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1

Redshift z ~ 1 Field Galaxies Observed with the Keck Telescope and the HST  

E-Print Network (OSTI)

We report results based on 35 new spectroscopic redshifts obtained with the Keck Telescope for field galaxies that also have photometry and morphology from survey images taken by the refurbished HST. A sample of 24 redshifts for galaxies fainter than I = 22 has a median redshift of z ~ 0.81. This result is inconsistent with the lower median redshift of z ~ 0.6 predicted by the ``maximal merger models'' of Carlberg (1996), which otherwise fit existing data. The data match an extrapolation of the CFRS, as well as predictions of certain mild luminosity-evolution models. Nearly half of the redshifts lie in two structures at z ~ 0.81 and z ~ 1.0, showing the presence of high density concentrations spanning scales of ~ 1/h Mpc, i.e., the size of groups. We find emission lines or the presence of possible neighbors in 7 of 9 otherwise luminous galaxies with red central regions at redshifts beyond z ~ 0.7. We also note a diversity of morphological types among blue galaxies at z ~ 1, including small compact galaxies, ``chains,'' and ``blue nucleated galaxies.'' These morphologies are found among local, but generally less luminous, galaxies. Distant blue galaxies also include apparently normal late-type spirals. These findings could imply modest bursts of star formation caused by mergers or interactions of small, gas-rich galaxies with each other or with larger, well-formed galaxies. This first glimpse of very faint z ~ 1 field galaxies of diverse colors and morphologies suggests that a mixture of physical processes is at work in the formation and evolution of faint field galaxies.

David C. Koo; Nicole P. Vogt; Andrew C. Phillips; Rafael Guzman; K. L. Wu; S. M. Faber; Caryl Gronwall; Duncan A. Forbes; Garth D. Illingworth; Edward J. Groth; Marc Davis; Richard G. Kron; Alexander S. Szalay

1996-04-19T23:59:59.000Z

2

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

E-Print Network (OSTI)

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

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

2015-01-01T23:59:59.000Z

3

NASA Keck Time Solicitation For Professional Research Using the NASA Allocation of  

E-Print Network (OSTI)

#12;#12;NASA Keck Time Solicitation For Professional Research Using the NASA Allocation Information The NASA Exoplanet Science Institute (NExScI) is calling for proposals to use NASA's share of observing time at the W.M. Keck Observatory (WMKO). On average, NASA receives an allocation of 45 telescope

Abu-Mostafa, Yaser S.

4

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

E-Print Network (OSTI)

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

Enomoto, Ryoji

5

PHOTOMETRICALLY TRIGGERED KECK SPECTROSCOPY OF FERMI BL LACERTAE OBJECTS  

SciTech Connect

We report on Keck spectra of 10 Fermi blazars. J0622+3326, previously unobserved, is shown to be a flat-spectrum radio quasar at redshift z = 1.062. The others are known BL Lac type objects that have resisted previous attempts to secure redshifts. Using a photometric monitoring campaign with the 0.76 m Katzman Automatic Imaging Telescope at Lick Observatory, we identified epochs when the relativistic jet emission was fainter than usual, thus triggering the Keck spectroscopy. This strategy gives improved sensitivity to stars and ionized gas in the host galaxy, thereby providing improved redshift constraints for seven of these sources.

Shaw, Michael S.; Romani, Roger W. [Department of Physics/KIPAC, Stanford University, Stanford, CA 94305 (United States); Filippenko, Alexei V.; Cenko, S. Bradley; Li, Weidong [Department of Astronomy, University of California, Berkeley, CA 94720-3411 (United States)

2013-11-01T23:59:59.000Z

6

THE INNER KILOPARSEC OF Mrk 273 WITH KECK ADAPTIVE OPTICS  

SciTech Connect

There is X-ray, optical, and mid-infrared imaging and spectroscopic evidence that the late-stage ultraluminous infrared galaxy merger Mrk 273 hosts a powerful active galactic nucleus (AGN). However, the exact location of the AGN and the nature of the nucleus have been difficult to determine due to dust obscuration and the limited wavelength coverage of available high-resolution data. Here we present near-infrared integral-field spectra and images of the nuclear region of Mrk 273 taken with OSIRIS and NIRC2 on the Keck II Telescope with laser guide star adaptive optics. We observe three spatially resolved components, and analyze the nuclear molecular and ionized gas emission lines and their kinematics. We confirm the presence of the hard X-ray AGN in the southwest nucleus. In the north nucleus, we find a strongly rotating gas disk whose kinematics indicate a central black hole of mass 1.04 ± 0.1 × 10{sup 9} M{sub ?}. The H{sub 2} emission line shows an increase in velocity dispersion along the minor axis in both directions, and an increased flux with negative velocities in the southeast direction; this provides direct evidence for a collimated molecular outflow along the axis of rotation of the disk. The third spatially distinct component appears to the southeast, 640 and 750 pc from the north and southwest nuclei, respectively. This component is faint in continuum emission but shows several strong emission line features, including [Si VI] 1.964 ?m which traces an extended coronal-line region. The geometry of the [Si VI] emission combined with shock models and energy arguments suggest that [Si VI] in the southeast component must be at least partly ionized by the SW AGN or a putative AGN in the northern disk, either through photoionization or through shock-heating from strong AGN- and circumnuclear-starburst-driven outflows. This lends support to a scenario in which Mrk 273 may be a dual AGN system.

U, Vivian; Sanders, David; Kewley, Lisa [Institute for Astronomy, University of Hawaii, 2680 Woodlawn Dr., Honolulu, HI 96822 (United States); Medling, Anne; Max, Claire [Department of Astronomy and Astrophysics, University of California, Santa Cruz, 1156 High Street, Santa Cruz, CA 95064 (United States); Armus, Lee [Spitzer Science Center, California Institute of Technology, 1200 E. California Blvd., Pasadena, CA 91125 (United States); Iwasawa, Kazushi [ICREA and Institut del Ciències del Cosmos, Universitat de Barcelona (IEEC-UB), Martí i Franquès, 1, E-08028 Barcelona (Spain); Evans, Aaron [Department of Astronomy, University of Virginia, 530 McCormick Road, Charlottesville, VA 22904 (United States); Fazio, Giovanni, E-mail: vivianu@ucr.edu [Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138 (United States)

2013-10-01T23:59:59.000Z

7

KECK OBSERVATIONS OF THE GALACTIC CENTER SOURCE G2: GAS CLOUD OR STAR?  

SciTech Connect

We present new observations and analysis of G2-the intriguing red emission-line object which is quickly approaching the Galaxy's central black hole. The observations were obtained with the laser guide star adaptive optics systems on the W. M. Keck I and II telescopes (2006-2012) and include spectroscopy (R {approx} 3600) centered on the hydrogen Br{gamma} line as well as K' (2.1 {mu}m) and L' (3.8 {mu}m) imaging. Analysis of these observations shows the Br{gamma} line emission has a positional offset from the L' continuum. This offset is likely due to background source confusion at L'. We therefore present the first orbital solution derived from Br{gamma} line astrometry, which, when coupled with radial velocity measurements, results in a later time of closest approach (2014.21 {+-} 0.14), closer periastron (130 AU, 1600 R{sub s}), and higher eccentricity (0.9814 {+-} 0.0060) compared to a solution using L' astrometry. It is shown that G2 has no K' counterpart down to K' {approx} 20 mag. G2's L' continuum and the Br{gamma} line emission appears unresolved in almost all epochs, which implies that the bulk of the emission resides in a compact region. The observations altogether suggest that while G2 has a gaseous component that is tidally interacting with the central black hole, there is likely a central star providing the self-gravity necessary to sustain the compact nature of this object.

Phifer, K.; Meyer, L.; Ghez, A. M.; Witzel, G.; Yelda, S.; Boehle, A.; Morris, M. R.; Becklin, E. E. [Department of Physics and Astronomy, University of California, Los Angeles, CA 90095 (United States); Do, T. [Dunlap Institute for Astronomy and Astrophysics, University of Toronto, Toronto, Ontario, M5S 3H4 (Canada); Lu, J. R. [Institute for Astronomy, University of Hawaii, Hilo, HI 96720 (United States); Matthews, K., E-mail: ghez@astro.ucla.edu [Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA 91125 (United States)

2013-08-10T23:59:59.000Z

8

KECK ADAPTIVE OPTICS OBSERVATIONS OF THE PROTOSTELLAR DISK AROUND RADIO SOURCE I IN THE ORION KLEINMANN-LOW NEBULA  

SciTech Connect

We have made the first detection of a near-infrared counterpart associated with the disk around Radio Source ''I'', a massive protostar in the Kleinmann-Low nebula in Orion, using imaging with laser guide star adaptive optics on the Keck II telescope. The infrared emission is evident in images acquired using L' (3.8 {mu}m) and Ms (4.7 {mu}m) filters and is not detectable at K' (2.1 {mu}m). The observed morphology strongly suggests that we are seeing some combination of scattered and thermal light emanating from the disk. The disk is also manifest in the L'/Ms flux ratio image. We interpret the near-infrared emission as the illuminated surface of a nearly edge-on disk, oriented so that only the northern face is visible; the opposite surface remains hidden by the disk. We do not see infrared radiation associated directly with the star proposed to be associated with Source ''I''. The data also suggest that there is a cavity above and below the disk that is oriented perpendicular to the disk and is sculpted by the known, strong outflow from the inner disk of Source I. We compare our data to models of a protostar with a surrounding disk, envelope, and wind-blown cavity in order to elucidate the nature of the disk around Radio Source I.

Sitarski, Breann N.; Morris, Mark R.; Becklin, E. E.; Ghez, Andrea M. [Department of Physics and Astronomy, University of California, Los Angeles, 430 Portola Plaza, Los Angeles, CA 90095-1547 (United States); Lu, Jessica R. [Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822 (United States); Duchene, Gaspard [Department of Astronomy, University of California, Berkeley, C-203 Hearst Field Annex, Berkeley, CA 94720-3411 (United States); Stolte, Andrea [Argelander Institut fuer Astronomie, Universitaet Bonn, Auf dem Huegel 71, D-53121 Bonn (Germany); Zinnecker, Hans, E-mail: bsitarski@astro.ucla.edu [NASA-Ames Research Center, MS 232-12, Moffett Field, CA 94035 (United States)

2013-06-20T23:59:59.000Z

9

Titan Imagery with Keck AO during and after Probe Entry  

SciTech Connect

We present adaptive optics data from the 10-m W.M. Keck telescope that were taken during the time the Huygens probe descended through Titan's atmosphere, and on the days following touch-down. The spatial resolution of the images is typically {approx}0.04-inch, or {approx}240 km on Titan (60 km/pixel). No probe entry signal was detected at levels exceeding 0.8 {micro}Jy (3-{sigma}) per pixel (0.01-inch), which although within the range of predicted flux levels, cannot constrain any models. We present data on Titan's surface, troposphere and stratosphere during the days following probe entry, when the solar phase angle varied from 0.05{sup o} up to 0.8{sup o}, with the Sun in the West. Contrary to expectation, the data often showed the East side to be brightest. Adding data obtained with Keck and Gemini over the past few years reveals that the East-West asymmetry can be explained by a combination of the solar phase angle effect together with a general preponderance of haze on Titan's East or morning hemisphere. The troposphere was characterized by quiescent weather; only a few small clouds were present near the south pole, at typical altitudes of 30-40 km. While stratospheric haze was prominent over the northern hemisphere, tropospheric haze dominated the south, from the S. pole up to latitudes of {approx} -45{sup o}. An intriguing observation is that obtained at 1.22 {micro}m, which revealed haze in the form of a collar at -60{sup o}, in contrast to the polar haze cap as usually seen. A comparison of narrow band JHK images of Titan's surface with that obtained by Cassini ISS shows a striking resemblance in small-scale features. After a decent attempt to remove the atmosphere from the images, the surface contrast between dark and bright areas may be larger at 2 {micro}m than at 1.6 and 1.3 {micro}m. If true, this could imply that the dark areas on Titan's surface are covered by a coarser grained frost than the bright areas, and/or that there are more absorbers, such as NH{sub 3}/NH{sub 4}SH frost, in these dark areas.

de Pater, I; Adamkovics, M; Bouchez, A H; Brown, M E; Gibbard, S G; Marchis, F; Roe, H G; Schaller, E L; Young, E

2006-02-03T23:59:59.000Z

10

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

11

Hubble Space Telescope Imaging of the Optical Transient Associated with GRB970508  

E-Print Network (OSTI)

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

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

1997-10-29T23:59:59.000Z

12

A Spitzer Space Telescope Far-infrared Spectral Atlas of Compact Sources in the Magellanic Clouds. II. The Small Magellanic Cloud  

Science Journals Connector (OSTI)

We present far-infrared spectra, ? = 52-93 ?m, obtained with the Spitzer Space Telescope in the spectral energy distribution mode of its Multiband Imaging Photometer for Spitzer instrument, of a selection of luminous compact far-infrared sources in the Small Magellanic Cloud (SMC). These comprise nine young stellar objects (YSOs), the compact H II region N 81 and a similar object within N 84, and two red supergiants (RSGs). We use the spectra to constrain the presence and temperature of cool dust and the excitation conditions within the neutral and ionized gas, in the circumstellar environments and interfaces with the surrounding interstellar medium. We compare these results with those obtained in the Large Magellanic Cloud (LMC). The spectra of the sources in N 81 (of which we also show the Infrared Space Observatory-Long-wavelength Spectrograph spectrum between 50 and 170 ?m) and N 84 both display strong [O I] ?63 ?m and [O III] ?88 ?m fine-structure line emission. We attribute these lines to strong shocks and photo-ionized gas, respectively, in a "champagne flow" scenario. The nitrogen content of these two H II regions is very low, definitely N(N)/N(O) N(N)/N(O) efficiency of the photo-electric effect to heat the gas is found to be indistinguishable to that measured in the same manner in the LMC, ?0.1%-0.3%. This may result from higher cloud-core densities, or smaller grains, in the SMC. The dust associated with the two RSGs in our SMC sample is cool, and we argue that it is swept-up interstellar dust, or formed (or grew) within the bow-shock, rather than dust produced in these metal-poor RSGs themselves. Strong emission from crystalline water-ice is detected in at least one YSO. The spectra constitute a valuable resource for the planning and interpretation of observations with the Herschel Space Observatory and the Stratospheric Observatory For Infrared Astronomy.

Jacco Th. van Loon; Joana M. Oliveira; Karl D. Gordon; G. C. Sloan; C. W. Engelbracht

2010-01-01T23:59:59.000Z

13

Keck Spectroscopy of Redshift z~3 Galaxies in the Hubble Deep Field  

E-Print Network (OSTI)

We have obtained spectra with the 10-m Keck telescope of a sample of 24 galaxies having colors consistent with star-forming galaxies at redshifts 22. Combined with 5 previously confirmed high-redshift galaxies in the HDF, the 16 confirmed sources yield a comoving volume density of n>2.5^-4 h50^3 Mpc^-3 for q0=0.05, or n>1.2^-3 h50^3 Mpc^-3 for q0=0.5. These densities are comparable to estimates of the local volume density of galaxies brighter than L*, and could be almost three times higher still if all 29 of the unconfirmed candidates in our original sample are indeed also at high redshift. The galaxies are small but luminous, with half-light radii 1.8 M_B > -23. The HST images show a wide range of morphologies, including several with very close, small knots of emission embedded in wispy extended structures. Using rest-frame UV continuum fluxes with no dust correction, we calculate star formation rates in the range 7 - 24 or 3 - 9 h50^-2 Msun/yr for q0=0.05 and q0=0.5, respectively. The variety of morphologies and the high number density of z=3 galaxies in the HDF suggest that they represent a range of physical processes and stages of galaxy formation and evolution, rather than any one class of object, such as massive ellipticals. A key issue remains the measurement of masses. These high-redshift objects are likely to be the low-mass, starbursting building blocks of more massive galaxies seen today.

James D. Lowenthal; David C. Koo; Rafael Guzman; Jesus Gallego; Andrew C. Phillips; S. M. Faber; Nicole P. Vogt; Garth D. Illingworth; Caryl Gronwall

1996-12-30T23:59:59.000Z

14

W. M. Keck Center for Collaborative Neuroscience THE SPINAL CORD INJURY PROJECT  

E-Print Network (OSTI)

W. M. Keck Center for Collaborative Neuroscience THE SPINAL CORD INJURY PROJECT THE MASCIS IMPACTOR model that is used in over 100 laboratories around the world. Most of the recommended procedures

Chen, Kuang-Yu

15

KECK SPECTROSCOPY OF THE HUBBLE DEEP FIELD G.D ILLINGWORTH, J. GALLEGO, R. GUZM '  

E-Print Network (OSTI)

of elucidating the physical processes and time scales of the formation and evolution of galaxies. The Keck published paper using HST data largely from the high latitude WFPC GTO field (the ``Groth'' strip), Vogt et

16

Circumnuclear Star Clusters in the Galaxy Merger NGC 6240, Observed with Keck Adaptive Optics and HST  

SciTech Connect

We discuss images of the central {approx} 10 kpc (in projection) of the galaxy merger NGC 6240 at H and K{prime} bands, taken with the NIRC2 narrow camera on Keck II using natural guide star adaptive optics. We detect 28 star clusters in the NIRC2 images, of which only 7 can be seen in the similar-spatial-resolution, archival WFPC2 Planetary Camera data at either B or I bands. Combining the NIRC2 narrow camera pointings with wider NICMOS NIC2 images taken with the F110W, F160W, and F222M filters, we identify a total of 32 clusters that are detected in at least one of these 5 infrared ({lambda}{sub c} > 1 {micro}m) bandpasses. By comparing to instantaneous burst, stellar population synthesis models (Bruzual & Charlot 2003), we estimate that most of the clusters are consistent with being {approx} 15 Myr old and have photometric masses ranging from 7 x 10{sup 5} M{sub {circle_dot}} to 4 x 10{sup 7}M{sub {circle_dot}}. The total contribution to the star formation rate (SFR) from these clusters is approximately 10M{sub {circle_dot}} yr{sup -1}, or {approx} 10% of the total SFR in the nuclear region. We use these newly discovered clusters to estimate the extinction toward NGC 6240's double nuclei, and find values of A{sub v} as high as 14 magnitudes along some sightlines, with an average extinction of A{sub v} {approx} 7 mag toward sightlines within {approx} 3-inches of the double nuclei.

Pollack, L K; Max, C E; Schneider, G

2007-02-12T23:59:59.000Z

17

THE CIRCUMNUCLEAR STAR FORMATION ENVIRONMENT OF NGC 6946: Br ? AND H{sub 2} RESULTS FROM KECK INTEGRAL FIELD SPECTROSCOPY  

SciTech Connect

We present a three-dimensional data cube of the K-band continuum and the Br ?, H{sub 2} S(0), and S(1) lines within the central 18.''5 × 13.''8 (520 pc × 390 pc) region of NGC 6946. Data were obtained using OSIRIS, a near-infrared Integral Field Spectrograph at Keck Observatory, with Laser Guide Star Adaptive Optics. The 0.''3 resolution allows us to investigate the stellar bulge and the forming star clusters in the nuclear region on 10 pc scales. We detect giant H II regions associated with massive young star clusters in the nuclear spiral/ring (R ? 30 pc) and in the principal shocks along the nuclear bar. Comparisons of the Br ? fluxes with Pa ? line emission and radio continuum indicate A{sub K} ? 3, A{sub V} ? 25 for the nuclear star-forming regions. The most luminous H II regions are restricted to within 70 pc of the center, despite the presence of high gas columns at larger radii (R ? 200 pc). H{sub 2} emission is restricted to clouds within R ? 60 pc of the center, resembling the distribution of HCN line emission. We propose that gas-assisted migration of the young star clusters is contributing to the buildup of the nuclear bar and nuclear star cluster (R < 30 pc) in this galaxy.

Tsai, Chao-Wei [Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125 (United States); Turner, Jean L. [Department of Physics and Astronomy, UCLA, Los Angeles, CA 90095-1547 (United States); Beck, Sara C. [Department of Physics and Astronomy, Tel Aviv University, Ramat Aviv (Israel); Meier, David S. [Department of Physics, New Mexico Institute of Mining and Technology, Socorro, NM 87801 (United States); Wright, Shelley A., E-mail: Chao-Wei.Tsai@jpl.nasa.gov [Dunlap Institute for Astronomy and Astrophysics, University of Toronto, Toronto, Ontario (Canada)

2013-10-20T23:59:59.000Z

18

W. M. Keck Center for Collaborative Neuroscience THE SPINAL CORD INJURY PROJECT  

E-Print Network (OSTI)

W. M. Keck Center for Collaborative Neuroscience THE SPINAL CORD INJURY PROJECT WORKSHOP Liberty International, EWR, is the closest airport.) Transportation from airport to hotel arranged Newark Liberty International Airport (EWR) · State Shuttle. Call 1-800-427-3207 for reservations. #12

Chen, Kuang-Yu

19

W. M. Keck Center for Collaborative Neuroscience THE SPINAL CORD INJURY PROJECT  

E-Print Network (OSTI)

W. M. Keck Center for Collaborative Neuroscience THE SPINAL CORD INJURY PROJECT WORKSHOP in registration. #12;Transportation from Newark Liberty International Airport (EWR) State Shuttle. Cost is $56.) Animal Contact Form returned. Hotel reservations made Travel plans made. (Newark Liberty International

Chen, Kuang-Yu

20

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

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.


21

The Cherenkov Telescope Array Large Size Telescope  

E-Print Network (OSTI)

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

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

2013-01-01T23:59:59.000Z

22

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 - ,

23

CHARACTERIZING THE ORBITAL AND DYNAMICAL STATE OF THE HD 82943 PLANETARY SYSTEM WITH KECK RADIAL VELOCITY DATA  

SciTech Connect

We present an updated analysis of radial velocity data of the HD 82943 planetary system based on 10 yr of measurements obtained with the Keck telescope. Previous studies have shown that the HD 82943 system has two planets that are likely in 2:1 mean-motion resonance (MMR), with orbital periods about 220 and 440 days. However, alternative fits that are qualitatively different have also been suggested, with two planets in a 1:1 resonance or three planets in a Laplace 4:2:1 resonance. Here we use ?{sup 2} minimization combined with a parameter grid search to investigate the orbital parameters and dynamical states of the qualitatively different types of fits, and we compare the results to those obtained with the differential evolution Markov chain Monte Carlo method. Our results support the coplanar 2:1 MMR configuration for the HD 82943 system, and show no evidence for either the 1:1 or three-planet Laplace resonance fits. The inclination of the system with respect to the sky plane is well constrained at 20{sup +4.9}{sub -5.5} degrees, and the system contains two planets with masses of about 4.78 M{sub J} and 4.80 M{sub J} (where M{sub J} is the mass of Jupiter) and orbital periods of about 219 and 442 days for the inner and outer planet, respectively. The best fit is dynamically stable with both eccentricity-type resonant angles ?{sub 1} and ?{sub 2} librating around 0°.

Tan, Xianyu; Lee, Man Hoi [Department of Earth Sciences, The University of Hong Kong, Pokfulam Road, Hong Kong (China); Payne, Matthew J.; Ford, Eric B. [Department of Astronomy, University of Florida, FL 32611-2055 (United States); Howard, Andrew W. [Institute for Astronomy, University of Hawaii at Manoa, 2680 Woodlawn Drive, Honolulu, HI 96822 (United States); Johnson, John A. [Department of Planetary Sciences, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125 (United States); Marcy, Geoff W. [Department of Astronomy, University of California, Berkeley, CA 94720-3411 (United States); Wright, Jason T., E-mail: xianyut@lpl.arizona.edu [Department of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802 (United States)

2013-11-10T23:59:59.000Z

24

CONTAMINATION OF BROADBAND PHOTOMETRY BY NEBULAR EMISSION IN HIGH-REDSHIFT GALAXIES: INVESTIGATIONS WITH KECK'S MOSFIRE NEAR-INFRARED SPECTROGRAPH  

SciTech Connect

Earlier work has raised the potential importance of nebular emission in the derivation of the physical characteristics of high-redshift Lyman break galaxies. Within certain redshift ranges, and especially at z ? 6-7, such lines may be strong enough to reduce estimates of the stellar masses and ages of galaxies compared with those derived assuming the broadband photometry represents stellar light alone. To test this hypothesis at the highest redshifts where such lines can be probed with ground-based facilities, we examine the near-infrared spectra of a representative sample of 28 3.0 < z < 3.8 Lyman break galaxies using the newly commissioned MOSFIRE near-infrared spectrograph at the Keck I telescope. We use these data to derive the rest-frame equivalent widths (EWs) of [O III] emission and show that these are comparable with estimates derived using the spectral energy distribution (SED) fitting technique introduced for sources of known redshift by Stark et al. Although our current sample is modest, its [O III] EW distribution is consistent with that inferred for H? based on SED fitting of Stark et al.'s larger sample of 3.8 < z < 5 galaxies. For a subset of survey galaxies, we use the combination of optical and near-infrared spectroscopy to quantify kinematics of outflows in z ? 3.5 star-forming galaxies and discuss the implications for reionization measurements. The trends we uncover underline the dangers of relying purely on broadband photometry to estimate the physical properties of high-redshift galaxies and emphasize the important role of diagnostic spectroscopy.

Schenker, Matthew A; Ellis, Richard S; Konidaris, Nick P [Department of Astrophysics, California Institute of Technology, MC 249-17, Pasadena, CA 91125 (United States); Stark, Daniel P, E-mail: schenker@astro.caltech.edu [Department of Astronomy and Steward Observatory, University of Arizona, Tucson, AZ 85721 (United States)

2013-11-01T23:59:59.000Z

25

In Space Telescopes and Instruments V, Bely & Breckinridge, eds., Proc. SPIE 3356, Kona, HI, March 1998. A Phase Diversity Experiment to Measure Piston Misalignment on  

E-Print Network (OSTI)

1998. A Phase Diversity Experiment to Measure Piston Misalignment on the Segmented Primary Mirror of an experiment to measure piston errors on the Keck II primary segmented mirror, through atmospheric turbulence, using phase­diverse phase retrieval. The segment piston errorss are separated from the random turbulence

Löfdahl, Mats

26

A DUSTY Mg II ABSORBER ASSOCIATED WITH THE QUASAR SDSS J003545.13+011441.2  

SciTech Connect

We report on a dusty Mg II absorber associated with the quasar SDSS J003545.13+011441.2 (hereafter J0035+0114) at z = 1.5501, the strongest of the three Mg II absorbers along the sight line of the quasar. The two low-redshift intervening absorbers are at z = 0.7436 and 0.5436. Based on the photometric and spectroscopic data of the Sloan Digital Sky Survey (SDSS), we infer that the rest-frame color excess E(B - V) due to the associated dust is more than 0.07 by assuming a Small Magellanic Cloud (SMC) type extinction curve. Our follow-up moderate resolution spectroscopic observation with the ESI spectrometer at the 10 m Keck telescope enables us to reliably identify most of the important metal elements, such as Zn, Fe, Mn, Mg, Al, Si, Cr, and Ni, in the associated system. We measure the column density of each species and detect significant dust depletion. In addition, we develop a simulation technique to gauge the significance of a 2175 A dust absorption bump in the SDSS quasar spectra. By using this technique, we analyze the SDSS spectrum of J0035+0114 for the presence of an associated 2175 A extinction feature and report a tentative detection at a {approx}2{sigma} significant level.

Jiang, P.; Lu, H. L.; Zhou, H. Y. [Key Laboratory for Research in Galaxies and Cosmology, University of Science and Technology of China, Chinese Academy of Sciences, Hefei, Anhui, 230026 (China); Ge, J. [Astronomy Department, University of Florida, 211 Bryant Space Science Center, P. O. Box 112055, Gainesville, FL 32611 (United States); Prochaska, J. X. [University of California Observatories-Lick Observatory, University of California, Santa Cruz, CA 95064 (United States); Kulkarni, V. P., E-mail: jpaty@mail.ustc.edu.c [Department of Physics and Astronomy, University of South Carolina, Columbia, SC 29208 (United States)

2010-09-01T23:59:59.000Z

27

Ca II H and K Chromospheric Emission Lines in Late K and M Dwarfs  

E-Print Network (OSTI)

We have measured the profiles of the Ca II H and K chromospheric emission lines in 147 main sequence stars of spectral type M5-K7 (0.30-0.55 solar masses) using multiple high resolution spectra obtained during six years with the HIRES spectrometer on the Keck 1 telescope. Remarkably, the average FWHM, equivalent widths, and line luminosities of Ca II H and K increase by a factor of 3 with increasing stellar mass over this small range of stellar masses. We fit the H and K lines with a double Gaussian model to represent both the chromospheric emission and the non-LTE central absorption. Most of the sample stars display a central absorption that is typically redshifted by ~0.1 km/s relative to the emission, but the nature of this velocity gradient remains unknown. The FWHM of the H and K lines increase with stellar luminosity, reminiscent of the Wilson-Bappu effect in FGK-type stars. Both the equivalent widths and FWHM exhibit modest temporal variability in individual stars. At a given value of M_v, stars exhibit a spread in both the equivalent width and FWHM of Ca II H and K, due both to a spread in fundamental stellar parameters including rotation rate, age, and possibly metallicity, and to the spread in stellar mass at a given M_v. The K line is consistently wider than the H line, as expected, and its central absorption is more redshifted, indicating that the H and K lines form at slightly different heights in the chromosphere where the velocities are slightly different. The equivalent width of H-alpha correlates with Ca II H and K only for stars having Ca II equivalent widths above ~2 angstroms, suggesting the existence of a magnetic threshold above which the lower and upper chromospheres become thermally coupled.

Emily Rauscher; Geoffrey W. Marcy

2006-02-14T23:59:59.000Z

28

Alignment telescope for Antares  

SciTech Connect

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

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

1983-01-01T23:59:59.000Z

29

Three-Mirror Anastigmat Telescope with an Unvignetted Flat Focal Plane  

Science Journals Connector (OSTI)

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

Kyoji Nariai; Masanori Iye

2005-04-25T23:59:59.000Z

30

Upgrade of the MAGIC telescopes  

E-Print Network (OSTI)

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

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

2014-01-01T23:59:59.000Z

31

High Energy Neutrino Telescopes  

E-Print Network (OSTI)

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

Hoffman, K D

2008-01-01T23:59:59.000Z

32

High Energy Neutrino Telescopes  

E-Print Network (OSTI)

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

K. D. Hoffman

2008-12-18T23:59:59.000Z

33

Space Telescope Programs Hubble Observatory  

E-Print Network (OSTI)

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

Colorado at Boulder, University of

34

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

35

MASSIVE AND NEWLY DEAD: DISCOVERY OF A SIGNIFICANT POPULATION OF GALAXIES WITH HIGH-VELOCITY DISPERSIONS AND STRONG BALMER LINES AT z {approx} 1.5 FROM DEEP KECK SPECTRA AND HST/WFC3 IMAGING  

SciTech Connect

We present deep Keck/LRIS spectroscopy and Hubble Space Telescope/WFC3 imaging in the rest-frame optical for a sample of eight galaxies at z {approx} 1.5 with high photometrically determined stellar masses. The data are combined with five Very Large Telescope/X-Shooter spectra. We find that these 13 galaxies have high velocity dispersions, with a median of {sigma} = 301 km s{sup -1}. This high value is consistent with their relatively high stellar masses and compact sizes. We study their stellar populations using the strength of Balmer absorption lines, which are not sensitive to dust absorption. We find a large range in Balmer absorption strength, with many galaxies showing very strong lines indicating young ages. The median H{delta}{sub A} equivalent width, determined directly or inferred from the H10 line, is 5.4 A, indicating a luminosity-weighted age of {approx}1 Gyr. Although this value may be biased toward higher values because of selection effects, high-dispersion galaxies with such young ages are extremely rare in the local universe. Interestingly, we do not find a simple correlation with rest-frame U - V color: some of the reddest galaxies have very strong Balmer absorption lines, which may indicate the importance of multiple bursts of star formation. These results demonstrate that many high-dispersion galaxies at z {approx} 1.5 were recently quenched. This implies that there must be a population of star-forming progenitors at z {approx} 2 with high velocity dispersions or linewidths, which are notoriously absent from CO/H{alpha} selected surveys.

Bezanson, Rachel; Van Dokkum, Pieter [Department of Astronomy, Yale University, New Haven, CT 06520-8101 (United States); Van de Sande, Jesse; Franx, Marijn [Sterrewacht Leiden, Leiden University, NL-2300 RA Leiden (Netherlands); Kriek, Mariska [Department of Astronomy, University of California, Berkeley, CA 94720 (United States)

2013-02-10T23:59:59.000Z

36

Wide field of view telescope  

DOE Patents (OSTI)

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

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

2008-01-15T23:59:59.000Z

37

Neutrino telescopes in the World  

SciTech Connect

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

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

2007-01-12T23:59:59.000Z

38

FIRST KECK NULLING OBSERVATIONS OF A YOUNG STELLAR OBJECT: PROBING THE CIRCUMSTELLAR ENVIRONMENT OF THE HERBIG Ae STAR MWC 325  

SciTech Connect

We present the first N-band nulling plus K- and L-band V{sup 2} observations of a young stellar object, MWC 325, taken with the 85 m baseline Keck Interferometer. The Keck nuller was designed for the study of faint dust signatures associated with debris disks, but it also has a unique capability for studying the temperature and density distribution of denser disks found around young stellar objects. Interferometric observations of MWC 325 at K, L, and N encompass a factor of five in spectral range and thus, especially when spectrally dispersed within each band, enable characterization of the structure of the inner disk regions where planets form. Fitting our observations with geometric models such as a uniform disk or a Gaussian disk show that the apparent size increases monotonically with wavelength in the 2-12 {mu}m wavelength region, confirming the widely held assumption based on radiative transfer models, now with spatially resolved measurements over a broad wavelength range, that disks are extended with a temperature gradient. The effective size is a factor of about 1.4 and 2.2 larger in the L band and N band, respectively, compared to that in the K band. The existing interferometric measurements and the spectral energy distribution can be reproduced by a flat disk or a weakly shadowed nearly flat disk model, with only slight flaring in the outer regions of the disk, consisting of representative 'sub-micron' (0.1 {mu}m) and 'micron' (2 {mu}m) grains of a 50:50 ratio of silicate and graphite. This is in marked contrast to the disks previously found in other Herbig Ae/Be stars, suggesting a wide variety in the disk properties among Herbig Ae/Be stars.

Ragland, S.; Hrynevich, M. [W. M. Keck Observatory, Kamuela, HI 96743 (United States); Ohnaka, K. [Max-Planck-Institut fuer Radioastronomie, 53121 Bonn (Germany); Hillenbrand, L. [Astrophysics Department, California Institute of Technology, Pasadena, CA 91125 (United States); Ridgway, S. T. [National Optical Astronomy Observatories, Tucson, AZ 85726-6732 (United States); Colavita, M. M.; Traub, W. A. [Jet Propulsion Laboratory, California Institute of Technology, Pasadena CA, 91109 (United States); Akeson, R. L.; Millan-Gabet, R. [NExScI, California Institute of Technology, Pasadena, CA 91125 (United States); Cotton, W. [National Radio Astronomy Observatory, Charlottesville, VA 22903-2475 (United States); Danchi, W. C., E-mail: sragland@keck.hawaii.edu [NASA Goddard Space Flight Center, Exoplanets and Stellar Astrophysics, Greenbelt, MD 20771 (United States)

2012-02-20T23:59:59.000Z

39

THE OPTIMAL GRAVITATIONAL LENS TELESCOPE  

SciTech Connect

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

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

2010-05-15T23:59:59.000Z

40

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

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41

Large aperture diffractive space telescope  

DOE Patents (OSTI)

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

Hyde, Roderick A. (Livermore, CA)

2001-01-01T23:59:59.000Z

42

The UCSD HIRES/KECK I Damped Lya Abundance Database: IV. Probing Galactic Enrichment Histories with Nitrogen  

E-Print Network (OSTI)

We present 14 N^0 measurements from our HIRES/Keck database of damped Lya abundances. These data are combined with measurements from the recent and past literature to build an homogeneous, uniform set of observations. We examine photoionization diagnostics like Fe^++ and Ar^0 in the majority of the complete sample and assess the impact of ionization corrections on N/alpha and alpha/H values derived from observed ionic column densities of N^0, Si^+, H^0, and S^+. Our final sample of 19 N/alpha, alpha/H pairs appears bimodal; the majority of systems show N/alpha values consistent with metal-poor emission regions in the local universe but a small sub-sample exhibit significantly lower N/alpha ratios. Contrary to previous studies of N/alpha in the damped systems, our sample shows little scatter within each sub-sample. We consider various scenarios to explain the presence of the low N/alpha sightlines and account for the apparent bimodality. We favor a model where at least some galaxies undergo an initial burst of star formation with suppressed formation of intermediate-mass stars. We found a power-law IMF with slope 0.10 or a mass cut of ~5-8 Msolar would successfully reproduce the observed LN-DLA values. If the bimodal distribution is confirmed by a larger sample of measurements, this may present the first observational evidence for a top heavy initial mass function in some early stellar populations.

Jason X. Prochaska; Richard B. C. Henry; John M. O'Meara; David Tytler; Arthur M. Wolfe; David Kirkman; Dan Lubin; Nao Suzuki

2002-06-17T23:59:59.000Z

43

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

Energy Savers (EERE)

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

44

General surface equations for glancing incidence telescopes  

Science Journals Connector (OSTI)

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

Saha, Timo T

1987-01-01T23:59:59.000Z

45

Absolute calibration of imaging atmospheric Cherenkov telescopes  

E-Print Network (OSTI)

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

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

2005-07-04T23:59:59.000Z

46

Mapping Large-Scale Gaseous Outflows in Ultraluminous Galaxies with Keck II ESI Spectra: Variations in Outflow Velocity with Galactic Mass  

E-Print Network (OSTI)

Measurements of interstellar absorption lines in 18 ultraluminous infrared galaxies (ULIGs) have been combined with published data, in order to reassess the dependence of galactic outflow speeds on starburst luminosity and galactic mass. The Doppler shifts reveal outflows of relatively cool gas at $330 \\pm 100$km/s. The outflow speeds increase with the star formation rate (SFR) as roughly $v \\propto SFR^{0.35}$. This result is surprising since, in the traditional model for starburst-driven winds, these relatively cool gas clouds are accelerated by the ram pressure of a hot, supernova-heated wind that exhibits weak (if any) \\x temperature variation with increasing galactic mass. The lack of evidence for much hotter winds is partly a sensitivity issue; but the outflow velocities in ultraluminous starbursts actually are consistent with acceleration by the tepid wind, indicating a hotter component is unlikely to dominate the momentum flux. The \

Crystal L. Martin

2004-10-09T23:59:59.000Z

47

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

E-Print Network (OSTI)

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

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

2013-01-01T23:59:59.000Z

48

Simulation of the Simbol-X Telescope  

SciTech Connect

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

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

2009-05-11T23:59:59.000Z

49

Telescopic nanotube device for hot nanolithography  

DOE Patents (OSTI)

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

Popescu, Adrian; Woods, Lilia M

2014-12-30T23:59:59.000Z

50

Multimessenger astronomy with the Einstein Telescope  

E-Print Network (OSTI)

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

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

2010-04-12T23:59:59.000Z

51

4 m Davies-Cotton telescope for the Cherenkov Telescope Array  

E-Print Network (OSTI)

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

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

2013-01-01T23:59:59.000Z

52

Optical Technology Needs for Future Space Telescopes  

E-Print Network (OSTI)

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

Van Stryland, Eric

53

Pendular seismometer for correcting telescope vibrations  

Science Journals Connector (OSTI)

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

A. Tokovinin

2000-08-11T23:59:59.000Z

54

The High Energy Telescope on EXIST  

E-Print Network (OSTI)

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

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

2009-01-01T23:59:59.000Z

55

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

E-Print Network (OSTI)

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

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

2014-01-01T23:59:59.000Z

56

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

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

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

57

Large-Aperture Segmented Mirror Telescope Design Concept  

E-Print Network (OSTI)

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

Sirianni, Marco

58

Telescoping MATLAB for DSP Applications PhD Thesis Defense  

E-Print Network (OSTI)

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

Chauhan, Arun

59

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

SciTech Connect

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

60

Telescoping magnetic ball bar test gage  

DOE Patents (OSTI)

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

Bryan, J.B.

1982-03-15T23:59:59.000Z

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

Telescoping magnetic ball bar test gage  

DOE Patents (OSTI)

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

Bryan, James B. (Pleasanton, CA)

1984-01-01T23:59:59.000Z

62

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

SciTech Connect

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

Cameron, Robert A.

2012-06-28T23:59:59.000Z

63

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

E-Print Network (OSTI)

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

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

2013-01-01T23:59:59.000Z

64

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

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

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

65

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

E-Print Network (OSTI)

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

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

2013-07-18T23:59:59.000Z

66

ANTARES deep sea neutrino telescope results  

SciTech Connect

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

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

2014-06-24T23:59:59.000Z

67

LOFAR, a new low frequency radio telescope  

E-Print Network (OSTI)

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

H. J. A. Rottgering

2003-09-19T23:59:59.000Z

68

HALO GAS AND GALAXY DISK KINEMATICS DERIVED FROM OBSERVATIONS AND LAMBDACDM SIMULATIONS OF Mg II ABSORPTION-SELECTED GALAXIES AT INTERMEDIATE REDSHIFT  

SciTech Connect

We obtained ESI/Keck rotation curves of 10 Mg II absorption-selected galaxies (0.3 <= z <= 1.0) for which we have WFPC-2/HST images and high-resolution HIRES/Keck and UVES/VLT quasar spectra of the Mg II absorption profiles. We perform a kinematic comparison of these galaxies and their associated halo Mg II absorption. For all 10 galaxies, the majority of the absorption velocities lie in the range of the observed galaxy rotation velocities. In 7/10 cases, the absorption velocities reside fully to one side of the galaxy systemic velocity and usually align with one arm of the rotation curve. In all cases, a constant rotating thick-disk model poorly reproduces the full spread of observed Mg II absorption velocities when reasonably realistic parameters are employed. In 2/10 cases, the galaxy kinematics, star formation surface densities, and absorption kinematics have a resemblance to those of high-redshift galaxies showing strong outflows. We find that Mg II absorption velocity spread and optical depth distribution may be dependent on galaxy inclination. To further aid in the spatial-kinematic relationships of the data, we apply quasar absorption-line techniques to a galaxy (v{sub c} = 180 km s{sup -1}) embedded in LAMBDACDM simulations. In the simulations, Mg II absorption selects metal-enriched 'halo' gas out to {approx}100 kpc from the galaxy, tidal streams, filaments, and small satellite galaxies. Within the limitations inherent in the simulations, the majority of the simulated Mg II absorption arises in the filaments and tidal streams and is infalling toward the galaxy with velocities between -200 km s{sup -1} <= v{sub r} <= -180 km s{sup -1}. The Mg II absorption velocity offset distribution (relative to the simulated galaxy) spans {approx}200 km s{sup -1} with the lowest frequency of detecting Mg II at the galaxy systematic velocity.

Kacprzak, Glenn G.; Murphy, Michael T. [Swinburne University of Technology, Victoria 3122 (Australia); Churchill, Christopher W.; Ceverino, Daniel; Klypin, Anatoly [New Mexico State University, Las Cruces, NM 88003 (United States); Steidel, Charles C., E-mail: gkacprzak@astro.swin.edu.a, E-mail: mmurphy@astro.swin.edu.a, E-mail: cwc@nmsu.ed, E-mail: ceverino@nmsu.ed, E-mail: aklypin@nmsu.ed, E-mail: ceverino@phys.huji.ac.i, E-mail: ccs@astro.caltech.ed [California Institute of Technology, Pasadena, CA 91125 (United States)

2010-03-10T23:59:59.000Z

69

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

E-Print Network (OSTI)

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

Sirianni, Marco

70

AGN Physics with the Cherenkov Telescope Array  

E-Print Network (OSTI)

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

Zech, A

2012-01-01T23:59:59.000Z

71

Fermi Large Area Telescope Third Source Catalog  

E-Print Network (OSTI)

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

,

2015-01-01T23:59:59.000Z

72

The X-ray Telescope of CAST  

E-Print Network (OSTI)

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

M. Kuster; H. Bräuninger; S. Cébrian; M. Davenport; C. Elefteriadis; J. Englhauser; H. Fischer; J. Franz; P. Friedrich; R. Hartmann; F. H. Heinsius; D. H. H. Hoffmann; G. Hoffmeister; J. N. Joux; D. Kang; K. Königsmann; R. Kotthaus; T. Papaevangelou; C. Lasseur; A. Lippitsch; G. Lutz; J. Morales; A. Rodríguez; L. Strüder; J. Vogel; K. Zioutas

2007-05-10T23:59:59.000Z

73

Integral Field Spectroscopy with the Gemini 8-m Telescopes  

E-Print Network (OSTI)

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

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

2002-03-20T23:59:59.000Z

74

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

75

Photosystem II  

ScienceCinema (OSTI)

James Barber, Ernst Chain Professor of Biochemistry at Imperial College, London, gives a BSA Distinguished Lecture titled, "The Structure and Function of Photosystem II: The Water-Splitting Enzyme of Photosynthesis."

James Barber

2010-09-01T23:59:59.000Z

76

The Robotic Super-LOTIS Telescope: Results & Future Plans  

E-Print Network (OSTI)

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

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

2008-02-29T23:59:59.000Z

77

Automation of the design of a telescopic zoom system  

Science Journals Connector (OSTI)

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

Van Luen, Nguen

2013-01-01T23:59:59.000Z

78

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

E-Print Network (OSTI)

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

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

2011-01-01T23:59:59.000Z

79

TECHNOLOGY DEVELOPMENT PROJECT PLAN Advanced Technology Large Aperture Space Telescope  

E-Print Network (OSTI)

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

Sirianni, Marco

80

THE CHERENKOV TELESCOPE ARRAY for the CTA Consortium  

E-Print Network (OSTI)

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

Boyer, Edmond

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.


81

Muon Telescope By Nandita Sampath and Izzy Harrison  

E-Print Network (OSTI)

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

California at Santa Cruz, University of

82

Atmospheric dispersion in very large telescopes with adaptive optics  

Science Journals Connector (OSTI)

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

Charles G. Wynne

1997-02-11T23:59:59.000Z

83

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

E-Print Network (OSTI)

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

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

2013-01-01T23:59:59.000Z

84

Metal multilayer mirrors for EUV wide field telescopes  

SciTech Connect

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

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

1989-01-01T23:59:59.000Z

85

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

E-Print Network (OSTI)

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

86

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

E-Print Network (OSTI)

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

87

Real-time condition assessment of RAPTOR telescope systems  

SciTech Connect

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

88

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

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

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

89

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

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

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

90

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

91

Minimizing high spatial frequency residual in active space telescope mirrors  

E-Print Network (OSTI)

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

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

2008-01-01T23:59:59.000Z

92

Cross section dependence of event rates at neutrino telescopes  

E-Print Network (OSTI)

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

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

2006-10-20T23:59:59.000Z

93

An Australian Icon - Planning and Construction of the Parkes Telescope  

E-Print Network (OSTI)

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

Robertson, Peter

2012-01-01T23:59:59.000Z

94

The next generation Cherenkov Telescope Array observatory: CTA  

E-Print Network (OSTI)

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

Vercellone, Stefano

2014-01-01T23:59:59.000Z

95

3D acoustic imaging applied to the Baikal Neutrino Telescope  

E-Print Network (OSTI)

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

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

2008-11-07T23:59:59.000Z

96

The next generation Cherenkov Telescope Array observatory: CTA  

Science Journals Connector (OSTI)

Abstract The Cherenkov Telescope Array (CTA) is a large collaborative effort aimed at the design and operation of an observatory dedicated to the very high-energy gamma-ray astrophysics in the energy range 30 GeV–100 TeV, which will improve by about one order of magnitude the sensitivity with respect to the current major arrays (H.E.S.S., MAGIC, and VERITAS). In order to achieve such improved performance, for both the northern and southern CTA sites, four units of 23 m diameter Large Size Telescopes (LSTs) will be deployed close to the centre of the array with telescopes separated by about 100 m. A larger number (about 25 units) of 12 m Medium Size Telescopes (MSTs, separated by about 150 m), will cover a larger area. The southern site will also include up to 24 Schwarzschild–Couder dual-mirror medium-size Telescopes (SCTs) with the primary mirror diameter of 9.5 m. Above a few TeV, the Cherenkov light intensity is such that showers can be detected even well outside the light pool by telescopes significantly smaller than the MSTs. To achieve the required sensitivity at high energies, a huge area on the ground needs to be covered by Small Size Telescopes (SSTs) with a field of view of about 10° and an angular resolution of about 0.2°, making the dual-mirror configuration very effective. The SST sub-array will be composed of 50–70 telescopes with a mirror area of about 5–10 m2 and about 300 m spacing, distributed across an area of about 10 km2. In this presentation we will focus on the innovative solution for the optical design of the medium and small size telescopes based on a dual-mirror configuration. This layout will allow us to reduce the dimension and the weight of the camera at the focal plane of the telescope, to adopt Silicon-based photo-multipliers as light detectors thanks to the reduced plate-scale, and to have an optimal imaging resolution on a wide field of view.

S. Vercellone

2014-01-01T23:59:59.000Z

97

Cryogenic optical performance of the ASTRO-F SiC telescope  

Science Journals Connector (OSTI)

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

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

2005-01-01T23:59:59.000Z

98

Advanced Dark Energy Physics Telescope (ADEPT)  

SciTech Connect

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

Charles L. Bennett

2009-03-26T23:59:59.000Z

99

Summary of One Year Operation of the EUDET CMOS Pixel Telescope  

E-Print Network (OSTI)

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

Ingrid-Maria Gregor

2009-01-06T23:59:59.000Z

100

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

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

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

E-Print Network (OSTI)

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

Jarrett, Thomas H.

102

NEWLY IDENTIFIED EXTENDED GREEN OBJECTS (EGOs) FROM THE SPITZER GLIMPSE II SURVEY. II. MOLECULAR CLOUD ENVIRONMENTS  

SciTech Connect

We have undertaken a survey of molecular lines in the 3 mm band toward 57 young stellar objects using the Australia Telescope National Facility Mopra 22 m radio telescope. The target sources were young stellar objects with active outflows (extended green objects (EGOs)) newly identified from the GLIMPSE II survey. We observe a high detection rate (50%) of broad line wing emission in the HNC and CS thermal lines, which combined with the high detection rate of class I methanol masers toward these sources (reported in Paper I) further demonstrates that the GLIMPSE II EGOs are associated with outflows. The physical and kinematic characteristics derived from the 3 mm molecular lines for these newly identified EGOs are consistent with these sources being massive young stellar objects with ongoing outflow activity and rapid accretion. These findings support our previous investigations of the mid-infrared properties of these sources and their association with other star formation tracers (e.g., infrared dark clouds, methanol masers and millimeter dust sources) presented in Paper I. The high detection rate (64%) of the hot core tracer CH{sub 3}CN reveals that the majority of these new EGOs have evolved to the hot molecular core stage. Comparison of the observed molecular column densities with predictions from hot core chemistry models reveals that the newly identified EGOs from the GLIMPSE II survey are members of the youngest hot core population, with an evolutionary time scale of the order of 10{sup 3} yr.

Chen Xi; Gan Conggui; Shen Zhiqiang [Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030 (China); Ellingsen, Simon P.; Titmarsh, Anita [School of Mathematics and Physics, University of Tasmania, Hobart, Tasmania (Australia); He Jinhua, E-mail: chenxi@shao.ac.cn [Key Laboratory for the Structure and Evolution of Celestial Objects, Yunnan Astronomical Observatory/National Astronomical Observatory, Chinese Academy of Sciences, P.O. Box 110, Kunming 650011, Yunnan Province (China)

2013-06-01T23:59:59.000Z

103

The Hubble Space Telescope Cluster Supernova Survey. V. Improving the Dark-energy Constraints above z > 1 and Building an Early-type-hosted Supernova Sample  

Science Journals Connector (OSTI)

We present Advanced Camera for Surveys, NICMOS, and Keck adaptive-optics-assisted photometry of 20 Type Ia supernovae (SNe Ia) from the Hubble Space Telescope (HST) Cluster Supernova Survey. The SNe Ia were discovered over the redshift interval 0.623 z z = 1, thereby nearly doubling the statistical weight of HST-discovered SNe Ia beyond this redshift. Our detailed analysis corrects for the recently identified correlation between SN Ia luminosity and host galaxy mass and corrects the NICMOS zero point at the count rates appropriate for very distant SNe Ia. Adding these SNe improves the best combined constraint on dark-energy density, ?DE(z), at redshifts 1.0 z ? = 0.729 ± 0.014 (68% confidence level (CL) including systematic errors). For a flat wCDM model, we measure a constant dark-energy equation-of-state parameter w = –1.013+0.068 –0.073 (68% CL). Curvature is constrained to ?0.7% in the owCDM model and to ?2% in a model in which dark energy is allowed to vary with parameters w 0 and wa . Further tightening the constraints on the time evolution of dark energy will require several improvements, including high-quality multi-passband photometry of a sample of several dozen z > 1 SNe Ia. We describe how such a sample could be efficiently obtained by targeting cluster fields with WFC3 on board HST. The updated supernova Union2.1 compilation of 580 SNe is available at http://supernova.lbl.gov/Union.

N. Suzuki; D. Rubin; C. Lidman; G. Aldering; R. Amanullah; K. Barbary; L. F. Barrientos; J. Botyanszki; M. Brodwin; N. Connolly; K. S. Dawson; A. Dey; M. Doi; M. Donahue; S. Deustua; P. Eisenhardt; E. Ellingson; L. Faccioli; V. Fadeyev; H. K. Fakhouri; A. S. Fruchter; D. G. Gilbank; M. D. Gladders; G. Goldhaber; A. H. Gonzalez; A. Goobar; A. Gude; T. Hattori; H. Hoekstra; E. Hsiao; X. Huang; Y. Ihara; M. J. Jee; D. Johnston; N. Kashikawa; B. Koester; K. Konishi; M. Kowalski; E. V. Linder; L. Lubin; J. Melbourne; J. Meyers; T. Morokuma; F. Munshi; C. Mullis; T. Oda; N. Panagia; S. Perlmutter; M. Postman; T. Pritchard; J. Rhodes; P. Ripoche; P. Rosati; D. J. Schlegel; A. Spadafora; S. A. Stanford; V. Stanishev; D. Stern; M. Strovink; N. Takanashi; K. Tokita; M. Wagner; L. Wang; N. Yasuda; H. K. C. Yee; The Supernova Cosmology Project

2012-01-01T23:59:59.000Z

104

Fine tracking system for balloon-borne telescopes  

E-Print Network (OSTI)

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

Ricci, M; Lorenzetti, D

2011-01-01T23:59:59.000Z

105

The Atmospheric Monitoring Strategy for the Cherenkov Telescope Array  

E-Print Network (OSTI)

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

Daniel, M K

2015-01-01T23:59:59.000Z

106

A WFI survey in the Chamaeleon II dark cloud  

E-Print Network (OSTI)

We present the results of an optical multi-band survey for low-mass Pre-Main Sequence (PMS) stars and young Brown Dwarfs (BDs) in the Chamaeleon II (Cha II) dark cloud. This survey constitutes the complementary optical data to the c2d Spitzer Legacy survey in Cha II. Using the Wide-Field Imager (WFI) at the ESO 2.2m telescope, we surveyed a sky area of about 1.75 square degrees in Cha II. The region was observed in the Rc, Ic and z broad-bands, in H-alpha and in two medium-band filters centered at 856 and 914 nm. We select PMS star and young BD candidates using colour-magnitude diagrams (CMDs) and theoretical isochrones reproduced ad-hoc for the WFI at the ESO2.2m telescope system. The selection criteria are also reinforced by using the previously known PMS stars in Cha II to define the PMS locus on the CMDs and by investigating the infrared (IR) colours of the candidates. By exploiting the WFI intermediate-band photometry we also estimate the effective temperature and the level of H-alpha emission of the can...

Spezzi, L; Frasca, A; Covino, E; Gandolfi, D

2007-01-01T23:59:59.000Z

107

Simbol-X Telescope Scientific Calibrations: Requirements and Plans  

SciTech Connect

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

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

2009-05-11T23:59:59.000Z

108

Integrating Seeing Measurements into the Operations of Solar Telescopes  

E-Print Network (OSTI)

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

109

THE JAMES WEBB SPACE TELESCOPE JONATHAN P. GARDNER1,  

E-Print Network (OSTI)

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

Colorado at Boulder, University of

110

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

E-Print Network (OSTI)

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

Johnson, Eric E.

111

The Atacama Cosmology Telescope Project: A Progress Report  

E-Print Network (OSTI)

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

Arthur Kosowsky; for the ACT Collaboration

2006-08-25T23:59:59.000Z

112

Results of a Si/CdTe Compton Telescope  

E-Print Network (OSTI)

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

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

2005-09-21T23:59:59.000Z

113

Review of the Solar Array Telescopes David A. Smith  

E-Print Network (OSTI)

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

Paris-Sud XI, Université de

114

Adaptive Optics Simulations for the European Extremely Large Telescope  

E-Print Network (OSTI)

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

Liske, Jochen

115

New challenges for adaptive optics: extremely large telescopes  

Science Journals Connector (OSTI)

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

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

2000-09-21T23:59:59.000Z

116

Calculus For Technology II  

E-Print Network (OSTI)

MA 22200, Spring 2012. Calculus For Technology II ... Other Information. Emergency procedures · Exam info (A Hoffman) ...

117

Si and Fe depletion in Galactic star-forming regions observed by the Spitzer Space Telescope  

E-Print Network (OSTI)

We report the results of the mid-infrared spectroscopy of 14 Galactic star-forming regions with the high-resolution modules of the Infrared Spectrograph (IRS) on board the Spitzer Space Telescope. We detected [SiII] 35um, [FeII] 26um, and [FeIII] 23um as well as [SIII] 33um and H2 S(0) 28um emission lines. Using the intensity of [NII] 122um or 205um and [OI] 146um or 63um reported by previous observations in four regions, we derived the ionic abundance Si+/N+ and Fe+/N+ in the ionized gas and Si+/O0 and Fe+/O0 in the photodissociation gas. For all the targets, we derived the ionic abundance of Si+/S2+ and Fe2+/S2+ for the ionized gas. Based on photodissociation and HII region models the gas-phase Si and Fe abundance are suggested to be 3-100% and solar abundance, respectively, for the ionized gas and 16-100% and 2-22% of the solar abundance, respectively, for the photodissociation region gas. Since the [FeII] 26um and [FeIII] 23um emissions are weak, the high sensitivity of the IRS enables to derive the gas-phase Fe abundance widely in star-forming regions. The derived gas-phase Si abundance is much larger than that in cool interstellar clouds and that of Fe. The present study indicates that 3-100% of Si atoms and <22% of Fe atoms are included in dust grains which are destroyed easily in HII regions, probably by the UV radiation. We discuss possible mechanisms to account for the observed trend; mantles which are photodesorbed by UV photons, organometallic complexes, or small grains.

Yoko Okada; Takashi Onaka; Takashi Miyata; Yoshiko K. Okamoto; Itsuki Sakon; Hiroshi Shibai; Hidenori Takahashi

2008-04-10T23:59:59.000Z

118

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

E-Print Network (OSTI)

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

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

2013-01-01T23:59:59.000Z

119

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

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

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

120

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

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

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

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.


121

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

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

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

122

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

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

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

123

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

Science Journals Connector (OSTI)

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

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

1995-01-01T23:59:59.000Z

124

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

E-Print Network (OSTI)

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

Cataldo, Giuseppe

2014-12-19T23:59:59.000Z

125

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

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

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

126

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

E-Print Network (OSTI)

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

Thomas, Nicholas E

2011-01-01T23:59:59.000Z

127

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

Science Journals Connector (OSTI)

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

Kassim, Abd M; Shealy, David L

1984-01-01T23:59:59.000Z

128

KECK SPECTROSCOPY OF 3 < z < 7 FAINT LYMAN BREAK GALAXIES: THE IMPORTANCE OF NEBULAR EMISSION IN UNDERSTANDING THE SPECIFIC STAR FORMATION RATE AND STELLAR MASS DENSITY  

SciTech Connect

The physical properties inferred from the spectral energy distributions (SEDs) of z > 3 galaxies have been influential in shaping our understanding of early galaxy formation and the role galaxies may play in cosmic reionization. Of particular importance is the stellar mass density at early times, which represents the integral of earlier star formation. An important puzzle arising from the measurements so far reported is that the specific star formation rates (sSFRs) evolve far less rapidly than expected in most theoretical models. Yet the observations underpinning these results remain very uncertain, owing in part to the possible contamination of rest-optical broadband light from strong nebular emission lines. To quantify the contribution of nebular emission to broadband fluxes, we investigate the SEDs of 92 spectroscopically confirmed galaxies in the redshift range 3.8 < z < 5.0 chosen because the H{alpha} line lies within the Spitzer/IRAC 3.6 {mu}m filter. We demonstrate that the 3.6 {mu}m flux is systematically in excess of that expected from stellar continuum alone, which we derive by fitting the SED with population synthesis models. No such excess is seen in a control sample of spectroscopically confirmed galaxies with 3.1 < z < 3.6 in which there is no nebular contamination in the IRAC filters. From the distribution of our 3.6 {mu}m flux excesses, we derive an H{alpha} equivalent width distribution and consider the implications for both the derived stellar masses and the sSFR evolution. The mean rest-frame H{alpha} equivalent width we infer at 3.8 < z < 5.0 (270 A) indicates that nebular emission contributes at least 30% of the 3.6 {mu}m flux and, by implication, nebular emission is likely to have a much greater impact for galaxies with z {approx_equal} 6-7 where both warm IRAC filters are contaminated. Via our empirically derived equivalent width distribution, we correct the available stellar mass densities and show that the sSFR evolves more rapidly at z > 4 than previously thought, supporting up to a 5 Multiplication-Sign increase between z {approx_equal} 2 and 7. Such a trend is much closer to theoretical expectations. Given our findings, we discuss the prospects for verifying quantitatively the nebular emission line strengths prior to the launch of the James Webb Space Telescope.

Stark, Daniel P.; Robertson, Brant [Department of Astronomy, Steward Observatory, University of Arizona, 933 North Cherry Avenue, Rm N204, Tucson, AZ 85721 (United States)] [Department of Astronomy, Steward Observatory, University of Arizona, 933 North Cherry Avenue, Rm N204, Tucson, AZ 85721 (United States); Schenker, Matthew A.; Ellis, Richard [Cahill Center of Astronomy and Astrophysics, California Institute of Technology, MS 249-17, Pasadena, CA 91125 (United States)] [Cahill Center of Astronomy and Astrophysics, California Institute of Technology, MS 249-17, Pasadena, CA 91125 (United States); McLure, Ross; Dunlop, James, E-mail: dpstark@email.arizona.edu [Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh EH9 3HJ (United Kingdom)] [Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh EH9 3HJ (United Kingdom)

2013-02-15T23:59:59.000Z

129

Thermal characteristics of a classical solar telescope primary mirror  

E-Print Network (OSTI)

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

Banyal, Ravinder K

2011-01-01T23:59:59.000Z

130

SLAC All Access: Fermi Gamma-ray Space Telescope  

SciTech Connect

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

Romani, Roger

2013-05-31T23:59:59.000Z

131

FERMI LARGE AREA TELESCOPE OBSERVATIONS OF GRB 110625A  

SciTech Connect

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

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

2012-08-01T23:59:59.000Z

132

SLAC All Access: Fermi Gamma-ray Space Telescope  

ScienceCinema (OSTI)

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

Romani, Roger

2014-06-24T23:59:59.000Z

133

Gamma-Ray Imaging with the Coded Mask IBIS Telescope  

E-Print Network (OSTI)

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

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

2000-01-01T23:59:59.000Z

134

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

135

The data acquisition system for the ANTARES neutrino telescope  

E-Print Network (OSTI)

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

J. A. Aguilar; ANTARES collaboration

2006-10-02T23:59:59.000Z

136

The Balloon-borne Large Aperture Submillimeter Telescope: BLAST  

Science Journals Connector (OSTI)

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

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

2008-01-01T23:59:59.000Z

137

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

138

Abstracts ii Schedule....................................................................................................................................................... iii  

E-Print Network (OSTI)

.........................................................................................88 Dark Matter & Dark Energy ...............................................................................................3 HAD II Special: Neptune after One Orbit: Reflections on the Discovery of a Planet

Ciotti, Luca

139

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.

140

I IIII1IiI II1Ii  

Office of Legacy Management (LM)

* * 'I I IIII1IiI II1Ii 1111 1111 I - I' p. r. * *: * * * .** I I ,e L 'I r - I OFFICIAL PHOTOGRAPH ADEC ?Date ______ Time - Location /oie_ / I C 4'.'-?- 1D& Reason for Photo ' 1 By _________ Ro1 # 7'93 Frame' # ,'9 I *.' ' .- - . *c *\ I '' . *. , * " . ... *l; .; . '' N 1 * ' ' * ' '" ), q . L *" ' r 'I . I ' , * I ", * _; . ':. -* - - ! .) f' '' . . * 'i; . ,- , . F) .* :-- .' *, 'I 1 - . '.. ' t; , çv ' . ,* I i * #' *. '3 "' i * '- *1 '4 *' ,:- - a 4 t ' - * ', % & ; 1 ¶ * :' *.' ,. : -A r ;v ' :" - .r " 'a - -" -; & ' * - * - - ) : S , ,,, --- S *J %I *' * S .. c .* - Z '- .- '- .., ' . -" ' I * . * ' * S- * , * - 4 .- a * , . V . ,. * i .-- 4. * -Y * / -, *. .' *' ,t r A. _-. *, , *' ** l. . * '' .4 "1 j. ' 1. - ' ' * 4 I - . * - - , _% * I-. , 4 .r- ( J -: '- , *, ' v - I 9 , ' , 1 ** , . * -"J * -" I * - c-- . ;- . '--- - A ... * ' ' - * 'A r? -: * '; ' ' - ' .: 1', - '. *, , .. I ,, *,, . * .t 1- ) ' , ** J' * *I :* : - - I j-- - - * I- , -j -. -** :- * * . *' ' _, 9 ;* 3 . . -. . 5 4 - 9. - .** -.* . - *- .c .- * -. :. .- - - - 4, N 9 - * 9 t * - - 4 2

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141

Design constraints on Cherenkov telescopes with Davies-Cotton reflectors  

E-Print Network (OSTI)

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

Bretz, Thomas

2013-01-01T23:59:59.000Z

142

The Trigger Algorithm for the Burst Alert Telescope on Swift  

E-Print Network (OSTI)

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

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

2004-01-01T23:59:59.000Z

143

THE HUBBLE SPACE TELESCOPE CLUSTER SUPERNOVA SURVEY. V. IMPROVING THE DARK-ENERGY CONSTRAINTS ABOVE z > 1 AND BUILDING AN EARLY-TYPE-HOSTED SUPERNOVA SAMPLE  

SciTech Connect

We present Advanced Camera for Surveys, NICMOS, and Keck adaptive-optics-assisted photometry of 20 Type Ia supernovae (SNe Ia) from the Hubble Space Telescope (HST) Cluster Supernova Survey. The SNe Ia were discovered over the redshift interval 0.623 < z < 1.415. Of these SNe Ia, 14 pass our strict selection cuts and are used in combination with the world's sample of SNe Ia to derive the best current constraints on dark energy. Of our new SNe Ia, 10 are beyond redshift z = 1, thereby nearly doubling the statistical weight of HST-discovered SNe Ia beyond this redshift. Our detailed analysis corrects for the recently identified correlation between SN Ia luminosity and host galaxy mass and corrects the NICMOS zero point at the count rates appropriate for very distant SNe Ia. Adding these SNe improves the best combined constraint on dark-energy density, {rho}{sub DE}(z), at redshifts 1.0 < z < 1.6 by 18% (including systematic errors). For a flat {Lambda}CDM universe, we find {Omega}{sub {Lambda}} = 0.729 {+-} 0.014 (68% confidence level (CL) including systematic errors). For a flat wCDM model, we measure a constant dark-energy equation-of-state parameter w = -1.013{sup +0.068}{sub -0.073} (68% CL). Curvature is constrained to {approx}0.7% in the owCDM model and to {approx}2% in a model in which dark energy is allowed to vary with parameters w{sub 0} and w{sub a} . Further tightening the constraints on the time evolution of dark energy will require several improvements, including high-quality multi-passband photometry of a sample of several dozen z > 1 SNe Ia. We describe how such a sample could be efficiently obtained by targeting cluster fields with WFC3 on board HST. The updated supernova Union2.1 compilation of 580 SNe is available at http://supernova.lbl.gov/Union.

Suzuki, N.; Rubin, D.; Aldering, G.; Barbary, K.; Faccioli, L.; Fakhouri, H. K. [E.O. Lawrence Berkeley National Lab, Berkeley, CA 94720 (United States); Lidman, C. [Australian Astronomical Observatory, Epping, NSW 1710 (Australia); Amanullah, R.; Botyanszki, J. [Department of Physics, University of California Berkeley, Berkeley, CA 94720 (United States); Barrientos, L. F. [Departamento de Astronomia y Astrofisica, Pontificia Universidad Catolica de Chile, Santiago (Chile); Brodwin, M. [Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138 (United States); Connolly, N. [Department of Physics, Hamilton College, Clinton, NY 13323 (United States); Dawson, K. S. [Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112 (United States); Dey, A. [National Optical Astronomy Observatory, Tucson, AZ 85726-6732 (United States); Doi, M. [Institute of Astronomy, Graduate School of Science, University of Tokyo 2-21-1 Osawa, Mitaka, Tokyo 181-0015 (Japan); Donahue, M. [Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824 (United States); Deustua, S. [Space Telescope Science Institute, Baltimore, MD 21218 (United States); Eisenhardt, P. [Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109 (United States); Ellingson, E. [Center for Astrophysics and Space Astronomy, 389 UCB, University of Colorado, Boulder, CO 80309 (United States); Fadeyev, V., E-mail: nsuzuki@lbl.gov, E-mail: rubind@berkeley.edu, E-mail: clidman@aao.gov.au [Santa Cruz Institute for Particle Physics, University of California Santa Cruz, Santa Cruz, CA 94064 (United States); Collaboration: Supernova Cosmology Project; and others

2012-02-10T23:59:59.000Z

144

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

145

ACRA-II  

Energy Science and Technology Software Center (OSTI)

003089IBMPC00 ACRA-II: Kernel Integration Code System for Estimation of Radiation Doses Caused by a Hypothetical Reactor Accident   

146

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

Science Journals Connector (OSTI)

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

Upton, Robert; Cho, Myung; Rimmele, Thomas

2010-01-01T23:59:59.000Z

147

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

E-Print Network (OSTI)

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

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

2006-06-22T23:59:59.000Z

148

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

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

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

149

Aplanatic two mirror telescope from near-normal to grazing incidence  

Science Journals Connector (OSTI)

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

Korsch, Dietrich

1980-01-01T23:59:59.000Z

150

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

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

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

151

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

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

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

152

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?

153

The Balloon-borne Large Aperture Sub-millimetre Telescope  

E-Print Network (OSTI)

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

Douglas Scott; the BLAST Team

2001-04-03T23:59:59.000Z

154

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

E-Print Network (OSTI)

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

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

2014-01-01T23:59:59.000Z

155

BOOMERANG: A Balloon-borne Millimeter-Wave Telescope  

Science Journals Connector (OSTI)

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

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

2003-01-01T23:59:59.000Z

156

Exact Optics A unification of optical telescope design  

E-Print Network (OSTI)

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

Lynden-Bell, Donald

2002-01-01T23:59:59.000Z

157

THE ATACAMA COSMOLOGY TELESCOPE: DATA CHARACTERIZATION AND MAPMAKING  

SciTech Connect

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

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

2013-01-01T23:59:59.000Z

158

Abstract Presented at Synchrotron Environmental Science II (SES-II)  

E-Print Network (OSTI)

Abstract Presented at Synchrotron Environmental Science II (SES-II) Argonne National Laboratory - 6 such as dioxins and furans, polychlorinated biphenyls (PCBs), and polynuclear aromatic hydrocarbons (PAHs). *Work

Brookhaven National Laboratory

159

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

E-Print Network (OSTI)

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

Morselli, Aldo

160

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

E-Print Network (OSTI)

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

Martin, Chris

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.


161

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

E-Print Network (OSTI)

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

162

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

E-Print Network (OSTI)

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

Sirianni, Marco

163

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

E-Print Network (OSTI)

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

164

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

E-Print Network (OSTI)

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

Rutten, Rob

165

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

E-Print Network (OSTI)

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

Sirianni, Marco

166

Jan Hendrik Bruinier II Anna von Pippich Fabrizio Andreatta -Milan, Italy II Massimo Bertolini -Essen, Germany II Siegfried Bcherer -  

E-Print Network (OSTI)

Massimo Bertolini - Essen, Germany II Siegfried Böcherer - Mannheim, Germany II Thanasis Bouganis - Durham II Jay Jorgenson - New York, USA II Winfried Kohnen - Heidelberg, Germany II Jürg Kramer - Berlin, Germany II Siddarth Sankaran - Bonn, Germany II Maryna Viazovska - Bonn, Germany II Tonghai Yang - Madison

Haller-Dintelmann, Robert

167

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

SciTech Connect

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

Chauvin, Maxime; Roques, Jean-Pierre

2010-07-20T23:59:59.000Z

168

Digital Frequency Domain Multiplexer for mm-Wavelength Telescopes  

SciTech Connect

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

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

2007-07-23T23:59:59.000Z

169

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

E-Print Network (OSTI)

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

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

2013-01-01T23:59:59.000Z

170

AS2: Surveys with the APO 2.5m Telescope After SDSS-II April 3, 2007  

E-Print Network (OSTI)

-field cosmology" tests of galaxy formation physics and the small scale distribution of dark matter. The Multi Spectroscopic Survey, which will use significantly upgraded versions of the SDSS spectrographs, will become

171

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

172

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

173

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

Science Journals Connector (OSTI)

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

Chauvin, Maxime; Roques, Jean-Pierre

2010-01-01T23:59:59.000Z

174

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

Science Journals Connector (OSTI)

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

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

175

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

Science Journals Connector (OSTI)

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

Seery, Bernard D; Smith, Eric P

1998-01-01T23:59:59.000Z

176

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

E-Print Network (OSTI)

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

Postman, Marc

2009-01-01T23:59:59.000Z

177

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

178

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

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

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

179

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

Science Journals Connector (OSTI)

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

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

2010-06-21T23:59:59.000Z

180

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

E-Print Network (OSTI)

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

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

2013-01-01T23:59:59.000Z

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.


181

Digital signal processing hardware for a fast fourier transform radio telescope  

E-Print Network (OSTI)

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

Losh, Jonathan L

2012-01-01T23:59:59.000Z

182

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

183

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

184

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

SciTech Connect

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

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

2004-09-28T23:59:59.000Z

185

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

E-Print Network (OSTI)

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

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

2010-01-01T23:59:59.000Z

186

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

187

FAKULTT II MATHEMATIK UND  

E-Print Network (OSTI)

OF A NETWORK CREATION GAME WITH EXPONENTIAL PAYOFF by NADINE BAUMANN SEBASTIAN STILLER No. 2007/19 #12;The Price of Anarchy of a Network Creation Game with Exponential Payoff Nadine Baumann Sebastian Stiller May/5-3. Technische Universität Berlin, Fakultät II, Stra�e des 17. Juni 136, 10623 Berlin, Germany. Email: stiller

Nabben, Reinhard

188

APPENDIX II WESTFLISCHE  

E-Print Network (OSTI)

- 1 - APPENDIX II WESTF�LISCHE WILHELMS-UNIVERSIT�T M�NSTER Instructions for the experiment ,,Stock information about how the experiment works. Please keep general questions until the end of the introduction either 100 or 0 monetary units (MU). Due to the fact that the outcome of the event is uncertain during

Greer, Julia R.

189

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

E-Print Network (OSTI)

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

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

2013-01-01T23:59:59.000Z

190

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

191

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

192

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.

193

PARS II TRAINING | Department of Energy  

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

TRAINING PARS II TRAINING BASICS TRAINING WORKBOOK PARS II TRAINING More Documents & Publications PARS II PARS II Training Workbook (Course 103) PARSIIUserGuideV1.0Draft.pdf...

194

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

E-Print Network (OSTI)

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

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

2013-01-01T23:59:59.000Z

195

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

E-Print Network (OSTI)

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

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

2015-01-01T23:59:59.000Z

196

Wide Field Hard X-ray Survey Telescope: ProtoEXIST1  

E-Print Network (OSTI)

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

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

2007-01-01T23:59:59.000Z

197

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,

198

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

E-Print Network (OSTI)

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

Vasilev, V V

2007-01-01T23:59:59.000Z

199

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

200

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

E-Print Network (OSTI)

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

V. V. Vassiliev; S. J. Fegan

2007-08-21T23:59:59.000Z

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.


201

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

202

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

SciTech Connect

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

NONE

2013-03-01T23:59:59.000Z

203

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

204

_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

205

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

206

Mod II Stirling engine overviews  

SciTech Connect

The Mod II engine is a second-generation automotive Stirling engine (ASE) optimized for part-power operation. It has been designed specifically to meet the fuel economy and exhaust emissions objectives of the ASE development program. The design, test experience, performance, and comparison of data to analytical performance estimates of the Mod II engine to date are reviewed. Estimates of Mod II performance in its final configuration are also given. 12 references.

Farrell, R.A.

1988-01-01T23:59:59.000Z

207

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

E-Print Network (OSTI)

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

P. F. Bloser; S. D. Hunter

2004-05-14T23:59:59.000Z

208

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

E-Print Network (OSTI)

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

209

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

210

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

Science Journals Connector (OSTI)

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

Brian C. Lacki

2014-01-01T23:59:59.000Z

211

Design Considerations for the Next Generation of Atmospheric Imaging Cherenkov Telescopes  

E-Print Network (OSTI)

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

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

2007-09-29T23:59:59.000Z

212

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

E-Print Network (OSTI)

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

213

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

E-Print Network (OSTI)

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

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

2015-01-01T23:59:59.000Z

214

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

E-Print Network (OSTI)

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

Shayduk, M; Schwanke, U

2013-01-01T23:59:59.000Z

215

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

E-Print Network (OSTI)

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

Tokovinin, Andrei A.

216

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

E-Print Network (OSTI)

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

Liske, Jochen

217

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

ScienceCinema (OSTI)

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

Isabelle Grenier

2010-01-08T23:59:59.000Z

218

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

E-Print Network (OSTI)

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

T. D. Willis

2002-01-30T23:59:59.000Z

219

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

E-Print Network (OSTI)

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

Collar, Juan I.

220

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

E-Print Network (OSTI)

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

California at Berkeley, University of

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

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

E-Print Network (OSTI)

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

Duffy, Alan R

2014-01-01T23:59:59.000Z

222

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":""}]}

223

TURBULENT CHARACTERISTICS IN THE INTENSITY FLUCTUATIONS OF A SOLAR QUIESCENT PROMINENCE OBSERVED BY THE HINODE SOLAR OPTICAL TELESCOPE  

SciTech Connect

We focus on Hinode Solar Optical Telescope (SOT) calcium II H-line observations of a solar quiescent prominence (QP) that exhibits highly variable dynamics suggestive of turbulence. These images capture a sufficient range of scales spatially ({approx}0.1-100 arcsec) and temporally ({approx}16.8 s-4.5 hr) to allow the application of statistical methods used to quantify finite range fluid turbulence. We present the first such application of these techniques to the spatial intensity field of a long-lived solar prominence. Fully evolved inertial range turbulence in an infinite medium exhibits multifractal scale invariance in the statistics of its fluctuations, seen as power-law power spectra and as scaling of the higher order moments (structure functions) of fluctuations which have non-Gaussian statistics; fluctuations {delta}I(r, L) = I(r + L) - I(r) on length scale L along a given direction in observed spatial field I have moments that scale as ({delta}I(r, L){sup p}) {approx} L{sup {zeta}(p)}. For turbulence in a system that is of finite size, or that is not fully developed, one anticipates a generalized scale invariance or extended self-similarity (ESS) ({delta}I(r, L){sup p}) {approx} G(L){sup {zeta}(p)}. For these QP intensity measurements we find scaling in the power spectra and ESS. We find that the fluctuation statistics are non-Gaussian and we use ESS to obtain ratios of the scaling exponents {zeta}(p): these are consistent with a multifractal field and show distinct values for directions longitudinal and transverse to the bulk (driving) flow. Thus, the intensity fluctuations of the QP exhibit statistical properties consistent with an underlying turbulent flow.

Leonardis, E.; Chapman, S. C.; Foullon, C. [Centre for Fusion Space and Astrophysics, Department of Physics, University of Warwick, Coventry, CV4 7AL (United Kingdom)

2012-02-01T23:59:59.000Z

224

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

225

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

226

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

227

Mod II engine performance  

SciTech Connect

The Automotive Stirling Engine Program (ASE) is directed at the development of a kinematic Stirling engine for automotive use. This program is sponsored by the Department of Energy (DOE) and managed by the NASA-Lewis Research Center (NASA-LeRC). Following proof-of-concept testing and development of promising performance values with early versions of the Stirling engine, a production-type automotive design, the Mod II engine, was developed. The design of this engine and its systems has been previously presented. Based on this design, the first engine has been built and development testing has started. Projections for this first engine build are presented in this paper. Results of initial tests are also given including identification of development items and formulation of plans for resolution of existing deficiencies.

Richey, A.E.; Huang, S.C.

1987-01-01T23:59:59.000Z

228

Phase II Final Report  

SciTech Connect

The SkyTrough DSP will advance the state-of-the-art in parabolic troughs for utility applications, with a larger aperture, higher operating temperature, and lower cost. The goal of this project was to develop a parabolic trough collector that enables solar electricity generation in the 2020 marketplace for a 216MWe nameplate baseload power plant. This plant requires an LCOE of 9¢/kWhe, given a capacity factor of 75%, a fossil fuel limit of 15%, a fossil fuel cost of $6.75/MMBtu, $25.00/kWht thermal storage cost, and a domestic installation corresponding to Daggett, CA. The result of our optimization was a trough design of larger aperture and operating temperature than has been fielded in large, utility scale parabolic trough applications: 7.6m width x 150m SCA length (1,118m2 aperture), with four 90mm diameter × 4.7m receivers per mirror module and an operating temperature of 500°C. The results from physical modeling in the System Advisory Model indicate that, for a capacity factor of 75%: The LCOE will be 8.87¢/kWhe. SkyFuel examined the design of almost every parabolic trough component from a perspective of load and performance at aperture areas from 500 to 2,900m2. Aperture-dependent design was combined with fixed quotations for similar parts from the commercialized SkyTrough product, and established an installed cost of $130/m2 in 2020. This project was conducted in two phases. Phase I was a preliminary design, culminating in an optimum trough size and further improvement of an advanced polymeric reflective material. This phase was completed in October of 2011. Phase II has been the detailed engineering design and component testing, which culminated in the fabrication and testing of a single mirror module. Phase II is complete, and this document presents a summary of the comprehensive work.

Schuknecht, Nate [Project Manager; White, David [Principle Investigator; Hoste, Graeme [Research Engineer

2014-09-11T23:59:59.000Z

229

Kinematic Viscosity of Helium II  

Science Journals Connector (OSTI)

By observing the time of formation of the meniscus in a cylindrical vessel suddenly given a rotation, it has been found possible to determine, directly, the kinematic viscosity of both He I and He II. At the angular velocities used (?15 rev/sec) it appears that, for He II, all the liquid rotates rather than the normal component alone.

R. J. Donnelly; G. V. Chester; R. H. Walmsley; C. T. Lane

1956-04-01T23:59:59.000Z

230

THE HETDEX PILOT SURVEY. IV. THE EVOLUTION OF [O II] EMITTING GALAXIES FROM z {approx} 0.5 TO z {approx} 0  

SciTech Connect

We present an analysis of the luminosities and equivalent widths of the 284 z < 0.56 [O II]-emitting galaxies found in the 169 arcmin{sup 2} pilot survey for the Hobby-Eberly Telescope Dark Energy Experiment (HETDEX). By combining emission-line fluxes obtained from the Mitchell spectrograph on the McDonald 2.7 m telescope with deep broadband photometry from archival data, we derive each galaxy's dereddened [O II] {lambda}3727 luminosity and calculate its total star formation rate. We show that over the last {approx}5 Gyr of cosmic time, there has been substantial evolution in the [O II] emission-line luminosity function, with L* decreasing by {approx}0.6 {+-} 0.2 dex in the observed function, and by {approx}0.9 {+-} 0.2 dex in the dereddened relation. Accompanying this decline is a significant shift in the distribution of [O II] equivalent widths, with the fraction of high equivalent-width emitters declining dramatically with time. Overall, the data imply that the relative intensity of star formation within galaxies has decreased over the past {approx}5 Gyr, and that the star formation rate density of the universe has declined by a factor of {approx}2.5 between z {approx} 0.5 and z {approx} 0. These observations represent the first [O II]-based star formation rate density measurements in this redshift range, and foreshadow the advancements which will be generated by the main HETDEX survey.

Ciardullo, Robin; Gronwall, Caryl; Schneider, Donald P.; Zeimann, Gregory R., E-mail: rbc@astro.psu.edu, E-mail: caryl@astro.psu.edu, E-mail: dps@astro.psu.edu, E-mail: grzeimann@psu.edu [Department of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802 (United States); and others

2013-05-20T23:59:59.000Z

231

A DETAILED COMPARISON BETWEEN THE OBSERVED AND SYNTHESIZED PROPERTIES OF A SIMULATED TYPE II SPICULE  

SciTech Connect

We have performed a three-dimensional radiative MHD simulation of the solar atmosphere. This simulation shows a jet-like feature that shows similarities to the type II spicules observed for the first time with Hinode's Solar Optical Telescope. Rapid blueshifted events (RBEs) on the solar disk are associated with these spicules. Observational results suggest they may contribute significantly in supplying the corona with hot plasma. We perform a detailed comparison of the properties of the simulated jet with those of type II spicules (observed with Hinode) and RBEs (with ground-based instruments). We analyze a wide variety of synthetic emission and absorption lines from the simulations including chromospheric (Ca II 8542 A, Ca II H, and H{alpha}) to transition region and coronal temperatures (10,000 K to several million K). We compare their synthetic intensities, line profiles, Doppler shifts, line widths, and asymmetries with observations from Hinode/SOT and EIS, SOHO/SUMER, the Swedish 1 m Solar Telescope, and SDO/AIA. Many properties of the synthetic observables resemble the observations, and we describe in detail the physical processes that lead to these observables. Detailed analysis of the synthetic observables provides insight into how observations should be analyzed to derive information about physical variables in such a dynamic event. For example, we find that line-of-sight superposition in the optically thin atmosphere requires the combination of Doppler shifts and spectral line asymmetry to determine the velocity in the jet. In our simulated type II spicule, the lifetime of the asymmetry of the transition region lines is shorter than that of the coronal lines. Other properties differ from the observations, especially in the chromospheric lines. The mass density of the part of the spicule with a chromospheric temperature is too low to produce significant opacity in chromospheric lines. The synthetic Ca II 8542 A and H{alpha} profiles therefore do not show signal resembling RBEs. These and other discrepancies are described in detail, and we discuss which mechanisms and physical processes may need to be included in the MHD simulations to mimic the thermodynamic processes of the chromosphere and corona, in particular to reproduce type II spicules.

Martinez-Sykora, Juan; De Pontieu, Bart; Pereira, Tiago M. D.; Stern, Julie V. [Lockheed Martin Solar and Astrophysics Laboratory, Palo Alto, CA 94304 (United States); Leenaarts, Jorrit; Carlsson, Mats; Hansteen, Viggo; Van der Voort, Luc Rouppe [Institute of Theoretical Astrophysics, University of Oslo, P.O. Box 1029 Blindern, N-0315 Oslo (Norway); Tian Hui [Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138 (United States); McIntosh, Scott W., E-mail: j.m.sykora@astro.uio.no [High Altitude Observatory, National Center for Atmospheric Research, Boulder, CO 80307 (United States)

2013-07-01T23:59:59.000Z

232

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.

233

Sílabo del curso de Redes II.  

E-Print Network (OSTI)

??El curso de Redes II, es de naturaleza Teórico–Práctica, pertenece al área de infraestructura de tecnologías de información Redes II es un curso que aporta… (more)

[No author

2014-01-01T23:59:59.000Z

234

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

235

The Anti-Coincidence Detector for the GLAST Large Area Telescope  

SciTech Connect

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

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

2007-03-23T23:59:59.000Z

236

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

SciTech Connect

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

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

2008-12-24T23:59:59.000Z

237

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

E-Print Network (OSTI)

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

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

2015-01-01T23:59:59.000Z

238

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

E-Print Network (OSTI)

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

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

2008-08-01T23:59:59.000Z

239

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

E-Print Network (OSTI)

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

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

2008-01-01T23:59:59.000Z

240

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

Science Journals Connector (OSTI)

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

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

2014-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "keck ii telescope" from the National Library of EnergyBeta (NLEBeta).
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241

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

E-Print Network (OSTI)

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

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

2008-06-13T23:59:59.000Z

242

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

SciTech Connect

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

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

1990-01-01T23:59:59.000Z

243

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

SciTech Connect

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

Lang, Robert J.

2010-06-24T23:59:59.000Z

244

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

E-Print Network (OSTI)

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

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

1998-01-01T23:59:59.000Z

245

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

E-Print Network (OSTI)

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

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

1998-03-17T23:59:59.000Z

246

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":""}]}

247

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":""}]}

248

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":""}]}

249

Category II Dixon Recreation Center  

E-Print Network (OSTI)

Category II Dixon Recreation Center BB or VB court $30 RB/Squash court $23 Multipurpose Room $30 for any rental that is cancelled with less than seven days notice Department of Recreational Sports

Escher, Christine

250

Super KEKB / Belle II Project  

E-Print Network (OSTI)

We present the status of the KEKB collider and the Belle detector upgrade, along with several examples of physics measurements to be performed with Belle II at Super KEKB.

B. Golob

2010-06-22T23:59:59.000Z

251

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":""}]}

252

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

253

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

E-Print Network (OSTI)

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

The Pierre Auger Collaboration; L. Perrone

2005-07-20T23:59:59.000Z

254

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

E-Print Network (OSTI)

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

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

2007-08-28T23:59:59.000Z

255

The KM3NeT deep-sea neutrino telescope  

E-Print Network (OSTI)

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

Margiotta, Annarita

2014-01-01T23:59:59.000Z

256

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

257

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

258

Woods In and Around Towns: Phase II  

E-Print Network (OSTI)

Policy WIAT Woods In and Around Towns: Phase II #12;2 | Woods In and Around Towns: Phase II working with Forestry Commission Scotland on Woods In and Around Towns #12;Woods In and Around Towns: Phase II Woods In and Around Towns: Phase II | 3 What is this about? The Woods In and Around Towns (WIAT) Programme provides

259

[Fe II] 1.64 ?m FEATURES OF JETS AND OUTFLOWS FROM YOUNG STELLAR OBJECTS IN THE CARINA NEBULA  

SciTech Connect

We present [Fe II] 1.64 ?m imaging observations for jets and outflows from young stellar objects (YSOs) over the northern part (?24' × 45') of the Carina Nebula, a massive star-forming region. The observations were performed with IRIS2 of the Anglo-Australian Telescope and the seeing was ?1.''5 ± 0.''5. Eleven jet and outflow features are detected at eight different regions and are termed ionized Fe objects (IFOs). One Herbig-Haro candidate that was missed in Hubble Space Telescope H? observations is newly identified as HHc-16, referring to our [Fe II] images. IFOs have knotty or longish shapes, and the detection rate of IFOs against previously identified YSOs is 1.4%, which should be treated as a lower limit. Four IFOs show anti-correlated peak intensities in [Fe II] and H?, where the ratio I([Fe II])/I(H?) is higher for longish IFOs than for knotty IFOs. We estimate the outflow mass loss rate from the [Fe II] flux using two different methods. The jet-driving objects are identified for three IFOs (IFO-2, -4, and -7) for which we study the relations between the outflow mass loss rate and the YSO physical parameters from the radiative transfer model fitting. The ratios of the outflow mass loss rate over the disk accretion rate for IFO-4 and -7 are consistent with the previously reported values (10{sup –2}-10{sup +1}), while the ratio is higher for IFO-2. This excess may result from underestimating the disk accretion rate. The jet-driving objects are likely to be low- or intermediate-mass stars. Other YSO physical parameters, such as luminosity and age, show reasonable relations or trends.

Shinn, Jong-Ho; Lee, Jae-Joon; Chun, Moo-Young; Lyo, A.-Ran; Moon, Dae-Sik; Kyeong, Jaemann; Park, Byeong-Gon [Korea Astronomy and Space Science Institute, 776 Daeduk-daero, Yuseong-gu, Daejeon 305-348 (Korea, Republic of); Pyo, Tae-Soo [Subaru Telescope, National Astronomical Observatory of Japan, 650 North A'oh?k? Place, Hilo, HI 96720 (United States); Lee, Ho-Gyu [Department of Astronomy, Graduate School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033 (Japan); Kim, Hyun-Jeong; Koo, Bon-Chul; Lee, Yong-Hyun [Department of Physics and Astronomy, Seoul National University, 599 Gwanangno, Gwanak-gu, Seoul 151-747 (Korea, Republic of); Sung, Hwankyung; Hur, Hyeonoh, E-mail: jhshinn@kasi.re.kr [Department of Astronomy and Space Science, Sejong University, 98 Kunja-dong, Kwangjin-gu, Seoul 143-747 (Korea, Republic of)

2013-11-01T23:59:59.000Z

260

EMISSION-LINE GALAXIES FROM THE HUBBLE SPACE TELESCOPE PROBING EVOLUTION AND REIONIZATION SPECTROSCOPICALLY (PEARS) GRISM SURVEY. I. THE SOUTH FIELDS  

SciTech Connect

We present results of a search for emission-line galaxies (ELGs) in the southern fields of the Hubble Space Telescope Probing Evolution And Reionization Spectroscopically (PEARS) grism survey. The PEARS South Fields consist of five Advanced Camera for Surveys pointings (including the Hubble Ultra Deep Field) with the G800L grism for a total of 120 orbits, revealing thousands of faint object spectra in the GOODS-South region of the sky. ELGs are one subset of objects that are prevalent among the grism spectra. Using a two-dimensional detection and extraction procedure, we find 320 emission lines originating from 226 galaxy 'knots' within 192 individual galaxies. Line identification results in 118 new grism-spectroscopic redshifts for galaxies in the GOODS-South Field. We measure emission-line fluxes using standard Gaussian fitting techniques. At the resolution of the grism data, the H{beta} and [O III] doublet are blended. However, by fitting two Gaussian components to the H{beta} and [O III] features, we find that many of the PEARS ELGs have high [O III]/H{beta} ratios compared to other galaxy samples of comparable luminosities. The star formation rates of the ELGs are presented, as well as a sample of distinct giant star-forming regions at z {approx} 0.1-0.5 across individual galaxies. We find that the radial distances of these H II regions in general reside near the galaxies' optical continuum half-light radii, similar to those of giant H II regions in local galaxies.

Straughn, Amber N.; Gardner, Jonathan P. [Astrophysics Science Division, Observational Cosmology Laboratory, Goddard Space Flight Center, Code 665, Greenbelt, MD 20771 (United States); Pirzkal, Norbert; Grogin, Norman; Panagia, Nino [Space Telescope Science Institute, Baltimore, MD 21218 (United States); Meurer, Gerhardt R. [Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218 (United States); Cohen, Seth H.; Windhorst, Rogier A.; Malhotra, Sangeeta; Rhoads, James; Jansen, Rolf A. [School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287 (United States); Hathi, Nimish P. [Department of Physics and Astronomy, University of California, Riverside, CA 92521 (United States); Di Serego Alighieri, Sperello [INAF-Osservatorio Astrofisico di Arcetri, I-50125 Firenze (Italy); Gronwall, Caryl [Department of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802 (United States); Walsh, Jeremy [ESO Space Telescope European Co-ordinating Facility, D-85748 Garching bei Muenchen (Germany); Pasquali, Anna [Max-Planck-Institut for Astronomie, Koenigstuhl 17, D-69117 Heidelberg (Germany); Xu, Chun [Shanghai Institute of Technical Physics, 200083 Shanghai (China)], E-mail: Amber.N.Straughn@nasa.gov

2009-10-15T23:59:59.000Z

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.


261

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":""}]}

262

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":""}]}

263

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":""}]}

264

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":""}]}

265

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":""}]}

266

Near-Infrared [Fe II] and H2 Line Observations of the Supernova Remnant 3C 396: Probing the Pre-supernova Circumstellar Materials  

E-Print Network (OSTI)

We present the results of near-infrared [Fe II] and H2 line imaging and spectroscopic observations of the supernova remnant 3C 396 using the Palomar 5 m Hale telescope. We detect long, filamentary [Fe II] emission delineating the inner edge of the radio emission in the western boundary of the remnant in imaging observations, together with a bright [Fe II] emission clump close to the remnant center. There appears to be faint, diffuse [Fe II] emission between the central clump and the western filamentary emission. The spectroscopic observations determine the expansion velocity of the central clump to be ~56 km/s. This is far smaller than the expansion velocity of 3C 396 obtained from X-ray observations, implying the inhomogeneity of the ambient medium. The electron number density of the [Fe II] emission gas is < 2,000 cm-3. The H2 line emission, on the other hand, lies slightly outside the filamentary [Fe II] emission in the western boundary, and forms a rather straight filament. We suggest that the [Fe II] ...

Lee, Ho-Gyu; Koo, Bon-Chul; Lee, Jae-Joon; Matthews, Keith

2008-01-01T23:59:59.000Z

267

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

268

Telescope Guiding with a HyViSI H2RG Used in Guide Mode  

SciTech Connect

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

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

2010-06-04T23:59:59.000Z

269

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) [SLAC

2011-03-30T23:59:59.000Z

270

The Sun -II Alexei Gilchrist  

E-Print Network (OSTI)

The Sun - II Alexei Gilchrist #12;Some resources · http://www.nineplanets.org/sol.html · "The Universe: Secrets of the Sun" video ­ Search on youtube (references are to clips here http in these slides Secrets of the Sun #12;Why does the sun shine? Long and fascinating history involving - geology

Wardle, Mark

271

Advanced Toroidal Facility II studies  

SciTech Connect

Design studies for a low-aspect-ratio, large next-generation stellarator, Advanced Toroidal Facility II (ATF-II), with high-current-density, high-field, stable NbTi/Cu helical windings are described. The design parameters are an average plasma radius of 0.52 m, a major radius of 2 m, and a field on axis of 4 to 5 T, with 10 to 15 MW of heating power. Such a device would be comparable in cope to other next-generation stellarators but would have roughly the same aspect ratio as the tokamaks without, however, the need for current drive to sustain steady-state operation. A number of low-aspect-ratio physics issues need to be addressed in the design of ATF-II, primarily compromises between high-beta capability and good confinement properties. A six-field-period compact torsatron is chosen as a reference design for ATF-II, and its main features and performance predictions are discussed. An integrated (beta capability and confinement) optimization approach and optimization of superconducting windings are also discussed.

Lyon, J.F.; Carreras, B.A.; Dominguez, N.; Dresner, L.; Hedrick, C.L.; Hirshman, S.P.; Lubell, M.S.; Lue, J.W.; Painter, S.L.; Rome, J.A. (Oak Ridge National Lab., TN (USA)); Morris, R.N.; van Rij, W.I. (Martin Marietta Energy Systems, Computing and Telecommunications Div., Oak Ridge, TN (US))

1990-01-01T23:59:59.000Z

272

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

E-Print Network (OSTI)

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

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

2014-01-01T23:59:59.000Z

273

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

E-Print Network (OSTI)

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

Abdo, A A

2009-01-01T23:59:59.000Z

274

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

Science Journals Connector (OSTI)

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

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

1996-01-01T23:59:59.000Z

275

Fermi Large Area Telescope Observations of the Cygnus Loop Supernova Remnant  

SciTech Connect

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

276

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

E-Print Network (OSTI)

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

G. Carminati; A. Margiotta; M. Spurio

2008-02-05T23:59:59.000Z

277

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

E-Print Network (OSTI)

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

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

2014-01-01T23:59:59.000Z

278

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

E-Print Network (OSTI)

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

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

2014-01-01T23:59:59.000Z

279

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

E-Print Network (OSTI)

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

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

2015-01-01T23:59:59.000Z

280

PARS II Process Document - Project Phasing | Department of Energy  

Energy Savers (EERE)

PARS II Process Document - Project Phasing.pdf More Documents & Publications Proposed Data Elements for PARS II Web Application Slide 1 PARS II Standard Operating Procedure (SOP)...

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

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

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

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 &...

282

PARS II - Integrated Project Team Meeting | Department of Energy  

Energy Savers (EERE)

Meeting PARS II - Integrated Project Team Meeting More Documents & Publications PARS II 104 Contractor Monthly Upload Proposed Data Elements for PARS II Web Application Slide 1...

283

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

E-Print Network (OSTI)

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

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

2005-04-29T23:59:59.000Z

284

High resolution far-infrared observations of the evolved H II region M16  

SciTech Connect

M16 is an evolved, extremely density bounded H II region, which now consists only of a series of ionization fronts at molecular cloud boundaries. The source of ionization is the OB star cluster (NGC 6611) which is about 5 x 10/sup 6/ years old. We used the CFA/UA 102 cm balloon-borne telescope to map this region and detected three far-infrared (far-IR) sources embedded in an extended ridge of emission. Source I is an unresolved far-IR source embedded in a molecular cloud near a sharp ionization front. An H/sub 2/O maser is associated with this source, but no radio continuum emission has been observed. The other two far-IR sources (II and III) are associated with ionized gas-molecular cloud interfaces, with the far-IR radiation arising from dust at the boundary heated by the OB cluster. Source II is located at the southern prominent neutral intrusion with its associated bright rims and dark ''elephant trunk'' globules that delineate the current progress of the ionization front into the neutral material, and Source III arises at the interface of the northern molecular cloud fragment.

McBreen, B.; Fazio, G.G.; Jaffe, D.T.

1982-03-01T23:59:59.000Z

285

PARS II Training | Department of Energy  

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

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 hands-on. In...

286

Part II: Project Summaries Project Summaries  

E-Print Network (OSTI)

Part II: Project Summaries Part II Project Summaries #12 generally cannot be achieved for reasonable computational cost. Applications that require modeling, and in nondestructive testing. The objective of this project is to advance the state of the art in electromagnetic

Perkins, Richard A.

287

PARS II Training Schedule | Department of Energy  

Office of Environmental Management (EM)

will certify that user to receive a PARS II user account. PARSIITrainingSchedule03-06-2014.pdf More Documents & Publications Slide 1 Slide 1 PARS II Course Registration Form...

288

Swift Progress on NSLS-II Booster  

ScienceCinema (OSTI)

Get an inside look around the booster ring at the National Synchrotron Light Source II. The booster is part of the injector complex for NSLS-II, now under construction at Brookhaven Lab.

None

2013-07-17T23:59:59.000Z

289

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

E-Print Network (OSTI)

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

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

2008-10-27T23:59:59.000Z

290

Algebraic L-theory II Tibor Macko  

E-Print Network (OSTI)

Tibor Macko (Uni-Bonn) Algebraic L-theory II GKSS THDM 2013 1 / 29 #12;The surgery obstruction? Recall on simply-connected manifolds. Tibor Macko (Uni-Bonn) Algebraic L-theory II GKSS THDM 2013 2 / 29 #12;The GKSS THDM 2013 3 / 29 #12;The suspension maps II Recall the 1-chain W %(I) alias : I W %(I) from

Ferrari, Patrik L.

291

I I I I II I I I II I I I II I I I II I I I II I I I II I I I II I I I II I I I II I I I IIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIIII  

E-Print Network (OSTI)

Laboratory during 1996. The department is undertaking research within Simulation and Optimisation of Energy I II I I I II I I I II I I I I I CONTENTS 4 Introduction 6 Simulation and Optimisation of Energy Related to Power Production 16 Energy and Environment in Developing Countries 16 UNEP Support Activities

292

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

Science Journals Connector (OSTI)

Neutrino telescopes will open, in the next years, new opportunities in observational high energy astrophysics. In these detectors, atmospheric muons from primary cosmic ray interactions in the atmosphere play an important role, because they provide the most abundant source of events for calibration and test. On the other side, they represent the major background source. In this paper a fast Monte Carlo generator (called MUPAGE) of bundles of atmospheric muons for underwater/ice neutrino telescopes is presented. MUPAGE is based on parametric formulas [Y. Becherini, A. Margiotta, M. Sioli, M. Spurio, Astrop. Phys. 25 (2006) 1] obtained from a full Monte Carlo simulation of cosmic ray showers generating muons in bundle, which are propagated down to 5 km w.e. It produces the event kinematics on the surface of a user-defined cylinder, surrounding the virtual detector. The multiplicity of the muons in the bundle, the muon lateral distribution and energy spectrum are simulated according to a specific model of primary cosmic ray flux, with constraints from measurements of the muon flux with underground experiments. As an example of application, the result of the generation of events on a cylindrical surface of ?1.4 km2 at a depth of 2450 m of water is presented. Program summary Program title: MUPAGE Catalogue identifier: AEBT_v1_0 Program summary URL: http://cpc.cs.qub.ac.uk/summaries/AEBT_v1_0.html Program obtainable from: CPC Program Library, Queen's University, Belfast, N. Ireland Licensing provisions: Standard CPC licence, http://cpc.cs.qub.ac.uk/licence/licence.html No. of lines in distributed program, including test data, etc.: 3534 No. of bytes in distributed program, including test data, etc.: 61?383 Distribution format: tar.gz Programming language: C++ Computer: Pentium M, 2.0 GHz; 2x Intel Xeon Quad Core, 2.33 \\{GHz\\} Operating system: Scientific Linux 3.x; Scientific Linux 4.x; Slackware 12.0.0 RAM: 50 MB Word size: 32 bits Classification: 1.1, 11.3 External routines: The ROOT system (http://root.cern.ch) Nature of problem: Fast simulation of atmospheric muon bundles for underwater/ice neutrino telescopes. Solution method: Atmospheric muon events are generated according to parametric formulas [1] giving the flux, the multiplicity, the radial distribution and the energy spectrum. Restrictions: Water vertical depth range from 1.5 to 5 km w.e.; zenith angle range from 0 to 85 degrees. Additional comments: The program requires the ROOT libraries for the pseudorandom number generator. References: [1]  Y. Becherini, A. Margiotta, M. Sioli, M. Spurio, Astrop. Phys. 25 (2006) 1–13.

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

2008-01-01T23:59:59.000Z

293

CHARACTERIZING THE ATMOSPHERES OF TRANSITING PLANETS WITH A DEDICATED SPACE TELESCOPE  

SciTech Connect

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

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

2012-02-10T23:59:59.000Z

294

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.

295

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

296

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

297

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)

298

PEP-II Operations Report  

SciTech Connect

PEP-II is a two-ring asymmetric B factory operating at the Upsilon(4S) resonance. It was constructed by a SLAC-LBNL-LLNL collaboration. The collider comprises two rings, a High-Energy Ring (HER) storing 9 GeV electrons, and a Low-Energy Ring (LER) storing 3.1 GeV positrons. Commissioning of the HER began in mid-1997 and commissioning of the LER began in mid-1998. First evidence for collisions was obtained on July 23, 1998. The BaBar detector was installed in early 1999, and commissioning with the detector commenced in May 1999. By September 1999, PEP-II had reached a peak luminosity of 1.35 x 10{sup 33} cm{sup {minus}2} s{sup {minus}1}. In the present run, which began in October 1999, the peak luminosity has reached 3.1 x 10{sup 33} cm{sup {minus}2} s{sup {minus}1} and the integrated luminosity delivered is 25 fb{sup {minus}1}. At present, PEP-II is the world's highest luminosity collider. In this paper we describe the startup experience and summarize the operational experience during fiscal year 2000 (from October 1999 through September 2000). Plan s for luminosity upgrades are briefly described.

Zisman, Michael S.

2000-11-01T23:59:59.000Z

299

Volume II, Issue 2 February 2012  

E-Print Network (OSTI)

of dark matter, dark energy, and the standard cosmological model. One of the tools they'll be using the properties of the mysterious dark energy and to test Einstein's theory of gravity over enor- mous distances www.lsst.org. Rendering of the Large Synoptic Survey Telescope #12;ENERGY U.S. DEPARTMENT OF Lab

Johnson, Peter D.

300

Astronomy 135 ELEMENTARY ASTRONOMY LABORATORY II  

E-Print Network (OSTI)

by or make an appointment for other times. Required supplies: Lab exercises- available from the course web observing. Web site: www.physics.umt.edu/astr135 COURSE CONTENT By the time you finish this course you a chance to see deep-sky objects through a telescope, use modern computer software to explore deep

Vonessen, Nikolaus

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

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

SciTech Connect

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

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

2006-10-27T23:59:59.000Z

302

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

E-Print Network (OSTI)

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

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

2014-01-01T23:59:59.000Z

303

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

E-Print Network (OSTI)

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

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

2004-11-08T23:59:59.000Z

304

Opto-thermal analysis of a lightweighted mirror for solar telescope  

E-Print Network (OSTI)

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

Banyal, Ravinder K; Chatterjee, S

2013-01-01T23:59:59.000Z

305

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

E-Print Network (OSTI)

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

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

2014-01-01T23:59:59.000Z

306

BOOMERanG: a scanning telescope for 10 arcminutes resolution CMB maps  

Science Journals Connector (OSTI)

The BOOMERanG experiment is a stratospheric balloon telescope intended to measure the Cosmic Microwave Background anisotropy at angular scales between a few degrees and ten arcminutes. The experiment features a wide focal plane with 16 detectors in the frequency bands centered at 90 150 220 400 GHz with FWHM ranging between 18 and 10 arcmin. It will be flown on a long duration (7–14 days) flight circumnavigating Antarctica at the end of 1998. The instrument was flown with a reduced focal plane (6 detectors 90 and 150 GHz bands 25 to 15 arcmin FWHM) on a qualification flight from Texas in August 1997. A wide (?300 deg2 i.e. about 5000 independent beams at 150 GHz) sky area was mapped in the constellations of Capricornus Aquarius Cetus with very low foreground contamination. The instrument was calibrated using the CMB dipole and observations of Jupiter. The LDB version of the instrument has been qualified and shipped to Antarctica.

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

1999-01-01T23:59:59.000Z

307

BOOMERanG: a scanning telescope for 10 arcminutes resolution CMB maps  

E-Print Network (OSTI)

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

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

1999-11-30T23:59:59.000Z

308

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

E-Print Network (OSTI)

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

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

2007-01-01T23:59:59.000Z

309

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

E-Print Network (OSTI)

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

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

2007-10-10T23:59:59.000Z

310

Observations of Active Galactic Nuclei with Ground-Based Cherenkov Telescopes  

E-Print Network (OSTI)

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

Henric Krawczynski

2005-08-29T23:59:59.000Z

311

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

SciTech Connect

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

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

1987-10-01T23:59:59.000Z

312

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

E-Print Network (OSTI)

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

Courtois, Helene M

2014-01-01T23:59:59.000Z

313

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

Science Journals Connector (OSTI)

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

R. Abbasi et al. (IceCube Collaboration)

2011-07-29T23:59:59.000Z

314

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

315

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

316

Postdoctoral Prize Fellowship Application, M. L. Balogh Page 1 Research Proposal of Michael L. Balogh  

E-Print Network (OSTI)

studies of their galaxies and hot gas. I describe three related projects, including observational--object spectra (MOS) data to observational programs involving the W. M. Keck and Hale telescopes, designed

Balogh, Michael L.

317

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

318

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

319

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

320

II  

Annual Energy Outlook 2012 (EIA)

Ecology Laboratory, Colorado Air and Radiation. Energy Information AdministrationMonthly Energy Review November 1995 formation in some urban and rural regions of the United...

Note: This page contains sample records for the topic "keck ii telescope" from the National Library of EnergyBeta (NLEBeta).
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321

II*  

Gasoline and Diesel Fuel Update (EIA)

Federal, State, local, and foreign governments; EIA survey respondents; and the media. For further information and for answers to questions on energy statistics, please...

322

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

323

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

E-Print Network (OSTI)

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

Dewey, Daniel

324

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

E-Print Network (OSTI)

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

California at Berkeley, University of

325

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

E-Print Network (OSTI)

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

Taniguchi, Y

2003-01-01T23:59:59.000Z

326

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

SciTech Connect

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

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

2005-10-01T23:59:59.000Z

327

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

E-Print Network (OSTI)

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

328

Belle II Technical Design Report  

E-Print Network (OSTI)

The Belle detector at the KEKB electron-positron collider has collected almost 1 billion Y(4S) events in its decade of operation. Super-KEKB, an upgrade of KEKB is under construction, to increase the luminosity by two orders of magnitude during a three-year shutdown, with an ultimate goal of 8E35 /cm^2 /s luminosity. To exploit the increased luminosity, an upgrade of the Belle detector has been proposed. A new international collaboration Belle-II, is being formed. The Technical Design Report presents physics motivation, basic methods of the accelerator upgrade, as well as key improvements of the detector.

Abe, T; Adamczyk, K; Ahn, S; Aihara, H; Akai, K; Aloi, M; Andricek, L; Aoki, K; Arai, Y; Arefiev, A; Arinstein, K; Arita, Y; Asner, D M; Aulchenko, V; Aushev, T; Aziz, T; Bakich, A M; Balagura, V; Ban, Y; Barberio, E; Barvich, T; Belous, K; Bergauer, T; Bhardwaj, V; Bhuyan, B; Blyth, S; Bondar, A; Bonvicini, G; Bozek, A; Bracko, M; Brodzicka, J; Brovchenko, O; Browder, T E; Cao, G; Chang, M -C; Chang, P; Chao, Y; Chekelian, V; Chen, A; Chen, K -F; Chen, P; Cheon, B G; Chiang, C -C; Chistov, R; Cho, K; Choi, S -K; Chung, K; Comerma, A; Cooney, M; Cowley, D E; Critchlow, T; Dalseno, J; Danilov, M; Dieguez, A; Dierlamm, A; Dillon, M; Dingfelder, J; Dolenec, R; Dolezal, Z; Drasal, Z; Drutskoy, A; Dungel, W; Dutta, D; Eidelman, S; Enomoto, A; Epifanov, D; Esen, S; Fast, J E; Feindt, M; Garcia, M Fernandez; Fifield, T; Fischer, P; Flanagan, J; Fourletov, S; Fourletova, J; Freixas, L; Frey, A; Friedl, M; Fruehwirth, R; Fujii, H; Fujikawa, M; Fukuma, Y; Funakoshi, Y; Furukawa, K; Fuster, J; Gabyshev, N; Cueto, A Gaspar de Valenzuela; Garmash, A; Garrido, L; Geisler, Ch; Gfall, I; Goh, Y M; Golob, B; Gorton, I; Grzymkowski, R; Guo, H; Ha, H; Haba, J; Hara, K; Hara, T; Haruyama, T; Hayasaka, K; Hayashi, K; Hayashii, H; Heck, M; Heindl, S; Heller, C; Hemperek, T; Higuchi, T; Horii, Y; Hou, W -S; Hsiung, Y B; Huang, C -H; Hwang, S; Hyun, H J; Igarashi, Y; Iglesias, C; Iida, Y; Iijima, T; Imamura, M; Inami, K; Irmler, C; Ishizuka, M; Itagaki, K; Itoh, R; Iwabuchi, M; Iwai, G; Iwai, M; Iwasaki, M; Iwasaki, M; Iwasaki, Y; Iwashita, T; Iwata, S; Jang, H; Ji, X; Jinno, T; Jones, M; Julius, T; Kageyama, T; Kah, D H; Kakuno, H; Kamitani, T; Kanazawa, K; Kapusta, P; Kataoka, S U; Katayama, N; Kawai, M; Kawai, Y; Kawasaki, T; Kennedy, J; Kichimi, H; Kikuchi, M; Kiesling, C; Kim, B K; Kim, G N; Kim, H J; Kim, H O; Kim, J -B; Kim, J H; Kim, M J; Kim, S K; Kim, K T; Kim, T Y; Kinoshita, K; Kishi, K; Kisielewski, B; van Dam, K Kleese; Knopf, J; Ko, B R; Koch, M; Kodys, P; Koffmane, C; Koga, Y; Kohriki, T; Koike, S; Koiso, H; Kondo, Y; Korpar, S; Kouzes, R T; Kreidl, Ch; Kreps, M; Krizan, P; Krokovny, P; Krueger, H; Kruth, A; Kuhn, W; Kuhr, T; Kumar, R; Kumita, T; Kupper, S; Kuzmin, A; Kvasnicka, P; Kwon, Y -J; Lacasta, C; Lange, J S; Lee, I -S; Lee, M J; Lee, M W; Lee, S -H; Lemarenko, M; Li, J; Li, W D; Li, Y; Libby, J; Limosani, A; Liu, C; Liu, H; Liu, Y; Liu, Z; Liventsev, D; Virto, A Lopez; Makida, Y; Mao, Z P; Marinas, C; Masuzawa, M; Matvienko, D; Mitaroff, W; Miyabayashi, K; Miyata, H; Miyazaki, Y; Miyoshi, T; Mizuk, R; Mohanty, G B; Mohapatra, D; Moll, A; Mori, T; Morita, A; Morita, Y; Moser, H -G; Martin, D Moya; Mueller, T; Muenchow, D; Murakami, J; Myung, S S; Nagamine, T; Nakamura, I; Nakamura, T T; Nakano, E; Nakano, H; Nakao, M; Nakazawa, H; Nam, S -H; Natkaniec, Z; Nedelkovska, E; Negishi, K; Neubauer, S; Ng, C; Ninkovic, J; Nishida, S; Nishimura, K; Novikov, E; Nozaki, T; Ogawa, S; Ohmi, K; Ohnishi, Y; Ohshima, T; Ohuchi, N; Oide, K; Olsen, S L; Ono, M; Ono, Y; Onuki, Y; Ostrowicz, W; Ozaki, H; Pakhlov, P; Pakhlova, G; Palka, H; Park, H; Park, H K; Peak, L S; Peng, T; Peric, I; Pernicka, M; Pestotnik, R; Petric, M; Piilonen, L E; Poluektov, A; Prim, M; Prothmann, K; Regimbal, K; Reisert, B; Richter, R H; Riera-Babures, J; Ritter, A; Ritter, A; Ritter, M; Roehrken, M; Rorie, J; Rosen, M; Rozanska, M; Ruckman, L; Rummel, S; Rusinov, V; Russell, R M; Ryu, S; Sahoo, H; Sakai, K; Sakai, Y; Santelj, L; Sasaki, T; Sato, N; Sato, Y; Scheirich, J; Schieck, J; Schwanda, C; Schwartz, A J; Schwenker, B; Seljak, A; Senyo, K; Seon, O -S; Sevior, M E; Shapkin, M; Shebalin, V; Shen, C P; Shibuya, H; Shiizuka, S; Shiu, J -G; Shwartz, B; Simon, F; Simonis, H J; Singh, J B; Sinha, R; Sitarz, M; Smerkol, P; Sokolov, A; Solovieva, E; Stanic, S; Staric, M; Stypula, J; Suetsugu, Y; Sugihara, S; Sugimura, T; Sumisawa, K; Sumiyoshi, T; Suzuki, K; Suzuki, S Y; Takagaki, H; Takasaki, F; Takeichi, H; Takubo, Y; Tanaka, M; Tanaka, S; Taniguchi, N; Tarkovsky, E; Tatishvili, G; Tawada, M; Taylor, G N; Teramoto, Y; Tikhomirov, I; Trabelsi, K; Tsuboyama, T; Tsunada, K; Tu, Y -C; Uchida, T; Uehara, S; Ueno, K; Uglov, T; Unno, Y; Uno, S; Urquijo, P; Ushiroda, Y; Usov, Y; Vahsen, S; Valentan, M; Vanhoefer, P; Varner, G; Varvell, K E; Vazquez, P; Vila, I; Vilella, E; Vinokurova, A; Visniakov, J; Vos, M; Wang, C H; Wang, J; Wang, M -Z; Wang, P; Wassatch, A; Watanabe, M; Watase, Y; Weiler, T; Wermes, N; Wescott, R E; White, E; Wicht, J; Widhalm, L; Williams, K M; Won, E; Xu, H; Yabsley, B D; Yamamoto, H; Yamaoka, H; Yamaoka, Y; Yamauchi, M; Yin, Y; Yoon, H; Yu, J; Yuan, C Z; Yusa, Y; Zander, D; Zdybal, M; Zhang, Z P; Zhao, J; Zhao, L; Zhao, Z; Zhilich, V; Zhou, P; Zhulanov, V; Zivko, T; Zupanc, A; Zyukova, O

2010-01-01T23:59:59.000Z

329

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

330

THE SPECTRUM OF Fe II  

SciTech Connect

The spectrum of singly ionized iron (Fe II) has been recorded using high-resolution Fourier transform (FT) and grating spectroscopy over the wavelength range 900 A to 5.5 {mu}m. The spectra were observed in high-current continuous and pulsed hollow cathode discharges using FT spectrometers at the Kitt Peak National Observatory, Tucson, AZ and Imperial College, London and with the 10.7 m Normal Incidence Spectrograph at the National Institute of Standards and Technology. Roughly 12,900 lines were classified using 1027 energy levels of Fe II that were optimized to measured wavenumbers. The wavenumber uncertainties of lines in the FT spectra range from 10{sup -4} cm{sup -1} for strong lines around 4 {mu}m to 0.05 cm{sup -1} for weaker lines around 1500 A. The wavelength uncertainty of lines in the grating spectra is 0.005 A. The ionization energy of (130,655.4 {+-} 0.4) cm{sup -1} was estimated from the 3d{sup 6}({sup 5}D)5g and 3d{sup 6}({sup 5}D)6h levels.

Nave, Gillian [National Institute of Standards and Technology, Gaithersburg, MD 20899-8422 (United States); Johansson, Sveneric, E-mail: gillian.nave@nist.gov [Lund Observatory, University of Lund, Box 43, SE-22100 Lund (Sweden)

2013-01-15T23:59:59.000Z

331

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

332

Start II, red ink, and Boris Yeltsin  

SciTech Connect

Apart from the vulnerability implied by the START II treaty, it will bear the burden of the general political opposition to the Yeltsin administration. START II will be seen as part of an overall Yeltsin-Andrei Kozyrev foreign policy that is under fire for selling out Russian national interests in Yugoslavia, the Persian Gulf, and elsewhere. This article discusses public opinion concerning START II, the cost of its implementation, and the general purpose of the treaty.

Arbatov, A.

1993-04-01T23:59:59.000Z

333

Comparative study on kinetic adsorption of Cu(II), Cd(II) and Ni(II) ions from aqueous solutions using activated sludge and dried sludge  

Science Journals Connector (OSTI)

The adsorption of Cu(II), Cd(II) and Ni(II) ions from aqueous solutions by activated sludge and dried sludge was investigated under laboratory conditions to assess ... The adsorption behavior of metal ions onto a...

Soon-An Ong; Eiichi Toorisaka; Makoto Hirata; Tadashi Hano

2013-03-01T23:59:59.000Z

334

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

335

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

SciTech Connect

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

336

Near-Infrared [Fe II] and H2 Line Observations of the Supernova Remnant 3C 396: Probing the Pre-supernova Circumstellar Materials  

E-Print Network (OSTI)

We present the results of near-infrared [Fe II] and H2 line imaging and spectroscopic observations of the supernova remnant 3C 396 using the Palomar 5 m Hale telescope. We detect long, filamentary [Fe II] emission delineating the inner edge of the radio emission in the western boundary of the remnant in imaging observations, together with a bright [Fe II] emission clump close to the remnant center. There appears to be faint, diffuse [Fe II] emission between the central clump and the western filamentary emission. The spectroscopic observations determine the expansion velocity of the central clump to be ~56 km/s. This is far smaller than the expansion velocity of 3C 396 obtained from X-ray observations, implying the inhomogeneity of the ambient medium. The electron number density of the [Fe II] emission gas is < 2,000 cm-3. The H2 line emission, on the other hand, lies slightly outside the filamentary [Fe II] emission in the western boundary, and forms a rather straight filament. We suggest that the [Fe II] emission represents dense clumps in the wind material from the red supergiant phase of a Type IIL/b progenitor of 3C 396 which have been swept up by the supernova remnant shocks. The H2 emission may represent either the boundary of a wind bubble produced during the main-sequence phase of the progenitor or molecular clumps left over inside the bubble. We propose that the near-infrared [Fe II] and H2 emission observed in several supernova remnants of Type IIL/b SNe likely has the same origin.

Ho-Gyu Lee; Dae-Sik Moon; Bon-Chul Koo; Jae-Joon Lee; Keith Matthews

2008-10-05T23:59:59.000Z

337

Site Environmental Report for 2008, Volume II  

E-Print Network (OSTI)

Air; Soil Creeks; Rainwater; Stormwater; Sewer Sewer AmbientAir Ambient Air Rainwater Creeks Stormwater Sewer FixedII section Stormwater Ambient Air; Rainwater Ambient Air

Lackner, Regina

2009-01-01T23:59:59.000Z

338

Mass Spectrometer: Single Particle (SPLAT II) | EMSL  

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

and micro-scales. SPLAT II's applications include but are not limited to climate, air pollution, human health, bioterrorism, and emerging nanotechnologies. Portability is a...

339

ACCURATE RITZ WAVELENGTHS OF PARITY-FORBIDDEN [Co II] AND [V II] LINES OF ASTROPHYSICAL INTEREST  

SciTech Connect

We report a comprehensive list of accurate Ritz wavelengths for parity-forbidden [Co II] and [V II] lines obtained from the analysis of energy levels measured in the laboratory with Fourier transform emission spectroscopy. Such lines, particularly those in the infrared, are in demand for the analysis of low-density astrophysical plasmas in and around objects such as planetary nebulae, star-forming regions, and active galactic nuclei. Transitions between all known metastable levels of Co II and V II are included in our analysis, producing wavelengths for 1477 [V II] lines and 782 [Co II] lines. Of these, 170 [V II] lines and 171 [Co II] lines arise from transitions with calculated transition probabilities greater than 1 Multiplication-Sign 10{sup -2} s{sup -1} and upper level excitations of less than 5 eV, and thus are likely to be observed in astrophysical spectra.

Ruffoni, M. P.; Pickering, J. C., E-mail: m.ruffoni@imperial.ac.uk [Blackett Laboratory, Department of Physics, Imperial College London, London SW7 2AZ (United Kingdom)

2013-08-15T23:59:59.000Z

340

NEWLY IDENTIFIED EXTENDED GREEN OBJECTS (EGOs) FROM THE SPITZER GLIMPSE II SURVEY. I. CATALOG  

SciTech Connect

We have produced a catalog containing 98 newly identified massive young stellar object (MYSO) candidates associated with ongoing outflows (known as extended green objects, or EGOs). These have been identified from the Spitzer Galactic Legacy Infrared Mid-Plane Survey Extraordinaire (GLIMPSE) II data set and our new identifications increase the number of known EGOs to {approx}400 in our Galaxy, adding to the {approx}300 previously identified EGOs reported by Cyganowski et al. from the GLIMPSE I survey. The high detection rate ({approx}70%) of 95 GHz class I methanol masers achieved in a survey toward 57 of these new EGOs with the Mopra 22 m radio telescope demonstrates that the new EGOs are associated with outflows. Investigations of the mid-infrared properties and physical associations with other star formation tracers (e.g., infrared dark clouds, class I and II methanol masers, and millimeter Bolocam Galactic Plane Survey sources) reveal that the newly identified EGOs are very similar in nature to those in the sample of Cyganowski et al. All of the observational evidence supports the hypothesis that EGOs correspond to MYSOs at the earliest evolutionary stage, with ongoing outflow activity, and active rapid accretion.

Chen, Xi; Gan, Cong-Gui; Shen, Zhi-Qiang [Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030 (China)] [Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030 (China); Ellingsen, Simon P.; Titmarsh, Anita [School of Mathematics and Physics, University of Tasmania, Hobart, Tasmania (Australia)] [School of Mathematics and Physics, University of Tasmania, Hobart, Tasmania (Australia); He, Jin-Hua, E-mail: chenxi@shao.ac.cn [Key Laboratory for the Structure and Evolution of Celestial Objects, Yunnan Astronomical Observatory/National Astronomical Observatory, Chinese Academy of Sciences, P.O. Box 110, Kunming, 650011 Yunnan Province (China)] [Key Laboratory for the Structure and Evolution of Celestial Objects, Yunnan Astronomical Observatory/National Astronomical Observatory, Chinese Academy of Sciences, P.O. Box 110, Kunming, 650011 Yunnan Province (China)

2013-05-01T23:59:59.000Z

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.


341

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

SciTech Connect

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

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

2012-05-01T23:59:59.000Z

342

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

SciTech Connect

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

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

2012-02-20T23:59:59.000Z

343

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

E-Print Network (OSTI)

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

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

2015-01-01T23:59:59.000Z

344

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

SciTech Connect

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

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

2009-05-11T23:59:59.000Z

345

BUSCA A Telescope Instrumentation for Simultaneous Imaging in 4 Optical Bands  

E-Print Network (OSTI)

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

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

1999-01-01T23:59:59.000Z

346

IceCube-Plus: An Ultra-High Energy Neutrino Telescope  

E-Print Network (OSTI)

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

Halzen, F; Halzen, Francis; Hooper, Dan

2004-01-01T23:59:59.000Z

347

IceCube-Plus: An Ultra-High Energy Neutrino Telescope  

E-Print Network (OSTI)

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

Francis Halzen; Dan Hooper

2003-12-22T23:59:59.000Z

348

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

SciTech Connect

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

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

2013-10-01T23:59:59.000Z

349

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

E-Print Network (OSTI)

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

Yang, Shuhong; Xiang, Yongyuan

2014-01-01T23:59:59.000Z

350

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

E-Print Network (OSTI)

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

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

2008-06-01T23:59:59.000Z

351

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

E-Print Network (OSTI)

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

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

2007-09-17T23:59:59.000Z

352

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

E-Print Network (OSTI)

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

Godon, P; Starrfield, S; Livio, M; Williams, R E; Woodward, C E; Kuin, P; Page, K L

2014-01-01T23:59:59.000Z

353

Hubble Space Telescope ACS mosaic of the prototypical starburst galaxy M82  

E-Print Network (OSTI)

In March 2006, the Hubble Heritage Team obtained a large four-filter (B, V, I, and H-alpha) six-point mosaic dataset of the prototypical starburst galaxy NGC 3034 (M82), with the Advanced Camera for Surveys (ACS) onboard the Hubble Space Telescope (HST). The resulting color composite Heritage image was released in April 2006, to celebrate Hubble's 16th anniversary. Cycle 15 HST proposers were encouraged to submit General Observer and Archival Research proposals to complement or analyze this unique dataset. Since our M82 mosaics represent a significant investment of expert processing beyond the standard archival products, we will also release our drizzle combined FITS data as a High Level Science Product via the Multimission Archive at STScI (MAST) on December 31, 2006. This paper documents the key aspects of the observing program and image processing: calibration, image registration and combination (drizzling), and the rejection of cosmic rays and detector artifacts. Our processed FITS mosaics and related inf...

Mutchler, M; Christian, C A; Frattare, L M; Hamilton, F; Januszewski, W; Levay, Z G; Mountain, M; Noll, K S; Royle, P; Gallagher, J S; Puxley, P

2006-01-01T23:59:59.000Z

354

Atmospheric Characterization of 5 Hot Jupiters with Wide Field Camera 3 on the Hubble Space Telescope  

E-Print Network (OSTI)

We probe the structure and composition of the atmospheres of 5 hot Jupiter exoplanets using the Hubble Space Telescope Wide Field Camera 3 (WFC3) instrument. We use the G141 grism (1.1-1.7 $\\mu$m) to study TrES-2b, TrES-4b, and CoRoT-1b in transit, TrES-3b in secondary eclipse, and WASP-4b in both. This wavelength region includes a predicted absorption feature from water at 1.4 $\\mu$m, which we expect to be nondegenerate with the other molecules that are likely to be abundant for hydrocarbon-poor (e.g. solar composition) hot Jupiter atmospheres. We divide our wavelength regions into 10 bins. For each bin we produce a spectrophotometric light curve spanning the time of transit and/or eclipse. We correct these light curves for instrumental systematics without reference to an instrument model. For our transmission spectra, our mean $1-\\sigma$ precision per bin corresponds to variations of 2.1, 2.8, and 3.0 atmospheric scale heights for TrES-2b, TrES-4b, and CoRoT-1b, respectively. We find featureless spectra for...

Ranjan, Sukrit; Désert, Jean-Michel; Madhusudhan, Nikku; Deming, Drake; Wilkins, Ashlee; Mandell, Avi M

2014-01-01T23:59:59.000Z

355

Development of mirrors made of chemically tempered glass foils for future X-ray telescopes  

E-Print Network (OSTI)

Thin slumped glass foils are considered good candidates for the realization of future X-ray telescopes with large effective area and high spatial resolution. However, the hot slumping process affects the glass strength, and this can be an issue during the launch of the satellite because of the high kinematical and static loads occurring during that phase. In the present work we have investigated the possible use of Gorilla glass (produced by Corning), a chemical tempered glass that, thanks to its strength characteristics, would be ideal. The un-tempered glass foils were curved by means of an innovative hot slumping technique and subsequently chemically tempered. In this paper we show that the chemical tempering process applied to Gorilla glass foils does not affect the surface micro-roughness of the mirrors. On the other end, the stress introduced by the tempering process causes a reduction in the amplitude of the longitudinal profile errors with a lateral size close to the mirror length. The effect of the ov...

Salmaso, B; Brizzolari, B; Basso, S; Ghigo, M; Pareschi, G; Spiga, D; Proserpio, L; Suppiger, Y

2015-01-01T23:59:59.000Z

356

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

357

ULTRASPEC: a high-speed imaging photometer on the 2.4-m Thai National Telescope  

E-Print Network (OSTI)

ULTRASPEC is a high-speed imaging photometer mounted permanently at one of the Nasmyth focii of the 2.4-m Thai National Telescope (TNT) on Doi Inthanon, Thailand's highest mountain. ULTRASPEC employs a 1024x1024 pixel frame-transfer, electron-multiplying CCD (EMCCD) in conjunction with re-imaging optics to image a field of 7.7'x7.7' at (windowed) frame rates of up to ~200 Hz. The EMCCD has two outputs - a normal output that provides a readout noise of 2.3 e- and an avalanche output that can provide essentially zero readout noise. A six-position filter wheel enables narrow-band and broad-band imaging over the wavelength range 330-1000 nm. The instrument saw first light on the TNT in November 2013 and will be used to study rapid variability in the Universe. In this paper we describe the scientific motivation behind ULTRASPEC, present an outline of its design and report on its measured performance on the TNT.

Dhillon, V S; Atkinson, D C; Bezawada, N; Bours, M C P; Copperwheat, C M; Gamble, T; Hardy, L K; Hickman, R D H; Irawati, P; Ives, D J; Kerry, P; Leckngam, A; Littlefair, S P; McLay, S A; O'Brien, K; Peacocke, P T; Poshyachinda, S; Richichi, A; Soonthornthum, B; Vick, A

2014-01-01T23:59:59.000Z

358

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

359

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.

360

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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361

SWAMI II technology transfer plan  

SciTech Connect

Thousands of drums of radioactive/hazardous/mixed waste are currently stored at DOE sites throughout US; they are stored in warehouse facilities on an interim basis, pending final disposition. Recent emphasis on anticipated decommissioning of facilities indicates that many more drums of waste will be generated, requiring additional storage. Federal and state regulations dictate that hazardous waste covered by RCRA be inspected periodically for container degradation and to verify inventories. All known DOE waste storage facilities are currently inspected manually. A system to perform robotic inspection of waste drums is under development by the SRTC Robotics Group of WSRC; it is called the Stored Waste Autonomous Mobile Inspector (SWAMI). The first version, SWAMI I, was developed by the Savannah River Technology Center (SRTC) as a proof of principle system for autonomous inspection of drums in a warehouse. SWAMI I was based on the Transitions Research Corporation (TRC) HelpMate mobile robot. TRC modified the Helpmate to navigate in aisles of drums. SRTC added subsystems to SWAMI I to determine its position in open areas, read bar code labels on the drums up to three levels high, capture images of the drums and perform a radiation survey of the floor in the aisles. The radiation survey was based on SRTC patented technology first implemented on the Semi-Intelligent Mobile Observing Navigator (SIMON). The radiation survey is not essential for the inspection of drums, but is an option that can increase the utility and effectiveness of SWAMI in warehouses with radioactive and/or mixed waste. All the sensors on SWAMI I were fixed on the vehicle. From the success of SWAMI I, a second version, SWAMI II, was developed; it will be evaluated at Fernald and tested with two other mobile robots. Intent is to transfer the technology developed for SWAMI I and II to industry so that it can supply additional units for purchase for drum inspection.

Ward, C.R.; Peterson, K.D.; Harpring, L.J.; Immel, D.M.; Jones, J.D.; Mallet, W.R.

1995-12-31T23:59:59.000Z

362

Ii.p'r":~.~~  

E-Print Network (OSTI)

HISTORY LITERATURE - Select 9 hours MUS 3114 Symphonic Literature 3 MUS 3124 20th Century Literature 3 MUS MUS 3055 Music and Media Production I 3 MUS 3056 Music and Media Production II 3 MUS 3065 Camp. Mus. and Multimedia I 3 MUS 3066 Camp. Mus. and Multimedia II 3 (1) __ (1) __ (1) __ (1) __ (1) __ (1)-_ VIII

Virginia Tech

363

LABORATORY II ELECTRIC FIELDS AND ELECTRIC POTENTIALS  

E-Print Network (OSTI)

Lab II - 1 LABORATORY II ELECTRIC FIELDS AND ELECTRIC POTENTIALS In this lab you will continue to investigate the abstract concept of electric field. If you know the electric field at a point in space, you). With this simulation you can construct a complicated charge configuration and read out the resulting electric field

Minnesota, University of

364

Part II: Project Summaries Project Summaries  

E-Print Network (OSTI)

Part II: Project Summaries Part II Project Summaries #12;22 Math & Computational Sciences Division generally cannot be achieved for reasonable computational cost. Applications that require modeling of this project is to advance the state of the art in electromagnetic computations by eliminating three existing

Perkins, Richard A.

365

Title II Disposal Sites Annual Report  

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

This report presents the results of long-term surveillance and maintenance activities conducted by the DOE Office of Legacy Management in 2013 at six uranium mill tailings disposal sites reclaimed under Title II of the Uranium Mill Tailings Radiation Control Act (UMTRCA) of 1978. These activities verified that the UMTRCA Title II disposal sites remain in compliance with license requirements.

366

Exoplanet Science with the European Extremely Large Telescope. The Case for Visible and Near-IR Spectroscopy at High Resolution  

E-Print Network (OSTI)

Exoplanet science is booming. In 20 years our knowledge has expanded considerably, from the first discovery of a Hot Jupiter, to the detection of a large population of Neptunes and super-Earths, to the first steps toward the characterization of exoplanet atmospheres. Between today and 2025, the field will evolve at an even faster pace with the advent of several space-based transit search missions, ground-based spectrographs, high-contrast imaging facilities, and the James Webb Space Telescope. Especially the ESA M-class PLATO mission will be a game changer in the field. From 2024 onwards, PLATO will find transiting terrestrial planets orbiting within the habitable zones of nearby, bright stars. These objects will require the power of Extremely Large Telescopes (ELTs) to be characterized further. The technique of ground-based high-resolution spectroscopy is establishing itself as a crucial pathway to measure chemical composition, atmospheric structure and atmospheric circulation in transiting exoplanets. A hig...

Udry, S; Bouchy, F; Cameron, A Collier; Henning, T; Mayor, M; Pepe, F; Piskunov, N; Pollacco, D; Queloz, D; Quirrenbach, A; Rauer, H; Rebolo, R; Santos, N C; Snellen, I; Zerbi, F

2014-01-01T23:59:59.000Z

367

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.

368

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":""}]}

369

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":""}]}

370

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

371

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":""}]}

372

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

373

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

374

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

375

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

376

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.

377

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":""}]}

378

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":""}]}

379

The Introduction of Tech Pan lm at the UK Schmidt Telescope Quentin A Parker 1;3 David Malin 2  

E-Print Network (OSTI)

The Introduction of Tech Pan #12;lm at the UK Schmidt Telescope Quentin A Parker 1;3 David Malin 2.parker@roe.ac.uk Abstract Kodak Technical Pan (Tech Pan) emulsion on a #12;lm base has been in use at the U.K. Schmidt 1981), though it was introduced somewhat earlier as 35mm solar patrol #12;lm (as special order SO-115

Tittley, Eric

380

AN INITIAL LOOK AT THE FAR-INFRAREDRADIO CORRELATION WITHIN NEARBY STAR-FORMING GALAXIES USING THE SPITZER SPACE TELESCOPE  

E-Print Network (OSTI)

THE SPITZER SPACE TELESCOPE E. J. Murphy,1 R. Braun,2 G. Helou,3 L. Armus,3 J. D. P. Kenney,1 K. D. Gordon,4 G. Cannon,6 B. T. Draine,8 C. W. Engelbracht,4 D. J. Hollenbach,9 T. H. Jarrett,3 L. J. Kewley,10 C. Leitherer,7 A. Li,11 M. J. Meyer,7 M. W. Regan,7 G. H. Rieke,4 M. J. Rieke,4 H. Roussel,3 K. Sheth,3 J. D. T

Draine, Bruce T.

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.


381

New Results from Observations of Massive Star Formation in the Mid-Infrared with Large Aperture Telescopes  

E-Print Network (OSTI)

Thanks to the high spatial resolution afforded by 8-10m class telescopes, we are beginning to learn that some sources are extended in their mid-infrared emission because of dusty outflows or heated outflow cavity walls. Therefore one must be extremely careful in interpreting the nature of extended mid-infrared sources (i.e. just because it is extended does not automatically mean it is a disk!).

James M. De Buizer

2006-10-18T23:59:59.000Z

382

Nickel(II) and copper(II) complexes with pyridine-containing macrocycles bearing an aminopropyl pendant arm: synthesis,  

E-Print Network (OSTI)

Nickel(II) and copper(II) complexes with pyridine-containing macrocycles bearing an aminopropyl that were used for the preparation of the copper(II) complexes. The structures of three nickel(II) complexes and two copper(II) complexes were determined by X-ray crystallography. Protonation of the pendant arm (p

Nazarenko, Alexander

383

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

E-Print Network (OSTI)

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

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

2007-08-04T23:59:59.000Z

384

PARS II CPP Upload Template File | Department of Energy  

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

teProjectTemplate.zip More Documents & Publications Proposed Data Elements for PARS II Web Application PARS II - Integrated Project Team Meeting PARS II End-of-Month Checklist...

385

HUBBLE SPACE TELESCOPE AND GROUND-BASED OBSERVATIONS OF V455 ANDROMEDAE POST-OUTBURST  

SciTech Connect

Hubble Space Telescope spectra obtained in 2010 and 2011, 3 and 4 yr after the large amplitude dwarf nova outburst of V455 And, were combined with optical photometry and spectra to study the cooling of the white dwarf, its spin, and possible pulsation periods after the outburst. The modeling of the ultraviolet (UV) spectra shows that the white dwarf temperature remains ?600 K hotter than its quiescent value at 3 yr post-outburst, and still a few hundred degrees hotter at 4 yr post-outburst. The white dwarf spin at 67.6 s and its second harmonic at 33.8 s are visible in the optical within a month of outburst and are obvious in the later UV observations in the shortest wavelength continuum and the UV emission lines, indicating an origin in high-temperature regions near the accretion curtains. The UV light curves folded on the spin period show a double-humped modulation consistent with two-pole accretion. The optical photometry 2 yr after outburst shows a group of frequencies present at shorter periods (250-263 s) than the periods ascribed to pulsation at quiescence, and these gradually shift toward the quiescent frequencies (300-360 s) as time progresses past outburst. The most surprising result is that the frequencies near this period in the UV data are only prominent in the emission lines, not the UV continuum, implying an origin away from the white dwarf photosphere. Thus, the connection of this group of periods with non-radial pulsations of the white dwarf remains elusive.

Szkody, Paula; Mukadam, Anjum S.; Brown, Justin; Funkhouser, Kelsey [Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195 (United States); Gänsicke, Boris T. [Department of Physics, University of Warwick, Coventry CV4 7AL (United Kingdom); Henden, Arne [AAVSO, 49 Bay State Road, Cambridge, MA 02138 (United States); Sion, Edward M. [Department of Astronomy and Astrophysics, Villanova University, Villanova, PA 19085 (United States); Townsley, Dean M. [Department of Physics and Astronomy, University of Alabama, Tuscaloosa, AL 35487 (United States); Christian, Damian [Department of Physics and Astronomy, California State University, Northridge, CA 91330 (United States); Falcon, Ross E. [Department of Astronomy, University of Texas, Austin, TX 78712 (United States); Pyrzas, Stylianos, E-mail: szkody@astro.washington.edu, E-mail: anjum@astro.washington.edu, E-mail: boris.gaensicke@warwick.ac.uk, E-mail: arne@aavso.org, E-mail: edward.sion@villanova.edu, E-mail: Dean.M.Townsley@ua.edu, E-mail: damian.christian@csun.edu, E-mail: cylver@astro.as.utexas.edu, E-mail: stylianos.pyrzas@gmail.com [Instituto de Astronomia, Universidad Catolica del Norte, Avenida Angamos 0619, Antofagasta (Chile)

2013-09-20T23:59:59.000Z

386

HUBBLE SPACE TELESCOPE PIXEL ANALYSIS OF THE INTERACTING S0 GALAXY NGC 5195 (M51B)  

SciTech Connect

We report the properties of the interacting S0 galaxy NGC 5195 (M51B), revealed in a pixel analysis using the Hubble Space Telescope/Advanced Camera for Surveys images in the F435W, F555W, and F814W (BVI) bands. We analyze the pixel color-magnitude diagram (pCMD) of NGC 5195, focusing on the properties of its red and blue pixel sequences and the difference from the pCMD of NGC 5194 (M51A; the spiral galaxy interacting with NGC 5195). The red pixel sequence of NGC 5195 is redder than that of NGC 5194, which corresponds to the difference in the dust optical depth of 2 < {Delta}{tau}{sub V} < 4 at fixed age and metallicity. The blue pixel sequence of NGC 5195 is very weak and spatially corresponds to the tidal bridge between the two interacting galaxies. This implies that the blue pixel sequence is not an ordinary feature in the pCMD of an early-type galaxy, but that it is a transient feature of star formation caused by the galaxy-galaxy interaction. We also find a difference in the shapes of the red pixel sequences on the pixel color-color diagrams (pCCDs) of NGC 5194 and NGC 5195. We investigate the spatial distributions of the pCCD-based pixel stellar populations. The young population fraction in the tidal bridge area is larger than that in other areas by a factor >15. Along the tidal bridge, young populations seem to be clumped particularly at the middle point of the bridge. On the other hand, the dusty population shows a relatively wide distribution between the tidal bridge and the center of NGC 5195.

Lee, Joon Hyeop; Kim, Sang Chul; Ree, Chang Hee; Kim, Minjin; Jeong, Hyunjin; Lee, Jong Chul; Kyeong, Jaemann, E-mail: jhl@kasi.re.kr, E-mail: sckim@kasi.re.kr, E-mail: chr@kasi.re.kr, E-mail: mkim@kasi.re.kr, E-mail: hyunjin@kasi.re.kr, E-mail: jclee@kasi.re.kr, E-mail: jman@kasi.re.kr [Korea Astronomy and Space Science Institute, Daejeon 305-348 (Korea, Republic of)

2012-08-01T23:59:59.000Z

387

ON THE FERMI LARGE AREA TELESCOPE SURPLUS OF DIFFUSE GALACTIC GAMMA-RAY EMISSION  

SciTech Connect

Recent observations of diffuse Galactic ?-ray emission (DGE) by the Fermi Large Area Telescope (Fermi-LAT) have shown significant deviations, above a few GeV to about 100 GeV, from DGE models that use the GALPROP code for the propagation of cosmic ray (CR) particles outside their sources in the Galaxy and their interaction with the target distributions of the interstellar gas and radiation fields. The surplus of radiation observed is most pronounced in the inner Galaxy, where the concentration of CR sources is strongest. The present study investigates this 'Fermi-LAT Galactic Plane Surplus' by estimating the ?-ray emission from the sources themselves, which is disregarded in the above DGE models. It is shown that the expected hard spectrum of CRs, still confined in their sources (source cosmic rays, SCRs), can indeed explain this surplus. The method is based on earlier studies regarding the so-called EGRET GeV excess, which by now is generally interpreted as an instrumental effect. The contribution from SCRs is also predicted to increasingly exceed the DGE models above 100 GeV, up to ?-ray energies of about 10 TeV, where the corresponding surplus exceeds the hadronic part of the DGE by about one order of magnitude. Above such energies, the emission surplus should decrease again with energy due to the finite lifetime of the assumed supernova remnant sources. Observations of the DGE in the inner Galaxy at 15 TeV with the ground-based Milagro ?-ray detector and, at TeV energies, with the ARGO-YBJ detector are interpreted to provide confirmation of a significant SCR contribution to the DGE.

Völk, H. J. [Max-Planck-Institut für Kernphysik, P.O. Box 103980, D-69029 Heidelberg (Germany); Berezhko, E. G., E-mail: Heinrich.Voelk@mpi-hd.mpg.de [Yu. G. Shafer Institute of Cosmophysical Research and Aeronomy, 31 Lenin Avenue, 677980 Yakutsk (Russian Federation)

2013-11-10T23:59:59.000Z

388

HUBBLE SPACE TELESCOPE OBSERVATIONS OF DUSTY FILAMENTS IN HERCULES A: EVIDENCE FOR ENTRAINMENT  

SciTech Connect

We present U-, V-, and I-band images of the host galaxy of Hercules A (3C 348) obtained with HST/WFC3/UVIS. We find a network of dusty filaments which are more complex and extended than seen in earlier Hubble Space Telescope (HST) observations. The filaments are associated with a faint blue continuum light (possibly from young stars) and faint H{alpha} emission. It seems likely that the cold gas and dust has been stripped from a companion galaxy now seen as a secondary nucleus. There are dusty filaments aligned with the base of the jets on both eastern and western sides of the galaxy. The morphology of the filaments is different on the two sides-the western filaments are fairly straight, while the eastern filaments are mainly in two loop-like structures. We suggest that despite the difference in morphologies, both sets of filaments have been entrained in a slow-moving boundary layer outside the relativistic flow. As suggested by Fabian et al., magnetic fields in the filaments may stabilize them against disruption. We consider a speculative scenario to explain the relation between the radio source and the shock and cavities in the hot intracluster medium seen in the Chandra data. We suggest that the radio source originally ({approx}60 Myr ago) propagated along a position angle of {approx}35 Degree-Sign where it created the shock and cavities. The radio source axis changed to its current orientation ({approx}100 Degree-Sign ) possibly due to a supermassive black hole merger and began its current epoch of activity about 20 Myr ago.

O'Dea, C. P.; Kharb, P. [School of Physics and Astronomy, and Laboratory for Multiwavelength Astrophysics, Rochester Institute of Technology, 84 Lomb Memorial Dr., Rochester, NY 14623 (United States); Baum, S. A. [Chester F. Carlson Center for Imaging Science, Rochester Institute of Technology, 84 Lomb Memorial Dr., Rochester, NY 14623 (United States); Tremblay, G. R. [European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748 Garching bei Muenchen (Germany); Cotton, W. [National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903 (United States); Perley, R. [National Radio Astronomy Observatory, P.O. Box 0, Socorro, NM 87801 (United States)

2013-07-01T23:59:59.000Z

389

A DUAL-BAND MILLIMETER-WAVE KINETIC INDUCTANCE CAMERA FOR THE IRAM 30 m TELESCOPE  

SciTech Connect

The Neel IRAM KIDs Array (NIKA) is a fully integrated measurement system based on kinetic inductance detectors (KIDs) currently being developed for millimeter wave astronomy. The instrument includes dual-band optics allowing simultaneous imaging at 150 GHz and 220 GHz. The imaging sensors consist of two spatially separated arrays of KIDs. The first array, mounted on the 150 GHz branch, is composed of 144 lumped-element KIDs. The second array (220 GHz) consists of 256 antenna-coupled KIDs. Each of the arrays is sensitive to a single polarization; the band splitting is achieved by using a grid polarizer. The optics and sensors are mounted in a custom dilution cryostat, with an operating temperature of {approx}70 mK. Electronic readout is realized using frequency multiplexing and a transmission line geometry consisting of a coaxial cable connected in series with the sensor array and a low-noise 4 K amplifier. The dual-band NIKA was successfully tested in 2010 October at the Institute for Millimetric Radio Astronomy (IRAM) 30 m telescope at Pico Veleta, Spain, performing in-line with laboratory predictions. An optical NEP was then calculated to be around 2 x 10{sup -16} W Hz{sup -1/2} (at 1 Hz) while under a background loading of approximately 4 pW pixel{sup -1}. This improvement in comparison with a preliminary run (2009) verifies that NIKA is approaching the target sensitivity for photon-noise limited ground-based detectors. Taking advantage of the larger arrays and increased sensitivity, a number of scientifically relevant faint and extended objects were then imaged including the Galactic Center SgrB2 (FIR1), the radio galaxy Cygnus A, and the NGC1068 Seyfert galaxy. These targets were all observed simultaneously in the 150 GHz and 220 GHz atmospheric windows.

Monfardini, A.; Benoit, A.; Bideaud, A.; Swenson, L.; Cruciani, A.; Camus, P.; Hoffmann, C. [Institut Neel, CNRS and Universite Joseph Fourier (UJF), Grenoble F-38042 (France); Desert, F. X. [Institut de Planetologie et d'Astrophysique, UJF and CNRS-INSU, Grenoble F-38041 (France); Doyle, S.; Ade, P.; Mauskopf, P.; Tucker, C. [Cardiff School of Physics and Astronomy, Cardiff University, Cardiff CF24 3AA (United Kingdom); Roesch, M.; Leclercq, S.; Schuster, K. F. [Institut de RadioAstronomie Millimetrique (IRAM), Saint Martin d'Heres F-38406 (France); Endo, A. [Kavli Institute of NanoScience, Delft University of Technology, 2628 CJ Delft (Netherlands); Baryshev, A.; Baselmans, J. J. A.; Ferrari, L.; Yates, S. J. C, E-mail: monfardini@grenoble.cnrs.fr [SRON, Netherlands Institute for Space Research, 3584 CA Utrecht and 9700 AV Groningen (Netherlands)

2011-06-01T23:59:59.000Z

390

Investigation of the spectrum of high-energy muons by the method of multiple interactions on the basis of data from the Baksan underground scintillation telescope  

Science Journals Connector (OSTI)

Experimental data obtained with the aid of the Baksan underground scintillation telescope over a long period of its operation are analyzed with the aim of searches for an excess flux of ultrahigh-energy (?100 TeV...

A. G. Bogdanov; R. P. Kokoulin; Yu. F. Novoseltsev…

2009-12-01T23:59:59.000Z

391

A Letter from the Rev. Mr. James Pound, Rector of Wanstead, F. R. S. to Dr. Jurin, Secr. R. S. concerning Observations Made with Mr. Hadley's Reflecting Telescope  

Science Journals Connector (OSTI)

...Mr. James Pound, Rector of Wanstead, F. R. S. to Dr. Jurin, Secr. R. S. concerning Observations Made with Mr. Hadley's Reflecting Telescope James Pound The Royal Society is collaborating with JSTOR to digitize, preserve, and extend access...

1722-01-01T23:59:59.000Z

392

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.

393

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.

394

NEPA Implementation Procedures: Appendices I, II, and III | Department...  

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

Implementation Procedures: Appendices I, II, and III NEPA Implementation Procedures: Appendices I, II, and III These appendices were prepared by the Council on Environmental...

395

ARM - Radiative Heating in Underexplored Bands Campaign-II (RHUBC...  

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

Eli Mlawer, Principal Investigator Dave Turner, Principal Investigator Radiative Heating in Underexplored Bands Campaign-II (RHUBC-II) At an elevation of more than 5000...

396

Contractor-specific Documentation & Information in PARS II |...  

Energy Savers (EERE)

Contractor-specific Documentation & Information in PARS II Contractor-specific Documentation & Information in PARS II DOE Office of Acquisition and Project Management established...

397

High Level Overview of DOE Biomass Logistics II Project Activities...  

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

High Level Overview of DOE Biomass Logistics II Project Activities High Level Overview of DOE Biomass Logistics II Project Activities Breakout Session 1B-Integration of Supply...

398

PARS II Data Quality Memorandum from Deputy Secretary Poneman...  

Energy Savers (EERE)

II Data Quality Memorandum from Deputy Secretary Poneman (June 19, 2012) PARS II Data Quality.pdf More Documents & Publications Project Assessment and Reporting System (PARS...

399

Newby Island II Biomass Facility | Open Energy Information  

Open Energy Info (EERE)

Island II Biomass Facility Facility Newby Island II Sector Biomass Facility Type Landfill Gas Location Santa Clara County, California Coordinates 37.2938907, -121.7195459...

400

Friction Stir Spot Welding of Advanced High Strength Steels II...  

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

II Friction Stir Spot Welding of Advanced High Strength Steels II 2011 DOE Hydrogen and Fuel Cells Program, and Vehicle Technologies Program Annual Merit Review and Peer Evaluation...

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.


401

Honda Gen II Insight HEV Accelerated Testing - August 2012  

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

Honda Gen II Insight HEV Accelerated Testing - August 2012 Two model year 2010 Honda Generation II Insight hybrid electric vehicles (HEVs) entered Accelerated testing during July...

402

Two-dimensional Radiative Transfer in Protostellar Envelopes. II. An Evolutionary Sequence  

Science Journals Connector (OSTI)

We present model spectral energy distributions (SEDs), colors, polarization, and images for an evolutionary sequence of a low-mass protostar from the early collapse stage (Class 0) to the remnant disk stage (Class III). We find a substantial overlap in colors and SEDs between protostars embedded in envelopes (Class 0-I) and T Tauri disks (Class II), especially at mid-IR wavelengths. Edge-on Class I-II sources show double-peaked SEDs, with a short-wavelength hump due to scattered light and a long-wavelength hump due to thermal emission. These are the bluest sources in mid-IR color-color diagrams. Since Class 0 and I sources are diffuse, the size of the aperture over which fluxes are integrated has a substantial effect on the computed colors, with larger aperture results showing significantly bluer colors. Viewed through large apertures, the Class 0 colors fall in the same regions of mid-IR color-color diagrams as Class I sources and are even bluer than Class II-III sources in some colors. It is important to take this into account when comparing color-color diagrams of star formation regions at different distances or different sets of observations of the same region. However, the near-IR polarization of the Class 0 sources is much higher than the Class I-II sources, providing a means to separate these evolutionary states. We varied the grain properties in the circumstellar envelope, allowing for larger grains in the disk midplane and smaller grains in the envelope. In comparing with models with the same grain properties throughout, we find that the SED of the Class 0 source is sensitive to the grain properties of the envelope only—that is, grain growth in the disk in Class 0 sources cannot be detected from the SED. Grain growth in disks of Class I sources can be detected at wavelengths greater than 100 ?m. Our image calculations predict that the diffuse emission from edge-on Class I and II sources should be detectable in the mid-IR with the Space Infrared Telescope Facility (SIRTF) in nearby star-forming regions (out to several hundred parsecs).

Barbara A. Whitney; Kenneth Wood; J. E. Bjorkman; Martin Cohen

2003-01-01T23:59:59.000Z

403

Microsoft Word - Vol II-091009.doc  

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

Volume II Volume II Institutional Controls Plan April 2010 U.S. Department of Energy Revision 4 Final This page intentionally left blank Emergency Contact Grand Junction 24-hour Monitored Security Telephone Number (877) 695-5322 This page intentionally left blank U.S. Department of Energy Comprehensive Legacy Management and Institutional Controls Plan Doc. No. S03496-4.0-Final Volume II-Institutional Controls Plan April 2010 Page i Contents Acronyms and Abbreviations ........................................................................................................ iii Executive Summary .........................................................................................................................v 1.0 Introduction......................................................................................................................1-1

404

Kibby Mountain II | Open Energy Information  

Open Energy Info (EERE)

Kibby Mountain II Kibby Mountain II Jump to: navigation, search Name Kibby Mountain II Facility Kibby Mountain II Sector Wind energy Facility Type Commercial Scale Wind Facility Status Under Construction Owner TransCanada Power Mktg Ltd Developer TransCanada Power Mktg Ltd Location Kibby Mountain ME Coordinates 45.354154°, -70.65412° 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":45.354154,"lon":-70.65412,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

405

Nobles Wind Farm II | Open Energy Information  

Open Energy Info (EERE)

Wind Farm II Wind Farm II Jump to: navigation, search Name Nobles Wind Farm II Facility Nobles Wind Farm II Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner Xcel Energy Developer EnXco Energy Purchaser Xcel Energy Location Nobles County MN Coordinates 43.682956°, -95.728425° 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":43.682956,"lon":-95.728425,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

406

Timber Road II | Open Energy Information  

Open Energy Info (EERE)

II II Jump to: navigation, search Name Timber Road II Facility Timber Road II Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner Horizon Wind Energy Developer Horizon Wind Energy Energy Purchaser American Electric Power Location Near Payne OH Coordinates 41.023524°, -84.717185° 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":41.023524,"lon":-84.717185,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

407

Little Pringle II | Open Energy Information  

Open Energy Info (EERE)

Pringle II Pringle II Jump to: navigation, search Name Little Pringle II Facility Little Pringle II Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner SWI Wind Farms Developer SWI Wind Farms Energy Purchaser Xcel Energy Location 50 miles north of Amarillo TX Coordinates 35.803356°, -101.43352° 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":35.803356,"lon":-101.43352,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

408

Salty Dog II | Open Energy Information  

Open Energy Info (EERE)

II II Facility Salty Dog II Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner Salty Dog II LLC Energy Purchaser Xcel Energy Location Lake Benton MN Coordinates 44.3144°, -96.3256° 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":-96.3256,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

409

Vansycle Ridge II | Open Energy Information  

Open Energy Info (EERE)

Vansycle Ridge II Vansycle Ridge II Jump to: navigation, search Name Vansycle Ridge II Facility Vansycle Ridge II Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner NextEra Energy Resources Developer NextEra Energy Resources Location OR Coordinates 45.8515°, -118.458° 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":45.8515,"lon":-118.458,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

410

NCPA II Geothermal Facility | Open Energy Information  

Open Energy Info (EERE)

NCPA II Geothermal Facility NCPA II Geothermal Facility General Information Name NCPA II Geothermal Facility Facility NCPA II Sector Geothermal energy Location Information Location The Geysers, California Coordinates 38.74837690774°, -122.71119117737° Loading map... {"minzoom":false,"mappingservice":"googlemaps3","type":"ROADMAP","zoom":14,"types":["ROADMAP","SATELLITE","HYBRID","TERRAIN"],"geoservice":"google","maxzoom":false,"width":"600px","height":"350px","centre":false,"title":"","label":"","icon":"","visitedicon":"","lines":[],"polygons":[],"circles":[],"rectangles":[],"copycoords":false,"static":false,"wmsoverlay":"","layers":[],"controls":["pan","zoom","type","scale","streetview"],"zoomstyle":"DEFAULT","typestyle":"DEFAULT","autoinfowindows":false,"kml":[],"gkml":[],"fusiontables":[],"resizable":false,"tilt":0,"kmlrezoom":false,"poi":true,"imageoverlays":[],"markercluster":false,"searchmarkers":"","locations":[{"text":"","title":"","link":null,"lat":38.74837690774,"lon":-122.71119117737,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

411

Elm Creek II | Open Energy Information  

Open Energy Info (EERE)

Elm Creek II Elm Creek II Jump to: navigation, search Name Elm Creek II Facility Elm Creek II Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner Iberdrola Renewables Developer Iberdrola Renewables Location Jackson and Martin County MN Coordinates 43.756372°, -94.956014° 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":43.756372,"lon":-94.956014,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

412

PARS II - Integrated Project Team Meeting  

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

John Makepeace (OECM) Kai Mong (EES), Ken Henderson (EES), Norm Ayers (EES) October 29, 2009 2 2 Agenda * PARS II OA & CPP Software * PARS II Deployment Timeline * Deployment Overview * Organizational Roles & Responsibilities * Project List and Schedule * Next Steps 3 PARS II OA & CPP Software * Oversight & Assessment (OA) * Web interface collects summary-level project data: status assessments, forecasts, PB, KPPs * Used by FPD, Program and OECM each month * Contractor Project Performance (CPP) * Web interface for uploading contractor's project files: earned value, schedule, variance, MR, risk * Used by contractor each month 4 PARS II Deployment Timeline 4 11/1/2009 12/1/2009 1/1/2010 2/1/2010 3/1/2010 4/1/2010 5/1/2010 6/1/2010 7/1/2010 8/1/2010 9/1/2010 10/1/2010 11/1/2010

413

Instrument Series: Mass Spectrometry SPLAT II  

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

Mass Spectrometry Mass Spectrometry SPLAT II SPLAT II is a one-of-a-kind single particle mass spectrometer that was designed, constructed, and deployed at EMSL to allow users to precisely characterize the physical and chemical properties of nanoparticles. SPLAT II yields quantitative information on particle physical and chemical properties in the laboratory or in the field-even aboard an aircraft. In the context of EMSL's integrated problem-solving environment, the unique capabilities of SPLAT II enable vital research across a range of scientific fields. Research Applications Fundamental science - characterizing the properties and behavior of matter on the nanoscale Atmospheric chemistry - understanding the processes that control atmospheric aerosol life cycle Climate change - uncovering and helping

414

Steel Winds II | Open Energy Information  

Open Energy Info (EERE)

Winds II Winds II Jump to: navigation, search Name Steel Winds II Facility Steel Winds II Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner First Wind Developer First Wind Energy Purchaser Merchant Location Lackawanna NY Coordinates 42.81756607°, -78.86672974° 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":42.81756607,"lon":-78.86672974,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

415

Sunray II Wind Farm | Open Energy Information  

Open Energy Info (EERE)

Sunray II Wind Farm Sunray II Wind Farm Jump to: navigation, search Name Sunray II Wind Farm Facility Sunray II Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner Valero Developer Valero Energy Purchaser McKee Refinery for 34.5; Xcel Energy for remainder Location TX Coordinates 35.961137°, -101.804602° 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":35.961137,"lon":-101.804602,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

416

Bishop Hill II | Open Energy Information  

Open Energy Info (EERE)

II II Jump to: navigation, search Name Bishop Hill II Facility Bishop Hill II Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner MidAmerican Energy Developer Ivenergy Energy Purchaser Ameren Illinois Location Cambridge IL Coordinates 41.24438513°, -90.09338379° 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":41.24438513,"lon":-90.09338379,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

417

Pinyon Pines II | Open Energy Information  

Open Energy Info (EERE)

Pinyon Pines II Pinyon Pines II Jump to: navigation, search Name Pinyon Pines II Facility Pinyon Pines II (Alta IX) Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner MidAmerican Energy Developer Terra-Gen Power Energy Purchaser Southern California Edison Co Location Tehachapi Pass CA Coordinates 35.01917213°, -118.3031845° 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":35.01917213,"lon":-118.3031845,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

418

CWES II Wind Farm | Open Energy Information  

Open Energy Info (EERE)

II Wind Farm II Wind Farm Jump to: navigation, search Name CWES II Wind Farm Facility CWES II Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner SeaWest Developer SeaWest Energy Purchaser Pacific Gas & Electric Co Location Altamont Pass CA Coordinates 37.7347°, -121.652° 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":37.7347,"lon":-121.652,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

419

Springview II Wind Project | Open Energy Information  

Open Energy Info (EERE)

Springview II Wind Project Springview II Wind Project Jump to: navigation, search Name Springview II Wind Project Facility Springview II Wind Project Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner Bluestem LLC Developer Bluestem LLC Energy Purchaser NPPD Location Springview NE Coordinates 42.82578163°, -99.77630854° 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":42.82578163,"lon":-99.77630854,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

420

Los Vientos II | Open Energy Information  

Open Energy Info (EERE)

II II Jump to: navigation, search Name Los Vientos II Facility Los Vientos II Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner Duke Energy Developer Duke Enegy Energy Purchaser Austin Energy Location Lyford TX Coordinates 26.33903762°, -97.66176224° 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":26.33903762,"lon":-97.66176224,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

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421

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 Edison Phase II Compute Cabinets Arrive at NERSC June 27, 2013 by Zhengji Zhao (1 Comments) The compute cabinets were shiped to NERSC between June 24 and 25, 2013.They have been installed on the machine room floor in Oakland. The 28 canbinets that comprise the Phase II system were powered up on June 27, 2013. Post your comment You cannot post comments until you have logged in. Login Here. Comments I re-compiled my program on Edison with Intel compiler. Once submitted the job, the waiting time in the regular queue was very short compared to Hopper. The run on Edison was smooth and with no problems. Comparing the CPU time for the run, I found that the job run almost twice as faster as in Hopper (using PGI compilers). (In Edison it took 111 seconds and in Hopper/PGI 203

422

PARS II Training Materials | Department of Energy  

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

Training Materials 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. Slides from the APM "Road Show" Earned Value (EV) Analysis and Project Assessment & Reporting System (PARS II) 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

423

Pillar Mountain II | Open Energy Information  

Open Energy Info (EERE)

Pillar Mountain II Pillar Mountain II Jump to: navigation, search Name Pillar Mountain II Facility Pillar Mountain II Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner Kodiak Electric Assoc. Developer Kodiak Electric Assoc. Energy Purchaser Kodiak Electric Assoc. Location Kodiak AK Coordinates 57.78667872°, -152.4434781° 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":57.78667872,"lon":-152.4434781,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

424

Shiloh II Wind Farm | Open Energy Information  

Open Energy Info (EERE)

Shiloh II Wind Farm Shiloh II Wind Farm Jump to: navigation, search Name Shiloh II Wind Farm Facility Shiloh II Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner EnXco Developer EnXco Energy Purchaser Pacific Gas & Electric Co Location Northern CA CA Coordinates 38.179998°, -121.822° Loading map... {"minzoom":false,"mappingservice":"googlemaps3","type":"ROADMAP","zoom":14,"types":["ROADMAP","SATELLITE","HYBRID","TERRAIN"],"geoservice":"google","maxzoom":false,"width":"600px","height":"350px","centre":false,"title":"","label":"","icon":"","visitedicon":"","lines":[],"polygons":[],"circles":[],"rectangles":[],"copycoords":false,"static":false,"wmsoverlay":"","layers":[],"controls":["pan","zoom","type","scale","streetview"],"zoomstyle":"DEFAULT","typestyle":"DEFAULT","autoinfowindows":false,"kml":[],"gkml":[],"fusiontables":[],"resizable":false,"tilt":0,"kmlrezoom":false,"poi":true,"imageoverlays":[],"markercluster":false,"searchmarkers":"","locations":[{"text":"","title":"","link":null,"lat":38.179998,"lon":-121.822,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

425

ii Colorado Climate Table of Contents  

E-Print Network (OSTI)

#12;ii Colorado Climate Table of Contents Web: http://climate.atmos.colostate.edu Colorado Climate Spring 2002 Vol. 3, No. 2 Lightning in Colorado . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .4 Colorado Climate in Review

426

H II region abundances in Seyfert galaxies  

SciTech Connect

The theoretical H II region abundance sequence calibration reported by Dopita and Evans in 1986 has been applied to optical spectrophotometry of 23 H II regions located in the inner disk regions of two Seyfert 1 and two Seyfert 2 galaxies, including the prototype Seyfert 2, NGC 1068, in order to determine oxygen, nitrogen, and sulfur abundances. The mean oxygen abundance derived for each galaxy ranges between solar abundance and twice solar abundance. There is no evidence for abnormal N/O or S/O abundance ratios in any of the H II regions observed. The observations suggest that the abundances derived for the H II regions may be adopted as nuclear abundances and employed to constrain theoretical models of the Seyfert nucleus. The observations then place limits on the influence which the active nucleus can have on chemical enrichment of the local interstellar medium. 47 references.

Evans, I.N.; Dopita, M.A.

1987-08-01T23:59:59.000Z

427

Stormwater Pollution Prevention Plan Seismic Phase II  

E-Print Network (OSTI)

Stormwater Pollution Prevention Plan Seismic Phase II Prepared by: Environment, Health and Safety Division Environmental Services Group May 2010 Revision 1 Ernest Orlando Lawrence Berkeley National ..................................................................................................................... 15 2.1.1 Demolition of Building 25/25B

428

NSLS-II Transport Line Progress  

SciTech Connect

The National Synchrotron Light Source II (NSLS-II) is a state-of-the-art 3-GeV third generation light source currently under construction at Brookhaven National Laboratory. The NSLS-II injection system consists of a 200 MeV linac, a 3-GeV booster synchrotron and associated transfer lines. The first part of the Linac to Booster Transport (LBT) line has been installed for linac commissioning. This part includes all components necessary to commission the NSLS-II linac. The second part of this transport line is undergoing installation. Initial results of hardware commissioning will be discussed. The Booster to Storage Ring (BSR) transport line underwent a design review. The first part of the BSR transport line, consisting of all components necessary to commission the booster will be installed in 2012 for booster commissioning. We report on the final design of the BSR line along with the plan to commission the booster.

Fliller R. P.; Wahl, W.; Anderson, A.; Benish, B.; DeBoer, W.; Ganetis, G.; Heese, R.; Hseuh, H.-C.; Hu, J.-P.; Johanson, M.P.; Kosciuk, B.N.; Padrazo, D.; Roy, K.; Shaftan, T.; Singh, O.; Tuozzolo, J.; Wang, G.

2012-05-20T23:59:59.000Z

429

PARS II User Guide | Department of Energy  

Office of Environmental Management (EM)

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 the major functions...

430

Montezuma Winds II | Open Energy Information  

Open Energy Info (EERE)

Winds II Winds II Jump to: navigation, search Name Montezuma Winds II Facility Montezuma Winds II Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner NextEra Energy Resources Developer NextEra Energy Resources Energy Purchaser Pacific Gas & Electric Co Location Rio Vista CA Coordinates 38.16867552°, -121.8061924° Loading map... {"minzoom":false,"mappingservice":"googlemaps3","type":"ROADMAP","zoom":14,"types":["ROADMAP","SATELLITE","HYBRID","TERRAIN"],"geoservice":"google","maxzoom":false,"width":"600px","height":"350px","centre":false,"title":"","label":"","icon":"","visitedicon":"","lines":[],"polygons":[],"circles":[],"rectangles":[],"copycoords":false,"static":false,"wmsoverlay":"","layers":[],"controls":["pan","zoom","type","scale","streetview"],"zoomstyle":"DEFAULT","typestyle":"DEFAULT","autoinfowindows":false,"kml":[],"gkml":[],"fusiontables":[],"resizable":false,"tilt":0,"kmlrezoom":false,"poi":true,"imageoverlays":[],"markercluster":false,"searchmarkers":"","locations":[{"text":"","title":"","link":null,"lat":38.16867552,"lon":-121.8061924,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

431

Difwind II Wind Farm | Open Energy Information  

Open Energy Info (EERE)

II Wind Farm II Wind Farm Jump to: navigation, search Name Difwind II Wind Farm Facility Difwind II Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner EnXco Energy Purchaser Southern California Edison Co Location San Gorgonio CA Coordinates 33.9095°, -116.734° 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":33.9095,"lon":-116.734,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

432

UNIFORM INFALL TOWARD THE COMETARY H II REGION IN THE G34.26+0.15 COMPLEX?  

SciTech Connect

Gas accretion is a key process in star formation. However, gas infall detections in high-mass, star-forming regions with high spatial resolution observations are rare. Here, we report the detection of gas infall toward a cometary ultracompact H II region ({sup C)} in the G34.26+0.15 complex. The observations were made with the IRAM 30 m, the James Clerk Maxwell Telescope 15 m telescope, and the Submillimeter Array (SMA). The hot core associated with 'C' has a mass of ?76 ± 11 M{sub ?} and a volume density of (1.1 ± 0.2) × 10{sup 8} cm{sup –3}. The HCN (3-2) and HCO{sup +} (1-0) lines observed by single dishes and the CN (2-1) lines observed by the SMA show redshifted absorption features, indicating gas infall. We found a linear relationship between the line width and optical depth of the CN (2-1) lines. Those transitions with larger optical depths and line widths have larger absorption areas. However, the infall velocities measured from different lines seem to be constant, indicating that the gas infall is uniform. We also investigated the evolution of gas infall in high-mass, star-forming regions. A tight relationship was found between the infall velocity and the total dust/gas mass. At stages prior to the hot core phase, the typical infall velocity and mass infall rate are ?1 km s{sup –1} and ?10{sup –4} M{sub ?} yr{sup –1}, respectively. While in more evolved regions, the infall velocity and mass infall rates can reach as high as several km s{sup –1} and ?10{sup –3}-10{sup –2} M{sub ?} yr{sup –1}, respectively. Accelerated infall has been detected toward some hypercompact H II and ultracompact H II regions. However, the acceleration phenomenon is not seen in more evolved ultracompact H II regions (e.g., G34.26+0.15)

Liu, Tie; Wu, Yuefang; Zhang, Huawei, E-mail: liutiepku@gmail.com, E-mail: ywu@pku.edu.cn [Department of Astronomy, Peking University, 100871 Beijing (China)

2013-10-10T23:59:59.000Z

433

THE Ly{alpha} LINES OF H I AND He II: A DIFFERENTIAL HANLE EFFECT FOR EXPLORING THE MAGNETISM OF THE SOLAR TRANSITION REGION  

SciTech Connect

The Ly{alpha} line of He II at 304 Angstrom-Sign is one of the spectral lines of choice for EUV channels of narrowband imagers on board space telescopes, which provide spectacular intensity images of the outer solar atmosphere. Since the magnetic field information is encoded in the polarization of the spectral line radiation, it is important to investigate whether the He II line radiation from the solar disk can be polarized, along with its magnetic sensitivity. Here we report some theoretical predictions concerning the linear polarization signals produced by scattering processes in this strong emission line of the solar transition region, taking into account radiative transfer and the Hanle effect caused by the presence of organized and random magnetic fields. We find that the fractional polarization amplitudes are significant ({approx}1%), even when considering the wavelength-integrated signals. Interestingly, the scattering polarization of the Ly{alpha} line of He II starts to be sensitive to the Hanle effect for magnetic strengths B {approx}> 100 G (i.e., for magnetic strengths of the order of and larger than the Hanle saturation field of the hydrogen Ly{alpha} line at 1216 Angstrom-Sign ). We therefore propose simultaneous observations of the scattering polarization in both Ly{alpha} lines to facilitate magnetic field measurements in the upper solar chromosphere. Even the development of a narrowband imaging polarimeter for the He II 304 Angstrom-Sign line alone would be already of great diagnostic value for probing the solar transition region.

Trujillo Bueno, Javier; Stepan, Jiri; Belluzzi, Luca, E-mail: jtb@iac.es, E-mail: stepan@iac.es, E-mail: belluzzi@iac.es [Instituto de Astrofisica de Canarias, 38205 La Laguna, Tenerife (Spain)

2012-02-10T23:59:59.000Z

434

M-BAND IMAGING OF THE HR 8799 PLANETARY SYSTEM USING AN INNOVATIVE LOCI-BASED BACKGROUND SUBTRACTION TECHNIQUE  

SciTech Connect

Multi-wavelength observations/spectroscopy of exoplanetary atmospheres are the basis of the emerging exciting field of comparative exoplanetology. The HR 8799 planetary system is an ideal laboratory to study our current knowledge gap between massive field brown dwarfs and the cold 5 Gyr old solar system planets. The HR 8799 planets have so far been imaged at J- to L-band, with only upper limits available at M-band. We present here deep high-contrast Keck II adaptive optics M-band observations that show the imaging detection of three of the four currently known HR 8799 planets. Such detections were made possible due to the development of an innovative LOCI-based background subtraction scheme that is three times more efficient than a classical median background subtraction for Keck II AO data, representing a gain in telescope time of up to a factor of nine. These M-band detections extend the broadband photometric coverage out to {approx}5 {mu}m and provide access to the strong CO fundamental absorption band at 4.5 {mu}m. The new M-band photometry shows that the HR 8799 planets are located near the L/T-type dwarf transition, similar to what was found by other studies. We also confirm that the best atmospheric fits are consistent with low surface gravity, dusty, and non-equilibrium CO/CH{sub 4} chemistry models.

Galicher, Raphael; Marois, Christian [National Research Council Canada, Herzberg Institute of Astrophysics, 5071 West Saanich Road, Victoria, BC, V9E 2E7 (Canada); Macintosh, Bruce; Konopacky, Quinn [Lawrence Livermore National Laboratory, 7000 East Ave., Livermore, CA 94550 (United States); Barman, Travis, E-mail: raphael.galicher@nrc-cnrc.gc.ca [Lowell Observatory, 1400 West Mars Hill Road, Flagstaff, AZ 86001 (United States)

2011-10-01T23:59:59.000Z

435

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

436

Results from a Prototype MAPS Sensor Telescope and Readout Systemwith Zero Suppression for the Heavy Flavor Tracker at STAR  

SciTech Connect

We describe a three Mimostar-2 Monolithic Active PixelSensor (MAPS) sensor telescope prototype with an accompanying readoutsystem incorporating on-the-fly data sparsification. The system has beencharacterized and we report on the measured performance of the sensortelescope and readout system in beam tests conducted both at the AdvancedLight Source (ALS) at Lawrence Berkeley National Laboratory (LBNL) and inthe STAR experiment at the Relativistic Heavy Ion Collider (RHIC). Thiseffort is part of the development and prototyping work that will lead toa vertex detector for the STAR experiment.

Greiner, Leo C.; Matis, Howard S.; Ritter, Hans G.; Rose, AndrewA.; Stezelberger, Thorsten; Sun, Xiangming; Szelezniak, Michal A.; Thomas, James H.; Vu, Chinh Q.; Wieman, Howard H.

2008-02-11T23:59:59.000Z

437

Neutrino Induced Upward Going Muons from a Gamma Ray Burst in a Neutrino Telescope of Km^2 Area  

E-Print Network (OSTI)

The number of neutrino induced upward going muons from a single Gamma Ray Burst (GRB) expected to be detected by the proposed kilometer scale IceCube detector at the South Pole location has been calculated. The effects of the Lorentz factor, total energy of the GRB emitted in neutrinos and its distance from the observer (red shift) on the number of neutrino events from the GRB have been examined. The present investigation reveals that there is possibility of exploring the early Universe with the proposed kilometer scale IceCube neutrino telescope.

Nayantara Gupta

2002-01-30T23:59:59.000Z

438

AT2 DS II - Accelerator System Design (Part II) - CCC Video Conference  

SciTech Connect

Discussion Session - Accelerator System Design (Part II) Tutors: C. Darve, J. Weisend II, Ph. Lebrun, A. Dabrowski, U. Raich Video Conference with the CERN Control Center. Experts in the field of Accelerator science will be available to answer the students questions. This session will link the CCC and SA (using Codec VC).

None

2010-12-17T23:59:59.000Z

439

APPLIED BIOLOGY 360 ~ FOOD & ENVIRONMENT II (Agroecology II) Faculty of Land and Food Systems  

E-Print Network (OSTI)

: APBI 360 uses a systems approach to investigate the functions and interactions of plants and animals/ 204 pp Gliessman, S.R. 2007. Agroecology ­ The Ecology of Sustainable Food Systems. Second Edition1 APPLIED BIOLOGY 360 ~ FOOD & ENVIRONMENT II (Agroecology II) Faculty of Land and Food Systems

Farrell, Anthony P.

440

Hubble Space Telescope Near-Ultraviolet Spectroscopy of the Bright CEMP-no Star BD+44 493  

E-Print Network (OSTI)

We present an elemental-abundance analysis, in the near-ultraviolet (NUV) spectral range, for the extremely metal-poor star BD+44 493, a 9th magnitude sub-giant with [Fe/H] = -3.8 and enhanced carbon, based on data acquired with the Space Telescope Imaging Spectrograph on the Hubble Space Telescope. This star is the brightest example of a class of objects that, unlike the great majority of carbon-enhanced metal-poor (CEMP) stars, does not exhibit over-abundances of heavy neutron-capture elements (CEMP-no). In this paper, we validate the abundance determinations for a number of species that were previously studied in the optical region, and obtain strong upper limits for beryllium and boron, as well as for neutron-capture elements from zirconium to platinum, many of which are not accessible from ground-based spectra. The boron upper limit we obtain for BD+44 493, logeps(B) < -0.70, the first such measurement for a CEMP star, is the lowest yet found for very and extremely metal-poor stars. In addition, we ob...

Placco, Vinicius; Roederer, Ian; Cowan, John; Frebel, Anna; Filler, Dan; Ivans, Inese I; Lawler, James E; Schatz, Hendrik; Sneden, Christopher; Sobeck, Jennifer; Aoki, Wako; Smith, Verne

2014-01-01T23:59:59.000Z

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441

PROSPECTS FOR A DARK MATTER ANNIHILATION SIGNAL TOWARD THE SAGITTARIUS DWARF GALAXY WITH GROUND-BASED CHERENKOV TELESCOPES  

SciTech Connect

Dwarf galaxies are widely believed to be among the best targets for indirect dark matter searches using high-energy gamma rays and indeed gamma-ray emission from these objects has long been a subject of detailed study for ground-based atmospheric Cherenkov telescopes. Here, we update current exclusion limits obtained on the closest dwarf, the Sagittarius dwarf galaxy, in light of recent realistic dark matter halo models. The constraints on the velocity-weighted annihilation cross-section of the dark matter particle are of a few 10{sup -23} cm{sup 3} s{sup -1} in the TeV energy range for a 50 hr exposure. The limits are extrapolated to the sensitivities of future Cherenkov Telescope Arrays. For 200 hr of observation time, the sensitivity at the 95% confidence level reaches 10{sup -25} cm{sup 3} s{sup -1}. Possible astrophysical backgrounds from gamma-ray sources dissembled in the Sagittarius dwarf are studied. It is shown that with long enough observation times, gamma-ray background from millisecond pulsars in a globular cluster contained within the Sagittarius dwarf may limit the sensitivity to dark matter annihilations.

Viana, A.; Medina, M. C.; Brun, P.; Glicenstein, J. F.; Kosack, K.; Moulin, E.; Naumann-Godo, M.; Peyaud, B. [IRFU/DSM, CEA Saclay, F-91191 Gif-sur-Yvette, Cedex (France); Penarrubia, J. [Institute of Astronomy, University of Cambridge, Cambridge CB3 0HA (United Kingdom)

2012-02-10T23:59:59.000Z

442

The ASTRI Project: prototype status and future plans for a Cherenkov dual-mirror small-telescope array  

E-Print Network (OSTI)

ASTRI ("Astrofisica con Specchi a Tecnologia Replicante Italiana") is a flagship project of the Italian Ministry of Education, University and Research. Within this framework, INAF is currently developing a wide field of view (9.6 degrees in diameter) end-to-end prototype of the CTA small-size telescope (SST), devoted to the investigation of the energy range from a fraction of TeV up to tens of TeVs, and scheduled to start data acquisition in 2014. For the first time, a dual-mirror Schwarzschild-Couder optical design will be adopted on a Cherenkov telescope, in order to obtain a compact optical configuration. A second challenging, but innovative technical solution consists of a modular focal surface camera based on Silicon photo-multipliers with a logical pixel size of 6.2mm x 6.2mm. Here we describe the current status of the project, the expected performance, and its possible evolution in terms of an SST mini-array. This CTA-SST precursor, composed of a few SSTs and developed in collaboration with CTA interna...

Vercellone, S; Maccarone, M C; Di Pierro, F; Vallania, P; Bonnoli, G; Canestrari, R; Pareschi, G; Tosti, G

2013-01-01T23:59:59.000Z

443

The ASTRI project: Prototype status and future plans for a Cherenkov dual-mirror small-telescope array  

Science Journals Connector (OSTI)

ASTRI ("Astrofisica con Specchi a Tecnologia Replicante Italiana") is a flagship project of the Italian Ministry of Education University and Research. Within this framework INAF is currently developing a wide field of view (9.6° in diameter) end-to-end prototype of the CTA smallsize telescope (SST) devoted to the investigation of the energy range from a fraction of TeV up to (possibly) hundreds of TeV and scheduled to start data acquisition in 2014. For the first time a dualmirror Schwarzschild-Couder optical design will be adopted on a Cherenkov telescope in order to obtain a compact (F? = 0.5) optical configuration. A second challenging but innovative technical solution consists of a focal plane camera based on Silicon photo-multipliers with a logical pixel size of 0.17° (6.2mm × 6.2mm). We will describe the current status of the project the results obtained so far the expected performance and its possible evolution in terms of a SST mini-array (composed of 5-7 SSTs and developed in collaboration with CTA international partners) which could peruse not only the adopted technological solutions but also address a few scientific test cases.

S. Vercellone; ASTRI Collaboration

2012-01-01T23:59:59.000Z

444

Searches for Point-like and extended neutrino sources close to the Galactic Centre using the ANTARES neutrino Telescope  

E-Print Network (OSTI)

A search for cosmic neutrino sources using six years of data collected by the ANTARES neutrino telescope has been performed. Clusters of muon neutrinos over the expected atmospheric background have been looked for. No clear signal has been found. The most signal-like accumulation of events is located at equatorial coordinates RA=$-$46.8$^{\\circ}$ and Dec=$-$64.9$^{\\circ}$ and corresponds to a 2.2$\\sigma$ background fluctuation. In addition, upper limits on the flux normalization of an E$^{-2}$ muon neutrino energy spectrum have been set for 50 pre-selected astrophysical objects. Finally, motivated by an accumulation of 7 events relatively close to the Galactic Centre in the recently reported neutrino sample of the IceCube telescope, a search for point sources in a broad region around this accumulation has been carried out. No indication of a neutrino signal has been found in the ANTARES data and upper limits on the flux normalization of an E$^{-2}$ energy spectrum of neutrinos from point sources in that region have been set. The 90% confidence level upper limits on the muon neutrino flux normalization vary between 3.5 and 5.1$\\times$10$^{-8}$ GeV$\\,$cm$^{-2}$s$^{-1}$, depending on the exact location of the source.

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

2014-02-25T23:59:59.000Z

445

Wide-Field InfraRed Survey Telescope (WFIRST) Mission and Synergies with LISA and LIGO-Virgo  

E-Print Network (OSTI)

The Wide-Field InfraRed Survey Telescope (WFIRST) is a NASA space mission in study for launch in 2024. It has a 2.4 m telescope, wide-field IR instrument operating in the 0.7 - 2.0 micron range and an exoplanet imaging coronagraph instrument operating in the 400 - 1000 nm range. The observatory will perform galaxy surveys over thousands of square degrees to J=27 AB for dark energy weak lensing and baryon acoustic oscillation measurements and will monitor a few square degrees for dark energy SN Ia studies. It will perform microlensing observations of the galactic bulge for an exoplanet census and direct imaging observations of nearby exoplanets with a pathfinder coronagraph. The mission will have a robust and well-funded guest observer program for 25% of the observing time. WFIRST will be a powerful tool for time domain astronomy and for coordinated observations with gravitational wave experiments. Gravitational wave events produced by mergers of nearby binary neutron stars (LIGO-Virgo) or extragalactic superm...

Gehrels, Neil

2014-01-01T23:59:59.000Z

446

Tatanka Wind Project II | Open Energy Information  

Open Energy Info (EERE)

Tatanka Wind Project II Tatanka Wind Project II Jump to: navigation, search Name Tatanka Wind Project II Facility Tatanka Wind Project Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner Acciona Energy Developer Acciona Energy Location Dickey and McIntosh Counties ND Coordinates 45.951884°, -98.940482° 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":45.951884,"lon":-98.940482,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

447

Cannon II Wind Farm | Open Energy Information  

Open Energy Info (EERE)

Cannon II Wind Farm Cannon II Wind Farm Facility Cannon II Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Energy Purchaser Southern California Edison Co Location Tehachapi CA Coordinates 35.1317°, -118.451° 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":35.1317,"lon":-118.451,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

448

Carleton College II | Open Energy Information  

Open Energy Info (EERE)

Carleton College II Carleton College II Facility Carleton College II Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner Carleton College Developer Carleton College Energy Purchaser Xcel Energy Location Northfield MN Coordinates 44.46881856°, -93.12780976° 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":fal