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1

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

E-Print Network (OSTI)

March 18, 2010 James Webb Space Telescope Studies of Dark Energy Jonathan P. Gardner (NASA. Introduction The Hubble Space Telescope (HST) has contributed significantly to studies of dark energy) was due to dark energy rather than observational or astrophysical effects such as systematic errors

Sirianni, Marco

2

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

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

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

3

THE SPITZER SPACE TELESCOPE MISSION M. W. Werner,1  

E-Print Network (OSTI)

with a cryogenic telescope in space with the great imaging and spectroscopic power of modern detector arraysTHE SPITZER SPACE TELESCOPE MISSION M. W. Werner,1 T. L. Roellig,2 F. J. Low,3 G. H. Rieke,3 M2 Receivved 2004 March 26; accepted 2004 May 26 ABSTRACT The Spitzer Space Telescope, NASA's Great

Galis, Frietson

4

Very Large Aperture Diffractive Space Telescope  

DOE Patents (OSTI)

A very large (10's of meters) aperture space telescope including two separate spacecraft--an optical primary 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 magnifying glass 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 magnifying glass, 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.

Hyde, Roderick Allen

1998-04-20T23:59:59.000Z

5

A Short and Personal History of the Spitzer Space Telescope  

E-Print Network (OSTI)

The Spitzer Space Telescope, born as the Shuttle Infrared Telescope Facility (SIRTF) and later the Space Infrared Telescope Facility (still SIRTF), was under discussion and development within NASA and the scientific community for more than 30 years prior to its launch in 2003. This brief history chronicles a few of the highlights and the lowlights of those 30 years from the authors personal perspective. A much more comprehensive history of SIRTF/Spitzer has been written by George Rieke (2006).

Michael Werner

2005-03-29T23:59:59.000Z

6

The Space Infrared Interferometric Telescope (SPIRIT): High-resolution imaging and spectroscopy in the far-infrared  

E-Print Network (OSTI)

We report results of a recently-completed pre-Formulation Phase study of SPIRIT, a candidate NASA Origins Probe mission. SPIRIT is a spatial and spectral interferometer with an operating wavelength range 25 - 400 microns. SPIRIT will provide sub-arcsecond resolution images and spectra with resolution R = 3000 in a 1 arcmin field of view to accomplish three primary scientific objectives: (1) Learn how planetary systems form from protostellar disks, and how they acquire their inhomogeneous composition; (2) characterize the family of extrasolar planetary systems by imaging the structure in debris disks to understand how and where planets of different types form; and (3) learn how high-redshift galaxies formed and merged to form the present-day population of galaxies. Observations with SPIRIT will be complementary to those of the James Webb Space Telescope and the ground-based Atacama Large Millimeter Array. All three observatories could be operational contemporaneously.

David Leisawitz; Charles Baker; Amy Barger; Dominic Benford; Andrew Blain; Rob Boyle; Richard Broderick; Jason Budinoff; John Carpenter; Richard Caverly; Phil Chen; Steve Cooley; Christine Cottingham; Julie Crooke; Dave DiPietro; Mike DiPirro; Michael Femiano; Art Ferrer; Jacqueline Fischer; Jonathan P. Gardner; Lou Hallock; Kenny Harris; Kate Hartman; Martin Harwit; Lynne Hillenbrand; Tupper Hyde; Drew Jones; Jim Kellogg; Alan Kogut; Marc Kuchner; Bill Lawson; Javier Lecha; Maria Lecha; Amy Mainzer; Jim Mannion; Anthony Martino; Paul Mason; John Mather; Gibran McDonald; Rick Mills; Lee Mundy; Stan Ollendorf; Joe Pellicciotti; Dave Quinn; Kirk Rhee; Stephen Rinehart; Tim Sauerwine; Robert Silverberg; Terry Smith; Gordon Stacey; H. Philip Stahl; Johannes Staguhn; Steve Tompkins; June Tveekrem; Sheila Wall; Mark Wilson

2007-07-05T23:59:59.000Z

7

Hubble space telescope; A new window opens on the universe  

Science Conference Proceedings (OSTI)

This paper reports on the Hubble space telescope. The telescope is expected to help answer key questions in astronomy, astrophysics, and cosmology, such as how stars and galaxies form and evolve; the size and age of the universe; the nature of quasars, black holes, and other exotic objects; the characteristics of planets in our solar system; and evidence for existence of planets orbiting other stars.

Seltzer, R.J. (C and EN, Washington, DC (US))

1990-04-09T23:59:59.000Z

8

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

SciTech Connect

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

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

2009-05-15T23:59:59.000Z

9

HUBBLE SPACE TELESCOPE OBSERVATIONS OF THE HD 202628 DEBRIS DISK  

SciTech Connect

A ring-shaped debris disk around the G2V star HD 202628 (d = 24.4 pc) was imaged in scattered light at visible wavelengths using the coronagraphic mode of the Space Telescope Imaging Spectrograph on the Hubble Space Telescope. The ring is inclined by {approx}64 Degree-Sign from face-on, based on the apparent major/minor axis ratio, with the major axis aligned along P.A. = 130 Degree-Sign . It has inner and outer radii (>50% maximum surface brightness) of 139 AU and 193 AU in the northwest ansae and 161 AU and 223 AU in the southeast ({Delta}r/r Almost-Equal-To 0.4). The maximum visible radial extent is {approx}254 AU. With mean surface brightness of V Almost-Equal-To 24 mag arcsec{sup -2}, this is the faintest debris disk observed to date in reflected light. The center of the ring appears offset from the star by {approx}28 AU (deprojected). An ellipse fit to the inner edge has an eccentricity of 0.18 and a = 158 AU. This offset, along with the relatively sharp inner edge of the ring, suggests the influence of a planetary-mass companion. There is a strong similarity with the debris ring around Fomalhaut, though HD 202628 is a more mature star with an estimated age of about 2 Gyr. We also provide surface brightness limits for nine other stars in our study with strong Spitzer excesses around which no debris disks were detected in scattered light (HD 377, HD 7590, HD 38858, HD 45184, HD 73350, HD 135599, HD 145229, HD 187897, and HD 201219).

Krist, John E.; Bryden, Geoffrey [Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109 (United States); Stapelfeldt, Karl R. [Laboratory for Exoplanets and Stellar Astrophysics, Code 667, NASA Goddard Space Flight Center, Greenbelt, MD 20771 (United States); Plavchan, Peter [NASA Exoplanet Science Institute, California Institute of Technology, 770 S Wilson Ave., Pasadena, CA 91125 (United States)

2012-08-15T23:59:59.000Z

10

HUBBLE SPACE TELESCOPE PHOTOMETRY OF GLOBULAR CLUSTERS IN M81  

SciTech Connect

We perform aperture photometry and profile fitting on 419 globular cluster (GC) candidates with m{sub V} {<=} 23 mag identified in Hubble Space Telescope/Advanced Camera for Surveys BVI imaging, and estimate the effective radii of the clusters. We identify 85 previously known spectroscopically confirmed clusters, and newly identify 136 objects as good cluster candidates within the 3{sigma} color and size ranges defined by the spectroscopically confirmed clusters, yielding a total of 221 probable GCs. The luminosity function peak for the 221 probable GCs with estimated total dereddening applied is V {approx} (20.26 {+-} 0.13) mag, corresponding to a distance of {approx}3.7 {+-} 0.3 Mpc. The blue and red GC candidates, and the metal-rich and metal-poor spectroscopically confirmed clusters, respectively, are similar in half-light radius. Red confirmed clusters are about 6% larger in median half-light radius than blue confirmed clusters, and red and blue good GC candidates are nearly identical in half-light radius. The total population of confirmed and 'good' candidates shows an increase in half-light radius as a function of galactocentric distance.

Nantais, Julie B. [Departamento de Astronomia, Universidad de Concepcion Av. Esteban Iturra s/n Barrio Universitario Casilla 160-C Concepcion (Chile); Huchra, John P.; Zezas, Andreas; Gazeas, Kosmas; Strader, Jay [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States)

2011-12-15T23:59:59.000Z

11

HUBBLE SPACE TELESCOPE IMAGING OF POST-STARBURST QUASARS  

Science Conference Proceedings (OSTI)

We present images of 29 post-starburst quasars (PSQs) from a Hubble Space Telescope (HST) Advanced Camera for Surveys (ACS) Wide Field Channel Snapshot program. These broadlined active galactic nuclei (AGNs) possess the spectral signatures of massive (M{sub burst} {approx} 10{sup 10} M{sub sun}), moderate-aged stellar populations (hundreds of Myr). Thus, their composite nature provides insight into the AGN-starburst connection. We measure quasar-to-host galaxy light contributions via semi-automated two-dimensional light profile fits of point-spread-function-subtracted images. We examine the host morphologies and model the separate bulge and disk components. The HST/ACS-F606W images reveal an equal number of spiral (13/29) and early-type (13/29) hosts, with the remaining three hosts having indeterminate classifications. AGNs hosted by early-type galaxies have on average greater luminosity than those hosted by spiral galaxies. Disturbances such as tidal tails, shells, star-forming knots, and asymmetries are seen as signposts of interaction/merger activity. Disturbances like these were found in 17 of the 29 objects and are evenly distributed among early-type and spiral galaxies. Two of these systems are clearly merging with their companions. Compared to other AGNs of similar luminosity and redshift, these PSQs have a higher fraction of early-type hosts and disturbances. Our most luminous objects with disturbed early-type host galaxies appear to be consistent with merger products. Thus, these luminous galaxies may represent a phase in an evolutionary scenario for merger-driven activity. Our less luminous objects appear to be consistent with Seyfert galaxies not requiring triggering by major mergers. Many of these Seyferts are barred spiral galaxies.

Cales, S. L.; Brotherton, M. S.; Shang Zhaohui [Department of Physics and Astronomy, University of Wyoming, Laramie, WY 82071 (United States); Bennert, Vardha Nicola [Department of Physics, University of California, Santa Barbara, CA 93106 (United States); Canalizo, G. [Department of Physics and Astronomy, University of California, Riverside, CA 92521 (United States); Stoll, R. [Department of Astronomy, Ohio State University, Columbus, OH 43210 (United States); Ganguly, R. [Department of Computer Science, Engineering, and Physics, University of Michigan-Flint, Flint, MI 48502 (United States); Vanden Berk, D. [Department of Physics, Saint Vincent College, Latrobe, PA 15650 (United States); Paul, C. [Physics Department, University of California, Davis, CA 95616 (United States); Diamond-Stanic, A., E-mail: scales@uwyo.edu, E-mail: mbrother@uwyo.edu, E-mail: shang@uwyo.edu, E-mail: bennert@physics.ucsb.edu, E-mail: gabriela.canalizo@ucr.edu, E-mail: stoll@astronomy.ohio-state.edu, E-mail: ganguly@umflint.edu, E-mail: daniel.vandenberk@email.stvincent.edu, E-mail: capaul@ucdavis.edu, E-mail: aleks@ucsd.edu [Center for Astrophysics and Space Sciences, University of California, San Diego, La Jolla, CA 92093 (United States)

2011-11-10T23:59:59.000Z

12

Experience with the Hubble Space Telescope: 20 years of an archetype  

E-Print Network (OSTI)

The Hubble Space Telescope's mission is summarized, with special emphasis placed on the Space Telescope Science Institute's unique experience with Hubble's behavior as an astronomical telescope in the environment of low earth orbit for over two decades. Historical context and background are given, and the project's early scientific expectations are described. A general overview of the spacecraft is followed by a more detailed look at the optical design, both as intended and as built. Basic characteristics of the complete complement of science instruments are also summarized. Experience with the telescope on-orbit is reviewed, starting with the major initial problems, solutions, human servicing missions, and the associated expansion of the observatory's capabilities over this time. Specific attention is then given to understanding Hubble's optical quality and pointing/jitter performance, two fundamental characteristics of a telescope. Experience with-and the important mitigation of-radiation damage and contami...

Lallo, Matthew

2012-01-01T23:59:59.000Z

13

Fundamental physics in space with the Fermi Gamma-ray Space Telescope  

E-Print Network (OSTI)

Successfully launched in June 2008, the Fermi Gamma-ray Space Telescope, formerly named GLAST, has been observing the high-energy gamma-ray sky with unprecedented sensitivity for more than two years, opening a new window on a wide variety of exotic astrophysical objects. This paper is a short overview of the main science highlights, aimed at non-specialists, with emphasis on those which are more directly connected with the study of fundamental physics---particularly the search for signals of new physics in the diffuse gamma-ray emission and in the cosmic radiation and the study of Gamma-Ray Burst as laboratories for testing possible violations of the Lorentz invariance.

Luca Baldini for the Fermi LAT Collaboration

2011-01-09T23:59:59.000Z

14

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

E-Print Network (OSTI)

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

Van Stryland, Eric

15

The Honorable Wellington E. Webb  

Office of Legacy Management (LM)

' ' , i Department of Energy Washington, DC 20585 ,, ,' ,, FEB 1 6 i& ;. .I I. ,' . ., i The Honorable Wellington E. Webb 350, City-County Building Denver, Colorado 8D202 ,' I ,..' ., .' Dear Mayors Webb: , : Secretary of Energy,Hazel O'Leary has announced anew approach to openness in the Department-of ,Energy '(DOE)',and -its communications with the public. In support of this initiative, we are pleased to forward~the enclosed information, related to the former Denver:Equipment Co..in your jurisdiction that performed, work for DOE's predecessor agencies. ..This' information' is provided for'your 1 : information,>use? and retention. DOE's Formerly Utilized Sites Remedial Action .Program is respons'tble for identificationof sites used by/DOE's predecessor agencies, determining.their

16

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)

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.

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

1992-01-01T23:59:59.000Z

17

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)

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.

Norbert, M.A.; Yale, O.

1992-04-28T23:59:59.000Z

18

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

DOE Green Energy (OSTI)

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

Ketchum, Christina; /SLAC

2006-09-01T23:59:59.000Z

19

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

E-Print Network (OSTI)

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

Baldesarra, Mark

2007-01-01T23:59:59.000Z

20

Discovery and Characterization of Transiting Super Earths Using an All-Sky Transit Survey and Follow-up by the James Webb Space Telescope  

E-Print Network (OSTI)

Doppler and transit surveys are finding extrasolar planets of ever smaller mass and radius, and are now sampling the domain of super Earths (1–3R?). Recent results from the Doppler surveys suggest that discovery of a ...

Seager, Sara

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


21

Hubble Space Telescope Imaging of the Young Planetary Nebula GL 618  

E-Print Network (OSTI)

We present narrow-band Hubble Space Telescope images of the young planetary nebula GL 618. These images have allowed us to study the detailed morphology of shock-excited emission present in the bipolar lobes of this object. These images reveal the presence of three highly collimated outflows emanating from the central regions of GL 618. We discuss the significance of the detection of these outflows and the possible origins of these features.

Susan R. Trammell

2000-01-10T23:59:59.000Z

22

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

SciTech Connect

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.

Grenier, Isabelle (University Paris Diderot and CEA Saclay, France)

2009-04-01T23:59:59.000Z

23

NEW HUBBLE SPACE TELESCOPE OBSERVATIONS OF HEAVY ELEMENTS IN FOUR METAL-POOR STARS  

Science Conference Proceedings (OSTI)

Elements heavier than the iron group are found in nearly all halo stars. A substantial number of these elements, key to understanding neutron-capture nucleosynthesis mechanisms, can only be detected in the near-ultraviolet. We report the results of an observing campaign using the Space Telescope Imaging Spectrograph on board the Hubble Space Telescope to study the detailed heavy-element abundance patterns in four metal-poor stars. We derive abundances or upper limits from 27 absorption lines of 15 elements produced by neutron-capture reactions, including seven elements (germanium, cadmium, tellurium, lutetium, osmium, platinum, and gold) that can only be detected in the near-ultraviolet. We also examine 202 heavy-element absorption lines in ground-based optical spectra obtained with the Magellan Inamori Kyocera Echelle Spectrograph on the Magellan-Clay Telescope at Las Campanas Observatory and the High Resolution Echelle Spectrometer on the Keck I Telescope on Mauna Kea. We have detected up to 34 elements heavier than zinc. The bulk of the heavy elements in these four stars are produced by r-process nucleosynthesis. These observations affirm earlier results suggesting that the tellurium found in metal-poor halo stars with moderate amounts of r-process material scales with the rare earth and third r-process peak elements. Cadmium often follows the abundances of the neighboring elements palladium and silver. We identify several sources of systematic uncertainty that must be considered when comparing these abundances with theoretical predictions. We also present new isotope shift and hyperfine structure component patterns for Lu II and Pb I lines of astrophysical interest.

Roederer, Ian U.; Thompson, Ian B. [Carnegie Observatories, Pasadena, CA 91101 (United States); Lawler, James E. [Department of Physics, University of Wisconsin, Madison, WI 53706 (United States); Sobeck, Jennifer S. [Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637 (United States); Beers, Timothy C. [National Optical Astronomy Observatory, Tucson, AZ 85719 (United States); Cowan, John J. [Homer L. Dodge Department of Physics and Astronomy, University of Oklahoma, Norman, OK 73019 (United States); Frebel, Anna [Massachusetts Institute of Technology, Kavli Institute for Astrophysics and Space Research, Cambridge, MA 02139 (United States); Ivans, Inese I. [Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112 (United States); Schatz, Hendrik [Department of Physics and Astronomy, Michigan State University, E. Lansing, MI 48824 (United States); Sneden, Christopher [Department of Astronomy, University of Texas at Austin, Austin, TX 78712 (United States)

2012-12-15T23:59:59.000Z

24

High Precision CTE-Measurement of SiC-100 for Cryogenic Space-Telescopes  

E-Print Network (OSTI)

We present the results of high precision measurements of the thermal expansion of the sintered SiC, SiC-100, intended for use in cryogenic space-telescopes, in which minimization of thermal deformation of the mirror is critical and precise information of the thermal expansion is needed for the telescope design. The temperature range of the measurements extends from room temperature down to $\\sim$ 10 K. Three samples, #1, #2, and #3 were manufactured from blocks of SiC produced in different lots. The thermal expansion of the samples was measured with a cryogenic dilatometer, consisting of a laser interferometer, a cryostat, and a mechanical cooler. The typical thermal expansion curve is presented using the 8th order polynomial of the temperature. For the three samples, the coefficients of thermal expansion (CTE), $\\bar{\\alpha}_{#1}$, $\\bar{\\alpha}_{#2}$, and $\\bar{\\alpha}_{#3}$ were derived for temperatures between 293 K and 10 K. The average and the dispersion (1 $\\sigma$ rms) of these three CTEs are 0.816 and 0.002 ($\\times 10^{-6}$/K), respectively. No significant difference was detected in the CTE of the three samples from the different lots. Neither inhomogeneity nor anisotropy of the CTE was observed. Based on the obtained CTE dispersion, we performed an finite-element-method (FEM) analysis of the thermal deformation of a 3.5 m diameter cryogenic mirror made of six SiC-100 segments. It was shown that the present CTE measurement has a sufficient accuracy well enough for the design of the 3.5 m cryogenic infrared telescope mission, the Space Infrared telescope for Cosmology and Astrophysics (SPICA).

K. Enya; N. Yamada; T. Onaka; T. Nakagawa; H. Kaneda; M. Hirabayashi; Y. Toulemont; D. Castel; Y. Kanai; N. Fujishiro

2007-04-12T23:59:59.000Z

25

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

SciTech Connect

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

Bloom, Elliott (SLAC)

2011-03-30T23:59:59.000Z

26

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

E-Print Network (OSTI)

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

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

2007-07-10T23:59:59.000Z

27

Fermi Gamma-ray Space Telescope: High-Energy Results from the First Year  

E-Print Network (OSTI)

The Fermi Gamma-ray Space Telescope (Fermi) was launched on June 11, 2008 and began its first year sky survey on August 11, 2008. The Large Area Telescope (LAT), a wide field-of-view pair-conversion telescope covering the energy range from 20 MeV to more than 300 GeV, is the primary instrument on Fermi. While this review focuses on results obtained with the LAT, the Gamma-ray Burst Monitor (GBM) complements the LAT in its observations of transient sources and is sensitive to X-rays and gamma-rays with energies between 8 keV and 40 MeV. During the first year in orbit, the Fermi LAT has observed a large number of sources that include active galaxies, pulsars, compact binaries, globular clusters, supernova remnants, as well as the Sun, the Moon and the Earth. The GBM and LAT together have uncovered surprising characteristics in the high-energy emission of gamma-ray bursts (GRBs) that have been used to set significant new limits on violations of Lorentz invariance. The Fermi LAT has also made important new measurements of the Galactic diffuse radiation and has made precise measurements of the spectrum of cosmic-ray electrons and positrons from 20 GeV to 1 TeV.

Peter F. Michelson; William B. Atwood; Steven Ritz

2010-10-31T23:59:59.000Z

28

Detection of H2 Emission from Mira B in UV Spectra from the Hubble Space Telescope  

E-Print Network (OSTI)

We present ultraviolet spectra of Mira's companion star from the Space Telescope Imaging Spectrograph (STIS) instrument on board the Hubble Space Telescope (HST). The companion is generally assumed to be a white dwarf surrounded by an accretion disk fed by Mira's wind, which dominates the UV emission from the system. The STIS UV spectrum is dominated by numerous, narrow H2 lines fluoresced by H I Ly-alpha, which were not detected in any of the numerous observations of Mira B by the International Ultraviolet Explorer (IUE). The high temperature lines detected by IUE (e.g., C IV 1550) still exist in the STIS spectrum but with dramatically lower fluxes. The continuum fluxes in the STIS spectra are also much lower, being more than an order of magnitude lower than ever observed by IUE, and also an order of magnitude lower than fluxes observed in more recent HST Faint Object Camera objective prism spectra from 1995. Thus, the accretion rate onto Mira B was apparently much lower when STIS observed the star, and this change altered the character of Mira B's UV spectrum.

Brian E. Wood; Margarita Karovska; Warren Hack

2001-07-02T23:59:59.000Z

29

An Efficient Strategy to Select Targets for Gas-Dynamical Measurements of Black Hole Masses Using the Hubble Space Telescope  

E-Print Network (OSTI)

Gas-dynamical studies using the Hubble Space Telescope are an integral component for future progress in the search for massive black holes in galactic nuclei. Here we present an extensive set of gas rotation curves obtained with the Space Telescope Imaging Spectrograph for the central regions of 23 disk galaxies. We find that the bulges of randomly selected, nearby spiral and S0 galaxies generally do not contain well-defined gaseous disks. Only 15%-20% of disk galaxies have regular, symmetric velocity fields useful for dynamical analysis. Through comparison of the kinematics with Hubble Space Telescope images of the nuclear regions, we show that the probability of success can be significantly boosted by preselecting objects whose central dust lanes follow a well-ordered, circularly symmetric pattern. The dust morphology can be ascertained efficiently by visual inspection of unsharp-masked images.

Luis C. Ho; Marc Sarzi; Hans-Walter Rix; Joseph C. Shields; Greg Rudnick; Alexei V. Filippenko; Aaron J. Barth

2001-10-30T23:59:59.000Z

30

An Efficient Strategy to Select Targets for Gas-Dynamical Measurements of Black Hole Masses Using the Hubble Space Telescope  

E-Print Network (OSTI)

Gas-dynamical studies using the Hubble Space Telescope are an integral component for future progress in the search for massive black holes in galactic nuclei. Here we present an extensive set of gas rotation curves obtained with the Space Telescope Imaging Spectrograph for the central regions of 23 disk galaxies. We find that the bulges of randomly selected, nearby spiral and S0 galaxies generally do not contain well-defined gaseous disks. Only 15%-20% of disk galaxies have regular, symmetric velocity fields useful for dynamical analysis. Through comparison of the kinematics with Hubble Space Telescope images of the nuclear regions, we show that the probability of success can be significantly boosted by preselecting objects whose central dust lanes follow a well-ordered, circularly symmetric pattern. The dust morphology can be ascertained efficiently by visual inspection of unsharp-masked images.

Ho, L C; Rix, H W; Shields, J C; Rudnick, G; Filippenko, A V; Barth, A J; Ho, Luis C.; Sarzi, Marc; Rix, Hans-Walter; Shields, Joseph C.; Rudnick, Greg; Filippenko, Alexei V.; Barth, Aaron J.

2001-01-01T23:59:59.000Z

31

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

E-Print Network (OSTI)

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

Enya, Keigo; Kaneda, Hidehiro; Onaka, Takashi; Ozaki, Tuyoshi; Kume, Masami

2007-01-01T23:59:59.000Z

32

The Beginning of the End: Hubble Space Telescope Images of Seyfert's Sextet  

E-Print Network (OSTI)

Hubble Space Telescope Wide Field Planetary Camera 2 images of Hickson Compact Group 79, Seyfert's Sextet, are presented. Both point sources and extended sources detected on the three WF chips were photometered in four filters: F336W, F439W, F555W, and F814W. Unlike other HCGs that have been imaged with HST, there do not appear to be any candidate young star clusters among the detected point sources. The majority of the point sources that may be star clusters associated with the Sextet have red colors consistent with stellar populations older than 1 Gyr. A similar conclusion is drawn with regard to the extended sources. The majority of these appear to be background galaxies, but a few candidate dwarf galaxies are identified as potentially associated with Seyfert's Sextet. However, no blue, star forming objects similar to the tidal dwarf galaxy candidates identified in other HCGs are found among the extended objects identified in this study. A redshift for one dwarf galaxy candidate was measured from a spectrum obtained with the Hobby-Eberly Telescope, and this object was found to have a redshift similar to NGC6027e, the discordant spiral formerly identified as a member of this compact group. The HST observations presented here and previous radio observations of the neutral gas content of this group suggest that the interactions that have taken place in the Sextet only redistributed the stars from the member galaxies within the group. We speculate that future interactions may be strong enough to strip the gas from NGC6027d and trigger star cluster formation.

C. Palma; S. Zonak; S. Hunsberger; J. Charlton; S. Gallagher; P. Durrell; J. English

2002-08-14T23:59:59.000Z

33

Webb, Alabama: Energy Resources | Open Energy Information  

Open Energy Info (EERE)

Webb, Alabama: Energy Resources Webb, Alabama: Energy Resources Jump to: navigation, search Equivalent URI DBpedia Coordinates 31.2604534°, -85.2732658° Loading map... {"minzoom":false,"mappingservice":"googlemaps3","type":"ROADMAP","zoom":14,"types":["ROADMAP","SATELLITE","HYBRID","TERRAIN"],"geoservice":"google","maxzoom":false,"width":"600px","height":"350px","centre":false,"title":"","label":"","icon":"","visitedicon":"","lines":[],"polygons":[],"circles":[],"rectangles":[],"copycoords":false,"static":false,"wmsoverlay":"","layers":[],"controls":["pan","zoom","type","scale","streetview"],"zoomstyle":"DEFAULT","typestyle":"DEFAULT","autoinfowindows":false,"kml":[],"gkml":[],"fusiontables":[],"resizable":false,"tilt":0,"kmlrezoom":false,"poi":true,"imageoverlays":[],"markercluster":false,"searchmarkers":"","locations":[{"text":"","title":"","link":null,"lat":31.2604534,"lon":-85.2732658,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

34

A LYMAN BREAK GALAXY IN THE EPOCH OF REIONIZATION FROM HUBBLE SPACE TELESCOPE GRISM SPECTROSCOPY  

SciTech Connect

We present observations of a luminous galaxy at z = 6.573-the end of the reionization epoch-which has been spectroscopically confirmed twice. The first spectroscopic confirmation comes from slitless Hubble Space Telescope Advanced Camera for Surveys grism spectra from the PEARS survey (Probing Evolution And Reionization Spectroscopically), which show a dramatic continuum break in the spectrum at rest frame 1216 A. The second confirmation is done with Keck + DEIMOS. The continuum is not clearly detected with ground-based spectra, but high wavelength resolution enables the Ly{alpha} emission line profile to be determined. We compare the line profile to composite line profiles at z = 4.5. The Ly{alpha} line profile shows no signature of a damping wing attenuation, confirming that the intergalactic gas is ionized at z = 6.57. Spectra of Lyman breaks at yet higher redshifts will be possible using comparably deep observations with IR-sensitive grisms, even at redshifts where Ly{alpha} is too attenuated by the neutral intergalactic medium to be detectable using traditional spectroscopy from the ground.

Rhoads, James E.; Malhotra, Sangeeta; Cohen, Seth; Zheng Zhenya [School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287 (United States); Stern, Daniel [Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109 (United States); Dickinson, Mark [National Optical Astronomy Observatory, Tucson, AZ (United States); Pirzkal, Norbert; Grogin, Norman; Koekemoer, Anton; Peth, Michael A. [Space Telescope Science Institute, Baltimore, MD (United States); Spinrad, Hyron [University of California, Berkeley, CA (United States); Reddy, Naveen [University of California, Riverside, CA (United States); Hathi, Nimish [Observatories of the Carnegie Institution of Washington, Pasadena, CA (United States); Budavari, Tamas [Johns Hopkins University, Baltimore, MD (United States); Ferreras, Ignacio [Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT (United Kingdom); Gardner, Jonathan P. [NASA Goddard Space Flight Center, Astrophysics Science Division, Observational Cosmology Laboratory, Code 665, Greenbelt, MD 20771 (United States); Gronwall, Caryl [Department of Astronomy and Astrophysics, and Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA 16802 (United States); Haiman, Zoltan [Columbia University, New York, NY (United States); Kuemmel, Martin [Universitaets-Sternwarte Muenchen, Scheinerstr. 1, D-81679 Muenchen (Germany); Meurer, Gerhardt, E-mail: James.Rhoads@asu.edu [International Centre for Radio Astronomy Research, University of Western Australia, M468, 35 Stirling Highway, Crawley, WA 6009 (Australia); and others

2013-08-10T23:59:59.000Z

35

Physical Properties of Kuiper Belt and Centaur Objects: Constraints from Spitzer Space Telescope  

E-Print Network (OSTI)

Detecting heat from minor planets in the outer solar system is challenging, yet it is the most efficient means for constraining the albedos and sizes of Kuiper Belt Objects (KBOs) and their progeny, the Centaur objects. These physical parameters are critical, e.g., for interpreting spectroscopic data, deriving densities from the masses of binary systems, and predicting occultation tracks. Here we summarize Spitzer Space Telescope observations of 47 KBOs and Centaurs at wavelengths near 24 and 70 microns. We interpret the measurements using a variation of the Standard Thermal Model (STM) to derive the physical properties (albedo and diameter) of the targets. We also summarize the results of other efforts to measure the albedos and sizes of KBOs and Centaurs. The three or four largest KBOs appear to constitute a distinct class in terms of their albedos. From our Spitzer results, we find that the geometric albedo of KBOs and Centaurs is correlated with perihelion distance (darker objects having smaller perihelia), and that the albedos of KBOs (but not Centaurs) are correlated with size (larger KBOs having higher albedos). We also find hints that albedo may be correlated with with visible color (for Centaurs). Interestingly, if the color correlation is real, redder Centaurs appear to have higher albedos. Finally, we briefly discuss the prospects for future thermal observations of these primitive outer solar system objects.

John Stansberry; Will Grundy; Mike Brown; Dale Cruikshank; John Spencer; David Trilling; Jean-Luc Margot

2007-02-20T23:59:59.000Z

36

Hubble Space Telescope Fine Guidance Sensor Parallaxes of Galactic Cepheid Variable Stars: Period-Luminosity Relations  

E-Print Network (OSTI)

(abridged) We present new absolute trigonometric parallaxes and relative proper motions for nine Galactic Cepheid variable stars: l Car, zeta Gem, beta Dor, W Sgr, X Sgr, Y Sgr, FF Aql, T Vul, and RT Aur. We obtain these results with astrometric data from Fine Guidance Sensor 1r, a white-light interferometer on Hubble Space Telescope. We find absolute parallaxes with an average sigma_pi/pi = 8%. Two stars (FF Aql and W Sgr) required the inclusion of binary astrometric perturbations, providing Cepheid mass estimates. With these parallaxes we compute absolute magnitudes in V, I, K, and Wesenheit W_{VI} bandpasses corrected for interstellar extinction and Lutz-Kelker-Hanson bias. Adding our previous absolute magnitude determination for delta Cep, we construct Period-Luminosity relations for ten Galactic Cepheids. We compare our new Period-Luminosity relations with those adopted by several recent investigations, including the Freedman and Sandage H_0 projects. Adopting our Period-Luminosity relationship would tend to increase the Sandage H_$ value, but leave the Freedman H_0 unchanged. Comparing our Galactic Cepheid PLR with those derived from LMC Cepheids, we find the slopes for K and W_{VI} identical in the two galaxies within their respective errors. Our data lead to a W_{VI} distance modulus for the Large Magellanic Cloud, m-M = 18.50\\pm0.03, uncorrected for any metallicity effects. Applying recently derived metalllcity corrections yields a corrected LMC distance modulus of (m-M)_0=18.40\\pm0.05. Comparing our Period-Luminosity relationship to solar-metallicity Cepheids in NGC 4258 results in a distance modulus, 29.28 \\pm 0.08, which agrees with that derived from maser studies.

G. Fritz Benedict; Barbara E. McArthur; Michael W. Feast; Thomas G. Barnes; Thomas E. Harrison; Richard J. Patterson; John W. Menzies; Jacob L. Bean; Wendy L. Freedman

2006-12-16T23:59:59.000Z

37

HUBBLE SPACE TELESCOPE NARROWBAND SEARCH FOR EXTENDED Ly{alpha} EMISSION AROUND TWO z > 6 QUASARS  

Science Conference Proceedings (OSTI)

We search for extended Ly{alpha} emission around two z > 6 quasars, SDSS J1030+0524 (z = 6.309) and SDSS J1148+5251 (z = 6.419) using Wide Field Camera 3 narrowband filters on board the Hubble Space Telescope. For each quasar, we collected two deep, narrowband images, one sampling the Ly{alpha} line+continuum at the quasar redshifts and one of the continuum emission redward of the line. After carefully modeling the point-spread function, we find no evidence for extended Ly{alpha} emission. These observations set 2{sigma} limits of L(Ly{alpha}, extended) rates typically inferred from (rest-frame) far-infrared measurements of z {approx} 6 quasars, these limits are well below the intrinsic bright Ly{alpha} emission expected from the recombination of gas photoionized by the quasars or by the star formation in the host galaxies, and point toward significant Ly{alpha} suppression or dust attenuation. However, small extinction values have been observed along the line of sight to the nuclei, thus reddening has to be coupled with other mechanisms for Ly{alpha} suppression (e.g., resonance scattering). No Ly{alpha} emitting companions are found, down to a 5{sigma} sensitivity of {approx}1 Multiplication-Sign 10{sup -17} erg s{sup -1} cm{sup -2} arcsec{sup -2} (surface brightness) and {approx}5 Multiplication-Sign 10{sup -17} erg s{sup -1} cm{sup -2} (assuming point sources).

Decarli, Roberto; Walter, Fabian; Yang Yujin; Hennawi, Joseph F.; Rix, Hans-Walter; Venemans, Bram P. [Max-Planck Institut fuer Astronomie, Koenigstuhl 17, D-69117 Heidelberg (Germany); Carilli, Chris L. [NRAO, Pete V. Domenici Array Science Center, P.O. Box O, Socorro, NM 87801 (United States); Fan Xiahoui [Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721 (United States); Kurk, Jaron [Max-Planck-Institut fuer Extraterrestrische Physik, Giessenbachstrasse 1, D-85748 Garching (Germany); Riechers, Dominik [Astronomy Department, Caltech, 1200 East California boulevard, Pasadena, CA 91125 (United States); Strauss, Michael A., E-mail: decarli@mpia.de [Department of Astrophysical Sciences, Princeton University, Peyton Hall, Ivy Lane, Princeton, NJ 08544 (United States)

2012-09-10T23:59:59.000Z

38

INFRARED SPECTROSCOPY OF COMET 73P/SCHWASSMANN-WACHMANN 3 USING THE SPITZER SPACE TELESCOPE  

Science Conference Proceedings (OSTI)

We have used the Spitzer Space Telescope Infrared Spectrograph (IRS) to observe the 5-37 {mu}m thermal emission of comet 73P/Schwassmann-Wachmann 3 (SW3), components B and C. We obtained low spectral resolution (R {approx} 100) data over the entire wavelength interval, along with images at 16 and 22 {mu}m. These observations provided an unprecedented opportunity to study nearly pristine material from the surface and what was until recently the interior of an ecliptic comet-the cometary surface having experienced only two prior perihelion passages, and including material that was totally fresh. The spectra were modeled using a variety of mineral types including both amorphous and crystalline components. We find that the degree of silicate crystallinity, {approx}35%, is somewhat lower than most other comets with strong emission features, while its abundance of amorphous carbon is higher. Both suggest that SW3 is among the most chemically primitive solar system objects yet studied in detail, and that it formed earlier or farther from the Sun than the bulk of the comets studied so far. The similar dust compositions of the two fragments suggest that these are not mineralogically heterogeneous, but rather uniform throughout their volumes. The best-fit particle size distribution for SW3B has a form dn/da {approx} a{sup -3.5}, close to that expected for dust in collisional equilibrium, while that for SW3C has dn/da {approx} a{sup -4.0}, as seen mostly in active comets with strong directed jets, such as C/1995 O1 Hale-Bopp. The total mass of dust in the comae plus nearby tail, extrapolated from the field of view of the IRS peak-up image arrays, is (3-5) x 10{sup 8} kg for B and (7-9) x 10{sup 8} kg for C. Atomic abundances derived from the spectral models indicate a depletion of O compared to solar photospheric values, despite the inclusion of water ice and gas in the models. Atomic C may be solar or slightly sub-solar, but its abundance is complicated by the potential contribution of spectrally featureless mineral species to the portion of the spectra most sensitive to the derivation of the C abundance. We find a relatively high bolometric albedo, {approx}0.13 for the dust, considering the large amount of dark carbonaceous material, but consistent with the presence of abundant small particles and strong emission features.

Sitko, Michael L.; Whitney, Barbara A.; Wolff, Michael J. [Space Science Institute, Boulder, CO 80301 (United States); Lisse, Carey M. [Applied Physics Lab, Johns Hopkins University, Laurel, MD 20723 (United States); Kelley, Michael S. [Department of Astronomy, University of Maryland, College Park, MD 20742 (United States); Polomski, Elisha F. [Department of Physics and Astronomy, University of Wisconsin, Eau Claire, WI 54702 (United States); Lynch, David K.; Russell, Ray W. [Aerospace Corporation, Los Angeles, CA 90009 (United States); Kimes, Robin L. [Department of Physics, University of Cincinnati, Cincinnati, OH 45221 (United States); Harker, David E., E-mail: sitko@spacescience.org, E-mail: bwhitney@wisc.edu, E-mail: mjwolff@spacescience.org, E-mail: carey.lisse@jhuapl.edu, E-mail: msk@astro.umd.edu, E-mail: epolomsk@uwec.edu, E-mail: David.K.Lynch@aero.org, E-mail: Ray.W.Russell@aero.org, E-mail: rlk824@gmail.com, E-mail: dharker@ucsd.edu [Center for Astrophysics and Space Science, University of California at San Diego, La Jolla, CA 92093 (United States)

2011-09-15T23:59:59.000Z

39

Status of GLAST, the Gamma-ray Large-area Space Telescope  

SciTech Connect

GLAST is a satellite-based observatory consisting of the Large-Area Telescope (LAT), a modular 4 x 4-tower pair-conversion telescope with a field-of-view greater than 2 steradians, capable of measuring gamma-ray energies in the range 20 MeV to 300 GeV, and the GLAST Burst Monitor (GBM), a set of NaI and BGO detectors covering 8 steradians and sensitive to photons with energies between 10 keV and 25 MeV, allowing for correlative observations of transient events. The observatory is currently being constructed and is scheduled to be launched in August 2007.

Rochester, L.; /SLAC

2005-12-14T23:59:59.000Z

40

Speckle nulling for exoplanet detection with space-based coronagraphic telescopes  

E-Print Network (OSTI)

To detect Earth-like planets in the visible with a coronagraphic telescope, two major noise sources have to be overcome: the photon noise of the diffracted star light, and the speckle noise due to the star light scattered by instrumental defects. Coronagraphs tackle only the photon noise contribution. In order to decrease the speckle noise below the planet level, an active control of the wave front is required. We have developed analytical methods to measure and correct the speckle noise behind a coronagraph with a deformable mirror. In this paper, we summarize these methods, present numerical simulations, and discuss preliminary experimental results obtained with the High-Contrast Imaging Testbed at NASA's Jet Propulsion Laboratory.

Pascal J. Borde; Wesley A. Traub; Brian D. Kern; John T. Trauger; Andreas C. Kuhnert

2006-06-13T23:59:59.000Z

Note: This page contains sample records for the topic "webb space telescope" from the National Library of EnergyBeta (NLEBeta).
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41

Background and Scattered Light Subtraction in the High-Resolution Echelle Modes of the Space Telescope Imaging Spectrograph  

E-Print Network (OSTI)

We present a simple, effective approach for estimating the on-order backgrounds of spectra taken with the highest-resolution modes of the Space Telescope Imaging Spectrograph (STIS) on-board the Hubble Space Telescope. Our scheme for determining the on-order background spectrum uses polynomial fits to the inter-order scattered light visible in the two-dimensional STIS MAMA images. We present a suite of high-resolution STIS spectra to demonstrate that our background subtraction routine produces the correct overall zero point, as judged by the small residual flux levels in the centers of strongly-saturated interstellar absorption lines. Although there are multiple sources of background light in STIS echelle mode data, this simple approach works very well for wavelengths longward of Lyman-alpha. At shorter wavelengths, the smaller order separation and generally lower signal-to-noise ratios of the data can reduce the effectiveness of our background estimation procedure. Slight artifacts in the background-subtracted spectrum can be seen in some cases, particularly at wavelengths light. We discuss the limitations of high-resolution STIS data in light of the uncertainties associated with our background subtraction procedure. We compare our background-subtracted STIS spectra with GHRS Ech-A observations of the DA white dwarf G191-B2B and GHRS first-order G160M observations of the early-type star HD 218915. We find no significant differences between the GHRS data and the STIS data reduced with our method in either case.

J. Christopher Howk; Kenneth R. Sembach

1999-12-17T23:59:59.000Z

42

HUBBLE SPACE TELESCOPE SPECTRAL OBSERVATIONS NEAR THE He II Ly{alpha} BREAK: IMPLICATIONS FOR He II REIONIZATION  

SciTech Connect

Quasars that allow the study of intergalactic medium (IGM) He II are very rare, since they must be at high redshift along sightlines free of substantial hydrogen absorption, but recent work has dramatically expanded the number of such quasars known. We analyze two dozen higher-redshift (z = 3.1-3.9) low-resolution He II quasar spectra from the Hubble Space Telescope and find that their He II Gunn-Peterson troughs suggest exclusion of very early and very late reionization models, favoring a reionization redshift of z {approx} 3. Although the data quality is not sufficient to reveal details such as the expected redshift evolution of helium opacity, we obtain the first ensemble measure of helium opacity at high redshift averaged over many sightlines: {tau} = 4.90 at z {approx} 3.3. We also find that it would be very difficult to observe the IGM red wing of absorption from the beginning of He II reionization, but depending on the redshift of reionization and the size of ionization zones, it might be possible to do so in some objects with the current generation of UV spectrographs.

Syphers, David [CASA, Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80309 (United States); Anderson, Scott F.; Haggard, Daryl [Astronomy Department, University of Washington, Seattle, WA 98195 (United States); Zheng Wei [Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218 (United States); Meiksin, Avery [Scottish Universities Physics Alliance (SUPA), Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh EH9 3HJ (United Kingdom); Schneider, Donald P. [Department of Physics and Astronomy, Pennsylvania State University, 525 Davey Lab, University Park, PA 16802 (United States); York, Donald G., E-mail: David.Syphers@colorado.edu, E-mail: anderson@astro.washington.edu, E-mail: zheng@pha.jhu.edu [Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637 (United States)

2011-01-10T23:59:59.000Z

43

Hubble Space Telescope Imaging of the Circumnuclear Environments of the CfA Seyfert Galaxies: Nuclear Spirals and Fueling  

E-Print Network (OSTI)

We present archival Hubble Space Telescope images of the nuclear regions of 43 of the 46 Seyfert galaxies found in the volume-limited, spectroscopically-complete CfA Redshift Survey sample. Using an improved method of image contrast enhancement, we create detailed high-quality structure maps that allow us to study the distributions of dust, star clusters, and emission-line gas in the circumnuclear regions (100-1000 pc scales) and in the associated host galaxy. Essentially all of these Seyfert galaxies have circumnuclear dust structures with morphologies ranging from grand-design two-armed spirals to chaotic dusty disks. In most Seyferts there is a clear physical connection between the nuclear dust spirals on hundreds of parsec scales and large-scale bars and spiral arms in the host galaxies proper. These connections are particularly striking in the interacting and barred galaxies. Such structures are predicted by numerical simulations of gas flows in barred and interacting galaxies, and may be related to the fueling of AGN by matter inflow from the host galaxy disks. We see no significant differences in the circumnuclear dust morphologies of Seyfert 1s and 2s, and very few Seyfert 2 nuclei are obscured by large-scale dust structures in the host galaxies. If Seyfert 2s are obscured Seyfert 1s, then the obscuration must occur on smaller scales than those probed by HST.

Richard W. Pogge; Paul Martini

2002-01-11T23:59:59.000Z

44

High resolution telescope  

DOE Patents (OSTI)

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 2.1m in a circle-of-nine configuration. The telescope array has an effective aperture of 12m 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 activities. The cost of the telescope scales with the first power of the aperture rather than its third power as in conventional telescopes. 9 figs., 1 tab.

Massie, N.A.; Oster, Y.

1990-01-01T23:59:59.000Z

45

High resolution telescope  

DOE Patents (OSTI)

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.

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

1992-01-01T23:59:59.000Z

46

High resolution telescope  

DOE Patents (OSTI)

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 2.1m in a circle-of-nine configuration. The telescope array has an effective aperture of 12m 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 activities. The cost of the telescope scales with the first power of the aperture rather than its third power as in conventional telescopes. 9 figs., 1 tab.

Massie, N.A.; Oster, Y.

1990-12-31T23:59:59.000Z

47

THE EXTENDED HUBBLE SPACE TELESCOPE SUPERNOVA SURVEY: THE RATE OF CORE COLLAPSE SUPERNOVAE TO z {approx} 1  

SciTech Connect

We use a sample of 45 core collapse supernovae detected with the Advanced Camera for Surveys on board the Hubble Space Telescope to derive the core collapse supernova rate in the redshift range 0.1 < z < 1.3. In redshift bins centered on (z) = 0.39, (z) = 0.73, and (z) = 1.11, we find rates of 3.00{sup +1.28}{sub -0.94} {sup +1.04}{sub -0.57}, 7.39{sup +1.86}{sub -1.52} {sup +3.20}{sub -1.60}, and 9.57{sup +3.76}{sub -2.80} {sup +4.96}{sub -2.80}, respectively, given in units of yr{sup -1} Mpc{sup -3} 10{sup -4} h {sup 3}{sub 70}. The rates have been corrected for host galaxy extinction, including supernovae missed in highly dust-enshrouded environments in infrared bright galaxies. The first errors are statistical while the second ones are the estimated systematic errors. We perform a detailed discussion of possible sources of systematic errors and note that these start to dominate over statistical errors at z > 0.5, emphasizing the need to better control the systematic effects. For example, a better understanding of the amount of dust extinction in the host galaxies and knowledge of the supernova luminosity function, in particular the fraction of faint M {approx}> -15 supernovae, is needed to better constrain the rates. When comparing our results with the core collapse supernova rate based on the star formation rate, we find a good agreement, consistent with the supernova rate following the star formation rate, as expected.

Dahlen, Tomas; Riess, Adam G. [Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States); Strolger, Louis-Gregory [Department of Physics and Astronomy, Western Kentucky University, Bowling Green, KY 42101 (United States); Mattila, Seppo; Kankare, Erkki [Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Vaeisaelaentie 20, FI-21500 Piikkioe (Finland); Mobasher, Bahram, E-mail: dahlen@stsci.edu [Department of Physics and Astronomy, University of California, Riverside, CA 92521 (United States)

2012-09-20T23:59:59.000Z

48

Discovery of Pulsations from the Pulsar J0205 6449 in SNR 3C 58 with the Fermi Gamma-Ray Space Telescope  

SciTech Connect

We report the discovery of {gamma}-ray pulsations ({ge}0.1 GeV) from the young radio and X-ray pulsar PSR J0205 + 6449 located in the Galactic supernova remnant 3C 58. Data in the {gamma}-ray band were acquired by the Large Area Telescope aboard the Fermi Gamma-ray Space Telescope (formerly GLAST), while the radio rotational ephemeris used to fold {gamma}-rays was obtained using both the Green Bank Telescope and the Lovell telescope at Jodrell Bank. The light curve consists of two peaks separated by 0.49 {+-} 0.01 {+-} 0.01 cycles which are aligned with the X-ray peaks. The first {gamma}-ray peak trails the radio pulse by 0.08 {+-} 0.01 {+-} 0.01, while its amplitude decreases with increasing energy as for the other {gamma}-ray pulsars. Spectral analysis of the pulsed {gamma}-ray emission suggests a simple power law of index -2.1 {+-} 0.1 {+-} 0.2 with an exponential cutoff at 3.0{sub -0.7}{sup +1.1} {+-} 0.4 GeV. The first uncertainty is statistical and the second is systematic. The integral {gamma}-ray photon flux above 0.1 GeV is (13.7 {+-} 1.4 {+-} 3.0) x 10{sup -8} cm{sup -2} s{sup -1}, which implies for a distance of 3.2 kpc and assuming a broad fan-like beam a luminosity of 8.3 x 10{sup 34} erg s{sup -1} and an efficiency {eta} of 0.3%. Finally, we report a 95% upper limit on the flux of 1.7 x 10{sup -8} cm{sup -2} s{sup -1} for off-pulse emission from the object.

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

2011-12-01T23:59:59.000Z

49

Astrometry with the Hubble Space Telescope: Trigonometric Parallaxes of Planetary Nebula Nuclei: NGC 6853, NGC 7293, Abell 31, and DeHt 5  

E-Print Network (OSTI)

We present absolute parallaxes and relative proper motions for the central stars of the planetary nebulae NGC 6853 (The Dumbbell), NGC 7293 (The Helix), Abell 31, and DeHt 5. This paper details our reduction and analysis using DeHt 5 as an example. We obtain these planetary nebula nuclei (PNNi) parallaxes with astrometric data from Fine Guidance Sensors FGS 1R and FGS 3, white-light interferometers on the Hubble Space Telescope (HST). Proper motions, spectral classifications and VJHKT_2M and DDO51 photometry of the stars comprising the astrometric reference frames provide spectrophotometric estimates of reference star absolute parallaxes. Introducing these into our model as observations with error, we determine absolute parallaxes for each PNN. Weighted averaging with previous independent parallax measurements yields an average parallax precision, \\sigma_{\\pi}/\\pi = 5 %. Derived distances are: d_{NGC 6853}=405^{+28}_{-25}pc, d_{NGC 7293}=216^{+14}_{-12} pc, d_{Abell 31} = 621^{+91}_{-70} pc, and d_{DeHt 5} = ...

Benedict, G Fritz; Napiwotzki, Ralf; Harrison, Thomas E; Harris, Hugh C; Nelan, Edmund; Bond, Howard E; Patterson, Richard J; Ciardullo, Robin

2009-01-01T23:59:59.000Z

50

Hubble Space Telescope hot Jupiter Transmission Spectral Survey: detection of water in HAT-P-1b from Wide Field Camera 3 near-infrared spatial scan observations  

E-Print Network (OSTI)

We present Hubble Space Telescope near-infrared transmission spectroscopy of the transiting hot-Jupiter HAT-P-1b. We observed one transit with Wide Field Camera 3 using the G141 low-resolution grism to cover the wavelength range 1.087- 1.678 {\\mu}m. These time series observations were taken with the newly available spatial scan mode that increases the duty cycle by nearly a factor of two, thus improving the resulting photometric precision of the data. We measure a planet-to-star radius ratio of Rp/R*=0.11709+/-0.00038 in the white light curve with the centre of transit occurring at 2456114.345+/-0.000133 (JD). We achieve S/N levels per exposure of 1840 (0.061%) at a resolution of {\\Delta\\lambda}=19.2nm (R~70) in the 1.1173 - 1.6549{\\mu}m spectral region, providing the precision necessary to probe the transmission spectrum of the planet at close to the resolution limit of the instrument. We compute the transmission spectrum using both single target and differential photometry with similar results. The resultan...

Wakeford, H R; Deming, D; Gibson, N P; Fortney, J J; Burrows, A S; Ballester, G; Nikolov, N; Aigrain, S; Henry, G; Knutson, H; Etangs, A Lecavelier des; Pont, F; Showman, A P; Vidal-Madjar, A; Zahnle, K

2013-01-01T23:59:59.000Z

51

ANALYZING STAR CLUSTER POPULATIONS WITH STOCHASTIC MODELS: THE HUBBLE SPACE TELESCOPE/WIDE FIELD CAMERA 3 SAMPLE OF CLUSTERS IN M83  

SciTech Connect

The majority of clusters in the universe have masses well below 10{sup 5} M{sub Sun }. Hence, their integrated fluxes and colors can be affected by the presence or absence of a few bright stars introduced by stochastic sampling of the stellar mass function. Specific methods are being developed to extend the analysis of cluster energy distributions into the low-mass regime. In this paper, we apply such a method to real observations of star clusters, in the nearby spiral galaxy M83. We reassess the ages and masses of a sample of 1242 clusters for which UBVIH{alpha} fluxes were obtained from observations with the Wide Field Camera 3 instrument on board the Hubble Space Telescope. Synthetic clusters with known properties are used to characterize the limitations of the method (valid range and resolution in age and mass, method artifacts). The ensemble of color predictions of the discrete cluster models are in good agreement with the distribution of observed colors. We emphasize the important role of the H{alpha} data in the assessment of the fraction of young objects, particularly in breaking the age-extinction degeneracy that hampers an analysis based on UBVI data only. We find the mass distribution of the cluster sample to follow a power law of index -2.1 {+-} 0.2, and the distribution of ages a power law of index -1.0 {+-} 0.2 for log (M/ M{sub Sun }) > 3.5, and ages between 10{sup 7} and 10{sup 9} yr. An extension of our main method, which makes full use of the probability distributions of age and mass obtained for the individual clusters of the sample, is explored. It produces similar power-law slopes and will deserve further investigation. Although the properties derived for individual clusters significantly differ from those obtained with traditional, non-stochastic models in about 30% of the objects, the first-order aspect of the age and mass distributions is similar to those obtained previously for this M83 sample in the range of overlap of the studies. We extend the power-law description to lower masses with better mass and age resolution and without most of the artifacts produced by the classical method.

Fouesneau, Morgan; Lancon, Ariane [Observatoire astronomique and CNRS UMR 7550, Universite de Strasbourg, Strasbourg (France); Chandar, Rupali [Department of Physics and Astronomy, University of Toledo, Toledo, OH (United States); Whitmore, Bradley C., E-mail: morgan.fouesneau@astro.u-strasbg.fr [Space Telescope Science Institute, Baltimore, MD (United States)

2012-05-01T23:59:59.000Z

52

The extragalactic distance scale Key Project. III. The discovery of Cepheids and a new distance to M101 using the {ital Hubble} {ital Space} {ital Telescope}  

Science Conference Proceedings (OSTI)

We report on the discovery of 29 Cepheid variables in the galaxy M101 using the original Wide Field Camera (WFC) and the new Wide Field and Planetary Camera 2 (WFPC2) on the {ital Hubble} {ital Space} {ital Telescope}. We observed a field in M101 at 17 independent epochs in {ital V} (F555W), five epochs in {ital I} (F785LP/F814W), and one epoch in {ital B} (F439W), with a time interval baseline of 381 days. We have found Cepheids with periods ranging from 10 to 60 days. The data have been calibrated using WFPC2 observations with zero points derived from {omega} Cen, Pal 4, and NGC 2419 observations. This calibration has been verified by using the Medium Deep Survey (MDS) WFC photometric zero points, and ground-based secondary standards in {ital V} and {ital I}. The {ital V} calibrations agree to {plus_minus}0.06 mag, and the {ital I} calibrations agree to {plus_minus}0.04 mag. We have constructed {ital V} and {ital I} period-luminosity (PL) relations and have derived apparent distance moduli based on a distance modulus for the Large Magellanic Cloud (LMC) of 18.50 mag and a reddening of {ital E}({ital B}{minus}{ital V})=0.10 mag to the LMC Cepheids. Period-residual minimization was used to minimize the effects of Malmquist bias on the period-luminosity relation fitting process. Using a Galactic extinction law and the apparent {ital V} and {ital I} distance moduli, we have found a mean reddening for the M101 sample of {ital E}({ital B}{minus}{ital V})=0.03 mag and a true distance modulus to M101 of 29.34{plus_minus}0.17 mag, corresponding to a distance of 7.4{plus_minus}0.6 Mpc. The sources of error have been rigorously tracked through an error budget; systematic and random errors contribute roughly equally to the quoted error. The mean gas-phase metal abundances in the LMC and in the M101 outer field are similar so we expect metallicity effects to be minimal. (Abstract Truncated)

Kelson, D.D.; Illingworth, G.D. [UCO/Lick Observatory, University of California, Santa Cruz, California 95064 (United States); Freedman, W.F. [Carnegie Observatories, 813 Santa Barbara Street, Pasadena, California 91101 (United States); Graham, J.A. [Department of Terrestrial Magnetism, Carnegie Institution of Washington, 5241 Broad Branch Road NW, Washington, District of Columbia 20015 (United States); Hill, R. [Carnegie Observatories, 813 Santa Barbara Street, Pasadena, California 91101 (United States); Madore, B.F. [NASA/IPAC Extragalactic Database, Infrared Processing and Analysis Center, Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91125 (United States); Saha, A. [Space Telescope Institute, Homewood Campus, Baltimore, Maryland 21218 (United States); Stetson, P.B. [Dominion Astrophysical Observatory, National Research Council, 5071 West Saanich Road, Victoria, BC, V8X 4M6 (CANADA); Kennicutt, R.C. Jr. [Steward Observatory, University of Arizona, Tucson, Arizona 85721 (United States); Mould, J.R. [Mt. Stromlo and Siding Springs Observatories, Private Bag, Weston Creek Post Office ACT 2611 (Australia); Hughes, S.M. [Royal Greenwich Observatory, Madingley Road, Cambridge, (United Kingdom) CB3 0EZ; Ferrarese, L. [Space Telescope Institute, Homewood Campus, Baltimore, Maryland 21218 (United States)]|[Department of Physics and Astronomy, Bloomberg 501, Johns Hopkins University, 3400 North Charles Street, Baltimore, Maryland 21218 (United States); Phelps, R. [Carnegie Observatories, 813 Santa Barbara Street, Pasadena, California 91101 (United States); Turner, A. [Steward Observatory, University of Arizona, Tucson, Arizona 85721 (United States); Cook, K.H. [Lawrence Livermore National Laboratory, Mississippi L-401, P.O. Box 808, Livermore, California 94550 (United States); Ford, H. [Space Telescope Institute, Homewood Campus, Baltimore, Maryland 21218 (United States)

1996-05-01T23:59:59.000Z

53

Morphological themes of informal housing in Colonias: impacts of sociocultural identity on Webb County housing form  

E-Print Network (OSTI)

Informal settlements are a form of housing found in many parts of the world. Self-help housing in informal settlements has different influences that are denoted in the customs and preferences of the residents, which in turn, are reflected on the elements of house exteriors as well as its interior. Colonias in the U.S-Mexico border region are a model of informal settlements. The purpose of this study is to analyze the social and cultural influences on housing fronts in Webb County Colonias. The study focuses on investigating traditional features, vernacular forms, building rituals, and social features as they relate to the morphology of house fronts and their production. The housing model of Geddes and Bertalanffy explained by Turner (1972) was the premise of establishing the argument of this study. A mixed-method approach was used in data gathering from the following three Colonias: Los Altos, Larga Vista, and Rio Bravo. Utilized methods included image-based research through systematic random sampling of housing fronts in the Colonias, as well as a group-administered structured survey distributed during community monthly gathering for food distribution. The development of the research process and methodology incorporated the input of the local community and local leaders and volunteers assisted in its implementation. The study concluded that past and present experiences of Colonias residents have intense impacts on different aspects contributing to the themes comprising the morphology of Colonias housing fronts. A classical pattern of migration as well as maintained contact and continuous dialogue between residents and their kin were found to result in preserving the inherent native culture of the Colonias� residents and can thus be considered as core elements. This preservation of native culture was indicated by utilization of semi-private space, traditional roof forms, privacy and security elements, and building rituals. The study also identified additional secondary modified elements, represented by the lack of gates utilization as a measure of security. These core and modified elements coincide with the Geddes and Bertalanffy model and therefore it can be deduced that this model can be applied in the case of the Colonias.

Mohamed Kamal El Sayed Ibrahim, Azza

2005-08-01T23:59:59.000Z

54

BNL | Large Synoptic Survey Telescope (LSST)  

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

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

55

The First VERITAS Telescope  

E-Print Network (OSTI)

The first atmospheric Cherenkov telescope of VERITAS (the Very Energetic Radiation Imaging Telescope Array System) has been in operation since February 2005. We present here a technical description of the instrument and a summary of its performance. The calibration methods are described, along with the results of Monte Carlo simulations of the telescope and comparisons between real and simulated data. The analysis of TeV $\\gamma$-ray observations of the Crab Nebula, including the reconstructed energy spectrum, is shown to give results consistent with earlier measurements. The telescope is operating as expected and has met or exceeded all design specifications.

J. Holder; R. W. Atkins; H. M. Badran; G. Blaylock; S. M. Bradbury; J. H. Buckley; K. L. Byrum; D. A. Carter-Lewis; O. Celik; Y. C. K. Chow; P. Cogan; W. Cui; M. K. Daniel; I. de la Calle Perez; C. Dowdall; P. Dowkontt; C. Duke; A. D. Falcone; S. J. Fegan; J. P. Finley; P. Fortin; L. F. Fortson; K. Gibbs; G. Gillanders; O. J. Glidewell; J. Grube; K. J. Gutierrez; G. Gyuk; J. Hall; D. Hanna; E. Hays; D. Horan; S. B. Hughes; T. B. Humensky; A. Imran; I. Jung; P. Kaaret; G. E. Kenny; D. Kieda; J. Kildea; J. Knapp; H. Krawczynski; F. Krennrich; M. J. Lang; S. LeBohec; E. Linton; E. K. Little; G. Maier; H. Manseri; A. Milovanovic; P. Moriarty; R. Mukherjee; P. A. Ogden; R. A. Ong; J. S. Perkins; F. Pizlo; M. Pohl; J. Quinn; K. Ragan; P. T. Reynolds; E. T. Roache; H. J. Rose; M. Schroedter; G. H. Sembroski; G. Sleege; D. Steele; S. P. Swordy; A. Syson; J. A. Toner; L. Valcarcel; V. V. Vassiliev; S. P. Wakely; T. C. Weekes; R. J. White; D. A. Williams; R. Wagner

2006-04-06T23:59:59.000Z

56

Gas-Phase Diffusion in Porous Media: Comparison of Models Stephen W. Webb  

Office of Scientific and Technical Information (OSTI)

Gas-Phase Diffusion in Porous Media: Comparison of Models Gas-Phase Diffusion in Porous Media: Comparison of Models Stephen W. Webb Sandia National Laboratories Albuquerque, New Mexico 87 185 ABSTRACT Two models are commonly used to analyze gas- phase diffusion in porous media in the presence of advection, the Advective-Dispersive Model (ADM) and the Dusty-gas Model (DGM). The ADM, which is used in TOUGH2, is based on a simple linear addition of advection calculated by Darcy's law and ordinary diffusion using Fick's law with a porosity- tortuosity-gas saturation multiplier to account for the porous medium. Another approach for gas-phase transport in porous media is the Dusty-Gas Model. This model applies the kinetic theory of gases to the gaseous components and the porous media (or "dust") to combine transport due to diffusion and

57

OVERVIEW OF THE ATACAMA COSMOLOGY TELESCOPE: RECEIVER, INSTRUMENTATION, AND TELESCOPE SYSTEMS  

SciTech Connect

The Atacama Cosmology Telescope was designed to measure small-scale anisotropies in the cosmic microwave background and detect galaxy clusters through the Sunyaev-Zel'dovich effect. The instrument is located on Cerro Toco in the Atacama Desert, at an altitude of 5190 m. A 6 m off-axis Gregorian telescope feeds a new type of cryogenic receiver, the Millimeter Bolometer Array Camera. The receiver features three 1000-element arrays of transition-edge sensor bolometers for observations at 148 GHz, 218 GHz, and 277 GHz. Each detector array is fed by free space millimeter-wave optics. Each frequency band has a field of view of approximately 22' x 26'. The telescope was commissioned in 2007 and has completed its third year of operations. We discuss the major components of the telescope, camera, and related systems, and summarize the instrument performance.

Swetz, D. S.; Devlin, M. J.; Dicker, S. R. [Department of Physics and Astronomy, University of Pennsylvania, 209 South 33rd Street, Philadelphia, PA 19104 (United States); Ade, P. A. R. [School of Physics and Astronomy, Cardiff University, The Parade, Cardiff, Wales CF24 3AA (United Kingdom); Amiri, M.; Battistelli, E. S.; Burger, B.; Halpern, M.; Hasselfield, M. [Department of Physics and Astronomy, University of British Columbia, Vancouver, BC V6T 1Z4 (Canada); Appel, J. W.; Essinger-Hileman, T.; Fisher, R. P.; Fowler, J. W.; Hincks, A. D.; Jarosik, N. [Joseph Henry Laboratories of Physics, Jadwin Hall, Princeton University, Princeton, NJ 08544 (United States); Chervenak, J. [Code 553/665, NASA/Goddard Space Flight Center, Greenbelt, MD 20771 (United States); Doriese, W. B.; Hilton, G. C.; Irwin, K. D. [NIST Quantum Devices Group, 325 Broadway Mailcode 817.03, Boulder, CO 80305 (United States); Duenner, R. [Departamento de Astronomia y Astrofisica, Facultad de Fisica, PontificIa Universidad Catolica, Casilla 306, Santiago 22 (Chile)

2011-06-01T23:59:59.000Z

58

The South Pole Telescope  

E-Print Network (OSTI)

A new 10 meter diameter telescope is being constructed for deployment at the NSF South Pole research station. The telescope is designed for conducting large-area millimeter and sub-millimeter wave surveys of faint, low contrast emission, as required to map primary and secondary anisotropies in the cosmic microwave background. To achieve the required sensitivity and resolution, the telescope design employs an off-axis primary with a 10m diameter clear aperture. The full aperture and the associated optics will have a combined surface accuracy of better than 20 microns rms to allow precision operation in the submillimeter atmospheric windows. The telescope will be surrounded with a large reflecting ground screen to reduce sensitivity to thermal emission from the ground and local interference. The optics of the telescope will support a square degree field of view at 2mm wavelength and will feed a new 1000-element micro-lithographed planar bolometric array with superconducting transition-edge sensors and frequency-multiplexed readouts. The first key project will be to conduct a survey over approximately 4000 degrees for galaxy clusters using the Sunyaev-Zel'dovich Effect. This survey should find many thousands of clusters with a mass selection criteria that is remarkably uniform with redshift. Armed with redshifts obtained from optical and infrared follow-up observations, it is expected that the survey will enable significant constraints to be placed on the equation of state of the dark energy.

SPT Collaboration; J. E. Ruhl; P. A. R. Ade; J. E. Carlstrom; H. M. Cho; T. Crawford; M. Dobbs; C. H. Greer; N. W. Halverson; W. L. Holzapfel; T. M. Lantin; A. T. Lee; J. Leong; E. M. Leitch; W. Lu; M. Lueker; J. Mehl; S. S. Meyer; J. J. Mohr; S. Padin; T. Plagge; C. Pryke; D. Schwan; M. K. Sharp; M. C. Runyan; H. Spieler; Z. Staniszewski; A. A. Stark

2004-11-04T23:59:59.000Z

59

Fast Fourier transform telescope  

Science Conference Proceedings (OSTI)

We propose an all-digital telescope for 21 cm tomography, which combines key advantages of both single dishes and interferometers. The electric field is digitized by antennas on a rectangular grid, after which a series of fast Fourier transforms recovers simultaneous multifrequency images of up to half the sky. Thanks to Moore's law, the bandwidth up to which this is feasible has now reached about 1 GHz, and will likely continue doubling every couple of years. The main advantages over a single dish telescope are cost and orders of magnitude larger field-of-view, translating into dramatically better sensitivity for large-area surveys. The key advantages over traditional interferometers are cost (the correlator computational cost for an N-element array scales as Nlog{sub 2}N rather than N{sup 2}) and a compact synthesized beam. We argue that 21 cm tomography could be an ideal first application of a very large fast Fourier transform telescope, which would provide both massive sensitivity improvements per dollar and mitigate the off-beam point source foreground problem with its clean beam. Another potentially interesting application is cosmic microwave background polarization.

Tegmark, Max; Zaldarriaga, Matias [Department of Physics and MIT Kavli Institute, Massachusetts Institute of Technology, Cambridge, Massachusetts 02139 (United States); Center for Astrophysics, Harvard University, Cambridge, Massachusetts 02138 (United States)

2009-04-15T23:59:59.000Z

60

The Large Synoptic Survey Telescope  

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

night sky. Below: The telescope depicted at its future site atop Cerro Pachn in Chile. (Top image by Todd Mason, Mason Productions Inc. LSST Corporation. Bottom image...

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


61

The world-wide telescope  

Science Conference Proceedings (OSTI)

Mining vast databases of astronomical data, this new online way to see the global structure of the universe promises to be not only a wonderful virtual telescope but an archetype for the evolution of computational science.

Jim Gray; Alex Szalay

2002-11-01T23:59:59.000Z

62

Optical-level structural modelling of membrane mirrors for spaceborne telescopes  

E-Print Network (OSTI)

The astronomy and Earth observation communities desire ever-larger space telescopes, but launch costs limit mass and technology limits size. Current research in large aperture mirrors largely supports deployed rigid optics, ...

De Blonk, Brett Jeffrey, 1971-

2003-01-01T23:59:59.000Z

63

In January 2013, a new Earth-observing instrument was installed on the International Space Station (ISS). ISERV Pathfinder consists of a commercial camera, a telescope, and a pointing system, all  

E-Print Network (OSTI)

to show officials where the bridge is out or where a road is washed out or a power substation is inundated the space station is at each moment and to calculate the next chance to view a particular area on the ground

64

SLAC National Accelerator Laboratory - Bringing Telescope Tech...  

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

Telescope Tech to X-ray Lasers By Glenn Roberts Jr July 10, 2012 Technology that helps ground-based telescopes cut through the haze of Earth's atmosphere to get a clearer view of...

65

Design of a telescope-occulter system for THEIA  

E-Print Network (OSTI)

The Telescope for Habitable Exoplanets and Interstellar/Intergalactic Astronomy (THEIA) is a mission concept study for a flagship-class telescope-occulter system to search for terrestrial planets and perform general astrophysics with a space-based 4m telescope. A number of design options were considered for the occulter and telescope optical systems; in this paper we discuss the design of occulters and coronagraphs for THEIA and examine their merits. We present two optimized occulters: a 25.6m-radius occulter with 19m petals that achieves 10^-12 suppression from 250-1000nm with a 75mas inner working angle, and a 20.0m-radius occulter with 10m petals that achieves 10^-12 suppression from 250-700nm with a 75mas inner working angle. For more widely separated planets (IWA > 108mas), this second occulter is designed to operate at a second closer distance where it provides 10^-12 suppression from 700-1000nm. We have also explored occulter/coronagraph hybrid systems, and found that an AIC coronagraph that exploits t...

Cady, Eric; Dumont, Philip; Egerman, Robert; Kasdin, N Jeremy; Linfield, Roger; Lisman, Doug; Savransky, Dmitry; Seager, Sara; Shaklan, Stuart; Spergel, David; Tenerelli, Domenick; Vanderbei, Robert

2009-01-01T23:59:59.000Z

66

Scientific Potential of Einstein Telescope  

E-Print Network (OSTI)

Einstein gravitational-wave Telescope (ET) is a design study funded by the European Commission to explore the technological challenges of and scientific benefits from building a third generation gravitational wave detector. The three-year study, which concluded earlier this year, has formulated the conceptual design of an observatory that can support the implementation of new technology for the next two to three decades. The goal of this talk is to introduce the audience to the overall aims and objectives of the project and to enumerate ET's potential to influence our understanding of fundamental physics, astrophysics and cosmology.

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

2011-08-05T23:59:59.000Z

67

Space-based Telescopes for Actionable Refinement of Ephemeris (STARE)  

Current Weather. Protocol Office. Where to stay. Tri ... The STARE system would be a great addition to this proposed approach as a tool to implement the conjunction ...

68

The Ultraviolet Imaging Telescope: Instrument and Data Characteristics  

E-Print Network (OSTI)

The Ultraviolet Imaging Telescope (UIT) was flown as part of the Astro observatory on the Space Shuttle Columbia in December 1990 and again on the Space Shuttle Endeavor in March 1995. Ultraviolet (1200-3300?A) images of a variety of astronomical objects, with a 40 ? field of view and a resolution of about 3 ? ? , were recorded on photographic film. The data recorded during the first flight are available to the astronomical community through the National Space Science Data Center (NSSDC); the data recorded during the second flight will soon be available as well. This paper discusses in detail the design, operation, data reduction, and calibration of UIT, providing the user of the data with information for understanding and using the data. It also provides guidelines for analyzing other astronomical imagery made with image intensifiers and photographic film. – 3 –

Theodore P. Stecher; Robert H. Cornett; Michael R. Greason; Wayne B. L; Jesse K. Hill; Robert S. Hill; Ralph C. Bohlin; Peter C. Chen; Nicholas R; Michael N. Fanelli; Joan I. Hollis; Susan G. Neff; Robert W. O’connell; Joel D. Offenberg; Ronald A. Parise; Joel Wm. Parker; Morton S. Roberts; M. Smith; William H. Waller

1997-01-01T23:59:59.000Z

69

The ANTARES underwater neutrino telescope  

E-Print Network (OSTI)

ANTARES is the first undersea neutrino telescope. It is in its complete configuration since May 2008 at about 2.5 km below the sea surface close to Marseille. Data from 12 lines are being analyzed and are producing first results. Here we discuss first analysis results for 5 lines and 10 lines, and we also comment on the performance of the full detector. We show that the detector has capabilities for discriminating upgoing neutrino events from the much larger amount of downgoing atmospheric muons and that data and simulation are in good agreement. We then discuss the physics reach of the detector for what concerns point-like source and dark matter searches.

Teresa Montaruli; for the ANTARES Collaboration

2008-10-21T23:59:59.000Z

70

NIST Telescope Calibration May Help Explain Mystery of ...  

Science Conference Proceedings (OSTI)

... They will use this information to calibrate a much larger telescope–the Large Synoptic Survey Telescope, planned for construction in Chile. ...

2011-01-05T23:59:59.000Z

71

Measuring Neutrinos with the ANTARES Telescope  

Science Conference Proceedings (OSTI)

The ANTARES underwater neutrino telescope has been taking data since construction began in 2006. The telescope, completed in May of 2008, detects the Cerenkov radiation of charged leptons produced by high energy neutrinos interacting in or around the detector. The lepton trajectory is reconstructed with high precision, revealing the direction of the incoming neutrino. The performance of the detector will be discussed and recent data showing muons, electromagnetic showers and atmospheric neutrinos will be presented. Studies have been underway to search for neutrino point sources in the ANTARES data since 2007. Results from these studies will be presented, and the sensitivity of the telescope will be discussed.

Reed, Corey [National Institute for Subatomic Physics (Nikhef), Amsterdam (Netherlands)

2009-12-17T23:59:59.000Z

72

Fermi Large Area Telescope Operations: Progress Over 4 Years  

SciTech Connect

The Fermi Gamma-ray Space Telescope was launched into orbit in June 2008, and is conducting a multi-year gamma-ray all-sky survey, using the main instrument on Fermi, the Large Area Telescope (LAT). Fermi began its science mission in August 2008, and has now been operating for almost 4 years. The SLAC National Accelerator Laboratory hosts the LAT Instrument Science Operations Center (ISOC), which supports the operation of the LAT in conjunction with the Mission Operations Center (MOC) and the Fermi Science Support Center (FSSC), both at NASA's Goddard Space Flight Center. The LAT has a continuous output data rate of about 1.5 Mbits per second, and data from the LAT are stored on Fermi and transmitted to the ground through TDRS and the MOC to the ISOC about 10 times per day. Several hundred computers at SLAC are used to process LAT data to perform event reconstruction, and gamma-ray photon data are subsequently delivered to the FSSC for public release with a few hours of being detected by the LAT. We summarize the current status of the LAT, and the evolution of the data processing and monitoring performed by the ISOC during the first 4 years of the Fermi mission, together with future plans for further changes to detected event data processing and instrument operations and monitoring.

Cameron, Robert A.; /SLAC

2012-06-28T23:59:59.000Z

73

SCIENTIFIC EFFICIENCY OF GROUND-BASED TELESCOPES  

SciTech Connect

I scanned the six major astronomical journals of 2008 for all 1589 papers that are based on new data obtained from ground-based optical/IR telescopes worldwide. Then I collected data on numbers of papers, citations to them in 3+ years, the most-cited papers, and annual operating costs. These data are assigned to four groups by telescope aperture. For instance, while the papers from telescopes with an aperture >7 m average 1.29 more citations than those with an aperture of 2 to <4 m, this represents a small return for a factor of four difference in operating costs. Among the 17 papers that have received {>=}100 citations in 3+ years, only half come from the large (>7 m) telescopes. I wonder why the large telescopes do so relatively poorly and suggest possible reasons. I also found that papers based on archival data, such as the Sloan Digital Sky Survey, produce 10.6% as many papers and 20.6% as many citations as those based on new data. Also, the 577.2 papers based on radio data produced 36.3% as many papers and 33.6% as many citations as the 1589 papers based on optical/IR telescopes.

Abt, Helmut A., E-mail: abt@noao.edu [Kitt Peak National Observatory, P.O. Box 26732, Tucson, AZ 85726-6732 (United States)

2012-10-01T23:59:59.000Z

74

Energy Blog | Department of Energy  

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

14, 2012 14, 2012 SLAC staff scientist Yiping Feng examines a chamber at LCLS' Front End Enclosure, where a thin crystal spectrometer is installed to measure the shot-by-shot characteristics of X-ray laser pulses. | SLAC National Accelerator Photo by Matt Beardsley Four Crazy Uses for Lasers in the National Labs The top five craziest things our researchers do with lasers in their pursuit to understand our physical world. September 14, 2012 The James Webb Space Telescope is a large, infrared-optimized telescope that is anticipated to launch in 2018. The spider-like sheets and tubes of wires you see here are the Optical Telescope Simulator (OSIM) for the telescope itself. OSIM will help scientists prepare the Webb telescope for flight by generating a beam of light that the telescope optics will feed into its actual flight instruments.

75

Positioning system of the ANTARES Neutrino Telescope  

E-Print Network (OSTI)

Completed in May 2008, the ANTARES neutrino telescope is located 40 km off the coast of Toulon, at a depth of about 2500 m. The telescope consists of 12 detect or lines housing a total of 884 optical modules. Each line is anchored to the seabed and pulled taught by the buoyancy of the individual optical modules and a top buoy. Due to the fluid nature of the sea-water detecting medium and the flexible nature of the detector lines, the optical modules of the ANTARES telescope can suffer from deviations of up to several meters from the vertical and as such, real time positioning is needed. Real time positioning of the ANTARES telescope is achieved by a combination of an acoustic positioning system and a lattice of tiltmeters and compasses. These independent and complementary systems are used to compute a global fit to each individual detector line, allowing us to construct a 3 dimensional picture of the ANTARES neutrino telescope with an accuracy of less than 10 cm. In this paper we describe the positioning syst...

Brown, Anthony M

2009-01-01T23:59:59.000Z

76

Wavefront control in space with MEMS deformable mirrors  

E-Print Network (OSTI)

To meet the high contrast requirement of 1 × 10[superscript ?10] to image an Earth-like planet around a Sun-like star, space telescopes equipped with coronagraphs require wavefront control systems. Deformable mirrors (DMs) ...

Cahoy, Kerri L.

77

Mirror Development for the Cherenkov Telescope Array  

E-Print Network (OSTI)

The Cherenkov Telescope Array (CTA) is a planned observatory for very-high energy gamma-ray astronomy. It will consist of several tens of telescopes of different sizes, with a total mirror area of up to 10,000 square meters. Most mirrors of current installations are either polished glass mirrors or diamond-turned aluminium mirrors, both labour intensive technologies. For CTA, several new technologies for a fast and cost-efficient production of light-weight and reliable mirror substrates have been developed and industrial pre-production has started for most of them. In addition, new or improved aluminium-based and dielectric surface coatings have been developed to increase the reflectance over the lifetime of the mirrors compared to those of current Cherenkov telescope instruments.

Förster, A; Baba, H; Bähr, J; Bonardi, A; Bonnoli, G; Brun, P; Canestrari, R; Chadwick, P; Chikawa, M; Carton, P -H; De Souza, V; Dipold, J; Doro, M; Durand, D; Dyrda, M; Giro, E; Glicenstein, J -F; Hanabata, Y; Hayashida, M; Hrabovski, M; Jeanney, C; Kagaya, M; Katagiri, H; Lessio, L; MANDAT, D; Mariotti, M; Medina, C; Micha?owski, J; Micolon, P; Nakajima, D; Niemiec, J; Nozato, A; Palatka, M; Pareschi, G; Pech, M; Peyaud, B; Pühlhofer, G; Rataj, M; Rodeghiero, G; Rojas, G; Rousselle, J; Sakonaka, R; Schovanek, P; Seweryn, K; Schultz, C; Shu, S; Stinzing, F; Stodulski, M; Teshima, M; Travniczek, P; Van Eldik, C; Vassiliev, V; Wi?niewski, ?; Wörnlein, A; Yoshida, T

2013-01-01T23:59:59.000Z

78

FERMI LARGE AREA TELESCOPE OBSERVATION OF SUPERNOVA REMNANT S147  

Science Conference Proceedings (OSTI)

We present an analysis of gamma-ray data obtained with the Large Area Telescope on board the Fermi Gamma-ray Space Telescope in the region around supernova remnant (SNR) S147 (G180.0-1.7). A spatially extended gamma-ray source detected in an energy range of 0.2-10 GeV is found to coincide with SNR S147. We confirm its spatial extension at >5{sigma} confidence level. The gamma-ray flux is (3.8 {+-} 0.6) Multiplication-Sign 10{sup -8} photons cm{sup -2} s{sup -1}, corresponding to a luminosity of 1.3 Multiplication-Sign 10{sup 34} (d/1.3 kpc){sup 2} erg s{sup -1} in this energy range. The gamma-ray emission exhibits a possible spatial correlation with the prominent H{alpha} filaments of SNR S147. There is no indication that the gamma-ray emission comes from the associated pulsar PSR J0538+2817. The gamma-ray spectrum integrated over the remnant is likely dominated by the decay of neutral {pi} mesons produced through the proton-proton collisions in the filaments. The reacceleration of the pre-existing cosmic rays and subsequent adiabatic compression in the filaments is sufficient to provide the energy density required of high-energy protons.

Katsuta, J.; Uchiyama, Y.; Tanaka, T.; Tajima, H.; Bechtol, K.; Funk, S.; Lande, J. [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); Ballet, J. [Laboratoire AIM, CEA-IRFU/CNRS/Universite Paris Diderot, Service d'Astrophysique, CEA Saclay, 91191 Gif sur Yvette (France); Hanabata, Y. [Department of Physical Sciences, Hiroshima University, Higashi-Hiroshima, Hiroshima 739-8526 (Japan); Lemoine-Goumard, M. [Universite Bordeaux 1, CNRS/IN2p3, Centre d'Etudes Nucleaires de Bordeaux Gradignan, 33175 Gradignan (France); Takahashi, T., E-mail: katsuta@slac.stanford.edu, E-mail: uchiyama@slac.stanford.edu [Institute of Space and Astronautical Science, Japanese Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa 252-5210 (Japan)

2012-06-20T23:59:59.000Z

79

HIGH-PRECISION ASTROMETRY WITH A DIFFRACTIVE PUPIL TELESCOPE  

SciTech Connect

Astrometric detection and mass determination of Earth-mass exoplanets require sub-{mu}as accuracy, which is theoretically possible with an imaging space telescope using field stars as an astrometric reference. The measurement must, however, overcome astrometric distortions, which are much larger than the photon noise limit. To address this issue, we propose to generate faint stellar diffraction spikes using a two-dimensional grid of regularly spaced small dark spots added to the surface of the primary mirror (PM). Accurate astrometric motion of the host star is obtained by comparing the position of the spikes to the background field stars. The spikes do not contribute to scattered light in the central part of the field and therefore allow unperturbed coronagraphic observation of the star's immediate surroundings. Because the diffraction spikes are created on the PM and imaged on the same focal plane detector as the background stars, astrometric distortions affect equally the diffraction spikes and the background stars and are therefore calibrated. We describe the technique, detail how the data collected by the wide-field camera are used to derive astrometric motion, and identify the main sources of astrometric error using numerical simulations and analytical derivations. We find that the 1.4 m diameter telescope, 0.3 deg{sup 2} field we adopt as a baseline design achieves 0.2 {mu}as single measurement astrometric accuracy. The diffractive pupil concept thus enables sub-{mu}as astrometry without relying on the accurate pointing, external metrology, or high-stability hardware required with previously proposed high-precision astrometry concepts.

Guyon, Olivier; Eisner, Josh A.; Angel, Roger; Woolf, Neville J. [Steward Observatory, University of Arizona, Tucson, AZ 85721 (United States); Bendek, Eduardo A.; Milster, Thomas D. [College of Optical Sciences, University of Arizona, Tucson, AZ 85721 (United States); Mark Ammons, S. [Lawrence Livermore National Laboratory, Physics Division L-210, 7000 East Ave., Livermore, CA 94550 (United States); Shao, Michael; Shaklan, Stuart; Levine, Marie; Nemati, Bijan [Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109 (United States); Pitman, Joe [Exploration Sciences, P.O. Box 24, Pine, CO 80470 (United States); Woodruff, Robert A. [2081 Evergreen Avenue, Boulder, CO 80304 (United States); Belikov, Ruslan, E-mail: guyon@naoj.org [NASA Ames Research Center, Moffett Field, CA 94035 (United States)

2012-06-01T23:59:59.000Z

80

The TACTIC atmospheric Cherenkov Imaging telescope  

E-Print Network (OSTI)

The TACTIC $\\gamma$-ray telescope, equipped with a light collector of area $\\sim$9.5m$^2$ and a medium resolution imaging camera of 349-pixels, has been in operation at Mt.Abu, India since 2001. This paper describes the main features of its various subsystems and its overall performance with regard to (a) tracking accuracy of its 2-axes drive system, (b) spot size of the light collector, (c) back-end signal processing electronics and topological trigger generation scheme, (d) data acquisition and control system and (e) relative and absolute gain calibration methodology. Using a trigger field of view of 11$\\times$11 pixels ($\\sim$ 3.4$^\\circ$$\\times3.4^\\circ$), the telescope records a cosmic ray event rate of $\\sim$2.5 Hz at a typical zenith angle of 15$^\\circ$. Monte Carlo simulation results are also presented in the paper for comparing the expected performance of the telescope with actual observational results. The consistent detection of a steady signal from the Crab Nebula above $\\sim$1.2 TeV energy, at a sensitivity level of $\\sim5.0\\sigma$ in $\\sim$25 h, alongwith excellent matching of its energy spectrum with that obtained by other groups, reassures that the performance of the TACTIC telescope is quite stable and reliable. Furthermore, encouraged by the detection of strong $\\gamma$-ray signals from Mrk 501 (during 1997 and 2006 observations) and Mrk 421 (during 2001 and 2005-2006 observations), we believe that there is considerable scope for the TACTIC telescope to monitor similar TeV $\\gamma$-ray emission activity from other active galactic nuclei on a long term basis.

R. Koul; A. K. Tickoo; S. K. Kaul; S. R. Kaul; N. Kumar; K. K. Yadav; N. Bhatt; K. Venugopal; H. C. Goyal; M. Kothari; P. Chandra; R. C. Rannot; V. K. Dhar; M. K. Koul; R. K. Kaul; S. Kotwal; K. Chanchalani; S. Thoudam; N. Chouhan; M. Sharma; S. Bhattacharyya; S. Sahayanathan

2007-06-14T23:59:59.000Z

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


81

An Analog Trigger System for Atmospheric Cherenkov Telescopes  

E-Print Network (OSTI)

Arrays of Cherenkov telescopes typically use multi-level trigger schemes to keep the rate of random triggers from the night sky background low. At a first stage, individual telescopes produce a trigger signal from the pixel information in the telescope camera. The final event trigger is then formed by combining trigger signals from several telescopes. In this poster, we present a possible scheme for the Cherenkov Telescope Array telescope trigger, which is based on the analog pulse information of the pixels in a telescope camera. Advanced versions of all components of the system have been produced and working prototypes have been tested, showing a performance that meets the original specifications. Finally, issues related to integrating the trigger system in a telescope camera and in the whole array will be dealt with.

Barcelo, M; Bigas, O Blanch; Boix, J; Delgado, C; Herranz, D; Lopez-Coto, R; Martinez, G

2013-01-01T23:59:59.000Z

82

Cornell Caltech Atacama Telescope (CCAT): a 25 m aperture telescope above 5000 m altitude  

E-Print Network (OSTI)

Cornell, California Institute of Technology (Caltech), and Jet Propulsion Lab (JPL) have joined together to study development of a 25 meter sub-millimeter telescope (CCAT) on a high peak in the Atacama region of northern Chile, where the atmosphere is so dry as to permit observation at wavelengths as short as 200 micron. The telescope is designed to deliver high efficiency images at that wavelength with a total 1/2 wavefront error of about 10 microns. With a 20 arc min field of view, CCAT will be able to accommodate large format bolometer arrays and will excel at carrying out surveys as well as resolving structures to the 2 arc sec. resolution level. The telescope will be an ideal complement to ALMA. Initial instrumentation will include both a wide field bolometer camera and a medium resolution spectrograph. Studies of the major telescope subsystems have been performed as part of an initial Feasibility Concept Study. Novel aspects of the telescope design include kinematic mounting and active positioning of primary mirror segments, high bandwidth secondary mirror segment motion control for chopping, a Calotte style dome of 50 meter diameter, a mount capable of efficient scanning modes of operation, and some new approaches to panel manufacture. Analysis of telescope performance and of key subsystems will be presented to illustrate the technical feasibility and pragmatic cost of CCAT. Project plans include an Engineering Concept Design phase followed by detailed design and development. First Light is planned for early 2012.

Thomas A. Sebring; Riccardo Giovanelli; Simon Radford; Jonas Zmuidzinas

2006-10-17T23:59:59.000Z

83

Ultra Violet Imaging Telescope (UVIT) on ASTROSAT  

E-Print Network (OSTI)

Ultra Violet Imaging Telescope on ASTROSAT Satellite mission is a suite of Far Ultra Violet (FUV 130 to 180 nm), Near Ultra Violet (NUV 200 to 300 nm) and Visible band (VIS 320 to 550nm) imagers. ASTROSAT is the first multi wavelength mission of INDIA. UVIT will image the selected regions of the sky simultaneously in three channels and observe young stars, galaxies, bright UV Sources. FOV in each of the 3 channels is about 28 arc-minute. Targeted angular resolution in the resulting UV images is better than 1.8 arc-second (better than 2.0 arc-second for the visible channel). Two identical co-aligned telescopes (T1, T2) of Ritchey-Chretien configuration (Primary mirror of 375 mm diameter) collect celestial radiation and feed to the detector system via a selectable filter on a filter wheel mechanism; gratings are available in filter wheels of FUV and NUV channels for slit-less low resolution spectroscopy. The detector system for each of the 3 channels is generically identical. One of the telescopes images in the...

Kumar, Amit; Hutchings, J; Kamath, P U; Kathiravan, S; Mahesh, P K; Murthy, J; S, Nagbhushana; Pati, A K; Rao, M N; Rao, N K; Sriram, S; Tandon, S N

2012-01-01T23:59:59.000Z

84

A Cosmic Ray Telescope For Educational Purposes  

SciTech Connect

Cosmic ray detectors are widely used, for educational purposes, in order to motivate students to the physics of elementary particles and astrophysics. Using a 'telescope' of scintillation counters, the directional characteristics, diurnal variation, correlation with solar activity, can be determined, and conclusions about the composition, origin and interaction of elementary particles with the magnetic field of earth can be inferred. A telescope was built from two rectangular scintillator panels with dimensions: 91.6x1.9x3.7 cm{sup 3}. The scintillators are placed on top of each other, separated by a fixed distance of 34.6 cm. They are supported by a wooden frame which can be rotated around a horizontal axis. Direction is determined by the coincidence of the signals of the two PMTs. Standard NIM modules are used for readout. This device is to be used in the undergraduate nuclear and particle physics laboratory. The design and construction of the telescope as well as some preliminary results are presented.

Voulgaris, G.; Kazanas, S.; Chamilothoris, I. [Department of Physics, National and Kapodistrian University of Athens (Greece)

2010-01-21T23:59:59.000Z

85

Extending the Sensitivity of Air Cerenkov Telescopes  

E-Print Network (OSTI)

Over the last decade, the Imaging Air Cerenkov technique has proven itself to be an extremely powerful means to study very energetic gamma-radiation from a number of astrophysical sources in a regime which is not practically accessible to satellite-based instruments. The further development of this approach in recent years has generally concentrated on increasing the density of camera pixels, increasing the mirror area and using multiple telescopes. Here we present a practical method to substantially improve the sensitivity of Atmospheric Cerenkov Telescopes using wide-field cameras with a relatively course density of photomultiplier tubes. The 2-telescope design considered here is predicted to be more than ~3 times more sensitive than existing/planned arrays in the regime above 300 GeV for continuously emitting sources; up to ~10 times more sensitive for hour-scale emission (relevant for episodic sources, such as AGN); significantly more sensitive in the regime above 10 TeV; and possessing a sky coverage which is roughly an order of magnitude larger than existing instruments. It should be possible to extend this approach for even further improvement in sensitivity and sky coverage.

I. de la Calle Perez; S. D. Biller

2006-02-13T23:59:59.000Z

86

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

E-Print Network (OSTI)

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

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

2013-07-18T23:59:59.000Z

87

The On-Orbit Calibrations for the Fermi Large Area Telescope  

SciTech Connect

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.

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..

2011-11-17T23:59:59.000Z

88

Fermi Large Area Telescope Observations of the Cosmic-Ray Induced  

SciTech Connect

We report on measurements of the cosmic-ray induced {gamma}-ray emission of Earth's atmosphere by the Large Area Telescope onboard the Fermi Gamma-ray Space Telescope. The LAT has observed the Earth during its commissioning phase and with a dedicated Earth-limb following observation in September 2008. These measurements yielded {approx} 6.4 x 10{sup 6} photons with energies > 100 MeV and {approx} 250 hours total livetime for the highest quality data selection. This allows the study of the spatial and spectral distributions of these photons with unprecedented detail. The spectrum of the emission - often referred to as Earth albedo gamma-ray emission - has a power-law shape up to 500 GeV with spectral index {Lambda} = 2.79 {+-} 0.06.

Abdo, A.

2012-02-29T23:59:59.000Z

89

Imaging Atmospheric Cerenkov Telescopes: Techniques and Results  

E-Print Network (OSTI)

The hunt for cosmic TeV particle accelerators is prospering through Imaging Atmospheric Cerenkov Telescopes. We face challenges such as low light levels and MHz trigger rates, and the need to distinguish between particle air showers stemming from primary gamma rays and those due to the hadronic cosmic ray background. Our test beam is provided by the Crab Nebula, a steady accelerator of particles to energies beyond 20 TeV. Highly variable gamma-ray emission, coincident with flares at longer wavelengths, is revealing the particle acceleration mechanisms at work in the relativistic jets of Active Galaxies. These 200 GeV to 20 TeV photons propagating over cosmological distances allow us to place a limit on the infra-red background linked to galaxy formation and, some speculate, to the decay of massive relic neutrinos. Gamma rays produced in neutralino annihilation or the evaporation of primordial black holes may also be detectable. These phenomena and a zoo of astrophysical objects will be the targets of the next generation multi-national telescope facilities.

S. M. Bradbury

2001-01-30T23:59:59.000Z

90

The ROTSE-IIIa Telescope System  

E-Print Network (OSTI)

We report on the current operating status of the ROTSE-IIIa telescope, currently undergoing testing at Los Alamos National Laboratories in New Mexico. It will be shipped to Siding Spring Observatory, Australia, in first quarter 2002. ROTSE-IIIa has been in automated observing mode since early October, 2001, after completing several weeks of calibration and check-out observations. Calibrated lists of objects in ROTSE-IIIa sky patrol data are produced routinely in an automated pipeline, and we are currently automating analysis procedures to compile these lists, eliminate false detections, and automatically identify transient and variable objects. The manual application of these procedures has already led to the detection of a nova that rose over six magnitudes in two days to a maximum detected brightness of m_R~13.9 and then faded two magnitudes in two weeks. We also readily identify variable stars, includings those suspected to be variables from the Sloan Digital Sky Survey. We report on our system to allow public monitoring of the telescope operational status in real time over the WWW.

D. A. Smith; C. Akerlof; M. C. B. Ashley; D. Casperson; G. Gisler; R. Kehoe; S. Marshall; K. McGowan; T. McKay; M. A. Phillips; E. Rykoff; W. T. Vestrand; P. Wozniak; J. Wren

2002-04-24T23:59:59.000Z

91

The ANTARES neutrino telescope: a status report  

E-Print Network (OSTI)

ANTARES is a large volume neutrino telescope currently under construction off La Seyne-sur-mer, France, at 2475m depth. Neutrino telescopes aim at detecting neutrinos as a new probe for a sky study at energies greater than 1 TeV. The detection principle relies on the observation, using photomultipliers, of the Cherenkov light emitted by charged leptons induced by neutrino interactions in the surrounding detector medium. Since late January 2007, the ANTARES detector consists of 5 lines, comprising 75 optical detectors each, connected to the shore via a 40 km long undersea cable. The data from these lines not only allow an extensive study of the detector properties but also the reconstruction of downward going cosmic ray muons and the search for the first upward going neutrino induced muons.The operation of these lines follows on from that of the ANTARES instrumentation line, which has provided data for more than a year on the detector stability and the environmental conditions. The full 12 line detector is planned to be fully operational early 2008.

A. Kouchner; for the Antares collaboration

2007-10-01T23:59:59.000Z

92

Status of the second phase of the MAGIC telescope  

E-Print Network (OSTI)

The MAGIC 17m diameter Cherenkov telescope will be upgraded with a second telescope with advanced photon detectors and ultra fast readout within the year 2007. The sensitivity of MAGIC-II, the two telescope system, will be improved by a factor of 2. In addition the energy threshold will be reduced and the energy and angular resolution will be improved. The design, status and expected performance of MAGIC-II is presented here.

Florian Goebel; for the MAGIC collaboration

2007-09-17T23:59:59.000Z

93

Platek Spaces  

Science Conference Proceedings (OSTI)

The aim of this work is to axiomatize and enhance the recursion theory on monotonic hierarchies of operative spaces developed in [1]. This is to be accomplished by employing a special new variety of operative spaces called Platek spaces. The original ... Keywords: Platek spaces, combinatory algebra, computability, generalised recursion theory, lightface recursion

Lyubomir Ivanov

2000-08-01T23:59:59.000Z

94

Platek Spaces  

Science Conference Proceedings (OSTI)

The aim of this work is to axiomatize and enhance the recursion theory on monotonic hierarchies of operative spaces developed in [1]. This is to be accomplished by employing a special new variety of operative spaces called Platek spaces. The original ... Keywords: Platek spaces, combinatory algebra, computability, generalised recursion theory, lightface recursion

Lyubomir Ivanov

2000-01-01T23:59:59.000Z

95

Novel instrument for Dust Astronomy: Dust Telescope  

Science Conference Proceedings (OSTI)

The analysis of dust particles in space can tell us about their origin and interaction with the space environment that helps understanding the evolution of the solar system and the universe.1 2 There has been a significant advancement in dust detector/analyzer ...

Zoltan Sternovsky; Eberhard Grun; Keith Drake; Jianfeng Xie; Mihaly Horanyi; Ralf Srama; Sascha Kempf; Frank Postberg; Anna Mocker; Siegfried Auer; Harald Kruger

2011-03-01T23:59:59.000Z

96

Dynamic tailoring and tuning for space-based precision optical structures  

E-Print Network (OSTI)

Next-generation space telescopes in NASA's Origins missions require use of advanced imaging techniques to achieve high optical performance with limited launch mass. Structurally-connected Michelson interferometers meet ...

Masterson, Rebecca A. (Rebecca Ann)

2005-01-01T23:59:59.000Z

97

Deployment of a Pair of 3 M telescopes in Utah  

SciTech Connect

Two 3 m telescopes are being installed in Grantsville Utah. They are intended for the testing of various approaches to the implementation of intensity interferometry using Cherenkov Telescopes in large arrays as receivers as well as for the testing of novel technology cameras and electronics for ground based gamma-ray astronomy.

Finnegan, G.; Adams, B.; Butler, K.; Cardoza, J.; Colin, P.; Hui, C. M.; Kieda, D.; Kirkwood, D.; Kress, D.; Kress, M.; LeBohec, S.; McGuire, C.; Newbold, M.; Nunez, P.; Pham, K. [University of Utah, Department of Physics, Salt Lake City, Utah 84112 (United States)

2008-12-24T23:59:59.000Z

98

Searching for Transient Pulses with the ETA Radio Telescope  

Science Conference Proceedings (OSTI)

Array-based, direct-sampling radio telescopes have computational and communication requirements unsuited to conventional computer and cluster architectures. Synchronization must be strictly maintained across a large number of parallel data streams, from ... Keywords: Direct sampling radio telescope array, FPGA cluster computing, RFI mitigation, signal dedispersion

C. D. Patterson; S. W. Ellingson; B. S. Martin; K. Deshpande; J. H. Simonetti; M. Kavic; S. E. Cutchin

2009-01-01T23:59:59.000Z

99

Optimal Networks of Future Gravitational-Wave Telescopes  

E-Print Network (OSTI)

We aim to find the optimal site locations for a hypothetical network of 1-3 triangular gravitational-wave telescopes. We define the following N-telescope figures of merit and construct three corresponding metrics: (a) capability of reconstructing the signal polarization; (b) accuracy in source localization; and (c) accuracy in reconstructing the parameters of a standard binary source. We also define a combined metric that takes into account the three figures of merit with practically equal weight. After constructing a geomap of possible telescope sites, we give the optimal 2-telescope networks for the four figures of merit separately in example cases where the location of the first telescope has been predetermined. We found that the optimal site locations for a second telescope based on the combined metric form a +/-7 deg annulus at an angular distance of ~130 deg from the location of the first telescope. Based on this result we conclude that placing the first telescope to Australia provides the most options ...

Raffai, Peter; Heng, Ik Siong; Kelecsenyi, Nandor; Logue, Josh; Marka, Zsuzsa; Marka, Szabolcs

2013-01-01T23:59:59.000Z

100

Fermi Large Area Telescope Measurements of the Diffuse Gamma-Ray Emission at Intermediate Galactic Latitudes  

SciTech Connect

The diffuse galactic {gamma}-ray emission is produced by cosmic rays (CRs) interacting with the interstellar gas and radiation field. Measurements by the Energetic Gamma-Ray Experiment Telescope (EGRET) instrument on the Compton Gamma-Ray Observatory indicated excess {gamma}-ray emission {ge}1 GeV relative to diffuse galactic {gamma}-ray emission models consistent with directly measured CR spectra (the so-called 'EGRET GeV excess'). The Large Area Telescope (LAT) instrument on the Fermi Gamma-Ray Space Telescope has measured the diffuse {gamma}-ray emission with improved sensitivity and resolution compared to EGRET. We report on LAT measurements for energies 100 MeV to 10 GeV and galactic latitudes 10{sup o} {le} |b| {le} 20{sup o}. The LAT spectrum for this region of the sky is well reproduced by a diffuse galactic {gamma}-ray emission model that is consistent with local CR spectra and inconsistent with the EGRET GeV excess.

Abdo, A.A.; /Naval Research Lab, Wash., D.C.; Ackermann, M.; Ajello, M.; /SLAC; Anderson, B.; Atwood, W.B.; /UC, Santa Cruz; Axelsson, M.; /Stockholm U. /Stockholm U., OKC; Baldini, L.; /INFN, Pisa; Ballet, J.; /DAPNIA, Saclay; Barbiellini, G.; /INFN, Trieste /Trieste U.; Bastieri, D.; /INFN, Padua /Padua U.; Baughman, B.M.; /Taiwan, Natl. Taiwan U. /Ohio State U.; Bechtol, K.; /SLAC; Bellazzini, R.; /INFN, Pisa; Berenji, B.; Blandford, R.D.; Bloom, E.D.; /SLAC; Bonamente, E.; /INFN, Perugia /Perugia U.; Borgland, A.W.; /SLAC; Bregeon, J.; Brez, A.; /INFN, Pisa; Brigida, M.; /Bari U. /INFN, Bari /Ecole Polytechnique /Washington U., Seattle /Bari U. /INFN, Bari /Stanford U., HEPL /KIPAC, Menlo Park /SLAC /IASF, Milan /DAPNIA, Saclay /INFN, Perugia /Perugia U. /Stanford U., HEPL /KIPAC, Menlo Park /SLAC /Naval Research Lab, Wash., D.C. /George Mason U. /NASA, Goddard /Stanford U., HEPL /KIPAC, Menlo Park /SLAC /INFN, Perugia /Perugia U. /Stanford U., HEPL /KIPAC, Menlo Park /SLAC /Montpellier U. /Stockholm U. /Stockholm U., OKC /Royal Inst. Tech., Stockholm /Padua U. /Naval Research Lab, Wash., D.C. /Udine U. /INFN, Trieste /Bari U. /INFN, Bari /Stanford U., HEPL /KIPAC, Menlo Park /SLAC /INFN, Pisa /UC, Santa Cruz /Stanford U., HEPL /KIPAC, Menlo Park /SLAC /CENBG, Gradignan /CENBG, Gradignan /Stanford U., HEPL /KIPAC, Menlo Park /SLAC /Montpellier U. /Bari U. /INFN, Bari /Ecole Polytechnique /Stanford U., HEPL /KIPAC, Menlo Park /SLAC /Udine U. /INFN, Trieste /Hiroshima U. /Stanford U., HEPL /KIPAC, Menlo Park /SLAC /Bari U. /INFN, Bari /INFN, Pisa /INFN, Bari /NASA, Goddard /Maryland U.; /more authors..

2012-04-11T23:59:59.000Z

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101

In-Flight Measurement of the Absolute Energy Scale of the Fermi Large Area Telescope  

Science Conference Proceedings (OSTI)

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.

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..

2012-09-20T23:59:59.000Z

102

Real-time condition assessment of RAPTOR telescope systems  

Science Conference Proceedings (OSTI)

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

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

2010-11-30T23:59:59.000Z

103

A retrospective of the GREGOR solar telescope in scientific literature  

E-Print Network (OSTI)

In this review, we look back upon the literature, which had the GREGOR solar telescope project as its subject including science cases, telescope subsystems, and post-focus instruments. The articles date back to the year 2000, when the initial concepts for a new solar telescope on Tenerife were first presented at scientific meetings. This comprehensive bibliography contains literature until the year 2012, i.e., the final stages of commissioning and science verification. Taking stock of the various publications in peer-reviewed journals and conference proceedings also provides the "historical" context for the reference articles in this special issue of Astronomische Nachrichten/Astronomical Notes.

Denker, C; Feller, A; Arlt, K; Balthasar, H; Bauer, S -M; González, N Bello; Berkefeld, T; Caligari, P; Collados, M; Fischer, A; Granzer, T; Hahn, T; Halbgewachs, C; Heidecke, F; Hofmann, A; Kentischer, T; Klva?a, M; Kneer, F; Lagg, A; Nicklas, H; Popow, E; Puschmann, K G; Rendtel, J; Schmidt, D; Schmidt, W; Sobotka, M; Solanki, S K; Soltau, D; Staude, J; Strassmeier, K G; Volkmer, R; Waldmann, T; Wiehr, E; Wittmann, A D; Woche, M

2012-01-01T23:59:59.000Z

104

Application of an EMCCD Camera for Calibration of Hard X-Ray Telescopes  

SciTech Connect

Recent technological innovations now make it feasible to construct hard x-ray telescopes for space-based astronomical missions. Focusing optics are capable of improving the sensitivity in the energy range above 10 keV by orders of magnitude compared to previously used instruments. The last decade has seen focusing optics developed for balloon experiments and they will soon be implemented in approved space missions such as the Nuclear Spectroscopic Telescope Array (NuSTAR) and ASTRO-H. The full characterization of x-ray optics for astrophysical and solar imaging missions, including measurement of the point spread function (PSF) as well as scattering and reflectivity properties of substrate coatings, requires a very high spatial resolution, high sensitivity, photon counting and energy discriminating, large area detector. Novel back-thinned Electron Multiplying Charge-Coupled Devices (EMCCDs) are highly suitable detectors for ground-based calibrations. Their chip can be optically coupled to a microcolumnar CsI(Tl) scintillator via a fiberoptic taper. Not only does this device exhibit low noise and high spatial resolution inherent to CCDs, but the EMCCD is also able to handle high frame rates due to its controllable internal gain. Additionally, thick CsI(Tl) yields high detection efficiency for x-rays. This type of detector has already proven to be a unique device very suitable for calibrations in astrophysics: such a camera was used to support the characterization of the performance for all NuSTAR optics. Further optimization will enable similar cameras to be improved and used to calibrate x-ray telescopes for future space missions. In this paper, we discuss the advantages of using an EMCCD to calibrate hard x-ray optics. We will illustrate the promising features of this detector solution using examples of data obtained during the ground calibration of the NuSTAR telescopes performed at Columbia University during 2010/2011. Finally, we give an outlook on ongoing development and optimizations, such as the use of single photon counting mode to enhance spectral resolution.

Vogel, J K; Pivovaroff, M J; Nagarkar, V V; Kudrolli, H; Madsen, K K; Koglin, J E; Christensen, F E; Brejnholt, N F

2011-11-08T23:59:59.000Z

105

Studying the Imaging Characteristics of Ultra Violet Imaging Telescope (UVIT) through Numerical Simulations  

E-Print Network (OSTI)

Ultra-Violet Imaging Telescope (UVIT) is one of the five payloads aboard the Indian Space Research Organization (ISRO)'s ASTROSAT space mission. The science objectives of UVIT are broad, extending from individual hot stars, star-forming regions to active galactic nuclei. Imaging performance of UVIT would depend on several factors in addition to the optics, e.g. resolution of the detectors, Satellite Drift and Jitter, image frame acquisition rate, sky background, source intensity etc. The use of intensified CMOS-imager based photon counting detectors in UVIT put their own complexity over reconstruction of the images. All these factors could lead to several systematic effects in the reconstructed images. A study has been done through numerical simulations with artificial point sources and archival image of a galaxy from GALEX data archive, to explore the effects of all the above mentioned parameters on the reconstructed images. In particular the issues of angular resolution, photometric accuracy and photometric...

Srivastava, Mudit K; Tandon, Shyam N

2009-01-01T23:59:59.000Z

106

Space Systems  

Science Conference Proceedings (OSTI)

Oct 20, 2010 ... Three months after installation, vibration was observed in a camera ... Space Station (ISS) experienced a failure with its starboard Solar Array ...

107

The Solar Optical Telescope for the Hinode Mission: An Overview  

E-Print Network (OSTI)

The Solar Optical Telescope (SOT) aboard the Hinode satellite (formerly called Solar-B) consists of the Optical Telescope Assembly (OTA) and the Focal Plane Package (FPP). The OTA is a 50 cm diffraction-limited Gregorian telescope, and the FPP includes the narrow-band (NFI) and wide-band (BFI) filtergraphs, plus the Stokes spectro-polarimeter (SP). SOT provides unprecedented high resolution photometric and vector magnetic images of the photosphere and chromosphere with a very stable point spread function, and is equipped with an image stabilization system that reduces the error to less than 0.01 arcsec rms. Together with the other two instruments on Hinode (the X-Ray Telescope (XRT) and EUV Imaging Spectrometer (EIS)), SOT is poised to address many fundamental questions about solar magneto-hydrodynamics. Note that this is an overview, and the details of the instrument are presented in a series of companion papers.

S. Tsuneta

2007-11-12T23:59:59.000Z

108

Geomagnetic Effects on the Performance of Atmospheric Cerenkov Telescopes  

E-Print Network (OSTI)

Atmospheric Cerenkov telescopes are used to detect electromagnetic showers from primary gamma rays of energy > 300 GeV and to discriminate these from cascades due to hadrons using the shape and orientation of the Cerenkov images. The geomagnetic field affects the development of showers and diffuses and distorts the images. When the component of the field normal to the shower axis is sufficiently large (> 0.4 G) the performance of gamma ray telescopes may be affected.

P. M. Chadwick; K. Lyons; T. J. L. McComb; K. J. Orford; J. L. Osborne; S. M. Rayner; S. E. Shaw; K. E. Turver

1999-06-08T23:59:59.000Z

109

The Sloan Digital Sky Survey Monitor Telescope Pipeline  

E-Print Network (OSTI)

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

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

2006-08-26T23:59:59.000Z

110

Space design  

Science Conference Proceedings (OSTI)

Space stations, Moon bases and Mars bases are artificial habitats intended to support human life in extreme conditions. Their purpose is to pursue human progress and to gain knowledge and experience of the environment surrounding our planet. This research ... Keywords: Human factors, Interior design, Space habitability, Sustainability, Vision

Irene Lia Schlacht; Henrik Birke

2011-06-01T23:59:59.000Z

111

"GiGa": the Billion Galaxy HI Survey -- Tracing Galaxy Assembly from Reionization to the Present  

E-Print Network (OSTI)

In this paper, we review the Billion Galaxy Survey that will be carried out at radio--optical wavelengths to micro--nanoJansky levels with the telescopes of the next decades. These are the Low-Frequency Array, the Square Kilometer Array and the Large Synoptic Survey Telescope as survey telescopes, and the Thirty Meter class Telescopes for high spectral resolution+AO, and the James Webb Space Telescope (JWST) for high spatial resolution near--mid IR follow-up. With these facilities, we will be addressing fundamental questions like how galaxies assemble with super-massive black-holes inside from the epoch of First Light until the present, how these objects started and finished the reionization of the universe, and how the processes of star-formation, stellar evolution, and metal enrichment of the IGM proceeded over cosmic time. We also summarize the high-resolution science that has been done thus far on high redshift galaxies with the Hubble Space Telescope (HST). Faint galaxies have steadily decreasing sizes at fainter fluxes and higher redshifts, reflecting the hierarchical formation of galaxies over cosmic time. HST has imaged this process in great structural detail to zsub-clumps. Finally, we summarize how the 6.5 meter James Webb Space Telescope (JWST) will measure first light, reionization, and galaxy assembly in the near--mid-IR.

R. A. Windhorst; S. H. Cohen; N. P. Hathi; R. A. Jansen; R. E. Ryan Jr

2008-06-12T23:59:59.000Z

112

Scientific Investigations Planned for the Lidar In-Space Technology Experiment (LITE)  

Science Conference Proceedings (OSTI)

The Lidar In-Space Technology Experiment (LITE) is being developed by NASA/Langley Research Center for a series of flights on the space shuttle beginning in 1994. Employing a three-wave-length Nd:YAG laser and a 1-m-diameter telescope, the system ...

M. P. McCormick; D. M. Winker; E. V. Browell; J. A. Coakley; C. S. Gardner; R. M. Hoff; G. S. Kent; S. H. Melfi; R. T. Menzies; C. M. R. Platt; D. A. Randall; J. A. Reagan

1993-02-01T23:59:59.000Z

113

Metric spaces with unique pretangent spaces  

E-Print Network (OSTI)

We find necessary and sufficient conditions under which an arbitrary metric space $X$ has a unique pretangent space at the marked point $a\\in X$. Key words: Metric spaces; Tangent spaces to metric spaces; Uniqueness of tangent metric spaces; Tangent space to the Cantor set.

Dovgoshey, Oleksiy; Kugukaslan, Mehmet

2009-01-01T23:59:59.000Z

114

Fermi Large Area Telescope Observations of the Cygnus Loop Supernova Remnant  

Science Conference Proceedings (OSTI)

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

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

2011-11-08T23:59:59.000Z

115

Atmospheric characterization of cold exoplanets using a 1.5-m coronagraphic space telescope  

E-Print Network (OSTI)

Context: High-contrast imaging is currently the only available technique for the study of the thermodynamical and compositional properties of exoplanets in long-period orbits, comparable to the range from Venus to Jupiter. ...

Maire, A.-L.

116

Using Hubble Space Telescope Imaging of Nuclear Dust Morphology to Rule Out Bars Fueling Seyfert Nuclei  

E-Print Network (OSTI)

If AGN are powered by the accretion of matter onto massive black holes, how does the gas in the host galaxy lose the required angular momentum to approach the black hole? Gas easily transfers angular momentum to stars in strong bars, making them likely candidates. Although ground-based searches for bars in active galaxies using both optical and near infrared surface brightness have not found any excess of bars relative to quiescent galaxies, the searches have not been able to rule out small-scale nuclear bars. To look for these nuclear bars we use HST WFPC2-NICMOS color maps to search for the straight dust lane signature of strong bars. Of the twelve Seyfert galaxies in our sample, only three have dust lanes consistent with a strong nuclear bar. Therefore, strong nuclear bars cannot be the primary fueling mechanism for Seyfert nuclei. We do find that a majority of the galaxies show an spiral morphology in their dust lanes. These spiral arms may be a possible fueling mechanism.

Michael W. Regan; John S. Mulchaey

1999-03-03T23:59:59.000Z

117

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

E-Print Network (OSTI)

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. ...

Roederer, Ian U.

118

RSTN (Radio Solar Telescope Network) observations of the 16 February 1984 cosmic-ray flare  

SciTech Connect

The radio Solar Telescope Network (RSTN) are located at Sagamore Hill (Massachusetts), Palehua (Hawaii), and Learmonth (Australia). A fourth site at San Vito (Italy) will begin making observations in 1986. The RSTN stations monitor the quiet and disturbed Sun at eight fixed frequencies logarithmically spaced from 245-15400 MHz. The radiometer patrols are operated from sunrise to sunset. Data are stored on magnetic tape with 1 second time resolution and archived at the World Data Center A in Boulder for dissemination to the scientific community. The Palehua site became operational in July 1980, followed by Learmonth in August 1980, and Sagamore Hill in October 1981. Thus digitized radiometer observations of the Sun are available for a significant fraction of the maximum phase of solar cycle 21.

Cliver, E.W.; Gentile, L.C.; Wells, G.D.

1987-07-01T23:59:59.000Z

119

A Compact High Energy Camera for the Cherenkov Telescope Array  

E-Print Network (OSTI)

The Compact High Energy Camera (CHEC) is a camera-development project involving UK, US, Japanese and Dutch institutes for the dual-mirror Small-Sized Telescopes (SST-2M) of the Cherenkov Telescope Array (CTA). Two CHEC prototypes, based on different photosensors are funded and will be assembled and tested in the UK over the next ~18 months. CHEC is designed to record flashes of Cherenkov light lasting from a few to a hundred nanoseconds, with typical RMS image width and length of ~0.2 x 1.0 degrees, and has a 9 degree field of view. The physical camera geometry is dictated by the telescope optics: a curved focal surface with radius of curvature 1m and diameter ~35cm is required. CHEC is designed to work with both the ASTRI and GATE SST-2M telescope structures and will include an internal LED flasher system for calibration. The first CHEC prototype will be based on multi-anode photomultipliers (MAPMs) and the second on silicon photomultipliers (SiPMs or MPPCs). The first prototype will soon be installed on the...

Daniel, M K; Berge, D; Buckley, J; Chadwick, P M; Cotter, G; Funk, S; Greenshaw, T; Hidaka, N; Hinton, J; Lapington, J; Markoff, S; Moore, P; Nolan, S; Ohm, S; Okumura, A; Ross, D; Sapozhnikov, L; Schmoll, J; Sutcliffe, P; Sykes, J; Tajima, H; Varner, G S; Vandenbroucke, J; Vink, J; Williams, D

2013-01-01T23:59:59.000Z

120

TeV Dark Matter detection by Atmospheric Cerenkov Telescopes  

E-Print Network (OSTI)

Ground based Atmospheric Cerenkov Telescopes have recently unveiled a TeV gamma-ray signal from the direction of the Galactic Centre. We examine whether these gamma-rays, observed by the VERITAS, CANGAROO-II and HESS collaborations, may arise from annihilations of dark matter particles. Emission from nearby dwarf spheroidals, such as Sagittarius, could provide a test of this scenario.

Francesc Ferrer

2005-05-19T23:59:59.000Z

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


121

Google Sky, WorldWide Telescope & Celestia in the  

E-Print Network (OSTI)

Google Sky, WorldWide Telescope & Celestia in the Undergraduate Non-Science Major Classroom & Lab of Public Outreach Dept.Astronomy & Astrophysics University of Chicago Sky #12;Google Sky, World interactive labs and self-directed modules that utilize new, emerging, software tools, specifically Google Sky

Collar, Juan I.

122

Indirect Search for Dark Matter with the ANTARES Neutrino Telescope  

Science Conference Proceedings (OSTI)

One of the goals of the ANTARES underwater neutrino telescope is the search for dark matter in the universe. In this paper the first results on the search for dark matter in the Sun with ANTARES in its 5 line configuration, as well as sensitivity studies with the full ANTARES detector are presented.

Loucatos, S. [IRFU-SPP, CEA-Saclay, 91191 Gif sur Yvette (France)

2010-02-10T23:59:59.000Z

123

Dynamics of multi-body space interferometers including reaction wheel gyroscopic stiffening effects : structurally connected and electromagnetic formation of flying architectures  

E-Print Network (OSTI)

Space telescopes have the potential to revolutionize astronomy and our search for life-supporting planets beyond our Solar System. Free of atmospheric distortions, they are able to provide a much "clearer" view of the ...

Elias, Laila Mireille, 1977-

2004-01-01T23:59:59.000Z

124

The Timepix Telescope for High Performance Particle Tracking  

E-Print Network (OSTI)

The Timepix particle tracking telescope has been developed as part of the LHCb VELO Upgrade project, supported by the Medipix Collaboration and the AIDA framework. It is a primary piece of infrastructure for the VELO Upgrade project and is being used for the development of new sensors and front end technologies for several upcoming LHC trackers and vertexing systems. The telescope is designed around the dual capability of the Timepix ASICs to provide information about either the deposited charge or the timing information from tracks traversing the 14 x 14mm matrix of 55 x 55 um pixels. The rate of reconstructed tracks available is optimised by taking advantage of the shutter driven readout architecture of the Timepix chip, operated with existing readout systems. Results of tests conducted in the SPS North Area beam facility at CERN show that the telescope typically provides reconstructed track rates during the beam spills of between 3.5 and 7.5 kHz, depending on beam conditions. The tracks are time stamped with 1 ns resolution with an efficiency of above 98% and provide a pointing resolution at the centre of the telescope of 1.6 um . By dropping the time stamping requirement the rate can be increased to 15 kHz, at the expense of a small increase in background. The telescope infrastructure provides CO2 cooling and a flexible mechanical interface to the device under test, and has been used for a wide range of measurements during the 2011-2012 data taking campaigns.

Kazuyoshi Akiba; Per Arne Ronning; Martin van Beuzekom; Vincent van Beveren; Silvia Borghi; Henk Boterenbrood; Jan Buytaert; Paula Collins; Alvaro Dosil Suarez; Raphael Dumps; Lars Eklund; Daniel Esperante; Abraham Gallas; Hamish Gordon; Bas van der Heijden; Christoph Hombach; Daniel Hynds; Malcolm John; Alexander Leflat; Yi Ming Li; Ian Longstaff; Alexander Morton; Noritsugu Nakatsuka; Andre Nomerotski; Chris Parkes; Eliseo Perez Trigo; Richard Plackett; Matthew M. Reid; Pablo Rodriguez Perez; Heinrich Schindler; Tomasz Szumlak; Panagiotis Tsopelas; Carlos Vazquez Sierra; Jaap Velthuis; Michal Wysokinski

2013-04-18T23:59:59.000Z

125

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

E-Print Network (OSTI)

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

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

2008-01-01T23:59:59.000Z

126

Building a better flat-field : an instrumental calibration projector for the Large Synoptic Survey Telescope  

E-Print Network (OSTI)

The Large Synoptic Survey Telescope (LSST) is a next-generation ground-based survey telescope whose science objectives demand photometric precision at the 1% level. Recent efforts towards 1% photometry have advocated in-situ ...

Vaz, Amali L

2011-01-01T23:59:59.000Z

127

Development of a New Laser Beacon for Time Calibration in the ANTARES Neutrino Telescope  

Science Conference Proceedings (OSTI)

The ANTARES collaboration has built a deep sea neutrino telescope in the Mediterranean Sea consisting of a matrix of pressure resistant glass spheres holding large area photomultipliers. The aim of the telescope is to observe cosmic neutrinos through ... Keywords: Deep Sea Instrumentation, Time Calibration Device, Neutrino Telescope, Laser Beacon.

Umberto Emanuele; Diego Real; Fernando Urbano; Juan de Dios Zornoza; Juan Zuniga

2011-10-01T23:59:59.000Z

128

Design of light concentrators for Cherenkov telescope observatories  

E-Print Network (OSTI)

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

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

2013-01-01T23:59:59.000Z

129

Thermal characteristics of a classical solar telescope primary mirror  

E-Print Network (OSTI)

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

Banyal, Ravinder K

2011-01-01T23:59:59.000Z

130

The ANTARES Neutrino Telescope: status and first results  

E-Print Network (OSTI)

Completed in May 2008, the ANTARES neutrino telescope is located in the Mediterranean Sea, 40 km off the coast of Toulon, at a depth of about 2500 m. Consisting of 12 detector lines housing nearly 900 optical modules, the ANTARES telescope is currently the largest neutrino detector in the northern hemisphere. Utilising the Mediterranean Sea as a detecting medium, the detection principle of ANTARES relies on the observation of Cherenkov photons emitted by charged relativistic leptons, produced through neutrino interactions with the surrounding water and seabed, using a 3 dimensional lattice of photomultiplier tubes. In this paper we review the current status of the ANTARES experiment, highlighting some of the results from it's first year of full operation.

Brown, Anthony M

2009-01-01T23:59:59.000Z

131

FERMI LARGE AREA TELESCOPE OBSERVATIONS OF GRB 110625A  

SciTech Connect

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

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

2012-08-01T23:59:59.000Z

132

Mid-Infrared Instrumentation for the European Extremely Large Telescope  

E-Print Network (OSTI)

MIDIR is the proposed thermal/mid-IR imager and spectrograph for the European Extremely Large Telescope (E-ELT). It will cover the wavelength range of 3 to at least 20 microns. Designed for diffraction-limited performance over the entire wavelength range, MIDIR will require an adaptive optics system; a cryogenically cooled system could offer optimal performance in the IR, and this is a critical aspect of the instrument design. We present here an overview of the project, including a discussion of MIDIR's science goals and a comparison with other infrared (IR) facilities planned in the next decade; top level requirements derived from these goals are outlined. We describe the optical and mechanical design work carried out in the context of a conceptual design study, and discuss some important issues to emerge from this work, related to the design, operation and calibration of the instrument. The impact of telescope optical design choices on the requirements for the MIDIR instrument is demonstrated.

S. Kendrew; B. Brandl; R. Lenzen; L. Venema; H. U. Käufl; G. Finger; A. Glasse; R. Stuik

2007-08-23T23:59:59.000Z

133

Observation of GRBs by the MAGIC Telescope, Status and Outlook  

E-Print Network (OSTI)

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.

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

2007-09-10T23:59:59.000Z

134

Minimal Stereoscopic Analysis for Imaging Atmospheric Cherenkov Telescope Arrays  

E-Print Network (OSTI)

The trajectory of a primary gamma-ray detected with an array of at least four atmospheric Cherenkov imaging telescopes can be reconstructed from the shower image centroid positions and geometrical considerations independent of the primary energy. Using only the image centroid positions some cosmic-ray discrimination is also possible. This minimal approach opens the possibility of pushing the analysis threshold to lower values, close to the hardware threshold.

S. LeBohec; C. Duke; P. Jordan

2006-08-15T23:59:59.000Z

135

Tests & Calibration on Ultra Violet Imaging Telescope (UVIT)  

E-Print Network (OSTI)

Ultra Violet Imaging Telescope on ASTROSAT Satellite mission is a suite of Far Ultra Violet (FUV; 130 to 180 nm), Near Ultra Violet (NUV; 200 to 300 nm) and Visible band (VIS; 320 to 550nm) imagers. ASTROSAT is a first multi wavelength mission of INDIA. UVIT will image the selected regions of the sky simultaneously in three channels & observe young stars, galaxies, bright UV Sources. FOV in each of the 3 channels is about 28 arc-minute. Targeted angular resolution in the resulting UV images is better than 1.8 arc-second (better than 2.0 arc-second for the visible channel). Two identical co-aligned telescopes (T1, T2) of Ritchey-Chretien configuration (Primary mirror of 375 mm diameter) collect the celestial radiation and feed to the detector system via a selectable filter on a filter wheel mechanism; gratings are available in the filter wheels of FUV and NUV channels for slit-less low resolution spectroscopy. The detector system for each of the 3 channels is generically identical. One telescope images in ...

Kumar, Amit; Kamath, P U; Postma, Joe; Kathiravan, S; Mahesh, P K; S, Nagbhushana; Navalgund, K H; Rajkumar, N; Rao, M N; Sarma, K S; Sriram, S; Stalin, C S; Tandon, S N

2012-01-01T23:59:59.000Z

136

A Central Laser Facility for the Cherenkov Telescope Array  

E-Print Network (OSTI)

A Central Laser Facility is a system often used in astroparticle experiments based on arrays of fluorescence or Cherenkov light detectors. The instrument is based on a laser source positioned at a certain distance from the array, emitting fast light pulses in the vertical direction with the aim of calibrating the array and/or measuring the atmospheric transmission. In view of the future Cherenkov Telescope Array (CTA), a similar device could provide a calibration of the whole installation, both relative, i.e. each individual telescope with respect to the rest of the array, and absolute, with a precision better than 10%, if certain design requirements are met. Additionally, a precise monitoring of the sensitivity of each telescope can be made on time-scales of days to years. During calibration runs of the central laser facility, all detectors will be pointed towards the same portion of the laser beam at a given altitude. Simulations of the possible configurations of a Central Laser Facility for CTA (varying la...

Gaug, Markus; Cilmo, Marco; Di Pierro, Federico; Tonachini, Aurelio; Vallania, Piero

2013-01-01T23:59:59.000Z

137

Telescope Spectrophotometric and Absolute Flux Calibration, and National Security Applications, Using a Tunable Laser on a Satellite  

E-Print Network (OSTI)

We propose a tunable laser-based satellite-mounted spectrophotometric and absolute flux calibration system, to be utilized by ground- and space-based telescopes. As spectrophotometric calibration may play a significant role in the accuracy of photometric redshift measurement, and photometric redshift accuracy is important for measuring dark energy using SNIa, weak gravitational lensing, and baryon oscillations, a method for reducing such uncertainties is needed. We propose to improve spectrophotometric calibration, currently obtained using standard stars, by placing a tunable laser and a wide-angle light source on a satellite by early next decade (perhaps included in the upgrade to the GPS satellite network) to improve absolute flux calibration and relative spectrophotometric calibration across the visible and near-infrared spectrum. As well as fundamental astrophysical applications, the system proposed here potentially has broad utility for defense and national security applications such as ground target illumination and space communication.

Justin Albert; William Burgett; Jason Rhodes

2006-04-16T23:59:59.000Z

138

Exploring the Dynamic Radio Sky with the Allen Telescope Array  

E-Print Network (OSTI)

Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and SpacePropulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space

Williams, Peter Kelsey George

2012-01-01T23:59:59.000Z

139

Research and Education in Basic Space Science: The Approach Pursued in the UN/ESA Workshops  

E-Print Network (OSTI)

Since 1990, the United Nations in cooperation with the European Space Agency is holding annually a workshop on basic space science for the benefit of the worldwide development of astronomy. These workshops have been held in countries of Asia and the Pacific (India, Sri Lanka), Latin America and the Caribbean (Costa Rica, Colombia, Honduras), Africa (Nigeria), Western Asia (Egypt, Jordan), and Europe (Germany, France). Additional to the scientific benefits of the workshops and the strengthening of international cooperation, the workshops lead to the establishment of astronomical telescope facilities in Colombia, Egypt, Honduras, Jordan, Morocco, Paraguay, Peru, Philippines, Sri Lanka, and Uruguay. The annual UN/ESA Workshops continue to pursue an agenda to network these astronomical telescope facilities through similar research and education programmes. Teaching material and hands-on astrophysics material has been developed for the operation of such astronomical telescope facilities in an university environment.

H. M. K. Al-Naimiy; C. P. Celebre; K. Chamcham; H. S. P. de Alwis; M. C. P. de Carias; H. J. Haubold; A. E. Troche Boggino

2000-02-22T23:59:59.000Z

140

Pulte/Del Webb | Open Energy Information  

Open Energy Info (EERE)

MI Information About Partnership with NREL Partnership with NREL Yes Partnership Type Test & Evaluation Partner Partnering Center within NREL Electricity Resources & Building...

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


141

The SiRi Particle-Telescope System  

E-Print Network (OSTI)

A silicon particle-telescope system for light-ion nuclear reactions is described. In particular, the system is designed to be optimized for level density and gamma-ray strength function measurements with the so-called Oslo method. Eight trapezoidal modules are mounted at 5 cm distance from the target, covering 8 forward angles between theta = 40 and 54 degrees. The thin front dE detectors (130 micrometer) are segmented into eight pads, determining the reaction angle for the outgoing charged ejectile. Guard rings on the thick back E detectors (1550 micrometer) guarantee low leakage current at high depletion voltage.

M. Guttormsen; A. Bürger; T. E. Hansen; N. Lietaer

2011-04-07T23:59:59.000Z

142

Volume 4 Issue 5 www.nasa.gov/centers/stennis May 2009 Under a dry, hot Florida sky, space shuttle  

E-Print Network (OSTI)

Atlantis roars off Launch Pad 39A at NASA's Kennedy Space Center in Florida with its crew of sevenVolume 4 Issue 5 www.nasa.gov/centers/stennis May 2009 Under a dry, hot Florida sky, space shuttle for a rendezvous with NASA's Hubble Space Telescope. The launch was on time at 1:01 p.m. on May 11. With a perfect

143

Qualification and selection of flight diode lasers for the NuSTAR space mission  

Science Conference Proceedings (OSTI)

Reliability and lifetime of diode lasers is critical to space missions. 12Rigorous tests were conducted on diode lasers to qualify them to be deployed on the Nuclear Spectroscopic Telescope Array (NuSTAR) mission. This mission includes a metrology system ...

Patrick Meras; Mark Cooper; R. Peter Dillon; Siamak Forouhar; Ivair Gontijo; Carl Christian Liebe; Andrew Shapiro

2011-03-01T23:59:59.000Z

144

Laser metrology for coherent multi-telescope arrays - Energy ...  

Solar Photovoltaic; Solar ... ENG-48 between the United States Department of Energy and the ... of space objects such as satellites requires an improved ...

145

Challenges in optics for Extremely Large Telescope instrumentation  

E-Print Network (OSTI)

We describe and summarize the optical challenges for future instrumentation for Extremely Large Telescopes (ELTs). Knowing the complex instrumental requirements is crucial for the successful design of 30-60m aperture telescopes. After all, the success of ELTs will heavily rely on its instrumentation and this, in turn, will depend on the ability to produce large and ultra-precise optical components like light-weight mirrors, aspheric lenses, segmented filters, and large gratings. New materials and manufacturing processes are currently under study, both at research institutes and in industry. In the present paper, we report on its progress with particular emphasize on volume-phase-holographic gratings, photochromic materials, sintered silicon-carbide mirrors, ion-beam figuring, ultra-precision surfaces, and free-form optics. All are promising technologies opening new degrees of freedom to optical designers. New optronic-mechanical systems will enable efficient use of the very large focal planes. We also provide exploratory descriptions of "old" and "new" optical technologies together with suggestions to instrument designers to overcome some of the challenges placed by ELT instrumentation.

P. Spanò; F. M. Zerbi; C. J. Norrie; C. R. Cunningham; K. G. Strassmeier; A. Bianco; P. A. Blanche; M. Bougoin; M. Ghigo; P. Hartmann; L. Zago; E. Atad-Ettedgui; B. Delabre; H. Dekker; M. Melozzi; B. Snyders; R. Takke; D. D. Walker

2006-03-28T23:59:59.000Z

146

GRB 090926A AND BRIGHT LATE-TIME FERMI LARGE AREA TELESCOPE GAMMA-RAY BURST AFTERGLOWS  

SciTech Connect

GRB 090926A was detected by both the Gamma-ray Burst Monitor and Large Area Telescope (LAT) instruments on board the Fermi Gamma-ray Space Telescope. Swift follow-up observations began {approx}13 hr after the initial trigger. The optical afterglow was detected for nearly 23 days post trigger, placing it in the long-lived category. The afterglow is of particular interest due to its brightness at late times, as well as the presence of optical flares at T0+10{sup 5} s and later, which may indicate late-time central engine activity. The LAT has detected a total of 16 gamma-ray bursts; nine of these bursts, including GRB 090926A, also have been observed by Swift. Of the nine Swift-observed LAT bursts, six were detected by UVOT, with five of the bursts having bright, long-lived optical afterglows. In comparison, Swift has been operating for five years and has detected nearly 500 bursts, but has only seen {approx}30% of bursts with optical afterglows that live longer than 10{sup 5} s. We have calculated the predicted gamma-ray fluence, as would have been seen by the Burst Alert Telescope (BAT) on board Swift, of the LAT bursts to determine whether this high percentage of long-lived optical afterglows is unique, when compared to BAT-triggered bursts. We find that, with the exception of the short burst GRB 090510A, the predicted BAT fluences indicate that the LAT bursts are more energetic than 88% of all Swift bursts and also have brighter than average X-ray and optical afterglows.

Swenson, C. A.; Roming, P. W. A.; Vetere, L.; Kennea, J. A. [Pennsylvania State University, 525 Davey Lab, University Park, PA 16802 (United States); Maxham, A.; Zhang, B. B.; Zhang, B. [University of Nevada, Las Vegas, Box 454002, 4505 Maryland Parkway, Las Vegas, NV 89154 (United States); Schady, P. [Max-Planck-Institut fuer extraterrestrische Physik, Garching (Germany); Holland, S. T. [Universities Space Research Association, 10227 Wincopin Circle, Suite 500, Columbia, MD 21044 (United States); Kuin, N. P. M.; Oates, S. R.; De Pasquale, M. [The UCL Mullard Space Science Laboratory, Holmbury St Mary, Surrey, RH5 6NT (United Kingdom); Page, K. L., E-mail: cswenson@astro.psu.ed [Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH (United Kingdom)

2010-07-20T23:59:59.000Z

147

Six years of GRB follow up with MITSuME Okayama Telescope  

Science Conference Proceedings (OSTI)

MITSuME Okayama Telescope is an autonomous telescope with a diameter of 50 cm dedicated primarily to follow-up {gamma}-ray bursts. The telescope has successfully been in operation since 2004. We have made 131 observations of {gamma}-ray bursts and submitted 47 reports to GCN circulars. In this article, we present an overview of the instrumentation and scientific results obtained so far.

Yanagisawa, Kenshi; Kuroda, Daisuke; Shimizu, Yasuhiro; Nagayama, Shogo; Toda, Hiroyuki [Okayama Astrophysical Observatory, Kamogata, Asakuchi, Okayama 719-0232 (Japan); Yoshida, Michitoshi [Hiroshima University, Higashi-Hiroshima, Hiroshima, 739-8526 (Japan); Ohta, Kouji [Kyoto University, Sakyo-ku, Kita-shirakawa, Kyoto, 606-8502 (Japan); Kawai, Nobuyuki [Tokyo Institute of Technology, Ookayama, Meguro, Tokyo, 152-8551 (Japan)

2010-10-15T23:59:59.000Z

148

Deployable telescope having a thin-film mirror and metering structure  

Science Conference Proceedings (OSTI)

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.

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

2010-08-24T23:59:59.000Z

149

On the detection of relativistic magnetic monopoles by deep underwater and underice neutrino telescopes  

E-Print Network (OSTI)

I present here some reflections and very speculative remarks on the detection of relativistic magnetic monopoles by currently operating deep underwater/ice neutrino telescopes.

B. K. Lubsandorzhiev

2005-06-13T23:59:59.000Z

150

PROPERTIES OF UMBRAL DOTS AS MEASURED FROM THE NEW SOLAR TELESCOPE DATA AND MHD SIMULATIONS  

SciTech Connect

We studied bright umbral dots (UDs) detected in a moderate size sunspot and compared their statistical properties to recent MHD models. The study is based on high-resolution data recorded by the New Solar Telescope at the Big Bear Solar Observatory and three-dimensional (3D) MHD simulations of sunspots. Observed UDs, living longer than 150 s, were detected and tracked in a 46 minute long data set, using an automatic detection code. A total of 1553 (620) UDs were detected in the photospheric (low chromospheric) data. Our main findings are (1) none of the analyzed UDs is precisely circular, (2) the diameter-intensity relationship only holds in bright umbral areas, and (3) UD velocities are inversely related to their lifetime. While nearly all photospheric UDs can be identified in the low chromospheric images, some small closely spaced UDs appear in the low chromosphere as a single cluster. Slow-moving and long-living UDs seem to exist in both the low chromosphere and photosphere, while fast-moving and short-living UDs are mainly detected in the photospheric images. Comparison to the 3D MHD simulations showed that both types of UDs display, on average, very similar statistical characteristics. However, (1) the average number of observed UDs per unit area is smaller than that of the model UDs, and (2) on average, the diameter of model UDs is slightly larger than that of observed ones.

Kilcik, A.; Yurchyshyn, V. B.; Abramenko, V.; Goode, P. R.; Cao, W. [Big Bear Solar Observatory, Big Bear City, CA 92314 (United States); Rempel, M. [High Altitude Observatory, NCAR, Boulder, CO 80307-3000 (United States); Kitai, R.; Watanabe, H. [Kwasan and Hida Observatories, Kyoto University, Kyoto 607-8417 (Japan)

2012-02-01T23:59:59.000Z

151

SENSITIVITY OF BLIND PULSAR SEARCHES WITH THE FERMI LARGE AREA TELESCOPE  

SciTech Connect

We quantitatively establish the sensitivity to the detection of young to middle-aged, isolated, gamma-ray pulsars through blind searches of Fermi Large Area Telescope (LAT) data using a Monte Carlo simulation. We detail a sensitivity study of the time-differencing blind search code used to discover gamma-ray pulsars in the first year of observations. We simulate 10,000 pulsars across a broad parameter space and distribute them across the sky. We replicate the analysis in the Fermi LAT First Source Catalog to localize the sources, and the blind search analysis to find the pulsars. We analyze the results and discuss the effect of positional error and spin frequency on gamma-ray pulsar detections. Finally, we construct a formula to determine the sensitivity of the blind search and present a sensitivity map assuming a standard set of pulsar parameters. The results of this study can be applied to population studies and are useful in characterizing unidentified LAT sources.

Dormody, M.; Johnson, R. P.; Atwood, W. B.; Belfiore, A.; Razzano, M.; Saz Parkinson, P. M. [Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California at Santa Cruz, Santa Cruz, CA 95064 (United States); Grenier, I. A. [Laboratoire AIM, CEA-IRFU/CNRS/Universite Paris Diderot, Service d'Astrophysique, CEA Saclay, F-91191 Gif sur Yvette (France); Johnson, T. J., E-mail: dormody@scipp.ucsc.edu [National Academy of Sciences, Washington, DC 20001 (United States)

2011-12-01T23:59:59.000Z

152

Science Yield of an Improved Wide Field Infrared Survey Telescope (WFIRST)  

E-Print Network (OSTI)

The Astronomy and Astrophysics Decadal Survey's highest recommended space mission was a Wide-Field Infrared Survey Telescope (WFIRST) to efficiently conduct three kinds of studies: dark energy surveys, exoplanet surveys, and guest surveys. In this paper we illustrate four potential WFIRST payloads that accomplish these objectives and that fully utilize optical and technical advances made since the community input to the Decadal Survey. These improvements, developed by our group, are: unobscured 1.3 or 1.5 m apertures; simultaneous dual focal lengths delivering pixel scales of 0.18" for imaging and 0.38" or 0.45" for slitless spectroscopy; the use of a prism in converging light for slitless spectroscopy; and payload features that allow up to 270 days/year observing the Galactic Bulge. These factors combine to allow WFIRST payloads that provide improved survey rates compared to previous mission concepts. In this report we perform direct comparisons of survey speeds for constant survey depth using our optical an...

Levi, Michael E; Lampton, Michael L; Sholl, Michael J

2011-01-01T23:59:59.000Z

153

Sculpting space through sound  

E-Print Network (OSTI)

How does one experience space? What kind of information do humans collect in the process of constructing space in their mind? How does one begin to understand volume, light, texture, material, smell and sense of space? The ...

Nakagawa, Junko, 1975-

2002-01-01T23:59:59.000Z

154

Space Solar Power Program  

DOE Green Energy (OSTI)

Information pertaining to the Space Solar Power Program is presented on energy analysis; markets; overall development plan; organizational plan; environmental and safety issues; power systems; space transportation; space manufacturing, construction, operations; design examples; and finance.

Arif, H.; Barbosa, H.; Bardet, C.; Baroud, M.; Behar, A.; Berrier, K.; Berthe, P.; Bertrand, R.; Bibyk, I.; Bisson, J.; Bloch, L.; Bobadilla, G.; Bourque, D.; Bush, L.; Carandang, R.; Chiku, T.; Crosby, N.; De Seixas, M.; De Vries, J.; Doll, S.; Dufour, F.; Eckart, P.; Fahey, M.; Fenot, F.; Foeckersperger, S.; Fontaine, J.E.; Fowler, R.; Frey, H.; Fujio, H.; Gasa, J.M.; Gleave, J.; Godoe, J.; Green, I.; Haeberli, R.; Hanada, T.; Ha

1992-08-01T23:59:59.000Z

155

Electric:SpaceCharge  

Science Conference Proceedings (OSTI)

... OOF2: The Manual. Electric:SpaceCharge. Prev, 6.4.1. Material Properties, Next. Name. Electric:SpaceCharge — Spatial charge density. Details. ...

2013-07-05T23:59:59.000Z

156

Exhibit Space Reservation (PDF)  

Science Conference Proceedings (OSTI)

Zip: Country: E-mail Address: Telephone Number: Fax Number: Signature: Date: Please reserve _____ (quantity) 10' x 10' space at $1,100 each. Exhibit space ...

157

Affordable Digital Planetariums with WorldWide Telescope  

E-Print Network (OSTI)

Digital planetariums can provide a broader range of educational experiences than the more classical planetariums that use star-balls. This is because of their ability to project images, content from current research and the 3D distribution of the stars and galaxies. While there are hundreds of planetariums in the country the reason that few of these are full digital is the cost. In collaboration with Microsoft Research (MSR) we have developed a way to digitize existing planetariums for approximately \\$40,000 using software freely available. We describe here how off the shelf equipment, together with MSR's WorldWide Telescope client can provide a rich and truly interactive experience. This will enable students and the public to pan though multi-wavelength full-sky scientific data sets, explore 3d visualizations of our Solar System (including trajectories of millions of minor planets), near-by stars, and the SDSS galaxy catalog.

Rosenfield, Philip; Fay, Jonathan; Carey, Larry; Sayres, Conor; Tofflemire, Benjamin

2010-01-01T23:59:59.000Z

158

Fourier transform method for imaging atmospheric Cherenkov telescopes  

E-Print Network (OSTI)

We propose Fourier transform (FT) method for processing images of extensive air showers (EAS) detected by imaging atmospheric Cherenkov telescopes (IACT) used in the very high energy (VHE) gamma-ray astronomy. The method is based on the discrete Fourier transforms (DFT) on compact Lie groups, and the use of continuous extension of the inverse discrete transforms to approximate the discrete EAS images by continuous EAS brightness distribution functions. Here we describe the FT-method in case of SU(3) group. It allows practical realization of the DFT technique for functions sampled on hexagonal symmetry grids. The proposed method can also be implemented in case of IACT cameras with grids of rectangular symmetry by using the DFT on the SU(2)xSU(2) group. The proposed FT-method is applied to the Monte-Carlo simulated bank of TeV proton and gamma-ray EAS images for a stand-alone telescope. Comparing between the FT-method and the currently used standard method shows that the FT technique allows a better and systematic enhancement of the gamma-ray signal. The relative difference between these two methods becomes more profound especially for `photon poor' images. It suggests that the EAS detection thresholds of IACTs could be effectively reduced with the use of FT technique. This prediction is further supported by a significant noise suppression capability of the method using simple low-pass filters in the image frequency domain. The FT-method allows very deep `tail' (and `height') image cuts, differentiation of images, operations in the image frequency domain, etc., that can be used for development of new effective parameters for the EAS image processing.

A. Atoyan; J. Patera; V. Sahakian; A. Akpherjanian

2004-09-15T23:59:59.000Z

159

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

SciTech Connect

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

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

2011-11-30T23:59:59.000Z

160

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

Science Conference Proceedings (OSTI)

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

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

2012-09-14T23:59:59.000Z

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


161

Large Synoptic Survey Telescope (LSST) Posters from the 215th Meeting of the American Astronomical Society  

DOE Data Explorer (OSTI)

The 8.4 meter Large LSST will survey the entire visible sky deeply in multiple colors every week with its three-billion pixel digital camera, probing the mysteries of Dark Matter and Dark Energy, and opening a movie-like window on objects that change or move rapidly: exploding supernovae, potentially hazardous near-Earth asteroids, and distant Kuiper Belt Objects. [Copied from http://www.lsst.org/lsst/about]

The LSST is still in the design and development phase and will be ready for its scientific work approximately four years after construction starts in Chile. The scientific posters prepared by members of the LSST Project Team for the 215 meeting of the American Astronomical Society in January of 2010 provide a detailed, technical look at the project components. Titles of posters available online include:

  • LSST Observatory and Science Opportunities
  • The LSST: A System of Systems
  • LSST: from Science Drivers to Data Products
  • LSST Education and Public Outreach
  • LSST Operations Simulator
  • Simulating the LSST
  • Inventorying the Solar System with LSST
  • Stellar Population Science with LSST
  • Eclipsing Binary Science with the Large Synoptic Survey Telescope
  • Mapping Milky Way and Local Volume Structure with LSST
  • Galaxy Evolution with LSST
  • Photometric Redshift Performance of LSST
  • LSST Cosmological Probes
  • Probing Dark Energy with Weak Lensing: Ground versus Space
  • Strong Gravitational Lensing with LSST
  • AGN Science with the LSST
  • Exploring the Transient and Variable Universe with LSST
  • Investigation of LSST RR Lyrae Lightcurve Recovery
  • Calibation of LSST Instrument and Data
  • White Dwarf Starts as LSST Calibrators
  • The Camera for LSST and its Focal Plane Array
  • LSST Telescope and Optics Status
  • Data Management R&D for the LSST Project
  • The Spectrum of LSST Data Analysis Challenges: Kiloscale to Petascale
  • Accelerating LSST Source Catalog Simulations with Graphics Processing Units

LSST Project Team Members

162

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

E-Print Network (OSTI)

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

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

2008-02-04T23:59:59.000Z

163

A 610-MHz Galactic Plane Pulsar Search with the Giant Meterwave Radio Telescope  

E-Print Network (OSTI)

We report on the discovery of three new pulsars in the first blind survey of the north Galactic plane (45 < l < 135 ; |b| < 1) with the Giant Meterwave Radio telescope (GMRT) at an intermediate frequency of 610 MHz. The timing parameters, obtained in follow up observations with the Lovell Telescope at Jodrell Bank Observatory and the GMRT, are presented.

B. C. Joshi; M. A. McLaughlin; M. Kramer; A. G. Lyne; D. R. Lorimer; D. A. Ludovici; M. Davies; A. J. Faulkner

2007-10-16T23:59:59.000Z

164

The Universe Viewed in Gamma-Rays 1 Pachmarhi Array of Cerenkov Telescopes  

E-Print Network (OSTI)

The Universe Viewed in Gamma-Rays 1 Pachmarhi Array of Cerenkov Telescopes P.Majumdar, B of Cerenkov Telescopes (PACT) has been designed to search for celestial TeV -rays using the wavefront sampling Atmospheric Cerenkov technique is the only method which has been suc- cessfully used to probe the sky

Enomoto, Ryoji

165

First Light Adaptive Optics System for Large Binocular Telescope S. Espositoa  

E-Print Network (OSTI)

First Light Adaptive Optics System for Large Binocular Telescope S. Espositoa , A. Tozzia , D of the single conjugate Adaptive Optics system to be installed on the LBT telescope. This system will be located optics is supposed to start from the beginning. The Adaptive Optics system to be used in first light

Fini, Luca

166

Before this decade is out: a student project to place a telescope on the internet  

Science Conference Proceedings (OSTI)

This paper describes a student project to place a telescope on the internet: such a telescope can be pointed via a web interface, and images from it displayed on a user's computer. We discuss recent developments in astronomy hardware and computer software ...

Michael P. Rogers

2001-10-01T23:59:59.000Z

167

In Outer Space without a Space Suit?  

E-Print Network (OSTI)

The author proposes and investigates his old idea - a living human in space without the encumbrance of a complex space suit. Only in this condition can biological humanity seriously attempt to colonize space because all planets of Solar system (except the Earth) do not have suitable atmospheres. Aside from the issue of temperature, a suitable partial pressure of oxygen is lacking. In this case the main problem is how to satiate human blood with oxygen and delete carbonic acid gas (carbon dioxide). The proposed system would enable a person to function in outer space without a space suit and, for a long time, without food. That is useful also in the Earth for sustaining working men in an otherwise deadly atmosphere laden with lethal particulates (in case of nuclear, chemical or biological war), in underground confined spaces without fresh air, under water or a top high mountains above a height that can sustain respiration.

Alexander Bolonkin

2008-06-24T23:59:59.000Z

168

Transformations of Grassman Spaces  

E-Print Network (OSTI)

This is a version of a part of the book ``Transformations of Grassman Spaces'' (in progress). We study transformations of Grassman spaces preserving certain geometrical constructions related to buildings. The next part will be devoted to Grassman spaces associated with polar spaces.

Mark Pankov

2004-04-05T23:59:59.000Z

169

Space System Architecture  

E-Print Network (OSTI)

Final Report of SSPARC: the Space Systems, Policy, and Architecture Research Consortium (Thrust II and III)

McManus, Dr. Hugh

170

The Integration of Telescopes, Instruments, and User Interfaces at KPNO and WIYN  

E-Print Network (OSTI)

. The telescopes at KPNO and WIYN use various methods to integrate the control of the telescopes and instruments with the user interfaces. These methods are described, showing the evolution from FORTH based serial connections to ethernet based RPC protocols and then to the WIYN message system and the GWC protocol in use at WIYN. The integration at WIYN is highlighted, including the operation of the message routers. 1. Introduction The six telescopes at Kitt Peak operated by NOAO for KPNO and WIYN use a variety of methods for control of the telescopes, sub-systems, and instruments. There is also a variety of user interfaces used with these systems. We first give an overview of these methods and then describe the integration of these systems. The KPNO telescopes discussed are: Mayall 4 meter, 2.1 meter, Coude Feed, 0.9 meter, and the Burrell-Schmidt. The WIYN telescope is a 3.5 meter telescope operated by NOAO for the WIYN Consortium (University of Wisconsin, Indiana University, Yale U...

B. Marshall; K. Gillies; J. Lewis

1996-01-01T23:59:59.000Z

171

Software Spectral Correlator for the 44-Element Ooty Radio Telescope  

E-Print Network (OSTI)

A Spectral Correlator is the main component of the real time signal processing for a Radio Telescope array. The correlation of signals received at each element with every other element of the array is a classic case of an application requiring a complete graph connectivity between its data sources, as well as a very large number of simple operations to carry out the correlation. Datarates can be extremely large in order to achieve high sensitivities required for the detection of weak celestial signals. Hence, correlators are prime targets for HPC implementations. In this paper, we present the design and implementation of a massively parallel software spectral Correlator for a 44 element array. The correlator handles ~735 MB/s of incoming data from the 44 spatially distributed sources, and concurrently sustains a computational load of ~100 Gflops. We first describe how we partition the large incoming data stream into grouped datasets suited for transport over high speed serial networks, as well as ideal for pr...

Prasad, Peeyush

2011-01-01T23:59:59.000Z

172

Position-sensitive detector for the 6-meter optical telescope  

E-Print Network (OSTI)

The Position-Sensitive Detector (PSD) for photometrical and spectral observation on the 6-meter optical telescope of the Special Astrophysical Observatory (Russia) is described. The PSD consists of a position-sensitive tube, amplifiers of output signals, analog-to-digital converters (ADC) and a digital logic plate, which produces a signal for ADC start and an external strob pulse for reading information by registration system. If necessary, the thermoelectric cooler can be used. The position-sensitive tube has the following main elements: a photocathode, electrodes of inverting optics, a block of microchannel plates (MCP) and a position-sensitive collector of quadrant type. The main parameters of the PSD are the diameter of the sensitive surface is 25 mm, the spatial resolution is better than 100 (\\mu)m in the centre and a little worse on the periphery; the dead time is near 0.5 (\\mu)s; the detection quantum efficiency is defined by the photocathode and it is not less than 0.1, as a rule; dark current is about hundreds of cps, or less, when cooling. PSD spectral sensitivity depends on the type of photocathode and input window material. We use a multialkali photocathode and a fiber or UV-glass, which gives the short- wave cut of 360 nm or 250 nm, respectively.

V. Debur; T. Arkhipova; G. Beskin; V. Plokhotnichenko; M. Pakhomov; M. Smirnova; A. Solin

2003-10-14T23:59:59.000Z

173

The Allen Telescope Array Search for Electrostatic Discharges on Mars  

E-Print Network (OSTI)

The Allen Telescope Array was used to monitor Mars between 9 March and 2 June 2010, over a total of approximately 30 hours, for radio emission indicative of electrostatic discharge. The search was motivated by the report from Ruf et al. (2009) of the detection of non-thermal microwave radiation from Mars characterized by peaks in the power spectrum of the kurtosis, or kurtstrum, at 10 Hz, coinciding with a large dust storm event on 8 June 2006. For these observations, we developed a wideband signal processor at the Center for Astronomy Signal Processing and Electronics Research (CASPER). This 1024-channel spectrometer calculates the accumulated power and power-squared, from which the spectral kurtosis is calculated post-observation. Variations in the kurtosis are indicative of non-Gaussianity in the signal, which can be used to detect variable cosmic signals as well as radio frequency interference (RFI). During the three month period of observations, dust activity occurred on Mars in the form of small-scale d...

Anderson, Marin M; Barott, William C; Bower, Geoffrey C; Delory, Gregory T; de Pater, Imke; Werthimer, Dan

2011-01-01T23:59:59.000Z

174

The Burst Alert Telescope (BAT) on the Swift MIDEX Mission  

E-Print Network (OSTI)

The Burst Alert Telescope (BAT) is one of 3 instruments on the Swift MIDEX spacecraft to study gamma-ray bursts (GRBs). The BAT first detects the GRB and localizes the burst direction to an accuracy of 1-4 arcmin within 20 sec after the start of the event. The GRB trigger initiates an autonomous spacecraft slew to point the two narrow field-of-view (FOV) instruments at the burst location within 20-70 sec so to make follow-up x-ray and optical observations. The BAT is a wide-FOV, coded-aperture instrument with a CdZnTe detector plane. The detector plane is composed of 32,768 pieces of CdZnTe (4x4x2mm), and the coded-aperture mask is composed of approximately 52,000 pieces of lead (5x5x1mm) with a 1-m separation between mask and detector plane. The BAT operates over the 15-150 keV energy range with approximately 7 keV resolution, a sensitivity of approximately 10E-8 erg*cm^-2*s^-1, and a 1.4 sr (half-coded) FOV. We expect to detect >100 GRBs/yr for a 2-year mission. The BAT also performs an all-sky hard x-ray survey with a sensitivity of approximately 2 mCrab (systematic limit) and it serves as a hard x-ray transient monitor.

S. D. Barthelmy; L. M. Barbier; J. R. Cummings; E. E. Fenimore; N. Gehrels; D. Hullinger; H. A. Krimm; C. B. Markwardt; D. M. Palmer; A. Parsons; G. Sato; M. Suzuki; T. Takahashi; M. Tashiro; J. Tueller

2005-07-18T23:59:59.000Z

175

Calibration systems and methods for the ANTARES neutrino telescope  

E-Print Network (OSTI)

The ANTARES neutrino telescope is currently being constructed in the Mediterranean Sea. The complete detector will consist of 12 strings, supplemented by an additional instrumentation line. Nine strings are at present deployed of which five are already connected to the shore and operating. Each string is equipped with 75 Optical Modules (OMs) housing the photomultipliers to detect the Cherenkov light induced by the charged particles produced in neutrino reactions. An accurate measurement of the Cherenkov photon arrival times as well as the positions and orientations of the OMs is required for a precise reconstruction of the direction of the detected neutrinos. For this purpose the ANTARES detector is provided with several system s to facilitate the calibration of the detector. The time calibration is performed using light pulses emitted from LED and laser devices. The positioning is done via acoustic triangulation using hydrophones. Additionally, local tilt angles and the orientations of the modules are measured with a set of tiltmeters and compasses. In this paper, it is demonstrated that the ANTARES time and alignment calibration systems operate successfully in situ. In particular, it is shown that the ANTARES read-out electronics is capable of reaching a sub-nanosecond time resolution.

Felix Fehr; for the ANTARES Collaboration

2007-11-14T23:59:59.000Z

176

Cosmic String constraints from WMAP and the South Pole Telescope  

E-Print Network (OSTI)

The predictions of the inflationary LCDM paradigm match today's high-precision measurements of the cosmic microwave background anisotropy extremely well. The same data put tight limits on other sources of anisotropy. Cosmic strings are a particularly interesting alternate source to constrain. Strings are topological defects, remnants of inflationary-era physics that persist after the big bang. They are formed in a variety of models of inflation, including string theory models such as brane inflation. We assume a "Nambu-Goto" model for strings, approximated by a collection of unconnected segments with zero width, and show that measurements of temperature anisotropy by the South Pole Telescope break a parameter degeneracy in the WMAP data, permitting us to place a strong upper limit on the possible string contribution to the CMB anisotropy: the power sourced by zero-width strings must be <1.75% (95% CL) of the total or the string tension Gmu <1.7x10^{-7}. These limits imply that the best hope for detecting strings in the CMB will come from B-mode polarization measurements at arcminute scales rather than the degree scale measurements pursued for gravitational wave detection.

Cora Dvorkin; Mark Wyman; Wayne Hu

2011-09-22T23:59:59.000Z

177

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

E-Print Network (OSTI)

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

178

Space X-ray Solves Mysteries of Black Holes | Department of Energy  

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

Space X-ray Solves Mysteries of Black Holes Space X-ray Solves Mysteries of Black Holes Space X-ray Solves Mysteries of Black Holes March 13, 2013 - 3:57pm Addthis Space X-ray Solves Mysteries of Black Holes Anne M. Stark Senior Public Information Officer, Lawrence Livermore National Laboratory "We know that black holes have a strong link to their host galaxy." Astrophysicist Bill Craig, a member of the LLNL team An international team including Lawrence Livermore National Laboratory scientists has definitively measured the spin rate of a supermassive black hole for the first time. The findings, made by the two X-ray space observatories, NASA's Nuclear Spectroscopic Telescope Array (NuSTAR) and the European Space Agency's XMM-Newton, solve a long-standing debate about similar measurements in

179

Topological Test Spaces  

E-Print Network (OSTI)

A test space is the set of outcome-sets associated with a collection of experiments. This notion provides a simple mathematical framework for the study of probabilistic theories -- notably, quantum mechanics -- in which one is faced with incommensurable random quantities. In the case of quantum mechanics, the relevant test space, the set of orthonormal bases of a Hilbert space, carries significant topological structure. This paper inaugurates a general study of topological test spaces. Among other things, we show that any topological test space with a compact space of outcomes is of finite rank. We also generalize results of Meyer and Clifton-Kent by showing that, under very weak assumptions, any second-countable topological test space contains a dense semi-classical test space.

Alexander Wilce

2004-05-28T23:59:59.000Z

180

NSLS Committees | Space Committee  

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

Photon Sciences Space Committee Charge Purpose The Photon Sciences Directorate (PS) Space Committee is convened by the PS Chief Operating Officer (COO) on an as-needed basis to...

Note: This page contains sample records for the topic "webb space telescope" from the National Library of EnergyBeta (NLEBeta).
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to obtain the most current and comprehensive results.


181

Small Space Heaters  

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

Small space heaters, also called portable heaters, are typically used when the main heating system is inadequate or when central heating is too costly to install or operate. Space heater capacities...

182

Neutron Tomography and Space  

E-Print Network (OSTI)

Propulsion Laboratory (JPL), uses a small Maxom motor on applications for manipulators in some of their space

Egbert, Hal; Walker, Ronald; Flocchini, R.

2007-01-01T23:59:59.000Z

183

Strongly exponential symmetric spaces  

E-Print Network (OSTI)

We study the exponential map of connected symmetric spaces and characterize, in terms of midpoints and of infinitesimal conditions, when it is a diffeomorphism, generalizing the Dixmier-Saito theorem for solvable Lie groups. We then give a geometric characterization of the (strongly) exponential solvable symmetric spaces as those spaces for which every triangle admits a unique double triangle. This work is motivated by Weinstein's quantization by groupoids program applied to symmetric spaces.

Yannick Voglaire

2013-03-24T23:59:59.000Z

184

Whither design space?  

Science Conference Proceedings (OSTI)

Design space exploration is a long-standing focus in computational design research. Its three main threads are accounts of designer action, development of strategies for amplification of designer action in exploration, and discovery of computational ... Keywords: Design Space Exploration, Knowledge Representation, Search, State Space, Typed Feature Structures

Robert F. Woodbury; Andrew L. Burrow

2006-04-01T23:59:59.000Z

185

Photovoltaic-Concentrator Based Power Beaming For Space Elevator Application  

SciTech Connect

The MClimber team, at the Student Space Systems Fabrication Laboratory of the University of Michigan, has developed a prototype robotic climber for competition in the NASA sponsored Power Beaming Challenge. This paper describes the development of the system that utilizes a simple telescope to deliver an 8 kW beam to a photovoltaic panel in order to power a one kilometer climb. Its unique approach utilizes a precision GPS signal to track the panel. Fundamental systems of the project were implemented using a design strategy focusing on robustness and modularity. Development of this design and its results are presented.

Becker, Daniel E.; Chiang, Richard; Keys, Catherine C.; Lyjak, Andrew W.; Starch, Michael D. [S3FL, University of Michigan, Ann Arbor, MI, 48109 (United States); Nees, John A. [Center for Ultrafast Optical Science-University of Michigan, Ann Arbor, MI, 48109 (United States)

2010-05-06T23:59:59.000Z

186

Green Bank Telescope Studies of Giant Pulses from Millisecond Pulsars  

E-Print Network (OSTI)

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.

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

2005-12-13T23:59:59.000Z

187

Large Synoptic Survey Telescope: Dark Energy Science Collaboration  

E-Print Network (OSTI)

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

LSST Dark Energy Science Collaboration

2012-11-01T23:59:59.000Z

188

User Interface for the Control of the Gemini Telescopes S. S. Smith and K. Gillies  

E-Print Network (OSTI)

on the science detectors is a primary goal. Keywords: Gemini Telescope Control User Interface Tcl/Tk EPICS 1 are being built using Tcl/Tk 1 and are implemented to follow the ESO Graphical User Interface Common

189

User Interface for the Control of the Gemini Telescopes S. S. Smith and K. Gillies  

E-Print Network (OSTI)

detectors is a primary goal. Keywords: Gemini Telescope Control User Interface Tcl/Tk EPICS 1. INTRODUCTION software to cover the requirements of both. Applications are being built using Tcl/Tk1 and are implemented

190

Thin optic surface analysis for high resolution X-ray telescopes  

E-Print Network (OSTI)

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

Akilian, Mireille

2004-01-01T23:59:59.000Z

191

FERMI LARGE AREA TELESCOPE DETECTION OF BRIGHT {gamma}-RAY OUTBURSTS FROM THE PECULIAR QUASAR 4C +21.35  

SciTech Connect

In this paper, we report on the two-year-long Fermi-Large Area Telescope observation of the peculiar blazar 4C +21.35 (PKS 1222+216). This source was in a quiescent state from the start of the science operations of the Fermi Gamma-ray Space Telescope in 2008 August until 2009 September, and then became more active, with gradually increasing flux and some moderately bright flares. In 2010 April and June, 4C +21.35 underwent a very strong GeV outburst composed of several major flares characterized by rise and decay timescales of the order of a day. During the outburst, the GeV spectra of 4C +21.35 displayed a broken power-law form with spectral breaks observed near 1-3 GeV photon energies. We demonstrate that, at least during the major flares, the jet in 4C +21.35 carried a total kinetic luminosity comparable to the total accretion power available to feed the outflow. We also discuss the origin of the break observed in the flaring spectra of 4C +21.35. We show that, in principle, a model involving annihilation of the GeV photons on the He II Lyman recombination continuum and line emission of 'broad-line region' clouds may account for such. However, we also discuss the additional constraint provided by the detection of 4C +21.35 at 0.07-0.4 TeV energies by the MAGIC telescope, which coincided with one of the GeV flares of the source. We argue that there are reasons to believe that the {approx}< TeV emission of 4C +21.35 (as well as the GeV emission of the source, if co-spatial) is not likely to be produced inside the broad-line region zone of highest ionization ({approx}10{sup 17} cm from the nucleus), but instead originates further away from the active center, namely, around the characteristic scale of the hot dusty torus surrounding the 4C +21.35 nucleus ({approx}10{sup 19} cm).

Tanaka, Y. T.; Stawarz, L.; Saito, S.; Ohno, M.; Takahashi, T. [Institute of Space and Astronautical Science, JAXA, 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa 252-5210 (Japan); Thompson, D. J. [NASA Goddard Space Flight Center, Greenbelt, MD 20771 (United States); D'Ammando, F. [IASF Palermo, 90146 Palermo (Italy); Fegan, S. J. [Laboratoire Leprince-Ringuet, Ecole Polytechnique, CNRS/IN2P3, Palaiseau (France); Lott, B.; Escande, L. [Universite Bordeaux 1, CNRS/IN2p3, Centre d'Etudes Nucleaires de Bordeaux Gradignan, 33175 Gradignan (France); Wood, D. L.; Finke, J. [Space Science Division, Naval Research Laboratory, Washington, DC 20375 (United States); Cheung, C. C. [National Research Council Research Associate, National Academy of Sciences, Washington, DC 20001 (United States); Buson, S. [Istituto Nazionale di Fisica Nucleare, Sezione di Padova, I-35131 Padova (Italy); Donato, D. [Center for Research and Exploration in Space Science and Technology (CRESST) and NASA Goddard Space Flight Center, Greenbelt, MD 20771 (United States); Chiang, J. [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); Giroletti, M. [INAF Istituto di Radioastronomia, 40129 Bologna (Italy); Schinzel, F. K. [Max-Planck-Institut fuer Radioastronomie, Auf dem Huegel 69, 53121 Bonn (Germany); Iafrate, G.; Longo, F., E-mail: tanaka@astro.isas.jaxa.jp [Istituto Nazionale di Fisica Nucleare, Sezione di Trieste, I-34127 Trieste (Italy)

2011-05-20T23:59:59.000Z

192

Pulsed Gamma-Rays From the Millisecond Pulsar J0030+0451 with the Fermi Large Area Telescope  

SciTech Connect

We report the discovery of gamma-ray pulsations from the nearby isolated millisecond pulsar PSR J0030+0451 with the Large Area Telescope (LAT) on the Fermi Gamma-ray Space Telescope (formerly GLAST). This discovery makes PSR J0030+0451 the second millisecond pulsar to be detected in gamma-rays after PSR J0218+4232, observed by the EGRET instrument on the Compton Gamma Ray Observatory. The spin-down power {dot E} = 3.5 x 10{sup 33} ergs s{sup -1} is an order of magnitude lower than the empirical lower bound of previously known gamma-ray pulsars. The emission profile is characterized by two narrow peaks, respectively 0.07 {+-} 0.01 and 0.08 {+-} 0.02 wide, separated by 0.44 {+-} 0.02 in phase. The first gamma-ray peak falls 0.15 {+-} 0.01 after the main radio peak. The pulse shape is similar to that of the 'normal' gamma-ray pulsars. An exponentially cut-off power-law fit of the emission spectrum leads to an integral photon flux above 100 MeV of (6.76 {+-} 1.05 {+-} 1.35) x 10{sup -8} cm{sup -2} s{sup -1} with cut-off energy (1.7 {+-} 0.4 {+-} 0.5) GeV. Based on its parallax distance of (300 {+-} 90) pc, we obtain a gamma-ray efficiency L{sub {gamma}}/{dot E} {approx_equal} 15% for the conversion of spin-down energy rate into gamma-ray radiation, assuming isotropic emission.

Abdo, Aous A.; /Naval Research Lab, Wash., D.C.; Ackermann, M.; /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept.; Atwood, W.B.; /UC, Santa Cruz; Axelsson, M. /Stockholm U., OKC /Stockholm U.; Baldini, L.; /INFN, Pisa; Ballet, J.; /DAPNIA, Saclay; Barbiellini, Guido; /INFN, Trieste /Trieste U.; Bastieri, Denis; /INFN, Padua /Padua U.; Battelino, M.; /Stockholm U., OKC /Royal Inst. Tech., Stockholm; Baughman, B.M.; /Ohio State U.; Bechtol, K.; /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept.; Bellazzini, R.; /INFN, Pisa; Berenji, B.; /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept.; Bloom, Elliott D.; /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept.; Bonamente, E.; /INFN, Perugia /Perugia U.; Borgland, A.W.; /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept.; Bregeon, J.; /INFN, Pisa; Brez, A.; /INFN, Pisa; Brigida, M.; /Bari U. /INFN, Bari; Bruel, P.; /Ecole Polytechnique; Burnett, Thompson H.; /Washington U., Seattle /Bari U. /INFN, Bari /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /IASF, Milan /IASF, Milan /DAPNIA, Saclay /INFN, Perugia /Perugia U. /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /George Mason U. /Naval Research Lab, Wash., D.C. /NASA, Goddard /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /INFN, Perugia /Perugia U. /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /LPCE, Orleans /Montpellier U. /Sonoma State U. /Stockholm U., OKC /Royal Inst. Tech., Stockholm /Stockholm U. /ASDC, Frascati /Naval Research Lab, Wash., D.C. /INFN, Trieste /Bari U. /INFN, Bari /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /UC, Santa Cruz /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /CENBG, Gradignan /CENBG, Gradignan /Montpellier U. /Bari U. /INFN, Bari /Stanford U., HEPL /KIPAC, Menlo Park /Stanford U., Phys. Dept. /INFN, Trieste /Hiroshima U.; /more authors..

2011-11-17T23:59:59.000Z

193

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

E-Print Network (OSTI)

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

Bernhard Rothenstein; Ioan Damian

2005-04-04T23:59:59.000Z

194

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

E-Print Network (OSTI)

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.

O. Fors; J. Nunez; A. Richichi

2001-08-27T23:59:59.000Z

195

On the afterglow and host galaxy of GRB 021004: A comprehensive study with the Hubble Space Telescope1  

E-Print Network (OSTI)

Training Network “Gamma-Ray Bursts: An Enigma and a Tool”,z = 2.33). Although this gamma-ray burst (GRB) is one of theobservations — gamma rays: bursts — Based on observations

2004-01-01T23:59:59.000Z

196

Large Synoptic Survey Telescope: From Science Drivers to Reference Design  

SciTech Connect

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

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

2011-10-14T23:59:59.000Z

197

Gymnastics in Phase Space  

SciTech Connect

As accelerator technology advances, the requirements on accelerator beam quality become increasingly demanding. Facing these new demands, the topic of phase space gymnastics is becoming a new focus of accelerator physics R&D. In a phase space gymnastics, the beam's phase space distribution is manipulated and precision tailored to meet the required beam qualities. On the other hand, all realization of such gymnastics will have to obey accelerator physics principles as well as technological limitations. Recent examples of phase space gymnastics include Emittance exchanges, Phase space exchanges, Emittance partitioning, Seeded FELs and Microbunched beams. The emittance related topics of this list are reviewed in this report. The accelerator physics basis, the optics design principles that provide these phase space manipulations, and the possible applications of these gymnastics, are discussed. This fascinating new field promises to be a powerful tool of the future.

Chao, Alexander Wu; /SLAC

2012-03-01T23:59:59.000Z

198

Berkeley Lab Space  

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

Space Space Committee Charter Articles Presentations Feedback Contact Us ANNOUNCEMENTS Space Planning Advisory Committee (SPAC) The LBNL Space Planning Advisory Committee (SPAC) was chartered in January 2010 to help manage the growth, both in the short term as well as long term. Specifically, SPAC will recommend to senior laboratory management policies and procedures for the allocation and utilization of space and opportunities for increased efficiency. (For the complete charter, click here.)We welcome comments and suggestions. Our email is: SPAC@lbl.gov. SPAC (Space Planning Advisory Committee) SPAC Members Telephone Number Email Rich Diamond 510-486-4459 RCDiamond@lbl.gov Rich McClure 510-486-4486 RMMcClure@lbl.gov Diana Attia 510-486-7399 DMAttia@lbl.gov Rebecca Rishell 510-486-6689

199

Tungsten-Rhenium Super Alloy Development for Ultra High ...  

Science Conference Proceedings (OSTI)

Presentation Title, Tungsten-Rhenium Super Alloy Development for Ultra High Temperature Space Fission and Fusion Reactors. Author(s), Jonathan Webb, ...

200

Section D: SPACE HEATING  

U.S. Energy Information Administration (EIA)

2005 Residential Energy Consumption Survey Form EIA-457A (2005)--Household Questionnaire OMB No.: 1905-0092, Expiring May 31, 2008 33 Section D: SPACE HEATING

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


201

Total Space Heat-  

Gasoline and Diesel Fuel Update (EIA)

Released: September, 2008 Total Space Heat- ing Cool- ing Venti- lation Water Heat- ing Light- ing Cook- ing Refrig- eration Office Equip- ment Com- puters Other All Buildings...

202

Total Space Heat-  

Gasoline and Diesel Fuel Update (EIA)

Revised: December, 2008 Total Space Heat- ing Cool- ing Venti- lation Water Heat- ing Light- ing Cook- ing Refrig- eration Office Equip- ment Com- puters Other All Buildings*...

203

Passive solar space heating  

DOE Green Energy (OSTI)

An overview of passive solar space heating is presented indicating trends in design, new developments, performance measures, analytical design aids, and monitored building results.

Balcomb, J.D.

1980-01-01T23:59:59.000Z

204

Total Space Heat-  

Gasoline and Diesel Fuel Update (EIA)

Released: September, 2008 Total Space Heat- ing Cool- ing Venti- lation Water Heat- ing Light- ing Cook- ing Refrig- eration Office Equip- ment Com- puters Other All Buildings*...

205

Total Space Heat-  

Gasoline and Diesel Fuel Update (EIA)

Revised: December, 2008 Total Space Heat- ing Cool- ing Venti- lation Water Heat- ing Light- ing Cook- ing Refrig- eration Office Equip- ment Com- puters Other All Buildings...

206

On Multi-Metric Spaces  

E-Print Network (OSTI)

A Smarandache multi-space is a union of $n$ spaces $A_1,A_2,..., A_n$ with some additional conditions holding. Combining Smarandache multi-spaces with classical metric spaces, the conception of multi-metric space is introduced. Some characteristics of a multi-metric space are obtained and Banach's fixed-point theorem is generalized in this paper.

Linfan Mao

2005-10-22T23:59:59.000Z

207

The drive system of the Major Atmospheric Gamma-ray Imaging Cherenkov Telescope  

E-Print Network (OSTI)

The MAGIC telescope is an imaging atmospheric Cherenkov telescope, designed to observe very high energy gamma-rays while achieving a low energy threshold. One of the key science goals is fast follow-up of the enigmatic and short lived gamma-ray bursts. The drive system for the telescope has to meet two basic demands: (1) During normal observations, the 72-ton telescope has to be positioned accurately, and has to track a given sky position with high precision at a typical rotational speed in the order of one revolution per day. (2) For successfully observing GRB prompt emission and afterglows, it has to be powerful enough to position to an arbitrary point on the sky within a few ten seconds and commence normal tracking immediately thereafter. To meet these requirements, the implementation and realization of the drive system relies strongly on standard industry components to ensure robustness and reliability. In this paper, we describe the mechanical setup, the drive control and the calibration of the pointing, as well as present measurements of the accuracy of the system. We show that the drive system is mechanically able to operate the motors with an accuracy even better than the feedback values from the axes. In the context of future projects, envisaging telescope arrays comprising about 100 individual instruments, the robustness and scalability of the concept is emphasized.

T. Bretz; D. Dorner; R. M. Wagner; P. Sawallisch

2008-10-27T23:59:59.000Z

208

DETECTION AND IMAGING OF THE CRAB NEBULA WITH THE NUCLEAR COMPTON TELESCOPE  

SciTech Connect

The Nuclear Compton Telescope (NCT) is a balloon-borne Compton telescope designed for the study of astrophysical sources in the soft gamma-ray regime (200 keV-20 MeV). NCT's 10 high-purity germanium crossed-strip detectors measure the deposited energies and three-dimensional positions of gamma-ray interactions in the sensitive volume, and this information is used to restrict the initial photon to a circle on the sky using the Compton scatter technique. Thus NCT is able to perform spectroscopy, imaging, and polarization analysis on soft gamma-ray sources. NCT is one of the next generation of Compton telescopes-the so-called compact Compton telescopes (CCTs)-which can achieve effective areas comparable to the Imaging Compton Telescope's with an instrument that is a fraction of the size. The Crab Nebula was the primary target for the second flight of the NCT instrument, which occurred on 2009 May 17 and 18 in Fort Sumner, New Mexico. Analysis of 29.3 ks of data from the flight reveals an image of the Crab at a significance of 4{sigma}. This is the first reported detection of an astrophysical source by a CCT.

Bandstra, M. S.; Bellm, E. C.; Boggs, S. E.; Perez-Becker, D.; Zoglauer, A. [Space Sciences Laboratory, University of California, Berkeley, CA 94720 (United States); Chang, H.-K.; Chiu, J.-L.; Liang, J.-S. [Department of Physics, National Tsing Hua University, Hsinchu 30013, Taiwan (China); Chang, Y.-H.; Liu, Z.-K.; Hung, W.-C. [Department of Physics, National Central University, Taoyuan 32001, Taiwan (China); Huang, M.-H. A. [Department of Energy Engineering, National United University, Miaoli 36003, Taiwan (China); Chiang, S. J. [Department of Electrical Engineering, National United University, Miaoli 36003, Taiwan (China); Run, R.-S. [Department of Electronic Engineering, National United University, Miaoli 36003, Taiwan (China); Lin, C.-H. [Institute of Physics, Academia Sinica, Taipei 11529, Taiwan (China); Amman, M.; Luke, P. N. [Lawrence Berkeley National Laboratory, Berkeley, CA 94720 (United States); Jean, P.; Von Ballmoos, P. [Centre d'Etude Spatiale des Rayonnements (CESR), 31028 Toulouse Cedex 4 (France); Wunderer, C. B., E-mail: bandstra@ssl.berkeley.edu [Deutsches Elektronen-Synchrotron (DESY), Notkestr. 85, 22607 Hamburg (Germany)

2011-09-01T23:59:59.000Z

209

Space bounds for resolution  

Science Conference Proceedings (OSTI)

We introduce a new way to measure the space needed in a resolution refutation of a CNF formula in propositional logic. With the former definition [6] the space required for the resolution of any unsatisfiable formula in CNF is linear in the number of ...

Juan Luis Esteban; Jacobo Torán

1999-03-01T23:59:59.000Z

210

The metaplastic virtual spaces  

Science Conference Proceedings (OSTI)

Virtual reality systems need new metaphors for their communication. This paper presents a fuzzy enhanced semantic virtual space model. The application of the model tries to improve its conceptualization and definition of a new virtual world system. The ... Keywords: fuzzy, metaphysical, semantic spaces, synaesthesia, virtual reality

Gianluca Mura

2007-09-01T23:59:59.000Z

211

Atoms for space  

SciTech Connect

Nuclear technology offers many advantages in an expanded solar system space exploration program. These cover a range of possible applications such as power for spacecraft, lunar and planetary surfaces, and electric propulsion; rocket propulsion for lunar and Mars vehicles; space radiation protection; water and sewage treatment; space mining; process heat; medical isotopes; and self-luminous systems. In addition, space offers opportunities to perform scientific research and develop systems that can solve problems here on Earth. These might include fusion and antimatter research, using the Moon as a source of helium-3 fusion fuel, and manufacturing perfect fusion targets. In addition, nuclear technologies can be used to reduce risk and costs of the Space Exploration Initiative. 1 fig.

Buden, D.

1990-10-01T23:59:59.000Z

212

Perspectives of a mid-rapidity dimuon program at the RHIC: a novel and compact muon telescope detector  

E-Print Network (OSTI)

Telescope Detector L. Ruan Brookhaven National Laboratory,Connecticut 06520 Z. Xu Brookhaven National Laboratory,York 11973 K. Asselta Brookhaven National Laboratory, Upton,

Ruan, L.

2010-01-01T23:59:59.000Z

213

South Pole Telescope helps Argonne scientists study earliest ages of the  

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

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

214

Metrology for x-ray telescope mirrors in a vertical configuration  

Science Conference Proceedings (OSTI)

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.

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

1995-09-01T23:59:59.000Z

215

Neutron Star Astronomy in the era of the European Extremely Large Telescope  

Science Conference Proceedings (OSTI)

About 25 isolated neutron stars (INSs) are now detected in the optical domain, mainly thanks to the HST and to VLT-class telescopes. The European Extremely Large Telescope(E-ELT) will yield {approx}100 new identifications, many of which from the follow-up of SKA, IXO, and Fermi observations. Moreover, the E-ELT will allow to carry out, on a much larger sample, INS observations which still challenge VLT-class telescopes, enabling studies on the structure and composition of the NS interior, of its atmosphere and magnetosphere, as well as to search for debris discs. In this contribution, I outline future perspectives for NS optical astronomy with the E-ELT.

Mignani, Roberto P. [Mullard Space Science Laboratory-University College London (United Kingdom)

2011-09-21T23:59:59.000Z

216

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

E-Print Network (OSTI)

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

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

2005-11-30T23:59:59.000Z

217

The Trigger System of the H.E.S.S. Telescope Array  

E-Print Network (OSTI)

H.E.S.S. -- The High Energy Stereoscopic System-- is a new system of large atmospheric Cherenkov telescopes for GeV/TeV Gamma-ray astronomy. This paper describes the trigger system of H.E.S.S. with emphasis on the multi-telescope array level trigger. The system trigger requires the simultaneous detection of air-showers by several telescopes at the hardware level. This requirement allows a suppression of background events which in turn leads to a lower system energy threshold for the detection of Gamma-rays. The implementation of the H.E.S.S. trigger system is presented along with data taken to characterise its performance.

S. Funk; G. Hermann; J. Hinton; D. Berge; K. Bernloehr; W. Hofmann; P. Nayman; F. Toussenel; P. Vincent

2004-08-20T23:59:59.000Z

218

KM3NeT:a large underwater neutrino telescope in the Mediterranean Sea  

E-Print Network (OSTI)

High energy neutrinos produced in astrophysical processes will allow for a new way of studying the universe. In order to detect the expected flux of high energy neutrinos from specific astrophysical sources, neutrino telescopes of a scale of a km^3 of water will be needed. A Northern Hemisphere detector is being proposed to be sited in a deep area of the Mediterranean Sea. This detector will provide complimentary sky coverage to the IceCube detector being built at the South Pole. The three neutrino telescope projects in the Mediterranean (ANTARES, NEMO and NESTOR) are partners in an effort to design, and build such a km^3 size neutrino telescope, the KM3NeT. The EU is funding a 3-year Design Study; the status of the Design Study is presented and some technical issues are discussed.

P. A. Rapidis; for the KM3NeT consortium

2008-03-17T23:59:59.000Z

219

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

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

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

220

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

SciTech Connect

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.

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

2008-06-02T23:59:59.000Z

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


221

Tangent spaces to metric spaces and to their subspaces  

E-Print Network (OSTI)

We investigate a tangent space at a point of a general metric space and metric space valued derivatives. The conditions under which two different subspace of a metric space have isometric tangent spaces in a common point of these subspaces are completely determinated.

Dovgoshey, O

2009-01-01T23:59:59.000Z

222

National Aeronautics and Space Administration Space Shuttle Era Facts  

E-Print Network (OSTI)

System (STS), began its flight career with Columbia roaring off Launch Pad 39A at NASA's Kennedy SpaceNational Aeronautics and Space Administration NASAfacts Space Shuttle Era Facts NASA's shuttle fleet achieved numerous firsts and opened up space to more people than ever before during the Space

223

Neutrino telescopes as a probe of active and sterile neutrino mixings  

E-Print Network (OSTI)

If the ultrahigh-energy (UHE) neutrino fluxes produced from a distant astrophysical source can be measured at a km^3-size neutrino telescope, they will provide a promising way to help determine the flavor mixing pattern of three active neutrinos. Considering the conventional UHE neutrino source with the flavor ratio \\phi_e : \\phi_\\mu : \\phi_\\tau = 1 : 2 : 0, I show that \\phi^D_e : \\phi^D_\\mu : \\phi^D_\\tau = (1 -2 \\Delta) : (1 +\\Delta) : (1 +\\Delta) holds at the detector of a neutrino telescope, where \\Delta characterizes the effect of \\mu-\\tau symmetry breaking (i.e., \\theta_13 \

Xing, Zhi-zhong

2007-01-01T23:59:59.000Z

224

Neutrino telescopes as a probe of active and sterile neutrino mixings  

E-Print Network (OSTI)

If the ultrahigh-energy (UHE) neutrino fluxes produced from a distant astrophysical source can be measured at a km^3-size neutrino telescope, they will provide a promising way to help determine the flavor mixing pattern of three active neutrinos. Considering the conventional UHE neutrino source with the flavor ratio \\phi_e : \\phi_\\mu : \\phi_\\tau = 1 : 2 : 0, I show that \\phi^D_e : \\phi^D_\\mu : \\phi^D_\\tau = (1 -2 \\Delta) : (1 +\\Delta) : (1 +\\Delta) holds at the detector of a neutrino telescope, where \\Delta characterizes the effect of \\mu-\\tau symmetry breaking (i.e., \\theta_13 \

Zhi-zhong Xing

2007-11-27T23:59:59.000Z

225

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

E-Print Network (OSTI)

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

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

2005-02-24T23:59:59.000Z

226

On globally Symmetric Finsler spaces  

E-Print Network (OSTI)

The paper consider the symmetric of Finsler spaces. We give some conditions about globally symmetric Finsler spaces. Then we prove that these spaces can be written as a coset space of Lie group with an invariant Finsler metric. Finally, we prove that such a space must be Berwaldian

Khatamy, R Chavosh

2011-01-01T23:59:59.000Z

227

Simplified Space Conditioning  

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

Simplified Space Conditioning Simplified Space Conditioning Duncan Prahl, RA IBACOS, Inc. Building America Technical Update April 29, 2013 Simplified Space Conditioning Rethinking HVAC Design * Traditional Method - Assume envelope losses dictate the load - Room by room load analysis - Pick Equipment and distribute to meet the load in each room * New Method - Consider how the occupants live in the building - Seriously consider internal gains in both heating and cooling - Consider ventilation strategy - Design system Simplified Space Conditioning If you are: * A production builder * Participating in "above code" programs * Following ACCA Manual RS or ASHRAE 55 * Need to prove "delivering heat to each habitable room" * Concerned about litigation * Play it safe, Use Manual J, S & D and condition every

228

Live From Outer Space  

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

Live from Outer Space: How Cells Influence the Growth of Nanostructures Live from Outer Space: How Cells Influence the Growth of Nanostructures Far above the heads of Earthlings, arrays of single-cell creatures embedded in nanostructures ride on the International Space Station (courtesy of Sandia National Laboratories and the University of New Mexico, NASA, and the U.S. Air Force) to test whether nanostructures whose formations were directed by yeast and other single cells can create more secure homes for their occupants-even in the vacuum and radiation of outer space-than those created by more standard chemical procedures. Cheap, tiny, and very lightweight sensors of chemical or biological agents could be made from long-lived cells that require no upkeep, yet sense and then communicate effectively with each other and their external

229

Total Space Heat-  

Gasoline and Diesel Fuel Update (EIA)

Survey: Energy End-Use Consumption Tables Total Space Heat- ing Cool- ing Venti- lation Water Heat- ing Light- ing Cook- ing Refrig- eration Office Equip- ment Com- puters Other...

230

Space Mapping - Optimization Online  

E-Print Network (OSTI)

Thus, we can usec oP–to locally minimize the surrogatecoP that the space. mappingP provides for the fine model“.An alternative surrogate introduced byMadsen ...

231

Beam Space Propulsion  

E-Print Network (OSTI)

Author offers a revolutionary method non-rocket transfer of energy and thrust into Space with distance of millions kilometers. The author has developed theory and made the computations. The method is more efficient than transmission of energy by high-frequency waves. The method may be used for space launch and for acceleration the spaceship and probes for very high speeds, up to relativistic speed by current technology. Research also contains prospective projects which illustrate the possibilities of the suggested method.

Alexander Bolonkin

2007-01-04T23:59:59.000Z

232

Space Weather 101  

Science Conference Proceedings (OSTI)

This report describes the basic physical concepts associated with space weather that pertain to the effects on high-voltage power transmission systems. Space weather is an extremely complex and multi-faceted phenomenon. To focus on power grid–related effects, the report addresses coronal mass ejections, which are known to be the most important driver of large geomagnetically induced currents, and describes ongoing research that is being conducted to better understand, predict, and mitigate the ...

2012-11-30T23:59:59.000Z

233

Verification and operation of adaptive materials in space.  

SciTech Connect

Piezoelectric polymers based on polyvinylidene fluoride (PVDF) are of interest as smart materials for novel space-based telescope applications. Dimensional adjustments of adaptive thin polymer films are achieved via controlled charge deposition. Predicting their long-term performance requires a detailed understanding of the piezoelectric property changes that develop during space environmental exposure. The overall materials performance is governed by a combination of chemical and physical degradation processes occurring in low Earth orbit as established by our past laboratory-based materials performance experiments (see report SAND 2005-6846). Molecular changes are primarily induced via radiative damage, and physical damage from temperature and atomic oxygen exposure is evident as depoling, loss of orientation and surface erosion. The current project extension has allowed us to design and fabricate small experimental units to be exposed to low Earth orbit environments as part of the Materials International Space Station Experiments program. The space exposure of these piezoelectric polymers will verify the observed trends and their degradation pathways, and provide feedback on using piezoelectric polymer films in space. This will be the first time that PVDF-based adaptive polymer films will be operated and exposed to combined atomic oxygen, solar UV and temperature variations in an actual space environment. The experiments are designed to be fully autonomous, involving cyclic application of excitation voltages, sensitive film position sensors and remote data logging. This mission will provide critically needed feedback on the long-term performance and degradation of such materials, and ultimately the feasibility of large adaptive and low weight optical systems utilizing these polymers in space.

Dargaville, Tim Richard; Elliott, Julie M.; Jones, Gary D.; Celina, Mathias Christopher

2006-12-01T23:59:59.000Z

234

Space Weather Effects on Imaging Detectors in Low Earth Orbit  

E-Print Network (OSTI)

The objective of this research is the statistical study of space weather e ects on im- age detectors in Low Earth Orbit. The Hubble Space Telescope is used as a resource for acquiring proton a ected images for statistical analysis. For the purpose of the present work, the space weather environment will consist of cosmic as well as solar proton particles. The proton occurrences evident in images from the Hubble Charge Coupled Device (CCD) have been used to calculate the probability of proton events, which is related to the local space weather particle ux. The proton particles transfer energy to the CCD silicon, which ultimately results in measured signal that is not originating from photon illumination. The signal due to the proton interactions is rst separated from the noise contribution and subsequently used in the determi- nation of a pulse height probability distribution. Separation of the noise from the proton events also leads to the measurement of proton streak lengths and orientations along with the associated probability distributions. The directionality of the space weather environment in Low Earth Orbit is examined using the distribution of proton streak angles. Statistics found from the Hubble are also used as a starting point for simulations that create synthetic proton signal images. The distributions resulting from the Hubble CCD analysis give the probability of the: number of proton events, which is related to the ux of the space weather protons; energy of proton events, which allows estimates of damaging proton interactions; length of proton streaks on the CCD, which shows the relative probability of a long traversing proton event; angle of proton event, which indicates the directionality of the space weather environment.

Johnson, Adam Alan

2010-08-01T23:59:59.000Z

235

Search for ultra-high energy photons using Telescope Array surface detector  

SciTech Connect

We search for ultra-high energy photons by analyzing geometrical properties of shower fronts of events registered by the Telescope Array surface detector. By making use of an event-by-event statistical method, we derive an upper limit on the absolute flux of primary photons with energies above 10{sup 19} eV.

Rubtsov, G. I.; Troitsky, S. V. [Institute for Nuclear Research of the Russian Academy of Sciences, Moscow, 117312 (Russian Federation); Ivanov, D.; Stokes, B. T. [Rutgers - State University of New Jersey, Piscataway (United States); Thomson, G. B. [University of Utah, High Energy Astrophysics Institute, Salt Lake City, Utah (United States)

2011-09-22T23:59:59.000Z

236

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

E-Print Network (OSTI)

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

California at Santa Cruz, University of

237

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

E-Print Network (OSTI)

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

Hörandel, Jörg R.

238

Focal plane instrumentation for the Wide-Field X-ray Telescope  

E-Print Network (OSTI)

The three X-ray imaging focal planes of the Wide-Field X-ray Telescope (WFXT) Mission will each have a field of view up to 1 degree square, pixel pitch smaller than 1 arcsec, excellent X-ray detection efficiency and spectral ...

Bautz, Marshall W.

239

Detection and Imaging of the Crab Nebula with the Nuclear Compton Telescope  

E-Print Network (OSTI)

The Nuclear Compton Telescope (NCT) is a balloon-borne Compton telescope designed for the study of astrophysical sources in the soft gamma-ray regime (200 keV--20 MeV). NCT's ten high-purity germanium crossed-strip detectors measure the deposited energies and three-dimensional positions of gamma-ray interactions in the sensitive volume, and this information is used to restrict the initial photon to a circle on the sky using the Compton scatter technique. Thus NCT is able to perform spectroscopy, imaging, and polarization analysis on soft gamma-ray sources. NCT is one of the next generation of Compton telescopes --- so-called compact Compton telescopes (CCTs) --- which can achieve effective areas comparable to COMPTEL's with an instrument that is a fraction of the size. The Crab Nebula was the primary target for the second flight of the NCT instrument, which occurred on 17--18 May 2009 in Fort Sumner, New Mexico. Analysis of 29.3 ks of data from the flight reveals an image of the Crab at a significance of 4-si...

Bandstra, M S; Boggs, S E; Perez-Becker, D; Zoglauer, A; Chang, H -K; Chiu, J -L; Liang, J -S; Chang, Y -H; Liu, Z -K; Hung, W -C; Huang, M -H A; Chiang, S J; Run, R -S; Lin, C -H; Amman, M; Luke, P N; Jean, P; von Ballmoos, P; Wunderer, C B

2011-01-01T23:59:59.000Z

240

Parabolic John-Nirenberg spaces  

E-Print Network (OSTI)

We introduce a parabolic version of John-Nirenberg space with exponent $p$ and show that it is contained in local weak-$L^p$ spaces.

Berkovits, Lauri

2011-01-01T23:59:59.000Z

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


241

Wide Field Hard X-ray Survey Telescope: ProtoEXIST1  

E-Print Network (OSTI)

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

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

2007-09-17T23:59:59.000Z

242

University of Michigan space Physics  

E-Print Network (OSTI)

below). Light from selected regions of the atmosphere is collected by the telescopes, that are fiber-optically (TOF) System. As the ions are collected, they first pass through the ESA. The ESA acts as an energy filtered, but before they pass into the TOF system, they are accelerated through a carbon foil. As the ion

Eustice, Ryan

243

Earth, Space Sciences  

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

Earth, Space Sciences Earth, Space Sciences /science-innovation/_assets/images/icon-science.jpg Earth, Space Sciences National security depends on science and technology. The United States relies on Los Alamos National Laboratory for the best of both. No place on Earth pursues a broader array of world-class scientific endeavors. Climate, Ocean and Sea Ice Modeling (COSIM)» Earth A team of scientists is working to understand how local changes in hydrology might bring about major changes to the Arctic landscape, including the possibility of a large-scale carbon release from thawing permafrost. Bryan Travis, an expert in fluid dynamics, is author of the Mars global hydrology numerical computer model, or MAGHNUM, used for calculating heat and fluid transport phenomena. (MAGHNUM was previously

244

Design and Application of an Electronic Logbook for Space System Integration and Test Operations  

Science Conference Proceedings (OSTI)

In the highly technological aerospace world paper is still widely used to document space system integration and test (I&T) operations. E-Logbook is a new technology designed to substitute the most commonly used paper logbooks in space system I&T, such as the connector mate/demate logbook, the flight hardware and flight software component installation logbook, the material mix record logbook and the electronic ground support equipment validation logbook. It also includes new logbook concepts, such as the shift logbook, which optimizes management oversight and the shift hand-over process, and the configuration logbook, which instantly reports on the global I&T state of the space system before major test events or project reviews. The design of E-Logbook focuses not only on a reliable and efficient relational database, but also on an ergonomic human-computer interactive (HCI) system that can help reduce human error and improve I&T management and oversight overall. E-Logbook has been used for the I&T operation of the Gamma-ray Large Area Space Telescope (GLAST) Large Area Telescope (LAT) at the Stanford Linear Accelerator Center (SLAC). More than 41,000 records have been created for the different I&T logbooks, with no data having been corrupted or critically lost. 94% of the operators and 100% of the management exposed to E-Logbook prefer it to paper logbooks and recommend its use in the aerospace industry.

Kavelaars, Alicia T.; /SLAC /Stanford U., Dept. Aeronaut. Astronaut.

2006-10-10T23:59:59.000Z

245

International Space Station Again  

E-Print Network (OSTI)

For the fifth time in 2 1/2 years, the International Space Station (ISS) had to execute a collision avoidance maneuver in early April to ensure a safe miss distance for a piece of orbital debris. As solar activity increases during the next few years, the frequency of ISS collision avoidance might increase as many hundreds of resident space objects drift down through the ISS orbital regime. The subject of concern in late March 2011 was a fragment from Cosmos 2251, the Russian communications satellite which had accidentally collided with the U.S. Iridium 33 communications satellite in February 2009, producing more than

Iss Airlock Shields; A Note On Active; A Publication Of

2011-01-01T23:59:59.000Z

246

Demystifying White Spaces Xuemin Hongl  

E-Print Network (OSTI)

white spaces. The term "white space" refers to "spatial white space" in the rest of this paper cellular (planned) networks [9] and ad-hoc networks [10]. Different from previous works, in this paper weDemystifying White Spaces Xuemin Hongl , Cheng-Xiang Wangl , John Thompson2 , and Yan Zhang3 1Joint

Wang, Cheng-Xiang

247

Programs on Product Spaces  

Science Conference Proceedings (OSTI)

We study program states that are described as tuples, i.e., product state spaces. We show how to add program variables and assignment notation to simply typed lambda calculus in order to describe functions, relations and predicate transformers on such ...

Ralph Back; Joakim Wright von

1997-12-01T23:59:59.000Z

248

Capacity on Finsler Spaces  

E-Print Network (OSTI)

Here, the concept of electric capacity on Finsler spaces is introduced and the fundamental conformal invariant property is proved, i.e. the capacity of a compact set on a connected non-compact Finsler manifold is conformal invariant. This work enables mathematicians and theoretical physicists to become more familiar with the global Finsler geometry and one of its new applications.

Bidabad, B

2009-01-01T23:59:59.000Z

249

2011 Confined Space Program Update  

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

Confined Space Entry Program Update Confined Space Entry Program Update IMPORTANT: After reading this document, click the "Get Course Credit" link at the bottom of the page. You will then log in to the EHS training system using your LDAP to get course credit. LBNL's confined space entry program was substantially improved this year. Several new features have been included which improve overall safety for Confined Space Entrants and better align the confined space entry program with the OSHA requirements. As an Activity Lead, Confined Space Entrant or Entry Supervisor, you should be aware of the following: We improved the procedures for safely working in confined spaces. Please review the new Chapter 34 in Publication 3000. Additionally, we have a new planning tool known as the confined space inventory which is a registry of LBNL's confined spaces, their potential hazards and safe work procedures unique to a particular confined space.

250

Conflict between the identification of a cosmic neutrino source and the sensitivity to mixing angles in a neutrino telescope  

SciTech Connect

Neutrino fluxes at telescopes depend on both initial fluxes out of astronomical bursts and flavor mixing during their travel to the Earth. However, since the information on the initial composition requires better precision in mixing angles and vice versa, neutrino detection at telescopes cannot provide solutions to both problems by itself. Thus, a probability to be measured at long-baseline oscillation is considered as a complement to the telescope, and problems like source identification and parameter degeneracy are examined under a few assumptions.

Hwang, Ggyoung-Riun; Siyeon, Kim [Department of Physics, Chung-Ang University, Seoul 156-756 (Korea, Republic of)

2008-11-01T23:59:59.000Z

251

Development and Performance of the PHOT (Portable High-Speed Occultation Telescope) Systems  

E-Print Network (OSTI)

The PHOT (Portable High-Speed Occultation Telescope) systems were developed for the specific purpose of observing stellar occultations by solar system objects. Stellar occultations have unique observing constraints: they may only be observable from certain parts of the globe; they often require a rapid observing cadence; and they require accurate timestamp information for each exposure. The PHOT systems consist of 14" telescopes, CCD cameras, camera mounting plates, GPS-based time standards, and data acquisition computers. The PHOT systems are similar in principle to the POETS systems (Portable Occultation, Eclipse and Transit Systems, described by Souza et al. 2006 and reported on by Gulbis et al. 2008), with the main differences being (a) different CCD/Cameras with slightly different specifications and (b) a stand-alone custom-built time standard used by PHOT, whereas POETS uses a commercial time-standard that is controlled from a computer. Since 2005, PHOT systems have been deployed on over two dozen occas...

Young, E F; Olkin, C B; Shoemaker, K; French, R G; Regester, J; Buie, M W

2011-01-01T23:59:59.000Z

252

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

Science Conference Proceedings (OSTI)

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.

Oertel, J.A.; Murphy, T.J.; Berggren, R.R. [and others

1998-12-31T23:59:59.000Z

253

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

E-Print Network (OSTI)

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.

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

2013-01-01T23:59:59.000Z

254

The MAGIC telescopes DAQ software and the on-the-fly online analysis client  

E-Print Network (OSTI)

In this contribution we describe the design of the Data AcQuisition (DAQ) and online analysis software of the MAGIC telescopes after the 2012 upgrade. Although the final stereo trigger requires coincidence between the two telescopes, the actual data acquisition is performed independently, producing two separate data streams. Events are first readout and built from the front-end electronics and then stored in the DAQs' internal ring buffer for further processing: pre-calibration and signal extraction. The pixel signals, previously used only for data quality monitoring, are now also sent "on-the-fly" to the centralized online analysis program MOLA, which acts as a single client for the two DAQ data streams, and uses this information to provide preliminary high level analysis results. The integrated DAQ and online analysis programs allows an immediate feedback in case of a rapid gamma-ray flare of the pointed astrophysical source.

Diego Tescaro; Alicia López-Oramas; Abelardo Moralejo; Daniel Mazin; Daniela Hadasch for the MAGIC Collaboration

2013-10-06T23:59:59.000Z

255

Influence of aerosols from biomass burning on the spectral analysis of Cherenkov telescopes  

E-Print Network (OSTI)

During the last decade, imaging atmospheric Cherenkov telescopes (IACTs) have proven themselves as astronomical detectors in the very-high-energy (VHE; E>0.1 TeV) regime. The IACT technique observes the VHE photons indirectly, using the Earth's atmosphere as a calorimeter. Much of the calibration of Cherenkov telescope experiments is done using Monte Carlo simulations of the air shower development, Cherenkov radiation and detector, assuming certain models for the atmospheric conditions. Any deviation of the real conditions during observations from the assumed atmospheric model will result in a wrong reconstruction of the primary gamma-ray energy and the resulting source spectra. During eight years of observations, the High Energy Stereoscopic System (H.E.S.S.) has experienced periodic natural as well as anthropogenic variations of the atmospheric transparency due to aerosols created by biomass burning. In order to identify data that have been taken under such long-term reductions in atmospheric transparency, ...

Reyes, R de los; Bernloehr, K; Krueger, P; Deil, C; Gast, H; Kosack, K; Marandon, V

2013-01-01T23:59:59.000Z

256

Search for neutrinos from Gamma-Ray Bursts with the Baikal neutrino telescope NT200  

E-Print Network (OSTI)

We present an analysis of neutrinos detected with the Baikal neutrino telescope NT200 for correlations with gamma-ray bursts (GRB). No neutrino events correlated with GRB were observed. Assuming a Waxman-Bahcall spectrum, a neutrino flux upper limit of {\\bf $E^2 \\Phi Green's Function fluence limit for this search, which extends two orders of magnitude beyond the energy range of the Super-Kamiokande limit.

Avrorin, A

2009-01-01T23:59:59.000Z

257

The european FAZIA initiative: a high-performance digital telescope array for heavy-ion studies  

E-Print Network (OSTI)

The european Fazia collaboration aims at building a new modular array for charged product identification to be employed for heavy-ion studies. The elementary module of the array is a Silicon-Silicon-CsI telescope, optimized for ion identification also via pulse shape analysis. The achievement of top performances imposes specific electronics which has been developed by FAZIA and features high quality charge and current preamplifiers, coupled to fully digital front-end. During the initial R&D phase, original and novel solutions have been tested in prototypes, obtaining unprecedented ion identification capabilities. FAZIA is now constructing a demonstrator array consisting of about two hundreds telescopes arranged in a compact and transportable configuration. In this contribution, we mainly summarize some aspects studied by FAZIA to improve the ion identification. Then we will briefly discuss the FAZIA program centered on experiments to be done with the demonstrator. First results on the isospin dynamics obtained with a reduced set-up demonstrate well the performance of the telescope and represent a good starting point towards future investigations with both stable and exotic beams.

G. Casini; S. Barlini; G. Pasquali; G. Pastore; M. Bini; S. Carboni; A. Olmi; S. Piantelli; G. Poggi; A. Stefanini; S. Valdre'; E. Bonnet; B. Borderie; R. Bougault; M. Bruno; A. Chbihi; M. Cinausero; M. Degerlier; P. Edelbruck; J. D. Frankland; F. Gramegna; D. Gruyer; M. Guerzoni; A. Kordjasz; T. Kozik; N. Le Neindre; O. Lopez; T. Marchi; P. Marini; L. Morelli; A. Ordine; M. Parlog; M. F. Rivet; E. Rosato; F. Salomon; G. Spadaccini; T. Twarog; E. Vient; M. Vigilante

2013-09-05T23:59:59.000Z

258

Aspects of mechanical design for an infrared robotic telescope in Antarctica: IRAIT  

E-Print Network (OSTI)

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.

Igor Di VArano

2006-09-22T23:59:59.000Z

259

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

E-Print Network (OSTI)

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

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

2005-11-01T23:59:59.000Z

260

Magnetic Space Launcher  

E-Print Network (OSTI)

A method and facilities for delivering payload and people into outer space are presented. This method uses, in general, engines located on a planetary surface. The installation consists of a space apparatus, power drive stations, which include a flywheel accumulator (for storage) of energy, a variable reducer, a powerful homopolar electric generator and electric rails. The drive stations accelerate the apparatus up to hypersonic speed. The estimations and computations show the possibility of making this project a reality in a short period of time (for payloads which can tolerate high g-forces). The launch will be very cheap at a projected cost of 3 - 5 dollars per pound. The authors developed a theory of this type of the launcher.

Alexander Bolonkin; Mark Krinker

2009-03-28T23:59:59.000Z

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


261

MHD Space Sailing  

E-Print Network (OSTI)

The rocket technology dates back as far as medieval China. Used initially for entertainment and religious practices over time rockets evolved into weapons and finally into means of transportation. Today, we are nearing the top of the rockets' capabilities. Although, for now they are the only way for us to send anything into space we are becoming more and more aware of the limitations of this technology. It is essential that we invent other means of propelling probes and other interplanetary vehicles through space. The authors had performed a series of magnetohydrodynamic simulations using the University of Chicago's Flash package to find out whether the interactions between the Solar Wind and the conducting ring with the electric current would occur. The MHD simulations gave the results similar to the monte-carlo calculations performed by dr Charles Danforth [1] from the University of Colorado. It is the authors' conclusion that the promising results should encourage further study of the phenomenon and the po...

Kisiel, T

2007-01-01T23:59:59.000Z

262

Orbit Spaces in Superconductivity  

E-Print Network (OSTI)

In the framework of Landau theory of phase transitions one is interested to describe all the possible low symmetry ``superconducting'' phases allowed for a given superconductor crystal and to determine the conditions under which this crystal undergoes a phase transition. These problems are best described and analyzed in the orbit space of the high symmetry group of the ``normal, non-superconducting'' phase of the crystal. In this article it is worked out a simple example concerning superconductivity, that shows the P-matrix method to determine the equations and inequalities defining the orbit space and its stratification. This approach is of general validity and can be used in all physical problems that make use of invariant functions, as long as the symmetry group is compact.

Vittorino Talamini

2006-07-30T23:59:59.000Z

263

Dendrite Arm Spacing  

Science Conference Proceedings (OSTI)

...Casting processes Cooling rate Dendrite arm spacing °C/s °F/s μm mils Plaster, investment 1 1.80 100â??1000 3.94â??39.4 Green sand, shell 10 18.0 50â??500 1.97â??19.7 Permanent mold 100 180.0 30â??70 1.18â??2.76 Die 1000 1800 5â??15 0.20â??0.59...

264

Space Time Matter inflation  

E-Print Network (OSTI)

We study a model of power-law inflationary inflation using the Space-Time-Matter (STM) theory of gravity for a five dimensional (5D) canonical metric that describes an apparent vacuum. In this approach the expansion is governed by a single scalar (neutral) quantum field. In particular, we study the case where the power of expansion of the universe is $p \\gg 1$. This kind of model is more successful than others in accounting for galaxy formation.

Mariano Anabitarte; Mauricio Bellini

2005-08-31T23:59:59.000Z

265

Nowcasting for Space Shuttle Landings at Kennedy Space Center, Florida  

Science Conference Proceedings (OSTI)

Space shuttle launches and landings at Kennedy Space Center (KSC) are subject to strict weather-related launch commit criteria and landing weather flight rules. Complex launch commit criteria and end-of-mission landing weather flight rules demand ...

William H. Bauman III; Steven Businger

1996-10-01T23:59:59.000Z

266

CRaTER: The Cosmic Ray Telescope for the Effects of Radiation Experiment on the Lunar Reconnaissance Orbiter Mission  

E-Print Network (OSTI)

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 ...

Spence, H. E.

267

Lens space surgeries and L-space homology spheres  

E-Print Network (OSTI)

We describe necessary and sufficient conditions for a knot in an L-space to have an L-space homology sphere surgery. We use these conditions to reformulate a conjecture of Berge about which knots in S^3 admit lens space surgeries.

Rasmussen, Jacob

2007-01-01T23:59:59.000Z

268

Symplectic space and orthogonal space of n qubits  

E-Print Network (OSTI)

In the Hilbert space of n qubits, we introduce the symplectic space (n odd) and the orthogonal space (n even) via the spin-flip operator. Under this mathematical structure we discuss some properties of n qubits, including homomorphically mapping the local operations of n qubits into the symplectic group or orthogonal group, and prove that the generalized ``magic basis'' is just the bi-orthonormal basis (that is, the orthonormal basis of both Hilbert space and the orthogonal space ). Finally, an example is given to discuss the application in physics of this mathematical structure.

Jian-Wei Xu

2010-11-14T23:59:59.000Z

269

Particle simulations of space weather  

Science Conference Proceedings (OSTI)

We review the application of particle simulation techniques to the full kinetic study of space weather events. We focus especially on the methods designed to overcome the difficulties created by the tremendous range of time and space scales present in ... Keywords: Adaptive, Implicit, Particle-in-cell, Space weather

Giovanni Lapenta

2012-02-01T23:59:59.000Z

270

Upgrading Below Grade Spaces  

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

Patrick H. Huelman, Sam Breidenbach, Steve Schirber Patrick H. Huelman, Sam Breidenbach, Steve Schirber NorthernSTAR Building America Partnership Upgrading Below Grade Spaces Residential Energy Efficiency Stakeholder March 1, 2012 Austin, TX * Act 1: Technical Challenges & Opportunities - Pat Huelman, University of Minnesota * Act 2: Assessing Homeowner Priorities & Risks - Sam Breidenbach, TDS Custom Construction * Act 3: An Industry Perspective - Steve Schirber, Cocoon Act 1. Upgrade Below Grade * Basement Remodeling: It Doesn't Get Any Riskier! - Combustion safety - Foundation moisture - Radon (& other soil gases) - Biologicals (mold, dust mites, etc.) - Garage gases (if attached) * And front and center are uncontrolled... - negative pressures in basements (beyond stack)

271

space booklet_DOE  

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

U U C L E A R E N E R G Y DOE/NE-0071 U . S . D e p a r t m e n t o f E n e r g y O f f i c e o f N u c l e a r E n e r g y , S c i e n c e a n d T e c h n o l o g y N UCLEAR Power in Space 2

272

MHD Space Sailing  

E-Print Network (OSTI)

The rocket technology dates back as far as medieval China. Used initially for entertainment and religious practices over time rockets evolved into weapons and finally into means of transportation. Today, we are nearing the top of the rockets' capabilities. Although, for now they are the only way for us to send anything into space we are becoming more and more aware of the limitations of this technology. It is essential that we invent other means of propelling probes and other interplanetary vehicles through space. The authors had performed a series of magnetohydrodynamic simulations using the University of Chicago's Flash package to find out whether the interactions between the Solar Wind and the conducting ring with the electric current would occur. The MHD simulations gave the results similar to the monte-carlo calculations performed by dr Charles Danforth [1] from the University of Colorado. It is the authors' conclusion that the promising results should encourage further study of the phenomenon and the possibility of using it in practice.

T. Kisiel; M. Soida

2007-12-10T23:59:59.000Z

273

Intelligent Satellite Teams Space Systems  

E-Print Network (OSTI)

This paper examines the development of Intelligent Satellite Teams (IST's) for complex space missions such as construction of space hardware, or Earth or space science. IST's are composed of many nanosatellites (mass control including formation flying, collision avoidance, knowledge sharing, and adaptive reconfiguration; microtechnology including microelectromechanical systems (MEMS), microfabricated sensors and actuators, nanotechnology, and integrated wireless communication; mission analysis -- high-level planning and control of mission, satellites, and procedures. Recent rapid technological advances in these fields open up exciting new possibilities for future space missions: space science missions such as testing gravitational variation, detecting and characterizing near-Earth asteroids and comets, and comprehensive exploration of the solar system; Earth science missions ...

Mark E. Campbell; Karl F. Böhringer

1999-01-01T23:59:59.000Z

274

Webb County, Texas: Energy Resources | Open Energy Information  

Open Energy Info (EERE)

7.8174487°, -99.0128926° 7.8174487°, -99.0128926° Loading map... {"minzoom":false,"mappingservice":"googlemaps3","type":"ROADMAP","zoom":14,"types":["ROADMAP","SATELLITE","HYBRID","TERRAIN"],"geoservice":"google","maxzoom":false,"width":"600px","height":"350px","centre":false,"title":"","label":"","icon":"","visitedicon":"","lines":[],"polygons":[],"circles":[],"rectangles":[],"copycoords":false,"static":false,"wmsoverlay":"","layers":[],"controls":["pan","zoom","type","scale","streetview"],"zoomstyle":"DEFAULT","typestyle":"DEFAULT","autoinfowindows":false,"kml":[],"gkml":[],"fusiontables":[],"resizable":false,"tilt":0,"kmlrezoom":false,"poi":true,"imageoverlays":[],"markercluster":false,"searchmarkers":"","locations":[{"text":"","title":"","link":null,"lat":27.8174487,"lon":-99.0128926,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

275

2000 TMS Annual Meeting Exhibitor: Jervis B. Webb  

Science Conference Proceedings (OSTI)

Overhead power and free conveyors will transport the rodded anodes to the ... In the smelting plant, our full line of power and free conveyors and integrated ...

276

The Honorable Wellington E. Webb 350 City County Building  

Office of Legacy Management (LM)

these records are'being furnished to.you. .If you have any questions, please feel free to call me at 301-,427-1721 or Dr. W. Alexander Willianp,301-427-1719 of'my staff....

277

Webb City, Oklahoma: Energy Resources | Open Energy Information  

Open Energy Info (EERE)

6.8069821°, -96.7086401° 6.8069821°, -96.7086401° Loading map... {"minzoom":false,"mappingservice":"googlemaps3","type":"ROADMAP","zoom":14,"types":["ROADMAP","SATELLITE","HYBRID","TERRAIN"],"geoservice":"google","maxzoom":false,"width":"600px","height":"350px","centre":false,"title":"","label":"","icon":"","visitedicon":"","lines":[],"polygons":[],"circles":[],"rectangles":[],"copycoords":false,"static":false,"wmsoverlay":"","layers":[],"controls":["pan","zoom","type","scale","streetview"],"zoomstyle":"DEFAULT","typestyle":"DEFAULT","autoinfowindows":false,"kml":[],"gkml":[],"fusiontables":[],"resizable":false,"tilt":0,"kmlrezoom":false,"poi":true,"imageoverlays":[],"markercluster":false,"searchmarkers":"","locations":[{"text":"","title":"","link":null,"lat":36.8069821,"lon":-96.7086401,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

278

Triggering of Imaging Air Cherenkov Telescopes: PMT trigger rates due to night-sky photons  

E-Print Network (OSTI)

Imaging air Cherenkov telescopes are usually triggered on a coincidence of two or sometimes more pixels, with discriminator thresholds in excess of 20 photoelectrons applied for each pixel. These thresholds required to suppress night-sky background are significantly higher than expected on the basis of a Poisson distribution in the number of night-sky photoelectrons generated during the characteristic signal integration time. We studied noise trigger rates under controlled conditions using an artificial background light source. Large tails in the PMT amplitude response to single photoelectrons are identified as a dominant contribution to noise triggers. The rate of such events is very sensitive to PMT operating parameters.

G. Hermann; C. Köhler; T. Kutter; W. Hofmann

1995-08-07T23:59:59.000Z

279

Three Advantages of the KANATA 1.5-m Telescope as a Powerful Partner for GLAST  

Science Conference Proceedings (OSTI)

KANATA is a 1.5-m optical--near infrared telescope of Hiroshima University, which has been developed for observations of astronomical transients and variables, such as {gamma}-ray bursts, blazars. X-ray transients, and cataclysmic variables. Here, we introduce three characteristics of KANATA with examples of observations, that is, i) high ability for prompt observations, ii) simultaneous optical and infrared observations, and iii) polarimetric observations. Collaborating with GLAST, we are planning to perform follow-up optical--infrared observations of {gamma}-ray sources with KANATA.

Uemura, M.; Yamashita, T.; Kawabata, K. [Astrophysical Science Center, Hiroshima University, Kagamiyama 1-3-1, Higashi-Hiroshima, Hiroshima, 739-8526 (Japan); Ohsugi, T. [Astrophysical Science Center, Hiroshima University, Kagamiyama 1-3-1, Higashi-Hiroshima, Hiroshima, 739-8526 (Japan); Department of Physical Science, School of Science, Hiroshima University, Kagamiyama 1-3-1, Higashi-Hiroshima, Hiroshima 739-8526 (Japan); Arai, A.; Nagae, O.; Chiyonobu, S.; Ueda, A.; Fukazawa, Y.; Mizuno, T.; Katagiri, H.; Takahashi, H. [Department of Physical Science, School of Science, Hiroshima University, Kagamiyama 1-3-1, Higashi-Hiroshima, Hiroshima 739-8526 (Japan); Hayashi, T. [Department of Education, Hiroshima University, Kagamiyama 1-1-1, Higashi-Hiroshima 739-8524 (Japan); Okita, K.; Yoshida, M.; Yanagisawa, K. [Okayama Astrophysical Observatory, National Astronomical Observatory of Japan, Kamogata Okayama, 719-0232 (Japan); Sato, S.; Kino, M.; Kitagawa, M. [Department of Physics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8602 (Japan); Sadakane, K. [Astronomical Institute, Osaka Kyoiku University, Asahigaoka, Kashiwara, Osaka 582-8582 (Japan)

2007-07-12T23:59:59.000Z

280

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

SciTech Connect

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 focusing far beyond the {approx}10 keV high-energy cutoff achieved by all previous X-ray satellites. The inherently low background associated with concentrating the X-ray light enables NuSTAR to probe the hard X-ray sky with a more than 100-fold improvement in sensitivity over the collimated or coded mask instruments that have operated in this bandpass. Using its unprecedented combination of sensitivity and spatial and spectral resolution, NuSTAR will pursue five primary scientific objectives: (1) probe obscured active galactic nucleus (AGN) activity out to the peak epoch of galaxy assembly in the universe (at z {approx}< 2) by surveying selected regions of the sky; (2) study the population of hard X-ray-emitting compact objects in the Galaxy by mapping the central regions of the Milky Way; (3) study the non-thermal radiation in young supernova remnants, both the hard X-ray continuum and the emission from the radioactive element {sup 44}Ti; (4) observe blazars contemporaneously with ground-based radio, optical, and TeV telescopes, as well as with Fermi and Swift, to constrain the structure of AGN jets; and (5) observe line and continuum emission from core-collapse supernovae in the Local Group, and from nearby Type Ia events, to constrain explosion models. During its baseline two-year mission, NuSTAR will also undertake a broad program of targeted observations. The observatory consists of two co-aligned grazing-incidence X-ray telescopes pointed at celestial targets by a three-axis stabilized spacecraft. Deployed into a 600 km, near-circular, 6 Degree-Sign inclination orbit, the observatory has now completed commissioning, and is performing consistent with pre-launch expectations. NuSTAR is now executing its primary science mission, and with an expected orbit lifetime of 10 yr, we anticipate proposing a guest investigator program, to begin in late 2014.

Harrison, Fiona A.; Cook, W. Rick; Forster, Karl; Grefenstette, Brian W.; Madsen, Kristin K.; Mao, Peter H.; Miyasaka, Hiromasa [Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA 91125 (United States); Craig, William W.; Pivovaroff, Michael J. [Lawrence Livermore National Laboratory, Livermore, CA 94550 (United States); Christensen, Finn E. [DTU Space, National Space Institute, Technical University of Denmark, Elektrovej 327, DK-2800 Lyngby (Denmark); Hailey, Charles J.; Koglin, Jason E.; Mori, Kaya [Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027 (United States); Zhang, William W. [NASA Goddard Space Flight Center, Greenbelt, MD 20771 (United States); Boggs, Steven E. [Space Sciences Laboratory, University of California, Berkeley, CA 94720 (United States); Stern, Daniel; Kim, Yunjin [Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109 (United States); Giommi, Paolo; Perri, Matteo [ASI Science Data Center, c/o ESRIN, via G. Galilei, I-00044 Frascati (Italy); Kitaguchi, Takao, E-mail: fiona@srl.caltech.edu [INAF-Osservatorio Astronomico di Roma, via di Frascati 33, I-00040 Monteporzio (Italy); and others

2013-06-20T23:59:59.000Z

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


281

Converting Unconditioned Basement to Conditioned Space - Code...  

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

Conditioned Space - Code Notes Converting a basement to conditioned space increases the living space of a house. As with most construction activities, the conversion or...

282

AERaSPACE CORPORATION  

Office of Legacy Management (LM)

THE ' THE ' AERaSPACE CORPORATION Suite 300, 955 L' &njon~ Pkzza. S. W., Washingvan. D.C. 200242174, Tekphanc (202) 488~6CllO 7117-03.87.cdy.43 23 September 1987 CA CA.Ot M r. Andrew Wallo, III. NE-23 Division of Facility & Site cr.05 Decommissioning Projects FL .0-d U.S. Department of Energy TAl.OL Germantown; Maryland 20545 JA/.OZ 1hJ . o-01 Dear M r. Wallo: flA.05 ELIMINATION RECOMMENDATION -- COLLEGES AND UNIVERSITIES M /4.0-* 11 D.OF The attached elimination recommendation was prepared in accordance ML.o= with your suggestion during our meeting on 22 September. The recommendation nO.o-02 includes 26 colleges and universities identified,in Enclosure 4 to Aerospace letter subject: Status of Actions - FUSRAP Site List, dated MO.03. 27 May 1987; three institutions (Tufts College, University of Virginia,

283

Hilbert space of wormholes  

E-Print Network (OSTI)

Wormhole boundary conditions for the Wheeler--DeWitt equation can be derived from the path integral formulation. It is proposed that the wormhole wave function must be square integrable in the maximal analytic extension of minisuperspace. Quantum wormholes can be invested with a Hilbert space structure, the inner product being naturally induced by the minisuperspace metric, in which the Wheeler--DeWitt operator is essentially self--adjoint. This provides us with a kind of probabilistic interpretation. In particular, giant wormholes will give extremely small contributions to any wormhole state. We also study the whole spectrum of the Wheeler--DeWitt operator and its role in the calculation of Green's functions and effective low energy interactions.

Garay, L J

1993-01-01T23:59:59.000Z

284

Exploring Lighting Spaces  

E-Print Network (OSTI)

We present a simple system for interactively specifying lighting parameters, including position, for high-quality image synthesis. Unlikeinverse approaches to the lighting-design problem, we do not require the user to indicate a priori the desired illuminative characteristics of an image. In our approach the computer proposes, culls, and organizes a set of candidate lights automatically, using an elementary measure of image similarityasthe basis for both culling and organization. The user then browses the set of candidate-light images, selects which lights to include, and combines them as desired. This work is a particular instance of a general strategy --- sampling a design space broadly and intelligently and organizing the results for rapid browsing by the user --- that may be applicable to many other design problems in computer graphics.

T. Kang; J. Seims; J. Marks; S. Shieber

1996-01-01T23:59:59.000Z

285

The Robinson Gravitational Wave Background Telescope (BICEP): a bolometric large angular scale CMB polarimeter  

E-Print Network (OSTI)

The Robinson Telescope (BICEP) is a ground-based millimeter-wave bolometric array designed to study the polarization of the cosmic microwave background radiation (CMB) and galactic foreground emission. Such measurements probe the energy scale of the inflationary epoch, tighten constraints on cosmological parameters, and verify our current understanding of CMB physics. Robinson consists of a 250-mm aperture refractive telescope that provides an instantaneous field-of-view of 17 degrees with angular resolution of 55 and 37 arcminutes at 100 GHz and 150 GHz, respectively. Forty-nine pair of polarization-sensitive bolometers are cooled to 250 mK using a 4He/3He/3He sorption fridge system, and coupled to incoming radiation via corrugated feed horns. The all-refractive optics is cooled to 4 K to minimize polarization systematics and instrument loading. The fully steerable 3-axis mount is capable of continuous boresight rotation or azimuth scanning at speeds up to 5 deg/s. Robinson has begun its first season of observation at the South Pole. Given the measured performance of the instrument along with the excellent observing environment, Robinson will measure the E-mode polarization with high sensitivity, and probe for the B-modes to unprecedented depths. In this paper we discuss aspects of the instrument design and their scientific motivations, scanning and operational strategies, and the results of initial testing and observations.

K. W. Yoon; P. A. R. Ade; D. Barkats; J. O. Battle; E. M. Bierman; J. J. Bock; J. A. Brevik; H. C. Chiang; A. Crites; C. D. Dowell; L. Duband; G. S. Griffin; E. F. Hivon; W. L. Holzapfel; V. V. Hristov; B. G. Keating; J. M. Kovac; C. L. Kuo; A. E. Lange; E. M. Leitch; P. V. Mason; H. T. Nguyen; N. Ponthieu; Y. D. Takahashi; T. Renbarger; L. C. Weintraub; D. Woolsey

2006-06-12T23:59:59.000Z

286

The forward inelastic telescope T2 for the TOTEM experiment at the LHC  

E-Print Network (OSTI)

The TOTEM Experiment will measure the total pp cross-section with the luminosity-independent method and study elastic and diffractive scattering at the LHC. To achieve optimum forward coverage for charged particles emitted by the pp collisions in the interaction point IP5, two tracking telescopes, T1 and T2, will be installed on each side in the pseudorapidity region $3.1 \\leq |\\eta| \\leq 6.5$ and Roman Pot stations will be placed at distances of 147 m and 220 m from the Interaction Point 5 (IP5). The triple Gas Electron Multiplier (GEM) technology has been chosen by the collaboration for its T2 telescope which will provide charged track reconstruction in the rapidity range $5.3 < \\eta < 6.5$ and a fully inclusive trigger for diffractive events. Results from the preliminary tests on the prototypes of the TOTEM Triple GEM detectors up to the data taking during the first pp collisions at the LHC will be described in this thesis.

Oliveri, Eraldo; Turini, Nicola

2010-01-01T23:59:59.000Z

287

Gamma-Hadron Separation Methods for the VERITAS Array of Four Imaging Atmospheric Cherenkov Telescopes  

E-Print Network (OSTI)

Ground-based arrays of imaging atmospheric Cherenkov telescopes have emerged as the most sensitive gamma-ray detectors in the energy range of about 100 GeV and above. The strengths of these arrays are a very large effective collection area on the order of 100,000 square meter, combined with excellent single photon angular and energy resolutions. The sensitivity of such detectors is limited by statistical fluctuations in the number of Cosmic Ray initiated air showers that resemble gamma-ray air showers in many ways. In this paper, we study the performance of simple event reconstruction methods when applied to simulated data of the Very Energetic Radiation Imaging Telescope Array System (VERITAS) experiment. We review methods for reconstructing the arrival direction and the energy of the primary photons, and examine means to improve on their performance. For a software threshold energy of 300 GeV (100 GeV), the methods achieve point source angular and energy resolutions of sigma[63%]= 0.1 degree (0.2 degree) and sigma[68%]= 15% (22%), respectively. The main emphasis of the paper is the discussion of gamma-hadron separation methods for the VERITAS experiment. We find that the information from several methods can be combined based on a likelihood ratio approach and the resulting algorithm achieves a gamma-hadron suppression with a quality factor that is substantially higher than that achieved with the standard methods used so far.

H. Krawczynski; D. A. Carter-Lewis; C. Duke; J. Holder; G. Maier; S. Le Bohec; G. Sembroski

2006-04-24T23:59:59.000Z

288

Perspectives of a Midrapidity Dimuon Program at RHIC: A Novel and Compact Muon Telescope Detector  

E-Print Network (OSTI)

We propose a large-area, cost-effective Muon Telescope Detector (MTD) for the Solenoidal Tracker at RHIC (STAR) at mid-rapidity and for the next generation of detectors at a possible electron-ion collider. We utilize Multi-gap Resistive Plate Chambers with large modules and long readout strips (Long-MRPC) in the detector design. The results from cosmic ray and beam tests show the intrinsic timing and spatial resolution for a Long-MRPC are 60-70 ps and $\\sim1$ cm, respectively. The prototype performance of such a novel muon telescope detector at STAR indicates that muon identification at the transverse momentum of a few GeV/$c$ can be achieved through the combined information of track matching with the MTD, ionization energy loss in the Time Projection Chamber, and time-of-flight measurements. A primary muon over secondary muon ratio of better than 1/3 can be achieved. This provides a promising device for future quarkonium programs and primordial dilepton measurements at RHIC. Simulations of the muon efficiency, the signal-to-background ratio of $J/\\psi$, the separation of $\\Upsilon$ 1S from 2S+3S states, and the electron-muon correlation from charm pair production in the RHIC environment are presented.

L. Ruan; G. Lin; Z. Xu; K. Asselta; H. F. Chen; W. Christie; H. J. Crawford; J. Engelage; G. Eppley; T. J. Hallman; C. Li; J. Liu; W. J. Llope; R. Majka; T. Nussbaum; J. Scheblein; M. Shao; R. Soja; Y. Sun; Z. Tang; X. Wang; Y. Wang

2009-04-24T23:59:59.000Z

289

Polarimeter Receiver Prototyping and Testing for the South Pole Telescope Upgrade  

E-Print Network (OSTI)

Experimental evidence has so far been supportive for the inflationary Big Bang model of cosmology, while imposing other mysteries, such as the fact that dark matter and dark energy actually consist of 95 % of the observable universe. The forthcoming upgrade of the South Pole Telescope, planned for 2010, will include a polarimeter with increased sensitivity. Measurements of the CMB polarization anisotropy to a high accuracy will describe the angular power spectrum of the B-mode polarization, which will help unravel some of the mysteries. We prototype and test a digital frequency multiplexed readout system for the SPT upgrade. The digital system has the advantage of being able to reconstruct the phase of the signals. We characterize the performance of the readout and we compare it to the theoretical expectations. The noise is found to be statistically insignificant (insert quantitative proof), and the system performs as expected, significantly better than the previous implementation. We conclude that the digital fMux readout system should be sent to the South Pole Telescope. 1

Constantinos Melachrinos

2009-01-01T23:59:59.000Z

290

TARGET: A multi-channel digitizer chip for very-high-energy gamma-ray telescopes  

SciTech Connect

The next-generation very-high-energy (VHE) gamma-ray observatory, the Cherenkov Telescope Array, will feature dozens of imaging atmospheric Cherenkov telescopes (IACTs), each with thousands of pixels of photosensors. To be affordable and reliable, reading out such a mega-channel array requires event recording technology that is highly integrated and modular, with a low cost per channel. We present the design and performance of a chip targeted to this application: the TeV Array Readout with GSa/s sampling and Event Trigger (TARGET). This application-specific integrated circuit (ASIC) has 16 parallel input channels, a 4096-sample buffer for each channel, adjustable input termination, self-trigger functionality, and tight window-selected readout. We report the performance of TARGET in terms of sampling frequency, power consumption, dynamic range, current-mode gain, analog bandwidth, and cross talk. The large number of channels per chip allows a low cost per channel ($10 to $20 including front-end and back-end electronics but not including photosensors) to be achieved with a TARGET-based IACT readout system. In addition to basic performance parameters of the TARGET chip itself, we present a camera module prototype as well as a second-generation chip (TARGET 2), both of which have been produced.

Bechtol, K.; Funk, S.; /Stanford U., HEPL /KIPAC, Menlo Park; Okumura, A.; /JAXA, Sagamihara /Stanford U., HEPL /KIPAC, Menlo Park; Ruckman, L.; /Hawaii U.; Simons, A.; Tajima, H.; Vandenbroucke, J.; /Stanford U., HEPL /KIPAC, Menlo Park; Varner, G.; /Hawaii U.

2011-08-11T23:59:59.000Z

291

The VERITAS Upgraded Telescope-Level Trigger Systems: Technical Details and Performance Characterization  

E-Print Network (OSTI)

VERITAS is an array of imaging atmospheric Cherenkov telescopes sensitive to gamma rays in the energy range between 85 GeV and 30 TeV. The instrument underwent an upgrade of the camera triggers in November 2011. The new systems use 400 MHz Xilinix Virtex-5 FPGAs for the pixel neighbor coincidence logic necessary to produce a camera-level trigger. The upgraded systems are capable of time-aligning individual triggering pixels to within ~0.2 nanoseconds, allowing for an operational pixel-to-pixel coincidence window of ~5 nanoseconds. This reduced coincidence window provides improved rejection of night-sky background (NSB) which permits a reduction of the energy threshold at the trigger level. The use of FPGAs allows for the future implementation of a topological trigger capable of discriminating events based on an image moment analysis of a bit-wise hit pattern. As part of the commissioning phase for the trigger upgrade, the hardware was initially installed in a single telescope in "parallel" to the (then) curre...

Zitzer, Benjamin

2013-01-01T23:59:59.000Z

292

A Strategy for Finding Near Earth Objects with the SDSS Telescope  

E-Print Network (OSTI)

We present a detailed observational strategy for finding Near Earth Objects (NEOs) with the Sloan Digital Sky Survey (SDSS) telescope. We investigate strategies in normal, unbinned mode as well as binning the CCDs 2x2 or 3x3, which affects the sky coverage rate and the limiting apparent magnitude. We present results from 1 month, 3 year and 10 year simulations of such surveys. For each cadence and binning mode, we evaluate the possibility of achieving the Spaceguard goal of detecting 90% of 1 km NEOs (absolute magnitude H <= 18 for an albedo of 0.1). We find that an unbinned survey is most effective at detecting H <= 20 NEOs in our sample. However, a 3x3 binned survey reaches the Spaceguard Goal after only seven years of operation. As the proposed large survey telescopes (PanStarss; LSST) are at least 5-10 years from operation, an SDSS NEO survey could make a significant contribution to the detection and photometric characterization of the NEO population.

Sean N. Raymond; Oliver J. Fraser; Arti Garg; Suzanne L. Hawley; Robert Jedicke; Gajus Miknaitis; Thomas Quinn; Constance M. Rockosi; Christopher W. Stubbs; Scott F. Anderson; Craig J. Hogan; Zeljko Ivezic; Robert H. Lupton; Andrew A. West; Howard Brewington; J. Brinkmann; Michael Harvanek; Scot J. Kleinman; Jurek Krzesinski; Dan Long; Eric H. Neilsen; Peter R. Newman; Atsuko Nitta; Stephanie A. Snedden

2004-01-21T23:59:59.000Z

293

A Strategy for Finding Near Earth Objects with the SDSS Telescope  

E-Print Network (OSTI)

We present a detailed observational strategy for finding Near Earth Objects (NEOs) with the Sloan Digital Sky Survey (SDSS) telescope. We investigate strategies in normal, unbinned mode as well as binning the CCDs 2x2 or 3x3, which affects the sky coverage rate and the limiting apparent magnitude. We present results from 1 month, 3 year and 10 year simulations of such surveys. For each cadence and binning mode, we evaluate the possibility of achieving the Spaceguard goal of detecting 90% of 1 km NEOs (absolute magnitude H <= 18 for an albedo of 0.1). We find that an unbinned survey is most effective at detecting H <= 20 NEOs in our sample. However, a 3x3 binned survey reaches the Spaceguard Goal after only seven years of operation. As the proposed large survey telescopes (PanStarss; LSST) are at least 5-10 years from operation, an SDSS NEO survey could make a significant contribution to the detection and photometric characterization of the NEO population.

Raymond, S N; Garg, A; Hawley, S L; Jedicke, R; Miknaitis, G; Quinn, T; Rockosi, C M; Stubbs, C W; Anderson, S F; Hogan, C J; Ivezic, Z; Lupton, R H; West, A A; Brewington, H; Brinkmann, J; Harvanek, M J; Kleinman, S J; Krzesínski, J; Long, D; Neilsen, E H; Newman, P R; Nitta, A; Snedden, S A; Raymond, Sean N.; Fraser, Oliver J.; Garg, Arti; Hawley, Suzanne L.; Jedicke, Robert; Miknaitis, Gajus; Quinn, Thomas; Rockosi, Constance M.; Stubbs, Christopher W.; Anderson, Scott F.; Hogan, Craig J.; Ivezic, Zeljko; Lupton, Robert H.; West, Andrew A.; Brewington, Howard; Harvanek, Michael; Kleinman, Scot J.; Krzesinski, Jurek; Long, Dan; Neilsen, Eric H.; Newman, Peter R.; Nitta, Atsuko; Snedden, Stephanie A.

2004-01-01T23:59:59.000Z

294

Orbit determination of space objects based on sparse optical data  

E-Print Network (OSTI)

While building up a catalog of Earth orbiting objects, if the available optical observations are sparse, not deliberate follow ups of specific objects, no orbit determination is possible without previous correlation of observations obtained at different times. This correlation step is the most computationally intensive, and becomes more and more difficult as the number of objects to be discovered increases. In this paper we tested two different algorithms (and the related prototype software) recently developed to solve the correlation problem for objects in geostationary orbit (GEO), including the accurate orbit determination by full least squares solutions with all six orbital elements. Because of the presence in the GEO region of a significant subpopulation of high area to mass objects, strongly affected by non-gravitational perturbations, it was actually necessary to solve also for dynamical parameters describing these effects, that is to fit between 6 and 8 free parameters for each orbit. The validation was based upon a set of real data, acquired from the ESA Space Debris Telescope (ESASDT) at the Teide observatory (Canary Islands). We proved that it is possible to assemble a set of sparse observations into a set of objects with orbits, starting from a sparse time distribution of observations, which would be compatible with a survey capable of covering the region of interest in the sky just once per night. This could result in a significant reduction of the requirements for a future telescope network, with respect to what would have been required with the previously known algorithm for correlation and orbit determination.

A. Milani; G. Tommei; D. Farnocchia; A. Rossi; T. Schildknecht; R. Jehn

2010-12-23T23:59:59.000Z

295

No Prejudice in Space  

SciTech Connect

We present a summary of recent results obtained from a scan of the 19-dimensional parameter space of the pMSSM and its implications for dark matter searches. We have generated a large set of points in parameter space (which we call 'models') for the 19-parameter CP-conserving pMSSM, where MFV has been assumed. We subjected these models to numerous experimental and theoretical constraints to obtain a set of {approx}68 K models which are consistent with existing data. We attempted to be somewhat conservative in our implementation of these constraints; in particular we only demanded that the relic density of the LSP not be greater than the measured value of {Omega}H{sup 2} for non-baryonic dark matter, rather than assuming that the LSP must account for the entire observed relic density. Examining the properties of the neutralinos in these models, we find that many are relatively pure gauge eigenstates with Higgsinos being the most common, followed by Winos. The relative prevalence of Higgsino and Wino LSPs leads many of our models to have a chargino as nLSP, often with a relatively small mass splitting between this nLSP and the LSP; this has important consequences in both collider and astroparticle phenomenology. We find that, in general, the LSP in our models provides a relatively small ({approx} 4%) contribution to the dark matter, however there is a long tail to this distribution and a substantial number of models for which the LSP makes up all or most of the dark matter. Typically these neutralinos are mostly Binos. Examining the signatures of our models in direct and indirect dark matter detection experiments, we find a wide range of signatures for both cases. In particular, we find a much larger range of WIMP-nucleon cross sections than is found in any particular model of SUSY-breaking. As these cross sections also enter the regions of parameter space suggested by non-SUSY models, it appears that the discovery of WIMPs in direct detection experiments might not be sufficient to determine the correct model of the underlying physics. As a first look at the signatures of these models in indirect detection experiments, we examined whether our models could explain the PAMELA excess in the positron to electron ratio at high energies. We find that there are models which fit the PAMELA data rather well, and some of these have significantly smaller boost factors than generally assumed for a thermal relic. The study of the pMSSM presents exciting new possibilities for SUSY phenomenology. The next few years will hopefully see important discoveries both in colliders and in satellite or ground-based astrophysical experiments. It is important that we follow the data and not our existing prejudices; hopefully this sort of relatively model-independent approach to collider and astrophysical phenomenology can be useful in this regard.

Cotta, R.C.; Gainer, J.S.; Hewett, J.L.; Rizzo, T.G.; /SLAC

2010-08-26T23:59:59.000Z

296

Acceptability of reactors in space  

SciTech Connect

Reactors are the key to our future expansion into space. However, there has been some confusion in the public as to whether they are a safe and acceptable technology for use in space. The answer to these questions is explored. The US position is that when reactors are the preferred technical choice, that they can be used safely. In fact, it does not appear that reactors add measurably to the risk associated with the Space Transportation System.

Buden, D.

1981-01-01T23:59:59.000Z

297

Acceptability of reactors in space  

SciTech Connect

Reactors are the key to our future expansion into space. However, there has been some confusion in the public as to whether they are a safe and acceptable technology for use in space. The answer to these questions is explored. The US position is that when reactors are the preferred technical choice, that they can be used safely. In fact, it dies not appear that reactors add measurably to the risk associated with the Space Transportation System.

Buden, D.

1981-04-01T23:59:59.000Z

298

Entropic Gravity in Rindler Space  

E-Print Network (OSTI)

We show that Rindler horizons are entropic screens and gravity is an entropic force in Rindler space by deriving the Verlinde entropy formula from the focusing of light due to a mass close to the horizon. Consequently, gravity is also entropic in the near horizon regions of Schwarzschild and de Sitter space-times. In different limits, the entropic nature of gravity in Rindler space leads to the Bekenstein entropy bound and the uncertainty principle.

Halyo, Edi

2011-01-01T23:59:59.000Z

299

Entropic Gravity in Rindler Space  

E-Print Network (OSTI)

We show that Rindler horizons are entropic screens and gravity is an entropic force in Rindler space by deriving the Verlinde entropy formula from the focusing of light due to a mass close to the horizon. Consequently, gravity is also entropic in the near horizon regions of Schwarzschild and de Sitter space-times. In different limits, the entropic nature of gravity in Rindler space leads to the Bekenstein entropy bound and the uncertainty principle.

Edi Halyo

2011-04-13T23:59:59.000Z

300

A characterization of separable conjugate spaces  

E-Print Network (OSTI)

Necessary and sufficient conditions for a separable Banach space to be a dual space are proved. Some applications are discussed

Rossi, Stefano

2010-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "webb space telescope" from the National Library of EnergyBeta (NLEBeta).
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301

Physics in discrete spaces (A): Space-Time organization  

E-Print Network (OSTI)

We put forward a model of discrete physical space that can account for the structure of space- time, give an interpretation to the postulates of quantum mechanics and provide a possible explanation to the organization of the standard model of particles.

P. Peretto

2010-12-29T23:59:59.000Z

302

Total Space Heat-  

Gasoline and Diesel Fuel Update (EIA)

Released: September, 2008 Released: September, 2008 Total Space Heat- ing Cool- ing Venti- lation Water Heat- ing Light- ing Cook- ing Refrig- eration Office Equip- ment Com- puters Other All Buildings* ........................... 3,037 115 397 384 52 1,143 22 354 64 148 357 Building Floorspace (Square Feet) 1,001 to 5,000 ........................... 386 19 43 18 11 93 7 137 8 12 38 5,001 to 10,000 .......................... 262 12 35 17 5 83 4 56 6 9 35 10,001 to 25,000 ........................ 407 20 46 44 8 151 3 53 9 19 54 25,001 to 50,000 ........................ 350 15 55 50 9 121 2 34 7 16 42 50,001 to 100,000 ...................... 405 16 57 65 7 158 2 29 6 18 45 100,001 to 200,000 .................... 483 16 62 80 5 195 1 24 Q 31 56 200,001 to 500,000 .................... 361 8 51 54 5 162 1 9 8 19 43 Over 500,000 ............................. 383 8 47 56 3 181 2 12 8 23 43 Principal Building Activity

303

Total Space Heat-  

Gasoline and Diesel Fuel Update (EIA)

Revised: December, 2008 Revised: December, 2008 Total Space Heat- ing Cool- ing Venti- lation Water Heat- ing Light- ing Cook- ing Refrig- eration Office Equip- ment Com- puters Other All Buildings ............................. 91.0 33.0 7.2 6.1 7.0 18.7 2.7 5.3 1.0 2.2 7.9 Building Floorspace (Square Feet) 1,001 to 5,000 ........................... 99.0 30.7 6.7 2.7 7.1 13.9 7.1 19.9 1.1 1.7 8.2 5,001 to 10,000 .......................... 80.0 30.1 5.5 2.6 6.1 13.6 5.2 8.2 0.8 1.4 6.6 10,001 to 25,000 ........................ 71.0 28.2 4.5 4.1 4.1 14.5 2.3 4.5 0.8 1.6 6.5 25,001 to 50,000 ........................ 79.0 29.9 6.8 5.9 6.3 14.9 1.7 3.9 0.8 1.8 7.1 50,001 to 100,000 ...................... 88.7 31.6 7.6 7.6 6.5 19.6 1.7 3.4 0.7 2.0 8.1 100,001 to 200,000 .................... 104.2 39.1 8.2 8.9 7.9 22.9 1.1 2.9 Q 3.2 8.7 200,001 to 500,000 ....................

304

Total Space Heat-  

Gasoline and Diesel Fuel Update (EIA)

Revised: December, 2008 Revised: December, 2008 Total Space Heat- ing Cool- ing Venti- lation Water Heat- ing Light- ing Cook- ing Refrig- eration Office Equip- ment Com- puters Other All Buildings ............................. 91.0 33.0 7.2 6.1 7.0 18.7 2.7 5.3 1.0 2.2 7.9 Building Floorspace (Square Feet) 1,001 to 5,000 ........................... 99.0 30.7 6.7 2.7 7.1 13.9 7.1 19.9 1.1 1.7 8.2 5,001 to 10,000 .......................... 80.0 30.1 5.5 2.6 6.1 13.6 5.2 8.2 0.8 1.4 6.6 10,001 to 25,000 ........................ 71.0 28.2 4.5 4.1 4.1 14.5 2.3 4.5 0.8 1.6 6.5 25,001 to 50,000 ........................ 79.0 29.9 6.8 5.9 6.3 14.9 1.7 3.9 0.8 1.8 7.1 50,001 to 100,000 ...................... 88.7 31.6 7.6 7.6 6.5 19.6 1.7 3.4 0.7 2.0 8.1 100,001 to 200,000 .................... 104.2 39.1 8.2 8.9 7.9 22.9 1.1 2.9 Q 3.2 8.7 200,001 to 500,000 ....................

305

On the Sensitivity of Neutrino Telescopes to a Modified Dispersion Relation  

SciTech Connect

We consider a modified dispersion relation and its effect on the flavour ratios of high-energy neutrinos originated at distant astrophysical sources such as active galactic nuclei. This dispersion relation arise naturally in different new physics (NP) effects such as violation of CPT invariance, of the equivalence principle and of Lorentz invariance. It is a common notion in the literature that by using the flux of high-energy neutrinos expected from distant astrophysical sources, the sensitivity to possible NP effects may be improved beyond the current bounds. However, performing a realistic analysis that takes into account the expected number of events in future neutrino telescopes, we find that the average detected flavour ratios with and without the inclusion of new physics have essentially the same value, making difficult to obtain an improved bound for this type of new physics.

Bustamante, M.; Gago, A. M.; Bazo, J. L. [Pontificia Universidad Catolica del Peru, Seccion Fisica, Lima (Peru); Miranda, O. G. [Centro de Investigacion y de Estudios Avanzados, Departamento de Fisica, Mexico D.F. (Mexico)

2008-07-02T23:59:59.000Z

306

Rotation Measure Synthesis of Galactic Polarized Emission with the DRAO 26-m Telescope  

E-Print Network (OSTI)

Radio polarimetry at decimetre wavelengths is the principal source of information on the Galactic magnetic field. The diffuse polarized emission is strongly influenced by Faraday rotation in the magneto-ionic medium and rotation measure is the prime quantity of interest, implying that all Stokes parameters must be measured over wide frequency bands with many frequency channels. The DRAO 26-m Telescope has been equipped with a wideband feed, a polarization transducer to deliver both hands of circular polarization, and a receiver, all operating from 1277 to 1762 MHz. Half-power beamwidth is between 40 and 30 arcminutes. A digital FPGA spectrometer, based on commercially available components, produces all Stokes parameters in 2048 frequency channels over a 485-MHz bandwidth. Signals are digitized to 8 bits and a Fast Fourier Transform is applied to each data stream. Stokes parameters are then generated in each frequency channel. This instrument is in use at DRAO for a Northern sky polarization survey. Observatio...

Wolleben, M; Hovey, G J; Messing, R; Davison, O S; House, N L; Somaratne, K H M S; Tashev, I

2010-01-01T23:59:59.000Z

307

Commissioning of the Dual-Beam Imaging Polarimeter for the UH 88-inch telescope  

E-Print Network (OSTI)

In this paper we present the design, calibration method, and initial results of the Dual-Beam Imaging Polarimeter (DBIP). This new instrument is designed to measure the optical polarization properties of point sources, in particular Main Belt asteroids. This instrument interfaces between the Tek 2048x2048 camera and the University of Hawaii's 88-inch telescope, and is available for facility use. Using DBIP we are able to measure linear polarization with a 1-sigma Poisson signal noise of 0.03% per measurement and a systematic error of order 0.06% +/- 0.02%. Additionally, we discuss measurements of the polarization of the asteroid 16 Psyche which were taken as part of the instrument commissioning. We confirm Psyche's negative polarization of -1.037% +/- 0.006% but find no significant modulation of the signal with rotation above the 0.05% polarization level.

Joseph Masiero; Klaus Hodapp; Dave Harrington; Haosheng Lin

2007-08-09T23:59:59.000Z

308

Transmission of light in deep sea water at the site of the Antares neutrino telescope  

E-Print Network (OSTI)

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.

ANTARES collaboration

2004-12-06T23:59:59.000Z

309

An Architecture Proposal for the ILC Test Beam Silicon Telescope at Fermilab  

SciTech Connect

The requirements for an ILC Test Beam silicon telescope system are foreseen to be very stringent. Resolution, noise, and throughput must be carefully managed in order to provide a useful instrument for the high energy physics community to develop detector technologies for the ILC. Since the ILC Test Beam is meant to test a wide variety of different detectors, it must employ universally accepted software techniques, hardware standards and protocols as well as easy integration of hardware and software with the various clients using the system. In this paper, we describe an open modular architecture to achieve these goals, including an analysis of the entire chain of software and hardware needed to meet the requirements.

Turqueti, M.A.; /Fermilab

2007-04-01T23:59:59.000Z

310

Sensitivity of an underwater Cerenkov km3 telescope to TeV neutrinos from Galactic Microquasars  

E-Print Network (OSTI)

In this paper are presented the results of Monte Carlo simulations on the capability of the proposed NEMO-km$^3$ telescope to detect TeV muon neutrinos from Galactic microquasars. For each known microquasar we compute the number of detectable events, together with the atmospheric neutrino and muon background events. We also discuss the detector sensitivity to neutrino fluxes expected from known microquasars, optimizing the event selection also to reject the background; the number of events surviving the event selection are given. The best candidates are the steady microquasars SS433 and GX339-4 for which we estimate a sensitivity of about $5\\cdot10^{-11}$ erg/cm$^2$ s; the predicted fluxes are expected to be well above this sensitivity. For bursting microquasars the most interesting candidates are Cygnus X-3, GRO J1655-40 and XTE J1118+480: their analyses are more complicated because of the stochastic nature of the bursts.

C. Distefano; the NEMO Collaboration

2006-08-02T23:59:59.000Z

311

Gamma-ray burst observations with new generation imaging atmospheric Cerenkov Telescopes in the FERMI era  

SciTech Connect

After the launch and successful beginning of operations of the FERMI satellite, the topics related to high-energy observations of gamma-ray bursts have obtained a considerable attention by the scientific community. Undoubtedly, the diagnostic power of high-energy observations in constraining the emission processes and the physical conditions of gamma-ray burst is relevant. We briefly discuss how gamma-ray burst observations with ground-based imaging array Cerenkov telescopes, in the GeV-TeV range, can compete and cooperate with FERMI observations, in the MeV-GeV range, to allow researchers to obtain a more detailed and complete picture of the prompt and afterglow phases of gamma-ray bursts.

Covino, S.; Campana, S. [INAF/Brera Astronomical Observatory, Via Bianchi 46, 23807, Merate (Saint Lucia) (Italy); Garczarczyk, M. [Max-Planck-Institut fuer Physik, Foehringer Ring 6, D-80805 Muenchen (Germany); IFAE, Edifici Cn., Campus UAB, 08193 Bellaterra (Spain); Galante, N. [Max-Planck-Institut fuer Physik, Foehringer Ring 6, D-80805 Muenchen (Germany); Gaug, M. [Instituto de Astrofisica de Canarias, via Lactea s/n, 38205 La Laguna, Tenerife (Spain); Antonelli, A. [INAF/Rome Astronomical Observatory, Via Frascati 33, 00044, Monte Porzio (Roma) (Italy); Bastieri, D. [Universita di Padova and Istituto Nazionale di Fisica Nucleare (INFN), 35131, Padova (Italy); Longo, F. [Dipartimento Fisica and INFN Trieste, 34127 Trieste (Italy); Scapin, V. [Universita di Udine, and INFN Trieste, 33100 Udine (Italy)

2009-04-08T23:59:59.000Z

312

Searches for cosmic-ray electron anisotropies with the Fermi Large Area Telescope  

SciTech Connect

The Large Area Telescope on board the Fermi satellite (Fermi LAT) detected more than 1.6x10{sup 6} cosmic-ray electrons/positrons with energies above 60 GeV during its first year of operation. The arrival directions of these events were searched for anisotropies of angular scale extending from {approx}10 deg. up to 90 deg., and of minimum energy extending from 60 GeV up to 480 GeV. Two independent techniques were used to search for anisotropies, both resulting in null results. Upper limits on the degree of the anisotropy were set that depended on the analyzed energy range and on the anisotropy's angular scale. The upper limits for a dipole anisotropy ranged from {approx}0.5% to {approx}10%.

Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Bloom, E. D.; Borgland, A. W.; Bouvier, A.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Couto e Silva, E. do; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G. [W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, California 94305 (United States)

2010-11-01T23:59:59.000Z

313

The Prototype of the Small Synoptic Second Solar Spectrum Telescope (S5T)  

E-Print Network (OSTI)

We present the design and the prototype of the Small Synoptic Second Solar Spectrum Telescope (S5T), which can autonomously measure scattering polarization signals on a daily basis with large sensitivity and accuracy. Its data will be used to investigate the nature of weak, turbulent magnetic fields through the Hanle effect in many lines. Also the relation between those fields and the global solar dynamo can be revealed by spanning the observations over a significant fraction of a solar cycle. The compact instrument concept is enabled by a radial polarization converter that allows for ``one-shot'' polarimetry over the entire limb of the Sun. A polarimetric sensitivity of ~10^-5 is achieved by minimizing the instrumental polarization and by FLC modulation in combination with a fast line-scan camera in the fiber-fed spectrograph. The first prototype results successfully show the feasibility of the concept.

Snik, Frans; Keller, Christoph

2009-01-01T23:59:59.000Z

314

The Trigger And Onboard Filter of the GLAST Large Area Telescope  

SciTech Connect

The GLAST Large Area Telescope (LAT) will measure the cosmic gamma-ray flux in the energy range 20 MeV to >300 GeV. The LAT will open a new and important window on a wide variety of high-energy phenomena. Achieving this capability requires a hardware trigger and onboard software event filters that are robust and highly efficient for gamma rays while keeping the event rates due to the much larger fluxes of charged particle backgrounds at an acceptable level. Because of the important discovery windows for science and the uncertainties in the background fluxes, configuration flexibility is a particularly important system feature. This poster describes the purposes and architecture of the system, the components and capabilities of the hardware trigger and onboard software filters, testing and operation experience on the ground, and the on-orbit operations plan and expected performance.

Hughes, R.; /Ohio State U.; Grove, J.E.; /Naval Research Lab, Wash., D.C.; Kocian, M.; /SLAC; Ritz, S.; /Maryland U.; Russell, J.J.; /SLAC; Siskind, E.; /NYCB Real-Time Computing; Smith, P.; Winer, B.; /Ohio State U.; Usher, T.; /SLAC

2007-11-13T23:59:59.000Z

315

A Fast Algorithm for Muon Track Reconstruction and its Application to the ANTARES Neutrino Telescope  

E-Print Network (OSTI)

An algorithm is presented, that provides a fast and robust reconstruction of neutrino induced upward-going muons and a discrimination of these events from downward-going atmospheric muon background in data collected by the ANTARES neutrino telescope. The algorithm consists of a hit merging and hit selection procedure followed by fitting steps for a track hypothesis and a point-like light source. It is particularly well-suited for real time applications such as online monitoring and fast triggering of optical follow-up observations for multi-messenger studies. The performance of the algorithm is evaluated with Monte Carlo simulations and various distributions are compared with that obtained in ANTARES data.

ANTARES collaboration; J. A. Aguilar; I. Al Samarai; A. Albert; M. Andre; M. Anghinolfi; G. Anton; S. Anvar; M. Ardid; A. C. Assis Jesus; T. Astraatmadja; J-J. Aubert; R. Auer; B. Baret; S. Basa; M. Bazzotti; V. Bertin; S. Biagi; C. Bigongiari; C. Bogazzi; M. Bou-Cabo; M. C. Bouwhuis; A. M. Brown; J. Brunner; J. Busto; F. Camarena; A. Capone; C. Carloganu; G. Carminati; J. Carr; S. Cecchini; Ph. Charvis; T. Chiarusi; M. Circella; R. Coniglione; H. Costantini; N. Cottini; P. Coyle; C. Curtil; M. P. Decowski; I. Dekeyser; A. Deschamps; C. Distefano; C. Donzaud; D. Dornic; Q. Dorosti; D. Drouhin; T. Eberl; U. Emanuele; J-P. Ernenwein; S. Escoffier; F. Fehr; V. Flaminio; U. Fritsch; J-L. Fuda; S. Galata; P. Gay; G. Giacomelli; J. P. Gomez-Gonzalez; K. Graf; G. Guillard; G. Halladjian; G. Hallewell; H. van Haren; A. J. Heijboer; Y. Hello; J. J. Hernandez-Rey; B. Herold; J. Hößl; C. C. Hsu; M. de Jong; M. Kadler; N. Kalantar-Nayestanaki; O. Kalekin; A. Kappes; U. Katz; P. Kooijman; C. Kopper; A. Kouchner; V. Kulikovskiy; R. Lahmann; P. Lamare; G. Larosa; D. Lefevre; G. Lim; D. Lo Presti; H. Loehner; S. Loucatos; F. Lucarelli; S. Mangano; M. Marcelin; A. Margiotta; J. A. Martinez-Mora; A. Mazure; A. Meli; T. Montaruli; M. Morganti; L. Moscoso; H. Motz; C. Naumann; M. Neff; D. Palioselitis; G. E. Pavalas; P. Payre; J. Petrovic; N. Picot-Clemente; C. Picq; V. Popa; T. Pradier; E. Presani; C. Racca; C. Reed; G. Riccobene; C. Richardt; R. Richter; A. Rostovtsev; M. Rujoiu; G. V. Russo; F. Salesa; P. Sapienza; F. Schöck; J-P. Schuller; R. Shanidze; F. Simeone; A. Spiess; M. Spurio; J. J. M. Steijger; Th. Stolarczyk; M. Taiuti; C. Tamburini; L. Tasca; S. Toscano; B. Vallage; V. Van Elewyck; G. Vannoni; M. Vecchi; P. Vernin; G. Wijnker; E. de Wolf; H. Yepes; D. Zaborov; J. D. Zornoza; J. Zuniga

2011-05-20T23:59:59.000Z

316

Long wavelength infrared camera (LWIRC): a 10 micron camera for the Keck Telescope  

Science Conference Proceedings (OSTI)

The Long Wavelength Infrared Camera (LWIRC) is a facility instrument for the Keck Observatory designed to operate at the f/25 forward Cassegrain focus of the Keck I telescope. The camera operates over the wavelength band 7-13 {micro}m using ZnSe transmissive optics. A set of filters, a circular variable filter (CVF), and a mid-infrared polarizer are available, as are three plate scales: 0.05``, 0.10``, 0.21`` per pixel. The camera focal plane array and optics are cooled using liquid helium. The system has been refurbished with a 128 x 128 pixel Si:As detector array. The electronics readout system used to clock the array is compatible with both the hardware and software of the other Keck infrared instruments NIRC and LWS. A new pre-amplifier/A-D converter has been designed and constructed which decreases greatly the system susceptibility to noise.

Wishnow, E.H.; Danchi, W.C.; Tuthill, P.; Wurtz, R.; Jernigan, J.G.; Arens, J.F.

1998-05-01T23:59:59.000Z

317

SWIFT X-RAY TELESCOPE MONITORING OF FERMI-LAT GAMMA-RAY SOURCES OF INTEREST  

Science Conference Proceedings (OSTI)

We describe a long-term Swift monitoring program of Fermi gamma-ray sources, particularly the 23 gamma-ray ''sources of interest''.We present a systematic analysis of the Swift X-Ray Telescope light curves and hardness ratios of these sources, and we calculate excess variability. We present data for the time interval of 2004 December 22 through 2012 August 31. We describe the analysis methods used to produce these data products, and we discuss the availability of these data in an online repository, which continues to grow from more data on these sources and from a growing list of additional sources. This database should be of use to the broad astronomical community for long-term studies of the variability of these objects and for inclusion in multiwavelength studies.

Stroh, Michael C.; Falcone, Abe D. [Department of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802 (United States)

2013-08-15T23:59:59.000Z

318

All Sky Cameras for the characterization of the Cherenkov Telescope Array candidate sites  

E-Print Network (OSTI)

The All Sky Camera (ASC) was developed as a universal device for the monitoring of the night sky quality. Eight ASCs are already installed and measure night sky parameters at eight of the candidate sites of the Cherenkov Telescope Array (CTA) gamma-ray observatory. The ACS system consists of an astronomical CCD camera, a fish eye lens, a control computer and associated electronics. The measurement is carried out during astronomical night. The images are automatically taken every 5 minutes and automatically processed using the control computer of the device. The analysis results are the cloud fraction (the percentage of the sky covered by clouds) and night sky brightness (in mag/arcsec$^{2}$)

Mandát, Dušan; Ebr, Jan; Hrabovský, Miroslav; Prouza, Michael; Bulik, Tomasz; Allekotte, Ingomar

2013-01-01T23:59:59.000Z

319

Prospects for the CERN Axion Solar Telescope Sensitivity to 14.4 keV Axions  

E-Print Network (OSTI)

The CERN Axion Solar Telescope (CAST) is searching for solar axions using the 9.0 T strong and 9.26 m long transverse magnetic field of a twin aperture LHC test magnet, where axions could be converted into X-rays via reverse Primakoff process. Here we explore the potential of CAST to search for 14.4 keV axions that could be emitted from the Sun in M1 nuclear transition between the first, thermally excited state, and the ground state of 57Fe nuclide. Calculations of the expected signals, with respect to the axion-photon coupling, axion-nucleon coupling and axion mass, are presented in comparison with the experimental sensitivity.

Jakovcic, K; Aune, S; Avignone, F T; Barth, K; Belov, A; Beltrn, B; Bruninger, H; Carmona, J M; Cebrin, S; Collar, J I; Dafni, T; Davenport, M; Di Lella, L; Eleftheriadis, C; Fanourakis, G K; Ferrer-Ribas, E; Fischer, H; Franz, J; Friedrich, P; Geralis, T; Giomataris, Ioanis; Gninenko, S; Hasinoff, M D; Heinsius, F H; Hoffmann, Dieter H H; Irastorza, I G; Jacoby, J; Kang, D; Knigsmann, K; Kotthaus, R; Krcmar, M; Kousouris, a K; Kuster, M; Laki, B; Lasseur, C; Liolios, A; Ljubici, A; Lutz, G; Luzn, G; Miller, D W; Morales, A; Morales, J; Ortiz, A; Papaevangelou, T; Placci, A; Raffelt, G; Ruz, J; Riege, H; Semertzidis, Y K; Serpico, Pasquale Dario; Stewart, o L; Vieira, J D; Villar, J; Vogel, J; Walckiers, L; Zioutas, K; Jakovcic, Kresimir

2007-01-01T23:59:59.000Z

320

SIGGMA: A SURVEY OF IONIZED GAS IN THE GALAXY, MADE WITH THE ARECIBO TELESCOPE  

SciTech Connect

A Survey of Ionized Gas in the Galaxy, made with the Arecibo telescope (SIGGMA), uses the Arecibo L-band Feed Array (ALFA) to fully sample the Galactic plane (30 Degree-Sign {<=} l {<=} 75 Degree-Sign and -2 Degree-Sign {<=} b {<=} 2 Degree-Sign ; 175 Degree-Sign {<=} l {<=} 207 Degree-Sign and -2 Degree-Sign {<=} b {<=} 1 Degree-Sign ) observable with the telescope in radio recombination lines (RRLs). Processed data sets are being produced in the form of data cubes of 2 Degree-Sign (along l) Multiplication-Sign 4 Degree-Sign (along b) Multiplication-Sign 151 (number of channels), archived and made public. The 151 channels cover a velocity range of 600 km s{sup -1} and the velocity resolution of the survey changes from 4.2 km s{sup -1} to 5.1 km s{sup -1} from the lowest frequency channel to the highest frequency channel. RRL maps with 3.'4 resolution and a line flux density sensitivity of {approx}0.5 mJy will enable us to identify new H II regions, measure their electron temperatures, study the physics of photodissociation regions with carbon RRLs, and investigate the origin of the extended low-density medium. Twelve Hn{alpha} lines fall within the 300 MHz bandpass of ALFA; they are resampled to a common velocity resolution to improve the signal-to-noise ratio (S/N) by a factor of three or more and preserve the line width. SIGGMA will produce the most sensitive fully sampled RRL survey to date. Here, we discuss the observing and data reduction techniques in detail. A test observation toward the H II region complex S255/S257 has detected Hn{alpha} and Cn{alpha} lines with S/N > 10.

Liu, B. [National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012 (China); McIntyre, T. [University of New Mexico, Albuquerque, NM 87131 (United States); Terzian, Y. [Cornell University, Ithaca, NY 14853 (United States); Minchin, R. [Arecibo Observatory, HC03 Box 53995, Arecibo 00612, PR (United States); Anderson, L. [West Virginia University, Morgantown, WV 26506 (United States); Churchwell, E. [University of Wisconsin-Madison, Madison, WI 53706 (United States); Lebron, M. [University of Puerto Rico, P.O. Box 23323, 00931-3323, San Juan (Puerto Rico); Roshi, D. Anish [National Radio Astronomy Observatory, Green Bank and Charlottesville, VA 22903 (United States)

2013-10-01T23:59:59.000Z

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


321

ROTATION MEASURE SYNTHESIS OF GALACTIC POLARIZED EMISSION WITH THE DRAO 26-m TELESCOPE  

SciTech Connect

Radio polarimetry at decimeter wavelengths is the principal source of information on the Galactic magnetic field. The diffuse polarized emission is strongly influenced by Faraday rotation in the magneto-ionic medium and rotation measure (RM) is the prime quantity of interest, implying that all Stokes parameters must be measured over wide frequency bands with many frequency channels. The Dominion Radio Astrophysical Observatory (DRAO) 26 m Telescope has been equipped with a wide-band feed, a polarization transducer to deliver both hands of circular polarization, and a receiver, all operating from 1277 to 1762 MHz. Half-power beamwidth is between 40 and 30 arcmin. A digital Field-Programmable Gate Array spectrometer, based on commercially available components, produces all Stokes parameters in 2048 frequency channels over a 485-MHz bandwidth. Signals are digitized to 8 bits and a Fast Fourier Transform is applied to each data stream. Stokes parameters are then generated in each frequency channel. This instrument is in use at DRAO for a Northern sky polarization survey. Observations consist of scans up and down the Meridian at a drive rate of {approx}0.{sup 0}9 per minute to give complete coverage of the sky between declinations -30 deg. and 90 deg. This paper presents a complete description of the receiver and data acquisition system. Only a small fraction of the frequency band of operation is allocated for radio astronomy, and about 20% of the data are lost to interference. The first 8% of data from the survey are used for a proof-of-concept study, which has led to the first application of RM-Synthesis to the diffuse Galactic emission obtained with a single-antenna telescope. We find RM values for the diffuse emission as high as {approx}{+-}100 rad m{sup -2}, much higher than recorded in earlier work.

Wolleben, M.; Landecker, T. L.; Hovey, G. J.; Messing, R.; Davison, O. S.; House, N. L.; Somaratne, K. H. M. S.; Tashev, I. [National Research Council of Canada, Herzberg Institute of Astrophysics, Dominion Radio Astrophysical Observatory, P.O. Box 248, Penticton, British Columbia V2A 6J9 (Canada)], E-mail: maik.wolleben@nrc.gc.ca

2010-04-15T23:59:59.000Z

322

Upper Estimates for Banach Spaces  

E-Print Network (OSTI)

We study the relationship of dominance for sequences and trees in Banach spaces. In the context of sequences, we prove that domination of weakly null sequences is a uniform property. More precisely, if $(v_i)$ is a normalized basic sequence and $X$ is a Banach space such that every normalized weakly null sequence in $X$ has a subsequence that is dominated by $(v_i)$, then there exists a uniform constant $C\\geq1$ such that every normalized weakly null sequence in $X$ has a subsequence that is $C$-dominated by $(v_i)$. We prove as well that if $V=(v_i)_{i=1}^\\infty$ satisfies some general conditions, then a Banach space $X$ with separable dual has subsequential $V$ upper tree estimates if and only if it embeds into a Banach space with a shrinking FDD which satisfies subsequential $V$ upper block estimates. We apply this theorem to Tsirelson spaces to prove that for all countable ordinals $\\alpha$ there exists a Banach space $X$ with Szlenk index at most $\\omega^{\\alpha \\omega +1}$ which is universal for all Banach spaces with Szlenk index at most $\\omega^{\\alpha\\omega}$.

Freeman, Daniel B.

2009-08-01T23:59:59.000Z

323

Integral Transforms Connecting the Hardy space with Barut-Girardello Spaces  

E-Print Network (OSTI)

We construct a one parameter family of integral transforms connecting the classical Hardy space with a class of weighted Bergman spaces called Barut-Girardello spaces.

Zouhair Mouayn

2010-03-16T23:59:59.000Z

324

Bayesian atmospheric retrieval for exoplanets : uniqueness of exoplanet spectra, characterizations of super-earths, and evaluations of dedicated space telescope designs  

E-Print Network (OSTI)

After centuries of studying the eight planets in our solar system, recent improvements in technology have given us the unprecedented opportunity to detect planets orbiting stars other than the sun, so-called exoplanets. ...

Benneke, Björn

2013-01-01T23:59:59.000Z

325

Spectral measurements of hydrogen Lyman-alpha in the atmospheres of Venus and Jupiter using a sounding rocket and the Hubble Space Telescope  

E-Print Network (OSTI)

The Lyman-alpha emission is a key signature of the presence of hydrogen, and from this emission many properties of planetary atmospheres can be analyzed. Two projects are studying this emission on two planets for two ...

Corbin, Benjamin Andrew

2011-01-01T23:59:59.000Z

326

Cone structure of $L^2$-Wasserstein spaces  

E-Print Network (OSTI)

In this paper, we prove that if a base space has a cone structure, then so does its $L^2$-Wasserstein space. Furthermore, we investigate relations between the base spaces of the both cones. Conversely, we show when an $L^2$-Wasserstein space has a cone structure satisfying certain conditions, then its underlying space is also a cone.

Takatsu, Asuka

2008-01-01T23:59:59.000Z

327

On Algebraic Multi-Ring Spaces  

E-Print Network (OSTI)

A Smarandache multi-space is a union of $n$ spaces $A_1,A_2,..., A_n$ with some additional conditions holding. Combining Smarandache multi-spaces with rings in classical ring theory, the conception of multi-ring spaces is introduced. Some characteristics of a multi-ring space are obtained in this paper.

Linfan Mao

2005-10-22T23:59:59.000Z

328

BNL NASA Space Radiation Laboratory  

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

Purpose: To use beams of heavy ions provided by the Booster accelerator at Brookhaven to study the effects of simulated space radiation on biological and physical systems, with the goal of developing methods and materials to reduce the risk to human beings on prolonged space missions of the effects of ionizing radiation Sponsor: National Aeronautics and Space Administration (NASA) Project cost $34 million over 4 years Operating costs Nearly $8 million per year in 2007 Features * beams of heavy ions extracted from the Booster accelerator with masses and energies similar to the cosmic rays encountered in space: * 1-billion electron volt (GeV)/nucleon iron-56 * 0.3-GeV/nucleon gold-97 * 0.6-GeV/nucleon silicon-28 * 1-GeV/nucleon protons * 1-GeV/nucleon titanium

329

Environmental Design Space model assessment  

E-Print Network (OSTI)

The Environmental Design Space (EDS) is a multi-disciplinary design tool used to explore trade-offs among aircraft fuel burn, emissions, and noise. This thesis uses multiple metrics to assess an EDS model of a Boeing 777 ...

Spindler, Phillip Michael

2007-01-01T23:59:59.000Z

330

TCP extensions for space communications  

Science Conference Proceedings (OSTI)

The space communication environment and mobile and wireless communication environments show many similarities when observed from the perspective of a transport protocol. Both types of environments exhibit loss caused by data corruption and link outage, ...

Robert C. Durst; Gregory J. Miller; Eric J. Travis

1997-10-01T23:59:59.000Z

331

Coordinate transformations in quaternion spaces  

E-Print Network (OSTI)

The quaternion spaces can be used to describe the property of electromagnetic field and gravitational field. In the quaternion space, some coordinate transformations can be deduced from the feature of quaternions, including Lorentz transformation and Galilean transformation etc., when the coordinate system is transformed into others. And some coordinate transformations with variable speed of light can be obtained in the electromagnetic field and gravitational field.

Zihua Weng

2008-08-31T23:59:59.000Z

332

Dynamical 3-Space: Emergent Gravity  

E-Print Network (OSTI)

The laws of gravitation devised by Newton, and by Hilbert and Einstein, have failed many experimental and observational tests, namely the bore hole g anomaly, flat rotation curves for spiral galaxies, supermassive black hole mass spectrum, uniformly expanding universe, cosmic filaments, laboratory G measurements, galactic EM bending, precocious galaxy formation,.. The response has been the introduction of the new epicycles: ``dark matter", ``dark energy", and others. To understand gravity we must restart with the experimental discoveries by Galileo, and following a heuristic argument we are led to a uniquely determined theory of a dynamical 3-space. That 3-space exists has been missed from the beginning of physics, although it was 1st directly detected by Michelson and Morley in 1887. Uniquely generalising the quantum theory to include this dynamical 3-space we deduce the response of quantum matter and show that it results in a new account of gravity, and explains the above anomalies and others. The dynamical theory for this 3-space involves G, which determines the dissipation rate of space by matter, and alpha, which experiments and observation reveal to be the fine structure constant. For the 1st time we have a comprehensive account of space and matter and their interaction - gravity.

Reginald T Cahill

2011-02-16T23:59:59.000Z

333

Spaces of Quantum Field Theories  

E-Print Network (OSTI)

The concept of a "space of quantum field theories" or "theory space" was set out in the 1970's in work of Wilson, Friedan and others. This structure should play an important role in organizing and classifying QFTs, and in the study of the string landscape, allowing us to say when two theories are connected by finite variations of the couplings or by RG flows, when a sequence of QFTs converges to another QFT, and bounding the amount of information needed to uniquely specify a QFT, enabling us to estimate their number. As yet we do not have any definition of theory space which can be used to make such arguments. In this talk, we will describe various concepts and tools which should be developed for this purpose, inspired by the analogous mathematical problem of studying the space of Riemannian manifolds. We state two general conjectures about the space of two-dimensional conformal field theories, and we define a distance function on this space, which gives a distance between any pair of theories, whether or not they are connected by varying moduli. Based on talks given at QTS6 (University of Kentucky), Erice, Texas A& M, and Northwestern University. To appear in the proceedings of QTS6.

Michael R. Douglas

2010-05-16T23:59:59.000Z

334

Deep Space Mission Radiation Shielding Optimization  

Science Conference Proceedings (OSTI)

Providing protection against the hazards of space radiation is a major challenge to the exploration and development of space. The great cost of added radiation shielding is a potential limiting factor in deep space missions. In the present report, we ...

Tripathi R. K.; Wilson J. W.; Cucinotta F. A.; Nealy J. E.; Clowdsley M. S.; Kim M-H. Y.

2001-07-01T23:59:59.000Z

335

Dark energy constraints from a space-based supernova survey  

E-Print Network (OSTI)

We present a forecast of dark energy constraints that could be obtained from a large sample of distances to Type Ia supernovae detected and measured from space. We simulate the supernova events as they would be observed by a EUCLID-like telescope with its two imagers, assuming those would be equipped with 4 visible and 3 near infrared swappable filters. We account for known systematic uncertainties affecting the cosmological constraints, including those arising through the training of the supernova model used to fit the supernovae light curves. Using conservative assumptions and Planck priors, we find that a 18 month survey would yield constraints on the dark energy equation of state comparable to the cosmic shear approach in EUCLID: a variable two-parameter equation of state can be constrained to ~0.03 at z~0.3. These constraints are derived from distances to about 13,000 supernovae out to z=1.5, observed in two cones of 10 and 50 deg^2. These constraints do not require measuring a nearby supernova sample fr...

Astier, P; Pain, R; Balland, C

2010-01-01T23:59:59.000Z

336

Sustainable Spaces Inc | Open Energy Information  

Open Energy Info (EERE)

Spaces Inc Jump to: navigation, search Name Sustainable Spaces Inc. Place San Francisco, California Zip 94103 Sector Carbon Product California-based provider of energy audits and...

337

Building Technologies Office: Simplified Space Conditioning Systems...  

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

Simplified Space Conditioning Systems for Energy Efficient Homes Expert Meeting to someone by E-mail Share Building Technologies Office: Simplified Space Conditioning Systems for...

338

Building Technologies Office: Simplified Space Conditioning Systems...  

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

Simplified Space Conditioning Systems for Energy Efficient Homes Expert Meeting Building America hosted the "Simplified Space Conditioning Systems for Energy Efficient Homes"...

339

Total Space Heating Water Heating Cook-  

Gasoline and Diesel Fuel Update (EIA)

Released: September, 2008 Total Space Heating Water Heating Cook- ing Other Total Space Heating Water Heating Cook- ing Other All Buildings* ... 222 194 17...

340

Total Space Heating Water Heating Cook-  

Gasoline and Diesel Fuel Update (EIA)

Released: September, 2008 Total Space Heating Water Heating Cook- ing Other Total Space Heating Water Heating Cook- ing Other All Buildings ... 2,100...

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


341

Total Space Heating Water Heating Cook-  

Gasoline and Diesel Fuel Update (EIA)

Released: September, 2008 Total Space Heating Water Heating Cook- ing Other Total Space Heating Water Heating Cook- ing Other All Buildings* ... 1,928 1,316...

342

Total Space Heating Water Heating Cook-  

Gasoline and Diesel Fuel Update (EIA)

Energy Consumption Survey: Energy End-Use Consumption Tables Total Space Heating Water Heating Cook- ing Other Total Space Heating Water Heating Cook- ing Other All...

343

Total Space Heating Water Heating Cook-  

Gasoline and Diesel Fuel Update (EIA)

Released: September, 2008 Total Space Heating Water Heating Cook- ing Other Total Space Heating Water Heating Cook- ing Other All Buildings* ... 1,870 1,276...

344

Total Space Heating Water Heating Cook-  

Gasoline and Diesel Fuel Update (EIA)

Released: September, 2008 Total Space Heating Water Heating Cook- ing Other Total Space Heating Water Heating Cook- ing Other All Buildings* ... 1,602 1,397...

345

Total Space Heating Water Heating Cook-  

Gasoline and Diesel Fuel Update (EIA)

Released: September, 2008 Total Space Heating Water Heating Cook- ing Other Total Space Heating Water Heating Cook- ing Other All Buildings ... 2,037...

346

Passive Solar Space Heat | Open Energy Information  

Open Energy Info (EERE)

Solar Space Heat Jump to: navigation, search TODO: Add description List of Passive Solar Space Heat Incentives Retrieved from "http:en.openei.orgwindex.php?titlePassive...

347

Solar Space Heat | Open Energy Information  

Open Energy Info (EERE)

icon Solar Space Heat Jump to: navigation, search TODO: Add description List of Solar Space Heat Incentives Retrieved from "http:en.openei.orgwindex.php?titleSolarS...

348

Verifying Mirror Technology for NGST with a Space-Qualified, Cryogenic 3.5 M Mirror  

E-Print Network (OSTI)

The lightweighting and surface accuracy targeted for NGST's 8 m primary mirror has been demonstrated in a 0.5 m prototype. Now a second, 2 m prototype weighing 40 kg in total is being fabricated at the University of Arizona under the NGST NMSD program. It will be tested in cryogenic operation in spring 1999. A third, advanced mirror system demonstrator (AMSD) is needed, the full size of an NGST segment, for flight qualification, including launch survival and extremely high reliability. The 3.5 m mirror, 1/6 the weight of HST's primary, would be made with a 2 mm thick glass face-sheet attached by adjustable screws to a carbon composite support. It would be figured as a fast telescope primary, and fully tested cryogenically to verify closed loop figure stability with simulated infrared starlight. If started in early 1999, this could be completed in 2001. Construction of the NGST mirror panels could then be undertaken on the basis of proven technology, and in time for a 2007 launch. With a diameter of 3.5 m and a weight of only 140 kg, the mirror could be incorporated into a telescope and launched to a high orbit by the Shuttle or number of other vehicles. Such a space mission would complement those already planned for scaled down tests of the unfolding of the NGST mirror segments (NEXUS) and the sunshade (ISIS). Much would be learned by running the mirror at cryogenic temperature, with a new infrared array to make preliminary observations in the 2 - 4 microns dark sky window, and a CCD to check optical image quality. This mission would be independent of the NGST, but would lay the scientific groundwork for the much more powerful telescope, as well as giving practical experience of mirror operation.

Roger Angel; Jim Burge

1998-08-11T23:59:59.000Z

349

Integration of space weather into space situational awareness  

SciTech Connect

Rapid assessment of space weather effects on satellites is a critical step in anomaly resolution and satellite threat assessment. That step, however, is often hindered by a number of factors including timely collection and delivery of space weather data and the inherent com plexity of space weather information. As part of a larger, integrated space situational awareness program, Los Alamos National Laboratory has developed prototype operational space weather tools that run in real time and present operators with customized, user-specific information. The Dynamic Radiation Environment Assimilation Model (DREAM) focuses on the penetrating radiation environment from natural or nuclear-produced radiation belts. The penetrating radiation environment is highly dynamic and highly orbit-dependent. Operators often must rely only on line plots of 2 MeV electron flux from the NOAA geosynchronous GOES satellites which is then assumed to be representative of the environment at the satellite of interest. DREAM uses data assimilation to produce a global, real-time, energy dependent specification. User tools are built around a distributed service oriented architecture (SOA) which will allow operators to select any satellite from the space catalog and examine the environment for that specific satellite and time of interest. Depending on the application operators may need to examine instantaneous dose rates and/or dose accumulated over various lengths of time. Further, different energy thresholds can be selected depending on the shielding on the satellite or instrument of interest. In order to rapidly assess the probability that space weather was the cause of anomalous operations, the current conditions can be compared against the historical distribution of radiation levels for that orbit. In the simplest operation a user would select a satellite and time of interest and immediately see if the environmental conditions were typical, elevated, or extreme based on how often those conditions occur in that orbit. This allows users to rapidly rule in or out environmental causes of anomalies. The same user interface can also allow users to drill down for more detailed quantitative information. DREAM can be run either from a distributed web-based user interface or as a stand-alone application for secure operations. In this paper we discuss the underlying structure of the DREAM model and demonstrate the user interface that we have developed . We also present some prototype data products and user interfaces for DREAM and discuss how space environment information can be seamlessly integrated into operational SSA systems.

Reeves, Geoffrey D [Los Alamos National Laboratory

2010-11-09T23:59:59.000Z

350

Infrared Transmission Spectra for Extrasolar Giant Planets  

E-Print Network (OSTI)

Among the hot Jupiters that transit their parent stars known to date, the two best candidates to be observed with transmission spectroscopy in the mid-infrared (MIR) are HD189733b and HD209458b, due to their combined characteristics of planetary density, orbital parameters and parent star distance and brightness. Here we simulate transmission spectra of these two planets during their primary eclipse in the MIR, and we present sensitivity studies of the spectra to the changes of atmospheric thermal properties, molecular abundances and C/O ratios. Our model predicts that the dominant species absorbing in the MIR on hot Jupiters are water vapor and carbon monoxide, and their relative abundances are determined by the C/O ratio. Since the temperature profile plays a secondary role in the transmission spectra of hot Jupiters compared to molecular abundances, future primary eclipse observations in the MIR of those objects might give an insight on EGP atmospheric chemistry. We find here that the absorption features caused by water vapor and carbon monoxide in a cloud-free atmosphere, are deep enough to be observable by the present and future generation of space-based observatories, such as Spitzer Space Telescope and James Webb Space Telescope. We discuss our results in light of the capabilities of these telescopes.

G. Tinetti; M. C. Liang; A. Vidal-Madjar; D. Ehrenreich; A. Lecavelier des Etangs; Y. Yung

2006-11-06T23:59:59.000Z

351

THE GREEN BANK TELESCOPE H II REGION DISCOVERY SURVEY. IV. HELIUM AND CARBON RECOMBINATION LINES  

SciTech Connect

The Green Bank Telescope H II Region Discovery Survey (GBT HRDS) found hundreds of previously unknown Galactic regions of massive star formation by detecting hydrogen radio recombination line (RRL) emission from candidate H II region targets. Since the HRDS nebulae lie at large distances from the Sun, they are located in previously unprobed zones of the Galactic disk. Here, we derive the properties of helium and carbon RRL emission from HRDS nebulae. Our target sample is the subset of the HRDS that has visible helium or carbon RRLs. This criterion gives a total of 84 velocity components (14% of the HRDS) with helium emission and 52 (9%) with carbon emission. For our highest quality sources, the average {sup 4}He{sup +}/H{sup +} abundance ratio by number, (y {sup +}), is 0.068 {+-} 0.023(1{sigma}). This is the same ratio as that measured for the sample of previously known Galactic H II regions. Nebulae without detected helium emission give robust y {sup +} upper limits. There are 5 RRL emission components with y {sup +} less than 0.04 and another 12 with upper limits below this value. These H II regions must have either a very low {sup 4}He abundance or contain a significant amount of neutral helium. The HRDS has 20 nebulae with carbon RRL emission but no helium emission at its sensitivity level. There is no correlation between the carbon RRL parameters and the 8 {mu}m mid-infrared morphology of these nebulae.

Wenger, Trey V.; Bania, T. M. [Astronomy Department, 725 Commonwealth Avenue, Boston University, Boston, MA 02215 (United States)] [Astronomy Department, 725 Commonwealth Avenue, Boston University, Boston, MA 02215 (United States); Balser, Dana S. [National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA, 22903-2475 (United States)] [National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA, 22903-2475 (United States); Anderson, L. D. [Department of Physics, West Virginia University, Morgantown, WV 26506 (United States)] [Department of Physics, West Virginia University, Morgantown, WV 26506 (United States)

2013-02-10T23:59:59.000Z

352

EXPECTED LARGE SYNOPTIC SURVEY TELESCOPE (LSST) YIELD OF ECLIPSING BINARY STARS  

Science Conference Proceedings (OSTI)

In this paper, we estimate the Large Synoptic Survey Telescope (LSST) yield of eclipsing binary stars, which will survey {approx}20,000 deg{sup 2} of the southern sky during a period of 10 years in six photometric passbands to r {approx} 24.5. We generate a set of 10,000 eclipsing binary light curves sampled to the LSST time cadence across the whole sky, with added noise as a function of apparent magnitude. This set is passed to the analysis-of-variance period finder to assess the recoverability rate for the periods, and the successfully phased light curves are passed to the artificial-intelligence-based pipeline ebai to assess the recoverability rate in terms of the eclipsing binaries' physical and geometric parameters. We find that, out of {approx}24 million eclipsing binaries observed by LSST with a signal-to-noise ratio >10 in mission lifetime, {approx}28% or 6.7 million can be fully characterized by the pipeline. Of those, {approx}25% or 1.7 million will be double-lined binaries, a true treasure trove for stellar astrophysics.

Prsa, Andrej [Department of Astronomy and Astrophysics, Villanova University, 800 East Lancaster Avenue, Villanova, PA 19085 (United States); Pepper, Joshua; Stassun, Keivan G., E-mail: andrej.prsa@villanova.edu [Physics and Astronomy Department, Vanderbilt University, 2201 West End Avenue, Nashville, TN 37235 (United States)

2011-08-15T23:59:59.000Z

353

THE COSMIC-RAY ENERGY SPECTRUM OBSERVED WITH THE SURFACE DETECTOR OF THE TELESCOPE ARRAY EXPERIMENT  

SciTech Connect

The Telescope Array (TA) collaboration has measured the energy spectrum of ultra-high energy cosmic rays (UHECRs) with primary energies above 1.6 Multiplication-Sign 10{sup 18} eV. This measurement is based upon four years of observation by the surface detector component of TA. The spectrum shows a dip at an energy of 4.6 Multiplication-Sign 10{sup 18} eV and a steepening at 5.4 Multiplication-Sign 10{sup 19} eV which is consistent with the expectation from the GZK cutoff. We present the results of a technique, new to the analysis of UHECR surface detector data, that involves generating a complete simulation of UHECRs striking the TA surface detector. The procedure starts with shower simulations using the CORSIKA Monte Carlo program where we have solved the problems caused by use of the ''thinning'' approximation. This simulation method allows us to make an accurate calculation of the acceptance of the detector for the energies concerned.

Abu-Zayyad, T.; Allen, M.; Anderson, R.; Barcikowski, E.; Belz, J. W.; Bergman, D. R.; Blake, S. A.; Cady, R.; Hanlon, W. [High Energy Astrophysics Institute and Department of Physics and Astronomy, University of Utah, Salt Lake City, Utah (United States); Aida, R. [University of Yamanashi, Interdisciplinary Graduate School of Medicine and Engineering, Kofu, Yamanashi (Japan); Azuma, R.; Fukuda, T. [Graduate School of Science and Engineering, Tokyo Institute of Technology, Meguro, Tokyo (Japan); Cheon, B. G.; Cho, E. J. [Department of Physics and Research Institute of Natural Science, Hanyang University, Seongdong-gu, Seoul (Korea, Republic of); Chiba, J. [Department of Physics, Tokyo University of Science, Noda, Chiba (Japan); Chikawa, M. [Department of Physics, Kinki University, Higashi Osaka, Osaka (Japan); Cho, W. R. [Department of Physics, Yonsei University, Seodaemun-gu, Seoul (Korea, Republic of); Fujii, H. [Institute of Particle and Nuclear Studies, KEK, Tsukuba, Ibaraki (Japan); Fujii, T. [Graduate School of Science, Osaka City University, Osaka, Osaka (Japan); Fukushima, M. [Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba (Japan); and others

2013-05-01T23:59:59.000Z

354

THE ATACAMA COSMOLOGY TELESCOPE: A MEASUREMENT OF THE PRIMORDIAL POWER SPECTRUM  

SciTech Connect

We present constraints on the primordial power spectrum of adiabatic fluctuations using data from the 2008 Southern Survey of the Atacama Cosmology Telescope (ACT) in combination with measurements from the Wilkinson Microwave Anisotropy Probe and a prior on the Hubble constant. The angular resolution of ACT provides sensitivity to scales beyond l = 1000 for resolution of multiple peaks in the primordial temperature power spectrum, which enables us to probe the primordial power spectrum of adiabatic scalar perturbations with wavenumbers up to k {approx_equal} 0.2 Mpc{sup -1}. We find no evidence for deviation from power-law fluctuations over two decades in scale. Matter fluctuations inferred from the primordial temperature power spectrum evolve over cosmic time and can be used to predict the matter power spectrum at late times; we illustrate the overlap of the matter power inferred from cosmic microwave background measurements (which probe the power spectrum in the linear regime) with existing probes of galaxy clustering, cluster abundances, and weak-lensing constraints on the primordial power. This highlights the range of scales probed by current measurements of the matter power spectrum.

Hlozek, Renee; Dunkley, Joanna; Addison, Graeme [Department of Astrophysics, Oxford University, Oxford OX1 3RH (United Kingdom); Appel, John William; Das, Sudeep; Essinger-Hileman, Thomas; Fowler, Joseph W.; Hajian, Amir; Hincks, Adam D. [Joseph Henry Laboratories of Physics, Jadwin Hall, Princeton University, Princeton, NJ 08544 (United States); Bond, J. Richard [Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON M5S 3H8 (Canada); Carvalho, C. Sofia [IPFN, IST, Av. RoviscoPais, 1049-001Lisboa, Portugal and RCAAM, Academy of Athens, Soranou Efessiou 4, 11-527 Athens (Greece); Devlin, Mark J.; Klein, Jeff [Department of Physics and Astronomy, University of Pennsylvania, 209 South 33rd Street, Philadelphia, PA 19104 (United States); Duenner, Rolando; Gallardo, Patricio [Departamento de Astronomia y Astrofisica, Facultad de Fisica, Pontificia Universidad Catolica de Chile, Casilla 306, Santiago 22 (Chile); Halpern, Mark; Hasselfield, Matthew [Department of Physics and Astronomy, University of British Columbia, Vancouver, BC V6T 1Z4 (Canada); Hilton, Matt [School of Physics and Astronomy, University of Nottingham, University Park, Nottingham, NG7 2RD (United Kingdom); Hughes, John P. [Department of Physics and Astronomy, Rutgers, The State University of New Jersey, Piscataway, NJ 08854-8019 (United States); Irwin, Kent D. [NIST Quantum Devices Group, 325 Broadway Mailcode 817.03, Boulder, CO 80305 (United States); and others

2012-04-10T23:59:59.000Z

355

THE CANADA-FRANCE-HAWAII TELESCOPE LEGACY SURVEY: STACKED IMAGES AND CATALOGS  

SciTech Connect

This paper describes the image stacks and catalogs of the Canada-France-Hawaii Telescope Legacy Survey produced using the MegaPipe data pipeline at the Canadian Astronomy Data Centre. The Legacy Survey is divided into two parts. The Deep Survey consists of four fields each of 1 deg{sup 2}, with magnitude limits (50% completeness for point sources) of u = 27.5, g = 27.9, r = 27.7, i = 27.4, and z = 26.2. It contains 1.6 Multiplication-Sign 10{sup 6} sources. The Wide Survey consists of 150 deg{sup 2} split over four fields, with magnitude limits of u = 26.0, g = 26.5, r = 25.9, i = 25.7, and z = 24.6. It contains 3 Multiplication-Sign 10{sup 7} sources. This paper describes the calibration, image stacking, and catalog generation process. The images and catalogs are available on the web through several interfaces: normal image and text file catalog downloads, a 'Google Sky' interface, an image cutout service, and a catalog database query service.

Gwyn, Stephen D. J., E-mail: Stephen.Gwyn@nrc-cnrc.gc.ca [Canadian Astronomy Data Centre, Herzberg Institute of Astrophysics, 5071 West Saanich Road, Victoria, British Columbia, V9E 2E7 (Canada)

2012-02-15T23:59:59.000Z

356

Background study for the pn-CCD detector of CERN Axion Solar Telescope  

E-Print Network (OSTI)

The CERN Axion Solar Telescope (CAST) experiment searches for axions from the Sun converted into photons with energies up to around 10 keV via the inverse Primakoff effect in the high magnetic field of a superconducting Large Hadron Collider (LHC) prototype magnet. A backside illuminated pn-CCD detector in conjunction with an X-ray mirror optics is one of the three detectors used in CAST to register the expected photon signal. Since this signal is very rare and different background components (environmental gamma radiation, cosmic rays, intrinsic radioactive impurities in the set-up, ...) entangle it, a detailed study of the detector background has been undertaken with the aim to understand and further reduce the background level of the detector. The analysis is based on measured data taken during the Phase I of CAST and on Monte Carlo simulations of different background components. This study will show that the observed background level (at a rate of (8.00+-0.07)10^-5 counts/cm^2/s/keV between 1 and 7 keV) seems to be dominated by the external gamma background due to usual activities at the experimental site, while radioactive impurities in the detector itself and cosmic neutrons could make just smaller contribution.

S. Cebrián; A. Rodríguez; M. Kuster; B. Beltrán; J. M. Carmona; H. Gómez; R. Hartmann; I. G. Irastorza; R. Kotthaus; G. Luzón; J. Morales; A. Ortiz de Solórzano; J. Ruz; L. Strüder; J. A. Villar

2007-04-23T23:59:59.000Z

357

Measurements of Secondary Cosmic Microwave Background Anisotropies with the South Pole Telescope  

E-Print Network (OSTI)

We report cosmic microwave background (CMB) power spectrum measurements from the first 100 sq. deg. field observed by the South Pole Telescope (SPT) at 150 and 220 GHz. On angular scales where the primary CMB anisotropy is dominant, ell ~ 50 at both frequencies. We combine the 150 and 220 GHz data to remove the majority of the point source power, and use the point source subtracted spectrum to detect Sunyaev-Zel'dovich (SZ) power at 2.6 sigma. At ell=3000, the SZ power in the subtracted bandpowers is 4.2 +/- 1.5 uK^2, which is significantly lower than the power predicted by a fiducial model using WMAP5 cosmological parameters. This discrepancy may suggest that contemporary galaxy cluster models overestimate the thermal pressure of intracluster gas. Alternatively, this result can be interpreted as evidence for lower values of sigma8. When combined with an estimate of the kinetic SZ contribution, the measured SZ amplitude shifts sigma8 from the primary CMB anisotropy derived constraint of 0.794 +/- 0.028 down t...

Lueker, M; Schaffer, K K; Zahn, O; Ade, P A R; Aird, K A; Benson, B A; Bleem, L E; Carlstrom, J E; Chang, C L; Cho, H M; Crawford, T M; Crites, A T; de Haan, T; Dobbs, M A; George, E M; Hall, N R; Halverson, N W; Holder, G P; Holzapfel, W L; Hrubes, J D; Joy, M; Keisler, R; Knox, L; Lee, A T; Leitch, E M; McMahon, J J; Mehl, J; Meyer, S S; Mohr, J J; Montroy, T E; Padin, S; Plagge, T; Pryke, C; Ruhl, J E; Shaw, L; Shirokoff, E; Spieler, H G; Staniszewski, Z; Stark, A A; Vanderlinde, K; Vieira, J D; Williamson, R

2009-01-01T23:59:59.000Z

358

Dielectric Analog Space-Times  

E-Print Network (OSTI)

We generalize the notion of a dielectric analog Schwarzschild black hole model to analog models of arbitrary space-times; in particular, the approach is not restricted to static space-times. This is done by establishing a correspondence between electrodynamics on a curved, vacuum manifold, with electrodynamics in a general linear dielectric residing in Minkowski space-time. The mapping is not unique, allowing for some freedom in the specification of equivalent materials, which could be useful for exploiting recent developments in the production of metamaterials. Some examples are considered, with special attention paid to the dielectric analog of the exterior Kerr geometry, which is found to be reproducible with regular, linear, dielectrics.

Robert T. Thompson; Jörg Frauendiener

2010-10-08T23:59:59.000Z

359

Quantum dynamics in dual spaces  

Science Conference Proceedings (OSTI)

Quantum mechanics gives us information about spectra of dynamical variables and transition rates including scattering cross sections. They can be exhibited as spectral information in analytically continued spaces and their duals. Quantum mechanics formulated in these generalized spaces is used to study scattering and time evolution. It is shown that the usual asymptotic condition is inadequate to deal with scattering of composite or unstable particles. Scattering theory needs amendment when the interacting system is not isospectral with the free Hamiltonian, and the amendment is formulated. Perturbation theory in generalized spaces is developed and used to study the deletion and augmentation of the spectrum of the Hamiltonian. A complete set of algebraically independent constants for an interacting system is obtained. The question of the breaking of time symmetry is discussed.

Sudarshan, E.C.G.

1993-12-31T23:59:59.000Z

360

National Aeronautics and Space Administration SpaceMathVI  

E-Print Network (OSTI)

data. The problems were designed to be `one-pagers' with a Teacher's Guide and Answer Key as a second;Answer Key Problem 1 - How many atoms of hydrogen (H), carbon (C) and oxygen (O) are contained the planets be after 6 years? Space Math http://spacemath.gsfc.nasa.gov #12;2Answer Key Problem 1 - Students

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361

Simulation and analysis of laser guide star adaptive optics systems for the eight to ten meter class telescopes  

Science Conference Proceedings (OSTI)

This paper discusses the design and analysis of laser-guided adaptive optic systems for the large, 8--10 meter class telescopes. We describe a technique for calculating the expected modulation transfer function and the point spread function for a closed loop adaptive optics system, parameterized by the degree of correction and the seeing conditions. The results agree closely with simulations and experimental data, and validate well known scaling law models even at low order correction. Scaling law.model analysis of a proposed adaptive optics system at the Keck telescope leads to the conclusion that a single laser guide star beacon will be adequate for diffraction limited imaging at wavelengths between 1 and 3 am with reasonable coverage of the sky. Cone anisoplanatism will dominate wavefront correction error at the visible wavelengths unless multiple laser guide stars are used.

Gavel, D.T.; Olivier, S.S.

1994-03-01T23:59:59.000Z

362

Monte Carlo Studies of Geomagnetic Field Effects on the Imaging Air Cherenkov Technique for the MAGIC Telescope Site  

E-Print Network (OSTI)

Imaging air Cherenkov telescopes (IACTs) detect the Cherenkov light from extensive air showers (EAS) initiated by very high energy (VHE) gamma-rays impinging on the Earth's atmosphere. Due to the overwhelming background from hadron induced EAS, the discrimination of the rare gamma-like events is vital. The influence of the geomagnetic field (GF) on the development of EAS can further complicate the imaging air Cherenkov technique. The amount and the angular distribution of Cherenkov light from EAS can be obtained by means of Monte Carlo (MC) simulations. Here we present the results from dedicated MC studies of GF effects on images from gamma-ray initiated EAS for the MAGIC telescope site, where the GF strength is ~40 micro Tesla. The results from the MC studies suggest that GF effects degrade not only measurements of very low energy gamma-rays below ~100 GeV but also those at TeV-energies.

S. C. Commichau; A. Biland; J. L. Contreras; R. de los Reyes; A. Moralejo; J. Sitarek; D. Sobczynska

2008-02-18T23:59:59.000Z

363

Exponential Smoothing and State-Space Modeling  

Science Conference Proceedings (OSTI)

Exponential Smoothing and State-Space Modeling. Purpose: Exponential smoothing methods for forecasting are sometimes ...

2010-09-08T23:59:59.000Z

364

Some moduli spaces of Bridgeland's stability conditions  

E-Print Network (OSTI)

We shall study some moduli spaces of Bridgeland's semi-stable objects on abelian surfaces and K3 surfaces with Picard number 1. Under some conditions, we show that the moduli spaces are isomorphic to the moduli spaces of Gieseker semi-stable sheaves. We also study the ample cone of the moduli spaces.

Minamide, Hiroki; Yoshioka, Kota

2011-01-01T23:59:59.000Z

365

Free loop spaces in topology and  

E-Print Network (OSTI)

Free loop spaces in topology and physics Kathryn Hess What is the space of free loops? Enumeration of geodesics Hochschild and cyclic homology Homological conformal field theories Free loop spaces in topology Meeting of the Edinburgh Mathematical Society Glasgow, 14 November 2008 #12;Free loop spaces in topology

Thévenaz, Jacques

366

Some necessary conditions for vector space partitions  

E-Print Network (OSTI)

Some new necessary conditions for the existence of vector space partitions are derived. They are applied to the problem of finding the maximum number of spaces of dimension t in a vector space partition of V(2t,q) that contains m_d spaces of dimension d, where t/2spaces of other dimensions. It is also discussed how this problem is related to maximal partial (t-1)-spreads in V(2t,q). We also give a lower bound for the number of spaces in a vector space partition and verify that this bound is tight.

Heden, Olof

2011-01-01T23:59:59.000Z

367

Debris and Future Space Activities  

E-Print Network (OSTI)

Debris and Future Space Activities Prof. Joel R. Primack Physics Department University eleven year cycle, it heats the upper atmosphere and makes it expand so that debris and spacecraft in low which overflows occasionally and washes only the lowest hillsides clear of debris. Debris in orbit

California at Santa Cruz, University of

368

National Aeronautics and Space Administration  

E-Print Network (OSTI)

and Contracting Processes. Developing adequate cost estimates, managing program costs, and ensuring that NASA, simultaneously, developing the next generation of space vehicles. · Managing Risk to People, Equipment to address continued problems such as NASA's internal controls over property, plant, and equipment

Christian, Eric

369

National Aeronautics and Space Administration  

E-Print Network (OSTI)

of turbulent flow with phase transitions and radiation · Extreme weather and climate change -> is essentially and carbon with the ocean/ land/ice surface are mediated by turbulence #12;National Aeronautics and Space-Diffusivity (ED) approach In ED closure the sub-grid flux is parameterized as where k is the diffusivity

Bordoni, Simona

370

Fusion for Earth and Space  

Science Conference Proceedings (OSTI)

The compact reactor concept (Williams, 2007) has the potential to provide clean, safe and unlimited supply of energy for Earth and Space applications. The concept is a potential fusion reactor wherein deuterium nuclei are preferentially fused into helium nuclei. Because the deuterium nuclei are preferentially fused into helium nuclei at temperatures and energies lower than specified by the standard model there is no harmful radiation as a byproduct of this fusion process. Therefore, a reactor using this reaction does not need any shielding to contain such radiation. The energy released from each reaction and the absence of shielding makes the deuterium-plus-deuterium-to-helium (DDH) reactor very compact when compared to other reactors, both fission and fusion types. Moreover, the potential energy output per reactor weight and the absence of harmful radiation makes the DDH reactor an ideal candidate for individual home and space power. The concept also would make it possible for each plant or remote location to have it's own power source, on site, without the need for a connection to the power grid. This would minimize, or eliminate, power blackouts. The concept could replace large fission reactors and fossil fuel power plants plus provide energy for ships, locomotives, trucks and autos. It would make an ideal source of energy for space power applications and for space propulsion.

Williams, Pharis E

2009-03-16T23:59:59.000Z

371

On Algebraic Multi-Group Spaces  

E-Print Network (OSTI)

A Smarandache multi-space is a union of $n$ spaces $A_1,A_2,..., A_n$ with some additional conditions holding. Combining classical of a group with Smarandache multi-spaces, the conception of a multi-group space is introduced in this paper, which is a generalization of the classical algebraic structures, such as the group, filed, body, $...$, etc.. Similar to groups, some characteristics of a multi-group space are obtained in this paper.

Linfan Mao

2005-10-20T23:59:59.000Z

372

THE GREEN BANK TELESCOPE H II REGION DISCOVERY SURVEY. III. KINEMATIC DISTANCES  

SciTech Connect

Using the H I emission/absorption method, we resolve the kinematic distance ambiguity and derive distances for 149 of 182 (82%) H II regions discovered by the Green Bank Telescope H II Region Discovery Survey (GBT HRDS). The HRDS is an X-band (9 GHz, 3 cm) GBT survey of 448 previously unknown H II regions in radio recombination line and radio continuum emission. Here, we focus on HRDS sources from 67 Degree-Sign {>=} l {>=} 18 Degree-Sign , where kinematic distances are more reliable. The 25 HRDS sources in this zone that have negative recombination line velocities are unambiguously beyond the orbit of the Sun, up to 20 kpc distant. They are the most distant H II regions yet discovered. We find that 61% of HRDS sources are located at the far distance, 31% at the tangent-point distance, and only 7% at the near distance. 'Bubble' H II regions are not preferentially located at the near distance (as was assumed previously) but average 10 kpc from the Sun. The HRDS nebulae, when combined with a large sample of H II regions with previously known distances, show evidence of spiral structure in two circular arc segments of mean Galactocentric radii of 4.25 and 6.0 kpc. We perform a thorough uncertainty analysis to analyze the effect of using different rotation curves, streaming motions, and a change to the solar circular rotation speed. The median distance uncertainty for our sample of H II regions is only 0.5 kpc, or 5%. This is significantly less than the median difference between the near and far kinematic distances, 6 kpc. The basic Galactic structure results are unchanged after considering these sources of uncertainty.

Anderson, L. D. [Department of Physics, West Virginia University, Morgantown, WV 26506 (United States); Bania, T. M. [Institute for Astrophysical Research, Department of Astronomy, Boston University, 725 Commonwealth Avenue, Boston, MA 02215 (United States); Balser, Dana S. [National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903-2475 (United States); Rood, Robert T., E-mail: Loren.Anderson@mail.wvu.edu [Astronomy Department, University of Virginia, P.O. Box 3818, Charlottesville, VA 22903-0818 (United States)

2012-07-20T23:59:59.000Z

373

DETECTION OF SMALL-SCALE GRANULAR STRUCTURES IN THE QUIET SUN WITH THE NEW SOLAR TELESCOPE  

SciTech Connect

Results of a statistical analysis of solar granulation are presented. A data set of 36 images of a quiet-Sun area on the solar disk center was used. The data were obtained with the 1.6 m clear aperture New Solar Telescope at Big Bear Solar Observatory and with a broadband filter centered at the TiO (705.7 nm) spectral line. The very high spatial resolution of the data (diffraction limit of 77 km and pixel scale of 0.''0375) augmented by the very high image contrast (15.5% {+-} 0.6%) allowed us to detect for the first time a distinct subpopulation of mini-granular structures. These structures are dominant on spatial scales below 600 km. Their size is distributed as a power law with an index of -1.8 (which is close to the Kolmogorov's -5/3 law) and no predominant scale. The regular granules display a Gaussian (normal) size distribution with a mean diameter of 1050 km. Mini-granular structures contribute significantly to the total granular area. They are predominantly confined to the wide dark lanes between regular granules and often form chains and clusters, but different from magnetic bright points. A multi-fractality test reveals that the structures smaller than 600 km represent a multi-fractal, whereas on larger scales the granulation pattern shows no multi-fractality and can be considered as a Gaussian random field. The origin, properties, and role of the population of mini-granular structures in the solar magnetoconvection are yet to be explored.

Abramenko, V. I.; Yurchyshyn, V. B.; Goode, P. R. [Big Bear Solar Observatory, 40386 N. Shore Lane, Big Bear City, CA 92314 (United States); Kitiashvili, I. N.; Kosovichev, A. G. [W. W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305 (United States)

2012-09-10T23:59:59.000Z

374

An observability study for the tentatively identified 3EG sources likely to be detected by the next-generation Cherenkov telescopes  

E-Print Network (OSTI)

We present a compilation of data on the 22 tentatively identified gamma-ray sources from the Third EGRET Catalog which may be detected by the next-generation imaging atmospheric Cherenkov telescopes.

D. Petry; O. Reimer

2001-06-07T23:59:59.000Z

375

High Energy Laser for Space Debris Removal  

SciTech Connect

The National Ignition Facility (NIF) and Photon Science Directorate at Lawrence Livermore National Laboratory (LLNL) has substantial relevant experience in the construction of high energy lasers, and more recently in the development of advanced high average power solid state lasers. We are currently developing new concepts for advanced solid state laser drivers for the Laser Inertial Fusion Energy (LIFE) application, and other high average power laser applications that could become central technologies for use in space debris removal. The debris population most readily addressed by our laser technology is that of 0.1-10 cm sized debris in low earth orbit (LEO). In this application, a ground based laser system would engage an orbiting target and slow it down by ablating material from its surface which leads to reentry into the atmosphere, as proposed by NASA's ORION Project. The ORION concept of operations (CONOPS) is also described in general terms by Phipps. Key aspects of this approach include the need for high irradiance on target, 10{sup 8} to 10{sup 9} W/cm{sup 2}, which favors short (i.e., picoseconds to nanoseconds) laser pulse durations and high energy per pulse ({approx} > 10 kJ). Due to the target's orbital velocity, the potential duration of engagement is only of order 100 seconds, so a high pulse repetition rate is also essential. The laser technology needed for this application did not exist when ORION was first proposed, but today, a unique combination of emerging technologies could create a path to enable deployment in the near future. Our concepts for the laser system architecture are an extension of what was developed for the National Ignition Facility (NIF), combined with high repetition rate laser technology developed for Inertial Fusion Energy (IFE), and heat capacity laser technology developed for military applications. The 'front-end' seed pulse generator would be fiber-optics based, and would generate a temporally, and spectrally tailored pulse designed for high transmission through the atmosphere, as well as efficient ablative coupling to the target. The main amplifier would use either diode-pumped or flashlamp-pumped solid state gain media, depending on budget constraints of the project. A continuously operating system would use the gas-cooled amplifier technology developed for Mercury, while a burst-mode option would use the heat capacity laser technology. The ground-based system that we propose is capable of rapid engagement of targets whose orbits cross over the site, with potential for kill on a single pass. Very little target mass is ablated per pulse so the potential to create additional hazardous orbiting debris is minimal. Our cost estimates range from $2500 to $5000 per J depending on choices for laser gain medium, amplifier pump source, and thermal management method. A flashlamp-pumped, Nd:glass heat-capacity laser operating in the burst mode would have costs at the lower end of this spectrum and would suffice to demonstrate the efficacy of this approach as a prototype system. A diode-pumped, gas-cooled laser would have higher costs but could be operated continuously, and might be desirable for more demanding mission needs. Maneuverability can be incorporated in the system design if the additional cost is deemed acceptable. The laser system would need to be coupled with a target pointing and tracking telescope with guide-star-like wavefront correction capability.

Barty, C; Caird, J; Erlandson, A; Beach, R; Rubenchik, A

2009-10-30T23:59:59.000Z

376

High Energy Laser for Space Debris Removal  

SciTech Connect

The National Ignition Facility (NIF) and Photon Science Directorate at Lawrence Livermore National Laboratory (LLNL) has substantial relevant experience in the construction of high energy lasers, and more recently in the development of advanced high average power solid state lasers. We are currently developing new concepts for advanced solid state laser drivers for the Laser Inertial Fusion Energy (LIFE) application, and other high average power laser applications that could become central technologies for use in space debris removal. The debris population most readily addressed by our laser technology is that of 0.1-10 cm sized debris in low earth orbit (LEO). In this application, a ground based laser system would engage an orbiting target and slow it down by ablating material from its surface which leads to reentry into the atmosphere, as proposed by NASA's ORION Project. The ORION concept of operations (CONOPS) is also described in general terms by Phipps. Key aspects of this approach include the need for high irradiance on target, 10{sup 8} to 10{sup 9} W/cm{sup 2}, which favors short (i.e., picoseconds to nanoseconds) laser pulse durations and high energy per pulse ({approx} > 10 kJ). Due to the target's orbital velocity, the potential duration of engagement is only of order 100 seconds, so a high pulse repetition rate is also essential. The laser technology needed for this application did not exist when ORION was first proposed, but today, a unique combination of emerging technologies could create a path to enable deployment in the near future. Our concepts for the laser system architecture are an extension of what was developed for the National Ignition Facility (NIF), combined with high repetition rate laser technology developed for Inertial Fusion Energy (IFE), and heat capacity laser technology developed for military applications. The 'front-end' seed pulse generator would be fiber-optics based, and would generate a temporally, and spectrally tailored pulse designed for high transmission through the atmosphere, as well as efficient ablative coupling to the target. The main amplifier would use either diode-pumped or flashlamp-pumped solid state gain media, depending on budget constraints of the project. A continuously operating system would use the gas-cooled amplifier technology developed for Mercury, while a burst-mode option would use the heat capacity laser technology. The ground-based system that we propose is capable of rapid engagement of targets whose orbits cross over the site, with potential for kill on a single pass. Very little target mass is ablated per pulse so the potential to create additional hazardous orbiting debris is minimal. Our cost estimates range from $2500 to $5000 per J depending on choices for laser gain medium, amplifier pump source, and thermal management method. A flashlamp-pumped, Nd:glass heat-capacity laser operating in the burst mode would have costs at the lower end of this spectrum and would suffice to demonstrate the efficacy of this approach as a prototype system. A diode-pumped, gas-cooled laser would have higher costs but could be operated continuously, and might be desirable for more demanding mission needs. Maneuverability can be incorporated in the system design if the additional cost is deemed acceptable. The laser system would need to be coupled with a target pointing and tracking telescope with guide-star-like wavefront correction capability.

Barty, C; Caird, J; Erlandson, A; Beach, R; Rubenchik, A

2009-10-30T23:59:59.000Z

377

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

E-Print Network (OSTI)

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

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

2010-01-01T23:59:59.000Z

378

Characterization, performance and optimization of PVDF as a piezoelectric film for advanced space mirror concepts.  

Science Conference Proceedings (OSTI)

Piezoelectric polymers based on polyvinylidene fluoride (PVDF) are of interest for large aperture space-based telescopes as adaptive or smart materials. Dimensional adjustments of adaptive polymer films depend on controlled charge deposition. Predicting their long-term performance requires a detailed understanding of the piezoelectric material features, expected to suffer due to space environmental degradation. Hence, the degradation and performance of PVDF and its copolymers under various stress environments expected in low Earth orbit has been reviewed and investigated. Various experiments were conducted to expose these polymers to elevated temperature, vacuum UV, {gamma}-radiation and atomic oxygen. The resulting degradative processes were evaluated. The overall materials performance is governed by a combination of chemical and physical degradation processes. Molecular changes are primarily induced via radiative damage, and physical damage from temperature and atomic oxygen exposure is evident as depoling, loss of orientation and surface erosion. The effects of combined vacuum UV radiation and atomic oxygen resulted in expected surface erosion and pitting rates that determine the lifetime of thin films. Interestingly, the piezo responsiveness in the underlying bulk material remained largely unchanged. This study has delivered a comprehensive framework for material properties and degradation sensitivities with variations in individual polymer performances clearly apparent. The results provide guidance for material selection, qualification, optimization strategies, feedback for manufacturing and processing, or alternative materials. Further material qualification should be conducted via experiments under actual space conditions.

Jones, Gary D.; Assink, Roger Alan; Dargaville, Tim Richard; Chaplya, Pavel Mikhail; Clough, Roger Lee; Elliott, Julie M.; Martin, Jeffrey W.; Mowery, Daniel Michael; Celina, Mathew Christopher

2005-11-01T23:59:59.000Z

379

Discrete space-time symmetries  

SciTech Connect

Symmetries have always fascinated human beings; they are found in nature, art, and architecture. Physicists, like other scientists have often used symmetries as a basis of their understanding of nature. When the dynamics is unknown, symmetries serve to delineate and define it. When the dynamics is known, symmetries are used to study structure. These two lectures review the theory and present understanding and status of two discrete space-time symmetries,, namely parity (P) and time reversal (T).

Henley, E.M.

1992-12-31T23:59:59.000Z

380

Discrete space-time symmetries  

SciTech Connect

Symmetries have always fascinated human beings; they are found in nature, art, and architecture. Physicists, like other scientists have often used symmetries as a basis of their understanding of nature. When the dynamics is unknown, symmetries serve to delineate and define it. When the dynamics is known, symmetries are used to study structure. These two lectures review the theory and present understanding and status of two discrete space-time symmetries,, namely parity (P) and time reversal (T).

Henley, E.M.

1992-01-01T23:59:59.000Z

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


381

National Aeronautics and Space Administration  

E-Print Network (OSTI)

Any opinions, findings, and conclusions or recommendations expressed in this volume are those of the author(s) and do not necessarily reflect the views of the National Aeronautics and Space Administration. Material in this volume may be copied without restraint for library, abstract service, education, or personal research purposes; however, republication of any paper or portion thereof requires the written permission of the authors as well as the appropriate acknowledgment of this publication. Abstracts in this volume may be cited as

Curt Niebur; Nasa Headquarters; Terry Hurford; Nasa Goddard; Curt Niebur; Nasa Headquarters

2007-01-01T23:59:59.000Z

382

TCP Extensions for Space Communications  

E-Print Network (OSTI)

The space communication environment and mobile and wireless communication environments show many similarities when observed from the perspective of a transport protocol. Both types of environments exhibit loss caused by data corruption and link outage, in addition to congestion-related loss. The constraints imposed by the two environments are also similar --- power, weight, and physical volume of equipment are scarce resources. Finally, it is not uncommon for communication channel data rates to be severely limited and highly asymmetric. We are working on solutions to these types of problems for space communication environments, and we believe that these solutions may be applicable to the mobile and wireless community. As part of our work, we have defined and implemented the Space Communications Protocol Standards-Transport Protocol (SCPSTP) , a set of extensions to TCP that address the problems that we have identified. The results of our performance tests, both in the laboratory and on actual satellites, indicate that the SCPS-TP extensions yield significant improvements in throughput over unmodified TCP on error-prone links. Additionally, the SCPS modifications significantly improve performance over links with highly asymmetric data rates.

Robert C. Durst; Gregory J. Miller; Eric J. Travis

1996-01-01T23:59:59.000Z

383

Embeddings and factorizations of Banach spaces  

E-Print Network (OSTI)

One problem, considered important in Banach space theory since at least the 1970’s, asks for intrinsic characterizations of subspaces of a Banach space with an unconditional basis. A more general question is to give necessary and sufficient conditions for operators from Lp (2 space, being a subspace of a reflexive space with an unconditional basis or being a quotient of such a space, is equivalent to having the unconditional tree property. I also show that a bounded linear operator from Lp (2 spaces.

Zheng, Bentuo

2007-08-01T23:59:59.000Z

384

A MEASUREMENT OF SECONDARY COSMIC MICROWAVE BACKGROUND ANISOTROPIES WITH TWO YEARS OF SOUTH POLE TELESCOPE OBSERVATIONS  

SciTech Connect

We present the first three-frequency South Pole Telescope (SPT) cosmic microwave background (CMB) power spectra. The band powers presented here cover angular scales 2000 < l < 9400 in frequency bands centered at 95, 150, and 220 GHz. At these frequencies and angular scales, a combination of the primary CMB anisotropy, thermal and kinetic Sunyaev-Zel'dovich (SZ) effects, radio galaxies, and cosmic infrared background (CIB) contributes to the signal. We combine Planck/HFI and SPT data at 220 GHz to constrain the amplitude and shape of the CIB power spectrum and find strong evidence for nonlinear clustering. We explore the SZ results using a variety of cosmological models for the CMB and CIB anisotropies and find them to be robust with one exception: allowing for spatial correlations between the thermal SZ effect and CIB significantly degrades the SZ constraints. Neglecting this potential correlation, we find the thermal SZ power at 150 GHz and l = 3000 to be 3.65 {+-} 0.69 {mu}K{sup 2}, and set an upper limit on the kinetic SZ power to be less than 2.8 {mu}K{sup 2} at 95% confidence. When a correlation between the thermal SZ and CIB is allowed, we constrain a linear combination of thermal and kinetic SZ power: D{sup tSZ}{sub 3000} + 0.5D{sub 3000}{sup kSZ} = 4.60 {+-} 0.63 {mu}K{sup 2}, consistent with earlier measurements. We use the measured thermal SZ power and an analytic, thermal SZ model calibrated with simulations to determine {sigma}{sub 8} = 0.807 {+-} 0.016. Modeling uncertainties involving the astrophysics of the intracluster medium rather than the statistical uncertainty in the measured band powers are the dominant source of uncertainty on {sigma}{sub 8}. We also place an upper limit on the kinetic SZ power produced by patchy reionization; a companion paper uses these limits to constrain the reionization history of the universe.

Reichardt, C. L.; George, E. M.; Holzapfel, W. L. [Department of Physics, University of California, Berkeley, CA 94720 (United States); Shaw, L. [Department of Physics, Yale University, P.O. Box 208210, New Haven, CT 06520-8120 (United States); Zahn, O. [Berkeley Center for Cosmological Physics, Department of Physics, University of California, and Lawrence Berkeley National Labs, Berkeley, CA 94720 (United States); Aird, K. A. [University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637 (United States); Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Hoover, S. [Kavli Institute for Cosmological Physics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637 (United States); Cho, H. M. [NIST Quantum Devices Group, 325 Broadway Mailcode 817.03, Boulder, CO 80305 (United States); De Haan, T.; Dobbs, M. A.; Dudley, J.; Holder, G. P. [Department of Physics, McGill University, 3600 Rue University, Montreal, Quebec H3A 2T8 (Canada); Halverson, N. W. [Department of Astrophysical and Planetary Sciences and Department of Physics, University of Colorado, Boulder, CO 80309 (United States); Hou, Z., E-mail: cr@bolo.berkeley.edu [Department of Physics, University of California, One Shields Avenue, Davis, CA 95616 (United States); and others

2012-08-10T23:59:59.000Z

385

Color spaces in digital video  

SciTech Connect

Whether it`s photography, computer graphics, publishing, or video; each medium has a defined color space, or gamut, which defines the extent that a given set of RGB colors can be mixed. When converting from one medium to another, an image must go through some form of conversion which maps colors into the destination color space. The conversion process isn`t always straight forward, easy, or reversible. In video, two common analog composite color spaces are Y`tjv (used in PAL) and Y`IQ (used in NTSC). These two color spaces have been around since the beginning of color television, and are primarily used in video transmission. Another analog scheme used in broadcast studios is Y`, R`-Y`, B`-Y` (used in Betacam and Mll) which is a component format. Y`, R`-Y`,B`-Y` maintains the color information of RGB but in less space. From this, the digital component video specification, ITU-Rec. 601-4 (formerly CCIR Rec. 601) was based. The color space for Rec. 601 is symbolized as Y`CbCr. Digital video formats such as DV, Dl, Digital-S, etc., use Rec. 601 to define their color gamut. Digital composite video (for D2 tape) is digitized analog Y`UV and is seeing decreased use. Because so much information is contained in video, segments of any significant length usually require some form of data compression. All of the above mentioned analog video formats are a means of reducing the bandwidth of RGB video. Video bulk storage devices, such as digital disk recorders, usually store frames in Y`CbCr format, even if no other compression method is used. Computer graphics and computer animations originate in RGB format because RGB must be used to calculate lighting and shadows. But storage of long animations in RGB format is usually cost prohibitive and a 30 frame-per-second data rate of uncompressed RGB is beyond most computers. By taking advantage of certain aspects of the human visual system, true color 24-bit RGB video images can be compressed with minimal loss of visual information. For example, humans `see` more white-to-black (luminance) detail then red, green, or blue color detail. Also, the eye is most sensitive to green colors. Taking advantage of this, both composite and component video allocates more bandwidth for the luma (Y`) signal than the chroma signals. Y`611 is composed of 59% green`, 30% red`, and 11% blue` (prime symbol denotes gamma corrected colors). This luma signal also maintains compatibility with black and white television receivers. Component digital video converts R`G`B` signals (either from a camera or a computer) to a monochromatic brightness signal Y` (referred here as luma to distinguish it from the CIE luminance linear- light quantity), and two color difference signals Cb and Cr. These last two are the blue and red signals with the luma component subtracted out. As you know, computer graphic images are composed of red, green, and blue elements defined in a linear color space. Color monitors do not display RGB linearly. A linear RGB color space image must be gamma corrected to be displayed properly on a CRT. Gamma correction, which is approximately a 0.45 power function, must also be employed before converting an RGB image to video color space. Gamma correction is defined for video in the international standard: ITU-Rec. BT.709-4. The gamma correction transform is the same for red, green, and blue. The color coding standard for component digital video and high definition video symbolizes gamma corrected luma by Y`, the blue difference signal by Cb (Cb = B` -Y`), and the red color difference signal by Cr (Cr = R` - Y`). Component analog HDTV uses Y`PbPr. To reduce conversion errors, clip in R`G`B`, not in Y`CbCr space. View video on a video monitor, computer monitor phosphors are wrong. Use a large word size (double precision) to avoid warp around, the0232n round the results to values between 0 and 255. And finally, recall that multiplying two 8- bit numbers results in a 16-bit number, so values need to be clipped to 8-bits.

Gaunt, R.

1997-05-01T23:59:59.000Z

386

Small Space Heater Basics | Department of Energy  

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

Small Space Heater Basics Small Space Heater Basics Small Space Heater Basics August 19, 2013 - 10:38am Addthis Small space heaters, also called portable heaters, are typically used when the main heating system is inadequate or when central heating is too costly to install or operate. Space heater capacities generally range between 10,000 Btu to 40,000 Btu per hour. Common fuels used for this purpose are electricity, propane, natural gas, and kerosene. Although most space heaters rely on convection (the circulation of air in a room), some rely on radiant heating; that is, they emit infrared radiation that directly heats up objects and people that are within their line of sight. Combustion Space Heaters Space heaters are classified as vented and unvented, or "vent free." Unvented combustion units are not recommended for inside use, as they

387

Precipitation from Space: Advancing Earth System Science  

Science Conference Proceedings (OSTI)

Advances to space-based observing systems and data processing techniques have made precipitation datasets quickly and easily available via various data portals and widely used in Earth sciences. The increasingly lengthy time span of space-based ...

Paul A. Kucera; Elizabeth E. Ebert; F. Joseph Turk; Vincenzo Levizzani; Dalia Kirschbaum; Francisco J. Tapiador; Alexander Loew; M. Borsche

2013-03-01T23:59:59.000Z

388

Defining digital space through a visual language  

E-Print Network (OSTI)

Current approaches toward digital spaces mainly mimic the physical space that surrounds us. While this approach is valid in a wide range of applications and research, the goal of this thesis is to propose an alternative ...

Kilian, Axel, 1971-

2000-01-01T23:59:59.000Z

389

A WRINKLE IN SPACE Christopher Adam Cross  

E-Print Network (OSTI)

committee. ii #12;Abstract Christopher Adam Cross We explore notions of curvature of regular surfaces be made between distant points in space and time by curving space until the two points touch. I would

390

Cyber-Physical Challenges for Space Systems  

Science Conference Proceedings (OSTI)

Modern space systems necessarily have a tight coupling between onboard cyber (processing, communication) and physical (sensing, actuation) elements to survive the harsh extraterrestrial environment and successfully complete ambitious missions. This article ... Keywords: attitude control, communication, robotics, space systems

Andrew T. Klesh; James W. Cutler; Ella M. Atkins

2012-04-01T23:59:59.000Z

391

Solar space heating | Open Energy Information  

Open Energy Info (EERE)

heating heating Jump to: navigation, search (The following text is derived from the United States Department of Energy's description of solar space heating technology.)[1] Contents 1 Space Heating 2 Passive Solar Space Heating 3 Active Solar Space Heating 4 References Space Heating A solar space-heating system can consist of a passive system, an active system, or a combination of both. Passive systems are typically less costly and less complex than active systems. However, when retrofitting a building, active systems might be the only option for obtaining solar energy. Passive Solar Space Heating Passive solar space heating takes advantage of warmth from the sun through design features, such as large south-facing windows, and materials in the floors or walls that absorb warmth during the day and release that warmth

392

Mapping densities in a noisy state space  

E-Print Network (OSTI)

Weak noise smooths out fractals in a chaotic state space and introduces a maximum attainable resolution to its structure. The balance of noise and deterministic stretching/contraction in each neighborhood introduces local invariants of the dynamics that can be used to partition the state space. We study the local discrete-time evolution of a density in a two-dimensional hyperbolic state space, and use the asymptotic eigenfunctions for the noisy dynamics to formulate a new state space partition algorithm.

Domenico Lippolis

2013-03-05T23:59:59.000Z

393

National Aeronautics and Space Administration Technologies ...  

National Aeronautics and Space Administration Technologies Available for Licensing ... solar system and universe beyond; ... power, energy storage and conversion, ...

394

All Universal Coverings Are Spanier Spaces  

E-Print Network (OSTI)

In this paper, we study necessary and sufficient conditions for existence of categorical universal coverings using open covers of a given space $X$. In fact, we define several homotopy theoretic conditions which we then prove are equivalent to the existence of a categorical universal covering space. As an application, we show that all universal coverings of a connected and locally path connected space are Spanier spaces.

Pakdaman, Ali; Mashayekhy, Behrooz

2011-01-01T23:59:59.000Z

395

Atomic Power in Space: A History  

DOE R&D Accomplishments (OSTI)

"Atomic Power in Space," a history of the Space Isotope Power Program of the United States, covers the period from the program's inception in the mid-1950s through 1982. Written in non-technical language, the history is addressed to both the general public and those more specialized in nuclear and space technologies. Interplanetary space exploration successes and achievements have been made possible by this technology, for which there is no known substitue.

1987-03-00T23:59:59.000Z

396

Exploring indoor white spaces in metropolises  

Science Conference Proceedings (OSTI)

It is a promising vision to utilize white spaces, i.e., vacant VHF and UHF TV channels, to satisfy skyrocketing wireless data demand in both outdoor and indoor scenarios. While most prior works have focused on exploring outdoor white spaces, the indoor ... Keywords: TV white spaces, clustering algorithms, sensor placement

Xuhang Ying, Jincheng Zhang, Lichao Yan, Guanglin Zhang, Minghua Chen, Ranveer Chandra

2013-09-01T23:59:59.000Z

397

Space-Conditioning System Selection Guide  

Science Conference Proceedings (OSTI)

This handbook represents a single-source guide to the selection of space-conditioning equipment for commercial facilities. Written for the utility marketing representative, it provides information on these topics: heating, cooling, ventilation, and dehumidification requirements of commercial buildings; customer needs when selecting a space-conditioning system; and, the options among energy-efficient electric space-conditioning systems for commercial buildings.

1994-01-22T23:59:59.000Z

398

Efficient optimal design space characterization methodologies  

Science Conference Proceedings (OSTI)

One of the primary advantages of a high-level synthesis system is its ability to explore the design space. This paper presents several methodologies for design space exploration that compute all optimal tradeoff points for the combined ... Keywords: bounding, clock-length determination, design space exploration, efficient searching, high-level synthesis, module selection, scheduling

Stephen A. Blythe; Robert A. Walker

2000-07-01T23:59:59.000Z

399

On the design of potential collaboration spaces  

Science Conference Proceedings (OSTI)

In this paper, we introduce the concepts of Potential and Actual Collaboration Spaces. The former applies to the initial space where opportunities for collaboration are identified and an initial interaction is established, while the latter relates to ... Keywords: Doc2U, casual and informal interactions, potential collaboration awareness, potential collaboration spaces

Alberto L. Moran; Jesus Favela; Ana M. Martinez Enriquez; Dominique Decouchant

2004-05-01T23:59:59.000Z

400

Atomic power in space: A history  

Science Conference Proceedings (OSTI)

''Atomic Power in Space,'' a history of the Space Isotope Power Program of the United States, covers the period from the program's inception in the mid-1950s through 1982. Written in non-technical language, the history is addressed to both the general public and those more specialized in nuclear and space technologies. 19 figs., 3 tabs.

Not Available

1987-03-01T23:59:59.000Z

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


401

State-space least mean square  

Science Conference Proceedings (OSTI)

In this paper, we present a generalized form of the well-known least mean square (LMS) filter. The proposed filter incorporates linear time-varying state-space model of the underlying environment and hence is termed as state-space LMS (SSLMS). This attribute ... Keywords: Adaptive filtering, SSLMS, State-space LMS, Tracking

Mohammad Bilal Malik; Muhammad Salman

2008-05-01T23:59:59.000Z

402

COTS-based applications in space avionics  

Science Conference Proceedings (OSTI)

The use of commercial electronic components is increasingly attractive for the space domain. This paper discusses the current degree of use of these components in space avionics, the selection and qualification phases to be successfully completed before ... Keywords: COTS, commercial electronic components, disruptive technology, fault-tolerant architectures, performance limitation, space avionics

Michel Pignol

2010-03-01T23:59:59.000Z

403

Earthwatch: The climate from space  

SciTech Connect

This concise textbook shows how observations from satellites can be used to derive variables important to the monitoring of the climate system. The aim of this book is not to provide a rigorous treatment of climate or of remote sensing and instrumentation, but to attempt to integrate the different disciplines at a level appropriate for undergraduate students of meteorology. The general topics covered are as follows: components of the climate system, basic physical laws (radiations and radiative transfer), current climate issues (greenhouse effect, ozone depletion, Southern Oscillations), remote sensing techniques, and operational principles of sensors aboard space platforms.

Harries, J.E.

1990-01-01T23:59:59.000Z

404

Free-space quantum cryptography  

Science Conference Proceedings (OSTI)

An experimental free-space quantum key distribution (QKD) system has been tested over an outdoor optical path of {approximately}1 km under nighttime conditions at Los Alamos National Laboratory. This system employs the Bennett 92 protocol; here the authors give a brief overview of this protocol, and describe the experimental implementation of it. An analysis of the system efficiency is presented, as well as a description of the error detection protocol, which employs a two-dimensional parity check scheme. Finally, the susceptibility of this system to eavesdropping by various techniques is determined. Possible applications include the rekeying of satellites in low earth orbit.

Hughes, R.J.; Buttler, W.T.; Kwiat, P.G.; Lamoreaux, S.K.; Morgan, G.L.; Nordholt, J.E.; Peterson, C.G.

1998-12-31T23:59:59.000Z

405

QUIESCENT PROMINENCE DYNAMICS OBSERVED WITH THE HINODE SOLAR OPTICAL TELESCOPE. I. TURBULENT UPFLOW PLUMES  

SciTech Connect

Hinode/Solar Optical Telescope (SOT) observations reveal two new dynamic modes in quiescent solar prominences: large-scale (20-50 Mm) 'arches' or 'bubbles' that 'inflate' from below into prominences, and smaller-scale (2-6 Mm) dark turbulent upflows. These novel dynamics are related in that they are always dark in visible-light spectral bands, they rise through the bright prominence emission with approximately constant speeds, and the small-scale upflows are sometimes observed to emanate from the top of the larger bubbles. Here we present detailed kinematic measurements of the small-scale turbulent upflows seen in several prominences in the SOT database. The dark upflows typically initiate vertically from 5 to 10 Mm wide dark cavities between the bottom of the prominence and the top of the chromospheric spicule layer. Small perturbations on the order of 1 Mm or less in size grow on the upper boundaries of cavities to generate plumes up to 4-6 Mm across at their largest widths. All plumes develop highly turbulent profiles, including occasional Kelvin-Helmholtz vortex 'roll-up' of the leading edge. The flows typically rise 10-15 Mm before decelerating to equilibrium. We measure the flowfield characteristics with a manual tracing method and with the Nonlinear Affine Velocity Estimator (NAVE) 'optical flow' code to derive velocity, acceleration, lifetime, and height data for several representative plumes. Maximum initial speeds are in the range of 20-30 km s{sup -1}, which is supersonic for a {approx}10,000 K plasma. The plumes decelerate in the final few Mm of their trajectories resulting in mean ascent speeds of 13-17 km s{sup -1}. Typical lifetimes range from 300 to 1000 s ({approx}5-15 minutes). The area growth rate of the plumes (observed as two-dimensional objects in the plane of the sky) is initially linear and ranges from 20,000 to 30,000 km{sup 2} s{sup -1} reaching maximum projected areas from 2 to 15 Mm{sup 2}. Maximum contrast of the dark flows relative to the bright prominence plasma in SOT images is negative and ranges from -10% for smaller flows to -50% for larger flows. Passive scalar 'cork movies' derived from NAVE measurements show that prominence plasma is entrained by the upflows, helping to counter the ubiquitous downflow streams in the prominence. Plume formation shows no clear temporal periodicity. However, it is common to find 'active cavities' beneath prominences that can spawn many upflows in succession before going dormant. The mean flow recurrence time in these active locations is roughly 300-500 s (5-8 minutes). Locations remain active on timescales of tens of minutes up to several hours. Using a column density ratio measurement and reasonable assumptions on plume and prominence geometries, we estimate that the mass density in the dark cavities is at most 20% of the visible prominence density, implying that a single large plume could supply up to 1% of the mass of a typical quiescent prominence. We hypothesize that the plumes are generated from a Rayleigh-Taylor instability taking place on the boundary between the buoyant cavities and the overlying prominence. Characteristics, such as plume size and frequency, may be modulated by the strength and direction of the cavity magnetic field relative to the prominence magnetic field. We conclude that buoyant plumes are a source of quiescent prominence mass as well as a mechanism by which prominence plasma is advected upward, countering constant gravitational drainage.

Berger, Thomas E.; Slater, Gregory; Hurlburt, Neal; Shine, Richard; Tarbell, Theodore; Title, Alan [Lockheed Martin Solar and Astrophysics Laboratory, B/252, 3251 Hanover Street, Palo Alto, CA 94304 (United States); Lites, Bruce W. [High Altitude Observatory, University Center for Atmospheric Research, Boulder, CO (United States); Okamoto, Takenori J.; Ichimoto, Kiyoshi; Katsukawa, Yukio; Magara, Tetsuya; Suematsu, Yoshinori [National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588 (Japan); Shimizu, Toshifumi, E-mail: berger@lmsal.co [Institute of Space and Astronautical Science/Japan Aerospace Exploration Agency, Sagamihara, Kanagawa 229-8510 (Japan)

2010-06-20T23:59:59.000Z

406

Better bases for kernel spaces  

E-Print Network (OSTI)

In this article we investigate the feasibility of constructing stable, local bases for computing with kernels. In particular, we are interested in constructing families $(b_{\\xi})_{\\xi\\in\\Xi}$ that function as bases for kernel spaces $S(k,\\Xi)$ so that each basis function is constructed using very few kernels. In other words, each function $b_{\\zeta}(x) = \\sum_{\\xi\\in\\Xi} A_{\\zeta,\\xi} k(x,\\xi)$ is a linear combination of samples of the kernel with few nonzero coefficients $A_{\\zeta,\\xi}$. This is reminiscent of the construction of the B-spline basis from the family of truncated power functions. We demonstrate that for a large class of kernels (the Sobolev kernels as well as many kernels of polyharmonic and related type) such bases exist. In fact, the basis elements can be constructed using a combination of roughly $O(\\log N)^d$ kernels, where $d$ is the local dimension of the manifold and $N$ is the dimension of the kernel space (i.e. $N=#\\Xi$). Viewing this as a preprocessing step -- the construction of the...

Fuselier, E J; Narcowich, F J; Ward, J D; Wright, G B

2011-01-01T23:59:59.000Z

407

Solar space heating | Open Energy Information  

Open Energy Info (EERE)

source source History View New Pages Recent Changes All Special Pages Semantic Search/Querying Get Involved Help Apps Datasets Community Login | Sign Up Search Page Edit History Facebook icon Twitter icon » Solar space heating (Redirected from - Solar Ventilation Preheat) Jump to: navigation, search (The following text is derived from the United States Department of Energy's description of solar space heating technology.)[1] Contents 1 Space Heating 2 Passive Solar Space Heating 3 Active Solar Space Heating 4 References Space Heating A solar space-heating system can consist of a passive system, an active system, or a combination of both. Passive systems are typically less costly and less complex than active systems. However, when retrofitting a building, active systems might be the only option for obtaining solar

408

Quantum L_p and Orlicz spaces  

E-Print Network (OSTI)

Let $\\A$ ($\\cM$) be a $C^*$-algebra (a von Neumann algebra respectively). By a quantum dynamical system we shall understand the pair $({\\A}, T)$ ($({\\cM}, T)$) where $T : {\\A} \\to {\\A}$ ($T : {\\cM} \\to {\\cM}$) is a linear, positive (normal respectively), and identity preserving map. In our lecture, we discuss how the techniques of quantum Orlicz spaces may be used to study quantum dynamical systems. To this end, we firstly give a brief exposition of the theory of quantum dynamical systems in quantum $L_p$ spaces. Secondly, we describe the Banach space approach to quantization of classical Orlicz spaces. We will discuss the necessity of the generalization of $L_p$-space techniques. Some emphasis will be put on the construction of non-commutative Orlicz spaces. The question of lifting dynamical systems defined on von Neumann algebra to a dynamical system defined in terms of quantum Orlicz space will be discussed.

L. E. Labuschagne; W. A. Majewski

2009-02-25T23:59:59.000Z

409

Before House Committee on Science, Space, and Technology | Department...  

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

Space, and Technology Before House Committee on Science, Space, and Technology Before House Committee on Science, Space, and Technology By: Peter Lyons Subject: Assessing America's...

410

Before House Committee on Science, Space and Technology | Department...  

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

Space and Technology Before House Committee on Science, Space and Technology Before House Committee on Science, Space and Technology By: Secretary Steven Chu Subject: FY 2013...

411

Before the House Committee on Science, Space and Technology ...  

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

the House Committee on Science, Space and Technology Before the House Committee on Science, Space and Technology Statement Before the Committee on Science, Space and Technology,...

412

Survivable pulse power space radiator  

DOE Patents (OSTI)

A thermal radiator system is described for use on an outer space vehicle, which must survive a long period of nonuse and then radiate large amounts of heat for a limited period of time. The radiator includes groups of radiator panels that are pivotally connected in tandem, so that they can be moved to deployed configuration wherein the panels lie largely coplanar, and to a stowed configuration wherein the panels lie in a stack to resist micrometerorite damage. The panels are mounted on a boom which separates a hot power source from a payload. While the panels are stowed, warm fluid passes through their arteries to keep them warm enough to maintain the coolant in a liquid state and avoid embrittlement of material. The panels can be stored in a largely cylindrical shell, with panels progressively further from the boom being of progressively shorter length. 5 figs.

Mims, J.; Buden, D.; Williams, K.

1988-03-11T23:59:59.000Z

413

Data structure as topological spaces  

E-Print Network (OSTI)

Abstract. In this paper, we propose a topological metaphor for computations: computing consists in moving through a path in a data space and making some elementary computations along this path. This idea underlies an experimental declarative programming language called mgs. mgs introduces the notion of topological collection: a set of values organized by a neighborhood relationship. The basic computation step in mgs relies on the notion of path: a path C is substituted for a path B in a topological collection A. This step is called a transformation and several features are proposed to control the transformation applications. By changing the topological structure of the collection, the underlying computational model is changed. Thus, mgs enables a unified view on several computational mechanisms. Some of them are initially inspired by biological or chemical processes (Gamma and the CHAM, Lindenmayer systems, Paun systems and cellular automata).

Jean-louis Giavitto; Olivier Michel

2002-01-01T23:59:59.000Z

414

Locating TeV Gamma-Ray Sources with Sub-Arcminute Precision: the Pointing Calibration of the HEGRA System of Imaging Atmospheric Cherenkov Telescopes  

E-Print Network (OSTI)

Stereoscopic viewing of TeV gamma-ray air showers with systems of Imaging Atmospheric Cherenkov Telescopes (IACTs) allows to reconstruct the origin of individual primary particles with an accuracy of 0.1 degree or better. The shower impact point can be determined within 15 meters. To actually achieve this resolution, the pointing of the telescopes of an IACT system needs to be controlled with high precision. For the HEGRA IACT system, a procedure to calibrate telescope pointing was established, using bright stars distributed over the sky as references. On the basis of these measurements, one determines parameters of a correction function which is valid for the complete hemisphere. After correction a pointing accuracy of 0.01 degree is achieved.

G. Puehlhofer; A. Daum; G. Hermann; M. Hess; W. Hofmann; C. Koehler; M. Panter

1998-01-12T23:59:59.000Z

415

Space Power Systems | Department of Energy  

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

Reactor Technologies » Space Power Systems Reactor Technologies » Space Power Systems Space Power Systems Through a strong partnership between the Energy Department's office of Nuclear Energy and NASA, Radioisotope Power Systems have been providing the energy for deep space exploration. Through a strong partnership between the Energy Department's office of Nuclear Energy and NASA, Radioisotope Power Systems have been providing the energy for deep space exploration. The Department of Energy (DOE) and its predecessors have provided radioisotope power systems that have safely enabled deep space exploration and national security missions for five decades. Radioisotope power systems (RPSs) convert the heat from the decay of the radioactive isotope plutonium-238 (Pu-238) into electricity. RPSs are capable of producing heat and electricity under the harsh conditions

416

Space reactors - past, present, and future  

SciTech Connect

In the 1990s and beyond, advanced-design nuclear reactors could represent the prime source of both space power and propulsion. Many sophisticated military and civilian space missions of the future will require first kilowatt and then megawatt levels of power. This paper reviews key technology developments that accompanied past US space nuclear power development efforts, describes on-going programs, and then explores reactor technologies that will satisfy megawatt power level needs and beyond.

Buden, D.; Angelo, J.

1983-01-01T23:59:59.000Z

417

Moduli spaces of PU(2)-monopoles  

E-Print Network (OSTI)

The goal of this article was the S^1-equivariant transversality-problem and the compactification-problem for the moduli spaces of (perturbed) PU(2)-monopoles. A substantially improved version entitled "Moduli spaces of PU(2)-monopoles (revised version)" which gives simpler, clearer proofs of the transversality results, has been published on arxiv in June 99 and appeared in Asian J. Math, see Moduli spaces of PU(2)-Monopoles, Asian J. Math. Vol. 4, No. 2 (2000), 391-436.

Andrei Teleman

1997-02-07T23:59:59.000Z

418

Upgrading Below-Grade Spaces: Assessing Priorities  

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

Below-Grade Spaces: Below-Grade Spaces: Assessing Priorities Sam Breidenbach [Cold climate bias] Gap-Balancing risk and homeowner expectations * Managing risk and challenges for contractors - Moisture, mold and liability - Durability/Sustainability - Design/build vs. owner's architect - Contract language to reduce liability - Aligning technical details with specific situations - Below grade spaces are business opportunities - Selling and Competition Gap-Balancing risk and homeowner expectations * Homeowner Expectations and Priorities - Focused on "house beautiful" until technical failure occurs - Health related issues - Opportunity to conserve energy - Cost vs. value-"inexpensive additional space" - Expectations not aligned with physical realities.

419

Models for multimegawatt space power systems  

SciTech Connect

This report describes models for multimegawatt, space power systems which Sandia's Advanced Power Systems Division has constructed to help evaluate space power systems for SDI's Space Power Office. Five system models and models for associated components are presented for both open (power system waste products are exhausted into space) and closed (no waste products) systems: open, burst mode, hydrogen cooled nuclear reactor -- turboalternator system; open, hydrogen-oxygen combustion turboalternator system; closed, nuclear reactor powered Brayton cycle system; closed, liquid metal Rankine cycle system; and closed, in-core, reactor therminonic system. The models estimate performance and mass for the components in each of these systems. 17 refs., 8 figs., 15 tabs.

Edenburn, M.W.

1990-06-01T23:59:59.000Z

420

Section D: SPACE HEATING - Energy Information Administration  

U.S. Energy Information Administration (EIA)

2001 Residential Energy Consumption Survey Form EIA-457A (2001)--Household Questionnaire OMB No.: 1905-0092, Expiring February 29, 2004 19 Section D: SPACE HEATING

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


421

National Aeronautics and Space Administration Technology ...  

National Aeronautics and Space Administration Technology Marketing Summaries. Here you’ll find marketing summaries for technologies available for licensing from the ...

422

Wider benefits of Space Science & Exploration  

E-Print Network (OSTI)

, batteries, fuel cells, supercapacitors (nuclear) · High impact technologies · Miniature systems · Facilities power sources Deep space missions Improved weather forecasting Climate monitoring Vehicle systems

Anand, Mahesh

423

User interfaces in space science instrumentation .  

E-Print Network (OSTI)

??This thesis examines user interaction with instrumentation in the specific context of space science. It gathers together existing practice in machine interfaces with a look… (more)

McCalden, A.J.

2006-01-01T23:59:59.000Z

424

Perspectives in Fundamental Physics in Space  

E-Print Network (OSTI)

We discuss the fundamental principles underlying the current physical theories and the prospects of further improving their knowledge through experiments in space.

Orfeu Bertolami; Clovis Jacinto de Matos; Jean Christophe Grenouilleau; Olivier Minster; Sergio Volonte

2004-05-07T23:59:59.000Z

425

Testbed Environment for Space Situational Awareness (TESSA)  

TESSA is a parallelized discrete event simulation for large-scale modeling and simulation of space events in a high performance computing environment.

426

Moduli spaces of PU(2)-monopoles  

E-Print Network (OSTI)

We study the S^1-equivariant transversality-problem and the compactification-problem for the moduli spaces of (perturbed) PU(2)-monopoles.

Andrei Teleman

1997-02-07T23:59:59.000Z

427

Space-time thermodynamics of the glass transition  

E-Print Network (OSTI)

Space-time Thermodynamics of the Glass Transition Maurobehavior in terms of a thermodynamics of trajectory space.

Merolle, Mauro; Garrahan, Juan P.; Chandler, David

2005-01-01T23:59:59.000Z

428

A CATALOG OF SOLAR X-RAY PLASMA EJECTIONS OBSERVED BY THE SOFT X-RAY TELESCOPE ON BOARD YOHKOH  

Science Conference Proceedings (OSTI)

A catalog of X-ray plasma ejections (XPEs) observed by the Soft X-ray Telescope on board the Yohkoh satellite has been recently developed in the Astronomical Institute of University of Wroclaw. The catalog contains records of 368 events observed in years 1991-2001 including movies and cross-references to associated events like flares and coronal mass ejections (CMEs). One hundred sixty-three XPEs out of 368 in the catalog were not reported until now. A new classification scheme of XPEs is proposed in which morphology, kinematics, and recurrence are considered. The relation between individual subclasses of XPEs and the associated events was investigated. The results confirm that XPEs are strongly inhomogeneous, responding to different processes that occur in the solar corona. A subclass of erupting loop-like XPEs is a promising candidate to be a high-temperature precursor of CMEs.

Tomczak, M.; Chmielewska, E., E-mail: tomczak@astro.uni.wroc.pl, E-mail: chmielewska@astro.uni.wroc.pl [Astronomical Institute, University of Wroclaw, ul. Kopernika 11, PL-51-622 Wroclaw (Poland)

2012-03-01T23:59:59.000Z

429

Active metasomatism in the Cerro Prieto geothermal system, Baja California, Mexico: a telescoped low pressure/temperature metamorphic facies series  

DOE Green Energy (OSTI)

In the Cerro Prieto geothermal field, carbonate-cemented, quartzofeldspathic sediments of the Colorado River delta are being actively metasomatized into calc-silicate metamorphic rocks by reaction with alkali chloride brines between 200/sup 0/ and 370/sup 0/C, low fluid and lithostatic pressures, and low oxygen fugacities. Petrologic investigations of drill cores and cutting from over 50 wells in this field identified a prograde series of calc-silicate mineral zones which include as index minerals: wairakite, epidote, prehnite, and clinopyroxene. Associated divariant mineral assemblages are indicative of a very low pressure/temperature metamorphic facies series which encompasses the clay-carbonate, zeolite, greenschist, and amphibolite facies. This hydrothermal metamorphic facies series, which is becoming increasingly recognized in other active geothermal systems, is characterized by temperature-telescoped dehydration and decarbonation mineral equilibria. Its equivalent should now be sought in fossil hydrothermal systems.

Schiffman, P.; Elders, W.A.; Williams, A.E.; McDowell, S.D.; Bird, D.K.

1983-01-01T23:59:59.000Z

430

Green Bank Telescope observations of the water masers of NGC 3079: accretion disk magnetic field and maser scintillation  

E-Print Network (OSTI)

We present observations of the 22 GHz water megamasers in the circumnuclear disk of NGC 3079 obtained with the Green Bank Telescope. The data are analyzed for circular polarization due to the Zeeman-induced splitting of the water maser lines. No circular polarization is detected and we derive a 1 sigma upper limit of 11 mG for the toroidal magnetic field at ~0.64 pc from the central black hole. This is the tightest upper limit for the magnetic field around a black hole to date. We use the magnetic field limit to derive an estimate of the mass accretion onto the central black hole. In addition to the polarimetric results, we present an observation of rapid variability in the maser lines, which we explain as weak interstellar scintillation. From the scintillation parameters, we estimate an intrinsic size of the mostly saturated maser features of ~12 microarcseconds. This is consistent with models assuming a thick, clumpy accretion disk.

W. H. T. Vlemmings; H. E. Bignall; P. J. Diamond

2006-10-30T23:59:59.000Z

431

The Spectrum of the Isotropic Diffuse Gamma-Ray Emission Derived From First-Year Fermi Large Area Telescope Data  

SciTech Connect

We report on the first Fermi Large Area Telescope (LAT) measurements of the so-called 'extra-galactic' diffuse {gamma}-ray emission (EGB). This component of the diffuse {gamma}-ray emission is generally considered to have an isotropic or nearly isotropic distribution on the sky with diverse contributions discussed in the literature. The derivation of the EGB is based on detailed modelling of the bright foreground diffuse Galactic {gamma}-ray emission (DGE), the detected LAT sources and the solar {gamma}-ray emission. We find the spectrum of the EGB is consistent with a power law with differential spectral index {gamma} = 2.41 {+-} 0.05 and intensity, I(> 100 MeV) = (1.03 {+-} 0.17) x 10{sup -5} cm{sup -2} s{sup -1} sr{sup -1}, where the error is systematics dominated. Our EGB spectrum is featureless, less intense, and softer than that derived from EGRET data.

Abdo, A. A.

2011-08-19T23:59:59.000Z

432

A MEASUREMENT OF THE CORRELATION OF GALAXY SURVEYS WITH CMB LENSING CONVERGENCE MAPS FROM THE SOUTH POLE TELESCOPE  

Science Conference Proceedings (OSTI)

We compare cosmic microwave background lensing convergence maps derived from South Pole Telescope (SPT) data with galaxy survey data from the Blanco Cosmology Survey, WISE, and a new large Spitzer/IRAC field designed to overlap with the SPT survey. Using optical and infrared catalogs covering between 17 and 68 deg{sup 2} of sky, we detect a correlation between the SPT convergence maps and each of the galaxy density maps at >4{sigma}, with zero correlation robustly ruled out in all cases. The amplitude and shape of the cross-power spectra are in good agreement with theoretical expectations and the measured galaxy bias is consistent with previous work. The detections reported here utilize a small fraction of the full 2500 deg{sup 2} SPT survey data and serve as both a proof of principle of the technique and an illustration of the potential of this emerging cosmological probe.

Bleem, L. E.; Becker, M. R.; Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T. [Kavli Institute for Cosmological Physics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637 (United States); Van Engelen, A.; Holder, G. P.; De Haan, T.; Dobbs, M. A. [Department of Physics, McGill University, 3600 Rue University, Montreal, Quebec H3A 2T8 (Canada); Aird, K. A. [University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637 (United States); Armstrong, R. [National Center for Supercomputing Applications, University of Illinois, 1205 West Clark Street, Urbana, IL 61801 (United States); Ashby, M. L. N. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Biesiadzinski, T. [Department of Physics, University of Michigan, 450 Church Street, Ann Arbor, MI 48109 (United States); Brodwin, M. [Department of Physics and Astronomy, University of Missouri, 5110 Rockhill Road, Kansas City, MO 64110 (United States); Busha, M. T. [Institute for Theoretical Physics, University of Zuerich, Zuerich (Switzerland); Cho, H. M. [NIST Quantum Devices Group, 325 Broadway, Mailcode 817.03, Boulder, CO 80305 (United States); Desai, S. [Department of Physics, Ludwig-Maximilians-Universitaet, Scheinerstr. 1, 81679 Muenchen (Germany); Dore, O. [Division of Physics, Mathematics, and Astronomy, California Institute of Technology, MS 249-17, 1216 East California Blvd., Pasadena, CA 91125 (United States); and others

2012-07-01T23:59:59.000Z

433

Chaotic eigenfunctions in phase space  

E-Print Network (OSTI)

We study individual eigenstates of quantized area-preserving maps on the 2-torus which are classically chaotic. In order to analyze their semiclassical behavior, we use the Bargmann-Husimi representations for quantum states, as well as their stellar parametrization, which encodes states through a minimal set of points in phase space (the constellation of zeros of the Husimi density). We rigorously prove that a semiclassical uniform distribution of Husimi densities on the torus entails a similar equidistribution for the corresponding constellations. We deduce from this property a universal behavior for the phase patterns of chaotic Bargmann eigenfunctions, which reminds of the WKB approximation for eigenstates of integrable systems (though in a weaker sense). In order to obtain more precise information on ``chaotic eigenconstellations", we then model their properties by ensembles of random states, generalizing former results on the 2-sphere to the torus geometry. This approach yields statistical predictions for the constellations, which fit quite well the chaotic data. We finally observe that specific dynamical information, e.g. the presence of high peaks (like scars) in Husimi densities, can be recovered from the knowledge of a few long-wavelength Fourier coefficients, which therefore appear as valuable order parameters at the level of individual chaotic eigenfunctions.

S. Nonnenmacher; A. Voros

1997-11-15T23:59:59.000Z

434

Is Interstellar Space Travel Possible?  

E-Print Network (OSTI)

It is shown that space travel, even in the most distant future, will remain confined to our own planetary system, and a similar conclusion will hold forth for any other civilization, no matter how advanced it might be, unless those extra-terrestrial species have life spans order of magnitude longer than ours. Even in such a case it is unlikely that they will travel much farther than their immediate stellar neighbourhood, as each such excursion will exhaust the resources of their home planet so much that those will dwindle rather fast and there might not be much left for the further scientific and technological advancements. So the science-fiction fancy of a "Galactic Empire" may ever remain in our fantasies only. And as for the mythical UFOs, whose quiet appearances do get reported in the press once in a while, recent explorations have shown no evidence that any such thing could have an origination within our own solar system itself. And a "quiet trip" back and forth from a distant star is almost impossible a...

Singal, Tanmay

2013-01-01T23:59:59.000Z

435

A SEARCH FOR RAPIDLY SPINNING PULSARS AND FAST TRANSIENTS IN UNIDENTIFIED RADIO SOURCES WITH THE NRAO 43 METER TELESCOPE  

SciTech Connect

We have searched 75 unidentified radio sources selected from the NRAO VLA Sky Survey catalog for the presence of rapidly spinning pulsars and short, dispersed radio bursts. The sources are radio bright, have no identifications or optical source coincidences, are more than 5% linearly polarized, and are spatially unresolved in the catalog. If these sources are fast-spinning pulsars (e.g., sub-millisecond pulsars), previous large-scale pulsar surveys may have missed detection due to instrumental and computational limitations, eclipsing effects, or diffractive scintillation. The discovery of a sub-millisecond pulsar would significantly constrain the neutron star equation of state and would have implications for models predicting a rapid slowdown of highly recycled X-ray pulsars to millisecond periods from, e.g., accretion disk decoupling. These same sources were previously searched unsuccessfully for pulsations at 610 MHz with the Lovell Telescope at Jodrell Bank. This new search was conducted at a different epoch with a new 800 MHz backend on the NRAO 43 m Telescope at a center frequency of 1200 MHz. Our search was sensitive to sub-millisecond pulsars in highly accelerated binary systems and to short transient pulses. No periodic or transient signals were detected from any of the target sources. We conclude that diffractive scintillation, dispersive smearing, and binary acceleration are unlikely to have prevented detection of the large majority of the sources if they are pulsars, though we cannot rule out eclipsing, nulling or intermittent emission, or radio interference as possible factors for some non-detections. Other (speculative) possibilities for what these sources might include radio-emitting magnetic cataclysmic variables or older pulsars with aligned magnetic and spin axes.

Schmidt, Deborah; Crawford, Fronefield; Gilpin, Claire [Department of Physics and Astronomy, Franklin and Marshall College, P.O. Box 3003, Lancaster, PA 17604 (United States); Langston, Glen [National Radio Astronomy Observatory, P.O. Box 2, Green Bank, WV 24944 (United States)

2013-04-15T23:59:59.000Z

436

Towards a routing framework in ad hoc space networks  

Science Conference Proceedings (OSTI)

A routing framework called Space Gateway Routing (SGR) is proposed for routing through Autonomous Regions (ARs) in ad hoc space networks. SGR has two integral parts: External SGR (ESGR) and Interior SGR (ISGR). ESGR ... Keywords: ad hoc networks, autonomous regions, contact allocation, data delivery, inter-region message scheduling, remote control messages, space communications, space gateway routing, space missions, space networks

Chao Chen; Zesheng Chen

2010-12-01T23:59:59.000Z

437

Reclaiming residual space from elevated transport infrastructure : time, space, and activity under the Chicago Brown Line  

E-Print Network (OSTI)

This thesis studies the non-transport functions of the residual space generated by elevated transport infrastructure and its relationship with abutting neighborhoods The space under the Chicago Brown Line, among all other ...

Su, Jing, S.M. Massachusetts Institute of Technology

2005-01-01T23:59:59.000Z

438

Design principles for the development of space technology maturation laboratories aboard the International Space Station  

E-Print Network (OSTI)

This thesis formulates seven design principles for the development of laboratories which utilize the International Space Station (ISS) to demonstrate the maturation of space technologies. The principles are derived from ...

Saenz Otero, Alvar, 1975-

2005-01-01T23:59:59.000Z

439

Building a time- and space-partitioned architecture for the next generation of space vehicle avionics  

Science Conference Proceedings (OSTI)

Future space systems require innovative computing system architectures, on account of their size, weight, power consumption, cost, safety and maintainability requisites. The AIR (ARINC 653 in Space Real-Time Operating System) architecture answers the ...

José Rufino; João Craveiro; Paulo Verissimo

2010-10-01T23:59:59.000Z

440