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Sample records for telescope baltay charles

  1. SciTech Connect:

    Office of Scientific and Technical Information (OSTI)

    Baltay, Charles" Name Name ORCID Search Authors Title: Subject: Identifier Numbers: Research Org: Sponsoring Org: Site: All Alaska Power Administration, Juneau, Alaska (United...

  2. High Statistics Study of Nearby Type 1a Supernovae. QUEST Camera...

    Office of Scientific and Technical Information (OSTI)

    Statistics Study of Nearby Type 1a Supernovae. QUEST Camera Short Term Maintenance: Final Technical Report Baltay, Charles 79 ASTRONOMY AND ASTROPHYSICS Study of Type 1a Supernovae...

  3. TITLE AUTHORS SUBJECT SUBJECT RELATED DESCRIPTION PUBLISHER AVAILABILI...

    Office of Scientific and Technical Information (OSTI)

    High Statistics Study of Nearby Type a Supernovae QUEST Camera Short Term Maintenance Final Technical Report Baltay Charles ASTRONOMY AND ASTROPHYSICS Study of Type a Supernovae...

  4. Charles Darwin University Press

    E-Print Network [OSTI]

    CDU Press Catalogue Charles Darwin University Press (CDU Press) (GLWHG E\\ -XGH &RQZD\\ 6WHS E\\ 6WHS Wildflowers Graham Brown CHARLES DARWIN UNIVERSITY PRESS #12;1 2 Welcome to Our Catalogue CDU Press. The Press was founded in 1989 and has developed a publication list which is a unique blend of titles, often

  5. Lake Charles CCS Project

    SciTech Connect (OSTI)

    Leib, Thomas; Cole, Dan

    2015-06-30

    In late September 2014 development of the Lake Charles Clean Energy (LCCE) Plant was abandoned resulting in termination of Lake Charles Carbon Capture and Sequestration (CCS) Project which was a subset the LCCE Plant. As a result, the project was only funded through Phase 2A (Design) and did not enter Phase 2B (Construction) or Phase 2C (Operations). This report was prepared relying on information prepared and provided by engineering companies which were engaged by Leucadia Energy, LLC to prepare or review Front End Engineering and Design (FEED) for the Lake Charles Clean Energy Project, which includes the Carbon Capture and Sequestration (CCS) Project in Lake Charles, Louisiana. The Lake Charles Carbon Capture and Sequestration (CCS) Project was to be a large-scale industrial CCS project intended to demonstrate advanced technologies that capture and sequester carbon dioxide (CO2) emissions from industrial sources into underground formations. The Scope of work was divided into two discrete sections; 1) Capture and Compression prepared by the Recipient Leucadia Energy, LLC, and 2) Transport and Sequestration prepared by sub-Recipient Denbury Onshore, LLC. Capture and Compression-The Lake Charles CCS Project Final Technical Report describes the systems and equipment that would be necessary to capture CO2 generated in a large industrial gasification process and sequester the CO2 into underground formations. The purpose of each system is defined along with a description of its equipment and operation. Criteria for selection of major equipment are provided and ancillary utilities necessary for safe and reliable operation in compliance with environmental regulations are described. Construction considerations are described including a general arrangement of the CCS process units within the overall gasification project. A cost estimate is provided, delineated by system area with cost breakdown showing equipment, piping and materials, construction labor, engineering, and other costs. The CCS Project Final Technical Report is based on a Front End Engineering and Design (FEED) study prepared by SK E&C, completed in [June] 2014. Subsequently, Fluor Enterprises completed a FEED validation study in mid-September 2014. The design analyses indicated that the FEED package was sufficient and as expected. However, Fluor considered the construction risk based on a stick-build approach to be unacceptable, but construction risk would be substantially mitigated through utilization of modular construction where site labor and schedule uncertainty is minimized. Fluor’s estimate of the overall EPC project cost utilizing the revised construction plan was comparable to SKE&C’s value after reflecting Fluor’s assessment of project scope and risk characteristic. Development was halted upon conclusion of Phase 2A FEED and the project was not constructed.Transport and Sequestration – The overall objective of the pipeline project was to construct a pipeline to transport captured CO2 from the Lake Charles Clean Energy project to the existing Denbury Green Line and then to the Hastings Field in Southeast Texas to demonstrate effective geologic sequestration of captured CO2 through commercial EOR operations. The overall objective of the MVA portion of the project was to demonstrate effective geologic sequestration of captured CO2 through commercial Enhanced Oil Recovery (EOR) operations in order to evaluate costs, operational processes and technical performance. The DOE target for the project was to capture and implement a research MVA program to demonstrate the sequestration through EOR of approximately one million tons of CO2 per year as an integral component of commercial operations.

  6. Charles L. Brown Department of Electrical & Computer

    E-Print Network [OSTI]

    Acton, Scott

    -imaging and -electronics, and superconducting electronics Every faculty member in the Charles L. Brown Department

  7. Charles Sturt University Q all campuses

    E-Print Network [OSTI]

    New South Wales, University of

    : Administration Office Charles Sturt University Tony McGrane Place Dubbo NSW Orange campus: Prospective Student

  8. INTERCOMMITTEE MEMORANDUM TO: DR. CHARLES MAULE

    E-Print Network [OSTI]

    Saskatchewan, University of

    INTERCOMMITTEE MEMORANDUM TO: DR. CHARLES MAULE CHAIR, FACULTY COUNCIL, COLLEGE OF ENGINEERING FROM: MR. CHRISTOPHER MARTIN ACADEMIC PROGRAMS COORDINATOR, COLLEGE OF ENGINEERING SUBJECT: PROGRAM ACADEMIC, COLLEGE OF ENGINEERING Dr. Charles Maule: At the recommendation of the Undergraduate Academic

  9. Lake Charles Urbanized Area MTP 2034 

    E-Print Network [OSTI]

    Lake Charles Urbanized Area Metropolitan Planning Organization

    2009-08-04

    CONSTRAINED AND UNCONSTRAINED PLAN PROJECTS . C-1 ? Lake Charles Urbanized Area MTP 2034 ? Page v Alliance Transportation Group, Inc. Adopted August 4, 2009 Table of Tables Table 2-1 Stakeholders Present... ......................................................................................................... 3-1 ? Lake Charles Urbanized Area MTP 2034 ? Page iii Alliance Transportation Group, Inc. Adopted August 4, 2009 LAKE CHARLES URBANIZED AREA TRAVEL DEMAND MODEL .............................................................. 3-2 SOCIOECONOMIC...

  10. "Title","Creator/Author","Publication Date","OSTI Identifier...

    Office of Scientific and Technical Information (OSTI)

    High Statistics Study of Nearby Type 1a Supernovae. QUEST Camera Short Term Maintenance: Final Technical Report","Baltay, Charles","2012-10-16T04:00:00Z",1053184,"10.2172...

  11. ANALYTIC COMPLETION (DRAFT) CHARLES REZK

    E-Print Network [OSTI]

    Rezk, Charles

    ANALYTIC COMPLETION (DRAFT) CHARLES REZK Abstract. This is an expository treatment of what we call "analytic completion" of R- modules, which is a kind of completion defined in terms of quotients of power series modules. It is closely related to the left derived functors of adic completion, in which guise

  12. Charles Baily Department of Physics!

    E-Print Network [OSTI]

    Colorado at Boulder, University of

    3/3/13 1 Charles Baily Department of Physics! University of Colorado Boulder! baily Educa1on 100,000 more STEM educators #12;3/3/13 2 APS/AAPT Doubling Ini1a1ve Mission Statement (2007) We advocate doubling the number of bachelor degrees in physics

  13. The Power 25 Charles Otto -POLICY MAKER

    E-Print Network [OSTI]

    The Power 25 Charles Otto - POLICY MAKER When Charles Otto was awarded swimming and lifesaving 2008 Power 25 By Aquatics International Staff Some of the most powerful people in the industry://www.aquaticsintl.com #12;The Power 25 Some of the most powerful people in the industry are not necessarily aquatics

  14. The Lake Charles CCS Project

    SciTech Connect (OSTI)

    Doug Cathro

    2010-06-30

    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.

  15. Charles Rousseaux | Department of Energy

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

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of Natural GasAdjustmentsShirley Ann JacksonDepartment of EnergyResearchersOctoberCharles Rousseaux - Senior Communications

  16. Ass. Charles Gide Justice & Economics Toulouse, June 16 &17, 2011

    E-Print Network [OSTI]

    Paris-Sud XI, Université de

    Ass. Charles Gide Justice & Economics Toulouse, June 16 &17, 2011 English corrections in progress in a specific assessment (Sen, 1992 and see Sen,1990). #12;Ass. Charles Gide Justice & Economics Toulouse, June

  17. Physical Geology Laboratory Manual Charles Merguerian and J Bret Bennington

    E-Print Network [OSTI]

    Merguerian, Charles

    Physical Geology Laboratory Manual Charles Merguerian and J Bret Bennington Geology Department Hofstra University © 2006 #12;i PHYSICAL GEOLOGY LABORATORY MANUAL Ninth Edition Professors Charles Merguerian and J Bret Bennington Geology Department Hofstra University #12;ii ACKNOWLEDGEMENTS We thank

  18. A Signal Processing Approach To Fair Surface Design Charles Robertson

    E-Print Network [OSTI]

    Kazhdan, Michael

    A Signal Processing Approach To Fair Surface Design Slide 1 Charles Robertson A Signal Processing: Charles Robertson A Signal Processing Approach To Fair Surface Design Slide 2 Charles Robertson Overview Introduction Fairing Subdivision Constraints Conclusions A Signal Processing Approach To Fair Surface Design

  19. MEDICAL STUDENT Charles E. Schmidt College of Medicine

    E-Print Network [OSTI]

    Fernandez, Eduardo

    MEDICAL STUDENT HANDBOOK 2014-2015 Charles E. Schmidt College of Medicine Boca Raton, FL #12;#12;i..................................................................................................................................................1 MISSION STATEMENT OF THE CHARLES E. SCHMIDT COLLEGE OF MEDICINE ..........................2 GUIDING PRINCIPLES OF THE CHARLES E. SCHMIDT COLLEGE OF MEDICINE ..........................2 DEFINITIONS

  20. Objects and Synchronous Programming Charles ANDR1

    E-Print Network [OSTI]

    André, Charles

    gener- ated by a synchronous language compiler, the user must provide an execution machine [AND 93]. Our­ 1 ­ Objects and Synchronous Programming Charles ANDR�1 , Frédéric BOULANGER2 , Marie logical correctness, is the essence of the synchronous paradigm. This paper proposes to combine these two

  1. The Roy R. Charles Center Annual Report

    E-Print Network [OSTI]

    Yu, Gexin

    Center's Mission The Roy R. Charles Center for Academic Excellence Faculty Development, Student Research of many new curricular ideas, including the freshman seminar program and our emphasis on research in developing an undergraduate research program that may be unmatched, both in quantity and quality

  2. High resolution telescope

    DOE Patents [OSTI]

    Massie, Norbert A. (San Ramon, CA); Oster, Yale (Danville, CA)

    1992-01-01

    A large effective-aperture, low-cost optical telescope with diffraction-limited resolution enables ground-based observation of near-earth space objects. The telescope has a non-redundant, thinned-aperture array in a center-mount, single-structure space frame. It employs speckle interferometric imaging to achieve diffraction-limited resolution. The signal-to-noise ratio problem is mitigated by moving the wavelength of operation to the near-IR, and the image is sensed by a Silicon CCD. The steerable, single-structure array presents a constant pupil. The center-mount, radar-like mount enables low-earth orbit space objects to be tracked as well as increases stiffness of the space frame. In the preferred embodiment, the array has elemental telescopes with subaperture of 2.1 m in a circle-of-nine configuration. The telescope array has an effective aperture of 12 m which provides a diffraction-limited resolution of 0.02 arc seconds. Pathlength matching of the telescope array is maintained by an electro-optical system employing laser metrology. Speckle imaging relaxes pathlength matching tolerance by one order of magnitude as compared to phased arrays. Many features of the telescope contribute to substantial reduction in costs. These include eliminating the conventional protective dome and reducing on-site construction activites. The cost of the telescope scales with the first power of the aperture rather than its third power as in conventional telescopes.

  3. -WIND STRUC-By Charles Fitzhugh Talman,

    E-Print Network [OSTI]

    -WIND STRUC- By Charles Fitzhugh Talman, Authority on Meteorology That the wind f o r:,II and that Houzea describes as the l~texturellof the wind, are now usually re- ferred t o as "wind structure.11*li In recent years they have been the subject of 1n.W~ Wind structure was "The wind as a whole is not a thing

  4. Declaration of Charles Wodrich in Support of Supplemental Comments...

    Energy Savers [EERE]

    the Economic Impacts of the Proposed Definition of "Showerhead," Docket No. EERE-2010-BT-NOA-0016 Declaration of Charles Wodrich in Support of Supplemental Comments of the...

  5. Charles Motel & Bathhouse Pool & Spa Low Temperature Geothermal...

    Open Energy Info (EERE)

    Motel & Bathhouse Pool & Spa Low Temperature Geothermal Facility Jump to: navigation, search Name Charles Motel & Bathhouse Pool & Spa Low Temperature Geothermal Facility Facility...

  6. The Wizard of Schenectady: Charles Proteus Steinmetz | GE Global...

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

    week the Smithsonian's "Past Imperfect" blog highlighted a man near and dear to the heart of GE Global Research, Charles Proteus Steinmetz. The article paints a really...

  7. EM Algorithms from a Non-Stochastic Perspective Charles Byrne

    E-Print Network [OSTI]

    Byrne, Charles

    EM Algorithms from a Non-Stochastic Perspective Charles Byrne Charles Byrne@uml.edu Department The EM algorithm is not a single algorithm, but a template for the con- struction of iterative algorithms a method for estimat- ing parameters in statistics, the essence of the EM algorithm is not stochastic

  8. TERMINATION OF NONSIMPLE REWRITE SYSTEMS CHARLES GLEN HOOT

    E-Print Network [OSTI]

    Dershowitz, Nachum

    TERMINATION OF NON­SIMPLE REWRITE SYSTEMS BY CHARLES GLEN HOOT B.A., University of California, San Diego, 1982 M.A., Princeton University, 1985 THESIS Submitted in partial fulfillment of the requirements at Urbana­Champaign, 1996 Urbana, Illinois #12; TERMINATION OF NON­SIMPLE REWRITE SYSTEMS Charles Glen Hoot

  9. TERMINATION OF NON-SIMPLE REWRITE SYSTEMS CHARLES GLEN HOOT

    E-Print Network [OSTI]

    Dershowitz, Nachum

    TERMINATION OF NON-SIMPLE REWRITE SYSTEMS BY CHARLES GLEN HOOT B.A., University of California, San Diego, 1982 M.A., Princeton University, 1985 THESIS Submitted in partial ful llment of the requirements at Urbana-Champaign, 1996 Urbana, Illinois #12;TERMINATION OF NON-SIMPLE REWRITE SYSTEMS Charles Glen Hoot

  10. Charles Townes, the Maser, and the Laser

    Office of Scientific and Technical Information (OSTI)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of NaturalDukeWakefield Municipal GasAdministration Medal01Technical Information-- Energy, science,BurtonCharles Townes

  11. Charles McConnell | Department of Energy

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

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of Natural GasAdjustmentsShirleyEnergy A plug-in electric vehicle (PEV) charging station in Rhode Island. | PhototheCharles

  12. Dipartimento di Biologia e Biotecnologie "Charles Darwin" Universit degli Studi di Roma "La Sapienza"

    E-Print Network [OSTI]

    Di Pillo, Gianni

    scientifico disciplinare BIO/18, presso il Dipartimento di Biologia e Biotecnologia "Charles Darwin" dell

  13. Chapter Fourteen Telescope Consortium

    E-Print Network [OSTI]

    Gustafsson, Torgny

    206 Chapter Fourteen Telescope Consortium Paul Leath (1995-2000) When Allen Robbins stepped down, and all other universities. Also in 1998, U.S. News & World Report ranked the Rutgers program 16th.S. in High Energy Elementary Particle Physics, 6th among public universities.4 This assessment was followed

  14. Lake Charles Carbon Capture and Sequestration Project U. S. Department...

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

    plant will not receive co-funding from DOE. The Lake Charles CCS Project will capture carbon dioxide (CO 2 ) from the LCCE Gasification plant and transport the CO 2 via a new...

  15. 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...

  16. DOE Zero Energy Ready Home Case Study: Charles Thomas Homes,...

    Energy Savers [EERE]

    under slab; a vented attic with R-100 blown cellulose; 95% AFUE furnace, 14 SEER AC, ERV; heat pump water heater. DOE Zero Energy Ready Home Case Study: Charles Thomas Homes,...

  17. Charles Eames and communication : from education to computers

    E-Print Network [OSTI]

    Lai, Constance Chunlan, 1972-

    1999-01-01

    This thesis looks at a variety of projects done by Charles and Ray Eames that emphasize their interest in communication leading up to their 1953 film A Communications Primer. The significance of this film is threefold: ...

  18. Perspectives on neutrino telescopes 2009

    SciTech Connect (OSTI)

    Quigg, Chris; /Fermilab /Karlsruhe U., TTP

    2009-04-01

    Remarks at the roundtable on plans for the future at the XIII International Workshop on Neutrino Telescopes.

  19. OPENENDED CONFIGURATIONS OF RADIO TELESCOPES

    E-Print Network [OSTI]

    Kreinovich, Vladik

    telescopes, devices that use the second observability window of radio waves. Why configurations of radioOPEN­ENDED CONFIGURATIONS OF RADIO TELESCOPES: A GEOMETRICAL ANALYSIS Vladik Kreinovich, Scott A. The quality of radio astronomical images drastically depends on where we place the radio telescopes. During

  20. The ANTARES Neutrino Telescope

    E-Print Network [OSTI]

    Perrina, Chiara

    2015-01-01

    At about 40 km off the coast of Toulon (France), anchored at 2475 m deep in the Mediterranean Sea, there is ANTARES: the first undersea neutrino telescope and the only one currently operating. The detector consists of 885 photomultiplier tubes arranged into 12 strings of 450-metres high, with the aim to detect the Cherenkov light induced by the charged superluminal interaction products of neutrinos. Its main scientific target is the search for high-energy (TeV and beyond) neutrinos from cosmic accelerators, as predicted by hadronic interaction models, and the measurement of the cosmic neutrino diffuse flux, focusing in particular on events coming from below the horizon (up-going events) in order to significantly reduce the atmospheric muons background. Thanks to the development of a strategy for the identification of neutrinos coming from above the horizon (down-going events) the field of view of the telescope will be extended.

  1. Comparing NEO Search Telescopes

    E-Print Network [OSTI]

    Myhrvold, Nathan

    2015-01-01

    Multiple terrestrial and space-based telescopes have been proposed for detecting and tracking near-Earth objects (NEOs). Detailed simulations of the search performance of these systems have used complex computer codes that are not widely available, which hinders accurate cross- comparison of the proposals and obscures whether they have consistent assumptions. Moreover, some proposed instruments would survey infrared (IR) bands, whereas others would operate in the visible band, and differences among asteroid thermal and visible light models used in the simulations further complicate like-to-like comparisons. I use simple physical principles to estimate basic performance metrics for the ground-based Large Synoptic Survey Telescope and three space-based instruments - Sentinel, NEOCam, and a Cubesat constellation. The performance is measured against two different NEO distributions, the Bottke et al. distribution of general NEOs, and the Veres et al. distribution of earth impacting NEO. The results of the comparis...

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

    Office of Environmental Management (EM)

    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...

  3. Grid Integration of Robotic Telescopes

    E-Print Network [OSTI]

    F. Breitling; T. Granzer; H. Enke

    2009-03-23

    Robotic telescopes and grid technology have made significant progress in recent years. Both innovations offer important advantages over conventional technologies, particularly in combination with one another. Here, we introduce robotic telescopes used by the Astrophysical Institute Potsdam as ideal instruments for building a robotic telescope network. We also discuss the grid architecture and protocols facilitating the network integration that is being developed by the German AstroGrid-D project. Finally, we present three user interfaces employed for this purpose.

  4. The KELT-South Telescope

    E-Print Network [OSTI]

    Pepper, Joshua; Siverd, Robert; James, David; Stassun, Keivan

    2012-01-01

    The Kilodegree Extremely Little Telescope (KELT) project is a survey for new transiting planets around bright stars. KELT-South is a small-aperture, wide-field automated telescope located at Sutherland, South Africa. The telescope surveys a set of 26 degree by 26 degree fields around the southern sky, and targets stars in the range of 8 solar-type main-sequence stars.

  5. OPENENDED CONFIGURATIONS OF RADIO TELESCOPES

    E-Print Network [OSTI]

    Kreinovich, Vladik

    telescopes, devices that use the second observability window of radio waves. #12; Why configurations of radioOPEN­ENDED CONFIGURATIONS OF RADIO TELESCOPES: TOWARDS OPTIMAL DESIGN VLADIK KREINOVICH, SCOTT A, Russia ABSTRACT The quality of radio astronomical images drastically depends on where we place the radio

  6. Space Telescope Programs Hubble Observatory

    E-Print Network [OSTI]

    Colorado at Boulder, University of

    Certifications required for all raw materials ­ Shelf Life (Polymerics) materials date controlled by QA · DesignsSpace Telescope Programs Hubble Observatory HST-COS FUV PER 11/8/00 FUV Detector System Materials;Space Telescope Programs Hubble Observatory HST-COS FUV PER 11/8/00 Materials and Processes · Materials

  7. Mechanical Summer Tipping of Tart Cherry Charles D. Kesner

    E-Print Network [OSTI]

    1 Mechanical Summer Tipping of Tart Cherry Charles D. Kesner Professor Emeritus Department common mistakes I see is the tendency to cut too deeply. The standard timing for mechanical summer: Our data indicates that mechanical summer hedging of tart cherries 45 days after full bloom

  8. EXECUTION MACHINE FOR SYNCHRONOUS LANGUAGES Charles ANDR Hdi BOUFAED

    E-Print Network [OSTI]

    André, Charles

    EXECUTION MACHINE FOR SYNCHRONOUS LANGUAGES Charles ANDR� Hédi BOUFAÏED Laboratoire I3S, Université on a the synchronous paradigm, and explains the role and the architecture of the execution machine. Keywords: synchronous programming, execution machine, control, implementation. NOMENCLATURE We use Courier as the font

  9. 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

  10. Volatility Persistence in Crude Oil Markets Amlie CHARLES

    E-Print Network [OSTI]

    Boyer, Edmond

    Volatility Persistence in Crude Oil Markets Amélie CHARLES Audencia Nantes, School of Management announcements on production reduction or US announcements on crude inventories. We find that the crude oil on the volatility modelling process improve the understanding of volatility in crude oil markets. Keywords: Crude

  11. View Dependent Isosurface Extraction Yarden Livnat Charles Hansen

    E-Print Network [OSTI]

    Livnat, Yarden

    triangles and is accomplished by the graphics hardware. While the latest isosurface extraction methods have isosurface extraction (NOISE) method. Both NOISE and the later optimal isosurface extraction methodView Dependent Isosurface Extraction Yarden Livnat Charles Hansen University of Utah Abstract We

  12. Managing Florida Ponds for Fishing 1 Charles E. Cichra2

    E-Print Network [OSTI]

    Hill, Jeffrey E.

    CIR802 Managing Florida Ponds for Fishing 1 Charles E. Cichra2 1. This document is CIR802, one. Millie Ferrer-Chancy, Interim Dean Florida has thousands of natural and man-made ponds which range in surface area from less than 1/10 acre to greater than ten acres. Man-made ponds include dug

  13. prop_num pi_lname title Abstract 71313 CHARLES

    E-Print Network [OSTI]

    Nishikawa, Ken-Ichi

    prop_num pi_lname title Abstract 71313 CHARLES DISENTANGLING DARK MATTER GAMMA-RAY SIGNALS FROM and describe a three step procedure we will use to extract constraints on dark matter (DM) signals: (i onwards are publicly available on the web, updated monthly, and being widely used, especially in Fermi

  14. QER- Comment of Lake Charles Harbor & Terminal District

    Broader source: Energy.gov [DOE]

    Good Afternoon, Please find the Lake Charles Harbor and Terminal District’s comments on Infrastructure Constraints in re: the QER Investigation hearing scheduled for Bismarck, ND on August 8, 2014. Please include these comments in the public record of the hearing. Thank you.

  15. FlrIXTER PAINTINGS By Charles Fitzhugh Talmn,

    E-Print Network [OSTI]

    FlrIXTER PAINTINGS By Charles Fitzhugh Talmn, Authority on Meteorology. There are painters who the consistency of the substance i t s e l f . He accordingly tr&iaad himself to paint v i t h amazing rapidity. He completes a large canvas a t a single sitting. Ask him how long i t took him t o paint i

  16. md Science Service Featuro By Dr. Charles F. Brooks

    E-Print Network [OSTI]

    No. 745 Sept. 30 md Science Service Featuro By Dr. Charles F. Brooks of Clark University. RAIN SKADOWS Mountains cast rain shadoms; often there is the greatest difference in rain- is fall between in me trade wind, laden with water vapor, blows persistently from one direction. is forced to rise

  17. By Dr. Charles F. Brooks o f Clark University.

    E-Print Network [OSTI]

    of the crop i t s e l f , (Tomorrow: Summer Drouths) A l l rights reserved by Science Service Science ServiceBy Dr. Charles F. Brooks o f Clark University. -\\EATHER AND CROP YIELDS If your garden fails t o e the yield of staple crops from 20 t o 30 Per cent* Plant diseases, insect and animal pests

  18. On the Genealogy of Asexual Diploids , Charles H. Langley2

    E-Print Network [OSTI]

    Song, Yun S.

    On the Genealogy of Asexual Diploids Fumei Lam1 , Charles H. Langley2 , and Yun S. Song3,4 1 of reconstructing diploid genealogies under the assump- tion of no sexual reproduction or recombination, with the ultimate goal being to devise genealogy-based tools for testing deviation from these assumptions. We first

  19. Cluster Observations with the South Pole Telescope

    E-Print Network [OSTI]

    Plagge, Thomas Jeffrey

    2009-01-01

    The South Pole Telescope during the last stages ofwater vapor at the South Pole relative to two otherSZ Survey Instrument . 3 The South Pole Telescope Observing

  20. Power operations in Morava E-theory Charles Rezk

    E-Print Network [OSTI]

    Rezk, Charles

    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

  1. Dy Charles Fitzhugn Tulnim Authority on I& teorology

    E-Print Network [OSTI]

    Dy Charles Fitzhugn Tulnim Authority on I& teorology Although the origin of ball 1i * "alther Brand, i n Germany, cofltains a c r i t i c a l analysis of Z l E cu6e6 Of b e l l lightning, 'selected from a auch l a r g e r numbar of r f p o r t s t o which t h e author Bull lightning occurs

  2. A Generalized Sharp Whitney Theorem for Jets Charles Fefferman

    E-Print Network [OSTI]

    Fefferman, Charles

    A Generalized Sharp Whitney Theorem for Jets by Charles Fefferman Department of Mathematics@math.princeton.edu Abstract. Suppose that, for each point x in a given subset E Rn, we are given an m-jet f(x) and a convex, symmetric set (x) of m-jets at x. We ask whether there exist a function F Cm,(Rn) and a finite constant M

  3. Review: Teaching Peter McLaren edited by Marc Pruyn and Luis M. Huerta-Charles

    E-Print Network [OSTI]

    Pozo, Mike Alexander

    2006-01-01

    Peter McLaren edited by Marc Pruyn and Luis M Huerta-Peter McLaren editors Marc Pruyn and Luis M. Huerta- Charles

  4. Wide field of view telescope

    DOE Patents [OSTI]

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

    2008-01-15

    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.

  5. Neutrino telescopes in the World

    SciTech Connect (OSTI)

    Ernenwein, J.-P.

    2007-01-12

    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.

  6. Brittle Fault Chronology of New York City (NYC) Charles Merguerian, Geology Department, Hofstra University, Hempstead, NY 11549

    E-Print Network [OSTI]

    Merguerian, Charles

    Brittle Fault Chronology of New York City (NYC) Charles Merguerian, Geology Department, Hofstra This Abstract: Merguerian, Charles, 2004a, Brittle fault chronology of New York City (NYC): Geological Society

  7. Merguerian, Charles, 1986a, Tunnel vision -A deep view of the bedrock geology of New York City (NYC).

    E-Print Network [OSTI]

    Merguerian, Charles

    Merguerian, Charles, 1986a, Tunnel vision - A deep view of the bedrock geology of New York City This Abstract: Merguerian, Charles, 1986a, Tunnel vision - A deep view of the bedrock geology of New York City

  8. Status of the Cherenkov Telescope Array's Large Size Telescopes

    E-Print Network [OSTI]

    Cortina, J

    2015-01-01

    The Cherenkov Telescope Array (CTA) observatory, will be deployed over two sites in the two hemispheres. Both sites will be equipped with four Large Size Telescopes (LSTs), which are crucial to achieve the science goals of CTA in the 20-200 GeV energy range. Each LST is equipped with a primary tessellated mirror dish of 23 m diameter, supported by a structure made mainly of carbon fibre reinforced plastic tubes and aluminum joints. This solution guarantees light weight (around 100 tons), essential for fast repositioning to any position in the sky in Canary island of La Palma (Spain). In this talk we will outline the technical solutions adopted to fulfill the design requirem...

  9. PRESS RELEASE Charles University in Prague opens its doors wide to the world -computer science

    E-Print Network [OSTI]

    Cerveny, Vlastislav

    PRESS RELEASE Charles University in Prague opens its doors wide to the world - computer science course in computer science in English. In 1952, when the Faculty of Mathematics and Physics, Charles's and master's study programs in computer science with English as the language of instruction. Attention

  10. Charles Darwin University Press www.cdu.edu.au/cdupress About CDU Press2

    E-Print Network [OSTI]

    Dry Season 2009 Charles Darwin University Press www.cdu.edu.au/cdupress #12;About CDU Press2 Season 2009 Catalog CDU Press is the publishing house of Charles Darwin University. We publish books publicatons. The Press is a small but adventurous organisation and we have books that include subject matter

  11. ontinuing the legacy of Dr. Charles D. Keeling in monitoring carbon dioxide, NOAA's Office

    E-Print Network [OSTI]

    C ontinuing the legacy of Dr. Charles D. Keeling in monitoring carbon dioxide, NOAA's Office provides funding to Charles D. Keeling to begin monitoring carbon dioxide (CO2) at the South Pole and Mauna-seasonal data on carbon dioxide, methane, carbon monoxide, and other gases in a region where rapid climate

  12. Physical Geology Laboratory J Bret Bennington, Charles Merguerian and John E. Sanders

    E-Print Network [OSTI]

    Merguerian, Charles

    Physical Geology Laboratory Manual J Bret Bennington, Charles Merguerian and John E. Sanders Geology Department Hofstra University © 1999 #12;PHYSICAL GEOLOGY LABORATORY MANUAL Third Edition (Revised) by J Bret Bennington, Charles Merguerian, and John E. Sanders Department of Geology Hofstra University

  13. Baskerville, C. A.; and Merguerian, Charles, 1982, Tectonic history of the New York Metropolitan area.

    E-Print Network [OSTI]

    Merguerian, Charles

    Baskerville, C. A.; and Merguerian, Charles, 1982, Tectonic history of the New York Metropolitan area. Urban field mapping of basement (literally in some cases) rocks in the New York Metropolitan area: Baskerville, C. A.; and Merguerian, Charles, 1982, Tectonic history of the New York Metropolitan area (abs

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

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIX ECoopButte County,Camilla,ThermalCubaParker, SouthCity of SaintOhioSpencer,Charles,

  15. OPEN-ENDED CONFIGURATIONS OF RADIO TELESCOPES

    E-Print Network [OSTI]

    Kreinovich, Vladik

    radio telescopes, devices that use the second observability window of radio waves. Why configurationsOPEN-ENDED CONFIGURATIONS OF RADIO TELESCOPES: A GEOMETRICAL ANALYSIS Vladik Kreinovich, Scott A. The quality of radio astronomical images drastically depends on where we place the radio telescopes. During

  16. Cherenkov Telescope Array Data Management

    E-Print Network [OSTI]

    Lamanna, G; Contreras, J L; Knödlseder, J; Kosack, K; Neyroud, N; Aboudan, A; Arrabito, L; Barbier, C; Bastieri, D; Boisson, C; Brau-Nogué, S; Bregeon, J; Bulgarelli, A; Carosi, A; Costa, A; De Cesare, G; Reyes, R de los; Fioretti, V; Gallozzi, S; Jacquemier, J; Khelifi, B; Kocot, J; Lombardi, S; Lucarelli, F; Lyard, E; Maier, G; Massimino, P; Osborne, J P; Perri, M; Rico, J; Sanchez, D A; Satalecka, K; Siejkowski, H; Stolarczyk, T; Szepieniec, T; Testa, V; Walter, R; Ward, J E; Zoli, A

    2015-01-01

    Very High Energy gamma-ray astronomy with the Cherenkov Telescope Array (CTA) is evolving towards the model of a public observatory. Handling, processing and archiving the large amount of data generated by the CTA instruments and delivering scientific products are some of the challenges in designing the CTA Data Management. The participation of scientists from within CTA Consortium and from the greater worldwide scientific community necessitates a sophisticated scientific analysis system capable of providing unified and efficient user access to data, software and computing resources. Data Management is designed to respond to three main issues: (i) the treatment and flow of data from remote telescopes; (ii) "big-data" archiving and processing; (iii) and open data access. In this communication the overall technical design of the CTA Data Management, current major developments and prototypes are presented.

  17. The Advanced Compton Telescope Mission

    E-Print Network [OSTI]

    Steven E. Boggs; James Kurfess; James Ryan; Elena Aprile; Neil Gehrels; Marc Kippen; Mark Leising; Uwe Oberlack; Cornelia Wunderer; Allen Zych; Peter Bloser; Michael Harris; Andrew Hoover; Alexei Klimenk; Dan Kocevski; Mark McConnell; Peter Milne; Elena I. Novikova; Bernard Phlips; Mark Polsen; Steven Sturner; Derek Tournear; Georg Weidenspointner; Eric Wulf; Andreas Zoglauer; Matthew Baring; John Beacom; Lars Bildsten; Charles Dermer; Dieter Hartmann; Margarita Hernanz; David Smith; Sumner Starrfield; for the larger ACT collaboration

    2006-08-24

    The Advanced Compton Telescope (ACT), the next major step in gamma-ray astronomy, will probe the fires where chemical elements are formed by enabling high-resolution spectroscopy of nuclear emission from supernova explosions. During the past two years, our collaboration has been undertaking a NASA mission concept study for ACT. This study was designed to (1) transform the key scientific objectives into specific instrument requirements, (2) to identify the most promising technologies to meet those requirements, and (3) to design a viable mission concept for this instrument. We present the results of this study, including scientific goals and expected performance, mission design, and technology recommendations.

  18. Large aperture diffractive space telescope

    DOE Patents [OSTI]

    Hyde, Roderick A. (Livermore, CA)

    2001-01-01

    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.

  19. Northwestern Charles Deering McCormick University Library Library of Special Collections

    E-Print Network [OSTI]

    Northwestern Charles Deering McCormick University Library Library of Special Collections Evanston political trends from a fascist perspective. Dr. Auhagen wrote regularly for the A.F.F.'s two serials, Today

  20. Public Information Charles W. Durham School of Architectural Engineering and Construction

    E-Print Network [OSTI]

    Powers, Robert

    Public Information for Charles W. Durham School of Architectural Engineering and Construction Construction Management (CM) Program #12;Table of Contents I. Institution Mission for Durham School of Architectural Engineering and Construction Construction Management (CM) Program I

  1. SEMI-ANNUAL REPORTS FOR LAKE CHARLES LNG EXPORT COMPANY, LLC...

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

    REPORTS FOR LAKE CHARLES EXPORTS, LLC - FE DKT. NO. 11-59-LNG - ORDER 3324 Summary of LNG Export Applications of the Lower 48 States EIS-0491: Draft Environmental Impact Statement...

  2. HIA 2015 DOE Zero Energy Ready Home Case Study: Charles Thomas...

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

    after Iowa. "Radon attaches to dust so the less dust, the less radon you get in your lungs," said Lowndes. To prove his point about the dust, Lowndes said Charles Thomas kept a...

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

    E-Print Network [OSTI]

    Taylor, Richard C.

    2010-01-01

    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...

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

    E-Print Network [OSTI]

    Merguerian, Charles

    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

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

    E-Print Network [OSTI]

    Haglund, Karl T

    1997-01-01

    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 ...

  6. Library of Charles Areskine (1680-1763): Scottish lawyers and book collecting, 1700-1760 

    E-Print Network [OSTI]

    Baston, Karen Grudzien

    2012-06-26

    The thesis uses the study of an individual’s book collection to examine wider themes in eighteenth century Scottish legal, social, political, and intellectual history. Charles Areskine’s library was made up of the books ...

  7. PRINCIPLES OF SEISMIC HOLOGRAPHY FOR DIAGNOSTICS OF THE SHALLOW SUBPHOTOSPHERE Charles Lindsey and D. C. Braun

    E-Print Network [OSTI]

    Braun, Douglas C.

    PRINCIPLES OF SEISMIC HOLOGRAPHY FOR DIAGNOSTICS OF THE SHALLOW SUBPHOTOSPHERE Charles Lindsey develop the wave-mechanical formalism for phase-correlation computational seismic holography headinggs: Sun: activity -- Sun: helioseismology -- sunspots 1. INTRODUCTION Computational seismic

  8. The use of turbulent jets to destratify the Charles River Basin

    E-Print Network [OSTI]

    Church, Jeffrey H. (Jeffrey Harrison)

    2012-01-01

    This study examines the feasibility of using turbulent jets to destratify the Lower Charles River Basin between the Longfellow and Craigie Bridges between Boston and Cambridge. The basin is currently filled with salt water ...

  9. Recent Results from Telescope Array

    E-Print Network [OSTI]

    Fukushima, M

    2015-01-01

    The Telescope Array (TA) is an experiment to observe Ultra-High Energy Cosmic Rays (UHECRs). TA's recent results, the energy spectrum and anisotropy based on the 6-year surface array data, and the primary composition obtained from the shower maximum Xmax are reported. The spectrum demonstrates a clear dip and cutoff. The shape of the spectrum is well described by the energy loss of extra-galactic protons interacting with the cosmic microwave background (CMB). Above the cutoff, a medium-scale (20 degrees radius) flux enhancement was observed near the Ursa-Major. A chance probability of creating this hotspot from the isotropic flux is 4.0 sigma. The measured Xmax is consistent with the primary being proton or light nuclei for energies 10^18.2 eV - 10^19.2 eV.

  10. Adaptive Optics for Large Telescopes

    SciTech Connect (OSTI)

    Olivier, S

    2008-06-27

    The use of adaptive optics was originally conceived by astronomers seeking to correct the blurring of images made with large telescopes due to the effects of atmospheric turbulence. The basic idea is to use a device, a wave front corrector, to adjust the phase of light passing through an optical system, based on some measurement of the spatial variation of the phase transverse to the light propagation direction, using a wave front sensor. Although the original concept was intended for application to astronomical imaging, the technique can be more generally applied. For instance, adaptive optics systems have been used for several decades to correct for aberrations in high-power laser systems. At Lawrence Livermore National Laboratory (LLNL), the world's largest laser system, the National Ignition Facility, uses adaptive optics to correct for aberrations in each of the 192 beams, all of which must be precisely focused on a millimeter scale target in order to perform nuclear physics experiments.

  11. Cross Calibration of Telescope Optical Throughput Efficiencies using Reconstructed Shower Energies for the Cherenkov Telescope Array

    E-Print Network [OSTI]

    Mitchell, A M W; Hofmann, W; Bernloehr, K

    2015-01-01

    For reliable event reconstruction of Imaging Atmospheric Cherenkov Telescopes (IACTs), calibration of the optical throughput efficiency is required. Within current facilities, this is achieved through the use of ring shaped images generated by muons. Here, a complementary approach is explored, achieving cross calibration of elements of IACT arrays through pairwise comparisons between telescopes, focussing on its applicability to the upcoming Cherenkov Telescope Array (CTA). Intercalibration of telescopes of a particular type using eventwise comparisons of shower image amplitudes has previously been demonstrated to recover the relative telescope optical responses. A method utilising the reconstructed energy as an alternative to image amplitude is presented, enabling cross calibration between telescopes of varying types within an IACT array. Monte Carlo studies for two plausible CTA layouts have shown that this calibration procedure recovers the relative telescope response efficiencies at the few percent level.

  12. Behavior Protocols: Fighting the "Spearhead" Problem* Charles University Prague, Faculty of Mathematics and Physics, Prague, Czech Republic.

    E-Print Network [OSTI]

    Behavior Protocols: Fighting the "Spearhead" Problem* J. Kofro Charles University Prague, Faculty: Fighting the "Spearhead" Problem approximate information about states, and (iii) use a symbolic state space

  13. 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,...

  14. "Thinking" Telescopes: An Autonomous Robotic Ecosystem for Persistent...

    Office of Scientific and Technical Information (OSTI)

    "Thinking" Telescopes: An Autonomous Robotic Ecosystem for Persistent Monitoring and Real-Time Response Citation Details In-Document Search Title: "Thinking" Telescopes: An...

  15. The Nuclear Spectroscopic Telescope Array (NuSTAR) Mission (Journal...

    Office of Scientific and Technical Information (OSTI)

    The Nuclear Spectroscopic Telescope Array (NuSTAR) Mission Citation Details In-Document Search Title: The Nuclear Spectroscopic Telescope Array (NuSTAR) Mission You are...

  16. The Nuclear Spectroscopic Telescope Array (NuSTAR) Mission (Journal...

    Office of Scientific and Technical Information (OSTI)

    The Nuclear Spectroscopic Telescope Array (NuSTAR) Mission Citation Details In-Document Search Title: The Nuclear Spectroscopic Telescope Array (NuSTAR) Mission Authors: Harrison,...

  17. The Nuclear Spectroscopic Telescope Array (NuSTAR) Mission (Journal...

    Office of Scientific and Technical Information (OSTI)

    Nuclear Spectroscopic Telescope Array (NuSTAR) Mission Citation Details In-Document Search Title: The Nuclear Spectroscopic Telescope Array (NuSTAR) Mission Authors: Harrison,...

  18. Merguerian, Charles, 1984, Revised stratigraphy of the Manhattan Schist, New York City. Field and petrographic data indicate that the "type" Manhattan Schist of Manhattan Island

    E-Print Network [OSTI]

    Merguerian, Charles

    Merguerian, Charles, 1984, Revised stratigraphy of the Manhattan Schist, New York City. Field of the stratigraphy is in progress. Merguerian, Charles, 1984, Revised stratigraphy of the Manhattan Schist, New York

  19. Merguerian, Charles, 1996a, Cameron's Line mylonite zone in Connecticut and New York City -evidence for Taconian accretionary tectonics.

    E-Print Network [OSTI]

    Merguerian, Charles

    Merguerian, Charles, 1996a, Cameron's Line mylonite zone in Connecticut and New York City, Charles, 1996a, Cameron's Line mylonite zone in Connecticut and New York City - evidence for Taconian miogeoclinal basement-cover rocks. Based on surface- and subsurface mapping in the New York-Connecticut segment

  20. Charles University Information System Compiled 21.1.2015 12:12:02 by Document Globe 1

    E-Print Network [OSTI]

    Cerveny, Vlastislav

    Charles University Information System Compiled 21.1.2015 12:12:02 by Document Globe ® 1 This page is the entry point to the Charles University Information System and its applications: · Study Information information about the system and its operations #12;

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

    Office of Science (SC) Website

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power AdministrationRobust,Field-effectWorkingLosThe 26thI D- 6 0GrantsTheBurtonCertified FederalCharles C.Charles E.

  2. Charles Roger Alcock, 1996 | U.S. DOE Office of Science (SC)

    Office of Science (SC) Website

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power AdministrationRobust,Field-effectWorkingLosThe 26thI D- 6 0GrantsTheBurtonCertified FederalCharles C.Charles

  3. Charles V. Shank, 2014 | U.S. DOE Office of Science (SC)

    Office of Science (SC) Website

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power AdministrationRobust,Field-effectWorkingLosThe 26thI D- 6 0GrantsTheBurtonCertified FederalCharlesCharles V.

  4. Telescopic nanotube device for hot nanolithography

    DOE Patents [OSTI]

    Popescu, Adrian; Woods, Lilia M

    2014-12-30

    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.

  5. Active Optics in Modern, Large Optical Telescopes

    E-Print Network [OSTI]

    Lothar Noethe

    2001-11-07

    Active optics is defined as the control of the shape and the alignment of the components of an optical system at low temporal frequencies. For modern large telescopes with flexible monolithic or segmented primary mirrors and also flexible structures this technique is indispensable to reach a performance which is either diffraction limited for an operation in space or limited by the atmosphere for an operation on the ground. This article first describes the theory of active optics, both of the wavefront analysis and the correction mechanisms, then the design of three representative active optics systems, two in telescopes of the four and eight meter class with meniscus mirrors and one in a telescope with a segmented primary mirror, and, finally, presents practical experience with these active optics systems.

  6. Accurate Telescope Mount Positioning with MEMS Accelerometers

    E-Print Network [OSTI]

    Mészáros, László; Pál, András; Csépány, Gergely

    2014-01-01

    This paper describes the advantages and challenges of applying microelectromechanical accelerometer systems (MEMS accelerometers) in order to attain precise, accurate and stateless positioning of telescope mounts. This provides a completely independent method from other forms of electronic, optical, mechanical or magnetic feedback or real-time astrometry. Our goal is to reach the sub-arcminute range which is well smaller than the field-of-view of conventional imaging telescope systems. Here we present how this sub-arcminute accuracy can be achieved with very cheap MEMS sensors and we also detail how our procedures can be extended in order to attain even finer measurements. In addition, our paper discusses how can a complete system design be implemented in order to be a part of a telescope control system.

  7. Information Sharing and Security in Dynamic Coalitions Charles E. Phillips, Jr.

    E-Print Network [OSTI]

    Lee, Ruby B.

    Information Sharing and Security in Dynamic Coalitions Charles E. Phillips, Jr. Computer Science in one crisis and adversaries in another, raising difficult security issues with respect to information on the information sharing and security risks when coalitions are formed in response to a crisis. This paper defines

  8. Charles Loring Brace and Dangerous Classes: Historical Analogues of the Urban Black Poor

    E-Print Network [OSTI]

    Cordasco, Francesco

    1971-01-01

    An overview of the work of Charles Loring Brace (1826-1890), one of the founders of the Children's Aid Study, and with particular attention to Brace's The Dangerous Classes of New York and Twenty Years' Work Among Them (1872). Brace was one...

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

    E-Print Network [OSTI]

    Stanford University

    Making Automated Building Code Checking A Reality1 Charles S. Han, John Kunz, Kincho H. Law Center for automated code-checking to be successful, the program that does the analysis of a building design must set of building codes. The complexity and changing nature of codes leads to delays in both the design

  10. The Life of Charles O. Fuller in Central Kansas, 1855-1879.

    E-Print Network [OSTI]

    Stratton, John M.

    2004-02-01

    The article presents a biography of Charles Oscar Fuller, 1928-1979, who established a ranch on Running Turkey Creek along the Santa Fe Trail n what is now McPherson County, Kansas. Fuller went on to other pursuits later in life, and served a term...

  11. Mechanism Mobility and a Local Dimension Test Charles W. Wampler1,2,

    E-Print Network [OSTI]

    Hauenstein, Jonathan

    is mathematically equivalent to the dimension of the solution set of the kinematic loop equations for the mechanismMechanism Mobility and a Local Dimension Test Charles W. Wampler1,2, General Motors Research The mobility of a mechanism is the number of degrees of freedom (DOF) with which it may move. This notion

  12. Improved Method for Specifying Solar Wind Speed Near the Sun Charles N. Arge*

    E-Print Network [OSTI]

    California at Berkeley, University of

    much better than one derived previously, which is a function of fs only. We focus here on the solarImproved Method for Specifying Solar Wind Speed Near the Sun Charles N. Arge* , Dusan Odstrcil solar wind flow speed near the Sun (~0.1 AU) us- ing a set of three simple inter-linked coronal/solar

  13. Apple watch: has its time come? Charles Arthur for guardian.co.uk

    E-Print Network [OSTI]

    South Bohemia, University of

    Apple watch: has its time come? Charles Arthur for guardian.co.uk Apple's next big thing will be a "smart watch" which will "fill a gaping hole in the Apple ecosystem" ­ at least according to one already being worked on inside Apple. With the company being sued by Greenlight Capital for hoarding its

  14. The Charles E. Via, Jr. Department of Civil and Environmental Engineering

    E-Print Network [OSTI]

    The Charles E. Via, Jr. Department of Civil and Environmental Engineering No. 27 #12;ON THE COVER to the Virginia Tech Chapters of the American Society of Civil Engineers and the American Institute of Steel: One of the engineers who traveled to the affected areas of the New Jersey shoreline after Hurricane

  15. 1. Charles Clore International House 2. David Lopatie Conference Centre; Caf Mada

    E-Print Network [OSTI]

    1. Charles Clore International House 2. David Lopatie Conference Centre; Café Mada 3. Barbara and Naomi Cohen Building 62. Mexico Building 63. Leon and Gina Fromer Building (main library) 64. Ecological Rd. Hanasi Harishon St. Pinsker St. Kipnis Residences Weizmann Estate Gate House Davidson Gate a b e

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

    E-Print Network [OSTI]

    Bailey, Scott

    . The heating leads to an increase in the density of nitric oxide at 140 km in the thermosphere. On some lead to increases in nitric oxide density at 110 km at the equator. [4] One of the reasons for studyingJoule heating and nitric oxide in the thermosphere, 2 Charles A. Barth1 Received 14 April 2010

  17. Electron-Nuclear-Double-Resonance Quantum Computer Jonathan P. Dowling and Charles M. Bowden

    E-Print Network [OSTI]

    Dowling, Jonathan P.

    Electron-Nuclear-Double-Resonance Quantum Computer Jonathan P. Dowling and Charles M. Bowden consider the use of Electron-Nuclear Double Resonance (ENDOR) techniques in quantum computing. ENDOR have sufficient resolution for quantum computing applications. Key Words: Quantum Computing, Nuclear

  18. A SUBBAND HYBRID BEAMFORMING FOR IN-CAR SPEECH ENHANCEMENT Charles Fox

    E-Print Network [OSTI]

    Badeau, Roland

    A SUBBAND HYBRID BEAMFORMING FOR IN-CAR SPEECH ENHANCEMENT Charles Fox , Guillaume Vitte , Maurice is pre- sented, dedicated to in-car communication. An experimental study of the acoustic field inside the car interior leads us to propose a hy- brid beamforming algorithm, taking two frequency ranges into ac

  19. BASICS OF DESIGN AND CONSTRUCTION OF A HUMAN POWERED SUBMARINE 'CharlesR. Lockert

    E-Print Network [OSTI]

    Wood, Stephen L.

    BASICS OF DESIGN AND CONSTRUCTION OF A HUMAN POWERED SUBMARINE 'CharlesR. Lockert Florid used by the author on the design and construction of the human powered submarine "Sea Panther Panther1!and the rational for those decisions. INTRODUCTION The design and construction of a human powered

  20. Merguerian, Charles; Baskerville, C. A.; and Harris, James, 1983, Engineering geology of New York City.

    E-Print Network [OSTI]

    Merguerian, Charles

    ; Baskerville, C. A.; and Harris, James, 1983, Engineering geology of New York City (abs.): Empire State GeogramMerguerian, Charles; Baskerville, C. A.; and Harris, James, 1983, Engineering geology of New York City. Bedrock geologic mapping of Manhattan Island has delineated an areally extensive, polydeformed

  1. Transdisciplinary electric power grid science Charles D. Brummitta,b,1

    E-Print Network [OSTI]

    D'Souza, Raissa

    OPINION Transdisciplinary electric power grid science Charles D. Brummitta,b,1 , Paul D. H. Hinesc-long feedbacks surrounding electrical infrastructure (includ- ing weather, policy, public sentiment, mar- kets storm damage or build distributed generation?). The "smart grid," which monitors and controls electrical

  2. Planning Glossary CharlesF.Schwarz EdwardC.Thor GaryH.Elsner

    E-Print Network [OSTI]

    . Oxford: 911(038)­(73) Retrieval Terms: wildland planning; land utilization; range management; forestWildland Planning Glossary CharlesF.Schwarz EdwardC.Thor GaryH.Elsner PACIFIC SOUTHWEST Forest., Edward C. Thor, and Gary H. Elsner. 1976. Wildland planning glossary. USDA Forest Serv. Gen Tech. Rep

  3. Sediment production from forest roads in western Oregon Charles H. Luce and Thomas A. Black

    E-Print Network [OSTI]

    Sediment production from forest roads in western Oregon Charles H. Luce and Thomas A. Black USDA erosion from forest roads requires an understanding of how road design and maintenance affect sediment the relationship between sediment production and road attributes such as distance between culverts, road slope

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

    E-Print Network [OSTI]

    Hilde, Thomas Christian

    1994-01-01

    the bourgeois New England manners of James nor the oblivious intensity of Charles Peirce. He was immensely, almost destructively, proud, yet deeply insecure about the indelible mark of the province, of the "out there", that he carried with him in Cambridge...

  5. MIDDLE SACRAMENTO RIVER REFUGE: A FEASIBILITY STUDY1 Charles J. Houghten and Frank J. Michny2

    E-Print Network [OSTI]

    MIDDLE SACRAMENTO RIVER REFUGE: A FEASIBILITY STUDY1 Charles J. Houghten and Frank J. Michny2 1 Resources Specialist, U.S. Fish and Wildlife Service, Division of Refuges and Wildlife Resources, Sacramento, Sacramento, California. The woodlands and other streamside habitat of the Sacramento River's riparian system

  6. Efficiencyof current drive by fast waves CharlesF. F. Karneyand NathanielJ. Fisch

    E-Print Network [OSTI]

    Karney, Charles

    Efficiencyof current drive by fast waves CharlesF. F. Karneyand NathanielJ. Fisch Plasma Physics Antonsen and Chu can then be used to calculatethe efficiencyof current driveby fast waves in a relativistic plasma. Accurate numerical results and analytic asymptotic limits for the efficienciesare given. I

  7. Electrical Engineering Graduate Handbook Charles L. Brown Department of Electrical & Computer Engineering

    E-Print Network [OSTI]

    Zhigilei, Leonid V.

    1 Electrical Engineering Graduate Handbook 2014-2015 Charles L. Brown Department of Electrical outlines the policies and procedures of the graduate program of the Department of Electrical and Computer from the Chairman Electrical engineers continue to provide technological leadership for developments

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

    E-Print Network [OSTI]

    Hill, Jeffrey E.

    FA17 Fertilization of Fresh Water Fish Ponds 1 Craig Watson and Charles E. Cichra2 1. This document to increase productivity of a field. One can also increase the productiv- ity of a pond by adding fertilizer, then pond fertilization can increase the production of these fish. Fertilizers provide nutrients

  9. Optimal Control of a Magnetic Bearing without Bias Flux Using Finite Voltage Charles Yang *, Research Assistant

    E-Print Network [OSTI]

    Knospe, Carl

    Optimal Control of a Magnetic Bearing without Bias Flux Using Finite Voltage Charles Yang, Sterling Heights, MI 48314 SUMMARY Conventional Active Magnetic Bearings (AMB) are operated using a bias. In this paper, optimal control of a magnetic bearing without bias is investigated. A single degree

  10. Merguerian, Charles, 1983a, The structural geology of Manhattan Island, New York City (NYC), New York.

    E-Print Network [OSTI]

    Merguerian, Charles

    Merguerian, Charles, 1983a, The structural geology of Manhattan Island, New York City (NYC), New of Manhattan Island, New York City (NYC), New York (abs.): Geological Society of America Abstracts York. A lithically distinct assemblage of massive, nodular sillimanite-rich schist and gneiss

  11. A Client/Server Framework for On-line Building Code Charles S. Han1

    E-Print Network [OSTI]

    Stanford University

    -4020 Abstract This paper outlines an integrated client/server framework for an automated code- checking system to develop an effective system to analyze a design for code-compliance. Key Words automation, building codesA Client/Server Framework for On-line Building Code Checking Charles S. Han1 , John C. Kunz2

  12. The Kilodegree Extremely Little Telescope (KELT): A Small Robotic Telescope for Large-Area Synoptic Surveys

    E-Print Network [OSTI]

    Joshua Pepper; Richard W. Pogge; D. L. DePoy; J. L. Marshall; K. Z. Stanek; Amelia M. Stutz; Shawn Poindexter; Robert Siverd; Thomas P. O'Brien; Mark Trueblood; Patricia Trueblood

    2007-07-30

    The Kilodegree Extremely Little Telescope (KELT) project is a survey for planetary transits of bright stars. It consists of a small-aperture, wide-field automated telescope located at Winer Observatory near Sonoita, Arizona. The telescope surveys a set of 26 x 26 degree fields, together covering about 25% of the Northern sky, targeting stars in the range of 8

  13. Prototype of the SST-1M Telescope Structure for the Cherenkov Telescope Array

    E-Print Network [OSTI]

    Niemiec, J; B?ocki, J; Bogacz, L; Borkowski, J; Bulik, T; Cadoux, F; Christov, A; Cury?o, M; della Volpe, D; Dyrda, M; Favre, Y; Frankowski, A; Grudnik, ?; Grudzi?ska, M; Heller, M; Id?kowski, B; Jamrozy, M; Janiak, M; Kasperek, J; Lalik, K; Lyard, E; Mach, E; Mandat, D; Marsza?ek, A; Micha?owski, J; Moderski, R; Montaruli, T; Neronov, A; Ostrowski, M; Pa?ko, P; Pech, M; Porcelli, A; Prandini, E; Rajda, P; Rameez, M; Schioppa, E jr; Schovanek, P; Seweryn, K; Skowron, K; Sliusar, V; Sowi?ski, M; Stawarz, ?; Stodulska, M; Stodulski, M; Pujadas, I Troyano; Toscano, S; Walter, R; Wi?cek, M; Zagda?ski, A; Zi?tara, K

    2015-01-01

    A single-mirror small-size (SST-1M) Davies-Cotton telescope with a dish diameter of 4 m has been built by a consortium of Polish and Swiss institutions as a prototype for one of the proposed small-size telescopes for the southern observatory of the Cherenkov Telescope Array (CTA). The design represents a very simple, reliable, and cheap solution. The mechanical structure prototype with its drive system is now being tested at the Institute of Nuclear Physics PAS in Krakow. Here we present the design of the prototype and results of the performance tests of the structure and the drive and control system.

  14. Optical Technology Needs for Future Space Telescopes

    E-Print Network [OSTI]

    Van Stryland, Eric

    , Visible, Near-IR, Far-IR, Sub-MM, Microwave, Radio Wave, Gravity Waves, etc. See Advanced Telescope / Spectroscopy (Vis-IR-FIR) Multi-Spectral Sensing (UV-Gamma) Laser / LIDAR Remote Sensing Microwave Instruments Structure #12;NASA's Science Missions Directorate Themes: Earth Science Sun-Solar System Connection Solar

  15. Dutch Open Telescope Virtual Solar Observatory

    E-Print Network [OSTI]

    Rutten, Rob

    telescope building. The DOT is open and is mounted on a 15 m high open tower to exploit the superior atmospheric seeing at La Palma brought by the oceanic trade wind. The clamshell bad-weather canopy is folded to feed the solar physics research by the small DOT group at Utrecht, but very much underexploits

  16. A Medium Sized Schwarzschild-Couder Cherenkov Telescope Mechanical Design Proposed for the Cherenkov Telescope Array

    E-Print Network [OSTI]

    Byrum, K; Benbow, W; Cameron, R; Criswell, S; Errando, M; Guarino, V; Kaaret, P; Kieda, D; Mukherjee, R; Naumann, D; Nieto, D; Northrop, R; Okumura, A; Roache, E; Rousselle, J; Schlenstedt, S; Sternberger, R; Vassiliev, V; Wakely, S; Zhao, H

    2015-01-01

    The Cherenkov Telescope Array (CTA) is an international next-generation ground-based gamma-ray observatory. CTA will be implemented as southern and northern hemisphere arrays of tens of small, medium and large-sized imaging Cherenkov telescopes with the goal of improving the sensitivity over the current-generation experiments by an order of magnitude. CTA will provide energy coverage from ~20 GeV to more than 300 TeV. The Schwarzschild-Couder (SC) medium size (9.5m) telescopes will feature a novel aplanatic two-mirror optical design capable of accommodating a wide field-of-view with significantly improved angular resolution as compared to the traditional Davies-Cotton optical design. A full-scale prototype SC medium size telescope structure has been designed and will be constructed at the Fred Lawrence Whipple Observatory in southern Arizona during the fall of 2015. concentrate on the novel features of the design.

  17. Analysis of Thermal Conditions of the 6-m BTA Telescope Elements and the Telescope Dome Space

    E-Print Network [OSTI]

    Emelianov, E V

    2015-01-01

    The results obtained using the temperature monitoring systems of the 6-m BTA telescope primary mirror, dome space, and external environment are reported. We consider the factors that affect the development of microturbulence in the near-mirror air layer and inside the dome space, variation of the telescope focal length with the temperature of its structures, variation of seeing due to temperature gradients inside the primary mirror of the 6-m telescope. The methods used in various observatories for reducing microturbulence are analyzed. We formulate suggestions concerning the improvement of the temperature monitoring system currently in operation and the system of automatic adjustment of the telescope focal length to compensate the thermal drift of the focus during observations.

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

    E-Print Network [OSTI]

    Langmuir, Charles H.

    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

  19. The New Hampshire Astronomical Society Library Telescope Program

    E-Print Network [OSTI]

    The New Hampshire Astronomical Society Library Telescope Program The NHAS's Library Telescope are borrowed. Over the past three years NHAS has placed telescopes in nearly 30 New Hampshire libraries is a clinical social worker in private practice. Some may even recognize him as New Hampshire's most favorite

  20. Hubble Space Telescope characterized by using phase-retrieval algorithms

    E-Print Network [OSTI]

    Fienup, James R.

    of the optical axis of a camera relay telescope relative to the main telescope. After we accounted for measured spherical aberration in the relay telescope,our estimate of the conicconstant of the primary mirror ofthe with the results of a blind test that was distributed to several groups. Section 4 describes some of the parameters

  1. Large fully retractable telescope enclosures still closable in strong wind

    E-Print Network [OSTI]

    Rutten, Rob

    are too small to deteriorate the image in normal observing situations with wind speeds up to 20 mLarge fully retractable telescope enclosures still closable in strong wind Felix C.M. Bettonvil a the telescopes are in operation. The telescopes and enclosures also operate in hard wind. The prototypes

  2. AUTOMATIC GUIDING OF THE PRIMARY IMAGE OF SOLAR GREGORY TELESCOPES

    E-Print Network [OSTI]

    AUTOMATIC GUIDING OF THE PRIMARY IMAGE OF SOLAR GREGORY TELESCOPES G. KÜVELER1, E. WIEHR2, D of solar Gregory telescopes is used for automatic guiding. This new system avoids temporal varying at the Gregory telescopes at Tenerife and at Locarno, is described. 1. Introduction Automatic guiding

  3. GLAST Large Area Telescope Multiwavelength Planning

    E-Print Network [OSTI]

    O. Reimer; P. F. Michelson; R. A. Cameron; S. W. Digel; D. J. Thompson; K. S. Wood

    2006-11-21

    Gamma-ray astrophysics depends in many ways on multiwavelength studies. The Gamma-ray Large Area Space Telescope (GLAST) Large Area Telescope (LAT) Collaboration has started multiwavelength planning well before the scheduled 2007 launch of the observatory. Some of the high-priority multiwavelength needs include: (1) availability of contemporaneous radio and X-ray timing of pulsars; (2) expansion of blazar catalogs, including redshift measurements; (3) improved observations of molecular clouds, especially at high galactic latitudes; (4) simultaneous broad-band blazar monitoring; (5) characterization of gamma-ray transients, including gamma ray bursts; (6) radio, optical, X-ray and TeV counterpart searches for reliable and effective sources identification and characterization. Several of these activities are needed to be in place before launch.

  4. The Automated Palomar 60-Inch Telescope

    E-Print Network [OSTI]

    S. Bradley Cenko; Derek B. Fox; Dae-Sik Moon; Fiona A. Harrison; S. R. Kulkarni; John R. Henning; C. Dani Guzman; Marco Bonati; Roger M. Smith; Robert P. Thicksten; Michael W. Doyle; Hal L. Petrie; Avishay Gal-Yam; Alicia M. Soderberg; Nathaniel L. Anagnostou; Anastasia C. Laity

    2006-08-15

    We have converted the Palomar 60-inch telescope (P60) from a classical night assistant-operated telescope to a fully robotic facility. The automated system, which has been operational since September 2004, is designed for moderately fast (t <~ 3 minutes) and sustained (R <~ 23 mag) observations of gamma-ray burst afterglows and other transient events. Routine queue-scheduled observations can be interrupted in response to electronic notification of transient events. An automated pipeline reduces data in real-time, which is then stored on a searchable web-based archive for ease of distribution. We describe here the design requirements, hardware and software upgrades, and lessons learned from roboticization. We present an overview of the current system performance as well as plans for future upgrades.

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

    E-Print Network [OSTI]

    Bryan N.S. Gooch

    2002-01-01

    still monarch is, in many ways, re- markable; good luck and wily management were locked in serious struggle with stubbornness, bouts of dangerous ineptitude, and numerous forays in social and diplomatic impropriety. Coote spares few sensibilities...) in the Boscobel oak tree (see 107- 8) is part of the story?and it has all the marks of deadly suspense, intrigue, and danger, stunningly reminding the reader just how close the Cromwellian side came to eliminating any chance of Charles? restoration. Chapter Six...

  6. A review of "A Companion to Juan Luis Vives" by Charles Fantazzi 

    E-Print Network [OSTI]

    Wright, Elizabeth R.

    2010-01-01

    Armas Wilson, and Isabel Lozano Renieblas when seeking to understand The Labors of Persiles and Sigismunda. Charles Fantazzi. A Companion to Juan Luis Vives. Leiden and Boston: Brill, 2008. viii + 430 pp. $185.00. Review by elizabeth r. wright..., university of georgia. This volume offers detailed analysis and rigorous contextual- ization of the diverse writings of Juan Luis Vives (Valencia, Spain 1492/93?Bruges, Belgium, 1540). In the course of some sixty differ- ent publications, this Valencian...

  7. A review of "The Regicides and the Execution of Charles I." by Jason Peacey, ed. 

    E-Print Network [OSTI]

    Michael Rogers

    2003-01-01

    obligation when it permitted the king?s death. 86 SEVENTEENTH-CENTURY NEWS The remaining chapters apply similar methodologies to several different facets of the Regicide. Sean Kelsey and Alan Orr analyze the trial itself and its vocabulary. Kelsey?s.... Alan Orr, in ?The Juristic Founda- tions of Regicide? clearly analyzes the legal vocabulary of the High Court of Justice?s treason charge against Charles, and demonstrates how that vocabulary blended English with Roman law concepts. Again we see...

  8. Telescoping magnetic ball bar test gage

    DOE Patents [OSTI]

    Bryan, J.B.

    1982-03-15

    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.

  9. The Small and Moderate Aperture Research Telescope System A Proposal to Operate the Small Telescopes at CTIO

    E-Print Network [OSTI]

    Walter, Frederick M.

    The Small and Moderate Aperture Research Telescope System (SMARTS) A Proposal to Operate the Small Observatory #12; The Small and Moderate Aperture Research Telescope System (SMARTS) ABSTRACT We propose to operate four telescopes located at the Cerro Tololo Interamerican Observatory (CTIO) for the period from

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

    SciTech Connect (OSTI)

    Cameron, Robert A.

    2012-06-28

    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.

  11. ANTARES deep sea neutrino telescope results

    SciTech Connect (OSTI)

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

    2014-01-01

    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.

  12. Review of the Solar Array Telescopes

    E-Print Network [OSTI]

    David A. Smith

    2006-08-11

    For several years the only experiments sensitive to astrophysical gamma rays with energies beyond the reach of EGRET but below that of the Cherenkov imaging telescopes have been the "solar tower" detectors. They use >2000 m2 mirror areas to sample the Cherenkov wavefront generated by <100 GeV gamma rays, obtaining Crab sensitivities of more than 6$\\sigma$ in one ON-source hour. I will review the history of the solar tower Cherenkov experiments from 1992 to the present and their key design features. I will describe some successful analysis strategies, then summarize the principal results obtained.

  13. The X-ray Telescope of CAST

    E-Print Network [OSTI]

    M. Kuster; H. Bräuninger; S. Cébrian; 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. Königsmann; R. Kotthaus; T. Papaevangelou; C. Lasseur; A. Lippitsch; G. Lutz; J. Morales; A. Rodríguez; L. Strüder; J. Vogel; K. Zioutas

    2007-05-10

    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.

  14. Fermi Large Area Telescope Third Source Catalog

    E-Print Network [OSTI]

    ,

    2015-01-01

    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...

  15. Beam calibration of radio telescopes with drones

    E-Print Network [OSTI]

    Chang, Chihway; Refregier, Alexandre; Amara, Adam; Glauser, Adrian; Casura, Sarah

    2015-01-01

    We present a multi-frequency far-field beam map for the 5m dish telescope at the Bleien Observatory measured using a commercially available drone. We describe the hexacopter drone used in this experiment, the design of the flight pattern, and the data analysis scheme. This is the first application of this calibration method to a single dish radio telescope in the far-field. The high signal-to-noise data allows us to characterise the beam pattern with high accuracy out to at least the 4th side-lobe. The resulting 2D beam pattern is compared with that derived from a more traditional calibration approach using an astronomical calibration source. We discuss the advantages of this method compared to other beam calibration methods. Our results show that this drone-based technique is very promising for ongoing and future radio experiments, where the knowledge of the beam pattern is key to obtaining high-accuracy cosmological and astronomical measurements.

  16. The University of Durham Mark 6 VHE gamma ray telescope

    SciTech Connect (OSTI)

    Chadwick, P. M.; Dickinson, M. R.; Dipper, N. A.; Holder, J.; Kendall, T. R.; McComb, T. J. L.; Orford, K. J.; Rayner, S. M.; Roberts, I. D.; Shaw, S. E.; Turver, K. E.

    1997-05-10

    The operation of the University of Durham Mark 6 atmospheric Cerenkov telescope is discussed. The telescope has been used to detect gamma rays at energies {>=}150 GeV and to achieve good discrimination between gamma ray and hadron initiated showers, using both conventional imaging and novel fluctuation measures. The telescope was commissioned in 1995 and a description of its operation is presented. Verification of the performance during observations of PSR B1706-44 is described.

  17. 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]

    Merguerian, Charles

    Sanders, J. E.; and Merguerian, Charles, 1995b, New York City region: Unique testing ground This Abstract: 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

  18. * Correspondence to: C. H. Morrell, Mathematical Sciences Department, Loyola College, 4501 North Charles Street, Baltimore, MD 21210 U.S.A.

    E-Print Network [OSTI]

    Morrell, Christopher H.

    Charles Street, Baltimore, MD 21210 U.S.A. Contract grant sponsor: National Institute on Deafness North Charles Street, Baltimore, MD 21210 U.S.A. Longitudinal Studies Branch, Gerontology Research Center, National Institute on Aging, Baltimore, MD 21224, U.S.A. Hearing and Speech Sciences, University

  19. The Robotic Super-LOTIS Telescope: Results & Future Plans

    E-Print Network [OSTI]

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

    2008-02-29

    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.

  20. A generation of astronomical telescopes, their users, and publications

    E-Print Network [OSTI]

    Trimble, V

    2010-01-01

    optical telescopes. Publications of the Astronomical Society737. Abt, H. A. (2009). Publications of the Astronomicaltelescopes, their users, and publications Table 3 Papers and

  1. Early science with the large millimeter telescope: exploring...

    Office of Scientific and Technical Information (OSTI)

    Early science with the large millimeter telescope: exploring the effect of AGN activity on the relationships between molecular gas, dust, and star formation Citation Details...

  2. SIMULATION STUDY OF BACKGROUND PARTICLES IN THE MUON TELESCOPE...

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

    SIMULATION STUDY OF BACKGROUND PARTICLES IN THE MUON TELESCOPE DETECTOR AT THE STAR EXPERIMENT Matthew Breen Thanks to Dr. Mioduszewski and Yanfang Liu Overview Background ...

  3. The Atacama Cosmology Telescope: Cosmology from Galaxy Clusters...

    Office of Scientific and Technical Information (OSTI)

    The Atacama Cosmology Telescope: Cosmology from Galaxy Clusters Detected via the Sunyaev-Zel'dovich Effect Citation Details In-Document Search Title: The Atacama Cosmology...

  4. A review of "The Spanish Match: Prince Charles’ Journey to Madrid, 1623." by Alexander Samson ed. 

    E-Print Network [OSTI]

    Pursell, Brennan C.

    2007-01-01

    of Wales in Madrid was sensa- tional in its own day and makes for one of the best stories of the early seventeenth century. Alexander Samson?s delightful volume is the result of an interdisciplinary gathering of experts in the fields of early modern...-CENTURY NEWS Alexander Samson, ed. The Spanish Match: Prince Charles? Journey to Madrid, 1623. Aldershot, Hampshire: Ashgate, 2006. x + 243 pp. + 20 illus. $99.95. Review by BRENNAN C. PURSELL, DESALES UNIVERSITY. The sudden appearance of the Prince...

  5. Charles C. Cremer, 1972 | U.S. DOE Office of Science (SC)

    Office of Science (SC) Website

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power AdministrationRobust,Field-effectWorkingLosThe 26thI D- 6 0GrantsTheBurtonCertified FederalCharles C. Cremer,

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

    Office of Science (SC) Website

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power AdministrationRobust,Field-effectWorkingLosThe 26thI D- 6 0GrantsTheBurtonCertified FederalCharles C.

  7. Charles V. Jakowatz, 1996 | U.S. DOE Office of Science (SC)

    Office of Science (SC) Website

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power AdministrationRobust,Field-effectWorkingLosThe 26thI D- 6 0GrantsTheBurtonCertified FederalCharles

  8. Lake Charles Carbon Capture and Sequestration Project U. S. Department of Energy

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

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration would likeUniverseIMPACTThousand CubicResourcelogo and mastheadLake Charles Carbon Capture and

  9. Liquid Mirror Telescopes: A progress report

    E-Print Network [OSTI]

    Ermanno F. Borra; Marc Ferrari; Luc Girard; Gilberto Moretto; Gregoire Tremblay; Gerard Lemaitre

    1996-08-23

    We review the present status of liquid mirror telescopes. Interferometric tests of liquid mirrors (the largest one having a diameter of 2.5 meters ) show excellent optical qualities. The basic technology is now sufficiently reliable that it can be put to work. Indeed, a handful of liquid mirrors have now been built that are used for scientific work. A 3.7-m diameter LMT is presently being built in the new Laval upgraded testing facilities. Construction of the mirror can be followed on the Web site: http://astrosun.phy.ulaval.ca/lmt/lmt- home.html. Finally we address the issue of the field accessible to LMTs equipped with novel optical correctors. Optical design work, and some exploratory laboratory work, indicate that a single LMT should be able to access, with excellent images, small regions anywhere inside fields as large as 45 degrees.

  10. The AMiBA Hexapod Telescope Mount

    E-Print Network [OSTI]

    Koch, Patrick M; Nishioka, Hiroaki; Jiang, Homin; Lin, Kai-Yang; Umetsu, Keiichi; Huang, Yau-De; Raffin, Philippe; Chen, Ke-Jung; Ibanez-Romano, Fabiola; Chereau, Guillaume; Chen, Ming-Tang; Ho, Paul T P; Pausch, Konrad; Willmeroth, Klaus; Altamirano, Pablo; Chang, Chia-Hao; Chang, Shu-Hao; Chang, Su-Wei; Han, Chih-Chiang; Kubo, Derek; Li, Chao-Te; Liu, Guo-Chin; Martin-Cocher, Pierre; Oshiro, Peter; Wei, Ta-Shun; Birkinshaw, Mark; Lancaster, Katy; Lo, Kwok Yung; Martin, Robert N; Molnar, Sandor M; Patt, Ferdinand; Romeo, Bob

    2009-01-01

    AMiBA is the largest hexapod astronomical telescope in current operation. We present a description of this novel hexapod mount with its main mechanical components -- the support cone, universal joints, jack screws, and platform -- and outline the control system with the pointing model and the operating modes that are supported. The AMiBA hexapod mount performance is verified based on optical pointing tests and platform photogrammetry measurements. The photogrammetry results show that the deformations in the inner part of the platform are less than 120 micron rms. This is negligible for optical pointing corrections, radio alignment and radio phase errors for the currently operational 7-element compact configuration. The optical pointing error in azimuth and elevation is successively reduced by a series of corrections to about 0.4 arcmin rms which meets our goal for the 7-element target specifications.

  11. Using SPICA Space Telescope to characterize Exoplanets

    E-Print Network [OSTI]

    J. R. Goicoechea; B. Swinyard; G. Tinetti; T. Nakagawa; K. Enya; M. Tamura; M. Ferlet; K. G. Isaak; M. Wyatt; A. D. Aylward; M. Barlow; J. P. Beaulieu; A. Boccaletti; J. Cernicharo; J. Cho; R. Claudi; H. Jones; H. Lammer; A. Leger; J. Martín-Pintado; S. Miller; F. Najarro; D. Pinfield; J. Schneider; F. Selsis; D. M. Stam; J. Tennyson; S. Viti; G. White

    2008-09-15

    We present the 3.5m SPICA space telescope, a proposed Japanese-led JAXA-ESA mission scheduled for launch around 2017. The actively cooled ( 18 um). SPICA is one of the few space missions selected to go to the next stage of ESA's Cosmic Vision 2015-2025 selection process. In this White Paper we present the main specifications of the three instruments currently baselined for SPICA: a mid-infrared (MIR) coronagraph (~3.5 to ~27 um) with photometric and spectral capabilities (R~200), a MIR wide-field camera and high resolution spectrometer (R~30,000), and a far-infrared (FIR ~30 to ~210 um) imaging spectrometer - SAFARI - led by a European consortium. We discuss their capabilities in the context of MIR direct observations of exo-planets (EPs) and multiband photometry/high resolution spectroscopy observations of transiting exo-planets. We conclude that SPICA will be able to characterize the atmospheres of transiting exo-planets down to the super-Earth size previously detected by ground- or space-based observatories. It will also directly detect and characterize Jupiter/Neptune-size planets orbiting at larger separation from their parent star (>5-10 AU), by performing quantitative atmospheric spectroscopy and studying proto-planetary and debris disks. In addition, SPICA will be a scientific and technological precursor for future, more ambitious, IR space missions for exo-planet direct detection as it will, for example, quantify the prevalence exo-zodiacal clouds in planetary systems and test coronographic techniques, cryogenic systems and lightweight, high quality telescopes. (abridged)

  12. Flasher and muon-based calibration of the GCT telescopes proposed for the Cherenkov Telescope Array

    E-Print Network [OSTI]

    Brown, Anthony M; Chadwick, Paula M; Daniel, Michael; White, Richard

    2015-01-01

    The GCT is a dual-mirror Small-Sized-Telescope prototype proposed for the Cherenkov Telescope Array. Calibration of the GCT's camera is primarily achieved with LED-based flasher units capable of producing $\\sim4$ ns FWHM pulses of 400 nm light across a large dynamic range, from 0.1 up to 1000 photoelectrons. The flasher units are housed in the four corners of the camera's focal plane and illuminate it via reflection from the secondary mirror. These flasher units are adaptable to allow several calibration scenarios to be accomplished: camera flat-fielding, linearity measurements (up to and past saturation), and gain estimates from both single pe measurements and from the photon statistics at various high illumination levels. In these proceedings, the performance of the GCT flashers is described, together with ongoing simulation work to quantify the efficiency of using muon rings as an end-to-end calibration for the optical throughput of the GCT.

  13. Imaging Fourier transform spectroscopy with multi-aperture telescopes

    E-Print Network [OSTI]

    Fienup, James R.

    Imaging Fourier transform spectroscopy with multi-aperture telescopes Samuel T. Thurman and James R Hanover St., Palo Alto, CA 94304 Abstract: Fourier spectroscopy can be performed with multi Society of America OCIS codes: (300.6300) Spectroscopy, Fourier transforms; (110.6770) Telescopes; (120

  14. Representations and image classification methods for Cherenkov telescopes

    SciTech Connect (OSTI)

    Malagon, C.; Parcerisa, D. S.; Barrio, J. A.; Nieto, D.

    2008-05-29

    The problem of identifying gamma ray events out of charged cosmic ray background (so called hadrons) in Cherenkov telescopes is one of the key problems in VHE gamma ray astronomy. In this contribution, we present a novel approach to this problem by implementing different classifiers relying on the information of each pixel of the camera of a Cherenkov telescope.

  15. VERITAS: Very LArge Energetic Radiation Imaging Telescope Array System

    E-Print Network [OSTI]

    T. C. Weekes; C. Akerlof; S. Biller; A. C. Breslin; J. H. Buckley; D. A. Carter-Lewis; M. Catanese; M. F. Cawley; B. Dingus; G. G. Fazio; D. J. Fegan; J. Finley; G. Fishman; J. Gaidos; G. H. Gillanders; P. Gorham; J. E. Grindlay; A. M. Hillas; J. Huchra; P. Kaaret; M. Kertzman; D. Kieda; F. Krennrich; R. C. Lamb; M. J. Lang; A. P. Marscher; S. Matz; T. McKay; D. Muller; R. Ong; W. Purcell; J. Rose; G. Sembroski; F. D. Seward; P. Slane; S. Swordy; T. Tumer; M. Ulmer; M. Urban; B. J. Wilkes

    1997-06-15

    A next generation atmospheric Cherenkov observatory is described based on the Whipple Observatory $\\gamma$-ray telescope. A total of nine such imaging telescopes will be deployed in an array that will permit the maximum versatility and give high sensitivity in the 50 GeV - 50 TeV band (with maximum sensitivity from 100 GeV to 10 TeV).

  16. VERITAS The Very Energetic Radiation Imaging Telescope Array System

    E-Print Network [OSTI]

    Weekes, T C; Biller, S D; Breslin, A C; Buckley, J H; Carter-Lewis, D A; Catanese, M; Cawley, M F; Dingus, B L; Fazio, G G; Fegan, D J; Finley, J; Fishman, G; Gaidos, J A; Gillanders, G H; Gorham, P W; Grindlay, J E; Hillas, A M; Huchra, J P; Kaaret, P E; Kertzman, M P; Kieda, D B; Krennrich, F; Lamb, R C; Lang, M J; Marscher, A P; Matz, S; McKay, T; Müller, D; Ong, R; Purcell, W; Rose, J; Sembroski, G H; Seward, F D; Slane, P O; Swordy, S P; Tümer, T O; Ulmer, M P; Urban, M; Wilkes, B J

    1997-01-01

    A next generation atmospheric Cherenkov observatory is described based on the Whipple Observatory $\\gamma$-ray telescope. A total of nine such imaging telescopes will be deployed in an array that will permit the maximum versatility and give high sensitivity in the 50 GeV - 50 TeV band (with maximum sensitivity from 100 GeV to 10 TeV).

  17. Rapid GRB Followup with the 2m Robotic Liverpool Telescope

    E-Print Network [OSTI]

    Gomboc, Andreja

    Rapid GRB Follow­up with the 2­m Robotic Liverpool Telescope Andreja Gomboc #,+ , Michael F. Bode. We present the capabilities of the 2­m robotic Liverpool Telescope (LT), owned and operated by Liverpool John Moores University and situated at ORM, La Palma. Robotic control and scheduling of the LT

  18. Collecting Light with Telescopes Two Fundamentally Different Spectral Mechanisms

    E-Print Network [OSTI]

    Shirley, Yancy

    ;Observing problems due to Earth's atmosphere 1. Light Pollution #12;Star viewed with ground-based telescope. · Location/technology can help overcome light pollution and turbulence. · Nothing short of going to space canCollecting Light with Telescopes #12;Two Fundamentally Different Spectral Mechanisms Spectral lines

  19. Adaptive Optics at the Subaru Telescope: current capabilities and development

    E-Print Network [OSTI]

    Guyon, Olivier

    Adaptive Optics at the Subaru Telescope: current capabilities and development Olivier Guyona Barbara, CA 93106, USA ABSTRACT Adaptive optics is a key component of Subaru Telescope's current-limited images in near-IR. In its LGS mode, laser light is transported from the solid state laser to the launch

  20. Silicon Photomultiplier Research and Development Studies for the Large Size Telescope of the Cherenkov Telescope Array

    E-Print Network [OSTI]

    Rando, Riccardo; Dazzi, Francesco; De Angelis, Alessandro; Dettlaff, Antonios; Dorner, Daniela; Fink, David; Fouque, Nadia; Grundner, Felix; Haberer, Werner; Hahn, Alexander; Hermel, Richard; Korpar, Samo; Mezek, Gašper Kukec; Maier, Ronald; Manea, Christian; Mariotti, Mosč; Mazin, Daniel; Mehrez, Fatima; Mirzoyan, Razmik; Podkladkin, Sergey; Reichardt, Ignasi; Rhode, Wolfgang; Rosier, Sylvie; Schultz, Cornelia; Stella, Carlo; Teshima, Masahiro; Wetteskind, Holger; Zavrtanik, Marko

    2015-01-01

    The Cherenkov Telescope Array (CTA) is the the next generation facility of imaging atmospheric Cherenkov telescopes; two sites will cover both hemispheres. CTA will reach unprecedented sensitivity, energy and angular resolution in very-high-energy gamma-ray astronomy. Each CTA array will include four Large Size Telescopes (LSTs), designed to cover the low-energy range of the CTA sensitivity ($\\sim$20 GeV to 200 GeV). In the baseline LST design, the focal-plane camera will be instrumented with 265 photodetector clusters; each will include seven photomultiplier tubes (PMTs), with an entrance window of 1.5 inches in diameter. The PMT design is based on mature and reliable technology. Recently, silicon photomultipliers (SiPMs) are emerging as a competitor. Currently, SiPMs have advantages (e.g. lower operating voltage and tolerance to high illumination levels) and disadvantages (e.g. higher capacitance and cross talk rates), but this technology is still young and rapidly evolving. SiPM technology has a strong pot...

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

    E-Print Network [OSTI]

    Design 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, California, U.S.A.; bNew Jersey Institute of Technology, Newark, New Jersey, U.S.A. ABSTRACT The New Solar

  2. Autism rate rises; disorder now affects 1 in 88 By LONA O'CONNOR AND CHARLES ELMORE

    E-Print Network [OSTI]

    Fernandez, Eduardo

    Autism rate rises; disorder now affects 1 in 88 children By LONA O'CONNOR AND CHARLES ELMORE Palm, 2012 A new estimate released Thursday says autism affects more children than ever - 1 in 88, like magnetic waves," said Jack Scott, executive director of the Center for Autism and Related

  3. A Field-Wise Wind Retrieval Algorithm for Satellite Scatterometers Charles G. Brown and David G . Long

    E-Print Network [OSTI]

    Long, David G.

    A Field-Wise Wind Retrieval Algorithm for Satellite Scatterometers Charles G. Brown and David G-378-6586 browncg@salt.ee.byii.edu Abstract-Traditional satellite scatterometer wind retrieval algorithms consist of point-wise wind estimation and point- wise ambiguity removal. Point-wise estimation yields mul- tiple

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

    E-Print Network [OSTI]

    Petrov, Dmitri

    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

  5. Smart grid research Viktor K. Prasanna is the Charles Lee Powell Chair in Engineering in the Ming Hsieh

    E-Print Network [OSTI]

    Levi, Anthony F. J.

    Smart grid research Viktor K. Prasanna is the Charles Lee Powell Chair in Engineering in the Ming of Water and Power Smart Grid Project funded under the Department of Energy Smart Grid Regional Integrated Asset Management LA Smart Grid Project Overview Demand Response Approach Research areas

  6. Fast Image Database Search using TreeStructured VQ #+ JauYuen Chen, Charles A. Bouman and Jan P. Allebach

    E-Print Network [OSTI]

    Fast Image Database Search using Tree­Structured VQ #+ Jau­Yuen Chen, Charles A. Bouman and Jan P the search of large image databases. Our method can reduce search computation required to locate images which for searching large image databases based on image content. The interest in im­ age search algorithms has grown

  7. Fast Image Database Search using Tree-Structured VQ Jau-Yuen Chen, Charles A. Bouman and Jan P. Allebach

    E-Print Network [OSTI]

    Fast Image Database Search using Tree-Structured VQ Jau-Yuen Chen, Charles A. Bouman and Jan P the search of large image databases. Our method can reduce search computation required to locate images which for searching large image databases based on image content. The interest in im- age search algorithms has grown

  8. The Use of Lime in Fish Ponds1 Andy M. Lazur, Charles E. Cichra and Craig Watson2

    E-Print Network [OSTI]

    Hill, Jeffrey E.

    FA38 The Use of Lime in Fish Ponds1 Andy M. Lazur, Charles E. Cichra and Craig Watson2 1. There are three main purposes for liming ponds: 1) to increase the availability of nutrients, 2) to increase pH and to buffer against daily pH fluctuations and 3) to steril- ize ponds prior to stocking. While these practices

  9. Avfs: An On-Access Anti-Virus File System Yevgeniy Miretskiy, Abhijith Das, Charles P. Wright, and Erez Zadok

    E-Print Network [OSTI]

    Zadok, Erez

    Avfs: An On-Access Anti-Virus File System Yevgeniy Miretskiy, Abhijith Das, Charles P. Wright (Security 2004) Abstract Viruses and other malicious programs are an ever- increasing threat to current to combat. Most cur- rent virus scanners perform scanning only when a file is opened, closed, or executed

  10. Charles Darwin University welcomes applications for Master by Research and PhD degrees from DIKTI scholarship awardees

    E-Print Network [OSTI]

    Charles Darwin University welcomes applications for Master by Research and PhD degrees from DIKTI to be eligible. Evidence of English language proficiency must be provided at initial Master by Research or PhD application stage. Tuition fee waiver for a third year (Master by Research) and fourth year (PhD) of study

  11. Lyapunov exponents for 2-D ray tracing without interfaces Ludek Klimes , Department of Geophysics, Charles University, Prague, Czech Republic

    E-Print Network [OSTI]

    Cerveny, Vlastislav

    Lyapunov exponents for 2-D ray tracing without interfaces Ludek Klimes , Department of Geophysics, Charles University, Prague, Czech Republic Summary The Lyapunov exponents asymptotically quantify the ex- ponential divergence of rays. The \\Lyapunov exponent" for a nite 2-D ray and the average \\Lyapunov exponents

  12. Lyapunov exponents for 2D ray tracing without interfaces Ludek Klimes \\Lambda , Department of Geophysics, Charles University, Prague, Czech Republic

    E-Print Network [OSTI]

    Cerveny, Vlastislav

    Lyapunov exponents for 2­D ray tracing without interfaces LudŸek KlimeŸs \\Lambda , Department of Geophysics, Charles University, Prague, Czech Republic Summary The Lyapunov exponents asymptotically quantify the ex­ ponential divergence of rays. The ``Lyapunov exponent'' for a finite 2­D ray and the average

  13. Page 390 Information Technology Sonoma State University 2015-2016 Catalog Jean and Charles Schulz Information Center 1000

    E-Print Network [OSTI]

    Ravikumar, B.

    Page 390 Information Technology Sonoma State University 2015-2016 Catalog Jean and Charles Schulz Information Technology provides the spectrum of services needed to deliver quality academic and administrative of information technology. Consultants are available by phone, 664-HELP; email, helpdesk@sonoma.edu; or in person

  14. Successes and Constraints in the Enactment of a Reform May Lee*, Melissa Dancy, Charles Henderson, and Eric Brewe

    E-Print Network [OSTI]

    Henderson, Charles

    Successes and Constraints in the Enactment of a Reform May Lee*, Melissa Dancy, Charles Henderson positive impacts of research-based instructional reforms in physics, few high school physics teachers in the US enact them. One of the more successfully disseminated reforms is Modeling Instruction. To discern

  15. The Gemini 8M Telescopes Project M. Mountain, F. Gillett, R. Kurz

    E-Print Network [OSTI]

    The Gemini 8­M Telescopes Project M. Mountain, F. Gillett, R. Kurz Gemini Telescopes Project, 950 N. Cherry Ave., Tucson AZ 85719 Gemini Preprint # 5 #12; The Gemini 8­M Telescopes Project Matt Mountain

  16. Real-time condition assessment of RAPTOR telescope systems

    SciTech Connect (OSTI)

    Stull, Chris; Taylor, Stuart; Wren, James; Farrar, Charles; Park, Gyuhae

    2010-11-30

    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.

  17. Measurements of Secodary Cosmic Microwave Background Anisotropies with the South Pole Telescope

    E-Print Network [OSTI]

    Lueker, Martin Van

    2010-01-01

    6 The South Pole Telescope Atmospheric Conditionsat the South Pole Telescope and Optical Design . . . . . . .interplay of cable delays, poles, resonances and zeroes in

  18. Software design for the control system for Small-Size Telescopes with single-mirror of the Cherenkov Telescope Array

    E-Print Network [OSTI]

    :,; B?ocki, J; Bogacz, L; Borkowski, J; Bulik, T; Cadoux, F; Christov, A; Cury?o, M; della Volpe, D; Dyrda, M; Favre, Y; Frankowski, A; Grudnik, ?; Grudzi?ska, M; Heller, M; Id?kowski, B; Jamrozy, M; Janiak, M; Kasperek, J; Lalik, K; Lyard, E; Mach, E; Mandat, D; Marsza?ek, A; Micha?owski, J; Moderski, R; Rameez, M; Montaruli, T; Neronov, A; Niemiec, J; Ostrowski, M; Pa?ko, P; Pech, M; Porcelli, A; Prandini, E; Rajda, P; Schioppa, E jr; Schovanek, P; Seweryn, K; Skowron, K; Sliusar, V; Sowi?ski, M; Stawarz, ?; Stodulska, M; Stodulski, M; Pujadas, I Troyano; Toscano, S; Walter, R; Wi?cek, M; Zagda?ski, A; Zi?tara, K; Zychowski, P

    2015-01-01

    The Small-Size Telescope with single-mirror (SST-1M) is a 4 m Davies-Cotton telescope and is among the proposed telescope designs for the Cherenkov Telescope Array (CTA). It is conceived to provide the high-energy ($>$ few TeV) coverage. The SST-1M contains proven technology for the telescope structure and innovative electronics and photosensors for the camera. Its design is meant to be simple, low-budget and easy-to-build industrially. Each device subsystem of an SST-1M telescope is made visible to CTA through a dedicated industrial standard server. The software is being developed in collaboration with the CTA Medium-Size Telescopes to ensure compatibility and uniformity of the array control. Early operations of the SST-1M prototype will be performed with a subset of the CTA central array control system based on the Alma Common Software (ACS). The triggered event data are time stamped, formatted and finally transmitted to the CTA data acquisition. The software system developed to control the devices of an SS...

  19. Xray Scatter Measurements from Thermally Slumped Thin Glass Substrates for the HEFT Hard Xray Telescopes

    E-Print Network [OSTI]

    , Charles J. Hailey b , Todd R. Decker b , Marcela Stern b David L. Windt c , Peter H. Mao d , Fiona A--50 keV range at a double­axis diffractometer at the Řrsted Laboratory, University of Copenhagen

  20. The South Pole Telescope bolometer array and the measurement of secondary Cosmic Microwave Background anisotropy at small angular scales

    E-Print Network [OSTI]

    Shirokoff, Erik D.

    2011-01-01

    iii 2 The South Pole Telescope 2.1 The Telescope . . . . .modifications . . . . II The South Pole Telescope SZ Cameraand exciting as the South Pole Telescope. Fewer still do so

  1. Multiobjective optimization of a radio telescope array with site constraints

    E-Print Network [OSTI]

    Cohanim, Babak, 1980-

    2004-01-01

    The next generation of radio telescope interferometric arrays requires careful design of the array configuration to optimize the performance and minimize the cost of the overall system while adhering to site constraints. ...

  2. Design and optimization of lightweight space telescope structures

    E-Print Network [OSTI]

    Stewart, Andrzej Matthew

    2007-01-01

    As mankind attempts to look deeper into the universe, increasingly larger space telescopes will be needed to achieve the levels of resolution required to perform these missions. Due to this increase in size, increasing ...

  3. Digital Frequency Domain Multiplexer for mm-Wavelength Telescopes

    E-Print Network [OSTI]

    Dobbs, Matt

    2008-01-01

    for Large Scale Bolometer Arrays”, Monterey Far-IR, Sub-mmand mm Detector Technology Workshop proceedings, 2002, pp.Domain Multiplexer for mm-Wavelength Telescopes Matt Dobbs,

  4. CTA telescopes as deep-space lasercom ground receivers

    E-Print Network [OSTI]

    Carrasco-Casado, Alberto; Vergaz, Ricardo

    2015-01-01

    The amount of scientific data to be transmitted from deep-space probes is very limited due to RF-communications constraints. Free-space optical communication can alleviate this bottleneck, increasing data rate while reducing weight, mass and power of communication onboard equipment. Nevertheless, optimizing the power delivery from spacecraft to Earth is needed. In RF communications, the strategy has been to increase the aperture of ground terminals. Free-space optical communications can also follow it, as they share the limitation of low power received on Earth. As the cost of big telescopes increases exponentially with aperture, new ideas are required to maximize the aperture-to-cost ratio. This work explores the feasibility of using telescopes of the future Cherenkov Telescope Array as optical-communication ground stations. Ground-based gamma-ray astronomy has the same power limitation, hence Cherenkov telescopes are designed to maximize receiver's aperture with minimum cost and some relaxed requirements. B...

  5. Robotic Telescopes and Networks: New Tools for Education and Science

    E-Print Network [OSTI]

    F. R. Querci; M. Querci

    1999-11-02

    Nowadays many telescopes around the world are automated and some networks of robotic telescopes are active or planned as shown by the lists we draw up. Such equipment could be used for the training of students and for science in the Universities of Developing Countries and of New Astronomical Countries, by sending them observational data via Internet or through remotely controlled telescopes. It seems that it is time to open up for discussion with UN and ESA organizations and also with IAU, how to implement links between robotic telescopes and such Universities applying for collaborations. Many scientific fields could thus be accessible to them, for example on stellar variability, near-earth object follow-up, gamma-ray burst counterpart tracking, and so on.

  6. South Pole Telescope Software Systems: Control, Monitoring, and Data Acquisition

    E-Print Network [OSTI]

    Story, K; Ade, P; Aird, K A; Austermann, J E; Beall, J A; Becker, D; Bender, A N; Benson, B A; Bleem, L E; Britton, J; Carlstrom, J E; Chang, C L; Chiang, H C; Cho, H-M; Crawford, T M; Crites, A T; Datesman, A; de Haan, T; Dobbs, M A; Everett, W; Ewall-Wice, A; George, E M; Halverson, N W; Harrington, N; Henning, J W; Hilton, G C; Holzapfel, W L; Hoover, S; Huang, N; Hubmayr, J; Irwin, K D; Karfunkle, M; Keisler, R; Kennedy, J; Lee, A T; Li, D; Lueker, M; Marrone, D P; McMahon, J J; Mehl, J; Meyer, S S; Montgomery, J; Montroy, T E; Nagy, J; Natoli, T; Nibarger, J P; Niemack, M D; Novosad, V; Padin, S; Pryke, C; Reichardt, C L; Ruhl, J E; Saliwanchik, B R; Sayre, J T; Schaffer, K K; Shirokoff, E; Smecher, G; Stalder, B; Tucker, C; Vanderlinde, K; Vieira, J D; Wang, G; Williamson, R; Yefremenko, V; Yoon, K W; Young, E; 10.1117/12.925808

    2012-01-01

    We present the software system used to control and operate the South Pole Telescope. The South Pole Telescope is a 10-meter millimeter-wavelength telescope designed to measure anisotropies in the cosmic microwave background (CMB) at arcminute angular resolution. In the austral summer of 2011/12, the SPT was equipped with a new polarization-sensitive camera, which consists of 1536 transition-edge sensor bolometers. The bolometers are read out using 36 independent digital frequency multiplexing (\\dfmux) readout boards, each with its own embedded processors. These autonomous boards control and read out data from the focal plane with on-board software and firmware. An overall control software system running on a separate control computer controls the \\dfmux boards, the cryostat and all other aspects of telescope operation. This control software collects and monitors data in real-time, and stores the data to disk for transfer to the United States for analysis.

  7. A generation of astronomical telescopes, their users, and publications

    E-Print Network [OSTI]

    Trimble, V

    2010-01-01

    Tele- scope in the Canary Islands, followed by 7 mirrors ofTelescopia Canarias in the Canary Islands. Table 3 attemptsKea, Hawaii, and the Canary Islands) have many telescopes

  8. The first GCT camera for the Cherenkov Telescope Array

    E-Print Network [OSTI]

    ,

    2015-01-01

    The Gamma Cherenkov Telescope (GCT) is proposed to be part of the Small Size Telescope (SST) array of the Cherenkov Telescope Array (CTA). The GCT dual-mirror optical design allows the use of a compact camera of diameter roughly 0.4 m. The curved focal plane is equipped with 2048 pixels of ~0.2{\\deg} angular size, resulting in a field of view of ~9{\\deg}. The GCT camera is designed to record the flashes of Cherenkov light from electromagnetic cascades, which last only a few tens of nanoseconds. Modules based on custom ASICs provide the required fast electronics, facilitating sampling and digitisation as well as first level of triggering. The first GCT camera prototype is currently being commissioned in the UK. On-telescope tests are planned later this year. Here we give a detailed description of the camera prototype and present recent progress with testing and commissioning.

  9. NectarCAM : a camera for the medium size telescopes of the Cherenkov Telescope Array

    E-Print Network [OSTI]

    Glicenstein, J-F; Barrio, J-A; Blanch~Bigas, O; Bolmont, J; Bouyjou, F; Brun, P; Chabanne, E; Champion, C; Colonges, S; Corona, P; Delagnes, E; Delgado, C; Ginzov, C Diaz; Durand, D; Ernenwein, J-P; Fegan, S; Ferreira, O; Fesquet, M; Fiasson, A; Fontaine, G; Fouque, N; Gascon, D; Giebels, B; Henault, F; Hermel, R; Hoffmann, D; Horan, D; Houles, J; Jean, P; Jocou, L; Karkar, S; Knoedlseder, J; Kossakowski, R; Lamanna, G; LeFlour, T; Lenain, J-P; Leveque, A; Louis, F; Martinez, G; Moudden, Y; Moulin, E; Nayman, P; Nunio, F; Olive, J-F; Panazol, J-L; Pavy, S; Petrucci, P-O; Pierre, E; Prast, J; Punch, M; Ramon, P; Rateau, S; Ravel, T; Rosier-Lees, S; Sanuy, A; Shayduk, M; Sizun, P-Y; Sulanke, K-H; Tavernet, J-P; Tejedor~Alvarez, L-A; Toussenel, F; Vasileiadis, G; Voisin, V; Waegebert, V; Wischnewski, R

    2015-01-01

    NectarCAM is a camera proposed for the medium-sized telescopes of the Cherenkov Telescope Array (CTA) covering the central energy range of ~100 GeV to ~30 TeV. It has a modular design and is based on the NECTAr chip, at the heart of which is a GHz sampling Switched Capacitor Array and a 12-bit Analog to Digital converter. The camera will be equipped with 265 7-photomultiplier modules, covering a field of view of 8 degrees. Each module includes the photomultiplier bases, high voltage supply, pre-amplifier, trigger, readout and Ethernet transceiver. The recorded events last between a few nanoseconds and tens of nanoseconds. The camera trigger will be flexible so as to minimize the read-out dead-time of the NECTAr chips. NectarCAM is designed to sustain a data rate of more than 4 kHz with less than 5\\% dead time. The camera concept, the design and tests of the various subcomponents and results of thermal and electrical prototypes are presented. The design includes the mechanical structure, cooling of the electro...

  10. A versatile digital camera trigger for telescopes in the Cherenkov Telescope Array

    E-Print Network [OSTI]

    Schwanke, U; Sulanke, K -H; Vorobiov, S; Wischnewski, R

    2015-01-01

    This paper describes the concept of an FPGA-based digital camera trigger for imaging atmospheric Cherenkov telescopes, developed for the future Cherenkov Telescope Array (CTA). The proposed camera trigger is designed to select images initiated by the Cherenkov emission of extended air showers from very-high energy (VHE, E>20 GeV) photons and charged particles while suppressing signatures from background light. The trigger comprises three stages. A first stage employs programmable discriminators to digitize the signals arriving from the camera channels (pixels). At the second stage, a grid of low-cost FPGAs is used to process the digitized signals for camera regions with 37 pixels. At the third stage, trigger conditions found independently in any of the overlapping 37-pixel regions are combined into a global camera trigger by few central FPGAs. Trigger prototype boards based on Xilinx FPGAs have been designed, built and tested and were shown to function properly. Using these components a full camera trigger wi...

  11. Satellite Characterization of four candidate sites for the Cherenkov Telescope Array telescope

    E-Print Network [OSTI]

    Cavazzani, S; Bulik, T; Ortolani, S

    2012-01-01

    In this paper we have evaluated the amount of available telescope time at four sites which are candidate to host the future Cherenkov Telescope Array (CTA). We use the GOES 12 data for the years 2008 and 2009. We use a homogeneous methodology presented in several previous papers to classify the nights as clear (completely cloud-free), mixed (partially cloud-covered), and covered. Additionally, for the clear nights, we have evaluated the amount of satellite stable nights which correspond to the amount of ground based photometric nights, and the clear nights corresponding to the spectroscopic nights. We have applied this model to two sites in the Northern Hemisphere (San Pedro Martir (SPM), Mexico; Izana, Canary Islands) and to two sites in the Southern Hemisphere (El Leoncito, Argentine; San Antonio de Los Cobres (SAC), Argentine). We have obtained, from the two years considered, a mean amount of cloud free nights of 68.6% at Izana, 76.0% at SPM, 70.6% at Leoncito and 70.0% at SAC. We have evaluated, among the...

  12. The Optical System for the Large Size Telescope of the Cherenkov Telescope Array

    E-Print Network [OSTI]

    Hayashida, M; Teshima, M; de Almeida, U Barres; Chikawa, M; Cho, N; Fukami, S; Gadola, A; Hanabata, Y; Horns, D; Jablonski, C; Katagiri, H; Kagaya, M; Ogino, M; Okumura, A; Saito, T; Stadler, R; Steiner, S; Straumann, U; Vollhardt, A; Wetteskind, H; Yamamoto, T; Yoshida, T

    2015-01-01

    The Large Size Telescope (LST) of the Cherenkov Telescope Array (CTA) is designed to achieve a threshold energy of 20 GeV. The LST optics is composed of one parabolic primary mirror 23 m in diameter and 28 m focal length. The reflector dish is segmented in 198 hexagonal, 1.51 m flat to flat mirrors. The total effective reflective area, taking into account the shadow of the mechanical structure, is about 368 m$^2$. The mirrors have a sandwich structure consisting of a glass sheet of 2.7 mm thickness, aluminum honeycomb of 60 mm thickness, and another glass sheet on the rear, and have a total weight about 47 kg. The mirror surface is produced using a sputtering deposition technique to apply a 5-layer coating, and the mirrors reach a reflectivity of $\\sim$94% at peak. The mirror facets are actively aligned during operations by an active mirror control system, using actuators, CMOS cameras and a reference laser. Each mirror facet carries a CMOS camera, which measures the position of the light spot of the optical ...

  13. Merguerian, Charles, 1996b, Evidence for post-glacial surface faulting in New York City. The dynamic relationship between earthquakes and movement on reactivated faults

    E-Print Network [OSTI]

    Merguerian, Charles

    Merguerian, Charles, 1996b, Evidence for post-glacial surface faulting in New York City in New York City (abs.): Geological Society of America Abstracts with Programs, v. 28, no. 3, p. 81

  14. Merguerian, Charles, 1995a, The Taconic problem -alive and well in New York City The Taconic problem in NYC, focuses on ductile-fault imbrication of three lithologically

    E-Print Network [OSTI]

    Merguerian, Charles

    Merguerian, Charles, 1995a, The Taconic problem - alive and well in New York City (NYC, 1995a, The Taconic problem - alive and well in New York City (NYC) (abs.): Geological Society

  15. Spectral lines and distribution of Hi in high rotational levels Dairene Uy, Charles M. Gabrys, Mary-Frances Jagod, and Takeshi Oka

    E-Print Network [OSTI]

    Oka, Takeshi

    Spectral lines and distribution of Hi in high rotational levels Dairene Uy, Charles M. Gabrys, Mary K in their simu- lation of the observed spectrum.) The first motive to study Hi in high rotational

  16. The Sloan Digital Sky Survey Monitor Telescope Pipeline

    E-Print Network [OSTI]

    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

    2006-08-26

    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).

  17. The Sloan Digital Sky Survey Monitor Telescope Pipeline

    E-Print Network [OSTI]

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

    2006-01-01

    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 s...

  18. 3D acoustic imaging applied to the Baikal Neutrino Telescope

    E-Print Network [OSTI]

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

    2008-11-07

    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.

  19. The software design of the Gemini 8m telescopes Stephen Wampler

    E-Print Network [OSTI]

    The software design of the Gemini 8m telescopes Stephen Wampler Gemini 8m Telescopes Project, 950 N. Cherry Ave, Tucson, AZ 85726 ABSTRACT The design of the software for the Gemini 8m Telescopes is nearly. Keywords: telescope software design, design processes, Gemini software 1. INTRODUCTION The Gemini 8m

  20. Deuteron frozen spin polarized target for nd experiements at the VdG accelerator of Charles University

    E-Print Network [OSTI]

    N. S. Borisov; N. A. Bazhanov; A. A. Belyaev; J. Broz; J. Cerny; Z. Dolezal; A. N. Fedorov; G. M. Gurevich; M. P. Ivanov; P. Kodys; P. Kubik; E. S. Kuzmin; A. B. Lazarev; F. Lehar; O. O. Lukhanin; V. N. Matafonov; A. B. Neganov; I. L. Pisarev; J. Svejda; S. N. Shilov; Yu. A. Usov; I. Wilhelm

    2007-12-09

    A frozen spin polarized deuteron target cooled by the 3He/4He dilution refrigerator is described. Fully deuterated 1,2-propanediol was used as a target material. Deuteron vector polarization about 40% was obtained for the target in the shape of a cylinder of 2 cm diameter and 6 cm length. The target is intended for a study of 3N interactions at the polarized neutron beam generated by the Van de Graaff accelerator at the Charles University in Prague.

  1. Ground-water flow and ground- and surface-water interaction at the Weldon Spring quarry, St. Charles County, Missouri

    SciTech Connect (OSTI)

    Imes, J.L.; Kleeschulte, M.J.

    1997-12-31

    Ground-water-level measurements to support remedial actions were made in 37 piezometers and 19 monitoring wells during a 19-month period to assess the potential for ground-water flow from an abandoned quarry to the nearby St. Charles County well field, which withdraws water from the base of the alluvial aquifer. From 1957 to 1966, low-level radioactive waste products from the Weldon Spring chemical plant were placed in the quarry a few hundred feet north of the Missouri River alluvial plain. Uranium-based contaminants subsequently were detected in alluvial ground water south of the quarry. During all but flood conditions, lateral ground-water flow in the bedrock from the quarry, as interpreted from water-table maps, generally is southwest toward Little Femme Osage Creek or south into the alluvial aquifer. After entering the alluvial aquifer, the ground water flows southeast to east toward a ground-water depression presumably produced by pumping at the St. Charles County well field. The depression position varies depending on the Missouri River stage and probably the number and location of active wells in the St. Charles County well field.

  2. Water Vapour Radiometers for the Australia Telescope Compact Array

    E-Print Network [OSTI]

    Indermuehle, Balthasar T; Crofts, Jonathan

    2012-01-01

    We have developed Water Vapour Radiometers (WVRs) for the Australia Telescope Compact Array (ATCA) that are capable of determining path fluctuations by virtue of measuring small temperature fluctuations in the atmosphere using the 22.2 GHz water vapour line for each of the six antennae. By measuring the line of sight variations of the water vapour, the induced path excess and thus the phase delay can be estimated and corrections can then be applied during data reduction. This reduces decorrelation of the source signal. We demonstrate how this recovers the telescope's efficiency and image quality as well as how this improves the telescope's ability to use longer baselines at higher frequencies, thereby resulting in higher spatial resolution. A description of the WVR hardware design, their calibration and water vapour retrieval mechanism is given.

  3. The Very Energetic Radiation Imaging Telescope Array System (VERITAS)

    E-Print Network [OSTI]

    Bradbury, S M; Breslin, A C; Buckley, J H; Carter-Lewis, D A; Catanese, M; Criswell, S; Dingus, B L; Fegan, D J; Finley, J P; Gaidos, J A; Grindlay, J; Hillas, A M; Harris, K; Hermann, G; Kaaret, P E; Kieda, D B; Knapp, J; Krennrich, F; Le Bohec, S; Lessard, R W; Lloyd-Evans, J; McKernan, B; Müller, D; Ong, R; Quenby, J J; Quinn, J; Rochester, G D; Rose, H J; Salamon, M B; Sembroski, G H; Sumner, T J; Swordy, S P; Vasilev, V; Weekes, T C

    1999-01-01

    We give an overview of the current status and scientific goals of VERITAS, a proposed hexagonal array of seven 10 m aperture imaging Cherenkov telescopes. The selected site is Montosa Canyon (1390 m a.s.l.) at the Whipple Observatory, Arizona. Each telescope, of 12 m focal length, will initially be equipped with a 499 element photomultiplier camera covering a 3.5 degree field of view. A central station will initiate the readout of 500 MHz FADCs upon receipt of multiple telescope triggers. The minimum detectable flux sensitivity will be 0.5% of the Crab Nebula flux at 200 GeV. Detailed simulations of the array's performance are presented elsewhere at this meeting. VERITAS will operate primarily as a gamma-ray observatory in the 50 GeV to 50 TeV range for the study of active galaxies, supernova remnants, pulsars and gamma-ray bursts.

  4. The Very Energetic Radiation Imaging Telescope Array System (VERITAS)

    E-Print Network [OSTI]

    S. M. Bradbury; I. H. Bond; A. C. Breslin; J. H. Buckley; D. A. Carter-Lewis; M. Catanese; S. Criswell; B. L. Dingus; D. J. Fegan; J. P. Finley; J. Gaidos; J. Grindlay; A. M. Hillas; K. Harris; G. Hermann; P. Kaaret; D. Kieda; J. Knapp; F. Krennrich; S. LeBohec; R. W. Lessard; J. Lloyd-Evans; B. McKernan; D. Mueller; R. Ong; J. J. Quenby; J. Quinn; G. Rochester; H. J. Rose; M. Salamon; G. H. Sembroski; T. Sumner; S. Swordy; V. V. Vassiliev; T. C. Weekes

    1999-07-19

    We give an overview of the current status and scientific goals of VERITAS, a proposed hexagonal array of seven 10 m aperture imaging Cherenkov telescopes. The selected site is Montosa Canyon (1390 m a.s.l.) at the Whipple Observatory, Arizona. Each telescope, of 12 m focal length, will initially be equipped with a 499 element photomultiplier camera covering a 3.5 degree field of view. A central station will initiate the readout of 500 MHz FADCs upon receipt of multiple telescope triggers. The minimum detectable flux sensitivity will be 0.5% of the Crab Nebula flux at 200 GeV. Detailed simulations of the array's performance are presented elsewhere at this meeting. VERITAS will operate primarily as a gamma-ray observatory in the 50 GeV to 50 TeV range for the study of active galaxies, supernova remnants, pulsars and gamma-ray bursts.

  5. The Antarctic Submillimeter Telescope and Remote Observatory (AST/RO)

    E-Print Network [OSTI]

    Antony A. Stark; John Bally; Simon P. Balm; T. M. Bania; Alberto D. Bolatto; Richard A. Chamberlin; Gregory Engargiola; Maohai Huang; James G. Ingalls; Karl Jacobs; James M. Jackson; Jacob W. Kooi; Adair P. Lane; K. -Y. Lo; Rodney D. Marks; Christopher L. Martin; Dennis Mumma; Roopesh Ojha; Rudolf Schieder; Johannes Staguhn; Juergen Stutzki; Christopher K. Walker; Robert W. Wilson; Gregory A. Wright; Xiaolei Zhang; Peter Zimmermann; Ruediger Zimmermann

    2000-12-15

    AST/RO, a 1.7 m diameter telescope for astronomy and aeronomy studies at wavelengths between 200 and 2000 microns, was installed at the South Pole during the 1994-1995 Austral summer. The telescope operates continuously through the Austral winter, and is being used primarily for spectroscopic studies of neutral atomic carbon and carbon monoxide in the interstellar medium of the Milky Way and the Magellanic Clouds. The South Pole environment is unique among observatory sites for unusually low wind speeds, low absolute humidity, and the consistent clarity of the submillimeter sky. Four heterodyne receivers, an array receiver, three acousto-optical spectrometers, and an array spectrometer are installed. A Fabry-Perot spectrometer using a bolometric array and a Terahertz receiver are in development. Telescope pointing, focus, and calibration methods as well as the unique working environment and logistical requirements of the South Pole are described.

  6. The X-ray Telescope of the CAST Experiment

    E-Print Network [OSTI]

    R. Kotthaus; H. Braeuninger; P. Friedrich; R. Hartmann; D. Kang; M. Kuster; G. Lutz; L. Strueder

    2005-11-14

    The CERN Axion Solar Telescope (CAST) searches for solar axions employing a 9 Tesla superconducting dipole magnet equipped with 3 independent detection systems for X-rays from axion-photon conversions inside the 10 m long magnetic field. Results of the first 6 months of data taking in 2003 imply a 95 % CL upper limit on the axion-photon coupling constant of 1.16x10(-10) GeV(-1) for axion masses CAST is a X-ray telescope consisting of a Wolter I type mirror system and a fully depleted pn-CCD as focal plane detector. Exploiting the full potential of background suppression by focussing X-rays emerging from the magnet bore, the axion sensitivity obtained with telescope data taken in 2004, for the first time in a controlled laboratory experiment, will supersede axion constraints derived from stellar energy loss arguments.

  7. An EUDET/AIDA Pixel Beam Telescope for Detector Development

    E-Print Network [OSTI]

    Rubinskiy, I

    2015-01-01

    Ahigh resolution(?International Linear Collider providing test beam infrastructure to detector R&D groups. The telescope consists of six sensor planes with a pixel pitch of either 18.4 ?m or 10 ?mand canbe operated insidea solenoidal magnetic fieldofupto1.2T.Ageneral purpose cooling, positioning, data acquisition (DAQ) and offine data analysis tools are available for the users. The excellent resolution, readout rate andDAQintegration capabilities made the telescopea primary beam tests tool also for several CERN based experiments. In this report the performance of the final telescope is presented. The plans for an even more flexible telescope with three differentpixel technologies(ATLASPixel, Mimosa,Timepix) withinthenew European detector infrastructure project AIDA are presented.

  8. MACHO Mass Determination Based on Space Telescope Observation

    E-Print Network [OSTI]

    Mareki Honma

    1999-03-24

    We investigate the possibility of lens mass determination for a caustic crossing microlensing event based on a space telescope observation. We demonstrate that the parallax due to the orbital motion of a space telescope causes a periodic fluctuation of the light curve, from which the lens distance can be derived. Since the proper motion of the lens relative to the source is also measurable for a caustic crossing event, one can find a full solution for microlensing properties of the event, including the lens mass. To determine the lens mass with sufficient accuracy, the light curve near the caustic crossing should be observed within uncertainty of $\\sim$ 1%. We argue that the Hubble Space Telescope observation of the caustic crossing supplied with ground-based observations of the full light curve will enable us to determine the mass of MACHOs, which is crucial for understanding the nature of MACHOs.

  9. Relay telescope for high power laser alignment system

    DOE Patents [OSTI]

    Dane, C. Brent; Hackel, Lloyd; Harris, Fritz B.

    2006-09-19

    A laser system includes an optical path having an intracavity relay telescope with a telescope focal point for imaging an output of the gain medium between an image location at or near the gain medium and an image location at or near an output coupler for the laser system. A kinematic mount is provided within a vacuum chamber, and adapted to secure beam baffles near the telescope focal point. An access port on the vacuum chamber is adapted for allowing insertion and removal of the beam baffles. A first baffle formed using an alignment pinhole aperture is used during alignment of the laser system. A second tapered baffle replaces the alignment aperture during operation and acts as a far-field baffle in which off angle beams strike the baffle a grazing angle of incidence, reducing fluence levels at the impact areas.

  10. Lee Sang Gak Telescope (LSGT): A Remotely Operated Robotic Telescope for Education and Research at Seoul National University

    E-Print Network [OSTI]

    Im, Myungshin; Kim, Kihyun

    2015-01-01

    We introduce the Lee Sang Gak Telescope (LSGT), a remotely operated, robotic 0.43-meter telescope. The telescope was installed at the Siding Spring Observatory, Australia, in 2014 October, to secure regular and exclusive access to the dark sky and excellent atmospheric conditions in the southern hemisphere from the Seoul National University (SNU) campus. Here, we describe the LSGT system and its performance, present example images from early observations, and discuss a future plan to upgrade the system. The use of the telescope includes (i) long-term monitoring observations of nearby galaxies, active galactic nuclei, and supernovae; (ii) rapid follow-up observations of transients such as gamma-ray bursts and gravitational wave sources; and (iii) observations for educational activities at SNU. Based on observations performed so far, we find that the telescope is capable of providing images to a depth of R=21.5 mag (point source detection) at 5-sigma with 15 min total integration time under good observing condi...

  11. An Optical Reflector System for the CANGAROO-II Telescope

    E-Print Network [OSTI]

    Akiko Kawachi

    1999-11-30

    We have developed light and durable mirrors made of CFRP (Carbon Fiber Reinforced Plastics) laminates for the reflector of the new CANGAROO-II 7 m telescope. The reflector has a parabolic shape (F/1.1) with a 30 m^2 effective area which consists of 60 small spherical mirrors. The attitude of each mirror can be remotely adjusted by stepping motors. After the first adjustment work, the re ector offers a point image of about 0.14 degree (FWHM) on the optic axis. The telescope has been in operation since May 1999 with an energy threshold of ~ 300 GeV.

  12. An Optical Reflector System for the CANGAROO-II Telescope

    E-Print Network [OSTI]

    Kawachi, A

    1999-01-01

    We have developed light and durable mirrors made of CFRP (Carbon Fiber Reinforced Plastics) laminates for the reflector of the new CANGAROO-II 7 m telescope. The reflector has a parabolic shape (F/1.1) with a 30 m^2 effective area which consists of 60 small spherical mirrors. The attitude of each mirror can be remotely adjusted by stepping motors. After the first adjustment work, the re ector offers a point image of about 0.14 degree (FWHM) on the optic axis. The telescope has been in operation since May 1999 with an energy threshold of ~ 300 GeV.

  13. Integrating Seeing Measurements into the Operations of Solar Telescopes

    E-Print Network [OSTI]

    years, experimental solar physics has seen renewed efforts to design, build and operate the nextIntegrating 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

  14. Status and First Results of the MAGIC Telescope

    E-Print Network [OSTI]

    J. Cortina; for the MAGIC collaboration

    2004-07-22

    The 17 m MAGIC Cherenkov telescope for gamma ray astronomy between 30 and 300 GeV started operations in its final configuration in October 2003 and is currently well into its calibration phase. Here I report on its present status and its first gamma ray source detections.

  15. The Atacama Cosmology Telescope Project: A Progress Report

    E-Print Network [OSTI]

    Arthur Kosowsky; for the ACT Collaboration

    2006-08-25

    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.

  16. The high resolution silicon telescope of the INSULAB group

    E-Print Network [OSTI]

    Bonfanti, Silvia; Lietti, Daniela; Vallazza, Erik

    This thesis has focused on the study of the performance of the high resolution tracking system (telescope) of the INSULAB group and on the implementation of a new data acquisition (DAQ) to comply with the high rate of the CERN North Area extracted beams. This system has allowed to increase the DAQ rate by a factor two with respect to the “standard” electronics. The INSULAB telescope is designed to test detectors ranging from calorimeters to more complex systems like in the case of the bent crystals studied by the COHERENT experiment. The telescope consists of four 300 $mu$m thick double side silicon strip detector modules with an area of 1.92$\times$1.92 cm$^{2}$ and 384 strips. The readout pitch is 50 $mu$m on both sides of the module but the junction side has an implant pitch of 25 $mu$m (and thus a floating strip) to improve the resolution. The telescope has been installed on the H4 beamline at the CERN SPS for the commissioning of the new readout system in June 2012. The results are analyzed in terms...

  17. Detecting Earth-impacting asteroids Pan-STARRS prototype telescope

    E-Print Network [OSTI]

    Veres, Peter

    Detecting Earth-impacting asteroids with the Pan-STARRS prototype telescope (Based on MS. Grav #12;10/14/2008 DPS, Ithaca, NY Granvik: Earth-impacting asteroids with PS1 Pan-STARRS 1 (PS1) Moving Object Processing System (MOPS) #12;10/14/2008 DPS, Ithaca, NY Granvik: Earth-impacting asteroids

  18. Fermi Large Area Telescope Observations of the Supernova Remnant...

    Office of Scientific and Technical Information (OSTI)

    of the Supernova Remnant G8.7-0.1 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...

  19. The Hobby-Eberly Telescope Low Resolution Spectrograph: mechanical design

    E-Print Network [OSTI]

    Hill, Gary J.

    The Hobby-Eberly Telescope Low Resolution Spectrograph: mechanical design G. J. Hilla* , H. Nicklas constraints make the LRS a challenging instrument, built on a limited budget. The mechanical design of the mechanical design of the LRS. Fabrication, assembly and testing of the LRS will be completed by mid 1998

  20. The HobbyEberly Telescope Low Resolution Spectrograph: mechanical design

    E-Print Network [OSTI]

    Hill, Gary J.

    The Hobby­Eberly Telescope Low Resolution Spectrograph: mechanical design G. J. Hill a* , H constraints make the LRS a challenging instrument, built on a limited budget. The mechanical design of the mechanical design of the LRS. Fabrication, assembly and testing of the LRS will be completed by mid 1998

  1. Parametric modeling and control of telescope wind-induced vibration

    E-Print Network [OSTI]

    MacMynowski, Douglas G. - MacMynowski, Douglas G.

    -buffeting is presented. The model is being developed to support the design of next generation segmented-mirror optical: Parametric modeling, extremely large telescope, control, wind-buffeting 1. INTRODUCTION Various design the predictions of the former at one or more points in the design space. An initial parametric model of wind

  2. Laser guide star projection for large telescopes Erez N. Ribak

    E-Print Network [OSTI]

    Ribak, Erez

    this projected pattern. Keywords: adaptive optics, laser guide stars 1. INTRODUCTION Telescopes of diameter will be corrected by active and adaptive optics, to remedy slow and fast variations of the optics beam diameter is set by the turbulence distorting the beam going up. Most systems use the light

  3. Performance of the MAGIC telescopes after the major upgrade

    E-Print Network [OSTI]

    Sitarek, Julian; Colin, Pierre; Mazin, Daniel

    2015-01-01

    MAGIC is a system of two Imaging Atmospheric Cherenkov Telescopes located on the Canary island of La Palma, Spain. During summer 2011 and 2012 it underwent a major upgrade. The main subsystems upgraded were the MAGIC-I camera and its trigger system and the readout system of both telescopes. We use observations of the Crab Nebula taken at low and medium zenith angles to assess the key performance parameters of the MAGIC stereo system. For low zenith angle observations, the standard trigger threshold of the MAGIC telescopes is about 50 GeV. The integral sensitivity for point-like sources with Crab Nebula-like spectra above 220 GeV is (0.66 +/- 0.03)% of Crab Nebula flux in 50 h of observations. The angular resolution, defined as the sigma of a 2-dimensional Gaussian distribution, at energies of a few hundred GeV is below 0.07degree, while the energy resolution is around 16%. We investigate the effect of the systematic uncertainty on the data taken with the MAGIC telescopes after the upgrade. We estimate that th...

  4. The pier and building of the European Solar Telescope (EST) F.C.M. Bettonvil*a

    E-Print Network [OSTI]

    Rutten, Rob

    The pier and building of the European Solar Telescope (EST) F.C.M. Bettonvil*a , R. Codinab , A surrounded by an open framework. Keywords: Telescope pier, building, solar telescope, CFD analysis, tower. ABSTRACT EST (European Solar Telescope) is a 4-m class solar telescope, which is currently

  5. Wide-Field InfrarRed Survey Telescope-Astrophysics Focused Telescope Assets WFIRST-AFTA 2015 Report

    E-Print Network [OSTI]

    Spergel, D; Baltay, C; Bennett, D; Breckinridge, J; Donahue, M; Dressler, A; Gaudi, B S; Greene, T; Guyon, O; Hirata, C; Kalirai, J; Kasdin, N J; Macintosh, B; Moos, W; Perlmutter, S; Postman, M; Rauscher, B; Rhodes, J; Wang, Y; Weinberg, D; Benford, D; Hudson, M; Jeong, W -S; Mellier, Y; Traub, W; Yamada, T; Capak, P; Colbert, J; Masters, D; Penny, M; Savransky, D; Sterns, D; Zimmerman, N; Barry, R; Bartusek, L; Carpenter, K; Cheng, E; Content, D; Dekens, F; Demers, R; Grady, K; Jackson, C; Kuan, G; Kruk, J; Melton, M; Nemati, B; Parvin, B; Poberezhskiy, I; Peddie, C; Ruffa, J; Wallace, J K; Whipple, A; Wollack, E; Zhao, F

    2015-01-01

    This report describes the 2014 study by the Science Definition Team (SDT) of the Wide-Field Infrared Survey Telescope (WFIRST) mission. It is a space observatory that will addresses the most compelling scientific problems in dark energy, exoplanets and general astrophysics using a 2.4m telescope with a wide-field infrared instrument and an optical coronagraph. The Astro2010 Decadal Survey recommended a Wide Field Infrared Survey Telescope as its top priority for a new large space mission. As conceived by the decadal survey, WFIRST would carry out a dark energy science program, a microlensing program to determine the demographics of exoplanets, and a general observing program utilizing its ultra wide field. In October 2012, NASA chartered a Science Definition Team (SDT) to produce, in collaboration with the WFIRST Study Office at GSFC and the Program Office at JPL, a Design Reference Mission (DRM) for an implementation of WFIRST using one of the 2.4-m, Hubble-quality telescope assemblies recently made availabl...

  6. The Zadko Telescope: the Australian Node of a Global Network of Fully Robotic Follow-up Telescopes

    E-Print Network [OSTI]

    Paris-Sud XI, Université de

    imaging between the east coast of Australia and South Africa at similar latitude. The Zadko Telescope in frontier optical transient science projects. The so called `transient Universe'' consists of astronomical image processing pipeline produces calibrated FITS images to external users via a web-based interface

  7. Ion implantation for figure correction of high-resolution x-ray telescope mirrors

    E-Print Network [OSTI]

    Chalifoux, Brandon D

    2014-01-01

    Fabricating mirrors for future high-resolution, large-aperture x-ray telescopes continues to challenge the x-ray astronomy instrumentation community. Building a large-aperture telescope requires thin, lightweight mirrors; ...

  8. Integrated modeling to facilitate control architecture design for lightweight space telescopes

    E-Print Network [OSTI]

    Cohan, Lucy Elizabeth

    2007-01-01

    The purpose of this thesis it to examine the effects of utilizing control to better meet performance and systematic requirements of future space telescopes. New telescope systems are moving toward tighter optical performance ...

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

    E-Print Network [OSTI]

    Cataldo, Giuseppe

    2014-12-19

    Humanity’s 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 ...

  10. THE NUCLEAR SPECTROSCOPIC TELESCOPE ARRAY (NuSTAR) HIGH-ENERGY...

    Office of Scientific and Technical Information (OSTI)

    NUCLEAR SPECTROSCOPIC TELESCOPE ARRAY (NuSTAR) HIGH-ENERGY X-RAY MISSION Citation Details In-Document Search Title: THE NUCLEAR SPECTROSCOPIC TELESCOPE ARRAY (NuSTAR) HIGH-ENERGY...

  11. An Efficient Work-Distribution Strategy for Gridding Radio-Telescope Data on GPUs

    E-Print Network [OSTI]

    Romein, John W.

    other telescopes in the world together -- the Square Kilometre Array (SKA) [4]. The imager is a critical

  12. Geohydrologic data for the St. Charles County well field and public-water supply 1985-91, and projected public-water supply, 1995 and 2000, for St. Charles County, Missouri

    SciTech Connect (OSTI)

    Mugel, D.N.

    1996-10-01

    Geohydrologic data for this well field and public water supply data for St. Charles County were compiled to assist US DOE in developing the St. Charles County well field contingency plan to ensure a supply of water in the event that the well field becomes contaminated from wastes (radioactive, nitroaromatic, other) stored in the Weldon Spring quarry. The well field consists of 8 wells penetrating the entire thickness of the Missouri River alluvial aquifer and is 98-116 feet deep. Aquifer tests were conducted on 3 occasions at 3 different locations in the well field. Calculated transmissivities range from 900 to 60,200 feet squared per day; hydraulic conductivities ranged from 23 to 602 feet/day. Calculated/estimated storage coefficients ranged from 0.005 to 0.2. Tracer test showed effective porosity of 0. 21-0.32. Point dilution showed a ground-water velocity of 0.83 foot/day. From 1985-91, ave daily water supply from the well field and water treatment plant increased from 5.76 to 10.23 Mgd; this is projected to increase to 11.0 Mgd in 1995 and to 12.2 Mgd in 2000. The water department`s projections of peak daily demands from customers indicate that these demands will exceed the capacity of the treatment plant in 1995 and will exceed the capacities of the well field and plant during 2000.

  13. Progress on the 1.6-meter New Solar Telescope at Big Bear Solar Observatory

    E-Print Network [OSTI]

    of the drivers for building solar telescopes with large apertures. Recent advances in adaptive optics (AO) make it possible to build solar telescopes in an open configuration and thus go beyond the conventional meterProgress on the 1.6-meter New Solar Telescope at Big Bear Solar Observatory C. Denkera, P. R

  14. EST: the European Solar Telescope D. Kiselman, M. Lofdahl & G. Scharmer

    E-Print Network [OSTI]

    Löfdahl, Mats

    is to construct a new large-aperture solar telescope: the European Solar Telescope (EST). 3. EST design studyEST: the European Solar Telescope D. Kiselman, M. L¨ofdahl & G. Scharmer The Institute for Solar of solar magnetism is to measure the structure and dynamics of the magnetic field at the solar surface down

  15. Early Optical Follow-up Observations of Gamma Ray Bursts with the Robotic Liverpool Telescope

    E-Print Network [OSTI]

    Gomboc, Andreja

    Early Optical Follow-up Observations of Gamma Ray Bursts with the Robotic Liverpool Telescope A, Slovenia 3 ITC-IRST and INFN, Trento, via Sommarive, 18 38050 Povo (TN), Italy Abstract Robotic telescopes of robotic telescopes is the rapid reaction to Targets of Opportunity, including short and unpredictable

  16. EarlyTime Observations of GRBs afterglow with 2m Robotic Telescopes

    E-Print Network [OSTI]

    Gomboc, Andreja

    Early­Time Observations of GRBs afterglow with 2­m Robotic Telescopes A. Melandri # , A. Gomboc time multi­wavelength light curves, obtained by space and ground­based robotic telescopes, have shown followup programme being conducted on a network of the world's three largest robotic telescopes that aims

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

    E-Print Network [OSTI]

    Rutten, Rob

    ; (iii) the design consequences for the new generation of high-resolution solar telescopes. Keywords to the open tower design. In section 3 we consider the interaction between the wind and the telescope 15 m and upward when there is some wind. The conclusion from this experience was the open telescope

  18. Management of the Gemini 8M Telescopes Project R. Kurz, M. Mountain

    E-Print Network [OSTI]

    Management of the Gemini 8­M Telescopes Project R. Kurz, M. Mountain Gemini Telescopes Project, 950 N. Cherry Ave., Tucson AZ 85719 Gemini Preprint #7 #12; Management of the Gemini 8­M Telescopes, organizations in the partner countries, and industrial contractors. The project organization and management

  19. A Wide-Field Infrared Camera for the Palomar 200-inch Telescope

    E-Print Network [OSTI]

    Galis, Frietson

    A Wide-Field Infrared Camera for the Palomar 200-inch Telescope J. C. Wilsona, S. S. Eikenberrya, C that provides the Palomar 200-inch telescope with such an imaging capability. WIRC features a field-of-view (FOV Camera (WIRC) at the Palomar 200-inch telescope. Mounted at prime focus to take advantage

  20. Observation of GRBs by the MAGIC Telescope, Status and Outlook

    E-Print Network [OSTI]

    D. Bastieri; N. Galante; M. Garczarczyk; M. Gaug; F. Longo; S. Mizobuchi; V. Scapin

    2007-09-10

    Observation of Gamma Ray Bursts (GRBs) in the Very High Energy (VHE) domain will provide important information on the physical conditions in GRB outflows. The MAGIC telescope is the best suited Imaging Atmospheric Cherenkov Telescope (IACT) for these observations. Thanks to its fast repositioning time and low energy threshold, MAGIC is able to start quickly the follow-up observation, triggered by an alert from the GRB Coordinates Network (GCN), and observe the prompt emission and early afterglow phase from GRBs. In the last two years of operation several GRB follow-up observations were performed by MAGIC, however, until now without successful detection of VHE gamma rays above threshold energies >100 GeV. In this paper we revise the expectations for the GRB observations with MAGIC, based on the experience from the last years of operation.

  1. Registration of atmospheric neutrinos with the Baikal neutrino telescope

    E-Print Network [OSTI]

    Baikal Collaboration; V. A. Balkanov et al

    1999-03-23

    We present first neutrino induced events observed with a deep underwater neutrino telescope. Data from 70 days effective life time of the BAIKAL prototype telescope NT-96 have been analyzed with two different methods. With the standard track reconstruction method, 9 clear upward muon candidates have been identified, in good agreement with 8.7 events expected from Monte Carlo calculations for atmospheric neutrinos. The second analysis is tailored to muons coming from close to the opposite zenith. It yields 4 events, compared to 3.5 from Monte Carlo expectations. From this we derive a 90 % upper flux limit of 1.1 * 10^-13 cm^-2 sec^-1 for muons in excess of those expected from atmospheric neutrinos with zenith angle > 150 degrees and energy > 10GeV.

  2. FERMI LARGE AREA TELESCOPE OBSERVATIONS OF GRB 110625A

    SciTech Connect (OSTI)

    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)

    2012-08-01

    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.

  3. SLAC All Access: Fermi Gamma-ray Space Telescope

    ScienceCinema (OSTI)

    Romani, Roger

    2014-06-24

    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.

  4. First images on the sky from a hyper telescope

    E-Print Network [OSTI]

    E. Pedretti; A. Labeyrie; L. Arnold; N. Thureau; O. Lardiere; A. Boccaletti; P. Riaud

    2000-09-28

    We show star images obtained with a miniature ``densified pupil imaging interferometer'' also called a hyper-telescope. The formation of such images violates a ``golden rule of imaging interferometers'' which appeared to forbid the use of interferometric arrangements differing from a Fizeau interferometer. These produce useless images when the sub-apertures spacing is much wider than their size, owing to diffraction through the sub-apertures. The hyper-telescope arrangement solves these problems opening the way towards multi-kilometer imaging arrays in space. We experimentally obtain an intensity gain of 24 +- 3X when a densified-pupil interferometer is compared to an equivalent Fizeau-type interferometer and show images of the double star alpha Gem. The initial results presented confirm the possibility of directly obtaining high resolution and high dynamic range images in the recombined focal plane of a large interferometer if enough elements are used.

  5. The reflecting surface of the MAGIC-II Telescope

    E-Print Network [OSTI]

    D. Bastieri; J. Arnold; C. Baixeras; O. Citterio; F. Dazzi; B. De Lotto; M. Doro; M. Ghigo; E. Giro; F. Goebel; R. Kosyra; E. Lorenz; M. Mariotti; R. Mirzoyan; R. Paoletti; G. Pareschi; D. Pascoli; A. Pepato; L. Peruzzo; A. Saggion; P. Sartori; A. Sillanpää

    2007-09-10

    The MAGIC Collaboration is building a second telescope, MAGIC II, improving the design of the current MAGIC Telescope. MAGIC II is being built at 85 m of distance from MAGIC I, and will also feature a huge reflecting surface of ~240 m$^2$ of area. One of the improvement is the design for the mirror of MAGIC II, that are lighter and larger, being square of 1 m of side and weighting around 15 kg. For the development and production of the new mirrors, two different techniques, both reliable and affordable in price, were selected: the diamond milling of aluminium surfaces and the cold slumping of thin glass panes. As tests for the second one are still ongoing, we present a description of the diamond milling technique, and its application and performance to the produced mirrors.

  6. Laser metrology for coherent multi-telescope arrays

    DOE Patents [OSTI]

    Shao, M.; Massie, N.A.

    1993-05-04

    In multi-telescope arrays that comprise multiple telescopes, a beam-combining module, and flat mirrors for directing light beams from the multiple telescopes to the beam combining module, a laser metrology system is used for monitoring various pathlengths along a beam path where deviations are likely. Some pathlengths are defined simply by a pair of retroreflectors or reflectors at both ends. Lengths between pairs of retroreflectors are measured and monitored by laser interferometers. One critical pathlength deviation is related to the displacement of the flat mirror. A reference frame is set up relative to the beam-combining module to form and define the coordinate system within which the positions of the flat mirrors are measured and monitored. In the preferred embodiment, a pair of retroreflectors along the optical axis of the beam-combining module defines a reference frame. A triangle is formed by the reference frame as the base and another retroreflector at the flat mirror as the vertex. The triangle is used to monitor the position of the flat mirror. A beam's pathlength is dynamically corrected in response to the monitored deviations.

  7. Laser metrology for coherent multi-telescope arrays

    DOE Patents [OSTI]

    Shao, Michael (Pasadena, CA); Massie, Norbert A. (San Ramon, CA)

    1993-01-01

    In multi-telescope arrays that comprise multiple telescopes, a beam-combining module, and flat mirrors for directing light beams from the multiple telescopes to the beam combining module, a laser metrology system is used for monitoring various pathlengths along a beam path where deviations are likely. Some pathlengths are defined simply by a pair of retroreflectors or reflectors at both ends. Lengths between pairs of retroreflectors are measured and monitored by laser interferometers. One critical pathlength deviation is related to the displacement of the flat mirror. A reference frame is set up relative to the beam-combining module to form and define the coordinate system within which the positions of the flat mirrors are measured and monitored. In the preferred embodiment, a pair of retroreflectors along the optical axis of the beam-combining module defines a reference frame. A triangle is formed by the reference frame as the base and another retroreflector at the flat mirror as the vertex. The triangle is used to monitor the position of the flat mirror. A beam's pathlength is dynamically corrected in response to the monitored deviations.

  8. SETI reloaded, Next Generation Radio Telescopes, Transients and Cognitive Computing

    E-Print Network [OSTI]

    Garrett, Michael A

    2015-01-01

    The Search for Extra-terrestrial Intelligence (SETI) using radio telescopes is an area of research that is now more than 50 years old. Thus far, both targeted and wide-area surveys have yet to detect artificial signals from intelligent civilisations. In this paper, I argue that the incidence of co-existing intelligent and communicating civilisations is probably small in the Milky Way. While this makes successful SETI searches a very difficult pursuit indeed, the huge impact of even a single detection requires us to continue the search. A substantial increase in the overall performance of radio telescopes (and in particular future wide-field instruments such as the Square Kilometre Array, SKA), provide renewed optimism in the field. Evidence for this is already to be seen in the success of SETI researchers in acquiring observations on some of the world's most sensitive radio telescope facilities via open, peer-reviewed processes. The increasing interest in the dynamic radio sky, and our ability to detect new a...

  9. The Instrument Response Function Format for the Cherenkov Telescope Array

    E-Print Network [OSTI]

    Ward, John E

    2015-01-01

    The Cherenkov Telescope Array (CTA) is a future ground-based observatory (with two locations, in the Northern and Southern Hemispheres) that will be used in the study of the very-high-energy gamma-ray sky. CTA observations will be proposed by external users or initiated by the observatory, with the resulting measurements being processed by the CTA observatory and the reduced data made accessible to the corresponding proposer. Instrument Response Functions (IRFs) will also be provided to convert the quantities measured by the array(s) into relevant science products (i.e. spectra, sky maps, light curves). As the response of the telescopes depend on many correlated observational and physical quantities (e.g. gamma-ray arrival direction, energy, telescope orientation, background light, weather conditions etc.) the CTA IRFs could grow into increasingly larger and larger file sizes, which can become unwieldy or impractical for use in specific observation cases. To this end, a customized IRF format (complying with t...

  10. Sloan Digital Sky Survey photometric telescope automation and observing software

    SciTech Connect (OSTI)

    Eric H. Neilsen, Jr. et al.

    2002-10-16

    The photometric telescope (PT) provides observations necessary for the photometric calibration of the Sloan Digital Sky Survey (SDSS). Because the attention of the observing staff is occupied by the operation of the 2.5 meter telescope which takes the survey data proper, the PT must reliably take data with little supervision. In this paper we describe the PT's observing program, MOP, which automates most tasks necessary for observing. MOP's automated target selection is closely modeled on the actions a human observer might take, and is built upon a user interface that can be (and has been) used for manual operation. This results in an interface that makes it easy for an observer to track the activities of the automating procedures and intervene with minimum disturbance when necessary. MOP selects targets from the same list of standard star and calibration fields presented to the user, and chooses standard star fields covering ranges of airmass, color, and time necessary to monitor atmospheric extinction and produce a photometric solution. The software determines when additional standard star fields are unnecessary, and selects survey calibration fields according to availability and priority. Other automated features of MOP, such as maintaining the focus and keeping a night log, are also built around still functional manual interfaces, allowing the observer to be as active in observing as desired; MOP's automated features may be used as tools for manual observing, ignored entirely, or allowed to run the telescope with minimal supervision when taking routine data.

  11. Cosmological Questions for the European Southern Observatory Very Large Telescope

    E-Print Network [OSTI]

    David Tytler

    1996-08-12

    The next decade promises an observational revolution which will change cosmology forever. The precise measurement of the angular anisotropy of the cosmic microwave background should specify to a few percent all of the parameters of the cosmological model which effect astrophysics. The growth of structure will then be determined (but not yet observed) until gravitational collapse becomes highly non-linear and stars, galaxies and active galactic nuclei (AGN) form. These processes are hard to model with basic physics because they are complex and allow a rich variety of expression. Instead observations will determine when the first stars and quasars formed, and how and when galaxies assembled. If we can reconcile the numerous contradictions which characterize the subject today, cosmology will become a mature subject, founded on the agreement between detailed, inclusive and realistic models, which make precise predictions, and the wealth of new data which will come from a wide variety of observations, at all wavelengths. This is an ambitious schedule, but nothing less is worthy of the outstanding capabilities of the 8 -- 10 m telescopes, the next generation space telescope, the opportunities at millimeterto sub-millimeter wavelengths and advanced computer modeling. The ESO Very Large Telescope (VLT) should play a major role in this revolution.

  12. INFN Camera demonstrator for the Cherenkov Telescope Array

    E-Print Network [OSTI]

    ,

    2015-01-01

    The Cherenkov Telescope Array is a world-wide project for a new generation of ground-based Cherenkov telescopes of the Imaging class with the aim of exploring the highest energy region of the electromagnetic spectrum. With two planned arrays, one for each hemisphere, it will guarantee a good sky coverage in the energy range from a few tens of GeV to hundreds of TeV, with improved angular resolution and a sensitivity in the TeV energy region better by one order of magnitude than the currently operating arrays. In order to cover this wide energy range, three different telescope types are envisaged, with different mirror sizes and focal plane features. In particular, for the highest energies a possible design is a dual-mirror Schwarzschild-Couder optical scheme, with a compact focal plane. A silicon photomultiplier (SiPM) based camera is being proposed as a solution to match the dimensions of the pixel (angular size of ~ 0.17 degrees). INFN is developing a camera demonstrator made by 9 Photo Sensor Modules (PSMs...

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

    E-Print Network [OSTI]

    Shefferson, Richard P.

    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

  14. PARAID: The Gear-Shifting Power-Aware RAID Charles Weddle, Mathew Oldham, Jin Qian, An-I Andy Wang, Florida State University

    E-Print Network [OSTI]

    Wang, Andy

    1 PARAID: The Gear-Shifting Power-Aware RAID Charles Weddle, Mathew Oldham, Jin Qian, An-I Andy of all the disks in the array for even light loads. This paper introduces the gear-shifting Power the performance demands. Based on our 4-gear PARAID prototype, PARAID consumes 19% less power than a conventional

  15. A Pervasive Computing Solution to Asset, Problem and Knowledge Management Suman K. Kalia, Charles C. Tappert, Allen Stix, and Fred Grossman

    E-Print Network [OSTI]

    Tappert, Charles

    A Pervasive Computing Solution to Asset, Problem and Knowledge Management Suman K. Kalia, Charles C the conceptualization, design, and construction of wireless laptop and PDA-based asset, problem and knowledge management Operating System PDA based asset, problem and knowledge management systems to assist a divisional desktop

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

    E-Print Network [OSTI]

    Leiserson, Charles E.

    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

  17. Sanders, J. E.; and Merguerian, Charles, 1991a, Pleistocene tills in the New York City region: new evidence confirms multiple (three and possibly four) glaciations from two

    E-Print Network [OSTI]

    Merguerian, Charles

    Sanders, J. E.; and Merguerian, Charles, 1991a, Pleistocene tills in the New York City region: new, Pleistocene tills in the New York City region: new evidence confirms multiple (three and possibly four Valley. At least two earlier glaciers, ages not yet known, flowed across the Hudson valley. New evidence

  18. Solvent Swelling Activation of a Mechanophore in a Polymer Corissa K. Lee, Charles E. Diesendruck, Enjiong Lu, Austin N. Pickett, Preston A. May, Jeffrey S. Moore,

    E-Print Network [OSTI]

    Braun, Paul

    Solvent Swelling Activation of a Mechanophore in a Polymer Network Corissa K. Lee, Charles E is incorporated as a cross-linker. A correlation is observed between solvent-induced polymer swelling and not solvent effects. Systematic studies varying solvents and cross-linking densities provide insight into how

  19. Merguerian, Charles, 1981c, Tectonic History of New York City area. An examination of bedrock in the New York City area indicates the presence of

    E-Print Network [OSTI]

    Merguerian, Charles

    Merguerian, Charles, 1981c, Tectonic History of New York City area. An examination of bedrock in the New York City area indicates the presence of lithologies that are not a part of the Cambro Connecticut and rocks mapped as the Manhattan B-C by Leo Hall in southeastern New York. Detailed mapping

  20. Merguerian, Charles, 1986c, The bedrock geology of New York City (abs.): Abstracts with Programs, Symposium on The Geology of Southern New York, Hofstra University, p. 8.

    E-Print Network [OSTI]

    Merguerian, Charles

    Merguerian, Charles, 1986c, The bedrock geology of New York City (abs.): Abstracts with Programs, Symposium on The Geology of Southern New York, Hofstra University, p. 8. Detailed mapping and sampling, and NW trends. Recent seismicity in southeastern New York has refocused attention on these faults

  1. Wind Display Device for Locomotion Interface in a Virtual Environment Sandip Kulkarni, Charles Fisher, Eric Pardyjak, Mark Minor and John Hollerbach

    E-Print Network [OSTI]

    Hollerbach, John M.

    on the user. These wind forces will be integrated with the graphical display [6, 7] and the Quick Urban Industrial Complex (QUIC) dispersion modeling system [8] to determine the wind flow patterns for improvedWind Display Device for Locomotion Interface in a Virtual Environment Sandip Kulkarni, Charles

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

    E-Print Network [OSTI]

    Moon, Un-Ku

    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

  3. High resolution telescope including an array of elemental telescopes aligned along a common axis and supported on a space frame with a pivot at its geometric center

    DOE Patents [OSTI]

    Norbert, M.A.; Yale, O.

    1992-04-28

    A large effective-aperture, low-cost optical telescope with diffraction-limited resolution enables ground-based observation of near-earth space objects. The telescope has a non-redundant, thinned-aperture array in a center-mount, single-structure space frame. It employes speckle interferometric imaging to achieve diffraction-limited resolution. The signal-to-noise ratio problem is mitigated by moving the wavelength of operation to the near-IR, and the image is sensed by a Silicon CCD. The steerable, single-structure array presents a constant pupil. The center-mount, radar-like mount enables low-earth orbit space objects to be tracked as well as increases stiffness of the space frame. In the preferred embodiment, the array has elemental telescopes with subaperture of 2.1 m in a circle-of-nine configuration. The telescope array has an effective aperture of 12 m which provides a diffraction-limited resolution of 0.02 arc seconds. Pathlength matching of the telescope array is maintained by a electro-optical system employing laser metrology. Speckle imaging relaxes pathlength matching tolerance by one order of magnitude as compared to phased arrays. Many features of the telescope contribute to substantial reduction in costs. These include eliminating the conventional protective dome and reducing on-site construction activities. The cost of the telescope scales with the first power of the aperture rather than its third power as in conventional telescopes. 15 figs.

  4. High resolution telescope including an array of elemental telescopes aligned along a common axis and supported on a space frame with a pivot at its geometric center

    DOE Patents [OSTI]

    Norbert, Massie A. (San Ramon, CA); Yale, Oster (Danville, CA)

    1992-01-01

    A large effective-aperture, low-cost optical telescope with diffraction-limited resolution enables ground-based observation of near-earth space objects. The telescope has a non-redundant, thinned-aperture array in a center-mount, single-structure space frame. It employes speckle interferometric imaging to achieve diffraction-limited resolution. The signal-to-noise ratio problem is mitigated by moving the wavelength of operation to the near-IR, and the image is sensed by a Silicon CCD. The steerable, single-structure array presents a constant pupil. The center-mount, radar-like mount enables low-earth orbit space objects to be tracked as well as increases stiffness of the space frame. In the preferred embodiment, the array has elemental telescopes with subaperture of 2.1 m in a circle-of-nine configuration. The telescope array has an effective aperture of 12 m which provides a diffraction-limited resolution of 0.02 arc seconds. Pathlength matching of the telescope array is maintained by a electro-optical system employing laser metrology. Speckle imaging relaxes pathlength matching tolerance by one order of magnitude as compared to phased arrays. Many features of the telescope contribute to substantial reduction in costs. These include eliminating the conventional protective dome and reducing on-site construction activities. The cost of the telescope scales with the first power of the aperture rather than its third power as in conventional telescopes.

  5. Extreme multiplex spectroscopy at wide-field 4-m telescopes

    E-Print Network [OSTI]

    Robert Content; Tom Shanks

    2008-08-18

    We describe the design and science case for a spectrograph for the prime focus of classical 4-m wide-field telescopes that can deliver at least 4000 MOS slits over a 1 degree field. This extreme multiplex capability means that 25000 galaxy redshifts can be measured in a single night, opening up the possibilities for large galaxy redshift surveys out to z~0.7 and beyond for the purpose of measuring the Baryon Acoustic Oscillation (BAO) scale and for many other science goals. The design features four cloned spectrographs and exploits the exclusive possibility of tiling the focal plane of wide-field 4-m telescopes with CCDs for multi-object spectroscopic purposes. In ~200 night projects, such spectrographs have the potential to make galaxy redshift surveys of ~6 million galaxies over a wide redshift range and thus may provide a low-cost alternative to other survey routes such as WFMOS and SKA. Two of these extreme multiplex spectrographs are currently being designed for the AAT (NG1dF) and Calar Alto (XMS) 4-m class telescopes. NG2dF, a larger version for the AAT 2 degree field, would have 12 clones and at least 12000 slits. The clones use a transparent design including a grism in which all optics are smaller than the clone square subfield so that the clones can be tightly packed with little gaps between the contiguous fields. Only low cost glasses are used; the variations in chromatic aberrations between bands are compensated by changing one or two of the lenses adjacent to the grism. The total weight and length is smaller with a few clones than a unique spectrograph which makes it feasible to place the spectrograph at the prime focus.

  6. An Optical Reflector for the CANGAROO-II Telescope

    E-Print Network [OSTI]

    Kawachi, A; Dazeley, S A; Edwards, P G; Gunji, S; Hara, S; Hara, T; Jinbo, J; Kifune, T; Kubo, H; Matsubara, Y; Mizumoto, Y; Mori, M; Moriya, M; Muraishi, H; Muraki, Y; Naito, T; Nishijima, K; Patterson, J R; Roberts, M D; Rowell, G P; Sako, T; Sakurazawa, K; Sato, Y; Susukita, R; Tamura, T; Tanimori, T; Yanagita, S; Yoshida, T; Yoshikoshi, T; Yuki, A; Kawachi, Akiko

    1999-01-01

    We have been successful in developing light and durable mirrors made of CFRP (Carbon Fiber Reinforced Plastic) laminates for the reflector of the new CANGAROO-II 7 m telescope. The reflector has a parabolic shape (F/1.1) with a 30 m^2 effective area which consists of 60 small spherical mirrors of CFRP laminates. The orientation of each mirror can be remotely adjusted by stepping motors. After the first adjustment work, the reflector offers a point image of about $0.^\\circ 14$ (FWHM) on the optic axis.

  7. An Optical Reflector for the CANGAROO-II Telescope

    E-Print Network [OSTI]

    Akiko Kawachi; J. Kushida; S. A. Dazeley; S. A. Dazeley; P. G. Edwards; S. Gunji; S. Hara; T. Hara; J. Jinbo; T. Kifune; H. Kubo; Y. Matsubara; Y. Mizumoto; M. Mori; M. Moriya; H. Muraishi; Y. Muraki; T. Naito; K. Nishijima; J. R. Patterson; M. D. Roberts; G. P. Rowell; T. Sako; K. Sakurazawa; Y. Sato; R. Susukita; T. Tamura; T. Tanimori; S. Yanagita; T. Yoshida; T. Yoshikoshi; A. Yuki

    1999-06-04

    We have been successful in developing light and durable mirrors made of CFRP (Carbon Fiber Reinforced Plastic) laminates for the reflector of the new CANGAROO-II 7 m telescope. The reflector has a parabolic shape (F/1.1) with a 30 m^2 effective area which consists of 60 small spherical mirrors of CFRP laminates. The orientation of each mirror can be remotely adjusted by stepping motors. After the first adjustment work, the reflector offers a point image of about $0.^\\circ 14$ (FWHM) on the optic axis.

  8. Edge Detection, Cosmic Strings and the South Pole Telescope

    E-Print Network [OSTI]

    Andrew Stewart; Robert Brandenberger

    2009-01-07

    We develop a method of constraining the cosmic string tension $G\\mu$ which uses the Canny edge detection algorithm as a means of searching CMB temperature maps for the signature of the Kaiser-Stebbins effect. We test the potential of this method using high resolution, simulated CMB temperature maps. By modeling the future output from the South Pole Telescope project (including anticipated instrumental noise), we find that cosmic strings with $G\\mu > 5.5\\times10^{-8}$ could be detected.

  9. Sites in Argentina for the Cherenkov Telescope Array Project

    E-Print Network [OSTI]

    Allekotte, Ingo; Etchegoyen, Alberto; García, Beatriz; Mancilla, Alexis; Maya, Javier; Ravignani, Diego; Rovero, Adrián

    2013-01-01

    The Cherenkov Telescope Array (CTA) Project will consist of two arrays of atmospheric Cherenkov telescopes to study high-energy gamma radiation in the range of a few tens of GeV to beyond 100 TeV. To achieve full-sky coverage, the construction of one array in each terrestrial hemisphere is considered. Suitable candidate sites are being explored and characterized. The candidate sites in the Southern Hemisphere include two locations in Argentina, one in San Antonio de los Cobres (Salta Province, Lat. 24:02:42 S, Long. 66:14:06 W, at 3600 m.a.s.l) and another one in El Leoncito (San Juan Province, Lat. 31:41:49 S, Long. 69:16:21 W, at 2600 m.a.s.l). Here we describe the two sites and the instrumentation that has been deployed to characterize them. We summarize the geographic, atmospheric and climatic data that have been collected for both of them.

  10. The Atacama Cosmology Telescope: Data Characterization and Map Making

    E-Print Network [OSTI]

    Dünner, Rolando; Marriage, Tobias A; Sievers, Jon; Acquaviva, Viviana; Addison, Graeme E; Ade, Peter A R; Aguirre, Paula; Amiri, Mandana; Appel, John William; Barrientos, L Felipe; Battistelli, Elia S; Bond, J Richard; Brown, Ben; Burger, Bryce; Calabarese, Erminia; Chervenak, Jay; Das, Sudeep; Devlin, Mark J; Dicker, Simon R; Doriese, W Bertrand; Dunkley, Joanna; Essinger-Hileman, Thomas; Fisher, Ryan P; Gralla, Megan B; Fowler, Joseph W; Hajian, Amir; Halpern, Mark; Hernández-Monteagudo, Carlos; Hilton, Gene C; Hilton, Matt; Hincks, Adam D; Hlozek, Renée; Huffenberger, Kevin M; Hughes, David H; Hughes, John P; Infante, Leopoldo; Irwin, Kent D; Juin, Jean Baptiste; Kaul, Madhuri; Klein, Jeff; Kosowsky, Arthur; Lau, Judy M; Limon, Michele; Lin, Yen-Ting; Louis, Thibaut; Lupton, Robert H; Marsden, Danica; Martocci, Krista; Mauskopf, Phil; Menanteau, Felipe; Moodley, Kavilan; Moseley, Harvey; Netterfield, Calvin B; Niemack, Michael D; Nolta, Michael R; Page, Lyman A; Parker, Lucas; Partridge, Bruce; Quintana, Hernán; Reid, Beth; Sehgal, Neelima; Sherwin, Blake D; Spergel, David N; Staggs, Suzanne T; Swetz, Daniel S; Switzer, Eric R; Thornton, Robert; Trac, Hy; Tucker, Carole; Warne, Ryan; Wilson, Grant; Wollack, Ed; Zhao, Yue

    2012-01-01

    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 hours of data (11 TB for the 148 GHz band only), with a daily average of 10.5 hours of observation. From these, 1085 hours were devoted to a 850 deg^2 stripe (11.2 hours by 9.1 deg) centered on a declination of -52.7 deg, while 175 hours were devoted to a 280 deg^2 stripe (4.5 hours by 4.8 deg) centered at the celestial equator. We discuss sources of statistical and systematic noise, calibration, telescope pointing, and data selection. Out of 1260 survey hours and 1024 detectors per array, 816 hours and 593 effective detectors remain after data selection for this frequency band, yielding a 38% survey efficiency. The total sensitivity in 2008, determined from the noise level between 5 Hz and 20 Hz in the time-o...

  11. Strong gravitational lensing of gravitational waves in Einstein Telescope

    SciTech Connect (OSTI)

    Piórkowska, Aleksandra; Biesiada, Marek [Department of Astrophysics and Cosmology, Institute of Physics, University of Silesia, Uniwersytecka 4, 40-007 Katowice (Poland); Zhu, Zong-Hong, E-mail: aleksandra.piorkowska@us.edu.pl, E-mail: marek.biesiada@us.edu.pl, E-mail: zhuzh@bnu.edu.cn [Department of Astronomy, Beijing Normal University, Beijing 100875 (China)

    2013-10-01

    Gravitational wave experiments have entered a new stage which gets us closer to the opening a new observational window on the Universe. In particular, the Einstein Telescope (ET) is designed to have a fantastic sensitivity that will provide with tens or hundreds of thousand NS-NS inspiral events per year up to the redshift z = 2. Some of such events should be gravitationally lensed by intervening galaxies. We explore the prospects of observing gravitationally lensed inspiral NS-NS events in the Einstein telescope. Being conservative we consider the lens population of elliptical galaxies. It turns out that depending on the local insipral rate ET should detect from one per decade detection in the pessimistic case to a tens of detections per year for the most optimistic case. The detection of gravitationally lensed source in gravitational wave detectors would be an invaluable source of information concerning cosmography, complementary to standard ones (like supernovae or BAO) independent of the local cosmic distance ladder calibrations.

  12. The On-Site Analysis of the Cherenkov Telescope Array

    E-Print Network [OSTI]

    Bulgarelli, Andrea; Zoli, Andrea; Aboudan, Alessio; Rodríguez-Vázquez, Juan José; De Cesare, Giovanni; De Rosa, Adriano; Maier, Gernot; Lyard, Etienne; Bastieri, Denis; Lombardi, Saverio; Tosti, Gino; Bergamaschi, Sonia; Beneventano, Domenico; Lamanna, Giovanni; Jacquemier, Jean; Kosack, Karl; Antonelli, Lucio Angelo; Boisson, Catherine; Borkowski, Jerzy; Buson, Sara; Carosi, Alessandro; Conforti, Vito; Colomé, Pep; Reyes, Raquel de los; Dumm, Jon; Evans, Phil; Fortson, Lucy; Fuessling, Matthias; Gotz, Diego; Graciani, Ricardo; Gianotti, Fulvio; Grandi, Paola; Hinton, Jim; Humensky, Brian; Inoue, Susumu; Knödlseder, Jürgen; Flour, Thierry Le; Lindemann, Rico; Malaguti, Giuseppe; Markoff, Sera; Marisaldi, Martino; Neyroud, Nadine; Nicastro, Luciano; Ohm, Stefan; Osborne, Julian; Oya, Igor; Rodriguez, Jerome; Rosen, Simon; Ribo, Marc; Tacchini, Alessandro; Schüssler, Fabian; Stolarczyk, Thierry; Torresi, Eleonora; Testa, Vincenzo; Wegner, Peter

    2015-01-01

    The Cherenkov Telescope Array (CTA) observatory will be one of the largest ground-based very high-energy gamma-ray observatories. The On-Site Analysis will be the first CTA scientific analysis of data acquired from the array of telescopes, in both northern and southern sites. The On-Site Analysis will have two pipelines: the Level-A pipeline (also known as Real-Time Analysis, RTA) and the level-B one. The RTA performs data quality monitoring and must be able to issue automated alerts on variable and transient astrophysical sources within 30 seconds from the last acquired Cherenkov event that contributes to the alert, with a sensitivity not worse than the one achieved by the final pipeline by more than a factor of 3. The Level-B Analysis has a better sensitivity (not be worse than the final one by a factor of 2) and the results should be available within 10 hours from the acquisition of the data: for this reason this analysis could be performed at the end of an observation or next morning. The latency (in part...

  13. Deployable telescope having a thin-film mirror and metering structure

    DOE Patents [OSTI]

    Krumel, Leslie J. (Cedar Crest, NM); Martin, Jeffrey W. (Albuquerque, NM)

    2010-08-24

    A deployable thin-film mirror telescope comprises a base structure and a metering structure. The base structure houses a thin-film mirror, which can be rolled for stowage and unrolled for deployment. The metering structure is coupled to the base structure and can be folded for stowage and unfolded for deployment. In the deployed state, the unrolled thin-film mirror forms a primary minor for the telescope and the unfolded metering structure positions a secondary minor for the telescope.

  14. Observation of solar flares through the ART-P telescope side shield

    E-Print Network [OSTI]

    A. Lutovinov; M. Pavlinsky; S. Grebenev

    2001-06-13

    Some preliminary results of observations of six solar flares though the ART-P telescop side shield in 1990-1992 are presented.

  15. Measurement of the Cosmic Microwave Background Polarization with the BICEP Telescope at the South Pole

    E-Print Network [OSTI]

    Takahashi, Yuki David

    2010-01-01

    South Pole Dark Sector and LC-130 . . . . . . .2.2 South Pole site . . . . . . . . . . . . . .Bicep Telescope at the South Pole by Yuki David Takahashi A

  16. Development of the photomultiplier tube readout system for the first Large-Sized Telescope of the Cherenkov Telescope Array

    E-Print Network [OSTI]

    Masuda, Shu; Barrio, Juan Abel; Bigas, Oscar Blanch; Delgado, Carlos; Coromina, Lluís Freixas; Gunji, Shuichi; Hadasch, Daniela; Hatanaka, Kenichiro; Ikeno, Masahiro; Laguna, Jose Maria Illa; Inome, Yusuke; Ishio, Kazuma; Katagiri, Hideaki; Kubo, Hidetoshi; Martínez, Gustavo; Mazin, Daniel; Nakajima, Daisuke; Nakamori, Takeshi; Ohoka, Hideyuki; Paoletti, Riccardo; Ritt, Stefan; Rugliancich, Andrea; Saito, Takayuki; Sulanke, Karl-Heinz; Takeda, Junki; Tanaka, Manobu; Tanigawa, Shunsuke; Tejedor, Luis Ángel; Teshima, Masahiro; Tsuchiya, Yugo; Uchida, Tomohisa; Yamamoto, Tokonatsu

    2015-01-01

    The Cherenkov Telescope Array (CTA) is the next generation ground-based very high energy gamma-ray observatory. The Large-Sized Telescope (LST) of CTA targets 20 GeV -- 1 TeV gamma rays and has 1855 photomultiplier tubes (PMTs) installed in the focal plane camera. With the 23 m mirror dish, the night sky background (NSB) rate amounts to several hundreds MHz per pixel. In order to record clean images of gamma-ray showers with minimal NSB contamination, a fast sampling of the signal waveform is required so that the signal integration time can be as short as the Cherenkov light flash duration (a few ns). We have developed a readout board which samples waveforms of seven PMTs per board at a GHz rate. Since a GHz FADC has a high power consumption, leading to large heat dissipation, we adopted the analog memory ASIC "DRS4". The sampler has 1024 capacitors per channel and can sample the waveform at a GHz rate. Four channels of a chip are cascaded to obtain deeper sampling depth with 4096 capacitors. After a trigger ...

  17. Design of a prototype device to calibrate the Large Size Telescope camera of the Cherenkov Telescope Array

    E-Print Network [OSTI]

    Iori, M; De Persio, F; Chatterjee, A; Ferrarotto, F; Nagesh, B K; Saha, L; Singh, B B

    2015-01-01

    The Cherenkov Telescope Array is a project that aims to exploring the highest energy region of electromagnetic spectrum. Two arrays, one for each hemisphere, will cover the full sky in a range from few tens of GeV to hundreds of TeV improving the sensitivity and angular resolution of the present operating arrays. A prototype of the Large Size Telescope (LST) for the study of gamma ray astronomy above some tens of GeV will be installed at the Canary Island of La Palma in 2016. The LST camera, made by an array of photomultipliers (PMTs), requires an accurate and systematic calibration over a wide dynamic range. In this contribution, we present an optical calibration system made by a 355 nm wavelength laser with 400 ps pulse width, 1 muJ output energy, up to 4k Hz repetition rate and a set of neutral density filters to obtain a wide range of photon intensities, up to 1000 photoelectrons/PMT, to be sent to the camera plane 28 m away. The number of photons after the diffuser of the calibration box, located in the ...

  18. Photometric Calibration of the Swift Ultraviolet/Optical Telescope

    E-Print Network [OSTI]

    Poole, T S; Page, M J; Landsman, W; Holland, S T; Roming, P; Kuin, N P M; Brown, P J; Gronwall, C; Hunsberger, S; Koch, S; Mason, K O; Schady, P; Berk, D Vanden; Blustin, A J; Boyd, P; Broos, P; Carter, M; Chester, M M; Cucchiara, A; Hancock, B; Huckle, H; Immler, S; Ivanushkina, M; Kennedy, T; Marshall, F; Morgan, A; Pandey, S; de Pasquale, M; Smith, P J; Still, M

    2007-01-01

    We present the photometric calibration of the Swift UltraViolet/Optical Telescope (UVOT) which includes: optimum photometric and background apertures, effective area curves, colour transformations, conversion factors for count rates to flux, and the photometric zero points (which are accurate to better than 4 per cent) for each of the seven UVOT broadband filters. The calibration was performed with observations of standard stars and standard star fields that represent a wide range of spectral star types. The calibration results include the position dependent uniformity, and instrument response over the 1600-8000A operational range. Because the UVOT is a photon counting instrument, we also discuss the effect of coincidence loss on the calibration results. We provide practical guidelines for using the calibration in UVOT data analysis. The results presented here supersede previous calibration results.

  19. Paper II: Calibration of the Swift ultraviolet/optical telescope

    E-Print Network [OSTI]

    Breeveld, A A; Hoversten, E A; Koch, S; Landsman, W; Marshall, F E; Page, M J; Poole, T S; Roming, P; Smith, P J; Still, M; Yershov, V; Blustin, A J; Brown, P J; Gronwall, C; Holland, S T; Kuin, N P M; McGowan, K; Rosen, S; Boyd, P; Broos, P; Carter, M; Chester, M M; Hancock, B; Huckle, H; Immler, S; Ivanushkina, M; Kennedy, T; Mason, K O; Morgan, A N; Oates, S; de Pasquale, M; Schady, P; Siegel, M; Berk, D Vanden

    2010-01-01

    The Ultraviolet/Optical Telescope (UVOT) is one of three instruments onboard the Swift observatory. The photometric calibration has been published, and this paper follows up with details on other aspects of the calibration including a measurement of the point spread function with an assessment of the orbital variation and the effect on photometry. A correction for large scale variations in sensitivity over the field of view is described, as well as a model of the coincidence loss which is used to assess the coincidence correction in extended regions. We have provided a correction for the detector distortion and measured the resulting internal astrometric accuracy of the UVOT, also giving the absolute accuracy with respect to the International Celestial Reference System. We have compiled statistics on the background count rates, and discuss the sources of the background, including instrumental scattered light. In each case we describe any impact on UVOT measurements, whether any correction is applied in the st...

  20. Photometric Calibration of the Swift Ultraviolet/Optical Telescope

    E-Print Network [OSTI]

    T. S. Poole; A. A. Breeveld; M. J. Page; W. Landsman; S. T. Holland; P. Roming; N. P. M. Kuin; P. J. Brown; C. Gronwall; S. Hunsberger; S. Koch; K. O. Mason; P. Schady; D. Vanden Berk; A. J. Blustin; P. Boyd; P. Broos; M. Carter; M. M. Chester; A. Cucchiara; B. Hancock; H. Huckle; S. Immler; M. Ivanushkina; T. Kennedy; F. Marshall; A. Morgan; S. Pandey; M. de Pasquale; P. J. Smith; M. Still

    2007-11-09

    We present the photometric calibration of the Swift UltraViolet/Optical Telescope (UVOT) which includes: optimum photometric and background apertures, effective area curves, colour transformations, conversion factors for count rates to flux, and the photometric zero points (which are accurate to better than 4 per cent) for each of the seven UVOT broadband filters. The calibration was performed with observations of standard stars and standard star fields that represent a wide range of spectral star types. The calibration results include the position dependent uniformity, and instrument response over the 1600-8000A operational range. Because the UVOT is a photon counting instrument, we also discuss the effect of coincidence loss on the calibration results. We provide practical guidelines for using the calibration in UVOT data analysis. The results presented here supersede previous calibration results.

  1. Data model issues in the Cherenkov Telescope Array project

    E-Print Network [OSTI]

    Contreras, J L; Bernlöhr, K; Boisson, C; Bregeon, J; Bulgarelli, A; de Cesare, G; Reyes, R de los; Fioretti, V; Kosack, K; Lavalley, C; Lyard, E; Marx, R; Rico, J; Sanguillot, M; Servillat, M; Walter, R; Ward, J E

    2015-01-01

    The planned Cherenkov Telescope Array (CTA), a future ground-based Very-High-Energy (VHE) gamma-ray observatory, will be the largest project of its kind. It aims to provide an order of magnitude increase in sensitivity compared to currently operating VHE experiments and open access to guest observers. These features, together with the thirty years lifetime planned for the installation, impose severe constraints on the data model currently being developed for the project. In this contribution we analyze the challenges faced by the CTA data model development and present the requirements imposed to face them. While the full data model is still not completed we show the organization of the work, status of the design, and an overview of the prototyping efforts carried out so far. We also show examples of specific aspects of the data model currently under development.

  2. Data compression for the First G-APD Cherenkov Telescope

    E-Print Network [OSTI]

    Ahnen, M L; Bergmann, M; Biland, A; Bretz, T; Buß, J; Dorner, D; Einecke, S; Freiwald, J; Hempfling, C; Hildebrand, D; Hughes, G; Lustermann, W; Lyard, E; Mannheim, K; Meier, K; Mueller, S; Neise, D; Neronov, A; Overkemping, A -K; Paravac, A; Pauss, F; Rhode, W; Steinbring, T; Temme, F; Thaele, J; Toscano, S; Vogler, P; Walter, R; Wilbert, A

    2015-01-01

    The First Geiger-mode Avalanche photodiode (G-APD) Cherenkov Telescope (FACT) has been operating on the Canary island of La Palma since October 2011. Operations were automated so that the system can be operated remotely. Manual interaction is required only when the observation schedule is modified due to weather conditions or in case of unexpected events such as a mechanical failure. Automatic operations enabled high data taking efficiency, which resulted in up to two terabytes of FITS files being recorded nightly and transferred from La Palma to the FACT archive at ISDC in Switzerland. Since long term storage of hundreds of terabytes of observations data is costly, data compression is mandatory. This paper discusses the design choices that were made to increase the compression ratio and speed of writing of the data with respect to existing compression algorithms. Following a more detailed motivation, the FACT compression algorithm along with the associated I/O layer is discussed. Eventually, the performances...

  3. Methods for point source analysis in high energy neutrino telescopes

    E-Print Network [OSTI]

    Jim Braun; Jon Dumm; Francesco De Palma; Chad Finley; Albrecht Karle; Teresa Montaruli

    2008-01-10

    Neutrino telescopes are moving steadily toward the goal of detecting astrophysical neutrinos from the most powerful galactic and extragalactic sources. Here we describe analysis methods to search for high energy point-like neutrino sources using detectors deep in the ice or sea. We simulate an ideal cubic kilometer detector based on real world performance of existing detectors such as AMANDA, IceCube, and ANTARES. An unbinned likelihood ratio method is applied, making use of the point spread function and energy distribution of simulated neutrino signal events to separate them from the background of atmospheric neutrinos produced by cosmic ray showers. The unbinned point source analyses are shown to perform better than binned searches and, depending on the source spectral index, the use of energy information is shown to improve discovery potential by almost a factor of two.

  4. Crystal diffraction lens telescope for focusing nuclear gamma rays

    SciTech Connect (OSTI)

    Smither, R.K.; Fernandez, P.B.; Graber, T. [Argonne National Lab., IL (United States). Advanced Photon Source; Ballmoos, P. von; Naya, J.; Albernhe, F.; Vedrenne, G. [Centre d`Etude Spatiale des Rayonnements, Toulouse (France); Faiz, M. [KFUPM, Dhahran (Saudi Arabia). Physics Dept.

    1996-08-01

    A crystal diffraction lens was constructed at Argonne National Laboratory for use as a telescope to focus nuclear gamma rays. It consisted of 600 single crystals of germanium arranged in 8 concentric rings. The mounted angle of each crystal was adjusted to intercept and diffract the incoming gamma rays with an accuracy of a few arc sec. The performance of the lens was tested in two ways. In one case, the gamma rays were focused on a single medium size germanium detector. In the second case, the gamma rays were focused on the central germanium detector of a 3 x 3 matrix of small germanium detectors. The efficiency, image concentration and image quality, and shape were measured. The tests performed with the 3 x 3 matrix detector system were particularly interesting. The wanted radiation was concentrated in the central detector. The 8 other detectors were used to detect the Compton scattered radiation, and their energy was summed with coincident events in the central detector. This resulted in a detector with the efficiency of a large detector (all 9 elements) and the background of a small detector (only the central element). The use of the 3 x 3 detector matrix makes it possible to tell if the source is off axis and, if so, to tell in which direction. The crystal lens acts very much like a simple convex lens for visible light. Thus if the source is off to the left then the image will focus off to the right illuminating the detector on the right side: telling one in which direction to point the telescope. Possible applications of this type of crystal lens to balloon and satellite experiments will be discussed.

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

    E-Print Network [OSTI]

    For large-diameter solar telescopes operating at the theoretical diffraction limit, one of the main designThe 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

  6. 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

  7. Hopkins Ultraviolet Telescope Observations of Nova Circini 1995 and Nova Aquilae 1995

    E-Print Network [OSTI]

    Hopkins Ultraviolet Telescope Observations of Nova Circini 1995 and Nova Aquilae 1995 Bradford W 1995 and Nova Aql 1995 with the Hopkins Ultraviolet Telescope during the Astro­2 space shuttle mission in 1995 March. The spectra cover the wavelength range from 820 š A to 1840 š A with a spectral resolution

  8. End-to-end absolute energy calibration of atmospheric fluorescence telescopes by an electron linear accelerator

    E-Print Network [OSTI]

    End-to-end absolute energy calibration of atmospheric fluorescence telescopes by an electron linear of fluorescence telescopes by using air showers induced by electron beams from a linear accelerator, which and constructing a compact linear accelerator with a maximum electron energy of 40 MeV and an intensity of 6.4 m

  9. THE NUCLEAR SPECTROSCOPIC TELESCOPE ARRAY (NuSTAR) HIGH-ENERGY X-RAY MISSION

    E-Print Network [OSTI]

    Chakrabarty, Deepto

    The Nuclear Spectroscopic Telescope Array (NuSTAR) mission, launched on 2012 June 13, is the first focusing high-energy X-ray telescope in orbit. NuSTAR operates in the band from 3 to 79 keV, extending the sensitivity of ...

  10. In-orbit performance of the XMM-Newton X-ray telescopes: images and spectra

    E-Print Network [OSTI]

    B. Aschenbach

    2001-09-21

    The performance of the three X-ray telescopes on-board of XMM-Newton is evaluated addressing imaging characteristics and effective collecting area. The agreement with ground calibration data is excellent. The analysis of images and spectra of cosmic X-ray sources, emphazising supernova and supernova remnants, prooves that the telescopes are even better than originally required.

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

    E-Print Network [OSTI]

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

    2009-03-16

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

  12. Wind tunnel testing of a generic telescope enclosure Tait S. Pottebaum*a

    E-Print Network [OSTI]

    MacMynowski, Douglas G. - MacMynowski, Douglas G.

    -buffeting, wind tunnel, DPIV 1. INTRODUCTION Various design studies are currently underway for the next generation that CFD can be used with confidence in future design work. Keywords: Extremely-Large-Telescopes, Wind with confidence in future design work. For an 80m diameter telescope dome in a 12m/s external wind (roughly the 85

  13. Multilayer coating facility for the HEFT hard X-ray telescope Carsten P. Jensena

    E-Print Network [OSTI]

    . Christensena , Hubert Chenb , Erik B. W.Smitta , Eric Zieglerc a Danish Space Research Institute (Denmark); b) for the production coating of depth graded multilayers on the thermally slumped glass segments which form the basis, Hard X-ray telescope 1. INTRODUCTION The High Energy Focusing Telescope (HEFT) is a balloon borne

  14. IL NUOVO CIMENTO Vol. ?, N. ? ? The Liverpool Telescope Automatic Pipeline for Realtime GRB

    E-Print Network [OSTI]

    Gomboc, Andreja

    IL NUOVO CIMENTO Vol. ?, N. ? ? The Liverpool Telescope Automatic Pipeline for Real­time GRB pipeline. PACS 95.55.Cs -- Ground­based ultraviolet, optical and infrared telescopes. PACS 95.75.Mn of the system is the subsequent pipelined data reduction, analysis and automatic identification of possible GRB

  15. CMS Pixel Telescope Addition to T-980 Bent Crystal Collimation Experiment at the Tevatron

    E-Print Network [OSTI]

    Rivera, Ryan; Johnson, Todd; Kwan, Simon; Lundberg, Carl; Still, Dean; Prosser, Alan; Uplegger, Lorenzo; Zagel, Jim; Zvodaya, Viktoriya

    2012-01-01

    An enhancement to the T-980 bent crystal collimation experiment at the Tevatron has been completed. The enhancement was the installation of a pixel telescope inside the vacuum-sealed beam pipe of the Tevatron. The telescope is comprised of six CMS PSI46 pixel plaquettes, arranged as three stations of horizontal and vertical planes, with the CAPTAN system for data acquisition and control. The purpose of the pixel telescope is to measure beam profiles produced by bent crystals under various conditions. The telescope electronics inside the beam pipe initially were not adequately shielded from the image current of the passing beams. A new shielding approach was devised and installed, which resolved the problem. The noise issues encountered and the mitigating techniques are presented herein, as well as some preliminary results from the telescope.

  16. CMS Pixel Telescope Addition to T-980 Bent Crystal Collimation Experiment at the Tevatron

    SciTech Connect (OSTI)

    Rivera, Ryan; Annala, Jerry; Johnson, Todd; Kwan, Simon; Lundberg, Carl; Still, Dean; Prosser, Alan; Uplegger, Lorenzo; Zagel, Jim; Zvodaya, Viktoriya; /Fermilab

    2011-09-14

    An enhancement to the T-980 bent crystal collimation experiment at the Tevatron has been completed. The enhancement was the installation of a pixel telescope inside the vacuum-sealed beam pipe of the Tevatron. The telescope is comprised of six CMS PSI46 pixel plaquettes, arranged as three stations of horizontal and vertical planes, with the CAPTAN system for data acquisition and control. The purpose of the pixel telescope is to measure beam profiles produced by bent crystals under various conditions. The telescope electronics inside the beam pipe initially were not adequately shielded from the image current of the passing beams. A new shielding approach was devised and installed, which resolved the problem. The noise issues encountered and the mitigating techniques are presented herein, as well as some preliminary results from the telescope.

  17. The MAGIC Telescope Project for Gamma Astronomy above 10 GeV

    E-Print Network [OSTI]

    N. Magnussen

    1998-05-14

    A project to construct a 17 m diameter imaging air Cherenkov telescope, called the MAGIC Telescope, is described. The aim of the project is to close the observation gap in the gamma-ray sky extending from 10 GeV as the highest energy measurable by space-borne experiments to 300 GeV, the lowest energy measurable by the current generation of ground-based Cherenkov telescopes. The MAGIC Telescope will incorporate several new features in order to reach the very low energy threshold. At the same time the new technology will yield an improvement in sensitivity in the energy region where current Cherenkov telescopes are measuring by about an order of magnitude.

  18. Receive Transmit Telescope Telescope

    E-Print Network [OSTI]

    technologies for the Bifocal Relay Mirror Spacecraft and verify these technologies with the experimental test for Bifocal Relay Mirror Spacecraft Jae Jun Kim* , Tim Sands , and Brij N. Agrawal Naval Postgraduate School Relay Mirror Spacecraft. In this paper, development of the Bifocal Relay Mirror Spacecraft experimental

  19. Investigation of Umbral Dots with the New Vacuum Solar Telescope

    E-Print Network [OSTI]

    Kaifan, Ji; Song, Feng; Yunfei, Yang; Hui, Deng; Feng, Wang

    2015-01-01

    Umbral dots (UDs) are small isolated brightening observed in sunspot umbrae. They are convective phenomena existing inside umbrae. UDs are usually divided into central UDs (CUDs) and peripheral UDs (PUDs) with respect to their positions inside an umbra. Our purpose is to investigate UD properties and analyze their relationships, and further to find whether or not the properties depend on the umbral magnetic field variation. For the purpose, we selected the high-resolution TiO images of four active regions (ARs) obtained under the best seeing conditions with the \\emph{New Vacuum Solar Telescope} (NVST) in Fuxian Solar Observatory of Yunnan Astronomical Observatory, China. The four ARs (NOAA 11598, 11801, 12158, and 12178) include six sunspots. A total of 1220 CUDs were extracted from six sunspots, and 603 PUDs from three sunspots. Meanwhile, the radial component of the magnetic field of the sunspots obtained with the \\emph{Helioseismic and Magnetic Imager} onboard the \\emph{Solar Dynamics Observatory} was used...

  20. THE INFRARED TELESCOPE FACILITY (IRTF) SPECTRAL LIBRARY: COOL STARS

    SciTech Connect (OSTI)

    Rayner, John T.; Cushing, Michael C.; Vacca, William D. E-mail: michael.cushing@gmail.com

    2009-12-01

    We present a 0.8-5 {mu}m spectral library of 210 cool stars observed at a resolving power of R {identical_to} {lambda}/{delta}{lambda} {approx} 2000 with the medium-resolution infrared spectrograph, SpeX, at the 3.0 m NASA Infrared Telescope Facility (IRTF) on Mauna Kea, Hawaii. The stars have well-established MK spectral classifications and are mostly restricted to near-solar metallicities. The sample not only contains the F, G, K, and M spectral types with luminosity classes between I and V, but also includes some AGB, carbon, and S stars. In contrast to some other spectral libraries, the continuum shape of the spectra is measured and preserved in the data reduction process. The spectra are absolutely flux calibrated using the Two Micron All Sky Survey photometry. Potential uses of the library include studying the physics of cool stars, classifying and studying embedded young clusters and optically obscured regions of the Galaxy, evolutionary population synthesis to study unresolved stellar populations in optically obscured regions of galaxies and synthetic photometry. The library is available in digital form from the IRTF Web site.

  1. Fast minimum variance wavefront reconstruction for extremely large telescopes

    E-Print Network [OSTI]

    Eric Thiebaut; Michel Tallon

    2010-03-01

    We present a new algorithm, FRiM (FRactal Iterative Method), aiming at the reconstruction of the optical wavefront from measurements provided by a wavefront sensor. As our application is adaptive optics on extremely large telescopes, our algorithm was designed with speed and best quality in mind. The latter is achieved thanks to a regularization which enforces prior statistics. To solve the regularized problem, we use the conjugate gradient method which takes advantage of the sparsity of the wavefront sensor model matrix and avoids the storage and inversion of a huge matrix. The prior covariance matrix is however non-sparse and we derive a fractal approximation to the Karhunen-Loeve basis thanks to which the regularization by Kolmogorov statistics can be computed in O(N) operations, N being the number of phase samples to estimate. Finally, we propose an effective preconditioning which also scales as O(N) and yields the solution in 5-10 conjugate gradient iterations for any N. The resulting algorithm is therefore O(N). As an example, for a 128 x 128 Shack-Hartmann wavefront sensor, FRiM appears to be more than 100 times faster than the classical vector-matrix multiplication method.

  2. Testing and Performance of UFFO Burst Alert & Trigger Telescope

    E-Print Network [OSTI]

    Ripa, J; Lee, J; Park, I H; Kim, J E; Lim, H; Jeong, S; Castro-Tirado, A J; Connell, P H; Eyles, C; Reglero, V; Rodrigo, J M; Bogomolov, V; Panasyuk, M I; Petrov, V; Svertilov, S; Yashin, I; Brandt, S; Budtz-Jorgensen, C; Chang, Y -Y; Chen, P; Huang, M A; Liu, T -C; Nam, J W; Wang, M -Z; Chen, C R; Choi, H S; Kim, S -W; Min, K W

    2015-01-01

    The Ultra-Fast Flash Observatory pathfinder (UFFO-p) is a new space mission dedicated to detect Gamma-Ray Bursts (GRBs) and rapidly follow their afterglows in order to provide early optical/ultraviolet measurements. A GRB location is determined in a few seconds by the UFFO Burst Alert & Trigger telescope (UBAT) employing the coded mask imaging technique and the detector combination of Yttrium Oxyorthosilicate (YSO) scintillating crystals and multi-anode photomultiplier tubes. The results of the laboratory tests of UBAT's functionality and performance are described in this article. The detector setting, the pixel-to-pixel response to X-rays of different energies, the imaging capability for rays, the localization accuracy measurements, and the combined test with the Block for X-ray and Gamma-Radiation Detection (BDRG) scintillator detector to check the efficiency of UBAT are all described. The UBAT instrument has been assembled and integrated with other equipment on UFFO-p and should be launche...

  3. Hubble Space Telescope Observations of Novae in M49

    E-Print Network [OSTI]

    Laura Ferrarese; Patrick Cote; Andres Jordan

    2003-09-30

    A search for novae in M49 (NGC 4472) has been undertaken with the Hubble Space Telescope. A 55-day observing campaign in F555W (19 epochs) and F814W (five epochs) has led to the discovery of nine novae. We find that M49 may be under-abundant in slow, faint novae relative to the Milky Way and M31. Instead, the decline rates of the M49 novae are remarkably similar to those of novae in the LMC. This fact argues against a simple classification of novae in "bulge" and "disk" sub-classes. We examine the Maximum-Magnitude versus Rate of Decline (MMRD) relation for novae in M49, finding only marginal agreement with the Galactic and M31 MMRD relations. A recalibration of the Buscombe-de Vaucouleurs relation gives an absolute magnitude 15 days past maximum of M_{V,15} = -6.36+/-0.19, which is substantially brighter than previous calibrations based on Galactic novae. Monte Carlo simulations yield a global nova rate for M49 of 100{+35}{-30} per year, and a luminosity-specific nova rate in the range \

  4. Construction of a medium-sized Schwarzschild-Couder telescope as a candidate for the Cherenkov Telescope Array: development of the optical alignment system

    E-Print Network [OSTI]

    Nieto, D; Humensky, B; Kaaret, P; Limon, M; Mognet, I; Peck, A; Petrashyk, A; Ribeiro, D; Rousselle, J; Stevenson, B; Vassiliev, V; Yu, P

    2015-01-01

    The Cherenkov Telescope Array (CTA) is an international project for a next-generation ground-based gamma-ray observatory. CTA, conceived as an array of tens of imaging atmospheric Cherenkov telescopes, comprising small, medium and large-size telescopes, is aiming to improve on the sensitivity of current-generation experiments by an order of magnitude and provide energy coverage from 20 GeV to more than 300 TeV. The Schwarzschild-Couder (SC) medium-size candidate telescope model features a novel aplanatic two-mirror optical design capable of a wide field-of-view with significantly improved imaging resolution as compared to the traditional Davis-Cotton optics design. Achieving this imaging resolution imposes strict alignment requirements to be accomplished by a dedicated alignment system. In this contribution we present the status of the development of the SC optical alignment system, soon to be materialized in a full-scale prototype SC medium-size telescope at the Fred Lawrence Whipple Observatory in southern ...

  5. A Small Multi-Wire Telescope for High Energy Cosmic Ray Muon Detection

    E-Print Network [OSTI]

    Maghrabi, Abdullrahnan; Aldosari, A; Almuteri, M

    2016-01-01

    Different types of ground-based detectors have been developed and deployed around the world to monitor and study CR variations. We have designed, constructed and operated a three layer small (20x20 cm2) multiwire proportional chamber MWPC telescope for cosmic ray muon observations. In this paper, the technical aspects of this detector will be briefly discussed. The abilities of the telescope in detecting high nergy cosmic ray muons (primaries higher than 20 GeV) were established. The telescope performs well in this sense and showed comparable results with a 1 m2 scintillator detector.

  6. KM3NeT: A Next Generation Neutrino Telescope in the Mediterranean Sea

    E-Print Network [OSTI]

    A. Kappes; for the KM3NeT Consortium

    2007-11-05

    To complement the IceCube neutrino telescope currently under construction at the South Pole, the three Mediterranean neutrino telescope projects ANTARES, NEMO and NESTOR have joined forces to develop, construct and operate a km^3-scale neutrino telescope in the Mediterranean Sea. Since February 2006, the technical specifications and performance of such a detector are studied in the framework of a 3-year EU-funded Design Study. In 2009 a technical design report will be released laying the foundations for the construction of the detector. In the following, the current status of the Design Study is presented and examples of solutions for the technical challenges are discussed.

  7. Distance determinations to shield galaxies from Hubble space telescope imaging

    SciTech Connect (OSTI)

    McQuinn, Kristen B. W.; Skillman, Evan D. [Minnesota Institute for Astrophysics, School of Physics and Astronomy, University of Minnesota, 116 Church Street, S.E., Minneapolis, MN 55455 (United States); Cannon, John M.; Cave, Ian [Department of Physics and Astronomy, Macalester College, 1600 Grand Avenue, Saint Paul, MN 55105 (United States); Dolphin, Andrew E. [Raytheon Company, 1151 E. Hermans Road, Tucson, AZ 85756 (United States); Salzer, John J. [Department of Astronomy, Indiana University, 727 East 3rd Street, Bloomington, IN 47405 (United States); Haynes, Martha P.; Adams, Elizabeth; Giovanelli, Riccardo [Center for Radiophysics and Space Research, Space Sciences Building, Cornell University, Ithaca, NY 14853 (United States); Elson, Ed C. [Astrophysics, Cosmology and Gravity Centre (ACGC), Department of Astronomy, University of Cape Town, Private Bag X3, Rondebosch 7701 (South Africa); Ott, Juërgen [National Radio Astronomy Observatory, P.O. Box O, 1003 Lopezville Road, Socorro, NM 87801 (United States); Saintonge, Amélie, E-mail: kmcquinn@astro.umn.edu [Max-Planck-Institute for Astrophysics, D-85741 Garching (Germany)

    2014-04-10

    The Survey of H I in Extremely Low-mass Dwarf (SHIELD) galaxies is an ongoing multi-wavelength program to characterize the gas, star formation, and evolution in gas-rich, very low-mass galaxies. The galaxies were selected from the first ?10% of the H I Arecibo Legacy Fast ALFA (ALFALFA) survey based on their inferred low H I mass and low baryonic mass, and all systems have recent star formation. Thus, the SHIELD sample probes the faint end of the galaxy luminosity function for star-forming galaxies. Here, we measure the distances to the 12 SHIELD galaxies to be between 5 and 12 Mpc by applying the tip of the red giant method to the resolved stellar populations imaged by the Hubble Space Telescope. Based on these distances, the H I masses in the sample range from 4 × 10{sup 6} to 6 × 10{sup 7} M {sub ?}, with a median H I mass of 1 × 10{sup 7} M {sub ?}. The tip of the red giant branch distances are up to 73% farther than flow-model estimates in the ALFALFA catalog. Because of the relatively large uncertainties of flow-model distances, we are biased toward selecting galaxies from the ALFALFA catalog where the flow model underestimates the true distances. The measured distances allow for an assessment of the native environments around the sample members. Five of the galaxies are part of the NGC 672 and NGC 784 groups, which together constitute a single structure. One galaxy is part of a larger linear ensemble of nine systems that stretches 1.6 Mpc from end to end. Three galaxies reside in regions with 1-9 neighbors, and four galaxies are truly isolated with no known system identified within a radius of 1 Mpc.

  8. Green Bank Telescope Studies of Giant Pulses from Millisecond Pulsars

    E-Print Network [OSTI]

    H. S. Knight; M. Bailes; R. N. Manchester; S. M. Ord; B. A. Jacoby

    2005-12-13

    We have conducted a search for giant pulses from four millisecond pulsars using the 100m Green Bank Telescope. Coherently dedispersed time-series from PSR J0218+4232 were found to contain giant pulses of very short intrinsic duration whose energies follow power-law statistics. The giant pulses are in phase with the two minima of the radio integrated pulse profile but are phase aligned with the peaks of the X-ray profile. Historically, individual pulses more than 10-20 times the mean pulse energy have been deemed to be ``giant pulses''. As only 4 of the 155 pulses had energies greater than 10 times the mean pulse-energy, we argue the emission mechanism responsible for giant pulses should instead be defined through: (a) intrinsic timescales of microsecond or nanosecond duration; (b) power-law energy statistics; and (c) emission occurring in narrow phase-windows coincident with the phase windows of non-thermal X-ray emission. Four short-duration pulses with giant-pulse characteristics were also observed from PSR B1957+20. As the inferred magnetic fields at the light cylinders of the millisecond pulsars that emit giant pulses are all very high, this parameter has previously been considered to be an indicator of giant pulse emissivity. However, the frequency of giant pulse emission from PSR~B1957+20 is significantly lower than for other millisecond pulsars that have similar magnetic fields at their light cylinders. This suggests that the inferred magnetic field at the light cylinder is a poor indicator of the rate of emission of giant pulses.

  9. Large Synoptic Survey Telescope: Dark Energy Science Collaboration

    E-Print Network [OSTI]

    LSST Dark Energy Science Collaboration

    2012-11-01

    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.

  10. Fermi Gamma-Ray Space Telescope: High-Energy Results From the...

    Office of Scientific and Technical Information (OSTI)

    Gamma-Ray Space Telescope: High-Energy Results From the First Year Michelson, P.F.; KIPAC, Menlo Park; Atwood, W.B.; Ritz, S.; UC, Santa Cruz UC, Santa Cruz, Phys. Dept....

  11. Minimizing actuator-induced residual error in active space telescope primary mirrors

    E-Print Network [OSTI]

    Smith, Matthew William, Ph. D. Massachusetts Institute of Technology

    2010-01-01

    Heritage space telescope mirror technology-i.e. large, monolithic glass primary mirrors-has reached an upper limit on allowable aperture diameter given launch vehicle volume and mass constraints. The next generation of ...

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

    E-Print Network [OSTI]

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

    2013-01-01

    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...

  13. A Continuous Homologation of Esters: An Efficient Telescoped Reduction–Olefination Sequence

    E-Print Network [OSTI]

    Webb, Damien

    A continuous protocol for the two-carbon homologation of esters to ?,?-unsaturated esters is described. This multireactor homologation telescopes an ester reduction, phosphonate deprotonation, and Horner–Wadsworth–Emmons ...

  14. Thin optic surface analysis for high resolution X-ray telescopes

    E-Print Network [OSTI]

    Akilian, Mireille

    2004-01-01

    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 ...

  15. ISIS polarimetry for ING support astronomers Isaac Newton Group of Telescopes

    E-Print Network [OSTI]

    ISIS polarimetry for ING support astronomers Isaac Newton Group of Telescopes Pablo Rodr 0.1 Document history . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 1 1 ISIS . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 4 1.2 Setting up ISIS for spectropolarimetry . . . . . . . . . . . . . . . . . . . . . 4 1

  16. Hubble Space Telescope Cycle 5 General Observer Pro* Imaging of Two Dwarf Galaxies in Tidal Tails

    E-Print Network [OSTI]

    Hibbard, John

    Hubble Space Telescope Cycle 5 General Observer Pro* *posal Woodlawn Drive Honolulu, HI 96822 Telephone: 808:Galaxies & Clusters Instruments: WFPC2 Cycle 5 primary orbits:11 Cycle 5 parallel orbits:0 Abstract

  17. New strategies for an extremely large telescope dedicated to extremely high contrast: The Colossus Project**

    E-Print Network [OSTI]

    Berdyugina, Svetlana

    New strategies for an extremely large telescope dedicated to extremely high contrast: The Colossus and adaptive optics and cophasing for the designing and for building such dedicated to extremely high contrast

  18. The optical reflector system for the CANGAROO-II imaging atmospheric Cherenkov telescope

    E-Print Network [OSTI]

    A. Kawachi; Y. Hayami; J. Jimbo; S. Kamei; T. Kifune; H. Kubo; J. Kushida; S. LeBohec; K. Miyawaki; M. Mori; K. Nishijima; J. R. Patterson; R. Suzuki; T. Tanimori; S. Yanagita; T. Yoshikoshi; A. Yuki

    2000-07-14

    A new imaging atmospheric Cherenkov telescope (CANGAROO-II) with a light-weight reflector has been constructed. Light, robust, and durable mirror facets of containing CFRP (Carbon Fiber Reinforced Plastic) laminates were developed for the telescope. The attitude of each facet can be adjusted by stepping motors. In this paper, we describe the design, manufacturing, alignment procedure, and the performance of the CANGAROO-II optical reflector system.

  19. The optical reflector system for the CANGAROO-II imaging atmospheric Cherenkov telescope

    E-Print Network [OSTI]

    Kawachi, A; Jimbo, J; Kamei, S; Kifune, T; Kubo, H; Kushida, J; Le Bohec, S; Miyawaki, K; Mori, M; Nishijima, K; Patterson, J R; Suzuki, R; Tanimori, T; Yanagita, S; Yoshikoshi, T; Yuki, A

    2001-01-01

    A new imaging atmospheric Cherenkov telescope (CANGAROO-II) with a light-weight reflector has been constructed. Light, robust, and durable mirror facets of containing CFRP (Carbon Fiber Reinforced Plastic) laminates were developed for the telescope. The attitude of each facet can be adjusted by stepping motors. In this paper, we describe the design, manufacturing, alignment procedure, and the performance of the CANGAROO-II optical reflector system.

  20. CCD drift-scan imaging lunar occultations: a feasible approach for sub-meter class telescopes

    E-Print Network [OSTI]

    O. Fors; J. Nunez; A. Richichi

    2001-08-27

    A CCD drift-scanning technique for lunar occultation (LO) observations is presented. While this approach has been addressed before by Sturmann (1994) for the case of large telescopes, the technical validity has never been discussed for sub-meter class telescopes. In contrast to Sturmann's scheme, the proposed technique places the CCD in the image plane of the telescope. This does not represent a problem in the case of small telescopes, where the practical angular resolution attainable by LO is not limited by aperture smoothing. Photon-generated charge is read out at millisecond rate on a column-per-column basis, as the diffraction pattern of the occulted star is being tracked. Two LO events (SAO 79031 and SAO 77911) were observed to demonstrate the feasibility of the method. Data analysis was carried out and no angular diameter the observed stars were resolved. We show, however, that the technique could be useful for close binary detections with small telescopes. A discussion of the limiting resolution and magnitude imposed by our instrumentation is carried out, showing that drift-scanning technique could be extended to 1-2m telescopes for stellar diameter determination purposes. Finally, we point out that the technical demands required by this technique can be easily met by most small professional observatories and advanced amateurs.

  1. Liverpool Telescope 2: a new robotic facility for rapid transient follow-up

    E-Print Network [OSTI]

    Copperwheat, C M; Barnsley, R M; Bates, S D; Bersier, D; Bode, M F; Carter, D; Clay, N R; Collins, C A; Darnley, M J; Davis, C J; Gutierrez, C M; Harman, D J; James, P A; Knapen, J; Kobayashi, S; Marchant, J M; Mazzali, P A; Mottram, C J; Mundell, C G; Newsam, A; Oscoz, A; Palle, E; Piascik, A; Rebolo, R; Smith, R J

    2014-01-01

    The Liverpool Telescope is one of the world's premier facilities for time domain astronomy. The time domain landscape is set to radically change in the coming decade, with synoptic all-sky surveys such as LSST providing huge numbers of transient detections on a nightly basis; transient detections across the electromagnetic spectrum from other major facilities such as SVOM, SKA and CTA; and the era of `multi-messenger astronomy', wherein astrophysical events are detected via non-electromagnetic means, such as neutrino or gravitational wave emission. We describe here our plans for the Liverpool Telescope 2: a new robotic telescope designed to capitalise on this new era of time domain astronomy. LT2 will be a 4-metre class facility co-located with the Liverpool Telescope at the Observatorio del Roque de Los Muchachos on the Canary island of La Palma. The telescope will be designed for extremely rapid response: the aim is that the telescope will take data within 30 seconds of the receipt of a trigger from another...

  2. Response of rice to ammonium and nitrate nitrogen applied at various stages of plant growth on limed and unlimed Beaumont and Lake Charles clays 

    E-Print Network [OSTI]

    Gay, William Blalock, III

    1962-01-01

    and Patna1k (1 ) partially support th1s explanation. They found that lime at ths rate of one percent of the weight of the so11 increased mineralisat1on of nitrogen, but most of the n1trogen in their tests accumulated as ammonia rather than nitrate under...RESPONSE OF RICE TO AMMONIUM AND NITRATE NITROGEN APPLIED AT VARIOUS STAGES OF PLANT GROWTH ON LIMED AND UNLINED BEAUNONT AND LAKE CHARLES CLAYS A Thesis By William B. Gay, III Submitted to the Graduate Sohool of the Agricultural...

  3. The Jay Baum Rich telescope: a Centurion 28 at the Wise Observatory

    E-Print Network [OSTI]

    Brosch, Noah; Niv, Saar; Manulis, Ilan

    2015-01-01

    We describe the third telescope of the Wise Observatory, a 0.70-m Centurion 28 (C28IL) installed in 2013 and named the Jay Baum Rich telescope to enhance significantly the wide-field imaging possibilities of the observatory. The telescope operates from a 5.5-m diameter dome and is equipped with a large-format red-sensitive CCD camera, offering a ~one square degree imaged field sampled at 0".83/pixel. The telescope was acquired to provide an alternative to the existing 1-m telescope for studies such as microlensing, photometry of transiting exo-planets, the follow-up of supernovae and other optical transients, and the detection of very low surface brightness extended features around galaxies. The operation of the C28IL is robotic, requiring only the creation of a night observing plan that is loaded in the afternoon prior to the observations. The entire facility was erected for a component and infrastructure cost of well under 300k$ and a labor investment of about two person-year. The successful implementation ...

  4. In-orbit focal adjustment of the AKARI telescope with IRC images

    E-Print Network [OSTI]

    H. Kaneda; W. Kim; T. Onaka; T. Wada; Y. Ita; I. Sakon; T. Takagi

    2007-06-01

    AKARI currently in space carries onboard a cryogenically-cooled lightweight telescope with silicon carbide mirrors. The wavefront error of the AKARI telescope obtained in laboratory measurements at 9 K showed that expected in-orbit imaging performance was diffraction-limited at a wavelength of 6.2 um. The AKARI telescope has a function of focus adjustment by shifting the secondary mirror in parallel to the optical axis. On the 4th day after the jettison of the cryostat aperture lid in the orbit, we observed a star with the InfraRed Camera (IRC) onboard AKARI. Since the initial star images observed in the near-infrared (IR) bands were significantly blurred, we twice moved the secondary mirror for the focal adjustment based on the results of model analyses as well as data analyses of the near-IR images. In consequence, we have successfully adjusted the focus of the telescope. The in-orbit imaging performance thus obtained for the AKARI telescope is diffraction-limited at a wavelength of 7.3 um, slightly degraded from that expected from the laboratory measurement.

  5. Merguerian, Charles; and Sanders, J. E., 1996a, Diversion of the Bronx River in New York City -evidence for postglacial surface faulting?, p. 131-145 in Hanson, G. N., chm., Geology

    E-Print Network [OSTI]

    Merguerian, Charles

    Merguerian, Charles; and Sanders, J. E., 1996a, Diversion of the Bronx River in New York City Program with Abstracts, 177 p. DIVERSION OF THE BRONX RIVER IN NEW YORK CITY - EVIDENCE FOR POSTGLACIAL valleys that we have obtained from the archives of the City of New York. We conclude that the new tectonic

  6. 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]

    Merguerian, Charles

    Sanders, J. E., and Merguerian, Charles, 1994b, The glacial geology of New York City and vicinity of the New York City region is: "Did one glacier do it all? or was more than one glacier involved?" Prior to SSW, down the Hudson Valley (the same direction as Flint's Hamden Till in CT). In the New York City

  7. Merguerian, Charles, 1994a, Stratigraphy, structural geology, and ductile-and brittle faults of the New York City area, p. 49-56 in Hanson, G. N., chm., Geology of Long Island

    E-Print Network [OSTI]

    Merguerian, Charles

    Merguerian, Charles, 1994a, Stratigraphy, structural geology, and ductile- and brittle faults with Abstracts, 165 p. STRATIGRAPHY, STRUCTURAL GEOLOGY, AND DUCTILE- AND BRITTLE FAULTS OF THE NEW YORK CITY of the stratigraphy and structure of the region and has delineated a number of ductile- and brittle faults. The belt

  8. THE DEEP BLUE COLOR OF HD 189733b: ALBEDO MEASUREMENTS WITH HUBBLE SPACE TELESCOPE/SPACE TELESCOPE IMAGING SPECTROGRAPH AT VISIBLE WAVELENGTHS

    SciTech Connect (OSTI)

    Evans, Thomas M.; Aigrain, Suzanne; Barstow, Joanna K.; Pont, Frederic; Sing, David K.; Desert, Jean-Michel; Knutson, Heather A.; Gibson, Neale; Heng, Kevin; Lecavelier des Etangs, Alain

    2013-08-01

    We present a secondary eclipse observation for the hot Jupiter HD 189733b across the wavelength range 290-570 nm made using the Space Telescope Imaging Spectrograph on the Hubble Space Telescope. We measure geometric albedos of A{sub g} = 0.40 {+-} 0.12 across 290-450 nm and A{sub g} < 0.12 across 450-570 nm at 1{sigma} confidence. The albedo decrease toward longer wavelengths is also apparent when using six wavelength bins over the same wavelength range. This can be interpreted as evidence for optically thick reflective clouds on the dayside hemisphere with sodium absorption suppressing the scattered light signal beyond {approx}450 nm. Our best-fit albedo values imply that HD 189733b would appear a deep blue color at visible wavelengths.

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

    E-Print Network [OSTI]

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

    2005-11-30

    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.

  10. A Review of Early-Time Optical Follow-ups with 2-m Robotic Telescopes

    E-Print Network [OSTI]

    A. Gomboc; C. Guidorzi; C. G. Mundell; A. Melandri; A. Monfardini; D. Bersier; M. F. Bode; D. Carter; S. Kobayashi; C. J. Mottram; R. J. Smith; I. A. Steele

    2006-12-28

    We summarise recent deep, rapid GRB follow-up observations using the RoboNet-1.0 network which comprises three fully-robotic 2-m telescopes, the Liverpool Telescope and the Faulkes Telescopes North and South. Observations begin automatically within minutes of receipt of a GRB alert and may continue for hours or days to provide well-sampled multi-colour light curves or deep upper limits. Our light curves show a variety of early afterglow behaviour, from smooth, simple or broken power laws to 'bumpy', for a wide range of optical brightness (from the unprecedented faint detections of GRB 060108 and GRB 060510B to classical bright ones). We discuss GRB 051111 as an example of how the combination of optical and X-ray light curves can provide insight into the circumburst environment, in particular the role played by intrinsic extinction soon after the burst.

  11. pt5m - a 0.5m robotic telescope on La Palma

    E-Print Network [OSTI]

    Hardy, L K; Dhillon, V S; Littlefair, S P; Wilson, R W

    2015-01-01

    pt5m is a 0.5m robotic telescope located on the roof of the 4.2m William Herschel Telescope (WHT) building, at the Roque de los Muchachos Observatory, La Palma. Using a 5-position filter wheel and CCD detector, and bespoke control software, pt5m provides a high quality robotic observing facility. The telescope first began robotic observing in 2012, and is now contributing to transient follow-up and time-resolved astronomical studies. In this paper we present the scientific motivation behind pt5m, as well as the specifications and unique features of the facility. We also present an example of the science we have performed with pt5m, where we measure the radius of the transiting exoplanet WASP-33b. We find a planetary radius of 1.603 +/- 0.014 R(J).

  12. The High-Resolution Lightweight Telescope for the EUV (HiLiTE)

    SciTech Connect (OSTI)

    Martinez-Galarce, D S; Boerner, P; Soufli, R; De Pontieu, B; Katz, N; Title, A; Gullikson, E M; Robinson, J C; Baker, S L

    2008-06-02

    The High-resolution Lightweight Telescope for the EUV (HiLiTE) is a Cassegrain telescope that will be made entirely of Silicon Carbide (SiC), optical substrates and metering structure alike. Using multilayer coatings, this instrument will be tuned to operate at the 465 {angstrom} Ne VII emission line, formed in solar transition region plasma at {approx}500,000 K. HiLiTE will have an aperture of 30 cm, angular resolution of {approx}0.2 arc seconds and operate at a cadence of {approx}5 seconds or less, having a mass that is about 1/4 that of one of the 20 cm aperture telescopes on the Atmospheric Imaging Assembly (AIA) instrument aboard NASA's Solar Dynamics Observatory (SDO). This new instrument technology thus serves as a path finder to a post-AIA, Explorer-class missions.

  13. Platform Deformation Refined Pointing and Phase Correction for the AMiBA Hexapod Telescope

    E-Print Network [OSTI]

    Koch, Patrick M; Chang, Yu-Yen; Huang, Yau-De; Raffin, Philippe; Chen, Ke-Yung; Chereau, Guillaume; Chen, Ming-Tang; Ho, Paul T P; Huang, Chih-Wie; Ibanez-Romano, Fabiola; Jiang, Homin; Liao, Yu-Wei; Lin, Kai-Yang; Liu, Guo-Chin; Molnar, Sandor M; Nishioka, Hiroaki; Umetsu, Keiichi; Wang, Fu-Cheng; Wu, Jiun-Huei Proty; Altamirano, Pablo; Chang, Chia-Hao; Chang, Shu-Hao; Chang, Su-Wei; Han, Chi-Chiang; Kubo, Derek; Li, Chao-Te; Martin-Cocher, Pierre; Oshiro, Peter

    2009-01-01

    The Array for Microwave Background Anisotropy (AMiBA) is a radio interferometer for research in cosmology, currently operating 7 0.6m diameter antennas co-mounted on a 6m diameter platform driven by a hexapod mount. AMiBA is currently the largest hexapod telescope. We briefly summarize the hexapod operation with the current pointing error model. We then focus on the upcoming 13-element expansion with its potential difficulties and solutions. Photogrammetry measurements of the platform reveal deformations at a level which can affect the optical pointing and the receiver radio phase. In order to prepare for the 13-element upgrade, two optical telescopes are installed on the platform to correlate optical pointing tests. Being mounted on different locations, the residuals of the two sets of pointing errors show a characteristic phase and amplitude difference as a function of the platform deformation pattern. These results depend on the telescope's azimuth, elevation and polarization position. An analytical model ...

  14. Small Solutions to the Large Telescope Problem: A Massively Replicated MEMS Spectrograph

    E-Print Network [OSTI]

    Nicholas Konidaris; Joel Kubby; Andrew Sheinis

    2008-07-15

    In traditional seeing-limited observations the spectrograph aperture scales with telescope aperture, driving sizes and costs to enormous proportions. We propose a new solution to the seeing-limited spectrograph problem. A massively fiber-sliced configuration feeds a set of small diffraction-limited spectrographs. We present a prototype, tunable, J-band, diffraction grating, designed specifically for Astronomical applications: The grating sits at the heart of a spectrograph, no bigger than a few inches on a side. Throughput requirements dictate using tens-of-thousands of spectrographs on a single 10 to 30 meter telescope. A full system would cost significantly less than typical instruments on 10m or 30m telescopes.

  15. Metrology for x-ray telescope mirrors in a vertical configuration

    SciTech Connect (OSTI)

    Li, Haizhang; Li, Xiaodan; Grindel, M.W.

    1995-09-01

    Mirrors used in x-ray telescope systems for observations outside of the earth`s atmosphere are usually made of several thin nested shells, each formed by a pair of paraboloidal and hyperboloidal surfaces. The thin shells are very susceptible to self-weight deflection caused by gravity and are nearly impossible to test by conventional interferometric techniques. The metrology requirements for these mirrors are extremely challenging. This paper presents a prototype of a Vertical Scanning Long Trace Profiler (VSLTP) which is optimized to measure the surface figure of x-ray telescope mirrors in a vertical orientation. The optical system of the VSLTP is described. Experimental results from measurements on an x-ray telescope mandrel and tests of the accuracy and repeatability of the prototype VSLTP are presented. The prototype instrument has achieved a height measurement accuracy of about 50 nanometers with a repeatability of better than 20 nanometers, and a slope measurement accuracy of about 1 microradian.

  16. Development of Atmospheric Monitoring System at Akeno Observatory for the Telescope Array Project

    E-Print Network [OSTI]

    T. Yamamoto; M. Teshima; M. Chikawa; N. Hayashida; S. Kawakami; N. Minagawa; Y. Morizane; M. Sasano; K. Yasui

    2002-08-09

    We have developed an atmospheric monitoring system for the Telescope Array experiment at Akeno Observatory. It consists of a Nd:YAG laser with an alt-azimuth shooting system and a small light receiver. This system is installed inside an air conditioned weather-proof dome. All parts, including the dome, laser, shooter, receiver, and optical devices are fully controlled by a personal computer utilizing the Linux operating system. It is now operated as a back-scattering LIDAR System. For the Telescope Array experiment, to estimate energy reliably and to obtain the correct shower development profile, the light transmittance in the atmosphere needs to be calibrated with high accuracy. Based on observational results using this monitoring system, we consider this LIDAR to be a very powerful technique for Telescope Array experiments. The details of this system and its atmospheric monitoring technique will be discussed.

  17. Relay telescope including baffle, and high power laser amplifier utilizing the same

    DOE Patents [OSTI]

    Dane, C. Brent; Hackel, Lloyd; Harris, Fritz B.

    2006-09-19

    A laser system includes an optical path having an intracavity relay telescope with a telescope focal point for imaging an output of the gain medium between an image location at or near the gain medium and an image location at or near an output coupler for the laser system. A kinematic mount is provided within a vacuum chamber, and adapted to secure beam baffles near the telescope focal point. An access port on the vacuum chamber is adapted for allowing insertion and removal of the beam baffles. A first baffle formed using an alignment pinhole aperture is used during alignment of the laser system. A second tapered baffle replaces the alignment aperture during operation and acts as a far-field baffle in which off angle beams strike the baffle a grazing angle of incidence, reducing fluence levels at the impact areas.

  18. DC 12m telescope. Preliminary calculations. Investigation of elevation axis position.

    SciTech Connect (OSTI)

    Guarino, V. J.; High Energy Physics

    2009-12-18

    This paper examines some simple calculations of a 2D model of a telescope in order to understand how different design parameters affect the design. For the design of a telescope it is assumed that they need a design that minimizes deflections of the dish and also minimizes the size of the motors and torques needed to rotate in elevation. A common belief is that a lighter dish and minimum counterweight is desirable. However, these calculations show this is not necessarily true. The torque needed for rotation depends on the moment of inertia and if the telescope is balanced about the elevation axis. A light dish with no CW requires that the elevation axis be several meters in front of the dish (8-9m) in order to be balanced. This is not practical from a structural point of view. If the elevation axis is only 2m in front of the dish and there is no counterweight then the telescope will be unbalanced and the toruqes required will be very high - much higher than the torques needed only to overcome inertia. A heavy dish though can act as its own counterweight and the elevation axis only has to be 2-3m in front of the dish in order to achieve a balanced telescope. Also the struts that support the camera from the dish place a load on the dish which will put a bending moment on the dish. This bending moment will deform the dish and require it to be stiffer. A counterweight structure performs two functions. First, it allows the telescope to be balanced about the elevation axis. Second, it applies a force on the dish that opposes the forces from the camera struts, thereby reducing the bending moment and deformations of the dish.

  19. Cross-Calibrating Sunspot Magnetic Field Strength Measurements from the McMath-Pierce Solar Telescope and the Dunn Solar Telescope

    E-Print Network [OSTI]

    Watson, Fraser T; Penn, Matthew J; Tritschler, Alexandra; Pillet, Valentin Martinez; Livingston, William C

    2015-01-01

    In this article we describe a recent effort to cross-calibrate data from an infrared detector at the McMath-Pierce Solar Telescope and the Facility InfraRed Spectropolarimeter (FIRS) at the Dunn Solar Telescope. A synoptic observation program at the McMath-Pierce has measured umbral magnetic field strengths since 1998, and this data set has recently been compared with umbral magnetic field observations from SOHO MDI and SDO HMI. To further improve on the data from McMath-Pierce, we compared the data with measurements taken at the Dunn Solar Telescope with far greater spectral resolution than has been possible with space instrumentation. To minimise potential disruption to the study, concurrent umbral measurements were made so that the relationship between the two datasets can be most accurately characterised. We find that there is a strong agreement between the umbral magnetic field strengths recorded by each instrument, and we reduced the FIRS data in two different ways to successfully test this correlation ...

  20. Expected Performance of a Neutrino Telescope for Seeing AGN/GC Behind a Mountain

    E-Print Network [OSTI]

    George W. S. Hou; M. A. Huang

    2002-04-09

    We study the expected performance of building a neutrino telescope, which targets at energy greater than $10^{14}$ eV utilizing a mountain to interact with neutrinos. The telescope's efficiency in converting neutrinos into leptons is first examined. Then using a potential site on the Big Island of Hawaii, we estimate the acceptance of the proposed detector. The neutrino flux limit at event rate 0.3/year/half decade of energy is estimated to be comparable to that of AMANDA neutrino flux limit at above $10^{16}$ eV.

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

    SciTech Connect (OSTI)

    NONE

    2013-03-01

    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 TeV–PeV 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.

  2. Converters Charles N Johnson

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

    to predict the propagation of sound underwater solve variations of the Helmholtz wave equation. These models become self-limiting to the problems they can most effectively solve...

  3. Electronic Transmission and Computation of Very Long Baseline Interferometry and Its Application to Next Generation Radio Telescopes

    E-Print Network [OSTI]

    Melbourne, University of

    @atnf.csiro.au Abstract Australia is contributing to the next generation radio telescope, the Square Kilometre Array (SKA processors. 1. Introduction The Square Kilometre Array (SKA) is a next- generation radio telescope planned for operation around 2015. As the name implies, it will encompass a square kilometre of collecting area

  4. A Hubble Space Telescope Survey of X-ray Luminous Galaxy Clusters: Gravitationally Lensed Arcs and EROs

    E-Print Network [OSTI]

    Graham P. Smith

    2002-01-15

    We are conducting a systematic lensing survey of X-ray luminous galaxy clusters at z~0.2 using the Hubble Space Telescope and large ground-based telescopes. We summarize initial results from our survey, including a measurement of the inner slope of the mass profile of A383, and a search for gravitationally lensed Extremely Red Objects.

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

    E-Print Network [OSTI]

    Morselli, Aldo

    but there are competing astrophysical sources, such as pulsars, that can give a strong flux of primary positrons Gamma-ray Space Telescope, has detected the largest amount of gamma rays, in the 20MeV 300GeV energy and electrons (see [10], [11], [12], [13] and references therein). At energies between 100 GeV and 1 Te

  6. Facility class Rayleigh beacon AO system for the 4.2m William Herschel Telescope

    E-Print Network [OSTI]

    R. G. M. Rutten; P. Clark; R. M. Myers; R. W. Wilson; R. G. Bingham; E. Emsellem; T. Gregory; R. A. Humphreys; J. H. Knapen; G. Moretto; S. L. Morris; G. Talbot

    2002-08-07

    A rationale is presented for the use of a relatively low-altitude Rayleigh Laser Guide Star to provide partial adaptive optics correction across a large fraction of the sky on the 4.2m William Herschel Telescope. The scientific motivation is highlighted and supported by model calculations. An overview the technical implementation of the system is presented.

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

    E-Print Network [OSTI]

    T. D. Willis

    2002-01-30

    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.

  8. Liverpool Telescope Optical Photometry Following the 2006 Outburst of RS Ophiuchi

    E-Print Network [OSTI]

    M. J. Darnley; R. A. Hounsell; M. F. Bode

    2008-09-26

    We present a preliminary report on the broadband optical photometry of the 2006 outburst of the recurrent nova RS Ophiuchi. These data were obtained using the robotic 2m Liverpool Telescope and cover the outburst from day 27 through day 548.

  9. Imaging Performance of the XMM-Newton X-ray telescopes

    E-Print Network [OSTI]

    B. Aschenbach; U. Briel; F. Haberl; H. Braeuninger; W. Burkert; A. Oppitz; P. Gondoin; D. Lumb

    2000-07-18

    The in-orbit imaging performance of the three X-ray telescopes on board of the X-ray astronomy observatory XMM-Newton is presented and compared with the performance measured on ground at the MPE PANTER test facility. The comparison shows an excellent agreement between the on ground and in-orbit performance.

  10. ALLSTOKES PARAMETERIZATION OF THE MAIN BEAM AND FIRST SIDELOBE FOR THE ARECIBO RADIO TELESCOPE

    E-Print Network [OSTI]

    Heiles, Carl

    ALL­STOKES PARAMETERIZATION OF THE MAIN BEAM AND FIRST SIDELOBE FOR THE ARECIBO RADIO TELESCOPE and beamwidth. We describe a scheme that characterizes the main beam and sidelobe in all Stokes parameters to see how the beam changes with azimuth, zenith angle, and time. For the main beam in Stokes I

  11. What we need to return at the telescope New array at 1mm with better sensitvity

    E-Print Network [OSTI]

    Leclercq, Samuel

    What we need to return at the telescope New array at 1mm with better sensitvity Magnetic field pixels with 3 preamplifiers (1 at 2mm and 2 at 1mm) · 300 pixels at 2mm · 600 pixels at 1mm Automatic

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

    E-Print Network [OSTI]

    McEwen, Jason

    Synergy between the Large Synoptic Survey Telescope and the Square Kilometre Array David Bacon1 waveband, and the time resolution of the SKA. Advancing Astrophysics with the Square Kilometre Array June 8 provide an overview of the science benefits of combining information from the Square Kilo- metre Array

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

    E-Print Network [OSTI]

    California at Santa Cruz, University of

    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

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

    E-Print Network [OSTI]

    Martin, Chris

    The Cosmic Web Imager : An integral field spectrograph for the Hale Telescope at Palomar ABSTRACT We describe the Cosmic Web Imager (CWI), a UV-VIS integral field spectrograph designed Spectroscopy, VPH Gratings, Cosmic Web Imager 1. THE COSMIC WEB IMAGER INSTRUMENT 1.1. CWI Mission The Cosmic

  15. A High Speed Networked Signal Processing Platform for Multi-element Radio Telescopes

    E-Print Network [OSTI]

    Prasad, Peeyush; 10.1007/s10686-011-9216-7

    2011-01-01

    A new architecture is presented for a Networked Signal Processing System (NSPS) suitable for handling the real-time signal processing of multi-element radio telescopes. In this system, a multi-element radio telescope is viewed as an application of a multi-sensor, data fusion problem which can be decomposed into a general set of computing and network components for which a practical and scalable architecture is enabled by current technology. The need for such a system arose in the context of an ongoing program for reconfiguring the Ooty Radio Telescope (ORT) as a programmable 264-element array, which will enable several new observing capabilities for large scale surveys on this mature telescope. For this application, it is necessary to manage, route and combine large volumes of data whose real-time collation requires large I/O bandwidths to be sustained. Since these are general requirements of many multi-sensor fusion applications, we first describe the basic architecture of the NSPS in terms of a Fusion Tree ...

  16. THE WHITE MOUNTAIN POLARIMETER TELESCOPE AND AN UPPER LIMIT ON COSMIC MICROWAVE BACKGROUND POLARIZATION

    E-Print Network [OSTI]

    Timbie, Peter

    THE WHITE MOUNTAIN POLARIMETER TELESCOPE AND AN UPPER LIMIT ON COSMIC MICROWAVE BACKGROUND. Wuensche5 Received 2007 June 10; accepted 2008 March 16 ABSTRACT The White Mountain Polarimeter (WMPol microwave background. WMPol is located at an altitude of 3880 m on a plateau in the White Mountains

  17. Status and Plans for the Array Control and Data Acquisition System of the Cherenkov Telescope Array

    E-Print Network [OSTI]

    Oya, I; Schwanke, U; Wegner, P; Balzer, A; Berge, D; Borkowski, J; Camprecios, J; Colonges, S; Colome, J; Champion, C; Conforti, V; Gianotti, F; Flour, T Le; Lindemann, R; Lyard, E; Mayer, M; Melkumyan, D; Punch, M; Tanci, C; Schmidt, T; Schwarz, J; Tosti, G; Verma, K; Weinstein, A; Wiesand, S; Wischnewski, R

    2015-01-01

    The Cherenkov Telescope Array (CTA) is the next-generation atmospheric Cherenkov gamma-ray observatory. CTA will consist of two installations, one in the northern, and the other in the southern hemisphere, containing tens of telescopes of different sizes. The CTA performance requirements and the inherent complexity associated with the operation, control and monitoring of such a large distributed multi-telescope array leads to new challenges in the field of the gamma-ray astronomy. The ACTL (array control and data acquisition) system will consist of the hardware and software that is necessary to control and monitor the CTA arrays, as well as to time-stamp, read-out, filter and store -at aggregated rates of few GB/s- the scientific data. The ACTL system must be flexible enough to permit the simultaneous automatic operation of multiple sub-arrays of telescopes with a minimum personnel effort on site. One of the challenges of the system is to provide a reliable integration of the control of a large and heterogene...

  18. 30TH INTERNATIONAL COSMIC RAY CONFERENCE The Central Laser Facility at the Telescope Array

    E-Print Network [OSTI]

    -8582, Japan 2 Department of Physics, Univ. of Utah, 115 S 1400 E, Salt Lake City, UT 84112-0830, USA shige at the middle of three FD stations has a 355 nm wave- length laser as test beam for FD telescopes. It has is roughly equal to the fluorescence light generated by 1020 eV cosmic ray. Therefore the information about

  19. The Microchannel X-ray Telescope on Board the SVOM Satellite

    E-Print Network [OSTI]

    Gotz, D; Basa, S; Beckmann, V; Burwitz, V; Chipaux, R; Cordier, B; Evans, P; Godet, O; Goosmann, R; Meidinger, N; Meuris, A; Motch, C; Nandra, K; O'Brien, P; Osborne, J; Perinati, E; Rau, A; Willingale, R; Mercier, K; Gonzalez, F

    2015-01-01

    We present the Micro-channel X-ray Telescope (MXT), a new narrow-field (about 1{\\deg}) telescope that will be flying on the Sino-French SVOM mission dedicated to Gamma-Ray Burst science, scheduled for launch in 2021. MXT is based on square micro pore optics (MPOs), coupled with a low noise CCD. The optics are based on a "Lobster Eye" design, while the CCD is a focal plane detector similar to the type developed for the seven eROSITA telescopes. MXT is a compact and light (<35 kg) telescope with a 1 m focal length, and it will provide an effective area of about 45 cmsq on axis at 1 keV. The MXT PSF is expected to be better than 4.2 arc min (FWHM) ensuring a localization accuracy of the afterglows of the SVOM GRBs to better than 1 arc min (90\\% c.l. with no systematics) provided MXT data are collected within 5 minutes after the trigger. The MXT sensitivity will be adequate to detect the afterglows for almost all the SVOM GRBs as well as to perform observations of non-GRB astrophysical objects. These performan...

  20. Wind Loads on Ground-Based Telescopes Douglas G. MacMynowskia*

    E-Print Network [OSTI]

    MacMynowski, Douglas G. - MacMynowski, Douglas G.

    distribution of wind disturbances are defined as a function of relevant design parameters, providing Introduction Design studies are underway for the next generation of large ground-based optical telescopes still lead to significant vibration1,2 . Estimates of the wind loads are required early in the design

  1. Mees Observatory telescope and camera checklist Last revised 1 September 2011 DMW

    E-Print Network [OSTI]

    Mamajek, Eric E.

    in control room. Computers, left to right on the console: the (downstairs) user interface computer (UIC), telescope control system (TCS). Further right, on the lab table, is the CCD camera's laptop computer. TCS the bottom stair. 2. Plug in computer console in the control room (Figure 1). Figure 1: computer console

  2. WAVEFRONT RECONSTRUCTION METHODS FOR ADAPTIVE OPTICS SYSTEMS ON GROUND-BASED TELESCOPES

    E-Print Network [OSTI]

    Bardsley, John

    WAVEFRONT RECONSTRUCTION METHODS FOR ADAPTIVE OPTICS SYSTEMS ON GROUND-BASED TELESCOPES JOHNATHAN M that interfere with the propagation of light. As a result, wavefronts are non-planar when they reach the ground the refractive blurring of images. Adaptive optics systems seek to remove phase error from incoming wavefronts

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

    ScienceCinema (OSTI)

    Isabelle Grenier

    2010-01-08

    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.

  4. A facility to evaluate the focusing performance of mirrors for Cherenkov Telescopes

    E-Print Network [OSTI]

    Canestrari, Rodolfo; Bonnoli, Giacomo; Farisato, Giancarlo; Lessio, Luigi; Rodeghiero, Gabriele; Spiga, Rossella; Toso, Giorgio; Pareschi, Giovanni

    2015-01-01

    With the advent of the imaging atmospheric Cherenkov technique in late 1980's, ground-based observations of Very High-Energy gamma rays came into reality. Since the first source detected at TeV energies in 1989 by Whipple, the number of high energy gamma-ray sources has rapidly grown up to more than 150 thanks to the second generation experiments like MAGIC, H.E.S.S. and VERITAS. The Cherenkov Telescope Array observatory is the next generation of Imaging Atmospheric Cherenkov Telescopes, with at least 10 times higher sensitivity than current instruments. Cherenkov Telescopes have to be equipped with optical dishes of large diameter -- in general based on segmented mirrors -- with typical angular resolution of a few arc-minutes. To evaluate the mirror's quality specific metrological systems are required that possibly take into account the environmental conditions in which typically Cherenkov telescopes operate (in open air without dome protection). For this purpose a new facility for the characterization of mi...

  5. Solar Physics, Space Weather, and Wide-field X-ray Telescopes

    E-Print Network [OSTI]

    Van Stryland, Eric

    Solar Physics, Space Weather, and Wide-field X-ray Telescopes CREOL & FPCE: The College of Optics of the Earth). The detrimental effects of solar storm induced "space weather" ranges from disruption of our. The National Oceanic & Atmospheric Administration (NOAA) and NASA are cooperating on a Solar X-ray Imager (SXI

  6. Domain-Specific Type Inference for Library Generation in a Telescoping Compiler

    E-Print Network [OSTI]

    Chauhan, Arun

    Domain-Specific Type Inference for Library Generation in a Telescoping Compiler Cheryl McCosh Rice variants specialized to the different possible types of input parameters to the library routines. We showed that, if this is done, the library procedures automatically generated from MATLAB proto- type code had

  7. Type-Based Speculative Specialization in a Telescoping Compiler for Matlab

    E-Print Network [OSTI]

    Chauhan, Arun

    libraries from prototype Matlab code for the linear algebra library, ARPACK. ARGen uses variable types of generated libraries can lead to more than 50% speedup. ARGen needs to infer Matlab types in order of ARGen--a telescoping library gen- erator for ARPACK driven by type-based procedure spe- cialization

  8. (Astro)Physics 343 Spring 2010 Lab # 1: Measuring the Telescope Beamwidth with the Sun

    E-Print Network [OSTI]

    Gustafsson, Torgny

    (Astro)Physics 343 ­ Spring 2010 Lab # 1: Measuring the Telescope Beamwidth with the Sun) and geosyn- chronous satellites can be used to do this for the SRT, the best strategy is to use the Sun also already have written a command file to (1) point at the Sun (2) set the observing frequency

  9. New Hubble Space Telescope Observations of Heavy Elements in Four Metal-Poor Stars

    E-Print Network [OSTI]

    Roederer, Ian U; Sobeck, Jennifer S; Beers, Timothy C; Cowan, John J; Frebel, Anna; Ivans, Inese I; Schatz, Hendrik; Sneden, Christopher; Thompson, Ian B

    2012-01-01

    Elements heavier than the iron group are found in nearly all halo stars. A substantial number of these elements, key to understanding neutron-capture nucleosynthesis mechanisms, can only be detected in the near-ultraviolet. We report the results of an observing campaign using the Space Telescope Imaging Spectrograph on board the Hubble Space Telescope to study the detailed heavy element abundance patterns in four metal-poor stars. We derive abundances or upper limits from 27 absorption lines of 15 elements produced by neutron-capture reactions, including seven elements (germanium, cadmium, tellurium, lutetium, osmium, platinum, and gold) that can only be detected in the near-ultraviolet. We also examine 202 heavy element absorption lines in ground-based optical spectra obtained with the Magellan Inamori Kyocera Echelle Spectrograph on the Magellan-Clay Telescope at Las Campanas Observatory and the High Resolution Echelle Spectrometer on the Keck I Telescope on Mauna Kea. We have detected up to 34 elements hea...

  10. THE ARMAGH-DUNSINK-HARVARD TELESCOPE: FROM DREAM TO OBLIVION C. J. BUTLER

    E-Print Network [OSTI]

    and they made important contributions to the emerging disciplines of cosmology, solar physics and stellar recognised achievements was his part in the setting up of a large Schmidt telescope, the ADH, in South Africa, nebulosity's - gosh!" At last, the project could move forward, now with the newly reopened Dunsink

  11. Wide Field Hard X-ray Survey Telescope: ProtoEXIST1

    E-Print Network [OSTI]

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

    2007-09-17

    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 crystal units (DCUs) to a full detector module (DM). We have built the first units of each component for the detector plane and have completed a few Rev2 DCUs (2x2 cm2), which are under a series of tests. Bare DCUs (pre-crystal bonding) show high, uniform ASIC yield (~70%) and ~30% reduction in electronics noise compared to the Rev1 equivalent. A Rev1 DCU already achieved ~1.2% FWHM at 662 keV, and preliminary analysis of the initial radiation tests on a Rev2 DCU shows ~ 4 keV FWHM at 60 keV (vs. 4.7 keV for Rev1). We therefore expect about <~1% FWHM at 662 keV with the Rev2 detectors.

  12. Weak-Lensing Mass Calibration of the Atacama Cosmology Telescope Equatorial Sunyaev-Zeldovich Cluster Sample with the Canada-France-Hawaii Telescope Stripe 82 Survey

    E-Print Network [OSTI]

    Battaglia, N; Miyatake, H; Hasselfield, M; Gralla, M B; Allison, R; Bond, J R; Calabrese, E; Crichton, D; Devlin, M J; Dunkley, J; Dünner, R; Erben, T; Ferrara, S; Halpern, M; Hilton, M; Hill, J C; Hincks, A D; Hložek, R; Huffenberger, K M; Hughes, J P; Kneib, J P; Kosowsky, A; Makler, M; Marriage, T A; Menanteau, F; Miller, L; Moodley, K; Moraes, B; Niemack, M D; Page, L; Shan, H; Sehgal, N; Sherwin, B D; Sievers, J L; Sifón, C; Spergel, D N; Staggs, S T; Taylor, J; Thornton, R; van Waerbeke, L; Wollack, E J

    2015-01-01

    Mass calibration uncertainty is the largest systematic effect for using clusters of galaxies to constrain cosmological parameters. We present weak lensing mass measurements from the Canada-France-Hawaii Telescope Stripe 82 Survey for galaxy clusters selected through their high signal-to-noise thermal Sunyaev-Zeldovich (tSZ) signal measured with the Atacama Cosmology Telescope (ACT). The average weak lensing mass is $\\left(4.8\\pm0.8\\right)\\,\\times10^{14}\\,\\mathrm{M}_\\odot$, consistent with the tSZ mass estimate of $\\left(4.70\\pm1.0\\right)\\,\\times10^{14}\\,\\mathrm{M}_\\odot$ which assumes a universal pressure profile for the cluster gas. Our results are consistent with previous weak-lensing measurements of tSZ-detected clusters from the Planck satellite. When comparing our results, we estimate the Eddington bias correction for the sample intersection of Planck and weak-lensing clusters which was previously neglected.

  13. ULTRAVIOLET NUMBER COUNTS OF GALAXIES FROM SWIFT ULTRAVIOLET/OPTICAL TELESCOPE DEEP IMAGING OF THE CHANDRA DEEP FIELD SOUTH

    SciTech Connect (OSTI)

    Hoversten, E. A.; Gronwall, C.; Koch, T. S.; Roming, P. W. A.; Siegel, M. H.; Berk, D. E. Vanden; Breeveld, A. A.; Curran, P. A.; Still, M.

    2009-11-10

    Deep Swift UV/Optical Telescope (UVOT) imaging of the Chandra Deep Field South is used to measure galaxy number counts in three near-ultraviolet (NUV) filters (uvw2: 1928 A, uvm2: 2246 A, and uvw1: 2600 A) and the u band (3645 A). UVOT observations cover the break in the slope of the NUV number counts with greater precision than the number counts by the Hubble Space Telescope Space Telescope Imaging Spectrograph and the Galaxy Evolution Explorer, spanning a range 21 approx< m{sub AB} approx< 25. Model number counts confirm earlier investigations in favoring models with an evolving galaxy luminosity function.

  14. Ultraviolet number counts of galaxies from Swift UV/Optical Telescope deep imaging of the Chandra Deep Field South

    E-Print Network [OSTI]

    Hoversten, E A; Berk, D E Vanden; Koch, T S; Breeveld, A A; Curran, P A; Hinshaw, D A; Marshall, F E; Roming, P W A; Siegel, M H; Still, M

    2009-01-01

    Deep Swift UV/Optical Telescope (UVOT) imaging of the Chandra Deep Field South is used to measure galaxy number counts in three near ultraviolet (NUV) filters (uvw2: 1928 A, uvm2: 2246 A, uvw1: 2600 A) and the u band (3645 A). UVOT observations cover the break in the slope of the NUV number counts with greater precision than the number counts by the Hubble Space Telescope (HST) Space Telescope Imaging Spectrograph (STIS) and the Galaxy Evolution Explorer (GALEX), spanning a range from 21 < m_AB < 25. Number counts models confirm earlier investigations in favoring models with an evolving galaxy luminosity function.

  15. A multipurpose TIM-based optical telescope for Omega and the Trident laser facilities

    SciTech Connect (OSTI)

    Oertel, J.A.; Murphy, T.J.; Berggren, R.R.

    1998-12-31

    The authors have recently designed and are building a telescope which acts as an imaging light collector relaying the image to an optical table for experiment dependent analysis and recording. The expected primary use of this instrument is a streaked optical pyrometer for witness plate measurements of Hohlraum drive temperature. The telescope is based on University of Rochester`s Ten-Inch Manipulator (TIM) which allows compatibility between Omega, Trident, and the NIF lasers. The optics capture a f/7 cone of light, have a field of view of 6-mm, have a spatial resolution of 5 to 7-{micro}m per line pair at the object plane, and are optimized for operation at 280-nm. The image is at a magnification of 11.7x, which is convenient for many experiments, but can be changed using additional optics that reside outside the TIM.

  16. Multipurpose 10 in. manipulator-based optical telescope for Omega and the Trident laser facilities

    SciTech Connect (OSTI)

    Oertel, J.A.; Murphy, T.J.; Berggren, R.R.; Faulkner, J.; Schmell, R.; Little, D.; Archuleta, T.; Lopez, J.; Velarde, J.; Horton, R.F.

    1999-01-01

    We have recently designed and are building a telescope which acts as an imaging light collector relaying the image to an optical table for experiment dependent analysis and recording. The expected primary use of this instrument is a streaked optical pyrometer for witness plate measurements of the hohlraum drive temperature. The telescope is based on the University of Rochester{close_quote}s 10 in. manipulator (TIM) which allows compatibility between Omega, Trident, and the NIF lasers. The optics capture a f/7 cone of light, have a field of view of 6 mm, have a spatial resolution of 5{endash}7 {mu}m per line pair at the object plane, and are optimized for operation at 280 nm. The image is at a magnification of 11.7{times}, which is convenient for many experiments, but can be changed using additional optics that reside outside the TIM. {copyright} {ital 1999 American Institute of Physics.}

  17. Remote control and telescope auto-alignment system for multiangle LIDAR under development at CEILAP, Argentina

    E-Print Network [OSTI]

    Pallotta, Juan; Otero, Lidia; Chouza, Fernando; Raul, Delia; Gonzalez, Francisco; Etchegoyen, Alberto; Quel, Eduardo

    2013-01-01

    At CEILAP (CITEDEF-CONICET), a multiangle LIDAR is under development to monitor aerosol extinction coefficients in the frame of the CTA (Cherenkov Telescope Array) Project. This is an initiative to build the next generation of ground-based instruments to collect very high energy gamma-ray radiation (>10 GeV). The atmospheric conditions are very important for CTA observations, and LIDARs play an important role in the measurement of the aerosol optical depth at any direction. The LIDAR being developed at CEILAP was conceived to operate in harsh environmental conditions during the shifts, and these working conditions may produce misalignments. To minimize these effects, the telescopes comprising the reception unit are controlled by a self-alignment system. This paper describes the self-alignment method and hardware automation.

  18. The On-Orbit Calibrations for the Fermi Large Area Telescope

    SciTech Connect (OSTI)

    Abdo, Aous A.; /Naval Research Lab, Wash., D.C.; Ackermann, M.; /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept.; Ajello, M.; /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept.; Ampe, J.; /Naval Research Lab, Wash., D.C.; Anderson, B.; /UC, Santa Cruz; Atwood, W.B.; /UC, Santa Cruz; Axelsson, M.; /Stockholm U., OKC /Stockholm U.; Bagagli, R.; /INFN, Pisa; Baldini, L.; /INFN, Pisa; Ballet, J.; /DAPNIA, Saclay; 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; Belli, F.; /Frascati /Rome U.,Tor Vergata; Berenji, B.; /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept.; Bisello, D.; /INFN, Padua /Padua U. /Garching, Max Planck Inst., MPE /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /Ecole Polytechnique /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /INFN, Perugia /Perugia U. /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /DAPNIA, Saclay /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. /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /IASF, Milan /IASF, Milan /Kalmar U. /Stockholm U., OKC /Royal Inst. Tech., Stockholm /DAPNIA, Saclay /ASDC, Frascati /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.; /more authors..

    2011-11-17

    The Large Area Telescope (LAT) on-board the Fermi Gamma-ray Space Telescope began its on-orbit operations on June 23, 2008. Calibrations, defined in a generic sense, correspond to synchronization of trigger signals, optimization of delays for latching data, determination of detector thresholds, gains and responses, evaluation of the perimeter of the South Atlantic Anomaly (SAA), measurements of live time, of absolute time, and internal and spacecraft boresight alignments. Here we describe on-orbit calibration results obtained using known astrophysical sources, galactic cosmic rays, and charge injection into the front-end electronics of each detector. Instrument response functions will be described in a separate publication. This paper demonstrates the stability of calibrations and describes minor changes observed since launch. These results have been used to calibrate the LAT datasets to be publicly released in August 2009.

  19. A Pair Production Telescope for Medium-Energy Gamma-Ray Polarimetry

    SciTech Connect (OSTI)

    Hunter , Stanley D.; Bloser, Peter F.; Depaola, Gerardo O.; Dion, Michael P.; DeNolfo, Georgia A.; Hanu, Andrei; Iparraguirre, Marcos; Legere, Jason; Longo, Francesco; McConnell, Mark L.; Nowicki, Suzanne F.; Ryan, James M.; Son, Seunghee; Stecker, Floyd W.

    2014-08-01

    We describe the science motivation and development of a pair production telescope for medium-13 energy gamma-ray polarimetry. Our instrument concept, the Advanced Energetic Pair Telescope 14 (AdEPT), takes advantage of the Three-Dimensional Track Imager, a low-density gaseous time 15 projection chamber, to achieve angular resolution within a factor of two of the pair production 16 kinematics limit (~0.6° at 70 MeV), continuum sensitivity comparable with the Fermi-LAT front 17 detector (<3×10-6 MeV cm-2 s-1 at 70 MeV), and minimum detectable polarization less than 10% 18 for a 10 millicrab source in 106 seconds.

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

    E-Print Network [OSTI]

    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

    2015-01-01

    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.

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

    SciTech Connect (OSTI)

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

    2014-08-19

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

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

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

    Abbasi, R.; Takai, H.; Allen, C.; Beard, L.; Belz, J.; Besson, D.; Byrne, M.; Abou Bakr Othman, M.; Farhang-Boroujeny, B.; Gardner, A.; et al

    2014-08-19

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

  3. Design and Deployment of a Multichroic Polarimeter Array on the Atacama Cosmology Telescope

    E-Print Network [OSTI]

    Datta, R; Beall, J A; Becker, D; Coughlin, K P; Duff, S M; Gallardo, P A; Grace, E; Hasselfield, M; Henderson, S W; Hilton, G C; Ho, S P; Hubmayr, J; Koopman, B J; Lanen, J V; Li, D; McMahon, J; Munson, C D; Nati, F; Niemack, M D; Page, L; Pappas, C G; Salatino, M; Schmitt, B L; Schillaci, A; Simon, S M; Staggs, S T; Stevens, J R; Vavagiakis, E M; Ward, J T; Wollack, E J

    2015-01-01

    We present the design and the preliminary on sky performance with respect to beams and pass-bands of a multichroic polarimeter array covering the 90 and 146 GHz Cosmic Microwave Background (CMB) bands and its enabling broadband optical system recently deployed on the Atacama Cosmology Telescope (ACT). The constituent pixels are feedhorn-coupled multichroic polarimeters fabricated at NIST. This array is coupled to the ACT telescope via a set of three silicon lenses incorporating novel broad-band metamaterial anti-reflection coatings. This receiver represents the first multichroic detector array deployed for a CMB experiment and paves the way for the extensive use of multichroic detectors and broadband optical systems in the next generation of CMB experiments.

  4. A Prototype for the Cherenkov Telescope Array Pipelines Framework: Modular Efficiency Simple System (MESS)

    E-Print Network [OSTI]

    ,

    2015-01-01

    The Cherenkov Telescope Array (CTA) is a ground-based $\\gamma$-ray observatory that will observe the full sky in the energy range from 20 GeV to 100 TeV from facilities in both hemispheres. It is proposed to consist of more than 100 telescopes, producing large amounts of data. Apart from the storage system, there are also requirements on the software framework to allow efficient data processing, i.e. robustness, execution speed and coding efficiency. This contribution will present a plain and simple pipeline framework design prototype for CTA that builds upon well-known tools, allowing the users to focus on physics problems without learning complicated software paradigms.

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

    SciTech Connect (OSTI)

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

    2014-12-01

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

  6. Cooling Tests of the NectarCAM camera for the Cherenkov Telescope Array

    E-Print Network [OSTI]

    Moulin, E; Durand, D; Feirreira, O; Fesquet, M; Giebels, B; Glicenstein, J -F; Loiseau, D; Louis, F; Nunio, F; Rateau, S; consortia, CTA

    2015-01-01

    The NectarCAM is a camera proposed for the medium-sized telescopes in the framework of the Cherenkov Telescope Array (CTA), the next-generation observatory for very-high-energy gamma-ray astronomy. The cameras are designed to operate in an open environment and their mechanics must provide protection for all their components under the conditions defined for the CTA observatory. In order to operate in a stable environment and ensure the best physics performance, each NectarCAM will be enclosed in a slightly overpressurized, nearly air-tight, camera body, to prevent dust and water from entering. The total power dissipation will be ~7.7 kW for a 1855-pixel camera. The largest fraction is dissipated by the readout electronics in the modules. We present the design and implementation of the cooling system together with the test bench results obtained on the NectarCAM thermal demonstrator.

  7. Planning Near Earth Asteroid Observations on a 1m Class Telescope

    E-Print Network [OSTI]

    Ovidiu Vaduvescu; Mirel Birlan

    2007-02-01

    The number of known Near Earth Asteroids (NEAs) and Potentially Hazardous Asteroids (PHAs) has continued to grow in the last decade. Follow-up and recovery of newly discovered objects, as well as new astrometry at second or third oppositions are necessary to improve their orbits and predict any potential collision with the Earth in the future. A project to follow-up and recovery PHAs and NEAs is proposed, using 1m class telescopes in the next two years. Two incoming runs will take place first at Pic du Midi Observatory (France) and SAAO (South Africa), both to use 1m telescopes. Other observing runs are sought in the future. Collaborators to extend this project are welcomed.

  8. Liverpool Telescope 2: a new robotic facility for time domain astronomy in 2020+

    E-Print Network [OSTI]

    Copperwheat, C M; Bates, S D; Smith, R J; Bode, M F; Baker, I; Peacocke, T; Thomson, K

    2014-01-01

    The robotic 2m Liverpool Telescope, based on the Canary island of La Palma, has a diverse instrument suite and a strong track record in time domain science, with highlights including early time photometry and spectra of supernovae, measurements of the polarization of gamma-ray burst afterglows, and high cadence light curves of transiting extrasolar planets. In the next decade the time domain will become an increasingly prominent part of the astronomical agenda with new facilities such as LSST, SKA, CTA and Gaia, and promised detections of astrophysical gravitational wave and neutrino sources opening new windows on the transient universe. To capitalise on this exciting new era we intend to build Liverpool Telescope 2: a new robotic facility on La Palma dedicated to time domain science. The next generation of survey facilities will discover large numbers of new transient sources, but there will be a pressing need for follow-up observations for scientific exploitation, in particular spectroscopic follow-up. Live...

  9. Recent progress of GaAsP HPD development for the MAGIC telescope project

    E-Print Network [OSTI]

    T. Y. Saito; M. Shayduk; M. V. Fonseca; M. Hayashida; E. Lorenz; K. Mannheim; R. Mirzoyan; T. Schweizer; M. Teshima

    2007-09-13

    Today the Hybrid Photon Detector (HPD) is one of the few low light level (LLL) sensors that can provide an excellent single and multiple photoelectron (ph.e.) amplitude resolution. The recently developed HPDs for the MAGIC telescope project with a GaAsP photocathode, namely the R9792U-40, provide a peak quantum efficiency (QE) of more than 50% and a pulse width of ~2 nsec. In addition, the afterpulsing rate of these tubes is very low compared to that of conventional photomultiplier tubes (PMTs), i.e. the value is ~300 times lower. Photocathode aging measurements showed life time of more than 10 years under standard operating conditions of the Cherenkov Telescopes. Here we want to report on the recent progress with the above mentioned HPDs.

  10. Astrometrical Observations of Pluto - Charon System with the Automated Telescopes of Pulkovo Observatory

    E-Print Network [OSTI]

    Devyatkin, Alexander V; Slesarenko, Vyacheslav Yu

    2015-01-01

    The space probe 'New Horizon' was launched on 19th of January 2006 in order to study Pluto and its moons. Spacecraft will fly by Pluto as close as 12500 km in the middle of July 2015 and will get the most detailed images of Pluto and its moon until this moment. At the same time, observation obtained by the ground-based telescopes may also be helpful for the research of such distant system. Thereby, the Laboratory of observational astrometry of Pulkovo Observatory of RAS made a decision to reprocess observations obtained during last decade. More than 350 positional observations of Pluto - Charon system were carried out with the mirror astrograph ZA-320M at Pulkovo and Maksutov telescope MTM-500M near Kislovodsk. These observations were processed by means of software system APEX-II developed in Pulkovo observatory and numerical simulation was performed to calculate the differences between positions of photocenter and barycenter of Pluto - Charon system.

  11. Whipple Telescope Observations of LS I +61 303: 2004-2006

    E-Print Network [OSTI]

    Andy Smith

    2006-09-26

    In this paper we present the results of the past two years' observations on the galactic microquasar LS I +61 303 with the Whipple 10m gamma-ray telescope. The recent MAGIC detection of the source between 200 GeV and 4 TeV suggests that the source is periodic with very high energy (VHE) gamma-ray emission linked to its orbital cycle. The entire 50-hour data set obtained with Whipple from 2004 to 2006 was analyzed with no reliable detection resulting. The upper limits obtained in the 2005-2006 season covered several of the same epochs as the MAGIC Telescope detections, albeit with lower sensitivity. Upper limits are placed on emission during the orbital phases of 0->0.1 and 0.8->1, phases which are not included in the MAGIC data set.

  12. PONDER - A Real time software backend for pulsar and IPS observations at the Ooty Radio Telescope

    E-Print Network [OSTI]

    Naidu, Arun; Manoharan, P K; Krishnakumar, M A

    2015-01-01

    This paper describes a new real-time versatile backend, the Pulsar Ooty Radio Telescope New Digital Efficient Receiver (PONDER), which has been designed to operate along with the legacy analog system of the Ooty Radio Telescope (ORT). PONDER makes use of the current state of the art computing hardware, a Graphical Processing Unit (GPU) and sufficiently large disk storage to support high time resolution real-time data of pulsar observations, obtained by coherent dedispersion over a bandpass of 16 MHz. Four different modes for pulsar observations are implemented in PONDER to provide standard reduced data products, such as time-stamped integrated profiles and dedispersed time series, allowing faster avenues to scientific results for a variety of pulsar studies. Additionally, PONDER also supports general modes of interplanetary scintillation (IPS) measurements and very long baseline interferometry data recording. The IPS mode yields a single polarisation correlated time series of solar wind scintillation over a b...

  13. Off-disk straylight measurements for the Swedish 1-meter Solar Telescope

    E-Print Network [OSTI]

    Löfdahl, Mats G

    2015-01-01

    Context. Accurate photometry with ground based solar telescopes requires characterization of straylight. Scattering in Earth's atmosphere and in the telescope optics are potentially significant sources of straylight, for which the point spread function (PSF) has wings that reach very far. This kind of straylight produces an aureola, extending several solar radii off the solar disk. Aims. Measure such straylight using the ordinary science instrumentation. Methods. We scanned the intensity on and far off the solar disk by use of the science cameras in several different wavelength bands on a day with low-dust conditions. We characterized the far wing straylight by fitting a model to the recorded intensities involving a multi-component straylight PSF and the limb darkening of the disk. Results. The measured scattered light adds an approximately constant fraction of the local granulation intensity to science images at any position on the disk. The fraction varied over the day but never exceeded a few percent. The ...

  14. Searches for clustering in the time integrated skymap of the ANTARES neutrino telescope

    E-Print Network [OSTI]

    Adrián-Martínez, S; André, M; Anton, G; Ardid, M; Aubert, J -J; Baret, B; Barrios-Martí, J; Basa, S; Bertin, V; Biagi, S; Bogazzi, C; Bormuth, R; Bou-Cabo, M; Bouwhuis, M C; Bruijn, R; Brunner, J; Busto, J; Capone, A; Caramete, L; Carr, J; Cecchini, S; Chiarusi, T; Circella, M; Coniglione, R; Core, L; Costantini, H; Coyle, P; Creusot, A; Curtil, C; De Rosa, G; Dekeyser, I; Deschamps, A; De Bonis, G; Donzaud, C; Dornic, D; Dorosti, Q; Drouhin, D; Dumas, A; Eberl, T; Elsässer, D; Enzenhöfer, A; Escoffier, S; Fehn, K; Felis, I; Fermani, P; Folger, F; Fusco, L A; Galatŕ, S; Gay, P; Geißelsöder, S; Geyer, K; Giordano, V; Gleixner, A; Gómez-González, J P; Graf, K; Guillard, G; van Haren, H; Heijboer, A J; Hello, Y; Hernández-Rey, J J; Herold, B; Herrero, A; Hößl, J; Hofestädt, J; Hugon, C; James, C W; de Jong, M; Kadler, M; Kalekin, O; Katz, U; Kießling, D; Kooijman, P; Kouchner, A; Kreykenbohm, I; Kulikovskiy, V; Lahmann, R; Lambard, E; Lambard, G; Lattuada, D; Lefčvre, D; Leonora, E; Loehner, H; Loucatos, S; Mangano, S; Marcelin, M; Margiotta, A; Martínez-Mora, J A; Martini, S; Mathieu, A; Michael, T; Migliozzi, P; Mueller, C; Neff, M; Nezri, E; Palioselitis, D; Pavalas, G E; Perrina, C; Piattelli, P; Popa, V; Pradier, T; Racca, C; Riccobene, G; Richter, R; Roensch, K; Rostovtsev, A; Saldańa, M; Samtleben, D F E; Sánchez-Losa, A; Sanguineti, M; Schmid, J; Schnabel, J; Schulte, S; Schüssler, F; Seitz, T; Sieger, C; Spies, A; Spurio, M; Steijger, J J M; Stolarczyk, Th; Taiuti, M; Tamburini, C; Tayalati, Y; Trovato, A; Vallage, B; Vallée, C; Van Elewyck, V; Visser, E; Vivolo, D; Wagner, S; Wilms, J; de Wolf, E; Yatkin, K; Yepes, H; Zornoza, J D; Zúńiga, J

    2014-01-01

    This paper reports a search for spatial clustering of the arrival directions of high energy muon neutrinos detected by the ANTARES neutrino telescope. An improved two-point correlation method is used to study the autocorrelation of 3058 neutrino candidate events as well as cross-correlations with other classes of astrophysical objects: sources of high energy gamma rays, massive black holes and nearby galaxies. No significant deviations from the isotropic distribution of arrival directions expected from atmospheric backgrounds are observed.

  15. The Australia Telescope campaign to study southern class I methanol masers

    E-Print Network [OSTI]

    M. A. Voronkov; K. J. Brooks; A. M. Sobolev; S. P. Ellingsen; A. B. Ostrovskii; J. L. Caswell

    2007-05-02

    The Australia Telescope Compact Array (ATCA) and the Mopra facility have been used to search for new southern class I methanol masers at 9.9, 25 (J=5) and 104 GHz, which are thought to trace more energetic conditions in the interface regions of molecular outflows, than the widespread class I masers at 44 and 95 GHz. One source shows a clear outflow association.

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

    SciTech Connect (OSTI)

    Lang, Robert J.

    2010-06-24

    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.

  17. Discovery and Upper Limits in Search for Exotic Physics with Neutrino Telescopes

    E-Print Network [OSTI]

    Jan Conrad

    2006-12-04

    This note gives a short review of the statistical issues concerning upper limit calculation and claiming of discovery arising in the search for exotic physics with neutrino telescopes. Low sample sizes and significant instrumental uncertainties require special consideration. Methods for treating instrumental or theoretical uncertainties in the calculation of limits or discovery are described. Software implementing these methods is presented. The issue of optimization of analysis cuts and definition of sensitivity is briefly discussed.

  18. OSCILLATORY BEHAVIOR IN THE QUIET SUN OBSERVED WITH THE NEW SOLAR TELESCOPE

    SciTech Connect (OSTI)

    Andic, A.; Goode, P. R.; Cao, W.; Yurchyshyn, V.; Abramenko, V.; Chae, J.; Ahn, K.

    2010-07-10

    Surface photometry of the quiet Sun has achieved an angular resolution of 0.''1 with the New Solar Telescope at Big Bear Solar Observatory, revealing that a disproportionate fraction of the oscillatory events appear above observed bright point-like structures. During the tracking of these structures, we noted that the more powerful oscillatory events are cospatial with them, indicating that observed flux tubes may be the source of many observed oscillatory events.

  19. In-Flight Measurement of the Absolute Energy Scale of the Fermi Large Area Telescope

    SciTech Connect (OSTI)

    Ackermann, M.; /Stanford U., HEPL /SLAC /KIPAC, Menlo Park; Ajello, M.; /Stanford U., HEPL /SLAC /KIPAC, Menlo Park; Allafort, A.; /Stanford U., HEPL /SLAC /KIPAC, Menlo Park; Atwood, W.B.; /UC, Santa Cruz; Axelsson, M.; /Stockholm U. /Stockholm U., OKC /Royal Inst. Tech., Stockholm; Baldini, L.; /INFN, Pisa; Barbiellini, G.; /INFN, Trieste /Trieste U.; Bastieri, D.; /INFN, Padua /Padua U.; Bechtol, K.; /Stanford U., HEPL /SLAC /KIPAC, Menlo Park; Bellazzini, R.; /INFN, Pisa; Berenji, B.; /Stanford U., HEPL /SLAC /KIPAC, Menlo Park; Bloom, E.D.; /Stanford U., HEPL /SLAC /KIPAC, Menlo Park; Bonamente, E.; /INFN, Perugia /Perugia U.; Borgland, A.W.; /Stanford U., HEPL /SLAC /KIPAC, Menlo Park; Bouvier, A.; /UC, Santa Cruz; Bregeon, J.; /INFN, Pisa; Brez, A.; /INFN, Pisa; Brigida, M.; /Bari Polytechnic /INFN, Bari; Bruel, P.; /Ecole Polytechnique; Buehler, R.; /Stanford U., HEPL /SLAC /KIPAC, Menlo Park; Buson, S.; /INFN, Padua /Padua U. /CSIC, Catalunya /Stanford U., HEPL /SLAC /KIPAC, Menlo Park /IASF, Milan /DAPNIA, Saclay /INFN, Perugia /Perugia U. /Stanford U., HEPL /SLAC /KIPAC, Menlo Park /Unlisted, US /Stanford U., HEPL /SLAC /KIPAC, Menlo Park /ASDC, Frascati /Perugia U. /Stanford U., HEPL /SLAC /KIPAC, Menlo Park /Montpellier U. /ASDC, Frascati /Bari Polytechnic /INFN, Bari /Naval Research Lab, Wash., D.C. /Stanford U., HEPL /SLAC /KIPAC, Menlo Park /Stanford U., HEPL /SLAC /KIPAC, Menlo Park /Stanford U., HEPL /SLAC /KIPAC, Menlo Park /Stanford U., HEPL /SLAC /KIPAC, Menlo Park /Stanford U., HEPL /SLAC /KIPAC, Menlo Park /Stanford U., HEPL /SLAC /KIPAC, Menlo Park /Montpellier U. /Bari Polytechnic /INFN, Bari /Ecole Polytechnique /Stanford U., HEPL /SLAC /KIPAC, Menlo Park /Ecole Polytechnique /Hiroshima U. /Stanford U., HEPL /SLAC /KIPAC, Menlo Park /Bari Polytechnic /INFN, Bari /INFN, Bari /NASA, Goddard /INFN, Perugia /Perugia U.; /more authors..

    2012-09-20

    The Large Area Telescope (LAT) on-board the Fermi Gamma-ray Space Telescope is a pair-conversion telescope designed to survey the gamma-ray sky from 20 MeV to several hundreds of GeV. In this energy band there are no astronomical sources with sufficiently well known and sharp spectral features to allow an absolute calibration of the LAT energy scale. However, the geomagnetic cutoff in the cosmic ray electron-plus-positron (CRE) spectrum in low Earth orbit does provide such a spectral feature. The energy and spectral shape of this cutoff can be calculated with the aid of a numerical code tracing charged particles in the Earth's magnetic field. By comparing the cutoff value with that measured by the LAT in different geomagnetic positions, we have obtained several calibration points between {approx}6 and {approx}13 GeV with an estimated uncertainty of {approx}2%. An energy calibration with such high accuracy reduces the systematic uncertainty in LAT measurements of, for example, the spectral cutoff in the emission from gamma ray pulsars.

  20. Developments of a new mirror technology for the Cherenkov Telescope Array

    E-Print Network [OSTI]

    ,

    2015-01-01

    The Cherenkov Telescope Array (CTA) observatory for very high-energy gamma rays will consist of about a hundred of imaging atmospheric Cherenkov telescopes (IACTs) of different size with a total reflective area of about 10,000 m$^2$. Here we present a novel technology for the production of IACT mirrors that has been developed in the Institute of Nuclear Physics PAS in Krakow, Poland. The mirrors are made by cold-slumping of the front reflecting aluminium-coated panel and the rear panel interspaced with aluminium spacers. Each panel is built of two glass panels laminated with a layer of a fibreglass tissue in between for reinforcement of the structure against mechanical damage. The mirror structure is open and does not require a perfect sealing needed in closed-type designs. It prohibits water to be trapped inside and enables a proper ventilation of the mirror. Full-size hexagonal prototype mirrors produced for the medium-sized CTA telescopes will be presented together with the results of recent comprehensive ...

  1. The KM3NeT deep-sea neutrino telescope

    E-Print Network [OSTI]

    Margiotta, Annarita

    2014-01-01

    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...

  2. THE PECULIAR EXTINCTION LAW OF SN 2014J MEASURED WITH THE HUBBLE SPACE TELESCOPE

    SciTech Connect (OSTI)

    Amanullah, R.; Goobar, A.; Johansson, J.; Petrushevska, T. [Oskar Klein Centre, Physics Department, Stockholm University, SE-106 91 Stockholm (Sweden); Banerjee, D. P. K.; Venkataraman, V.; Joshi, V.; Ashok, N. M. [Physical Research Laboratory, Ahmedabad 380009 (India); Cao, Y.; Kulkarni, S. R. [Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125 (United States); Kasliwal, M. M. [Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101 (United States); Nugent, P. E. [Department of Astronomy, University of California Berkeley, B-20 Hearst Field, Annex # 3411, Berkeley, CA 94720-3411 (United States); Stanishev, V., E-mail: rahman@fysik.su.se [CENTRA—Centro Multidisciplinar de Astrofísica, Instituto Superior Técnico, Av. Rovisco Pais 1, 1049-001 Lisbon (Portugal)

    2014-06-20

    The wavelength dependence of the extinction of Type Ia SN 2014J in the nearby galaxy M82 has been measured using UV to near-IR photometry obtained with the Hubble Space Telescope, the Nordic Optical Telescope, and the Mount Abu Infrared Telescope. This is the first time that the reddening of an SN Ia is characterized over the full wavelength range of 0.2-2 ?m. A total-to-selective extinction, R{sub V} ? 3.1, is ruled out with high significance. The best fit at maximum using a Galactic type extinction law yields R{sub V} = 1.4 ± 0.1. The observed reddening of SN 2014J is also compatible with a power-law extinction, A {sub ?}/A{sub V} = (?/? {sub V}) {sup p} as expected from multiple scattering of light, with p = –2.1 ± 0.1. After correcting for differences in reddening, SN 2014J appears to be very similar to SN 2011fe over the 14 broadband filter light curves used in our study.

  3. Aspects of mechanical design for an infrared robotic telescope in Antarctica: IRAIT

    E-Print Network [OSTI]

    Igor Di VArano

    2006-09-22

    The purpose of this thesis is to focus attention on the mechanical aspects in designing an infrared telescope, IRAIT (International Robotic Antarctic Infrared Telescope), with aperture size of 80 cm, f#=21, entirely robotic and remote controlled, which must operate at Dome C, on Antarctic Plateau, starting on Summer 2007. Before illustrating in detail the choice criteria of different mechanical components, in order to satisfy stress requirements and structural verification, and the final design solutions we have adopted,firstly a few tissues must be considered. They mainly concern the preference for Dome C as probably the best observing site in the world, the scientific targets, instruments and tools necessary to reach such goals. The mechanical structure of telescope has been analyzed, and results retrieved by the static and dynamic analysis through a finite element software are illustrated. They concern the behavior of single parts, subassemblies and overall structure to active loads applied. It is shown that, as a matter of fact, thermal stress can be reckoned as the most influent of all static loads. A dynamic analysis of some critical subassemblies was used,in order to determine the frequency response of the system aiming at its best insulation from vibrations.

  4. Prospects for Gamma-Ray Bursts detection by the Cherenkov Telescope Array

    E-Print Network [OSTI]

    ,

    2015-01-01

    The first Gamma-Ray Burst (GRB) catalog presented by the Fermi-Large Area Telescope (LAT) collaboration includes 28 GRBs, detected above 100 MeV over the first three years since the launch of the Fermi mission. However, more than 100 GRBs are expected to be found over a period of six years of data collection thanks to a new detection algorithm and to the development of a new LAT event reconstruction, the so-called "Pass 8." Our aim is to provide revised prospects for GRB alerts in the CTA era in light of these new LAT discoveries. We focus initially on the possibility of GRB detection with the Large Size Telescopes (LSTs). Moreover, we investigate the contribution of the Middle Size Telescopes (MSTs), which are crucial for the search of larger areas on short post trigger timescales. The study of different spectral components in the prompt and afterglow phase, and the limits on the Extragalactic background light are highlighted. Different strategies to repoint part of - or the entire array - are studied in det...

  5. DEEP MULTI-TELESCOPE PHOTOMETRY OF NGC 5466. I. BLUE STRAGGLERS AND BINARY SYSTEMS

    SciTech Connect (OSTI)

    Beccari, G.; Dalessandro, E.; Lanzoni, B.; Ferraro, F. R.; Miocchi, P.; Sollima, A.; Bellazzini, M.

    2013-10-10

    We present a detailed investigation of the radial distribution of blue straggler star (BSS) and binary populations in the Galactic globular cluster NGC 5466, over the entire extension of the system. We used a combination of data acquired with the Advanced Camera for Survey on board the Hubble Space Telescope, the LBC-blue mounted on the Large Binocular Telescope, and MEGACAM on the Canada-France-Hawaii Telescope. BSSs show a bimodal distribution with a mild central peak and a quite internal minimum. This feature is interpreted in terms of a relatively young dynamical age in the framework of the 'dynamical clock' concept proposed by Ferraro et al. The estimated fraction of binaries is ?6%-7% in the central region (r < 90'') and slightly lower (?5.5%) in the outskirts, at r > 200''. Quite interestingly, the comparison with the results of Milone et al. suggests that binary systems may also display a bimodal radial distribution, with the position of the minimum consistent with that of BSSs. If confirmed, this feature would give additional support to the scenario where the radial distribution of objects more massive than the average cluster stars is primarily shaped by the effect of dynamical friction. Moreover, this would also be consistent with the idea that the unperturbed evolution of primordial binaries could be the dominant BSS formation process in low-density environments.

  6. The ASTRI mini-array within the future Cherenkov Telescope Array

    E-Print Network [OSTI]

    Vercellone, Stefano

    2015-01-01

    The Cherenkov Telescope Array (CTA) is a large collaborative effort aimed at the design and operation of an observatory dedicated to very high-energy gamma-ray astrophysics in the energy range from a few tens of GeV to above 100 TeV, which will yield about an order of magnitude improvement in sensitivity with respect to the current major arrays (H.E.S.S., MAGIC, and VERITAS). Within this framework, the Italian National Institute for Astrophysics is leading the ASTRI project, whose main goals are the design and installation on Mt. Etna (Sicily) of an end-to-end dual-mirror prototype of the CTA small size telescope (SST) and the installation at the CTA Southern site of a dual-mirror SST mini-array composed of nine units with a relative distance of about 300 m. The innovative dual-mirror Schwarzschild-Couder optical solution adopted for the ASTRI Project allows us to substantially reduce the telescope plate-scale and, therefore, to adopt silicon photo-multipliers as light detectors. The ASTRI mini-array is a wid...

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

    E-Print Network [OSTI]

    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

    2005-11-01

    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.

  8. IMAGING THE SUPERMASSIVE BLACK HOLE SHADOW AND JET BASE OF M87 WITH THE EVENT HORIZON TELESCOPE

    E-Print Network [OSTI]

    Lu, Ru-Sen

    The Event Horizon Telescope (EHT) is a project to assemble a Very Long Baseline Interferometry (VLBI) network of millimeter wavelength dishes that can resolve strong field general relativistic signatures near a supermassive ...

  9. CRaTER: The Cosmic Ray Telescope for the Effects of Radiation Experiment on the Lunar Reconnaissance Orbiter Mission

    E-Print Network [OSTI]

    Spence, H. E.

    The Cosmic Ray Telescope for the Effects of Radiation (CRaTER) on the Lunar Reconnaissance Orbiter (LRO) characterizes the radiation environment to be experienced by humans during future lunar missions. CRaTER measures the ...

  10. Pierre Auger Observatory and Telescope Array: Joint Contributions to the 34th International Cosmic Ray Conference (ICRC 2015)

    E-Print Network [OSTI]

    Abbasi, R U; Abu-Zayyad, T; Allen, M; Azuma, R; Barcikowski, E; Belz, J W; Bergman, D R; Blake, S A; Cady, R; Chae, M J; Cheon, B G; Chiba, J; Chikawa, M; Cho, W R; Fujii, T; Fukushima, M; Goto, T; Hanlon, W; Hayashi, Y; Hayashida, N; Hibino, K; Honda, K; Ikeda, D; Inoue, N; Ishii, T; Ishimori, R; Ito, H; Ivanov, D; Jui, C C H; Kadota, K; Kakimoto, F; Kalashev, O; Kasahara, K; Kawai, H; Kawakami, S; Kawana, S; Kawata, K; Kido, E; Kim, H B; Kim, J H; Kim, J H; Kitamura, S; Kitamura, Y; Kuzmin, V; Kwon, Y J; Lan, J; Lim, S I; Lundquist, J P; Machida, K; Martens, K; Matsuda, T; Matsuyama, T; Matthews, J N; Minamino, M; Mukai, Y; Myers, I; Nagasawa, K; Nagataki, S; Nakamura, T; Nonaka, T; Nozato, A; Ogio, S; Ogura, J; Ohnishi, M; Ohoka, H; Oki, K; Okuda, T; Ono, M; Oshima, A; Ozawa, S; Park, I H; Pshirkov, M S; Rodriguez, D C; Rubtsov, G; Ryu, D; Sagawa, H; Sakurai, N; Scott, L M; Shah, P D; Shibata, F; Shibata, T; Shimodaira, H; Shin, B K; Shin, H S; Smith, J D; Sokolsky, P; Springer, R W; Stokes, B T; Stratton, S R; Stroman, T A; Suzawa, T; Takamura, M; Takeda, M; Takeishi, R; Taketa, A; Takita, M; Tameda, Y; Tanaka, H; Tanaka, K; Tanaka, M; Thomas, S B; Thomson, G B; Tinyakov, P; Tkachev, I; Tokuno, H; Tomida, T; Troitsky, S; Tsunesada, Y; Tsutsumi, K; Uchihori, Y; Udo, S; Urban, F; Vasiloff, G; Wong, T; Yamane, R; Yamaoka, H; Yamazaki, K; Yang, J; Yashiro, K; Yoneda, Y; Yoshida, S; Yoshii, H; Zollinger, R; Zundel, Z; :,; Aab, A; Abreu, P; Aglietta, M; Ahn, E J; Samarai, I Al; Albuquerque, I F M; Allekotte, I; Allison, P; Almela, A; Castillo, J Alvarez; Alvarez-Muńiz, J; Batista, R Alves; Ambrosio, M; Aminaei, A; Anastasi, G A; Anchordoqui, L; Andringa, S; Aramo, C; Arqueros, F; Arsene, N; Asorey, H; Assis, P; Aublin, J; Avila, G; Awal, N; Badescu, A M; Baus, C; Beatty, J J; Becker, K H; Bellido, J A; Berat, C; Bertaina, M E; Bertou, X; Biermann, P L; Billoir, P; Blaess, S G; Blanco, A; Blanco, M; Blazek, J; Bleve, C; Blümer, H; Bohá?ová, M; Boncioli, D; Bonifazi, C; Borodai, N; Brack, J; Brancus, I; Bretz, T; Bridgeman, A; Brogueira, P; Buchholz, P; Bueno, A; Buitink, S; Buscemi, M; Caballero-Mora, K S; Caccianiga, B; Caccianiga, L; Candusso, M; Caramete, L; Caruso, R; Castellina, A; Cataldi, G; Cazon, L; Cester, R; Chavez, A G; Chiavassa, A; Chinellato, J A; Chudoba, J; Cilmo, M; Clay, R W; Cocciolo, G; Colalillo, R; Coleman, A; Collica, L; Coluccia, M R; Conceiçăo, R; Contreras, F; Cooper, M J; Cordier, A; Coutu, S; Covault, C E; Dallier, R; Daniel, B; Dasso, S; Daumiller, K; Dawson, B R; de Almeida, R M; de Jong, S J; De Mauro, G; Neto, J R T de Mello; De Mitri, I; de Oliveira, J; de Souza, V; del Peral, L; Deligny, O; Dhital, N; Di Giulio, C; Di Matteo, A; Diaz, J C; Castro, M L Díaz; Diogo, F; Dobrigkeit, C; Docters, W; D'Olivo, J C; Dorofeev, A; Hasankiadeh, Q Dorosti; Anjos, R C dos; Dova, M T; Ebr, J; Engel, R; Erdmann, M; Erfani, M; Escobar, C O; Espadanal, J; Etchegoyen, A; Falcke, H; Fang, K; Farrar, G; Fauth, A C; Fazzini, N; Ferguson, A P; Fick, B; Figueira, J M; Filevich, A; Filip?i?, A; Fratu, O; Freire, M M; Fujii, T; García, B; García-Gámez, D; Garcia-Pinto, D; Gate, F; Gemmeke, H; Gherghel-Lascu, A; Ghia, P L; Giaccari, U; Giammarchi, M; Giller, M; G?as, D; Glaser, C; Glass, H; Golup, G; Berisso, M Gómez; Vitale, P F Gómez; González, N; Gookin, B; Gordon, J; Gorgi, A; Gorham, P; Gouffon, P; Griffith, N; Grillo, A F; Grubb, T D; Guarino, F; Guedes, G P; Hampel, M R; Hansen, P; Harari, D; Harrison, T A; Hartmann, S; Harton, J L; Haungs, A; Hebbeker, T; Heck, D; Heimann, P; Hervé, A E; Hill, G C; Hojvat, C; Hollon, N; Holt, E; Homola, P; Hörandel, J R; Horvath, P; Hrabovský, M; Huber, D; Huege, T; Insolia, A; Isar, P G; Jandt, I; Jansen, S; Jarne, C; Johnsen, J A; Josebachuili, M; Kääpä, A; Kambeitz, O; Kampert, K H; Kasper, P; Katkov, I; Keilhauer, B; Kemp, E; Kieckhafer, R M; Klages, H O; Kleifges, M; Kleinfeller, J; Krause, R; Krohm, N; Kuempel, D; Mezek, G Kukec; Kunka, N; Awad, A W Kuotb; LaHurd, D; Latronico, L; Lauer, R; Lauscher, M; Lautridou, P; Coz, S Le; Lebrun, D; Lebrun, P; de Oliveira, M A Leigui; Letessier-Selvon, A; Lhenry-Yvon, I; Link, K; Lopes, L; López, R; Casado, A López; Louedec, K; Lucero, A; Malacari, M; Mallamaci, M; Maller, J; Mandat, D; Mantsch, P; Mariazzi, A G; Marin, V; Mari?, I C; Marsella, G; Martello, D; Martinez, H; Bravo, O Martínez; Martraire, D; Meza, J J Masías; Mathes, H J; Mathys, S; Matthews, J; Matthews, J A J; Matthiae, G; Maurizio, D; Mayotte, E; Mazur, P O; Medina, C; Medina-Tanco, G; Meissner, R; Mello, V B B; Melo, D; Menshikov, A; Messina, S; Micheletti, M I; Middendorf, L; Minaya, I A; Miramonti, L; Mitrica, B; Molina-Bueno, L; Mollerach, S; Montanet, F; Morello, C; Mostafá, M; Moura, C A; Müller, G; Muller, M A; Müller, S; Navas, S; Necesal, P; Nellen, L; Nelles, A; Neuser, J; Nguyen, P H

    2015-01-01

    Joint contributions of the Pierre Auger Collaboration and the Telescope Array Collaboration to the 34th International Cosmic Ray Conference, 30 July - 6 August 2015, The Hague, The Netherlands.

  11. A Monte Carlo template-based analysis for very high definition imaging atmospheric Cherenkov telescopes as applied to the VERITAS telescope array

    E-Print Network [OSTI]

    ,

    2015-01-01

    We present a sophisticated likelihood reconstruction algorithm for shower-image analysis of imaging Cherenkov telescopes. The reconstruction algorithm is based on the comparison of the camera pixel amplitudes with the predictions from a Monte Carlo based model. Shower parameters are determined by a maximisation of a likelihood function. Maximisation of the likelihood as a function of shower fit parameters is performed using a numerical non-linear optimisation technique. A related reconstruction technique has already been developed by the CAT and the H.E.S.S. experiments, and provides a more precise direction and energy reconstruction of the photon induced shower compared to the second moment of the camera image analysis. Examples are shown of the performance of the analysis on simulated gamma-ray data from the VERITAS array.

  12. An integral monitoring of GRS1915+105: simultaneous observations with INTEGRAL, RXTE, the Ryle and Nancay radio telescopes

    E-Print Network [OSTI]

    J. Rodriguez; G. Pooley; D. C. Hannikainen; H. J. Lehto

    2006-11-07

    Since the launch of INTEGRAL in late 2002 we have monitored the Galactic microquasar GRS 1915+105 with long exposures (~100 ks) pointings. All the observations have been conducted simultaneously with other instruments, in particular RXTE and the Ryle Telescope, and in some cases with others (Spitzer, Nancay, GMRT, Suzaku,...). We report here the results of 3 observations performed simultaneously with INTEGRAL, RXTE, the Ryle and Nancay radio telescopes. These observations show the so-called $\

  13. The Standing Wave Phenomenon in Radio Telescopes; Frequency Modulation of the WSRT Primary Beam

    E-Print Network [OSTI]

    Attila Popping; Robert Braun

    2007-12-14

    Inadequacies in the knowledge of the primary beam response of current interferometric arrays often form a limitation to the image fidelity. We hope to overcome these limitations by constructing a frequency-resolved, full-polarization empirical model for the primary beam of the Westerbork Synthesis Radio Telescope (WSRT). Holographic observations, sampling angular scales between about 5 arcmin and 11 degrees, were obtained of a bright compact source (3C147). These permitted measurement of voltage response patterns for seven of the fourteen telescopes in the array and allowed calculation of the mean cross-correlated power beam. Good sampling of the main-lobe, near-in, and far-side-lobes out to a radius of more than 5 degrees was obtained. A robust empirical beam model was detemined in all polarization products and at frequencies between 1322 and 1457 MHz with 1 MHz resolution. Substantial departures from axi-symmetry are apparent in the main-lobe as well as systematic differences between the polarization properties. Surprisingly, many beam properties are modulated at the 5 to 10% level with changing frequency. These include: (1) the main beam area, (2) the side-lobe to main-lobe power ratio, and (3) the effective telescope aperture. These semi-sinusoidsal modulations have a basic period of about 17 MHz, consistent with the natural 'standing wave' period of a 8.75 m focal distance. The deduced frequency modulations of the beam pattern were verified in an independent long duration observation using compact continuum sources at very large off-axis distances. Application of our frequency-resolved beam model should enable higher dynamic range and improved image fidelity for interferometric observations in complex fields. (abridged)

  14. Empirical Calibration of Hubble Space Telescope WFPC2 F606W and F814W Photometry

    E-Print Network [OSTI]

    Samir Salim; Andrew Gould

    1998-09-30

    Using the ground-based V and I photometry of a sample of stars from the Groth Strip, we obtain the first empirical calibration of the F606W and F814W Hubble Space Telescope WFPC2 filters for 0.5

  15. Local Group and Star Cluster Dynamics from HSTPROMO (The Hubble Space Telescope Proper Motion Collaboration)

    E-Print Network [OSTI]

    van der Marel, Roeland P; Bellini, Andrea; Besla, Gurtina; Bianchini, Paolo; Boylan-Kolchin, Mike; Chaname, Julio; Deason, Alis; Do, Tuan; Guhathakurta, Puragra; Kallivayalil, Nitya; Lennon, Danny; Massari, Davide; Meyer, Eileen; Platais, Imants; Sabbi, Elena; Sohn, Sangmo Tony; Soto, Mario; Trenti, Michele; Watkins, Laura

    2013-01-01

    The Hubble Space Telescope (HST) has proven to be uniquely suited for the measurement of proper motions (PMs) of stars and galaxies in the nearby Universe. Here we summarize the main results and ongoing studies of the HSTPROMO collaboration, which over the past decade has executed some two dozen observational and theoretical HST projects on this topic. This is continuing to revolutionize our dynamical understanding of many objects, including: globular clusters; young star clusters; stars and stellar streams in the Milky Way halo; Local Group galaxies, including dwarf satellite galaxies, the Magellanic Clouds, and the Andromeda galaxy; and AGN Black Hole Jets.

  16. Search of Dark Matter Annihilation in the Galactic Centre using the ANTARES Neutrino Telescope

    E-Print Network [OSTI]

    Adrián-Martínez, S; André, M; Anton, G; Ardid, M; Aubert, J -J; Baret, B; Barrios-Martí, J; Basa, S; Bertin, V; Biagi, S; Bogazzi, C; Bormuth, R; Bou-Cabo, M; Bouwhuis, M C; Bruijn, R; Brunner, J; Busto, J; Capone, A; Caramete, L; Carr, J; Chiarusi, T; Circella, M; Coniglione, R; Costantini, H; Coyle, P; Creusot, A; Dekeyser, I; Deschamps, A; DeBonis, G; Distefano, C; Donzaud, C; Dornic, D; Drouhin, D; Dumas, A; Eberl, T; Elsässer, D; Enzenhöfer, A; Fehn, K; Felis, I; Fermani, P; Folger, F; Fusco, L A; Galatŕ, S; Gay, P; Geißelsöder, S; Geyer, K; Giordano, V; Gleixner, A; Gracia-Ruiz, R; Graf, K; vanHaren, H; Heijboer, A J; Hello, Y; Hernández-Rey, J J; Herrero, A; Hößl, J; Hofestädt, J; Hugon, C; WJames, C; deJong, M; Kadler, M; Kalekin, O; Katz, U; Kießling, D; Kooijman, P; Kouchner, A; Kreykenbohm, I; Kulikovskiy, V; Lahmann, R; Lambard, G; Lattuada, D; Lefčvre, D; Leonora, E; Loucatos, S; Marcelin, M; Margiotta, A; Martínez-Mora, J A; Martini, S; Mathieu, A; Michael, T; Migliozzi, P; Moussa, A; Mueller, C; Neff, M; Nezri, E; P?v?la?, G E; Pellegrino, C; Perrina, C; Piattelli, P; Popa, V; Pradier, T; Racca, C; Riccobene, G; Richter, R; Roensch, K; Rostovtsev, A; Saldańa, M; Samtleben, D F E; Sanguineti, M; Sapienza, P; Schmid, J; Schnabel, J; Schulte, S; Schüssler, F; Seitz, T; Sieger, C; Spurio, M; Steijger, J J M; Stolarczyk, Th; Sánchez-Losa, A; Taiuti, M; Tamburini, C; Trovato, A; Tselengidou, M; Tönnis, C; Vallage, B; Vallée, C; VanElewyck, V; Visser, E; Vivolo, D; Wagner, S; Wilms, J; Zornoza, J D; Zúńiga, J

    2015-01-01

    A search for high-energy neutrinos coming from the direction of the Galactic Centre is performed using the data recorded by the ANTARES neutrino telescope from 2007 to 2012. The event selection criteria are chosen to maximise the sensitivity to possible signals produced by the self-annihilation of weakly interacting massive particles accumulated around the centre of the Milky Way with respect to the atmospheric background. After data unblinding, the number of neutrinos observed in the line of sight of the Galactic Centre is found to be compatible with background expectations. The 90% C.L. upper limits in terms of the neutrino+anti-neutrino flux, $\\rm \\Phi_{\

  17. Indirect Searches for Dark Matter with the Fermi Large Area Telescope1

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

    Albert, Andrea

    2015-01-01

    There is overwhelming evidence that non-baryonic dark matter constitutes ~ 27% of the energy density of the Universe. Weakly Interacting Massive Particles (WIMPs) are promising dark matter candidates that may produce ? rays via annihilation or decay detectable by the Fermi Large Area Telescope (LAT). A detection of WIMPs would also indicate the existence of physics beyond the Standard Model. We present recent results from the two cleanest indirect WIMP searches by the Fermi-LAT Collaboration: searches for ?-ray spectral lines and ?-ray emission associated with Milky Way dwarf spheroidal satellite galaxies.

  18. Indirect Detection of Dark Matter in km-size Neutrino Telescopes

    E-Print Network [OSTI]

    Lars Bergstrom; Joakim Edsjo; Paolo Gondolo

    1999-06-02

    Neutrino telescopes of kilometer size are currently being planned. They will be two or three orders of magnitude larger than presently operating detectors, but they will have a much higher muon energy threshold. We discuss the trade-off between area and energy threshold for indirect detection of neutralino dark matter captured in the Sun and in the Earth and annihilating into high energy neutrinos. We also study the effect of a higher threshold on the complementarity of different searches for supersymmetric dark matter.

  19. Indirect searches for dark matter with the Fermi large area telescope

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

    Albert, Andrea

    2015-03-24

    There is overwhelming evidence that non-baryonic dark matter constitutes ~ 27% of the energy density of the Universe. Weakly Interacting Massive Particles (WIMPs) are promising dark matter candidates that may produce ? rays via annihilation or decay detectable by the Fermi Large Area Telescope (LAT). A detection of WIMPs would also indicate the existence of physics beyond the Standard Model. We present recent results from the two cleanest indirect WIMP searches by the Fermi-LAT Collaboration: searches for ?-ray spectral lines and ?-ray emission associated with Milky Way dwarf spheroidal satellite galaxies.

  20. Fermi Large Area Telescope Constraints on the Gamma-ray Opacity of the

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

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration would likeUniverse (Journal Article) | SciTech Connect Large Area Telescope Constraints on

  1. Measurements of Antenna Surface for Millimeter-Wave Space Radio Telescope

    E-Print Network [OSTI]

    Kamegai, Kazuhisa; Doi, Akihiro; Sato, Eiichi

    2011-01-01

    In the construction of a space radio telescope, it is essential to use materials with a low noise factor and high mechanical robustness for the antenna surface. We present the results of measurements of the reflection performance of two candidates for antenna surface materials for use in a radio telescope installed in a new millimeter-wave astronomical satellite, ASTRO-G. To estimate the amount of degradation caused by fluctuations in the thermal environment in the projected orbit of the satellite, a thermal cycle test was carried out for two candidates, namely, copper foil carbon fiber reinforced plastic (CFRP) and aluminum-coated CFRP. At certain points during the thermal cycle test, the reflection loss of the surfaces was measured precisely by using a radiometer in the 41-45 GHz band. In both candidates, cracks appeared on the surface after the thermal cycle test, where the number density of the cracks increased as the thermal cycle progressed. The reflection loss also increased in proportion to the number...

  2. Beyond 31 mag/arcsec^2: the low surface brightness frontier with the largest optical telescopes

    E-Print Network [OSTI]

    Trujillo, Ignacio

    2015-01-01

    The detection of optical surface brightness structures in the sky with magnitudes fainter than 30 mag/arcsec^2 (3sigma in 10x10 arcsec boxes; r-band) has remained elusive in current photometric deep surveys. Here we show how present-day 10 meter class telescopes can provide broadband imaging 1.5-2 mag deeper than most previous results within a reasonable amount of time (i.e. <10h on source integration). In particular, we illustrate the ability of the 10.4 m Gran Telescopio de Canarias (GTC) telescope to produce imaging with a limiting surface brightness of 31.5 mag/arcsec^2 (3sigma in 10x10 arcsec boxes; r-band) using 8.1 hours on source. We apply this power to explore the stellar halo of the galaxy UGC00180, a galaxy analogous to M31 located at ~150 Mpc, by obtaining a surface brightness radial profile down to mu_r~33 mag/arcsec^2. This depth is similar to that obtained using star counts techniques of Local Group galaxies, but is achieved at a distance where this technique is unfeasible. We find that the ...

  3. Prototype secondary mirror assembly design for the space infrared telescope facility

    SciTech Connect (OSTI)

    Stier, M.; Duffy, M.; Gullapalli, S.; Rockwell, R.; Sileo, F.; Krim, M.

    1989-02-01

    The authors describe their design of a liquid helium temperature prototype secondary mirror assembly (PSMA) under development for the NASA Space Infrared Telescope Facility (SIRTF) program. The SIRTF secondary mirror assembly must operate below 4 K and provide the functions of highly precise 2-axis dynamic tilting (chopping) in addition to the conventional functions needed by the SIRTF observatory. Their PSMA design employs a fused quartz mirror kinematically attached at its center to an aluminium cruciform. The mirror/cruciform assembly is driven in tilt about its combined center of mass using a unique flexure pivot and a four-actuator control system with feedback provided by pairs of differential position sensors. The voice coil actuators are mounted on a second flexure-pivoted mass enhancing servo system stability and isolating the telescope from vibration-induced disturbances. The mirror/cruciform and the reaction mass are attached to opposite sides of an aluminum mounting plate whose dimensional characteristics are nominally identical to that of the aluminum flexure pivot material. The mounting plate is connected to the outer housing by a six degree of freedom focus and centering mechanism using pivoted actuation levers driven by lead screw/harmonic drive/stepper motor assemblies.

  4. A Near-Infrared Spectroscopic Survey at the SDSS 2.5-meter Telescope?

    E-Print Network [OSTI]

    Skrutskie, Michael F

    2015-01-01

    We are posting this 10-year-old white paper to support an upcoming survey description paper for the SDSS-III Apache Point Galactic Evolution Experiment (APOGEE) led by PI Dr. Steven Majewski. The white paper presented here was a contribution to a 2005 "futures" planning process for the Astrophysical Research Consortium led by Dr. Donald York that examined both prospects for extending the work of SDSS and SDSS-II as well as enhancing the capabilities of the Apache Point 3.5-meter telescope and the overall scientific reach of the Consortium. This particular white paper describes the potential for using the Sloan 2.5-meter telescope and its fiber optic infrastructure to conduct a galactic plane chemical abundance survey in the low-extinction 1.6um H-band. The survey would target >1000 red giant stars per night selected from the Two Micron All Sky Survey using a >200 fiber near-infrared spectrograph operating at spectral resolution of R~24,000 with a magnitude limit of H~12 - very close to the final APOGEE implem...

  5. The First Swift Ultra-Violet/Optical Telescope GRB Afterglow Catalog

    E-Print Network [OSTI]

    Roming, P W A; Oates, S R; Porterfield, B L; Berk, D E Vanden; Boyd, P T; Holland, S T; Hoversten, E A; Immler, S; Marshall, F E; Page, M J; Racusin, J L; Schneider, D P; Breeveld, A A; Brown, P J; Chester, M M; Cucchiara, A; De Pasquale, M; Gronwall, C; Hunsberger, S D; Kuin, N P M; Landsman, W B; Schady, P; Still, M

    2008-01-01

    We present the first Swift Ultra-Violet/Optical Telescope (UVOT) gamma-ray burst (GRB) afterglow catalog. The catalog contains data from over 64,000 independent UVOT image observations of 229 GRBs first detected by Swift, the High Energy Transient Explorer 2 (HETE2), the INTErnational Gamma-Ray Astrophysics Laboratory (INTEGRAL), and the Interplanetary Network (IPN). The catalog covers GRBs occurring during the period from 2005 Jan 17 to 2007 Jun 16 and includes ~86% of the bursts detected by the Swift Burst Alert Telescope (BAT). The catalog provides detailed burst positional, temporal, and photometric information extracted from each of the UVOT images. Positions for bursts detected at the 3-sigma-level are provided with a nominal accuracy, relative to the USNO-B1 catalog, of ~0.25 arcseconds. Photometry for each burst is given in three UV bands, three optical bands, and a 'white' or open filter. Upper limits for magnitudes are reported for sources detected below 3-sigma. General properties of the burst samp...

  6. A space bourne crystal diffraction telescope for the energy range of nuclear transitions

    SciTech Connect (OSTI)

    von Ballmoos, P.; Naya, J.E.; Albernhe, F.; Vedrenne, G. [Centre d`Etude Spatial des Rayonnements, Toulouse (France); Smither, R.K.; Faiz, M.; Fernandez, P.; Graber, T. [Argonne National Lab., IL (United States)

    1995-10-01

    Recent experimental work of the Toulouse-Argonne collaboration has opened for perspective of a focusing gamma-ray telescope operating in the energy range of nuclear transitions, featuring unprecedented sensitivity, angular and energy resolution. The instrument consists of a tunable crystal diffraction lens situated on a stabilized spacecraft, focusing gamma-rays onto a small array of Germanium detectors perched on an extendible boom. While the weight of such an instrument is less than 500 kg, it features an angular resolution of 15 in., an energy resolution of 2 keV and a 3 {sigma} narrow line sensitivity of a few times 10{sup {minus}7} photons s{sup {minus}1} cm{sup {minus}2} (10{sup 6} sec observation). This instrumental concept permits observation of any identified source at any selected line-energy in a range of typically 200 keV to 1300 keV. The resulting ``sequential`` operation mode makes sites of explosive nucleosynthesis natural scientific objectives for such a telescope: the nuclear lines of extragalactic supernovae ({sup 56}Ni, {sup 44}Ti, {sup 60}Fe) and galactic novae (p{sup {minus}}p{sup +} line, {sup 7}Be) are accessible to observation, one at a time, due to the erratic appearance and the sequence of half-lifes of these events. Other scientific objectives, include the narrow 511 keV line from galactic broad class annihilators (such as 1E1740-29, nova musca) and possible redshifted annihilation lines from AGN`s.

  7. Parallel waveform extraction algorithms for the Cherenkov Telescope Array Real-Time Analysis

    E-Print Network [OSTI]

    Zoli, Andrea; De Rosa, Adriano; Aboudan, Alessio; Fioretti, Valentina; De Cesare, Giovanni; Marx, Ramin

    2015-01-01

    The Cherenkov Telescope Array (CTA) is the next generation observatory for the study of very high-energy gamma rays from about 20 GeV up to 300 TeV. Thanks to the large effective area and field of view, the CTA observatory will be characterized by an unprecedented sensitivity to transient flaring gamma-ray phenomena compared to both current ground (e.g. MAGIC, VERITAS, H.E.S.S.) and space (e.g. Fermi) gamma-ray telescopes. In order to trigger the astrophysics community for follow-up observations, or being able to quickly respond to external science alerts, a fast analysis pipeline is crucial. This will be accomplished by means of a Real-Time Analysis (RTA) pipeline, a fast and automated science alert trigger system, becoming a key system of the CTA observatory. Among the CTA design key requirements to the RTA system, the most challenging is the generation of alerts within 30 seconds from the last acquired event, while obtaining a flux sensitivity not worse than the one of the final analysis by more than a fac...

  8. The Infrared Cloud Monitor for the MAGNUM Robotic Telescope at Haleakala

    E-Print Network [OSTI]

    M. Suganuma; Y. Kobayashi; N. Okada; Y. Yoshii; T. Minezaki; T. Aoki; K. Enya; H. Tomita; S. Koshida

    2007-04-18

    We present the most successful infrared cloud monitor for a robotic telescope. This system was originally developed for the MAGNUM 2-m telescope, which has been achieving unmanned and automated monitoring observation of active galactic nuclei at Haleakala on the Hawaiian island of Maui since 2001. Using a thermal imager and two aspherical mirrors, it at once sees almost the whole sky at a wavelength of $\\lambda\\sim 10\\mu{\\rm m}$. Its outdoor part is weather-proof and is totally maintenance-free. The images obtained every one or two minutes are analysed immediately into several ranks of weather condition, from which our automated observing system not only decides to open or close the dome, but also selects what types of observations should be done. The whole-sky data accumulated over four years show that 50$-$60 % of all nights are photometric, and about 75 % are observable with respect to cloud condition at Haleakala. Many copies of this system are now used all over the world such as Mauna Kea in Hawaii, Atacama in Chile, and Okayama and Kiso in Japan.

  9. Warm molecular Hydrogen at high redshift with the James Webb Space Telescope

    E-Print Network [OSTI]

    Guillard, P; Lehnert, M D; Appleton, P N; Foręts, G Pineau des

    2015-01-01

    The build-up of galaxies is regulated by a complex interplay between gravitational collapse, galaxy merging and feedback related to AGN and star formation. The energy released by these processes has to dissipate for gas to cool, condense, and form stars. How gas cools is thus a key to understand galaxy formation. \\textit{Spitzer Space Telescope} infrared spectroscopy revealed a population of galaxies with weak star formation and unusually powerful H$_2$ line emission. This is a signature of turbulent dissipation, sustained by large-scale mechanical energy injection. The cooling of the multiphase interstellar medium is associated with emission in the H$_2$ lines. These results have profound consequences on our understanding of regulation of star formation, feedback and energetics of galaxy formation in general. The fact that H$_2$ lines can be strongly enhanced in high-redshift turbulent galaxies will be of great importance for the \\textit{James Webb Space Telescope} observations which will unveil the role tha...

  10. Optical module HEW simulations for the X-ray telescopes SIMBOL-X, EDGE and XEUS

    E-Print Network [OSTI]

    Spiga, D

    2015-01-01

    One of the most important parameters defining the angular resolution of an X-ray optical module is its Half-Energy Width (HEW) as a function of the photon energy. Future X-ray telescopes with imaging capabilities (SIMBOL-X, Constellation-X, NeXT, EDGE, XEUS,...) should be characterized by a very good angular resolution in soft ( 10 keV) X-rays. As a consequence, an important point in the optics development for these telescopes is the simulation of the achievable HEW for a system of X-ray mirrors. This parameter depends on the single mirror profile and nesting accuracy, but also on the mirrors surface microroughness that causes X-ray Scattering (XRS). In particular, owing to its dependence on the photon energy, XRS can dominate the profile errors in hard X-rays: thus, its impact has to be accurately evaluated in every single case, in order to formulate surface finishing requirements for X-ray mirrors. In this work we provide with some simulations of the XRS term of the HEW for some future soft and hard X-ray t...

  11. Near-infrared detection of WD 0806-661 B with the Hubble space telescope

    SciTech Connect (OSTI)

    Luhman, K. L.; Esplin, T. L.; Morley, C. V.; Burgasser, A. J.; Bochanski, J. J.

    2014-10-10

    WD 0806-661 B is one of the coldest known brown dwarfs (T {sub eff} = 300-345 K) based on previous mid-infrared photometry from the Spitzer Space Telescope. In addition, it is a benchmark for testing theoretical models of brown dwarfs because its age and distance are well constrained via its primary star (2 ± 0.5 Gyr, 19.2 ± 0.6 pc). We present the first near-infrared detection of this object, which has been achieved through F110W imaging (?Y + J) with the Wide Field Camera 3 on board the Hubble Space Telescope. We measure a Vega magnitude of m {sub 110} = 25.70 ± 0.08, which implies J ? 25.0. When combined with the Spitzer photometry, our estimate of J helps to better define the empirical sequence of the coldest brown dwarfs in M {sub 4.5} versus J – [4.5]. The positions of WD 0806-661 B and other Y dwarfs in that diagram are best matched by the cloudy models of Burrows et al. and the cloudless models of Saumon et al., both of which employ chemical equilibrium. The calculations by Morley et al. for 50% cloud coverage differ only modestly from the data. Spectroscopy would enable a more stringent test of the models, but based on our F110W measurement, such observations are currently possible only with Hubble, and would require at least ?10 orbits to reach a signal-to-noise ratio of ?5.

  12. Second Einstein Telescope Mock Data and Science Challenge: Low Frequency Binary Neutron Star Data Analysis

    E-Print Network [OSTI]

    Meacher, Duncan; Hanna, Chad; Regimbau, Tania; Sathyaprakash, B S

    2015-01-01

    The Einstein Telescope is a conceived third generation gravitational-wave detector that is envisioned to be an order of magnitude more sensitive than advanced LIGO, Virgo and Kagra, which would be able to detect gravitational-wave signals from the coalescence of compact objects with waveforms starting as low as 1Hz. With this level of sensitivity, we expect to detect sources at cosmological distances. In this paper we introduce an improved method for the generation of mock data and analyse it with a new low latency compact binary search pipeline called gstlal. We present the results from this analysis with a focus on low frequency analysis of binary neutron stars. Despite compact binary coalescence signals lasting hours in the Einstein Telescope sensitivity band when starting at 5 Hz, we show that we are able to discern various overlapping signals from one another. We also determine the detection efficiency for each of the analysis runs conducted and and show a proof of concept method for estimating the numbe...

  13. TARGET: toward a solution for the readout electronics of the Cherenkov Telescope Array

    E-Print Network [OSTI]

    Tibaldo, L; Albert, A M; Funk, S; Kawashima, T; Kraus, M; Okumura, A; Sapozhnikov, L; Tajima, H; Varner, G S; Wu, T; Zink, A

    2015-01-01

    TARGET is an application specific integrated circuit (ASIC) designed to read out signals recorded by the photosensors in cameras of very-high-energy gamma-ray telescopes exploiting the imaging of Cherenkov radiation from atmospheric showers. TARGET capabilities include sampling at a high rate (typically 1 GSample/s), digitization, and triggering on the sum of four adjacent pixels. The small size, large number of channels read out per ASIC (16), low cost per channel, and deep buffer for trigger latency (~16 $\\mu$s at 1 GSample/s) make TARGET ideally suited for the readout in systems with a large number of telescopes instrumented with compact photosensors like multi-anode or silicon photomultipliers combined with dual-mirror optics. The possible advantages of such systems are better sensitivity, a larger field of view, and improved angular resolution. The two latest generations of TARGET ASICs, TARGET 5 and TARGET 7, are soon to be used for the first time in two prototypes of small-sized and medium-sized dual-m...

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

    E-Print Network [OSTI]

    ,

    2011-01-01

    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) onboard the \\emph{Fermi} Gamma-ray Space Telescope. An investigation of the relationship among 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 $\\pm$ 0.6 (stat) $\\pm$ 1.2 (sys) GeV, and photon indices of 2.10 $\\pm$ 0.06 (stat) $\\pm$ 0.10 (sys) below the break and 2.70 $\\pm$ 0.12 (stat) $\\pm$ 0.14...

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

    E-Print Network [OSTI]

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

    2015-01-01

    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...

  16. Fermi Large Area Telescope Observations of the Cygnus Loop Supernova Remnant

    SciTech Connect (OSTI)

    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.

    2011-11-08

    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.

  17. Cosmology with the Very Large Telescope Interferometer using a space based astrometric reference frame

    E-Print Network [OSTI]

    David Tytler

    1997-01-26

    Cosmology with large interferometric telescopes is a rich and largely unexplored subject, involving three types of measurement: astrometric measurement of absolute distances and proper motions, dispersions of relative proper motions, and images. The ground based interferometers can have huge apertures, which are necessary for faint cosmological targets. But, alone, they are limited to astrometry within the isoplanatic patch, and hence to relative positions, which are of little use for parallaxes and proper motions because reference stars have unknown parallaxes and huge (500 \\mu arcsec) unknown motions. We propose that space missions should measure global astrometric parallaxes and proper motions for (V > 16) reference stars within the isoplanatic patches of important cosmological and Galactic targets. Ground based interferometers can then measure absolute distances (parallaxes) and proper motions to 10 \\mu arcsec, tied to these reference stars. But cosmological observations stretch the VLTI technically. To observe the few best targets, we need to be able to measure positions to 16) near to important targets. Most of the science is at 1 --2 microns, where excellent adaptive optics will be needed on the 8-m telescopes.

  18. Investigation of intergranular bright points from the New Vacuum Solar Telescope

    E-Print Network [OSTI]

    Ji, Kai-Fan; Xiang, Yong-yuan; Feng, Song; Deng, Hui; Wang, Feng; Yang, Yun-Fei

    2015-01-01

    Six high-resolution TiO-band image sequences from the New Vacuum Solar Telescope (NVST) are used to investigate the properties of intergranular bright points (igBPs). We detect the igBPs using a Laplacian and morphological dilation algorithm (LMD) and track them using a three-dimensional segmentation algorithm automatically, and then investigate the morphologic, photometric and dynamic properties of igBPs, in terms of equivalent diameter, the intensity contrast, lifetime, horizontal velocity, diffusion index, motion range and motion type. The statistical results confirm the previous studies based on G-band or TiO-band igBPs from the other telescopes. It illustrates that the TiO data from the NVST have a stable and reliable quality, which are suitable for studying the igBPs. In addition, our method is feasible to detect and track the igBPs in the TiO data from the NVST. With the aid of the vector magnetograms obtained from the Solar Dynamics Observatory /Helioseismic and Magnetic Imager, the properties of igBP...

  19. Performance of the Mechanical Structure of the SST-2M GCT Proposed for the Cherenkov Telescope Array

    E-Print Network [OSTI]

    Dournaux, Jean-Laurent; Dumas, Delphine; Amans, Jean-Philippe; Fasola, Gilles; Laporte, Philippe; Bousquet, Jean-Jacques; Sol, Hélčne

    2015-01-01

    The Cherenkov Telescope Array (CTA) consortium aims to create the next generation Very High Energy gamma-ray observatory. It will be devoted to the observation of gamma rays over a wide band of energy, from 20 GeV to 300 TeV. Three different classes, Large, Medium and Small Size Telescopes, are foreseen to cover the low, intermediate and high energy regions, respectively. The energy range of the Small Size Telescopes (SSTs) extends from 1 TeV to 300 TeV. Among them, the Gamma-ray Cherenkov Telescope (GCT), a telescope based on a Schwarzschild-Couder dual-mirror optical design, is one of the prototypes under construction proposed for the SST sub-array of CTA. This contribution focuses on the mechanical structure of GCT. It reports on last progress on the mechanical design and discusses this in the context of CTA specifications. Recent advances in the assembly and installation of the opto-mechanical prototype of GCT on the French site of the Paris Observatory are also described.

  20. Astron. Nachr. / AN 327, No. 8, 800 802 (2006) / DOI 10.1002/asna.200610682 The WASP project in the era of robotic telescope networks

    E-Print Network [OSTI]

    Norton, Andrew J.

    2006-01-01

    in the era of robotic telescope networks D.J. Christian1, D.L. Pollacco1 , I. Skillen2 , J. Irwin3 , W-mountain reductions that could be used to automatically drive alerts via a small robotic telescope network://www.superwasp.org/. c 2006 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim 1 Introduction The era of small robotic telescopes

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

    E-Print Network [OSTI]

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

    2008-10-27

    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.

  2. Early-Time Flux Measurements of SN 2014J Obtained with Small Robotic Telescopes: Extending the AAVSO Light Curve

    E-Print Network [OSTI]

    Poppe, B; Zheng, W; Shivvers, I; Itagaki, K; Filippenko, A V; Kunz, J

    2015-01-01

    In this work, early-time photometry of supernova (SN) 2014J is presented, extending the AAVSO CCD database to prediscovery dates. The applicability of NASA's small robotic MicroObservatory Network telescopes for photometric measurements is evaluated. Prediscovery and postdiscovery photometry of SN 2014J is measured from images taken by two different telescopes of the network, and is compared to measurements from the Katzman Automatic Imaging Telescope and the Itagaki Observatory. In the early light-curve phase (which exhibits stable spectral behavior with constant color indices), these data agree with reasonably high accuracy (better than 0.05 mag around maximum brightness, and 0.15 mag at earlier times). Owing to the changing spectral energy distribution of the SN and the different spectral characteristics of the systems used, differences increase after maximum light. We augment light curves of SN 2014J downloaded from the American Association of Variable Star Observers (AAVSO) online database with these dat...

  3. CHARACTERIZING THE ATMOSPHERES OF TRANSITING PLANETS WITH A DEDICATED SPACE TELESCOPE

    SciTech Connect (OSTI)

    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)

    2012-02-10

    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.

  4. Fermi large area telescope detection of a break in the gamma-ray spectrum of the supernova remnant Cassiopeia A

    SciTech Connect (OSTI)

    Yuan, Yajie; Funk, Stefan; Lande, Joshua; Tibaldo, Luigi [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); Jóhannesson, Gülauger [Science Institute, University of Iceland, IS-107 Reykjavik (Iceland); Uchiyama, Yasunobu, E-mail: yuanyj@stanford.edu, E-mail: funk@slac.stanford.edu, E-mail: joshualande@gmail.com, E-mail: uchiyama@slac.stanford.edu [3-34-1 Nishi-Ikebukuro, Toshima-ku, Tokyo 171-8501 (Japan)

    2013-12-20

    We report on observations of the supernova remnant Cassiopeia A in the energy range from 100 MeV to 100 GeV using 44 months of observations from the Large Area Telescope on board the Fermi Gamma-Ray Space Telescope. We perform a detailed spectral analysis of this source and report on a low-energy break in the spectrum at 1.72{sub ?0.89}{sup +1.35} GeV. By comparing the results with models for the gamma-ray emission, we find that hadronic emission is preferred for the GeV energy range.

  5. Design and construction of a multi-layer CsI(Tl) telescope for high-energy reaction studies

    E-Print Network [OSTI]

    Yan, D; Yue, K; Wang, S T; Zhang, X H; Yu, Y H; Chen, J L; Tang, S W; Fang, F; Zhou, Y; Sun, Y; Wang, Z M; Sun, Y Z

    2015-01-01

    A prototype of a new CsI(Tl) telescope, which will be used in the reaction studies of light isotopes with energy of several hundred AMeV, has been constructed and tested at the Institute of Modern Physics, Chinese Academy of Sciences. The telescope has a multi-layer structure and the range information will be obtained to improve the particle identification performance. This prototype has seven layers of different thickness. A 5.0% (FWHM) energy resolution has been extracted for one of the layers in a beam test experiment. Obvious improvement for the identification of $^{14}$O and $^{15}$O isotopes was achieved by using the range information.

  6. Photometric Properties of Ceres from Telescopic Observations using Dawn Framing Camera Color Filters

    E-Print Network [OSTI]

    Reddy, Vishnu; Gary, Bruce L; Sanchez, Juan A; Stephens, Robert D; Megna, Ralph; Coley, Daniel; Nathues, Andreas; Corre, Lucille Le; Hoffmann, Martin

    2015-01-01

    The dwarf planet Ceres is likely differentiated similar to the terrestrial planets but with a water/ice dominated mantle and an aqueously altered crust. Detailed modeling of Ceres' phase function has never been performed to understand its surface properties. The Dawn spacecraft began orbital science operations at the dwarf planet in April 2015. We observed Ceres with flight spares of the seven Dawn Framing Camera color filters mounted on ground-based telescopes over the course of three years to model its phase function versus wavelength. Our analysis shows that the modeled geometric albedos derived from both the IAU HG model and the Hapke model are consistent with a flat and featureless spectrum of Ceres, although the values are ~10% higher than previous measurements. Our models also suggest a wavelength dependence of Ceres' phase function. The IAU G-parameter and the Hapke single-particle phase function parameter, g, are both consistent with decreasing (shallower) phase slope with increasing wavelength. Such...

  7. Square Kilometer Array Telescope - Precision Reference Frequency Synchronisation via 1f-2f Dissemination

    E-Print Network [OSTI]

    Wang, B; Gao, C; Bai, Y; Dong, J W; Wang, L J

    2015-01-01

    The Square Kilometer Array (SKA) is an international effort to build the world's largest radio telescope, with one square kilometer collecting area. Besides its ambitious scientific objectives, such as probing the cosmic dawn and cradle of life, SKA also demands several revolutionary technological breakthroughs, with ultra-high precision synchronisation of the frequency references for thousands of antennas being one of them. In this report, aimed at applications to SKA, we demonstrate a frequency reference synchronization and dissemination scheme with the phase noise compensation function placed at the client site. Hence, one central hub can be linked to a large number of client sites, forming a star-shaped topology. As a performance test, the 100 MHz reference signal from a Hydrogen maser clock is disseminated and recovered at two remote sites. Phase noise characteristics of the recovered reference frequency signal coincides with that of the hydrogen-maser source and satisfies SKA requirement.

  8. First Results From the Large Binocular Telescope: Deep Photometry of New dSphs

    E-Print Network [OSTI]

    Matthew G. Coleman; Jelte de Jong

    2007-08-20

    This contribution describes photometry for two Galactic dSphs obtained with the Large Binocular Telescope to a magnitude of ~25.5. Using the Large Binocular Camera, a purpose-built wide-field imager for the LBT, we have examined the structure and star formation histories of two newly-discovered Local Group members, the Hercules dSph and the Leo T dSph/dIrr system. We have constructed a structural map for the Hercules system using three-filter photometry to V ~ 25.5. This is the first deep photometry for this system, and it indicates that Hercules is unusually elongated, possibly indicating distortion due to the Galactic tidal field. We have also derived the first star formation history for the Leo T system, and find that its oldest population of stars (age ~ 13 Gyr) were relatively metal-rich, with [Fe/H] ~ -1.5.

  9. The White Mountain Polarimeter Telescope and an Upper Limit on CMB Polarization

    E-Print Network [OSTI]

    Alan R. Levy; Rodrigo Leonardi; Markus Ansmann; Marco Bersanelli; Jeffery Childers; Terrence D. Cole; Ocleto D'Arcangelo; G. Vietor Davis; Philip M. Lubin; Joshua Marvil; Peter R. Meinhold; Gerald Miller; Hugh O`Neill; Fabrizio Stavola; Nathan C. Stebor; Peter T. Timbie; Maarten van der Heide; Fabrizio Villa; Thyrso Villela; Brian D. Williams; Carlos A. Wuensche

    2008-04-23

    The White Mountain Polarimeter (WMPol) is a dedicated ground-based microwave telescope and receiver system for observing polarization of the Cosmic Microwave Background. WMPol is located at an altitude of 3880 meters on a plateau in the White Mountains of Eastern California, USA, at the Barcroft Facility of the University of California White Mountain Research Station. Presented here is a description of the instrument and the data collected during April through October 2004. We set an upper limit on $E$-mode polarization of 14 $\\mu\\mathrm{K}$ (95% confidence limit) in the multipole range $170<\\ell<240$. This result was obtained with 422 hours of observations of a 3 $\\mathrm{deg}^2$ sky area about the North Celestial Pole, using a 42 GHz polarimeter. This upper limit is consistent with $EE$ polarization predicted from a standard $\\Lambda$-CDM concordance model.

  10. Umbral Fine Structures in Sunspots Observed with Hinode Solar Optical Telescope

    E-Print Network [OSTI]

    Reizaburo Kitai; Hiroko Watanabe; Tahei Nakamura; Ken-ichi Otsuji; Takuma Matsumoto; Satoru UeNo; Shin-ichi Nagata; Kazunari Shibata; Richard Muller; Kiyoshi Ichimoto; Saku Tsuneta; Yoshinori Suematsu; Yukio Katsukawa; Toshifumi Shimizu; Theodore D. Tarbell; Richard A. Shine; Alan M. Title; Bruce W. Lites

    2007-11-21

    High resolution imaging observation of a sunspot umbra was done with Hinode Solar Optical Telescope (SOT). Filtergrams in wavelengths of blue and green continuum were taken during three consecutive days. The umbra consisted of a dark core region, several diffuse components and numerous umbral dots. We derived basic properties of umbral dots (UDs), especially their temperatures, lifetimes, proper motions, spatial distribution and morphological evolution. Brightness of UDs is confirmed to depend on the brightness of their surrounding background. Several UDs show fission and fusion. Thanks to the stable condition of space observation, we could first follow the temporal behavior of these events. The derived properties of internal structure of the umbra are discussed in viewpoint of magnetoconvection in a strong magnetic field.

  11. On-orbit Performance of the Solar Optical Telescope aboard Hinode

    E-Print Network [OSTI]

    K. Ichimoto; Y. Katsukawa; T. Tarbell; R. A. Shine; C. Hoffmann; T. Berger; T. Cruz; Y. Suematsu; S. Tsuneta; T. Shimizu; B. W. Lites

    2008-04-21

    On-orbit performance of the Solar Optical Telescope (SOT) aboard Hinode is described with some attentions on its unpredicted aspects. In general, SOT revealed an excellent performance and has been providing outstanding data. Some unexpected features exist, however, in behaviors of the focus position, throughput and structural stability. Most of them are recovered by the daily operation i.e., frequent focus adjustment, careful heater setting and corrections in data analysis. The tunable filter contains air bubbles which degrade the data quality significantly. Schemes for tuning the filter without disturbing the bubbles have been developed and tested, and some useful procedures to obtain Dopplergram and magnetogram are now available. October and March when the orbit of satellite becomes nearly perpendicular to the direction towards the sun provide a favorable condition for continuous runs of the narrow-band filter imager.

  12. Optimized focal and pupil plane masks for vortex coronagraphs on telescopes with obstructed apertures

    E-Print Network [OSTI]

    Ruane, Garreth J; Huby, Elsa; Mawet, Dimitri; Delacroix, Christian; Carlomagno, Brunella; Piron, Pierre; Swartzlander, Grover A

    2015-01-01

    We present methods for optimizing pupil and focal plane optical elements that improve the performance of vortex coronagraphs on telescopes with obstructed or segmented apertures. Phase-only and complex masks are designed for the entrance pupil, focal plane, and the plane of the Lyot stop. Optimal masks are obtained using both analytical and numerical methods. The latter makes use of an iterative error reduction algorithm to calculate "correcting" optics that mitigate unwanted diffraction from aperture obstructions. We analyze the achieved performance in terms of starlight suppression, contrast, off-axis image quality, and chromatic dependence. Manufacturing considerations and sensitivity to aberrations are also discussed. This work provides a path to joint optimization of multiple coronagraph planes to maximize sensitivity to exoplanets and other faint companions.

  13. Transmission of light in deep sea water at the site of the Antares neutrino telescope

    E-Print Network [OSTI]

    ANTARES collaboration

    2004-12-06

    The ANTARES neutrino telescope is a large photomultiplier array designed to detect neutrino-induced upward-going muons by their Cherenkov radiation. Understanding the absorption and scattering of light in the deep Mediterranean is fundamental to optimising the design and performance of the detector. This paper presents measurements of blue and UV light transmission at the ANTARES site taken between 1997 and 2000. The derived values for the scattering length and the angular distribution of particulate scattering were found to be highly correlated, and results are therefore presented in terms of an absorption length lambda_abs and an effective scattering length lambda_sct^eff. The values for blue (UV) light are found to be lambda_abs ~ 60(26) m, lambda_sct^eff ~ 265(122) m, with significant (15%) time variability. Finally, the results of ANTARES simulations showing the effect of these water properties on the anticipated performance of the detector are presented.

  14. Measurement of atmospheric neutrino oscillations with very large volume neutrino telescopes

    E-Print Network [OSTI]

    J. P. Yańez; A. Kouchner

    2015-09-28

    Neutrino oscillations have been probed during the last few decades using multiple neutrino sources and experimental set-ups. In the recent years, very large volume neutrino telescopes have started contributing to the field. First ANTARES and then IceCube have relied on large and sparsely instrumented volumes to observe atmospheric neutrinos for combinations of baselines and energies inaccessible to other experiments. Using this advantage, the latest result from IceCube starts approaching the precision of other established technologies, and is paving the way for future detectors, such as ORCA and PINGU. These new projects seek to provide better measurements of neutrino oscillation parameters, and eventually determine the neutrino mass ordering. The results from running experiments and the potential from proposed projects are discussed in this review, emphasizing the experimental challenges involved in the measurements.

  15. Measurement of atmospheric neutrino oscillations with very large volume neutrino telescopes

    E-Print Network [OSTI]

    Yańez, J P

    2015-01-01

    Neutrino oscillations have been probed during the last few decades using multiple neutrino sources and experimental set-ups. In the recent years, very large volume neutrino telescopes have started contributing to the field. First ANTARES and then IceCube have relied on large and sparsely instrumented volumes to observe atmospheric neutrinos for combinations of baselines and energies inaccessible to other experiments. Using this advantage, the latest result from IceCube starts approaching the precision of other established technologies, and is paving the way for future detectors, such as ORCA and PINGU. These new projects seek to provide better measurements of neutrino oscillation parameters, and eventually determine the neutrino mass ordering. The results from running experiments and the potential from proposed projects are discussed in this review, emphasizing the experimental challenges involved in the measurements.

  16. Enabling a High Throughput Real Time Data Pipeline for a Large Radio Telescope Array with GPUs

    E-Print Network [OSTI]

    Edgar, R G; Dale, K; Mitchell, D A; Ord, S M; Wayth, R B; Pfister, H; Greenhill, L J

    2010-01-01

    The Murchison Widefield Array (MWA) is a next-generation radio telescope currently under construction in the remote Western Australia Outback. Raw data will be generated continuously at 5GiB/sec. This high throughput motivates the development of on-site, real time processing and reduction in preference to archiving, transport and off-line processing. Maintaining real time operation will require a sustained performance of around 2.5TFLOP/sec (including convolutions, FFTs, interpolations and matrix multiplications). We describe a scalable heterogeneous computing pipeline implementation, exploiting both the high computing density and FLOP-per-Watt ratio of modern GPUs. The architecture is highly parallel within and across nodes, with all major processing elements performed by GPUs. Necessary scatter-gather operations along the pipeline are loosely synchronized and implemented in MPI. The MWA will be a frontier scientific instrument and a pathfinder for planned peta- and exascale facilities.

  17. Simulations of GRB detections with the ECLAIRs telescope onboard the future SVOM mission

    E-Print Network [OSTI]

    S. Antier; S. Schanne; B. Cordier; A. Gros; D. Götz; C. Lachaud

    2015-08-22

    The soft gamma-ray telescope ECLAIRs with its Scientific Trigger Unit is in charge of detecting Gamma-Ray Bursts (GRBs) on-board the future SVOM satellite. Using the "scientific software model" (SSM), we study the efficiency of both implemented trigger algorithms, the Count-Rate Trigger for time-scales below 20s and the Image Trigger for larger ones. The SMM provides a simulation of ECLAIRs with photon projection through the coded-mask onto the detection plane. We developed an input GRB database for the SSM based on GRBs light curves detected by the Fermi GBM instrument. We extrapolated the GRB spectra into the ECLAIRs band (4-120 keV) and projected them onto the detection plane, superimposed with cosmic extragalactic background photons (CXB). Several simulations were performed by varying the GRB properties (fluxes and positions in the field of view). We present first results of this study in this paper.

  18. Time calibration with atmospheric muon tracks in the ANTARES neutrino telescope

    E-Print Network [OSTI]

    Adrián-Martínez, S; André, M; Anton, G; Ardid, M; Aubert, J -J; Baret, B; Barrios-Martí, J; Basa, S; Bertin, V; Biagi, S; Bogazzi, C; Bormuth, R; Bou-Cabo, M; Bouwhuis, M C; Bruijn, R; Brunner, J; Busto, J; Capone, A; Caramete, L; Carr, J; Chiarusi, T; Circella, M; Coniglione, R; Costantini, H; Coyle, P; Creusot, A; Dekeyser, I; Deschamps, A; De Bonis, G; Distefano, C; Donzaud, C; Dornic, D; Drouhin, D; Dumas, A; Eberl, T; Elsässer, D; Enzenhöfer, A; Fehn, K; Felis, I; Fermani, P; Flaminio, V; Folger, F; Fusco, L A; Galatŕ, S; Gay, P; Geißelsöder, S; Geyer, K; Giordano, V; Gleixner, A; Gracia-Ruiz, R; Gómez-González, J P; Graf, K; van Haren, H; Heijboer, A J; Hello, Y; Hernández-Rey, J J; Herrero, A; Hößl, J; Hofestädt, J; Hugon, C; James, C W; de Jong, M; Kadler, M; Kalekin, O; Katz, U; Kießling, D; Kooijman, P; Kouchner, A; Kreykenbohm, I; Kulikovskiy, V; Lahmann, R; Lambard, G; Lattuada, D; Lefčvre, D; Leonora, E; Loucatos, S; Mangano, S; Marcelin, M; Margiotta, A; Marinelli, A; Martínez-Mora, J A; Martini, S; Mathieu, A; Michael, T; Migliozzi, P; Moussa, A; Mueller, C; Neff, M; Nezri, E; P?v?la?, G E; Pellegrino, C; Perrina, C; Piattelli, P; Popa, V; Pradier, T; Racca, C; Riccobene, G; Richter, R; Roensch, K; Rostovtsev, A; Saldańa, M; Samtleben, D F E; Sánchez-Losa, A; Sanguineti, M; Sapienza, P; Schmid, J; Schnabel, J; Schulte, S; Schüssler, F; Seitz, T; Sieger, C; Spurio, M; Steijger, J J M; Stolarczyk, Th; Taiuti, M; Tamburini, C; Trovato, A; Tselengidou, M; Tönnis, C; Turpin, D; Vallage, B; Vallée, C; Van Elewyck, V; Visser, E; Vivolo, D; Wagner, S; Wilms, J; Zornoza, J D; Zúńiga, J

    2015-01-01

    The ANTARES experiment consists of an array of photomultipliers distributed along 12 lines and located deep underwater in the Mediterranean Sea. It searches for astrophysical neutrinos collecting the Cherenkov light induced by the charged particles, mainly muons, produced in neutrino interactions around the detector. Since at energies of $\\sim$10 TeV the muon and the incident neutrino are almost collinear, it is possible to use the ANTARES detector as a neutrino telescope and identify a source of neutrinos in the sky starting from a precise reconstruction of the muon trajectory. To get this result, the arrival times of the Cherenkov photons must be accurately measured. A to perform time calibrations with the precision required to have optimal performances of the instrument is described. The reconstructed tracks of the atmospheric muons in the ANTARES detector are used to determine the relative time offsets between photomultipliers. Currently, this method is used to obtain the time calibration constants for ph...

  19. Simulations of GRB detections with the ECLAIRs telescope onboard the future SVOM mission

    E-Print Network [OSTI]

    Antier, S; Cordier, B; Gros, A; Götz, D; Lachaud, C

    2015-01-01

    The soft gamma-ray telescope ECLAIRs with its Scientific Trigger Unit is in charge of detecting Gamma-Ray Bursts (GRBs) on-board the future SVOM satellite. Using the "scientific software model" (SSM), we study the efficiency of both implemented trigger algorithms, the Count-Rate Trigger for time-scales below 20s and the Image Trigger for larger ones. The SMM provides a simulation of ECLAIRs with photon projection through the coded-mask onto the detection plane. We developed an input GRB database for the SSM based on GRBs light curves detected by the Fermi GBM instrument. We extrapolated the GRB spectra into the ECLAIRs band (4-120 keV) and projected them onto the detection plane, superimposed with cosmic extragalactic background photons (CXB). Several simulations were performed by varying the GRB properties (fluxes and positions in the field of view). We present first results of this study in this paper.

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

    E-Print Network [OSTI]

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

    1999-06-24

    The Milagrito water Cherenkov telescope operated for over a year. The most probable gamma-ray energy was ~1 TeV and the trigger rate was as high as 400 Hz. We have developed an efficient technique for searching the entire sky for short duration bursts of TeV photons. Such bursts may result from "traditional" gamma-ray bursts that were not in the field-of-view of any other instruments, the evaporation of primordial black holes, or some as yet undiscovered phenomenon. We have begun to search the Milagrito data set for bursts of duration 10 seconds. Here we will present the technique and the expected results. Final results will be presented at the conference.

  1. Search for Short Duration Bursts of TeV $\\gamma$ Rays with the Milagrito Telescope

    E-Print Network [OSTI]

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

    1999-01-01

    The Milagrito water Cherenkov telescope operated for over a year. The most probable gamma-ray energy was ~1 TeV and the trigger rate was as high as 400 Hz. We have developed an efficient technique for searching the entire sky for short duration bursts of TeV photons. Such bursts may result from "traditional" gamma-ray bursts that were not in the field-of-view of any other instruments, the evaporation of primordial black holes, or some as yet undiscovered phenomenon. We have begun to search the Milagrito data set for bursts of duration 10 seconds. Here we will present the technique and the expected results. Final results will be presented at the conference.

  2. New method for atmospheric calibration at the Pierre Auger Observatory using FRAM, a robotic astronomical telescope

    E-Print Network [OSTI]

    Segev BenZvi; Martina Bohacova; Brian Connolly; Jiri Grygar; Miroslav Hrabovsky; Tatiana Karova; Dusan Mandat; Petr Necesal; Dalibor Nosek; Libor Nozka; Miroslav Palatka; Miroslav Pech; Michael Prouza; Jan Ridky; Petr Schovanek; Radomir Smida; Petr Travnicek; Primo Vitale; Stefan Westerhoff; for the Pierre Auger Collaboration

    2007-06-12

    FRAM - F/(Ph)otometric Robotic Atmospheric Monitor is the latest addition to the atmospheric monitoring instruments of the Pierre Auger Observatory. An optical telescope equipped with CCD camera and photometer, it automatically observes a set of selected standard stars and a calibrated terrestrial source. Primarily, the wavelength dependence of the attenuation is derived and the comparison between its vertical values (for stars) and horizontal values (for the terrestrial source) is made. Further, the integral vertical aerosol optical depth can be obtained. A secondary program of the instrument, the detection of optical counterparts of gamma-ray bursts, has already proven successful. The hardware setup, software system, data taking procedures, and first analysis results are described in this paper.

  3. The Mid-Infrared Instrument for the James Webb Space Telescope, III: MIRIM, The MIRI Imager

    E-Print Network [OSTI]

    Bouchet, P; Lagage, P -O; Amiaux, J; Augueres, J -L; Bauwens, E; Blommaert, J A D L; Chen, C H; Detre, O H; Dicken, D; Dubreuil, D; Galdemard, Ph; Gastaud, R; Glasse, A; Gordon, K D; Gougnaud, F; Guillard, P; Justtanont, K; Krause, O; Leboeuf, D; Longval, Y; Martin, L; Mazy, E; Moreau, V; Olofsson, G; Ray, T P; Reess, J -M; Renotte, E; Ressler, M E; Ronayette, S; Salasca, S; Scheithauer, S; Sykes, J; Thelen, M P; Wells, M; Wright, D; Wright, G S

    2015-01-01

    In this article, we describe the MIRI Imager module (MIRIM), which provides broad-band imaging in the 5 - 27 microns wavelength range for the James Webb Space Telescope. The imager has a 0"11 pixel scale and a total unobstructed view of 74"x113". The remainder of its nominal 113"x113" field is occupied by the coronagraphs and the low resolution spectrometer. We present the instrument optical and mechanical design. We show that the test data, as measured during the test campaigns undertaken at CEA-Saclay, at the Rutherford Appleton Laboratory, and at the NASA Goddard Space Flight Center, indicate that the instrument complies with its design requirements and goals. We also discuss the operational requirements (multiple dithers and exposures) needed for optimal scientific utilization of the MIRIM.

  4. CONFRONTING THREE-DIMENSIONAL TIME-DEPENDENT JET SIMULATIONS WITH HUBBLE SPACE TELESCOPE OBSERVATIONS

    SciTech Connect (OSTI)

    Staff, Jan E.; Niebergal, Brian P.; Ouyed, Rachid; Pudritz, Ralph E.; Cai, Kai

    2010-10-20

    We perform state-of-the-art, three-dimensional, time-dependent simulations of magnetized disk winds, carried out to simulation scales of 60 AU, in order to confront optical Hubble Space Telescope observations of protostellar jets. We 'observe' the optical forbidden line emission produced by shocks within our simulated jets and compare these with actual observations. Our simulations reproduce the rich structure of time-varying jets, including jet rotation far from the source, an inner (up to 400 km s{sup -1}) and outer (less than 100 km s{sup -1}) component of the jet, and jet widths of up to 20 AU in agreement with observed jets. These simulations when compared with the data are able to constrain disk wind models. In particular, models featuring a disk magnetic field with a modest radial spatial variation across the disk are favored.

  5. Detecting extended gamma-ray emission with the next generation Cherenkov telescopes

    E-Print Network [OSTI]

    Alonso, M Fernandez; Rovero, A C

    2015-01-01

    Very high energy (VHE $>$100 GeV) gamma rays coming from blazars can produce pairs when interacting with the Extragalactic Background Light (EBL) and the Cosmic Microwave Background, generating an electromagnetic cascade. Depending on the Intergalactic Magnetic Field (IGMF) intensity, this cascade may result in an extended isotropic emission of photons around the source (halo), or in a broadening of the emission beam. The detection of these effects might lead to important constrains both on the IGMF intensity and the EBL density, quantities of great relevance in cosmological models. Using a Monte Carlo program, we simulate electromagnetic cascades for different values of the IGMF intensities and coming from a source similar to 1ES0229+200, a blazar with hard intrinsic spectrum at redshift $z=0.14$, which is an ideal distance for potentially observing the effect. We study the possible response of a generic future Cherenkov telescope using a simplified model for the sensitivity, effective area and angular resol...

  6. A Generic and Efficient E-field Parallel Imaging Correlator for Next-Generation Radio Telescopes

    E-Print Network [OSTI]

    Thyagarajan, Nithyanandan; Bowman, Judd D; Morales, Miguel F

    2015-01-01

    Modern radio telescopes are favoring densely packed array layouts consisting of large numbers of antennas ($N_\\textrm{a}\\gtrsim 1000$). Since the complexity of traditional correlators scales as $\\mathcal{O}(N_\\textrm{a}^2)$, there will be a steep cost for realizing the full imaging potential of these powerful instruments. Through our generic and efficient E-field Parallel Imaging Correlator (EPIC), we present the first software demonstration of a generalized direct imaging algorithm known as the Modular Optimal Frequency Fourier (MOFF) imager. It takes advantage of the multiplication-convolution theorem of Fourier transforms. Not only does it bring down the cost for dense layouts to $\\mathcal{O}(N_\\textrm{a}\\log_2 N_\\textrm{a})$ but can also image from irregularly arranged heterogeneous antenna arrays. EPIC is highly modular and parallelizable, implemented in object oriented Python, and publicly available. We have verified the images produced to be equivalent to those produced using traditional techniques. We...

  7. A New Approach to Space Situational Awareness using Small Ground-Based Telescopes

    SciTech Connect (OSTI)

    Anheier, Norman C.; Chen, Cliff S.

    2014-12-01

    This report discusses a new SSA approach evaluated by Pacific Northwest National Laboratory (PNNL) that may lead to highly scalable, small telescope observing stations designed to help manage the growing space surveillance burden. Using the methods and observing tools described in this report, the team was able to acquire and track very faint satellites (near Pluto’s apparent brightness). Photometric data was collected and used to correlate object orbital position as a function of atomic clock-derived time. Object apparent brightness was estimated by image analysis and nearby star calibration. The measurement performance was only limited by weather conditions, object brightness, and the sky glow at the observation site. In the future, these new SSA technologies and techniques may be utilized to protect satellite assets, detect and monitor orbiting debris fields, and support Outer Space Treaty monitoring and transparency.

  8. Fermi large area telescope observations of blazar 3C 279 occultations by the sun

    SciTech Connect (OSTI)

    Barbiellini, G.; Bastieri, D.; Buson, S.; Bechtol, K.; Blandford, R. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Chiang, J.; Bellazzini, R.; Bregeon, J.; Bruel, P.; Caraveo, P. A.; Cavazzuti, E.; Ciprini, S.; Cecchi, C.; Chaves, R. C. G.; Cheung, C. C. E-mail: phdmitry@stanford.edu; and others

    2014-04-01

    Observations of occultations of bright ?-ray sources by the Sun may reveal predicted pair halos around blazars and/or new physics, such as, e.g., hypothetical light dark matter particles—axions. We use Fermi Gamma-Ray Space Telescope (Fermi) data to analyze four occultations of blazar 3C 279 by the Sun on October 8 each year from 2008 to 2011. A combined analysis of the observations of these occultations allows a point-like source at the position of 3C 279 to be detected with significance of ?3?, but does not reveal any significant excess over the flux expected from the quiescent Sun. The likelihood ratio test rules out complete transparency of the Sun to the blazar ?-ray emission at a 3? confidence level.

  9. The Environments of Supernovae in Post-Refurbishment Hubble Space Telescope Images

    E-Print Network [OSTI]

    Van Dyk, S D; Barth, A J; Filippenko, A V

    1999-01-01

    The locations of supernovae in the local stellar and gaseous environment in galaxies contain important clues to their progenitor stars. Access to this information, however, has been hampered by the limited resolution achieved by ground-based observations. High spatial resolution Hubble Space Telescope (HST) images of galaxy fields in which supernovae had been observed can improve the situation considerably. We have examined the immediate environments of a few dozen supernovae using archival post-refurbishment HST images. Although our analysis is limited due to signal-to-noise ratio and filter bandpass considerations, the images allow us for the first time to resolve individual stars in, and to derive detailed color-magnitude diagrams for, several environments. We are able to place more rigorous constraints on the masses of these supernovae. A search was made for late-time emission from supernovae in the archival images, and for the progenitor stars in presupernova images of the host galaxies. We have detected...

  10. Detection of ultra-high energy cosmic ray showers with a single-pixel fluorescence telescope

    E-Print Network [OSTI]

    Fujii, T; Bertaina, M; Casolino, M; Dawson, B; Horvath, P; Hrabovsky, M; Jiang, J; Mandat, D; Matalon, A; Matthews, J N; Motloch, P; Palatka, M; Pech, M; Privitera, P; Schovanek, P; Takizawa, Y; Thomas, S B; Travnicek, P; Yamazaki, K

    2015-01-01

    We present a concept for large-area, low-cost detection of ultra-high energy cosmic rays (UHECRs) with a Fluorescence detector Array of Single-pixel Tele- scopes (FAST), addressing the requirements for the next generation of UHECR experiments. In the FAST design, a large field of view is covered by a few pixels at the focal plane of a mirror or Fresnel lens. We report first results of a FAST prototype installed at the Telescope Array site, consisting of a single 200 mm photomultiplier tube at the focal plane of a 1 m2 Fresnel lens system taken from the prototype of the JEM-EUSO experiment. The FAST prototype took data for 19 nights, demonstrating remarkable operational stability. We detected laser shots at distances of several kilometres as well as 16 highly significant UHECR shower candidates.

  11. Direct measurement of the size of 2003 UB313 from the Hubble Space Telescope

    E-Print Network [OSTI]

    M. E. Brown; E. L. Schaller; H. G. Roe; D. L. Rabinowitz; C. A. Trujillo

    2006-04-11

    We have used the Hubble Space Telescope to directly measure the angular size of the large Kuiper belt object 2003 UB313. By carefully calibrating the point spread function of a nearby field star, we measure the size of 2003 UB313 to be 34.3$\\pm$1.4 milliarcseconds, corresponding to a diameter of 2400$\\pm$100 km or a size $\\sim5$% larger than Pluto. The V band geometric albedo of 2003 UB313 is $86\\pm7$%. The extremely high albedo is consistent with the frosty methane spectrum, the lack of red coloring, and the lack of observed photometric variation on the surface of 2003 UB313. Methane photolysis should quickly darken the surface of 2003 UB313, but continuous evaporation and redeposition of surface ices appears capable of maintaining the extreme alebdo of this body.

  12. Simulating the High Energy Gamma-ray sky seen by the GLAST Large Area Telescope

    E-Print Network [OSTI]

    F. Longo; P. Azzi; D. Bastieri; G. Busetto; Y. Lei; R. Rando; O. Tibolla; L. Baldini; M. Kuss; L. Latronico; N. Omodei; M. Razzano; G. Spandre; P. Boinee; A. De Angelis; M. Frailis; M. Brigida; F. Gargano; N. Giglietto; F. Loparco; M. N. Mazziotta; C. Cecchi; P. Lubrano; F. Marcucci; M. Pepe; G. Tosti; A. Lionetto; A. Morselli; C. Pittori

    2005-03-24

    This paper presents the simulation of the GLAST high energy gamma-ray telescope. The simulation package, written in C++, is based on the Geant4 toolkit, and it is integrated into a general framework used to process events. A detailed simulation of the electronic signals inside Silicon detectors has been provided and it is used for the particle tracking, which is handled by a dedicated software. A unique repository for the geometrical description of the detector has been realized using the XML language and a C++ library to access this information has been designed and implemented. A new event display based on the HepRep protocol was implemented. The full simulation was used to simulate a full week of GLAST high energy gamma-ray observations. This paper outlines the contribution developed by the Italian GLAST software group.

  13. The First Swift Ultra-Violet/Optical Telescope GRB Afterglow Catalog

    E-Print Network [OSTI]

    P. W. A. Roming; T. S. Koch; S. R. Oates; B. L. Porterfield; D. E. Vanden Berk; P. T. Boyd; S. T. Holland; E. A. Hoversten; S. Immler; F. E. Marshall; M. J. Page; J. L. Racusin; D. P. Schneider; A. A. Breeveld; P. J. Brown; M. M. Chester; A. Cucchiara; M. De Pasquale; C. Gronwall; S. D. Hunsberger; N. P. M. Kuin; W. B. Landsman; P. Schady; M. Still

    2008-09-24

    We present the first Swift Ultra-Violet/Optical Telescope (UVOT) gamma-ray burst (GRB) afterglow catalog. The catalog contains data from over 64,000 independent UVOT image observations of 229 GRBs first detected by Swift, the High Energy Transient Explorer 2 (HETE2), the INTErnational Gamma-Ray Astrophysics Laboratory (INTEGRAL), and the Interplanetary Network (IPN). The catalog covers GRBs occurring during the period from 2005 Jan 17 to 2007 Jun 16 and includes ~86% of the bursts detected by the Swift Burst Alert Telescope (BAT). The catalog provides detailed burst positional, temporal, and photometric information extracted from each of the UVOT images. Positions for bursts detected at the 3-sigma-level are provided with a nominal accuracy, relative to the USNO-B1 catalog, of ~0.25 arcseconds. Photometry for each burst is given in three UV bands, three optical bands, and a 'white' or open filter. Upper limits for magnitudes are reported for sources detected below 3-sigma. General properties of the burst sample and light curves, including the filter-dependent temporal slopes, are also provided. The majority of the UVOT light curves, for bursts detected at the 3-sigma-level, can be fit by a single power-law, with a median temporal slope (alpha) of 0.96, beginning several hundred seconds after the burst trigger and ending at ~1x10^5 s. The median UVOT v-band (~5500 Angstroms) magnitude at 2000 s for a sample of "well" detected bursts is 18.02. The UVOT flux interpolated to 2000 s after the burst, shows relatively strong correlations with both the prompt Swift BAT fluence, and the Swift X-ray flux at 11 hours after the trigger.

  14. Concept study and validation of Antarctic telescope tower SPIE vol. 6268, Advances in Stellar Interferometry, paper 41, 2006

    E-Print Network [OSTI]

    Rutten, Rob

    project surveyed relevant tower design approaches, then generated and evaluated six concept designs for telescope towers. Using data for typical and extreme wind at Dome C to generate wind loads, finite element analysis yielded lateral deflections at the top of 0.3 mm for typical winds and 12.1 mm for extreme gusts

  15. MACHETE: A transit Imaging Atmospheric Cherenkov Telescope to survey half of the Very High Energy $\\gamma$-ray sky

    E-Print Network [OSTI]

    Cortina, J; Moralejo, A

    2015-01-01

    Current Imaging Atmospheric Cherenkov Telescopes for Very High Energy $\\gamma$-ray astrophysics are pointing instruments with a Field of View up to a few tens of sq deg. We propose to build an array of two non-steerable (drift) telescopes. Each of the telescopes would have a camera with a FOV of 5$\\times$60 sq deg oriented along the meridian. About half of the sky drifts through this FOV in a year. We have performed a Montecarlo simulation to estimate the performance of this instrument. We expect it to survey this half of the sky with an integral flux sensitivity of $\\sim$0.77\\% of the steady flux of the Crab Nebula in 5 years, an analysis energy threshold of $\\sim$150 GeV and an angular resolution of $\\sim$0.1$^{\\circ}$. For astronomical objects that transit over the telescope for a specific night, we can achieve an integral sensitivity of 12\\% of the Crab Nebula flux in a night, making it a very powerful tool to trigger further observations of variable sources using steerable IACTs or instruments at other w...

  16. A Bayesian-based Method for Particle Track Identification in Low-energy Pair-creation Telescopes

    E-Print Network [OSTI]

    California at Berkeley, University of

    .32.147.236. Redistribution subject to AIP license or copyright; see http://proceedings.aip.org/proceedings/cpcr.jsp #12;A LOW-ENERGYA Bayesian-based Method for Particle Track Identification in Low-energy Pair-creation Telescopes optimized for energies up to 50 MeV, we describe a low-energy pair event reconstruction approach partly

  17. In-Flight Performance of the Balloon-Borne High Energy Focusing Telescope C. M. Hubert Chena

    E-Print Network [OSTI]

    The High Energy Focusing Telescope (HEFT) is a balloon-borne instrument consisting of three multilayer-coated-long primary mirror, 20 cm-long secondary mirror Ż 70 mirror shells Ż Depth-graded W/Si multilayer coating encoders Ż Motor for elevation control; flywheels for yaw and roll The Flight HEFT was launched at 19

  18. Minutes of the Final Design Review of the M4 mount designed by ERIA for the 30-m telescope,

    E-Print Network [OSTI]

    Leclercq, Samuel

    from SN): - All the big parts are in aluminum, except the support frame that serves to attach the mount to the horizontal tube of the telescope, which is in steel. All the small parts (screws, bolts, etc.) are also on the circular support that allow to adjust the orientation of the mount around the vertical axis. This hole can

  19. Observational results of a multi-telescope campaign in search of interstellar urea [(NH{sub 2}){sub 2}CO

    SciTech Connect (OSTI)

    Remijan, Anthony J.; Snyder, Lewis E.; Kuo, Hsin-Lun; Looney, Leslie W.; Friedel, Douglas N.; McGuire, Brett A.; Golubiatnikov, G. Yu; Lovas, Frank J.; Ilyushin, V. V.; Alekseev, E. A.; Dyubko, S. F.; McCall, Benjamin J.; Hollis, Jan M.

    2014-03-10

    In this paper, we present the results of an observational search for gas phase urea [(NH{sub 2}){sub 2}CO] observed toward the Sgr B2(N-LMH) region. We show data covering urea transitions from ?100 GHz to 250 GHz from five different observational facilities: the Berkeley-Illinois-Maryland-Association (BIMA) Array, the Combined Array for Research in Millimeter-wave Astronomy (CARMA), the NRAO 12 m telescope, the IRAM 30 m telescope, and the Swedish-ESO Submillimeter Telescope (SEST). The results show that the features ascribed to urea can be reproduced across the entire observed bandwidth and all facilities by best-fit column density, temperature, and source size parameters which vary by less than a factor of two between observations merely by adjusting for telescope-specific parameters. Interferometric observations show that the emission arising from these transitions is cospatial and compact, consistent with the derived source sizes and emission from a single species. Despite this evidence, the spectral complexity of both (NH{sub 2}){sub 2}CO and of Sgr B2(N) makes the definitive identification of this molecule challenging. We present observational spectra, laboratory data, and models, and discuss our results in the context of a possible molecular detection of urea.

  20. THE M31 VELOCITY VECTOR. I. HUBBLE SPACE TELESCOPE PROPER-MOTION MEASUREMENTS

    SciTech Connect (OSTI)

    Sohn, Sangmo Tony; Anderson, Jay; Van der Marel, Roeland P.

    2012-07-01

    We present the first proper-motion (PM) measurements for the galaxy M31. We obtained new V-band imaging data with the Hubble Space Telescope ACS/WFC and the WFC3/UVIS instruments of three fields: a spheroid field near the minor axis, an outer disk field along the major axis, and a field on the Giant Southern Stream. The data provide five to seven year time baselines with respect to pre-existing deep first-epoch observations of the same fields. We measure the positions of thousands of M31 stars and hundreds of compact background galaxies in each field. High accuracy and robustness is achieved by building and fitting a unique template for each individual object. The average PM for each field is obtained from the average motion of the M31 stars between the epochs with respect to the background galaxies. For the three fields, the observed PMs ({mu}{sub W}, {mu}{sub N}) are, in units of mas yr{sup -1}, (- 0.0458, -0.0376) {+-} (0.0165, 0.0154), (- 0.0533, -0.0104) {+-} (0.0246, 0.0244), and (- 0.0179, -0.0357) {+-} (0.0278, 0.0272), respectively. The ability to average over large numbers of objects and over the three fields yields a final displacement accuracy of a few thousandths of a pixel, corresponding to only 12 {mu}as yr{sup -1}. This is comparable to what has been achieved for other Local Group galaxies using Very Long Baseline Array observations of water masers. Potential systematic errors are controlled by an analysis strategy that corrects for detector charge transfer inefficiency, spatially and time-dependent geometric distortion, and point-spread function variations. The robustness of the PM measurements and uncertainties are supported by the fact that data from different instruments, taken at different times and with different telescope orientations, as well as measurements of different fields, all yield statistically consistent results. Papers II and III of this series explore the implications of the new measurements for our understanding of the history, future, and mass of the Local Group.