiec, J; Ostrowski, M; P?atos, ?; Rajda, P J; Rameez, M; Romaszkan, W; Rupi?ski, M; Seweryn, K; Stodulska, M; Stodulski, M; Walter, R; Winiarski, K; Wi?niewski, ?; Zagda?ski, A; Zietara, K; Zi?kowski, P; ?ychowski, P

2013-01-01T23:59:59.000Z

139

Optical Technology Needs for Future Space Telescopes  

E-Print Network [OSTI]

instruments & sensors. Future Space Telescopes will operate over broad spectrum: Gamma Rays, X-Rays, XUV and Sensors Direct Sensing of Particles, Fields and Waves See Scientific Instruments and Sensors (SIS Structure #12;NASA's Science Missions Directorate Themes: Earth Science Sun-Solar System Connection Solar

Van Stryland, Eric

140

Pendular seismometer for correcting telescope vibrations  

Science Journals Connector (OSTI)

......Southern Observatory, Karl Schwarzschild Strabetae, 2, D-85748 Garching...is suggested that a pendular mirror in front of the telescope is...optics system or by a secondary mirror. An alternative technique...angular motions of the primary mirror cell. One may suggest monitoring......

A. Tokovinin

2000-08-11T23:59:59.000Z

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


141

The High Energy Telescope on EXIST  

E-Print Network [OSTI]

The Energetic X-ray Imaging Survey Telescope (EXIST) is a proposed next generation multi-wavelength survey mission. The primary instrument is a High Energy telescope (HET) that conducts the deepest survey for Gamma-ray Bursts (GRBs), obscured-accreting and dormant Supermassive Black Holes and Transients of all varieties for immediate followup studies by the two secondary instruments: a Soft X-ray Imager (SXI) and an Optical/Infrared Telescope (IRT). EXIST will explore the early Universe using high redshift GRBs as cosmic probes and survey black holes on all scales. The HET is a coded aperture telescope employing a large array of imaging CZT detectors (4.5 m^2, 0.6 mm pixel) and a hybrid Tungsten mask. We review the current HET concept which follows an intensive design revision by the HET imaging working group and the recent engineering studies in the Instrument and Mission Design Lab at the Goddard Space Flight Center. The HET will locate GRBs and transients quickly (<10-30 sec) and accurately (< 20") f...

Hong, J; Allen, B; Barthelmy, S D; Skinner, G K; Gehrels, N

2009-01-01T23:59:59.000Z

142

Abstract In the years since Charles Elton proposed that more diverse communities should be less susceptible to  

E-Print Network [OSTI]

: J.S. Dukes, Department of Biology, University of Utah, 257 S. 1400 East, Salt Lake City, UT 84112Abstract In the years since Charles Elton proposed that more diverse communities should be less

Dukes, Jeffrey

143

Thermal Decomposition of a Melt-Castable High Explosive: Isoconversional Analysis of Gregory T. Long and Charles A. Wight*  

E-Print Network [OSTI]

, Salt Lake City, Utah 84112 ReceiVed: July 24, 2001; In Final Form: December 6, 2001 The thermal. Long and Charles A. Wight* Center for Thermal Analysis, Department of Chemistry, UniVersity of Utah

Utah, University of

144

A Prototype System For Synergistic Data Display J. Dean Brederson Milan Ikits Christopher R. Johnson Charles D. Hansen  

E-Print Network [OSTI]

of Utah 50 Central Campus Drive Rm 3490 Salt Lake City, UT 84112-9205, USA {jdb, ikits, crj, hansen. Johnson Charles D. Hansen Scientific Computing and Imaging Institute School of Computing, University

Utah, University of

145

Lithium isotopes in global mid-ocean ridge basalts Paul B. Tomascak a,*, Charles H. Langmuir b  

E-Print Network [OSTI]

Lithium isotopes in global mid-ocean ridge basalts Paul B. Tomascak a,*, Charles H. Langmuir b January 2008 Abstract The lithium isotope compositions of 30 well-characterized samples of glassy lavas

Langmuir, Charles H.

146

The Department of Anthropology, International Relations, The Fares Center for Eastern Mediterranean Studies, The Charles Smith Endowment Fund, Commu-  

E-Print Network [OSTI]

Studies, The Charles Smith Endowment Fund, Commu- nications and Media Studies, The Institute for Global from state pressures and challenged Palestinian political norms about news media. This is also a story

Tufts University

147

E-Print Network 3.0 - apex telescope large Sample Search Results  

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

Telescopes Reference Reading Summary: telescopes are good for small telescopes (<1 meter) because it's very difficult to manufacture large lenses... fast system bright...

148

Universit Charles-de-Gaulle Lille III Ecole doctorale Sciences de l'Homme et de la Socit  

E-Print Network [OSTI]

à Salt Lake City, ancienne directrice du département de danse moderne de l'Université dUniversité Charles-de-Gaulle ­ Lille III Ecole doctorale « Sciences de l'Homme et de la Société,version1-8Nov2013 #12;Université Charles-de-Gaulle ­ Lille III Ecole doctorale « Sciences de l'Homme et de

Paris-Sud XI, Université de

149

Large-Aperture Segmented Mirror Telescope Design Concept  

E-Print Network [OSTI]

(ATLAS) Telescope: A Technology Roadmap for the Next Decade Principal Investigator: Dr. Marc Postman .............................................................................................13 5 Technology Roadmap................................................................109 #12;Advanced Technology Large-Aperture Space Telescope: A Technology Roadmap for the Next Decade 2

Sirianni, Marco

150

Categorical Exclusion Determination Form Proposed Action Title: (0473-1529) Charles River Associates International Inc. -  

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

29) Charles River Associates International Inc. - 29) Charles River Associates International Inc. - Transmission Topology Control for Infrastructure Resilience to the Integration of Renewable Generation Program or Field Office: Advanced Research Projects Agency - Energy Location(s) (City/County/State): Massachusetts, Pennsylvania, Washington Proposed Action Description: Funding will support development of Topology Control, an algorithmic and software technology framework that will improve the efficiency of the electrical grid by implementing appropriate short-term changes of transmission line status to manage transmission congestion and uncertainties associated with integration of renewable generation sources into the electricity grid. Proposed work consists of (1) developing and validating a large power system model that accurately simulates day-ahead and intra-day power

151

AUTHORS: Annika Todd, Peter Cappers, Charles Goldman Environmental Energy Technologies Division  

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

AUTHORS: AUTHORS: Annika Todd, Peter Cappers, Charles Goldman Environmental Energy Technologies Division Lawrence Berkeley National Laboratory June 2013 LBNL-6247E Residential Customer Enrollment in Time-based Rate and Enabling Technology Programs iii Acknowledgments The work described in this report was supported by the U.S. Department of Energy's Office of Electricity Delivery and Energy Reliability (DOE OE) under Lawrence Berkeley National Laboratory Contract No. DE-AC02-05CH11231. The authors would like to thank Joe Paladino (DOE OE) for his support. The authors would also like to thank the members of the LBNL Technical Advisory Group who contributed their wisdom and guidance: Peter Cappers, Annika Todd, Charles Goldman and Andy Satchwell (LBNL); Catherine Wolfram, Meredith Fowlie, and Lucas Davis (University of

152

An integrated decision aid system for the development of Saint Charles River alluvial plain, Quebec, Canada  

Science Journals Connector (OSTI)

We describe an integrated decision aid system designed to assist land-use planning and management of the alluvial plain of Saint Charles River, Quebec. The first stages of the development of the system consisted in building a georeferenced database managed by a geographical information system (GIS), and to elaborate eight different development scenarios along the Saint Charles River in a multiple decision-maker context. Multicriteria analysis (MCA) was then used to evaluate and compare the scenarios according to eleven criteria, using a combination of GIS analysis with Mapinfo and multicriteria processing carried out in PROMCALC & GAIA 3.5. This process leads to a partial ranking (PROMETHEE I) and a complete ranking of the scenarios (PROMETHEE II) for each individual decision-maker as well as for the whole group. We show that this approach helps multiple decision-makers to reach rational decisions based on scientific data and political considerations.

Nadine J. Martin; Benoit St Onge; Jean-Philippe Waaub

1999-01-01T23:59:59.000Z

153

Charles Motel & Bathhouse Pool & Spa Low Temperature Geothermal Facility |  

Open Energy Info (EERE)

Motel & Bathhouse Pool & Spa Low Temperature Geothermal Facility Motel & Bathhouse Pool & Spa Low Temperature Geothermal Facility Jump to: navigation, search Name Charles Motel & Bathhouse Pool & Spa Low Temperature Geothermal Facility Facility Charles Motel & Bathhouse Sector Geothermal energy Type Pool and Spa Location Truth or Consequences, New Mexico Coordinates 33.1284047°, -107.2528069° Loading map... {"minzoom":false,"mappingservice":"googlemaps3","type":"ROADMAP","zoom":14,"types":["ROADMAP","SATELLITE","HYBRID","TERRAIN"],"geoservice":"google","maxzoom":false,"width":"600px","height":"350px","centre":false,"title":"","label":"","icon":"","visitedicon":"","lines":[],"polygons":[],"circles":[],"rectangles":[],"copycoords":false,"static":false,"wmsoverlay":"","layers":[],"controls":["pan","zoom","type","scale","streetview"],"zoomstyle":"DEFAULT","typestyle":"DEFAULT","autoinfowindows":false,"kml":[],"gkml":[],"fusiontables":[],"resizable":false,"tilt":0,"kmlrezoom":false,"poi":true,"imageoverlays":[],"markercluster":false,"searchmarkers":"","locations":[]}

154

Telescoping MATLAB for DSP Applications PhD Thesis Defense  

E-Print Network [OSTI]

Telescoping MATLAB for DSP Applications PhD Thesis Defense Arun Chauhan Computer Science, Rice University PhD Thesis Defense July 10, 2003 #12;Two True Stories PhD Thesis Defense: Telescoping MATLABD Thesis Defense: Telescoping MATLAB for DSP Applications July 10, 2003 #12;Two True Stories · the world

Chauhan, Arun

155

A review of "The Long Parliament of Charles II" by Annabel Patterson  

E-Print Network [OSTI]

52 seventeenth-century news Annabel Patterson. The Long Parliament of Charles II. New Haven: YaleUniversity Press, 2008. vii + 283 pp. $45.00. Review by richard c. taylor, east carolina university. On one level, this audacious, frustrating... involved in resisting chronological narrative. She chides those of her colleagues who present copious concat- enations of sources without engaging those sources with the sort of reviews 53 rhetorical skill and sensitivity she can bring to her more...

Taylor, Richard C.

2010-01-01T23:59:59.000Z

156

High Energy Cosmic Rays from Local GRBs Armen Atoyan 1 and Charles D. Dermer 2  

E-Print Network [OSTI]

. The origin of the ankle in the CR spectrum at Eank # 4 ? 10 18 eV is due to photopair energy losses of UHECRsHigh Energy Cosmic Rays from Local GRBs Armen Atoyan 1 and Charles D. Dermer 2 1 CRM, Universit rays with energies E between # 0.1 - 1 PeV and the energy of the second knee at E2 # 3 ? 10 17 e

157

Telescoping magnetic ball bar test gage  

DOE Patents [OSTI]

A telescoping magnetic ball bar test gage for determining the accuracy of machine tools, including robots, and those measuring machines having non-disengagable servo drives which cannot be clutched out. Two gage balls are held and separated from one another by a telescoping fixture which allows them relative radial motional freedom but not relative lateral motional freedom. The telescoping fixture comprises a parallel reed flexure unit and a rigid member. One gage ball is secured by a magnetic socket knuckle assembly which fixes its center with respect to the machine being tested. The other gage ball is secured by another magnetic socket knuckle assembly which is engaged or held by the machine in such manner that the center of that ball is directed to execute a prescribed trajectory, all points of which are equidistant from the center of the fixed gage ball. As the moving ball executes its trajectory, changes in the radial distance between the centers of the two balls caused by inaccuracies in the machine are determined or measured by a linear variable differential transformer (LVDT) assembly actuated by the parallel reed flexure unit. Measurements can be quickly and easily taken for multiple trajectories about several different fixed ball locations, thereby determining the accuracy of the machine.

Bryan, J.B.

1982-03-15T23:59:59.000Z

158

Telescoping magnetic ball bar test gage  

DOE Patents [OSTI]

A telescoping magnetic ball bar test gage for determining the accuracy of machine tools, including robots, and those measuring machines having non-disengageable servo drives which cannot be clutched out. Two gage balls (10, 12) are held and separated from one another by a telescoping fixture which allows them relative radial motional freedom but not relative lateral motional freedom. The telescoping fixture comprises a parallel reed flexure unit (14) and a rigid member (16, 18, 20, 22, 24). One gage ball (10) is secured by a magnetic socket knuckle assembly (34) which fixes its center with respect to the machine being tested. The other gage ball (12) is secured by another magnetic socket knuckle assembly (38) which is engaged or held by the machine in such manner that the center of that ball (12) is directed to execute a prescribed trajectory, all points of which are equidistant from the center of the fixed gage ball (10). As the moving ball (12) executes its trajectory, changes in the radial distance between the centers of the two balls (10, 12) caused by inaccuracies in the machine are determined or measured by a linear variable differential transformer (LVDT) assembly (50, 52, 54, 56, 58, 60) actuated by the parallel reed flexure unit (14). Measurements can be quickly and easily taken for multiple trajectories about several different fixed ball (10) locations, thereby determining the accuracy of the machine.

Bryan, James B. (Pleasanton, CA)

1984-01-01T23:59:59.000Z

159

Development of a mid-sized Schwarzschild-Couder Telescope for the Cherenkov Telescope Array  

SciTech Connect (OSTI)

The Cherenkov Telescope Array (CTA) is a ground-based observatory for very high-energy (10 GeV to 100 TeV) gamma rays, planned for operation starting in 2018. It will be an array of dozens of optical telescopes, known as Atmospheric Cherenkov Telescopes (ACTs), of 8 m to 24 m diameter, deployed over an area of more than 1 square km, to detect flashes of Cherenkov light from showers initiated in the Earth's atmosphere by gamma rays. CTA will have improved angular resolution, a wider energy range, larger fields of view and an order of magnitude improvement in sensitivity over current ACT arrays such as H.E.S.S., MAGIC and VERITAS. Several institutions have proposed a research and development program to eventually contribute 36 medium-sized telescopes (9 m to 12 m diameter) to CTA to enhance and optimize its science performance. The program aims to construct a prototype of an innovative, Schwarzschild-Couder telescope (SCT) design that will allow much smaller and less expensive cameras and much larger fields of view than conventional Davies-Cotton designs, and will also include design and testing of camera electronics for the necessary advances in performance, reliability and cost. We report on the progress of the mid-sized SCT development program.

Cameron, Robert A.

2012-06-28T23:59:59.000Z

160

The dual-mirror Small Size Telescope for the Cherenkov Telescope Array  

E-Print Network [OSTI]

In this paper, the development of the dual mirror Small Size Telescopes (SST) for the Cherenkov Telescope Array (CTA) is reviewed. Up to 70 SST, with a primary mirror diameter of 4 m, will be produced and installed at the CTA southern site. These will allow investigation of the gamma-ray sky at the highest energies accessible to CTA, in the range from about 1 TeV to 300 TeV. The telescope presented in this contribution is characterized by two major innovations: the use of a dual mirror Schwarzschild-Couder configuration and of an innovative camera using as sensors either multi-anode photomultipliers (MAPM) or silicon photomultipliers (SiPM). The reduced plate-scale of the telescope, achieved with the dual-mirror optics, allows the camera to be compact (40 cm in diameter), and low-cost. The camera, which has about 2000 pixels of size 6x6 mm^2, covers a field of view of 10{\\deg}. The dual mirror telescopes and their cameras are being developed by three consortia, ASTRI (Astrofisica con Specchi a Tecnologia Repl...

Pareschi, G; Antonelli, L A; Bastieri, D; Bellassai, G; Belluso, M; Bigongiari, C; Billotta, S; Biondo, B; Bonanno, G; Bonnoli, G; Bruno, P; Bulgarelli, A; Canestrari, R; Capalbi, M; Caraveo, P; Carosi, A; Cascone, E; Catalano, O; Cereda, M; Conconi, P; Conforti, V; Cusumano, G; De Caprio, V; De Luca, A; Di Paola, A; Di Pierro, F; Fantinel, D; Fiorini, M; Fugazza, D; Gardiol, D; Ghigo, M; Gianotti, F; Giarrusso, S; Giro, E; Grillo, A; Impiombato, D; Incorvaia, S; La Barbera, A; La Palombara, N; La Parola, V; La Rosa, G; Lessio, L; Leto, G; Lombardi, S; Lucarelli, F; Maccarone, M C; Malaguti, G; Malaspina, G; Mangano, V; Marano, D; Martinetti, E; Millul, R; Mineo, T; Mist, A; Morello, C; Morlino, G; Panzera, M R; Rodeghiero, G; Romano, P; Russo, F; Sacco, B; Sartore, N; Schwarz, J; Segreto, A; Sironi, G; Sottile, G; Stamerra, A; Strazzeri, E; Stringhetti, L; Tagliaferri, G; Testa, V; Timpanaro, M C; Toso, G; Tosti, G; Trifoglio, M; Vallania, P; Vercellone, S; Zitelli, V; Amans, J P; Boisson, C; Costille, C; Dournaux, J L; Dumas, D; Fasola, G; Hervet, O; Huet, J M; Laporte, P; Rulten, C; Sol, H; Zech, A; White, R; Hinton, J; Ross, D; Sykes, J; Ohm, S; Schmoll, J; Chadwick, P; Greenshaw, T; Daniel, M; Cotter, G; Varner, G S; Funk, S; Vandenbroucke, J; Sapozhnikov, L; Buckley, J; Moore, P; Williams, D; Markoff, S; Vink, J; Berge, D; Hidaka, N; Okumura, A; Tajima, H

2013-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "telescope baltay charles" 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

E-Print Network 3.0 - antares neutrino telescope Sample Search...  

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

oscillation parameters. Keywords: neutrino oscillations, ANTARES, neutrino telescope 1 Introduction It is now... energy neutrino telescopes, whose energy threshold is...

162

The dual-mirror Small Size Telescope for the Cherenkov Telescope Array  

E-Print Network [OSTI]

In this paper, the development of the dual mirror Small Size Telescopes (SST) for the Cherenkov Telescope Array (CTA) is reviewed. Up to 70 SST, with a primary mirror diameter of 4 m, will be produced and installed at the CTA southern site. These will allow investigation of the gamma-ray sky at the highest energies accessible to CTA, in the range from about 1 TeV to 300 TeV. The telescope presented in this contribution is characterized by two major innovations: the use of a dual mirror Schwarzschild-Couder configuration and of an innovative camera using as sensors either multi-anode photomultipliers (MAPM) or silicon photomultipliers (SiPM). The reduced plate-scale of the telescope, achieved with the dual-mirror optics, allows the camera to be compact (40 cm in diameter), and low-cost. The camera, which has about 2000 pixels of size 6x6 mm^2, covers a field of view of 10{\\deg}. The dual mirror telescopes and their cameras are being developed by three consortia, ASTRI (Astrofisica con Specchi a Tecnologia Replicante Italiana, Italy/INAF), GATE (Gamma-ray Telescope Elements, France/Paris Observ.) and CHEC (Compact High Energy Camera, universities in UK, US and Japan) which are merging their efforts in order to finalize an end-to-end design that will be constructed for CTA. A number of prototype structures and cameras are being developed in order to investigate various alternative designs. In this contribution, these designs are presented, along with the technological solutions under study.

G. Pareschi; G. Agnetta; L. A. Antonelli; D. Bastieri; G. Bellassai; M. Belluso; C. Bigongiari; S. Billotta; B. Biondo; G. Bonanno; G. Bonnoli; P. Bruno; A. Bulgarelli; R. Canestrari; M. Capalbi; P. Caraveo; A. Carosi; E. Cascone; O. Catalano; M. Cereda; P. Conconi; V. Conforti; G. Cusumano; V. De Caprio; A. De Luca; A. Di Paola; F. Di Pierro; D. Fantinel; M. Fiorini; D. Fugazza; D. Gardiol; M. Ghigo; F. Gianotti; S. Giarrusso; E. Giro; A. Grillo; D. Impiombato; S. Incorvaia; A. La Barbera; N. La Palombara; V. La Parola; G. La Rosa; L. Lessio; G. Leto; S. Lombardi; F. Lucarelli; M. C. Maccarone; G. Malaguti; G. Malaspina; V. Mangano; D. Marano; E. Martinetti; R. Millul; T. Mineo; A. Mist; C. Morello; G. Morlino; M. R. Panzera; G. Rodeghiero; P. Romano; F. Russo; B. Sacco; N. Sartore; J. Schwarz; A. Segreto; G. Sironi; G. Sottile; A. Stamerra; E. Strazzeri; L. Stringhetti; G. Tagliaferri; V. Testa; M. C. Timpanaro; G. Toso; G. Tosti; M. Trifoglio; P. Vallania; S. Vercellone; V. Zitelli; For The Astri Collaboration; J. P. Amans; C. Boisson; C. Costille; J. L. Dournaux; D. Dumas; G. Fasola; O. Hervet; J. M. Huet; P. Laporte; C. Rulten; H. Sol; A. Zech; For The Gate Collaboration; R. White; J. Hinton; D. Ross; J. Sykes; S. Ohm; J. Schmoll; P. Chadwick; T. Greenshaw; M. Daniel; G. Cotter; G. S. Varner; S. Funk; J. Vandenbroucke; L. Sapozhnikov; J. Buckley; P. Moore; D. Williams; S. Markoff; J. Vink; D. Berge; N. Hidaka; A. Okumura; H. Tajima; For The Chec Collaboration; For The Cta Consortium

2013-07-18T23:59:59.000Z

163

ANTARES deep sea neutrino telescope results  

SciTech Connect (OSTI)

The ANTARES experiment is currently the largest underwater neutrino telescope in the Northern Hemisphere. It is taking high quality data since 2007. Its main scientific goal is to search for high energy neutrinos that are expected from the acceleration of cosmic rays from astrophysical sources. This contribution reviews the status of the detector and presents several analyses carried out on atmospheric muons and neutrinos. For example it shows the results from the measurement of atmospheric muon neutrino spectrum and of atmospheric neutrino oscillation parameters as well as searches for neutrinos from steady cosmic point-like sources, for neutrinos from gamma ray bursts and for relativistic magnetic monopoles.

Mangano, Salvatore [IFIC - Instituto de Fsica Corpuscular, Edificio Institutos de Investigatin, 46071 Valencia (Spain); Collaboration: ANTARES Collaboration

2014-06-24T23:59:59.000Z

164

LOFAR, a new low frequency radio telescope  

E-Print Network [OSTI]

LOFAR, the Low Frequency Array, is a large radio telescope consisting of approximately 100 soccer-field sized antenna stations spread over a region of 400 km in diameter. It will operate at frequencies from ~10 to 240 MHz, with a resolution at 240 MHz of better than an arcsecond. Its superb sensitivity will allow for studies of a broad range of astrophysical topics, including reionisation, transient radio sources and cosmic rays, distant galaxies and AGNs. In this contribution a status rapport of the LOFAR project and an overview of the science case is presented.

H. J. A. Rottgering

2003-09-19T23:59:59.000Z

165

David D. Celentano, Charles Armstrong Chair and Professor, Department of Epidemiology 615 North Wolfe Street, Suite W6041 Baltimore, MD 21205 Tel: 410.955.3286 Fax: 410.614.0467 dcelenta@jhsph.edu  

E-Print Network [OSTI]

David D. Celentano, Charles Armstrong Chair and Professor, Department of Epidemiology 615 North and infectious diseases who despite his premature #12;David D. Celentano, Charles Armstrong Chair and Professor

Scharfstein, Daniel

166

A 16-m Telescope for the Advanced Technology Large Aperture Telescope (ATLAST) Mission  

E-Print Network [OSTI]

for the telescope and its instruments. Solar array panels, an antenna and a solar sail are also folded up against compartment which is attached to a spacecraft bus which provides power, attitude control and communications and is separated from the launch vehicle, its solar arrays and high gain antenna will be deployed

Sirianni, Marco

167

AGN Physics with the Cherenkov Telescope Array  

E-Print Network [OSTI]

The Cherenkov Telescope Array (CTA), currently in its Preparatory Phase, will be the first open observatory for very high energy gamma-rays from galactic and extragalactic sources. The international consortium behind CTA is preparing the construction of two large arrays of Cherenkov telescopes in the Northern and Southern Hemispheres with a performance that will be significantly improved compared to the current generation of arrays. Its increased sensitivity and energy range will give CTA access to a large population of Active Galactic Nuclei (AGN) not yet detected at very high energies and provide much more details on known TeV sources. While the low end of the CTA energy coverage will close the current gap with the Fermi-LAT band, its high energy coverage will open a new window on the sky and help us understand the intrinsic shape of the hardest blazar spectra. We outline the current status of CTA and discuss the science case for AGN physics with the observatory. Predictions for source detections based on e...

Zech, A

2012-01-01T23:59:59.000Z

168

Fermi Large Area Telescope Third Source Catalog  

E-Print Network [OSTI]

We present the third Fermi Large Area Telescope source catalog (3FGL) of sources in the 100~MeV--300~GeV range. Based on the first four years of science data from the Fermi Gamma-ray Space Telescope mission, it is the deepest yet in this energy range. Relative to the 2FGL catalog, the 3FGL catalog incorporates twice as much data as well as a number of analysis improvements, including improved calibrations at the event reconstruction level, an updated model for Galactic diffuse gamma-ray emission, a refined procedure for source detection, and improved methods for associating LAT sources with potential counterparts at other wavelengths. The 3FGL catalog includes 3033 sources above 4 sigma significance, with source location regions, spectral properties, and monthly light curves for each. Of these, 78 are flagged as potentially being due to imperfections in the model for Galactic diffuse emission. Twenty-five sources are modeled explicitly as spatially extended, and overall 232 sources are considered as identifie...

,

2015-01-01T23:59:59.000Z

169

The X-ray Telescope of CAST  

E-Print Network [OSTI]

The Cern Axion Solar Telescope (CAST) is in operation and taking data since 2003. The main objective of the CAST experiment is to search for a hypothetical pseudoscalar boson, the axion, which might be produced in the core of the sun. The basic physics process CAST is based on is the time inverted Primakoff effect, by which an axion can be converted into a detectable photon in an external electromagnetic field. The resulting X-ray photons are expected to be thermally distributed between 1 and 7 keV. The most sensitive detector system of CAST is a pn-CCD detector combined with a Wolter I type X-ray mirror system. With the X-ray telescope of CAST a background reduction of more than 2 orders off magnitude is achieved, such that for the first time the axion photon coupling constant g_agg can be probed beyond the best astrophysical constraints g_agg < 1 x 10^-10 GeV^-1.

M. Kuster; H. Bruninger; S. Cbrian; M. Davenport; C. Elefteriadis; J. Englhauser; H. Fischer; J. Franz; P. Friedrich; R. Hartmann; F. H. Heinsius; D. H. H. Hoffmann; G. Hoffmeister; J. N. Joux; D. Kang; K. Knigsmann; R. Kotthaus; T. Papaevangelou; C. Lasseur; A. Lippitsch; G. Lutz; J. Morales; A. Rodrguez; L. Strder; J. Vogel; K. Zioutas

2007-05-10T23:59:59.000Z

170

Sanders, J. E.; and Merguerian, Charles, 1995b, New York City region: Unique testing ground for flow models of Quaternary continental glaciers.  

E-Print Network [OSTI]

Sanders, J. E.; and Merguerian, Charles, 1995b, New York City region: Unique testing ground City came from the NNE (from the "Labrador center"). When ice blocked the N end of Hudson Bay and Lake This Abstract: Sanders, J. E.; and Merguerian, Charles, 1995b, New York City region: Unique testing ground

Merguerian, Charles

171

Integral Field Spectroscopy with the Gemini 8-m Telescopes  

E-Print Network [OSTI]

We give an overview of the current and future IFU capabilities on the Gemini 8-m telescopes. The telescopes are well-suited to integral field spectroscopy and both telescopes will have optical and near-infrared IFUs within the next few years. Commissioning for the GMOS IFU on Gemini North has begun recently and it is now available to the community. Future integral field instruments will take advantage of wide-field adaptive optics systems.

B. W. Miller; J. Turner; M. Takamiya; D. Simons; I. Hook

2002-03-20T23:59:59.000Z

172

MEMORANDUM FOR DISTRIBUTION FROM: CHARLES E. ANDERSON PRINCIPAL DEPUTY ASSISTANT SECRETARY FOR  

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

- - - Washington, DC 20585 April 4 , 2007 MEMORANDUM FOR DISTRIBUTION FROM: CHARLES E. ANDERSON PRINCIPAL DEPUTY ASSISTANT SECRETARY FOR ENVIRONMENTAL MANAGEMENT SUBJECT: Requirements to Coordinate Regulatory Negotiations with the Office of Regulatory Compliance In a memorandum dated December 28,2006, Assistant Secretary Rispoli announced the dissolution of the Office of Environmental Management (EM) Configuration Control Board and . the creation of a new EM Acquisition Advisory Board (EMAAB). In addition to setting forth the matters that now fall within the EMAABYs purview, the December 28,2006, memorandum also made clear that EM will maintain configuration control over, among other things, regulatory decision documents. Accordingly, the relevant Acquisition Executive must approve any

173

A review of "Royal Survivor: A Life of Charles II." by Stephen Coote  

E-Print Network [OSTI]

of Charles II. New York: St. Martin?s Press, 2000. xiv + 396 pp. Includes b & w plates. $27.95. (First published in the UK by Hodder and Stoughton.) Review by BRYAN N.S. GOOCH, UNIVERSITY OF VICTORIA. Stephen Coote?s Royal Survivor is more than a well... Duke of Buckingham in 1628), experiencing some forays in matters aca- demic (Thomas Hobbes made a sometime august tutor in math- ematics), meeting the young Louis XIV, tasting the fringes (amatory and otherwise) of the French court under the less than...

Bryan N.S. Gooch

2002-01-01T23:59:59.000Z

174

The Robotic Super-LOTIS Telescope: Results & Future Plans  

E-Print Network [OSTI]

We provide an overview of the robotic Super-LOTIS (Livermore Optical Transient Imaging System) telescope and present results from gamma-ray burst (GRB) afterglow observations using Super-LOTIS and other Steward Observatory telescopes. The 0.6-m Super-LOTIS telescope is a fully robotic system dedicated to the measurement of prompt and early time optical emission from GRBs. The system began routine operations from its Steward Observatory site atop Kitt Peak in April 2000 and currently operates every clear night. The telescope is instrumented with an optical CCD camera and a four position filter wheel. It is capable of observing Swift Burst Alert Telescope (BAT) error boxes as early or earlier than the Swift UV/Optical Telescope (UVOT). Super-LOTIS complements the UVOT observations by providing early R- and I-band imaging. We also use the suite of Steward Observatory telescopes including the 1.6-m Kuiper, the 2.3-m Bok, the 6.5-m MMT, and the 8.4-m Large Binocular Telescope to perform follow-up optical and near infrared observations of GRB afterglows. These follow-up observations have traditionally required human intervention but we are currently working to automate the 1.6-m Kuiper telescope to minimize its response time.

G. G. Williams; P. A. Milne; H. S. Park; S. D. Barthelmy; D. H. Hartmann; A. Updike; K. Hurley

2008-02-29T23:59:59.000Z

175

Automation of the design of a telescopic zoom system  

Science Journals Connector (OSTI)

This paper discusses the theoretical bases of the construction and computation of the parameters of a telescopic zoom system. A mathematical model and algorithm has been developed,...

Van Luen, Nguen

2013-01-01T23:59:59.000Z

176

Development of an ASIC for Dual Mirror Telescopes of the Cherenkov Telescope Array  

E-Print Network [OSTI]

We have developed an application-specific integrated circui (ASIC) for photomultipler tube (PMT) waveform digitization which is well-suited for the Schwarzschild-Couder optical system under development for the Cherenkov Telescope Array (CTA) project. The key feature of the "TARGET" ASIC is the ability to read 16 channels in parallel at a sampling speed of 1 GSa/s or faster. In combination with a focal plane instrumented with 64-channel multi-anode PMTs (MAPMTs), TARGET digitizers will enable CTA to achieve a wider field of view than the current Cherenkov telescopes and significantly reduce the cost per channel of the camera and readout electronics. We have also developed a prototype camera module, consisting of 4 TARGET ASICs and a 64-channel MAPMT. We report results from performance testing of the camera module and of the TARGET ASIC itself.

Vandenbroucke, Justin; Funk, Stefan; Okumura, Akira; Tajima, Hiro; Varner, Gary

2011-01-01T23:59:59.000Z

177

TECHNOLOGY DEVELOPMENT PROJECT PLAN Advanced Technology Large Aperture Space Telescope  

E-Print Network [OSTI]

(ATLAST) A Roadmap for UVIOR Technology, 2010-2020 24 April, 2009 T. Tupper Hyde, ATLAST TechnologistTECHNOLOGY DEVELOPMENT PROJECT PLAN for the Advanced Technology Large Aperture Space Telescope, and Ronald Polidan. #12;Advanced Technology Large-Aperture Space Telescope (ATLAST) 22 TABLE OF CONTENTS 1

Sirianni, Marco

178

THE CHERENKOV TELESCOPE ARRAY for the CTA Consortium  

E-Print Network [OSTI]

The Cherenkov Telescope Array (CTA) is a next-generation observatory proposed for very high-energy gamma rays imaging air Cherenkov telescopes (IACTs), cover an energy range of about four decades (from a few tens of GeV to above 100 TeV), and to enhance angular and energy resolutions. CTA will have a large discovery

Boyer, Edmond

179

Muon Telescope By Nandita Sampath and Izzy Harrison  

E-Print Network [OSTI]

Muon Telescope By Nandita Sampath and Izzy Harrison #12;Abstract We wanted to determine whether the count rate of muons per hour would be affected if we changed the angle that our muon telescope pointed to the roof of the parking garage so the muons could not be affected by surrounding

California at Santa Cruz, University of

180

Atmospheric dispersion in very large telescopes with adaptive optics  

Science Journals Connector (OSTI)

......be put facing the telescope mirrors and theplano-convex lens...the beam of light from the mirrors to the focus to a collimated...lenses, and similarly the Schwarzschild (1905a, b, c) coefficients...31 cmto telescope focus mirror I I I I I T I~ 6.540 0......

Charles G. Wynne

1997-02-11T23:59:59.000Z

Note: This page contains sample records for the topic "telescope baltay charles" 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

SST-GATE: A dual mirror telescope for the Cherenkov Telescope Array  

E-Print Network [OSTI]

The Cherenkov Telescope Array (CTA) will be the world's first open observatory for very high energy gamma-rays. Around a hundred telescopes of different sizes will be used to detect the Cherenkov light that results from gamma-ray induced air showers in the atmosphere. Amongst them, a large number of Small Size Telescopes (SST), with a diameter of about 4 m, will assure an unprecedented coverage of the high energy end of the electromagnetic spectrum (above ~1TeV to beyond 100 TeV) and will open up a new window on the non-thermal sky. Several concepts for the SST design are currently being investigated with the aim of combining a large field of view (~9 degrees) with a good resolution of the shower images, as well as minimizing costs. These include a Davies-Cotton configuration with a Geiger-mode avalanche photodiode (GAPD) based camera, as pioneered by FACT, and a novel and as yet untested design based on the Schwarzschild-Couder configuration, which uses a secondary mirror to reduce the plate-scale and to all...

Zech, A; Blake, S; Boisson, C; Costille, C; De-Frondat, F; Dournaux, J -L; Dumas, D; Fasola, G; Greenshaw, T; Hervet, O; Huet, J -M; Laporte, P; Rulten, C; Savoie, D; Sayede, F; Schmoll, J

2013-01-01T23:59:59.000Z

182

The Large Genome Constraint Hypothesis: Evolution, Ecology and Phenotype CHARLES A. KNIGHT1,* , NICOLE A. MOLINARI1  

E-Print Network [OSTI]

The Large Genome Constraint Hypothesis: Evolution, Ecology and Phenotype CHARLES A. KNIGHT1 Accepted: 18 March 2004 Background and Aims If large genomes are truly saturated with unnecessary `junk genome constraint'. We examine the large genome constraint at three scales: evolution, ecology

Petrov, Dmitri

183

The Role of Adsorbed Water on the Friction of a Layer of Submicron Particles CHARLES G. SAMMIS,1  

E-Print Network [OSTI]

The Role of Adsorbed Water on the Friction of a Layer of Submicron Particles CHARLES G. SAMMIS,1 of a one nanometer thick layer of water adsorbed on the particles. The observed tran- sition from normal the extrusion time and the particles in a force chain never come into direct contact. If the adsorbed water

Ze'ev, Reches

184

Quantifying Wasted Write Energy in the Memory Hierarchy Charles Shelor, Jim Buchanan, and Krishna Kavi Ron Cytron  

E-Print Network [OSTI]

Quantifying Wasted Write Energy in the Memory Hierarchy Charles Shelor, Jim Buchanan, and Krishna. Wasted writes consume energy, consume execution time as memory bandwidth and consume component lifetime of potential energy savings that can be obtained from eliminating wasted writes. If all of the wasted writes

Kavi, Krishna

185

Measure the Crack Instead of Construction Vibrations by Charles H. Dowding, Ph.D., P.E.  

E-Print Network [OSTI]

Measure the Crack Instead of Construction Vibrations by Charles H. Dowding, Ph.D., P.E. Figure 1 to address fears of vibration-induced cracking by directly measuring crack response. Relatively inexpensive. HOUSE AND CRACK RESPONSE TO VIBRATIONS Crack measurement concepts are illustrated by the response

186

School of Arts and Sciences and Engineering Student Financial Services 3400 N Charles Street 146 Garland Hall Baltimore, MD 21218  

E-Print Network [OSTI]

School of Arts and Sciences and Engineering Student Financial Services 3400 N Charles Street 146 Cancel Fall/Spring Fall Only Spring Only Summer Only Fall/Spring/Summer $ _________ $ _________ Unsubsidized Increase Decrease Cancel Fall/Spring Fall Only Spring Only Summer Only Fall/Spring

Weaver, Harold A. "Hal"

187

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

188

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

E-Print Network [OSTI]

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

189

Real-time condition assessment of RAPTOR telescope systems  

SciTech Connect (OSTI)

The RAPid Telescopes for Optical Response (RAPTOR) observatory network consists of several robotic astronomical telescopes primarily designed to search for astrophysical transients called a gamma-ray bursts (GRBs). Although intrinsically bright, GRBs are difficult to detect because of their short duration. Typically, they are first observed by satellites that then relay the coordinates of the GRB to a ground station which, in turn, distributes the coordinates over the internet so that ground based observers can perform follow-up observations. Typically the ground based observations begin after the GRB has ended and only residual emiSSion (the 'afterglow') is left. However, if the satellite relays the GRB coordinates quickly enough, a 'fast' robotic telescope on the ground may be able to catch the GRB in progress. The RAPTOR telescope system is one of only a few in the world to have accomplished this feat. In order to achieve these results, the RAPTOR telescopes must operate autonomously at a high duty-cycle and in peak operating condition. Currently the telescopes are maintained in an ad hoc manner, often in a run-to-failure mode. The RAPTOR project could benefit greatly from a structural health monitoring (SHM) system, especially as more complex units are added to the suite of telescopes. This paper will summarize preliminary results from an SHM study performed on one of the RAPTOR telescopes. Damage scenarios that are of concern and that have been previously observed are first summarized. Then a specific study of damage to the telescope drive mechanism is presented where the data acquisition system is first described. Next, damage detection algorithms are developed with LANL's new publically available software SHMTools and the results of this process are discussed in detail. The paper will conclude with a summary of future planned refinemenls of the RAPTOR SHM system.

Stull, Chris [Los Alamos National Laboratory; Taylor, Stuart [Los Alamos National Laboratory; Wren, James [Los Alamos National Laboratory; Farrar, Charles [Los Alamos National Laboratory; Park, Gyuhae [Los Alamos National Laboratory

2010-11-30T23:59:59.000Z

190

Charles McMillan to lead Los Alamos National Laboratory's Weapons Program  

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

McMillan to Lead Weapons Program McMillan to Lead Weapons Program Charles McMillan to lead Los Alamos National Laboratory's Weapons Program He will provide oversight and direction for the nuclear weapons program at Los Alamos to accomplish the Laboratory's core mission. July 28, 2009 Los Alamos National Laboratory sits on top of a once-remote mesa in northern New Mexico with the Jemez mountains as a backdrop to research and innovation covering multi-disciplines from bioscience, sustainable energy sources, to plasma physics and new materials. Los Alamos National Laboratory sits on top of a once-remote mesa in northern New Mexico with the Jemez mountains as a backdrop to research and innovation covering multi-disciplines from bioscience, sustainable energy sources, to plasma physics and new materials.

191

E-Print Network 3.0 - advanced compton telescope Sample Search...  

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

Detector Subsystem Summary: COMPTEL Compton Telescope on CGRO COS-B European Gamma-ray Astronomy Satellite DAPNIA Departement d... Telescope AGILE Astro-rivelatore Gamma a...

192

E-Print Network 3.0 - area telescope measurements Sample Search...  

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

focused telescope: Requirement of on-off- measurements With exception of: gamma-ray bursts & solar flares short time... Compton telescopes would measure: ... Source:...

193

The Large Area Telescope on the Fermi Gamma-ray Space Telescope Mission  

SciTech Connect (OSTI)

The Large Area Telescope (Fermi/LAT, hereafter LAT), the primary instrument on the Fermi Gamma-ray Space Telescope (Fermi) mission, is an imaging, wide field-of-view (FoV), high-energy {gamma}-ray telescope, covering the energy range from below 20 MeV to more than 300 GeV. The LAT was built by an international collaboration with contributions from space agencies, high-energy particle physics institutes, and universities in France, Italy, Japan, Sweden, and the United States. This paper describes the LAT, its preflight expected performance, and summarizes the key science objectives that will be addressed. On-orbit performance will be presented in detail in a subsequent paper. The LAT is a pair-conversion telescope with a precision tracker and calorimeter, each consisting of a 4 x 4 array of 16 modules, a segmented anticoincidence detector that covers the tracker array, and a programmable trigger and data acquisition system. Each tracker module has a vertical stack of 18 (x, y) tracking planes, including two layers (x and y) of single-sided silicon strip detectors and high-Z converter material (tungsten) per tray. Every calorimeter module has 96 CsI(Tl) crystals, arranged in an eight-layer hodoscopic configuration with a total depth of 8.6 radiation lengths, giving both longitudinal and transverse information about the energy deposition pattern. The calorimeter's depth and segmentation enable the high-energy reach of the LAT and contribute significantly to background rejection. The aspect ratio of the tracker (height/width) is 0.4, allowing a large FoV (2.4 sr) and ensuring that most pair-conversion showers initiated in the tracker will pass into the calorimeter for energy measurement. Data obtained with the LAT are intended to (1) permit rapid notification of high-energy {gamma}-ray bursts and transients and facilitate monitoring of variable sources, (2) yield an extensive catalog of several thousand high-energy sources obtained from an all-sky survey, (3) measure spectra from 20 MeV to more than 50 GeV for several hundred sources, (4) localize point sources to 0.3-2 arcmin, (5) map and obtain spectra of extended sources such as SNRs, molecular clouds, and nearby galaxies, (6) measure the diffuse isotropic {gamma}-ray background up to TeV energies, and (7) explore the discovery space for dark matter.

Atwood, W.B.; /UC, Santa Cruz; Abdo, Aous A.; /Naval Research Lab, Wash., D.C.; Ackermann, M.; /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept.; Anderson, B. /UC, Santa Cruz; Axelsson, M.; /Stockholm U.; Baldini, L.; /INFN, Pisa; Ballet, J.; /DAPNIA, Saclay; Band, D.L.; /NASA, Goddard /NASA, Goddard; Barbiellini, Guido; /INFN, Trieste /Trieste U.; Bartelt, J.; /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept.; Bastieri, Denis; /INFN, Padua /Padua U.; Baughman, B.M.; /Ohio State U.; Bechtol, K.; /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept.; Bederede, D.; /DAPNIA, Saclay; Bellardi, F.; /INFN, Pisa; Bellazzini, R.; /INFN, Pisa; Berenji, B.; /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept.; Bignami, G.F.; /Pavia U.; Bisello, D.; /INFN, Padua /Padua U.; Bissaldi, E.; /Garching, Max Planck Inst., MPE; Blandford, R.D.; /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /INFN, Perugia /Perugia U. /NASA, Goddard /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /INFN, Pisa /INFN, Pisa /Bari U. /INFN, Bari /Ecole Polytechnique /Washington U., Seattle /INFN, Padua /Padua U. /Bari U. /INFN, Bari /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /IASF, Milan /IASF, Milan /Kalmar U. /Royal Inst. Tech., Stockholm /DAPNIA, Saclay /ASI, Rome /INFN, Pisa /INFN, Perugia /Perugia U. /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /George Mason U. /Naval Research Lab, Wash., D.C. /NASA, Goddard /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /DAPNIA, Saclay /NASA, Goddard /INFN, Perugia /Perugia U. /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /Montpellier U. /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept.; /more authors.; ,

2009-05-15T23:59:59.000Z

194

Minimizing high spatial frequency residual in active space telescope mirrors  

E-Print Network [OSTI]

The trend in future space telescopes is towards large apertures and lightweight, rib-stiffened, and actively controlled deformable mirrors. These mirror architectures permit the development of segmented and deployed primary ...

Gray, Thomas, S.M. (Thomas L.) Massachusetts Institute of Technology

2008-01-01T23:59:59.000Z

195

Cross section dependence of event rates at neutrino telescopes  

E-Print Network [OSTI]

We examine the dependence of event rates at neutrino telescopes on the neutrino-nucleon cross section for neutrinos with energy above 1 PeV, and contrast the results with those for cosmic ray experiments. Scaling of the ...

Marfatia, Danny; Seckel, D.; McKay, D. W.; Hussain, S.

2006-10-20T23:59:59.000Z

196

An Australian Icon - Planning and Construction of the Parkes Telescope  

E-Print Network [OSTI]

By almost any measure, the Parkes Radio Telescope is the most successful scientific instrument ever built in Australia. The telescope is unsurpassed in terms of the number of astronomers, both national and international, who have used the instrument, the number of research papers that have flowed from their research, and the sheer longevity of its operation (now over fifty years). The original planners and builders could not have envisaged that the telescope would have such an extraordinarily long and productive future. From the start, it was an international project by CSIRO that in the 1950s launched Australia into the world of `big science'. Partly funded by the US Carnegie and Rockefeller foundations, it was designed in England by Freeman Fox & Partners, and built by the German firm MAN. This article will give an overview of the origins of the idea for the telescope and the funding, planning and construction of the Parkes dish over the period 1954 to 1961.

Robertson, Peter

2012-01-01T23:59:59.000Z

197

Isosurfacing in Span Space with Utmost E ciency (ISSUE) Han-Wei Sheny Charles D. Hansenz Yarden Livnaty Christopher R. Johnsony  

E-Print Network [OSTI]

University of Utah Los Alamos National Laboratory Salt Lake City, UT Los Alamos, New Mexico Abstract WeIsosurfacing in Span Space with Utmost E ciency (ISSUE) Han-Wei Sheny Charles D. Hansenz Yarden

Utah, University of

198

Isosurfacing in Span Space with Utmost Efficiency (ISSUE) HanWei Shen y Charles D. Hansen z Yarden Livnat y Christopher R. Johnson y  

E-Print Network [OSTI]

University of Utah Los Alamos National Laboratory Salt Lake City, UT Los Alamos, New Mexico Abstract WeIsosurfacing in Span Space with Utmost Efficiency (ISSUE) Han­Wei Shen y Charles D. Hansen z Yarden

Livnat, Yarden

199

A review of "Defining the Jacobean Church: the Politics of Religious Controversy, 1603-1625." by Charles W.A. Prior  

E-Print Network [OSTI]

REVIEWS 151 Charles W.A. Prior. Defining the Jacobean Church: the Politics of Religious Controversy, 1603-1625. Cambridge: Cambridge University Press, 2005. xiv + 294 pp. $85.00. Review by GRAHAM PARRY, UNIVERSITY OF YORK. Defining the Jacobean...

Parry, Graham

2006-01-01T23:59:59.000Z

200

The Sloan Digital Sky Survey Monitor Telescope Pipeline  

E-Print Network [OSTI]

The photometric calibration of the Sloan Digital Sky Survey (SDSS) is a multi-step process which involves data from three different telescopes: the 1.0-m telescope at the US Naval Observatory (USNO), Flagstaff Station, Arizona (which was used to establish the SDSS standard star network); the SDSS 0.5-m Photometric Telescope (PT) at the Apache Point Observatory (APO), New Mexico (which calculates nightly extinctions and calibrates secondary patch transfer fields); and the SDSS 2.5-m telescope at APO (which obtains the imaging data for the SDSS proper). In this paper, we describe the Monitor Telescope Pipeline, MTPIPE, the software pipeline used in processing the data from the single-CCD telescopes used in the photometric calibration of the SDSS (i.e., the USNO 1.0-m and the PT). We also describe transformation equations that convert photometry on the USNO-1.0m u'g'r'i'z' system to photometry the SDSS 2.5m ugriz system and the results of various validation tests of the MTPIPE software. Further, we discuss the semi-automated PT factory, which runs MTPIPE in the day-to-day standard SDSS operations at Fermilab. Finally, we discuss the use of MTPIPE in current SDSS-related projects, including the Southern u'g'r'i'z' Standard Star project, the u'g'r'i'z' Open Star Clusters project, and the SDSS extension (SDSS-II).

D. L. Tucker; S. Kent; M. W. Richmond; J. Annis; J. A. Smith; S. S. Allam; C. T. Rodgers; J. L. Stute; J. K. Adelman-McCarthy; J. Brinkmann; M. Doi; D. Finkbeiner; M. Fukugita; J. Goldston; B. Greenway; J. E. Gunn; J. S. Hendry; D. W. Hogg; S. -I. Ichikawa; Z. Ivezic; G. R. Knapp; H. Lampeitl; B. C. Lee; H. Lin; T. A. McKay; A. Merrelli; J. A. Munn; E. H. Neilsen, Jr.; H. J. Newberg; G. T. Richards; D. J. Schlegel; C. Stoughton; A. Uomoto; B. Yanny

2006-08-26T23:59:59.000Z

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201

The next generation Cherenkov Telescope Array observatory: CTA  

E-Print Network [OSTI]

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

Vercellone, Stefano

2014-01-01T23:59:59.000Z

202

3D acoustic imaging applied to the Baikal Neutrino Telescope  

E-Print Network [OSTI]

A hydro-acoustic imaging system was tested in a pilot study on distant localization of elements of the Baikal underwater neutrino telescope. For this innovative approach, based on broad band acoustic echo signals and strictly avoiding any active acoustic elements on the telescope, the imaging system was temporarily installed just below the ice surface, while the telescope stayed in its standard position at 1100 m depth. The system comprised an antenna with four acoustic projectors positioned at the corners of a 50 meter square; acoustic pulses were "linear sweep-spread signals" - multiple-modulated wide-band signals (10-22 kHz) of 51.2 s duration. Three large objects (two string buoys and the central electronics module) were localized by the 3D acoustic imaging, with a accuracy of ~0.2 m (along the beam) and ~1.0 m (transverse). We discuss signal forms and parameters necessary for improved 3D acoustic imaging of the telescope, and suggest a layout of a possible stationary bottom based 3D imaging setup. The presented technique may be of interest for neutrino telescopes of km3-scale and beyond, as a flexible temporary or as a stationary tool to localize basic telescope elements, while these are completely passive.

K. G. Kebkal; R. Bannasch; O. G. Kebkal; A. I. Panfilov; R. Wischnewski

2008-11-07T23:59:59.000Z

203

The next generation Cherenkov Telescope Array observatory: CTA  

Science Journals Connector (OSTI)

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

S. Vercellone

2014-01-01T23:59:59.000Z

204

Cryogenic optical performance of the ASTRO-F SiC telescope  

Science Journals Connector (OSTI)

The lightweight cryogenic telescope on board the Japanese infrared astronomical satellite, ASTRO-F, which

Kaneda, Hidehiro; Onaka, Takashi; Nakagawa, Takao; Enya, Keigo; Murakami, Hiroshi; Yamashiro, Ryoji; Ezaki, Tatsuhiko; Numao, Yasuyuki; Sugiyama, Yoshikazu

2005-01-01T23:59:59.000Z

205

Advanced Dark Energy Physics Telescope (ADEPT)  

SciTech Connect (OSTI)

In 2006, we proposed to NASA a detailed concept study of ADEPT (the Advanced Dark Energy Physics Telescope), a potential space mission to reliably measure the time-evolution of dark energy by conducting the largest effective volume survey of the universe ever done. A peer-review panel of scientific, management, and technical experts reported back the highest possible 'excellent' rating for ADEPT. We have since made substantial advances in the scientific and technical maturity of the mission design. With this Department of Energy (DOE) award we were granted supplemental funding to support specific extended research items that were not included in the NASA proposal, many of which were intended to broadly advance future dark energy research, as laid out by the Dark Energy Task Force (DETF). The proposed work had three targets: (1) the adaptation of large-format infrared arrays to a 2 micron cut-off; (2) analytical research to improve the understanding of the dark energy figure-of- merit; and (3) extended studies of baryon acoustic oscillation systematic uncertainties. Since the actual award was only for {approx}10% of the proposed amount item (1) was dropped and item (2) work was severely restricted, consistent with the referee reviews of the proposal, although there was considerable contradictions between reviewer comments and several comments that displayed a lack of familiarity with the research. None the less, item (3) was the focus of the work. To characterize the nature of the dark energy, ADEPT is designed to observe baryon acoustic oscillations (BAO) in a large galaxy redshift survey and to obtain substantial numbers of high-redshift Type Ia supernovae (SNe Ia). The 2003 Wilkinson Microwave Anisotropy Probe (WMAP) made a precise determination of the BAO 'standard ruler' scale, as it was imprinted on the cosmic microwave background (CMB) at z {approx} 1090. The standard ruler was also imprinted on the pattern of galaxies, and was first detected in 2005 in Sloan Digital Sky Survey (SDSS) data. A measurement of the BAO standard ruler as a function of time (or redshift) would provide powerful and reliable observational data to shed light on dark energy. In particular, the BAO data provide the angular diameter distance to each redshift, and directly give the expansion rate, H(z), at each redshift. The SNe measurements provide luminosity distances. A space mission is required to obtain the three-dimensional position of enormous numbers of galaxies at high redshift. As recognized by the Dark Energy Task Force, BAO systematic errors are naturally low. The following are the key findings: (1) The BAO method is robust. (2) Separation of the spectral and imaging detection focal planes vastly improves spectral identifications. (3) Prisms instead of grisms provide higher throughput and cleaner spectra. Prisms are clearly superior. (4) Lower prism dispersions improve signal-to-noise but high prism dispersions improve systematic. To ensure that the experiment is not systematic limited, a high dispersion should be used. (5) Counter-dispersion of the spectra reduces systematic errors on the redshift determination and assists in the reduction of confusion. (6) Small rolls are very effective for the reduction of confusion. (7) Interlopers can be recognized by a variety of methods, which combine to produce a sufficiently 'clean' survey data set so as not to limit the dark energy results. (8) A space mission can measure the BAO signature to the cosmic variance limit, limited only by statistics and not by systematic. (9) Density field reconstruction allows for significant BAO accuracy improvements, well beyond that assumed by the Dark Energy Task Force. (10) The BAO method is statistically powerful. It is more powerful than previously estimated, and far more powerful than high redshift Type 1a supernovae, for which the ultimate distance accuracy is limited by flux calibration accuracy. (11) The BAO technique is far simpler than the weak lensing technique and likely to produce more robust dark energy solutions.

Charles L. Bennett

2009-03-26T23:59:59.000Z

206

Summary of One Year Operation of the EUDET CMOS Pixel Telescope  

E-Print Network [OSTI]

Within the EUDET consortium a high resolution pixel beam telescope is being developed. The telescope consists of up to six planes of monolithic active pixel sensors. A flexible data acquisition environment is available for the telescope and the system is equipped with all the required infrastructure. Since the first installation of a demonstrator telescope in 2007, it has been extensively tested and used by various detector R&D groups. The results of test beam measurements are described here, demonstrating the telescope performance.

Ingrid-Maria Gregor

2009-01-06T23:59:59.000Z

207

SKA SA test telescope reveals binary star system South Africa's test telescope reveals secrets of a binary star system and proves the country is able to  

E-Print Network [OSTI]

SKA SA test telescope reveals binary star system South Africa's test telescope reveals secrets, has created huge research and job opportunities. South Africa's Karoo Array Telescope (KAT-7) has at the SKA South Africa. The 64-dish MeerKAT ­ which SKA South Africa director Bernie Fanaroff once described

Jarrett, Thomas H.

208

Fine tracking system for balloon-borne telescopes  

E-Print Network [OSTI]

We present the results of a study along with a first prototype of a high precision system (? 1 arcsec) for pointing and tracking light (near-infrared) telescopes on board stratospheric balloons. Such a system is essentially composed by a star sensor and by a star tracker, able to recognize the field and to adequately track the telescope, respectively. We present the software aimed at processing the star sensor image and the predictive algorithm that allows the fine tracking of the source at a sub-pixel level. The laboratory tests of the system are described and its performance is analyzed. We demonstrate how such a device, when used at the focal plane of enough large telescopes (2-4m, F/10), is capable to provide (sub-)arcsec diffraction limited images in the near infrared bands.

Ricci, M; Lorenzetti, D

2011-01-01T23:59:59.000Z

209

The Atmospheric Monitoring Strategy for the Cherenkov Telescope Array  

E-Print Network [OSTI]

The Imaging Atmospheric Cherenkov Technique (IACT) is unusual in astronomy as the atmosphere actually forms an intrinsic part of the detector system, with telescopes indirectly detecting very high energy particles by the generation and transport of Cherenkov photons deep within the atmosphere. This means that accurate measurement, characterisation and monitoring of the atmosphere is at the very heart of successfully operating an IACT system. The Cherenkov Telescope Array (CTA) will be the next generation IACT observatory with an ambitious aim to improve the sensitivity of an order of magnitude over current facilities, along with corresponding improvements in angular and energy resolution and extended energy coverage, through an array of Large (23m), Medium (12m) and Small (4m) sized telescopes spread over an area of order ~km$^2$. Whole sky coverage will be achieved by operating at two sites: one in the northern hemisphere and one in the southern hemisphere. This proceedings will cover the characterisation of...

Daniel, M K

2015-01-01T23:59:59.000Z

210

Simbol-X Telescope Scientific Calibrations: Requirements and Plans  

SciTech Connect (OSTI)

The Simbol-X telescope characteristics and the mission scientific requirements impose a challenging calibration plan with a number of unprecedented issues. The 20 m focal length implies for the incoming X-ray beam a divergence comparable to the incidence angle of the mirror surface also for 100 m-long facilities. Moreover this is the first time that a direct focussing X-ray telescope will be calibrated on an energy band covering about three decades, and with a complex focal plane. These problems require a careful plan and organization of the measurements, together with an evaluation of the calibration needs in terms of both hardware and software.

Malaguti, G.; Raimondi, L.; Trifoglio, M. [INAF-IASF Bologna (Italy); Angelini, L. [NASA/Goddard Space Flight Center (United States); Moretti, A. [INAF-OABrera (Italy)

2009-05-11T23:59:59.000Z

211

Integrating Seeing Measurements into the Operations of Solar Telescopes  

E-Print Network [OSTI]

conditions for solar observations: Big Bear Solar Observatory in California, Haleakala on Maui, HawaiiIntegrating Seeing Measurements into the Operations of Solar Telescopes C. Denker and A. P. Verdoni New Jersey Institute of Technology, Center for Solar-Terrestrial Research 323 Martin Luther King Blvd

212

THE JAMES WEBB SPACE TELESCOPE JONATHAN P. GARDNER1,  

E-Print Network [OSTI]

Institute of Technology (ETH-Zurich), ETH H¨onggerberg, CH-8093 Zurich, Switzerland 8Space Telescope Science¨ur Astronomie, K¨onigstuhl 17, Heidelberg D-69117, Germany 15NASA Headquarters, 300 E Street Southwest Light and Reionization theme is to identify the first luminous sources to form and to determine

Colorado at Boulder, University of

213

NMSU's 1m Altaz telescope located at the Apache Point  

E-Print Network [OSTI]

Research Projects National Solar Observa- tory's facilities in Sacra- mento Peak, New Mexico NMSU RESEARCHNMSU's 1m Altaz telescope located at the Apache Point Observatory in Sunspot, New Mexico. Dr has been awarded NSF funding to enhance the quality and quantity of New Mexico State University

Johnson, Eric E.

214

The Atacama Cosmology Telescope Project: A Progress Report  

E-Print Network [OSTI]

The Atacama Cosmology Telescope is a project to map the microwave background radiation at arcminute angular resolution and high sensitivity in three frequency bands over substantial sky areas. Cosmological signals driving such an experiment are reviewed, and current progress in hardware construction is summarized. Complementary astronomical observations in other wavebands are also discussed.

Arthur Kosowsky; for the ACT Collaboration

2006-08-25T23:59:59.000Z

215

Results of a Si/CdTe Compton Telescope  

E-Print Network [OSTI]

We have been developing a semiconductor Compton telescope to explore the universe in the energy band from several tens of keV to a few MeV. We use a Si strip and CdTe pixel detector for the Compton telescope to cover an energy range from 60 keV. For energies above several hundred keV, the higher efficiency of CdTe semiconductor in comparison with Si is expected to play an important role as an absorber and a scatterer. In order to demonstrate the spectral and imaging capability of a CdTe-based Compton Telescope, we have developed a Compton telescope consisting of a stack of CdTe pixel detectors as a small scale prototype. With this prototype, we succeeded in reconstructing images and spectra by solving the Compton equation from 122 keV to 662 keV. The energy resolution (FWHM) of reconstructed spectra is 7.3 keV at 511 keV and 3.1 keV at 122 keV, respectively. The angular resolution obtained at 511 keV is measured to be 12.2 degree (FWHM).

Kousuke Oonuki; Takaaki Tanaka; Shin Watanabe; Shin'ichiro Takeda; Kazuhiro Nakazawa; Takefumi Mitani; Tadayuki Takahashi; Hiroyasu Tajima; Yasushi Fukazawa; Masaharu Nomachi

2005-09-21T23:59:59.000Z

216

Review of the Solar Array Telescopes David A. Smith  

E-Print Network [OSTI]

to believe that at lower energy, wavefront sampling could have advantages [34]. After the 1973 oil crisisReview of the Solar Array Telescopes David A. Smith Centre d'Etudes Nucl´eaires de Bordeaux sensitive to astrophysical gamma rays with energies beyond the reach of EGRET but below

Paris-Sud XI, Université de

217

Adaptive Optics Simulations for the European Extremely Large Telescope  

E-Print Network [OSTI]

Louarn, Sylvain Oberti, and A. Garcia-Rissman European Southern Observatory, Karl-Schwarzschild-Stra?e 2 large telescopes (ELTs) of primary mirror diameters 20-42 m are in the design stages, such as the thirty of view (FOV) with a single deformable mirror (DM). Due to the sky coverage constraints of NGS systems

Liske, Jochen

218

New challenges for adaptive optics: extremely large telescopes  

Science Journals Connector (OSTI)

......Southern Observatory, Karl Schwarzschild Str. 2, D-85748 Garching...and up to three deformable mirrors, which increase up to 8-fold...optical telescopes has primary mirrors with diameters in the 8...the diameter of the primary mirror lies in a range between 40......

M. Le Louarn; N. Hubin; M. Sarazin; A. Tokovinin

2000-09-21T23:59:59.000Z

219

Sanders, J. E., and Merguerian, Charles, 1994b, The glacial geology of New York City and vicinity, p. 93-200 in A. I. Benimoff, ed., The Geology of Staten Island, New York, Field  

E-Print Network [OSTI]

Sanders, J. E., and Merguerian, Charles, 1994b, The glacial geology of New York City and vicinity Valley (the same direction as reported by Flint from the Lake Chamberlain Till in CT). In New York City and proceedings, The Geological Association of New Jersey, XI Annual Meeting, 296 p. John E. Sanders* and Charles

Merguerian, Charles

220

The use of rhetorical appeals to convey a Christian world-view in Charles Williams' All hallows' eve  

E-Print Network [OSTI]

Williams seemed to have no choice: having decided to hold to his I Christian world-view, Williams could not have imitated reality as he knew it without allowing at least three aspects of his novel to progress in a prescribed course. These aspects are... (Chairman of Ccnmittee) Paul A. Parri h (Member) David A. Wlandson (Member) David . Stewar (Head of Department) August 1984 The Use of Rhetorical Appeals to Convey a Christian World-View In Charles Williams' All Hallow's Eve (August 1984) Marilyn R...

Kok, Marilyn R

1984-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "telescope baltay charles" 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

A review of "England's Wars of Religion, Revisited" edited by Charles W. A. Prior and Glenn Burgess  

E-Print Network [OSTI]

engagement, it is likely to #23; nd only a very limited audience. Charles W. A. Prior and Glenn Burgess, eds. England?s Wars of Religion, Revisited. Farnham and Burlington: Ashgate, 2011. xiv + 335 pp. + 2 illustrations. $115.00. Review by #8;#7; #2... presented engage with what Glenn Burgess calls ?one of the most stubborn of historiographi- 156 #2;#3;#4;#3;#5;#6;#3;#3;#5;#6;#7;-#8;#3;#5;#6; #11; #5;#3;#12;#2; cal puzzles? (xiii) with exceptional clarity, showing the intricate and shifting ways...

Langley, Chris R.

2012-01-01T23:59:59.000Z

222

The Photodetector Plane of the 4m Davies Cotton Small Size Telescope for the Cherenkov Telescope Array  

E-Print Network [OSTI]

Photomultipliers (PMTs) are currently adopted for the photodetector plane of Imaging Atmospheric Cherenkov Telescopes (IACTs). Even though PMT quantum efficiency has improved impressively in the recent years, one of the main limitation for their application in the gamma-astronomy field - the impossibility to operate with moon light - still remains. As a matter of fact, the light excess would lead to significant and faster camera ageing. Solid state detectors, in particular Geiger-mode avalanche photo-diodes (G-APDs) represent a valuable alternative solution to overcome this limitation as demonstrated in the field by the FACT experiment (The First G- APD Cherenkov Telescope). They can be regarded as a more promising long term approach, which can be easily adopted for the new generation of cameras and for the Cherenkov Telescope Array (CTA). We describe here the Photo-Detector Plane (PDP) of the camera for the 4 m Davies Cotton CTA Small Size Telescopes, for which large area G-APD coupled to non-imaging light c...

Boccone, V; Basili, A; Christov, A; della Volpe, M; Montaruli, T

2013-01-01T23:59:59.000Z

223

E-Print Network 3.0 - area telescope observations Sample Search...  

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

<< < 1 2 3 4 5 > >> 1 NASSP OT1: Telescopes I-217 Feb 2010 1 OpticalIR Observational Astronomy Summary: NASSP OT1: Telescopes I-217 Feb 2010 1 OpticalIR Observational Astronomy...

224

E-Print Network 3.0 - area telescope view Sample Search Results  

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

<< < 1 2 3 4 5 > >> 1 NASSP OT1: Telescopes I-217 Feb 2010 1 OpticalIR Observational Astronomy Summary: NASSP OT1: Telescopes I-217 Feb 2010 1 OpticalIR Observational Astronomy...

225

E-Print Network 3.0 - area telescope bright Sample Search Results  

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

<< < 1 2 3 4 5 > >> 1 NASSP OT1: Telescopes I-217 Feb 2010 1 OpticalIR Observational Astronomy Summary: ms images of a bright star 12;NASSP OT1: Telescopes I-217 Feb 2010 13...

226

E-Print Network 3.0 - area telescope points Sample Search Results  

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

<< < 1 2 3 4 5 > >> 1 NASSP OT1: Telescopes I-217 Feb 2010 1 OpticalIR Observational Astronomy Summary: NASSP OT1: Telescopes I-217 Feb 2010 1 OpticalIR Observational Astronomy...

227

Experimental Results Obtained with the Positron-Annihilation Radiation Telescope of the Toulouse-Argonne Collaboration  

Science Journals Connector (OSTI)

We present laboratory measurements obtained with a ground-based prototype of a focusing positron-annihilation-radiation telescope developed by the Toulouse-Argonne collaboration. This balloon-borne telescope has ...

J. E. Naya; P. von Ballmoos; F. Albernhe; G. Vedrenne

1995-01-01T23:59:59.000Z

228

Tradespace Investigation of a Telescope Architecture for Next-generation Space Astronomy and Exploration  

E-Print Network [OSTI]

Humanitys endeavor to further its scientific understanding of the celestial heavens has led to the creation and evolution of increasingly powerful and complex space telescopes. Space telescopes provide a view of the solar ...

Cataldo, Giuseppe

2014-12-19T23:59:59.000Z

229

E-Print Network 3.0 - axion solar telescope Sample Search Results  

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

solar telescope Search Powered by Explorit Topic List Advanced Search Sample search results for: axion solar telescope Page: << < 1 2 3 4 5 > >> 1 In Search Of Axions: The CAST...

230

The Balloon-borne Large Aperture Submillimeter Telescope and Its Rebirth as a Polarimeter.  

E-Print Network [OSTI]

??The Balloon-borne Large Aperture Submillimeter Telescope (BLAST) is a 1.8 meter Cassegrain telescope that operates in three bands (250, 350, and 500 ?m), each with (more)

Thomas, Nicholas E

2011-01-01T23:59:59.000Z

231

Design and analysis of a two-channel three-mirror x-ray telescope: errata  

Science Journals Connector (OSTI)

Alternate configurations for a two-channel three-mirror glancing incidence x-ray telescope have been designed and evaluated. A Wolter-Schwarzschild type I telescope is used as a base...

Kassim, Abd M; Shealy, David L

1984-01-01T23:59:59.000Z

232

Thermal characteristics of a classical solar telescope primary mirror  

E-Print Network [OSTI]

We present a detailed thermal and structural analysis of a 2m class solar telescope mirror which is subjected to a varying heat load at an observatory site. A 3-dimensional heat transfer model of the mirror takes into account the heating caused by a smooth and gradual increase of the solar flux during the day-time observations and cooling resulting from the exponentially decaying ambient temperature at night. The thermal and structural response of two competing materials for optical telescopes, namely Silicon Carbide -best known for excellent heat conductivity and Zerodur -preferred for its extremely low coefficient of thermal expansion, is investigated in detail. The insight gained from these simulations will provide a valuable input for devising an efficient and stable thermal control system for the primary mirror.

Banyal, Ravinder K

2011-01-01T23:59:59.000Z

233

SLAC All Access: Fermi Gamma-ray Space Telescope  

SciTech Connect (OSTI)

Three hundred and fifty miles overhead, the Fermi Gamma-ray Space Telescope silently glides through space. From this serene vantage point, the satellite's instruments watch the fiercest processes in the universe unfold. Pulsars spin up to 700 times a second, sweeping powerful beams of gamma-ray light through the cosmos. The hyperactive cores of distant galaxies spew bright jets of plasma. Far beyond, something mysterious explodes with unfathomable power, sending energy waves crashing through the universe. Stanford professor and KIPAC member Roger W. Romani talks about this orbiting telescope, the most advanced ever to view the sky in gamma rays, a form of light at the highest end of the energy spectrum that's created in the hottest regions of the universe.

Romani, Roger

2013-05-31T23:59:59.000Z

234

FERMI LARGE AREA TELESCOPE OBSERVATIONS OF GRB 110625A  

SciTech Connect (OSTI)

Gamma-ray bursts (GRBs) that emit photons at GeV energies form a small but significant population of GRBs. However, the number of GRBs whose GeV-emitting period is simultaneously observed in X-rays remains small. We report {gamma}-ray observations of GRB 110625A using Fermi's Large Area Telescope in the energy range 100 MeV-20 GeV. Gamma-ray emission at these energies was clearly detected using data taken between 180 s and 580 s after the burst, an epoch after the prompt emission phase. The GeV light curve differs from a simple power-law decay, and probably consists of two emission periods. Simultaneous Swift X-Ray Telescope observations did not show flaring behaviors as in the case of GRB 100728A. We discuss the possibility that the GeV emission is the synchrotron self-Compton radiation of underlying ultraviolet flares.

Tam, P. H. T.; Kong, A. K. H. [Institute of Astronomy and Department of Physics, National Tsing Hua University, Hsinchu 30013, Taiwan (China); Fan Yizhong, E-mail: phtam@phys.nthu.edu.tw [Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008 (China)

2012-08-01T23:59:59.000Z

235

SLAC All Access: Fermi Gamma-ray Space Telescope  

ScienceCinema (OSTI)

Three hundred and fifty miles overhead, the Fermi Gamma-ray Space Telescope silently glides through space. From this serene vantage point, the satellite's instruments watch the fiercest processes in the universe unfold. Pulsars spin up to 700 times a second, sweeping powerful beams of gamma-ray light through the cosmos. The hyperactive cores of distant galaxies spew bright jets of plasma. Far beyond, something mysterious explodes with unfathomable power, sending energy waves crashing through the universe. Stanford professor and KIPAC member Roger W. Romani talks about this orbiting telescope, the most advanced ever to view the sky in gamma rays, a form of light at the highest end of the energy spectrum that's created in the hottest regions of the universe.

Romani, Roger

2014-06-24T23:59:59.000Z

236

Gamma-Ray Imaging with the Coded Mask IBIS Telescope  

E-Print Network [OSTI]

The IBIS telescope onboard INTEGRAL, the ESA gamma-ray space mission to be launched in 2002, is a soft gamma-ray (20 keV - 10 MeV) device based on a coded aperture imaging system. We describe here basic concepts of coded masks, the imaging system of the IBIS telescope, and the standard data analysis procedures to reconstruct sky images. This analysis includes, for both the low-energy detector layer (ISGRI) and the high energy layer (PICSIT), iterative procedures which decode recorded shadowgrams, search for and locate sources, clean for secondary lobes, and then rotate and compose sky images. These procedures will be implemented in the Quick Look and Standard Analysis of the INTEGRAL Science Data Center (ISDC) as IBIS Instrument Specific Software.

Goldwurm, A; Gros, A; Stephen, J; Foschini, L; Gianotti, F; Natalucci, L; De Cesare, G; Santo, M D

2000-01-01T23:59:59.000Z

237

The data acquisition system for the ANTARES neutrino telescope  

E-Print Network [OSTI]

The ANTARES neutrino telescope is being constructed in the Mediterranean Sea. It consists of a large three-dimensional array of photo-multiplier tubes. The data acquisition system of the detector takes care of the digitisation of the photo-multiplier tube signals, data transport, data filtering, and data storage. The detector is operated using a control program interfaced with all elements. The design and the implementation of the data acquisition system are described.

J. A. Aguilar; ANTARES collaboration

2006-10-02T23:59:59.000Z

238

The Balloon-borne Large Aperture Submillimeter Telescope: BLAST  

Science Journals Connector (OSTI)

The Balloon-borne Large Aperture Submillimeter Telescope (BLAST) is a suborbital surveying experiment designed to study the evolutionary history and processes of star formation in local galaxies (including the Milky Way) and galaxies at cosmological distances. The BLAST continuum camera, which consists of 270 detectors distributed between three arrays, observes simultaneously in broadband (30%) spectral windows at 250, 350, and 500 ?m. The optical design is based on a 2 m diameter telescope, providing a diffraction-limited resolution of 30 -->'' at 250 ?m. The gondola pointing system enables raster mapping of arbitrary geometry, with a repeatable positional accuracy of ~30 -->''; postflight pointing reconstruction to 5 -->'' rms is achieved. The onboard telescope control software permits autonomous execution of a preselected set of maps, with the option of manual override. In this paper we describe the primary characteristics and measured in-flight performance of BLAST. BLAST performed a test flight in 2003 and has since made two scientifically productive long-duration balloon flights: a 100 hr flight from ESRANGE (Kiruna), Sweden to Victoria Island, northern Canada in 2005 June; and a 250 hr, circumpolar flight from McMurdo Station, Antarctica, in 2006 December.

E. Pascale; P. A. R. Ade; J. J. Bock; E. L. Chapin; J. Chung; M. J. Devlin; S Dicker; M. Griffin; J. O. Gundersen; M. Halpern; P. C. Hargrave; D. H. Hughes; J. Klein; C. J. MacTavish; G. Marsden; P. G. Martin; T. G. Martin; P. Mauskopf; C. B. Netterfield; L. Olmi; G. Patanchon; M. Rex; D. Scott; C. Semisch; N. Thomas; M. D. P. Truch; C. Tucker; G. S. Tucker; M. P. Viero; D. V. Wiebe

2008-01-01T23:59:59.000Z

239

Trigger electronics of the new Fluorescence Detectors of the Telescope Array Experiment  

E-Print Network [OSTI]

of Physics, University of Utah, Salt Lake City, UT 84112-0830, USA d Institute of Particle and Nuclear Tameda a,?, Akimichi Taketa b , Jeremy D. Smith c , Manobu Tanaka d , Masaki Fukushima b , Charles C Studies, KEK, Oho, Tsukuba, Ibaraki 305-0801, Japan e Graduate School of Science, Osaka City University

240

Multi-Ported Memories for FPGAs via XOR Charles Eric LaForest, Ming G. Liu, Emma Rae Rapati, and J. Gregory Steffan  

E-Print Network [OSTI]

Multi-Ported Memories for FPGAs via XOR Charles Eric LaForest, Ming G. Liu, Emma Rae Rapati, and J,steffan}@eecg.toronto.edu, {emma.rapati,minggang.liu}@utoronto.ca ABSTRACT Multi-ported memories are challenging to implement with FPGAs since the block RAMs included in the fabric typically have only two ports. Any design

Steffan, J. Gregory

Note: This page contains sample records for the topic "telescope baltay charles" 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

Mycorrhizal Species Dominate the Soil-Fungal Community in Estonian Oil Shale-Ash Hills Charles Cowden, Sam Willis, and Richard Shefferson  

E-Print Network [OSTI]

Mycorrhizal Species Dominate the Soil-Fungal Community in Estonian Oil Shale-Ash Hills Charles 30602 Introduction Estonia relies on vast reserves of oil shale to produce electricity. The mining and burning of oil shale is extremely inefficient and produces large quantities of tailings and ash (Vallner

Shefferson, Richard P.

242

On-the-Fly Pipeline Parallelism I-Ting Angelina Lee* Charles E. Leiserson* Tao B. Schardl* Jim Sukha Zhunping Zhang*  

E-Print Network [OSTI]

On-the-Fly Pipeline Parallelism I-Ting Angelina Lee* Charles E. Leiserson* Tao B. Schardl* Jim Pipeline parallelism organizes a parallel program as a linear se- quence of s stages. Each stage processes element before the subsequent stages have nec- essarily completed their processing. Pipeline parallelism

Leiserson, Charles E.

243

Sea Level Rise Summit June 20-22 in Boca Raton FAU's Center for Environmental Studies within the Charles E. Schmidt College of Science will host a "Risk  

E-Print Network [OSTI]

Sea Level Rise Summit June 20-22 in Boca Raton FAU's Center for Environmental Studies within the Charles E. Schmidt College of Science will host a "Risk and Response: Sea Level Rise Summit" on Wednesday planning of agencies, institutions and civic society to sea level rise and compare the Florida situation

Fernandez, Eduardo

244

SnapShot: Visualization to Propel Ice Hockey Analytics Hannah Pileggi, Charles D. Stolper, J. Michael Boyle, and John T. Stasko, Senior Member, IEEE  

E-Print Network [OSTI]

SnapShot: Visualization to Propel Ice Hockey Analytics Hannah Pileggi, Charles D. Stolper, J A of eight radial heat maps displaying patterns of shot lengths at each of the indicated rinks during into tables of numbers, divorced from the rinks, pitches, and courts where they were generated. Currently

Stasko, John T.

245

Procurement Office, The University of Edinburgh, Charles Stewart House, 9-16 Chambers Street, Edinburgh, EH1 1HT PURCHASE OF EQUIPMENT  

E-Print Network [OSTI]

Procurement Office, The University of Edinburgh, Charles Stewart House, 9-16 Chambers Street, Edinburgh, EH1 1HT PURCHASE OF EQUIPMENT 1. STANDARD TERMS & CONDITIONS RELATING TO THE PURCHASE and having its principal administrative offices at Old College, South Bridge, Edinburgh, EH8 9YL (the

Schnaufer, Achim

246

Procurement Office, The University of Edinburgh, Charles Stewart House, 9-16 Chambers Street, Edinburgh, EH1 1HT PURCHASE OF SERVICES  

E-Print Network [OSTI]

Procurement Office, The University of Edinburgh, Charles Stewart House, 9-16 Chambers Street, Edinburgh, EH1 1HT PURCHASE OF SERVICES 1. STANDARD TERMS & CONDITIONS RELATING TO THE PURCHASE OF SERVICES its principal administrative offices at Old College, South Bridge, Edinburgh, EH8 9YL (the "University

Schnaufer, Achim

247

Procurement Office, The University of Edinburgh, Charles Stewart House, 9-16 Chambers Street, Edinburgh, EH1 1HT PURCHASE OF IT EQUIPMENT  

E-Print Network [OSTI]

Procurement Office, The University of Edinburgh, Charles Stewart House, 9-16 Chambers Street, Edinburgh, EH1 1HT PURCHASE OF IT EQUIPMENT 1. STANDARD TERMS AND CONDITIONS RELATING TO THE PURCHASE and having its principal administrative offices at Old College, South Bridge, Edinburgh, EH8 9YL (the

Schnaufer, Achim

248

Procurement Office, The University of Edinburgh, Charles Stewart House, 9-16 Chambers Street, Edinburgh, EH1 1HT PURCHASE OF GOODS  

E-Print Network [OSTI]

Procurement Office, The University of Edinburgh, Charles Stewart House, 9-16 Chambers Street, Edinburgh, EH1 1HT PURCHASE OF GOODS 1. STANDARD TERMS AND CONDITIONS RELATING TO THE PURCHASE OF GOODS its principal administrative offices at Old College, South Bridge, Edinburgh, EH8 9YL (the "University

Schnaufer, Achim

249

Low Voltage High-SNR Pipeline Data Converters Charles Myers, Jipeng Li, Dong-Young Chang, and Un-Ku Moon  

E-Print Network [OSTI]

Low Voltage High-SNR Pipeline Data Converters Charles Myers, Jipeng Li, Dong-Young Chang, and Un pipeline data converter. This is accomplished with the removal of the S/H input stage and the use of a rail limitations. In pipeline data converters, noise reduction options such as oversampling and noise shaping

Moon, Un-Ku

250

[article MS-151 for the Encyclopedia of Atmospheric Sciences] Charles A. Doswell III, NOAA/National Severe Storms Laboratory, 1313 Halley Circle,  

E-Print Network [OSTI]

Flooding [article MS-151 for the Encyclopedia of Atmospheric Sciences] Charles A. Doswell III, NOAA/National Severe Storms Laboratory, 1313 Halley Circle, Norman, Oklahoma 73069, U.S.A. Introduction Flooding anywhere. A flood is defined as water overflowing onto land that usually is dry. Flooding is often thought

Doswell III, Charles A.

251

Photo of the Week: The Webb Telescope's "Golden Spider" | Department of  

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

The Webb Telescope's "Golden Spider" The Webb Telescope's "Golden Spider" Photo of the Week: The Webb Telescope's "Golden Spider" September 14, 2012 - 2:32pm Addthis The James Webb Space Telescope is a large, infrared-optimized telescope that is anticipated to launch in 2018. The spider-like sheets and tubes of wires you see here are the Optical Telescope Simulator (OSIM) for the telescope itself. OSIM will help scientists prepare the Webb telescope for flight by generating a beam of light that the telescope optics will feed into its actual flight instruments. In this photo, engineers have blanketed the OSIM with special insulating material to help control its temperature while it goes into the deep freeze testing of the Space Environment Simulator at NASA's Goddard Space Flight Center in Greenbelt, Maryland. The simulator will mimic the environment that the telescope will experience in operational orbit, more than 1 million miles from Earth. | Photo credit: Chris Gunn/NASA.

252

Design constraints on Cherenkov telescopes with Davies-Cotton reflectors  

E-Print Network [OSTI]

This paper discusses the construction of high-performance ground-based gamma-ray Cherenkov telescopes with a Davies-Cotton reflector. For the design of such telescopes, usually physics constrains the field-of-view, while the photo-sensor size is defined by limited options. Including the effect of light-concentrators in front of the photo sensor, it is demonstrated that these constraints are enough to mutually constrain all other design parameters. The dependability of the various design parameters naturally arises once a relationship between the value of the point-spread functions at the edge of the field-of-view and the pixel field-of-view is introduced. To be able to include this constraint into a system of equations, an analytical description for the point-spread function of a tessellated Davies-Cotton reflector is derived from Taylor developments and ray-tracing simulations. Including higher order terms renders the result precise on the percent level. Design curves are provided within the typical phase sp...

Bretz, Thomas

2013-01-01T23:59:59.000Z

253

The Trigger Algorithm for the Burst Alert Telescope on Swift  

E-Print Network [OSTI]

The Swift Burst Alert Telescope (BAT) is a huge (5200 cm2) coded aperture imager that will detect gamma-ray bursts in real time and provide a location that the Swift satellite will use to slew the optical and x-ray telescopes. The huge size of BAT is a challenge for the on-board triggering: a change as small as 1% is equivalent to a 1 sigma statistical variation in 1 second. There will be three types of triggers, two based on rates and one based on images. The first type of trigger is for short time scales (4 msec to 64 msec). These will be traditional triggers (single background) and we check about 25,000 combinations of time-energy-focal plane subregions per second. The second type of trigger will be similar to what is used on HETE: fits to multiple background regions to remove trends for time scales between 64 msec and 64 seconds. About 500 triggers will be checked per second. For these rate triggers, false triggers and variable non-GRB sources will be rejected by requiring a new source to be present in an...

Fenimore, E; Galassi, M; Gehrels, N; Palmer, D; Parsons, A; Tavenner, T; Tller, J

2004-01-01T23:59:59.000Z

254

Force-optimized alignment for optical control of the Advanced Technology Solar Telescope  

Science Journals Connector (OSTI)

We present formalism and analysis of three active alignment reconstruction techniques applied to the Advanced Technology Solar Telescope. The three reconstructors generate optical...

Upton, Robert; Cho, Myung; Rimmele, Thomas

2010-01-01T23:59:59.000Z

255

First Fruits of the Spitzer Space Telescope: Galactic and Solar System Studies  

E-Print Network [OSTI]

This article provides a brief overview of the Spitzer Space Telescope and discusses its initial scientific results on galactic and solar system science.

M. Werner; G. Fazio; G. Rieke; T. Roellig; D. Watson

2006-06-22T23:59:59.000Z

256

E-Print Network 3.0 - atacama telescope ccat Sample Search Results  

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

applicability of Electric Vehicles (EVs) is the scarce capacity of Summary: a main solar panel on the roof and a secondary, telescopic panel under the main panel. When...

257

Aplanatic two mirror telescope from near-normal to grazing incidence  

Science Journals Connector (OSTI)

Surface equations for strictly aplanatic two-mirror telescopes of any configuration are given. They were used in a comparative performance analysis of the general Cassegrainian...

Korsch, Dietrich

1980-01-01T23:59:59.000Z

258

E-Print Network 3.0 - avec les telescopes Sample Search Results  

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

2010 Summary: arcsec ou plus. Possible avec optique adaptative, ou telescopes hors atmosphere. 3- v V + 5 log10... etecter a cause de la turbulence atmospherique,...

259

E-Print Network 3.0 - avec le telescope Sample Search Results  

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

12;Allen Telescope Array ATA Team Source: New Jersey Institute of Technology, Center for Solar-Terrestrial Research Collection: Physics 5 Remerciements Yannick Mellier m'a...

260

July 24, 2009; Visiting Speakers Program - Crossing the Valley of Death - The Role of the SBIR Program by Dr. Charles Wessner  

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

Crossing the Valley of Death Crossing the Valley of Death Crossing the Valley of Death Crossing the Valley of Death The Role of the SBIR Program Department of Energy-NAPA HSS Visiting Speaker Program July 24, 2009 Charles W. Wessner, Ph.D. Director, Technology, Innovation, and Entrepreneurship The National Academies 1 © Charles W. Wessner Ph.D. The Good News and the Bad News New, Substantial Commitments for Technology Innovation, but Myths about the Innovation Process Remain 2009 Stimulus Bill Provides $21.5 Billion: A Short Term Boost for Federal R&D * Basic competitiveness-related research, biomedical research, energy R&D, and climate change programs are high priorities - National Science Foundation - $3.0 billion - National Institutes of Health - $10.4 billion

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


261

The Balloon-borne Large Aperture Sub-millimetre Telescope  

E-Print Network [OSTI]

The Balloon-borne Large-Aperture Sub-millimetre Telescope (BLAST) will operate on a Long Duration Balloon platform with large format bolometer arrays at 250, 350 and 500 microns, initially using a 2m mirror, with plans to increase to 2.5m. BLAST is a collaboration between scientists in the USA, Canada, UK, Italy and Mexico. Funding has been approved and it is now in its building phase. The test flight is scheduled for 2002, with the first long duration flight the following year. The scientific goals are to learn about the nature of distant extragalactic star forming galaxies and cold pre-stellar sources by making deep maps both at high and low galactic latitudes. BLAST will be useful for planning Herschel key projects which use SPIRE.

Douglas Scott; the BLAST Team

2001-04-03T23:59:59.000Z

262

The Greenland Telescope (GLT): Antenna status and future plans  

E-Print Network [OSTI]

The ALMA North America Prototype Antenna was awarded to the Smithsonian Astrophysical Observatory (SAO) in 2011. SAO and the Academia Sinica Institute of Astronomy & Astrophysics (ASIAA), SAO's main partner for this project, are working jointly to relocate the antenna to Greenland to carry out millimeter and submillimeter VLBI observations. This paper presents the work carried out on upgrading the antenna to enable operation in the Arctic climate by the GLT Team to make this challenging project possible, with an emphasis on the unexpected telescope components that had to be either redesigned or changed. Five-years of inactivity, with the antenna laying idle in the desert of New Mexico, coupled with the extreme weather conditions of the selected site in Greenland have it necessary to significantly refurbish the antenna. We found that many components did need to be replaced, such as the antenna support cone, the azimuth bearing, the carbon fiber quadrupod, the hexapod, the HVAC, the tiltmeters, the antenna ...

Raffin, Philippe; Asada, Keichi; Blundell, Raymond; Burgos, Roberto; Chang, Chih-Cheng; Chen, Ming-Tang; Christensen, Robert; Grimes, Paul K; Han, C C; Ho, Paul T P; Huang, Yau-De; Inoue, Makoto; Koch, Patrick M; Kubo, Derek; Leiker, Steve; Liu, Ching-Tang; Martin-Cocher, Pierre; Matsushita, Satoki; Nakamura, Masanori; Nishioka, Hiroaki; Nystrom, George; Paine, Scott N; Patel, Nimesh A; Pradel, Nicolas; Pu, Hung-Yi; Shen, H -Y; Snow, William; Sridharan, T K; Srinivasan, Ranjani; Tong, Edward; Wang, Jackie

2014-01-01T23:59:59.000Z

263

BOOMERANG: A Balloon-borne Millimeter-Wave Telescope  

Science Journals Connector (OSTI)

We describe BOOMERANG, a balloon-borne microwave telescope designed to map the cosmic microwave background at a resolution of 10' from the Long Duration Balloon (LDB) platform. The millimeter-wave receiver employs new technology in bolometers, readout electronics, cold reimaging optics, millimeter-wave filters, and cryogenics to obtain high sensitivity to cosmic microwave background anisotropy. Sixteen detectors observe in four spectral bands centered at 90, 150, 240, and 410 GHz. The wide frequency coverage, the long-duration flight, the optical design, and the observing strategy provide strong rejection of systematic effects. We report the flight performance of the instrument during a 10.5 day stratospheric balloon flight launched from McMurdo Station, Antarctica, that mapped ~2000 square degrees of the sky.

B. P. Crill; P. A. R. Ade; D. R. Artusa; R. S. Bhatia; J. J. Bock; A. Boscaleri; P. Cardoni; S. E. Church; K. Coble; P. de Bernardis; G. de Troia; P. Farese; K. M. Ganga; M. Giacometti; C. V. Haynes; E. Hivon; V. V. Hristov; A. Iacoangeli; W. C. Jones; A. E. Lange; L. Martinis; S. Masi; P. V. Mason; P. D. Mauskopf; L. Miglio; T. Montroy; C. B. Netterfield; C. G. Paine; E. Pascale; F. Piacentini; G. Polenta; F. Pongetti; G. Romeo; J. E. Ruhl; F. Scaramuzzi; D. Sforna; A. D. Turner

2003-01-01T23:59:59.000Z

264

Exact Optics A unification of optical telescope design  

E-Print Network [OSTI]

A perfect focus telescope is one in which all rays parallel to the axis meet at a point and give equal magnification there. It is shown that these two conditions define the shapes of both primary and secondary mirrors. Apart from scale, the solution depends upon two parameters, $s$, which gives the mirror separation in terms of the effective focal length, and $K$, which gives the relative position of the final focus in that unit. The two conditions ensure that the optical systems have neither spherical aberration nor coma, no matter how fast the $f$ ratio. All known coma--free systems emerge as approximate special cases. In his classical paper, K. Schwarzschild studied all two mirror systems whose profiles were conic sections. We make no such a priori shape conditions but demand a perfect focus and solve for the mirrors' shapes.

Lynden-Bell, Donald

2002-01-01T23:59:59.000Z

265

THE ATACAMA COSMOLOGY TELESCOPE: DATA CHARACTERIZATION AND MAPMAKING  

SciTech Connect (OSTI)

We present a description of the data reduction and mapmaking pipeline used for the 2008 observing season of the Atacama Cosmology Telescope (ACT). The data presented here at 148 GHz represent 12% of the 90 TB collected by ACT from 2007 to 2010. In 2008 we observed for 136 days, producing a total of 1423 hr of data (11 TB for the 148 GHz band only), with a daily average of 10.5 hr of observation. From these, 1085 hr were devoted to an 850 deg{sup 2} stripe (11.2 hr by 9. Degree-Sign 1) centered on a declination of -52. Degree-Sign 7, while 175 hr were devoted to a 280 deg{sup 2} stripe (4.5 hr by 4. Degree-Sign 8) centered at the celestial equator. The remaining 163 hr correspond to calibration runs. We discuss sources of statistical and systematic noise, calibration, telescope pointing, and data selection. For the 148 GHz band, out of 1260 survey hours and 1024 detectors in the array, 816 hr and 593 effective detectors remain after data selection, yielding a 38% survey efficiency. The total sensitivity in 2008, determined from the noise level between 5 Hz and 20 Hz in the time-ordered data stream (TOD), is 32 {mu}K{radical}s in cosmic microwave background units. Atmospheric brightness fluctuations constitute the main contaminant in the data and dominate the detector noise covariance at low frequencies in the TOD. The maps were made by solving the least-squares problem using the Preconditioned Conjugate Gradient method, incorporating the details of the detector and noise correlations. Simulations, as well as cross-correlations with Wilkinson Microwave Anisotropy Probe sky maps on large angular scales, reveal that our maps are unbiased at multipoles l > 300. This paper accompanies the public release of the 148 GHz southern stripe maps from 2008. The techniques described here will be applied to future maps and data releases.

Duenner, Rolando; Aguirre, Paula; Barrientos, L. Felipe [Departamento de Astronomia y Astrofisica, Facultad de Fisica, Pontificia Universidad Catolica de Chile, Casilla 306, Santiago 22 (Chile)] [Departamento de Astronomia y Astrofisica, Facultad de Fisica, Pontificia Universidad Catolica de Chile, Casilla 306, Santiago 22 (Chile); Hasselfield, Matthew; Amiri, Mandana; Battistelli, Elia S.; Burger, Bryce [Department of Physics and Astronomy, University of British Columbia, Vancouver, BC V6T 1Z4 (Canada)] [Department of Physics and Astronomy, University of British Columbia, Vancouver, BC V6T 1Z4 (Canada); Marriage, Tobias A.; Acquaviva, Viviana; Das, Sudeep [Department of Astrophysical Sciences, Peyton Hall, Princeton University, Princeton, NJ 08544 (United States)] [Department of Astrophysical Sciences, Peyton Hall, Princeton University, Princeton, NJ 08544 (United States); Sievers, Jon; Appel, John William [Joseph Henry Laboratories of Physics, Jadwin Hall, Princeton University, Princeton, NJ 08544 (United States)] [Joseph Henry Laboratories of Physics, Jadwin Hall, Princeton University, Princeton, NJ 08544 (United States); Addison, Graeme E.; Calabrese, Erminia [Department of Astrophysics, Oxford University, Oxford OX1 3RH (United Kingdom)] [Department of Astrophysics, Oxford University, Oxford OX1 3RH (United Kingdom); Ade, Peter A. R. [School of Physics and Astronomy, Cardiff University, The Parade, Cardiff CF24 3AA (United Kingdom)] [School of Physics and Astronomy, Cardiff University, The Parade, Cardiff CF24 3AA (United Kingdom); Bond, J. Richard [Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON M5S 3H8 (Canada)] [Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON M5S 3H8 (Canada); Brown, Ben [Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260 (United States)] [Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260 (United States); Chervenak, Jay [Code 553/665, NASA/Goddard Space Flight Center, Greenbelt, MD 20771 (United States)] [Code 553/665, NASA/Goddard Space Flight Center, Greenbelt, MD 20771 (United States); Devlin, Mark J.; Dicker, Simon R. [Department of Physics and Astronomy, University of Pennsylvania, 209 South 33rd Street, Philadelphia, PA 19104 (United States)] [Department of Physics and Astronomy, University of Pennsylvania, 209 South 33rd Street, Philadelphia, PA 19104 (United States); and others

2013-01-01T23:59:59.000Z

266

The Fermi Large Area gamma ray Telescope and the current searches for dark matter in space  

E-Print Network [OSTI]

production [6],[7] [9]. The temptation to claim the discovery of dark matter is strongThe Fermi Large Area gamma ray Telescope and the current searches for dark matter in space Aldo Gamma-ray Space Telescope, has detected the largest amount of gamma rays, in the 20MeV 300GeV energy

Morselli, Aldo

267

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

E-Print Network [OSTI]

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

Martin, Chris

268

Proceedings of ICRC 2001: 741 c Copernicus Gesellschaft 2001 Calibration of the Auger Fluorescence Telescopes  

E-Print Network [OSTI]

Norte 304, (5613) Malarg¨ue, Argentina Abstract. Thirty fluorescence telescopes in four stations development (Xmax) and determi- nation of the absolute energy of EHE events. A telescope camera contains 440 in Argentina are discussed. 1 Introduction The southern hemisphere experiment of the Pierre Auger Ob- servatory

269

Design study of 8 meter monolithic mirror UV/optical space telescope H. Philip Stahl  

E-Print Network [OSTI]

Design study of 8 meter monolithic mirror UV/optical space telescope H. Philip Stahl NASA Marshall Space Flight Center, Huntsville, AL 35812 ABSTRACT The planned Ares V launch vehicle with its 10 meter to 8 meter class monolithic primary mirror telescope to Sun-Earth L2 using an Ares V. Specific

Sirianni, Marco

270

Active Optics Performance Study of the Primary Mirror of the Gemini Telescopes Project  

E-Print Network [OSTI]

Active Optics Performance Study of the Primary Mirror of the Gemini Telescopes Project Myung K. Cho Optical Sciences Center in the University of Arizona Tucson, AZ 85721 and Gemini Telescopes Project P. O. Box 26732 Tucson, AZ 85726­6732 Gemini Preprint #9 #12; Active optics performance study of the primary

271

Cornelis Zwaan, open principle, and the future of high-resolution solar telescopes  

E-Print Network [OSTI]

Cornelis Zwaan, open principle, and the future of high-resolution solar telescopes Robert H erected up till 30 m height with sensors at several heights for the measurement of temperature; (iii) the design consequences for the new generation of high-resolution solar telescopes. Keywords

Rutten, Rob

272

March 18, 2010 James Webb Space Telescope Studies of Dark Energy  

E-Print Network [OSTI]

cosmological parameters and dark energy through weak lensing measurements in the COSMOS survey (Massey et al March 18, 2010 James Webb Space Telescope Studies of Dark Energy Jonathan P. Gardner (NASA. Introduction The Hubble Space Telescope (HST) has contributed significantly to studies of dark energy

Sirianni, Marco

273

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

SciTech Connect (OSTI)

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

Ketchum, Christina; /SLAC

2006-09-01T23:59:59.000Z

274

DynamiX, numerical tool for design of next-generation x-ray telescopes  

SciTech Connect (OSTI)

We present a new code aimed at the simulation of grazing-incidence x-ray telescopes subject to deformations and demonstrate its ability with two test cases: the Simbol-X and the International X-ray Observatory (IXO) missions. The code, based on Monte Carlo ray tracing, computes the full photon trajectories up to the detector plane, accounting for the x-ray interactions and for the telescope motion and deformation. The simulation produces images and spectra for any telescope configuration using Wolter I mirrors and semiconductor detectors. This numerical tool allows us to study the telescope performance in terms of angular resolution, effective area, and detector efficiency, accounting for the telescope behavior. We have implemented an image reconstruction method based on the measurement of the detector drifts by an optical sensor metrology. Using an accurate metrology, this method allows us to recover the loss of angular resolution induced by the telescope instability. In the framework of the Simbol-X mission, this code was used to study the impacts of the parameters on the telescope performance. In this paper we present detailed performance analysis of Simbol-X, taking into account the satellite motions and the image reconstruction. To illustrate the versatility of the code, we present an additional performance analysis with a particular configuration of IXO.

Chauvin, Maxime; Roques, Jean-Pierre

2010-07-20T23:59:59.000Z

275

Digital Frequency Domain Multiplexer for mm-Wavelength Telescopes  

SciTech Connect (OSTI)

An FPGA based digital signal processing (DSP) system for biasing and reading out multiplexed bolometric detectors for mm-wavelength telescopes is presented. This readout system is being deployed for balloon-borne and ground based cosmology experiments with the primary goal of measuring the signature of inflation with the Cosmic Microwave Background Radiation. The system consists of analog superconducting electronics running at 250 mK and 4 K, coupled to digital room temperature backend electronics described here. The digital electronics perform the real time functionality with DSP algorithms implemented in firmware. A soft embedded processor provides all of the slow housekeeping control and communications. Each board in the system synthesizes multi-frequency combs of 8 to 32 carriers in the MHz band to bias the detectors. After the carriers have been modulated with the sky-signal by the detectors, the same boards digitize the comb directly. The carriers are mixed down to base-band and low pass filtered. The signal bandwidth of 0.050Hz-100 Hz places extreme requirements on stability and requires powerful filtering techniques to recover the sky-signal from the MHz carriers.

Spieler, Helmuth G; Dobbs, Matt; Bissonnette, Eric; Spieler, Helmuth G.

2007-07-23T23:59:59.000Z

276

The ASTRI Project: a mini-array of dual-mirror small Cherenkov telescopes for CTA  

E-Print Network [OSTI]

ASTRI is a flagship project of the Italian Ministry of Education, University and Research, which aims to develop an end-to-end prototype of the CTA small-size telescope. The proposed design is characterized by a dual-mirror Schwarzschild-Couder configuration and a camera based on Silicon photo-multipliers, two challenging but innovative technological solutions which will be adopted for the first time on a Cherenkov telescope. Here we describe the current status of the project, the expected performance and the possibility to realize a mini-array composed by a few small-size telescopes, which shall be placed at the final CTA Southern Site.

La Palombara, N; Antonelli, L A; Bastieri, D; Bellassai, G; Belluso, M; Bigongiari, C; Billotta, S; Biondo, B; Bonanno, G; Bonnoli, G; Bruno, P; Bulgarelli, A; Canestrari, R; Capalbi, M; Caraveo, P; Carosi, A; Cascone, E; Catalano, O; Cereda, M; Conconi, P; Conforti, V; Cusumano, G; De Caprio, V; De Luca, A; Di Paola, A; Di Pierro, F; Fantinel, D; Fiorini, M; Fugazza, D; Gardiol, D; Ghigo, M; Gianotti, F; Giarrusso, S; Giro, E; Grillo, A; Impiombato, D; Incorvaia, S; La Barbera, A; La Parola, V; La Rosa, G; Lessio, L; Leto, G; Lombardi, S; Lucarelli, F; Maccarone, M C; Malaguti, G; Malaspina, G; Mangano, V; Marano, D; Martinetti, E; Millul, R; Mineo, T; Mist, A; Morello, C; Morlino, G; Panzera, M R; Pareschi, G; Rodeghiero, G; Romano, P; Russo, F; Sacco, B; Sartore, N; Schwarz, J; Segreto, A; Sironi, G; Sottile, G; Stamerra, A; Strazzeri, E; Stringhetti, L; Tagliaferri, G; Testa, V; Timpanaro, M C; Toso, G; Tosti, G; Trifoglio, M; Vallania, P; Vercellone, S; Zitelli, V

2013-01-01T23:59:59.000Z

277

Metal multilayer mirrors for EUV wide field telescopes  

SciTech Connect (OSTI)

Metal multilayer mirrors have been designed for the ALEXIS satellite, which is to carry six wide field telescopes to perform an all-sky survey in three or four narrow wavelength bands in the EUV. Comprised of alternating layers of molybdenum and silicon, the mirrors are optimized to provide maximum reflectivity at angles from 11.5 to 17/degree/ off normal incidence and at wavelengths of 133, 171, or 186A. Simultaneously, the mirrors use a ''wavetrap'' described below to suppress reflectivity at 304A, where the extremely strong geocoronal line of He II causes severe background problems. Low reflectivity at 304A is achieved by superposing two layer pairs that provide destructive interference with an effective 2d spacing of 152A. The Mo layers in this wavetrap must be very thin, about 10A each, in order to allow the shorter wavelengths desired for peak reflectivity to penetrate without significant attenuation. Because refraction changes the effective angle of passage through the wavetrap, a joint optimization between layer thicknesses in the deep layers and the wavetrap layers must be performed for each target peak wavelength. For the 186A mirror, the optimum design from substrate upward is 40 layer pairs, each 74A Si and 31A Mo, followed by 2 layer pairs, each 55A Si and 10A Mo. Calculations predict this design will have a peak reflectivity at 186A of 35 percent and a 304A reflectivity less than 10/sup /minus/5/, if available optical constants are correct and the multilayer can be fabricated without difficulty. We will present details of the calculations and laboratory measurements of the reflectivity performance attained with prototype mirrors. 6 refs., 2 figs.

Smith, B.W.; Bloch, J.J.; Roussel-Dupre,D.

1989-01-01T23:59:59.000Z

278

Large Synoptic Survey Telescope: Dark Energy Science Collaboration  

E-Print Network [OSTI]

This white paper describes the LSST Dark Energy Science Collaboration (DESC), whose goal is the study of dark energy and related topics in fundamental physics with data from the Large Synoptic Survey Telescope (LSST). It provides an overview of dark energy science and describes the current and anticipated state of the field. It makes the case for the DESC by laying out a robust analytical framework for dark energy science that has been defined by its members and the comprehensive three-year work plan they have developed for implementing that framework. The analysis working groups cover five key probes of dark energy: weak lensing, large scale structure, galaxy clusters, Type Ia supernovae, and strong lensing. The computing working groups span cosmological simulations, galaxy catalogs, photon simulations and a systematic software and computational framework for LSST dark energy data analysis. The technical working groups make the connection between dark energy science and the LSST system. The working groups have close linkages, especially through the use of the photon simulations to study the impact of instrument design and survey strategy on analysis methodology and cosmological parameter estimation. The white paper describes several high priority tasks identified by each of the 16 working groups. Over the next three years these tasks will help prepare for LSST analysis, make synergistic connections with ongoing cosmological surveys and provide the dark energy community with state of the art analysis tools. Members of the community are invited to join the LSST DESC, according to the membership policies described in the white paper. Applications to sign up for associate membership may be made by submitting the Web form at http://www.slac.stanford.edu/exp/lsst/desc/signup.html with a short statement of the work they wish to pursue that is relevant to the LSST DESC.

LSST Dark Energy Science Collaboration

2012-11-01T23:59:59.000Z

279

DynamiX, numerical tool for design of next-generation x-ray telescopes  

Science Journals Connector (OSTI)

We present a new code aimed at the simulation of grazing-incidence x-ray telescopes subject to deformations and demonstrate its ability with two test cases: the Simbol-X and the...

Chauvin, Maxime; Roques, Jean-Pierre

2010-01-01T23:59:59.000Z

280

Advanced Technology Solar Telescope 4.2 m Off-axis Primary Mirror Fabrication  

Science Journals Connector (OSTI)

Advanced optical surfacing technologies are applied for the Advanced Technology Solar Telescope 4.2 m off-axis primary mirror fabrication. A newly developed Stressed lap and IR...

Kim, Dae Wook; Oh, Chang Jin; Su, Peng; Burge, James H

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281

NASA'S NEXT GENERATION SPACE TELESCOPE: VISITING A TIME WHEN GALAXIES WERE YOUNG  

Science Journals Connector (OSTI)

NASA's next great endeavor, a space telescope to study the origin of galaxies, is in its formulative phase. Seery and Smith update readers on the paradigms, processes, and optical...

Seery, Bernard D; Smith, Eric P

1998-01-01T23:59:59.000Z

282

Advanced Technology Large-Aperture Space Telescope (ATLAST): A Technology Roadmap for the Next Decade  

E-Print Network [OSTI]

The Advanced Technology Large-Aperture Space Telescope (ATLAST) is a set of mission concepts for the next generation of UVOIR space observatory with a primary aperture diameter in the 8-m to 16-m range that will allow us to perform some of the most challenging observations to answer some of our most compelling questions, including "Is there life elsewhere in the Galaxy?" We have identified two different telescope architectures, but with similar optical designs, that span the range in viable technologies. The architectures are a telescope with a monolithic primary mirror and two variations of a telescope with a large segmented primary mirror. This approach provides us with several pathways to realizing the mission, which will be narrowed to one as our technology development progresses. The concepts invoke heritage from HST and JWST design, but also take significant departures from these designs to minimize complexity, mass, or both. Our report provides details on the mission concepts, shows the extraordinary s...

Postman, Marc

2009-01-01T23:59:59.000Z

283

Thin optic surface analysis for high resolution X-ray telescopes  

E-Print Network [OSTI]

The art of glass developed throughout the years has covered artifacts ranging from crude ornaments to high precision optics used in flat panel displays, hard disk drives, and x-ray telescopes. Methods for manufacturing ...

Akilian, Mireille

2004-01-01T23:59:59.000Z

284

E-Print Network 3.0 - african large telescope Sample Search Results  

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

The Anglo-Australian Telescope 12;15 12;16 The 2dF 6 element... Midi Observatory (French Pyrenees) 12;42 The Overwhelmingly Large ... Source: Parker, Quentin A. -...

285

A wide field X-ray telescope for astronomical survey purposes: from theory to practice  

Science Journals Connector (OSTI)

......act directly on the mirror design. The Wolter-Schwarzschild telescope eliminates...Wolter I and Wolter-Schwarzschild single mirror shells. Figure 3 Differences...analysis for a Wolter-Schwarzschild mirror shell and for our optimized......

Paolo Conconi; Sergio Campana; Gianpiero Tagliaferri; Giovanni Pareschi; Oberto Citterio; Vincenzo Cotroneo; Laura Proserpio; Marta Civitani

2010-06-21T23:59:59.000Z

286

Photosensor Characterization for the Cherenkov Telescope Array: Silicon Photomultiplier versus Multi-Anode Photomultiplier Tube  

E-Print Network [OSTI]

Photomultiplier tube technology has been the photodetector of choice for the technique of imaging atmospheric Cherenkov telescopes since its birth more than 50 years ago. Recently, new types of photosensors are being contemplated for the next generation Cherenkov Telescope Array. It is envisioned that the array will be partly composed of telescopes using a Schwarzschild-Couder two mirror design never built before which has significantly improved optics. The camera of this novel optical design has a small plate scale which enables the use of compact photosensors. We present an extensive and detailed study of the two most promising devices being considered for this telescope design: the silicon photomultiplier and the multi-anode photomultiplier tube. We evaluated their most critical performance characteristics for imaging gamma-ray showers, and we present our results in a cohesive manner to clearly evaluate the advantages and disadvantages that both types of device have to offer in the context of GeV-TeV gamma...

Bouvier, Aurelien; Johnson, Caitlin; Kuznetsov, Andrey; Williams, David; Otte, Nepomuk; Strausbaugh, Robert; Hidaka, Naoya; Tajima, Hiroyasu; Hinton, Jim; White, Richard; Errando, Manel; Mukherjee, Reshmi

2013-01-01T23:59:59.000Z

287

Three-Mirror Anastigmat Telescope with an Unvignetted Flat Focal Plane  

Science Journals Connector (OSTI)

......anastigmat with a two-mirror system except for some special cases (Schwarzschild 1905; Burch 1947). 3. Three-Mirror System In our three-mirror...Academic Press). Schwarzschild K. 1905, Investigations...Optics II, Theory of Mirror Telescopes, English......

Kyoji Nariai; Masanori Iye

2005-04-25T23:59:59.000Z

288

Digital signal processing hardware for a fast fourier transform radio telescope  

E-Print Network [OSTI]

21-cm tomography is a devoloping technique for measuring the Epoch of Reionization in the universe's history. The nature of the signal measured in 21-cm tomography is such that a new kind of radio telescope is needed: one ...

Losh, Jonathan L

2012-01-01T23:59:59.000Z

289

Watching an uniformly moving source of light using a telescope and a frequency-meter  

E-Print Network [OSTI]

We propose a scenario that involves a stationary observer who detects a point like source of light moving with constant velocity at a constant altitude, using a telescope and a frequency-meter. We derive a formula for the angular velocity at which we should rotate the axis of the telescope and a formula that relates the proper period at which the source emits successive wave crests and the proper period at which the stationary observer receives them

Bernhard Rothenstein; Ioan Damian

2005-04-04T23:59:59.000Z

290

Calibration of Cangaroo II Telescope Using a Fast Blue LED Light Flasher  

E-Print Network [OSTI]

Calibration of Cangaroo II Telescope Using a Fast Blue LED Light Flasher John R. Patterson, David L;=460 nm) LED type Nichia (NSPB 510S), which has a temperature stable light output and a risetime of #24; 1.physics.adelaide.edu.au/astrophysics/cangaroo.html #12; FIGURE 1. The LED asher/telescope with the Ramsden eyepiece #12;tted and a previous LED holder

Enomoto, Ryoji

291

Watcher: A Telescope for Rapid Gamma-Ray Burst Follow-Up Observations  

SciTech Connect (OSTI)

The Watcher telescope is planned to begin operation in Spring 2004 in South Africa.The system has been designed to respond primarily to very precise (arcminute) gamma-ray burst locations distributed via the internet by the GCN. Watcher will be fully automatic and the planned response time for GRBs is {approx} 30 seconds or better. In addition, the telescope will be used for blazar monitoring and the photometric detection of extra-solar planets when GRBs are not being observed.

French, J.; Hanlon, L.; McBreen, B.; McBreen, S.; Moran, L. [Department of Experimental Physics, University College Dublin, Dublin 4 (Ireland); Smith, N.; Giltinan, A. [Department of Applied Physics and Instrumentation, Cork Institute of Technology, Bishopstown, Co. Cork (Ireland); Meintjes, P.; Hoffman, M. [Physics Department, University of the Free State, Bloemfontein (South Africa)

2004-09-28T23:59:59.000Z

292

Proto-Model of an Infrared Wide-Field Off-Axis Telescope  

E-Print Network [OSTI]

We develop a proto-model of an off-axis reflective telescope for infrared wide-field observations based on the design of Schwarzschild-Chang type telescope. With only two mirrors, this design achieves an entrance pupil diameter of 50 mm and an effective focal length of 100 mm. We can apply this design to a mid-infrared telescope with a field of view of 8 deg X 8 deg. In spite of the substantial advantages of off-axis telescopes in the infrared compared to refractive or on-axis reflective telescopes, it is known to be difficult to align the mirrors in off-axis systems because of their asymmetric structures. Off-axis mirrors of our telescope are manufactured at the Korea Basic Science Institute (KBSI). We analyze the fabricated mirror surfaces by fitting polynomial functions to the measured data. We accomplish alignment of this two-mirror off-axis system using a ray tracing method. A simple imaging test is performed to compare a pinhole image with a simulated prediction.

Kim, Sanghyuk; Chang, Seunghyuk; Kim, Geon Hee; Yang, Sun Choel; Kim, Myung Sang; Lee, Sungho; Lee, Hanshin; 10.5303/JKAS.2010.43.5.169

2010-01-01T23:59:59.000Z

293

Design of a 7m Davies-Cotton Cherenkov telescope mount for the high energy section of the Cherenkov Telescope Array  

E-Print Network [OSTI]

The Cherenkov Telescope Array is the next generation ground-based observatory for the study of very-high-energy gamma-rays. It will provide an order of magnitude more sensitivity and greater angular resolution than present systems as well as an increased energy range (20 GeV to 300 TeV). For the high energy portion of this range, a relatively large area has to be covered by the array. For this, the construction of ~7 m diameter Cherenkov telescopes is an option under study. We have proposed an innovative design of a Davies-Cotton mount for such a telescope, within Cherenkov Telescope Array specifications, and evaluated its mechanical and optical performance. The mount is a reticulated-type structure with steel tubes and tensioned wires, designed in three main parts to be assembled on site. In this work we show the structural characteristics of the mount and the optical aberrations at the focal plane for three options of mirror facet size caused by mount deformations due to wind and gravity.

Rovero, A C; Vallejo, G; Supanitsky, A D; Actis, M; Botani, A; Ochoa, I; Hughes, G

2013-01-01T23:59:59.000Z

294

Large Synoptic Survey Telescope: From Science Drivers to Reference Design  

SciTech Connect (OSTI)

In the history of astronomy, major advances in our understanding of the Universe have come from dramatic improvements in our ability to accurately measure astronomical quantities. Aided by rapid progress in information technology, current sky surveys are changing the way we view and study the Universe. Next-generation surveys will maintain this revolutionary progress. We focus here on the most ambitious survey currently planned in the visible band, the Large Synoptic Survey Telescope (LSST). LSST will have unique survey capability in the faint time domain. The LSST design is driven by four main science themes: constraining dark energy and dark matter, taking an inventory of the Solar System, exploring the transient optical sky, and mapping the Milky Way. It will be a large, wide-field ground-based system designed to obtain multiple images covering the sky that is visible from Cerro Pachon in Northern Chile. The current baseline design, with an 8.4 m (6.5 m effective) primary mirror, a 9.6 deg{sup 2} field of view, and a 3,200 Megapixel camera, will allow about 10,000 square degrees of sky to be covered using pairs of 15-second exposures in two photometric bands every three nights on average. The system is designed to yield high image quality, as well as superb astrometric and photometric accuracy. The survey area will include 30,000 deg{sup 2} with {delta} < +34.5{sup o}, and will be imaged multiple times in six bands, ugrizy, covering the wavelength range 320-1050 nm. About 90% of the observing time will be devoted to a deep-wide-fast survey mode which will observe a 20,000 deg{sup 2} region about 1000 times in the six bands during the anticipated 10 years of operation. These data will result in databases including 10 billion galaxies and a similar number of stars, and will serve the majority of science programs. The remaining 10% of the observing time will be allocated to special programs such as Very Deep and Very Fast time domain surveys. We describe how the LSST science drivers led to these choices of system parameters.

Ivezic, Z.; Axelrod, T.; Brandt, W.N.; Burke, D.L.; Claver, C.F.; Connolly, A.; Cook, K.H.; Gee, P.; Gilmore, D.K.; Jacoby, S.H.; Jones, R.L.; Kahn, S.M.; Kantor, J.P.; Krabbendam, V.; Lupton, R.H.; Monet, D.G.; Pinto, P.A.; Saha, A.; Schalk, T.L.; Schneider, D.P.; Strauss, Michael A.; /Washington U., Seattle, Astron. Dept. /LSST Corp. /Penn State U., Astron. Astrophys. /KIPAC, Menlo Park /NOAO, Tucson /LLNL, Livermore /UC, Davis /Princeton U., Astrophys. Sci. Dept. /Naval Observ., Flagstaff /Arizona U., Astron. Dept. - Steward Observ. /UC, Santa Cruz /Harvard U. /Johns Hopkins U. /Illinois U., Urbana

2011-10-14T23:59:59.000Z

295

Expected performance of the ASTRI-SST-2M telescope prototype  

E-Print Network [OSTI]

ASTRI (Astrofisica con Specchi a Tecnologia Replicante Italiana) is an Italian flagship project pursued by INAF (Istituto Nazionale di Astrofisica) strictly linked to the development of the Cherenkov Telescope Array, CTA. Primary goal of the ASTRI program is the design and production of an end-to-end prototype of a Small Size Telescope for the CTA sub-array devoted to the highest gamma-ray energy region. The prototype, named ASTRI SST-2M, will be tested on field in Italy during 2014. This telescope will be the first Cherenkov telescope adopting the double reflection layout in a Schwarzschild-Couder configuration with a tessellated primary mirror and a monolithic secondary mirror. The collected light will be focused on a compact and light-weight camera based on silicon photo-multipliers covering a 9.6 deg full field of view. Detailed Monte Carlo simulations have been performed to estimate the performance of the planned telescope. The results regarding its energy threshold, sensitivity and angular resolution ar...

Bigongiari, C; Morello, C; Stamerra, A; Vallania, P; Agnetta, G; Antonelli, L A; Bastieri, D; Bellassai, G; Belluso, M; Billotta, S; Biondo, B; Bonanno, G; Bonnoli, G; Bruno, P; Bulgarelli, A; Canestrari, R; Capalbi, M; Caraveo, P; Carosi, A; Cascone, E; Catalano, O; Cereda, M; Conconi, P; Conforti, V; Cusumano, G; De Caprio, V; De Luca, A; Di Paola, A; Fantinel, D; Fiorini, M; Fugazza, D; Gardiol, D; Ghigo, M; Gianotti, F; Giarrusso, S; Giro, E; Grillo, A; Impiombato, D; Incorvaia, S; La Barbera, A; La Palombara, N; La Parola, V; La Rosa, G; Lessio, L; Leto, G; Lombardi, S; Lucarelli, F; Maccarone, M C; Malaguti, G; Malaspina, G; Mangano, V; Marano, D; Martinetti, E; Millul, R; Mineo, T; Mist, A; Morlino, G; Panzera, M R; Pareschi, G; Rodeghiero, G; Romano, P; Russo, F; Sacco, B; Sartore, N; Schwarz, J; Segreto, A; Sironi, G; Sottile, G; Strazzeri, E; Stringhetti, L; Tagliaferri, G; Testa, V; Timpanaro, M C; Toso, G; Tosti, G; Trifoglio, M; Vercellone, S; Zitelli, V; Arrabito, L; Bernlohr, K; Maier, G; Komin, N

2013-01-01T23:59:59.000Z

296

Monte Carlo simulations of alternative sky observation modes with the Cherenkov Telescope Array  

E-Print Network [OSTI]

We investigate possible sky survey modes with the Middle Sized Telescopes (MST, aimed at covering the energy range from $\\sim$100 GeV to 10 TeV) subsystem of the Cherenkov Telescope Array (CTA). We use the standard CTA tools, CORSIKA and sim_telarray, to simulate the development of gamma-ray showers, proton background and the telescope response. We perform simulations for the H.E.S.S.-site in Namibia, which is one of the candidate sites for the CTA experiment. We study two previously considered modes, parallel and divergent, and we propose a new, convergent mode with telescopes tilted toward the array center. For each mode we provide performance parameters crucial for choosing the most efficient survey strategy. For the non-parallel modes we study the dependence on the telescope offset angle. We show that use of both the divergent and convergent modes results in potential advantages in comparison with use of the parallel mode. The fastest source detection can be achieved in the divergent mode with larger offs...

Szanecki, M; Nied?wiecki, A; Sitarek, J; Bednarek, W

2015-01-01T23:59:59.000Z

297

Wide Field Hard X-ray Survey Telescope: ProtoEXIST1  

E-Print Network [OSTI]

We report our progress on the development of pixellated imaging CZT detector arrays for our first-generation balloon-borne wide-field hard X-ray (20 - 600 keV) telescope, ProtoEXIST1. Our ProtoEXIST program is a pathfinder for the High Energy Telescope (HET) on the Energetic X-ray Imaging Survey telescope (EXIST), a proposed implementation of the Black Hole Finder Probe. ProtoEXIST1 consists of four independent coded-aperture telescopes with close-tiled (~0.4 mm gaps) CZT detectors that preserve their 2.5mm pixel pitch. Multiple shielding/field-of-view configurations are planned to identify optimal geometry for the HET in EXIST. The primary technical challenge in ProtoEXIST is the development of large area, close-tiled modules of imaging CZT detectors (1000 cm2 for ProtoEXIST1), with all readout and control systems for the ASIC readout vertically stacked. We describe the overall telescope configuration of ProtoEXIST1 and review the current development status of the CZT detectors, from individual detector crys...

Hong, J; Chammas, N; Allen, B; Copete, A; Said, B; Burke, M; Howell, J; Gauron, T; Baker, R G; Barthelmy, S D; Sheikh, S; Gehrels, N; Cook, W R; Burnham, J A; Harrison, F A; Collins, J; Labov, S; Garson, A; Krawczynski, H

2007-01-01T23:59:59.000Z

298

An Improved Calibration Framework for Electromagnetic Tracking Devices Milan Ikits 1;2 J. Dean Brederson 1;2 Charles D. Hansen 1;2 John M. Hollerbach 2  

E-Print Network [OSTI]

School of Computing University of Utah 50 Central Campus Drive Rm 3490 Salt Lake City, UT 84112­9205, USA Brederson 1;2 Charles D. Hansen 1;2 John M. Hollerbach 2 1 Scientific Computing and Imaging Institute, 2

Utah, University of

299

Statement of Charles G. Groat Director, U.S. Geological Survey, U.S. Depa...rce and Agency Organization, On The Yucca Mountain Project, April 5, 2005 Congressional Testimony, 2005  

E-Print Network [OSTI]

Organization, On The Yucca Mountain Project, April 5, 2005 Congressional Testimony, 2005 Statement of Charles G on Government Reform, Subcommittee on the Federal Workforce and Agency Organization On The Yucca Mountain's (DOE) Yucca Mountain Project. Let me emphasize from the outset how seriously USGS takes this situation

Torgersen, Christian

300

Profile of Charles Stanish  

Science Journals Connector (OSTI)

...endeavor marks a shift in emphasis from shovel-and-pick site scouring to model-based social science. To explain the discipline, Stanish...the trade routes, he adds. Goods, including pottery, wool, jaguar pelts, and cocoa leaves, likely traveled along these...

Prashant Nair

2012-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "telescope baltay charles" 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

PAIGE NOVAK CHARLES FAIRHURST  

E-Print Network [OSTI]

awards. I am thrilled to report our building remediation is nearly complete. We are making the inside's Research and Innovative Technology Administrati

Levinson, David M.

302

South Pole Telescope helps Argonne scientists study earliest ages of the  

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

Related Content Related Content Employee Spotlight: Clarence Chang South Pole Telescope helps Argonne scientists study earliest ages of the universe By Louise Lerner * October 28, 2013 Tweet EmailPrint For physicist Clarence Chang at the U.S. Department of Energy's (DOE) Argonne National Laboratory, looking backward in time to the earliest ages of the universe is all in a day's work. Chang helped design and operate part of the South Pole Telescope, a project that aims a giant telescope at the night sky to track tiny bits of radiation that are still traveling across the universe from the period just after it was born. "Basically, what we're looking at is the afterglow light of the Big Bang," Chang said. In the wake of the Big Bang, all the matter in the universe was just hot,

303

Schwarzschild-Couder two-mirror telescope for ground-based gamma-ray astronomy  

E-Print Network [OSTI]

Schwarzschild-type aplanatic telescopes with two aspheric mirrors, configured to correct spherical and coma aberrations, are considered for application in gamma-ray astronomy utilizing the ground-based atmospheric Cherenkov technique. We use analytical descriptions for the figures of primary and secondary mirrors and, by means of numerical ray-tracing, we find telescope configurations which minimize astigmatism and maximize effective light collecting area. It is shown that unlike the traditional prime-focus Davies-Cotton design, such telescopes provide a solution for wide field of view gamma-ray observations. The designs are isochronous, can be optimized to have no vignetting across the field, and allow for significant reduction of the plate scale, making them compatible with finely-pixilated cameras, which can be constructed from modern, cost-effective image sensors such as multi-anode PMTs, SiPMs, or image intensifiers.

Vasilev, V V

2007-01-01T23:59:59.000Z

304

Autonomous Observing and Control Systems for PAIRITEL, a 1.3m Infrared Imaging Telescope  

E-Print Network [OSTI]

The Peters Automated Infrared Imaging Telescope (PAIRITEL) is the first meter-class telescope operating as a fully robotic IR imaging system. Dedicated in October 2004, PAIRITEL began regular observations in mid-December 2004 as part of a 1.5 year commissioning period. The system was designed to respond without human intervention to new gamma-ray burst transients: this milestone was finally reached on November 9, 2005 but the telescope had a number of semi-automated sub-10 minute responses throughout early commissioning. When not operating in Target of Opportunity mode, PAIRITEL performs a number of queue scheduled transient monitoring campaigns. To achieve this level of automation, we have developed communicating tools to connect the various sub-systems: an intelligent queue scheduling database, run-time configurable observation sequence software, a data reduction pipeline, and a master state machine which monitors and controls all functions within and affecting the observatory.

J. S. Bloom; Dan L. Starr; Cullen H. Blake; M. F. Skrutskie; Emilio E. Falco

2005-11-30T23:59:59.000Z

305

Schwarzschild-Couder two-mirror telescope for ground-based gamma-ray astronomy  

E-Print Network [OSTI]

Schwarzschild-type aplanatic telescopes with two aspheric mirrors, configured to correct spherical and coma aberrations, are considered for application in gamma-ray astronomy utilizing the ground-based atmospheric Cherenkov technique. We use analytical descriptions for the figures of primary and secondary mirrors and, by means of numerical ray-tracing, we find telescope configurations which minimize astigmatism and maximize effective light collecting area. It is shown that unlike the traditional prime-focus Davies-Cotton design, such telescopes provide a solution for wide field of view gamma-ray observations. The designs are isochronous, can be optimized to have no vignetting across the field, and allow for significant reduction of the plate scale, making them compatible with finely-pixilated cameras, which can be constructed from modern, cost-effective image sensors such as multi-anode PMTs, SiPMs, or image intensifiers.

V. V. Vassiliev; S. J. Fegan

2007-08-21T23:59:59.000Z

306

Frozen Telescope Looks to Ends of the Earth for Answers | Department of  

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

Frozen Telescope Looks to Ends of the Earth for Answers Frozen Telescope Looks to Ends of the Earth for Answers Frozen Telescope Looks to Ends of the Earth for Answers May 3, 2012 - 2:20pm Addthis Researchers drilled holes in the ice to a depth of almost 1.5 miles, and lowered 60 basketball-sized detectors called digital optical modules (DOMs) into each of the 86 holes. They then had to pull cables to connect the sensors to IceCube Lab’s servers in order to collect data. | Photo courtesy of the National Science Foundation Researchers drilled holes in the ice to a depth of almost 1.5 miles, and lowered 60 basketball-sized detectors called digital optical modules (DOMs) into each of the 86 holes. They then had to pull cables to connect the sensors to IceCube Lab's servers in order to collect data. | Photo

307

First search for neutrinos in correlation with gamma-ray bursts with the ANTARES neutrino telescope  

SciTech Connect (OSTI)

A search for neutrino-induced muons in correlation with a selection of 40 gamma-ray bursts that occurred in 2007 has been performed with the ANTARES neutrino telescope. During that period, the detector consisted of 5 detection lines. The ANTARES neutrino telescope is sensitive to TeVPeV neutrinos that are predicted from gamma-ray bursts. No events were found in correlation with the prompt photon emission of the gamma-ray bursts and upper limits have been placed on the flux and fluence of neutrinos for different models.

NONE

2013-03-01T23:59:59.000Z

308

The Liverpool Telescope Automatic Pipeline for Real-time GRB Afterglow Detection  

E-Print Network [OSTI]

The 2-m robotic Liverpool Telescope (LT) is ideally suited to the rapid follow-up of unpredictable and transient events such as GRBs. Our GRB follow-up strategy is designed to identify optical/IR counterparts in real time; it involves the automatic triggering of initial observations, on receipt of an alert from Gamma Ray Observatories HETE-2, INTEGRAL and Swift, followed by automated data reduction, analysis, OT identification and subsequent observing mode choice. The lack of human intervention in this process requires robustness at all stages of the procedure. Here we describe the telescope, its instrumentation and GRB pipeline.

A. Gomboc; A. Monfardini; C. Guidorzi; C. G. Mundell; C. J. Mottram; S. N. Fraser; R. J. Smith; I. A. Steele; D. Carter; M. F. Bode; A. M. Newsam

2005-02-24T23:59:59.000Z

309

collab meeting-5-1_split.xls  

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

Zeroth order agenda Zeroth order agenda SNAP Collaboration Meeting 6, 7, and 8 June, 2005 Plenary 9:00am SNAP Progress (30) Saul/Levi Project Status (30) Heetderks CCD development Holland 10:30am Break (30) 11:00am CCD assembly Baltay NIR development Tarle Focal Plane Bebek Telescope/ TMA-68 Lampton 12:30pm Lunch (90) 2:00pm Dark Energy Task Force (15) Cahn SDT Panel Discussion (30) Baltay SN Factory (30) Aldering Computing (30) McKee 3:30pm Break (30) 4:00pm Electronics Hvd Lippe Calibration Deustua Spectrograph Demo Ealet 6:00pm reception @ Henry's Monday Tuesday Parallel 1 Parallel 2 Parallel 3 NIR 1 Tarle W / L, Simulation, & LSST Sim Team Rhodes Tests of Raytheon HgCdTe SRA #141(15+3) Brown Tests of Rockwell Banded Array FPA#25 (15+3) Schubnell NIR Detector Noise (15+3) Smith GSFC (10+2) Woodgate Status of InGaAs Testing at JPL(10+2)

310

Pixelized Gas Micro-well Detectors for Advanced Gamma-ray Telescopes  

E-Print Network [OSTI]

We describe possible applications of pixelized micro-well detectors (PMWDs) as three-dimensional charged particle trackers in advanced gamma-ray telescope concepts. A micro-well detector consists of an array of individual micro-patterned gas proportional counters opposite a planar drift electrode. When combined with pixelized thin film transistor (TFT) array readouts, large gas volumes may be imaged with very good spatial and energy resolution at reasonable cost. The third dimension is determined by timing the drift of the ionization electrons. The primary advantage of this technique is the very low scattering that the charged particles experience in a gas tracking volume, and the very accurate determination of the initial particle momenta that is thus achieved. We consider two applications of PMWDs to gamma-ray astronomy: 1) A tracker for an Advanced Compton Telescope (ACT) in which the recoil electron from the initial Compton scatter may be accurately tracked, greatly reducing the telescope's point spread function and increasing its polarization sensitivity; and 2) an Advanced Pair Telescope (APT) whose angular resolution is limited primarily by the nuclear recoil and which achieves useful polarization sensitivity near 100 MeV. We have performed Geant4 simulations of both these concepts to estimate their angular resolution and sensitivity for reasonable mission designs.

P. F. Bloser; S. D. Hunter

2004-05-14T23:59:59.000Z

311

Constellation-X Spectroscopy X-Ray Telescope Segmented Optic Assembly and Alignment Implementation  

E-Print Network [OSTI]

. ABSTRACT The Constellation-X mission will perform X-Ray science with improvements in energy resolutionConstellation-X Spectroscopy X-Ray Telescope Segmented Optic Assembly and Alignment Implementation and effective area over its predecessor missions. The primary instrument on each of the four Constellation

312

Search for Short Duration Bursts of TeV Gamma Rays with the Milagrito Telescope  

E-Print Network [OSTI]

OG 2.3.07 Search for Short Duration Bursts of TeV Gamma Rays with the Milagrito Telescope Gus for short duration bursts of TeV photons. Such bursts may result from "traditional" gamma-ray bursts to gamma-ray bursts, the final stages of black hole evaporation) the most compelling reason may

California at Santa Cruz, University of

313

On the use of Cherenkov Telescopes for outer Solar system body occultations  

Science Journals Connector (OSTI)

......and constrain models of Solar system dynamics (e...distant reaches of the Solar system, our ability...objects in the outer Solar system is . Objects larger...VERITAS) 2 and the High Energy Stereoscopic System...telescope, we first project their positions on to......

Brian C. Lacki

2014-01-01T23:59:59.000Z

314

Design Considerations for the Next Generation of Atmospheric Imaging Cherenkov Telescopes  

E-Print Network [OSTI]

We estimate the limiting angular resolution and detection area for an array of 3 large-aperture Imaging Atmospheric Cherenkov Telescopes. We consider an idealized IACT system in order to understand the limitations imposed by the intrinsic nature of the atmospheric showers and geometry of the detector configuration. The idealization includes the assumptions of a perfect optical system and the absence of the night sky background with the goal of finding the optimum camera geometry and array configuration independent of detailed assumptions about the telescope design. The showers are simulated using the ALTAI code for the altitude of 2700 m corresponding to one of possible future sites for a new northern-hemisphere array. The optimal design depends on the target energy range; for each energy we vary both the cell length (telescope spacing) and the image processing parameters in order to maximize the signal-to-noise ratio. We then present the resulting values of the detection area and the angular resolution for this energy dependent optimization. We discuss the dependence of these quantities on the field of view of the telescopes and pixel size of the camera.

V. V. Bugaev; J. H. Buckley; H. Krawczynski

2007-09-29T23:59:59.000Z

315

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

316

Evryscope science: exploring the potential of all-sky gigapixel-scale telescopes  

E-Print Network [OSTI]

Low-cost mass-produced sensors and optics have recently made it feasible to build telescope arrays which observe the entire accessible sky simultaneously. In this article we discuss the scientific motivation for these telescopes, including exoplanets, stellar variability and extragalactic transients. To provide a concrete example we detail the goals and expectations for the Evryscope, an under-construction 780 MPix telescope which covers 8,660 square degrees in each two-minute exposure; each night, 18,400 square degrees will be continuously observed for an average of approximately 6 hours. Despite its small 61mm aperture, the system's large field of view provides an etendue which is ~10% of LSST. The Evryscope, which places 27 separate individual telescopes into a common mount which tracks the entire accessible sky with only one moving part, will return 1%-precision, many-year-length, high-cadence light curves for every accessible star brighter than mV=16.5, with brighter stars having few-millimagnitude photo...

Law, Nicholas M; Ratzloff, Jeffrey; Wulfken, Philip; Kavanaugh, Dustin; Sitar, David J; Pruett, Zachary; Birchart, Mariah; Barlow, Brad; Cannon, Kipp; Cenko, S Bradley; Dunlap, Bart; Kraus, Adam; Maccarone, Thomas J

2015-01-01T23:59:59.000Z

317

Comparison of Different Trigger and Readout Approaches for Cameras in the Cherenkov Telescope Array Project  

E-Print Network [OSTI]

The Cherenkov Telescope Array (CTA) is a next-generation ground-based observatory for g -rays with energies between some ten GeV and a few hundred TeV. CTA is currently in the advanced design phase and will consist of arrays with different size of prime-focus Cherenkov telescopes, to ensure a proper energy coverage from the threshold up to the highest energies. The extension of the CTA array with double-mirror Schwarzschild- Couder telescopes is planned to improve the array angular resolution over wider field of view.We present an end-to-end Monte-Carlo comparison of trigger concepts for the different imaging cameras that will be used on the Cherenkov telescopes. The comparison comprises three alternative trigger schemes (analog, majority, flexible pattern analysis) for each camera design. The study also addresses the influence of the properties of the readout system (analog bandwidth of the electronics, length of the readout window in time) and uses an offline shower reconstruction to investigate the impact ...

Shayduk, M; Schwanke, U

2013-01-01T23:59:59.000Z

318

Disentangling between low order telescope aberrations and segmentation errors using a Shack-Hartmann sensor  

E-Print Network [OSTI]

in the Southern Hemisphere Karl-Schwarzschild-Str. 2, Garching, Germany A BST R A C T The shape correction of the mirrors is a crucial operation to obtain diffraction limited images in actively controlled telescopes. If the mirror is not monolithic, the segmentation errors introduced by piston, tip and tilt of the segments

Liske, Jochen

319

The Animated Gamma-ray Sky Revealed by the Fermi Gamma-ray Space Telescope  

ScienceCinema (OSTI)

The Fermi Gamma-ray Space Telescope has been observing the sky in gamma-rays since August 2008. In addition to breakthrough capabilities in energy coverage (20 MeV-300 GeV) and angular resolution, the wide field of view of the Large Area Telescope enables observations of 20% of the sky at any instant, and of the whole sky every three hours. It has revealed a very animated sky with bright gamma-ray bursts flashing and vanishing in minutes, powerful active galactic nuclei flaring over hours and days, many pulsars twinkling in the Milky Way, and X-ray binaries shimmering along their orbit. Most of these variable sources had not been seen by the Fermi predecessor, EGRET, and the wealth of new data already brings important clues to the origin of the high-energy emission and particles powered by the compact objects. The telescope also brings crisp images of the bright gamma-ray emission produced by cosmic-ray interactions in the interstellar medium, thus allowing to measure the cosmic nuclei and electron spectra across the Galaxy, to weigh interstellar clouds, in particular in the dark-gas phase. The telescope sensitivity at high energy will soon provide useful constraints on dark-matter annihilations in a variety of environments. I will review the current results and future prospects of the Fermi mission.

Isabelle Grenier

2010-01-08T23:59:59.000Z

320

Observations of the Isotropic Diffuse Gamma-ray Background with the EGRET Telescope  

E-Print Network [OSTI]

An Isotropic Diffuse Gamma-Ray Background (IDGRB) in the spectral range 30-10,000 MeV was first reported in the early 1970's using measurements made by the SAS-2 instrument. Data recorded by the Energetic Gamma Ray Experiment Telescope (EGRET) on board the Compton Gamma Ray Observatory (CGRO) over the last 4 years are analysed in order to extract the best measurement yet made of the IDGRB. Extensive analysis of the EGRET instrumental background is presented in order to demonstrate that an uncontaminated data set can be extracted from the EGRET data. A model of the high latitude galactic diffuse foreground emission is presented and the existence of an IDGRB is confirmed. Spatial and spectral analysis of this background is presented. In addition, point source analysis at high galactic latitudes is performed to reveal the existence of a population of extragalactic sources. The characteristics of this population are examined and models of its flux distribution are reported. The question of whether the IDGRB is composed of unresolved point sources is addressed using fluctuation analysis. Finally, possible future directions for gamma ray astronomy are examined through simulations of a future gamma ray telescope: the Gamma-ray Large Area Space Telescope (GLAST). The GLAST baseline design is described and its scientific performance is evaluated. The ability of this telescope to detect 1,000-10,000 new extragalactic sources is demonstrated and the likely impact on the study of the IDGRB is considered.

T. D. Willis

2002-01-30T23:59:59.000Z

Note: This page contains sample records for the topic "telescope baltay charles" 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

The South Pole Telescope: A white paper for the Dark Energy Task Force  

E-Print Network [OSTI]

redshifts, the statistical power of the survey yields are sufficient to measure the dark energy equation energy constraints are derived from the SPT SZE survey results. To test theories of dark energyThe South Pole Telescope: A white paper for the Dark Energy Task Force J. E. Carlstrom, C. Chang, T

Collar, Juan I.

322

Science Yield of an Improved Wide Field Infrared Survey Telescope (WFIRST) M. E. Levi1  

E-Print Network [OSTI]

Survey Telescope (WFIRST) to efficiently conduct three kinds of studies: dark energy surveys, exoplanet (WFIRST); it was based largely on the NASA DOE Joint Dark Energy Mission (JDEM) family, in particular JDEM- (Gehrels 2010). WFIRST will operate for five to ten years and will combine the three leading dark energy

California at Berkeley, University of

323

Probing the nature of dark energy through galaxy redshift surveys with radio telescopes  

E-Print Network [OSTI]

Galaxy redshift surveys using optical telescopes have, in combination with other cosmological probes, enabled precision measurements of the nature of dark energy. We show that radio telescopes are rapidly becoming competitive with optical facilities in spectroscopic surveys of large numbers of galaxies. Two breakthroughs are driving this change. Firstly, individual radio telescopes are more efficient at mapping the sky thanks to the large field-of-view of new phased-array feeds. Secondly, ever more dishes can be correlated in a cost-effective manner with rapid increases in computing power. The next decade will see the coming of age of the 21cm radio wavelength as a cosmological probe as first the Pathfinders then, ultimately, the Square Kilometre Array is constructed. The latter will determine precise 3D positions for a billion galaxies, mapping the distribution of matter in the Universe over the last 12 billion years. This radio telescope will be able to constrain the equation of state of dark energy, and it...

Duffy, Alan R

2014-01-01T23:59:59.000Z

324

The Anti-Coincidence Detector for the GLAST Large Area Telescope  

SciTech Connect (OSTI)

This paper describes the design, fabrication and testing of the Anti-Coincidence Detector (ACD) for the Gamma-ray Large Area Space Telescope (GLAST) Large Area Telescope (LAT). The ACD is LAT's first-level defense against the charged cosmic ray background that outnumbers the gamma rays by 3-5 orders of magnitude. The ACD covers the top and 4 sides of the LAT tracking detector, requiring a total active area of {approx}8.3 square meters. The ACD detector utilizes plastic scintillator tiles with wave-length shifting fiber readout. In order to suppress self-veto by shower particles at high gamma-ray energies, the ACD is segmented into 89 tiles of different sizes. The overall ACD efficiency for detection of singly charged relativistic particles entering the tracking detector from the top or sides of the LAT exceeds the required 0.9997.

Moiseev, A.A.; Hartman, R.C.; Ormes, J.F.; Thompson, D.J.; Amato, M.J.; Johnson, T.E.; Segal, K.N.; Sheppard, D.A.

2007-03-23T23:59:59.000Z

325

The Advanced Gamma-ray Imaging System (AGIS) Telescope Optical System Designs  

SciTech Connect (OSTI)

AGIS is a conceptual design for a future ground-based gamma-ray observatory operating in the energy range 25 GeV-100 TeV, which is based on an array of {approx}20-100 imaging atmospheric Cherenkov telescopes (IACTs). The desired improvement in sensitivity, angular resolution, and reliability of operation of AGIS imposes demanding technological and cost requirements on the design of the IACTs. We are considering several options for the optical system (OS) of the AGIS telescopes, which include the traditional Davies-Cotton design as well as novel two-mirror design. Emerging mirror production technologies based on replication processes such as cold and hot glass slumping, cured carbon fiber reinforced plastic (CFRP), and electroforming provide new opportunities for cost-effective solutions for the design of the OS.

Bugaev, V.; Buckley, J.; Krawczynski, H. [Washington University (United States); Diegel, S.; Romani, R. [Stanford University (United States); Falcone, A. [Penn State University (United States); Fegan, S.; Vassiliev, V. [UCLA (United States); Finley, J. [Purdue University (United States); Guarino, V. [ANL (United States); Hanna, D. [McGill University (Canada); Kaaret, P. [University of Iowa (United States); Konopelko, A. [Pittsburg State University (United States); Ramsey, B. [MSFC (United States); Weekes, T. [CfA (United States)

2008-12-24T23:59:59.000Z

326

Synergy between the Large Synoptic Survey Telescope and the Square Kilometre Array  

E-Print Network [OSTI]

We provide an overview of the science benefits of combining information from the Square Kilometre Array (SKA) and the Large Synoptic Survey Telescope (LSST). We first summarise the capabilities and timeline of the LSST and overview its science goals. We then discuss the science questions in common between the two projects, and how they can be best addressed by combining the data from both telescopes. We describe how weak gravitational lensing and galaxy clustering studies with LSST and SKA can provide improved constraints on the causes of the cosmological acceleration. We summarise the benefits to galaxy evolution studies of combining deep optical multi-band imaging with radio observations. Finally, we discuss the excellent match between one of the most unique features of the LSST, its temporal cadence in the optical waveband, and the time resolution of the SKA.

Bacon, David; Abdalla, Filipe B; Brown, Michael; Bull, Philip; Camera, Stefano; Fender, Rob; Grainge, Keith; Ivezic, Zeljko; Jarvis, Matt; Jackson, Neal; Kirk, Donnacha; Mann, Bob; McEwen, Jason; McKean, John; Newman, Jeffrey A; Raccanelli, Alvise; Sahlen, Martin; Santos, Mario; Tyson, Anthony; Zhao, Gong-Bo

2015-01-01T23:59:59.000Z

327

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

328

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

329

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

Science Journals Connector (OSTI)

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

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

2014-01-01T23:59:59.000Z

330

O:\IM-20\E-Government Program Office\FDMS\FDMS database\DOE\2011\DOE-HQ-2011-0014 - Daniel Cohen - GC\Comments from FDMS\Charles W Adams DRAFT-0005.html  

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

%20Daniel%20Cohen%20-%20GC/Comments%20from%20FDMS/Charles%20W%20Adams%20DRAFT-0005.html[3/23/2011 2:17:13 PM] %20Daniel%20Cohen%20-%20GC/Comments%20from%20FDMS/Charles%20W%20Adams%20DRAFT-0005.html[3/23/2011 2:17:13 PM] PUBLIC SUBMISSION As of: March 23, 2011 Received: March 21, 2011 Status: Pending_Post Tracking No. 80c0d05f Comments Due: April 04, 2011 Submission Type: Web Docket: DOE-HQ-2011-0014 Reducing Regulatory Burden Comment On: DOE-HQ-2011-0014-0001 Reducing Regulatory Burden Document: DOE-HQ-2011-0014-DRAFT-0005 Comment on FR Doc # 2011-02368 Submitter Information Name: Charles W Adams Address: A.O. Smith Corporation 11270 W. PARK PLACE MILWAUKEE, WI, 53224 Email: cadams@aosmith.com Phone: 414-359-4274 Organization: A.O. Smith Corporation General Comment I am commenting on behalf of A.O. Smith Water Products Company, the largest manufacturer of residential and commercial water heaters in the USA. We are members of the Air-conditioning,

331

A cryogenic liquid-mirror telescope on the moon to study the early universe  

E-Print Network [OSTI]

We have studied the feasibility and scientific potential of zenith observing liquid mirror telescopes having 20 to 100 m diameters located on the moon. They would carry out deep infrared surveys to study the distant universe and follow up discoveries made with the 6 m James Webb Space Telescope (JWST), with more detailed images and spectroscopic studies. They could detect objects 100 times fainter than JWST, observing the first, high-red shift stars in the early universe and their assembly into galaxies. We explored the scientific opportunities, key technologies and optimum location of such telescopes. We have demonstrated critical technologies. For example, the primary mirror would necessitate a high-reflectivity liquid that does not evaporate in the lunar vacuum and remains liquid at less than 100K: We have made a crucial demonstration by successfully coating an ionic liquid that has negligible vapor pressure. We also successfully experimented with a liquid mirror spinning on a superconducting bearing, as will be needed for the cryogenic, vacuum environment of the telescope. We have investigated issues related to lunar locations, concluding that locations within a few km of a pole are ideal for deep sky cover and long integration times. We have located ridges and crater rims within 0.5 degrees of the North Pole that are illuminated for at least some sun angles during lunar winter, providing power and temperature control. We also have identified potential problems, like lunar dust. Issues raised by our preliminary study demand additional in-depth analyses. These issues must be fully examined as part of a scientific debate we hope to start with the present article.

Roger Angel; Simon P. Worden; Ermanno F. Borra; Daniel J. Eisenstein; Bernard Foing; Paul Hickson; Jean-Luc Josset; Ki Bui Ma; Omar Seddiki; Suresh Sivanandam; Simon Thibault; Paul van Susante

2008-06-13T23:59:59.000Z

332

A logarithmic, large-solid-angle detector telescope for nuclear fragmentation  

SciTech Connect (OSTI)

Properties of a logarithmic, large-solid-angle detector telescope for measuring the spectra of light charged particles and/or complex fragments produced in intermediate-energy nuclear reactions are described. Light-ion identification with a phoswich detector which consists of transmission photodiode {Delta}E and CsI(T{ell}) E elements is also discussed, as is the response of silicon microstrip detectors to fission fragments. 6 figs., 4 figs.

Kwiatkowski, K.; Komisarcik, K.; Wile, J.L.; Yennello, S.J.; Fields, D.E.; Viola, V.E. (Indiana Univ., Bloomington, IN (USA)); Glagola, B.G. (Argonne National Lab., IL (USA))

1990-01-01T23:59:59.000Z

333

From Flapping Birds to Space Telescopes: The Modern Science of Origami (BNL Women in Science Lecture)  

SciTech Connect (OSTI)

During the 1990s, the development and application of mathematical techniques to origami revolutionized this centuries-old Japanese art of paper folding. In his talk, Lang will describe how geometric concepts led to the solution of a broad class of origami-folding problems. Conversely, algorithms and theorems of origami design have shed light on long-standing mathematical questions and have solved practical engineering problems. Lang will discuss how origami has led to huge space telescopes, safer airbags, and more.

Lang, Robert J.

2010-06-24T23:59:59.000Z

334

Prototype Tests for the CELESTE Solar Array $\\gamma$-Ray Telescope  

E-Print Network [OSTI]

The CELESTE experiment will be an Atmospheric Cherenkov detector designed to bridge the gap in energy sensitivity between current satellite and ground-based gamma-ray telescopes, 20 to 300 GeV. We present test results made at the former solar power plant, Themis, in the French Pyrenees. The tests confirm the viability of using a central tower heliostat array for Cherenkov wavefront sampling.

Giebels, B; Bergeret, H; Cordier, A; Debiais, G; De Naurois, Mathieu; Dezalay, J P; Dumora, D; Eschstruth, P T; Espigat, P; Fabre, B; Fleury, P; Ghesquire, C; Herault, N; Malet, I; Merkel, B; Meynadier, C; Palatka, M; Par, E; Procureur, J; Punch, M; Qubert, J; Ragan, K; Rob, L; Schovanek, P; Smith, D A; Vrana, J

1998-01-01T23:59:59.000Z

335

Prototype Tests for the CELESTE Solar Array Gamma--Ray Telescope  

E-Print Network [OSTI]

The CELESTE experiment will be an Atmospheric Cherenkov detector designed to bridge the gap in energy sensitivity between current satellite and ground-based gamma-ray telescopes, 20 to 300 GeV. We present test results made at the former solar power plant, Themis, in the French Pyrenees. The tests confirm the viability of using a central tower heliostat array for Cherenkov wavefront sampling.

B. Giebels; R. Bazer-Bachi; H. Bergeret; A. Cordier; G. Debiais; M. De Naurois; J. P. Dezalay; D. Dumora; P. Eschstruth; P. Espigat; B. Fabre; P. Fleury; C. Ghesquire; N. Herault; I. Malet; B. Merkel; C. Meynadier; M. Palatka; E. Par; J. Procureur; M. Punch; J. Qubert; K. Ragan; L. Rob; P. Schovanek; D. A. Smith; J. Vrana

1998-03-17T23:59:59.000Z

336

Microscopic surface structure of C/SiC composite mirrors for space cryogenic telescopes  

E-Print Network [OSTI]

We report on the microscopic surface structure of carbon-fiber-reinforced silicon carbide (C/SiC) composite mirrors that have been improved for the Space Infrared Telescope for Cosmology and Astrophysics (SPICA) and other cooled telescopes. The C/SiC composite consists of carbon fiber, silicon carbide, and residual silicon. Specific microscopic structures are found on the surface of the bare C/SiC mirrors after polishing. These structures are considered to be caused by the different hardness of those materials. The roughness obtained for the bare mirrors is 20 nm rms for flat surfaces and 100 nm rms for curved surfaces. It was confirmed that a SiSiC slurry coating is effective in reducing the roughness to 2 nm rms. The scattering properties of the mirrors were measured at room temperature and also at 95 K. No significant change was found in the scattering properties through cooling, which suggests that the microscopic surface structure is stable with changes in temperature down to cryogenic values. The C/SiC mirror with the SiSiC slurry coating is a promising candidate for the SPICA telescope.

Keigo Enya; Takao Nakagawa; Hidehiro Kaneda; Takashi Onaka; Tuyoshi Ozaki; Masami Kume

2007-07-10T23:59:59.000Z

337

Validation of the Real and Simulated Data of the Pierre Auger Fluorescence Telescopes  

E-Print Network [OSTI]

The fluorescence detector (FD) of the Pierre Auger Observatory is currently operating 18 fluorescence telescopes of the 24 that will be employed in the completed detector. These telescopes, grouped in 4 eyes each consisting of 6 telescopes, measure the longitudinal profile of cosmic ray showers with a 14% duty cycle. The reconstruction capability and triggering efficiency have been studied using a complete simulation and reconstruction production chain, employing both simulated CORSIKA showers and parameterised Gaisser-Hillas profiles. The propagation through the atmosphere and the detector response are taken into account and simulated in detail. These simulated data have been generated in a preliminary analysis using the method of importance sampling to efficiently cover the energy region of 0.3 - 300 EeV, various shower geometries and impact points and different primary particles. The distributions of observables have then been investigated in both real and simulated data, facilitating the validation of the reconstruction and simulation software. Comparisons of real and simulated data are discussed and used to assess their impact on the data analysis.

The Pierre Auger Collaboration; L. Perrone

2005-07-20T23:59:59.000Z

338

The Automatic Real-Time GRB Pipeline of the 2-m Liverpool Telescope  

E-Print Network [OSTI]

The 2-m Liverpool Telescope (LT), owned by Liverpool John Moores University, is located in La Palma (Canary Islands) and operates in fully robotic mode. In 2005, the LT began conducting an automatic GRB follow-up program. On receiving an automatic GRB alert from a Gamma-Ray Observatory (Swift, INTEGRAL, HETE-II, IPN) the LT initiates a special override mode that conducts follow-up observations within 2-3 min of the GRB onset. This follow-up procedure begins with an initial sequence of short (10-s) exposures acquired through an r' band filter. These images are reduced, analyzed and interpreted automatically using pipeline software developed by our team called "LT-TRAP" (Liverpool Telescope Transient Rapid Analysis Pipeline); the automatic detection and successful identification of an unknown and potentially fading optical transient triggers a subsequent multi-color imaging sequence. In the case of a candidate brighter than r'=15, either a polarimetric (from 2006) or a spectroscopic observation (from 2007) will be triggered on the LT. If no candidate is identified, the telescope continues to obtain z', r' and i' band imaging with increasingly longer exposure times. Here we present a detailed description of the LT-TRAP and briefly discuss the illustrative case of the afterglow of GRB 050502a, whose automatic identification by the LT just 3 min after the GRB, led to the acquisition of the first early-time (< 1 hr) multi-color light curve of a GRB afterglow.

C. Guidorzi; A. Monfardini; A. Gomboc; C. J. Mottram; C. G. Mundell; I. A. Steele; D. Carter; M. F. Bode; R. J. Smith; S. N. Fraser; M. J. Burgdorf; A. M. Newsam

2005-11-01T23:59:59.000Z

339

Compton telescope with coded aperture mask: Imaging with the INTEGRAL/IBIS Compton mode  

E-Print Network [OSTI]

Compton telescopes provide a good sensitivity over a wide field of view in the difficult energy range running from a few hundred keV to several MeV. Their angular resolution is, however, poor and strongly energy dependent. We present a novel experimental design associating a coded mask and a Compton detection unit to overcome these pitfalls. It maintains the Compton performance while improving the angular resolution by at least an order of magnitude in the field of view subtended by the mask. This improvement is obtained only at the expense of the efficiency that is reduced by a factor of two. In addition, the background corrections benefit from the coded mask technique, i.e. a simultaneous measurement of the source and background. This design is implemented and tested using the IBIS telescope on board the INTEGRAL satellite to construct images with a 12' resolution over a 29 degrees x 29 degrees field of view in the energy range from 200 keV to a few MeV. The details of the analysis method and the resulting telescope performance, particularly in terms of sensitivity, are presented.

M. Forot; P. Laurent; F. Lebrun; O. Limousin

2007-08-28T23:59:59.000Z

340

The KM3NeT deep-sea neutrino telescope  

E-Print Network [OSTI]

KM3NeT is a deep-sea research infrastructure being constructed in the Mediterranean Sea. It will host the next generation Cherenkov neutrino telescope and nodes for a deep sea multidisciplinary observatory, providing oceanographers, marine biologists, and geophysicists with real time measurements. The neutrino telescope will complement IceCube in its field of view and exceed it substantially in sensitivity. Its main goal is the detection of high energy neutrinos of astrophysical origin. The detector will have a modular structure with six building blocks, each consisting of about one hundred Detection Units (DUs). Each DU will be equipped with 18 multi-PMT digital optical modules. The first phase of construction has started and shore and deep-sea infrastructures hosting the future KM3NeT detector are being prepared offshore Toulon, France and offshore Capo Passero on Sicily, Italy. The technological solutions for the neutrino detector of KM3NeT and the expected performance of the neutrino telescope are present...

Margiotta, Annarita

2014-01-01T23:59:59.000Z

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341

A decision-making framework to determine the value of on-orbit servicing compared to replacement of space telescopes  

E-Print Network [OSTI]

The Hubble Space Telescope has demonstrated that on-orbit servicing can provide significant benefits for scientific space programs. Specifically, servicing missions can replace failed components to keep spacecraft operational, ...

Baldesarra, Mark

2007-01-01T23:59:59.000Z

342

The major upgrade of the MAGIC telescopes, Part I: The hardware improvements and the commissioning of the system  

E-Print Network [OSTI]

The MAGIC telescopes are two Imaging Atmospheric Cherenkov Telescopes (IACTs) located on the Canary island of La Palma. The telescopes are designed to measure Cherenkov light from air showers initiated by gamma rays in the energy regime from around 50 GeV to more than 50 TeV. The two telescopes were built in 2004 and 2009, respectively, with different cameras, triggers and readout systems. In the years 2011-2012 the MAGIC collaboration undertook a major upgrade to make the stereoscopic system uniform, improving its overall performance and easing its maintenance. In particular, the camera, the receivers and the trigger of the first telescope were replaced and the readout of the two telescopes was upgraded. This paper (Part I) describes the details of the upgrade as well as the basic performance parameters of MAGIC such as raw data treatment, dead time of the system, linearity in the electronic chain and sources of noise. In Part II, we describe the physics performance of the upgraded system.

Aleksic, J; Antonelli, L A; Antoranz, P; Babic, A; Bangale, P; Barcelo, M; Barrio, J A; Gonzalez, J Becerra; Bednarek, W; Bernardini, E; Biasuzzi, B; Biland, A; Bitossi, M; Blanch, O; Bonnefoy, S; Bonnoli, G; Borracci, F; Bretz, T; Carmona, E; Carosi, A; Cecchi, R; Colin, P; Colombo, E; Contreras, J L; Corti, D; Cortina, J; Covino, S; Da Vela, P; Dazzi, F; De Angelis, A; De Caneva, G; De Lotto, B; Wilhelmi, E de Ona; Mendez, C Delgado; Dettlaff, A; Prester, D Dominis; Dorner, D; Doro, M; Einecke, S; Eisenacher, D; Elsaesser, D; Fidalgo, D; Fink, D; Fonseca, M V; Font, L; Frantzen, K; Fruck, C; Galindo, D; Lopez, R J Garcia; Garczarczyk, M; Terrats, D Garrido; Gaug, M; Giavitto, G; Godinovic, N; Munoz, A Gonzalez; Gozzini, S R; Haberer, W; Hadasch, D; Hanabata, Y; Hayashida, M; Herrera, J; Hildebrand, D; Hose, J; Hrupec, D; Idec, W; Illa, J M; Kadenius, V; Kellermann, H; Knoetig, M L; Kodani, K; Konno, Y; Krause, J; Kubo, H; Kushida, J; La Barbera, A; Lelas, D; Lemus, J L; Lewandowska, N; Lindfors, E; Lombardi, S; Longo, F; Lopez, M; Lopez-Coto, R; Lopez-Oramas, A; Lorca, A; Lorenz, E; Lozano, I; Makariev, M; Mallot, K; Maneva, G; Mankuzhiyil, N; Mannheim, K; Maraschi, L; Marcote, B; Mariotti, M; Martinez, M; Mazin, D; Menzel, U; Miranda, J M; Mirzoyan, R; Moralejo, A; Munar-Adrover, P; Nakajima, D; Negrello, M; Neustroev, V; Niedzwiecki, A; Nilsson, K; Nishijima, K; Noda, K; Orito, R; Overkemping, A; Paiano, S; Palatiello, M; Paneque, D; Paoletti, R; Paredes, J M; Paredes-Fortuny, X; Persic, M; Poutanen, J; Moroni, P G Prada; Prandini, E; Puljak, I; Reinthal, R; Rhode, W; Ribo, M; Rico, J; Garcia, J Rodriguez; Rugamer, S; Saito, T; Saito, K; Satalecka, K; Scalzotto, V; Scapin, V; Schultz, C; Schlammer, J; Schmidl, S; Schweizer, T; Sillanpaa, A; Sitarek, J; Snidaric, I; Sobczynska, D; Spanier, F; Stamerra, A; Steinbring, T; Storz, J; Strzys, M; Takalo, L; Takami, H; Tavecchio, F; Tejedor, L A; Temnikov, P; Terzic, T; Tescaro, D; Teshima, M; Thaele, J; Tibolla, O; Torres, D F; Toyama, T; Treves, A; Vogler, P; Wetteskind, H; Will, M; Zanin, R

2014-01-01T23:59:59.000Z

343

Telescope Guiding with a HyViSI H2RG Used in Guide Mode  

SciTech Connect (OSTI)

We report on long exposure results obtained with a Teledyne HyViSI H2RG detector operating in guide mode. The sensor simultaneously obtained nearly seeing-limited data while also guiding the Kitt Peak 2.1 m telescope. Results from unguided and guided operation are presented and used to place lower limits on flux/fluence values for accurate centroid measurements. We also report on significant noise reduction obtained in recent laboratory measurements that should further improve guiding capability with higher magnitude stars.

Simms, Lance M.; /SLAC; Figerb, Donald F.; Hanold, Brandon J.; /Rochester Inst. Tech.; Kahn, Steven M.; Gilmore, D.Kirk; /SLAC

2010-06-04T23:59:59.000Z

344

The Search for Dark Matter with the Fermi Gamma Ray Space Telescope  

SciTech Connect (OSTI)

The Fermi Gamma-Ray Space Telescope has been scanning the gamma ray sky since it was launched by NASA in June 2008 and has a mission lifetime goal of 10 years. Largely due to our particle physics heritage, one of the main physics topics being studied by the Fermi LAT Collaboration is the search for dark matter via indirect detection. My talk will review the progress of these studies, something on how the LAT detector enables them, and expectations for the future. I will discuss both gamma-ray and (electron + positron) searches for dark matter, and some resulting theoretical implications.

Bloom, Elliott (SLAC) [SLAC

2011-03-30T23:59:59.000Z

345

The GAMMA-400 gamma-ray telescope characteristics. Angular resolution and electrons/protons separation  

E-Print Network [OSTI]

The measurements of gamma-ray fluxes and cosmic-ray electrons and positrons in the energy range from 100 MeV to several TeV, which will be implemented by the specially designed GAMMA-400 gamma-ray telescope, concern with the following broad range of science topics. Searching for signatures of dark matter, surveying the celestial sphere in order to study gamma-ray point and extended sources, measuring the energy spectra of Galactic and extragalactic diffuse gamma-ray emission, studying gamma-ray bursts and gamma-ray emission from the Sun, as well as high precision measuring spectra of high-energy electrons and positrons, protons and nuclei up to the knee. To clarify these scientific problems with the new experimental data the GAMMA-400 gamma-ray telescope possesses unique physical characteristics comparing with previous and present experiments. For gamma-ray energies more than 100 GeV GAMMA-400 provides the energy resolution of ~1% and angular resolution better than 0.02 deg. The methods developed to reconstru...

Leonov, A A; Bonvicini, V; Topchiev, N P; Adriani, O; Aptekar, R L; Arkhangelskaja, I V; Arkhangelskiy, A I; Bergstrom, L; Berti, E; Bigongiari, G; Bobkov, S G; Boezio, M; Bogomolov, E A; Bonechi, S; Bongi, M; Bottai, S; Boyarchuk, K A; Castellini, G; Cattaneo, P W; Cumani, P; Dedenko, G L; De Donato, C; Dogiel, V A; Gorbunov, M S; Gusakov, Yu V; Hnatyk, B I; Kadilin, V V; Kaplin, V A; Kaplun, A A; Kheymits, M D; Korepanov, V E; Larsson, J; Loginov, V A; Longo, F; Maestro, P; Marrocchesi, P S; Mikhailov, V V; Mocchiutti, E; Moiseev, A A; Mori, N; Moskalenko, I V; Naumov, P Yu; Papini, P; Pearce, M; Picozza, P; Popov, A V; Rappoldi, A; Ricciarini, S; Runtso, M F; Ryde, F; Serdin, O V; Sparvoli, R; Spillantini, P; Suchkov, S I; Tavani, M; Taraskin, A A; Tiberio, A; Tyurin, E M; Ulanov, M V; Vacchi, A; Vannuccini, E; Vasilyev, G I; Yurkin, Yu T; Zampa, N; Zirakashvili, V N; Zverev, V G

2014-01-01T23:59:59.000Z

346

Pulsed Gamma-rays from PSR J2021+3651 with the Fermi Large Area Telescope  

E-Print Network [OSTI]

We report the detection of pulsed gamma-rays from the young, spin-powered radio pulsar PSR J2021+3651 using data acquired with the Large Area Telescope (LAT) on the Fermi Gamma-ray Space Telescope (formerly GLAST). The light curve consists of two narrow peaks of similar amplitude separated by 0.468 +/- 0.002 in phase. The first peak lags the maximum of the 2 GHz radio pulse by 0.162 +/- 0.004 +/- 0.01 in phase. The integral gamma-ray photon flux above 100 MeV is (56 +/- 3 +/- 11) x 10^{-8} /cm2/s. The photon spectrum is well-described by an exponentially cut-off power law of the form dF/dE = kE^{-\\Gamma} e^(-E/E_c) where the energy E is expressed in GeV. The photon index is \\Gamma = 1.5 +/- 0.1 +/- 0.1 and the exponential cut-off is E_c = 2.4 +/- 0.3 +/- 0.5 GeV. The first uncertainty is statistical and the second is systematic. The integral photon flux of the bridge is approximately 10% of the pulsed emission, and the upper limit on off-pulse gamma-ray emission from a putative pulsar wind nebula is <10% o...

Abdo, A A

2009-01-01T23:59:59.000Z

347

Experimental results obtained with the positron-annihilation-radiation telescope of the Toulouse-Argonne collaboration  

Science Journals Connector (OSTI)

We present laboratory measurements obtained with a ground-based prototype of the focusing positron-annihilation-radiation telescope developed by the Toulouse-Argonne collaboration. This instrument has been designed to collect 511-keV photons from astrophysical sources when operating as a balloon borne observatory. The ground-based prototype consists of a crystal lens holding small cubes of diffracting germanium crystals and a 33 germanium array that detects the concentrated beam in the focal plane. Measured performances of the instrument at different line energies (511 and 662 keV) are presented and compared with Monte Carlo simulations; also the advantages of combining the lens with a detector array are discussed. The results obtained in the laboratory have strengthened interest in a crystal-diffraction telescope: the balloon instrument will provide a combination of high spatial and energy resolution (15 arc sec and 2 keV, respectively) with an extremely low instrumental background resulting in a sensitivity of ?3 10?5 photons cm?2s?1. These features will allow us to resolve a possible narrow 511-keV line both energetically and spatially within a Galactic center microquasar or in other broad-class annihilators.

J.E. Naya; P. von Ballmoos; R.K. Smither; M. Faiz; P.B. Fernandez; T. Graber; F. Albernhe; G. Vedrenne

1996-01-01T23:59:59.000Z

348

Fermi Large Area Telescope Observations of the Cygnus Loop Supernova Remnant  

SciTech Connect (OSTI)

We present an analysis of the gamma-ray measurements by the Large Area Telescope (LAT) onboard the Fermi Gamma-ray Space Telescope in the region of the supernova remnant (SNR) Cygnus Loop (G74.0-8.5). We detect significant gamma-ray emission associated with the SNR in the energy band 0.2-100 GeV. The gamma-ray spectrum shows a break in the range 2-3 GeV. The gamma-ray luminosity is {approx} 1 x 10{sup 33} erg s{sup -1} between 1-100 GeV, much lower than those of other GeV-emitting SNRs. The morphology is best represented by a ring shape, with inner/outer radii 0{sup o}.7 {+-} 0{sup o}.1 and 1{sup o}.6 {+-} 0{sup o}.1. Given the association among X-ray rims, H{alpha} filaments and gamma-ray emission, we argue that gamma rays originate in interactions between particles accelerated in the SNR and interstellar gas or radiation fields adjacent to the shock regions. The decay of neutral pions produced in nucleon-nucleon interactions between accelerated hadrons and interstellar gas provides a reasonable explanation for the gamma-ray spectrum.

Katagiri, H.; /Ibaraki U., Mito; Tibaldo, L.; /INFN, Padua /Padua U. /Paris U., VI-VII; Ballet, J.; /Paris U., VI-VII; Giordano, F.; /Bari U. /Bari Polytechnic /INFN, Bari; Grenier, I.A.; /Paris U., VI-VII; Porter, T.A.; /Stanford U., HEPL /KIPAC, Menlo Park /SLAC; Roth, M.; /Washington U., Seattle; Tibolla, O.; /Wurzburg U.; Uchiyama, Y.; /Stanford U., HEPL /KIPAC, Menlo Park /SLAC; Yamazaki, R.; /Sagamihara, Aoyama Gakuin U.

2011-11-08T23:59:59.000Z

349

Atmospheric MUons from PArametric formulas: a fast GEnerator for neutrino telescopes (MUPAGE)  

E-Print Network [OSTI]

Neutrino telescopes will open, in the next years, new opportunities in observational high energy astrophysics. For these experiments, atmospheric muons from primary cosmic ray interactions in the atmosphere play an important role, because they provide the most abundant source of events for calibration and test. On the other side, they represent the major background source. In this paper a fast Monte Carlo generator (called MUPAGE) of bundles of atmospheric muons for underwater/ice neutrino telescopes is presented. MUPAGE is based on parametric formulas [APP25(2006)1] obtained from a full Monte Carlo simulation of cosmic ray showers generating muons in bundle, which are propagated down to 5 km w.e. It produces the event kinematics on the surface of a user-defined virtual cylinder, surrounding the detector. The multiplicity of the muons in the bundle, the muon spatial distribution and energy spectrum are simulated according to a specific model of primary cosmic ray flux, with constraints from measurements of the muon flux with underground experiments. As an example of the application, the result of the generation of events on a cylindrical surface of 3 km^2 at a depth of 2450 m of water is presented.

G. Carminati; A. Margiotta; M. Spurio

2008-02-05T23:59:59.000Z

350

Hubble Space Telescope Imaging of the Optical Transient Associated with GRB970508  

E-Print Network [OSTI]

We report on Hubble Space Telescope (HST) observations of the optical transient (OT) discovered in the error box of the gamma-ray burst GRB970508. The object was imaged on 1997 June 2 with the Space Telescope Imaging Spectrograph (STIS) and Near-Infrared Camera and Multi-Object Spectrometer (NICMOS). The observations reveal a point-like source with R = 23.1 +- 0.2 and H = 20.6 +- 0.3, in agreement with the power-law temporal decay seen in ground-based monitoring. Unlike the case of GRB970228, no nebulosity is detected surrounding the OT of GRB970508. We set very conservative upper limits of R ~ 24.5 and H ~ 22.2 on the brightness of any underlying extended source. If this subtends a substantial fraction of an arcsecond, then the R band limit is ~25.5. In combination with Keck spectra that show Mg I absorption and [O II] emission at a redshift of z = 0.835, our observations suggest that the OT is located in a star-forming galaxy with total luminosity one order of magnitude lower than the knee of the galaxy luminosity function, L*. Such galaxies are now thought to harbor the majority of star formation at z ~ 1; therefore, these observations may provide support for a link between GRBs and star formation.

Elena Pian; Andrew S. Fruchter; Louis E. Bergeron; Steve E. Thorsett; Filippo Frontera; Marco Tavani; Enrico Costa; Marco Feroci; Jules Halpern; Ray A. Lucas; Luciano Nicastro; Eliana Palazzi; Luigi Piro; William Sparks; Alberto J. Castro-Tirado; Ted Gull; Kevin Hurley; Holger Pedersen

1997-10-29T23:59:59.000Z

351

Developing Engineering Model Cobra fiber positioners for the Subaru Telescope Prime Focus Spectrometer  

E-Print Network [OSTI]

The Cobra fiber positioner is being developed by the California Institute of Technology (CIT) and the Jet Propulsion Laboratory (JPL) for the Prime Focus Spectrograph (PFS) instrument that will be installed at the Subaru Telescope on Mauna Kea, Hawaii. PFS is a fiber fed multi-object spectrometer that uses an array of Cobra fiber positioners to rapidly reconfigure 2394 optical fibers at the prime focus of the Subaru Telescope that are capable of positioning a fiber to within 5um of a specified target location. A single Cobra fiber positioner measures 7.7mm in diameter and is 115mm tall. The Cobra fiber positioner uses two piezo-electric rotary motors to move a fiber optic anywhere in a 9.5mm diameter patrol area. In preparation for full-scale production of 2550 Cobra positioners an Engineering Model (EM) version was developed, built and tested to validate the design, reduce manufacturing costs, and improve system reliability. The EM leveraged the previously developed prototype versions of the Cobra fiber posi...

Fisher, Charles; Braun, David; Seiffert, Michael; Aghazarian, Hrand; Partos, Eamon; King, Matthew; Hovland, Larry; Schwochert, Mark; Kaluzny, Joel; Capocasale, Christopher; Houck, Andrew; Gross, Johannes; Reiley, Dan; Mao, Peter; Riddle, Reed; Bui, Khanh; Henderson, David; Haran, Todd; Culhane, Rob; Piazza, Daniele; Walkama, Eric

2014-01-01T23:59:59.000Z

352

First Lunar Occultation Results from the 2.4 m Thai National Telescope equipped with ULTRASPEC  

E-Print Network [OSTI]

The recently inaugurated 2.4\\,m Thai National Telescope (TNT) is equipped, among other instruments, with the ULTRASPEC low-noise, frame-transfer EMCCD camera. At the end of its first official observing season, we report on the use of this facility to record high time resolution imaging using small detector subarrays with sampling as fast as several $10^2$\\,Hz. In particular, we have recorded lunar occultations of several stars which represent the first contribution to this area of research made from South-East Asia with a telescope of this class. Among the results, we discuss an accurate measurement of $\\alpha $~Cnc, which has been reported previously as a suspected close binary. Attempts to resolve this star by several authors have so far met with a lack of unambiguous confirmation. With our observation we are able to place stringent limits on the projected angular separation ($ 5$) of a putative companion. We also present a measurement of the binary {HR~7072}, which extends considerably the time coverage av...

Richichi, A; Soonthornthum, B; Dhillon, V S; Marsh, T R

2014-01-01T23:59:59.000Z

353

Status of the Silicon Photomultiplier Telescope FAMOUS for the Fluorescence Detection of UHECRs  

E-Print Network [OSTI]

An established technique for the measurement of ultra-high-energy-cosmic-rays is the detection of the fluorescence light induced in the atmosphere of the Earth, by means of telescopes equipped with photomultiplier tubes. Silicon photomultipliers (SiPMs) promise an increase in the photon detection efficiency which outperforms conventional photomultiplier tubes. In combination with their compact package, a moderate bias voltage of several ten volt and single photon resolution, the use of SiPMs can improve the energy and spatial resolution of air fluorescence measurements, and lead to a gain in information on the primary particle. Though, drawbacks like a high dark-noise-rate and a strong temperature dependency have to be managed. FAMOUS is a refracting telescope prototype instrumented with 64 SiPMs of which the main optical element is a Fresnel lens of 549.7 mm diameter and 502.1 mm focal length. The sensitive area of the SiPMs is increased by a special light collection system consisting of Winston cones. The t...

Niggemann, Tim; Brogueira, Pedro; Bueno, Antonio; Eichler, Hans Michael; Ferreira, Miguel; Hebbeker, Thomas; Lauscher, Markus; Mendes, Lus; Middendorf, Lukas; Navas, Sergio; Peters, Christine; Pimenta, Mrio; Ruiz, Angel; Schumacher, Johannes; Stephan, Maurice

2015-01-01T23:59:59.000Z

354

Science Programs for a 2 m-class Telescope at Dome C, Antarctica: PILOT, the Pathfinder for an International Large Optical Telescope  

E-Print Network [OSTI]

The cold, dry and stable air above the summits of the Antarctic plateau provides the best ground-based observing conditions from optical to sub-mm wavelengths to be found on the Earth. PILOT is a proposed 2 m telescope, to be built at Dome C in Antarctica, able to exploit these conditions for conducting astronomy at optical and infrared wavelengths. While PILOT is intended as a pathfinder towards the construction of future grand-design facilities, it will also be able to undertake a range of fundamental science investigations in its own right. This paper provides the performance specifications for PILOT, including its instrumentation. It then describes the kinds of science projects that it could best conduct. These range from planetary science to the search for other solar systems, from star formation within the Galaxy to the star formation history of the Universe, and from gravitational lensing caused by exo-planets to that produced by the cosmic web of dark matter. PILOT would be particularly powerful for wide-field imaging at infrared wavelengths, achieving near-diffraction limited performance with simple tip-tilt wavefront correction. PILOT would also be capable of near-diffraction limited performance in the optical wavebands, as well be able to open new wavebands for regular ground based observation; in the mid-IR from 17 to 40 microns and in the sub-mm at 200 microns.

M. G. Burton; J. Lawrence; M. C. B. Ashley; J. A. Bailey; C. Blake; T. R. Bedding; J. Bland-Hawthorn; I. A. Bond; K. Glazebrook; M. G. Hidas; G. Lewis; S. N. Longmore; S. T. Maddison; S. Mattila; V. Minier; S. D. Ryder; R. Sharp; C. H. Smith; J. W. V. Storey; C. G. Tinney; P. Tuthill; A. J. Walsh; W. Walsh; M. Whiting; T. Wong; D. Woods; P. C. M. Yock

2005-04-29T23:59:59.000Z

355

Forbush decreases and solar events seen in the 10 - 20GeV energy range by the Karlsruhe Muon Telescope  

E-Print Network [OSTI]

Since 1993, a muon telescope located at Forschungszentrum Karlsruhe (Karlsruhe Muon Telescope) has been recording the flux of single muons mostly originating from primary cosmic-ray protons with dominant energies in the 10 - 20 GeV range. The data are used to investigate the influence of solar effects on the flux of cosmic-rays measured at Earth. Non-periodic events like Forbush decreases and ground level enhancements are detected in the registered muon flux. A selection of recent events will be presented and compared to data from the Jungfraujoch neutron monitor. The data of the Karlsruhe Muon Telescope help to extend the knowledge about Forbush decreases and ground level enhancements to energies beyond the neutron monitor regime.

I. Braun; J. Engler; J. R. Hrandel; J. Milke

2008-10-27T23:59:59.000Z

356

Atmospheric \\{MUons\\} from \\{PArametric\\} formulas: a fast \\{GEnerator\\} for neutrino telescopes (MUPAGE)  

Science Journals Connector (OSTI)

Neutrino telescopes will open, in the next years, new opportunities in observational high energy astrophysics. In these detectors, atmospheric muons from primary cosmic ray interactions in the atmosphere play an important role, because they provide the most abundant source of events for calibration and test. On the other side, they represent the major background source. In this paper a fast Monte Carlo generator (called MUPAGE) of bundles of atmospheric muons for underwater/ice neutrino telescopes is presented. MUPAGE is based on parametric formulas [Y. Becherini, A. Margiotta, M. Sioli, M. Spurio, Astrop. Phys. 25 (2006) 1] obtained from a full Monte Carlo simulation of cosmic ray showers generating muons in bundle, which are propagated down to 5 km w.e. It produces the event kinematics on the surface of a user-defined cylinder, surrounding the virtual detector. The multiplicity of the muons in the bundle, the muon lateral distribution and energy spectrum are simulated according to a specific model of primary cosmic ray flux, with constraints from measurements of the muon flux with underground experiments. As an example of application, the result of the generation of events on a cylindrical surface of ?1.4 km2 at a depth of 2450 m of water is presented. Program summary Program title: MUPAGE Catalogue identifier: AEBT_v1_0 Program summary URL: http://cpc.cs.qub.ac.uk/summaries/AEBT_v1_0.html Program obtainable from: CPC Program Library, Queen's University, Belfast, N. Ireland Licensing provisions: Standard CPC licence, http://cpc.cs.qub.ac.uk/licence/licence.html No. of lines in distributed program, including test data, etc.: 3534 No. of bytes in distributed program, including test data, etc.: 61?383 Distribution format: tar.gz Programming language: C++ Computer: Pentium M, 2.0 GHz; 2x Intel Xeon Quad Core, 2.33 \\{GHz\\} Operating system: Scientific Linux 3.x; Scientific Linux 4.x; Slackware 12.0.0 RAM: 50 MB Word size: 32 bits Classification: 1.1, 11.3 External routines: The ROOT system (http://root.cern.ch) Nature of problem: Fast simulation of atmospheric muon bundles for underwater/ice neutrino telescopes. Solution method: Atmospheric muon events are generated according to parametric formulas [1] giving the flux, the multiplicity, the radial distribution and the energy spectrum. Restrictions: Water vertical depth range from 1.5 to 5 km w.e.; zenith angle range from 0 to 85 degrees. Additional comments: The program requires the ROOT libraries for the pseudorandom number generator. References: [1] Y. Becherini, A. Margiotta, M. Sioli, M. Spurio, Astrop. Phys. 25 (2006) 113.

G. Carminati; M. Bazzotti; A. Margiotta; M. Spurio

2008-01-01T23:59:59.000Z

357

CHARACTERIZING THE ATMOSPHERES OF TRANSITING PLANETS WITH A DEDICATED SPACE TELESCOPE  

SciTech Connect (OSTI)

Exoplanetary science is one of the fastest evolving fields of today's astronomical research, continuously yielding unexpected and surprising results. Ground-based planet-hunting surveys, together with dedicated space missions such as Kepler and CoRoT, are delivering an ever-increasing number of exoplanets, over 690, and ESA's Gaia mission will escalate the exoplanetary census into the several thousands. The next logical step is the characterization of these new worlds. What is their nature? Why are they as they are? Use of the Hubble Space Telescope and Spitzer Space Telescope to probe the atmospheres of transiting hot, gaseous exoplanets has opened perspectives unimaginable even just 10 years ago, demonstrating that it is indeed possible with current technology to address the ambitious goal of characterizing the atmospheres of these alien worlds. However, these successful measurements have also shown the difficulty of understanding the physics and chemistry of these exotic environments when having to rely on a limited number of observations performed on a handful of objects. To progress substantially in this field, a dedicated facility for exoplanet characterization, able to observe a statistically significant number of planets over time and a broad spectral range will be essential. Additionally, the instrument design (e.g., detector performances, photometric stability) will be tailored to optimize the extraction of the astrophysical signal. In this paper, we analyze the performance and tradeoffs of a 1.2/1.4 m space telescope for exoplanet transit spectroscopy from the visible to the mid-IR. We present the signal-to-noise ratio as a function of integration time and stellar magnitude/spectral type for the acquisition of spectra of planetary atmospheres for a variety of scenarios: hot, warm, and temperate planets orbiting stars ranging in spectral type from hot F- to cooler M-dwarfs. Our results include key examples of known planets (e.g., HD 189733b, GJ 436b, GJ 1214b, and Cancri 55 e) and simulations of plausible terrestrial and gaseous planets, with a variety of thermodynamical conditions. We conclude that even most challenging targets, such as super-Earths in the habitable zone of late-type stars, are within reach of an M-class, space-based spectroscopy mission.

Tessenyi, M.; Tinetti, G.; Swinyard, B.; Aylward, A.; Tennyson, J. [Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT (United Kingdom); Ollivier, M. [Institut d'Astrophysique Spatiale, Universite de Paris-Sud and CNRS (UMR 8617), IAS UMR8617, Orsay F-91405 (France); Beaulieu, J. P. [Institut d'Astrophysique de Paris, CNRS, UMR7095, Universite Paris VI, 98bis Boulevard Arago, Paris (France); Coude du Foresto, V.; Encrenaz, T. [Observatoire de Paris, LESIA, Meudon (France); Micela, G. [INAF-Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo (Italy); Ribas, I. [Institut de Ciencies de l'Espai (CSIC-IEEC), Campus UAB, 08193 Bellaterra (Spain); Swain, M. R.; Vasisht, G.; Deroo, P. [Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109-8099 (United States); Sozzetti, A. [INAF-Osservatorio Astronomico di Torino, Strada Osservatorio 20, 10025 Pino Torinese (Italy)

2012-02-10T23:59:59.000Z

358

Air Fluorescence Calorimetry with the High Resolution Fly's Eye and Telescope Array Experiments  

SciTech Connect (OSTI)

The air fluorescence technique was first successfully deployed on the Fly's Eye Experiment (1981-1993) by the University of Utah. Its successor, the High Resolution Fly's Eye (HiRes) experiment has further exploited this technique, first in hybrid mode with the MIA muon array (1993-1996), and then in monocular and stereoscopic modes (1997-2006). Results from HiRes will be presented, including evidence for the Greisen-Zatsepin-K'uzmin (GZK) Effect predicted 40 years ago. Most recently, members of the HiRes are collaborating with groups from Japan, led by University of Tokyo, to construct and operate the Telescope Array (TA) experiment, which will deploy a large scintillation-based ground array in combination with fluorescence detectors. Funding for TA in the US has already been approved by NSF. TA will begin operation in 2007.

Jui, Charles C. H. [Department of Physics, University of Utah Salt Lake City, Utah (United States)

2006-10-27T23:59:59.000Z

359

High-precision photometry by telescope defocussing. VI. WASP-24, WASP-25 and WASP-26  

E-Print Network [OSTI]

We present time-series photometric observations of thirteen transits in the planetary systems WASP-24, WASP-25 and WASP-26. All three systems have orbital obliquity measurements, WASP-24 and WASP-26 have been observed with Spitzer, and WASP-25 was previously comparatively neglected. Our light curves were obtained using the telescope-defocussing method and have scatters of 0.5 to 1.2 mmag relative to their best-fitting geometric models. We used these data to measure the physical properties and orbital ephemerides of the systems to high precision, finding that our improved measurements are in good agreement with previous studies. High-resolution Lucky Imaging observations of all three targets show no evidence for faint stars close enough to contaminate our photometry. We confirm the eclipsing nature of the star closest to WASP-24 and present the detection of a detached eclipsing binary within 4.25 arcmin of WASP-26.

Southworth, John; Burgdorf, M; Novati, S Calchi; Dominik, M; Galianni, P; Gerner, T; Giannini, E; Gu, S -H; Hundertmark, M; Jorgensen, U G; Juncher, D; Kerins, E; Mancini, L; Rabus, M; Ricci, D; Schaefer, S; Skottfelt, J; Tregloan-Reed, J; Wang, X -B; Wertz, O; Alsubai, K A; Andersen, J M; Bozza, V; Bramich, D M; Browne, P; Ciceri, S; D'Ago, G; Damerdji, Y; Diehl, C; Dodds, P; Elyiv, A; Fang, X -S; Finet, F; Jaimes, R Figuera; Hardis, S; Harpsoe, K; Jessen-Hansen, J; Kains, N; Kjeldsen, H; Korhonen, H; Liebig, C; Lund, M N; Lundkvist, M; Mathiasen, M; Penny, M T; Popovas, A; Proft, S; Rahvar, S; Sahu, K; Scarpetta, G; Schmidt, R W; Schoenebeck, F; Snodgrass, C; Street, R A; Surdej, J; Tsapras, Y; Vilela, C

2014-01-01T23:59:59.000Z

360

Whole Earth Telescope observations of BPM 37093: a seismological test of crystallization theory in white dwarfs  

E-Print Network [OSTI]

BPM 37093 is the only hydrogen-atmosphere white dwarf currently known which has sufficient mass (~ 1.1 M_sun) to theoretically crystallize while still inside the ZZ Ceti instability strip (T_eff ~ 12,000 K). As a consequence, this star represents our first opportunity to test crystallization theory directly. If the core is substantially crystallized, then the inner boundary for each pulsation mode will be located at the top of the solid core rather than at the center of the star, affecting mainly the average period spacing. This is distinct from the "mode trapping" caused by the stratified surface layers, which modifies the pulsation periods more selectively. In this paper we report on Whole Earth Telescope observations of BPM 37093 obtained in 1998 and 1999. Based on a simple analysis of the average period spacing we conclude that a large fraction of the total stellar mass is likely to be crystallized.

A. Kanaan; A. Nitta; D. E. Winget; S. O. Kepler; M. H. Montgomery; T. S. Metcalfe

2004-11-08T23:59:59.000Z

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361

Opto-thermal analysis of a lightweighted mirror for solar telescope  

E-Print Network [OSTI]

In this paper, an opto-thermal analysis of a moderately heated lightweighted solar telescope mirror is carried out using 3D finite element analysis (FEA). A physically realistic heat transfer model is developed to account for the radiative heating and energy exchange of the mirror with surroundings. The numerical simulations show the non-uniform temperature distribution and associated thermo-elastic distortions of the mirror blank clearly mimicking the underlying discrete geometry of the lightweighted substrate. The computed mechanical deformation data is analyzed with surface polynomials and the optical quality of the mirror is evaluated with the help of a ray-tracing software. The thermal print-through distortions are further shown to contribute to optical figure changes and mid-spatial frequency errors of the mirror surface. A comparative study presented for three commonly used substrate materials, namely, Zerodur, Pyrex and Silicon Carbide (SiC) is relevant to vast area of large optics requirements in gro...

Banyal, Ravinder K; Chatterjee, S

2013-01-01T23:59:59.000Z

362

Design and construction of a carbon fiber gondola for the SPIDER balloon-borne telescope  

E-Print Network [OSTI]

We introduce the light-weight carbon fiber and aluminum gondola designed for the SPIDER balloon-borne telescope. SPIDER is designed to measure the polarization of the Cosmic Microwave Background radiation with unprecedented sensitivity and control of systematics in search of the imprint of inflation: a period of exponential expansion in the early Universe. The requirements of this balloon-borne instrument put tight constrains on the mass budget of the payload. The SPIDER gondola is designed to house the experiment and guarantee its operational and structural integrity during its balloon-borne flight, while using less than 10% of the total mass of the payload. We present a construction method for the gondola based on carbon fiber reinforced polymer tubes with aluminum inserts and aluminum multi-tube joints. We describe the validation of the model through Finite Element Analysis and mechanical tests.

Soler, J D; Amiri, M; Benton, S J; Bock, J J; Bond, J R; Bryan, S A; Chiang, C; Contaldi, C C; Crill, B P; Dor, O P; Farhang, M; Filippini, J P; Fissel, L M; Fraisse, A A; Gambrel, A E; Gandilo, N N; Golwala, S; Gudmundsson, J E; Halpern, M; Hasselfield, M; Hilton, G C; Holmes, W A; Hristov, V V; Irwin, K D; Jones, W C; Kermish, Z D; Kuo, C L; MacTavish, C J; Mason, P V; Megerian, K G; Moncelsi, L; Nagy, J M; Netterfield, C B; O'Brient, R; Rahlin, A S; Reintsema, C D; Ruhl, J E; Runyan, M C; Shariff, J A; Trangsrud, A; Tucker, C; Tucker, R S; Turner, A D; Weber, A C; Wiebe, D V; Young, E Y

2014-01-01T23:59:59.000Z

363

BOOMERanG: a scanning telescope for 10 arcminutes resolution CMB maps  

Science Journals Connector (OSTI)

The BOOMERanG experiment is a stratospheric balloon telescope intended to measure the Cosmic Microwave Background anisotropy at angular scales between a few degrees and ten arcminutes. The experiment features a wide focal plane with 16 detectors in the frequency bands centered at 90 150 220 400 GHz with FWHM ranging between 18 and 10 arcmin. It will be flown on a long duration (714 days) flight circumnavigating Antarctica at the end of 1998. The instrument was flown with a reduced focal plane (6 detectors 90 and 150 GHz bands 25 to 15 arcmin FWHM) on a qualification flight from Texas in August 1997. A wide (?300 deg2 i.e. about 5000 independent beams at 150 GHz) sky area was mapped in the constellations of Capricornus Aquarius Cetus with very low foreground contamination. The instrument was calibrated using the CMB dipole and observations of Jupiter. The LDB version of the instrument has been qualified and shipped to Antarctica.

S. Masi; P. A. R. Ade; R. Artusa; J. J. Bock; A. Boscaleri; B. P. Crill; P. de Bernardis; G. De Troia; P. C. Farese; M. Giacometti; V. V. Hristov; A. Iacoangeli; A. E. Lange; A. T. Lee; L. Martinis; P. V. Mason; P. D. Mauskopf; F. Melchiorri; L. Miglio; T. Montroy; C. B. Netterfield; E. Pascale; F. Piacentini; P. L. Richards; G. Romeo; J. E. Ruhl; F. Scaramuzzi

1999-01-01T23:59:59.000Z

364

BOOMERanG: a scanning telescope for 10 arcminutes resolution CMB maps  

E-Print Network [OSTI]

The BOOMERanG experiment is a stratospheric balloon telescope intended to measure the Cosmic Microwave Background anisotropy at angular scales between a few degrees and ten arcminutes. The experiment features a wide focal plane with 16 detectors in the frequency bands centered at 90, 150, 220, 400 GHz, with FWHM ranging between 18 and 10 arcmin. It will be flown on a long duration (7-14 days) flight circumnavigating Antarctica at the end of 1998. The instrument was flown with a reduced focal plane (6 detectors, 90 and 150 GHz bands, 25 to 15 arcmin FWHM) on a qualification flight from Texas, in August 1997. A wide (~300 sq. deg, i.e. about 5000 independent beams at 150 GHz) sky area was mapped in the constellations of Capricornus, Aquarius, Cetus, with very low foreground contamination. The instrument was calibrated using the CMB dipole and observations of Jupiter. The LDB version of the instrument has been qualified and shipped to Antarctica.

S. Masi; P. A. R. Ade; R. Artusa; J. J. Bock; A. Boscaleri; B. P. Crill; P. de Bernardis; G. De Troia; P. C. Farese; M. Giacometti; V. V. Hristov; A. Iacoangeli; A. E. Lange; A. T. Lee; L. Martinis; P. V. Mason; P. D. Mauskopf; F. Melchiorri; L. Miglio; T. Montroy; C. B. Netterfield; E. Pascale; F. Piacentini; P. L. Richards; G. Romeo; J. E. Ruhl; F. Scaramuzzi

1999-11-30T23:59:59.000Z

365

TenTen: A New Array of Multi-TeV Imaging Cherenkov Telescopes  

E-Print Network [OSTI]

The exciting results from H.E.S.S. point to a new population of gamma-ray sources at energies E > 10 TeV, paving the way for future studies and new discoveries in the multi-TeV energy range. Connected with these energies is the search for sources of PeV cosmic-rays (CRs) and the study of multi-TeV gamma-ray production in a growing number of astrophysical environments. TenTen is a proposed stereoscopic array (with a suggested site in Australia) of modest-sized (10 to 30m^2) Cherenkov imaging telescopes with a wide field of view (8 to 10deg diameter) optimised for the E~10 to 100 TeV range. TenTen will achieve an effective area of ~10 km^2 at energies above 10 TeV. We outline here the motivation for TenTen and summarise key performance parameters.

Rowell, G; Clay, R; Dawson, B; Denman, J; Protheroe, R; Smith, A G K; Thornton, G; Wild, N

2007-01-01T23:59:59.000Z

366

TenTen: A New Array of Multi-TeV Imaging Cherenkov Telescopes  

E-Print Network [OSTI]

The exciting results from H.E.S.S. point to a new population of gamma-ray sources at energies E > 10 TeV, paving the way for future studies and new discoveries in the multi-TeV energy range. Connected with these energies is the search for sources of PeV cosmic-rays (CRs) and the study of multi-TeV gamma-ray production in a growing number of astrophysical environments. TenTen is a proposed stereoscopic array (with a suggested site in Australia) of modest-sized (10 to 30m^2) Cherenkov imaging telescopes with a wide field of view (8 to 10deg diameter) optimised for the E~10 to 100 TeV range. TenTen will achieve an effective area of ~10 km^2 at energies above 10 TeV. We outline here the motivation for TenTen and summarise key performance parameters.

G. Rowell; V. Stamatescu; R. Clay; B. Dawson; J. Denman; R. Protheroe; A. G. K. Smith; G. Thornton; N. Wild

2007-10-10T23:59:59.000Z

367

Observations of Active Galactic Nuclei with Ground-Based Cherenkov Telescopes  

E-Print Network [OSTI]

Imaging Atmospheric Cherenkov Telescopes (IACTs) allow us to observe Active Galactic Nuclei (AGNs) in the 100 GeV to 20 TeV energy range with high sensitivity. The TeV gamma-ray observations of the nine blazars detected so far in this energy range reveal rapid flux and spectral variability on time scales of several hours, sometimes even on time scales of a few minutes. While simple synchrotron-Compton models can explain the observed non-thermal emission, alternative models which involve high-energy protons are not yet ruled out. After reviewing the status of the major IACT experiments, we describe some recent observational results and their astrophysical implications. We conclude with a discussion of possible avenues for future research.

Henric Krawczynski

2005-08-29T23:59:59.000Z

368

Gamma-ray observations of the Crab Region using a coded-aperture telescope  

SciTech Connect (OSTI)

The region of the Galactic anticenter, including the Crab Nebula, was observed during a balloon flight of the University of New Hampshire Directional Gamma-Ray Telescope employing the coded-aperture imaging technique to image celestial gamma-radiation between 160 keV and 9.3 MeV. The background systematics are treated with a simple and relatively straightforward correction procedure. The results demonstrate that the coded-aperture procedure is a viable approach for imaging not only point sources of radiation, but also extended sources of emission. The results for the Crab's photon spectrum are consistent with a power-law spectrum. Upper limits on the flux levels of line emission at 405 keV and 1050 keV and on the flux from the X-ray binary source A0535 + 26 and diffuse Galactic emission from the anticenter region are derived. 35 references.

Mcconnell, M.L.; Dunphy, P.P.; Forrest, D.J.; Chupp, E.L.; Owens, A.

1987-10-01T23:59:59.000Z

369

Update on HI data collection from GBT, Parkes and Arecibo telescopes for the Cosmic Flows project  

E-Print Network [OSTI]

Cosmic Flows is an international multi-element project with the goal to map motions of galaxies in the Local Universe. Kinematic information from observations in the radio HI line and photometry at optical or near-infrared bands are acquired to derive the large majority of distances that are obtained through the luminosity-linewidth or Tully-Fisher relation. This paper gathers additional observational radio data, frequently unpublished, retrieved from the archives of Green Bank, Parkes and Arecibo telescopes. Extracted HI profiles are consistently processed to produce linewidth measurements. Our current "All-Digital HI Catalog" contains a total of 20,343 HI spectra for 17,738 galaxies with 14,802 galaxies with accurate linewidth measurement useful for Tully-Fisher galaxy distances. This addition of 4,117 new measurements represents an augmentation of 34\\% compared to our last release.

Courtois, Helene M

2014-01-01T23:59:59.000Z

370

Search for dark matter from the Galactic halo with the IceCube Neutrino Telescope  

Science Journals Connector (OSTI)

Self-annihilating or decaying dark matter in the Galactic halo might produce high energy neutrinos detectable with neutrino telescopes. We have conducted a search for such a signal using 276days of data from the IceCube 22-string configuration detector acquired during 2007 and 2008. The effect of halo model choice in the extracted limit is reduced by performing a search that considers the outer halo region and not the Galactic Center. We constrain any large-scale neutrino anisotropy and are able to set a limit on the dark matter self-annihilation cross section of ??Av??10-22??cm3?s-1 for weakly interacting massive particle masses above 1TeV, assuming a monochromatic neutrino line spectrum.

R. Abbasi et al. (IceCube Collaboration)

2011-07-29T23:59:59.000Z

371

A Diffractive-Optic Telescope for X-Ray Astronomy D. Dewey, T.H. Markert, and M.L. Schattenburg  

E-Print Network [OSTI]

A Diffractive-Optic Telescope for X-Ray Astronomy D. Dewey, T.H. Markert, and M.L. Schattenburg for a light-weight X-ray astronomical telescope that uses a diffractive optical element is described (200-1000 cm2 ) through the use of a blazed diffractive optic. State-of-the-art grating technology

Dewey, Daniel

372

SNAP Telescope Performance for Weak Lensing Surveys M.Lampton1, M.Sholl1, P.Jelinsky1, and H.Stabenau2 for the SNAP Collaboration  

E-Print Network [OSTI]

.7 µm * 0.7 deg2 instantaneous pixellized field * 70 deg solar avoidance angle Telescope basics Annular of Energy, through contract DE-AC02-05CH11231. Expect extreme PSF Stability * telescope is thermally isolated from outer baffle * no deployed panels, antennas, or radiators * active thermal control on optics

California at Berkeley, University of

373

The MAHOROBA Project -- Deep Survey with an Optical Intermediate-Band Filter System on the Subaru Telescope  

E-Print Network [OSTI]

We present a summary of the new optical intermediate-band filter system for the prime-focus camera, Suprime-Cam, on the Subaru telescope at Mauna Kea Observatories. We also discuss a future plan to promote a new deep survey with this filter system (the MAHOROBA project).

Taniguchi, Y

2003-01-01T23:59:59.000Z

374

Prospects for detecting dark matter with neutrino telescopes in light of recent results from direct detection experiments  

SciTech Connect (OSTI)

Direct detection dark matter experiments, lead by the CDMS collaboration, have placed increasingly stronger constraints on the cross sections for elastic scattering of WIMPs on nucleons. These results impact the prospects for the indirect detection of dark matter using neutrino telescopes. With this in mind, we revisit the prospects for detecting neutrinos produced by the annihilation of WIMPs in the Sun. We find that the latest bounds do not seriously limit the models most accessible to next generation kilometer-scale neutrino telescopes such as IceCube. This is largely due to the fact that models with significant spin-dependent couplings to protons are the least constrained and, at the same time, the most promising because of the efficient capture of WIMPs in the Sun. We identify models where dark matter particles are beyond the reach of any planned direct detection experiments while within reach of neutrino telescopes. In summary, we find that, even when contemplating recent direct detection results, neutrino telescopes still have the opportunity to play an important as well as complementary role in the search for particle dark matter.

Halzen, Francis; /Wisconsin U., Madison; Hooper, Dan; /Fermilab

2005-10-01T23:59:59.000Z

375

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

376

Charles F. McMillan  

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

Los Alamos National Laboratory | Los Alamos National Laboratory | April 2013 | UNCLASSIFIED | 1 Operated by Los Alamos National Security, LLC for the U.S. Department of Energy's NNSA UNCLASSIFIED UNCLASSIFIED Operated by Los Alamos National Security, LLC for the U.S. Department of Energy's NNSA Ultra-deep Water Risk Assessment DV Rao September 17, 2013 | Los Alamos National Laboratory | April 2013 | UNCLASSIFIED | 2 Operated by Los Alamos National Security, LLC for the U.S. Department of Energy's NNSA UNCLASSIFIED 1. Real-time data from the bottom-hole 2. VSP (see also No. 9 below) 3. Automated kick detect (with 1 above) 4. Human performance improvement: - MWD alerts during swabbing, fishing, etc. - Rotating control device - 'quick-response' BHP control (closed cycle)

377

Charles F. McMillan  

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

Improving neutron capture rate predictions using Apollo + HELIOS Experiment development : A. Couture, M. Devlin, H. Y. Lee and J. M. O'Donnell (LANSCE-NS) Nuclear reaction model...

378

Profile of Charles L. Sawyers  

Science Journals Connector (OSTI)

...prostate tumors in mice. The compound, dubbed MDV3100, became a poster child of the pharmaceutical company Medivation, which is testing the drug in...Sawyers. | Biography Historical Article Journal Article | Education, Medical History, 20th Century History, 21st Century Humans...

Prashant Nair

2011-01-01T23:59:59.000Z

379

Charles Darwin University 1 INTERNATIONAL  

E-Print Network [OSTI]

in Australia; to safeguard Australia's international reputation as a provider of high quality education

380

Charles Forsberg | ornl.gov  

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

at Bechtel. He led research activities that successfully separated actinide and rare earth elements from acidic high-level waste solutions and provided leadership on nuclear...

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381

Pulsed Gamma-Rays From PSR J2021 3651 with the Fermi Large Area Telescope  

SciTech Connect (OSTI)

We report the detection of pulsed gamma-rays from the young, spin-powered radio pulsar PSR J2021+3651 using data acquired with the Large Area Telescope (LAT) on the Fermi Gamma-ray Space Telescope (formerly GLAST). The light curve consists of two narrow peaks of similar amplitude separated by 0.468 {+-} 0.002 in phase. The first peak lags the maximum of the 2 GHz radio pulse by 0.162 {+-} 0.004 {+-} 0.01 in phase. The integral gamma-ray photon flux above 100 MeV is (56 {+-} 3 {+-} 11) x 10{sup -8} cm{sup -2} s{sup -1}. The photon spectrum is well-described by an exponentially cut-off power law of the form dF/dE = kE{sup -{Gamma}}e{sup (-E/E{sub c})} where the energy E is expressed in GeV. The photon index is {Gamma} = 1.5 {+-} 0.1 {+-} 0.1 and the exponential cut-off is E{sub c} = 2.4 {+-} 0.3 {+-} 0.5 GeV. The first uncertainty is statistical and the second is systematic. The integral photon flux of the bridge is approximately 10% of the pulsed emission, and the upper limit on off-pulse gamma-ray emission from a putative pulsar wind nebula is < 10% of the pulsed emission at the 95% confidence level. Radio polarization measurements yield a rotation measure of RM = 524 {+-} 4 rad m{sup -2} but a poorly constrained magnetic geometry. Re-analysis of Chandra data enhanced the significance of the weak X-ray pulsations, and the first peak is roughly phase-aligned with the first gamma-ray peak. We discuss the emission region and beaming geometry based on the shape and spectrum of the gamma-ray light curve combined with radio and X-ray measurements, and the implications for the pulsar distance. Gamma-ray emission from the polar cap region seems unlikely for this pulsar.

Abdo, Aous A.; /Naval Research Lab, Wash., D.C.; Ackermann, M.; /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept.; Ajello, Marco; /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept.; Atwood, William B.; /UC, Santa Cruz; Baldini, L.; /INFN, Pisa; Ballet, J.; /DAPNIA, Saclay; Barbiellini, Guido; /INFN, Trieste /Trieste U.; Bastieri, Denis; /INFN, Padua /Padua U.; Battelino, Milan; /Royal Inst. Tech., Stockholm; Baughman, B.M.; /Ohio State U.; Bechtol, K.; /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept.; Bellazzini, Ronaldo; /INFN, Pisa; Berenji, Bijan; /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept.; Bloom, Elliott D.; /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept.; Bogaert, G.; /Ecole Polytechnique; Borgland, Anders W.; /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept.; Bregeon, J.; /INFN, Pisa; Brez, A.; /INFN, Pisa; Brigida, M.; /Bari U. /INFN, Bari; Bruel, P.; /Ecole Polytechnique; Burnett, Thompson H.; /Washington U., Seattle /Bari U. /INFN, Bari /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /Columbia U. /IASF, Milan /IASF, Milan /DAPNIA, Saclay /INFN, Perugia /Perugia U. /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /George Mason U. /Naval Research Lab, Wash., D.C. /IASF, Milan /IASF, Milan /NASA, Goddard /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /INFN, Perugia /Perugia U. /LPCE, Orleans /Montpellier U. /Sonoma State U. /Royal Inst. Tech., Stockholm /Stockholm U. /ASI, Rome /NRAO, Charlottesville /Naval Research Lab, Wash., D.C. /INFN, Trieste /Pavia U. /Bari U. /INFN, Bari /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /UC, Santa Cruz /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /CENBG, Gradignan /CENBG, Gradignan /Manchester U. /Montpellier U. /Bari U. /INFN, Bari; /more authors..

2011-11-30T23:59:59.000Z

382

Fermi Large Area Telescope Observations of the Supernova Remnant G8.7-0.1  

SciTech Connect (OSTI)

We present a detailed analysis of the GeV gamma-ray emission toward the supernova remnant (SNR) G8.7-0.1 with the Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope. An investigation of the relationship between G8.7-0.1 and the TeV unidentified source HESS J1804-216 provides us with an important clue on diffusion process of cosmic rays if particle acceleration operates in the SNR. The GeV gamma-ray emission is extended with most of the emission in positional coincidence with the SNR G8.7-0.1 and a lesser part located outside the western boundary of G8.7-0.1. The region of the gamma-ray emission overlaps spatially connected molecular clouds, implying a physical connection for the gamma-ray structure. The total gamma-ray spectrum measured with LAT from 200 MeV-100 GeV can be described by a broken power-law function with a break of 2.4 {+-} 0.6 (stat) {+-} 1.2 (sys) GeV, and photon indices of 2.10 {+-} 0.06 (stat) {+-} 0.10 (sys) below the break and 2.70 {+-} 0.12 (stat) {+-} 0.14 (sys) above the break. Given the spatial association among the gamma rays, the radio emission of G8.7-0.1, and the molecular clouds, the decay of p0s produced by particles accelerated in the SNR and hitting the molecular clouds naturally explains the GeV gamma-ray spectrum. We also find that the GeV morphology is not well represented by the TeV emission from HESS J1804-216 and that the spectrum in the GeV band is not consistent with the extrapolation of the TeV gamma-ray spectrum. The spectral index of the TeV emission is consistent with the particle spectral index predicted by a theory that assumes energy-dependent diffusion of particles accelerated in an SNR. We discuss the possibility that the TeV spectrum originates from the interaction of particles accelerated in G8.7-0.1 with molecular clouds, and we constrain the diffusion coefficient of the particles.

Ajello, M.; Allafort, A.; /Stanford U., HEPL /KIPAC, Menlo Park /SLAC; Baldini, L.; /INFN, Pisa; Ballet, J.; /AIM, Saclay; Barbiellini, G.; /INFN, Trieste /Trieste U.; Bastieri, D.; /INFN, Padua /Padua U.; Bechtol, K.; /Stanford U., HEPL /KIPAC, Menlo Park /SLAC; Bellazzini, R.; /INFN, Pisa; Berenji, B.; Blandford, R.D.; Bloom, E.D.; /Stanford U., HEPL /KIPAC, Menlo Park /SLAC; Bonamente, E.; /INFN, Perugia /Perugia U.; Borgland, A.W.; /Stanford U., HEPL /KIPAC, Menlo Park /SLAC; Bregeon, J.; /INFN, Pisa; Brigida, M.; /Bari Polytechnic /INFN, Bari; Bruel, P.; /Ecole Polytechnique; Buehler, R.; /Stanford U., HEPL /KIPAC, Menlo Park /SLAC; Buson, S.; /INFN, Padua /Padua U.; Caliandro, G.A.; /CSIC, Catalunya; Cameron, R.A.; /Stanford U., HEPL /KIPAC, Menlo Park /SLAC; Caraveo, P.A.; /IASF, Milan /AIM, Saclay /INFN, Perugia /Perugia U. /Stanford U., HEPL /KIPAC, Menlo Park /SLAC /Unlisted, US /Naval Research Lab, Wash., D.C. /Perugia U. /ASDC, Frascati /Stanford U., HEPL /KIPAC, Menlo Park /SLAC /Montpellier U. /ASDC, Frascati /Udine U. /INFN, Trieste /Bari Polytechnic /INFN, Bari /Naval Research Lab, Wash., D.C. /Stanford U., HEPL /KIPAC, Menlo Park /SLAC /Bari Polytechnic /INFN, Bari /Ecole Polytechnique /NASA, Goddard /Stanford U., HEPL /KIPAC, Menlo Park /SLAC /Udine U. /INFN, Trieste /Trieste Observ. /Hiroshima U. /Nagoya U. /Bari Polytechnic /INFN, Bari /INFN, Bari /ASDC, Frascati /INFN, Perugia /Perugia U. /Bari Polytechnic /INFN, Bari /ASDC, Frascati /Bari Polytechnic /INFN, Bari /Bologna Observ. /Stanford U., HEPL /KIPAC, Menlo Park /SLAC /Naval Research Lab, Wash., D.C. /Alabama U., Huntsville /CSIC, Catalunya /Hiroshima U. /NASA, Goddard /Hiroshima U.; /more authors..

2012-09-14T23:59:59.000Z

383

A SPITZER SPACE TELESCOPE STUDY OF THE DEBRIS DISKS AROUND FOUR SDSS WHITE DWARFS  

SciTech Connect (OSTI)

We present Spitzer Space Telescope data of four isolated white dwarfs that were previously known to harbor circumstellar gaseous disks. Infrared Array Camera photometry shows a significant infrared excess in all of the systems, SDSS0738+1835, SDSS0845+2257, SDSS1043+0855, and SDSS1617+1620, indicative of a dusty extension to those disks. The 4.5 {mu}m excesses seen in SDSS0738, SDSS0845, and SDSS1617 are 7.5, 5.7, and 4.5 times the white dwarf contribution, respectively. In contrast, in SDSS1043, the measured flux density at 4.5 {mu}m is only 1.7 times the white dwarf contribution. We compare the measured IR excesses in the systems to models of geometrically thin, optically thick disks, and find that we are able to match the measured spectral energy distributions to within 3{sigma} of the uncertainties, although disks with unfeasibly hot inner dust temperatures generally provide a better fit than those below the dust sublimation temperature. Possible explanations for the dearth of dust around SDSS1043+0855 are briefly discussed. Including our previous study of SDSS1228+1040, all five white dwarfs with gaseous debris disks have significant amounts of dust around them. It is evident that gas and dust can coexist around these relatively warm, relatively young white dwarfs.

Brinkworth, C. S.; Girven, J. M.; Hoard, D. W. [Spitzer Science Center, California Institute of Technology, Pasadena, CA 91125 (United States); Gaensicke, B. T.; Marsh, T. R.; Parsons, S. G. [Department of Physics and Astronomy, University of Warwick, Warwick CV4 7AL (United Kingdom); Koester, D. [Institut fuer Theoretische Physik und Astrophysik, University of Kiel, 24098 Kiel (Germany)

2012-05-01T23:59:59.000Z

384

THERMAL PROPERTIES OF A SOLAR CORONAL CAVITY OBSERVED WITH THE X-RAY TELESCOPE ON HINODE  

SciTech Connect (OSTI)

Coronal cavities are voids in coronal emission often observed above high latitude filament channels. Sometimes, these cavities have areas of bright X-ray emission in their centers. In this study, we use data from the X-ray Telescope (XRT) on the Hinode satellite to examine the thermal emission properties of a cavity observed during 2008 July that contains bright X-ray emission in its center. Using ratios of XRT filters, we find evidence for elevated temperatures in the cavity center. The area of elevated temperature evolves from a ring-shaped structure at the beginning of the observation, to an elongated structure two days later, finally appearing as a compact round source four days after the initial observation. We use a morphological model to fit the cavity emission, and find that a uniform structure running through the cavity does not fit the observations well. Instead, the observations are reproduced by modeling several short cylindrical cavity 'cores' with different parameters on different days. These changing core parameters may be due to some observed activity heating different parts of the cavity core at different times. We find that core temperatures of 1.75 MK, 1.7 MK, and 2.0 MK (for July 19, July 21, and July 23, respectively) in the model lead to structures that are consistent with the data, and that line-of-sight effects serve to lower the effective temperature derived from the filter ratio.

Reeves, Katharine K. [Harvard-Smithsonian Center for Astrophysics, 60 Garden St. MS 58, Cambridge, MA 02138 (United States); Gibson, Sarah E. [HAO/NCAR, P.O. Box 3000, Boulder, CO 80307-3000 (United States); Kucera, Therese A. [NASA Goddard Space Flight Center, Code 671, Greenbelt, MD 20771 (United States); Hudson, Hugh S. [Space Sciences Laboratories, University of California, Berkeley, 7 Gauss Way, Berkeley, CA 94720 (United States); Kano, Ryouhei, E-mail: kreeves@cfa.harvard.edu [National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 (Japan)

2012-02-20T23:59:59.000Z

385

Fine-scale structures and material flows of quiescent filaments observed by New Vacuum Solar Telescope  

E-Print Network [OSTI]

Study on the small-scale structures and material flows of solar quiescent filaments is very important for understanding the formation and equilibrium of solar filaments. Using the high resolution H{\\alpha} data observed by the New Vacuum Solar Telescope (NVST), we present the structures of the barbs and the material flows along the threads across the spine in two quiescent filaments on 2013 September 29 and on 2012 November 2, respectively. During the evolution of the filament barb, several parallel tube-shaped structures formed and the width of the structures ranges from about 2.3 Mm to 3.3 Mm. The parallel tube-shaped structures merged together accompanied with the material flows from the spine to the barb. Moreover, the boundary between the barb and surrounding atmosphere is very neat. The counter-streaming flows were not found to appear alternately in the adjacent threads of the filament. However, the large-scale patchy counter-streaming flows are detected in the filament. The flows in one patch of the fi...

Yan, X L; Xiang, Y Y; Yang, L H

2015-01-01T23:59:59.000Z

386

Background Rejection of Charged Particles in the Simbol-X Telescope: Preliminary Study of Protons Scattering  

SciTech Connect (OSTI)

X-ray telescopes equipped with focusing optics in high eccentric orbit, as e.g. Newton-XMM and Chandra, showed a degradation of the detector performance and an important increase of the noise due to soft protons with energy between a few tens of keV and a few MeV, that are focused on the detector through the mirror module. It should be noted that the focusing of the protons by Wolter optics was an unexpected phenomenon. In Simbol-X a magnetic diverter will be implemented to deflect protons, in order to reduce the flux of charged particles impinging upon the focal plane. Obviously the design of the diverter should take into consideration the protons distribution at the exit of the mirror module; for this reason a detailed simulation about the interaction of particles with the mirror surface is necessary. Here we will present the scattering protons models currently under consideration, suggesting a preliminary solution for the design of the magnetic diverter. We will also discuss an ad hoc experiment to study this problem.

Dell'Orto, E. [INAF-OAB-Merate-Italy (Italy); Universita dell'Insubria-Como (Italy); Barbera, M. [INAF-OAPa-Palermo (Italy); Bulgarelli, A.; Fioretti, V.; Malaguti, G. [INAF-IASF-Bo-Bologna (Italy); Mineo, T. [INAF-IASF-Pa-Palermo (Italy); Pareschi, G.; Spiga, D.; Tagliaferri, G. [INAF-OAB-Merate (Italy); Rigato, V. [INFN-LNL-Legnar (Italy)

2009-05-11T23:59:59.000Z

387

BUSCA A Telescope Instrumentation for Simultaneous Imaging in 4 Optical Bands  

E-Print Network [OSTI]

The "Bonn University Simultaneous CAmera" (BUSCA) is a CCD camera system which allows simultaneous direct imaging of the same sky area in four colors. The optics are designed for an f/8 beam and four 4Kx4K CCDs with 15m pixels covering a field of view of 12 arcmin x 12 arcmin at a 2m class telescope. In September 1998 BUSCA has seen "First Light". The instrument is based on three dichroic beam splitters which separate optical wavelength bands such (at 430nm, 540nm, 730nm) that standard astronomical intermediate-band filter systems can be used. The dichroics are made of plane-parallel glass plates mounted at an angle of 45 degrees. Astigmatism in the transmitted beams (f/8) is completely cancelled by identical plane-parallel glass plates of suitable orientation. BUSCA offers new perspectives in astronomical multicolor photometry: i) The broadband spectral properties (e.g. color indices) of astronomical objects in the optical can be determined with high reliability even in non-photometric atmospheric conditions...

Reif, K; De Boer, K S; Schmoll, J; Mller, P; Poschmann, H; Klink, G; Kohley, R; Heber, U; Mebold, U; Mueller, Ph.

1999-01-01T23:59:59.000Z

388

IceCube-Plus: An Ultra-High Energy Neutrino Telescope  

E-Print Network [OSTI]

While the first kilometer-scale neutrino telescope, IceCube, is under constructi on, alternative plans exist to build even larger detectors that will, however, b e limited by a much higher neutrino energy threshold of 10 PeV or higher rather than 10 to 100 GeV. These future projects detect radio and acoustic pulses as w ell as air showers initiated by ultra-high energy neutrinos. As an alternative, we here propose an expansion of IceCube, using the same strings, placed on a gri d with a spacing of order 500 m. Unlike other proposals, the expanded detector uses methods that are understood and calibrated on atmospheric neutrinos. Atmosp heric neutrinos represent the only background at the energies under consideratio n and is totally negligible. Also, the cost of such a detector is understood. We conclude that supplementing the 81 IceCube strings with a modest number of addi tional strings spaced at large distances can almost double the effective volume of the detector. Doubling the number of strings on a 800 m ...

Halzen, F; Halzen, Francis; Hooper, Dan

2004-01-01T23:59:59.000Z

389

IceCube-Plus: An Ultra-High Energy Neutrino Telescope  

E-Print Network [OSTI]

While the first kilometer-scale neutrino telescope, IceCube, is under construction, alternative plans exist to build even larger detectors that will, however, b e limited by a much higher neutrino energy threshold of 10 PeV or higher rather than 10 to 100 GeV. These future projects detect radio and acoustic pulses as w ell as air showers initiated by ultra-high energy neutrinos. As an alternative, we here propose an expansion of IceCube, using the same strings, placed on a gri d with a spacing of order 500 m. Unlike other proposals, the expanded detector uses methods that are understood and calibrated on atmospheric neutrinos. Atmosp heric neutrinos represent the only background at the energies under consideratio n and is totally negligible. Also, the cost of such a detector is understood. We conclude that supplementing the 81 IceCube strings with a modest number of addi tional strings spaced at large distances can almost double the effective volume of the detector. Doubling the number of strings on a 800 m grid can deliver a d etector that this a factor of 5 larger for horizontal muons at modest cost.

Francis Halzen; Dan Hooper

2003-12-22T23:59:59.000Z

390

THE SECOND FERMI LARGE AREA TELESCOPE CATALOG OF GAMMA-RAY PULSARS  

SciTech Connect (OSTI)

This catalog summarizes 117 high-confidence ?0.1 GeV gamma-ray pulsar detections using three years of data acquired by the Large Area Telescope (LAT) on the Fermi satellite. Half are neutron stars discovered using LAT data through periodicity searches in gamma-ray and radio data around LAT unassociated source positions. The 117 pulsars are evenly divided into three groups: millisecond pulsars, young radio-loud pulsars, and young radio-quiet pulsars. We characterize the pulse profiles and energy spectra and derive luminosities when distance information exists. Spectral analysis of the off-peak phase intervals indicates probable pulsar wind nebula emission for four pulsars, and off-peak magnetospheric emission for several young and millisecond pulsars. We compare the gamma-ray properties with those in the radio, optical, and X-ray bands. We provide flux limits for pulsars with no observed gamma-ray emission, highlighting a small number of gamma-faint, radio-loud pulsars. The large, varied gamma-ray pulsar sample constrains emission models. Fermi's selection biases complement those of radio surveys, enhancing comparisons with predicted population distributions.

Abdo, A. A. [Center for Earth Observing and Space Research, College of Science, George Mason University, Fairfax, VA 22030 (United States); Ajello, M. [Space Sciences Laboratory, 7 Gauss Way, University of California, Berkeley, CA 94720-7450 (United States); Allafort, A.; Bloom, E. D.; Bottacini, E. [W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305 (United States); Baldini, L. [Universit di Pisa and Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa (Italy); Ballet, J. [Laboratoire AIM, CEA-IRFU/CNRS/Universit Paris Diderot, Service d'Astrophysique, CEA Saclay, F-91191 Gif sur Yvette (France); Barbiellini, G. [Istituto Nazionale di Fisica Nucleare, Sezione di Trieste, I-34127 Trieste (Italy); Baring, M. G. [Rice University, Department of Physics and Astronomy, MS-108, P.O. Box 1892, Houston, TX 77251 (United States); Bastieri, D. [Istituto Nazionale di Fisica Nucleare, Sezione di Padova, I-35131 Padova (Italy); Belfiore, A. [Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California at Santa Cruz, Santa Cruz, CA 95064 (United States); Bellazzini, R.; Bregeon, J. [Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa (Italy); Bhattacharyya, B. [National Centre for Radio Astrophysics, Tata Institute of Fundamental Research, Pune 411 007 (India); Bissaldi, E. [Istituto Nazionale di Fisica Nucleare, Sezione di Trieste, and Universit di Trieste, I-34127 Trieste (Italy); Bonamente, E. [Istituto Nazionale di Fisica Nucleare, Sezione di Perugia, I-06123 Perugia (Italy); Brandt, T. J. [NASA Goddard Space Flight Center, Greenbelt, MD 20771 (United States); Brigida, M., E-mail: hartog@stanford.edu [Dipartimento di Fisica ''M. Merlin'' dell'Universit e del Politecnico di Bari, I-70126 Bari (Italy); and others

2013-10-01T23:59:59.000Z

391

Magnetic reconnection between small-scale loops observed with the New Vacuum Solar Telescope  

E-Print Network [OSTI]

Using the high tempo-spatial resolution H$\\alpha$ images observed with the New Vacuum Solar Telescope, we report the solid observational evidence of magnetic reconnection between two sets of small-scale anti-parallel loops with an X-shaped topology. The reconnection process contains two steps: a slow step with the duration of more than several tens of minutes, and a rapid step lasting for only about three minutes. During the slow reconnection, two sets of anti-parallel loops reconnect gradually, and new loops are formed and stacked together. During the rapid reconnection, the anti-parallel loops approach each other quickly, and then the rapid reconnection takes place, resulting in the disappearance of former loops. In the meantime, new loops are formed and separate. The region between the approaching loops is brightened, and the thickness and length of this region are determined to be about 420 km and 1.4 Mm, respectively. During the rapid reconnection process, obvious brightenings at the reconnection site an...

Yang, Shuhong; Xiang, Yongyuan

2014-01-01T23:59:59.000Z

392

The Hobby-Eberly Telescope Dark Energy Experiment (HETDEX): Description and Early Pilot Survey Results  

E-Print Network [OSTI]

The Hobby-Eberly Telescope Dark Energy Experiment (HETDEX) will outfit the 10 m HET with a new wide field and an array of 150 integral-field spectrographs to survey a 420 sq. deg. area in the north Galactic cap. Each fiber-coupled unit spectrograph will cover 350-550 nm, simultaneously. This instrument, called VIRUS, will produce ~34,000 spectra per exposure, and will open up the emission-line universe to large surveys for the first time. The survey will detect 0.8 million Lyman-alpha emitting (LAE) galaxies with 1.9measure the expansion history at this early epoch using baryonic acoustic oscillations and the shape of the power spectrum. The aim of HETDEX is to provide a direct detection of dark energy at z~3. The measurement will constrain the evolution of dark energy and will also provide 0.1%-level accuracy on the curvature of the Universe, ten times better than current. The prototype of the VIRUS unit spectrograph (VIRUS-P) is a powerful instrument in its own right. Used on the McDonald 2.7 m, it covers the largest area of any integral field spectrograph, and reaches wavelengths down to 340 nm. VIRUS-P is being used for a pilot survey to better measure the properties of LAE galaxies in support of HETDEX. We report initial results from this survey.

G. J. Hill; K. Gebhardt; E. Komatsu; N. Drory; P. J. MacQueen; J. Adams; G. A. Blanc; R. Koehler; M. Rafal; M. M. Roth; A. Kelz; C. Gronwall; R. Ciardullo; D. P. Schneider

2008-06-01T23:59:59.000Z

393

Formation Process of a Light Bridge Revealed with the Hinode Solar Optical Telescope  

E-Print Network [OSTI]

The Solar Optical Telescope (SOT) aboard HINODE successfully and continuously observed a formation process of a light bridge in a matured sunspot of the NOAA active region 10923 for several days with high spatial resolution. During its formation, many umbral dots were observed emerging from the leading edges of penumbral filaments, and intruding into the umbra rapidly. The precursor of the light bridge formation was also identified as the relatively slow inward motion of the umbral dots which emerged not near the penumbra, but inside the umbra. The spectro-polarimeter on SOT provided physical conditions in the photosphere around the umbral dots and the light bridges. We found the light bridges and the umbral dots had significantly weaker magnetic fields associated with upflows relative to the core of the umbra, which implies that there was hot gas with weak field strength penetrating from subphotosphere to near the visible surface inside those structures. There needs to be a mechanism to drive the inward motion of the hot gas along the light bridges. We suggest that the emergence and the inward motion are triggered by a buoyant penumbral flux tube as well as the subphotospheric flow crossing the sunspot.

Y. Katsukawa; T. Yokoyama; T. E. Berger; K. Ichimoto; M. Kubo; B. W. Lites; S. Nagata; T. Shimizu; R. A. Shine; Y. Suematsu; T. D. Tarbell; A. M. Title; S. Tsuneta

2007-09-17T23:59:59.000Z

394

Hubble Space Telescope Far Ultraviolet Spectroscopy of the Recurrent Nova T Pyxidis  

E-Print Network [OSTI]

With six recorded nova outbursts, the prototypical recurrent nova T Pyxidis is the ideal cataclysmic variable system to assess the net change of the white dwarf mass within a nova cycle. Recent estimates of the mass ejected in the 2011 outburst ranged from a few 1.E-5 sollar mass to 3.3E-4 sollar mass, and assuming a mass accretion rate of 1.E-8 to 1.E-7 Sollar mass/yr for 44yrs, it has been concluded that the white dwaf in T Pyx is actually losing mass. Using NLTE disk modeling spectra to fit our recently obtained Hubble Space Telescope (HST) COS and STIS spectra, we find a mass accretion rate of up to two orders of magnitude larger than previously estimated. Our larger mass accretion rate is due mainly to the newly derived distance of T Pyx (4.8kpc; Sokoloski et al. 2013, larger than the previous 3.5kpc estimate), our derived reddening of E(B-V)=0.35 (based on combined IUE and GALEX spectra) and NLTE disk modeling (compared to black body and raw flux estimates in earlier works). We find that for most values...

Godon, P; Starrfield, S; Livio, M; Williams, R E; Woodward, C E; Kuin, P; Page, K L

2014-01-01T23:59:59.000Z

395

Hubble Space Telescope ACS mosaic of the prototypical starburst galaxy M82  

E-Print Network [OSTI]

In March 2006, the Hubble Heritage Team obtained a large four-filter (B, V, I, and H-alpha) six-point mosaic dataset of the prototypical starburst galaxy NGC 3034 (M82), with the Advanced Camera for Surveys (ACS) onboard the Hubble Space Telescope (HST). The resulting color composite Heritage image was released in April 2006, to celebrate Hubble's 16th anniversary. Cycle 15 HST proposers were encouraged to submit General Observer and Archival Research proposals to complement or analyze this unique dataset. Since our M82 mosaics represent a significant investment of expert processing beyond the standard archival products, we will also release our drizzle combined FITS data as a High Level Science Product via the Multimission Archive at STScI (MAST) on December 31, 2006. This paper documents the key aspects of the observing program and image processing: calibration, image registration and combination (drizzling), and the rejection of cosmic rays and detector artifacts. Our processed FITS mosaics and related inf...

Mutchler, M; Christian, C A; Frattare, L M; Hamilton, F; Januszewski, W; Levay, Z G; Mountain, M; Noll, K S; Royle, P; Gallagher, J S; Puxley, P

2006-01-01T23:59:59.000Z

396

Atmospheric Characterization of 5 Hot Jupiters with Wide Field Camera 3 on the Hubble Space Telescope  

E-Print Network [OSTI]

We probe the structure and composition of the atmospheres of 5 hot Jupiter exoplanets using the Hubble Space Telescope Wide Field Camera 3 (WFC3) instrument. We use the G141 grism (1.1-1.7 $\\mu$m) to study TrES-2b, TrES-4b, and CoRoT-1b in transit, TrES-3b in secondary eclipse, and WASP-4b in both. This wavelength region includes a predicted absorption feature from water at 1.4 $\\mu$m, which we expect to be nondegenerate with the other molecules that are likely to be abundant for hydrocarbon-poor (e.g. solar composition) hot Jupiter atmospheres. We divide our wavelength regions into 10 bins. For each bin we produce a spectrophotometric light curve spanning the time of transit and/or eclipse. We correct these light curves for instrumental systematics without reference to an instrument model. For our transmission spectra, our mean $1-\\sigma$ precision per bin corresponds to variations of 2.1, 2.8, and 3.0 atmospheric scale heights for TrES-2b, TrES-4b, and CoRoT-1b, respectively. We find featureless spectra for...

Ranjan, Sukrit; Dsert, Jean-Michel; Madhusudhan, Nikku; Deming, Drake; Wilkins, Ashlee; Mandell, Avi M

2014-01-01T23:59:59.000Z

397

Development of mirrors made of chemically tempered glass foils for future X-ray telescopes  

E-Print Network [OSTI]

Thin slumped glass foils are considered good candidates for the realization of future X-ray telescopes with large effective area and high spatial resolution. However, the hot slumping process affects the glass strength, and this can be an issue during the launch of the satellite because of the high kinematical and static loads occurring during that phase. In the present work we have investigated the possible use of Gorilla glass (produced by Corning), a chemical tempered glass that, thanks to its strength characteristics, would be ideal. The un-tempered glass foils were curved by means of an innovative hot slumping technique and subsequently chemically tempered. In this paper we show that the chemical tempering process applied to Gorilla glass foils does not affect the surface micro-roughness of the mirrors. On the other end, the stress introduced by the tempering process causes a reduction in the amplitude of the longitudinal profile errors with a lateral size close to the mirror length. The effect of the ov...

Salmaso, B; Brizzolari, B; Basso, S; Ghigo, M; Pareschi, G; Spiga, D; Proserpio, L; Suppiger, Y

2015-01-01T23:59:59.000Z

398

THE CANADA-FRANCE-HAWAII TELESCOPE LEGACY SURVEY: STACKED IMAGES AND CATALOGS  

SciTech Connect (OSTI)

This paper describes the image stacks and catalogs of the Canada-France-Hawaii Telescope Legacy Survey produced using the MegaPipe data pipeline at the Canadian Astronomy Data Centre. The Legacy Survey is divided into two parts. The Deep Survey consists of four fields each of 1 deg{sup 2}, with magnitude limits (50% completeness for point sources) of u = 27.5, g = 27.9, r = 27.7, i = 27.4, and z = 26.2. It contains 1.6 Multiplication-Sign 10{sup 6} sources. The Wide Survey consists of 150 deg{sup 2} split over four fields, with magnitude limits of u = 26.0, g = 26.5, r = 25.9, i = 25.7, and z = 24.6. It contains 3 Multiplication-Sign 10{sup 7} sources. This paper describes the calibration, image stacking, and catalog generation process. The images and catalogs are available on the web through several interfaces: normal image and text file catalog downloads, a 'Google Sky' interface, an image cutout service, and a catalog database query service.

Gwyn, Stephen D. J., E-mail: Stephen.Gwyn@nrc-cnrc.gc.ca [Canadian Astronomy Data Centre, Herzberg Institute of Astrophysics, 5071 West Saanich Road, Victoria, British Columbia, V9E 2E7 (Canada)

2012-02-15T23:59:59.000Z

399

ULTRASPEC: a high-speed imaging photometer on the 2.4-m Thai National Telescope  

E-Print Network [OSTI]

ULTRASPEC is a high-speed imaging photometer mounted permanently at one of the Nasmyth focii of the 2.4-m Thai National Telescope (TNT) on Doi Inthanon, Thailand's highest mountain. ULTRASPEC employs a 1024x1024 pixel frame-transfer, electron-multiplying CCD (EMCCD) in conjunction with re-imaging optics to image a field of 7.7'x7.7' at (windowed) frame rates of up to ~200 Hz. The EMCCD has two outputs - a normal output that provides a readout noise of 2.3 e- and an avalanche output that can provide essentially zero readout noise. A six-position filter wheel enables narrow-band and broad-band imaging over the wavelength range 330-1000 nm. The instrument saw first light on the TNT in November 2013 and will be used to study rapid variability in the Universe. In this paper we describe the scientific motivation behind ULTRASPEC, present an outline of its design and report on its measured performance on the TNT.

Dhillon, V S; Atkinson, D C; Bezawada, N; Bours, M C P; Copperwheat, C M; Gamble, T; Hardy, L K; Hickman, R D H; Irawati, P; Ives, D J; Kerry, P; Leckngam, A; Littlefair, S P; McLay, S A; O'Brien, K; Peacocke, P T; Poshyachinda, S; Richichi, A; Soonthornthum, B; Vick, A

2014-01-01T23:59:59.000Z

400

Exoplanet Science with the European Extremely Large Telescope. The Case for Visible and Near-IR Spectroscopy at High Resolution  

E-Print Network [OSTI]

Exoplanet science is booming. In 20 years our knowledge has expanded considerably, from the first discovery of a Hot Jupiter, to the detection of a large population of Neptunes and super-Earths, to the first steps toward the characterization of exoplanet atmospheres. Between today and 2025, the field will evolve at an even faster pace with the advent of several space-based transit search missions, ground-based spectrographs, high-contrast imaging facilities, and the James Webb Space Telescope. Especially the ESA M-class PLATO mission will be a game changer in the field. From 2024 onwards, PLATO will find transiting terrestrial planets orbiting within the habitable zones of nearby, bright stars. These objects will require the power of Extremely Large Telescopes (ELTs) to be characterized further. The technique of ground-based high-resolution spectroscopy is establishing itself as a crucial pathway to measure chemical composition, atmospheric structure and atmospheric circulation in transiting exoplanets. A hig...

Udry, S; Bouchy, F; Cameron, A Collier; Henning, T; Mayor, M; Pepe, F; Piskunov, N; Pollacco, D; Queloz, D; Quirrenbach, A; Rauer, H; Rebolo, R; Santos, N C; Snellen, I; Zerbi, F

2014-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "telescope baltay charles" from the National Library of EnergyBeta (NLEBeta).
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to obtain the most current and comprehensive results.


401

The Introduction of Tech Pan lm at the UK Schmidt Telescope Quentin A Parker 1;3 David Malin 2  

E-Print Network [OSTI]

The Introduction of Tech Pan #12;lm at the UK Schmidt Telescope Quentin A Parker 1;3 David Malin 2.parker@roe.ac.uk Abstract Kodak Technical Pan (Tech Pan) emulsion on a #12;lm base has been in use at the U.K. Schmidt 1981), though it was introduced somewhat earlier as 35mm solar patrol #12;lm (as special order SO-115

Tittley, Eric

402

AN INITIAL LOOK AT THE FAR-INFRAREDRADIO CORRELATION WITHIN NEARBY STAR-FORMING GALAXIES USING THE SPITZER SPACE TELESCOPE  

E-Print Network [OSTI]

THE SPITZER SPACE TELESCOPE E. J. Murphy,1 R. Braun,2 G. Helou,3 L. Armus,3 J. D. P. Kenney,1 K. D. Gordon,4 G. Cannon,6 B. T. Draine,8 C. W. Engelbracht,4 D. J. Hollenbach,9 T. H. Jarrett,3 L. J. Kewley,10 C. Leitherer,7 A. Li,11 M. J. Meyer,7 M. W. Regan,7 G. H. Rieke,4 M. J. Rieke,4 H. Roussel,3 K. Sheth,3 J. D. T

Draine, Bruce T.

403

New Results from Observations of Massive Star Formation in the Mid-Infrared with Large Aperture Telescopes  

E-Print Network [OSTI]

Thanks to the high spatial resolution afforded by 8-10m class telescopes, we are beginning to learn that some sources are extended in their mid-infrared emission because of dusty outflows or heated outflow cavity walls. Therefore one must be extremely careful in interpreting the nature of extended mid-infrared sources (i.e. just because it is extended does not automatically mean it is a disk!).

James M. De Buizer

2006-10-18T23:59:59.000Z

404

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

405

HUBBLE SPACE TELESCOPE AND GROUND-BASED OBSERVATIONS OF V455 ANDROMEDAE POST-OUTBURST  

SciTech Connect (OSTI)

Hubble Space Telescope spectra obtained in 2010 and 2011, 3 and 4 yr after the large amplitude dwarf nova outburst of V455 And, were combined with optical photometry and spectra to study the cooling of the white dwarf, its spin, and possible pulsation periods after the outburst. The modeling of the ultraviolet (UV) spectra shows that the white dwarf temperature remains ?600 K hotter than its quiescent value at 3 yr post-outburst, and still a few hundred degrees hotter at 4 yr post-outburst. The white dwarf spin at 67.6 s and its second harmonic at 33.8 s are visible in the optical within a month of outburst and are obvious in the later UV observations in the shortest wavelength continuum and the UV emission lines, indicating an origin in high-temperature regions near the accretion curtains. The UV light curves folded on the spin period show a double-humped modulation consistent with two-pole accretion. The optical photometry 2 yr after outburst shows a group of frequencies present at shorter periods (250-263 s) than the periods ascribed to pulsation at quiescence, and these gradually shift toward the quiescent frequencies (300-360 s) as time progresses past outburst. The most surprising result is that the frequencies near this period in the UV data are only prominent in the emission lines, not the UV continuum, implying an origin away from the white dwarf photosphere. Thus, the connection of this group of periods with non-radial pulsations of the white dwarf remains elusive.

Szkody, Paula; Mukadam, Anjum S.; Brown, Justin; Funkhouser, Kelsey [Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195 (United States); Gnsicke, Boris T. [Department of Physics, University of Warwick, Coventry CV4 7AL (United Kingdom); Henden, Arne [AAVSO, 49 Bay State Road, Cambridge, MA 02138 (United States); Sion, Edward M. [Department of Astronomy and Astrophysics, Villanova University, Villanova, PA 19085 (United States); Townsley, Dean M. [Department of Physics and Astronomy, University of Alabama, Tuscaloosa, AL 35487 (United States); Christian, Damian [Department of Physics and Astronomy, California State University, Northridge, CA 91330 (United States); Falcon, Ross E. [Department of Astronomy, University of Texas, Austin, TX 78712 (United States); Pyrzas, Stylianos, E-mail: szkody@astro.washington.edu, E-mail: anjum@astro.washington.edu, E-mail: boris.gaensicke@warwick.ac.uk, E-mail: arne@aavso.org, E-mail: edward.sion@villanova.edu, E-mail: Dean.M.Townsley@ua.edu, E-mail: damian.christian@csun.edu, E-mail: cylver@astro.as.utexas.edu, E-mail: stylianos.pyrzas@gmail.com [Instituto de Astronomia, Universidad Catolica del Norte, Avenida Angamos 0619, Antofagasta (Chile)

2013-09-20T23:59:59.000Z

406

HUBBLE SPACE TELESCOPE PIXEL ANALYSIS OF THE INTERACTING S0 GALAXY NGC 5195 (M51B)  

SciTech Connect (OSTI)

We report the properties of the interacting S0 galaxy NGC 5195 (M51B), revealed in a pixel analysis using the Hubble Space Telescope/Advanced Camera for Surveys images in the F435W, F555W, and F814W (BVI) bands. We analyze the pixel color-magnitude diagram (pCMD) of NGC 5195, focusing on the properties of its red and blue pixel sequences and the difference from the pCMD of NGC 5194 (M51A; the spiral galaxy interacting with NGC 5195). The red pixel sequence of NGC 5195 is redder than that of NGC 5194, which corresponds to the difference in the dust optical depth of 2 < {Delta}{tau}{sub V} < 4 at fixed age and metallicity. The blue pixel sequence of NGC 5195 is very weak and spatially corresponds to the tidal bridge between the two interacting galaxies. This implies that the blue pixel sequence is not an ordinary feature in the pCMD of an early-type galaxy, but that it is a transient feature of star formation caused by the galaxy-galaxy interaction. We also find a difference in the shapes of the red pixel sequences on the pixel color-color diagrams (pCCDs) of NGC 5194 and NGC 5195. We investigate the spatial distributions of the pCCD-based pixel stellar populations. The young population fraction in the tidal bridge area is larger than that in other areas by a factor >15. Along the tidal bridge, young populations seem to be clumped particularly at the middle point of the bridge. On the other hand, the dusty population shows a relatively wide distribution between the tidal bridge and the center of NGC 5195.

Lee, Joon Hyeop; Kim, Sang Chul; Ree, Chang Hee; Kim, Minjin; Jeong, Hyunjin; Lee, Jong Chul; Kyeong, Jaemann, E-mail: jhl@kasi.re.kr, E-mail: sckim@kasi.re.kr, E-mail: chr@kasi.re.kr, E-mail: mkim@kasi.re.kr, E-mail: hyunjin@kasi.re.kr, E-mail: jclee@kasi.re.kr, E-mail: jman@kasi.re.kr [Korea Astronomy and Space Science Institute, Daejeon 305-348 (Korea, Republic of)

2012-08-01T23:59:59.000Z

407

ON THE FERMI LARGE AREA TELESCOPE SURPLUS OF DIFFUSE GALACTIC GAMMA-RAY EMISSION  

SciTech Connect (OSTI)

Recent observations of diffuse Galactic ?-ray emission (DGE) by the Fermi Large Area Telescope (Fermi-LAT) have shown significant deviations, above a few GeV to about 100 GeV, from DGE models that use the GALPROP code for the propagation of cosmic ray (CR) particles outside their sources in the Galaxy and their interaction with the target distributions of the interstellar gas and radiation fields. The surplus of radiation observed is most pronounced in the inner Galaxy, where the concentration of CR sources is strongest. The present study investigates this 'Fermi-LAT Galactic Plane Surplus' by estimating the ?-ray emission from the sources themselves, which is disregarded in the above DGE models. It is shown that the expected hard spectrum of CRs, still confined in their sources (source cosmic rays, SCRs), can indeed explain this surplus. The method is based on earlier studies regarding the so-called EGRET GeV excess, which by now is generally interpreted as an instrumental effect. The contribution from SCRs is also predicted to increasingly exceed the DGE models above 100 GeV, up to ?-ray energies of about 10 TeV, where the corresponding surplus exceeds the hadronic part of the DGE by about one order of magnitude. Above such energies, the emission surplus should decrease again with energy due to the finite lifetime of the assumed supernova remnant sources. Observations of the DGE in the inner Galaxy at 15 TeV with the ground-based Milagro ?-ray detector and, at TeV energies, with the ARGO-YBJ detector are interpreted to provide confirmation of a significant SCR contribution to the DGE.

Vlk, H. J. [Max-Planck-Institut fr Kernphysik, P.O. Box 103980, D-69029 Heidelberg (Germany); Berezhko, E. G., E-mail: Heinrich.Voelk@mpi-hd.mpg.de [Yu. G. Shafer Institute of Cosmophysical Research and Aeronomy, 31 Lenin Avenue, 677980 Yakutsk (Russian Federation)

2013-11-10T23:59:59.000Z

408

HUBBLE SPACE TELESCOPE OBSERVATIONS OF DUSTY FILAMENTS IN HERCULES A: EVIDENCE FOR ENTRAINMENT  

SciTech Connect (OSTI)

We present U-, V-, and I-band images of the host galaxy of Hercules A (3C 348) obtained with HST/WFC3/UVIS. We find a network of dusty filaments which are more complex and extended than seen in earlier Hubble Space Telescope (HST) observations. The filaments are associated with a faint blue continuum light (possibly from young stars) and faint H{alpha} emission. It seems likely that the cold gas and dust has been stripped from a companion galaxy now seen as a secondary nucleus. There are dusty filaments aligned with the base of the jets on both eastern and western sides of the galaxy. The morphology of the filaments is different on the two sides-the western filaments are fairly straight, while the eastern filaments are mainly in two loop-like structures. We suggest that despite the difference in morphologies, both sets of filaments have been entrained in a slow-moving boundary layer outside the relativistic flow. As suggested by Fabian et al., magnetic fields in the filaments may stabilize them against disruption. We consider a speculative scenario to explain the relation between the radio source and the shock and cavities in the hot intracluster medium seen in the Chandra data. We suggest that the radio source originally ({approx}60 Myr ago) propagated along a position angle of {approx}35 Degree-Sign where it created the shock and cavities. The radio source axis changed to its current orientation ({approx}100 Degree-Sign ) possibly due to a supermassive black hole merger and began its current epoch of activity about 20 Myr ago.

O'Dea, C. P.; Kharb, P. [School of Physics and Astronomy, and Laboratory for Multiwavelength Astrophysics, Rochester Institute of Technology, 84 Lomb Memorial Dr., Rochester, NY 14623 (United States); Baum, S. A. [Chester F. Carlson Center for Imaging Science, Rochester Institute of Technology, 84 Lomb Memorial Dr., Rochester, NY 14623 (United States); Tremblay, G. R. [European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748 Garching bei Muenchen (Germany); Cotton, W. [National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903 (United States); Perley, R. [National Radio Astronomy Observatory, P.O. Box 0, Socorro, NM 87801 (United States)

2013-07-01T23:59:59.000Z

409

A DUAL-BAND MILLIMETER-WAVE KINETIC INDUCTANCE CAMERA FOR THE IRAM 30 m TELESCOPE  

SciTech Connect (OSTI)

The Neel IRAM KIDs Array (NIKA) is a fully integrated measurement system based on kinetic inductance detectors (KIDs) currently being developed for millimeter wave astronomy. The instrument includes dual-band optics allowing simultaneous imaging at 150 GHz and 220 GHz. The imaging sensors consist of two spatially separated arrays of KIDs. The first array, mounted on the 150 GHz branch, is composed of 144 lumped-element KIDs. The second array (220 GHz) consists of 256 antenna-coupled KIDs. Each of the arrays is sensitive to a single polarization; the band splitting is achieved by using a grid polarizer. The optics and sensors are mounted in a custom dilution cryostat, with an operating temperature of {approx}70 mK. Electronic readout is realized using frequency multiplexing and a transmission line geometry consisting of a coaxial cable connected in series with the sensor array and a low-noise 4 K amplifier. The dual-band NIKA was successfully tested in 2010 October at the Institute for Millimetric Radio Astronomy (IRAM) 30 m telescope at Pico Veleta, Spain, performing in-line with laboratory predictions. An optical NEP was then calculated to be around 2 x 10{sup -16} W Hz{sup -1/2} (at 1 Hz) while under a background loading of approximately 4 pW pixel{sup -1}. This improvement in comparison with a preliminary run (2009) verifies that NIKA is approaching the target sensitivity for photon-noise limited ground-based detectors. Taking advantage of the larger arrays and increased sensitivity, a number of scientifically relevant faint and extended objects were then imaged including the Galactic Center SgrB2 (FIR1), the radio galaxy Cygnus A, and the NGC1068 Seyfert galaxy. These targets were all observed simultaneously in the 150 GHz and 220 GHz atmospheric windows.

Monfardini, A.; Benoit, A.; Bideaud, A.; Swenson, L.; Cruciani, A.; Camus, P.; Hoffmann, C. [Institut Neel, CNRS and Universite Joseph Fourier (UJF), Grenoble F-38042 (France); Desert, F. X. [Institut de Planetologie et d'Astrophysique, UJF and CNRS-INSU, Grenoble F-38041 (France); Doyle, S.; Ade, P.; Mauskopf, P.; Tucker, C. [Cardiff School of Physics and Astronomy, Cardiff University, Cardiff CF24 3AA (United Kingdom); Roesch, M.; Leclercq, S.; Schuster, K. F. [Institut de RadioAstronomie Millimetrique (IRAM), Saint Martin d'Heres F-38406 (France); Endo, A. [Kavli Institute of NanoScience, Delft University of Technology, 2628 CJ Delft (Netherlands); Baryshev, A.; Baselmans, J. J. A.; Ferrari, L.; Yates, S. J. C, E-mail: monfardini@grenoble.cnrs.fr [SRON, Netherlands Institute for Space Research, 3584 CA Utrecht and 9700 AV Groningen (Netherlands)

2011-06-01T23:59:59.000Z

410

Si and Fe depletion in Galactic star-forming regions observed by the Spitzer Space Telescope  

E-Print Network [OSTI]

We report the results of the mid-infrared spectroscopy of 14 Galactic star-forming regions with the high-resolution modules of the Infrared Spectrograph (IRS) on board the Spitzer Space Telescope. We detected [SiII] 35um, [FeII] 26um, and [FeIII] 23um as well as [SIII] 33um and H2 S(0) 28um emission lines. Using the intensity of [NII] 122um or 205um and [OI] 146um or 63um reported by previous observations in four regions, we derived the ionic abundance Si+/N+ and Fe+/N+ in the ionized gas and Si+/O0 and Fe+/O0 in the photodissociation gas. For all the targets, we derived the ionic abundance of Si+/S2+ and Fe2+/S2+ for the ionized gas. Based on photodissociation and HII region models the gas-phase Si and Fe abundance are suggested to be 3-100% and solar abundance, respectively, for the ionized gas and 16-100% and 2-22% of the solar abundance, respectively, for the photodissociation region gas. Since the [FeII] 26um and [FeIII] 23um emissions are weak, the high sensitivity of the IRS enables to derive the gas-phase Fe abundance widely in star-forming regions. The derived gas-phase Si abundance is much larger than that in cool interstellar clouds and that of Fe. The present study indicates that 3-100% of Si atoms and <22% of Fe atoms are included in dust grains which are destroyed easily in HII regions, probably by the UV radiation. We discuss possible mechanisms to account for the observed trend; mantles which are photodesorbed by UV photons, organometallic complexes, or small grains.

Yoko Okada; Takashi Onaka; Takashi Miyata; Yoshiko K. Okamoto; Itsuki Sakon; Hiroshi Shibai; Hidenori Takahashi

2008-04-10T23:59:59.000Z

411

Redshift z ~ 1 Field Galaxies Observed with the Keck Telescope and the HST  

E-Print Network [OSTI]

We report results based on 35 new spectroscopic redshifts obtained with the Keck Telescope for field galaxies that also have photometry and morphology from survey images taken by the refurbished HST. A sample of 24 redshifts for galaxies fainter than I = 22 has a median redshift of z ~ 0.81. This result is inconsistent with the lower median redshift of z ~ 0.6 predicted by the ``maximal merger models'' of Carlberg (1996), which otherwise fit existing data. The data match an extrapolation of the CFRS, as well as predictions of certain mild luminosity-evolution models. Nearly half of the redshifts lie in two structures at z ~ 0.81 and z ~ 1.0, showing the presence of high density concentrations spanning scales of ~ 1/h Mpc, i.e., the size of groups. We find emission lines or the presence of possible neighbors in 7 of 9 otherwise luminous galaxies with red central regions at redshifts beyond z ~ 0.7. We also note a diversity of morphological types among blue galaxies at z ~ 1, including small compact galaxies, ``chains,'' and ``blue nucleated galaxies.'' These morphologies are found among local, but generally less luminous, galaxies. Distant blue galaxies also include apparently normal late-type spirals. These findings could imply modest bursts of star formation caused by mergers or interactions of small, gas-rich galaxies with each other or with larger, well-formed galaxies. This first glimpse of very faint z ~ 1 field galaxies of diverse colors and morphologies suggests that a mixture of physical processes is at work in the formation and evolution of faint field galaxies.

David C. Koo; Nicole P. Vogt; Andrew C. Phillips; Rafael Guzman; K. L. Wu; S. M. Faber; Caryl Gronwall; Duncan A. Forbes; Garth D. Illingworth; Edward J. Groth; Marc Davis; Richard G. Kron; Alexander S. Szalay

1996-04-19T23:59:59.000Z

412

Investigation of the spectrum of high-energy muons by the method of multiple interactions on the basis of data from the Baksan underground scintillation telescope  

Science Journals Connector (OSTI)

Experimental data obtained with the aid of the Baksan underground scintillation telescope over a long period of its operation are analyzed with the aim of searches for an excess flux of ultrahigh-energy (?100 TeV...

A. G. Bogdanov; R. P. Kokoulin; Yu. F. Novoseltsev

2009-12-01T23:59:59.000Z

413

A Letter from the Rev. Mr. James Pound, Rector of Wanstead, F. R. S. to Dr. Jurin, Secr. R. S. concerning Observations Made with Mr. Hadley's Reflecting Telescope  

Science Journals Connector (OSTI)

...Mr. James Pound, Rector of Wanstead, F. R. S. to Dr. Jurin, Secr. R. S. concerning Observations Made with Mr. Hadley's Reflecting Telescope James Pound The Royal Society is collaborating with JSTOR to digitize, preserve, and extend access...

1722-01-01T23:59:59.000Z

414

GRB 090926A AND BRIGHT LATE-TIME FERMI LARGE AREA TELESCOPE GAMMA-RAY BURST AFTERGLOWS  

SciTech Connect (OSTI)

GRB 090926A was detected by both the Gamma-ray Burst Monitor and Large Area Telescope (LAT) instruments on board the Fermi Gamma-ray Space Telescope. Swift follow-up observations began {approx}13 hr after the initial trigger. The optical afterglow was detected for nearly 23 days post trigger, placing it in the long-lived category. The afterglow is of particular interest due to its brightness at late times, as well as the presence of optical flares at T0+10{sup 5} s and later, which may indicate late-time central engine activity. The LAT has detected a total of 16 gamma-ray bursts; nine of these bursts, including GRB 090926A, also have been observed by Swift. Of the nine Swift-observed LAT bursts, six were detected by UVOT, with five of the bursts having bright, long-lived optical afterglows. In comparison, Swift has been operating for five years and has detected nearly 500 bursts, but has only seen {approx}30% of bursts with optical afterglows that live longer than 10{sup 5} s. We have calculated the predicted gamma-ray fluence, as would have been seen by the Burst Alert Telescope (BAT) on board Swift, of the LAT bursts to determine whether this high percentage of long-lived optical afterglows is unique, when compared to BAT-triggered bursts. We find that, with the exception of the short burst GRB 090510A, the predicted BAT fluences indicate that the LAT bursts are more energetic than 88% of all Swift bursts and also have brighter than average X-ray and optical afterglows.

Swenson, C. A.; Roming, P. W. A.; Vetere, L.; Kennea, J. A. [Pennsylvania State University, 525 Davey Lab, University Park, PA 16802 (United States); Maxham, A.; Zhang, B. B.; Zhang, B. [University of Nevada, Las Vegas, Box 454002, 4505 Maryland Parkway, Las Vegas, NV 89154 (United States); Schady, P. [Max-Planck-Institut fuer extraterrestrische Physik, Garching (Germany); Holland, S. T. [Universities Space Research Association, 10227 Wincopin Circle, Suite 500, Columbia, MD 21044 (United States); Kuin, N. P. M.; Oates, S. R.; De Pasquale, M. [The UCL Mullard Space Science Laboratory, Holmbury St Mary, Surrey, RH5 6NT (United Kingdom); Page, K. L., E-mail: cswenson@astro.psu.ed [Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH (United Kingdom)

2010-07-20T23:59:59.000Z

415

Results from a Prototype MAPS Sensor Telescope and Readout Systemwith Zero Suppression for the Heavy Flavor Tracker at STAR  

SciTech Connect (OSTI)

We describe a three Mimostar-2 Monolithic Active PixelSensor (MAPS) sensor telescope prototype with an accompanying readoutsystem incorporating on-the-fly data sparsification. The system has beencharacterized and we report on the measured performance of the sensortelescope and readout system in beam tests conducted both at the AdvancedLight Source (ALS) at Lawrence Berkeley National Laboratory (LBNL) and inthe STAR experiment at the Relativistic Heavy Ion Collider (RHIC). Thiseffort is part of the development and prototyping work that will lead toa vertex detector for the STAR experiment.

Greiner, Leo C.; Matis, Howard S.; Ritter, Hans G.; Rose, AndrewA.; Stezelberger, Thorsten; Sun, Xiangming; Szelezniak, Michal A.; Thomas, James H.; Vu, Chinh Q.; Wieman, Howard H.

2008-02-11T23:59:59.000Z

416

Neutrino Induced Upward Going Muons from a Gamma Ray Burst in a Neutrino Telescope of Km^2 Area  

E-Print Network [OSTI]

The number of neutrino induced upward going muons from a single Gamma Ray Burst (GRB) expected to be detected by the proposed kilometer scale IceCube detector at the South Pole location has been calculated. The effects of the Lorentz factor, total energy of the GRB emitted in neutrinos and its distance from the observer (red shift) on the number of neutrino events from the GRB have been examined. The present investigation reveals that there is possibility of exploring the early Universe with the proposed kilometer scale IceCube neutrino telescope.

Nayantara Gupta

2002-01-30T23:59:59.000Z

417

Hubble Space Telescope Near-Ultraviolet Spectroscopy of the Bright CEMP-no Star BD+44 493  

E-Print Network [OSTI]

We present an elemental-abundance analysis, in the near-ultraviolet (NUV) spectral range, for the extremely metal-poor star BD+44 493, a 9th magnitude sub-giant with [Fe/H] = -3.8 and enhanced carbon, based on data acquired with the Space Telescope Imaging Spectrograph on the Hubble Space Telescope. This star is the brightest example of a class of objects that, unlike the great majority of carbon-enhanced metal-poor (CEMP) stars, does not exhibit over-abundances of heavy neutron-capture elements (CEMP-no). In this paper, we validate the abundance determinations for a number of species that were previously studied in the optical region, and obtain strong upper limits for beryllium and boron, as well as for neutron-capture elements from zirconium to platinum, many of which are not accessible from ground-based spectra. The boron upper limit we obtain for BD+44 493, logeps(B) < -0.70, the first such measurement for a CEMP star, is the lowest yet found for very and extremely metal-poor stars. In addition, we ob...

Placco, Vinicius; Roederer, Ian; Cowan, John; Frebel, Anna; Filler, Dan; Ivans, Inese I; Lawler, James E; Schatz, Hendrik; Sneden, Christopher; Sobeck, Jennifer; Aoki, Wako; Smith, Verne

2014-01-01T23:59:59.000Z

418

PROSPECTS FOR A DARK MATTER ANNIHILATION SIGNAL TOWARD THE SAGITTARIUS DWARF GALAXY WITH GROUND-BASED CHERENKOV TELESCOPES  

SciTech Connect (OSTI)

Dwarf galaxies are widely believed to be among the best targets for indirect dark matter searches using high-energy gamma rays and indeed gamma-ray emission from these objects has long been a subject of detailed study for ground-based atmospheric Cherenkov telescopes. Here, we update current exclusion limits obtained on the closest dwarf, the Sagittarius dwarf galaxy, in light of recent realistic dark matter halo models. The constraints on the velocity-weighted annihilation cross-section of the dark matter particle are of a few 10{sup -23} cm{sup 3} s{sup -1} in the TeV energy range for a 50 hr exposure. The limits are extrapolated to the sensitivities of future Cherenkov Telescope Arrays. For 200 hr of observation time, the sensitivity at the 95% confidence level reaches 10{sup -25} cm{sup 3} s{sup -1}. Possible astrophysical backgrounds from gamma-ray sources dissembled in the Sagittarius dwarf are studied. It is shown that with long enough observation times, gamma-ray background from millisecond pulsars in a globular cluster contained within the Sagittarius dwarf may limit the sensitivity to dark matter annihilations.

Viana, A.; Medina, M. C.; Brun, P.; Glicenstein, J. F.; Kosack, K.; Moulin, E.; Naumann-Godo, M.; Peyaud, B. [IRFU/DSM, CEA Saclay, F-91191 Gif-sur-Yvette, Cedex (France); Penarrubia, J. [Institute of Astronomy, University of Cambridge, Cambridge CB3 0HA (United Kingdom)

2012-02-10T23:59:59.000Z

419

The ASTRI Project: prototype status and future plans for a Cherenkov dual-mirror small-telescope array  

E-Print Network [OSTI]

ASTRI ("Astrofisica con Specchi a Tecnologia Replicante Italiana") is a flagship project of the Italian Ministry of Education, University and Research. Within this framework, INAF is currently developing a wide field of view (9.6 degrees in diameter) end-to-end prototype of the CTA small-size telescope (SST), devoted to the investigation of the energy range from a fraction of TeV up to tens of TeVs, and scheduled to start data acquisition in 2014. For the first time, a dual-mirror Schwarzschild-Couder optical design will be adopted on a Cherenkov telescope, in order to obtain a compact optical configuration. A second challenging, but innovative technical solution consists of a modular focal surface camera based on Silicon photo-multipliers with a logical pixel size of 6.2mm x 6.2mm. Here we describe the current status of the project, the expected performance, and its possible evolution in terms of an SST mini-array. This CTA-SST precursor, composed of a few SSTs and developed in collaboration with CTA interna...

Vercellone, S; Maccarone, M C; Di Pierro, F; Vallania, P; Bonnoli, G; Canestrari, R; Pareschi, G; Tosti, G

2013-01-01T23:59:59.000Z

420

The ASTRI project: Prototype status and future plans for a Cherenkov dual-mirror small-telescope array  

Science Journals Connector (OSTI)

ASTRI ("Astrofisica con Specchi a Tecnologia Replicante Italiana") is a flagship project of the Italian Ministry of Education University and Research. Within this framework INAF is currently developing a wide field of view (9.6 in diameter) end-to-end prototype of the CTA smallsize telescope (SST) devoted to the investigation of the energy range from a fraction of TeV up to (possibly) hundreds of TeV and scheduled to start data acquisition in 2014. For the first time a dualmirror Schwarzschild-Couder optical design will be adopted on a Cherenkov telescope in order to obtain a compact (F? = 0.5) optical configuration. A second challenging but innovative technical solution consists of a focal plane camera based on Silicon photo-multipliers with a logical pixel size of 0.17 (6.2mm 6.2mm). We will describe the current status of the project the results obtained so far the expected performance and its possible evolution in terms of a SST mini-array (composed of 5-7 SSTs and developed in collaboration with CTA international partners) which could peruse not only the adopted technological solutions but also address a few scientific test cases.

S. Vercellone; ASTRI Collaboration

2012-01-01T23:59:59.000Z

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421

Searches for Point-like and extended neutrino sources close to the Galactic Centre using the ANTARES neutrino Telescope  

E-Print Network [OSTI]

A search for cosmic neutrino sources using six years of data collected by the ANTARES neutrino telescope has been performed. Clusters of muon neutrinos over the expected atmospheric background have been looked for. No clear signal has been found. The most signal-like accumulation of events is located at equatorial coordinates RA=$-$46.8$^{\\circ}$ and Dec=$-$64.9$^{\\circ}$ and corresponds to a 2.2$\\sigma$ background fluctuation. In addition, upper limits on the flux normalization of an E$^{-2}$ muon neutrino energy spectrum have been set for 50 pre-selected astrophysical objects. Finally, motivated by an accumulation of 7 events relatively close to the Galactic Centre in the recently reported neutrino sample of the IceCube telescope, a search for point sources in a broad region around this accumulation has been carried out. No indication of a neutrino signal has been found in the ANTARES data and upper limits on the flux normalization of an E$^{-2}$ energy spectrum of neutrinos from point sources in that region have been set. The 90% confidence level upper limits on the muon neutrino flux normalization vary between 3.5 and 5.1$\\times$10$^{-8}$ GeV$\\,$cm$^{-2}$s$^{-1}$, depending on the exact location of the source.

ANTARES Collaboration; S. Adrin-Martnez; A. Albert; M. Andr; M. Anghinolfi; G. Anton; M. Ardid; J. -J. Aubert; B. Baret; J. Barrios-Mart; S. Basa; V. Bertin; S. Biagi; C. Bogazzi; R. Bormuth; M. Bou-Cabo; M. C. Bouwhuis; R. Bruijn; J. Brunner; J. Busto; A. Capone; L. Caramete; C. Crloganu; J. Carr; T. Chiarusi; M. Circella; L. Core; H. Costantini; P. Coyle; A. Creusot; C. Curtil; G. De Rosa; I. Dekeyser; A. Deschamps; G. De Bonis; C. Distefano; C. Donzaud; D. Dornic; Q. Dorosti; D. Drouhin; A. Dumas; T. Eberl; D. Elssser; A. Enzenhfer; S. Escoffier; K. Fehn; I. Felis; P. Fermani; F. Folger; L. A. Fusco; S. Galat; P. Gay; S. Geielsder; K. Geyer; V. Giordano; A. Gleixner; J. P. Gmez-Gonzlez; K. Graf; G. Guillard; H. van Haren; A. J. Heijboer; Y. Hello; J. J. Hernndez-Rey; B. Herold; A. Herrero; J. Hl; J. Hofestdt; C. W James; M. de Jong; M. Kadler; O. Kalekin; U. Katz; D. Kieling; P. Kooijman; A. Kouchner; I. Kreykenbohm; V. Kulikovskiy; R. Lahmann; E. Lambard; G. Lambard; D. Lattuada; D. Lefvre; E. Leonora; H. Loehner; S. Loucatos; S. Mangano; M. Marcelin; A. Margiotta; J. A. Martnez-Mora; S. Martini; A. Mathieu; T. Michael; P. Migliozzi; C. Mueller; M. Neff; E. Nezri; D. Palioselitis; G. E. P?v?la?; C. Perrina; P. Piattelli; V. Popa; T. Pradier; C. Racca; G. Riccobene; R. Richter; K. Roensch; A. Rostovtsev; M. Saldaa; D. F. E. Samtleben; A. Snchez-Losa; M. Sanguineti; P. Sapienza; J. Schmid; J. Schnabe; S. Schulte; F. Schssler; T. Seitz; C. Sieger; A. Spies; M. Spurio; J. J. M. Steijger; Th. Stolarczyk; M. Taiuti; C. Tamburini; Y. Tayalati; A. Trovato; B. Vallage; C. Valle; V. Van Elewyck; E. Visser; D. Vivolo; S. Wagner; J. Wilms; E. de Wolf; K. Yatkin; H. Yepes; J. D. Zornoza; J. Ziga

2014-02-25T23:59:59.000Z

422

Wide-Field InfraRed Survey Telescope (WFIRST) Mission and Synergies with LISA and LIGO-Virgo  

E-Print Network [OSTI]

The Wide-Field InfraRed Survey Telescope (WFIRST) is a NASA space mission in study for launch in 2024. It has a 2.4 m telescope, wide-field IR instrument operating in the 0.7 - 2.0 micron range and an exoplanet imaging coronagraph instrument operating in the 400 - 1000 nm range. The observatory will perform galaxy surveys over thousands of square degrees to J=27 AB for dark energy weak lensing and baryon acoustic oscillation measurements and will monitor a few square degrees for dark energy SN Ia studies. It will perform microlensing observations of the galactic bulge for an exoplanet census and direct imaging observations of nearby exoplanets with a pathfinder coronagraph. The mission will have a robust and well-funded guest observer program for 25% of the observing time. WFIRST will be a powerful tool for time domain astronomy and for coordinated observations with gravitational wave experiments. Gravitational wave events produced by mergers of nearby binary neutron stars (LIGO-Virgo) or extragalactic superm...

Gehrels, Neil

2014-01-01T23:59:59.000Z

423

Reconstruction efficiency and discovery potential of a Mediterranean neutrino telescope: A simulation study using the Hellenic Open University Simulation & Reconstruction (HOURS) package  

E-Print Network [OSTI]

We report on the evaluation of the performance of a Mediterranean very large volume neutrino telescope. We present results of our studies concerning the capability of the telescope in detecting/discovering galactic (steady point sources) and extragalactic, transient (Gamma Ray Bursts) high energy neutrino sources as well as measuring ultra high energy diffuse neutrino fluxes. The neutrino effective area and angular resolution are presented as a function of the neutrino energy, and the background event rate (atmospheric neutrinos and muons) is estimated. The discovery potential of the neutrino telescope is evaluated and the experimental time required for a significant discovery of potential neutrino emitters (known from their gamma ray emission, assumedly produced by hadronic interactions) is estimated. For the simulation we use the HOU Reconstruction & Simulation (HOURS) software package.

Tsirigotis, A G; Tzamarias, S E

2012-01-01T23:59:59.000Z

424

HIGH-FREQUENCY RADIO SPECTRAL ENERGY DISTRIBUTIONS AND POLARIZATION FRACTIONS OF SOURCES IN AN ATACAMA COSMOLOGY TELESCOPE SURVEY FIELD  

SciTech Connect (OSTI)

We present flux densities and polarization percentages of 159 radio galaxies based on nearly simultaneous Very Large Array observations at four frequencies, 4.86, 8.46, 22.46, and 43.34 GHz. This sample is selected from the high-frequency Australia Telescope 20 GHz (AT20G) survey and consists of all sources with flux density S{sub 20GHz} > 40 mJy in an equatorial field of the Atacama Cosmology Telescope (ACT) survey. For a subset of 25 of these sources, we used the Green Bank Telescope (GBT) to obtain 90 GHz data. The goals of this program are: (1) a characterization of the spectra, polarization, and variability of high-frequency-selected radio sources, (2) extrapolating from the few GHz regime to the {approx}150 GHz regime of the ACT survey, allowing for more accurate removal of the radio source signal in our particular field, and (3) providing a data set that will allow more accurate modeling of the high-frequency radio source contamination in current and future Sunyaev-Zeldovich and cosmic microwave background experiments. We find that, as expected, this sample consists of flatter spectrum and more compact or point-like sources than low-frequency-selected samples. In the K band, variability is typically {approx}<20%, although there are exceptions. The higher frequency data are well suited to the detection of extreme gigahertz peak spectrum sources. The inclusion of the 43 GHz data causes the relative fraction of inverted spectrum sources to go down and of peaked spectrum sources to go up when compared with the AT20G survey results. The trend largely continues with the inclusion of the 90 GHz data, although {approx}10% of the sources with GBT data show a spectral upturn from 43 GHz to 90 GHz. The measured polarization fractions are typically <5%, although in some cases they are measured to be up to {approx}20%. For sources with detected polarized flux in all four bands, about 40% of the sample, the polarization fractions typically increase with frequency. This trend is stronger for steeper spectrum sources as well as for the lower flux density sources.

Sajina, Anna [Department of Physics and Astronomy, Tufts University, Medford, MA 02155 (United States); Partridge, Bruce; Evans, Tyler; Vechik, Nicholas [Department of Physics and Astronomy, Haverford College, Haverford, PA 19041 (United States); Stefl, Shannon [Kent State University, Kent, OH 44242 (United States); Myers, Steve [National Radio Astronomy Observatory, Socorro, NM 87801 (United States); Dicker, Simon; Korngut, Phillip [Department of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104 (United States)

2011-05-01T23:59:59.000Z

425

Prospects for observing ultra-compact binaries with space-based gravitational wave interferometers and optical telescopes  

E-Print Network [OSTI]

Space-based gravitational wave interferometers are sensitive to the galactic population of ultra-compact binaries. An important subset of the ultra-compact binary population are those stars that can be individually resolved by both gravitational wave interferometers and electromagnetic telescopes. The aim of this paper is to quantify the multi-messenger potential of space-based interferometers with arm-lengths between 1 and 5 Gm. The Fisher Information Matrix is used to estimate the number of binaries from a model of the Milky Way which are localized on the sky by the gravitational wave detector to within 1 and 10 square degrees and bright enough to be detected by a magnitude limited survey. We find, depending on the choice of GW detector characteristics, limiting magnitude, and observing strategy, that up to several hundred gravitational wave sources could be detected in electromagnetic follow-up observations.

Tyson B. Littenberg; Shane L. Larson; Gijs Nelemans; Neil J. Cornish

2012-07-20T23:59:59.000Z

426

Prospects for observing ultra-compact binaries with space-based gravitational wave interferometers and optical telescopes  

E-Print Network [OSTI]

Space-based gravitational wave interferometers are sensitive to the galactic population of ultra-compact binaries. An important subset of the ultra-compact binary population are those stars that can be individually resolved by both gravitational wave interferometers and electromagnetic telescopes. The aim of this paper is to quantify the multi-messenger potential of space-based interferometers with arm-lengths between 1 and 5 Gm. The Fisher Information Matrix is used to estimate the number of binaries from a model of the Milky Way which are localized on the sky by the gravitational wave detector to within 1 deg$^2$ and bright enough to be detected by a magnitude limited survey. We find, depending on the choice of GW detector characteristics, limiting magnitude, and observing strategy, that up to a few hundred gravitational wave sources could be detected in electromagnetic follow-up observations.

Littenberg, Tyson B; Nelemans, Gijs; Cornish, Neil J

2012-01-01T23:59:59.000Z

427

Green Bank Telescope observations of the water masers of NGC 3079: accretion disk magnetic field and maser scintillation  

E-Print Network [OSTI]

We present observations of the 22 GHz water megamasers in the circumnuclear disk of NGC 3079 obtained with the Green Bank Telescope. The data are analyzed for circular polarization due to the Zeeman-induced splitting of the water maser lines. No circular polarization is detected and we derive a 1 sigma upper limit of 11 mG for the toroidal magnetic field at ~0.64 pc from the central black hole. This is the tightest upper limit for the magnetic field around a black hole to date. We use the magnetic field limit to derive an estimate of the mass accretion onto the central black hole. In addition to the polarimetric results, we present an observation of rapid variability in the maser lines, which we explain as weak interstellar scintillation. From the scintillation parameters, we estimate an intrinsic size of the mostly saturated maser features of ~12 microarcseconds. This is consistent with models assuming a thick, clumpy accretion disk.

W. H. T. Vlemmings; H. E. Bignall; P. J. Diamond

2006-10-30T23:59:59.000Z

428

SPIRou: the near-infrared spectropolarimeter/high-precision velocimeter for the Canada-France-Hawaii telescope  

E-Print Network [OSTI]

SPIRou is a near-IR \\'echelle spectropolarimeter and high-precision velocimeter under construction as a next-generation instrument for the Canada-France-Hawaii-Telescope. It is designed to cover a very wide simultaneous near-IR spectral range (0.98-2.35 {\\mu}m) at a resolving power of 73.5K, providing unpolarized and polarized spectra of low-mass stars at a radial velocity (RV) precision of 1m/s. The main science goals of SPIRou are the detection of habitable super-Earths around low-mass stars and the study of how critically magnetic fields impact star / planet formation. Following a successful final design review in Spring 2014, SPIRou is now under construction and is scheduled to see first light in late 2017. We present an overview of key aspects of SPIRou's optical and mechanical design.

Artigau, tienne; Donati, Jean-Franois; Doyon, Ren; Delfosse, Xavier; Baratchart, Sbastien; Lacombe, Marielle; Moutou, Claire; Rabou, Patrick; Pars, Laurent P; Micheau, Yoan; Thibault, Simon; Reshetov, Vladimir A; Dubois, Bruno; Hernandez, Olivier; Valle, Philippe; Wang, Shiang-Yu; Dolon, Franois; Pepe, Francesco A; Bouchy, Franois; Striebig, Nicolas; Hnault, Franois; Loop, David; Saddlemyer, Leslie; Barrick, Gregory; Vermeulen, Tom; Dupieux, Michel; Hbrard, Guillaume; Boisse, Isabelle; Martioli, Eder; Alencar, Silvia H P; Nascimento, Jos-Diaz do; Figueira, Pedro

2014-01-01T23:59:59.000Z

429

BOOMERANG: A Balloon-borne Millimeter Wave Telescope and Total Power Receiver for Mapping Anisotropy in the Cosmic Microwave Background  

E-Print Network [OSTI]

We describe BOOMERANG; a balloon-borne microwave telescope designed to map the Cosmic Microwave Background (CMB) at a resolution of 10' from the Long Duration Balloon (LDB) platform. The millimeter-wave receiver employs new technology in bolometers, readout electronics, cold re-imaging optics, millimeter-wave filters, and cryogenics to obtain high sensitivity to CMB anisotropy. Sixteen detectors observe in 4 spectral bands centered at 90, 150, 240 and 410 GHz. The wide frequency coverage, the long duration flight, the optical design and the observing strategy provide strong rejection of systematic effects. We report the flight performance of the instrument during a 10.5 day stratospheric balloon flight launched from McMurdo Station, Antarctica that mapped ~2000 square degrees of the sky.

B. P. Crill; P. A. R. Ade; D. R. Artusa; R. S. Bhatia; J. J. Bock; A. Boscaleri; P. Cardoni; S. E. Church; K. Coble; P. deBernardis; G. deTroia; P. Farese; K. M. Ganga; M. Giacometti; C. V. Haynes; E. Hivon; V. V. Hristov; A. Iacoangeli; W. C. Jones; A. E. Lange; L. Martinis; S. Masi; P. V. Mason; P. D. Mauskopf; L. Miglio; T. Montroy; C. B. Netterfield; C. G. Paine; E. Pascale; F. Piacentini; G. Polenta; F. Pongetti; G. Romeo; J. E. Ruhl; F. Scaramuzzi; D. Sforna; A. D. Turner

2002-06-14T23:59:59.000Z

430

The Spectrum of the Isotropic Diffuse Gamma-Ray Emission Derived From First-Year Fermi Large Area Telescope Data  

SciTech Connect (OSTI)

We report on the first Fermi Large Area Telescope (LAT) measurements of the so-called 'extra-galactic' diffuse {gamma}-ray emission (EGB). This component of the diffuse {gamma}-ray emission is generally considered to have an isotropic or nearly isotropic distribution on the sky with diverse contributions discussed in the literature. The derivation of the EGB is based on detailed modelling of the bright foreground diffuse Galactic {gamma}-ray emission (DGE), the detected LAT sources and the solar {gamma}-ray emission. We find the spectrum of the EGB is consistent with a power law with differential spectral index {gamma} = 2.41 {+-} 0.05 and intensity, I(> 100 MeV) = (1.03 {+-} 0.17) x 10{sup -5} cm{sup -2} s{sup -1} sr{sup -1}, where the error is systematics dominated. Our EGB spectrum is featureless, less intense, and softer than that derived from EGRET data.

Abdo, A. A.

2011-08-19T23:59:59.000Z

431

A limit on the ultra-high-energy neutrino flux from lunar observations with the Parkes radio telescope  

E-Print Network [OSTI]

We report a limit on the ultra-high-energy neutrino flux based on a non-detection of radio pulses from neutrino-initiated particle cascades in the Moon, in observations with the Parkes radio telescope undertaken as part of the LUNASKA project. Due to the improved sensitivity of these observations, which had an effective duration of 127 hours and a frequency range of 1.2-1.5 GHz, this limit extends to lower neutrino energies than those from previous lunar radio experiments, with a detection threshold below 10^20 eV. The calculation of our limit allows for the possibility of lunar-origin pulses being misidentified as local radio interference, and includes the effect of small-scale lunar surface roughness. The targeting strategy of the observations also allows us to place a directional limit on the neutrino flux from the nearby radio galaxy Centaurus A.

Bray, J D; Roberts, P; Reynolds, J E; James, C W; Phillips, C J; Protheroe, R J; McFadden, R A; Aartsen, M G

2015-01-01T23:59:59.000Z

432

A Simple Guide to Backyard Astronomy Using Binoculars or a Small Telescope www.carolrpt.com/astroguide.htm P.1 A Simple Guide to Backyard AstronomyA Simple Guide to Backyard Astronomy  

E-Print Network [OSTI]

A Simple Guide to Backyard Astronomy Using Binoculars or a Small Telescope www.carolrpt.com/astroguide.htm P.1 A Simple Guide to Backyard AstronomyA Simple Guide to Backyard Astronomy Using BinocularsCharts BooksBooks GizmosGizmos Binoculars for AstronomyBinoculars for Astronomy Telescopes for Backyard

Kiss, Emil

433

Development of Volume Phase Holographic (VPH) Grism for Visible to Near Infrared Instruments of the 8.2m Subaru Telescope  

E-Print Network [OSTI]

@riken.go.jp; http://atlas.riken.go.jp/~ebizuka/ebi-e.html; http://atlas.riken.go.jp/~ebizuka/ebi.html (Japanese (FOCAS) is one of its seven common-use facility instruments of the 8.2m Subaru Telescope on Mauna Kea

Iye, Masanori

434

New challenges for adaptive optics: the OWL 100m telescope N. Hubin, M. Le Louarn, M. Sarazin, A. Tokovinin, E. Viard  

E-Print Network [OSTI]

. Tokovinin, E. Viard European Southern Observatory Karl Schwarzschild str., 2 D-85748 Garching bei M deformable mirrors it is realistic to obtain a FOV diameter of 30 00 {60 00 in the visible, or 3 0 {6 0 mirror of current ground based optical telescopes is between 8 and 10 m. Proposals have arisen

Liske, Jochen

435

DETECTION OF E-CYANOMETHANIMINE TOWARD SAGITTARIUS B2(N) IN THE GREEN BANK TELESCOPE PRIMOS SURVEY  

SciTech Connect (OSTI)

The detection of E-cyanomethanimine (E-HNCHCN) toward Sagittarius B2(N) is made by comparing the publicly available Green Bank Telescope (GBT) PRIMOS survey spectra to laboratory rotational spectra from a reaction product screening experiment. The experiment uses broadband molecular rotational spectroscopy to monitor the reaction products produced in an electric discharge source using a gas mixture of NH{sub 3} and CH{sub 3}CN. Several transition frequency coincidences between the reaction product screening spectra and previously unassigned interstellar rotational transitions in the PRIMOS survey have been assigned to E-cyanomethanimine. A total of eight molecular rotational transitions of this molecule between 9 and 50 GHz are observed with the GBT. E-cyanomethanimine, often called the HCN dimer, is an important molecule in prebiotic chemistry because it is a chemical intermediate in proposed synthetic routes of adenine, one of the two purine nucleobases found in DNA and RNA. New analyses of the rotational spectra of both E-cyanomethanimine and Z-cyanomethanimine that incorporate previous millimeter-wave measurements are also reported.

Zaleski, Daniel P.; Seifert, Nathan A.; Steber, Amanda L.; Muckle, Matt T.; Loomis, Ryan A.; Vasquez, David; Nyiramahirwe, Jolie; Sciortino, Nicole; Johnson, Kennedy; Pate, Brooks H. [Department of Chemistry, University of Virginia, McCormick Road, Charlottesville, VA 22904 (United States); Corby, Joanna F. [Department of Astronomy, University of Virginia, McCormick Road, Charlottesville, VA 22904 (United States); Martinez, Oscar Jr.; Crabtree, Kyle N.; McCarthy, Michael C. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Jewell, Philip R.; Remijan, Anthony J. [National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903-2475 (United States); Hollis, Jan M. [NASA Goddard Space Flight Center, Greenbelt, MD 20771 (United States); Lovas, Frank J., E-mail: bp2k@virginia.edu, E-mail: mccarthy@cfa.harvard.edu, E-mail: aremijan@nrao.edu [National Institute of Standards and Technology, Gaithersburg, MD 20899 (United States)

2013-03-01T23:59:59.000Z

436

Discovery of 15-second oscillations in Hubble Space Telescope observations of WZ Sagittae following the 2001 outburst  

E-Print Network [OSTI]

We report the discovery of 15-s oscillations in ultraviolet observations of WZ Sge obtained with the Hubble Space Telescope approximately one month after the peak of the 2001 outburst. This is the earliest detection of oscillations in WZ Sge following an outburst and the first time that a signal near 15 s has been seen to be dominant. The oscillations are quite strong (amplitude about 5%), but not particularly coherent. In one instance, the oscillation period changed by 0.7 s between successive observations separated by less than 1 hour. We have also found evidence for weaker signals with periods near 6.5 s in some of our data. We discuss the implications of our results for the models that have been proposed to account for the 28-s oscillations seen in quiescence. If the periods of the 15-s oscillations can be identified with the periods of revolution of material rotating about the white dwarf, the mass of the white dwarf must satisfy M_WD > 0.71 M_sun. The corresponding limit for the 6.5-s signals is M_WD > 1.03 M_sun.

C. Knigge; R. I. Hynes; D. Steeghs; K. S. Long; S. Araujo-Betancor; T. R. Marsh

2002-10-17T23:59:59.000Z

437

Galaxy Clusters in the Swift/Burst Alert Telescope Era: Hard X-rays in the Intracluster Medium  

Science Journals Connector (OSTI)

We report the detection of 10 clusters of galaxies in the ongoing Swift/Burst Alert Telescope (BAT) all-sky survey. This sample, which mostly comprises merging clusters, was serendipitously detected in the 15-55 keV band. We use the BAT sample to investigate the presence of excess hard X-rays above the thermal emission. The BAT clusters do not show significant (e.g., ?2?) nonthermal hard X-ray emission. The only exception is represented by Perseus whose high-energy emission is likely due to NGC 1275. Using XMM-Newton, Swift/XRT, Chandra and BAT data, we are able to produce upper limits of the inverse Compton (IC) emission mechanism which are in disagreement with most of the previously-claimed hard X-ray excesses. The coupling of the X-ray upper limits of the IC mechanism to radio data shows that, in some clusters, the magnetic field might be larger than 0.5 ?G. We also derive the first log N-log S and luminosity function distributions of galaxy clusters above 15 keV.

M. Ajello; P. Rebusco; N. Cappelluti; O. Reimer; H. Bhringer; J. Greiner; N. Gehrels; J. Tueller; A. Moretti

2009-01-01T23:59:59.000Z

438

Mirrors for X-ray telescopes: Fresnel diffraction-based computation of Point Spread Functions from metrology  

E-Print Network [OSTI]

The imaging sharpness of an X-ray telescope is chiefly determined by the optical quality of its focusing optics, which in turn mostly depends on the shape accuracy and the surface finishing of the grazing incidence X-ray mirrors that compose the optical modules. In order to ensure the imaging performance during the mirror manufacturing, a fundamental step is represented by the prediction of the mirror Point Spread Function (PSF) from the metrology of its surface. Traditionally, the PSF computation in X-rays is assumed to be different depending on whether the surface defects are classified as figure errors or roughness [...] The aim of this work is to overcome this limit, providing analytical formulae, valid at any light wavelength, to compute the PSF of an X-ray mirror shell from the measured longitudinal profiles and the roughness Power Spectral Density (PSD), without distinguishing spectral ranges with different treatments. The method we adopted is based on the Huygens-Fresnel principle to compute the diffr...

Raimondi, Lorenzo

2014-01-01T23:59:59.000Z

439

Constraints on Lorentz invariance violation from Fermi-Large Area Telescope observations of gamma-ray bursts  

Science Journals Connector (OSTI)

We analyze the MeV/GeV emission from four bright gamma-ray bursts (GRBs) observed by the Fermi Large Area Telescope to produce robust, stringent constraints on a dependence of the speed of light invacuo on the photon energy (vacuum dispersion), a form of Lorentz invariance violation (LIV) allowed by some quantum gravity (QG) theories. First, we use three different and complementary techniques to constrain the total degree of dispersion observed in the data. Additionally, using a maximally conservative set of assumptions on possible source-intrinsic, spectral-evolution effects, we constrain any vacuum dispersion solely attributed to LIV. We then derive limits on the QG energy scale (the energy scale where LIV-inducing QG effects become strong, EQG) and the coefficients of the Standard Model Extension. For the subluminal case (where high-energy photons propagate more slowly than lower-energy photons) and without taking into account any source-intrinsic dispersion, our most stringent limits (at 95%C.L.) are obtained from GRB 090510 and are EQG,1>7.6 times the Planck energy (EPl) and EQG,2>1.31011??GeV for linear and quadratic leading-order LIV-induced vacuum dispersion, respectively. These limits improve the latest constraints by Fermi and H.E.S.S. by a factor of ?2. Our results disfavor any class of models requiring EQG,1?EPl.

V. Vasileiou; A. Jacholkowska; F. Piron; J. Bolmont; C. Couturier; J. Granot; F. W. Stecker; J. Cohen-Tanugi; F. Longo

2013-06-04T23:59:59.000Z

440

HUBBLE SPACE TELESCOPE AND OPTICAL DATA ON SDSSJ0804+5103 (EZ Lyn) ONE YEAR AFTER OUTBURST  

SciTech Connect (OSTI)

We present an ultraviolet (UV) spectrum and light curve of the short orbital period cataclysmic variable EZ Lyn obtained with the Cosmic Origins Spectrograph on the Hubble Space Telescope 14 months after its dwarf nova outburst, along with ground-based optical photometry. The UV spectrum can be fit with a 13,100 K, log g = 8 white dwarf using 0.5 solar composition, while fits to the individual lines are consistent with solar abundance for Si and Al, but only 0.3 solar for C. The Discrete Fourier Transforms of the UV and optical light curves at 14 months following outburst show a prominent period at 256 s. This is the same period reported by Pavlenko in optical data obtained seven months and one year after outburst, indicating its long-term stability over several months, but this period is not evident in the pre-outburst data and is much shorter than the 12.6 minute period that was seen in observations obtained during an interval from 8 months to 2.5 yr after the 2006 outburst. In some respects, the long and short periods are similar to the behavior seen in GW Lib after its outburst but the detailed explanation for the appearance and disappearance of these periods and their relation to non-radial pulsation modes remain to be explored with theoretical models.

Szkody, Paula; Mukadam, Anjum S. [Department of Astronomy, University of Washington, Seattle, WA 98195 (United States); Sion, Edward M. [Department of Astronomy and Astrophysics, Villanova University, Villanova, PA 19085 (United States); Gaensicke, Boris T. [Department of Physics, University of Warwick, Coventry CV4 7AL (United Kingdom); Henden, Arne [AAVSO, 49 Bay State Road, Cambridge, MA 02138 (United States); Townsley, Dean, E-mail: szkody@astro.washington.edu, E-mail: mukadam@astro.washington.edu, E-mail: edward.sion@villanova.edu, E-mail: boris.gaensicke@warwick.ac.uk, E-mail: arne@aavso.org, E-mail: Dean.M.Townsley@ua.edu [Department of Physics and Astronomy, University of Alabama, Tuscaloosa, AL 35487 (United States)

2013-05-15T23:59:59.000Z

Note: This page contains sample records for the topic "telescope baltay charles" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
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441

Constraining Dark Matter Models from a Combined Analysis of Milky Way Satellites with the Fermi Large Area Telescope  

SciTech Connect (OSTI)

Satellite galaxies of the Milky Way are among the most promising targets for dark matter searches in gamma rays. We present a search for dark matter consisting of weakly interacting massive particles, applying a joint likelihood analysis to 10 satellite galaxies with 24 months of data of the Fermi Large Area Telescope. No dark matter signal is detected. Including the uncertainty in the dark matter distribution, robust upper limits are placed on dark matter annihilation cross sections. The 95% confidence level upper limits range from about 10{sup -26} cm{sup 3} s{sup -1} at 5 GeV to about 5 x 10{sup -23} cm{sup 3} s{sup -1} at 1 TeV, depending on the dark matter annihilation final state. For the first time, using gamma rays, we are able to rule out models with the most generic cross section ({approx}3 x 10{sup -26} cm{sup 3} s{sup -1} for a purely s-wave cross section), without assuming additional boost factors.

Ackermann, M.; Ajello, M.; /Stanford U., HEPL /Taiwan, Natl. Taiwan U. /SLAC; Albert, A.; /Taiwan, Natl. Taiwan U. /Ohio State U.; Atwood, W.B.; /UC, Santa Cruz; Baldini, L.; /INFN, Pisa; Ballet, J.; /DAPNIA, Saclay; Barbiellini, G.; /INFN, Trieste /Trieste U.; Bastieri, D.; /INFN, Padua /Padua U.; Bechtol, K.; /Stanford U., HEPL /Taiwan, Natl. Taiwan U. /SLAC; Bellazzini, R.; /INFN, Pisa; Berenji, B.; Blandford, R.D.; Bloom, E.D.; /Stanford U., HEPL /Taiwan, Natl. Taiwan U. /SLAC; Bonamente, E.; /INFN, Perugia /Perugia U.; Borgland, A.W.; /Stanford U., HEPL /Taiwan, Natl. Taiwan U. /SLAC; Bregeon, J.; /INFN, Pisa; Brigida, M.; /Bari Polytechnic /INFN, Bari; Bruel, P.; /Ecole Polytechnique; Buehler, R.; /Stanford U., HEPL /Taiwan, Natl. Taiwan U. /SLAC; Burnett, T.H.; /Washington U., Seattle; Buson, S.; /INFN, Padua /Padua U. /ICE, Bellaterra /Stanford U., HEPL /Taiwan, Natl. Taiwan U. /SLAC /INFN, Rome /Rome U. /IASF, Milan /IASF, Milan /DAPNIA, Saclay /INFN, Perugia /Perugia U. /Stanford U., HEPL /Taiwan, Natl. Taiwan U. /SLAC /Artep Inc. /Stanford U., HEPL /Taiwan, Natl. Taiwan U. /SLAC /ASDC, Frascati /Perugia U. /Stanford U., HEPL /Taiwan, Natl. Taiwan U. /SLAC /Montpellier U. /Stockholm U. /Stockholm U., OKC /ASDC, Frascati /ASDC, Frascati /Udine U. /INFN, Trieste /Bari Polytechnic /INFN, Bari /Naval Research Lab, Wash., D.C. /Stanford U., HEPL /Taiwan, Natl. Taiwan U. /SLAC /Montpellier U. /Bari Polytechnic /INFN, Bari /Ecole Polytechnique /NASA, Goddard /Hiroshima U. /Stanford U., HEPL /Taiwan, Natl. Taiwan U. /SLAC /Bari Polytechnic /INFN, Bari /INFN, Bari /ASDC, Frascati /NASA, Goddard /INFN, Perugia /Perugia U. /Bari Polytechnic /INFN, Bari /Bologna Observ. /Stanford U., HEPL /Taiwan, Natl. Taiwan U. /SLAC /DAPNIA, Saclay /Alabama U., Huntsville; /more authors..

2012-09-14T23:59:59.000Z

442

A Detailed Study of FDIRC Prototype with Waveform Digitizing Electronics in Cosmic Ray Telescope Using 3D Tracks  

SciTech Connect (OSTI)

We present a detailed study of a novel Cherenkov imaging detector called the Focusing DIRC (FDIRC) with waveform digitizing electronics. In this test study, the FDIRC prototype has been instrumented with seven Hamamatsu H-8500 MaPMTs. Waveforms from {approx}450 pixels are digitized with waveform sampling electronics based on the BLAB2 ASIC, operating at a sampling speed of {approx}2.5 GSa/s. The FDIRC prototype was tested in a large cosmic ray telescope (CRT) providing 3D muon tracks with {approx}1.5 mrad angular resolution and muon energy of E{sub muon} > 1.6 GeV. In this study we provide a detailed analysis of the tails in the Cherenkov angle distribution as a function of various variables, compare experimental results with simulation, and identify the major contributions to the tails. We demonstrate that to see the full impact of these tails on the Cherenkov angle resolution, it is crucial to use 3D tracks, and have a full understanding of the role of ambiguities. These issues could not be fully explored in previous FDIRC studies where the beam was perpendicular to the quartz radiator bars. This work is relevant for the final FDIRC prototype of the PID detector at SuperB, which will be tested this year in the CRT setup.

Nishimura, K.; Dey, B.; /Hawaii U. /UC, Riverside; Aston, D.; Leith, D.W.G.S.; Ratcliff, B.; /SLAC; Roberts, D.; /Maryland U.; Ruckman, L.; /Hawaii U.; Shtol, D.; /Novosibirsk, IYF; Varner, G.S.; /Hawaii U.; Va'vra, J.; Vavra, Jerry; /SLAC; ,

2012-07-30T23:59:59.000Z

443

OBSERVATIONS OF BINARY STARS WITH THE DIFFERENTIAL SPECKLE SURVEY INSTRUMENT. IV. OBSERVATIONS OF KEPLER, CoRoT, AND HIPPARCOS STARS FROM THE GEMINI NORTH TELESCOPE  

SciTech Connect (OSTI)

We present the results of 71 speckle observations of binary and unresolved stars, most of which were observed with the DSSI speckle camera at the Gemini North Telescope in 2012 July. The main purpose of the run was to obtain diffraction-limited images of high-priority targets for the Kepler and CoRoT missions, but in addition, we observed a number of close binary stars where the resolution limit of Gemini was used to better determine orbital parameters and/or confirm results obtained at or below the diffraction limit of smaller telescopes. Five new binaries and one triple system were discovered, and first orbits are calculated for other two systems. Several systems are discussed in detail.

Horch, Elliott P. [Department of Physics, Southern Connecticut State University, 501 Crescent Street, New Haven, CT 06515 (United States); Howell, Steve B. [NASA Ames Research Center, Moffett Field, CA 94035 (United States); Everett, Mark E. [National Optical Astronomy Observatory, 950 N. Cherry Ave, Tucson, AZ 85719 (United States); Ciardi, David R., E-mail: horche2@southernct.edu, E-mail: steve.b.howell@nasa.gov, E-mail: everett@noao.edu, E-mail: ciardi@ipac.caltech.edu [NASA Exoplanet Science Institute, California Institute of Technology, 770 South Wilson Avenue, Mail Code 100-22, Pasadena, CA 91125 (United States)

2012-12-01T23:59:59.000Z

444

THE GREEN BANK TELESCOPE 350 MHz DRIFT-SCAN SURVEY. I. SURVEY OBSERVATIONS AND THE DISCOVERY OF 13 PULSARS  

SciTech Connect (OSTI)

Over the summer of 2007, we obtained 1191 hr of 'drift-scan' pulsar search observations with the Green Bank Telescope at a radio frequency of 350 MHz. Here we describe the survey setup, search procedure, and the discovery and follow-up timing of 13 pulsars. Among the new discoveries, one (PSR J1623-0841) was discovered only through its single pulses, two (PSRs J1327-0755 and J1737-0814) are millisecond pulsars, and another (PSR J2222-0137) is a mildly recycled pulsar. PSR J1327-0755 is a 2.7 ms pulsar at a dispersion measure (DM) of 27.9 pc cm{sup -3} in an 8.7 day orbit with a minimum companion mass of 0.22 M {sub Sun }. PSR J1737-0814 is a 4.2 ms pulsar at a DM of 55.3 pc cm{sup -3} in a 79.3 day orbit with a minimum companion mass of 0.06 M {sub Sun }. PSR J2222-0137 is a 32.8 ms pulsar at a very low DM of 3.27 pc cm{sup -3} in a 2.4 day orbit with a minimum companion mass of 1.11 M {sub Sun }. It is most likely a white-dwarf-neutron-star system or an unusual low-eccentricity double neutron star system. Ten other pulsars discovered in this survey are reported in the companion paper Lynch et al.

Boyles, J.; Lorimer, D. R.; McLaughlin, M. A.; Cardoso, R. F. [Department of Physics, West Virginia University, Morgantown, WV 26506 (United States)] [Department of Physics, West Virginia University, Morgantown, WV 26506 (United States); Lynch, R. S.; Kaspi, V. M.; Archibald, A.; Karako-Argaman, C. [Department of Physics, McGill University, 3600 University St., Montreal, Quebec, H3A 2T8 (Canada)] [Department of Physics, McGill University, 3600 University St., Montreal, Quebec, H3A 2T8 (Canada); Ransom, S. M. [National Radio Astronomy Observatory (NRAO), 520 Edgemont Road, Charlottesville, VA 22901 (United States)] [National Radio Astronomy Observatory (NRAO), 520 Edgemont Road, Charlottesville, VA 22901 (United States); Stairs, I. H.; Berndsen, A.; Cherry, A.; McPhee, C. A. [Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, British Columbia V6T 1Z1 (Canada)] [Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, British Columbia V6T 1Z1 (Canada); Hessels, J. W. T.; Kondratiev, V. I.; Van Leeuwen, J. [ASTRON, The Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA, Dwingeloo (Netherlands)] [ASTRON, The Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA, Dwingeloo (Netherlands); Epstein, C. R. [Department of Astronomy, Ohio State University, 140 W. 18th Avenue, Columbus, OH 43210 (United States)] [Department of Astronomy, Ohio State University, 140 W. 18th Avenue, Columbus, OH 43210 (United States); Pennucci, T. [Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325 (United States)] [Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325 (United States); Roberts, M. S. E. [Eureka Scientific, 2452 Delmer Street, Suite 100, Oakland, CA 94602-3017 (United States)] [Eureka Scientific, 2452 Delmer Street, Suite 100, Oakland, CA 94602-3017 (United States); Stovall, K., E-mail: jason.boyles@wku.edu [Center for Advanced Radio Astronomy and Department of Physics and Astronomy, University of Texas at Brownsville, Brownsville, TX 78520 (United States)

2013-02-15T23:59:59.000Z

445

THE SPACE DENSITY EVOLUTION OF WET AND DRY MERGERS IN THE CANADA-FRANCE-HAWAII TELESCOPE LEGACY SURVEY  

SciTech Connect (OSTI)

We analyze 1298 merging galaxies with redshifts up to z = 0.7 from the Canada-France-Hawaii Telescope Legacy Survey, taken from the catalog presented in the work of Bridge et al. By analyzing the internal colors of these systems, we show that the so-called wet and dry mergers evolve in different senses, and quantify the space densities of these systems. The local space density of wet mergers is essentially identical to the local space density of dry mergers. The evolution in the total merger rate is modest out to z {approx} 0.7, although the wet and dry populations have different evolutionary trends. At higher redshifts, dry mergers make a smaller contribution to the total merging galaxy population, but this is offset by a roughly equivalent increase in the contribution from wet mergers. By comparing the mass density function of early-type galaxies to the corresponding mass density function for merging systems, we show that not all the major mergers with the highest masses (M{sub stellar}>10{sup 11} M{sub sun}) will end up with the most massive early-type galaxies, unless the merging timescale is dramatically longer than that usually assumed. On the other hand, the usually assumed merging timescale of {approx}0.5-1 Gyr is quite consistent with the data if we suppose that only less massive early-type galaxies form via mergers. Since low-intermediate-mass ellipticals are 10-100 times more common than their most massive counterparts, the hierarchical explanation for the origin of early-type galaxies may be correct for the vast majority of early types, even if incorrect for the most massive ones.

Chou, Richard C. Y.; Abraham, Roberto G. [Department of Astronomy and Astrophysics, University of Toronto, 50 St. George Street, Toronto, ON M5S 3H4 (Canada); Bridge, Carrie R., E-mail: chou@astro.utoronto.ca, E-mail: abraham@astro.utoronto.ca, E-mail: bridge@astro.caltech.edu [California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125 (United States)

2011-03-15T23:59:59.000Z

446

TURBULENT CHARACTERISTICS IN THE INTENSITY FLUCTUATIONS OF A SOLAR QUIESCENT PROMINENCE OBSERVED BY THE HINODE SOLAR OPTICAL TELESCOPE  

SciTech Connect (OSTI)

We focus on Hinode Solar Optical Telescope (SOT) calcium II H-line observations of a solar quiescent prominence (QP) that exhibits highly variable dynamics suggestive of turbulence. These images capture a sufficient range of scales spatially ({approx}0.1-100 arcsec) and temporally ({approx}16.8 s-4.5 hr) to allow the application of statistical methods used to quantify finite range fluid turbulence. We present the first such application of these techniques to the spatial intensity field of a long-lived solar prominence. Fully evolved inertial range turbulence in an infinite medium exhibits multifractal scale invariance in the statistics of its fluctuations, seen as power-law power spectra and as scaling of the higher order moments (structure functions) of fluctuations which have non-Gaussian statistics; fluctuations {delta}I(r, L) = I(r + L) - I(r) on length scale L along a given direction in observed spatial field I have moments that scale as ({delta}I(r, L){sup p}) {approx} L{sup {zeta}(p)}. For turbulence in a system that is of finite size, or that is not fully developed, one anticipates a generalized scale invariance or extended self-similarity (ESS) ({delta}I(r, L){sup p}) {approx} G(L){sup {zeta}(p)}. For these QP intensity measurements we find scaling in the power spectra and ESS. We find that the fluctuation statistics are non-Gaussian and we use ESS to obtain ratios of the scaling exponents {zeta}(p): these are consistent with a multifractal field and show distinct values for directions longitudinal and transverse to the bulk (driving) flow. Thus, the intensity fluctuations of the QP exhibit statistical properties consistent with an underlying turbulent flow.

Leonardis, E.; Chapman, S. C.; Foullon, C. [Centre for Fusion Space and Astrophysics, Department of Physics, University of Warwick, Coventry, CV4 7AL (United Kingdom)

2012-02-01T23:59:59.000Z

447

Cosmic Ray Telescopes  

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

Cosmic Ray Muon Detectors Cosmic Ray Muon Detectors Particle Physics Using Nature's Accelerator Somewhere out there is a list of "10 Things a Physics Teacher is Least Likely to Say." If one were to find this list, it would have on it such gems as #7. Let's challenge the PE Dept to a game of rugby and #4. I don't care if you understand the concept, just give me the correct answer to 12 sig figs. Finally, you'd get down to the biggie, the thing physics teachers never say: #1. Let's do a particle physics lab right here at Podunk Corners High! The traditional reasons for this are that everyone knows that particle physics is only done with Vastly Expensive and Complicated Equipment run by casts of thousands of Highly Qualified Scientists and that particle physics is Difficult and Arcane.

448

Diamond Pixel Luminosity Telescopes  

SciTech Connect (OSTI)

In this document, Halyo summaries her key contributions to CMS at the LHC and provide an explanation of their importance and her role in each project. At the end Halyo describes her recent research interest that includes GPU/MIC Acceleration of the High Level Trigger (HLT) to Extend the Physics Research at the LHC. A descriptionof her work the recent promising results that she accomplished and the deliverable are also elaborated. These contribution were only possible thanks to DOE support of junior faculty research and their clear goal to promote research and innovations. #3;Princeton University i

Halyo, Valerie

2014-12-23T23:59:59.000Z

449

Allen Telescope Array Acknowledgements  

E-Print Network [OSTI]

polarization receivers § Analog RF transmitted by optical fiber to central Bunker § Diverse needs of potential

450

Low Cost Radio Telescope  

Science Journals Connector (OSTI)

A radio interferometer has been constructed at Haverford College as an aid to learning the fundamentals of radio astronomy. Its cost both in cash outlay and in construction time make it a feasible year-long project for an undergraduate. Its simplicity does not prevent it from being a useful instrument for instruction at the college or high-school level; among its capabilities are the measurement of the positions of at least four of the strongest discrete cosmic-noisesources and the diameter of the radio sun.

Joseph H. Taylor Jr.

1964-01-01T23:59:59.000Z

451

Charles Babbage, F.R.S  

Science Journals Connector (OSTI)

... of Babbage compiled by Dr. Buxton's grandfather. Babbage was born in Teignmouth on December 26, 1792, and died in London on October 18, 1871. He was educated privately ...

1933-12-23T23:59:59.000Z

452

Thomas H. Cormen Charles E. Leiserson  

E-Print Network [OSTI]

-0-262-03384-8 (hardcover : alk. paper)--ISBN 978-0-262-53305-8 (pbk. : alk. paper) 1. Computer programming. 2. Computer algorithms. I. Cormen, Thomas H. QA76.6.I5858 2009 005.1--dc22 2009008593 10 9 8 7 6 5 4 3 2 1 #12 implementation in practice. Parallel computers--computers with multiple processing units--have become

Leiserson, Charles E.

453

HISTORY OF HOMOLOGICAL ALGEBRA Charles A. Weibel  

E-Print Network [OSTI]

, including the development of derived categories. Number theory was infused with new results from Galois

Weibel, Charles

454

HISTORY OF HOMOLOGICAL ALGEBRA Charles A. Weibel  

E-Print Network [OSTI]

the development of derived categories. Number theory was infused with new results from Galois cohomology, which

Weibel, Charles

455

Charles A. S. Hall 354 Illick Hall  

E-Print Network [OSTI]

energy in resource exploitation, and how such investments change as the quality of resources changes. I, Argentina and Costa Rica. Most recently my interests have been toward integrative geographical modeling Fellow Fulbright Fellow (Argentina) Guest of honor, National Universities of Argentina Three of my papers

Hall, Charles A.S.

456

Interview of Sir Charles Chadwyck-Healey  

E-Print Network [OSTI]

-colourist and collector of paintings, books, including bibles, and clocks; some of his collecting was magpie-like and sadly he did not always collect the very best, but his book collecting was surer; most of the books were bought by Phillips and ended up in the Phillips... jobs, among others; in those days being a freelance photographer was actually quite easy; the extraordinary thing about photography around 1961-2 was that it wasn't even a craft, it was a trade; apart from the fact that Tony Armstrong-Jones, who married...

Chadwyck-Healey, Charles

2009-01-01T23:59:59.000Z

457

June 7, 2001 To: Charles Baker  

E-Print Network [OSTI]

days of listening to presentations and detail discussions with the Engineering Team of FIRE. While many of devices that could be considered. The team has created concepts for new machines that can explore most. 2. Then FOCUS, in an expeditious manner on one device, either Wedged or Bucked/Wedged (to

458

Imagining Chivalry: Charles V's Suits of Steel  

E-Print Network [OSTI]

Jacob Shrenkh von Notzing, 1603. German edition. Drawings byJacob Shrenkh von Notzing, 1603. German edition. Drawings byJacob Shrenkh von Notzing, 1603. German edition. Drawings by

Machado, Erin Jeannine

2012-01-01T23:59:59.000Z

459

Charles University, Faculty of Mathematics and Physics  

E-Print Network [OSTI]

Laboratory for Sustainable Energy, Technical University of Denmark - DTU Building 228, P.O. Box 49 DK-4000DXRD: new insights and new challenges Wolfgang Pantleon Materials Research Department, Risø National. The sharpness of the peaks in all directions of reciprocal space and their integrated intensity allows

460

Iterative Optimization in Inverse Charles L. Byrne  

E-Print Network [OSTI]

. . . . . . . . . . 34 2.4.3 Proximal Minimization . . . . . . . . . . . . . . . . . 35 2.4.4 The IPA . . . . . . . . . . . . . . . . . . . 52 4.6 The IPA . . . . . . . . . . . . . . . . . . . . .

Byrne, Charles

Note: This page contains sample records for the topic "telescope baltay charles" 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

Charles McVey Oral History  

E-Print Network [OSTI]

everybody knew everyone and they were likeit was really out of place for them. And I think even then like I was still kind of like an inside- outsider even amongst that group because they could neverl ike somem y mom was a substitute teacher so... sometimes people in high school would like narc on me to my mom about seeing me at a party and stuff like that, and drinking under age and stuff, so but anyway, yeah, the party was not a big success. We left real soon. AL BIN : So did youyou were...

McVey, Charles; Albin, Tami

2009-12-17T23:59:59.000Z

462

Sir Charles Parsons and Marine Propulsion  

Science Journals Connector (OSTI)

... it was not until the compound condensing turbine had shown its superiority over the best reciprocating ...engine that any steps were taken to apply it to ships. The speed at which ...

1938-12-10T23:59:59.000Z

463

Sir Charles Parsons and the Steam Turbine  

Science Journals Connector (OSTI)

... followed by some reminiscences of great interest. He touched upon his boyish attempts to construct models of such materials as were available-a far better thing for a boy than playing ... the turbo-alternator set supplied to Cambridge in 1892 showed an economy superior to the reciprocating ...

1926-11-06T23:59:59.000Z

464

Charles W. Davidson! College of Engineering!  

E-Print Network [OSTI]

-assisted hydrothermal synthesis of single-crystal TiO2-nanorod thin films. ! ­ Hydrothermal synthesis: cheaper process in autoclave bomb Characterize nanorod thin film with SEM Prepare hydrothermal solution Flow chart of the TiO2 nanorod thin film fabrication process. Parr 23mL Teflon lined stainless steel autoclave bomb. www

Su, Xiao

465

Charles Kerans Professional Summary January, 2011  

E-Print Network [OSTI]

, and the Persian Gulf. C. Research Scientist, Bureau of Economic Geology, The University of Texas at Austin (August, and Pennsylvanian carbonates, Permian Basin, West Texas, New Mexico, South Texas, and the Persian Gulf. D. Research Basin, West Texas, New Mexico, South Texas, and the Persian Gulf. E. Postdoctoral Senior Research Fellow

Yang, Zong-Liang

466

Information Gathering Session Gillian Charles & Ken Dragoon  

E-Print Network [OSTI]

and associated technologies. ­ Hydropower upgrades, new hydropower projects 3 Purpose Develop a hydro supply curve to determine the hydropower development potential in the NW region ­ Council's Seventh Power Plan-effectiveness Quantity-MWh Price - $/MWh 4 #12;3/27/2012 3 Hydro Assessment: 1980's National Hydropower Survey Hydro Site

467

By Charles Fitzhugh Talmn, Authority on Meteorology.  

E-Print Network [OSTI]

a t Bellefonte, Pa., and Hadley Field, N.Y. , the visibility was decreasing and clouds showed a tendency t o at Bellefonte i n case Hadley Field were foggy. impracticable. Reaching Bellefonte, the p i l o t found the f i e l d foggy and the landing Hadley Field was s t i l l clear. Vhen half way from Bellefonte

468

Charles E. Stillwell Nancy E. Kohler  

E-Print Network [OSTI]

BW are 1,43 for pups, and 0.86 for juveniles and adults. Annual food consumption is estimated to be 5, to define dietary differences and energy needs of pups, juveniles, and adults, and to estimate their daily at several coastal ports from Rhode Island to southern New Jersey, (2) on cruises using 138 #12;Stillwell

469

100 Times Faster and 3 Times Sharper: Background-Dominated Observations of Stellar Populations with an 8-meter Optical-UV Space Telescope  

E-Print Network [OSTI]

An 8 m successor to the Hubble Space Telescope (HST) would make incredible gains in the study of stellar populations, especially in the Local Group. If diffraction-limited at 0.5 microns, the "Next HST" could produce high-resolution imaging of faint sources over a wide field in 1 percent of the time needed with the HST. With these capabilities, photometry of the ancient main sequence could be obtained for many sight-lines through Local Group galaxies, thus determining directly the ages of their structures and providing a formation history for the Local Group populations.

Thomas M. Brown

2002-07-10T23:59:59.000Z

470

The Knee of the Cosmic Hydrogen and Helium Spectrum below 1 PeV Measured by ARGO-YBJ and a Cherenkov Telescope of LHAASO  

E-Print Network [OSTI]

The measurement of cosmic ray energy spectra, in particular for individual species, is an essential approach in finding their origin. Locating the "knees" of the spectra is an important part of the approach and has yet to be achieved. Here we report a measurement of the mixed Hydrogen and Helium spectrum using the combination of the ARGO-YBJ experiment and of a prototype Cherenkov telescope for the LHAASO experiment. A knee feature at 640+/-87 TeV, with a clear steepening of the spectrum, is observed. This gives fundamental inputs to galactic cosmic ray acceleration models.

Bartoli, B; Bi, X J; Branchini, P; Budano, A; Camarri, P; Cao, Z; Cardarelli, R; Catalanotti, S; Chen, S Z; Chen, T L; Creti, P; Cui, S W; Dai, B Z; D'Amone, A; Danzengluobu,; De Mitri, I; Piazzoli, B D'Ettorre; Di Girolamo, T; Di Sciascio, G; Feng, C F; Feng, Zhaoyang; Feng, Zhenyong; Gou, Q B; Guo, Y Q; He, H H; Hu, Haibing; Hu, Hongbo; Iacovacci, M; Iuppa, R; Jia, H Y; Labaciren,; Li, H J; Liguori, G; Liu, C; Liu, J; Liu, M Y; Lu, H; Ma, L L; Ma, X H; Mancarella, G; Mari, S M; Marsella, G; Martello, D; Mastroianni, S; Montini, P; Ning, C C; Panareo, M; Perrone, L; Pistilli, P; Ruggieri, F; Salvini, P; Santonico, R; Shen, P R; Sheng, X D; Shi, F; Surdo, A; Tan, Y H; Vallania, P; Vernetto, S; Vigorito, C; Wang, H; Wu, C Y; Wu, H R; Xue, L; Yang, Q Y; Yang, X C; Yao, Z G; Yuan, A F; Zha, M; Zhang, H M; Zhang, L; Zhang, X Y; Zhang, Y; Zhao, J; Zhaxiciren,; Zhaxisangzhu,; Zhou, X X; Zhu, F R; Zhu, Q Q; Zizzi, G; Bai, Y X; Chen, M J; Chen, Y; Feng, S H; Gao, B; Gu, M H; Hou, C; Li, X X; Liu, J L; Wang, X; Xiao, G; Zhang, B K; Zhang, S S; Zhou, B; Zuo, X

2015-01-01T23:59:59.000Z

471

Upper limit on the cross section for elastic neutralino-nucleon scattering in a neutrino experiment at the Baksan Underground Scintillator Telescope  

SciTech Connect (OSTI)

The results of a neutrino experiment that involved 24.12 yr of live time of observation of muons from the lower Earth's hemisphere with the aid of the Baksan Underground Scintillator Telescope are presented. In the problem of searches for a signal from the annihilation of dark matter in the Sun, an upper limit on the cross section for the elastic scattering of a weakly interacting massive particle (WIMP) on a nucleon was obtained at a 90% confidence level from an analysis of data accumulated within 21.15 yr of live time of observation. A neutralino in a nonminimal supersymmetric theory was considered for a WIMP. The best limit at the Baksan Underground Scintillator Telescope on the cross section for spin-dependent neutralino interactionwith a proton corresponds to 3 Multiplication-Sign 10{sup -4} pb for the neutralino mass of 210 GeV/c{sup 2}. This limit is three orders of magnitude more stringent than similar limits obtained in experiments that detected directly WIMP scattering on target nuclei.

Suvorova, O. V., E-mail: suvorova@cpc.inr.ac.ru; Boliev, M. M., E-mail: boliev2005@yandex.ru; Demidov, S. V., E-mail: demidov@inr.ac.ru; Mikheyev, S. P. [Russian Academy of Sciences, Institute for Nuclear Research (Russian Federation)] [Russian Academy of Sciences, Institute for Nuclear Research (Russian Federation)

2013-11-15T23:59:59.000Z

472

An Unprecedented Constraint on Water Content in the Sunlit Lunar Exosphere Seen by Lunar-Based Ultraviolet Telescope of Chang'e-3 Mission  

E-Print Network [OSTI]

The content of $\\mathrm{OH/H_2O}$ molecules in the tenuous exosphere of the Moon is still an open issue at present. We here report an unprecedented upper limit of the content of the OH radicals, which is obtained from the in-situ measurements carried out \\rm by the Lunar-based Ultraviolet Telescope, a payload of Chinese Chang'e-3 mission. By analyzing the diffuse background in the images taken by the telescope, the column density and surface concentration of the OH radicals are inferred to be $<10^{11}\\ \\mathrm{cm^{-2}}$ and $<10^{4}\\ \\mathrm{cm^{-3}}$ (by assuming a hydrostatic equilibrium with a scale height of 100km), respectively, by assuming that the recorded background is fully contributed by their resonance fluorescence emission. The resulted concentration is lower than the previously reported value by about two orders of magnitude, and is close to the prediction of the sputtering model. In addition, the same measurements and method allow us to derive a surface concentration of $<10^{2}\\ \\math...

Wang, J; Qiu, Y L; Meng, X M; Cai, H B; Cao, L; Deng, J S; Han, X H; Wei, J Y

2015-01-01T23:59:59.000Z

473

Kepler's Laws of Planetary Motion Charles Byrne (Charles Byrne@uml.edu)  

E-Print Network [OSTI]

strong evidence for Newton's law of universal gravitation. 1 Preliminaries Kepler worked from 1601's law of universal gravitation. How Kepler discovered these laws without the aid of analytic geometry's inverse square law for gravitational attraction. 2 A Little Vector Calculus We consider a body

Byrne, Charles

474

Design Concepts for the Cherenkov Telescope Array CTA: An Advanced Facility for Ground-Based High-Energy Gamma-Ray Astronomy  

SciTech Connect (OSTI)

Ground-based gamma-ray astronomy has had a major breakthrough with the impressive results obtained using systems of imaging atmospheric Cherenkov telescopes. Ground-based gamma-ray astronomy has a huge potential in astrophysics, particle physics and cosmology. CTA is an international initiative to build the next generation instrument, with a factor of 5-10 improvement in sensitivity in the 100 GeV-10 TeV range and the extension to energies well below 100 GeV and above 100 TeV. CTA will consist of two arrays (one in the north, one in the south) for full sky coverage and will be operated as open observatory. The design of CTA is based on currently available technology. This document reports on the status and presents the major design concepts of CTA.

Actis, M

2012-04-17T23:59:59.000Z

475

Search for muon signal from dark matter annihilations in the Sun with the Baksan Underground Scintillator Telescope for 24.12 years  

SciTech Connect (OSTI)

We present a new dataset analysis of the neutrino experiment at the Baksan Underground Scintillator Telescope with muon energy threshold about 1 GeV for the longest exposure time toward the Sun. In search for a signal from self-annihilations of dark matter particles in the center of the Sun we use an updated sample of upward through-going muons for 24.12 years of live time. No observable excess has been found in measured muons relative to expected background from neutrinos of atmospheric origin. We present an improved data analysis procedure and describe it in detail. We set the 90% C.L. new upper limits on expected neutrino and muon fluxes from dark matter annihilations in the Sun, on the corresponding annihilation rates and cross sections of their elastic scattering off proton.

Boliev, M.M. [Institute for Nuclear Research of Russian Academy of Sciences, Baksan Neutrino Observatory, Kabardino-Balkariya 400900 (Russian Federation); Demidov, S.V.; Mikheyev, S.P.; Suvorova, O.V., E-mail: boliev2005@yandex.ru, E-mail: demidov@ms2.inr.ac.ru, E-mail: mikheyev@pcbai10.inr.ruhep.ru, E-mail: suvorova@cpc.inr.ac.ru [Institute for Nuclear Research of Russian Academy of Sciences, prospect 60-th October 7A, Moscow 117312 (Russian Federation)

2013-09-01T23:59:59.000Z

476

GAMMA-RAY LOUDNESS, SYNCHROTRON PEAK FREQUENCY, AND PARSEC-SCALE PROPERTIES OF BLAZARS DETECTED BY THE FERMI LARGE AREA TELESCOPE  

SciTech Connect (OSTI)

The parsec-scale radio properties of 232 active galactic nuclei, most of which are blazars, detected by the Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope have been observed contemporaneously by the Very Long Baseline Array (VLBA) at 5 GHz. Data from both the first 11 months (1FGL) and the first 2 years (2FGL) of the Fermi mission were used to investigate these sources' {gamma}-ray properties. We use the ratio of the {gamma}-ray-to-radio luminosity as a measure of {gamma}-ray loudness. We investigate the relationship of several radio properties to {gamma}-ray loudness and to the synchrotron peak frequency. There is a tentative correlation between {gamma}-ray loudness and synchrotron peak frequency for BL Lac objects in both 1FGL and 2FGL, and for flat-spectrum radio quasars (FSRQs) in 2FGL. We find that the apparent opening angle tentatively correlates with {gamma}-ray loudness for FSRQs, but only when we use the 2FGL data. We also find that the total VLBA flux density correlates with the synchrotron peak frequency for BL Lac objects and FSRQs. The core brightness temperature also correlates with synchrotron peak frequency, but only for the BL Lac objects. The low-synchrotron-peaked (LSP) BL Lac object sample shows indications of contamination by FSRQs which happen to have undetectable emission lines. There is evidence that the LSP BL Lac objects are more strongly beamed than the rest of the BL Lac object population.

Linford, J. D.; Taylor, G. B.; Schinzel, F. K., E-mail: jlinford@unm.edu [Department of Physics and Astronomy, University of New Mexico, MSC07 4220, Albuquerque, NM 87131-0001 (United States)

2012-09-20T23:59:59.000Z

477

NEAR-INFRARED IMAGING OF A z = 6.42 QUASAR HOST GALAXY WITH THE HUBBLE SPACE TELESCOPE WIDE FIELD CAMERA 3  

SciTech Connect (OSTI)

We report on deep near-infrared F125W (J) and F160W (H) Hubble Space Telescope Wide Field Camera 3 images of the z = 6.42 quasar J1148+5251 to attempt to detect rest-frame near-ultraviolet emission from the host galaxy. These observations included contemporaneous observations of a nearby star of similar near-infrared colors to measure temporal variations in the telescope and instrument point-spread function (PSF). We subtract the quasar point source using both this direct PSF and a model PSF. Using direct subtraction, we measure an upper limit for the quasar host galaxy of m{sub J} > 22.8 and m{sub H} > 23.0 AB mag (2 {sigma}). After subtracting our best model PSF, we measure a limiting surface brightness from 0.''3 to 0.''5 radius of {mu}{sub J} > 23.5 and {mu}{sub H} > 23.7 AB mag arcsec{sup -2} (2 {sigma}). We test the ability of the model subtraction method to recover the host galaxy flux by simulating host galaxies with varying integrated magnitude, effective radius, and Sersic index, and conducting the same analysis. These models indicate that the surface brightness limit ({mu}{sub J} > 23.5 AB mag arcsec{sup -2}) corresponds to an integrated upper limit of m{sub J} > 22-23 AB mag, consistent with the direct subtraction method. Combined with existing far-infrared observations, this gives an infrared excess log (IRX) > 1.0 and corresponding ultraviolet spectral slope {beta} > -1.2 {+-} 0.2. These values match those of most local luminous infrared galaxies, but are redder than those of almost all local star-forming galaxies and z {approx_equal} 6 Lyman break galaxies.

Mechtley, M.; Windhorst, R. A.; Cohen, S. H.; Jansen, R. A.; Scannapieco, E. [School of Earth and Space Exploration, Arizona State University, P.O. Box 871404, Tempe, AZ 85287 (United States); Ryan, R. E.; Koekemoer, A. M. [Space Telescope Science Institute, Baltimore, MD 21218 (United States); Schneider, G.; Fan, X. [Steward Observatory, University of Arizona, Tucson, AZ 85721 (United States); Hathi, N. P. [Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101 (United States); Keel, W. C. [Department of Physics and Astronomy, University of Alabama, Box 870324, Tuscaloosa, AL 35487 (United States); Roettgering, H. [Leiden Observatory, Leiden University, P.O. Box 9513, 2300 RA, Leiden (Netherlands); Schneider, D. P. [Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802 (United States); Strauss, M. A. [Princeton University Observatory, Princeton, NJ 08544 (United States); Yan, H. J. [Department of Physics and Astronomy, The University of Missouri, 701 South College Ave, Columbia, MO 65211 (United States)

2012-09-10T23:59:59.000Z

478

GREEN BANK TELESCOPE OBSERVATIONS OF THE NH{sub 3} (3, 3) AND (6, 6) TRANSITIONS TOWARD SAGITTARIUS A MOLECULAR CLOUDS  

SciTech Connect (OSTI)

Ammonia (3, 3) and (6, 6) transitions have been observed using the Green Bank Telescope toward the Sgr A region. The gas is mainly concentrated in 50 km s{sup -1} and 20 km s{sup -1} clouds located in a plane inclined to the galactic plane. These 'main' clouds appear to be virialized and influenced by the expansion of the supernova remnant Sgr A East. The observed emission shows very complicated features in the morphology and velocity structure. Gaussian multi-component fittings of the observed spectra revealed that various 'streaming' gas components exist all over the observed region. These components include those previously known as 'streamers' and 'ridges', but most of these components appear not to be directly connected to the major gas condensations (the 50 km s{sup -1} and 20 km s{sup -1} clouds). They are apparently located out of the galactic plane, and they may have a different origin than the major gas condensations. Some of the streaming components are expected to be sources that feed the circumnuclear disk of our Galactic center directly and episodically. They may also evolve differently than major gas condensations under the influence of the activities of the Galactic center.

Minh, Young Chol [Korea Astronomy and Space Science Institute, Daeduk-daero 776, Yuseong, Daejeon 305-348 (Korea, Republic of); Liu, Hauyu Baobab; Ho, Paul T. P.; Hsieh, Pei-Ying; Su, Yu-Nung [Institute of Astronomy and Astrophysics, Academia Sinica, P.O. Box 23-141, Taipei 10617, Taiwan (China); Kim, Sungsoo S. [Department of Astronomy and Space Science, Kyung Hee University, Yongin, Kyungki-do 446-701 (Korea, Republic of); Wright, Melvyn [Radio Astronomy Laboratory, University of California, Berkeley, 601 Campbell Hall, Berkeley, CA 94720 (United States)

2013-08-10T23:59:59.000Z

479

CORRELATIONS OF THE ARRIVAL DIRECTIONS OF ULTRA-HIGH ENERGY COSMIC RAYS WITH EXTRAGALACTIC OBJECTS AS OBSERVED BY THE TELESCOPE ARRAY EXPERIMENT  

SciTech Connect (OSTI)

We search for correlations between the positions of extragalactic objects and the arrival directions of ultra-high energy cosmic rays (UHECRs) with primary energy E ? 40 EeV as observed by the surface detector array of the Telescope Array (TA) experiment during the first 40 months of operation. We examine several public astronomical object catalogs, including the Veron-Cetty and Veron catalog of active galactic nuclei. We count the number of TA events correlated with objects in each catalog as a function of three parameters: the maximum angular separation between a TA event and an object, the minimum energy of the events, and the maximum redshift of the objects. We determine the combination of these parameters that maximizes the correlations, and we calculate the probability of having the same levels of correlations from an isotropic distribution of UHECR arrival directions. No statistically significant correlations are found when penalties for scanning over the above parameters and for searching in several catalogs are taken into account.

Abu-Zayyad, T.; Allen, M.; Anderson, R.; Barcikowski, E.; Belz, J. W.; Bergman, D. R.; Blake, S. A.; Cady, R.; Hanlon, W. [High Energy Astrophysics Institute and Department of Physics and Astronomy, University of Utah, Salt Lake City, UT (United States); Aida, R. [Interdisciplinary Graduate School of Medicine and Engineering, University of Yamanashi, Kofu, Yamanashi (Japan); Azuma, R.; Fukuda, T. [Graduate School of Science and Engineering, Tokyo Institute of Technology, Meguro, Tokyo (Japan); Cheon, B. G.; Cho, E. J. [Department of Physics and The Research Institute of Natural Science, Hanyang University, Seongdong-gu, Seoul (Korea, Republic of); Chiba, J. [Department of Physics, Tokyo University of Science, Noda, Chiba (Japan); Chikawa, M. [Department of Physics, Kinki University, Higashi Osaka, Osaka (Japan); Cho, W. R. [Department of Physics, Yonsei University, Seodaemun-gu, Seoul (Korea, Republic of); Fujii, H. [Institute of Particle and Nuclear Studies, KEK, Tsukuba, Ibaraki (Japan); Fujii, T. [Graduate School of Science, Osaka City University, Osaka (Japan); Fukushima, M. [Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba (Japan); and others

2013-11-10T23:59:59.000Z

480

PRECISE THROUGHPUT DETERMINATION OF THE PanSTARRS TELESCOPE AND THE GIGAPIXEL IMAGER USING A CALIBRATED SILICON PHOTODIODE AND A TUNABLE LASER: INITIAL RESULTS  

SciTech Connect (OSTI)

We have used a precision-calibrated photodiode as the fundamental metrology reference in order to determine the relative throughput of the PanSTARRS telescope and the Gigapixel imager, from 400 nm to 1050 nm. Our technique uses a tunable laser as a source of illumination on a transmissive flat-field screen. We determine the full-aperture system throughput as a function of wavelength, including (in a single integral measurement) the mirror reflectivity, the transmission functions of the filters and the corrector optics, and the detector quantum efficiency, by comparing the light seen by each pixel in the CCD array to that measured by a precision-calibrated silicon photodiode. This method allows us to determine the relative throughput of the entire system as a function of wavelength, for each pixel in the instrument, without observations of celestial standards. We present promising initial results from this characterization of the PanSTARRS system, and we use synthetic photometry to assess the photometric perturbations due to throughput variation across the field of view.

Stubbs, Christopher W.; Doherty, Peter; Cramer, Claire; Narayan, Gautham; Brown, Yorke J. [Department of Physics, 17 Oxford Street Harvard University, Cambridge MA 02138 (United States); Lykke, Keith R.; Woodward, John T. [National Institute of Standards and Technology, 100 Bureau Drive, Gaithersburg MD 20899 (United States); Tonry, John L., E-mail: stubbs@physics.harvard.ed [Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu HI 96822 (United States)

2010-12-15T23:59:59.000Z

Note: This page contains sample records for the topic "telescope baltay charles" 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

Hubble Space Telescope Grism Spectroscopy of Extreme Starbursts Across Cosmic Time: The Role of Dwarf Galaxies in the Star Formation History of the Universe  

E-Print Network [OSTI]

Near infrared slitless spectroscopy with the Wide Field Camera 3, onboard the Hubble Space Telescope, offers a unique opportunity to study low-mass galaxy populations at high-redshift ($z\\sim$1-2). While most high$-z$ surveys are biased towards massive galaxies, we are able to select sources via their emission lines that have very-faint continua. We investigate the star formation rate (SFR)-stellar mass ($M_{\\star}$) relation for about 1000 emission-line galaxies identified over a wide redshift range of $0.3 \\lesssim z \\lesssim 2.3$. We use the H$_{\\alpha}$ emission as an accurate SFR indicator and correct the broadband photometry for the strong nebular contribution to derive accurate stellar masses down to $M_{\\star} \\sim 10^{7} M_{\\odot}$. We focus here on a subsample of galaxies that show extremely strong emission lines (EELGs) with rest-frame equivalent widths ranging from 200 to 1500 \\AA. This population consists of outliers to the normal SFR-$M_{\\star}$ sequence with much higher specific SFRs ($> 10$ Gy...

Atek, Hakim; Pacifici, Camilla; Malkan, Matthew; Charlot, Stephane; Lee, Janice; Bedregal, Alejandro; Bunker, Andrew J; Colbert, James W; Dressler, Alan; Hathi, Nimish; Lehnert, Matthew; Martin, Crystal L; McCarthy, Patrick; Rafelski, Marc; Ross, Nathaniel; Siana, Brian; Teplitz, Harry I

2014-01-01T23:59:59.000Z

482

Hubble Space Telescope observations of the Kepler-field cluster NGC 6819. I. The bottom of the white dwarf cooling sequence  

E-Print Network [OSTI]

We use Hubble Space Telescope (HST) to reach the end of the white dwarf (WD) cooling sequence (CS) in the solar-metallicity open cluster NGC 6819. Our photometry and completeness tests show a sharp drop in the number of WDs along the CS at magnitudes fainter than mF606W = 26.050+/- 0.075. This implies an age of 2.25+/-0.20 Gyr, consistent with the age of 2.25+/-0.30 Gyr obtained from fits to the main-sequence turn-off. The use of different WD cooling models and initial-final-mass relations have a minor impact the WD age estimate, at the level of ~0.1 Gyr. As an important by-product of this investigation we also release, in electronic format, both the catalogue of all the detected sources and the atlases of the region (in two filters). Indeed, this patch of sky studied by HST (of size ~70 arcmin sq.) is entirely within the main Kepler-mission field, so the high-resolution images and deep catalogues will be particularly useful.

Bedin, L R; Anderson, J; Cassisi, S; Milone, A P; Piotto, G; King, I R; Bergeron, P; .,

2015-01-01T23:59:59.000Z

483

The Energy Spectrum of TeV Gamma-Rays from the Crab Nebula as measured by the HEGRA system of imaging air Cherenkov telescopes  

E-Print Network [OSTI]

The Crab Nebula has been observed by the HEGRA (High-Energy Gamma-Ray Astronomy) stereoscopic system of imaging air Cherenkov telescopes (IACTs) for a total of about 200 hrs during two observational campaigns: from September 1997 to March 1998 and from August 1998 to April 1999. The recent detailed studies of system performance give an energy threshold and an energy resolution for gamma-rays of 500 GeV and ~ 18%, respectively. The Crab energy spectrum was measured with the HEGRA IACT system in a very broad energy range up to 20 TeV, using observations at zenith angles up to 65 degrees. The Crab data can be fitted in the energy range from 1 to 20 TeV by a simple power-law, which yields dJg/dE = (2.79+/-0.02 +/- 0.5) 10^{-7} E^{-2.59 +/- 0.03 +/- 0.05}, ph m^{-2} s^{-1} TeV^{-1} The Crab Nebula energy spectrum, as measured with the HEGRA IACT system, agrees within 15% in the absolute scale and within 0.1 units in the power law index with the latest measurements by the Whipple, CANGAROO and CAT groups, consistent within the statistical and systematic errors quoted by the experiments. The pure power-law spectrum of TeV gamma-rays from the Crab Nebula constrains the physics parameters of the nebula environment as well as the models of photon emission.

F. Aharonian; The HEGRA Collaboration

2000-03-13T23:59:59.000Z

484

The Structure of Nuclear Star Clusters in Nearby Late-type Spiral Galaxies from Hubble Space Telescope Wide Field Camera 3 Imaging  

E-Print Network [OSTI]

We obtained Hubble Space Telescope/Wide Field Camera 3 imaging of a sample of ten of the nearest and brightest nuclear clusters residing in late-type spiral galaxies, in seven bands that span the near-ultraviolet to the near-infrared. Structural properties of the clusters were measured by fitting two-dimensional surface brightness profiles to the images using GALFIT. The clusters exhibit a wide range of structural properties. For six of the ten clusters in our sample, we find changes in the effective radius with wavelength, suggesting radially varying stellar populations. In four of the objects, the effective radius increases with wavelength, indicating the presence of a younger population which is more concentrated than the bulk of the stars in the cluster. However, we find a general decrease in effective radius with wavelength in two of the objects in our sample, which may indicate extended, circumnuclear star formation. We also find a general trend of increasing roundness of the clusters at longer waveleng...

Carson, Daniel J; Seth, Anil C; Brok, Mark den; Cappelari, Michele; Greene, Jenny E; Ho, Luis C; Neumayer, Nadine

2015-01-01T23:59:59.000Z

485

Neutrino Telescope Array Letter of Intent: A Large Array of High Resolution Imaging Atmospheric Cherenkov and Fluorescence Detectors for Survey of Air Showers from Cosmic Tau Neutrinos in the PeV-EeV Energy Range  

E-Print Network [OSTI]

This Letter of Intent (LoI) describes the outline and plan for the Neutrino Telescope Array (NTA) project. High-energy neutrinos provide unique and indisputable evidence for hadronic acceleration, as well as a most accurate probe into the hidden sector of traditional astronomy or physics, such as dark matter. However, their extremely low flux and interaction cross section make their detection extraordinarily difficult. Recently, IceCube has reported astronomical neutrino candidates in excess of expectation from atmospheric secondaries, but is limited by the water Cherenkov detection method. A next generation high-energy neutrino telescope should be capable of establishing indisputable evidence for cosmic high-energy neutrinos. It should not only have orders-of-magnitude larger sensitivity, but also enough pointing accuracy to probe known or unknown astronomical objects, without suffering from atmospheric secondaries. The proposed installation is a large array of compound eye stations of imaging atmospheric Ch...

Sasaki, Makoto

2014-01-01T23:59:59.000Z

486

Type Ia Supernova Discoveries at z>1 From the Hubble Space Telescope: Evidence for Past Deceleration and Constraints on Dark Energy Evolution  

E-Print Network [OSTI]

We have discovered 16 Type Ia supernovae (SNe Ia) with the Hubble Space Telescope (HST) and have used them to provide the first conclusive evidence for cosmic deceleration that preceded the current epoch of cosmic acceleration. These objects, discovered during the course of the GOODS ACS Treasury program, include 6 of the 7 highest-redshift SNe Ia known, all at z>1.25, and populate the Hubble diagram in unexplored territory. The luminosity distances to these and 170 previous SNe Ia are provided. A purely kinematic interpretation of the SN Ia sample provides evidence at the > 99% confidence level for a transition from deceleration to acceleration or similarly, strong evidence for a cosmic jerk. Using a simple model of the expansion history, the transition between the two epochs is constrained to be at z=0.46 +/- 0.13. The data are consistent with the cosmic concordance model of Omega_M ~ 0.3, Omega_Lambda~0.7 (chi^2_dof=1.06), and are inconsistent with a simple model of evolution or dust as an alternative to dark energy. For a flat Universe with a cosmological constant. When combined with external flat-Universe constraints we find w=-1.02 + 0.13 - 0.19 (and $dark energy, P = w\\rho c^2. Joint constraints on both the recent equation of state of dark energy, $w_0$, and its time evolution, dw/dz, are a factor of ~8 more precise than its first estimate and twice as precise as those without the SNe Ia discovered with HST. Our constraints are consistent with the static nature of and value of w expected for a cosmological constant (i.e., w_0 = -1.0, dw/dz = 0), and are inconsistent with very rapid evolution of dark energy. We address consequences of evolving dark energy for the fate of the Universe.

Adam G. Riess; Louis-Gregory Strolger; John Tonry; Stefano Casertano; Henry C. Ferguson; Bahram Mobasher; Peter Challis; Alexei V. Filippenko; Saurabh Jha; Weidong Li; Ryan Chornock; Robert P. Kirshner; Bruno Leibundgut; Mark Dickinson; Mario Livio; Mauro Giavalisco; Charles C. Steidel; Narciso Benitez; Zlatan Tsvetanov

2004-02-23T23:59:59.000Z

487

New Hubble Space Telescope Discoveries of Type Ia Supernovae at z > 1: Narrowing Constraints on the Early Behavior of Dark Energy  

E-Print Network [OSTI]

We have discovered 21 new Type Ia supernovae (SNe Ia) with the Hubble Space Telescope (HST) and have used them to trace the history of cosmic expansion over the last 10 billion years. These objects, which include 13 spectroscopically confirmed SNe Ia at z > 1, were discovered during 14 epochs of reimaging of the GOODS fields North and South over two years with the Advanced Camera for Surveys on HST. Together with a recalibration of our previous HST-discovered SNe Ia, the full sample of 23 SNe Ia at z > 1 provides the highest-redshift sample known. Combined with previous SN Ia datasets, we measured H(z) at discrete, uncorrelated epochs, reducing the uncertainty of H(z>1) from 50% to under 20%, strengthening the evidence for a cosmic jerk--the transition from deceleration in the past to acceleration in the present. The unique leverage of the HST high-redshift SNe Ia provides the first meaningful constraint on the dark energy equation-of-state parameter at z >1. The result remains consistent with a cosmological constant (w(z)=-1), and rules out rapidly evolving dark energy (dw/dz >>1). The defining property of dark energy, its negative pressure, appears to be present at z>1, in the epoch preceding acceleration, with ~98% confidence in our primary fit. Moreover, the z>1 sample-averaged spectral energy distribution is consistent with that of the typical SN Ia over the last 10 Gyr, indicating that any spectral evolution of the properties of SNe Ia with redshift is still below our detection threshold.

Adam G. Riess; Louis-Gregory Strolger; Stefano Casertano; Henry C. Ferguson; Bahram Mobasher; Ben Gold; Peter J. Challis; Alexei V. Filippenko; Saurabh Jha; Weidong Li; John Tonry; Ryan Foley; Robert P. Kirshner; Mark Dickinson; Emily MacDonald; Daniel Eisenstein; Mario Livio; Josh Younger; Chun Xu; Tomas Dahlen; Daniel Stern

2006-11-17T23:59:59.000Z

488

SCALING RELATIONS AND OVERABUNDANCE OF MASSIVE CLUSTERS AT z {approx}> 1 FROM WEAK-LENSING STUDIES WITH THE HUBBLE SPACE TELESCOPE  

SciTech Connect (OSTI)

We present weak gravitational lensing analysis of 22 high-redshift (z {approx}> 1) clusters based on Hubble Space Telescope images. Most clusters in our sample provide significant lensing signals and are well detected in their reconstructed two-dimensional mass maps. Combining the current results and our previous weak-lensing studies of five other high-z clusters, we compare gravitational lensing masses of these clusters with other observables. We revisit the question whether the presence of the most massive clusters in our sample is in tension with the current {Lambda}CDM structure formation paradigm. We find that the lensing masses are tightly correlated with the gas temperatures and establish, for the first time, the lensing mass-temperature relation at z {approx}> 1. For the power-law slope of the M-T{sub X} relation (M{proportional_to}T{sup {alpha}}), we obtain {alpha} = 1.54 {+-} 0.23. This is consistent with the theoretical self-similar prediction {alpha} = 3/2 and with the results previously reported in the literature for much lower redshift samples. However, our normalization is lower than the previous results by 20%-30%, indicating that the normalization in the M-T{sub X} relation might evolve. After correcting for Eddington bias and updating the discovery area with a more conservative choice, we find that the existence of the most massive clusters in our sample still provides a tension with the current {Lambda}CDM model. The combined probability of finding the four most massive clusters in this sample after the marginalization over cosmological parameters is less than 1%.

Jee, M. J.; Lubin, L.; Stanford, S. A. [Department of Physics, University of California, Davis, One Shields Avenue, Davis, CA 95616 (United States); Dawson, K. S.; Harris, D. W. [Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112 (United States); Hoekstra, H. [Leiden Observatory, Leiden University, Leiden (Netherlands); Perlmutter, S.; Suzuki, N.; Meyers, J.; Barbary, K. [E.O. Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley CA 94720 (United States); Rosati, P. [European Southern Observatory, Karl-Schwarzschild-Strasse 2, D-85748, Garching (Germany); Brodwin, M. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Koester, B.; Gladders, M. D. [Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637 (United States); Postman, M. [Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States); Barrientos, F. [Department of Astronomy and Astrophysics, Universidad Catolica de Chile, Santiago (Chile); Eisenhardt, P. [Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109 (United States); Ford, H. C. [Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218 (United States); Gilbank, D. G. [Department of Physics and Astronomy, University Of Waterloo, Waterloo, Ontario N2L 3G1 (Canada); Gonzalez, A. [Department of Astronomy, University of Florida, Gainesville, FL 32611-2055 (United States)

2011-08-20T23:59:59.000Z

489

Hubble Space Telescope Imaging of the Ultracompact Blue Dwarf Galaxy HS 0822+3542: An Assembling Galaxy in a Local Void?  

E-Print Network [OSTI]

We present deep U, narrow-V, and I-band images of the ultracompact blue dwarf galaxy HS 0822+3542, obtained with the Advanced Camera for Surveys / High Resolution Channel of the Hubble Space Telescope. This object is extremely metal-poor (12 + log(O/H) = 7.45) and resides in a nearby void. The images resolve it into two physically separate components that were previously described as star clusters in a single galaxy. The primary component is only \\~100 pc in maximum extent, and consists of starburst region surrounded by a ring-like structure of relatively redder stars. The secondary component is ~50 pc in size and lies at a projected distance of ~80 pc away from the primary, and is also actively star-forming. We estimate masses ~10^7 M(sol) and ~10^6 M(sol) for the two components, based on their luminosities, with an associated dynamical timescale for the system of a few Myr. This timescale and the structure of the components suggests that a collision between them triggered their starbursts. The spectral energy distributions of both components can be fitted by the combination of recent (few Myr old) starburst and an evolved (several Gyr old) underlying stellar population, similar to larger blue compact dwarf galaxies. This indicates that despite its metal deficiency the object is not forming its first generation of stars. However, the small sizes and masses of the two components suggests that HS 0822+3542 represents a dwarf galaxy in the process of assembling from clumps of stars intermediate in size between globular clusters and objects previously classified as galaxies. Its relatively high ratio of neutral gas mass to stellar mass (~1) and high specific star formation rate, log(SFR/M(sol) = -9.2, suggests that it is still converting much of its gas to stars.

Michael R. Corbin; William D. Vacca; John E. Hibbard; Rachel Somerville; Rogier A. Windhorst

2005-07-20T23:59:59.000Z

490

EMISSION-LINE GALAXIES FROM THE HUBBLE SPACE TELESCOPE PROBING EVOLUTION AND REIONIZATION SPECTROSCOPICALLY (PEARS) GRISM SURVEY. I. THE SOUTH FIELDS  

SciTech Connect (OSTI)

We present results of a search for emission-line galaxies (ELGs) in the southern fields of the Hubble Space Telescope Probing Evolution And Reionization Spectroscopically (PEARS) grism survey. The PEARS South Fields consist of five Advanced Camera for Surveys pointings (including the Hubble Ultra Deep Field) with the G800L grism for a total of 120 orbits, revealing thousands of faint object spectra in the GOODS-South region of the sky. ELGs are one subset of objects that are prevalent among the grism spectra. Using a two-dimensional detection and extraction procedure, we find 320 emission lines originating from 226 galaxy 'knots' within 192 individual galaxies. Line identification results in 118 new grism-spectroscopic redshifts for galaxies in the GOODS-South Field. We measure emission-line fluxes using standard Gaussian fitting techniques. At the resolution of the grism data, the H{beta} and [O III] doublet are blended. However, by fitting two Gaussian components to the H{beta} and [O III] features, we find that many of the PEARS ELGs have high [O III]/H{beta} ratios compared to other galaxy samples of comparable luminosities. The star formation rates of the ELGs are presented, as well as a sample of distinct giant star-forming regions at z {approx} 0.1-0.5 across individual galaxies. We find that the radial distances of these H II regions in general reside near the galaxies' optical continuum half-light radii, similar to those of giant H II regions in local galaxies.

Straughn, Amber N.; Gardner, Jonathan P. [Astrophysics Science Division, Observational Cosmology Laboratory, Goddard Space Flight Center, Code 665, Greenbelt, MD 20771 (United States); Pirzkal, Norbert; Grogin, Norman; Panagia, Nino [Space Telescope Science Institute, Baltimore, MD 21218 (United States); Meurer, Gerhardt R. [Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218 (United States); Cohen, Seth H.; Windhorst, Rogier A.; Malhotra, Sangeeta; Rhoads, James; Jansen, Rolf A. [School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287 (United States); Hathi, Nimish P. [Department of Physics and Astronomy, University of California, Riverside, CA 92521 (United States); Di Serego Alighieri, Sperello [INAF-Osservatorio Astrofisico di Arcetri, I-50125 Firenze (Italy); Gronwall, Caryl [Department of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802 (United States); Walsh, Jeremy [ESO Space Telescope European Co-ordinating Facility, D-85748 Garching bei Muenchen (Germany); Pasquali, Anna [Max-Planck-Institut for Astronomie, Koenigstuhl 17, D-69117 Heidelberg (Germany); Xu, Chun [Shanghai Institute of Technical Physics, 200083 Shanghai (China)], E-mail: Amber.N.Straughn@nasa.gov

2009-10-15T23:59:59.000Z

491

The Hubble Space Telescope Cluster Supernova Survey. V. Improving the Dark-energy Constraints above z > 1 and Building an Early-type-hosted Supernova Sample  

Science Journals Connector (OSTI)

We present Advanced Camera for Surveys, NICMOS, and Keck adaptive-optics-assisted photometry of 20TypeIa supernovae (SNeIa) from the Hubble Space Telescope (HST) Cluster Supernova Survey. The SNeIa were discovered over the redshift interval 0.623 z z = 1, thereby nearly doubling the statistical weight of HST-discovered SNeIa beyond this redshift. Our detailed analysis corrects for the recently identified correlation between SNIa luminosity and host galaxy mass and corrects the NICMOS zero point at the count rates appropriate for very distant SNeIa. Adding these SNe improves the best combined constraint on dark-energy density, ?DE(z), at redshifts 1.0 z ? = 0.729 0.014 (68% confidence level (CL) including systematic errors). For a flat wCDM model, we measure a constant dark-energy equation-of-state parameter w = 1.013+0.068 0.073 (68% CL). Curvature is constrained to ?0.7% in the owCDM model and to ?2% in a model in which dark energy is allowed to vary with parameters w 0 and wa . Further tightening the constraints on the time evolution of dark energy will require several improvements, including high-quality multi-passband photometry of a sample of several dozen z > 1 SNeIa. We describe how such a sample could be efficiently obtained by targeting cluster fields with WFC3 on board HST. The updated supernova Union2.1 compilation of 580 SNe is available at http://supernova.lbl.gov/Union.

N. Suzuki; D. Rubin; C. Lidman; G. Aldering; R. Amanullah; K. Barbary; L. F. Barrientos; J. Botyanszki; M. Brodwin; N. Connolly; K. S. Dawson; A. Dey; M. Doi; M. Donahue; S. Deustua; P. Eisenhardt; E. Ellingson; L. Faccioli; V. Fadeyev; H. K. Fakhouri; A. S. Fruchter; D. G. Gilbank; M. D. Gladders; G. Goldhaber; A. H. Gonzalez; A. Goobar; A. Gude; T. Hattori; H. Hoekstra; E. Hsiao; X. Huang; Y. Ihara; M. J. Jee; D. Johnston; N. Kashikawa; B. Koester; K. Konishi; M. Kowalski; E. V. Linder; L. Lubin; J. Melbourne; J. Meyers; T. Morokuma; F. Munshi; C. Mullis; T. Oda; N. Panagia; S. Perlmutter; M. Postman; T. Pritchard; J. Rhodes; P. Ripoche; P. Rosati; D. J. Schlegel; A. Spadafora; S. A. Stanford; V. Stanishev; D. Stern; M. Strovink; N. Takanashi; K. Tokita; M. Wagner; L. Wang; N. Yasuda; H. K. C. Yee; The Supernova Cosmology Project

2012-01-01T23:59:59.000Z

492

Earthquakes Observed with a Telescope  

Science Journals Connector (OSTI)

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