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1

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

2

Keck Deep Fields. II. The UV Galaxy Luminosity Function at z~4, 3, and 2  

E-Print Network (OSTI)

We use very deep UGRI multi-field imaging obtained at the Keck telescope to study the evolution of the rest-frame 1700A galaxy luminosity function as the Universe doubles its age from z~4 to z~2. The depth of our imaging allows us to constrain the faint end of the luminosity function reaching M_1700A ~ -18.5 at z~3 (equivalent to ~1M_sun/yr) accounting for both N^1/2 uncertainty in the number of galaxies and for cosmic variance. We carefully examine many potential sources of systematic bias in our LF measurements before drawing the following conclusions. We find that the luminosity function of Lyman Break Galaxies evolves with time and that this evolution is likely differential with luminosity. The result is best constrained between the epochs at z~4 and z~3, where we find that the number density of sub-L* galaxies increases with time by at least a factor of 2.3 (11sigma statistical confidence); while the faint end of the LF evolves, the bright end appears to remain virtually unchanged, indicating that there may be differential, luminosity-dependent evolution significant at the 97% level. Potential systematic biases restric our ability to draw strong conclusions about continued evolution of the luminosity function to lower redshifts, z~2.2 and z~1.7, but, nevertheless, it appears certain that the number density of z~2.2 galaxies at all luminosities we studied, -22

Marcin Sawicki; David Thompson

2005-07-21T23:59:59.000Z

3

Keck II spectroscopy of mHz quasi-periodic oscillations in Hercules X-1  

E-Print Network (OSTI)

We present Keck II spectroscopy of an optical mHz quasi-periodic oscillations (QPOs) in the lightcurve of the X-ray pulsar binary Her X-1. In the power spectrum it appears as `peaked noise', with a coherency $\\sim$2, a central frequency of 35 mHz and a peak-to-peak amplitude of 5%. However, the dynamic power spectrum shows it to be an intermittent QPO, with a lifetime of $\\sim$hundred seconds, as expected if the lifetime of the orbiting material is equal to the thermal timescale of the inner disk. We have decomposed the spectral time series into constant and variable components and used blackbody fits to the resulting spectra to characterise the spectrum of the QPO variability and constrain possible production sites. We find that the spectrum of the QPO is best-fit by a small hot region, possibly the inner regions of the accretion disk, where the ballistic accretion stream impacts onto the disk. The lack of any excess power around the QPO frequency in the X-ray power spectrum, created using simultaneous lightcurves from XTE, implies that the QPO is not simply reprocessed X-ray variability.

K O'Brien; Keith Horne; B Boroson; M Still; R Gomer; JB Oke; P Boyd; S Vrtilek

2001-05-10T23:59:59.000Z

4

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

5

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

6

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

7

Dispersion in Neptune's Zonal Wind Velocities from NIR Keck AO Observations in July 2009  

E-Print Network (OSTI)

We report observations of Neptune made in H-(1.4-1.8 {\\mu}m) and K'-(2.0-2.4 {\\mu}m) bands on 14 and 16 July 2009 from the 10-m W.M. Keck II Telescope using the near-infrared camera NIRC2 coupled to the Adaptive Optics (AO) system. We track the positions of 54 bright atmospheric features over a few hours to derive their zonal and latitudinal velocities, and perform radiative transfer modeling to measure the cloud-top pressures of 50 features seen simultaneously in both bands. We observe one South Polar Feature (SPF) on 14 July and three SPFs on 16 July at ~65 deg S. The SPFs observed on both nights are different features, consistent with the high variability of Neptune's storms. There is significant dispersion in Neptune's zonal wind velocities about the smooth Voyager wind profile fit of Sromovsky et al., Icarus 105, 140 (1993), much greater than the upper limit we expect from vertical wind shear, with the largest dispersion seen at equatorial and southern mid-latitudes. Comparison of feature pressures vs. r...

Fitzpatrick, Patrick J; Luszcz-Cook, Statia; Wong, Michael H; Hammel, Heidi B

2013-01-01T23:59:59.000Z

8

Keck-Nirspec Infrared OH Lines: Oxygen Abundances in Metal-Poor Stars Down to [Fe/H] = -2.9  

E-Print Network (OSTI)

Infrared OH lines at 1.5 - 1.7 um in the H band were obtained with the NIRSPEC high-resolution spectrograph at the 10m Keck Telescope for a sample of seven metal-poor stars. Detailed analyses have been carried out, based on optical high-resolution data obtained with the FEROS spectrograph at ESO. Stellar parameters were derived by adopting infrared flux method effective temperatures, trigonometric and/or evolutionary gravities and metallicities from FeII lines. We obtain that the sample stars with metallicities [Fe/H] < -2.2 show a mean oxygen abundance [O/Fe] ~ 0.54, for a solar oxygen abundance of epsilon(O) = 8.87, or [O/Fe] ~ 0.64 if epsilon(O) = 8.77 is assumed.

Jorge Melendez; Beatriz Barbuy

2002-07-31T23:59:59.000Z

9

A KECK/LRIS SPATIALLY RESOLVED SPECTROSCOPIC STUDY OF A LINER GALAXY SDSS J091628.05+420818.7  

Science Conference Proceedings (OSTI)

Using spatially resolved spectra obtained with the Low Resolution Imaging Spectrometer at the Keck I telescope, we investigate the nature of ionizing sources and kinematic properties of emission-line gas in a LINER galaxy SDSS J091628.05+420818.7, which is a nearby (z = 0.0241) and bright (M{sub r} = -20.2) early-type galaxy. After subtracting stellar absorption features using a combination of simple stellar population models, we measure the flux, line-of-sight velocity, and velocity dispersion of four emission lines, i.e., H{alpha}, H{beta}, [O III] {lambda}5007, and [N II] {lambda}6584, to study radial change of emission-line fluxes and velocities. Compared to the point-spread function of the observation, the emission-line region is slightly extended but comparable to the seeing size. The central concentration of emission-line gas suggests that ionization is triggered by a nuclear source, excluding old stellar population as ionizing sources. We find that emission-line gas is counter-rotating with respect to stellar component and that the [O III] {lambda}5007 line is blueshifted compared to other emission lines, possibly due to an outflow.

Bae, Hyun-Jin; Yoon, Suk-Jin [Department of Astronomy and Center for Galaxy Evolution Research, Yonsei University, Seoul 120-749 (Korea, Republic of); Woo, Jong-Hak [Astronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul 151-742 (Korea, Republic of); Yagi, Masafumi [Optical and Infrared Astronomy Division, National Astronomical Observatory of Japan, Tokyo 181-8588 (Japan); Yoshida, Michitoshi, E-mail: woo@astro.snu.ac.kr [Hiroshima Astrophysical Science Center, Hiroshima University, Hiroshima 739-8526 (Japan)

2012-07-01T23:59:59.000Z

10

Keck Pencil-Beam Survey for Faint Kuiper Belt Objects  

E-Print Network (OSTI)

We present the results of a pencil-beam survey of the Kuiper Belt using the Keck 10-m telescope. A single 0.01 square degree field is imaged 29 times for a total integration time of 4.8 hr. Combining exposures in software allows the detection of Kuiper Belt Objects (KBOs) having visual magnitude V < 27.9. Two new KBOs are discovered. One object having V = 25.5 lies at a probable heliocentric distance d = 33 AU. The second object at V = 27.2 is located at d = 44 AU. Both KBOs have diameters of about 50 km, assuming comet-like albedos of 4%. Data from all surveys are pooled to construct the luminosity function from red magnitude R = 20 to 27. The cumulative number of objects per square degree, N (< R), is fitted to a power law of the form log_(10) N = 0.52 (R - 23.5). Differences between power laws reported in the literature are due mainly to which survey data are incorporated, and not to the method of fitting. The luminosity function is consistent with a power-law size distribution for objects having dia...

Chiang, E I

1999-01-01T23:59:59.000Z

11

Bounds on Dark Matter Properties from Radio Observations of Ursa Major II using the Green Bank Telescope  

E-Print Network (OSTI)

Radio observations of the Ursa Major II dwarf spheroidal galaxy obtained using the Green Bank Telescope are used to place bounds on WIMP dark matter properties. Dark matter annihilation releases energy in the form of charged particles which emit synchrotron radiation in the magnetic field of the dwarf galaxy. We compute the expected synchrotron radiation intensity from WIMP annihilation to various primary channels. The predicted synchrotron radiation is sensitive to the distribution of dark matter in the halo, the diffusion coefficient D_0, the magnetic field strength B, the particle mass m_\\chi, the annihilation rate , and the annihilation channel. Limits on , m_\\chi, B, and D_0 are obtained for the e^+ e^-, \\mu^+ \\mu^-, \\tau^+ \\tau^-, and b \\bar b channels. Constraints on these parameters are sensitive to uncertainties in the measurement of the dark matter density profile. For the best fit halo parameters derived from stellar kinematics, we exclude 10 GeV WIMPs annihilating directly to e^+ e^- at the thermal rate = 2.18 x 10^{-26} cm^3/s at the 2\\sigma level, for B > 0.6 microGauss (1.6 microGauss) and D_0 = 0.1 (1.0) x the Milky Way diffusion value.

Aravind Natarajan; Jeffrey B. Peterson; Tabitha C. Voytek; Kristine Spekkens; Brian Mason; James Aguirre; Beth Willman

2013-08-22T23:59:59.000Z

12

The endless mantra : innovation at the Keck Observatory  

E-Print Network (OSTI)

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

Bobra, Monica Godha

2005-01-01T23:59:59.000Z

13

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

14

Performance of the Keck Observatory adaptive optics system  

SciTech Connect

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

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

2004-01-19T23:59:59.000Z

15

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

16

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

17

THE GREEN BANK TELESCOPE 350 MHz DRIFT-SCAN SURVEY II: DATA ANALYSIS AND THE TIMING OF 10 NEW PULSARS, INCLUDING A RELATIVISTIC BINARY  

SciTech Connect

We have completed a 350 MHz Drift-scan Survey using the Robert C. Byrd Green Bank Telescope with the goal of finding new radio pulsars, especially millisecond pulsars that can be timed to high precision. This survey covered {approx}10,300 deg{sup 2} and all of the data have now been fully processed. We have discovered a total of 31 new pulsars, 7 of which are recycled pulsars. A companion paper by Boyles et al. describes the survey strategy, sky coverage, and instrumental setup, and presents timing solutions for the first 13 pulsars. Here we describe the data analysis pipeline, survey sensitivity, and follow-up observations of new pulsars, and present timing solutions for 10 other pulsars. We highlight several sources-two interesting nulling pulsars, an isolated millisecond pulsar with a measurement of proper motion, and a partially recycled pulsar, PSR J0348+0432, which has a white dwarf companion in a relativistic orbit. PSR J0348+0432 will enable unprecedented tests of theories of gravity.

Lynch, Ryan S.; Kaspi, Victoria M.; Archibald, Anne M.; Karako-Argaman, Chen [Department of Physics, McGill University, 3600 University Street, Montreal, QC H3A 2T8 (Canada)] [Department of Physics, McGill University, 3600 University Street, Montreal, QC H3A 2T8 (Canada); Boyles, Jason; Lorimer, Duncan R.; McLaughlin, Maura A.; Cardoso, Rogerio F. [Department of Physics, West Virginia University, 111 White Hall, Morgantown, WV 26506 (United States)] [Department of Physics, West Virginia University, 111 White Hall, Morgantown, WV 26506 (United States); Ransom, Scott M. [National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903 (United States)] [National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903 (United States); Stairs, Ingrid H.; Berndsen, Aaron; Cherry, Angus; McPhee, Christie A. [Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1 (Canada)] [Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1 (Canada); Hessels, Jason W. T.; Kondratiev, Vladislav I.; Van Leeuwen, Joeri [ASTRON, The Netherlands Institute for Radio Astronomy, Postbus 2, 7990-AA Dwingeloo (Netherlands)] [ASTRON, The Netherlands Institute for Radio Astronomy, Postbus 2, 7990-AA Dwingeloo (Netherlands); Epstein, Courtney R. [Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210 (United States)] [Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210 (United States); Pennucci, Tim [Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904 (United States)] [Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904 (United States); Roberts, Mallory S. E. [Eureka Scientific Inc., 2452 Delmer Street, Suite 100, Oakland, CA 94602 (United States)] [Eureka Scientific Inc., 2452 Delmer Street, Suite 100, Oakland, CA 94602 (United States); Stovall, Kevin, E-mail: rlynch@physics.mcgill.ca [Center for Advanced Radio Astronomy and Department of Physics and Astronomy, University of Texas at Brownsville, Brownsville, TX 78520 (United States)] [Center for Advanced Radio Astronomy and Department of Physics and Astronomy, University of Texas at Brownsville, Brownsville, TX 78520 (United States)

2013-02-15T23:59:59.000Z

18

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

19

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

20

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

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21

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

E-Print Network (OSTI)

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

J. T. Wright

2005-05-11T23:59:59.000Z

22

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

23

Keck Deep Fields. I. Observations, Reductions, and the Selection of Faint Star-Forming Galaxies at Redshifts z~4, 3, and 2  

E-Print Network (OSTI)

We introduce a very deep, R_lim~27, multicolor imaging survey of very faint star-forming galaxies at z~4, z~3, z~2.2, and z~1.7. This survey, carried out on the Keck I telescope, uses the very same UGRI filter system that is employed by the Steidel team to select galaxies at these redshifts, and thus allows us to construct identically-selected, but much fainter, samples. However, our survey reaches ~1.5 mag deeper than the work of Steidel and his group, letting us probe substantially below the characteristic luminosity L* and thus study the properties and redshift evolution of the faint component of the high-z galaxy population. The survey covers 169 square arcminutes in three spatially independent patches on the sky and -- to R<~27 -- contains 427 GRI-selected z~4 LBGs, 1481 UGR-selected z~3 LBGs, 2417 UGR-selected z~2.2 star-forming galaxies, and 2043 UGR-selected z~1.7 star-forming galaxies. In this paper, the first in a series, we introduce the survey, describe our observing and data reduction strategies, and outline the selection of our z~4, z~3, z~2.2, and z~1.7 samples.

Marcin Sawicki; David Thompson

2005-07-19T23:59:59.000Z

24

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

25

II  

Office of Legacy Management (LM)

II II c )3 c F r c L LI L rr c - r I P- c OAK RlDGE NATIONAL LABORATORY h U W -l\ &?ir;; ITi' m . 8 ORNL/RASA-92/l Results of the Radiological Survey at the Former Chapman Valve Manufacturing Company, Indian Orchard, Massachusetts (cIooo1) R. D. Foley M . S. Uziel MANAGED BY MARTIN MARIETTA ENERGY SYSTEMS, INC. FOR THE UNITED STATES DEPARTMENT OF ENERGY ORNLJRASA-92/l /- HEALTH AND SAFETY RESEARCH DIVISION Environmental Restoration and Waste Management Non-Defense Programs (Activity No. EX 20 20 01 0; ADS317OOOO) Results of the Radiological Survey at the Former Chapman Valve Manufacturing Company, Indian Orchard, Massachusetts (cIooo1) R. D. Foley and M. S. Uziel Date Issued - July 1992 Investigation learn R. E. Swaja - Measurement Applications and Development Manager

26

Solar voltaic research P. D. (Dan) Dapkus is the W. M. Keck Professor of Engineering in the Ming Hsieh Department  

E-Print Network (OSTI)

Solar voltaic research P. D. (Dan) Dapkus is the W. M. Keck Professor of Engineering in the Ming and at Rockwell International where he was a group leader and manger in charge of electronic materials, solar cell (MOCVD) technology and the demonstration of the first devices by that process, including the first solar

Levi, Anthony F. J.

27

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

28

II  

Office of Legacy Management (LM)

: " + ; . .Z + II . ? 8 . " ~. . . . a a' .; ,. ?> , . ' . : . ., ! , Environmental i r .,' : % , ~ ~ 9 . / ; i.3. -\ ,- I - 'I ' , 2 " .r: 1; . . , ~ . ,&- c . . a , ,, .,I;< . .' , , ? $ ; 1- !'I' . '...~ - .. :, , .I Closure Report for CAU No. 416 1: ' . Project Shoal Area I:' c!';,: .. 7. .. , . ~ 1 I' ,. Controlled Copy No. UNCONTROLLED { -* .. 4'. . 1 " . .. *. *" '.. . . , , ,I +' , ,.f.' I , I" I ', ', ctk;' . , I , '. :C, , I: : , . p . ? .,; . s . " . , k - ,

29

PROPER MOTIONS OF THE ARCHES CLUSTER WITH KECK LASER GUIDE STAR ADAPTIVE OPTICS: THE FIRST KINEMATIC MASS MEASUREMENT OF THE ARCHES  

SciTech Connect

We report the first detection of the intrinsic velocity dispersion of the Arches cluster-a young ({approx}2 Myr), massive (10{sup 4} M{sub Sun }) starburst cluster located only 26 pc in projection from the Galactic center. This was accomplished using proper motion measurements within the central 10'' Multiplication-Sign 10'' of the cluster, obtained with the laser guide star adaptive optics system at Keck Observatory over a three-year time baseline (2006-2009). This uniform data set results in proper motion measurements that are improved by a factor {approx}5 over previous measurements from heterogeneous instruments. By careful, simultaneous accounting of the cluster and field contaminant distributions as well as the possible sources of measurement uncertainties, we estimate the internal velocity dispersion to be 0.15 {+-} 0.01 mas yr{sup -1}, which corresponds to 5.4 {+-} 0.4 km s{sup -1} at a distance of 8.4 kpc. Projecting a simple model for the cluster onto the sky to compare with our proper motion data set, in conjunction with surface density data, we estimate the total present-day mass of the cluster to be M(r < 1.0 pc) = 1.5{sup +0.74}{sub -0.60} Multiplication-Sign 10{sup 4} M{sub Sun }. The mass in stars observed within a cylinder of radius R (for comparison to photometric estimates) is found to be M(R < 0.4 pc) = 0.90{sup +0.40}{sub -0.35} Multiplication-Sign 10{sup 4} M{sub Sun} at formal 3{sigma} confidence. This mass measurement is free from assumptions about the mass function of the cluster, and thus may be used to check mass estimates from photometry and simulation. Photometric mass estimates assuming an initially Salpeter mass function ({Gamma}{sub 0} = 1.35, or {Gamma} {approx} 1.0 at present, where dN/d(log M){proportional_to}M{sup {Gamma}}) suggest a total cluster mass M{sub cl} {approx} (4-6) Multiplication-Sign 10{sup 4} M{sub Sun} and projected mass ({approx} 2 {<=} M(R < 0.4 pc) {<=} 3) Multiplication-Sign 10{sup 4} M{sub Sun }. Photometric mass estimates assuming a globally top-heavy or strongly truncated present-day mass function (PDMF; with {Gamma} {approx} 0.6) yield mass estimates closer to M(R < 0.4 pc) {approx} 1-1.2 Multiplication-Sign 10{sup 4} M{sub Sun }. Consequently, our results support a PDMF that is either top-heavy or truncated at low mass, or both. Collateral benefits of our data and analysis include: (1) cluster membership probabilities, which may be used to extract a clean-cluster sample for future photometric work; (2) a refined estimate of the bulk motion of the Arches cluster with respect to the field, which we find to be 172 {+-} 15 km s{sup -1}, which is slightly slower than suggested by previous measurements using one epoch each with the Very Large Telescope and the Keck telescope; and (3) a velocity dispersion estimate for the field itself, which is likely dominated by the inner Galactic bulge and the nuclear disk.

Clarkson, W. I. [Division of Astronomy and Astrophysics, University of California, Los Angeles, Physics and Astronomy Building, 430 Portola Plaza, Box 951547, Los Angeles, CA 90095-1547 (United States); Ghez, A. M.; Morris, M. R.; Yelda, S. [Department of Astronomy, Indiana University, Bloomington, 727 East 3rd Street, Swain West 319, Bloomington, IN 47405-7105 (United States); Lu, J. R. [Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822-1839 (United States); Stolte, A. [Argelander Institut fuer Astronomie, Universitaet Bonn, Auf dem Huegel 71, 53121 Bonn (Germany); McCrady, N. [Department of Physics and Astronomy, University of Montana, 32 Campus Drive, No. 1080, Missoula, MT 59812 (United States); Do, T., E-mail: wiclarks@indiana.edu [Department of Physics and Astronomy, University of California, Irvine, 4129 Frederick Reines Hall, Irvine, CA 92697-4575 (United States)

2012-06-01T23:59:59.000Z

30

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...

31

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

32

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

33

Characterization of the gaseous companion {\\kappa} Andromedae b: New Keck and LBTI high-contrast observations  

E-Print Network (OSTI)

We previously reported the direct detection of a low mass companion at a projected separation of 55+-2 AU around the B9 type star {\\kappa} Andromedae. The properties of the system (mass ratio, separation) make it a benchmark for the understanding of the formation and evolution of gas giant planets and brown dwarfs on wide-orbits. We present new angular differential imaging (ADI) images of the Kappa Andromedae system at 2.146 (Ks), 3.776 (L'), 4.052 (NB 4.05) and 4.78 {\\mu}m (M') obtained with Keck/NIRC2 and LBTI/LMIRCam, as well as more accurate near-infrared photometry of the star with the MIMIR instrument. We derive a more accurate J = 15.86 +- 0.21, H = 14.95 +- 0.13, Ks = 14.32 +- 0.09 mag for {\\kappa} And b. We redetect the companion in all our high contrast observations. We confirm previous contrasts obtained at Ks and L' band. We derive NB 4.05 = 13.0 +- 0.2 and M' = 13.3 +- 0.3 mag and estimate Log10(L/Lsun) = -3.76 +- 0.06. We build the 1-5 microns spectral energy distribution of the companion and co...

Bonnefoy, M; Marleau, G -D; Schlieder, J E; Wisniewski, J; Carson, J; Covey, K R; Henning, T; Biller, B; Hinz, P; Klahr, H; Boyer, A N Marsh; Zimmerman, N; Janson, M; McElwain, M; Mordasini, C; Skemer, A; Bailey, V; Defrre, D; Thalmann, C; Skrutskie, M; Allard, F; Homeier, D; Tamura, M; Feldt, M; Cumming, A; Grady, C; Brandner, W; Kandori, R; Kuzuhara, M; Fukagawa, M; Kwon, J; Kudo, T; Hashimoto, J; Kusakabe, N; Abe, L; Brandt, T; Egner, S; Guyon, O; Hayano, Y; Hayashi, M; Hayashi, S; Hodapp, K; Ishii, M; Iye, M; Knapp, G; Matsuo, T; Mede, K; Miyama, M; Morino, J -I; Moro-Martin, A; Nishimura, T; Pyo, T; Serabyn, E; Suenaga, T; Suto, H; Suzuki, R; Takahashi,; Takami, M; Takato, N; Terada, H; Tomono, D; Turner, E; Watanabe, M; Yamada, T; Takami, H; Usuda, T

2013-01-01T23:59:59.000Z

34

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

35

PLANETS AROUND LOW-MASS STARS (PALMS). II. A LOW-MASS COMPANION TO THE YOUNG M DWARF GJ 3629 SEPARATED BY 0.''2  

SciTech Connect

We present the discovery of a 0.''2 companion to the young M dwarf GJ 3629 as part of our high-contrast adaptive optics imaging search for giant planets around low-mass stars with the Keck-II and Subaru telescopes. Two epochs of imaging confirm that the pair is comoving and reveal signs of orbital motion. The primary exhibits saturated X-ray emission which, together with its UV photometry from GALEX, points to an age younger than {approx}300 Myr. At these ages the companion lies below the hydrogen burning limit with a model-dependent mass of 46 {+-} 16 M{sub Jup} based on the system's photometric distance of 22 {+-} 3 pc. Resolved YJHK photometry of the pair indicates a spectral type of M7 {+-} 2 for GJ 3629 B. With a projected separation of 4.4 {+-} 0.6 AU and an estimated orbital period of 21 {+-} 5 yr, GJ 3629 AB is likely to yield a dynamical mass in the next several years, making it one of only a handful of brown dwarfs to have a measured mass and an age constrained from the stellar primary.

Bowler, Brendan P.; Liu, Michael C. [Institute for Astronomy, University of Hawai'i, 2680 Woodlawn Drive, Honolulu, HI 96822 (United States); Shkolnik, Evgenya L. [Lowell Observatory, 1400 W. Mars Hill Road, Flagstaff, AZ 86001 (United States); Tamura, Motohide, E-mail: bpbowler@ifa.hawaii.edu [National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 (Japan)

2012-09-01T23:59:59.000Z

36

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...

37

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. Grf; 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. Lck; E. Majorana; I. Mandel; V. Mandic; M. Mantovani; I. Martin; C. Michel; Y. Minenkov; N. Morgado; S. Mosca; B. Mours; H. Mller-Ebhardt; P. Murray; R. Nawrodt; J. Nelson; R. Oshaughnessy; C. D. Ott; C. Palomba; A. Paoli; G. Parguez; A. Pasqualetti; R. Passaquieti; D. Passuello; L. Pinard; W. Plastino; R. 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. Rdiger; 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. Thring; J. van den Brand; M van Veggel; C. Van Den Broeck; A. Vecchio; J. Veitch; F. Vetrano; A. Vicere; S. Vyatchanin; B. Willke; G. Woan; K. Yamamoto

2011-08-05T23:59:59.000Z

38

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

39

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

40

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

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41

Are AGN Broad Emission Lines Formed by Discrete Clouds? --- Analysis of Keck High Resolution Spectroscopy of NGC 4151  

E-Print Network (OSTI)

We search for a direct signature of discrete ''clouds'' in the broad line region (BLR) of the Seyfert galaxy NGC 4151. For this purpose we apply cross correlation (CC) analysis to a high resolution KECK spectrum of the galaxy. No such signature is found in the data. In order for cloud models to be compatible with this result, there must be at least $\\sim3\\times10^7$ emitting clouds in the BLR, where the limit is based on simulation of a homogeneous cloud population. More realistic distributions increase the lower limit to above $10^8$. These numbers are an order of magnitude improvement on our previous limit from Mrk 335, where the improvement comes from higher S/N, broader lines, and refined simulations. Combined with the predicted upper limit for the number of emitting clouds in NGC 4151 ($10^6-10^7$), the derived lower limit puts a strong constraint on the cloud scenario in the BLR of this object. Similar constraints can be paled on models where the emission originates in streams and sheets. Thus, this investigation suggests that the BELs in NGC 4151, and by extension in all AGNs, are not made of an ensemble of discrete independent emitters.

Nahum Arav; Thomas A. Barlow; Ari Laor; Wallace L. W. Sargent; Roger D. Blandford

1998-01-04T23:59:59.000Z

42

NIST Telescope Calibration May Help Explain Mystery of ...  

Science Conference Proceedings (OSTI)

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

2011-01-05T23:59:59.000Z

43

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

44

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

45

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

46

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.

Frster, A; Baba, H; Bhr, 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; Phlhofer, 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, ?; Wrnlein, A; Yoshida, T

2013-01-01T23:59:59.000Z

47

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

48

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

49

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

50

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

51

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

52

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

53

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

54

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

55

Stellar Archaeology a Keck Pilot Program on Extremely Metal-Poor Stars from the Hamburg\\/ESO Survey. II. Abundance Analysis  

E-Print Network (OSTI)

We present a detailed abundance analysis of 8 stars selected as extremely metal poor candidates from the Hamburg/ESO Survey (HES). For comparison, we have also analysed 3 extremely metal-poor candidates from the HK survey, and 3 additional bright metal-poor stars. With this work, we have doubled the number of extremely metal-poor stars ([Fe/H]$\\le 3.0$) with high-precision abundance analyses. Our sample of extremely metal-poor candidates from the HES contains 3 stars with [Fe/H] $\\le -3.0$, 3 more with [Fe/H]$\\le -2.8$, and 2 stars that are only slightly more metal rich. Thus, the chain of procedures that led to the selection of these stars from the HES successfully provides a high fraction of extremely metal-poor stars. We verify that our stellar parameters, derived in Paper I, lead to acceptable ionization and excitation balances for Fe, ruling out substantial non-LTE effects in Fe. For the $\\alpha-$elements Mg, Si, Ca, Ti, the light element Al, the iron-peak elements Sc, Cr, Mn, and the neutron capture ele...

Carretta, E; Cohen, J G; Beers, T C; Christlieb, N; Carretta, Eugenio; Gratton, Raffaele; Cohen, Judith G.; Beers, Timothy C.; Christlieb, Norbert

2002-01-01T23:59:59.000Z

56

Stellar Archaeology: a Keck Pilot Program on Extremely Metal-Poor Stars from the Hamburg/ESO Survey. II. Abundance Analysis  

E-Print Network (OSTI)

We present a detailed abundance analysis of 8 stars selected as extremely metal poor candidates from the Hamburg/ESO Survey (HES). For comparison, we have also analysed 3 extremely metal-poor candidates from the HK survey, and 3 additional bright metal-poor stars. With this work, we have doubled the number of extremely metal-poor stars ([Fe/H]$\\le 3.0$) with high-precision abundance analyses. Our sample of extremely metal-poor candidates from the HES contains 3 stars with [Fe/H] $\\le -3.0$, 3 more with [Fe/H]$\\le -2.8$, and 2 stars that are only slightly more metal rich. Thus, the chain of procedures that led to the selection of these stars from the HES successfully provides a high fraction of extremely metal-poor stars. We verify that our stellar parameters, derived in Paper I, lead to acceptable ionization and excitation balances for Fe, ruling out substantial non-LTE effects in Fe. For the $\\alpha-$elements Mg, Si, Ca, Ti, the light element Al, the iron-peak elements Sc, Cr, Mn, and the neutron capture elements Sr and Ba, we find trends in abundance ratios [X/Fe] similar to those found by previous studies. However,the scatter in most of these ratios, even at [Fe/H]$\\le -3.0$ dex, is surprisingly small. Only Sr and Ba show scatter larger than the expected errors. Future work (the 0Z project) will provide much stronger constraints on the scatter (or lack thereof) in abundances for a greater number of stars. We discuss the implications of these results for the early chemical evolution of the Galaxy, including such issues as the number of contributing SN, and the sizes of typical fragments in which they were born. In addition, we have identified a very metal poor star that appears to be the result of the s-process chain, operating in a very metal-poor environment, with extremely enhanced C, Ba, and Pb, and somewhat enhanced Sr.

Eugenio Carretta; Raffaele Gratton; Judith G. Cohen; Timothy C. Beers; Norbert Christlieb

2002-04-04T23:59:59.000Z

57

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

58

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

E-Print Network (OSTI)

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

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

2013-07-18T23:59:59.000Z

59

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

60

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

Note: This page contains sample records for the topic "keck ii 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

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

62

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

63

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

64

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

65

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

66

Keck Deep Fields. III. Luminosity-dependent Evolution of the Ultraviolet Luminosity and Star Formation Rate Densities at z~4, 3, and 2  

E-Print Network (OSTI)

We use the Keck Deep Fields UGRI catalog of z~4, 3, and 2 UV-selected galaxies to study the evolution of the rest-frame 1700A luminosity density at high redshift. The ability to reliably constrain the contribution of faint galaxies is critical and our data do so as they reach to M*+2 even at z~4 and deeper still at lower redshifts. We find that the luminosity density at high redshift is dominated by the hitherto poorly studied galaxies fainter than L*, and, indeed, the the bulk of the UV light in the high-z Universe comes from galaxies in the luminosity range L=0.1-1L*. It is these faint galaxies that govern the behavior of the total UV luminosity density. Overall, there is a gradual rise in luminosity density starting at z~4 or earlier, followed by a shallow peak or a plateau within z~3--1, and then followed by the well-know plunge at lower redshifts. Within this total picture, luminosity density in sub-L* galaxies evolves more rapidly at high redshift, z>~2, than that in more luminous objects. However, this is reversed at lower redshifts, z~2 and this dominance further highlights the need for follow-up studies that will teach us more about these very numerous but thus far largely unexplored systems.

Marcin Sawicki; David Thompson

2006-05-17T23:59:59.000Z

67

Keck Laser Guide Star Adaptive Optics Monitoring of 2MASS J1534-2952AB: First Dynamical Mass Determination of a Binary T Dwarf  

E-Print Network (OSTI)

(Abridged) We present multi-epoch imaging of the T5.0+T5.5 binary 2MASS J1534-2952AB obtained with the Keck laser guide star adaptive optics system. Combined with an extensive (re-)analysis of archival HST imaging, we find a total mass of 0.056+/-0.003 Msun (59+/-3 Mjup). This is the first field binary for which both components are directly confirmed to be substellar. This is also the coolest and lowest mass binary with a dynamical mass determination to date. Using evolutionary models, we derive an age of 0.78+/-0.09 Gyr for the system, and we find Teff = 1028+/-17 K and 978+/-17 K and masses of 0.0287+/-0.0016 Msun (30.1+/-1.7 Mjup) and 0.0269+/-0.0016 Msun (28.2+/-1.7 Mjup) for the individual components. These precise measurements generally agree with previous studies of T dwarfs and affirm the current theoretical models. However, (1) the temperatures are about 100 K cooler than derived for similar objects and suggest that the ages of field brown dwarfs may be overestimated. Also, (2) the H-R diagram positi...

Liu, Michael C; Ireland, Michael J

2008-01-01T23:59:59.000Z

68

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

69

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

70

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

71

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

72

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; Gonzlez, 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

73

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

74

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

75

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

76

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

77

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

78

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

79

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

80

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.

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


81

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

82

PARS II  

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

too rapidly to see): a. Loading -PARS II is loading the report definition and data query. b. Downloading (generating report) c. Opening Excel d. Formatting report Report...

83

IIS5  

Science Conference Proceedings (OSTI)

... 1) enabled/disabled, (1) Internet Information Services (IIS) Manager GUI: Right Click on Server > Properties > Home Directory tab > Read, Chapter 2 ...

2013-02-22T23:59:59.000Z

84

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

85

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

E-Print Network (OSTI)

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

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

2008-01-01T23:59:59.000Z

86

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

87

STELLAR KINEMATICS OF THE ANDROMEDA II DWARF SPHEROIDAL GALAXY  

Science Conference Proceedings (OSTI)

We present kinematical profiles and metallicity for the M31 dwarf spheroidal (dSph) satellite galaxy Andromeda II (And II) based on Keck DEIMOS spectroscopy of 531 red giant branch stars. Our kinematical sample is among the largest for any M31 satellite and extends out to two effective radii (r {sub eff} = 5.'3 = 1.1 kpc). We find a mean systemic velocity of -192.4 {+-} 0.5 km s{sup -1} and an average velocity dispersion of {sigma} {sub v} = 7.8 {+-} 1.1 km s{sup -1}. While the rotation velocity along the major axis of And II is nearly zero (<1 km s{sup -1}), the rotation along the minor axis is significant with a maximum rotational velocity of v {sub max} = 8.6 {+-} 1.8 km s{sup -1}. We find a kinematical major axis, with a maximum rotational velocity of v {sub max} = 10.9 {+-} 2.4 km s{sup -1}, misaligned by 67 Degree-Sign to the isophotal major axis. And II is thus the first dwarf galaxy with evidence for nearly prolate rotation with a v {sub max}/{sigma} {sub v} = 1.1, although given its ellipticity of {epsilon} = 0.10, this object may be triaxial. We measured metallicities for a subsample of our data, finding a mean metallicity of [Fe/H] = -1.39 {+-} 0.03 dex and an internal metallicity dispersion of 0.72 {+-} 0.03 dex. We find a radial metallicity gradient with metal-rich stars more centrally concentrated, but do not observe a significant difference in the dynamics of the two metallicity populations. And II is the only known dwarf galaxy to show minor axis rotation, making it a unique system whose existence offers important clues on the processes responsible for the formation of dSphs.

Ho, Nhung; Geha, M.; Tollerud, E. [Astronomy Department, Yale University, New Haven, CT 06520 (United States); Munoz, R. R. [Departamento de Astronomia, Universidad de Chile, Casilla 36-D, Santiago (Chile); Guhathakurta, P. [UCO/Lick Observatory, University of California, Santa Cruz, 1156 High Street, Santa Cruz, CA 95064 (United States); Kalirai, J. [Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States); Gilbert, K. M. [Department of Astronomy, University of Washington, Seattle, WA 98195 (United States); Bullock, J. [Center for Cosmology, Department of Physics and Astronomy, University of California, Irvine, CA 92697 (United States); Beaton, R. L.; Majewski, S. R., E-mail: ngocnhung.ho@yale.edu, E-mail: marla.geha@yale.edu [Department of Astronomy, University of Virginia, P.O. Box 3818, Charlottesville, VA 22903 (United States)

2012-10-20T23:59:59.000Z

88

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

89

ISLSCP II Project Page  

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

ISLSCP II The International Satellite Land Surface Climatology Project, Initiative II (ISLSCP II) Overview ISLSCP II Logo The International Satellite Land Surface Climatology...

90

Design of light concentrators for Cherenkov telescope observatories  

E-Print Network (OSTI)

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

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

2013-01-01T23:59:59.000Z

91

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

92

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

93

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

94

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. Kufl; G. Finger; A. Glasse; R. Stuik

2007-08-23T23:59:59.000Z

95

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

96

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

97

PARS II  

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

Peck 1.1 5102010 Exercise 6 -Monthly Status screen updated to PARS II 4152010 Version 30-31 Replaced screens and changed text. J. Peck 1.1 5102010 Ex 8 and 9 36-38...

98

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

99

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

100

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

Note: This page contains sample records for the topic "keck ii 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.


101

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

102

Geek-Up[12.10.2010]: A New Planet in Another Solar System, Fast-Tracked  

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

12.10.2010]: A New Planet in Another Solar System, 12.10.2010]: A New Planet in Another Solar System, Fast-Tracked Drug Treatments and Better Batteries Geek-Up[12.10.2010]: A New Planet in Another Solar System, Fast-Tracked Drug Treatments and Better Batteries December 10, 2010 - 3:46pm Addthis Schematic representation of the HR8799 system compared to our own solar system. | Photo Courtesy of NRC-HIA, Christian Marois and the W.M Keck Observatory Schematic representation of the HR8799 system compared to our own solar system. | Photo Courtesy of NRC-HIA, Christian Marois and the W.M Keck Observatory Niketa Kumar Niketa Kumar Public Affairs Specialist, Office of Public Affairs Using high-contrast, near infrared adaptive optics on the Keck II telescope in Hawaii, LLNL astronomers have identified a fourth planet that is part of

103

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.

104

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. Brger; T. E. Hansen; N. Lietaer

2011-04-07T23:59:59.000Z

105

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

106

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

107

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

108

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

109

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. Span; 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

110

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

111

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. Oconnell; Joel D. Offenberg; Ronald A. Parise; Joel Wm. Parker; Morton S. Roberts; M. Smith; William H. Waller

1997-01-01T23:59:59.000Z

112

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

113

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

114

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

115

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

116

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

117

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

118

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

119

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

120

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

Note: This page contains sample records for the topic "keck ii telescope" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
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We encourage you to perform a real-time search of NLEBeta
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121

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

122

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

123

Ii1  

Office of Legacy Management (LM)

-r -r Ii1 5uitc 79% 955 L%fan~Plu,S.W.. Worhingm. D.C.200242134, 7117-03.87.cdy.43 23 September 1987 Mr. Andrew Wallo, III, NE-23 Division of Facility & Site Decommissioning Projects U.S. Department of Energy Germantown, Maryland 20545 Dear Mr. Wallo: ELIMINATION RECOMMENDATION -- COLLEGES AND UNIVtRSITIES The attached elimination recommendation was prepared in accordance.)l- flL.o* with your suggestion during our meeting on 22 September, The recommendat:on y0.0-02 includes 26 colleges and universities identified.in Enclosure 4 to Aerospace letter subject: Status of Actions - FUSRAP Site List, dated i 27 May 1987; three institutions (Tufts College, University of Virginia, ! and the University of Washington) currently identified on the FUSRAP

124

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

125

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

126

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

127

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

128

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

129

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

130

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

131

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

132

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

133

Artificial Photosynthesis II -  

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

II - Artificial Photosynthesis II - Joint Center for Artificial Photosynthesis (JCAP) Simulations NathanLewis.png Schematic of a photoelectrochemical cell being designed to harness...

134

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

135

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

136

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

137

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

138

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

139

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

140

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

Note: This page contains sample records for the topic "keck ii 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

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

142

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

143

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

144

PARS II TRAINING  

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

10 (V1.1) PARS II 102 Monthly Updating and Reporting i 10 (V1.1) PARS II 102 Monthly Updating and Reporting i Project Assessment and Reporting System PARS II 102 Monthly Updating and Reporting Training Workbook (PARS II Release 1.1) Department of Energy September 13, 2010 September 13,, 2010 (V1.1) PARS II 102 Monthly Updating and Reporting ii Table of Contents OVERSIGHT and ASSESSMENT ........................................................................................................ 1 Exercise 1: Find and View a Project ............................................................................................ 1 Sort the Project List ................................................................................................................. 3

145

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

146

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

147

CHROMOSPHERIC SIGNATURES OF SMALL-SCALE FLUX EMERGENCE AS OBSERVED WITH NEW SOLAR TELESCOPE AND HINODE INSTRUMENTS  

SciTech Connect

With the ever-increasing influx of high-resolution images of the solar surface obtained at a multitude of wavelengths, various processes occurring at small spatial scales have become a greater focus of our attention. Complex small-scale magnetic fields have been reported that appear to have enough stored energy to heat the chromosphere. While significant progress has been made in understanding small-scale phenomena, many specifics remain elusive. We present here a detailed study of a single event of disappearance of a magnetic dipole and associated chromospheric activity. Based on New Solar Telescope H{alpha} data and Hinode photospheric line-of-sight magnetograms and Ca II H images, we report the following. (1) Our analysis indicates that even very small dipoles (elements separated by about 0.''5 or less) may reach the chromosphere and trigger non-negligible chromospheric activity. (2) Careful consideration of the magnetic environment where the new flux is deposited may shed light on the details of magnetic flux removal from the solar surface. We argue that the apparent collision and disappearance of two opposite polarity elements may not necessarily indicate their cancellation (i.e., reconnection, emergence of a 'U' tube, or submergence of {Omega} loops). In our case, the magnetic dipole disappeared by reconnecting with overlying large-scale inclined plage fields. (3) Bright points (BPs) seen in off-band H{alpha} images are very well correlated with the Ca II H BPs, which in turn are cospatial with G-band BPs. We further speculate that, in general, H{alpha} BPs are expected to be cospatial with photospheric BPs; however, a direct comparison is needed to refine their relationship.

Yurchyshyn, V. B.; Goode, P. R.; Abramenko, V. I.; Chae, J.; Cao, W.; Andic, A.; Ahn, K. [Big Bear Solar Observatory, New Jersey Institute of Technology, Big Bear City, CA 92314 (United States)

2010-10-20T23:59:59.000Z

148

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

149

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,

150

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

151

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

152

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

153

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

154

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

155

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

156

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

157

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

158

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

159

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

160

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

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161

I IIII1IiI II1Ii  

Office of Legacy Management (LM)

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162

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

163

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

164

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.

165

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.

166

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

167

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

168

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

169

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

170

PARS II TRAINING  

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

1 Viewing and Reporting 1 Viewing and Reporting Training Workbook V1.0 Department of Energy May 10, 2010 May 10, 2010 PARS II 101 Viewing and Reporting V1.0 ii May 10, 2010 PARS II 101 Viewing and Reporting V1.0 iii Table of Contents OVERSIGHT and ASSESSMENT ........................................................................................................ 1 Exercise 1 Find and View a Project ............................................................................................. 1 Sort the Project List ................................................................................................................. 3 Select a Project ....................................................................................................................... 3

171

NIST STARR II  

Science Conference Proceedings (OSTI)

... on board, a calibrated reference reflector, called a solar diffuser, is ... efficiently coupled to a monochromator, the tunable source power in STARR II ...

2012-11-14T23:59:59.000Z

172

PARS II FAQ  

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

V1.4.1 (June 25, 2011) 1 V1.4.1 (June 25, 2011) 1 PARS II Project Assessment and Reporting System Frequently Asked Questions (Click on a Question to go to Its Answer) General PARS II Project Information Q: What is the motivation, purpose and expected benefit from the PARS II system? Q: Where can I go to find out information on PARS II? Accessing and Using PARS II Q: Where can I go to access PARS II? Q: How do I obtain a PARS II User ID and Password? Q: PARS II will not allow me to log-in, it just keeps displaying the login window for User ID and Password. What should I do? Q: Upon log-in, I do not see a list of my projects. What should I do? Q: I am a FPD tracking a project and it does not appear on my project list. What should I do? Q: Upon log-in, I receive a white screen. What should I do?

173

Portable Automated Mesonet II  

Science Conference Proceedings (OSTI)

The Portable Automated Mesonet II (PAM II) system was developed by NCAR to provide surface mesoscale data for the research needs of the atmospheric science community. The PAM system has 60 remote stations with planned growth to 300. In such a ...

Fred V. Brock; George H. Saum; Steven R. Semmer

1986-12-01T23:59:59.000Z

174

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

175

PARS II Extraction Utility | Department of Energy  

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

Extraction Utility PARS II Extraction Utility PARS II Extraction Utility v8020130510.zip More Documents & Publications PARS II Extraction Utility Release Notes PARS II CPP...

176

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

177

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

178

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

179

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

180

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

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181

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 Lpez-Oramas; Abelardo Moralejo; Daniel Mazin; Daniela Hadasch for the MAGIC Collaboration

2013-10-06T23:59:59.000Z

182

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

183

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

184

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

185

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

186

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

187

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

188

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

189

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

190

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

191

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

192

NSLS-II Project Pages  

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

NSLS-II Project Pages Project Management Team Project Schedule Integrated Project Team (IPT) Monthly Status Meetings Advisory Committees Project Reviews Documents NSLS-II...

193

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

194

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.

195

PARS II User Guide  

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

This document serves as a reference manual to assist DOE end-users in performing their respective functions within the PARS II web application. The document provides a description and How To for...

196

NSLS II: Authentication Required  

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

Project Pages Login Access to this area of the NSLS-II website requires a valid username and password. Username: Password: Next > Last Modified: April 2, 2013 Please forward all...

197

Recovering the Line-Of-Sight Magnetic Field in the Chromosphere from Ca II IR Spectra  

E-Print Network (OSTI)

We propose a method to derive the line-of-sight magnetic flux density from measurements in the chromospheric Ca II IR line at 854.2 nm. The method combines two well-understood techniques, the center-of-gravity and bisector methods, in a single hybrid technique. The technique is tested with magneto-static simulations of a flux tube. We apply the method to observations with the Interferometric Bidimensional Spectrometer (IBIS) installed at the Dunn Solar Telescope of the NSO/SP to investigate the morphology of the lower chromosphere, with focus on the chromospheric counterparts to the underlying photospheric magnetic flux elements.

Wger, F; Uitenbroek, H; Rimmele, T

2009-01-01T23:59:59.000Z

198

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. Khler; T. Kutter; W. Hofmann

1995-08-07T23:59:59.000Z

199

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

200

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 "keck ii telescope" from the National Library of EnergyBeta (NLEBeta).
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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

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

202

Guidelines Volume II  

Gasoline and Diesel Fuel Update (EIA)

II II Sector-Specific Issues and Reporting Methodologies Supporting the General Guidelines for the Voluntary Reporting of Greenhouse Gases under Section 1605(b) of the Energy Policy Act of 1992 Part 4: Transportation Sector Part 5: Forestry Sector Part 6: Agricultural Sector Transportation Sector-Page 4.iii Contents of Volume II This volume, the second of two such volumes, contains sector-specific guidance in support of the General Guidelines for the voluntary reporting of greenhouse gas emissions and carbon sequestration. This voluntary reporting program was authorized by Congress in Section 1605(b) of the Energy Policy Act of 1992. The General Guidelines, bound separately from this volume, provide the overall rationale for the program, discuss in general how to analyze emissions and emission reduction/carbon sequestration projects, and

203

PARS II | Department of Energy  

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

Operational Management » Information Systems » PARS II Operational Management » Information Systems » PARS II PARS II Welcome to PARS II PARS II is the Department's official "System of Record" for capital asset project performance information. Because PARS II uses the same data as maintained in our contractors' project management systems, everyone from the Federal Project Director's staff to the Secretary of Energy will have easy access to the same data. The PARS II software application is managed by the MA Office of Engineering and Construction Management and is used by federal and contractor personnel across the nation to record and track the progress of major construction and environmental cleanup projects. Questions or comments about PARS II should be directed to the PARS II Help Desk via email at i-Manage.eas@hq.doe.gov or by calling 301-903-2500

204

VERY LARGE TELESCOPE/X-SHOOTER SPECTROSCOPY OF THE CANDIDATE BLACK HOLE X-RAY BINARY MAXI J1659-152 IN OUTBURST  

SciTech Connect

We present the optical to near-infrared spectrum of MAXI J1659-152 during the onset of its 2010 X-ray outburst. The spectrum was obtained with X-shooter on the ESO Very Large Telescope early in the outburst simultaneous with high-quality observations at both shorter and longer wavelengths. At the time of the observations, the source was in the low-hard state. The X-shooter spectrum includes many broad ({approx}2000 km s{sup -1}), double-peaked emission profiles of H, He I, and He II, characteristic signatures of a low-mass X-ray binary during outburst. We detect no spectral signatures of the low-mass companion star. The strength of the diffuse interstellar bands results in a lower limit to the total interstellar extinction of A{sub V} {approx_equal} 0.4 mag. Using the neutral hydrogen column density obtained from the X-ray spectrum we estimate A{sub V} {approx_equal} 1 mag. The radial velocity structure of the interstellar Na I D and Ca II H and K lines results in a lower limit to the distance of {approx}4 {+-} 1 kpc, consistent with previous estimates. With this distance and A{sub V} , the dereddened spectral energy distribution represents a flat disk spectrum. The two 10 minute X-shooter spectra show significant variability in the red wing of the emission-line profiles, indicating a global change in the density structure of the disk, though on a timescale much shorter than the typical viscous timescale of the disk.

Kaur, Ramanpreet; Kaper, Lex; Ellerbroek, Lucas E.; Russell, David M.; Altamirano, Diego; Wijnands, Rudy; Yang Yijung; Van der Horst, Alexander; Van der Klis, Michiel [Astronomical Institute 'Anton Pannekoek', University of Amsterdam, Science Park 904, 1098 XH Amsterdam (Netherlands); D'Avanzo, Paolo [INAF, Osservatorio Astronomico di Brera, via E. Bianchi 46, 23807 Merate (Italy); De Ugarte Postigo, Antonio; Fynbo, Johan P. U. [Dark Cosmology Centre, Niels Bohr Institute, Juliane Maries Vej 30, Copenhagen 2100 (Denmark); Flores, Hector [GEPI, Paris Observatory, CNRS, University of Paris-Diderot, 5 Place Jules Janssen, 92195 Meudon (France); Goldoni, Paolo [Laboratoire Astroparticule et Cosmologie, 10 rue A. Domon et L. Duquet, 75205 Paris Cedex 13 (France); Thoene, Christina C. [IAA-CSIC, Glorieta de la Astronomia s/n, 18008 Granada (Spain); Kouveliotou, Chryssa [Space Science Office, VP62, NASA/Marshall Space Flight Center, Huntsville, AL 35812 (United States); Wiersema, Klaas [Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH (United Kingdom); Kuulkers, Erik, E-mail: r.kaur@uva.nl [European Space Agency, European Space Astronomy Centre, P.O. Box 78, 28691 Villanueva de la Canada, Madrid (Spain)

2012-02-20T23:59:59.000Z

205

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

206

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

207

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

208

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

209

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

210

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

211

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

212

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

213

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

214

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

215

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

216

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; Krzesnski, 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

217

Synchrophasor Technologies Page ii  

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

August 2013 August 2013 Synchrophasor Technologies Page ii Table of Contents 1. Introduction ................................................................................................................... 1 2. Synchrophasor Technologies .......................................................................................... 1 3. Advanced Applications Software and their Benefits ........................................................ 4 3.1 Online (Near Real-Time Applications) ........................................................................... 5 3.2 Offline (Not real-time) Applications ............................................................................. 8 4. Recovery Act Synchrophasor Projects ............................................................................. 8

218

PARS II Training Schedule  

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

2 4 5 6 7 8 WEEK 3 11 12 13 14 15 WEEK 4 18 19 20 21 22 WEEK 5 25 26 27 28 PARS II Training Schedule FEBRUARY 2013 Webinar PARS 102: Session A) 10:00 - 12:00 1 Hour Break...

219

PHOTOMETRIC SUPERNOVA COSMOLOGY WITH BEAMS AND SDSS-II  

SciTech Connect

Supernova (SN) cosmology without spectroscopic confirmation is an exciting new frontier, which we address here with the Bayesian Estimation Applied to Multiple Species (BEAMS) algorithm and the full three years of data from the Sloan Digital Sky Survey II Supernova Survey (SDSS-II SN). BEAMS is a Bayesian framework for using data from multiple species in statistical inference when one has the probability that each data point belongs to a given species, corresponding in this context to different types of SNe with their probabilities derived from their multi-band light curves. We run the BEAMS algorithm on both Gaussian and more realistic SNANA simulations with of order 10{sup 4} SNe, testing the algorithm against various pitfalls one might expect in the new and somewhat uncharted territory of photometric SN cosmology. We compare the performance of BEAMS to that of both mock spectroscopic surveys and photometric samples that have been cut using typical selection criteria. The latter typically either are biased due to contamination or have significantly larger contours in the cosmological parameters due to small data sets. We then apply BEAMS to the 792 SDSS-II photometric SNe with host spectroscopic redshifts. In this case, BEAMS reduces the area of the {Omega}{sub m}, {Omega}{sub {Lambda}} contours by a factor of three relative to the case where only spectroscopically confirmed data are used (297 SNe). In the case of flatness, the constraints obtained on the matter density applying BEAMS to the photometric SDSS-II data are {Omega}{sup BEAMS}{sub m} = 0.194 {+-} 0.07. This illustrates the potential power of BEAMS for future large photometric SN surveys such as Large Synoptic Survey Telescope.

Hlozek, Renee [Oxford Astrophysics, Department of Physics, University of Oxford, Keble Road, Oxford, OX1 3RH (United Kingdom); Kunz, Martin [Department de physique theorique, Universite de Geneve, 30, quai Ernest-Ansermet, CH-1211 Geneve 4 (Switzerland); Bassett, Bruce; Smith, Mat; Newling, James [African Institute for Mathematical Sciences, 68 Melrose Road, Muizenberg 7945 (South Africa); Varughese, Melvin [Department of Mathematics and Applied Mathematics, University of Cape Town, Rondebosch, Cape Town, 7700 (South Africa); Kessler, Rick; Frieman, Joshua [The Kavli Institute for Cosmological Physics, The University of Chicago, 933 East 56th Street, Chicago, IL 60637 (United States); Bernstein, Joseph P.; Kuhlmann, Steve; Marriner, John [Argonne National Laboratory, 9700 South Cass Avenue, Argonne, IL 60439 (United States); Campbell, Heather; Lampeitl, Hubert; Nichol, Robert C. [Institute of Cosmology and Gravitation, Dennis Sciama Building Burnaby Road Portsmouth PO1 3FX (United Kingdom); Dilday, Ben [Las Cumbres Observatory Global Telescope Network, 6740 Cortona Drive, Suite 102, Goleta, CA 93117 (United States); Falck, Bridget; Riess, Adam G. [Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218 (United States); Sako, Masao [Department of Physics and Astronomy, University of Pennsylvania, 203 South 33rd Street, Philadelphia, PA 19104 (United States); Schneider, Donald P., E-mail: rhlozek@astro.princeton.edu [Department of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802 (United States)

2012-06-20T23:59:59.000Z

220

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

Note: This page contains sample records for the topic "keck ii 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

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

222

Giant Protease TPP II's Structure, Mechanism Uncovered  

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

Giant Protease TPP II's Structure, Mechanism Uncovered Print Tripeptidyl peptidase II (TPP II), the largest known eukaryotic enzyme that breaks down proteins (a protease), is...

223

Giant Protease TPP II's Structure, Mechanism Uncovered  

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

Giant Protease TPP II's Structure, Mechanism Uncovered Giant Protease TPP II's Structure, Mechanism Uncovered Print Wednesday, 23 February 2011 00:00 Tripeptidyl peptidase II (TPP...

224

PARS II Software Release Notes  

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

New and improved functionality was released in Version 8.0.20120308 of PARS II. This release offers PARS II Users a significant number of enhancements across all facets of the application. These...

225

Cloud Computing Forum & Workshop II  

Science Conference Proceedings (OSTI)

Cloud Computing Forum & Workshop II. Purpose: On May 20, 2010, NIST hosted the first Cloud Computing Forum & Workshop. ...

2013-08-07T23:59:59.000Z

226

Part II Energy Storage Technologies  

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

II. Energy Storage Technology Overview * Instructor - Haresh Kamath, EPRI PEAC * Short term - Flywheels, Cranking Batteries, Electrochemical Capacitors, SMES * Long term -...

227

RAMAN SCATTERED He II {lambda}4332 IN THE SYMBIOTIC STAR V1016 CYGNI  

SciTech Connect

Raman scattering of He II line photons with atomic hydrogen is important in studying the mass loss processes in many symbiotic stars and a number of young planetary nebulae. We calculate the scattering cross sections and branching ratios associated with the Raman scattered He II {lambda}4332 feature formed through inelastic scattering of He II {lambda}949 with a hydrogen atom. At the line center of He II {lambda}949, the total scattering cross section is computed to be {sigma}{sub tot} = 2.5 Multiplication-Sign 10{sup -22} cm{sup 2}, and the branching ratio into the level 2s is 0.12. We also present a high-resolution spectrum of the symbiotic star V1016 Cygni obtained with the 1.8 m telescope at Mt. Bohyun to investigate the Raman scattering origin of the broad feature blueward of He II {lambda}4338. Based on the atomic calculation, we perform Monte Carlo calculations for the line formation. The scattering region is assumed to be a part of a uniform spherical shell that subtends a solid angle {Delta}{Omega} = {pi} steradian with a neutral column density N{sub HI} = 1.0 x 10{sup 21} cm{sup -2}. By adding a far-UV continuum around He II {lambda}949 normalized by the equivalent width of He II {lambda}949 to be 2.3 Angstrom-Sign , we obtain a good fit for both the Raman scattered He II {lambda}4332 and the broad wings around H{gamma}. Our analysis of the Raman feature blueward of H{gamma} in V1016 Cyg is consistent with the previous study of the Raman features blueward of H{alpha} and H{beta} by Jung and Lee.

Lee, Hee-Won [Department of Astronomy and Space Science, Sejong University, Seoul 143-747 (Korea, Republic of)

2012-05-10T23:59:59.000Z

228

RHIC II Science Workshop  

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

Working Groups and Convenors Working Groups and Convenors The purpose of these Working Groups is to provide an organized way for the community to refine the science agenda for the RHIC II upgrades, and make a compelling case for these upgrades to the broad nuclear physics community. A document summarizing the Working Group results, with a sharp focus on the science case for RHIC II, will be produced early in 2006. Electromagnetic Probes Convenors: Ralf Rapp, Zhangbu Xu, Gabor David Email list info Website Heavy Flavor Convenors: Ramona Vogt, Thomas Ullrich, Tony Frawley Email list info Website High pT Convenors: Denes Molnar, Saskia Mioduszewski, Kirill Filimonov Internal working group web page Email list info Equation of State Convenors: Steffen Bass, Julia Velkovska, Helen Caines Email list info

229

NSLS II: Life Sciences  

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

Biological and Medical Imaging Biological and Medical Imaging Overview The high brightness of NSLS-II will make it possible to tightly focus the beam to create very intense nanoprobes for high-resolution cellular imaging and sensitive trace element mapping in biological specimens. The brightness will also provide highly collimated beams of high intensity and large transverse dimensions for novel forms of medical imaging and tomography. NSLS-II will also provide the broadest range of wavelengths to users in a single facility, extending from hard X-rays to the far-infrared and enabling a wide array of analytical techniques, including: X-ray microscopy (hard and soft; scanning and full-field), diffraction imaging, X-ray tomography, X-ray microprobe, diffraction-enhanced imaging (DEI), and infrared imaging. These diverse imaging tools will span the resolution scale from nanometers to millimeters, allowing non-destructive analysis of biological subjects ranging from sub-cellular structures to humans.

230

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

231

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

232

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

233

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

234

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

235

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

236

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

237

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

238

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

239

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

240

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

Note: This page contains sample records for the topic "keck ii 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

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

242

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

243

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

244

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. Hl; 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. Schck; 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

245

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

246

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$^{2}$)

Mandt, Duan; Ebr, Jan; Hrabovsk, Miroslav; Prouza, Michael; Bulik, Tomasz; Allekotte, Ingomar

2013-01-01T23:59:59.000Z

247

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

248

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

249

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

250

_Part II - Contract Clauses  

National Nuclear Security Administration (NNSA)

M515 dated 9/9/13 M515 dated 9/9/13 Contract DE-AC04-94AL85000 Modification No. M202 Part II - Contract Clauses Section I TABLE OF CONTENTS 1. FAR 52.202-1 DEFINITIONS (JAN 2012) (REPLACED M473) ............................................................... 8 2. FAR 52.203-3 GRATUITIES (APR 1984)..................................................................................................... 8 3. FAR 52.203-5 COVENANT AGAINST CONTINGENT FEES (APR 1984) ............................................. 9 4. FAR 52.203-6 RESTRICTIONS ON SUBCONTRACTOR SALES TO THE GOVERNMENT (SEP 2006) (REPLACED M264) ............................................................................................................................ 10 5. FAR 52.203-7 ANTI-KICKBACK PROCEDURES (OCT 2010) (REPLACED M443) ......................... 10

251

A 205 {mu}m [N II] MAP OF THE CARINA NEBULA  

Science Conference Proceedings (OSTI)

We present the results of a {approx}250 arcmin{sup 2} mapping of the 205 {mu}m [N II] fine-structure emission over the northern Carina Nebula, including the Car I and Car II H II regions. Spectra were obtained using the South Pole Imaging Fabry-Perot Interferometer (SPIFI) at the Antarctic Submillimeter Telescope and Remote Observatory (AST/RO) at the South Pole. We supplement the 205 {mu}m data with new reductions of far-IR fine-structure spectra from the Infrared Space Observatory (ISO) Long Wavelength Spectrometer (LWS) in 63 {mu}m [O I], 122 {mu}m [N II], 146 {mu}m [O I], and 158 {mu}m [C II]; the 146 {mu}m [O I] data include 90 raster positions which have not been previously published. Morphological comparisons are made with optical, radio continuum, and CO maps. The 122/205 line ratio is used to probe the density of the low-ionization gas, and the 158/205 line ratio is used to probe the fraction of C{sup +} arising from photodissociation regions (PDRs). The [O I] and [C II] lines are used to construct a PDR model of Carina. When the PDR properties are compared with other sources, Carina is found to be more akin to 30 Doradus than galactic star-forming regions such as Orion, M17, or W49; this is consistent with the view of Carina as a more evolved region, where much of the parent molecular cloud has been ionized or swept away. These data constitute the first ground-based detection of the 205 {mu}m [N II] line, and the third detection overall since those of COBE FIRAS and the Kuiper Airborne Observatory in the early 1990s.

Oberst, T. E.; Parshley, S. C.; Nikola, T.; Stacey, G. J. [Department of Astronomy, Cornell University, Ithaca, NY 14853 (United States); Loehr, A.; Lane, A. P.; Stark, A. A. [Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138 (United States); Kamenetzky, J., E-mail: oberstte@westminster.edu [Center for Astrophysics and Space Astronomy, University of Colorado, Boulder, CO 80303 (United States)

2011-10-01T23:59:59.000Z

252

PADD IV PADD II lakes PADD V - PADD II - inland  

U.S. Energy Information Administration (EIA)

228 U.S. Energy Information Administration Annual Energy Outlook 2013 Regional maps Source Maritime Canada Caribbean PADD V - other PADD II lakes PADD V -

253

PNE WIND USA II  

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

PNE WIND USA II PNE WIND USA II 1 PNE Wind USA Tribal Energy Partnerships Cherokee & Chilocco Wind Parks Buchholz wind farm, Germany André De Rosa Managing Director Andre.DeRosa@PNEWind.com p. (312) 919-8042 Hot Springs NP M is s i s s i ppi M iss is s i pp i Mis si ss ip p i M ississippi M iss iss ippi M i ss i ss i pp i M is s issippi Missis sip pi M i s s is s ip p i Bonny State Park Bonny State Park Buffalo River State Park Buffalo River State Park Caprock Caprock Canyons Canyons State Park State Park Robbers Cave State Park Robbers Cave State Park Clinton State Park Clinton State Park Hillsdale State Park Hillsdale State Park Indian Cave State Park Indian Cave State Park Lake Murray State Park Lake Murray State Park Lake of Lake of the Ozarks the Ozarks St Park St Park Little River State Park Little River State Park Palo Duro

254

MULTI-ELEMENT ABUNDANCE MEASUREMENTS FROM MEDIUM-RESOLUTION SPECTRA. II. CATALOG OF STARS IN MILKY WAY DWARF SATELLITE GALAXIES  

Science Conference Proceedings (OSTI)

We present a catalog of Fe, Mg, Si, Ca, and Ti abundances for 2961 stars in eight dwarf satellite galaxies of the Milky Way (MW): Sculptor, Fornax, Leo I, Sextans, Leo II, Canes Venatici I, Ursa Minor, and Draco. For the purposes of validating our measurements, we also observed 445 red giants in MW globular clusters and 21 field red giants in the MW halo. The measurements are based on Keck/DEIMOS medium-resolution spectroscopy (MRS) combined with spectral synthesis. We estimate uncertainties in [Fe/H] by quantifying the dispersion of [Fe/H] measurements in a sample of stars in monometallic globular clusters (GCs). We estimate uncertainties in Mg, Si, Ca, and Ti abundances by comparing to high-resolution spectroscopic abundances of the same stars. For this purpose, a sample of 132 stars with published high-resolution spectroscopy in GCs, the MW halo field, and dwarf galaxies has been observed with MRS. The standard deviations of the differences in [Fe/H] and ([{alpha}/Fe]) (the average of [Mg/Fe], [Si/Fe], [Ca/Fe], and [Ti/Fe]) between the two samples is 0.15 and 0.16, respectively. This catalog represents the largest sample of multi-element abundances in dwarf galaxies to date. The next papers in this series draw conclusions on the chemical evolution, gas dynamics, and star formation histories from the catalog presented here. The wide range of dwarf galaxy luminosity reveals the dependence of dwarf galaxy chemical evolution on galaxy stellar mass.

Kirby, Evan N.; Cohen, Judith G. [California Institute of Technology, Department of Astronomy, Mail Stop 249-17, Pasadena, CA 91106 (United States); Guhathakurta, Puragra; Rockosi, Constance M. [University of California Observatories/Lick Observatory, Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064 (United States); Simon, Joshua D. [Observatories of the Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, CA 91101 (United States); Geha, Marla C. [Astronomy Department, Yale University, New Haven, CT 06520 (United States); Sneden, Christopher [McDonald Observatory, University of Texas, Austin, TX 78712 (United States); Sohn, Sangmo Tony [Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States); Majewski, Steven R. [Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904-4325 (United States); Siegel, Michael [Pennsylvania State University, 525 Davey Lab, State College, PA 16801 (United States)

2010-12-15T23:59:59.000Z

255

Structural Materials - Irradiation Studies II  

Science Conference Proceedings (OSTI)

Mar 15, 2012 ... Materials and Fuels for the Current and Advanced Nuclear Reactors: Structural Materials - Irradiation Studies II Sponsored by: The Minerals,...

256

Electron Beam Melting (EBM) II  

Science Conference Proceedings (OSTI)

Oct 19, 2011 ... Additive Manufacturing of Metals: Electron Beam Melting (EBM) II Sponsored by: MS&T Organization Program Organizers: Ian D. Harris, EWI;...

257

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

258

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

259

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

260

Wilton Wind Energy Center II II | Open Energy Information  

Open Energy Info (EERE)

Wilton Wind Energy Center II II Wilton Wind Energy Center II II Facility Wilton Wind Energy Center II Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner NextEra Energy Resources Developer NextEra Energy Resources Energy Purchaser Basin Electric Location Burleigh County ND Coordinates 47.142638°, -100.730567° 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":47.142638,"lon":-100.730567,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

Note: This page contains sample records for the topic "keck ii 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
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261

II.1 Itic  

Office of Legacy Management (LM)

i! il i! il II.1 Itic ihl j' ieil - Department of Emrgy \ Washington, DC20585 1 ' . The Honorable Bill. Johnson 30 Church Street Rochester, New York, 14614, Dear Mayor Johnion: I. ,Se$retary of EnergL Hazel.O'Leary has annouqced a .new appro the Department of Energy (DOE) and its communications with' .,support of this initiative, we are pleased to forward ttie e related to the, former Eastman Kodak Research Laboratoryisit jurisdiction that performed work for DOE or its predecesior information is provided for yourinformation, use', and tete \ I DOE's.Formerly Utilized Sites Remedial Action,Prdgram is re identification. of sites used by DOE's predecessor age~ncies, currelt radiological cqndition and, where it has authority, reaiedral action to @et current radiological'protectionlreq

262

MS, II-J  

Office of Legacy Management (LM)

I' ; ,' I' ; ,' Departm&th of Energy 1 MS, II-J Washington. DC 20585 ' . I I The Honorable John Gallagher ,)fl', /',' ' 103 E. Michigan Avenue .i., ,.' Battle Creek, Michigan 49016 _. Dear Mayor Gallagheri d,---, " '/ approachto openness i.n: with the: public. In (FUSRAP)i.is responsible agencies, determining ~author~ity, performing remedial action to cleanup sites to meet current radiological protection requirements.. A conservative set of technical evaluation guidelines is used in these investigations to assure protection of public health,,~safety and then environment. Where.DQE does not,have .authority for proceeding; the available site information is forwarded to the appropriate Federal or State Agency. DOE studied the historical records of the former Oliver Corp. site, and it

263

L I II C  

Office of Legacy Management (LM)

-- -- - L I II C rr u c c c 7 i' :- ' r' ' 7 i ' -- A' t i ()lL.H~ ORAU 89/i-29 Prepared by Oak Ridge Associated Universities Prepared for Division of Facility and Site Decommissioning Projects U.S. Department of Energy VERIFICATION OF REMEDIAL ACTIONS ALBANYRESEARCHCENTER ALBANY, OREGON P. R. C O lTEN Environmental Survey and Site Assessment Program Energy/Environment Systems Division FINAL REPORT OCTOBER 1989 NOTICES Tha opiniona l xprSaaJd harJln do not n acoaa~rlly ranKI thy oplnioru of thJ l ponaorfng lnrtitutiona ot Oak RidgJ AaaociJ:d IJnivaraltiJa. This raport WJJ prsp~rad as an account ot work sponsorad by thJ Unttad Stslaa Govarnmant. Naithar the UnltSd Strtas Govammanl northa U.S. Daplrtmant of Enargy, norJny ofthairamployaa& makac anywarmnty, l xpraaa or impliad, oraaaumas my Iogrl liabillly

264

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

265

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

266

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

267

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

268

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

269

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

270

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

271

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

272

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. Cebrin; A. Rodrguez; M. Kuster; B. Beltrn; J. M. Carmona; H. Gmez; R. Hartmann; I. G. Irastorza; R. Kotthaus; G. Luzn; J. Morales; A. Ortiz de Solrzano; J. Ruz; L. Strder; J. A. Villar

2007-04-23T23:59:59.000Z

273

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

274

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

275

PARS II Course Presentation (Course 103) | Department of Energy  

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

Presentation (Course 103) PARS II Course Presentation (Course 103) PARS103Presentation.zip More Documents & Publications PARS II Training Workbook (Course 103) PARS II PARS II...

276

PARS II Training | Department of Energy  

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

II Training PARS II Training PARS II training is delivered as traditional, instructor-led, hands-on classroom training, and also, as instructor-led Webinars with limited...

277

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

278

LGS AO Science Impact: Present and Future Perspectives  

E-Print Network (OSTI)

The recent advent of laser guide star adaptive optics (LGS AO) on the largest ground-based telescopes has enabled a wide range of high angular resolution science, previously infeasible from ground-based and/or space-based observatories. As a result, scientific productivity with LGS has seen enormous growth in the last few years, with a factor of ~10 leap in publication rate compared to the first decade of operation. Of the 54 refereed science papers to date from LGS AO, half have been published in the last ~2 years, and these LGS results have already made a significant impact in a number of areas. At the same time, science with LGS AO can be considered in its infancy, as astronomers and instrumentalists are only beginning to understand its efficacy for measurements such as photometry, astrometry, companion detection, and quantitative morphology. We examine the science impact of LGS AO in the last few years of operations, largely due to the new system on the Keck II 10-meter telescope. We review currently achieved data quality, including results from our own ongoing brown dwarf survey with Keck LGS. We assess current and near-future performance with a critical eye to LGS AO's capabilities and deficiencies. From both qualitative and quantitative considerations, it is clear that the era of regular and important science from LGS AO has arrived.

Michael C. Liu

2008-07-03T23:59:59.000Z

279

II"ve  

Office of Legacy Management (LM)

J)£- J)£- II"ve /"/L 6 Ie- Cp~:A July 26, 2006 (J established 1959 Task Order ST06-120 Control Number: IOOO-T06-1573 Mr. Arthur W. Kleinrath Mound Site Manager U.S. Department of Energy Office of Legacy Management 955 Mound Road Miamisburg, OH 4534 2 SUBJECT: Contract No. DE-ACOI-0 2GJ79 491 Deliverable - Draft Long-Term Surveillance and Maintenance Plan for the Ashtabula Closure Project Dear Mr. Kleinrath: In response to the CPAF Deliverable, submittal of the Draft Long-Term Surveillance and Maintenance Plan for the Ashtabula Closure Project is enclosed. If you have any question s, please call Karen Williams of my staff at (937) 847-8350, Extension 307. Donna Gallaher Stoller Mound Site Manager DGljp Enclosure cc: S. Marutzky, Stoller K. Williams, Stoller cc wlo enclosures Correspondence Control File (Thru B. Bonnett) The S.M. Stoller Corpora tion 955 Mound Road Miamisburg.

280

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

Note: This page contains sample records for the topic "keck ii 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

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

282

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

283

TABLE OF CONTENTS TABLE OF CONTENTS ...........................................................................................................................................II  

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

i i ii TABLE OF CONTENTS TABLE OF CONTENTS ...........................................................................................................................................II EXECUTIVE SUMMARY ........................................................................................................................................... 3 INTRODUCTION......................................................................................................................................................... 4 COMPLIANCE SUMMARY ....................................................................................................................................... 6 COMPREHENSIVE ENVIRONMENTAL RESPONSE, COMPENSATION, AND LIABILITY ACT (CERCLA) .................... 6

284

NSLS-II Design and Performance  

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

NSLS-II Design & Performance NSLS-II CD-0 Proposal Preliminary Design Report (PDR) Conceptual Design Report (CDR) Source Properties (.pdf) Cell section Last Modified: April 2,...

285

PARS II FAQ | Department of Energy  

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

More Documents & Publications PARS 3.0 Data Model Project Assessment and Reporting System (PARS II) Earned Value (EV) Analysis and Project Assessment & Reporting System (PARS II)...

286

WIPP Volume II - EM - Final.PDF  

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

of the Secretary of Energy August 2002 Volume II INDEPENDENT OVERSIGHT INSPECTION OF EMERGENCY MANAGEMENT AT THE WASTE ISOLATION PILOT PLANT Volume II August 2002 i INDEPENDENT...

287

Options Study - Phase II  

SciTech Connect

The Options Study has been conducted for the purpose of evaluating the potential of alternative integrated nuclear fuel cycle options to favorably address the issues associated with a continuing or expanding use of nuclear power in the United States. The study produced information that can be used to inform decisions identifying potential directions for research and development on such fuel cycle options. An integrated nuclear fuel cycle option is defined in this study as including all aspects of the entire nuclear fuel cycle, from obtaining natural resources for fuel to the ultimate disposal of used nuclear fuel (UNF) or radioactive wastes. Issues such as nuclear waste management, especially the increasing inventory of used nuclear fuel, the current uncertainty about used fuel disposal, and the risk of nuclear weapons proliferation have contributed to the reluctance to expand the use of nuclear power, even though it is recognized that nuclear power is a safe and reliable method of producing electricity. In this Options Study, current, evolutionary, and revolutionary nuclear energy options were all considered, including the use of uranium and thorium, and both once-through and recycle approaches. Available information has been collected and reviewed in order to evaluate the ability of an option to clearly address the challenges associated with the current implementation and potential expansion of commercial nuclear power in the United States. This Options Study is a comprehensive consideration and review of fuel cycle and technology options, including those for disposal, and is not constrained by any limitations that may be imposed by economics, technical maturity, past policy, or speculated future conditions. This Phase II report is intended to be used in conjunction with the Phase I report, and much information in that report is not repeated here, although some information has been updated to reflect recent developments. The focus in this Options Study was to identify any nuclear fuel cycle technology or option that may result in a significant beneficial impact to the issues as compared to the current U.S. approach of once-through use of nuclear fuel in LWRs or similar reactors followed by direct disposal of UNF. This approach was taken because incremental differences may be difficult to clearly identify and justify due to the large uncertainties that can be associated with the specific causes of the issues. Phase II of this Options Study continued the review of nuclear fuel cycle options that was initiated and documented during Phase I, concentrating on reviewing and summarizing the potential of integrated nuclear fuel cycles. However, based on the reviews of previous studies and available data, it was not always possible to clearly determine sufficiently large differences between the various fuel cycle and technology options for some of the issues or evaluation measures, for example, in cases where only incremental differences with respect to the issues might be achieved regardless of the fuel cycle option or technologies being considered, or where differences were insufficient to clearly rise above the uncertainties.

R. Wigeland; T. Taiwo; M. Todosow; W. Halsey; J. Gehin

2010-09-01T23:59:59.000Z

288

Cimarron II | Open Energy Information  

Open Energy Info (EERE)

II II Jump to: navigation, search Name Cimarron II Facility Cimarron II Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner Duke Energy Developer CPV Renewable Energy Energy Purchaser Kansas City Power & Light Location Cimarron KS Coordinates 37.90154236°, -100.3934097° 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":37.90154236,"lon":-100.3934097,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

289

Limon II | Open Energy Information  

Open Energy Info (EERE)

Limon II Limon II Jump to: navigation, search Name Limon II Facility Limon II Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner NextEra Energy Resources Developer NextEra Energy Resources Energy Purchaser Xcel Energy Location Limon CO Coordinates 39.33323523°, -103.5521507° 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":39.33323523,"lon":-103.5521507,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

290

Aegir II | Open Energy Information  

Open Energy Info (EERE)

II II Jump to: navigation, search Name Aegir II Facility Aegir II Sector Wind energy Facility Type Offshore Wind Facility Status Proposed Location Lake Michigan MI Coordinates 43.098°, -86.597° Loading map... {"minzoom":false,"mappingservice":"googlemaps3","type":"ROADMAP","zoom":14,"types":["ROADMAP","SATELLITE","HYBRID","TERRAIN"],"geoservice":"google","maxzoom":false,"width":"600px","height":"350px","centre":false,"title":"","label":"","icon":"","visitedicon":"","lines":[],"polygons":[],"circles":[],"rectangles":[],"copycoords":false,"static":false,"wmsoverlay":"","layers":[],"controls":["pan","zoom","type","scale","streetview"],"zoomstyle":"DEFAULT","typestyle":"DEFAULT","autoinfowindows":false,"kml":[],"gkml":[],"fusiontables":[],"resizable":false,"tilt":0,"kmlrezoom":false,"poi":true,"imageoverlays":[],"markercluster":false,"searchmarkers":"","locations":[{"text":"","title":"","link":null,"lat":43.098,"lon":-86.597,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

291

Penascal II | Open Energy Information  

Open Energy Info (EERE)

Penascal II Penascal II Jump to: navigation, search Name Penascal II Facility Penascal II Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Developer Iberdrola Renewables Location Kenedy County TX Coordinates 27.003108°, -97.584014° 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":27.003108,"lon":-97.584014,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

292

Photovoltaics II - Programmaster.org  

Science Conference Proceedings (OSTI)

Mar 13, 2012 ... Energy Nanomaterials: Photovoltaics II ... and Their Application in Dye-Sensitized Solar Cells: Ziqi Sun1; Jung Ho Kim1; Yue Zhao1; ... the electron lifetime (?n) are examined by electrochemical impedance spectroscopy (EIS).

293

PARS II 102 Training Workbook  

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

2 Monthly Updating and Reporting 2 Monthly Updating and Reporting Training Workbook V8.0.20101108 Department of Energy March 30, 2011 March 30, 2011 PARS II 102 Monthly Updating and Reporting V8.0.20101108 ii Table of Contents OVERSIGHT and ASSESSMENT ........................................................................................................ 1 Exercise 1 - Find and View a Project............................................................................................ 1 Sort the Project List ................................................................................................................. 3 Select a Project ........................................................................................................................ 4 View a Project ......................................................................................................................... 4

294

The Sloan Digital Sky Survey-II Supernova Survey: Technical Summary  

E-Print Network (OSTI)

The Sloan Digital Sky Survey-II (SDSS-II) has embarked on a multi-year project to identify and measure light curves for intermediate-redshift (0.05 < z < 0.35) Type Ia supernovae (SNe Ia) using repeated five-band (ugriz) imaging over an area of 300 sq. deg. The survey region is a stripe 2.5 degrees wide centered on the celestial equator in the Southern Galactic Cap that has been imaged numerous times in earlier years, enabling construction of a deep reference image for discovery of new objects. Supernova imaging observations are being acquired between 1 September and 30 November of 2005-7. During the first two seasons, each region was imaged on average every five nights. Spectroscopic follow-up observations to determine supernova type and redshift are carried out on a large number of telescopes. In its first two three-month seasons, the survey has discovered and measured light curves for 327 spectroscopically confirmed SNe Ia, 30 probable SNe Ia, 14 confirmed SNe Ib/c, 32 confirmed SNe II, plus a large ...

Frieman, Joshua A; Becker, A; Choi, C; Cinabro, D; De Jongh, F; Depoy, D L; Dilday, B; Doi, M; Garnavich, P M; Hogan, C J; Holtzman, J; Im, M; Jha, S; Kessler, R; Konishi, K; Lampeitl, H; Marriner, J; Marshall, J L; McGinnis, D; Miknaitis, G; Nichol, R C; Prieto, J L; Riess, A G; Richmond, M W; Romani, R; Sako, M; Schneider, D P; Smith, M; Takanashi, N; Tokita, K; van der Heyden, K; Yasuda, N; Zheng, C; Adelman-McCarthy, J; Annis, J; Assef, R J; Barentine, J; Bender, R; Blandford, R D; Boroski, W N; Bremer, M; Brewington, H; Collins, C A; Crotts, A; Dembicky, J; Eastman, J; Edge, A; Edmondson, E; Elson, E; Eyler, M E; Filippenko, A V; Foley, R J; Frank, S; Goobar, A; Gueth, T; Gunn, J E; Harvanek, M; Hopp, U; Ihara, Y; Ivezi?, Ž; Kahn, S; Kaplan, J; Kent, S; Ketzeback, W; Kleinman, S J; Kollatschny, W; Kron, R G; Krzesi?ski, J; Lamenti, D; Leloudas, G; Lin, H; Long, D C; Lucey, J; Lupton, R H; Malanushenko, E; Malanushenko, V; McMillan, R J; Mndez, J; Morgan, C W; Morokuma, T; Nitta, A; Ostman, L; Pan, K; Rockosi, C M; Romer, A K; Ruiz-Lapuente, P; Saurage, G; Schlesinger, K; Snedden, S A; Sollerman, J; Stoughton, C; Stritzinger, M; Subba-Rao, M; Tucker, D; Visnen, P; Watson, L C; Watters, S; Wheeler, J C; Yanny, B; York, D

2007-01-01T23:59:59.000Z

295

The Sloan Digital Sky Survey-II Supernova Survey: Technical Summary  

Science Conference Proceedings (OSTI)

The Sloan Digital Sky Survey-II (SDSS-II) has embarked on a multi-year project to identify and measure light curves for intermediate-redshift (0.05 < z < 0.35) Type Ia supernovae (SNe Ia) using repeated five-band (ugriz) imaging over an area of 300 sq. deg. The survey region is a stripe 2.5 degrees wide centered on the celestial equator in the Southern Galactic Cap that has been imaged numerous times in earlier years, enabling construction of a deep reference image for discovery of new objects. Supernova imaging observations are being acquired between 1 September and 30 November of 2005-7. During the first two seasons, each region was imaged on average every five nights. Spectroscopic follow-up observations to determine supernova type and redshift are carried out on a large number of telescopes. In its first two three-month seasons, the survey has discovered and measured light curves for 327 spectroscopically confirmed SNe Ia, 30 probable SNe Ia, 14 confirmed SNe Ib/c, 32 confirmed SNe II, plus a large number of photometrically identified SNe Ia, 94 of which have host-galaxy spectra taken so far. This paper provides an overview of the project and briefly describes the observations completed during the first two seasons of operation.

Frieman, Joshua A.; /Fermilab /KICP, Chicago /Chicago U., Astron. Astrophys. Ctr.; Bassett, Bruce; /Cape Town U. /South African Astron. Observ.; Becker, Andrew; /Washington U., Seattle, Astron. Dept.; Choi, Changsu; /Seoul Natl. U.; Cinabro, David; /Wayne State U.; DeJongh, Don Frederic; /Fermilab; Depoy, Darren L.; /Ohio State U.; Doi, Mamoru; /Tokyo U.; Garnavich, Peter M.; /Notre Dame U.; Hogan, Craig J.; /Washington U., Seattle, Astron. Dept.; Holtzman, Jon; /New Mexico State U.; Im, Myungshin; /Seoul Natl. U.; Jha, Saurabh; /Stanford U., Phys. Dept.; Konishi, Kohki; /Tokyo U.; Lampeitl, Hubert; /Baltimore, Space Telescope Sci.; Marriner, John; /Fermilab; Marshall, Jennifer L.; /Ohio State U.; McGinnis, David; /Fermilab; Miknaitis, Gajus; /Fermilab; Nichol, Robert C.; /Portsmouth U.; Prieto, Jose Luis; /Ohio State U. /Rochester Inst. Tech. /Stanford U., Phys. Dept. /Pennsylvania U. /Penn State U., Astron. Astrophys. /Portsmouth U. /Tokyo U. /Tokyo U. /South African Astron. Observ. /Tokyo U. /Stanford U., Phys. Dept. /Fermilab /Fermilab /Ohio State U. /Stanford U., Phys. Dept. /Fermilab /Bristol U. /Apache Point Observ. /Liverpool John Moores U., ARI /Columbia U., CBA /Apache Point Observ. /Ohio State U. /Durham U. /Portsmouth U. /South African Astron. Observ. /Naval Academy, Annapolis /UC, Berkeley /UC, Berkeley /Ohio State U. /Stockholm U. /New Mexico State U. /Princeton U. Observ. /Tokyo U. /Washington U., Seattle, Astron. Dept. /Stanford U., Phys. Dept. /Jefferson Lab /Apache Point Observ. /Gottingen U. /Chicago U. /San Francisco State U. /DARK Cosmology Ctr. /Fermilab /Apache Point Observ. /Durham U. /Princeton U. Observ. /Apache Point Observ. /Apache Point Observ. /Apache Point Observ. /Barcelona U. /Stockholm U. /Apache Point Observ. /Lick Observ. /Sussex U. /Barcelona U. /Apache Point Observ. /Ohio State U. /Apache Point Observ. /Fermilab /DARK Cosmology Ctr. /Chicago U. /Fermilab /South African Astron. Observ. /Ohio State U. /Apache Point Observ. /Texas U., McDonald Observ. /Fermilab

2007-09-14T23:59:59.000Z

296

The Sloan Digital Sky Survey-II Supernova Survey: Technical Summary  

E-Print Network (OSTI)

The Sloan Digital Sky Survey-II (SDSS-II) has embarked on a multi-year project to identify and measure light curves for intermediate-redshift (0.05 < z < 0.35) Type Ia supernovae (SNe Ia) using repeated five-band (ugriz) imaging over an area of 300 sq. deg. The survey region is a stripe 2.5 degrees wide centered on the celestial equator in the Southern Galactic Cap that has been imaged numerous times in earlier years, enabling construction of a deep reference image for discovery of new objects. Supernova imaging observations are being acquired between 1 September and 30 November of 2005-7. During the first two seasons, each region was imaged on average every five nights. Spectroscopic follow-up observations to determine supernova type and redshift are carried out on a large number of telescopes. In its first two three-month seasons, the survey has discovered and measured light curves for 327 spectroscopically confirmed SNe Ia, 30 probable SNe Ia, 14 confirmed SNe Ib/c, 32 confirmed SNe II, plus a large number of photometrically identified SNe Ia, 94 of which have host-galaxy spectra taken so far. This paper provides an overview of the project and briefly describes the observations completed during the first two seasons of operation.

Joshua A. Frieman; B. Bassett; A. Becker; C. Choi; D. Cinabro; F. DeJongh; D. L. Depoy; B. Dilday; M. Doi; P. M. Garnavich; C. J. Hogan; J. Holtzman; M. Im; S. Jha; R. Kessler; K. Konishi; H. Lampeitl; J. Marriner; J. L. Marshall; D. McGinnis; G. Miknaitis; R. C. Nichol; J. L. Prieto; A. G. Riess; M. W. Richmond; R. Romani; M. Sako; D. P. Schneider; M. Smith; N. Takanashi; K. Tokita; K. van der Heyden; N. Yasuda; C. Zheng; J. Adelman-McCarthy; J. Annis; R. J. Assef; J. Barentine; R. Bender; R. D. Blandford; W. N. Boroski; M. Bremer; H. Brewington; C. A. Collins; A. Crotts; J. Dembicky; J. Eastman; A. Edge; E. Edmondson; E. Elson; M. E. Eyler; A. V. Filippenko; R. J. Foley; S. Frank; A. Goobar; T. Gueth; J. E. Gunn; M. Harvanek; U. Hopp; Y. Ihara; . Ivezi?; S. Kahn; J. Kaplan; S. Kent; W. Ketzeback; S. J. Kleinman; W. Kollatschny; R. G. Kron; J. Krzesi?ski; D. Lamenti; G. Leloudas; H. Lin; D. C. Long; J. Lucey; R. H. Lupton; E. Malanushenko; V. Malanushenko; R. J. McMillan; J. Mendez; C. W. Morgan; T. Morokuma; A. Nitta; L. Ostman; K. Pan; C. M. Rockosi; A. K. Romer; P. Ruiz-Lapuente; G. Saurage; K. Schlesinger; S. A. Snedden; J. Sollerman; C. Stoughton; M. Stritzinger; M. SubbaRao; D. Tucker; P. Vaisanen; L. C. Watson; S. Watters; J. C. Wheeler; B. Yanny; D. York

2007-08-21T23:59:59.000Z

297

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

298

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

299

Carbon Nanomaterials II & Computational Studies on Nanomaterials  

Science Conference Proceedings (OSTI)

2014 Functional Nanomaterials: Synthesis, Properties and Applications: Carbon Nanomaterials II & Computational Studies on Nanomaterials Sponsored by:...

300

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

Note: This page contains sample records for the topic "keck ii 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.


301

Superspace Type II 4D Supergravity from Type II Superstring  

E-Print Network (OSTI)

We derive the equations of motion of type II 4D supergravity in superspace. This is achieved by coupling the Type II Berkovits' hybrid superstring to an N=2 curved background and requiring that the sigma-model has N=(2,2) superconformal invariance at one loop. We show that there are no anomalies in the fermionic OPE's and the complete set of compensator's equations is derived from the energy-momentum tensor. The equations of motion describe a hypertensorial and vectorial multiplet coupled to a U(1)\\times U(1) N=2 Poincar\\`e Supergravity.

Daniel L. Nedel

2004-12-14T23:59:59.000Z

302

BEATRIX-II, phase II: Data summary report  

SciTech Connect

The BEATRIX-II experimental program was an International Energy Agency sponsored collaborative effort between Japan, Canada, and the United States to evaluate the performance of ceramic solid breeder materials in a fast-neutron environment at high burnup levels. This report addresses the Phase II activities, which included two in situ tritium-recovery canisters: temperature-change and temperature-gradient. The temperature-change canister contained a Li{sub 2}O ring specimen that had a nearly uniform temperature profile and was capable of temperature changes between 530 and 640{degrees}C. The temperature-gradient canister contained a Li{sub 2}ZrO{sub 3} pebble bed operating under a thermal gradient of 440 to 1100{degrees}C. Postirradiation examination was carried out to characterize the Phase II in situ specimens and a series of nonvented capsules designed to address the compatibility of beryllium with lithium-ceramic solid-breeder materials. The results of the BEATRIX-II, Phase II, irradiation experiment provided an extensive data base on the in situ tritium-release characteristics of Li{sub 2}O and Li{sub 2}ZrO{sub 3} for lithium burnups near 5%. The composition of the sweep gas was found to be a critical parameter in the recovery of tritium from both Li{sub 2}O and Li{sub 2}ZrO{sub 3}. Tritium inventories measured confirmed that Li{sub 2}O and Li{sub 2}ZrO{sub 3} exhibited very low tritium retention during the Phase II irradiation. Tritium inventories in Li{sub 2}ZrO{sub 3} after Phase II tended to be larger than those found for Li{sub 2}ZrO{sub 3} in other in situ experiments, but the larger values may reflect the larger generation rates in BEATRIX-II. A series of 20 capsules was irradiated to determine the compatibility of lithium ceramics and beryllium under conditions similar to a fusion blanket. It is concluded that Li{sub 2}O and Li{sub 2}ZrO{sub 3} should remain leading candidates for use in a solid-breeder fusion-blanket application.

Slagle, O.D.; Hollenberg, G.W.

1996-05-01T23:59:59.000Z

303

Ultra high energy neutrino-nucleon cross section from cosmic ray experiments and neutrino telescopes  

E-Print Network (OSTI)

We deduce the cosmogenic neutrino flux by jointly analysing ultra high energy cosmic ray data from HiRes-I and II, AGASA and the Pierre Auger Observatory. We make two determinations of the neutrino flux by using a model-dependent method and a model-independent method. The former is well-known, and involves the use of a power-law injection spectrum. The latter is a regularized unfolding procedure. We then use neutrino flux bounds obtained by the RICE experiment to constrain the neutrino-nucleon inelastic cross section at energies inaccessible at colliders. The cross section bounds obtained using the cosmogenic fluxes derived by unfolding are the most model-independent bounds to date.

V. Barger; Patrick Huber; Danny Marfatia

2006-06-29T23:59:59.000Z

304

Majestic II | Open Energy Information  

Open Energy Info (EERE)

II II Facility Majestic II Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner NextEra Energy Resources Developer NextEra Energy Resources Energy Purchaser SWEPCO Location Amarillo TX Coordinates 35.3672156°, -101.5474892° 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":35.3672156,"lon":-101.5474892,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

305

Harvest II | Open Energy Information  

Open Energy Info (EERE)

Harvest II Harvest II Facility Harvest II Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner Exelon Wind Developer Exelon Wind Energy Purchaser Consumers Energy Location Pigeon MI Coordinates 43.83861292°, -83.2171011° Loading map... {"minzoom":false,"mappingservice":"googlemaps3","type":"ROADMAP","zoom":14,"types":["ROADMAP","SATELLITE","HYBRID","TERRAIN"],"geoservice":"google","maxzoom":false,"width":"600px","height":"350px","centre":false,"title":"","label":"","icon":"","visitedicon":"","lines":[],"polygons":[],"circles":[],"rectangles":[],"copycoords":false,"static":false,"wmsoverlay":"","layers":[],"controls":["pan","zoom","type","scale","streetview"],"zoomstyle":"DEFAULT","typestyle":"DEFAULT","autoinfowindows":false,"kml":[],"gkml":[],"fusiontables":[],"resizable":false,"tilt":0,"kmlrezoom":false,"poi":true,"imageoverlays":[],"markercluster":false,"searchmarkers":"","locations":[{"text":"","title":"","link":null,"lat":43.83861292,"lon":-83.2171011,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

306

Luz II | Open Energy Information  

Open Energy Info (EERE)

Luz II Luz II Jump to: navigation, search Name Luz II Place Jerusalem, Israel Zip 91450 Sector Solar Product Jerusalem-based utility-scale solar power plant developer. Coordinates 31.7736°, 35.224998° 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":31.7736,"lon":35.224998,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

307

Musselshell II | Open Energy Information  

Open Energy Info (EERE)

Musselshell II Musselshell II Facility Musselshell II Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner Goldwind Developer Volkswind USA Energy Purchaser NorthWestern Energy Location Ryegate MT Coordinates 46.26733°, -109.499175° 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":46.26733,"lon":-109.499175,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

308

Glacier II | Open Energy Information  

Open Energy Info (EERE)

II II Facility Glacier II Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner NaturEner Developer NaturEner Energy Purchaser San Diego Gas & Electric Location Near Ethridge MT Coordinates 48.555639°, -112.120992° 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":48.555639,"lon":-112.120992,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

309

Tech Area II: A History  

E-Print Network (OSTI)

This report documents the history of the major buildings in Sandia National Laboratories' Technical Area II. It was prepared in support of the Department of Energy's compliance with Section 106 of the National Historic Preservation Act. Technical Area II was designed and constructed in 1948 specifically for the final assembly of the non-nuclear components of nuclear weapons, and was the primary site conducting such assembly until 1952. Both the architecture and location of the oldest buildings in the area reflect their original purpose. Assembly activities continued in Area II from 1952 to 1957, but the major responsibility for this work shifted to other sites in the Atomic Energy Commission's integrated contractor complex. Gradually, additional buildings were constructed and the original buildings were modified. After 1960, the Area's primary purpose was the research and testing of high-explosive components for nuclear weapons. In 1994, Sandia constructed new facilities for work on hi...

Rebecca Ullrich; Rebecca Ullrich

1998-01-01T23:59:59.000Z

310

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

311

Part II Energy Storage Technologies  

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

II. II. Energy Storage Technology Overview * Instructor - Haresh Kamath, EPRI PEAC * Short term - Flywheels, Cranking Batteries, Electrochemical Capacitors, SMES * Long term - Compressed Air, Pumped Hydro storage, Stationary, Flow Batteries 2 Overview * Technology Types - Batteries, flywheels, electrochemical capacitors, SMES, compressed air, and pumped hydro * Theory of Operation - Brief description of the technologies and the differences between them * State-of-the-art - Past demonstrations, existing hurdles and performance targets for commercialization * Cost and cost projections: - Prototype cost vs. fully commercialized targets Technology Choice for Discharge Time and Power Rating (From ESA) 4 Maturity Levels for Energy Storage Technologies * Mature Technologies - Conventional pumped hydro

312

CHARACTERIZATION OF COLLOIDS FROM HANFORD FORMATION SEDIMENTS REACTED WITH  

E-Print Network (OSTI)

LIGO Hanford, WA W. M. KECK OBSERVATORY Mauna Kea, HI #12;19Su m m E r 2012 ENGINEERING & SCIENCE in Millimeter- Wave Astronomy (CArMA), which consists of 23 radio telescopes working together to produce high Meter telescope (tMt) is in the works there, too, with tentative plans for it to take its place among

Flury, Markus

313

Arnold Schwarzenegger Preserving California's  

E-Print Network (OSTI)

LIGO Hanford, WA W. M. KECK OBSERVATORY Mauna Kea, HI #12;19Su m m E r 2012 ENGINEERING & SCIENCE in Millimeter- Wave Astronomy (CArMA), which consists of 23 radio telescopes working together to produce high Meter telescope (tMt) is in the works there, too, with tentative plans for it to take its place among

314

ReproducedfromSoilScienceSocietyofAmericaJournal.PublishedbySoilScienceSocietyofAmerica.Allcopyrightsreserved. DIVISION S-9--SOIL MINERALOGY  

E-Print Network (OSTI)

LIGO Hanford, WA W. M. KECK OBSERVATORY Mauna Kea, HI #12;19Su m m E r 2012 ENGINEERING & SCIENCE in Millimeter- Wave Astronomy (CArMA), which consists of 23 radio telescopes working together to produce high Meter telescope (tMt) is in the works there, too, with tentative plans for it to take its place among

Flury, Markus

315

2 0 1 0 1 1 California Institute of Technology  

E-Print Network (OSTI)

LIGO Hanford, WA W. M. KECK OBSERVATORY Mauna Kea, HI #12;19Su m m E r 2012 ENGINEERING & SCIENCE in Millimeter- Wave Astronomy (CArMA), which consists of 23 radio telescopes working together to produce high Meter telescope (tMt) is in the works there, too, with tentative plans for it to take its place among

Greer, Julia R.

316

DEEP: Pre-DEIMOS Surveys to I 24 of Galaxy Evolution and Kinematics  

E-Print Network (OSTI)

galaxies with the Keck Telescopes. The scienti#12;c goals include exploring galaxy formation and evolution key area has been rotation curve studies of distant spirals, as reviewed by N. Vogt-resolution data from 8-10 m class telescopes provide three powerful diagnostics for the analysis of distant

317

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

318

NSLS-II RF SYSTEMS  

Science Conference Proceedings (OSTI)

The NSLS-II is a new third generation light source being constructed at Brookhaven Lab. The storage ring is optimized for low emittance by use of damping wigglers to reduce the emittance to below 1 nm-rad. The RF systems are designed to provide stable beam through tight RF phase and amplitude stability requirements.

Rose, J.; Gash, W.; Holub, B.; Kawashima, Y.; Ma, H.; Towne, N.; Yeddulla, M.

2011-03-28T23:59:59.000Z

319

Proposed Data Elements for PARS II Web Application | Department...  

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

Proposed Data Elements for PARS II Web Application Proposed Data Elements for PARS II Web Application Proposed Data Elements for PARS II Web Application More Documents &...

320

Monoiodinated angiotensin II is a potent, full agonist analog of angiotensin II  

SciTech Connect

Mono /sup 125/I-angiotensin II (Ang II) has been used extensively as a radioligand to identify Ang II receptors whereas its receptor binding properties are well characterized, its biological activity has been less well studied. To examine this issue, nonradioisotopic monoiodo-Ang II was prepared and compared to Ang II. Monoiodo-Ang II was found to be a potent, full agonist in in vivo bioassays and a more potent (2.5-fold) pressor agent than the native hormone Ang II in the pithed rat. In eliciting dipsogenic responses monoiodo-Ang II was equipotent to Ang II, but was less potent (2.7-fold) than Ang II in contracting rat aortic strips. These results suggest that the well characterized binding affinity of monoiodo-Ang II is representative of its biological activity (40-250% of the activity of Ang II). The variation in relative peptide potency is consistent with the hypothesis of a heterogeneity of Ang II receptors. Most importantly, the similar efficacies between Ang II and monoiodo-Ang II indicate that the monoiodinated Ang II is a suitable ligand for the study of Ang II receptors.

Husain, A.; Pajka, S.F.; Taylor, S.M.; Speth, R.C.

1986-10-01T23:59:59.000Z

Note: This page contains sample records for the topic "keck ii 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

Edison Phase II Compute Cabinets Arrive  

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

Edison Phase II Compute Cabinets Arrive at NERSC Edison Phase II Compute Cabinets Arrive at NERSC June 27, 2013 by Zhengji Zhao (1 Comments) The compute cabinets were shiped to...

322

COMPUTER PROGRAM CCC USER'S MANUAL VERSION II.  

E-Print Network (OSTI)

1PUTER PROGRAM CCC USER'S MANUAL VERSION II D.C. Mangold,COMPUTER PROGRAM CCC USER'S MANUAL Version II (January,Ll COMPUTER PROGRAM CCC--USER'S MANUAL D. C. Mangold, M, J,

Mangold, D.C.

2013-01-01T23:59:59.000Z

323

MATERIALS FOR SPALLATION NEUTRON SOURCES: II: Radiation ...  

Science Conference Proceedings (OSTI)

MATERIALS FOR SPALLATION NEUTRON SOURCES: Session II: Radiation Effects, B. Sponsored by: Jt. SMD/MSD Nuclear Materials Committee Program...

324

Laser Applications in Materials Technology (II)  

Science Conference Proceedings (OSTI)

About this Symposium. Meeting, Materials Science & Technology 2011. Symposium, Laser Applications in Materials Technology (II). Sponsorship, MS&T ...

325

Spent Fuel Background Report Volume II  

Science Conference Proceedings (OSTI)

This Volume II contains tables that describe DOE fuel storage facilities and the fuel contained in those facilities.

Abbott, D.

1994-03-01T23:59:59.000Z

326

ALCC Allocation Final Report: HPC Colony II  

SciTech Connect

The report describes those activities of the HPC Colony II Project as they relate to their FY2013 ALCC Award.

Jones, Terry R [ORNL] [ORNL

2013-11-01T23:59:59.000Z

327

II.AdvancedTcl Advanced Tcl  

E-Print Network (OSTI)

119 P A R T II.AdvancedTcl II Advanced Tcl Part II describes advanced programming techniques that support sophisticated applications. The Tcl interfaces remain simple, so you can quickly construct pow- erful applications. Chapter 10 describes eval, which lets you create Tcl programs on the fly

Chen, Yuanzhu Peter

328

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

329

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

330

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

331

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

332

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

333

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

334

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

335

First-Year Spectroscopy for the SDSS-II Supernova Survey  

Science Conference Proceedings (OSTI)

This paper presents spectroscopy of supernovae discovered in the first season of the Sloan Digital Sky Survey-II Supernova Survey. This program searches for and measures multi-band light curves of supernovae in the redshift range z = 0.05-0.4, complementing existing surveys at lower and higher redshifts. Our goal is to better characterize the supernova population, with a particular focus on SNe Ia, improving their utility as cosmological distance indicators and as probes of dark energy. Our supernova spectroscopy program features rapid-response observations using telescopes of a range of apertures, and provides confirmation of the supernova and host-galaxy types as well as precise redshifts. We describe here the target identification and prioritization, data reduction, redshift measurement, and classification of 129 SNe Ia, 16 spectroscopically probable SNe Ia, 7 SNe Ib/c, and 11 SNe II from the first season. We also describe our efforts to measure and remove the substantial host galaxy contamination existing in the majority of our SN spectra.

Zheng, Chen; Romani, Roger W.; Sako, Masao; Marriner, John; Bassett, Bruce; Becker, Andrew; Choi, Changsu; Cinabro, David; DeJongh, Fritz; Depoy, Darren L.; Dilday, Ben; Doi, Mamoru; Frieman, Joshua A.; Garnavich, Peter M.; Hogan, Craig J.; Holtzman, Jon; Im, Myungshin; Jha, Saurabh; Kessler, Richard; Konishi, Kohki; Lampeitl, Hubert

2008-03-25T23:59:59.000Z

336

First-Year Spectroscopy for the SDSS-II Supernova Survey  

E-Print Network (OSTI)

This paper presents spectroscopy of supernovae discovered in the first season of the Sloan Digital Sky Survey-II Supernova Survey. This program searches for and measures multi-band light curves of supernovae in the redshift range z = 0.05 - 0.4, complementing existing surveys at lower and higher redshifts. Our goal is to better characterize the supernova population, with a particular focus on SNe Ia, improving their utility as cosmological distance indicators and as probes of dark energy. Our supernova spectroscopy program features rapid-response observations using telescopes of a range of apertures, and provides confirmation of the supernova and host-galaxy types as well as precise redshifts. We describe here the target identification and prioritization, data reduction, redshift measurement, and classification of 129 SNe Ia, 16 spectroscopically probable SNe Ia, 7 SNe Ib/c, and 11 SNe II from the first season. We also describe our efforts to measure and remove the substantial host galaxy contamination existing in the majority of our SN spectra.

Chen Zheng; Roger W. Romani; Masao Sako; John Marriner; Bruce Bassett; Andrew Becker; Changsu Choi; David Cinabro; Fritz DeJongh; Darren L. Depoy; Ben Dilday; Mamoru Doi; Joshua A. Frieman; Peter M. Garnavich; Craig J. Hogan; Jon Holtzman; Myungshin Im; Saurabh Jha; Richard Kessler; Kohki Konishi; Hubert Lampeitl; Jennifer L. Marshall; David McGinnis; Gajus Miknaitis; Robert C. Nichol; Jose Luis Prieto; Adam G. Riess; Michael W. Richmond; Donald P. Schneider; Mathew Smith; Naohiro Takanashi; Kouichi Tokita; Kurt van der Heyden; Naoki Yasuda; Roberto J. Assef; John Barentine; Ralf Bender; Roger D. Blandford; Malcolm Bremer; Howard Brewington; Chris A. Collins; Arlin Crotts; Jack Dembicky; Jason Eastman; Alastair Edge; Ed Elson; Michael E. Eyler; Alexei V. Filippenko; Ryan J. Foley; Stephan Frank; Ariel Goobar; Michael Harvanek; Ulrich Hopp; Yutaka Ihara; Steven Kahn; William Ketzeback; Scott J. Kleinman; Wolfram Kollatschny; Jurek Krzesi?ski; Giorgos Leloudas; Daniel C. Long; John Lucey; Elena Malanushenko; Viktor Malanushenko; Russet J. McMillan; Christopher W. Morgan; Tomoki Morokuma; Atsuko Nitta; Linda Ostman; Kaike Pan; A. Kathy Romer; Gabrelle Saurage; Katie Schlesinger; Stephanie A. Snedden; Jesper Sollerman; Maximilian Stritzinger; Linda C. Watson; Shannon Watters; J. Craig Wheeler; Donald York

2008-02-21T23:59:59.000Z

337

First-Year Spectroscopy for the SDSS-II Supernova Survey  

E-Print Network (OSTI)

This paper presents spectroscopy of supernovae discovered in the first season of the Sloan Digital Sky Survey-II Supernova Survey. This program searches for and measures multi-band light curves of supernovae in the redshift range z = 0.05 - 0.4, complementing existing surveys at lower and higher redshifts. Our goal is to better characterize the supernova population, with a particular focus on SNe Ia, improving their utility as cosmological distance indicators and as probes of dark energy. Our supernova spectroscopy program features rapid-response observations using telescopes of a range of apertures, and provides confirmation of the supernova and host-galaxy types as well as precise redshifts. We describe here the target identification and prioritization, data reduction, redshift measurement, and classification of 129 SNe Ia, 16 spectroscopically probable SNe Ia, 7 SNe Ib/c, and 11 SNe II from the first season. We also describe our efforts to measure and remove the substantial host galaxy contamination existi...

Zheng, Chen; Sako, Masao; Marriner, John; Bassett, Bruce; Becker, Andrew; Choi, Changsu; Cinabro, David; DeJongh, Fritz; Depoy, Darren L; Dilday, Ben; Doi, Mamoru; Frieman, Joshua A; Garnavich, Peter M; Hogan, Craig J; Holtzman, Jon; Im, Myungshin; Jha, Saurabh; Kessler, Richard; Konishi, Kohki; Lampeitl, Hubert; Marshall, Jennifer L; McGinnis, David; Miknaitis, Gajus; Nichol, Robert C; Prieto, Jose Luis; Riess, Adam G; Richmond, Michael W; Schneider, Donald P; Smith, Mathew; Takanashi, Naohiro; Tokita, Kouichi; van der Heyden, Kurt; Yasuda, Naoki; Assef, Roberto J; Barentine, John; Bender, Ralf; Blandford, Roger D; Bremer, Malcolm; Brewington, Howard; Collins, Chris A; Crotts, Arlin; Dembicky, Jack; Eastman, Jason; Edge, Alastair; Elson, Ed; Eyler, Michael E; Filippenko, Alexei V; Foley, Ryan J; Frank, Stephan; Goobar, Ariel; Harvanek, Michael; Hopp, Ulrich; Ihara, Yutaka; Kahn, Steven; Ketzeback, William; Kleinman, Scott J; Kollatschny, Wolfram; Krzesi?ski, Jurek; Leloudas, Giorgos; Long, Daniel C; Lucey, John; Malanushenko, Elena; Malanushenko, Viktor; McMillan, Russet J; Morgan, Christopher W; Morokuma, Tomoki; Nitta, Atsuko; Ostman, Linda; Pan, Kaike; Romer, A Kathy; Saurage, Gabrelle; Schlesinger, Katie; Snedden, Stephanie A; Sollerman, Jesper; Stritzinger, Maximilian; Watson, Linda C; Watters, Shannon; Wheeler, J Craig; York, Donald

2008-01-01T23:59:59.000Z

338

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

339

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

340

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

Note: This page contains sample records for the topic "keck ii telescope" from the National Library of EnergyBeta (NLEBeta).
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We encourage you to perform a real-time search of NLEBeta
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341

NSLS-II Project Schedule  

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

NSLS-II Project Schedule NSLS-II Project Schedule Major Milestone Event Major Milestone Event Preliminary Schedule CD-0 (approve Mission Need) 4th quarter, FY2005 CD-1 (approve Alternative Selection and Cost Range) 4th quarter, FY2007 CD-2 (approve Performance Baseline) 1st quarter, FY2008 CD-3 (approve Start of Construction) 2nd quarter, FY2009 CD-4 (approve Start of Operations) FY2015 Critical Decisions The five Critical Decisions are major milestones approved by the Secretarial Acquisition Executive or Acquisition Executive that establish the mission need, recommended alternative, Acquisition Strategy, the Performance Baseline, and other essential elements required to ensure that the project meets applicable mission, design, security, and safety requirements. Each Critical Decision marks an increase in commitment of

342

Oak Ridge Associated Universities II  

Office of Legacy Management (LM)

Prepared by Prepared by Oak Ridge Associated Universities II Prepared for Division of Fuel - Cycle and Material Safety II U.S. Nuclear Regulatory Commission L RADIOLOGICAL SURVEY OF THE W. R. GRACE PROPERTY WAYNE, NEW JERSEY P. W. FRAME Radiological Site Assessment Program Manpower Education, Research, and Training Division FINAL REPORT January 1983 RADIOLOGICAL SURVEY OF THE W.R. GRACE PROPERTY WAYNE, NEW JERSEY Prepared for Division of Fuel Cycle and Material Safety U.S. Nuclear Regulatory Commission P. W. Frame Project Staff J. D. Berger A. J. Liu R. D. Condra A. M. Pitt G. R. Foltz T. J. Sowell J. R. Frazier C. F. Weaver R. C. Gentry T. S. Yoo Prepared by Radiological Site Assessment Program Manpower Education, Research, and Training Division Oak Ridge Associated Universities

343

Tevatron Run II Physics Projections  

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

Run II Physics Projections (Spring 2006) Run II Physics Projections (Spring 2006) Document for the P5 Committee (version 8, September 30, 2005) Electroweak Precision Measurements and Standard Model Higgs Searches W Mass Measurement: 20 - 30 MeV Projections versus Integrated Luminosity (made by CDF): eps, gif, gif (log) Extrapolated from Run Ib measurement Uncertainties assumed to scale with luminosity: Statiscal uncertainties Systematic uncertainties such as Energy and momentum scale, Hadron Recoil against W Uncertainties assumed not to scale with luminosity: W production and decay: PDFs, d(sigma_W)/d(Pt), higher order QCD/QED effects Assumed to be beween 20 MeV (dashed lines) and 30 MeV (solid lines) Top Mass Measurement: ~1.5 GeV Assumptions Channel: only lepton+jets channle considered. Uncertainties that scale with luminosity - 1 / sqrt(lum)

344

RHIC II Science Working Groups  

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

Workshops Workshops The series of RHIC II Science Workshops began in November 2004, at which time seven Working Groups were initiated. These groups met in workshops through 2005, with the purpose of providing an organized forum for the community to address and describe quantitatively the most important science issues for the proposed RHIC II luminosity upgrade, and corresponding detector upgrades. Each Working Group was led by three convenors representing theory and experiment, and each has produced a detailed report (except for the "New Directions" group, which provided a sounding board and input to the other groups). The Working Group reports are linked below. The summary "white paper" document, "Future Science at the Relativistic Heavy Ion Collider" (PDF), is based on these reports, and was prepared by a Writing Committee that included at least one convenor from each of the Working Groups.

345

A FIRST MEASUREMENT OF THE PROPER MOTION OF THE LEO II DWARF SPHEROIDAL GALAXY  

Science Conference Proceedings (OSTI)

We use 14 year baseline images obtained with the Wide Field and Planetary Camera 2 on board the Hubble Space Telescope (HST) to derive a proper motion for one of the Milky Way's most distant dwarf spheroidal companions, Leo II, relative to an extragalactic background reference frame. Astrometric measurements are performed in the effective point-spread function formalism using our own developed code. An astrometric reference grid is defined using 3224 stars that are members of Leo II and brighter than a magnitude of 25 in the F814W band. We identify 17 compact extragalactic sources, for which we measure a systemic proper motion relative to this stellar reference grid. We derive a proper motion [{mu}{sub {alpha},{mu}{delta}}] = [+104 {+-}113,-33 {+-} 151] {mu}as yr{sup -1} for Leo II in the heliocentric reference frame. Though marginally detected, the proper motion yields constraints on the orbit of Leo II. Given a distance of d {approx_equal} 230 kpc and a heliocentric radial velocity v{sub r} = +79 km s{sup -1}, and after subtraction of the solar motion, our measurement indicates a total orbital motion v{sub G} = 266.1 {+-} 128.7 km s{sup -1} in the Galactocentric reference frame, with a radial component v{sub r{sub G}}=21.5{+-}4.3 km s{sup -1} and tangential component v{sub t{sub G}} = 265.2 {+-} 129.4 km s{sup -1}. The small radial component indicates that Leo II either has a low-eccentricity orbit or is currently close to perigalacticon or apogalacticon distance. We see evidence for systematic errors in the astrometry of the extragalactic sources which, while close to being point sources, are slightly resolved in the HST images. We argue that more extensive observations at later epochs will be necessary to better constrain the proper motion of Leo II. We provide a detailed catalog of the stellar and extragalactic sources identified in the HST data which should provide a solid early-epoch reference for future astrometric measurements.

Lepine, Sebastien [Division of Physical Sciences, Department of Astrophysics, American Museum of Natural History, Central Park West at 79th Street, New York, NY 10024 (United States); Koch, Andreas [Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH (United Kingdom); Rich, R. Michael [Department of Physics and Astronomy, UCLA, 430 Portola Plaza, Los Angeles, CA 90095 (United States); Kuijken, Konrad [Leiden Observatory, Leiden University, P.O. Box 9513, 2300 RA Leiden (Netherlands)

2011-11-10T23:59:59.000Z

346

PARS II Training Materials | Department of Energy  

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

PARS II Training Materials PARS II Training Materials PARS II Training Materials PARS II presentation hand-outs and step-by-step "how to" exercises for each course are available for download. Users who are attending Web classes should download these documents prior to attending the class. PARS 102 - Monthly Updating and Reporting Introduction to PARS II, finding and selecting projects in your domain, viewing Oversight and Assessment (OA) data, viewing Contractor Project Performance (CPP) dashboards, updating your monthly status assessment, adding attachments, and running standard, pre-built reports. PARS 102 Presentation PARS 102 Workbook PARS 103 - Updating Projects and Reporting Introduction to PARS II, finding and selecting projects in your domain, entering new projects into PARS II, entering and editing Oversight and

347

PARS II 104 Contractor Monthly Upload  

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

July 7, 2011 (V1.3) July 7, 2011 (V1.3) PARS II 104 Contractor Monthly Upload 2 July 7, 2011 (V1.3) PARS II 104 Contractor Monthly Upload Course Objectives * Upon completion of this course, users will be able to: - Navigate in the PARS II application - Select a Project to update - Update Project data by performing * An Upload of the latest monthly project performance data extracted from the contractor's local Earned Value Management System (EVMS) * Replace the current or a prior monthly upload in response to feedback or to correct data - Verify the success of the upload - View and interpret the import log generated by the upload process 3 July 7, 2011 (V1.3) PARS II 104 Contractor Monthly Upload Overview PARS II 4 July 7, 2011 (V1.3) PARS II 104 Contractor Monthly Upload PARS II Overview * Commercial-off-the-shelf (COTS) product

348

II  

Office of Legacy Management (LM)

LIST OF FIGURES LIST OF FIGURES 1 General location of Granite City, Illinois . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 6 2 General location of the South Plant facility, Granite City Steel Division, Granite City, Illinois . . . . . . . . . . . . . . . ' . . . . . . . . . . 7 3 Diagram of the New Betatron Building, Granite City Steel facility, Granite City, Illinois. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 8 4 View looking north northwest at the New Betatron Building, Granite City Steel facility, Granite City, Illinois . . . . . . . . . . . . . . . . . . . . . . . . . . . 9 5 View looking east at entrance to the New Betatron Building, Granite City Steel facility, Granite City, Illinois . . . . . . . . . . . . . . . . . . . . . . . . . . . 9

349

II  

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

Page 1 of2 Page 1 of2 (HIOlo U.S. DEPARTMENT OF ENERGY EERE PROJECT MANAGEMENT CENTER NEPA DETERMINATION RECIPIENT:State of Oklahoma PROJECT TITLE: OKLAHOMA SEP ARRA - Native American Cultural & Educational Authority STATE: OK Funding Opportunity Announcemcnt Number Procurement Instrument Number NEPA Control Number CID Number DE-FOA-0000052 EEOOOQ133 GF0-09-332-OO7 0 Based on my review oftbc information concerning the proposed adion, as NEPA Compliance Officer (authorized under DOE Order 45I.1A).1 have made tbe following determination: ex, EA, EIS APPENDIX AND NUMBER: Description: 85.1 Actions to conserve energy, demonstrate potential energy conservation, and promote energy-efficiency that do not increase the indoor concentrations of potentially harmful substances. These actions may involve financial and technical

350

II  

Office of Legacy Management (LM)

l7aa l7aa AMY y ~UJs,bp 7 DOE/OR/20722-20 *1 F F c Formerly Utilized Sites Remedial Action Program (FUSRAP) Contract No. DE-AC05-810R20722 RADIOLOGICAL SURVEY REPORT FOR THE FORMER MIDDLESEX SAMPLING PLANT Middlesex, New Jersey Bechtel Job 14501 Bechtel National, Inc. Advanced Technology Division March 1985 Technical Information Center Office of Scientific and Technical Information U.S. Department of Energy ---___- __-_ __~__ .-_. ..__ - ~-___ LEGAL NOTICE This report was prepared as an nccount of work sponsored by the United Static Government. Neither the United States nor the United States Department of Energy, nor any of their cmployaes, nor any of their contracton, subcontractors, or their employees, makes any warranty, crprem or implied, or aemmes any legal liability or responsibility for the accuracy, completeness

351

II  

Office of Legacy Management (LM)

LIST OF FIGURES 1 General location of Granite City, Illinois . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 6 2 General location of the South Plant facility, Granite City Steel Division, Granite City, Illinois . . . . . . . . . . . . . . . ' . . . . . . . . . . 7 3 Diagram of the New Betatron Building, Granite City Steel facility, Granite City, Illinois. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 8 4 View looking north northwest at the New Betatron Building, Granite City Steel facility, Granite City, Illinois . . . . . . . . . . . . . . . . . . . . . . . . . . . 9 5 View looking east at entrance to the New Betatron Building, Granite City Steel facility, Granite City, Illinois . . . . . . . . . . . . . . . . . . . . . . . . . . . 9

352

Ii  

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

Field Office - Base Period Task Order No.: 003 Task Title: (C) Office of Project Management Required Support: See attached Task Plan and Statement of Work. . Period of...

353

II.  

Gasoline and Diesel Fuel Update (EIA)

or as proposed for for small, highly valued energy services-consumer the Solar Enterprise Zone at the Nevada Test Site. devices, yard, security, and accent lighting, sensing...

354

Page not found | Department of Energy  

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

591 - 22600 of 26,764 results. 591 - 22600 of 26,764 results. Article Mississippi Residents Save Through Appliance Rebate Program April 22 was more than just Earth Day for Cowboy Maloney's Electric City. The Jackson store-one of 12 Cowboy Maloney's across Mississippi-opened at midnight to celebrate Mississippi's appliance rebate program launch. http://energy.gov/articles/mississippi-residents-save-through-appliance-rebate-program Article Geek-Up[12.10.2010]: A New Planet in Another Solar System, Fast-Tracked Drug Treatments and Better Batteries Using high-contrast, near infrared adaptive optics on the Keck II telescope in Hawaii, LLNL astronomers have identified a fourth planet that is part of a new planetary system discovered in 2008. http://energy.gov/articles/geek-up12102010-new-planet-another-solar-system-fast-tracked-drug-treatments-and-better

355

Optical Spectra of Type Ia Supernovae at z=0.46 and z=1.2  

E-Print Network (OSTI)

We present optical spectra, obtained with the Keck 10-m telescope, of two high-redshift type Ia supernovae (SNe Ia) discovered by the High-z Supernova Search Team: SN 1999ff at z=0.455 and SN 1999fv at z~1.2, the highest-redshift published SN Ia spectrum. Both SNe were at maximum light when the spectra were taken. We compare our high-z spectra with low-z normal and peculiar SNe Ia as well as with SNe Ic, Ib, and II. There are no significant differences between SN 1999ff and normal SNe Ia at low redshift. SN 1999fv appears to be a SN Ia and does not resemble the most peculiar nearby SNe Ia.

Coil, A L; Filippenko, A V; Leonard, D C; Tonry, J; Riess, A G; Challis, P M; Clocchiatti, A; Garnavich, P M; Hogan, C J; Jha, S; Kirshner, R P; Leibundgut, B; Phillips, M M; Schmidt, B P; Schommer, R A; Smith, R C; Soderberg, A M; Spyromilio, J; Stubbs, C; Suntzeff, N B; Woudt, P A; Coil, Alison L.; Matheson, Thomas; Filippenko, Alexei V.; Leonard, Douglas C.; Tonry, John; Riess, Adam G.; Challis, Peter; Clocchiatti, Alejandro; Garnavich, Peter M.; Hogan, Craig J.; Jha, Saurabh; Kirshner, Robert P.; Schmidt, Brian P.; Schommer, Robert A.; Soderberg, Alicia M.; Stubbs, Christopher; Suntzeff, Nicholas B.; Woudt, Patrick

2000-01-01T23:59:59.000Z

356

Ozone Conference II: Abstract Proceedings  

Science Conference Proceedings (OSTI)

Ozone Conference II: Pre- and Post-Harvest Applications Two Years After Gras, was held September 27-28, 1999 in Tulare, California. This conference, sponsored by EPRI's Agricultural Technology Alliance and Southern California Edison's AgTAC facility, was coordinated and organized by the on-site ATA-AgTAC Regional Center. Approximately 175 people attended the day-and-a-half conference at AgTAC. During the Conference twenty-two presentations were given on ozone food processing and agricultural applications...

1999-11-24T23:59:59.000Z

357

Giant Protease TPP II's Structure, Mechanism Uncovered  

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

Giant Protease TPP II's Giant Protease TPP II's Structure, Mechanism Uncovered Giant Protease TPP II's Structure, Mechanism Uncovered Print Wednesday, 23 February 2011 00:00 Tripeptidyl peptidase II (TPP II), the largest known eukaryotic enzyme that breaks down proteins (a protease), is implicated in numerous cellular processes including the degradation of the endogenous satiety agent cholecystokinin-8, making TPP II a target in the treatment of obesity. To gain insight into this molecular machine's mechanisms of activation and proteolysis, researchers from Berkeley Lab, the University of California, Berkeley, and the Max Planck Institute of Biochemistry combined single-particle cryo-electron microscopy and x-ray crystallography at ALS Beamline 8.2.2. Treating Obesity with Satiety

358

WIPP Volume II - EM - Final.PDF  

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

Waste Isolation Waste Isolation Pilot Plant Office of Independent Oversight and Performance Assurance Office of the Secretary of Energy August 2002 Volume II INDEPENDENT OVERSIGHT INSPECTION OF EMERGENCY MANAGEMENT AT THE WASTE ISOLATION PILOT PLANT Volume II August 2002 i INDEPENDENT OVERSIGHT INSPECTION OF EMERGENCY MANAGEMENT AT THE WASTE ISOLATION PILOT PLANT Volume II Table of Contents Acronyms .........................................................................................................................................iii 1.0 Introduction ................................................................................................................................1 2.0 Results .......................................................................................................................................3

359

Sample Exchange Evaluation (SEE) Report - Phase II  

SciTech Connect

This report describes the results from Phase II of the Sample Exchange Evaluation (SEE) Program, a joint effort to compare analytical laboratory performance on samples from the Hanford Site`s high-level waste tanks. In Phase II, the program has been expanded to include inorganic constituents in addition to radionuclides. Results from Phase II that exceeded 20% relative percent difference criteria are identified.

Winters, W.I.

1994-09-28T23:59:59.000Z

360

Nanotube Reinforced Metal Matrix Composites II  

Science Conference Proceedings (OSTI)

Symposium, Nanotube Reinforced Metal Matrix Composites II. Sponsorship, MS&T Organization. Organizer(s), Indrajit Charit, University of Idaho Sudipta Seal ...

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361

TRUPACT-II Container Maintenance Program Plan  

Science Conference Proceedings (OSTI)

This document details the maintenance, repair, and replacement of components, as well as the documentation required and the procedures to be followed to maintain the integrity of the TRUPACT-II container in accordance with OM-134, TRUPACT-II Container Operations and Maintenance Manual; and the TRUPACT-II Container Certificate of Compliance (Number 9218). The routine shipping and receiving inspections required by the Department of Transportation (DOT), Department of Energy (DOE), Nuclear Regulatory Commission (NRC) and other regulations are not addressed in this document. This document applies to all DOE shipping and receiving sites that use the TRUPACT-II containers.

Not Available

1991-05-01T23:59:59.000Z

362

INITIAL COMMISSIONING OF NDCX-II  

E-Print Network (OSTI)

INITIAL COMMISSIONING OF NDCX-II* S. Lidia # , D. Arbelaez,the results of early commissioning studies that characterizeschematic and commissioning phases. The commissioning phases

Lidia, S.

2013-01-01T23:59:59.000Z

363

Carlink II: Research Approach and Early Findings  

E-Print Network (OSTI)

Focus Group Protocol Homebased Users Palo Alto, Californiaasking for input as Homebased Users Questions & Answers PartII FOCUS GROUP ONE: HOMEBASED USERS Cubberley Community

Shaheen, Susan

2004-01-01T23:59:59.000Z

364

PARS II Extraction Utility | Department of Energy  

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

PARS II Extraction Utility DEC1387487110111DekkerPMISExtractionUtilityv8020101217.zip More Documents & Publications Dekker PMIS Extraction Utility Release Notes for the PARS...

365

Hydrogen Storage II - Programmaster.org  

Science Conference Proceedings (OSTI)

Aug 3, 2010 ... Symposium L: Energy Generation, Harvesting and Storage Materials: Hydrogen Storage II Program Organizers: Jian-Feng Nie, Monash...

366

NSLS-II Conceptual Design Report (CDR)  

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

Conceptual Design Report NSLS-II CDR cover Brookhaven National Laboratory has prepared a conceptual design for a world class user facility for scientific research using synchrotron...

367

Multics Security Evaluation (Volume II): Vulnerability Analysis  

Science Conference Proceedings (OSTI)

Page 1. ESD-TR-74-J93, Vor. II ' MULTICS SECURITY EVALUATION: VULNERABILITY ANALYSIS Pau r A. Karger, 2Lt ...

2013-04-15T23:59:59.000Z

368

Weak maser emission of methyl formate toward Sagittarius B2(N) in the Green Bank Telescope PRIMOS Survey  

E-Print Network (OSTI)

A non-LTE radiative transfer treatment of cis-methyl formate (HCOOCH3) rotational lines is presented for the first time using a set of theoretical collisional rate coefficients. These coefficients have been computed in the temperature range 5-30 K by combining coupled-channel scattering calculations with a high accuracy potential energy surface for HCOOCH3-He. The results are compared to observations toward the Sagittarius B2(N) molecular cloud using the publicly available PRIMOS survey from the Green Bank Telescope. A total of 49 low-lying transitions of methyl formate, with upper levels below 25 K, are identified. These lines are found to probe a presumably cold (~30 K), moderately dense (~1e4 cm-3) and extended region surrounding Sgr B2(N). The derived column density of ~4e14 cm-2 is only a factor of ~10 larger than the column density of the trans conformer in the same source. Provided that the two conformers have the same spatial distribution, this result suggests that strongly non-equilibrium processes m...

Faure, Alexandre; Szalewicz, Krzysztof; Wiesenfeld, Laurent

2014-01-01T23:59:59.000Z

369

Laboratory and tentative interstellar detection of trans-methyl formate using the publicly available Green Bank Telescope PRIMOS survey  

E-Print Network (OSTI)

The rotational spectrum of the higher-energy trans conformational isomer of methyl formate has been assigned for the first time using several pulsed-jet Fourier transform microwave spectrometers in the 6-60 GHz frequency range. This species has also been sought toward the Sagittarius B2(N) molecular cloud using the publicly available PRIMOS survey from the Green Bank Telescope. We detect seven absorption features in the survey that coincide with laboratory transitions of trans-methyl formate, from which we derive a column density of 3.1 (+2.6, -1.2) \\times 10^13 cm-2 and a rotational temperature of 7.6 \\pm 1.5 K. This excitation temperature is significantly lower than that of the more stable cis conformer in the same source but is consistent with that of other complex molecular species recently detected in Sgr B2(N). The difference in the rotational temperatures of the two conformers suggests that they have different spatial distributions in this source. As the abundance of trans-methyl formate is far higher ...

Neill, Justin L; Zaleski, Daniel P; Steber, Amanda L; Pate, Brooks H; Lattanzi, Valerio; Spezzano, Silvia; McCarthy, Michael C; Remijan, Anthony J

2012-01-01T23:59:59.000Z

370

DETECTION OF E-CYANOMETHANIMINE TOWARD SAGITTARIUS B2(N) IN THE GREEN BANK TELESCOPE PRIMOS SURVEY  

SciTech Connect

The detection of E-cyanomethanimine (E-HNCHCN) toward Sagittarius B2(N) is made by comparing the publicly available Green Bank Telescope (GBT) PRIMOS survey spectra to laboratory rotational spectra from a reaction product screening experiment. The experiment uses broadband molecular rotational spectroscopy to monitor the reaction products produced in an electric discharge source using a gas mixture of NH{sub 3} and CH{sub 3}CN. Several transition frequency coincidences between the reaction product screening spectra and previously unassigned interstellar rotational transitions in the PRIMOS survey have been assigned to E-cyanomethanimine. A total of eight molecular rotational transitions of this molecule between 9 and 50 GHz are observed with the GBT. E-cyanomethanimine, often called the HCN dimer, is an important molecule in prebiotic chemistry because it is a chemical intermediate in proposed synthetic routes of adenine, one of the two purine nucleobases found in DNA and RNA. New analyses of the rotational spectra of both E-cyanomethanimine and Z-cyanomethanimine that incorporate previous millimeter-wave measurements are also reported.

Zaleski, Daniel P.; Seifert, Nathan A.; Steber, Amanda L.; Muckle, Matt T.; Loomis, Ryan A.; Vasquez, David; Nyiramahirwe, Jolie; Sciortino, Nicole; Johnson, Kennedy; Pate, Brooks H. [Department of Chemistry, University of Virginia, McCormick Road, Charlottesville, VA 22904 (United States); Corby, Joanna F. [Department of Astronomy, University of Virginia, McCormick Road, Charlottesville, VA 22904 (United States); Martinez, Oscar Jr.; Crabtree, Kyle N.; McCarthy, Michael C. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Jewell, Philip R.; Remijan, Anthony J. [National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903-2475 (United States); Hollis, Jan M. [NASA Goddard Space Flight Center, Greenbelt, MD 20771 (United States); Lovas, Frank J., E-mail: bp2k@virginia.edu, E-mail: mccarthy@cfa.harvard.edu, E-mail: aremijan@nrao.edu [National Institute of Standards and Technology, Gaithersburg, MD 20899 (United States)

2013-03-01T23:59:59.000Z

371

VAST - a real-time pipeline for detecting radio transients and variables on the Australian SKA Pathfinder (ASKAP) telescope  

E-Print Network (OSTI)

The Australian SKA Pathfinder (ASKAP) is a next generation radio telescope currently under construction in Western Australia. The fast survey speed and wide field of view make it an ideal instrument for blind transients searches. The ASKAP Variable and Slow Transients (VAST) survey is a one of the major science programs planned for ASKAP. The scientific goals of VAST include the detection and characterisation of a wide range of transient and variable phenomena, from gamma-ray burst afterglows to extreme scattering events, on timescales of 5 seconds or longer. We describe the data and processing challenges involved in running the VAST real-time transient detection pipeline. ASKAP will produce 2.5 GB of visibility data per second, transformed into one 8GB image cube every 5 seconds. Each cube will contain approximately twenty 100 megapixel images with 100s of radio sources detected in each epoch. The VAST pipeline will measure and monitor all of these sources, detect variables and transients and generate alerts...

Banyer, Jay

2012-01-01T23:59:59.000Z

372

A Detailed Study of FDIRC Prototype with Waveform Digitizing Electronics in Cosmic Ray Telescope Using 3D Tracks  

SciTech Connect

We present a detailed study of a novel Cherenkov imaging detector called the Focusing DIRC (FDIRC) with waveform digitizing electronics. In this test study, the FDIRC prototype has been instrumented with seven Hamamatsu H-8500 MaPMTs. Waveforms from {approx}450 pixels are digitized with waveform sampling electronics based on the BLAB2 ASIC, operating at a sampling speed of {approx}2.5 GSa/s. The FDIRC prototype was tested in a large cosmic ray telescope (CRT) providing 3D muon tracks with {approx}1.5 mrad angular resolution and muon energy of E{sub muon} > 1.6 GeV. In this study we provide a detailed analysis of the tails in the Cherenkov angle distribution as a function of various variables, compare experimental results with simulation, and identify the major contributions to the tails. We demonstrate that to see the full impact of these tails on the Cherenkov angle resolution, it is crucial to use 3D tracks, and have a full understanding of the role of ambiguities. These issues could not be fully explored in previous FDIRC studies where the beam was perpendicular to the quartz radiator bars. This work is relevant for the final FDIRC prototype of the PID detector at SuperB, which will be tested this year in the CRT setup.

Nishimura, K.; Dey, B.; /Hawaii U. /UC, Riverside; Aston, D.; Leith, D.W.G.S.; Ratcliff, B.; /SLAC; Roberts, D.; /Maryland U.; Ruckman, L.; /Hawaii U.; Shtol, D.; /Novosibirsk, IYF; Varner, G.S.; /Hawaii U.; Va'vra, J.; Vavra, Jerry; /SLAC

2012-07-30T23:59:59.000Z

373

Dark Matter Constraints from Observations of 25 Milky Way Satellite Galaxies with the Fermi Large Area Telescope  

E-Print Network (OSTI)

The dwarf spheroidal satellite galaxies of the Milky Way are some of the most dark-matter-dominated objects known. Due to their proximity, high dark matter content, and lack of astrophysical backgrounds, dwarf spheroidal galaxies are widely considered to be among the most promising targets for the indirect detection of dark matter via gamma rays. Here we report on gamma-ray observations of 25 Milky Way dwarf spheroidal satellite galaxies based on 4 years of Fermi Large Area Telescope (LAT) data. None of the dwarf galaxies are significantly detected in gamma rays, and we present gamma-ray flux upper limits between 500 MeV and 500 GeV. We determine the dark matter content of 18 dwarf spheroidal galaxies from stellar kinematic data and combine LAT observations of 15 dwarf galaxies to constrain the dark matter annihilation cross section. We set some of the tightest constraints to date on the the annihilation of dark matter particles with masses between 2 GeV and 10 TeV into prototypical Standard Model channels. We find these results to be robust against systematic uncertainties in the LAT instrument performance, diffuse gamma-ray background modeling, and assumed dark matter density profile.

The Fermi-LAT Collaboration; :; M. Ackermann; A. Albert; B. Anderson; L. Baldini; J. Ballet; G. Barbiellini; D. Bastieri; K. Bechtol; R. Bellazzini; E. Bissaldi; E. D. Bloom; E. Bonamente; A. Bouvier; T. J. Brandt; J. Bregeon; M. Brigida; P. Bruel; R. Buehler; S. Buson; G. A. Caliandro; R. A. Cameron; M. Caragiulo; P. A. Caraveo; C. Cecchi; E. Charles; A. Chekhtman; J. Chiang; S. Ciprini; R. Claus; J. Cohen-Tanugi; J. Conrad; F. D'Ammando; A. de Angelis; C. D. Dermer; S. W. Digel; E. do Couto e Silva; P. S. Drell; A. Drlica-Wagner; R. Essig; C. Favuzzi; E. C. Ferrara; A. Franckowiak; Y. Fukazawa; S. Funk; P. Fusco; F. Gargano; D. Gasparrini; N. Giglietto; M. Giroletti; G. Godfrey; G. A. Gomez-Vargas; I. A. Grenier; Guiriec; M. Gustafsson; M. Hayashida; E. Hays; J. Hewitt; R. E. Hughes; T. Jogler; T. Kamae; J. Kndlseder; D. Kocevski; M. Kuss; . Larsson; L. Latronico; M. Llena Garde; F. Longo; F. Loparco; M. N. Lovellette; P. Lubrano; G. Martinez; M. Mayer; M. N. Mazziotta; P. F. Michelson; W. Mitthumsiri; T. Mizuno; A. A. Moiseev; M. E. Monzani; A. Morselli; I. V. Moskalenko; S. Murgia; R. Nemmen; E. Nuss; T. Ohsugi; E. Orlando; J. F. Ormes; J. S. Perkins; F. Piron; G. Pivato; T. A. Porter; S. Rain; R. Rando; M. Razzano; S. Razzaque; A. Reimer; O. Reimer; S. Ritz; M. Snchez-Conde; N. Sehgal; C. Sgr; E. J. Siskind; P. Spinelli; L. Strigari; D. J. Suson; H. Tajima; H. Takahashi; J. B. Thayer; L. Tibaldo; M. Tinivella; D. F. Torres; Y. Uchiyama; T. L. Usher; J. Vandenbroucke; G. Vianello; V. Vitale; M. Werner; B. L. Winer; K. S. Wood; M. Wood; G. Zaharijas; S. Zimmer

2013-10-02T23:59:59.000Z

374

Constraining Dark Matter Models from a Combined Analysis of Milky Way Satellites with the Fermi Large Area Telescope  

SciTech Connect

Satellite galaxies of the Milky Way are among the most promising targets for dark matter searches in gamma rays. We present a search for dark matter consisting of weakly interacting massive particles, applying a joint likelihood analysis to 10 satellite galaxies with 24 months of data of the Fermi Large Area Telescope. No dark matter signal is detected. Including the uncertainty in the dark matter distribution, robust upper limits are placed on dark matter annihilation cross sections. The 95% confidence level upper limits range from about 10{sup -26} cm{sup 3} s{sup -1} at 5 GeV to about 5 x 10{sup -23} cm{sup 3} s{sup -1} at 1 TeV, depending on the dark matter annihilation final state. For the first time, using gamma rays, we are able to rule out models with the most generic cross section ({approx}3 x 10{sup -26} cm{sup 3} s{sup -1} for a purely s-wave cross section), without assuming additional boost factors.

Ackermann, M.; Ajello, M.; /Stanford U., HEPL /Taiwan, Natl. Taiwan U. /SLAC; Albert, A.; /Taiwan, Natl. Taiwan U. /Ohio State U.; Atwood, W.B.; /UC, Santa Cruz; Baldini, L.; /INFN, Pisa; Ballet, J.; /DAPNIA, Saclay; Barbiellini, G.; /INFN, Trieste /Trieste U.; Bastieri, D.; /INFN, Padua /Padua U.; Bechtol, K.; /Stanford U., HEPL /Taiwan, Natl. Taiwan U. /SLAC; Bellazzini, R.; /INFN, Pisa; Berenji, B.; Blandford, R.D.; Bloom, E.D.; /Stanford U., HEPL /Taiwan, Natl. Taiwan U. /SLAC; Bonamente, E.; /INFN, Perugia /Perugia U.; Borgland, A.W.; /Stanford U., HEPL /Taiwan, Natl. Taiwan U. /SLAC; Bregeon, J.; /INFN, Pisa; Brigida, M.; /Bari Polytechnic /INFN, Bari; Bruel, P.; /Ecole Polytechnique; Buehler, R.; /Stanford U., HEPL /Taiwan, Natl. Taiwan U. /SLAC; Burnett, T.H.; /Washington U., Seattle; Buson, S.; /INFN, Padua /Padua U. /ICE, Bellaterra /Stanford U., HEPL /Taiwan, Natl. Taiwan U. /SLAC /INFN, Rome /Rome U. /IASF, Milan /IASF, Milan /DAPNIA, Saclay /INFN, Perugia /Perugia U. /Stanford U., HEPL /Taiwan, Natl. Taiwan U. /SLAC /Artep Inc. /Stanford U., HEPL /Taiwan, Natl. Taiwan U. /SLAC /ASDC, Frascati /Perugia U. /Stanford U., HEPL /Taiwan, Natl. Taiwan U. /SLAC /Montpellier U. /Stockholm U. /Stockholm U., OKC /ASDC, Frascati /ASDC, Frascati /Udine U. /INFN, Trieste /Bari Polytechnic /INFN, Bari /Naval Research Lab, Wash., D.C. /Stanford U., HEPL /Taiwan, Natl. Taiwan U. /SLAC /Montpellier U. /Bari Polytechnic /INFN, Bari /Ecole Polytechnique /NASA, Goddard /Hiroshima U. /Stanford U., HEPL /Taiwan, Natl. Taiwan U. /SLAC /Bari Polytechnic /INFN, Bari /INFN, Bari /ASDC, Frascati /NASA, Goddard /INFN, Perugia /Perugia U. /Bari Polytechnic /INFN, Bari /Bologna Observ. /Stanford U., HEPL /Taiwan, Natl. Taiwan U. /SLAC /DAPNIA, Saclay /Alabama U., Huntsville; /more authors..

2012-09-14T23:59:59.000Z

375

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

376

The Nature of Microjansky Radio Sources and Implications for the Design of the Next Generation Very Sensitive Radio Telescopes  

E-Print Network (OSTI)

Deep radio surveys show a population of very red counterparts of microjansky radio sources, which are unidentified to I = 25 in ground based images and I = 28.5 in the Hubble Deep Field. This population of optically faint radio sources, which comprises about 20% of the microjansky radio samples, may be dust enshrouded starburst galaxies, extreme redshift or dust reddened AGN, or due to displaced radio lobes. Even deeper radio surveys, which will be made possible by next generation radio telescopes such as the Expanded VLA or the Square Kilometer Array, will reach to nanojansky levels which may be dominated by this new population, but only if special care is taken to achieve high angular resolution and dynamic range better than 60 dB. This will reuire array dimensions up to 1000 km to achieve confusion limited performance at 1.4 GHz and up to 10,000 km at 300 MHz. But, even then, the ability to study individual nanojanksy radio sources may be limited by the finite extent of the sources and consequential blending of their images.

K. I. Kellermann; E. A. Richards

1999-09-06T23:59:59.000Z

377

A return to strong radio flaring by Circinus X-1 observed with the Karoo Array Telescope test array KAT-7  

E-Print Network (OSTI)

Circinus X-1 is a bright and highly variable X-ray binary which displays strong and rapid evolution in all wavebands. Radio flaring, associated with the production of a relativistic jet, occurs periodically on a ~17-day timescale. A longer-term envelope modulates the peak radio fluxes in flares, ranging from peaks in excess of a Jansky in the 1970s to an historic low of milliJanskys during the years 1994 to 2007. Here we report first observations of this source with the MeerKAT test array, KAT-7, part of the pathfinder development for the African dish component of the Square Kilometre Array (SKA), demonstrating successful scientific operation for variable and transient sources with the test array. The KAT-7 observations at 1.9 GHz during the period 13 December 2011 to 16 January 2012 reveal in temporal detail the return to the Jansky-level events observed in the 1970s. We compare these data to contemporaneous single-dish measurements at 4.8 and 8.5 GHz with the HartRAO 26-m telescope and X-ray monitoring from...

Armstrong, R P; Nicolson, G D; Ratcliffe, S; Linares, M; Horrell, J; Richter, L; Schurch, M P E; Coriat, M; Woudt, P; Jonas, J; Booth, R; Fanaroff, B

2013-01-01T23:59:59.000Z

378

PhaseII1.PDF  

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

Stakeholder Meeting Stakeholder Meeting DOE-NETL Proposed Phase II Large Scale Mercury Control Technology Field Testing Program September 12, 2002 Meeting Summary A meeting was held in Arlington, VA on September 12 on DOE-NETL's plans to go forward with a second phase of field testing of advanced mercury control technology. The meeting was held in conjunction with the Air Quality III Conference and was attended by approximately 53 representatives from the coal and electric-utility industries, technology developers, EPA, and other interested parties (see attached attendees list). Scott Renninger provided a brief overview of DOE-NETL's current mercury field testing program. A summary of the results from an earlier stakeholder meeting held in Washington on June 4 were also presented as a starting point for discussion to help

379

II.CONTRACT ID CODE  

National Nuclear Security Administration (NNSA)

1 1 II.CONTRACT ID CODE ~AGE 1 of AMENDMENT OF SOLICITATIONIMODIFICATION OF CONTRACT PAGES AC 5. PROJECT NO. (If applicable) 3. EFFECTNE DATE 2. AMENDMENTfMODIFICA TION NO. 4. REQUISITIONIPURCHASE REQ. NO. See Block 16c. NOPR 7. ADMINISTERED BY (If other than Item 6) CODE 05008 6. ISSUED BY CODE 05008 U.S. Department of Energy National Nuclear Security Administration U.S. Department of Energy National Nuclear Security Administration P.O. Box 2050 Oak Ridge, TN 37831 P.O. Box 2050 Oak Ridge, TN 37831 9A. AMENDMENT OF SOLICITATION NO. 8. NAME AND ADDRESS OF CONTRACTOR (No., street, county, state, ZIP Code) Babcock & Wilcox Technical Services Y-12, LLC P.O. Box 2009 MS 8014 9B. DATED (SEE ITEM 11) Oak Ridge, TN 37831-8014 lOA. MODIFICATION OF CONTRACT/ORDER NO.

380

GenII Gap Analysis  

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

GENII-Gap Analysis GENII-Gap Analysis Defense Nuclear Facilities Safety Board Recommendation 2002-1 Software Quality Assurance Improvement Plan Commitment 4.2.1.3: Software Quality Assurance Improvement Plan: GENII Gap Analysis Final Report U.S. Department of Energy Office of Environment, Safety, and Health 1000 Independence Ave., S.W. Washington, DC 20585-2040 May 2004 GENII Gap Analysis May 2004 Final Report INTENTIONALLY BLANK ii GENII Gap Analysis May 2004 Final Report FOREWORD This document provides an evaluation of the Software Quality Assurance (SQA) attributes of GENII, a radiological dispersion computer code, relative to established requirements. This evaluation, a "gap analysis", is performed to meet commitment 4.2.1.3 of the Department of

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381

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

382

Upper limit on the flux of photons with energies above 10^19 eV using the Telescope Array surface detector  

E-Print Network (OSTI)

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 upper limits on the absolute flux of primary photons with energies above 10^19, 10^19.5 and 10^20 eV based on the first three years of data taken.

T. Abu-Zayyad; R. Aida; M. Allen; R. Anderson; R. Azuma; E. Barcikowski; J. W. Belz; D. R. Bergman; S. A. Blake; R. Cady; B. G. Cheon; J. Chiba; M. Chikawa; E. J. Cho; W. R. Cho; H. Fujii; T. Fujii; T. Fukuda; M. Fukushima; D. Gorbunov; W. Hanlon; K. Hayashi; Y. Hayashi; N. Hayashida; K. Hibino; K. Hiyama; K. Honda; T. Iguchi; D. Ikeda; K. Ikuta; N. Inoue; T. Ishii; R. Ishimori; D. Ivanov; S. Iwamoto; C. C. H. Jui; K. Kadota; F. Kakimoto; O. Kalashev; T. Kanbe; K. Kasahara; H. Kawai; S. Kawakami; S. Kawana; E. Kido; H. B. Kim; H. K. Kim; J. H. Kim; J. H. Kim; K. Kitamoto; S. Kitamura; Y. Kitamura; K. Kobayashi; Y. Kobayashi; Y. Kondo; K. Kuramoto; V. Kuzmin; Y. J. Kwon; J. Lan; S. I. Lim; S. Machida; K. Martens; T. Matsuda; T. Matsuura; T. Matsuyama; J. N. Matthews; M. Minamino; K. Miyata; Y. Murano; I. Myers; K. Nagasawa; S. Nagataki; T. Nakamura; S. W. Nam; T. Nonaka; S. Ogio; M. Ohnishi; H. Ohoka; K. Oki; D. Oku; T. Okuda; A. Oshima; S. Ozawa; I. H. Park; M. S. Pshirkov; D. C. Rodriguez; S. Y. Roh; G. I. Rubtsov; D. Ryu; H. Sagawa; N. Sakurai; A. L. Sampson; L. M. Scott; P. D. Shah; F. Shibata; T. Shibata; H. Shimodaira; B. K. Shin; J. I. Shin; T. Shirahama; J. D. Smith; P. Sokolsky; B. T. Stokes; S. R. Stratton; T. Stroman; S. Suzuki; Y. Takahashi; M. Takeda; A. Taketa; M. Takita; Y. Tameda; H. Tanaka; K. Tanaka; M. Tanaka; S. B. Thomas; G. B. Thomson; P. Tinyakov; I. Tkachev; H. Tokuno; T. Tomida; S. Troitsky; Y. Tsunesada; K. Tsutsumi; Y. Tsuyuguchi; Y. Uchihori; S. Udo; H. Ukai; G. Vasiloff; Y. Wada; T. Wong; M. Wood; Y. Yamakawa; R. Yamane; H. Yamaoka; K. Yamazaki; J. Yang; Y. Yoneda; S. Yoshida; H. Yoshii; X. Zhou; R. Zollinger; Z. Zundel

2013-04-20T23:59:59.000Z

383

TRUPACT-II procedures and maintenance instructions  

Science Conference Proceedings (OSTI)

The purpose of this document is to provide the technical requirements for operation, inspection and maintenance of a TRUPACT-II Shipping Package and directly related components. This document shall supply the minimum requirements as specified in the TRUPACT-II Safety Analysis Report for Packaging (SARP) and Certificate of Compliance (C of C) 9218. In the event there is a conflict between this document and the TRUPACT-II SARP (NRC Certificate of Compliance No. 9218), the TRUPACT-II SARP shall govern. This document details the operations, maintenance, repair, replacement of components, as well as the documentation required and the procedures to be followed to maintain the integrity of the TRUPACT-II container. These procedures may be modified for site use, but as a minimum all parameters and format listed herein must be included in any site modified version. For convenience and where applicable steps may be performed out of sequence. Packaging and payload handling equipment and transport trailers have been specifically designed for use with the TRUPACT-II Packaging. This document discusses the minimum required procedures for use of the adjustable center of gravity lift fixture and the TRUPACT-II transport trailer in conjunction with the TRUPACT-II Packaging.

NONE

1994-01-14T23:59:59.000Z

384

TEMPEST II--A NEUTRON THERMALIZATION CODE  

SciTech Connect

The TEMPEST II neutron thermalization code in Fortran for IBM 709 or 7090 calculates thermal neutron flux spectra based upon the Wigner-Wilkins equation, the Wilkins equation, or the Maxwellian distribution. When a neutron spectrum is obtained, TEMPEST II provides microscopic and macroscopic cross section averages over that spectrum. Equations used by the code and sample input and output data are given. (auth)

Shudde, R.H.; Dyer, J.

1962-06-01T23:59:59.000Z

385

Photon Sciences | NSLS-II Beamlines  

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

NSLS-II Beamlines NSLS-II Beamlines beamlines Current NSLS-II Beamline Diagram The National Synchrotron Light Source II will accommodate more than 60 beamlines using 27 straight sections for insertion-device sources and 31 bending-magnet or three-pole-wiggler sources, with additional beamlines possible through canted insertion devices and multiple branches. Six beamlines were selected in 2008 and are now funded within the NSLS-II project. These project beamlines encompass research programs in inelastic x-ray scattering, hard x-ray nanoprobe, coherent hard x-ray scattering, coherent soft x-ray scattering and polarization, submicron resolution x-ray spectroscopy, and x-ray powder diffraction. For each beamline, a beamline advisory team, or BAT, has been established to represent the broader scientific community in a specific area of

386

ARM - Field Campaign - IPASRC II Campaign  

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

govCampaignsIPASRC II Campaign govCampaignsIPASRC II Campaign Comments? We would love to hear from you! Send us a note below or call us at 1-888-ARM-DATA. Send Campaign : IPASRC II Campaign 2001.03.05 - 2001.03.16 Lead Scientist : Rune Storvold Data Availability All IPASRC II related data will be collected from the different principal investigators at the University of Alaska in Fairbanks, Geophysical Institute. For further information, contact Chris Marty, (907) 474-7360, or Rune Storvold, (907) 474-6639. For data sets, see below. Summary The second IPASRC II was successfully carried out at the NSA-CART site at Barrow from March 5 to March 15, 2001. During most of the time, great weather and clear skies provided measurements of longwave downward irradiances between 130 and 170 Wm-2 and air temperatures between -25 and -35 degrees Celsius. All pyrgeometers were

387

NMMSS II Training | National Nuclear Security Administration  

National Nuclear Security Administration (NNSA)

II Training | National Nuclear Security Administration II Training | National Nuclear Security Administration Our Mission Managing the Stockpile Preventing Proliferation Powering the Nuclear Navy Emergency Response Recapitalizing Our Infrastructure Continuing Management Reform Countering Nuclear Terrorism About Us Our Programs Our History Who We Are Our Leadership Our Locations Budget Our Operations Media Room Congressional Testimony Fact Sheets Newsletters Press Releases Speeches Events Social Media Video Gallery Photo Gallery NNSA Archive Federal Employment Apply for Our Jobs Our Jobs Working at NNSA Blog NMMSS II Training Home > About Us > Our Programs > Nuclear Security > Nuclear Materials Management & Safeguards System > Training > NMMSS II Training NMMSS II Training U.S. Department of Energy / U.S. Nuclear Regulatory Commission

388

PARS II Change Request (CR) Form  

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

Title: Phone #: Office/Symbol: Email: CHANGE TYPE: Defect: New Requirement: PRIORITY: PARS II Change Request Form (APR 2011) PARS II Change Request (CR) Form 1 = Prevents the accomplishment of an essential PARS-II capability 3 = Adversely affects the accomplishment of an essential PARS-II capability, but a work-around solution is known 4 = Results in User / Operator inconvenience or annoyance, but does not affect an essential PARS-II capability 5 = Any other effect 1) Detailed description of problem/need. (If possible, provide project #(s) you are working with). PROBLEM/CHANGE DESCRIPTION: 2) Where in system defect is seen or where new functionality is required (i.e., which screen, which report). Screenshots (as separate attachments) are helpful.

389

Ormesa II Geothermal Facility | Open Energy Information  

Open Energy Info (EERE)

II Geothermal Facility II Geothermal Facility Jump to: navigation, search GEOTHERMAL ENERGYGeothermal Home Ormesa II Geothermal Facility General Information Name Ormesa II Geothermal Facility Facility Ormesa II Sector Geothermal energy Location Information Address 3300 East Evan Hewes Highway Location Holtville, California Zip 92250 Coordinates 32.787238448581°, -115.24778366089° 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":32.787238448581,"lon":-115.24778366089,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

390

Steamboat II Geothermal Facility | Open Energy Information  

Open Energy Info (EERE)

II Geothermal Facility II Geothermal Facility Jump to: navigation, search GEOTHERMAL ENERGYGeothermal Home Steamboat II Geothermal Facility General Information Name Steamboat II Geothermal Facility Facility Steamboat II Sector Geothermal energy Location Information Location Washoe, Nevada Coordinates 40.5608387°, -119.6035495° 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":40.5608387,"lon":-119.6035495,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

391

NSLS-II Integrated Project Team (IPT)  

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

NSLS-II Integrated Project Team NSLS-II Integrated Project Team DOE uses an integrated project teaming approach for managing the NSLS-II Project. This Integrated Project Team (IPT), organized and led by the NSLS-II Federal Project Director, is an essential element in DOE's acquisition process and is being used during all phases of the project's life cycle. This team consists of professionals representing diverse disciplines with the specific knowledge, skills, and abilities to support the Federal Project Director in successfully executing the project. The IPT for the NSLS-II Project will consist of members from both DOE and the contractor, Brookhaven Science Associates (BSA). The team membership will change as the project progresses from initiation to closeout to ensure the necessary skills are always represented to meet the project's needs.

392

Breezy Bucks II | Open Energy Information  

Open Energy Info (EERE)

Breezy Bucks II Breezy Bucks II Facility Breezy Bucks II Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner Breezy Bucks II LLC / John Deere Wind Energy Developer Breezy Bucks II LLC / John Deere Wind Energy Energy Purchaser Xcel Energy Location Lake Benton MN Coordinates 44.3144°, -96.3317° 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":44.3144,"lon":-96.3317,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

393

Heber II Geothermal Facility | Open Energy Information  

Open Energy Info (EERE)

II Geothermal Facility II Geothermal Facility Jump to: navigation, search GEOTHERMAL ENERGYGeothermal Home Heber II Geothermal Facility General Information Name Heber II Geothermal Facility Facility Heber II Sector Geothermal energy Location Information Location Imperial Valley, California Coordinates 33.03743°, -115.621591° 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":33.03743,"lon":-115.621591,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

394

PARS II User Account Access Guide  

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

Office of Management Office of Management Office of Engineering and Construction Management User Account Access Guide for PARS II Version 1.5 June 25, 2011 Submitted by: Energy Enterprise Solutions 20440 Century Blvd. Suite 150 Germantown, MD 20874 Phone 301-916-0050 Fax 301-916-0066 www.eesllc.net June 25, 2011 (V1.5) PARS II User Account Access Guide ii This page intentionally left blank. June 25, 2011 (V1.5) PARS II User Account Access Guide iii Title Page Document Name: User Account Access Guide for PARS II Version Number: V1.5 Publication Date: June 25, 2011 Contract Number: DE-AT01-06IM00102 Project Number: 1ME07 CLIN 4 Prepared by: Scott Burns, Energy Enterprise Solutions, LLC Reviewed by: Judith Bernsen, Energy Enterprise Solutions, LLC

395

Navy II Geothermal Facility | Open Energy Information  

Open Energy Info (EERE)

II Geothermal Facility II Geothermal Facility Jump to: navigation, search GEOTHERMAL ENERGYGeothermal Home Navy II Geothermal Facility General Information Name Navy II Geothermal Facility Facility Navy II Sector Geothermal energy Location Information Location Coso Junction, California Coordinates 36.018975669535°, -117.79197692871° 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":36.018975669535,"lon":-117.79197692871,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

396

TRUPACT-II container maintenance program plan  

SciTech Connect

This document details the maintenance/repair and replacement of components, as well as the documentation required and the procedures to be followed to maintain the integrity of the TRUPACT-II container, in accordance with requirements of the TRUPACT-II Container Operations and Maintenance Manual, OM-134, the TRUPACT-II Container Safety Analysis Report (SARP), and the TRUPACT-II Container Certificate of Compliance (Number 9218). The routine shipping and receiving inspections required by the Department of Transportation (DOT), Department of Energy (DOE), Nuclear Regulatory Commission (NRC) and other regulations are not addressed in this document. This document applies to all DOE shipping and receiving sites that use the TRUPACT-II containers.

Not Available

1990-11-01T23:59:59.000Z

397

TRUPACT-II Operating and Maintenance Instructions  

SciTech Connect

The purpose of this document is to provide the technical requirements for preparation for use, operation, inspection, and maintenance of a Transuranic Package Transporter Model II (TRUPACT-II) Shipping Package and directly related components. This document complies with the minimum requirements as specified in the TRUPACT-II Safety Analysis Report for Packaging (SARP) and Nuclear Regulatory Commission (NRC) Certificate of Compliance (C of C) 9218. In the event there is a conflict between this document and the TRUPACT-II SARP, the TRUPACT-II SARP shall govern. TRUPACT-II C of C number 9218 states, ''... each package must be prepared for shipment and operated in accordance with the procedures described in Chapter 7.0, Operating Procedures, of the application.'' It further states, ''... each package must be tested and maintained in accordance with the procedures described in Chapter 8.0, Acceptance Tests and Maintenance Program of the application.'' Chapter 9 of the TRUPACT-II SARP charges the Westinghouse Electric Corporation Waste Isolation Division (WID) with assuring that the TRUPACT-II is used in accordance with the requirements of the C of C. To meet this requirement and verify consistency of operations when loading and unloading the TRUPACT-II on the trailer, placing a payload in the packaging, unloading the payload from the packaging, or performing maintenance, the U.S. Department of Energy Carlsbad Area Office (U.S. DOE/CAO) finds it necessary to implement the changes that follow. This TRUPACT-II maintenance document represents a change to previous philosophy regarding site specific procedures for the use of the TRUPACT-II. This document details the instructions to be followed to consistently operate and maintain the TRUPACT-II. The intent of these instructions is to ensure that all users of the TRUPACT-II follow the same or equivalent instructions. Users may achieve this intent by any of the following methods: (1) Utilizing these instructions as is, or (2) Attaching a site-specific cover page/letter to this document stating that these are the instructions to be used at their location, or (3) Sites may prepare their own document using the steps in this document word-for-word, in-sequence, including Notes and Cautions. Site specific information may be included as deemed necessary. Submit the document to WID National TRU Programs for approval. Any revision made subsequent to WID TRU Program's approval shall be reviewed and approved by WID TRU Programs. A copy of the approval letter from WID National TRU Programs should be available for audit purposes. Users shall develop site-specific procedures addressing leak testing, preoperational activities, quality assurance, hoisting and rigging, and radiation health physics to be used in conjunction with the instructions contained in this document. Users desiring to recommend changes to this document may submit their recommendations to the WID National TRU Programs for evaluation. If approved, the change(s) will be incorporated into this document for use by all TRUPACT-II users. User sites will be audited to this document to ensure compliance within one year from the effective date of this revision. This document discusses operating instructions, required inspections and maintenance for the following: TRUPACT-II packaging, and Miscellaneous packaging, special tools, and equipment. Packaging and payload handling equipment and transport trailers have been specifically designed for use with the TRUPACT-II Packaging. This document discusses the required instructions for use of the following equipment in conjunction with the TRUPACT-II Packaging: TRUPACT-II Mobile Loading Unit (MLU), Adjustable Center-of-Gravity Lift Fixture (ACGLF), and TRUPACT-II Transport Trailer. Attachment E contains the various TRUPACT-II packaging interface control drawings, leak-test and vent-port tool drawings, ACGLF drawings, and tie-down drawings that identify the various system components.

Westinghouse Electric Corporation, Waste Isolation Division

1999-12-31T23:59:59.000Z

398

STELLAR TIDAL STREAMS IN SPIRAL GALAXIES OF THE LOCAL VOLUME: A PILOT SURVEY WITH MODEST APERTURE TELESCOPES  

Science Conference Proceedings (OSTI)

Within the hierarchical framework for galaxy formation, minor merging and tidal interactions are expected to shape all large galaxies to the present day. As a consequence, most seemingly normal disk galaxies should be surrounded by spatially extended stellar 'tidal features' of low surface brightness. As part of a pilot survey for such interaction signatures, we have carried out ultra deep, wide field imaging of eight isolated spiral galaxies in the Local Volume, with data taken at small (D = 0.1-0.5 m) robotic telescopes that provide exquisite surface brightness sensitivity ({mu}{sub lim}(V) {approx} 28.5 mag arcsec{sup -2}). This initial observational effort has led to the discovery of six previously undetected extensive (to {approx}30 kpc) stellar structures in the halos surrounding these galaxies, likely debris from tidally disrupted satellites. In addition, we confirm and clarify several enormous stellar over-densities previously reported in the literature, but never before interpreted as tidal streams. Even this pilot sample of galaxies exhibits strikingly diverse morphological characteristics of these extended stellar features: great circle-like features that resemble the Sagittarius stream surrounding the Milky Way, remote shells and giant clouds of presumed tidal debris far beyond the main stellar body, as well as jet-like features emerging from galactic disks. Together with presumed remains of already disrupted companions, our observations also capture surviving satellites caught in the act of tidal disruption. A qualitative comparison with available simulations set in a {Lambda}Cold Dark Matter cosmology (that model the stellar halo as the result of satellite disruption evolution) shows that the extraordinary variety of stellar morphologies detected in this pilot survey matches that seen in those simulations. The common existence of these tidal features around 'normal' disk galaxies and the morphological match to the simulations constitutes new evidence that these theoretical models also apply to a large number of other Milky Way-mass disk galaxies in the Local Volume.

MartInez-Delgado, David; Zibetti, Stefano; Rix, Hans-Walter [Max Planck Institut fuer Astronomie, Heidelberg (Germany); Gabany, R. Jay [Black Bird Observatory, Mayhill, NM (United States); Crawford, Ken [Rancho del Sol Observatory, Modesto, CA (United States); Majewski, Steven R.; McDavid, David A. [Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325 (United States); Fliri, Juergen; Carballo-Bello, Julio A.; Bardalez-Gagliuffi, Daniella C.; Trujillo, Ignacio [Instituto de Astrofisica de Canarias, La Laguna (Spain); Penarrubia, Jorge [Institute of Astronomy, University of Cambridge (United Kingdom); Chonis, Taylor S. [Department of Astronomy, University of Texas, Austin, TX 78712-0259 (United States); Madore, Barry [The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101 (United States); Schirmer, Mischa [Argelander Institut fuer Astronomie, Universitaet Bonn (Germany)

2010-10-15T23:59:59.000Z

399

GREEN BANK TELESCOPE DETECTION OF POLARIZATION-DEPENDENT H I ABSORPTION AND H I OUTFLOWS IN LOCAL ULIRGs AND QUASARS  

SciTech Connect

We present the results of a 21 cm H I survey of 27 local massive gas-rich late-stage mergers and merger remnants with the Robert C. Byrd Green Bank Telescope. These remnants were selected from the Quasar/ULIRG Evolution Study sample of ultraluminous infrared galaxies (ULIRGs; L{sub 8{sub -{sub 1000{sub {mu}m}}}} > 10{sup 12} L{sub Sun }) and quasars; our targets are all bolometrically dominated by active galactic nuclei (AGNs) and sample the later phases of the proposed ULIRG-to-quasar evolutionary sequence. We find the prevalence of H I absorption (emission) to be 100% (29%) in ULIRGs with H I detections, 100% (88%) in FIR-strong quasars, and 63% (100%) in FIR-weak quasars. The absorption features are associated with powerful neutral outflows that change from being mainly driven by star formation in ULIRGs to being driven by the AGN in the quasars. These outflows have velocities that exceed 1500 km s{sup -1} in some cases. Unexpectedly, we find polarization-dependent H I absorption in 57% of our spectra (88% and 63% of the FIR-strong and FIR-weak quasars, respectively). We attribute this result to absorption of polarized continuum emission from these sources by foreground H I clouds. About 60% of the quasars displaying polarized spectra are radio-loud, far higher than the {approx}10% observed in the general AGN population. This discrepancy suggests that radio jets play an important role in shaping the environments in these galaxies. These systems may represent a transition phase in the evolution of gas-rich mergers into ''mature'' radio galaxies.

Teng, Stacy H. [Observational Cosmology Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD 20771 (United States); Veilleux, Sylvain [Department of Astronomy, University of Maryland, College Park, MD 20742 (United States); Baker, Andrew J., E-mail: stacy.h.teng@nasa.gov [Department of Physics and Astronomy, Rutgers, State University of New Jersey, Piscataway, NJ 08854 (United States)

2013-03-10T23:59:59.000Z

400

THE GREEN BANK TELESCOPE 350 MHz DRIFT-SCAN SURVEY. I. SURVEY OBSERVATIONS AND THE DISCOVERY OF 13 PULSARS  

SciTech Connect

Over the summer of 2007, we obtained 1191 hr of 'drift-scan' pulsar search observations with the Green Bank Telescope at a radio frequency of 350 MHz. Here we describe the survey setup, search procedure, and the discovery and follow-up timing of 13 pulsars. Among the new discoveries, one (PSR J1623-0841) was discovered only through its single pulses, two (PSRs J1327-0755 and J1737-0814) are millisecond pulsars, and another (PSR J2222-0137) is a mildly recycled pulsar. PSR J1327-0755 is a 2.7 ms pulsar at a dispersion measure (DM) of 27.9 pc cm{sup -3} in an 8.7 day orbit with a minimum companion mass of 0.22 M {sub Sun }. PSR J1737-0814 is a 4.2 ms pulsar at a DM of 55.3 pc cm{sup -3} in a 79.3 day orbit with a minimum companion mass of 0.06 M {sub Sun }. PSR J2222-0137 is a 32.8 ms pulsar at a very low DM of 3.27 pc cm{sup -3} in a 2.4 day orbit with a minimum companion mass of 1.11 M {sub Sun }. It is most likely a white-dwarf-neutron-star system or an unusual low-eccentricity double neutron star system. Ten other pulsars discovered in this survey are reported in the companion paper Lynch et al.

Boyles, J.; Lorimer, D. R.; McLaughlin, M. A.; Cardoso, R. F. [Department of Physics, West Virginia University, Morgantown, WV 26506 (United States)] [Department of Physics, West Virginia University, Morgantown, WV 26506 (United States); Lynch, R. S.; Kaspi, V. M.; Archibald, A.; Karako-Argaman, C. [Department of Physics, McGill University, 3600 University St., Montreal, Quebec, H3A 2T8 (Canada)] [Department of Physics, McGill University, 3600 University St., Montreal, Quebec, H3A 2T8 (Canada); Ransom, S. M. [National Radio Astronomy Observatory (NRAO), 520 Edgemont Road, Charlottesville, VA 22901 (United States)] [National Radio Astronomy Observatory (NRAO), 520 Edgemont Road, Charlottesville, VA 22901 (United States); Stairs, I. H.; Berndsen, A.; Cherry, A.; McPhee, C. A. [Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, British Columbia V6T 1Z1 (Canada)] [Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, British Columbia V6T 1Z1 (Canada); Hessels, J. W. T.; Kondratiev, V. I.; Van Leeuwen, J. [ASTRON, The Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA, Dwingeloo (Netherlands)] [ASTRON, The Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA, Dwingeloo (Netherlands); Epstein, C. R. [Department of Astronomy, Ohio State University, 140 W. 18th Avenue, Columbus, OH 43210 (United States)] [Department of Astronomy, Ohio State University, 140 W. 18th Avenue, Columbus, OH 43210 (United States); Pennucci, T. [Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325 (United States)] [Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325 (United States); Roberts, M. S. E. [Eureka Scientific, 2452 Delmer Street, Suite 100, Oakland, CA 94602-3017 (United States)] [Eureka Scientific, 2452 Delmer Street, Suite 100, Oakland, CA 94602-3017 (United States); Stovall, K., E-mail: jason.boyles@wku.edu [Center for Advanced Radio Astronomy and Department of Physics and Astronomy, University of Texas at Brownsville, Brownsville, TX 78520 (United States)

2013-02-15T23:59:59.000Z

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401

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

402

NSLS-II | NEXT Integrated Project Team | Home  

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

NEXT Project NEXT stands for NSLS-II Experimental Tools, a set of five or six beamlines being developed for the National Synchrotron Light Source II (NSLS-II), with funding from...

403

Attachment 5 Volume II Pricing Matrix.xls | Department of...  

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

5 Volume II Pricing Matrix.xls&0; Attachment 5 Volume II Pricing Matrix.xls&0; Attachment 5 Volume II Pricing Matrix.xls&0; More Documents & Publications Attachment 6 Volume V...

404

NSLS II: The Future National Synchrotron Light Source  

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

NSLS-II Beamlines NSLS-II Ring Schematic The National Synchrotron Light Source II will accommodate at least 58 beamlines using 27 straight sections for insertion-device sources and...

405

Giant Protease TPP II's Structure, Mechanism Uncovered  

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

Giant Protease TPP II's Structure, Mechanism Uncovered Print Giant Protease TPP II's Structure, Mechanism Uncovered Print Tripeptidyl peptidase II (TPP II), the largest known eukaryotic enzyme that breaks down proteins (a protease), is implicated in numerous cellular processes including the degradation of the endogenous satiety agent cholecystokinin-8, making TPP II a target in the treatment of obesity. To gain insight into this molecular machine's mechanisms of activation and proteolysis, researchers from Berkeley Lab, the University of California, Berkeley, and the Max Planck Institute of Biochemistry combined single-particle cryo-electron microscopy and x-ray crystallography at ALS Beamline 8.2.2. Treating Obesity with Satiety Cholecystokinin (CCK) is a hormone in the brain and gastrointestinal system that helps stimulate the digestion of fat and protein and acts as a satiety agent, suppressing hunger and inhibiting food intake. Tripeptidyl peptidase II (TPP II) is known to partly regulate CCK-8 (a CCK with 8 amino acid residues) by cleaving the hormone into 5- and 3-residue chains, inactivating it.

406

Giant Protease TPP II's Structure, Mechanism Uncovered  

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

Giant Protease TPP II's Structure, Mechanism Uncovered Print Giant Protease TPP II's Structure, Mechanism Uncovered Print Tripeptidyl peptidase II (TPP II), the largest known eukaryotic enzyme that breaks down proteins (a protease), is implicated in numerous cellular processes including the degradation of the endogenous satiety agent cholecystokinin-8, making TPP II a target in the treatment of obesi