National Library of Energy BETA

Sample records for observatory calipso endstations

  1. ALS "Workhorse" Endstation Retires after 22 Years of Service

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

    "Workhorse" Endstation Retires after 22 Years of Service ALS "Workhorse" Endstation Retires after 22 Years of Service Print Following a career spanning over two decades, ALS ...

  2. FAMS DECOMMISSIONING END-STATE ALTERNATIVE EVALUATION

    SciTech Connect (OSTI)

    Grimm, B; Stephen Chostner, S; Brenda Green, B

    2006-05-25

    Nuclear Material Management (NMM) completed a comprehensive study at the request of the Department of Energy Savannah River Operations Office (DOE-SR) in 2004 (Reference 11.1). The study evaluated the feasibility of removal and/or mitigation of the Pu-238 source term in the F-Area Material Storage (FAMS) facility during on-going material storage operations. The study recommended different options to remove and/or mitigate the Pu-238 source term depending on its location within the facility. During April 2005, the Department of Energy (DOE) sent a letter of direction (LOD) to Washington Savannah River Company (WSRC) directing WSRC to implement a new program direction that would enable an accelerated shutdown and decommissioning of FAMS (Reference 11.2). Further direction in the LOD stated that effective December 1, 2006 the facility will be transitioned to begin deactivation and decommissioning (D&D) activities. To implement the LOD, Site D&D (SDD) and DOE agreed the planning end-state would be demolition of the FAMS structure to the building slab. SDD developed the D&D strategy, preliminary cost and schedule, and issued the deactivation project plan in December 2005 (Reference 11.3). Due to concerns and questions regarding the FAMS planning end-state and in support of the project's Critical Decision 1, an alternative study was performed to evaluate the various decommissioning end-states and the methods by which those end-states are achieved. This report documents the results of the alternative evaluation which was performed in a structured decision-making process as outlined in the E7 Manual, Procedure 2.15, ''Alternative Studies'' (Reference 11.4).

  3. ALS "Workhorse" Endstation Retires after 22 Years of Service

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

    "Workhorse" Endstation Retires after 22 Years of Service ALS "Workhorse" Endstation Retires after 22 Years of Service Print Following a career spanning over two decades, ALS endstation 8.0.1.1 retired last October. The endstation, which specializes in soft x-ray fluorescence, is one of many hosted by Beamline 8.0.1 and has been known as a "workhorse" for the more than 450 peer-reviewed publications to its credit. Endstation 8.0.1.1 during its heyday, pictured (from

  4. HSRL mass estimate based on CALIPSO

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

    OBSERVATIONS FROM THE NASA LANGLEY AIRBORNE HIGH SPECTRAL RESOLUTION LIDAR AND PLANS FOR ACTIVE-PASSIVE AEROSOL-CLOUD RETRIEVALS Chris A. Hostetler, Richard A. Ferrare, John W. Hair, Raymond R. Rogers, Mike Obland, Sharon P. Burton, Wenying Su, Anthony L. Cook, David B. Harper NASA HQ Science Mission Directorate Radiation Sciences Program Environmental Protection Agency (EPA) NASA CALIPSO Project Sponsors Department of Energy Atmospheric Science Program Texas Commission on Environmental Quality

  5. Endstates Initiative

    Broader source: Energy.gov [DOE]

    Scientific and technical, institutional and regulatory, and closure management challenges are currently hindering cleanup and closure of remaining environmental legacy waste sites across the...

  6. AREA FACTOR DETERMINATIONS FOR AN INDUSTRIAL WORKER EXPOSED TO A CONCRETE SLAB END-STATE

    SciTech Connect (OSTI)

    Jannik, T; Patricia Lee, P; Eduardo Farfan, E; Jesse Roach, J

    2007-02-08

    The U.S. Department of Energy's (DOE) Savannah River Site (SRS) is decommissioning many of its excess facilities through removal of the facility structures leaving only the concrete-slab foundations in place. Site-specific, risk-based derived concentration guideline levels (DCGLs) for radionuclides have been determined for a future industrial worker potentially exposed to residual contamination on these concrete slabs as described in Jannik [1]. These risk-based DCGLs were estimated for an exposure area of 100 m{sup 2}. During deactivation and decommissioning (D&D) operations at SRS, the need for area factors for larger and smaller contaminated areas arose. This paper compares the area factors determined for an industrial worker exposed to a concrete slab end-state for several radionuclides of concern at SRS with (1) the illustrative area factors provided in MARSSIM [2], (2) the area correction factors provided in the U.S. Environmental Protection Agency's (EPA) Soil Screening Guidance [3], and (3) the hot spot criterion for field application provided in the RESRAD User's Manual [4].

  7. Macrophysical Properties of Tropical Cirrus Clouds from the CALIPSO Satellite and from Ground-based Micropulse and Raman Lidars

    SciTech Connect (OSTI)

    Thorsen, Tyler J.; Fu, Qiang; Comstock, Jennifer M.; Sivaraman, Chitra; Vaughan, Mark A.; Winker, D.; Turner, David D.

    2013-08-27

    Lidar observations of cirrus cloud macrophysical properties over the U.S. Department of Energy Atmospheric Radiation Measurement (ARM) program Darwin, Australia site are compared from the Cloud-Aerosol Lidar and In- frared Pathfinder Satellite Observation (CALIPSO) satellite, the ground-based ARM micropulse lidar (MPL), and the ARM Raman lidar (RL). Comparisons are made using the subset of profiles where the lidar beam is not fully attenuated. Daytime measurements using the RL are shown to be relatively unaffected by the solar background and are therefore suited for checking the validity of diurnal cycles. RL and CALIPSO cloud fraction profiles show good agreement while the MPL detects significantly less cirrus, particularly during the daytime. Both MPL and CALIPSO observations show that cirrus clouds occur less frequently during the day than at night at all altitudes. In contrast, the RL diurnal cy- cle is significantly different than zero only below about 11 km; where it is the opposite sign (i.e. more clouds during the daytime). For cirrus geomet- rical thickness, the MPL and CALIPSO observations agree well and both datasets have signficantly thinner clouds during the daytime than the RL. From the examination of hourly MPL and RL cirrus cloud thickness and through the application of daytime detection limits to all CALIPSO data we find that the decreased MPL and CALIPSO cloud thickness during the daytime is very likely a result of increased daytime noise. This study highlights the vast im- provement the RL provides (compared to the MPL) in the ARM program's ability to observe tropical cirrus clouds as well as a valuable ground-based lidar dataset for the validation of CALIPSO observations and to help im- prove our understanding of tropical cirrus clouds.

  8. HAWC ?-Ray Observatory

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

    of the volcanoes Sierra Negra and Pico de Orizaba at the border between the states of Puebla and Veracruz. The observatory, which is still under construction, uses an array of...

  9. HAWC Observatory captures first image

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

    HAWC Observatory captures first image HAWC Observatory captures first image The facility is designed to detect cosmic rays and the highest energy gamma rays ever observed from astrophysical sources. April 30, 2013 The High-Altitude Water Cherenkov (HAWC) Observatory is under construction. The High-Altitude Water Cherenkov (HAWC) Observatory is under construction. HAWC is under construction inside the Parque Nacional Pico de Orizaba, a Mexican national park. An international team of researchers,

  10. HAWC γ-Ray Observatory

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

    HAWC γ-Ray Observatory HAWC γ-Ray Observatory Investigating the field of high energy physics through experiments that strengthen our fundamental understanding of matter, energy, space, and time. Get Expertise Rajan Gupta (505) 667-7664 Email Bruce Carlsten (505) 667-5657 Email HAWC γ-Ray Observatory On August 1, 2013, the High-Altitude Water Cherenkov (HAWC) Gamma Ray Observatory formally began operations. HAWC is designed to study the origin of very high-energy cosmic rays and observe the

  11. The Enriched Xenon Observatory

    SciTech Connect (OSTI)

    Dolinski, M. J. [Stanford University Physics Department, 382 Via Pueblo Mall, Stanford, CA 94305-4060 (United States)

    2009-12-17

    The Enriched Xenon Observatory (EXO) experiment will search for neutrinoless double beta decay of {sup 136}Xe. The EXO Collaboration is actively pursuing both liquid-phase and gas-phase Xe detector technologies with scalability to the ton-scale. The search for neutrinoless double beta decay of {sup 136}Xe is especially attractive because of the possibility of tagging the resulting Ba daughter ion, eliminating all sources of background other than the two neutrino decay mode. EXO-200, the first phase of the project, is a liquid Xe time projection chamber with 200 kg of Xe enriched to 80% in {sup 136}Xe. EXO-200, which does not include Ba-tagging, will begin taking data in 2009, with two-year sensitivity to the half-life for neutrinoless double beta decay of 6.4x10{sup 25} years. This corresponds to an effective Majorana neutrino mass of 0.13 to 0.19 eV.

  12. A high resolution and large solid angle x-ray Raman spectroscopy end-station at the Stanford Synchrotron Radiation Lightsource

    SciTech Connect (OSTI)

    Sokaras, D.; Nordlund, D.; Weng, T.-C.; Velikov, P.; Wenger, D.; Garachtchenko, A.; George, M.; Borzenets, V.; Johnson, B.; Rabedeau, T.; Mori, R. Alonso; Bergmann, U.; Qian, Q.

    2012-04-15

    We present a new x-ray Raman spectroscopy end-station recently developed, installed, and operated at the Stanford Synchrotron Radiation Lightsource. The end-station is located at wiggler beamline 6-2 equipped with two monochromators-Si(111) and Si(311) as well as collimating and focusing optics. It consists of two multi-crystal Johann type spectrometers arranged on intersecting Rowland circles of 1 m diameter. The first one, positioned at the forward scattering angles (low-q), consists of 40 spherically bent and diced Si(110) crystals with 100 mm diameters providing about 1.9% of 4{pi} sr solid angle of detection. When operated in the (440) order in combination with the Si (311) monochromator, an overall energy resolution of 270 meV is obtained at 6462.20 eV. The second spectrometer, consisting of 14 spherically bent Si(110) crystal analyzers (not diced), is positioned at the backward scattering angles (high-q) enabling the study of non-dipole transitions. The solid angle of this spectrometer is about 0.9% of 4{pi} sr, with a combined energy resolution of 600 meV using the Si (311) monochromator. These features exceed the specifications of currently existing relevant instrumentation, opening new opportunities for the routine application of this photon-in/photon-out hard x-ray technique to emerging research in multidisciplinary scientific fields, such as energy-related sciences, material sciences, physical chemistry, etc.

  13. the Large Aperture GRB Observatory

    SciTech Connect (OSTI)

    Bertou, Xavier

    2009-04-30

    The Large Aperture GRB Observatory (LAGO) aims at the detection of high energy photons from Gamma Ray Bursts (GRB) using the single particle technique (SPT) in ground based water Cherenkov detectors (WCD). To reach a reasonable sensitivity, high altitude mountain sites have been selected in Mexico (Sierra Negra, 4550 m a.s.l.), Bolivia (Chacaltaya, 5300 m a.s.l.) and Venezuela (Merida, 4765 m a.s.l.). We report on the project progresses and the first operation at high altitude, search for bursts in 6 months of preliminary data, as well as search for signal at ground level when satellites report a burst.

  14. New observatory studies universe's most energetic phenomena

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

    New observatory Community Connections: Your link to news and opportunities from Los Alamos National Laboratory Latest Issue: September 1, 2016 all issues All Issues » submit New observatory studies universe's most energetic phenomena Facility replaces Milagro Observatory near Los Alamos May 1, 2015 From its perch atop the highest accessible peak in Mexico, Milagro's replacement will have 15 percent of the sky within its sights at any given time. From its perch atop the highest accessible peak

  15. The Pierre Auger Cosmic Ray Observatory

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

    Aab, Alexander

    2015-07-08

    The Pierre Auger Observatory, located on a vast, high plain in western Argentina, is the world's largest cosmic ray observatory. The objectives of the Observatory are to probe the origin and characteristics of cosmic rays above 1017 eV and study the interactions of these, the most energetic particles observed in nature. The Auger design features an array of 1660 water Cherenkov particle detector stations spread over 3000 km2 overlooked by 24 air fluorescence telescopes. Additionally, three high elevation fluorescence telescopes overlook a 23.5 km2, 61-detector infilled array with 750 m spacing. The Observatory has been in successful operation since completionmore » in 2008 and has recorded data from an exposure exceeding 40,000 km2 sr yr. This paper describes the design and performance of the detectors, related subsystems and infrastructure that make up the Observatory.« less

  16. The Pierre Auger Cosmic Ray Observatory

    SciTech Connect (OSTI)

    Aab, Alexander

    2015-07-08

    The Pierre Auger Observatory, located on a vast, high plain in western Argentina, is the world's largest cosmic ray observatory. The objectives of the Observatory are to probe the origin and characteristics of cosmic rays above 1017 eV and study the interactions of these, the most energetic particles observed in nature. The Auger design features an array of 1660 water Cherenkov particle detector stations spread over 3000 km2 overlooked by 24 air fluorescence telescopes. Additionally, three high elevation fluorescence telescopes overlook a 23.5 km2, 61-detector infilled array with 750 m spacing. The Observatory has been in successful operation since completion in 2008 and has recorded data from an exposure exceeding 40,000 km2 sr yr. This paper describes the design and performance of the detectors, related subsystems and infrastructure that make up the Observatory.

  17. The Pierre Auger Cosmic Ray Observatory

    SciTech Connect (OSTI)

    2015-02-04

    The Pierre Auger Observatory, located on a vast, high plain in western Argentina, is the world's largest cosmic ray observatory. The objectives of the Observatory are to probe the origin and characteristics of cosmic rays above $10^{17}$ eV and to study the interactions of these, the most energetic particles observed in nature. The Auger design features an array of 1660 water-Cherenkov particle detector stations spread over 3000 km$^2$ overlooked by 24 air fluorescence telescopes. In addition, three high elevation fluorescence telescopes overlook a 23.5 km$^2$, 61 detector infill array. The Observatory has been in successful operation since completion in 2008 and has recorded data from an exposure exceeding 40,000 km$^2$ sr yr. This paper describes the design and performance of the detectors, related subsystems and infrastructure that make up the Auger Observatory.

  18. The Princeton Tritium Observatory for Light, Early Universe,...

    Office of Environmental Management (EM)

    The Princeton Tritium Observatory for Light, Early Universe, Massive Neutrino Yield (PTOLEMY) The Princeton Tritium Observatory for Light, Early Universe, Massive Neutrino Yield...

  19. Evaluation of tropical cloud and precipitation statistics of CAM3 using CloudSat and CALIPSO data

    SciTech Connect (OSTI)

    Zhang, Y; Klein, S; Boyle, J; Mace, G G

    2008-11-20

    The combined CloudSat and CALIPSO satellite observations provide the first simultaneous measurements of cloud and precipitation vertical structure, and are used to examine the representation of tropical clouds and precipitation in the Community Atmosphere Model Version 3 (CAM3). A simulator package utilizing a model-to-satellite approach facilitates comparison of model simulations to observations, and a revised clustering method is used to sort the subgrid-scale patterns of clouds and precipitation into principal cloud regimes. Results from weather forecasts performed with CAM3 suggest that the model underestimates the horizontal extent of low and mid-level clouds in subsidence regions, but overestimates that of high clouds in ascending regions. CAM3 strongly overestimates the frequency of occurrence of the deep convection with heavy precipitation regime, but underestimates the horizontal extent of clouds and precipitation at low and middle levels when this regime occurs. This suggests that the model overestimates convective precipitation and underestimates stratiform precipitation consistent with a previous study that used only precipitation observations. Tropical cloud regimes are also evaluated in a different version of the model, CAM3.5, which uses a highly entraining plume in the parameterization of deep convection. While the frequency of occurrence of the deep convection with heavy precipitation regime from CAM3.5 forecasts decreases, the incidence of the low clouds with precipitation and congestus regimes increases. As a result, the parameterization change does not reduce the frequency of precipitating convection that is far too high relative to observations. For both versions of CAM, clouds and precipitation are overly reflective at the frequency of the CloudSat radar and thin clouds that could be detected by the lidar only are underestimated.

  20. Operations of and Future Plans for the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Abraham, : J.; Abreu, P.; Aglietta, M.; Aguirre, C.; Ahn, E.J.; Allard, D.; Allekotte, I.; Allen, J.; Alvarez-Muniz, J.; Ambrosio, M.; Anchordoqui, L.

    2009-06-01

    These are presentations to be presented at the 31st International Cosmic Ray Conference, in Lodz, Poland during July 2009. It consists of the following presentations: (1) Performance and operation of the Surface Detectors of the Pierre Auger Observatory; (2) Extension of the Pierre Auger Observatory using high-elevation fluorescence telescopes (HEAT); (3) AMIGA - Auger Muons and Infill for the Ground Array of the Pierre Auger Observatory; (4) Radio detection of Cosmic Rays at the southern Auger Observatory; (5) Hardware Developments for the AMIGA enhancement at the Pierre Auger Observatory; (6) A simulation of the fluorescence detectors of the Pierre Auger Observatory using GEANT 4; (7) Education and Public Outreach at the Pierre Auger Observatory; (8) BATATA: A device to characterize the punch-through observed in underground muon detectors and to operate as a prototype for AMIGA; and (9) Progress with the Northern Part of the Pierre Auger Observatory.

  1. HAWC Observatory to study universe's most energetic phenomena

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

    HAWC Observatory to study universe's most energetic phenomena HAWC Observatory to study universe's most energetic phenomena Inaugural ceremony to mark completion of powerful system to detect gamma rays and cosmic rays March 20, 2015 HAWC Observatory HAWC Observatory to study universe's most energetic phenomena Contact Los Alamos National Laboratory Nancy Ambrosiano Communications Office (505) 667-0471 Email University of Maryland Matthew Wright (30) 405-9267 Email "HAWC will be more than 10

  2. Frontier Observatory for Research in Geothermal Energy (FORGE) | Department

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

    of Energy Frontier Observatory for Research in Geothermal Energy (FORGE) Frontier Observatory for Research in Geothermal Energy (FORGE) July 17, 2014 - 2:59pm Addthis Open Date: 07/17/2014 Close Date: 10/01/2014 Funding Organization: U.S. Department of Energy Summary: The objective of this announcement is to establish a dedicated Enhanced Geothermal Systems (EGS) field laboratory called the Frontier Observatory for Research in Geothermal Energy (FORGE). FORGE is envisioned as a dedicated

  3. ARM - Field Campaign - Black Carbon at the Mt. Bachelor Observatory

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

    govCampaignsBlack Carbon at the Mt. Bachelor Observatory Comments? We would love to hear from you! Send us a note below or call us at 1-888-ARM-DATA. Send Campaign : Black Carbon at the Mt. Bachelor Observatory 2016.06.15 - 2016.10.01 Lead Scientist : Daniel Jaffe Abstract Black carbon (BC) is a key component in the earth system and a significant climate forcing agent. Observations at remote sites and in free-tropospheric air are extremely sparse. We propose to utilize one of the ARM SP2 (Single

  4. NGEE Arctic Webcam Photographs, Barrow Environmental Observatory, Barrow, Alaska

    DOE Data Explorer [Office of Scientific and Technical Information (OSTI)]

    Bob Busey; Larry Hinzman

    2012-04-01

    The NGEE Arctic Webcam (PTZ Camera) captures two views of seasonal transitions from its generally south-facing position on a tower located at the Barrow Environmental Observatory near Barrow, Alaska. Images are captured every 30 minutes. Historical images are available for download. The camera is operated by the U.S. DOE sponsored Next Generation Ecosystem Experiments - Arctic (NGEE Arctic) project.

  5. NGEE Arctic Webcam Photographs, Barrow Environmental Observatory, Barrow, Alaska

    DOE Data Explorer [Office of Scientific and Technical Information (OSTI)]

    Bob Busey; Larry Hinzman

    The NGEE Arctic Webcam (PTZ Camera) captures two views of seasonal transitions from its generally south-facing position on a tower located at the Barrow Environmental Observatory near Barrow, Alaska. Images are captured every 30 minutes. Historical images are available for download. The camera is operated by the U.S. DOE sponsored Next Generation Ecosystem Experiments - Arctic (NGEE Arctic) project.

  6. New gamma-ray observatory begins operations at Sierra Negra volcano...

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

    New gamma-ray observatory begins operations New gamma-ray observatory begins operations at Sierra Negra volcano in the state of Puebla, Mexico The High-Altitude Water Cherenkov ...

  7. Sandia's Frontier Observatory for Research In Geothermal Energy (FORGE)

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

    Phase 1 Proposals Were Both Successful Frontier Observatory for Research In Geothermal Energy (FORGE) Phase 1 Proposals Were Both Successful - Sandia Energy Energy Search Icon Sandia Home Locations Contact Us Employee Locator Energy & Climate Secure & Sustainable Energy Future Stationary Power Energy Conversion Efficiency Solar Energy Wind Energy Water Power Supercritical CO2 Geothermal Natural Gas Safety, Security & Resilience of the Energy Infrastructure Energy Storage Nuclear

  8. James Cronin, CP Violation, and the Pierre Auger Observatory

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

    James Cronin, CP Violation and the Pierre Auger Observatory Resources with Additional Information James Cronin Courtesy Brookhaven National Laboratory James Watson Cronin "received his B.S. degree from Southern Methodist University in 1951. He then attended the University of Chicago for graduate school, earning his M.S. in 1953 and his Ph.D. in 1955. He began his scientific career at Brookhaven National Laboratory, where he served as an assistant physicist from 1955 to 1958. Cronin joined

  9. Technology Development for a Neutrino AstrophysicalObservatory

    SciTech Connect (OSTI)

    Chaloupka, V.; Cole, T.; Crawford, H.J.; He, Y.D.; Jackson, S.; Kleinfelder, S.; Lai, K.W.; Learned, J.; Ling, J.; Liu, D.; Lowder, D.; Moorhead, M.; Morookian, J.M.; Nygren, D.R.; Price, P.B.; Richards, A.; Shapiro, G.; Shen, B.; Smoot, George F.; Stokstad, R.G.; VanDalen, G.; Wilkes, J.; Wright, F.; Young, K.

    1996-02-01

    We propose a set of technology developments relevant to the design of an optimized Cerenkov detector for the study of neutrino interactions of astrophysical interest. Emphasis is placed on signal processing innovations that enhance significantly the quality of primary data. These technical advances, combined with field experience from a follow-on test deployment, are intended to provide a basis for the engineering design for a kilometer-scale Neutrino Astrophysical Observatory.

  10. Technology development for a neutrino astrophysical observatory. Letter of intent

    SciTech Connect (OSTI)

    Chaloupka, V.; Cole, T.; Crawford, H.J.

    1996-02-01

    The authors propose a set of technology developments relevant to the design of an optimized Cerenkov detector for the study of neutrino interactions of astrophysical interest. Emphasis is placed on signal processing innovations that enhance significantly the quality of primary data. These technical advances, combined with field experience from a follow-on test deployment, are intended to provide a basis for the engineering design for a kilometer-scale Neutrino Astrophysical Observatory.

  11. Identifying clouds over the Pierre Auger Observatory using infrared satellite data

    SciTech Connect (OSTI)

    Abreu, Pedro; et al.,

    2013-12-01

    We describe a new method of identifying night-time clouds over the Pierre Auger Observatory using infrared data from the Imager instruments on the GOES-12 and GOES-13 satellites. We compare cloud identifications resulting from our method to those obtained by the Central Laser Facility of the Auger Observatory. Using our new method we can now develop cloud probability maps for the 3000 km^2 of the Pierre Auger Observatory twice per hour with a spatial resolution of ~2.4 km by ~5.5 km. Our method could also be applied to monitor cloud cover for other ground-based observatories and for space-based observatories.

  12. Studies of Cosmic Ray Composition and Air Shower Structure with the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Abraham, : J.; Abreu, P.; Aglietta, M.; Aguirre, C.; Ahn, E.J.; Allard, D.; Allekotte, I.; Allen, J.; Alvarez-Muniz, J.; Ambrosio, M.; Anchordoqui, L.

    2009-06-01

    These are presentations to be presented at the 31st International Cosmic Ray Conference, in Lodz, Poland during July 2009. It consists of the following presentations: (1) Measurement of the average depth of shower maximum and its fluctuations with the Pierre Auger Observatory; (2) Study of the nuclear mass composition of UHECR with the surface detectors of the Pierre Auger Observatory; (3) Comparison of data from the Pierre Auger Observatory with predictions from air shower simulations: testing models of hadronic interactions; (4) A Monte Carlo exploration of methods to determine the UHECR composition with the Pierre Auger Observatory; (5) The delay of the start-time measured with the Pierre Auger Observatory for inclined showers and a comparison of its variance with models; (6) UHE neutrino signatures in the surface detector of the Pierre Auger Observatory; and (7) The electromagnetic component of inclined air showers at the Pierre Auger Observatory.

  13. Gravitational Waves Amber L. Stuver LIGO Livingston Observatory

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

    LIGO and the Detection of Gravitational Waves Amber L. Stuver LIGO Livingston Observatory July 27, 2016 4:00 p.m. - Wilson Hall, One West This colloquium will discuss what gravitational waves are and how they are used to observe the universe in a new way. The history of the search for gravitational waves will be reviewed leading up to today's advanced detectors and how they operate. Most sources of detectable gravitational waves are some of the most violent, energetic events in the universe from

  14. SPECKLE INTERFEROMETRY AT THE U.S. NAVAL OBSERVATORY. XVII

    SciTech Connect (OSTI)

    Mason, Brian D.; Hartkopf, William I.; Wycoff, Gary L. E-mail: wih@usno.navy.mil

    2011-08-15

    The results of 3362 intensified CCD observations of double stars, made with the 26 inch refractor of the U.S. Naval Observatory, are presented. Each observation of a system represents a combination of over 2000 short-exposure images. These observations are averaged into 1970 mean relative positions and range in separation from 0.''78 to 72.''17, with a mean separation of 14.''76. This is the 17th in this series of papers and covers the period 2010 January 6 through December 20. Also presented are 10 pairs that are resolved for the first time.

  15. Ultrahigh Energy Neutrinos at the Pierre Auger Observatory

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

    Abreu, P.; Aglietta, M.; Ahlers, M.; Ahn, E. J.; Albuquerque, I. F. M.; Allard, D.; Allekotte, I.; Allen, J.; Allison, P.; Almela, A.; et al

    2013-01-01

    The observation of ultrahigh energy neutrinos (UHE ν s) has become a priority in experimental astroparticle physics. UHE ν s can be detected with a variety of techniques. In particular, neutrinos can interact in the atmosphere (downward-going ν ) or in the Earth crust (Earth-skimming ν ), producing air showers that can be observed with arrays of detectors at the ground. With the surface detector array of the Pierre Auger Observatory we can detect these types of cascades. The distinguishing signature for neutrino events is the presence of very inclined showers produced close to the ground (i.e., after havingmore » traversed a large amount of atmosphere). In this work we review the procedure and criteria established to search for UHE ν s in the data collected with the ground array of the Pierre Auger Observatory. This includes Earth-skimming as well as downward-going neutrinos. No neutrino candidates have been found, which allows us to place competitive limits to the diffuse flux of UHE ν s in the EeV range and above.« less

  16. DOE Announces Notice of Intent for EGS Observatory | Department of Energy

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

    Notice of Intent for EGS Observatory DOE Announces Notice of Intent for EGS Observatory February 21, 2014 - 12:00am Addthis The Energy Department announced today its intent to issue a funding opportunity to establish a dedicated subsurface laboratory called the Frontier Observatory for Research in Geothermal Energy (FORGE). This first-of-its-kind effort will promote transformative and high-risk/high-reward science and engineering focused on addressing critical barriers to Enhanced Geothermal

  17. New gamma-ray observatory begins operations at Sierra Negra volcano...

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

    New gamma-ray observatory begins operations at Sierra Negra volcano in the state of Puebla, Mexico Community Connections: Your link to news and opportunities from Los Alamos...

  18. Cosmic-ray physics with the milagro gamma-ray observatory (Journal...

    Office of Scientific and Technical Information (OSTI)

    The Milagro gamma-ray observatory is a water Cherenkov detector with an energy response ... COUNTERS; COSMIC RADIATION; EMISSION; ENERGY; MODULATION; PHYSICS; TIME DEPENDENCE; WATER

  19. Informational Webinar: Frontier Observatory for Research in Geothermal Energy (FORGE) Funding Opportunity Announcement

    Broader source: Energy.gov [DOE]

    The Energy Department will present a live webinar titled “Frontier Observatory for Research in Geothermal Energy (FORGE) Funding Opportunity Announcement Informational Webinar," focusing on the...

  20. Digital Elevation Model, 0.5-m, Barrow Environmental Observatory, Alaska, 2012

    DOE Data Explorer [Office of Scientific and Technical Information (OSTI)]

    Rowland,Joel; Gangodagamage,Chandana; Wilson,Cathy

    2013-12-08

    The dataset is a digital elevation model, DEM, of a 2km by 7km region in the vicinity of the Barrow Environmental Observatory near Barrow, Ak.

  1. Astrophysical Sources of Cosmic Rays and Related Measurements with the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Abraham, : J.; Abreu, P.; Aglietta, M.; Aguirre, C.; Ahn, E.J.; Allard, D.; Allekotte, I.; Allen, J.; Alvarez-Muniz, J.; Ambrosio, M.; Anchordoqui, L.

    2009-06-01

    These are presentations to be presented at the 31st International Cosmic Ray Conference, in Lodz, Poland during July 2009. It consists of the following presentations: (1) Correlation of the highest energy cosmic rays with nearby extragalactic objects in Pierre Auger Observatory data; (2) Discriminating potential astrophysical sources of the highest energy cosmic rays with the Pierre Auger Observatory; (3) Intrinsic anisotropy of the UHECR from the Pierre Auger Observatory; (4) Ultra-high energy photon studies with the Pierre Auger Observatory; (5) Limits on the flux of diffuse ultra high energy neutrinos set using the Pierre Auger Observatory; (6) Search for sidereal modulation of the arrival directions of events recorded at the Pierre Auger Observatory; (7) Cosmic Ray Solar Modulation Studies in the Pierre Auger Observatory; (8) Investigation of the Displacement Angle of the Highest Energy Cosmic Rays Caused by the Galactic Magnetic Field; (9) Search for coincidences with astrophysical transients in Pierre Auger Observatory data; and (10) An alternative method for determining the energy of hybrid events at the Pierre Auger Observatory.

  2. The Cosmic Ray Energy Spectrum and Related Measurements with the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Abraham, : J.; Abreu, P.; Aglietta, M.; Aguirre, C.; Ahn, E.J.; Allard, D.; Allekotte, I.; Allen, J.; Alvarez-Muniz, J.; Ambrosio, M.; Anchordoqui, L.

    2009-06-01

    These are presentations to be presented at the 31st International Cosmic Ray Conference, in Lodz, Poland during July 2009. It consists of the following presentations: (1) Measurement of the cosmic ray energy spectrum above 10{sup 18} eV with the Pierre Auger Observatory; (2) The cosmic ray flux observed at zenith angles larger than 60 degrees with the Pierre Auger Observatory; (3) Energy calibration of data recorded with the surface detectors of the Pierre Auger Observatory; (4) Exposure of the Hybrid Detector of The Pierre Auger Observatory; and (5) Energy scale derived from Fluorescence Telescopes using Cherenkov Light and Shower Universality.

  3. Precision Solar Neutrino Measurements with the Sudbury Neutrino Observatory

    SciTech Connect (OSTI)

    Oblath, Noah

    2007-10-26

    The Sudbury Neutrino Observatory (SNO) is the first experiment to measure the total flux of active, high-energy neutrinos from the sun. Results from SNO have solved the long-standing 'Solar Neutrino Problem' by demonstrating that neutrinos change flavor. SNO measured the total neutrino flux with the neutral-current interaction of solar neutrinos with 1000 tonnes of D{sub 2}O. In the first two phases of the experiment we detected the neutron from that interaction by capture on deuterium and capture on chlorine, respectively. In the third phase an array of {sup 3}He proportional counters was deployed in the detector. This allows a measurement of the neutral-current neutrons that is independent of the Cherenkov light detected by the PMT array. We are currently developing a unique, detailed simulation of the current pulses from the proportional-counter array that will be used to help distinguish signal and background pulses.

  4. SPECKLE INTERFEROMETRY AT THE U.S. NAVAL OBSERVATORY. XVIII

    SciTech Connect (OSTI)

    Mason, Brian D.; Hartkopf, William I.; Friedman, Elizabeth A. E-mail: wih@usno.navy.mil

    2012-05-15

    The results of 2490 intensified CCD observations of double stars, made with the 26 inch refractor of the U.S. Naval Observatory, are presented. Each observation of a system represents a combination of over 2000 short-exposure images. These observations are averaged into 1462 mean relative positions and range in separation from 0.''56 to 71.''80, with a mean separation of 14.''81. This is the 18th in this series of papers and covers the period 2011 January 3 through 2011 December 18. Also presented are four pairs which are resolved for the first time, thirteen other pairs which appear to be lost, and linear elements for four additional pairs.

  5. SPECKLE INTERFEROMETRY AT THE U.S. NAVAL OBSERVATORY. XIX

    SciTech Connect (OSTI)

    Mason, Brian D.; Hartkopf, William I.; Hurowitz, Haley M. E-mail: wih@usno.navy.mil

    2013-09-15

    The results of 2916 intensified CCD observations of double stars, made with the 26 inch refractor of the U.S. Naval Observatory, are presented. Each observation of a system represents a combination of over two thousand short-exposure images. These observations are averaged into 1584 mean relative positions and range in separation from 0.''54 to 98.''09, with a median separation of 11.''73. This is the 19th in this series of papers and covers the period 2012 January 5 through 2012 December 18. Also presented are 10 pairs that are reported for the first time, 17 pairs that appear to be lost, linear elements for 18 pairs, and orbital elements for 2 additional pairs.

  6. SPECKLE INTERFEROMETRY AT THE U.S. NAVAL OBSERVATORY. XVI

    SciTech Connect (OSTI)

    Mason, Brian D.; Hartkopf, William I.; Wycoff, Gary L. E-mail: wih@usno.navy.mil

    2011-05-15

    The results of 1031 speckle-interferometric observations of double stars, made with the 26 inch refractor of the U.S. Naval Observatory, are presented. Each speckle-interferometric observation of a system represents a combination of over two thousand short-exposure images. These observations are averaged into 457 mean relative positions and range in separation from 0.''15 to 16.''94, with a median separation of 3.''03. The range in V-band magnitudes for the primary (secondary) of observed targets is 3.1-12.9 (3.2-13.3). This is the sixteenth in a series of papers presenting measurements obtained with this system and covers the period 2009 January 12 through 2009 December 17. Included in these data are 12 older measurements whose positions were previously deemed possibly aberrant, but are no longer classified this way following a confirming observation. Also, 10 pairs with a single observation are herein confirmed. This paper also includes the first data obtained using a new ICCD with fiber optic cables.

  7. Preliminary systems engineering evaluations for the National Ecological Observatory Network.

    SciTech Connect (OSTI)

    Robertson, Perry J.; Kottenstette, Richard Joseph; Crouch, Shannon M.; Brocato, Robert Wesley; Zak, Bernard Daniel; Osborn, Thor D.; Ivey, Mark D.; Gass, Karl Leslie; Heller, Edwin J.; Dishman, James Larry; Schubert, William Kent; Zirzow, Jeffrey A.

    2008-11-01

    The National Ecological Observatory Network (NEON) is an ambitious National Science Foundation sponsored project intended to accumulate and disseminate ecologically informative sensor data from sites among 20 distinct biomes found within the United States and Puerto Rico over a period of at least 30 years. These data are expected to provide valuable insights into the ecological impacts of climate change, land-use change, and invasive species in these various biomes, and thereby provide a scientific foundation for the decisions of future national, regional, and local policy makers. NEON's objectives are of substantial national and international importance, yet they must be achieved with limited resources. Sandia National Laboratories was therefore contracted to examine four areas of significant systems engineering concern; specifically, alternatives to commercial electrical utility power for remote operations, approaches to data acquisition and local data handling, protocols for secure long-distance data transmission, and processes and procedures for the introduction of new instruments and continuous improvement of the sensor network. The results of these preliminary systems engineering evaluations are presented, with a series of recommendations intended to optimize the efficiency and probability of long-term success for the NEON enterprise.

  8. The Final Results from the Sudbury Neutrino Observatory

    ScienceCinema (OSTI)

    None

    2011-04-25

    The Sudbury Neutrino Observatory (SNO) was a water Cherenkov detector dedicated to investigate elementary particles called neutrinos. It successfully took data between 1999 and 2006. The detector was unique in its use of heavy water as a detection medium, permitting it to make a solar model-independent test of solar neutrino mixing. In fact, SNO conclusively showed that solar neutrinos oscillate on their way from the core of the Sun to the Earth. This groundbreaking observation was made during three independent phases of the experiment. Even if data taking ended, SNO is still in a mode of precise determination of the solar neutrino oscillation parameters because all along SNO had developed several methods to tell charged-current events apart from neutral-current events. This ability is crucial for the final and ultimate data analysis of all the phases. The physics reach of a combined three-phase solar analysis will be reviewed together with results and subtleties about solar neutrino physics.

  9. SNO Data: Results from Experiments at the Sudbury Neutrino Observatory

    DOE Data Explorer [Office of Scientific and Technical Information (OSTI)]

    The Sudbury Neutrino Observatory (SNO) was built 6800 feet under ground, in INCO's Creighton mine near Sudbury, Ontario. SNO is a heavy-water Cherenkov detector that is designed to detect neutrinos produced by fusion reactions in the sun. It uses 1000 tonnes of heavy water, on loan from Atomic Energy of Canada Limited (AECL), contained in a 12 meter diameter acrylic vessel. Neutrinos react with the heavy water (D2O) to produce flashes of light called Cherenkov radiation. This light is then detected by an array of 9600 photomultiplier tubes mounted on a geodesic support structure surrounding the heavy water vessel. The detector is immersed in light (normal) water within a 30 meter barrel-shaped cavity (the size of a 10 story building!) excavated from Norite rock. Located in the deepest part of the mine, the overburden of rock shields the detector from cosmic rays. The detector laboratory is extremely clean to reduce background signals from radioactive elements present in the mine dust which would otherwise hide the very weak signal from neutrinos. (From http://www.sno.phy.queensu.ca/]

    The SNO website provides access to various datasets. See also the SNO Image Catalog at http://www.sno.phy.queensu.ca/sno/images/ and computer-generated images of SNO events at http://www.sno.phy.queensu.ca/sno/events/ and the list of published papers.

  10. The Astrophysical Plasmadynamic Explorer (APEX): A High Resolution Spectroscopic Observatory

    SciTech Connect (OSTI)

    Kowalski, M P; Cruddace, R G; Wood, K S; Yentis, D J; Gursky, H; Barbee, T W; Goldstein, W H; Kordas, J F; Fritz, G G; Hunter, W R; Barstow, M A; Bannister, N P; Culhane, J L; Lapington, J S

    2002-07-18

    EUVE and the ROSAT WFC have left a tremendous legacy in astrophysics at EUV wavelengths. More recently, Chandra and XMM-Newton have demonstrated at X-ray wavelengths the power of high-resolution astronomical spectroscopy, which allows the identification of weak emission lines, the measurement of Doppler shifts and line profiles, and the detection of narrow absorption features. This leads to a complete understanding of the density, temperature, abundance, magnetic, and dynamic structure of astrophysical plasmas. However, the termination of the EUVE mission has left a gaping hole in spectral coverage at crucial EUV wavelengths ({approx}100-300 {angstrom}), where hot (10{sup 5}-10{sup 8} K) plasmas radiate most strongly and produce critical spectral diagnostics. CHIPS will fill this hole only partially as it is optimized for diffuse emission and has only moderate resolution (R {approx} 150). For discrete sources, we have successfully flown a follow-on instrument to the EUVE spectrometer (A{sub eff} {approx} 1 cm{sup 2}, R {approx} 400), the high-resolution spectrometer J-PEX(A{sub eff} {approx} 3 cm{sup 2}, R {approx} 3000). Here we build on the J-PEX prototype and present a strawman design for an orbiting spectroscopic observatory, APEX, a SMEX-class instrument containing a suite of 8 spectrometers that together achieve both high effective area (A{sub eff} > 20 cm{sup 2}) and high spectral resolution (R {approx} 10,000) over the range 100-300 {angstrom}. We also discuss alternate configurations for shorter and longer wavelengths.

  11. INSIGHTS INTO FILAMENT ERUPTION ONSET FROM SOLAR DYNAMICS OBSERVATORY OBSERVATIONS

    SciTech Connect (OSTI)

    Sterling, Alphonse C.; Moore, Ronald L.; Freeland, Samuel L. E-mail: ron.moore@nasa.gov

    2011-04-10

    We examine the buildup to and onset of an active region filament confined eruption of 2010 May 12, using EUV imaging data from the Solar Dynamics Observatory (SDO) Atmospheric Imaging Array and line-of-sight magnetic data from the SDO Helioseismic and Magnetic Imager. Over the hour preceding eruption the filament undergoes a slow rise averaging {approx}3 km s{sup -1}, with a step-like trajectory. Accompanying a final rise step {approx}20 minutes prior to eruption is a transient preflare brightening, occurring on loops rooted near the site where magnetic field had canceled over the previous 20 hr. Flow-type motions of the filament are relatively smooth with speeds {approx}50 km s{sup -1} prior to the preflare brightening and appear more helical, with speeds {approx}50-100 km s{sup -1}, after that brightening. After a final plateau in the filament's rise, its rapid eruption begins, and concurrently an outer shell 'cocoon' of the filament material increases in emission in hot EUV lines, consistent with heating in a newly formed magnetic flux rope. The main flare brightenings start {approx}5 minutes after eruption onset. The main flare arcade begins between the legs of an envelope-arcade loop that is nearly orthogonal to the filament, suggesting that the flare results from reconnection among the legs of that loop. This progress of events is broadly consistent with flux cancellation leading to formation of a helical flux rope that subsequently erupts due to onset of a magnetic instability and/or runaway tether cutting.

  12. THE FOURTH US NAVAL OBSERVATORY CCD ASTROGRAPH CATALOG (UCAC4)

    SciTech Connect (OSTI)

    Zacharias, N.; Finch, C. T.; Bartlett, J. L.; Girard, T. M.; Henden, A.; Monet, D. G.; Zacharias, M. I.

    2013-02-01

    The fourth United States Naval Observatory (USNO) CCD Astrograph Catalog, UCAC4, was released in 2012 August (double-sided DVD and CDS data center Vizier catalog I/322). It is the final release in this series and contains over 113 million objects; over 105 million of them with proper motions (PMs). UCAC4 is an updated version of UCAC3 with about the same number of stars also covering all-sky. Bugs were fixed, Schmidt plate survey data were avoided, and precise five-band photometry was added for about half the stars. Astrograph observations have been supplemented for bright stars by FK6, Hipparcos, and Tycho-2 data to compile a UCAC4 star catalog complete from the brightest stars to about magnitude R = 16. Epoch 1998-2004 positions are obtained from observations with the 20 cm aperture USNO Astrograph's 'red lens', equipped with a 4k by 4k CCD. Mean positions and PMs are derived by combining these observations with over 140 ground- and space-based catalogs, including Hipparcos/Tycho and the AC2000.2, as well as unpublished measures of over 5000 plates from other astrographs. For most of the faint stars in the southern hemisphere, the first epoch plates from the Southern Proper Motion program form the basis for PMs, while the Northern Proper Motion first epoch plates serve the same purpose for the rest of the sky. These data are supplemented by 2MASS near-IR photometry for about 110 million stars and five-band (B, V, g, r, i) APASS data for over 51 million stars. Thus the published UCAC4, as were UCAC3 and UCAC2, is a compiled catalog with the UCAC observational program being a major component. The positional accuracy of stars in UCAC4 at mean epoch is about 15-100 mas per coordinate, depending on magnitude, while the formal errors in PMs range from about 1 to 10 mas yr{sup -1} depending on magnitude and observing history. Systematic errors in PMs are estimated to be about 1-4 mas yr{sup -1}.

  13. HSRL mass estimate based on CALIPSO

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

    NASA B-200 King Air ARCTASISDAC Operations and Science Richard Ferrare, Chris Hostetler, ... hours science *5 flights coordinated with NASA DC-8 *3 flights coordinated with NASA P-3 ...

  14. HSRL mass estimate based on CALIPSO

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

    NASA B-200 King Air ARCTAS/ISDAC Operations and Science Richard Ferrare, Chris Hostetler, John Hair, Anthony Cook, David Harper, Mike Obland, Ray Rogers, Sharon Burton, Matt Shupe, Dave Turner, Connor Flynn B200/HSRL Deployment During ARCTAS (Spring)  Independently measures aerosol/cloud extinction and backscatter profiles at 532 nm  Includes - Backscatter channels at 1064 nm - Polarization sensitivity at 532 and 1064 nm  Profile Measurement capabilities - Extensive measurements *

  15. Detecting gamma-ray bursts with the pierre auger observatory using the single particle technique

    SciTech Connect (OSTI)

    Allard, Denis; Parizot, E.; Bertou, Xavier; Beatty, J.; Vernois, M.Du; Nitz, D.; Rodriguez, G.

    2005-08-01

    During the past ten years, gamma-ray Bursts (GRB) have been extensively studied in the keV-MeV energy range but the higher energy emission still remains mysterious. Ground based observatories have the possibility to investigate energy range around one GeV using the ''single particle technique''. The aim of the present study is to investigate the capability of the Pierre Auger Observatory to detect the high energy emission of GRBs with such a technique. According to the detector response to photon showers around one GeV, and making reasonable assumptions about the high energy emission of GRBs, we show that the Pierre Auger Observatory is a competitive instrument for this technique, and that water tanks are very promising detectors for the single particle technique.

  16. Description of Atmospheric Conditions at the Pierre Auger Observatory using the Global Data Assimilation System (GDAS)

    SciTech Connect (OSTI)

    Abreu, P.; Aglietta, M.; Ahlers, M.; Ahn, E.J.; Albuquerque, I.F.M.; Allard, D.; Allekotte, I.; Allen, J.; Allison, P.; Almela, A.; Alvarez Castillo, J.; /Mexico U., ICN /Santiago de Compostela U.

    2012-01-01

    Atmospheric conditions at the site of a cosmic ray observatory must be known for reconstructing observed extensive air showers. The Global Data Assimilation System (GDAS) is a global atmospheric model predicated on meteorological measurements and numerical weather predictions. GDAS provides altitude-dependent profiles of the main state variables of the atmosphere like temperature, pressure, and humidity. The original data and their application to the air shower reconstruction of the Pierre Auger Observatory are described. By comparisons with radiosonde and weather station measurements obtained on-site in Malargue and averaged monthly models, the utility of the GDAS data is shown.

  17. Prospects for and Status of CUORE ? The Cryogenic Underground Observatory for Rare Events

    SciTech Connect (OSTI)

    Norman, E B

    2009-07-07

    CUORE (Cryogenic Underground Observatory for Rare Events) is a next generation experiment designed to search for the neutrinoless DBD of {sup 130}Te using a bolometric technique. The present status of the CUORE is presented along with the latest results from its prototype, CUORICINO.

  18. The search for extended air showers at the Jicamarca Radio Observatory

    SciTech Connect (OSTI)

    Wahl, D.; Chau, J.; Galindo, F.; Huaman, A.; Solano, C. J.

    2009-04-30

    This paper presents the status of the project to detect extended air showers at the Jicamarca Radio Observatory. We report on detected anomalous signals and present a toy model to estimate at what altitudes we might expect to see air shower signals. According to this model, a significant number of high altitude horizontal air showers could be observed by radar techniques.

  19. Reconstruction of inclined air showers detected with the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Aab, Alexander; et al.

    2014-08-08

    We describe the method devised to reconstruct inclined cosmic-ray air showers with zenith angles greater than 60° detected with the surface array of the Pierre Auger Observatory. The measured signals at the ground level are fitted to muon density distributions predicted with atmospheric cascade models to obtain the relative shower size as an overall normalization parameter. The method is evaluated using simulated showers to test its performance. The energy of the cosmic rays is calibrated using a sub-sample of events reconstructed with both the fluorescence and surface array techniques. The reconstruction method described here provides the basis of complementary analyses including an independent measurement of the energy spectrum of ultra-high energy cosmic rays using very inclined events collected by the Pierre Auger Observatory.

  20. High-Resolution Spectroscopy with the Chandra X-ray Observatory

    ScienceCinema (OSTI)

    Canizares, Claude R. [MIT, Cambridge, Massachusetts, United States

    2010-01-08

    The capabilities of the Chandra X-ray Observatory and XMM-Newton for high-resolution spectroscopy have brought tradition plasma diagnostic techniques to the study of cosmic plasma. Observations have probed nearly every class of astronomical object, from young proto-starts through massive O starts and black hole binaries, supernova remnants, active galactic nuclei, and the intergalactic medium. Many of these sources show remarkable rich spectra that reveal new physical information, such as emission measure distributions, elemental abundances, accretion disk and wind signatures, and time variability. This talk will present an overview of the Chandra instrumentaton and selected examples of spectral observations of astrophysical and cosmological importance.

  1. SPECKLE INTERFEROMETRY AT MOUNT WILSON OBSERVATORY: OBSERVATIONS OBTAINED IN 2006-2007 AND 35 NEW ORBITS

    SciTech Connect (OSTI)

    Hartkopf, William I.; Mason, Brian D. E-mail: bdm@usno.navy.mil

    2009-09-15

    Results are presented for 607 speckle interferometric observations of double stars, as well as 222 measures of single stars or unresolved pairs. All data were obtained in 2006 and 2007 at the Mount Wilson Observatory, using the 2.5 m Hooker telescope. Separations range from 0.''06 to 6.''31, with a median of 0.''34. These three observing runs concentrated on binaries in need of confirmation (mainly Hipparcos and Tycho pairs), as well as systems in need of improved orbital elements. New orbital solutions have been determined for 35 systems as a result.

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

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

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

    2014-08-19

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

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

    SciTech Connect (OSTI)

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

    2014-08-19

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

  4. Anisotropy studies around the Galactic Centre at EeV energies with the Auger Observatory

    SciTech Connect (OSTI)

    Aglietta, M.; Aguirre, C.; Allard, D.; Allekotte, I.; Allison, P.; Alvarez, C.; Alvarez-Muniz, J.; Ambrosio, M.; Anchordoqui, L.; Anjos, J.C.; Aramo, C.; ,

    2006-07-01

    Data from the Pierre Auger Observatory are analyzed to search for anisotropies near the direction of the Galactic Centre at EeV energies. The exposure of the surface array in this part of the sky is already significantly larger than that of the fore-runner experiments. Our results do not support previous findings of localized excesses in the AGASA and SUGAR data. We set an upper bound on a point-like flux of cosmic rays arriving from the Galactic Centre which excludes several scenarios predicting sources of EeV neutrons from Sagittarius A. Also the events detected simultaneously by the surface and fluorescence detectors (the ''hybrid'' data set), which have better pointing accuracy but are less numerous than those of the surface array alone, do not show any significant localized excess from this direction.

  5. The exposure of the hybrid detector of the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Not Available

    2010-06-01

    The Pierre Auger Observatory is a detector for ultra-high energy cosmic rays. It consists of a surface array to measure secondary particles at ground level and a fluorescence detector to measure the development of air showers in the atmosphere above the array. The 'hybrid' detection mode combines the information from the two subsystems. We describe the determination of the hybrid exposure for events observed by the fluorescence telescopes in coincidence with at least one water-Cherenkov detector of the surface array. A detailed knowledge of the time dependence of the detection operations is crucial for an accurate evaluation of the exposure. We discuss the relevance of monitoring data collected during operations, such as the status of the fluorescence detector, background light and atmospheric conditions, that are used in both simulation and reconstruction.

  6. The X-Ray Microcalorimeter Spectrometer for the International X-Ray Observatory

    SciTech Connect (OSTI)

    Kelley, R. L.; Bandler, S. R.; Kilbourne, C. A.; Porter, F. S.; Shirron, P.; Smith, S. J.; Whitehouse, P.; Ezoe, Y.; Ishisaki, Y.; Ohashi, T.; Fujimoto, R.; Sato, K.; Gottardi, L.; Hartog, R. den; Herder, J.-W. den; Hoevers, H.; Korte, P. de; Kuur, J. van der

    2009-12-16

    The International X-Ray Observatory (IXO) is under formulation by NASA, ESA and JAXA for deployment in 2022. IXO emerged over the last 18 months as the NASA Constellation-X and ESA/JAXA X-Ray Evolving Universe Spectrometer (XEUS) missions were combined. The driving performance requirements for the X-Ray Microcalorimeter Spectrometer (XMS) are a spectral resolution of 2.5 eV over the central 2'x2' in the 0.3-7.0 keV band, and 10 eV to the edge of the 5'x5' field of view (FOV). The XMS is now based on a microcalorimeter array of Transition-Edge Sensor (TES) thermometers with Au/Bi absorbers and a SQUID MUX readout. One of the concepts studied as part of the mission formulation has a core 40x40 array corresponding to a 2'x2' FOV with 3'' pixels surrounded by an outer, annular 52x52 array of 6'' pixels that extends the field of view to 5.4'x5.4' with better than 10 eV resolution. There are several options for implementing the readout and cooling system of the XMS under study in the US, Europe and Japan. The ADR system will have from two to five stages depending on the performance of the cryocooler. Mechanical coolers with sufficient cooling power at 4K are available now, and {approx}2K coolers are under development. In this paper we give an overview of the XMS instrument, and some of the tradeoffs to be addressed for this observatory instrument.

  7. Energy Estimation of Cosmic Rays with the Engineering Radio Array of the Pierre Auger Observatory

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

    Aab, Alexander

    2016-06-14

    The Auger Engineering Radio Array (AERA) is part of the Pierre Auger Observatory and is used to detect the radio emission of cosmic-ray air showers. These observations are compared to the data of the surface detector stations of the Observatory, which provide well-calibrated information on the cosmic-ray energies and arrival directions. The response of the radio stations in the 30 to 80MHz regime has been thoroughly calibrated to enable the reconstruction of the incoming electric field. For the latter, the energy density is determined from the radio pulses at each observer position and is interpolated using a two dimensional functionmore » that takes into account signal asymmetries due to interference between the geomagnetic and charge excess emission components. We found that the spatial integral over the signal distribution gives a direct measurement of the energy transferred from the primary cosmic ray into radio emission in the AERA frequency range. We measure 15.8MeV of radiation energy for a 1 EeV air shower arriving perpendicularly to the geomagnetic field. This radiation energy – corrected for geometrical effects – is used as a cosmic-ray energy estimator. Performing an absolute energy calibration against the surface-detector information, we observe that this radio-energy estimator scales quadratically with the cosmic-ray energy as expected for coherent emission. Finally we find an energy resolution of the radio reconstruction of 22% for the data set and 17% for a high-quality subset containing only events with at least five radio stations with signal.« less

  8. Energy Estimation of Cosmic Rays with the Engineering Radio Array of the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Aab, Alexander

    2015-08-19

    The Auger Engineering Radio Array (AERA) is part of the Pierre Auger Observatory and is used to detect the radio emission of cosmic-ray air showers. These observations are compared to the data of the surface detector stations of the Observatory, which provide well-calibrated information on the cosmic-ray energies and arrival directions. The response of the radio stations in the 30 to 80MHz regime has been thoroughly calibrated to enable the reconstruction of the incoming electric field. For the latter, the energy density is determined from the radio pulses at each observer position and is interpolated using a two dimensional function that takes into account signal asymmetries due to interference between the geomagnetic and charge excess emission components. We found that the spatial integral over the signal distribution gives a direct measurement of the energy transferred from the primary cosmic ray into radio emission in the AERA frequency range. We measure 15.8MeV of radiation energy for a 1 EeV air shower arriving perpendicularly to the geomagnetic field. This radiation energy – corrected for geometrical effects – is used as a cosmic-ray energy estimator. Performing an absolute energy calibration against the surface-detector information, we observe that this radio-energy estimator scales quadratically with the cosmic-ray energy as expected for coherent emission. Finally we find an energy resolution of the radio reconstruction of 22% for the data set and 17% for a high-quality subset containing only events with at least five radio stations with signal.

  9. The next generation of axion helioscopes: The international axion observatory (IAXO)

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

    Vogel, J. K.; Armengaud, E.; Avignone, F. T.; Betz, M.; Brax, P.; Brun, P.; Cantatore, G.; Carmona, J. M.; Carosi, G. P.; Caspers, F.; et al

    2015-03-24

    The International Axion Observatory (IAXO) is a proposed 4th-generation axion helioscope with the primary physics research goal to search for solar axions via their Primakoff conversion into photons of 1 – 10 keV energies in a strong magnetic field. IAXO will achieve a sensitivity to the axion-photon coupling gaγ down to a few ×10⁻¹² GeV⁻¹ for a wide range of axion masses up to ~ 0.25 eV. This is an improvement over the currently best (3rd generation) axion helioscope, the CERN Axion Solar Telescope (CAST), of about 5 orders of magnitude in signal strength, corresponding to a factor ~ 20more » in the axion photon coupling. IAXO’s sensitivity relies on the construction of a large superconducting 8-coil toroidal magnet of 20 m length optimized for axion research. Each of the eight 60 cm diameter magnet bores is equipped with x-ray optics focusing the signal photons into ~ 0.2 cm² spots that are imaged by very low background x-ray detectors. The magnet will be built into a structure with elevation and azimuth drives that will allow solar tracking for 12 hours each day. This contribution is a summary of our papers [1, 2, 3] and we refer to these for further details.« less

  10. High-Energy Cosmic Ray Event Data from the Pierre Auger Cosmic Ray Observatory

    DOE Data Explorer [Office of Scientific and Technical Information (OSTI)]

    The Pierre Auger Cosmic Ray Observatory in Mendoza, Argentina is the result of an international collaboration funded by 15 countries and many different organizations. Its mission is to capture high-energy cosmic ray events or air showers for research into their origin and nature. The Pierre Auger Collaboration agreed to make 1% of its data available to the public. The Public Event Explorer is a search tool that allows users to browse or search for and display figures and data plots of events collected since 2004. The repository is updated daily, and, as of June, 2014, makes more than 35,000 events publicly available. The energy of a cosmic ray is measured in Exa electron volts or EeV. These event displays can be browsed in order of their energy level from 0.1 to 41.1 EeV. Each event has an individual identification number.

    The event displays provide station data, cosmic ray incoming direction, various energy measurements, plots, vector-based images, and an ASCII data file.

  11. Prototype muon detectors for the AMIGA component of the Pierre Auger Observatory

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

    Aab, Alexander

    2016-02-17

    AMIGA (Auger Muons and Infill for the Ground Array) is an upgrade of the Pierre Auger Observatory to extend its range of detection and to directly measure the muon content of the particle showers. It consists of an infill of surface water-Cherenkov detectors accompanied by buried scintillator detectors used for muon counting. The main objectives of the AMIGA engineering array, referred to as the Unitary Cell, are to identify and resolve all engineering issues as well as to understand the muon-number counting uncertainties related to the design of the detector. The mechanical design, fabrication and deployment processes of the muonmore » counters of the Unitary Cell are described in this document. These muon counters modules comprise sealed PVC casings containing plastic scintillation bars, wavelength-shifter optical fibers, 64 pixel photomultiplier tubes, and acquisition electronics. The modules are buried approximately 2.25 m below ground level in order to minimize contamination from electromagnetic shower particles. The mechanical setup, which allows access to the electronics for maintenance, is also described in addition to tests of the modules' response and integrity. As a result, the completed Unitary Cell has measured a number of air showers of which a first analysis of a sample event is included here.« less

  12. THE VECTOR VORTEX CORONAGRAPH: LABORATORY RESULTS AND FIRST LIGHT AT PALOMAR OBSERVATORY

    SciTech Connect (OSTI)

    Mawet, D.; Serabyn, E.; Liewer, K.; Burruss, R.; Hickey, J.; Shemo, D.

    2010-01-20

    High-contrast coronagraphy will be needed to image and characterize faint extrasolar planetary systems. Coronagraphy is a rapidly evolving field, and many enhanced alternatives to the classical Lyot coronagraph have been proposed in the past 10 years. Here, we discuss the operation of the vector vortex coronagraph, which is one of the most efficient possible coronagraphs. We first present recent laboratory results and then first light observations at the Palomar observatory. Our near-infrared H-band (centered at approx1.65 mum) and K-band (centered at approx2.2 mum) vector vortex devices demonstrated excellent contrast results in the lab, down to approx10{sup -6} at an angular separation of approx3lambda/d. On sky, we detected a brown dwarf companion 3000 times fainter than its host star (HR 7672) in the K{sub s} band (centered at approx2.15 mum), at an angular separation of approx2.5lambda/d. Current and next-generation high-contrast instruments can directly benefit from the demonstrated capabilities of such a vector vortex: simplicity, small inner working angle, high optical throughput (>90%), and maximal off-axis discovery space.

  13. TARGET SELECTION FOR THE APACHE POINT OBSERVATORY GALACTIC EVOLUTION EXPERIMENT (APOGEE)

    SciTech Connect (OSTI)

    Zasowski, G.; Johnson, Jennifer A.; Andrews, B.; Epstein, C.; Frinchaboy, P. M.; Jackson, K.; Majewski, S. R.; Chojnowski, S. D.; Skrutskie, M. F.; Beaton, R. L.; Nidever, D. L.; Pinto, H. J. Rocha; Girardi, L.; Cudworth, K. M.; Munn, J.; Blake, C. H.; Covey, K.; Deshpande, R.; Fleming, S. W.; Fabbian, D. [Instituto de Astrofisica de Canarias, Calle Via Lactea s and others

    2013-10-01

    The Apache Point Observatory Galactic Evolution Experiment (APOGEE) is a high-resolution infrared spectroscopic survey spanning all Galactic environments (i.e., bulge, disk, and halo), with the principal goal of constraining dynamical and chemical evolution models of the Milky Way. APOGEE takes advantage of the reduced effects of extinction at infrared wavelengths to observe the inner Galaxy and bulge at an unprecedented level of detail. The survey's broad spatial and wavelength coverage enables users of APOGEE data to address numerous Galactic structure and stellar populations issues. In this paper we describe the APOGEE targeting scheme and document its various target classes to provide the necessary background and reference information to analyze samples of APOGEE data with awareness of the imposed selection criteria and resulting sample properties. APOGEE's primary sample consists of {approx}10{sup 5} red giant stars, selected to minimize observational biases in age and metallicity. We present the methodology and considerations that drive the selection of this sample and evaluate the accuracy, efficiency, and caveats of the selection and sampling algorithms. We also describe additional target classes that contribute to the APOGEE sample, including numerous ancillary science programs, and we outline the targeting data that will be included in the public data releases.

  14. Muons in air showers at the Pierre Auger Observatory: Mean number in highly inclined events

    SciTech Connect (OSTI)

    Aab, Alexander

    2015-03-09

    We present the first hybrid measurement of the average muon number in air showers at ultra-high energies, initiated by cosmic rays with zenith angles between 62° and 80° . Our measurement is based on 174 hybrid events recorded simultaneously with the Surface Detector array and the Fluorescence Detector of the Pierre Auger Observatory. The muon number for each shower is derived by scaling a simulated reference profile of the lateral muon density distribution at the ground until it fits the data. A 1019 eV shower with a zenith angle of 67°, which arrives at the Surface Detector array at an altitude of 1450 m above sea level, contains on average (2.68 ± 0.04 ± 0.48 (sys.)) × 107 muons with energies larger than 0.3 GeV. Finally, the logarithmic gain d ln Nµ/d ln E of muons with increasing energy between 4 × 1018 eV and 5 × 1019 eV is measured to be (1.029 ± 0.024 ± 0.030 (sys.)).

  15. Upper limit on the diffuse flux of UHE tau neutrinos from the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Collaboration, The Pierre Auger

    2007-12-01

    The surface detector array of the Pierre Auger Observatory is sensitive to Earth-skimming tau-neutrinos {nu}{sub {tau}} that interact in the Earth's crust. Tau leptons from {tau}{sub {tau}} charged-current interactions can emerge and decay in the atmosphere to produce a nearly horizontal shower with a significant electromagnetic component. The data collected between 1 January 2004 and 31 August 2007 is used to place an upper limit on the diffuse flux of {nu}{sub {tau}} at EeV energies. Assuming an E{sub {nu}}{sup -2} differential energy spectrum the limit set at 90 % C.L. is E{sub {nu}}{sup 2} dN{sub {nu}{sub {tau}}}/dE{sub {nu}} < 1.3 x 10{sup -7} GeV cm{sup -2} s{sup -1} sr{sup -1} in the energy range 2 x 10{sup 17} eV < E{sub {nu}} < 2 x 10{sup 19} eV.

  16. The search for TeV-scale dark matter with the HAWC observatory

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

    Harding, J. Patrick

    2015-01-01

    The High Altitude Water Cherenkov (HAWC) observatory is a wide field-of-view detector sensitive to 100 GeV - 100 TeV gamma rays and cosmic rays. Located at an elevation of 4100 m on the Sierra Negra mountain in Mexico, HAWC observes extensive air showers from gamma and cosmic rays with an array of water tanks which produce Cherenkov light in the presence of air showers. With a field-of-view capable of observing 2/3 of the sky each day, and a sensitivity of 1 Crab/day, HAWC will be able to map out the sky in gamma and cosmic rays in detail. In thismore » paper, we discuss the capabilities of HAWC to map out the directions and spectra of TeV gamma rays and cosmic rays coming from sources of dark matter annihilation. We discuss the HAWC sensitivity to multiple extended sources of dark matter annihilation and the possibility of HAWC observations of annihilations in nearby dark matter subhalos.« less

  17. Measurement of the Cosmic Ray and Neutrino-Induced Muon Flux at the Sudbury Neutrino Observatory

    DOE R&D Accomplishments [OSTI]

    SNO collaboration; Aharmim, B.; Ahmed, S. N.; Andersen, T. C.; Anthony, A. E.; Barros, N.; Beier, E. W.; Bellerive, A.; Beltran, B.; Bergevin, M.; Biller, S. D.; Boudjemline, K.; Boulay, M. G.; Burritt, T. H.; Cai, B.; Chan, Y. D.; Chen, M.; Chon, M. C.; Cleveland, B. T.; Cox-Mobrand, G. A.; Currat, C. A.; Dai, X.; Dalnoki-Veress, F.; Deng, H.; Detwiler, J.; Doe, P. J.; Dosanjh, R. S.; Doucas, G.; Drouin, P.-L.; Duncan, F. A.; Dunford, M.; Elliott, S. R.; Evans, H. C.; Ewan, G. T.; Farine, J.; Fergani, H.; Fleurot, F.; Ford, R. J.; Formaggio, J. A.; Gagnon, N.; Goon, J. TM.; Grant, D. R.; Guillian, E.; Habib, S.; Hahn, R. L.; Hallin, A. L.; Hallman, E. D.; Hargrove, C. K.; Harvey, P. J.; Harvey, P. J.; Heeger, K. M.; Heintzelman, W. J.; Heise, J.; Helmer, R. L.; Hemingway, R. J.; Henning, R.; Hime, A.; Howard, C.; Howe, M. A.; Huang, M.; Jamieson, B.; Jelley, N. A.; Klein, J. R.; Kos, M.; Kruger, A.; Kraus, C.; Krauss, C. B.; Kutter, T.; Kyba, C. C. M.; Lange, R.; Law, J.; Lawson, I. T.; Lesko, K. T.; Leslie, J. R.; Levine, I.; Loach, J. C.; Luoma, S.; MacLellan, R.; Majerus, S.; Mak, H. B.; Maneira, J.; Marino, A. D.; Martin, R.; McCauley, N.; McDonald, A. B.; McGee, S.; Mifflin, C.; Miller, M. L.; Monreal, B.; Monroe, J.; Noble, A. J.; Oblath, N. S.; Okada, C. E.; O'Keeffe, H. M.; Opachich, Y.; Orebi Gann, G. D.; Oser, S. M.; Ott, R. A.; Peeters, S. J. M.; Poon, A. W. P.; Prior, G.; Rielage, K.; Robertson, B. C.; Robertson, R. G. H.; Rollin, E.; Schwendener, M. H.; Secrest, J. A.; Seibert, S. R.; Simard, O.; Simpson, J. J.; Sinclair, D.; Skensved, P.; Smith, M. W. E.; Sonley, T. J.; Steiger, T. D.; Stonehill, L. C.; Tagg, N.; Tesic, G.; Tolich, N.; Tsui, T.; Van de Water, R. G.; VanDevender, B. A.; Virtue, C. J.; Waller, D.; Waltham, C. E.; Wan Chan Tseung, H.; Wark, D. L.; Watson, P.; Wendland, J.; West, N.; Wilkerson, J. F.; Wilson, J. R.; Wouters, J. M.; Wright, A.; Yeh, M.; Zhang, F.; Zuber, K.

    2009-07-10

    Results are reported on the measurement of the atmospheric neutrino-induced muon flux at a depth of 2 kilometers below the Earth's surface from 1229 days of operation of the Sudbury Neutrino Observatory (SNO). By measuring the flux of through-going muons as a function of zenith angle, the SNO experiment can distinguish between the oscillated and un-oscillated portion of the neutrino flux. A total of 514 muon-like events are measured between -1 {le} cos {theta}{sub zenith} 0.4 in a total exposure of 2.30 x 10{sup 14} cm{sup 2} s. The measured flux normalization is 1.22 {+-} 0.09 times the Bartol three-dimensional flux prediction. This is the first measurement of the neutrino-induced flux where neutrino oscillations are minimized. The zenith distribution is consistent with previously measured atmospheric neutrino oscillation parameters. The cosmic ray muon flux at SNO with zenith angle cos {theta}{sub zenith} > 0.4 is measured to be (3.31 {+-} 0.01 (stat.) {+-} 0.09 (sys.)) x 10{sup -10} {micro}/s/cm{sup 2}.

  18. Muons in air showers at the Pierre Auger Observatory: Mean number in highly inclined events

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

    Aab, Alexander

    2015-03-09

    We present the first hybrid measurement of the average muon number in air showers at ultra-high energies, initiated by cosmic rays with zenith angles between 62° and 80° . Our measurement is based on 174 hybrid events recorded simultaneously with the Surface Detector array and the Fluorescence Detector of the Pierre Auger Observatory. The muon number for each shower is derived by scaling a simulated reference profile of the lateral muon density distribution at the ground until it fits the data. A 1019 eV shower with a zenith angle of 67°, which arrives at the Surface Detector array at anmore » altitude of 1450 m above sea level, contains on average (2.68 ± 0.04 ± 0.48 (sys.)) × 107 muons with energies larger than 0.3 GeV. Finally, the logarithmic gain d ln Nµ/d ln E of muons with increasing energy between 4 × 1018 eV and 5 × 1019 eV is measured to be (1.029 ± 0.024 ± 0.030 (sys.)).« less

  19. HOMOLOGOUS FLUX ROPES OBSERVED BY THE SOLAR DYNAMICS OBSERVATORY ATMOSPHERIC IMAGING ASSEMBLY

    SciTech Connect (OSTI)

    Li, Ting; Zhang, Jun E-mail: zjun@nao.cas.cn

    2013-12-01

    We present the first Solar Dynamics Observatory observations of four homologous flux ropes in the active region (AR) 11745 on 2013 May 20-22. The four flux ropes are all above the neutral line of the AR, with endpoints anchoring at the same region, and have a generally similar morphology. The first three flux ropes rose with a velocity of less than 30km s{sup 1} after their appearance, and subsequently their intensities at 131 decreased and the flux ropes became obscure. The fourth flux rope erupted last, with a speed of about 130km s{sup 1} and formed a coronal mass ejection (CME). The associated filament showed an obvious anti-clockwise twist motion at the initial stage, and the twist was estimated at 4?. This indicates that kink instability possibly triggers the early rise of the fourth flux rope. The activated filament material was spatially within the flux rope and showed consistent evolution in the early stages. Our findings provide new clues for understanding the characteristics of flux ropes. Firstly, multiple flux ropes are successively formed at the same location during an AR evolution process. Secondly, a slow-rise flux rope does not necessarily result in a CME, and a fast-eruption flux rope does result in a CME.

  20. THREE-DIMENSIONAL RECONSTRUCTION OF AN ERUPTING FILAMENT WITH SOLAR DYNAMICS OBSERVATORY AND STEREO OBSERVATIONS

    SciTech Connect (OSTI)

    Li Ting; Zhang Jun; Zhang Yuzong; Yang Shuhong E-mail: zjun@nao.cas.cn

    2011-09-20

    On 2010 August 1, a global solar event was launched involving almost the entire Earth-facing side of the Sun. This event mainly consisted of a C3.2 flare, a polar crown filament eruption, and two Earth-directed coronal mass ejections. The observations from the Solar Dynamics Observatory (SDO) and STEREO showed that all the activities were coupled together, suggesting a global character of the magnetic eruption. We reconstruct the three-dimensional geometry of the polar crown filament using observations from three different viewpoints (STEREO A, STEREO B, and SDO) for the first time. The filament undergoes two eruption processes. First, the main body of the filament rises up, while it also moves toward the low-latitude region with a change in inclination by {approx}48{sup 0} and expands only in the altitudinal and latitudinal direction in the field of view of the Atmospheric Imaging Assembly. We investigate the true velocities and accelerations of different locations along the filament and find that the highest location always has the largest acceleration during this eruption process. During the late phase of the first eruption, part of the filament material separates from the eastern leg. This material displays a projectile motion and moves toward the west at a constant velocity of 141.8 km s{sup -1}. This may imply that the polar crown filament consists of at least two groups of magnetic systems.

  1. EMERGING DIMMINGS OF ACTIVE REGIONS OBSERVED BY THE SOLAR DYNAMICS OBSERVATORY

    SciTech Connect (OSTI)

    Zhang Jun; Yang Shuhong [Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012 (China); Liu Yang; Sun Xudong, E-mail: zjun@nao.cas.cn, E-mail: shuhongyang@nao.cas.cn, E-mail: yliu@sun.stanford.edu, E-mail: xudong@sun.stanford.edu [W. W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305-4085 (United States)

    2012-12-01

    Using the observations from the Atmospheric Imaging Assembly and the Helioseismic and Magnetic Imager on board the Solar Dynamics Observatory, we statistically investigate the emerging dimmings (EDs) of 24 isolated active regions (IARs) from 2010 June to 2011 May. All the IARs show EDs in lower-temperature lines (e.g., 171 A) at their early emerging stages. Meanwhile, in higher temperature lines (e.g., 211 A), the ED regions brighten continuously. There are two types of EDs: fan-shaped and halo-shaped. There are 19 fan-shaped EDs and 5 halo-shaped ones. The EDs appear to be delayed by several to more than ten hours relative to the first emergence of the IARs. The shortest delay is 3.6 hr and the longest is 19.0 hr. The EDs last from 3.3 hr to 14.2 hr, with a mean duration of 8.3 hr. Before the appearance of the EDs, the emergence rate of the magnetic flux of the IARs is between 1.2 Multiplication-Sign 10{sup 19} Mx hr{sup -1} to 1.4 Multiplication-Sign 10{sup 20} Mx hr{sup -1}. The larger the emergence rate is, the shorter the delay time is. While the dimmings appear, the magnetic flux of the IARs ranges from 8.8 Multiplication-Sign 10{sup 19} Mx to 1.3 Multiplication-Sign 10{sup 21} Mx. These observations imply that the reconfiguration of the coronal magnetic fields due to reconnection between the newly emerging flux and the surrounding existing fields results in a new thermal distribution which leads to a dimming for the cooler channel (171 A) and brightening in the warmer channels.

  2. URBAN ATMOSPHERIC OBSERVATORY (UAO) FIRST PLANNING WORKSHOP, JANUARY 27-28-2003. WORKSHOP SUMMARY.

    SciTech Connect (OSTI)

    REYNOLDS,R.M.; LEE,H.N.

    2003-03-27

    The Urban Atmospheric Observatory (UAO) First Planning Workshop was held on 27-28 January 2003 at the Environmental Measurements Laboratory (EML) in downtown Manhattan, New York City. The meeting was well attended by local, state, and national administrators, as well as scientists and engineers from the national laboratories and academia. The real-time intensive UAO is a necessary step toward the development and validation of new technologies in support of the New York City emergency management and anti-terrorism effort. The real-time intensive UAO will be a dense array of meteorological instrumentation, remote sensing and satellite products and model output, as well as radiation detection, gamma spectrometer and aerosol measurements focused onto a small area in the heart of Manhattan. Such a test-bed, developed in a somewhat homogeneous urban area, and with a well-developed communication and data collection backbone, will be of immense utility for understanding how models of all scales can be improved and how they can best be integrated into the city's emergency program. The goal of the First Planning Workshop was to bring together a small group of experts in the fields of urban meteorology, modeling from mesoscale to fine-mesh computational fluid dynamics, instrumentation, communications and visualization, in order to (1) establish the importance of the observational program, (2) define the most efficient and cost-effective design for the program, (3) define needed intensive observational efforts and establish a schedule, and (4) define the importance of the UAO in emergency operations. The workshop achieved its goals with the enthusiastic participation of over forty persons. There was a synthesis of ideas towards a world-class facility that would benefit both immediate emergency management activities and, over an extended time, the entire field of urban meteorology and contaminant dispersion modeling.

  3. Simulation of subsurface thermal regimes of polygonal tundra at Barrow Environmental Observatory

    DOE Data Explorer [Office of Scientific and Technical Information (OSTI)]

    Richard T. Mills; Jitendra Kumar; Vladimir Romanovsky; Peter E. Thornton; Gautam Bisht; Colleen M. Iversen; Nathan Collier

    2016-01-27

    Vast carbon stocks stored in permafrost soils of Arctic tundra are under risk of release to atmosphere under warming climate. Ice--wedge polygons in the low-gradient polygonal tundra create a complex mosaic of microtopographic features. The microtopography plays a critical role in regulating the fine scale variability in thermal and hydrological regimes in the polygonal tundra landscape underlain by continuous permafrost. Modeling of thermal regimes of this sensitive ecosystem is essential for understanding the landscape behaviour under current as well as changing climate. We present here an end-to-end effort for high resolution numerical modeling of thermal hydrology at real-world field sites, utilizing the best available data to characterize and parameterize the models. We develop approaches to model the thermal hydrology of polygonal tundra and apply them at four study sites at Barrow, Alaska spanning across low to transitional to high-centered polygon and representative of broad polygonal tundra landscape. A multi--phase subsurface thermal hydrology model (PFLOTRAN) was developed and applied to study the thermal regimes at four sites. Using high resolution LiDAR DEM, microtopographic features of the landscape were characterized and represented in the high resolution model mesh. Best available soil data from field observations and literature was utilized to represent the complex hetogeneous subsurface in the numerical model. This data collection provides the complete set of input files, forcing data sets and computational meshes for simulations using PFLOTRAN for four sites at Barrow Environmental Observatory. It also document the complete computational workflow for this modeling study to allow verification, reproducibility and follow up studies.

  4. Observations of comet ISON (C/2012 S1) from Lowell observatory

    SciTech Connect (OSTI)

    Knight, Matthew M.; Schleicher, David G.

    2015-01-01

    We observed the dynamically new sungrazing comet ISON (C/2012 S1) extensively at Lowell Observatory throughout 2013 in order to characterize its behavior prior to perihelion. ISON had typical abundances for an Oort Cloud comet. Its dust production, as measured by Af?, remained nearly constant during the apparition but its CN gas production increased by ?50 . The minimum active area necessary to support observed water production rates exceeded the likely surface area of the nucleus and suggests a population of icy grains in the coma. Together with the flattening of the dust radial profile over time, this is consistant with ejection of a large quantity of slow moving dust and icy grains in the coma at large heliocentric distance. The dust morphology was dominated by the tail, but a faint sunward dust fan was detected in March, April, May, and September. We imaged multiple gas species in September, October, and November. All gas species were more extended than the dust coma, although only CN had sufficient signal-to-noise for detailed morphological study. Excess CN signal was observed in the sunward hemisphere in September and early October. In November the excess CN signal was in the tailward hemisphere and two faint CN features appeared approximately orthogonal to the tail with position angles varying by about 20 from night to night. Using numerical modeling, we best reproduced the orientation and shape of these features as well as the bulk brightness with a pole oriented approximately toward the Sun and a single source located within ?35 of the equator. Variations in position angle and relative brightness of the CN features from night to night suggest a rotation period shorter than 24 hr. The production rates and coma morphology suggest a nucleus that was active over nearly its entire sunward facing hemisphere in September and October but which underwent a significant mass loss event, potentially including fragmentation, shortly before November 1. Significant

  5. Quartz tube extensometer for observation of Earth tides and local tectonic deformations at the Sopronbanfalva Geodynamic Observatory, Hungary

    SciTech Connect (OSTI)

    Mentes, Gy.

    2010-07-15

    In May 1990, a quartz tube extensometer was installed in the Sopronbanfalva Geodynamic Observatory of the Geodetic and Geophysical Research Institute (GGRI) of the Hungarian Academy of Sciences for recording Earth tides and recent tectonic movements. The paper describes the construction of the extensometer and a portable calibrator used for the in situ calibration of the instrument. The extensometer is very sensitive. Its scale factor is 2.093{+-}0.032 nm/mV according to the highly precise calibration method developed at the GGRI. Since the stability of extensometers is strongly influenced by the geological structure and properties of the rocks in the vicinity of the recording site, the observatory instrument system was tested by coherence analysis between theoretical (as the input signal) and measured tidal data series (as the output signal). In the semidiurnal tidal frequency band the coherence is better than 0.95, while in the diurnal band it is about 0.8. Probably this is due to the fact that the noise is higher in the diurnal band (0.4-0.5 nstr) than in the semidiurnal band (0.19-0.22 nstr). Coherence analysis between theoretical and measured data corrected for barometric changes yielded a small improvement of coherence in both frequency bands, while using temperature data correction, no observable improvement was obtained. Results of the tidal analysis also show that the observatory instrument system is suitable for recording very small tectonic movements. The 18 years of continuous data series measured by the extensometer prove the high quality of the extensometer. On the basis of investigations, it was pointed out that further efforts should be done to improve the barometric correction method and that correction for ocean load, as well as considering topographic and cavity effects are necessary to increase the accuracy of determining tidal parameters.

  6. Measurement of the Proton-Air Cross Section at ?s=57 TeV with the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Abreu, P.; Aglietta, M.; Ahn, E. J.; Albuquerque, I. F. M.; Allard, D.; Allekotte, I.; Allen, J.; Allison, P.; Almeda, A.; Alvarez Castillo, J.; Alvarez-Muiz, J.; Ambrosio, M.; Aminaei, A.; Anchordoqui, L.; Andringa, S.; Anti?i?, T.; Aramo, C.; Arganda, E.; Arqueros, F.; Asorey, H.; Assis, P.; Aublin, J.; Ave, M.; Avenier, M.; Avila, G.; Bcker, T.; Balzer, M.; Barber, K. B.; Barbosa, A. F.; Bardenet, R.; Barroso, S. L. C.; Baughman, B.; Buml, J.; Beatty, J. J.; Becker, B. R.; Becker, K. H.; Belltoile, A.; Bellido, J. A.; BenZvi, S.; Berat, C.; Bertou, X.; Biermann, P. L.; Billoir, P.; Blanco, F.; Blanco, M.; Bleve, C.; Blmer, H.; Boh?ov, M.; Boncioli, D.; Bonifazi, C.; Bonino, R.; Borodai, N.; Brack, J.; Brogueira, P.; Brown, W. C.; Bruijn, R.; Buchholz, P.; Bueno, A.; Burton, R. E.; Caballero-Mora, K. S.; Caramete, L.; Caruso, R.; Castellina, A.; Catalano, O.; Cataldi, G.; Cazon, L.; Cester, R.; Chauvin, J.; Cheng, S. H.; Chiavassa, A.; Chinellato, J. A.; Chirinos Diaz, J.; Chudoba, J.; Clay, R. W.; Coluccia, M. R.; Conceio, R.; Contreras, F.; Cook, H.; Cooper, M. J.; Coppens, J.; Cordier, A.; Coutu, S.; Covault, C. E.; Creusot, A.; Criss, A.; Cronin, J.; Curutiu, A.; Dagoret-Campagne, S.; Dallier, R.; Dasso, S.; Daumiller, K.; Dawson, B. R.; de Almeida, R. M.; De Domenico, M.; De Donato, C.; de Jong, S. J.; De La Vega, G.; de Mello Junior, W. J. M.; de Mello Neto, J. R. T.; De Mitri, I.; de Souza, V.; de Vries, K. D.; Decerprit, G.; del Peral, L.; del Ro, M.; Deligny, O.; Dembinski, H.; Dhital, N.; Di Giulio, C.; Daz Castro, M. L.; Diep, P. N.; Dobrigkeit, C.; Docters, W.; DOlivo, J. C.; Dong, P. N.; Dorofeev, A.; dos Anjos, J. C.; Dova, M. T.; DUrso, D.; Dutan, I.; Ebr, J.; Engel, R.; Erdmann, M.; Escobar, C. O.; Espadanal, J.; Etchegoyen, A.; Facal San Luis, P.; Fajardo Tapia, I.; Falcke, H.; Farrar, G.; Fauth, A. C.; Fazzini, N.; Ferguson, A. P.; Ferrero, A.; Fick, B.; Filevich, A.; Filip?i?, A.; Fliescher, S.; Fracchiolla, C. E.; Fraenkel, E. D.; Frhlich, U.; Fuchs, B.; Gaior, R.; Gamarra, R. F.; Gambetta, S.; Garca, B.; Garcia-Gamez, D.; Garcia-Pinto, D.; Gascon, A.; Gemmeke, H.; Gesterling, K.; Ghia, P. L.; Giaccari, U.; Giller, M.; Glass, H.; Gold, M. S.; Golup, G.; Gomez Albarracin, F.; Gmez Berisso, M.; Gonalves, P.; Gonzalez, D.; Gonzalez, J. G.; Gookin, B.; Gra, D.; Gorgi, A.; Gouffon, P.; Gozzini, S. R.; Grashorn, E.; Grebe, S.; Griffith, N.; Grigat, M.; Grillo, A. F.; Guardincerri, Y.; Guarino, F.; Guedes, G. P.; Guzman, A.; Hague, J. D.; Hansen, P.; Harari, D.; Harmsma, S.; Harrison, T. A.; Harton, J. L.; Haungs, A.; Hebbeker, T.; Heck, D.; Herve, A. E.; Hojvat, C.; Hollon, N.; Holmes, V. C.; Homola, P.; Hrandel, J. R.; Horneffer, A.; Horvath, P.; Hrabovsk, M.; Huege, T.; Insolia, A.; Ionita, F.; Italiano, A.; Jarne, C.; Jiraskova, S.; Josebachuili, M.; Kadija, K.; Kampert, K. H.; Karhan, P.; Kasper, P.; Kgl, B.; Keilhauer, B.; Keivani, A.; Kelley, J. L.; Kemp, E.; Kieckhafer, R. M.; Klages, H. O.; Kleifges, M.; Kleinfeller, J.; Knapp, J.; Koang, D.-H.; Kotera, K.; Krohm, N.; Krmer, O.; Kruppke-Hansen, D.; Kuehn, F.; Kuempel, D.; Kulbartz, J. K.; Kunka, N.; La Rosa, G.; Lachaud, C.; Lauer, R.; Lautridou, P.; Le Coz, S.; Leo, M. S. A. B.; Lebrun, D.; Lebrun, P.; Leigui de Oliveira, M. A.; Lemiere, A.; Letessier-Selvon, A.; Lhenry-Yvon, I.; Link, K.; Lpez, R.; Lopez Agera, A.; Louedec, K.; Lozano Bahilo, J.; Lu, L.; Lucero, A.; Ludwig, M.; Lyberis, H.; Macolino, C.; Maldera, S.; Mandat, D.; Mantsch, P.; Mariazzi, A. G.; Marin, J.; Marin, V.; Maris, I. C.; Marquez Falcon, H. R.; Marsella, G.; Martello, D.; Martin, L.; Martinez, H.; Martnez Bravo, O.; Mathes, H. J.; Matthews, J.; Matthews, J. A. J.; Matthiae, G.; Maurizio, D.; Mazur, P. O.; Medina-Tanco, G.; Melissas, M.; Melo, D.; Menichetti, E.; Menshikov, A.; Mertsch, P.; Meurer, C.; Mi?anovi?, S.; Micheletti, M. I.; Miller, W.; Miramonti, L.; Molina-Bueno, L.; Mollerach, S.; Monasor, M.; Monnier Ragaigne, D.; Montanet, F.; Morales, B.; Morello, C.; Moreno, E.; Moreno, J. C.; Morris, C.; Mostaf, M.; Moura, C. A.; Mueller, S.; Muller, M. A.; Mller, G.; Mnchmeyer, M.; Mussa, R.; Navarra, G.; Navarro, J. L.; Navas, S.; Necesal, P.; Nellen, L.; Nelles, A.; Neuser, J.; Nhung, P. T.; Niemietz, L.; Nierstenhoefer, N.; Nitz, D.; Nosek, D.; Noka, L.; Nyklicek, M.; Oehlschlger, J.; Olinto, A.; Olmos-Gilbaja, V. M.; Ortiz, M.; Pacheco, N.; Pakk Selmi-Dei, D.; Palatka, M.; Pallotta, J.; Palmieri, N.; Parente, G.; Parizot, E.; Parra, A.; Parsons, R. D.; Pastor, S.; Paul, T.; Pech, M.; P?kala, J.; Pelayo, R.; Pepe, I. M.; Perrone, L.; Pesce, R.; Petermann, E.; Petrera, S.; Petrinca, P.; Petrolini, A.; Petrov, Y.; Petrovic, J.; Pfendner, C.; Phan, N.

    2012-08-10

    We report a measurement of the proton-air cross section for particle production at the center-of-mass energy per nucleon of 57 TeV. This is derived from the distribution of the depths of shower maxima observed with the Pierre Auger Observatory: systematic uncertainties are studied in detail. Analyzing the tail of the distribution of the shower maxima, a proton-air cross section of [50522(stat)+28-36(syst)] mb is found.

  7. The Pierre Auger Observatory scaler mode for the study of solar activity modulation of galactic cosmic rays

    SciTech Connect (OSTI)

    Abreu, P.; Aglietta, M.; Ahn, E.J.; Allard, D.; Allekotte, I.; Allen, J.; Alvarez Castillo, J.; Alvarez-Muniz, J.; Ambrosio, M.; Aminaei, A.; Anchordoqui, L.; /Wisconsin U., Milwaukee /Lisbon, LIFEP /Lisbon, IST

    2011-01-01

    Since data-taking began in January 2004, the Pierre Auger Observatory has been recording the count rates of low energy secondary cosmic ray particles for the self-calibration of the ground detectors of its surface detector array. After correcting for atmospheric effects, modulations of galactic cosmic rays due to solar activity and transient events are observed. Temporal variations related with the activity of the heliosphere can be determined with high accuracy due to the high total count rates. In this study, the available data are presented together with an analysis focused on the observation of Forbush decreases, where a strong correlation with neutron monitor data is found.

  8. HIGH-RESOLUTION LABORATORY SPECTRA ON THE λ131 CHANNEL OF THE AIA INSTRUMENT ON BOARD THE SOLAR DYNAMICS OBSERVATORY

    SciTech Connect (OSTI)

    Träbert, Elmar; Beiersdorfer, Peter; Brickhouse, Nancy S.; Golub, Leon

    2014-03-01

    Extreme ultraviolet spectra of C, O, F, Ne, Si, S, Ar, Ca, Fe, and Ni have been excited in an electron beam ion trap and studied with much higher resolution than available on Solar Dynamics Observatory (SDO) in order to ascertain the spectral composition of the SDO observations. We presently show our findings in the wavelength range 124-134 Å, which encompasses the λ131 observation channel of the Atmospheric Imaging Assembly (AIA). While the general interpretation of the spectral composition of the λ131 Fe channel is being corroborated, a number of new lines have been observed that might help to improve the diagnostic value of the SDO/AIA data.

  9. Bounds on the density of sources of ultra-high energy cosmic rays from the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Collaboration: Pierre Auger Collaboration

    2013-05-01

    We derive lower bounds on the density of sources of ultra-high energy cosmic rays from the lack of significant clustering in the arrival directions of the highest energy events detected at the Pierre Auger Observatory. The density of uniformly distributed sources of equal intrinsic intensity was found to be larger than ∼ (0.06−5) × 10{sup −4} Mpc{sup −3} at 95% CL, depending on the magnitude of the magnetic deflections. Similar bounds, in the range (0.2−7) × 10{sup −4} Mpc{sup −3}, were obtained for sources following the local matter distribution.

  10. Search for patterns by combining cosmic-ray energy and arrival directions at the Pierre Auger Observatory

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

    Aab, A.; Abreu, P.; Aglietta, M.; Ahn, E. J.; Samarai, I. Al; Albuquerque, I. F. M.; Allekotte, I.; Allen, J.; Allison, P.; Almela, A.; et al

    2015-06-20

    Energy-dependent patterns in the arrival directions of cosmic rays are searched for using data of the Pierre Auger Observatory. We investigate local regions around the highest-energy cosmic rays with $E \\ge 6 \\times 10^{19}$ eV by analyzing cosmic rays with energies above $E \\ge 5 \\times 10^{18}$ eV arriving within an angular separation of approximately 15$^{\\circ }$ . We characterize the energy distributions inside these regions by two independent methods, one searching for angular dependence of energy-energy correlations and one searching for collimation of energy along the local system of principal axes of the energy distribution. No significant patterns aremorefound with this analysis. As a result, the comparison of these measurements with astrophysical scenarios can therefore be used to obtain constraints on related model parameters such as strength of cosmic-ray deflection and density of point sources.less

  11. Infrared Spectroscopic Data from the Apache Point Observatory Galactic Evolution Experiment (APOGEE), SDSS-III Data Release 10

    DOE Data Explorer [Office of Scientific and Technical Information (OSTI)]

    Sloan Digital Sky Survey (SDSS) Data Release 10 is the first spectroscopic release from the Apache Point Observatory Galactic Evolution Experiment (APOGEE), including spectra and derived stellar parameters for more than 50,000 stars. APOGEE is an ongoing survey of ~100,000 stars accessing all parts of the Milky Way. By operating in the infrared (H-band) portion of the electromagnetic spectrum, APOGEE is better able to detect light from stars lying in dusty regions of the Milky Way than surveys conducted in the optical, making this survey particularly well-suited for exploring the Galactic disk and bulge. APOGEE's high resolution spectra provide detailed information about the stellar atmospheres; DR10 provides derived effective temperatures, surface gravities, overall metallicities, and information on the abundances of several chemical elements. [copied from http://www.sdss3.org/dr10/irspec/

  12. Search for signatures of magnetically-induced alignment in the arrival directions measured by the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Abreu, P.; Aglietta, M.; Ahn, E.J.; Albuquerque, I.F.M.; Allard, D.; Allekotte, I.; Allen, J.; Allison, P.; Alvarez Castillo, J.; Alvarez-Muniz, J.; Ambrosio, M.; /Naples U. /INFN, Naples /Nijmegen U., IMAPP

    2011-11-01

    We present the results of an analysis of data recorded at the Pierre Auger Observatory in which we search for groups of directionally-aligned events (or ''multiplets'') which exhibit a correlation between arrival direction and the inverse of the energy. These signatures are expected from sets of events coming from the same source after having been deflected by intervening coherent magnetic fields. The observation of several events from the same source would open the possibility to accurately reconstruct the position of the source and also measure the integral of the component of the magnetic field orthogonal to the trajectory of the cosmic rays. We describe the largest multiplets found and compute the probability that they appeared by chance from an isotropic distribution. We find no statistically significant evidence for the presence of multiplets arising from magnetic deflections in the present data.

  13. Search for patterns by combining cosmic-ray energy and arrival directions at the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Aab, Alexander

    2015-06-20

    Energy-dependent patterns in the arrival directions of cosmic rays are searched for using data of the Pierre Auger Observatory. We investigate local regions around the highest-energy cosmic rays with E ≥ 6×1019 eV by analyzing cosmic rays with energies above E ≥ 5×1018 eV arriving within an angular separation of approximately 15°. We characterize the energy distributions inside these regions by two independent methods, one searching for angular dependence of energy-energy correlations and one searching for collimation of energy along the local system of principal axes of the energy distribution. No significant patterns are found with this analysis. As a result, the comparison of these measurements with astrophysical scenarios can therefore be used to obtain constraints on related model parameters such as strength of cosmic-ray deflection and density of point sources.

  14. Search for patterns by combining cosmic-ray energy and arrival directions at the Pierre Auger Observatory

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

    Aab, Alexander

    2015-06-20

    Energy-dependent patterns in the arrival directions of cosmic rays are searched for using data of the Pierre Auger Observatory. We investigate local regions around the highest-energy cosmic rays with E ≥ 6×1019 eV by analyzing cosmic rays with energies above E ≥ 5×1018 eV arriving within an angular separation of approximately 15°. We characterize the energy distributions inside these regions by two independent methods, one searching for angular dependence of energy-energy correlations and one searching for collimation of energy along the local system of principal axes of the energy distribution. No significant patterns are found with this analysis. As amore » result, the comparison of these measurements with astrophysical scenarios can therefore be used to obtain constraints on related model parameters such as strength of cosmic-ray deflection and density of point sources.« less

  15. Ocean pC02 Data from the Lamont-Doherty Earth Observatory of Columbia University, 1994 - 2009

    DOE Data Explorer [Office of Scientific and Technical Information (OSTI)]

    Takahashi, T.

    The Earth Institute of Columbia University has, as an overarching goal, to help achieve sustainable development primarily by expanding the world's understanding of Earth as one integrated system. The Earth Institute encompasses centers of excellence with an established reputation for groundbreaking research, including the renowned Lamont-Doherty Earth Observatory (LDEO), home to more than 200 researchers who study Earth and its systems. The Carbon Dioxide Research Group, led by Dr. Taro Takahashi, studies pCO2 in seawater, carbon sequestration models related to deep aquifers, and air-sea CO2 flux. Datasets from ocean cruises in the years 1994 to the present are made available from this website, along with a list of publications, and cruise maps.

  16. Measurement of the Muon Atmospheric Production Depth with the Water Cherenkov Detectors of the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Molina Bueno, Laura

    2015-09-01

    Ultra-high-energy cosmic rays (UHECR) are particles of uncertain origin and composition, with energies above 1 EeV (1018 eV or 0.16 J). The measured flux of UHECR is a steeply decreasing function of energy. The largest and most sensitive apparatus built to date to record and study cosmic ray Extensive Air Showers (EAS) is the Pierre Auger Observatory. The Pierre Auger Observatory has produced the largest and finest amount of data ever collected for UHECR. A broad physics program is being carried out covering all relevant topics of the field. Among them, one of the most interesting is the problem related to the estimation of the mass composition of cosmic rays in this energy range. Currently the best measurements of mass are those obtained by studying the longitudinal development of the electromagnetic part of the EAS with the Fluorescence Detector. However, the collected statistics is small, specially at energies above several tens of EeV. Although less precise, the volume of data gathered with the Surface Detector is nearly a factor ten larger than the fluorescence data. So new ways to study composition with data collected at the ground are under investigation. The subject of this thesis follows one of those new lines of research. Using preferentially the time information associated with the muons that reach the ground, we try to build observables related to the composition of the primaries that initiated the EAS. A simple phenomenological model relates the arrival times with the depths in the atmosphere where muons are produced. The experimental confirmation that the distributions of muon production depths (MPD) correlate with the mass of the primary particle has opened the way to a variety of studies, of which this thesis is a continuation, with the aim of enlarging and improving its range of applicability. We revisit the phenomenological model which is at the root of the analysis and discuss a new way to improve some aspects of the model. We carry

  17. A Search for Ultra-High Energy Neutrinos in Highly Inclined Events at the Pierre Auger Observatory

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

    Abreu, P

    2011-12-30

    The Surface Detector of the Pierre Auger Observatory is sensitive to neutrinos of all flavors above 0.1 EeV. These interact through charged and neutral currents in the atmosphere giving rise to extensive air showers. When interacting deeply in the atmosphere at nearly horizontal incidence, neutrinos can be distinguished from regular hadronic cosmic rays by the broad time structure of their shower signals in the water-Cherenkov detectors. In this paper we present for the first time an analysis based on down-going neutrinos. We describe the search procedure, the possible sources of background, the method to compute the exposure and the associatedmore » systematic uncertainties. No candidate neutrinos have been found in data collected from 1 January 2004 to 31 May 2010. Assuming an E-2 differential energy spectrum the limit on the single-flavor neutrino is E2dN/dE < 1.74 x 10-7 GeV cm-2s-1sr-1 at 90% C.L. in the energy range 1 x 1017eV < E < 1 x 1020 eV.« less

  18. Measurement of the proton-air cross-section at $\\sqrt{s}=57$ TeV with the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Collaboration, Auger

    2012-08-01

    We report a measurement of the proton-air cross section for particle production at the center-of-mass energy per nucleon of 57 TeV. This is derived from the distribution of the depths of shower maxima observed with the Pierre Auger Observatory: systematic uncertainties are studied in detail. Analyzing the tail of the distribution of the shower maxima, a proton-air cross section of [505 {+-} 22(stat){sub -36}{sup +28}(syst)] mb is found.

  19. Measurement of the Proton-Air Cross Section at √s=57 TeV with the Pierre Auger Observatory

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

    Abreu, P.; Aglietta, M.; Ahn, E. J.; Albuquerque, I. F. M.; Allard, D.; Allekotte, I.; Allen, J.; Allison, P.; Almeda, A.; Alvarez Castillo, J.; et al

    2012-08-10

    We report a measurement of the proton-air cross section for particle production at the center-of-mass energy per nucleon of 57 TeV. This is derived from the distribution of the depths of shower maxima observed with the Pierre Auger Observatory: systematic uncertainties are studied in detail. Analyzing the tail of the distribution of the shower maxima, a proton-air cross section of [505±22(stat)+28-36(syst)] mb is found.

  20. Searches for anisotropies in the arrival directions of the highest energy cosmic rays detected by the Pierre Auger Observatory

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

    Aab, A.; Abreu, P.; Aglietta, M.; Ahn, E. J.; Samarai, I. Al; Albuquerque, I. F. M.; Allekotte, I.; Allen, J.; Allison, P.; Almela, A.; et al

    2015-04-24

    In this study, we analyze the distribution of arrival directions of ultra-high-energy cosmic rays recorded at the Pierre Auger Observatory in 10 years of operation. The data set, about three times larger than that used in earlier studies, includes arrival directions with zenith angles up to 80, thus covering from $-90{}^\\circ $ to $+45{}^\\circ $ in declination. After updating the fraction of events correlating with the active galactic nuclei (AGNs) in the Vron-Cetty and Vron catalog, we subject the arrival directions of the data with energies in excess of 40 EeV to different tests for anisotropy. We search for localizedmoreexcess fluxes, self-clustering of event directions at angular scales up to 30, and different threshold energies between 40 and 80 EeV. We then look for correlations of cosmic rays with celestial structures both in the Galaxy (the Galactic Center and Galactic Plane) and in the local universe (the Super-Galactic Plane). We also examine their correlation with different populations of nearby extragalactic objects: galaxies in the 2MRS catalog, AGNs detected by Swift-BAT, radio galaxies with jets, and the Centaurus A (Cen A) galaxy. None of the tests show statistically significant evidence of anisotropy. The strongest departures from isotropy (post-trial probability $\\sim 1.4$%) are obtained for cosmic rays with $E\\gt 58$ EeV in rather large windows around Swift AGNs closer than 130 Mpc and brighter than 1044 erg/s (18 radius), and around the direction of Centaurus A (15 radius).less

  1. A digital seismogram archive of nuclear explosion signals, recorded at the Borovoye Geophysical Observatory, Kazakhstan, from 1966 to 1996

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

    An, Vadim A.; Ovtchinnikov, Vladimir M.; Kaazik, Pyotr B.; Adushkin, Vitaly V.; Sokolova, Inna N.; Aleschenko, Iraida B.; Mikhailova, Natalya N.; Kim, Won -Young; Richards, Paul G.; Patton, Howard J.; et al

    2015-03-27

    Seismologists from Kazakhstan, Russia, and the United States have rescued the Soviet-era archive of nuclear explosion seismograms recorded at Borovoye in northern Kazakhstan during the period 1966–1996. The signals had been stored on about 8000 magnetic tapes, which were held at the recording observatory. After hundreds of man-years of work, these digital waveforms together with significant metadata are now available via the project URL, namely http://www.ldeo.columbia.edu/res/pi/Monitoring/Data/ as a modern open database, of use to diverse communities. Three different sets of recording systems were operated at Borovoye, each using several different seismometers and different gain levels. For some explosions, more thanmore » twenty different channels of data are available. A first data release, in 2001, contained numerous glitches and lacked many instrument responses, but could still be used for measuring accurate arrival times and for comparison of the strengths of different types of seismic waves. The project URL also links to our second major data release, for nuclear explosions in Eurasia recorded in Borovoye, in which the data have been deglitched, all instrument responses have been included, and recording systems are described in detail. This second dataset consists of more than 3700 waveforms (digital seismograms) from almost 500 nuclear explosions in Eurasia, many of them recorded at regional distances. It is important as a training set for the development and evaluation of seismological methods of discriminating between earthquakes and underground explosions, and can be used for assessment of three-dimensional models of the Earth’s interior structure.« less

  2. Overview of the Manitou Experimental Forest Observatory: site description and selected science results from 2008 to 2013

    SciTech Connect (OSTI)

    Ortega, John; Turnipseed, A.; Guenther, Alex B.; Karl, Thomas G.; Day, D. A.; Gochis, David; Huffman, J. A.; Prenni, Anthony J.; Levin, E. J.; Kreidenweis, Sonia M.; DeMott, Paul J.; Tobo, Y.; Patton, E. G.; Hodzic, Alma; Cui, Y. Y.; Harley, P.; Hornbrook, R. S.; Apel, E. C.; Monson, Russell K.; Eller, A. S.; Greenberg, J. P.; Barth, Mary; Campuzano-Jost, Pedro; Palm, B. B.; Jiminez, J. L.; Aiken, A. C.; Dubey, Manvendra K.; Geron, Chris; Offenberg, J.; Ryan, M. G.; Fornwalt, Paula J.; Pryor, S. C.; Keutsch, Frank N.; DiGangi, J. P.; Chan, A. W.; Goldstein, Allen H.; Wolfe, G. M.; Kim, S.; Kaser, L.; Schnitzhofer, R.; Hansel, A.; Cantrell, Chris; Mauldin, R. L.; Smith, James N.

    2014-01-01

    The Bio-hydro-atmosphere interactions of Energy, Aerosols, Carbon, H2O, Organics & Nitrogen (BEACHON) project seeks to understand the feedbacks and interrelationships between hydrology, biogenic emissions, carbon assimilation, aerosol properties, clouds and associated feedbacks within water-limited ecosystems. The Manitou Experimental Forest Observatory (MEFO) was established in 2008 by the National Center for Atmospheric Research to address many of the BEACHON research objectives, and it now provides a fixed field site with significant infrastructure. MEFO is a mountainous, semi-arid ponderosa pine-dominated forest site that is normally dominated by clean continental air but is periodically influenced by anthropogenic sources from Colorado Front Range cities. This article summarizes the past and ongoing research activities at the site, and highlights some of the significant findings that have resulted from these measurements. These activities include soil property measurements; hydrological studies; measurements of high-frequency turbulence parameters; eddy covariance flux measurements of water, energy, aerosols and carbon dioxide through the canopy; determination of biogenic and anthropogenic volatile organic compound emissions and their influence on regional atmospheric chemistry; aerosol number and mass distributions; chemical speciation of aerosol particles; characterization of ice and cloud condensation nuclei; trace gas measurements; and model simulations using coupled chemistry and meteorology. In addition to various long-term continuous measurements, three focused measurement campaigns with state-of-the-art instrumentation have taken place since the site was established, and two of these studies are the subjects of this special issue: BEACHON-ROCS (Rocky Mountain Organic Carbon Study, 2010) and BEACHON-RoMBAS (Rocky Mountain Biogenic Aerosol Study, 2011).

  3. A search for anisotropy in the arrival directions of ultra high energy cosmic rays recorded at the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Abreu, P.; ,

    2012-01-01

    Observations of cosmic ray arrival directions made with the Pierre Auger Observatory have previously provided evidence of anisotropy at the 99% CL using the correlation of ultra high energy cosmic rays (UHECRs) with objects drawn from the Veron-Cetty Veron catalog. In this paper we report on the use of three catalog independent methods to search for anisotropy. The 2pt-L, 2pt+ and 3pt methods, each giving a different measure of self-clustering in arrival directions, were tested on mock cosmic ray data sets to study the impacts of sample size and magnetic smearing on their results, accounting for both angular and energy resolutions. If the sources of UHECRs follow the same large scale structure as ordinary galaxies in the local Universe and if UHECRs are deflected no more than a few degrees, a study of mock maps suggests that these three methods can efficiently respond to the resulting anisotropy with a P-value = 1.0% or smaller with data sets as few as 100 events. Using data taken from January 1, 2004 to July 31, 2010 we examined the 20, 30, ..., 110 highest energy events with a corresponding minimum energy threshold of about 51 EeV. The minimum P-values found were 13.5% using the 2pt-L method, 1.0% using the 2pt+ method and 1.1% using the 3pt method for the highest 100 energy events. In view of the multiple (correlated) scans performed on the data set, these catalog-independent methods do not yield strong evidence of anisotropy in the highest energy cosmic rays.

  4. OVERVIEW OF THE SDSS-IV MaNGA SURVEY: MAPPING NEARBY GALAXIES AT APACHE POINT OBSERVATORY

    SciTech Connect (OSTI)

    Bundy, Kevin; Bershady, Matthew A.; Wake, David A.; Tremonti, Christy; Diamond-Stanic, Aleksandar M.; Law, David R.; Cherinka, Brian; Yan, Renbin; Snchez-Gallego, Jos R.; Drory, Niv; MacDonald, Nicholas; Weijmans, Anne-Marie; Thomas, Daniel; Masters, Karen; Coccato, Lodovico; Aragn-Salamanca, Alfonso; Avila-Reese, Vladimir; Badenes, Carles; Falcn-Barroso, Jsus; Belfiore, Francesco; and others

    2015-01-01

    We present an overview of a new integral field spectroscopic survey called MaNGA (Mapping Nearby Galaxies at Apache Point Observatory), one of three core programs in the fourth-generation Sloan Digital Sky Survey (SDSS-IV) that began on 2014 July 1. MaNGA will investigate the internal kinematic structure and composition of gas and stars in an unprecedented sample of 10,000 nearby galaxies. We summarize essential characteristics of the instrument and survey design in the context of MaNGA's key science goals and present prototype observations to demonstrate MaNGA's scientific potential. MaNGA employs dithered observations with 17 fiber-bundle integral field units that vary in diameter from 12'' (19 fibers) to 32'' (127 fibers). Two dual-channel spectrographs provide simultaneous wavelength coverage over 3600-10300 at R ? 2000. With a typical integration time of 3 hr, MaNGA reaches a target r-band signal-to-noise ratio of 4-8 ({sup 1} per 2'' fiber) at 23 AB mag arcsec{sup 2}, which is typical for the outskirts of MaNGA galaxies. Targets are selected with M {sub *} ? 10{sup 9} M {sub ?} using SDSS-I redshifts and i-band luminosity to achieve uniform radial coverage in terms of the effective radius, an approximately flat distribution in stellar mass, and a sample spanning a wide range of environments. Analysis of our prototype observations demonstrates MaNGA's ability to probe gas ionization, shed light on recent star formation and quenching, enable dynamical modeling, decompose constituent components, and map the composition of stellar populations. MaNGA's spatially resolved spectra will enable an unprecedented study of the astrophysics of nearby galaxies in the coming 6yr.

  5. Radio-optical reference frame link using the U.S. Naval observatory astrograph and deep CCD imaging

    SciTech Connect (OSTI)

    Zacharias, N.; Zacharias, M. I.

    2014-05-01

    Between 1997 and 2004 several observing runs were conducted, mainly with the CTIO 0.9 m, to image International Celestial Reference Frame (ICRF) counterparts (mostly QSOs) in order to determine accurate optical positions. Contemporary to these deep CCD images, the same fields were observed with the U.S. Naval Observatory astrograph in the same bandpass. They provide accurate positions on the Hipparcos/Tycho-2 system for stars in the 10-16 mag range used as reference stars for the deep CCD imaging data. Here we present final optical position results of 413 sources based on reference stars obtained by dedicated astrograph observations that were reduced following two different procedures. These optical positions are compared to radio very long baseline interferometry positions. The current optical system is not perfectly aligned to the ICRF radio system with rigid body rotation angles of 3-5 mas (= 3σ level) found between them for all three axes. Furthermore, statistically, the optical-radio position differences are found to exceed the total, combined, known errors in the observations. Systematic errors in the optical reference star positions and physical offsets between the centers of optical and radio emissions are both identified as likely causes. A detrimental, astrophysical, random noise component is postulated to be on about the 10 mas level. If confirmed by future observations, this could severely limit the Gaia to ICRF reference frame alignment accuracy to an error of about 0.5 mas per coordinate axis with the current number of sources envisioned to provide the link. A list of 36 ICRF sources without the detection of an optical counterpart to a limiting magnitude of about R = 22 is provided as well.

  6. Searches for anisotropies in the arrival directions of the highest energy cosmic rays detected by the Pierre Auger Observatory

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

    Aab, Alexander

    2015-05-01

    We analyze the distribution of arrival directions of ultra-high-energy cosmic rays recorded at the Pierre Auger Observatory in 10 years of operation. The data set, about three times larger than that used in earlier studies, includes arrival directions with zenith angles up to 80°, thus covering from -90° to +45° in declination. After updating the fraction of events correlating with the active galactic nuclei (AGNs) in the Véron-Cetty and Véron catalog, we subject the arrival directions of the data with energies in excess of 40 EeV to different tests for anisotropy. We search for localized excess fluxes, self-clustering of event directions at angular scales up to 30°, and different threshold energies between 40 and 80 EeV. We then look for correlations of cosmic rays with celestial structures both in the Galaxy (the Galactic Center and Galactic Plane) and in the local universe (the Super-Galactic Plane). We also examine their correlation with different populations of nearby extragalactic objects: galaxies in the 2MRS catalog, AGNs detected by Swift-BAT, radio galaxies with jets, and the Centaurus A (Cen A) galaxy. None of the tests show statistically significant evidence of anisotropy. As a result, the strongest departures from isotropy (post-trial probabilitymore » $$\\sim 1.4$$%) are obtained for cosmic rays with $$E\\gt 58$$ EeV in rather large windows around Swift AGNs closer than 130 Mpc and brighter than 1044 erg s-1 (18° radius), and around the direction of Cen A (15° radius).« less

  7. Searches for anisotropies in the arrival directions of the highest energy cosmic rays detected by the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Aab, A.; Abreu, P.; Aglietta, M.; Ahn, E. J.; Samarai, I. Al; Albuquerque, I. F. M.; Allekotte, I.; Allen, J.; Allison, P.; Almela, A.; Castillo, J. Alvarez; Alvarez-Muiz, J.; Batista, R. Alves; Ambrosio, M.; Aminaei, A.; Anchordoqui, L.; Andringa, S.; Aramo, C.; Aranda, V. M.; Arqueros, F.; Asorey, H.; Assis, P.; Aublin, J.; Ave, M.; Avenier, M.; Avila, G.; Awal, N.; Badescu, A. M.; Barber, K. B.; Buml, J.; Baus, C.; Beatty, J. J.; Becker, K. H.; Bellido, J. A.; Berat, C.; Bertaina, M. E.; Bertou, X.; Biermann, P. L.; Billoir, P.; Blaess, S. G.; Blanco, M.; Bleve, C.; Blmer, H.; Boh?ov, M.; Boncioli, D.; Bonifazi, C.; Bonino, R.; Borodai, N.; Brack, J.; Brancus, I.; Bridgeman, A.; Brogueira, P.; Brown, W. C.; Buchholz, P.; Bueno, A.; Buitink, S.; Buscemi, M.; Caballero-Mora, K. S.; Caccianiga, B.; Caccianiga, L.; Candusso, M.; Caramete, L.; Caruso, R.; Castellina, A.; Cataldi, G.; Cazon, L.; Cester, R.; Chavez, A. G.; Chiavassa, A.; Chinellato, J. A.; Chudoba, J.; Cilmo, M.; Clay, R. W.; Cocciolo, G.; Colalillo, R.; Coleman, A.; Collica, L.; Coluccia, M. R.; Conceio, R.; Contreras, F.; Cooper, M. J.; Cordier, A.; Coutu, S.; Covault, C. E.; Cronin, J.; Curutiu, A.; Dallier, R.; Daniel, B.; Dasso, S.; Daumiller, K.; Dawson, B. R.; Almeida, R. M. de; Domenico, M. De; Jong, S. J. de; Neto, J. R. T. de Mello; Mitri, I. De; Oliveira, J. de; Souza, V. de; Peral, L. del; Deligny, O.; Dembinski, H.; Dhital, N.; Giulio, C. Di; Matteo, A. Di; Diaz, J. C.; Castro, M. L. Daz; Diogo, F.; Dobrigkeit, C.; Docters, W.; DOlivo, J. C.; Dorofeev, A.; Hasankiadeh, Q. Dorosti; Dova, M. T.; Ebr, J.; Engel, R.; Erdmann, M.; Erfani, M.; Escobar, C. O.; Espadanal, J.; Etchegoyen, A.; Luis, P. Facal San; Falcke, H.; Fang, K.; Farrar, G.; Fauth, A. C.; Fazzini, N.; Ferguson, A. P.; Fernandes, M.; Fick, B.; Figueira, J. M.; Filevich, A.; Filip?i?, A.; Fox, B. D.; Fratu, O.; Freire, M. M.; Frhlich, U.; Fuchs, B.; Fujii, T.; Gaior, R.; Garca, B.; Gamez, D. Garcia-; Pinto, D. Garcia-; Garilli, G.; Bravo, A. Gascon; Gate, F.; Gemmeke, H.; Ghia, P. L.; Giaccari, U.; Giammarchi, M.; Giller, M.; Glaser, C.; Glass, H.; Berisso, M. Gmez; Vitale, P. F. Gmez; Gonalves, P.; Gonzalez, J. G.; Gonzlez, N.; Gookin, B.; Gordon, J.; Gorgi, A.; Gorham, P.; Gouffon, P.; Grebe, S.; Griffith, N.; Grillo, A. F.; Grubb, T. D.; Guarino, F.; Guedes, G. P.; Hampel, M. R.; Hansen, P.; Harari, D.; Harrison, T. A.; Hartmann, S.; Harton, J. L.; Haungs, A.; Hebbeker, T.; Heck, D.; Heimann, P.; Herve, A. E.; Hill, G. C.; Hojvat, C.; Hollon, N.; Holt, E.; Homola, P.; Hrandel, J. R.; Horvath, P.; Hrabovsk, M.; Huber, D.; Huege, T.; Insolia, A.; Isar, P. G.; Jandt, I.; Jansen, S.; Jarne, C.; Josebachuili, M.; Kp, A.; Kambeitz, O.; Kampert, K. H.; Kasper, P.; Katkov, I.; Kgl, B.; Keilhauer, B.; Keivani, A.; Kemp, E.; Kieckhafer, R. M.; Klages, H. O.; Kleifges, M.; Kleinfeller, J.; Krause, R.; Krohm, N.; Krmer, O.; Hansen, D. Kruppke-; Kuempel, D.; Kunka, N.; LaHurd, D.; Latronico, L.; Lauer, R.; Lauscher, M.; Lautridou, P.; Coz, S. Le; Leo, M. S. A. B.; Lebrun, D.; Lebrun, P.; Leigui de Oliveira, M. A.; Letessier-Selvon, A.; Lhenry-Yvon, I.; Link, K.; Lpez, R.; Louedec, K.; Bahilo, J. Lozano; Lu, L.; Lucero, A.; Ludwig, M.; Malacari, M.; Maldera, S.; Mallamaci, M.; Maller, J.; Mandat, D.; Mantsch, P.; Mariazzi, A. G.; Marin, V.; Mari?, I. C.; Marsella, G.; Martello, D.; Martin, L.; Martinez, H.; Bravo, O. Martnez; Martraire, D.; Meza, J. J. Masas; Mathes, H. J.; Mathys, S.; Matthews, J.; Matthews, J. A. J.; Matthiae, G.; Maurel, D.; Maurizio, D.; Mayotte, E.; Mazur, P. O.; Medina, C.; Tanco, G. Medina-; Meissner, R.; Melissas, M.; Melo, D.; Menshikov, A.; Messina, S.; Meyhandan, R.; Mi?anovi?, S.; Micheletti, M. I.; Middendorf, L.; Minaya, I. A.; Miramonti, L.; Mitrica, B.; Bueno, L. Molina-; Mollerach, S.; Monasor, M.; Ragaigne, D. Monnier; Montanet, F.; Morello, C.; Mostaf, M.; Moura, C. A.; Muller, M. A.; Mller, G.; Mller, S.; Mnchmeyer, M.; Mussa, R.; Navarra, G.; Navas, S.; Necesal, P.; Nellen, L.; Nelles, A.; Neuser, J.; Nguyen, P. H.; Niechciol, M.; Niemietz, L.; Niggemann, T.; Nitz, D.; Nosek, D.; Novotny, V.; Noka, L.; Ochilo, L.; Oikonomou, F.; Olinto, A.; Oliveira, M.; Pacheco, N.; Dei, D. Pakk Selmi-; Palatka, M.; Pallotta, J.; Palmieri, N.; Papenbreer, P.; Parente, G.; Parra, A.; Paul, T.; Pech, M.; P?kala, J.; Pelayo, R.; Pepe, I. M.; Perrone, L.; Petermann, E.; Peters, C.; Petrera, S.; Petrov, Y.; Phuntsok, J.; Piegaia, R.; Pierog, T.; Pieroni, P.; Pimenta, M.; Pirronello, V.; Platino, M.; Plum, M.; Porcelli, A.; Porowski, C.; Prado, R. R.; Privitera, P.; Prouza, M.; Purrello, V.; Quel, E. J.; Querchfeld, S.; Quinn, S.; Rautenberg, J.; Ravel, O.; Ravignani, D.

    2015-04-24

    In this study, we analyze the distribution of arrival directions of ultra-high-energy cosmic rays recorded at the Pierre Auger Observatory in 10 years of operation. The data set, about three times larger than that used in earlier studies, includes arrival directions with zenith angles up to 80, thus covering from $-90{}^\\circ $ to $+45{}^\\circ $ in declination. After updating the fraction of events correlating with the active galactic nuclei (AGNs) in the Vron-Cetty and Vron catalog, we subject the arrival directions of the data with energies in excess of 40 EeV to different tests for anisotropy. We search for localized excess fluxes, self-clustering of event directions at angular scales up to 30, and different threshold energies between 40 and 80 EeV. We then look for correlations of cosmic rays with celestial structures both in the Galaxy (the Galactic Center and Galactic Plane) and in the local universe (the Super-Galactic Plane). We also examine their correlation with different populations of nearby extragalactic objects: galaxies in the 2MRS catalog, AGNs detected by Swift-BAT, radio galaxies with jets, and the Centaurus A (Cen A) galaxy. None of the tests show statistically significant evidence of anisotropy. The strongest departures from isotropy (post-trial probability $\\sim 1.4$%) are obtained for cosmic rays with $E\\gt 58$ EeV in rather large windows around Swift AGNs closer than 130 Mpc and brighter than 1044 erg/s (18 radius), and around the direction of Centaurus A (15 radius).

  8. Searches for anisotropies in the arrival directions of the highest energy cosmic rays detected by the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Aab, Alexander

    2015-05-01

    We analyze the distribution of arrival directions of ultra-high-energy cosmic rays recorded at the Pierre Auger Observatory in 10 years of operation. The data set, about three times larger than that used in earlier studies, includes arrival directions with zenith angles up to 80°, thus covering from -90° to +45° in declination. After updating the fraction of events correlating with the active galactic nuclei (AGNs) in the Véron-Cetty and Véron catalog, we subject the arrival directions of the data with energies in excess of 40 EeV to different tests for anisotropy. We search for localized excess fluxes, self-clustering of event directions at angular scales up to 30°, and different threshold energies between 40 and 80 EeV. We then look for correlations of cosmic rays with celestial structures both in the Galaxy (the Galactic Center and Galactic Plane) and in the local universe (the Super-Galactic Plane). We also examine their correlation with different populations of nearby extragalactic objects: galaxies in the 2MRS catalog, AGNs detected by Swift-BAT, radio galaxies with jets, and the Centaurus A (Cen A) galaxy. None of the tests show statistically significant evidence of anisotropy. As a result, the strongest departures from isotropy (post-trial probability $\\sim 1.4$%) are obtained for cosmic rays with $E\\gt 58$ EeV in rather large windows around Swift AGNs closer than 130 Mpc and brighter than 1044 erg s-1 (18° radius), and around the direction of Cen A (15° radius).

  9. A digital seismogram archive of nuclear explosion signals, recorded at the Borovoye Geophysical Observatory, Kazakhstan, from 1966 to 1996

    SciTech Connect (OSTI)

    An, Vadim A.; Ovtchinnikov, Vladimir M.; Kaazik, Pyotr B.; Adushkin, Vitaly V.; Sokolova, Inna N.; Aleschenko, Iraida B.; Mikhailova, Natalya N.; Kim, Won -Young; Richards, Paul G.; Patton, Howard J.; Scott Phillips, W.; Randall, George; Baker, Diane

    2015-03-27

    Seismologists from Kazakhstan, Russia, and the United States have rescued the Soviet-era archive of nuclear explosion seismograms recorded at Borovoye in northern Kazakhstan during the period 1966–1996. The signals had been stored on about 8000 magnetic tapes, which were held at the recording observatory. After hundreds of man-years of work, these digital waveforms together with significant metadata are now available via the project URL, namely http://www.ldeo.columbia.edu/res/pi/Monitoring/Data/ as a modern open database, of use to diverse communities. Three different sets of recording systems were operated at Borovoye, each using several different seismometers and different gain levels. For some explosions, more than twenty different channels of data are available. A first data release, in 2001, contained numerous glitches and lacked many instrument responses, but could still be used for measuring accurate arrival times and for comparison of the strengths of different types of seismic waves. The project URL also links to our second major data release, for nuclear explosions in Eurasia recorded in Borovoye, in which the data have been deglitched, all instrument responses have been included, and recording systems are described in detail. This second dataset consists of more than 3700 waveforms (digital seismograms) from almost 500 nuclear explosions in Eurasia, many of them recorded at regional distances. It is important as a training set for the development and evaluation of seismological methods of discriminating between earthquakes and underground explosions, and can be used for assessment of three-dimensional models of the Earth’s interior structure.

  10. HIGH-RESOLUTION LABORATORY SPECTRA OF THE λ193 CHANNEL OF THE ATMOSPHERIC IMAGING ASSEMBLY INSTRUMENT ON BOARD SOLAR DYNAMICS OBSERVATORY

    SciTech Connect (OSTI)

    Träbert, Elmar; Beiersdorfer, Peter; Brickhouse, Nancy S.; Golub, Leon

    2014-11-01

    Extreme ultraviolet spectra of C, O, F, Ne, S, Ar, Fe, and Ni have been excited in an electron beam ion trap and studied with much higher resolution than available on the Solar Dynamics Observatory (SDO) in order to ascertain the spectral composition of the SDO/Atmospheric Imaging Assembly (AIA) observations. We present our findings in the wavelength range 182-200 Å, which, overall, corroborate the working models of how to interpret the SDO/AIA data. We find, however, that the inclusion of a number of additional lines might improve the data interpretation.

  11. HYDRATE RESEARCH ACTIVITIES THAT BOTH SUPPORT AND DERIVE FROM THE MONITORING STATION/SEA-FLOOR OBSERVATORY, MISSISSIPPI CANYON 118, NORTHERN GULF OF MEXICO

    SciTech Connect (OSTI)

    Lutken, Carol

    2013-07-31

    A permanent observatory has been installed on the seafloor at Federal Lease Block, Mississippi Canyon 118 (MC118), northern Gulf of Mexico. Researched and designed by the Gulf of Mexico Hydrates Research Consortium (GOM-HRC) with the geological, geophysical, geochemical and biological characterization of in situ gas hydrates systems as the research goal, the site has been designated by the Bureau of Ocean Energy Management as a permanent Research Reserve where studies of hydrates and related ocean systems may take place continuously and cooperatively into the foreseeable future. The predominant seafloor feature at MC118 is a carbonate-hydrate complex, officially named Woolsey Mound for the founder of both the GOM-HRC and the concept of the permanent seafloor hydrates research facility, the late James Robert “Bob” Woolsey. As primary investigator of the overall project until his death in mid-2008, Woolsey provided key scientific input and served as chief administrator for the Monitoring Station/ Seafloor Observatory (MS-SFO). This final technical report presents highlights of research and accomplishments to date. Although not all projects reached the status originally envisioned, they are all either complete or positioned for completion at the earliest opportunity. All Department of Energy funds have been exhausted in this effort but, in addition, leveraged to great advantage with additional federal input to the project and matched efforts and resources. This report contains final reports on all subcontracts issued by the University of Mississippi, Administrators of the project, Hydrate research activities that both support and derive from the monitoring station/sea-floor Observatory, Mississippi Canyon 118, northern Gulf of Mexico, as well as status reports on the major components of the project. All subcontractors have fulfilled their primary obligations. Without continued funds designated for further project development, the Monitoring Station

  12. An upper limit to the photon fraction in cosmic rays above 10**19-eV from the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Abraham, J.; Aglietta, M.; Aguirre, C.; Allard, D.; Allekotte, I.; Allison, P.; Alvarez, C.; Alvarez-Muniz, J.; Ambrosio, M.; Anchordoqui, L.; Anjos, J.C.; ,

    2006-06-01

    An upper limit of 16% (at 95% c.l.) is derived for the photon fraction in cosmic rays with energies above 10{sup 19} eV, based on observations of the depth of shower maximum performed with the hybrid detector of the Pierre Auger Observatory. This is the first such limit on photons obtained by observing the fluorescence light profile of air showers. This upper limit confirms and improves on previous results from the Haverah Park and AGASA surface arrays. Additional data recorded with the Auger surface detectors for a subset of the event sample, support the conclusion that a photon origin of the observed events is not favored.

  13. Measurement of the cosmic ray spectrum above 4×1018 eV using inclined events detected with the Pierre Auger Observatory

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

    Aab, Alexander

    2015-08-26

    A measurement of the cosmic-ray spectrum for energies exceeding 4×1018 eV is presented, which is based on the analysis of showers with zenith angles greater than 60° detected with the Pierre Auger Observatory between 1 January 2004 and 31 December 2013. The measured spectrum confirms a flux suppression at the highest energies. Above 5.3×1018 eV, the ``ankle'', the flux can be described by a power law E–γ with index γ=2.70 ± 0.02 (stat) ± 0.1 (sys) followed by a smooth suppression region. For the energy (Es) at which the spectral flux has fallen to one-half of its extrapolated value inmore » the absence of suppression, we find Es=(5.12±0.25 (stat)+1.0–1.2 (sys))×1019 eV.« less

  14. On the possibility to discriminate the mass of the primary cosmic ray using the muon arrival times from extensive air showers: Application for Pierre Auger Observatory

    SciTech Connect (OSTI)

    Arsene, N.; Rebel, H.; Sima, O.

    2012-11-20

    In this paper we study the possibility to discriminate the mass of the primary cosmic ray by observing the muon arrival times in ground detectors. We analyzed extensive air showers (EAS) induced by proton and iron nuclei with the same energy 8 Multiplication-Sign 10{sup 17} eV simulated with CORSIKA, and analyzed the muon arrival times at ground measured by the infill array detectors of the Pierre Auger Observatory (PAO). From the arrival times of the core and of the muons the atmospheric depth of muon generation locus is evaluated. The results suggest a potential mass discrimination on the basis of muon arrival times and of the reconstructed atmospheric depth of muon production. An analysis of a larger set of CORSIKA simulations carried out for primary energies above 10{sup 18} eV is in progress.

  15. Large scale distribution of ultra high energy cosmic rays detected at the Pierre Auger Observatory with zenith angles up to 80°

    SciTech Connect (OSTI)

    Aab, Alexander

    2015-03-30

    In this study, we present the results of an analysis of the large angular scale distribution of the arrival directions of cosmic rays with energy above 4 EeV detected at the Pierre Auger Observatory including for the first time events with zenith angle between 60° and 80°. We perform two Rayleigh analyses, one in the right ascension and one in the azimuth angle distributions, that are sensitive to modulations in right ascension and declination, respectively. The largest departure from isotropy appears in the $E\\gt 8$ EeV energy bin, with an amplitude for the first harmonic in right ascension $r_{1}^{\\alpha }=(4.4\\pm 1.0)\\times {{10}^{-2}}$, that has a chance probability $P(\\geqslant r_{1}^{\\alpha })=6.4\\times {{10}^{-5}}$, reinforcing the hint previously reported with vertical events alone.

  16. Depth of maximum of air-shower profiles at the Pierre Auger Observatory. I. Measurements at energies above $$10^{17.8}$$ eV

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

    Aab, Alexander

    2014-12-31

    We report a study of the distributions of the depth of maximum, Xmax, of extensive air-shower profiles with energies above 1017.8 eV as observed with the fluorescence telescopes of the Pierre Auger Observatory. The analysis method for selecting a data sample with minimal sampling bias is described in detail as well as the experimental cross-checks and systematic uncertainties. Furthermore, we discuss the detector acceptance and the resolution of the Xmax measurement and provide parametrizations thereof as a function of energy. Finally, the energy dependence of the mean and standard deviation of the Xmax distributions are compared to air-shower simulations formore » different nuclear primaries and interpreted in terms of the mean and variance of the logarithmic mass distribution at the top of the atmosphere.« less

  17. Measurement of the cosmic ray spectrum above 4$\\times$10$^{18}$ eV using inclined events detected with the Pierre Auger Observatory

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

    Aab, Alexander; et al.

    2015-08-26

    A measurement of the cosmic-ray spectrum for energies exceeding 41018 eV is presented, which is based on the analysis of showers with zenith angles greater than 60 detected with the Pierre Auger Observatory between 1 January 2004 and 31 December 2013. The measured spectrum confirms a flux suppression at the highest energies. Above 5.31018 eV, the ``ankle'', the flux can be described by a power law E? with index ?=2.70 0.02 (stat) 0.1 (sys) followed by a smooth suppression region. For the energy (Es) at which the spectral flux has fallen to one-half of its extrapolated value inmorethe absence of suppression, we find Es=(5.120.25 (stat)+1.01.2 (sys))1019 eV.less

  18. Large scale distribution of ultra high energy cosmic rays detected at the Pierre Auger Observatory with zenith angles up to 80°

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

    Aab, Alexander

    2015-03-30

    In this study, we present the results of an analysis of the large angular scale distribution of the arrival directions of cosmic rays with energy above 4 EeV detected at the Pierre Auger Observatory including for the first time events with zenith angle between 60° and 80°. We perform two Rayleigh analyses, one in the right ascension and one in the azimuth angle distributions, that are sensitive to modulations in right ascension and declination, respectively. The largest departure from isotropy appears in themore » $$E\\gt 8$$ EeV energy bin, with an amplitude for the first harmonic in right ascension $$r_{1}^{\\alpha }=(4.4\\pm 1.0)\\times {{10}^{-2}}$$, that has a chance probability $$P(\\geqslant r_{1}^{\\alpha })=6.4\\times {{10}^{-5}}$$, reinforcing the hint previously reported with vertical events alone.« less

  19. A Proposal for Geologic Radioactive Waste Disposal Environmental Zero-State and Subsequent Monitoring Definition - First Lessons Learned from the French Environment Observatory - 13188

    SciTech Connect (OSTI)

    Landais, Patrick; Leclerc, Elisabeth; Mariotti, Andre

    2013-07-01

    Obtaining a reference state of the environment before the beginning of construction work for a geological repository is essential as it will be useful for further monitoring during operations and beyond, thus keeping a memory of the original environmental state. The area and the compartments of the biosphere to be observed and monitored as well as the choice of the markers (e.g. bio-markers, biodiversity, quality of the environment, etc.) to be followed must be carefully selected. In parallel, the choice and selection of the environmental monitoring systems (i.e. scientific and technical criteria, social requirements) will be of paramount importance for the evaluation of the perturbations that could be induced during the operational phase of the repository exploitation. This paper presents learning points of the French environment observatory located in the Meuse/Haute-Marne that has been selected for studying the feasibility of the underground disposal of high level wastes in France. (authors)

  20. LARGE-SCALE DISTRIBUTION OF ARRIVAL DIRECTIONS OF COSMIC RAYS DETECTED ABOVE 10{sup 18} eV AT THE PIERRE AUGER OBSERVATORY

    SciTech Connect (OSTI)

    Abreu, P.; Andringa, S.; Aglietta, M.; Ahlers, M.; Ahn, E. J.; Albuquerque, I. F. M.; Allard, D.; Allekotte, I.; Allen, J.; Allison, P.; Almela, A.; Alvarez Castillo, J.; Alvarez-Muniz, J.; Alves Batista, R.; Ambrosio, M.; Aramo, C.; Aminaei, A.; Anchordoqui, L.; Antici'c, T.; Arganda, E.; Collaboration: Pierre Auger Collaboration; and others

    2012-12-15

    A thorough search for large-scale anisotropies in the distribution of arrival directions of cosmic rays detected above 10{sup 18} eV at the Pierre Auger Observatory is presented. This search is performed as a function of both declination and right ascension in several energy ranges above 10{sup 18} eV, and reported in terms of dipolar and quadrupolar coefficients. Within the systematic uncertainties, no significant deviation from isotropy is revealed. Assuming that any cosmic-ray anisotropy is dominated by dipole and quadrupole moments in this energy range, upper limits on their amplitudes are derived. These upper limits allow us to test the origin of cosmic rays above 10{sup 18} eV from stationary Galactic sources densely distributed in the Galactic disk and predominantly emitting light particles in all directions.

  1. CONSTRAINTS ON THE ORIGIN OF COSMIC RAYS ABOVE 10{sup 18} eV FROM LARGE-SCALE ANISOTROPY SEARCHES IN DATA OF THE PIERRE AUGER OBSERVATORY

    SciTech Connect (OSTI)

    Abreu, P.; Andringa, S.; Aglietta, M.; Ahlers, M.; Ahn, E. J.; Albuquerque, I. F. M.; Allard, D.; Allekotte, I.; Allen, J.; Allison, P.; Almela, A.; Castillo, J. Alvarez; Alvarez-Muniz, J.; Alves Batista, R.; Ambrosio, M.; Aramo, C.; Aminaei, A.; Anchordoqui, L.; Antici'c, T.; Arganda, E.; Collaboration: Pierre Auger Collaboration; and others

    2013-01-01

    A thorough search for large-scale anisotropies in the distribution of arrival directions of cosmic rays detected above 10{sup 18} eV at the Pierre Auger Observatory is reported. For the first time, these large-scale anisotropy searches are performed as a function of both the right ascension and the declination and expressed in terms of dipole and quadrupole moments. Within the systematic uncertainties, no significant deviation from isotropy is revealed. Upper limits on dipole and quadrupole amplitudes are derived under the hypothesis that any cosmic ray anisotropy is dominated by such moments in this energy range. These upper limits provide constraints on the production of cosmic rays above 10{sup 18} eV, since they allow us to challenge an origin from stationary galactic sources densely distributed in the galactic disk and emitting predominantly light particles in all directions.

  2. The effect of the geomagnetic field on cosmic ray energy estimates and large scale anisotropy searches on data from the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Abreu, P.; Aglietta, M.; Ahn, E.J.; Albuquerque, I.F.M.; Allard, D.; Allekotte, I.; Allen, J.; Allison, P.; Alvarez Castillo, J.; Alvarez-Muniz, J.; Ambrosio, M.; ,

    2011-11-01

    We present a comprehensive study of the influence of the geomagnetic field on the energy estimation of extensive air showers with a zenith angle smaller than 60{sup o}, detected at the Pierre Auger Observatory. The geomagnetic field induces an azimuthal modulation of the estimated energy of cosmic rays up to the {approx} 2% level at large zenith angles. We present a method to account for this modulation of the reconstructed energy. We analyse the effect of the modulation on large scale anisotropy searches in the arrival direction distributions of cosmic rays. At a given energy, the geomagnetic effect is shown to induce a pseudo-dipolar pattern at the percent level in the declination distribution that needs to be accounted for. In this work, we have identified and quantified a systematic uncertainty affecting the energy determination of cosmic rays detected by the surface detector array of the Pierre Auger Observatory. This systematic uncertainty, induced by the influence of the geomagnetic field on the shower development, has a strength which depends on both the zenith and the azimuthal angles. Consequently, we have shown that it induces distortions of the estimated cosmic ray event rate at a given energy at the percent level in both the azimuthal and the declination distributions, the latter of which mimics an almost dipolar pattern. We have also shown that the induced distortions are already at the level of the statistical uncertainties for a number of events N {approx_equal} 32 000 (we note that the full Auger surface detector array collects about 6500 events per year with energies above 3 EeV). Accounting for these effects is thus essential with regard to the correct interpretation of large scale anisotropy measurements taking explicitly profit from the declination distribution.

  3. Mass composition studies of Ultra High Energy cosmic rays through the measurement of the Muon Production Depths at the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Collica, Laura

    2014-01-01

    The Pierre Auger Observatory (Auger) in Argentina studies Ultra High Energy Cosmic Rays (UHECRs) physics. The flux of cosmic rays at these energies (above 1018 eV) is very low (less than 100 particle/km2-year) and UHECR properties must be inferred from the measurements of the secondary particles that the cosmic ray primary produces in the atmosphere. These particles cascades are called Extensive Air Showers (EAS) and can be studied at ground by deploying detectors covering large areas. The EAS physics is complex, and the properties of secondary particles depend strongly on the first interaction, which takes place at an energy beyond the ones reached at accelerators. As a consequence, the analysis of UHECRs is subject to large uncertainties and hence many of their properties, in particular their composition, are still unclear. Two complementary techniques are used at Auger to detect EAS initiated by UHE- CRs: a 3000 km2 surface detector (SD) array of water Cherenkov tanks which samples particles at ground level and fluorescence detectors (FD) which collect the ultraviolet light emitted by the de-excitation of nitrogen nuclei in the atmosphere, and can operate only in clear, moonless nights. Auger is the largest cosmic rays detector ever built and it provides high-quality data together with unprecedented statistics. The main goal of this thesis is the measurement of UHECR mass composition using data from the SD of the Pierre Auger Observatory. Measuring the cosmic ray composition at the highest energies is of fundamental importance from the astrophysical point of view, since it could discriminate between different scenarios of origin and propagation of cosmic rays. Moreover, mass composition studies are of utmost importance for particle physics. As a matter of fact, knowing the composition helps in exploring the hadronic interactions at ultra-high energies, inaccessible to present accelerator experiments.

  4. EVIDENCE FOR THE WAVE NATURE OF AN EXTREME ULTRAVIOLET WAVE OBSERVED BY THE ATMOSPHERIC IMAGING ASSEMBLY ON BOARD THE SOLAR DYNAMICS OBSERVATORY

    SciTech Connect (OSTI)

    Shen Yuandeng; Liu Yu

    2012-07-20

    Extreme-ultraviolet (EUV) waves have been found for about 15 years. However, significant controversy remains over their physical natures and origins. In this paper, we report an EUV wave that was accompanied by an X1.9 flare and a partial halo coronal mass ejection (CME). Using high temporal and spatial resolution observations taken by the Solar Dynamics Observatory and the Solar-TErrestrial RElations Observatory, we are able to investigate the detailed kinematics of the EUV wave. We find several arguments that support the fast-mode wave scenario. (1) The speed of the EUV wave (570 km s{sup -1}) is higher than the sound speed of the quiet-Sun corona. (2) Significant deceleration of the EUV wave (-130 m s{sup -2}) is found during its propagation. (3) The EUV wave resulted in the oscillations of a loop and a filament along its propagation path, and a reflected wave from the polar coronal hole is also detected. (4) Refraction or reflection effect is observed when the EUV wave was passing through two coronal bright points. (5) The dimming region behind the wavefront stopped to expand when the wavefront started to become diffuse. (6) The profiles of the wavefront exhibited a dispersive nature, and the magnetosonic Mach number of the EUV wave derived from the highest intensity jump is about 1.4. In addition, triangulation indicates that the EUV wave propagated within a height range of about 60-100 Mm above the photosphere. We propose that the EUV wave observed should be a nonlinear fast-mode magnetosonic wave that propagated freely in the corona after it was driven by the CME expanding flanks during the initial period.

  5. Gravitational waves from individual supermassive black hole binaries in circular orbits: limits from the North American nanohertz observatory for gravitational waves

    SciTech Connect (OSTI)

    Arzoumanian, Z.; Brazier, A.; Chatterjee, S.; Cordes, J. M.; Dolch, T.; Lam, M. T.; Burke-Spolaor, S.; Chamberlin, S. J.; Ellis, J. A.; Demorest, P. B.; Deng, X.; Koop, M.; Ferdman, R. D.; Kaspi, V. M.; Garver-Daniels, N.; Lorimer, D. R.; Jenet, F.; Jones, G.; Lazio, T. J. W.; Lommen, A. N.; Collaboration: NANOGrav Collaboration; and others

    2014-10-20

    We perform a search for continuous gravitational waves from individual supermassive black hole binaries using robust frequentist and Bayesian techniques. We augment standard pulsar timing models with the addition of time-variable dispersion measure and frequency variable pulse shape terms. We apply our techniques to the Five Year Data Release from the North American Nanohertz Observatory for Gravitational Waves. We find that there is no evidence for the presence of a detectable continuous gravitational wave; however, we can use these data to place the most constraining upper limits to date on the strength of such gravitational waves. Using the full 17 pulsar data set we place a 95% upper limit on the strain amplitude of h {sub 0} ? 3.0 10{sup 14} at a frequency of 10 nHz. Furthermore, we place 95% sky-averaged lower limits on the luminosity distance to such gravitational wave sources, finding that d{sub L} ? 425 Mpc for sources at a frequency of 10 nHz and chirp mass 10{sup 10} M {sub ?}. We find that for gravitational wave sources near our best timed pulsars in the sky, the sensitivity of the pulsar timing array is increased by a factor of ?four over the sky-averaged sensitivity. Finally we place limits on the coalescence rate of the most massive supermassive black hole binaries.

  6. Measurement of the cosmic ray spectrum above 4×1018 eV using inclined events detected with the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Aab, Alexander

    2015-08-26

    A measurement of the cosmic-ray spectrum for energies exceeding 4×1018 eV is presented, which is based on the analysis of showers with zenith angles greater than 60° detected with the Pierre Auger Observatory between 1 January 2004 and 31 December 2013. The measured spectrum confirms a flux suppression at the highest energies. Above 5.3×1018 eV, the ``ankle'', the flux can be described by a power law E–γ with index γ=2.70 ± 0.02 (stat) ± 0.1 (sys) followed by a smooth suppression region. For the energy (Es) at which the spectral flux has fallen to one-half of its extrapolated value in the absence of suppression, we find Es=(5.12±0.25 (stat)+1.0–1.2 (sys))×1019 eV.

  7. A low-noise transimpedance amplifier for the detection of Violin-Mode resonances in advanced Laser Interferometer Gravitational wave Observatory suspensions

    SciTech Connect (OSTI)

    Lockerbie, N. A.; Tokmakov, K. V.

    2014-11-15

    This paper describes the design and performance of an extremely low-noise differential transimpedance amplifier, which takes its two inputs from separate photodiodes. The amplifier was planned to serve as the front-end electronics for a highly sensitive shadow-displacement sensing system, aimed at detecting very low-level Violin-Mode (VM) oscillations in 0.4 mm diameter by 600 mm long fused-silica suspension fibres. Four such highly tensioned fibres support the 40 kg test-masses/mirrors of the Advanced Laser Interferometer Gravitational wave Observatory interferometers. This novel design of amplifier incorporates features which prevent noise-gain peaking arising from large area photodiode (and cable) capacitances, and which also usefully separate the DC and AC photocurrents coming from the photodiodes. In consequence, the differential amplifier was able to generate straightforwardly two DC outputs, one per photodiode, as well as a single high-gain output for monitoring the VM oscillationsthis output being derived from the difference of the photodiodes two, naturally anti-phase, AC photocurrents. Following a displacement calibration, the amplifier's final VM signal output was found to have an AC displacement responsivity at 500 Hz of (9.43 1.20) MV(rms) m{sup ?1}(rms), and, therefore, a shot-noise limited sensitivity to such AC shadow- (i.e., fibre-) displacements of (69 13) picometres/?Hz at this frequency, over a measuring span of 0.1 mm.

  8. Measurement of the nue and Total 8B Solar Neutrino Fluxes with theSudbury Neutrino Observatory Phase I Data Set

    SciTech Connect (OSTI)

    Aharmim, B.; Ahmad, Q.R.; Ahmed, S.N.; Allen, R.C.; Andersen,T.C.; Anglin, J.D.; Buehler, G.; Barton, J.C.; Beier, E.W.; Bercovitch,M.; Bergevin, M.; Bigu, J.; Biller, S.D.; Black, R.A.; Blevis, I.; Boardman, R.J.; Boger, J.; Bonvin, E.; Boulay, M.G.; Bowler, M.G.; Bowles, T.J.; Brice, S.J.; Browne, M.C.; Bullard, T.V.; Burritt, T.H.; Cameron, J.; Chan, Y.D.; Chen, H.H.; Chen, M.; Chen, X.; Cleveland, B.T.; Cowan, J.H.M.; Cowen, D.F.; Cox, G.A.; Currat, C.A.; Dai, X.; Dalnoki-Veress, F.; Davidson, W.F.; Deng, H.; DiMarco, M.; Doe, P.J.; Doucas, G.; Dragowsky, M.R.; Duba, C.A.; Duncan, F.A.; Dunford, M.; Dunmore, J.A.; Earle, E.D.; Elliott, S.R.; Evans, H.C.; Ewan, G.T.; Farine, J.; Fergani, H.; Ferraris, A.P.; Fleurot, F.; Ford, R.J.; Formaggio, J.A.; Fowler, M.M.; Frame, K.; Frank, E.D.; Frati, W.; Gagnon,N.; Germani, J.V.; Gil, S.; Goldschmidt, A.; Goon, J.T.M.; Graham, K.; Grant, D.R.; Guillian, E.; Hahn, R.L.; Hallin, A.L.; Hallman, E.D.; Hamer, A.S.; Hamian, A.A.; Handler, W.B.; Haq, R.U.; Hargrove, C.K.; Harvey, P.J.; Hazama, R.; Heeger, K.M.; Heintzelman, W.J.; Heise, J.; Helmer, R.L.; Henning, R.; Hepburn, J.D.; Heron, H.; Hewett, J.; Hime,A.; Howard, C.; Howe, M.A.; Huang, M.; Hykawy, J.G.; Isaac, M.C.P.; Jagam, P.; Jamieson, B.; Jelley, N.A.; Jillings, C.; Jonkmans, G.; Kazkaz, K.; Keener, P.T.; Kirch, K.; Klein, J.R.; Knox, A.B.; Komar,R.J.; Kormos, L.L.; Kos, M.; Kouzes, R.; Krueger, A.; Kraus, C.; Krauss,C.B.; Kutter, T.; Kyba, C.C.M.; Labranche, H.; Lange, R.; Law, J.; Lawson, I.T.; Lay, M.; Lee, H.W.; Lesko, K.T.; Leslie, J.R.; Levine, I.; Loach, J.C.; Locke, W.; Luoma, S.; Lyon, J.; MacLellan, R.; Majerus, S.; Mak, H.B.; Maneira, J.; Marino, A.D.; Martin, R.; McCauley, N.; McDonald,A.B.; McDonald, D.S.; McFarlane, K.; McGee, S.; McGregor, G.; MeijerDrees, R.; Mes, H.; Mifflin, C.; Miknaitis, K.K.S.; Miller, M.L.; Milton,G.; Moffat, B.A.; Monreal, B.; Moorhead, M.; Morrissette, B.; Nally,C.W.; Neubauer, M.S.; et al.

    2007-02-01

    This article provides the complete description of resultsfrom the Phase I data set of the Sudbury Neutrino Observatory (SNO). ThePhase I data set is based on a 0.65 kt-year exposure of heavy water tothe solar 8B neutrino flux. Included here are details of the SNO physicsand detector model, evaluations of systematic uncertainties, andestimates of backgrounds. Also discussed are SNO's approach tostatistical extraction of the signals from the three neutrino reactions(charged current, neutral current, and elastic scattering) and theresults of a search for a day-night asymmetry in the ?e flux. Under theassumption that the 8B spectrum is undistorted, the measurements fromthis phase yield a solar ?e flux of ?(?e) =1.76+0.05?0.05(stat.)+0.09?0.09 (syst.) x 106 cm?2 s?1, and a non-?ecomponent ?(? mu) = 3.41+0.45?0.45(stat.)+0.48?0.45 (syst.) x 106 cm?2s?1. The sum of these components provides a total flux in excellentagreement with the predictions of Standard Solar Models. The day-nightasymmetry in the ?e flux is found to be Ae = 7.0 +- 4.9 (stat.)+1.3?1.2percent (sys.), when the asymmetry in the total flux is constrained to bezero.

  9. OBSERVATIONS AND MODELING OF THE EMERGING EXTREME-ULTRAVIOLET LOOPS IN THE QUIET SUN AS SEEN WITH THE SOLAR DYNAMICS OBSERVATORY

    SciTech Connect (OSTI)

    Chitta, L. P.; Van Ballegooijen, A. A.; DeLuca, E. E.; Kariyappa, R.; Hasan, S. S.; Hanslmeier, A.

    2013-05-01

    We used data from the Helioseismic and Magnetic Imager (HMI) and the Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory (SDO) to study coronal loops at small scales, emerging in the quiet Sun. With HMI line-of-sight magnetograms, we derive the integrated and unsigned photospheric magnetic flux at the loop footpoints in the photosphere. These loops are bright in the EUV channels of AIA. Using the six AIA EUV filters, we construct the differential emission measure (DEM) in the temperature range 5.7-6.5 in log T (K) for several hours of observations. The observed DEMs have a peak distribution around log T Almost-Equal-To 6.3, falling rapidly at higher temperatures. For log T < 6.3, DEMs are comparable to their peak values within an order of magnitude. The emission-weighted temperature is calculated, and its time variations are compared with those of magnetic flux. We present two possibilities for explaining the observed DEMs and temperatures variations. (1) Assuming that the observed loops are composed of a hundred thin strands with certain radius and length, we tested three time-dependent heating models and compared the resulting DEMs and temperatures with the observed quantities. This modeling used enthalpy-based thermal evolution of loops (EBTEL), a zero-dimensional (0D) hydrodynamic code. The comparisons suggest that a medium-frequency heating model with a population of different heating amplitudes can roughly reproduce the observations. (2) We also consider a loop model with steady heating and non-uniform cross-section of the loop along its length, and find that this model can also reproduce the observed DEMs, provided the loop expansion factor {gamma} {approx} 5-10. More observational constraints are required to better understand the nature of coronal heating in the short emerging loops on the quiet Sun.

  10. HAWC Observatory captures first image

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

    High Energy Physics program, the National Science Foundation and Consejo Nacional de Ciencia y Tecnologa (Mexico's science funding agency) fund the construction of HAWC. The...

  11. z {approx} 4 H{alpha} EMITTERS IN THE GREAT OBSERVATORIES ORIGINS DEEP SURVEY: TRACING THE DOMINANT MODE FOR GROWTH OF GALAXIES

    SciTech Connect (OSTI)

    Shim, Hyunjin; Chary, Ranga-Ram; Dickinson, Mark; Lin Lihwai; Yan, Chi-Hung; Spinrad, Hyron; Stern, Daniel

    2011-09-01

    We present evidence for strong H{alpha} emission in galaxies with spectroscopic redshifts in the range of 3.8 < z < 5.0 over the Great Observatories Origins Deep Survey fields. Among 74 galaxies detected in the Spitzer IRAC 3.6 and 4.5 {mu}m bands, more than 70% of the galaxies show clear excess at 3.6 {mu}m compared to the expected flux density from stellar continuum only. We provide evidence that this 3.6 {mu}m excess is due to H{alpha} emission redshifted into the 3.6 {mu}m band, and classify these 3.6 {mu}m excess galaxies to be H{alpha} emitter (HAE) candidates. The selection of HAE candidates using an excess in broadband filters is sensitive to objects whose rest-frame H{alpha} equivalent width (EW) is larger than 350 A. The H{alpha} inferred star formation rates (SFRs) of the HAEs range between 20 and 500 M{sub sun} yr{sup -1} and are a factor of {approx}6 larger than SFRs inferred from the UV continuum. The ratio between the H{alpha} luminosity and UV luminosity of HAEs is also on average larger than that of local starbursts. Possible reasons for such strong H{alpha} emission in these galaxies include different dust extinction properties, young stellar population ages, extended star formation histories, low metallicity, and a top-heavy stellar initial mass function. Although the correlation between UV slope {beta} and L{sub H{alpha}}/L{sub UV} raises the possibility that HAEs prefer a dust extinction curve which is steeper in the UV, the most dominant factor that results in strong H{alpha} emission appears to be star formation history. The H{alpha} EWs of HAEs are large despite their relatively old stellar population ages constrained by spectral energy distribution fitting, suggesting that at least 60% of HAEs produce stars at a constant rate. Under the assumption that the gas supply is sustained, HAEs are able to produce {approx}> 50% of the stellar mass density that is encompassed in massive (M{sub *} > 10{sup 11} M{sub sun}) galaxies at z {approx} 3

  12. Chemical composition, microstructure, and hygroscopic properties of aerosol particles at the Zotino Tall Tower Observatory (ZOTTO), Siberia, during a summer campaign

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

    Mikhailov, E. F.; Mironov, G. N.; Pöhlker, C.; Chi, X.; Krüger, M. L.; Shiraiwa, M.; Förster, J. -D.; Pöschl, U.; Vlasenko, S. S.; Ryshkevich, T. I.; et al

    2015-03-16

    In this study we describe the hygroscopic properties of accumulation- and coarse-mode aerosol particles sampled at the Zotino Tall Tower Observatory (ZOTTO) in Central Siberia (61° N; 89° E) from 16 to 21 June 2013. The hygroscopic growth measurements were supplemented with chemical analyses of the samples, including inorganic ions and organic/elemental carbon. In addition, the microstructure and chemical composition of aerosol particles were analyzed by X-ray micro-spectroscopy (STXM-NEXAFS) and transmission electron microscopy (TEM). A mass closure analysis indicates that organic carbon accounted for 61 and 38% of PM in the accumulation mode and coarse mode, respectively. The water solublemore » fraction of organic matter was estimated to be 52 and 8% of PM in these modes. Sulfate, predominantly in the form of ammoniated sulfate, was the dominant inorganic component in both size modes: ~ 34% in the accumulation vs. ~ 47% in the coarse mode. The hygroscopic growth measurements were conducted with a filter-based differential hygroscopicity analyzer (FDHA) over the range of 5–99.4% RH in the hydration and dehydration operation modes. The FDHA study indicates that both accumulation and coarse modes exhibit pronounced water uptake approximately at the same RH, starting at ~ 70%, while efflorescence occurred at different humidities, i.e., at ~ 35% RH for submicron particles vs. ~ 50% RH for supermicron particles. This ~ 15% RH difference was attributed to higher content of organic material in the submicron particles, which suppresses water release in the dehydration experiments. The kappa mass interaction model (KIM) was applied to characterize and parameterize non-ideal solution behavior and concentration-dependent water uptake by atmospheric aerosol samples in the 5–99.4% RH range. Based on KIM, the volume-based hygroscopicity parameter, κv, was calculated. The κv, ws value related to the water soluble (ws) fraction was estimated to be ~ 0.15 for the

  13. Searches for large-scale anisotropy in the arrival directions of cosmic rays detected above energy of 10{sup 19} eV at the Pierre Auger observatory and the telescope array

    SciTech Connect (OSTI)

    Aab, A.; Abreu, P.; Andringa, S.; Aglietta, M.; Ahn, E. J.; Al Samarai, I.; Albuquerque, I. F. M.; Allekotte, I.; Asorey, H.; Allen, J.; Allison, P.; Almela, A.; Castillo, J. Alvarez; Alvarez-Muñiz, J.; Batista, R. Alves; Ambrosio, M.; Aramo, C.; Aminaei, A.; Anchordoqui, L.; Arqueros, F.; Collaboration: Pierre Auger Collaboration; Telescope Array Collaboration; and others

    2014-10-20

    Spherical harmonic moments are well-suited for capturing anisotropy at any scale in the flux of cosmic rays. An unambiguous measurement of the full set of spherical harmonic coefficients requires full-sky coverage. This can be achieved by combining data from observatories located in both the northern and southern hemispheres. To this end, a joint analysis using data recorded at the Telescope Array and the Pierre Auger Observatory above 10{sup 19} eV is presented in this work. The resulting multipolar expansion of the flux of cosmic rays allows us to perform a series of anisotropy searches, and in particular to report on the angular power spectrum of cosmic rays above 10{sup 19} eV. No significant deviation from isotropic expectations is found throughout the analyses performed. Upper limits on the amplitudes of the dipole and quadrupole moments are derived as a function of the direction in the sky, varying between 7% and 13% for the dipole and between 7% and 10% for a symmetric quadrupole.

  14. Searches for Large-Scale Anisotropy in the Arrival Directions of Cosmic Rays Detected above Energy of $10^{19}$ eV at the Pierre Auger Observatory and the Telescope Array

    SciTech Connect (OSTI)

    Aab, Alexander; et al,

    2014-10-07

    Spherical harmonic moments are well-suited for capturing anisotropy at any scale in the flux of cosmic rays. An unambiguous measurement of the full set of spherical harmonic coefficients requires full-sky coverage. This can be achieved by combining data from observatories located in both the northern and southern hemispheres. To this end, a joint analysis using data recorded at the Telescope Array and the Pierre Auger Observatory above 1019 eV is presented in this work. The resulting multipolar expansion of the flux of cosmic rays allows us to perform a series of anisotropy searches, and in particular to report on the angular power spectrum of cosmic rays above 1019 eV. No significant deviation from isotropic expectations is found throughout the analyses performed. Upper limits on the amplitudes of the dipole and quadrupole moments are derived as a function of the direction in the sky, varying between 7% and 13% for the dipole and between 7% and 10% for a symmetric quadrupole.

  15. Integrated High-Level Waste System Planning - Utilizing an Integrated Systems Planning Approach to Ensure End-State Definitions are Met and Executed - 13244

    SciTech Connect (OSTI)

    Ling, Lawrence T.; Chew, David P.

    2013-07-01

    The Savannah River Site (SRS) is a Department of Energy site which has produced nuclear materials for national defense, research, space, and medical programs since the 1950's. As a by-product of this activity, approximately 37 million gallons of high-level liquid waste containing approximately 292 million curies of radioactivity is stored on an interim basis in 45 underground storage tanks. Originally, 51 tanks were constructed and utilized to support the mission. Four tanks have been closed and taken out of service and two are currently undergoing the closure process. The Liquid Waste System is a highly integrated operation involving safely storing liquid waste in underground storage tanks; removing, treating, and dispositioning the low-level waste fraction in grout; vitrifying the higher activity waste at the Defense Waste Processing Facility; and storing the vitrified waste in stainless steel canisters until permanent disposition. After waste removal and processing, the storage and processing facilities are decontaminated and closed. A Liquid Waste System Plan (hereinafter referred to as the Plan) was developed to integrate and document the activities required to disposition legacy and future High-Level Waste and to remove from service radioactive liquid waste tanks and facilities. It establishes and records a planning basis for waste processing in the liquid waste system through the end of the program mission. The integrated Plan which recognizes the challenges of constrained funding provides a path forward to complete the liquid waste mission within all regulatory and legal requirements. The overarching objective of the Plan is to meet all Federal Facility Agreement and Site Treatment Plan regulatory commitments on or ahead of schedule while preserving as much life cycle acceleration as possible through incorporation of numerous cost savings initiatives, elimination of non-essential scope, and deferral of other scope not on the critical path to compliance. There is currently a premium on processing and storage space in the radioactive liquid waste tank system. To enable continuation of risk reduction initiatives, the Plan establishes a processing strategy that provides tank space required to meet, or minimizes the impacts to meeting, programmatic objectives. The Plan also addresses perturbations in funding and schedule impacts. (authors)

  16. Evapotranspiration And Geochemical Controls On Groundwater Plumes At Arid Sites: Toward Innovative Alternate End-States For Uranium Processing And Tailings Facilities

    SciTech Connect (OSTI)

    Looney, Brian B.; Denham, Miles E.; Eddy-Dilek, Carol A.; Millings, Margaret R.; Kautsky, Mark

    2014-01-08

    Management of legacy tailings/waste and groundwater contamination are ongoing at the former uranium milling site in Tuba City AZ. The tailings have been consolidated and effectively isolated using an engineered cover system. For the existing groundwater plume, a system of recovery wells extracts contaminated groundwater for treatment using an advanced distillation process. The ten years of pump and treat (P&T) operations have had minimal impact on the contaminant plume – primarily due to geochemical and hydrological limits. A flow net analysis demonstrates that groundwater contamination beneath the former processing site flows in the uppermost portion of the aquifer and exits the groundwater as the plume transits into and beneath a lower terrace in the landscape. The evaluation indicates that contaminated water will not reach Moenkopi Wash, a locally important stream. Instead, shallow groundwater in arid settings such as Tuba City is transferred into the vadose zone and atmosphere via evaporation, transpiration and diffuse seepage. The dissolved constituents are projected to precipitate and accumulate as minerals such as calcite and gypsum in the deep vadose zone (near the capillary fringe), around the roots of phreatophyte plants, and near seeps. The natural hydrologic and geochemical controls common in arid environments such as Tuba City work together to limit the size of the groundwater plume, to naturally attenuate and detoxify groundwater contaminants, and to reduce risks to humans, livestock and the environment. The technical evaluation supports an alternative beneficial reuse (“brownfield”) scenario for Tuba City. This alternative approach would have low risks, similar to the current P&T scenario, but would eliminate the energy and expense associated with the active treatment and convert the former uranium processing site into a resource for future employment of local citizens and ongoing benefit to the Native American Nations.

  17. Chemical composition, microstructure, and hygroscopic properties of aerosol particles at the Zotino Tall Tower Observatory (ZOTTO), Siberia, during a summer campaign

    SciTech Connect (OSTI)

    Mikhailov, E. F.; Mironov, G. N.; Pöhlker, C.; Chi, X.; Krüger, M. L.; Shiraiwa, M.; Förster, J. -D.; Pöschl, U.; Vlasenko, S. S.; Ryshkevich, T. I.; Weigand, M.; Kilcoyne, A. L. D.; Andreae, M. O.

    2015-03-16

    In this study we describe the hygroscopic properties of accumulation- and coarse-mode aerosol particles sampled at the Zotino Tall Tower Observatory (ZOTTO) in Central Siberia (61° N; 89° E) from 16 to 21 June 2013. The hygroscopic growth measurements were supplemented with chemical analyses of the samples, including inorganic ions and organic/elemental carbon. In addition, the microstructure and chemical composition of aerosol particles were analyzed by X-ray micro-spectroscopy (STXM-NEXAFS) and transmission electron microscopy (TEM). A mass closure analysis indicates that organic carbon accounted for 61 and 38% of PM in the accumulation mode and coarse mode, respectively. The water soluble fraction of organic matter was estimated to be 52 and 8% of PM in these modes. Sulfate, predominantly in the form of ammoniated sulfate, was the dominant inorganic component in both size modes: ~ 34% in the accumulation vs. ~ 47% in the coarse mode.

    The hygroscopic growth measurements were conducted with a filter-based differential hygroscopicity analyzer (FDHA) over the range of 5–99.4% RH in the hydration and dehydration operation modes. The FDHA study indicates that both accumulation and coarse modes exhibit pronounced water uptake approximately at the same RH, starting at ~ 70%, while efflorescence occurred at different humidities, i.e., at ~ 35% RH for submicron particles vs. ~ 50% RH for supermicron particles. This ~ 15% RH difference was attributed to higher content of organic material in the submicron particles, which suppresses water release in the dehydration experiments.

    The kappa mass interaction model (KIM) was applied to characterize and parameterize non-ideal solution behavior and concentration-dependent water uptake by atmospheric aerosol samples in the 5–99.4% RH range. Based on KIM, the volume-based hygroscopicity parameter, κv, was calculated. The κv, ws value related to the water soluble (ws) fraction was

  18. Beamline 7.0.2

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

    Operational No Source characteristics 5-cm period undulator (U5) (first, third, and fifth harmonics) Energy range See endstation tables Monochromator See endstation tables ...

  19. Beamline 9.0.2

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

    ENDSTATION INFORMATION Endstation name Flame chamber Characteristics Low-pressure laminar-flow burner coupled to differentially pumped source and photoionization chamber...

  20. X6.9-CLASS FLARE-INDUCED VERTICAL KINK OSCILLATIONS IN A LARGE-SCALE PLASMA CURTAIN AS OBSERVED BY THE SOLAR DYNAMICS OBSERVATORY/ATMOSPHERIC IMAGING ASSEMBLY

    SciTech Connect (OSTI)

    Srivastava, A. K. [Aryabhatta Research Institute of Observational Sciences (ARIES), Manora Peak, Nainital 263 002 (India); Goossens, M. [Centre for Mathematical Plasma Astrophysics, Department of Mathematics, KU Leuven, Celestijnenlaan 200B, B-3001 Leuven (Belgium)

    2013-11-01

    We present rare observational evidence of vertical kink oscillations in a laminar and diffused large-scale plasma curtain as observed by the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory. The X6.9-class flare in active region 11263 on 2011 August 9 induces a global large-scale disturbance that propagates in a narrow lane above the plasma curtain and creates a low density region that appears as a dimming in the observational image data. This large-scale propagating disturbance acts as a non-periodic driver that interacts asymmetrically and obliquely with the top of the plasma curtain and triggers the observed oscillations. In the deeper layers of the curtain, we find evidence of vertical kink oscillations with two periods (795 s and 530 s). On the magnetic surface of the curtain where the density is inhomogeneous due to coronal dimming, non-decaying vertical oscillations are also observed (period ? 763-896 s). We infer that the global large-scale disturbance triggers vertical kink oscillations in the deeper layers as well as on the surface of the large-scale plasma curtain. The properties of the excited waves strongly depend on the local plasma and magnetic field conditions.

  1. X{sub max}{sup μ} vs. N{sup μ} from extensive air showers as estimator for the mass of primary UHECR's. Application for the Pierre Auger Observatory

    SciTech Connect (OSTI)

    Arsene, Nicusor; Sima, Octavian

    2015-02-24

    We study the possibility of primary mass estimation for Ultra High Energy Cosmic Rays (UHECR's) using the X{sub max}{sup μ} (the height where the number of muons produced on the core of Extensive Air Showers (EAS) is maximum) and the number N{sup μ} of muons detected on ground. We use the 2D distribution - X{sub max}{sup μ} against N{sup μ} in order to find its sensitivity to the mass of the primary particle. For that, we construct a 2D Probability Function Prob(p,Fe | X{sub max}{sup μ}, N{sup μ}) which estimates the probability that a certain point from the plane (X{sub max}{sup μ}, N{sup μ}) corresponds to a shower induced by a proton, respectively an iron nucleus. To test the procedure, we analyze a set of simulated EAS induced by protons and iron nuclei at energies of 10{sup 19}eV and 20° zenith angle with CORSIKA. Using the Bayesian approach and taking into account the geometry of the infill detectors from the Pierre Auger Observatory, we observe an improvement in the accuracy of the primary mass reconstruction in comparison with the results obtained using only the X{sub max}{sup μ} distributions.

  2. Search for correlations between the arrival directions of IceCube neutrino events and ultrahigh-energy cosmic rays detected by the Pierre Auger Observatory and the Telescope Array

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

    Aartsen, M. G.

    2016-01-20

    This study presents the results of different searches for correlations between very high-energy neutrino candidates detected by IceCube and the highest-energy cosmic rays measured by the Pierre Auger Observatory and the Telescope Array. We first consider samples of cascade neutrino events and of high-energy neutrino-induced muon tracks, which provided evidence for a neutrino flux of astrophysical origin, and study their cross-correlation with the ultrahigh-energy cosmic ray (UHECR) samples as a function of angular separation. We also study their possible directional correlations using a likelihood method stacking the neutrino arrival directions and adopting different assumptions on the size of the UHECRmore » magnetic deflections. Finally, we perform another likelihood analysis stacking the UHECR directions and using a sample of through-going muon tracks optimized for neutrino point-source searches with sub-degree angular resolution. No indications of correlations at discovery level are obtained for any of the searches performed. The smallest of the p-values comes from the search for correlation between UHECRs with IceCube high-energy cascades, a result that should continue to be monitored.« less

  3. THE ARIZONA RADIO OBSERVATORY CO MAPPING SURVEY OF GALACTIC MOLECULAR CLOUDS. IV. THE NGC 1333 CLOUD IN PERSEUS IN CO J = 2-1 AND {sup 13}CO J = 2-1

    SciTech Connect (OSTI)

    Bieging, John H.; Revelle, Melissa; Peters, William L.

    2014-09-01

    We mapped the NGC 1333 section of the Perseus Molecular Cloud in the J = 2-1 emission lines of {sup 12}CO and {sup 13}CO over a 50' 60' region (3.4 4.1 pc at the cloud distance of 235 pc), using the Arizona Radio Observatory Heinrich Hertz Submillimeter Telescope. The angular resolution is 38'' (0.04 pc) and velocity resolution is 0.3 km s{sup 1}. We compare our velocity moment maps with known positions of young stellar objects (YSOs) and (sub)millimeter dust continuum emission. The CO emission is brightest at the center of the cluster of YSOs, but is detected over the full extent of the mapped region at ?10 rms. The morphology of the CO channel maps shows a kinematically complex structure, with many elongated features extending from the YSO cluster outward by ?1 pc. One notable feature appears as a narrow serpentine structure that curves and doubles back, with a total length of ?3 pc. The {sup 13}CO velocity channel maps show evidence for many low-density cavities surrounded by partial shell-like structures, consistent with previous studies. Maps of the velocity moments show localized effects of bipolar outflows from embedded YSOs, as well as a large-scale velocity gradient around the central core of YSOs, suggestive of large-scale turbulent cloud motions determining the location of current star formation. The CO/{sup 13}CO intensity ratios show the distribution of the CO opacity, which exhibits a complex kinematic structure. Identified YSOs are located mainly at the positions of greatest CO opacity. The maps are available for download as FITS files.

  4. DIRECT IMAGING OF QUASI-PERIODIC FAST PROPAGATING WAVES OF {approx}2000 km s{sup -1} IN THE LOW SOLAR CORONA BY THE SOLAR DYNAMICS OBSERVATORY ATMOSPHERIC IMAGING ASSEMBLY

    SciTech Connect (OSTI)

    Liu Wei; Title, Alan M.; Schrijver, Carolus J.; Aschwanden, Markus J.; De Pontieu, Bart; Tarbell, Theodore D.; Zhao Junwei; Ofman, Leon

    2011-07-20

    Quasi-periodic propagating fast mode magnetosonic waves in the solar corona were difficult to observe in the past due to relatively low instrument cadences. We report here evidence of such waves directly imaged in EUV by the new Atmospheric Imaging Assembly instrument on board the Solar Dynamics Observatory. In the 2010 August 1 C3.2 flare/coronal mass ejection event, we find arc-shaped wave trains of 1%-5% intensity variations (lifetime {approx}200 s) that emanate near the flare kernel and propagate outward up to {approx}400 Mm along a funnel of coronal loops. Sinusoidal fits to a typical wave train indicate a phase velocity of 2200 {+-} 130 km s{sup -1}. Similar waves propagating in opposite directions are observed in closed loops between two flare ribbons. In the k-{omega} diagram of the Fourier wave power, we find a bright ridge that represents the dispersion relation and can be well fitted with a straight line passing through the origin. This k-{omega} ridge shows a broad frequency distribution with power peaks at 5.5, 14.5, and 25.1 mHz. The strongest signal at 5.5 mHz (period 181 s) temporally coincides with quasi-periodic pulsations of the flare, suggesting a common origin. The instantaneous wave energy flux of (0.1-2.6) x 10{sup 7} erg cm{sup -2} s{sup -1} estimated at the coronal base is comparable to the steady-state heating requirement of active region loops.

  5. THE 2011 FEBRUARY 15 X2 FLARE, RIBBONS, CORONAL FRONT, AND MASS EJECTION: INTERPRETING THE THREE-DIMENSIONAL VIEWS FROM THE SOLAR DYNAMICS OBSERVATORY AND STEREO GUIDED BY MAGNETOHYDRODYNAMIC FLUX-ROPE MODELING

    SciTech Connect (OSTI)

    Schrijver, Carolus J.; Title, Alan M.; Aulanier, Guillaume; Pariat, Etienne; Delannee, Cecile E-mail: title@lmsal.com E-mail: etienne.pariat@obspm.fr

    2011-09-10

    The 2011 February 15 X2.2 flare and associated Earth-directed halo coronal mass ejection were observed in unprecedented detail with high resolution in spatial, temporal, and thermal dimensions by the Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory, as well as by instruments on the two STEREO spacecraft, then at near-quadrature relative to the Sun-Earth line. These observations enable us to see expanding loops from a flux-rope-like structure over the shearing polarity-inversion line between the central {delta}-spot groups of AR 11158, developing a propagating coronal front ('EIT wave'), and eventually forming the coronal mass ejection moving into the inner heliosphere. The observations support the interpretation that all of these features, including the 'EIT wave', are signatures of an expanding volume traced by loops (much larger than the flux rope only), surrounded by a moving front rather than predominantly wave-like perturbations; this interpretation is supported by previously published MHD models for active-region and global scales. The lateral expansion of the eruption is limited to the local helmet-streamer structure and halts at the edges of a large-scale domain of connectivity (in the process exciting loop oscillations at the edge of the southern polar coronal hole). The AIA observations reveal that plasma warming occurs within the expansion front as it propagates over quiet Sun areas. This warming causes dimming in the 171 A (Fe IX and Fe X) channel and brightening in the 193 and 211 A (Fe XII-XIV) channels along the entire front, while there is weak 131 A (Fe VIII and Fe XXI) emission in some directions. An analysis of the AIA response functions shows that sections of the front running over the quiet Sun are consistent with adiabatic warming; other sections may require additional heating which MHD modeling suggests could be caused by Joule dissipation. Although for the events studied here the effects of volumetric expansion are much

  6. Beamline 9.0.1

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

    disciplines: Applied science, biology, polymers, soft materials. Endstations: Serial crystallography Diffractive imaging Nanosurveyor GENERAL BEAMLINE INFORMATION...

  7. Beamline 11.0.2

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

    11.0.2 Print Molecular Environmental Science (MES) Scientific disciplines: Surface chemistry, environmental, planetary, biological, and medical sciences Endstations: 11.0.2.1: Ambient-pressure x-ray photoemission spectroscopy (APXPS) 11.0.2.2: Scanning transmission x-ray microscope (STXM) GENERAL BEAMLINE INFORMATION Operational Yes Source characteristics 5.0-cm period elliptical polarization undulator (EPU5) Energy range See endstation tables Monochromator See endstation tables Endstations

  8. Beamline 11.0.2

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

    2 Print Molecular Environmental Science (MES) Scientific disciplines: Surface chemistry, environmental, planetary, biological, and medical sciences Endstations: 11.0.2.1: Ambient-pressure x-ray photoemission spectroscopy (APXPS) 11.0.2.2: Scanning transmission x-ray microscope (STXM) GENERAL BEAMLINE INFORMATION Operational Yes Source characteristics 5.0-cm period elliptical polarization undulator (EPU5) Energy range See endstation tables Monochromator See endstation tables Endstations 11.0.2.1:

  9. Beamline 11.0.2

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

    2 Print Molecular Environmental Science (MES) Scientific disciplines: Surface chemistry, environmental, planetary, biological, and medical sciences Endstations: 11.0.2.1: Ambient-pressure x-ray photoemission spectroscopy (APXPS) 11.0.2.2: Scanning transmission x-ray microscope (STXM) GENERAL BEAMLINE INFORMATION Operational Yes Source characteristics 5.0-cm period elliptical polarization undulator (EPU5) Energy range See endstation tables Monochromator See endstation tables Endstations 11.0.2.1:

  10. Beamline 11.0.2

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

    11.0.2 Print Molecular Environmental Science (MES) Scientific disciplines: Surface chemistry, environmental, planetary, biological, and medical sciences Endstations: 11.0.2.1: Ambient-pressure x-ray photoemission spectroscopy (APXPS) 11.0.2.2: Scanning transmission x-ray microscope (STXM) GENERAL BEAMLINE INFORMATION Operational Yes Source characteristics 5.0-cm period elliptical polarization undulator (EPU5) Energy range See endstation tables Monochromator See endstation tables Endstations

  11. Beamline 11.0.2

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

    2 Print Molecular Environmental Science (MES) Scientific disciplines: Surface chemistry, environmental, planetary, biological, and medical sciences Endstations: 11.0.2.1: Ambient-pressure x-ray photoemission spectroscopy (APXPS) 11.0.2.2: Scanning transmission x-ray microscope (STXM) GENERAL BEAMLINE INFORMATION Operational Yes Source characteristics 5.0-cm period elliptical polarization undulator (EPU5) Energy range See endstation tables Monochromator See endstation tables Endstations 11.0.2.1:

  12. Beamline 11.0.2

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

    0.2 Print Molecular Environmental Science (MES) Scientific disciplines: Surface chemistry, environmental, planetary, biological, and medical sciences Endstations: 11.0.2.1: Ambient-pressure x-ray photoemission spectroscopy (APXPS) 11.0.2.2: Scanning transmission x-ray microscope (STXM) GENERAL BEAMLINE INFORMATION Operational Yes Source characteristics 5.0-cm period elliptical polarization undulator (EPU5) Energy range See endstation tables Monochromator See endstation tables Endstations

  13. Beamline 11.0.2

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

    2 Print Molecular Environmental Science (MES) Scientific disciplines: Surface chemistry, environmental, planetary, biological, and medical sciences Endstations: 11.0.2.1: Ambient-pressure x-ray photoemission spectroscopy (APXPS) 11.0.2.2: Scanning transmission x-ray microscope (STXM) GENERAL BEAMLINE INFORMATION Operational Yes Source characteristics 5.0-cm period elliptical polarization undulator (EPU5) Energy range See endstation tables Monochromator See endstation tables Endstations 11.0.2.1:

  14. Beamline 11.0.2

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

    1.0.2 Print Molecular Environmental Science (MES) Scientific disciplines: Surface chemistry, environmental, planetary, biological, and medical sciences Endstations: 11.0.2.1: Ambient-pressure x-ray photoemission spectroscopy (APXPS) 11.0.2.2: Scanning transmission x-ray microscope (STXM) GENERAL BEAMLINE INFORMATION Operational Yes Source characteristics 5.0-cm period elliptical polarization undulator (EPU5) Energy range See endstation tables Monochromator See endstation tables Endstations

  15. Beamline 11.0.2

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

    2 Print Molecular Environmental Science (MES) Scientific disciplines: Surface chemistry, environmental, planetary, biological, and medical sciences Endstations: 11.0.2.1: Ambient-pressure x-ray photoemission spectroscopy (APXPS) 11.0.2.2: Scanning transmission x-ray microscope (STXM) GENERAL BEAMLINE INFORMATION Operational Yes Source characteristics 5.0-cm period elliptical polarization undulator (EPU5) Energy range See endstation tables Monochromator See endstation tables Endstations 11.0.2.1:

  16. Beamline 11.0.2

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

    2 Print Molecular Environmental Science (MES) Scientific disciplines: Surface chemistry, environmental, planetary, biological, and medical sciences Endstations: 11.0.2.1: Ambient-pressure x-ray photoemission spectroscopy (APXPS) 11.0.2.2: Scanning transmission x-ray microscope (STXM) GENERAL BEAMLINE INFORMATION Operational Yes Source characteristics 5.0-cm period elliptical polarization undulator (EPU5) Energy range See endstation tables Monochromator See endstation tables Endstations 11.0.2.1:

  17. Beamline 11.0.2

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

    1.0.2 Print Molecular Environmental Science (MES) Scientific disciplines: Surface chemistry, environmental, planetary, biological, and medical sciences Endstations: 11.0.2.1: Ambient-pressure x-ray photoemission spectroscopy (APXPS) 11.0.2.2: Scanning transmission x-ray microscope (STXM) GENERAL BEAMLINE INFORMATION Operational Yes Source characteristics 5.0-cm period elliptical polarization undulator (EPU5) Energy range See endstation tables Monochromator See endstation tables Endstations

  18. Beamline 11.0.2

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

    2 Print Molecular Environmental Science (MES) Scientific disciplines: Surface chemistry, environmental, planetary, biological, and medical sciences Endstations: 11.0.2.1: Ambient-pressure x-ray photoemission spectroscopy (APXPS) 11.0.2.2: Scanning transmission x-ray microscope (STXM) GENERAL BEAMLINE INFORMATION Operational Yes Source characteristics 5.0-cm period elliptical polarization undulator (EPU5) Energy range See endstation tables Monochromator See endstation tables Endstations 11.0.2.1:

  19. Beamline 11.0.2

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

    2 Print Molecular Environmental Science (MES) Scientific disciplines: Surface chemistry, environmental, planetary, biological, and medical sciences Endstations: 11.0.2.1: Ambient-pressure x-ray photoemission spectroscopy (APXPS) 11.0.2.2: Scanning transmission x-ray microscope (STXM) GENERAL BEAMLINE INFORMATION Operational Yes Source characteristics 5.0-cm period elliptical polarization undulator (EPU5) Energy range See endstation tables Monochromator See endstation tables Endstations 11.0.2.1:

  20. Beamline 11.0.2

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

    2 Print Molecular Environmental Science (MES) Scientific disciplines: Surface chemistry, environmental, planetary, biological, and medical sciences Endstations: 11.0.2.1: Ambient-pressure x-ray photoemission spectroscopy (APXPS) 11.0.2.2: Scanning transmission x-ray microscope (STXM) GENERAL BEAMLINE INFORMATION Operational Yes Source characteristics 5.0-cm period elliptical polarization undulator (EPU5) Energy range See endstation tables Monochromator See endstation tables Endstations 11.0.2.1:

  1. Beamline 11.0.2

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

    2 Print Molecular Environmental Science (MES) Scientific disciplines: Surface chemistry, environmental, planetary, biological, and medical sciences Endstations: 11.0.2.1: Ambient-pressure x-ray photoemission spectroscopy (APXPS) 11.0.2.2: Scanning transmission x-ray microscope (STXM) GENERAL BEAMLINE INFORMATION Operational Yes Source characteristics 5.0-cm period elliptical polarization undulator (EPU5) Energy range See endstation tables Monochromator See endstation tables Endstations 11.0.2.1:

  2. Beamline 9.0.1

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

    1 Print Diffraction Microscopy Scientific disciplines: Applied science, biology, polymers, soft materials. Endstations: Serial crystallography Diffractive imaging Nanosurveyor...

  3. Beamline 9.0.1

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

    0.1 Print Diffraction Microscopy Scientific disciplines: Applied science, biology, polymers, soft materials. Endstations: Serial crystallography Diffractive imaging Nanosurveyor...

  4. Beamline 9.3.2

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

    3.2 Print Chemical and Materials Scientific disciplines: Surfaces, interfaces, catalysis, environmental science, material science, electrochemistry Endstations: Ambient pressure...

  5. Beamline 9.3.2

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    2 Print Chemical and Materials Scientific disciplines: Surfaces, interfaces, catalysis, environmental science, material science, electrochemistry Endstations: Ambient pressure...

  6. Beamline 9.3.2

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    2009 09:06 Chemical and Materials Scientific disciplines: Surfaces, interfaces, catalysis, environmental science, material science, electrochemistry Endstations: Ambient...

  7. Beamline 4.0.2

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    disciplines: Magnetism, materials science Endstations: Eight-pole electromagnet Scattering Chamber 9T magnet GENERAL BEAMLINE INFORMATION Operational Yes Source...

  8. Beamline 9.3.2

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    Surfaces, interfaces, catalysis, environmental science, material science, electrochemistry Endstations: Ambient pressure X-ray Photoelectron Spectroscopy (APXPS)* Ambient...

  9. Beamline 9.0.1

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

    Print Diffraction Microscopy Scientific disciplines: Applied science, biology, polymers, soft materials. Endstations: Serial crystallography Diffractive imaging Nanosurveyor...

  10. Beamline 11.0.2

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

    2 Print Molecular Environmental Science (MES) Scientific disciplines: Surface chemistry, environmental, planetary, biological, and medical sciences Endstations: 11.0.2.1: Ambient-pressure x-ray photoemission spectroscopy (APXPS) 11.0.2.2: Scanning transmission x-ray microscope (STXM) GENERAL BEAMLINE INFORMATION Operational Yes Source characteristics 5.0-cm period elliptical polarization undulator (EPU5) Energy range See endstation tables Monochromator See endstation tables Endstations 11.0.2.1:

  11. Ener-Gee Whiz Answers Your Questions: Thermostat Settings and Solar Water

    Energy Savers [EERE]

    Endstates Initiative Endstates Initiative Endstates Initiative Scientific and technical, institutional and regulatory, and closure management challenges are currently hindering cleanup and closure of remaining environmental legacy waste sites across the Department of Energy (DOE) complex. There are no simple solutions for these integrated challenges and they demand innovative scientific and technical solutions and approaches, developed with the regulatory community. DOE Office of Environmental

  12. Frontier Observatory for Research in Geothermal Energy: Fallon, Nevada

    DOE Data Explorer [Office of Scientific and Technical Information (OSTI)]

    Doug Blankenship

    2016-05-23

    The data is associated to the Fallon FORGE project and includes mudlogs for all wells used to characterize the subsurface, as wells as gravity, magnetotelluric, earthquake seismicity, and temperature data from the Navy GPO and Ormat. Also included are geologic maps from the USGS and Nevada Bureau of Mines and Geology for the Fallon, NV area.

  13. The Pierre Auger Observatory Upgrade - Preliminary Design Report...

    Office of Scientific and Technical Information (OSTI)

    capabilities, with an emphasis on improved mass composition determination using the ... This Preliminary Design Report was produced by the Collaboration in April 2015 as an ...

  14. Adaptive optics and laser guide stars at Lick observatory

    SciTech Connect (OSTI)

    Brase, J.M.

    1994-11-15

    For the past several years LLNL has been developing adaptive optics systems for correction of both atmospheric turbulence effects and thermal distortions in optics for high-power lasers. Our early work focused on adaptive optics for beam control in laser isotope separation and ground-based free electron lasers. We are currently developing innovative adaptive optics and laser systems for sodium laser guide star applications at the University of California`s Lick and Keck Observeratories. This talk will describe our adaptive optics technology and some of its applications in high-resolution imaging and beam control.

  15. HAWC Observatory to study universe's most energetic phenomena

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

    ... followed by more keys in a defined order as you flatten your palm across the keyboard. ... and the active galactic nucleus Markarian 421. From its perch atop the highest accessible ...

  16. The Pierre Auger Observatory: Contributions to the 34th International...

    Office of Scientific and Technical Information (OSTI)

    Publication Date: 2015-09-12 OSTI Identifier: 1223251 Report Number(s): FERMILAB-CONF-15-396-AD-AE-CD-TD arXiv eprint number arXiv:1509.03732 DOE Contract Number: AC02-07CH11359 ...

  17. Observatory of Renewable Energy for Latin America and the Caribbean...

    Open Energy Info (EERE)

    Chile, Costa Rica, Colombia, Cuba, Dominican Republic, Ecuador, Mexico, Nicaragua, Paraguay, Peru, Uruguay UN Region Caribbean, Central America, South America References...

  18. The Princeton Tritium Observatory for Light, Early Universe,...

    Office of Environmental Management (EM)

    assembled at PPPL will test principles and equipment while providing preliminary data on neutrinos before the next phase of the experiment. Introduction * In a matter of...

  19. Simulations for a next-generation UHECR observatory

    SciTech Connect (OSTI)

    Oikonomou, Foteini; Abdalla, Filipe B.; Kotera, Kumiko E-mail: kotera@iap.fr

    2015-01-01

    We explore the potential of a future, ultra-high energy cosmic ray (UHECR) experiment, that is able to overcome the limitation of low statistics, to detect anisotropy in the arrival directions of UHECRs. We concentrate on the lower energy range of future instruments (E∼> 50 EeV), where, if the UHECR source number density is not too low, the sources should be numerous enough to imprint a clustering pattern in the sky, and thus possibly in the UHECR arrival directions. Under these limits, the anisotropy signal should be dominated by the clustering of astrophysical sources per se in the large-scale structures, and not the clustering of events around individual sources. We study the potential for a statistical discrimination between different astrophysical models which we parametrise by the number density of UHECR sources, the possible bias of the UHECR accelerators with respect to the galaxy distribution, and the unknown fraction of UHECRs that have been deflected by large angles. We demonstrate that an order-of-magnitude increase in statistics would allow to discriminate between a variety of astrophysical models, provided that a sub-sample of light elements can be extracted, and that it represents a fraction ∼> 70% of the overall flux, sensitive to the UHECR source number density. Discrimination should be possible even without knowledge of the composition of the UHECRs, as long as the data are proton-dominated. We find that an anisotropy at the 99.7% level should be detectable when the number of detected events exceeds 2000 beyond 50 EeV, as long as the composition is proton dominated, and the number density of UHECR sources is relatively high, n-bar  ≥ 10{sup −3} Mpc{sup −3}. If the UHECR sources are strongly biased relative to the galaxy distribution, as are for example galaxy clusters, in which the sources might be embedded, an anisotropy at the 99.7% level should be detectable once the number of detected events exceeds 1000, if the fraction of protons at the highest energies is ∼> 60%.

  20. Frontier Observatory for Research in Geothermal Energy: Fallon, Nevada

    DOE Data Explorer [Office of Scientific and Technical Information (OSTI)]

    Doug Blankenship

    2016-03-31

    The data is associated to the Fallon FORGE project and includes mudlogs for all wells used to characterize the subsurface, as wells as gravity, magnetotelluric, earthquake seismicity, and temperature data from the Navy GPO and Ormat. Also included are geologic maps from the USGS and Nevada Bureau of Mines and Geology for the Fallon, NV area.

  1. The Enriched Xenon Observatory (Journal Article) | SciTech Connect

    Office of Scientific and Technical Information (OSTI)

    Publication Date: 2009-12-17 OSTI Identifier: 21325784 Resource Type: Journal Article Resource Relation: Journal Name: AIP Conference Proceedings; Journal Volume: 1182; Journal ...

  2. Sandia's Frontier Observatory for Research In Geothermal Energy...

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

    ... The team will develop additional scientific data including detailed analyses of rock samples, natural seismicity, surface and borehole characteristics, and other geological ...

  3. Los Alamos observatory fingers cosmic ray 'hot spots'

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

    for these observations." Cosmic rays are high-energy particles that move through our Galaxy from sources far away. No one knows exactly where cosmic rays come from, but...

  4. Beamline 12.0.1

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

    2.0.1 Print EUV optics testing and interferometry, angle- and spin-resolved photoemission Scientific discipline: Applied science, correlated electron systems Endstations: Angle- and spin-resolved photoemission (12.0.1.1) Berkeley Dose Calibration Tool (DCT)(12.0.1.2) SEMATECH Berkeley Microfield Exposure Tool (MET) (12.0.1.3) GENERAL BEAMLINE INFORMATION Operational Yes Source characteristics 8-cm-period undulator (U8) Energy range See endstation tables Monochromator See endstation tables

  5. Beamline 12.0.1

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

    2.0.1 Print EUV optics testing and interferometry, angle- and spin-resolved photoemission Scientific discipline: Applied science, correlated electron systems Endstations: Angle- and spin-resolved photoemission (12.0.1.1) Berkeley Dose Calibration Tool (DCT)(12.0.1.2) SEMATECH Berkeley Microfield Exposure Tool (MET) (12.0.1.3) GENERAL BEAMLINE INFORMATION Operational Yes Source characteristics 8-cm-period undulator (U8) Energy range See endstation tables Monochromator See endstation tables

  6. Beamline 12.0.1

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

    2.0.1 Print EUV optics testing and interferometry, angle- and spin-resolved photoemission Scientific discipline: Applied science, correlated electron systems Endstations: Angle- and spin-resolved photoemission (12.0.1.1) Berkeley Dose Calibration Tool (DCT)(12.0.1.2) SEMATECH Berkeley Microfield Exposure Tool (MET) (12.0.1.3) GENERAL BEAMLINE INFORMATION Operational Yes Source characteristics 8-cm-period undulator (U8) Energy range See endstation tables Monochromator See endstation tables

  7. Beamline 12.0.1

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

    2.0.1 Print EUV optics testing and interferometry, angle- and spin-resolved photoemission Scientific discipline: Applied science, correlated electron systems Endstations: Angle- and spin-resolved photoemission (12.0.1.1) Berkeley Dose Calibration Tool (DCT)(12.0.1.2) SEMATECH Berkeley Microfield Exposure Tool (MET) (12.0.1.3) GENERAL BEAMLINE INFORMATION Operational Yes Source characteristics 8-cm-period undulator (U8) Energy range See endstation tables Monochromator See endstation tables

  8. Beamline 12.0.1

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

    2.0.1 Print EUV optics testing and interferometry, angle- and spin-resolved photoemission Scientific discipline: Applied science, correlated electron systems Endstations: Angle- and spin-resolved photoemission (12.0.1.1) Berkeley Dose Calibration Tool (DCT)(12.0.1.2) SEMATECH Berkeley Microfield Exposure Tool (MET) (12.0.1.3) GENERAL BEAMLINE INFORMATION Operational Yes Source characteristics 8-cm-period undulator (U8) Energy range See endstation tables Monochromator See endstation tables

  9. Beamline 12.0.1

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

    2.0.1 Print EUV optics testing and interferometry, angle- and spin-resolved photoemission Scientific discipline: Applied science, correlated electron systems Endstations: Angle- and spin-resolved photoemission (12.0.1.1) Berkeley Dose Calibration Tool (DCT)(12.0.1.2) SEMATECH Berkeley Microfield Exposure Tool (MET) (12.0.1.3) GENERAL BEAMLINE INFORMATION Operational Yes Source characteristics 8-cm-period undulator (U8) Energy range See endstation tables Monochromator See endstation tables

  10. Beamline 7.0.2

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    0.2 Print Surface and Materials Science, Spectromicroscopy Scientific disciplines: Correlated electron system, materials science Endstations: nanoARPES (nARPES) EmicroARPES (Branchline 7.0.2.1) GENERAL BEAMLINE INFORMATION Operational No Source characteristics 5-cm period undulator (U5) (first, third, and fifth harmonics) Energy range See endstation tables Monochromator See endstation tables Scientific disciplines Correlated electron system, materials science Website Beamline 7:

  11. Beamline 7.0.2

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

    0.2 Print Surface and Materials Science, Spectromicroscopy Scientific disciplines: Correlated electron system, materials science Endstations: nanoARPES (nARPES) EmicroARPES (Branchline 7.0.2.1) GENERAL BEAMLINE INFORMATION Operational No Source characteristics 5-cm period undulator (U5) (first, third, and fifth harmonics) Energy range See endstation tables Monochromator See endstation tables Scientific disciplines Correlated electron system, materials science Website Beamline 7:

  12. Beamline 7.0.2

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

    0.2 Print Surface and Materials Science, Spectromicroscopy Scientific disciplines: Correlated electron system, materials science Endstations: nanoARPES (nARPES) EmicroARPES (Branchline 7.0.2.1) GENERAL BEAMLINE INFORMATION Operational No Source characteristics 5-cm period undulator (U5) (first, third, and fifth harmonics) Energy range See endstation tables Monochromator See endstation tables Scientific disciplines Correlated electron system, materials science Website Beamline 7:

  13. Beamline 7.0.2

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

    7.0.2 Print Surface and Materials Science, Spectromicroscopy Scientific disciplines: Correlated electron system, materials science Endstations: nanoARPES (nARPES) EmicroARPES (Branchline 7.0.2.1) GENERAL BEAMLINE INFORMATION Operational No Source characteristics 5-cm period undulator (U5) (first, third, and fifth harmonics) Energy range See endstation tables Monochromator See endstation tables Scientific disciplines Correlated electron system, materials science Website Beamline 7:

  14. Beamline 7.0.2

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

    0.2 Print Surface and Materials Science, Spectromicroscopy Scientific disciplines: Correlated electron system, materials science Endstations: nanoARPES (nARPES) EmicroARPES (Branchline 7.0.2.1) GENERAL BEAMLINE INFORMATION Operational No Source characteristics 5-cm period undulator (U5) (first, third, and fifth harmonics) Energy range See endstation tables Monochromator See endstation tables Scientific disciplines Correlated electron system, materials science Website Beamline 7:

  15. Beamline 7.0.2

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

    0.2 Print Surface and Materials Science, Spectromicroscopy Scientific disciplines: Correlated electron system, materials science Endstations: nanoARPES (nARPES) EmicroARPES (Branchline 7.0.2.1) GENERAL BEAMLINE INFORMATION Operational No Source characteristics 5-cm period undulator (U5) (first, third, and fifth harmonics) Energy range See endstation tables Monochromator See endstation tables Scientific disciplines Correlated electron system, materials science Website Beamline 7:

  16. Beamline 7.0.2

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

    Beamline 7.0.2 Print Surface and Materials Science, Spectromicroscopy Scientific disciplines: Correlated electron system, materials science Endstations: nanoARPES (nARPES) EmicroARPES (Branchline 7.0.2.1) GENERAL BEAMLINE INFORMATION Operational No Source characteristics 5-cm period undulator (U5) (first, third, and fifth harmonics) Energy range See endstation tables Monochromator See endstation tables Scientific disciplines Correlated electron system, materials science Website Beamline 7:

  17. Beamline 7.0.2

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

    Beamline 7.0.2 Print Surface and Materials Science, Spectromicroscopy Scientific disciplines: Correlated electron system, materials science Endstations: nanoARPES (nARPES) EmicroARPES (Branchline 7.0.2.1) GENERAL BEAMLINE INFORMATION Operational No Source characteristics 5-cm period undulator (U5) (first, third, and fifth harmonics) Energy range See endstation tables Monochromator See endstation tables Scientific disciplines Correlated electron system, materials science Website Beamline 7:

  18. Beamline 7.0.2

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

    0.2 Print Surface and Materials Science, Spectromicroscopy Scientific disciplines: Correlated electron system, materials science Endstations: nanoARPES (nARPES) EmicroARPES (Branchline 7.0.2.1) GENERAL BEAMLINE INFORMATION Operational No Source characteristics 5-cm period undulator (U5) (first, third, and fifth harmonics) Energy range See endstation tables Monochromator See endstation tables Scientific disciplines Correlated electron system, materials science Website Beamline 7:

  19. Beamline 12.0.1

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

    2.0.1 Print EUV optics testing and interferometry, angle- and spin-resolved photoemission Scientific discipline: Applied science, correlated electron systems Endstations: Angle- and spin-resolved photoemission (12.0.1.1) Berkeley Dose Calibration Tool (DCT)(12.0.1.2) SEMATECH Berkeley Microfield Exposure Tool (MET) (12.0.1.3) GENERAL BEAMLINE INFORMATION Operational Yes Source characteristics 8-cm-period undulator (U8) Energy range See endstation tables Monochromator See endstation tables

  20. Beamline 12.0.1

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

    2.0.1 Print EUV optics testing and interferometry, angle- and spin-resolved photoemission Scientific discipline: Applied science, correlated electron systems Endstations: Angle- and spin-resolved photoemission (12.0.1.1) Berkeley Dose Calibration Tool (DCT)(12.0.1.2) SEMATECH Berkeley Microfield Exposure Tool (MET) (12.0.1.3) GENERAL BEAMLINE INFORMATION Operational Yes Source characteristics 8-cm-period undulator (U8) Energy range See endstation tables Monochromator See endstation tables

  1. Beamline 7.0.2

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

    0.2 Print Surface and Materials Science, Spectromicroscopy Scientific disciplines: Correlated electron system, materials science Endstations: nanoARPES (nARPES) EmicroARPES (Branchline 7.0.2.1) GENERAL BEAMLINE INFORMATION Operational No Source characteristics 5-cm period undulator (U5) (first, third, and fifth harmonics) Energy range See endstation tables Monochromator See endstation tables Scientific disciplines Correlated electron system, materials science Website Beamline 7:

  2. Beamline 7.0.2

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

    0.2 Print Surface and Materials Science, Spectromicroscopy Scientific disciplines: Correlated electron system, materials science Endstations: nanoARPES (nARPES) EmicroARPES (Branchline 7.0.2.1) GENERAL BEAMLINE INFORMATION Operational No Source characteristics 5-cm period undulator (U5) (first, third, and fifth harmonics) Energy range See endstation tables Monochromator See endstation tables Scientific disciplines Correlated electron system, materials science Website Beamline 7:

  3. Beamline 9.0.1

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

    9.0.1 Print Diffraction Microscopy Scientific disciplines: Applied science, biology, polymers, soft materials. Endstations: Serial crystallography Diffractive imaging Nanosurveyor...

  4. Center for Nanophase Materials Sciences (CNMS) - CNMS Research

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

    Endstation Effort Achievement: A team led by Thomas Schulthess, including Gonzalo ... at NCCS 7. A CNMS user project led by Jihui Yang from General Motors ...

  5. Beamline 12.2.2

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

    2.2 Print High-Pressure Endstations: High-pressure single-crystal diffraction(in development, February 2015) High pressure laser heating GENERAL BEAMLINE INFORMATION Operational...

  6. Beamline 12.2.2

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

    20 October 2009 09:31 High-Pressure Endstations: High-pressure single-crystal diffraction(in development, February 2015) High pressure laser heating GENERAL BEAMLINE...

  7. Beamline 11.0.2

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

    Endstations: Ambient-pressure photoemission spectroscopy Scanning transmission x-ray microscope (STXM) GENERAL BEAMLINE INFORMATION Operational Yes Source characteristics 5.0-cm...

  8. Beamline 1.4.4

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

    cm-1 Interferometer resolution up to 0.125 cm-1 Endstations Thermo Nicolet Nexus 870 FTIR, Continuum XL IR microscope (N2 purged) Characteristics Computerized sample stage,...

  9. Beamline 10.3.2

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

    (EE) 7000 Endstations Hutch with optical table Characteristics Sample mounted on x-y-z translation stage Detectors Seven-element Ge solid-state fluorescence detector (XIA),...

  10. Beamline 12.2.2

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

    High-pressure science Scientific disciplines Earth sciences, materials science, construction materials, chemistry, energy. Endstations High-pressure single-crystal...

  11. Beamline 12.0.2

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

    Applied science, magnetism, materials science Endstations: 12.0.2.1: Coherent optics 12.0.2.2: Coherent x-ray scattering GENERAL BEAMLINE INFORMATION Operational Yes...

  12. Beamline 12.0.1

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

    2.0.1 Print EUV optics testing and interferometry, angle- and spin-resolved photoemission Scientific discipline: Applied science, correlated electron systems Endstations: Angle-...

  13. Monroe Thomas, Mechanical Technician

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

    and endstation moves. Though he's training another mechanical technician to operate the crane, it's Monroe who is called upon for critical moves. He plays a key role in...

  14. Beamline 11.3.1

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

    (EE) 1000 Endstations Medium sized hutch with Bruker AXS D8 diffractometer and Oxford Cryosystems Cryostream Plus Detectors Bruker AXS APEXII CCD Spot size at sample 280...

  15. Beamline 10.0.1

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

    0.1 Print Angle- and Spin-Resolved Photoelectron Spectroscopy of Solids Scientific disciplines: Strongly correlated electron systems, magnetism Endstations: High energy resolution...

  16. Beamline 10.0.1

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

    0.0.1 Print Angle- and Spin-Resolved Photoelectron Spectroscopy of Solids Scientific disciplines: Strongly correlated electron systems, magnetism Endstations: High energy...

  17. Beamline 12.0.1

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

    2.0.1 Print EUV optics testing and interferometry, angle- and spin-resolved photoemission Scientific discipline: Applied science, correlated electron systems Endstations: Angle- ...

  18. Beamline 12.0.1

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

    1 Print EUV optics testing and interferometry, angle- and spin-resolved photoemission Scientific discipline: Applied science, correlated electron systems Endstations: Angle- and ...

  19. Beamline 5.3.2.1

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

    s at sample Resolving power (EE) 5,000 Endstations Scanning transmission x-ray microscope (STXM) Characteristics Active servo-stabilized toroidal premirror Spot size at...

  20. Beamline 5.3.2.2

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

    s at sample Resolving power (EE) 5,000 Endstations Scanning transmission x-ray microscope (STXM) Characteristics Active servo-stabilized toroidal premirror Spot size at...

  1. Beamline 11.0.1

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

    1 Print PEEM3, Soft X-Ray Scattering Scientific disciplines: Magnetism, materials, surface science, polymers Endstations: 11.0.1.1: Photoemission Electron Microscope (PEEM3)...

  2. Beamline 4.0.2

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

    2 Print Magnetic Spectroscopy and Scattering Scientific disciplines: Magnetism, materials science Endstations: Eight-pole electromagnet Scattering Chamber 9T magnet GENERAL...

  3. Beamline 10.0.1

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

    Spectroscopy of Solids Scientific disciplines: Strongly correlated electron systems, magnetism Endstations: High energy resolution spectrometer (HERS) Spin- and angle-resolved...

  4. Beamline 4.0.2

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

    Beamline 4.0.2 Print Magnetic Spectroscopy and Scattering Scientific disciplines: Magnetism, materials science Endstations: Eight-pole electromagnet Scattering Chamber 9T magnet...

  5. Microsoft PowerPoint - ARM_Trepte.ppt [Compatibility Mode]

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

    Results y from CALIPSO CALIPSO Chip Trepte Chip Trepte NASA Langley Research Center 1 with help from: M. Vaughan, A. Omar, B. Hunt, K. Powell, B. Pierce, O. Torres, K. McCann, R. Hoff, M. Pitts, S. Ackermann, R. Holz,,, C. Hostetler, Z. Liu, R. Ferrare, J. Mace, and D. Winker CALIPSO Mission Overview First polarization lidar in space Joint NASA-CNES collaboration Proposed: 1998 Objectives: Improved understanding of aerosol and cloud effects on radiation budget Improved understanding of

  6. ARM - Publications: Science Team Meeting Documents

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

    formation as part of a constellation of satellites including Aqua, CALIPSO, PARASOL and Aura. We develop an algorithm that will be implemented operationally to identify significant...

  7. Radiative Energy Balance in the Tropical Tropopause Layer: An...

    Office of Scientific and Technical Information (OSTI)

    tropical cirrus clouds from the CALIPSO satellite and from ground-based micropulse and Raman lidar observations; (v) improving the parameterization of optical properties of cirrus ...

  8. ARM - Publications: Science Team Meeting Documents: Stratocumulus...

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

    Platt, C. Colorado State University and CSIRO Atmospheric Research Bennett, John CSIRO Atmospheric Research The NASA CALIPSO satellite instrument due to be launched in mid-2005 ...

  9. 14655 Section C

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

    C Contract No. DE-AC06-05RL14655 226 C-i PART I - THE SCHEDULE SECTION C - STATEMENT OF WORK TABLE OF CONTENTS C.1 PURPOSE, OVERVIEW, END-STATES, AND ORGANIZATION ................................................... 1 C.1.1 PURPOSE AND OVERVIEW ................................................................................................ 1 C.1.2 END-STATES ........................................................................................................................ 1 C.1.3

  10. Azimuthal asymmetry in the risetime of the surface detector signals of the Pierre Auger Observatory

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

    Aab, Alexander

    2016-04-07

    The azimuthal asymmetry in the risetime of signals in Auger surface detector stations is a source of information on shower development. The azimuthal asymmetry is due to a combination of the longitudinal evolution of the shower and geometrical effects related to the angles of incidence of the particles into the detectors. The magnitude of the effect depends upon the zenith angle and state of development of the shower and thus provides a novel observable, (secθ)max, sensitive to the mass composition of cosmic rays above 3 x 1018 eV. By comparing measurements with predictions from shower simulations, we find for bothmore » of our adopted models of hadronic physics (QGSJETII-04 and EPOS-LHC) an indication that the mean cosmic-ray mass increases slowly with energy, as has been inferred from other studies. However, the mass estimates are dependent on the shower model and on the range of distance from the shower core selected. Furthermore, the method has uncovered further deficiencies in our understanding of shower modelling that must be resolved before the mass composition can be inferred from (secθ)max.« less

  11. Remote sensing-based characterization, 2-m, Plant Functional Type Distributions, Barrow Environmental Observatory, 2010

    DOE Data Explorer [Office of Scientific and Technical Information (OSTI)]

    Zachary Langford; Forrest Hoffman; Jitendra Kumar

    Arctic ecosystems have been observed to be warming faster than the global average and are predicted to experience accelerated changes in climate due to global warming. Arctic vegetation is particularly sensitive to warming conditions and likely to exhibit shifts in species composition, phenology and productivity under changing climate. Mapping and monitoring of changes in vegetation is essential to understand the effect of climate change on the ecosystem functions. Vegetation exhibits unique spectral characteristics which can be harnessed to discriminate plant types and develop quantitative vegetation indices. We have combined high resolution multi-spectral remote sensing from the WorldView 2 satellite with LIDAR-derived digital elevation models to characterize the tundra landscape on the North Slope of Alaska. Classification of landscape using spectral and topographic characteristics yields spatial regions with expectedly similar vegetation characteristics. A field campaign was conducted during peak growing season to collect vegetation harvests from a number of 1m x 1m plots in the study region, which were then analyzed for distribution of vegetation types in the plots. Statistical relationships were developed between spectral and topographic characteristics and vegetation type distributions at the vegetation plots. These derived relationships were employed to statistically upscale the vegetation distributions for the landscape based on spectral characteristics. Vegetation distributions developed are being used to provide Plant Functional Type (PFT) maps for use in the Community Land Model (CLM).

  12. Remote sensing-based characterization of plant functional type distributions at the Barrow Environmental Observatory

    DOE Data Explorer [Office of Scientific and Technical Information (OSTI)]

    Kumar, Jitendra; Hoffman, Forrest M.

    Arctic ecosystems have been observed to be warming faster than the global average and are predicted to experience accelerated changes in climate due to global warming. Arctic vegetation is particularly sensitive to warming conditions and likely to exhibit shifts in species composition, phenology and productivity under changing climate. Mapping and monitoring of changes in vegetation is essential to understand the effect of climate change on the ecosystem functions. Vegetation exhibits unique spectral characteristics which can be harnessed to discriminate plant types and develop quantitative vegetation indices. We have combined high resolution multi-spectral remote sensing from the WorldView 2 satellite with LIDAR-derived digital elevation models to characterize the tundra landscape on the North Slope of Alaska. Classification of landscape using spectral and topographic characteristics yields spatial regions with expectedly similar vegetation characteristics. A field campaign was conducted during peak growing season to collect vegetation harvests from a number of 1m x 1m plots in the study region, which were then analyzed for distribution of vegetation types in the plots. Statistical relationships were developed between spectral and topographic characteristics and vegetation type distributions at the vegetation plots. These derived relationships were employed to statistically upscale the vegetation distributions for the landscape based on spectral characteristics. Vegetation distributions developed are being used to provide Plant Functional Type (PFT) maps for use in the Community Land Model (CLM).

  13. The Princeton Tritium Observatory for Light, Early Universe, Massive Neutrino Yield (PTOLEMY)

    Broader source: Energy.gov [DOE]

    Presentation from the 34th Tritium Focus Group Meeting held in Idaho Falls, Idaho on September 23-25, 2014.

  14. The Pierre Auger Observatory: Contributions to the 34th International Cosmic Ray Conference (ICRC 2015)

    SciTech Connect (OSTI)

    Aab, Alexander; et al.

    2015-09-12

    One or more papers on each of the following topics are included in this volume: energy spectrum, arrival directions and anisotropies, composition, hadronic interactions, cosmology and geophysics, detectors, and otureach.

  15. A Nobel for Neutrinos: Sudbury Neutrino Observatory | U.S. DOE...

    Office of Science (SC) Website

    The success of nuclear-physics calculations of solar energy generation has been dramatically confirmed. The discovery, moreover, opens new doors to an understanding of such basic ...

  16. Remote sensing-based characterization, 2-m, Plant Functional Type Distributions, Barrow Environmental Observatory, 2010

    DOE Data Explorer [Office of Scientific and Technical Information (OSTI)]

    Zachary Langford; Forrest Hoffman; Jitendra Kumar

    2014-01-01

    Arctic ecosystems have been observed to be warming faster than the global average and are predicted to experience accelerated changes in climate due to global warming. Arctic vegetation is particularly sensitive to warming conditions and likely to exhibit shifts in species composition, phenology and productivity under changing climate. Mapping and monitoring of changes in vegetation is essential to understand the effect of climate change on the ecosystem functions. Vegetation exhibits unique spectral characteristics which can be harnessed to discriminate plant types and develop quantitative vegetation indices. We have combined high resolution multi-spectral remote sensing from the WorldView 2 satellite with LIDAR-derived digital elevation models to characterize the tundra landscape on the North Slope of Alaska. Classification of landscape using spectral and topographic characteristics yields spatial regions with expectedly similar vegetation characteristics. A field campaign was conducted during peak growing season to collect vegetation harvests from a number of 1m x 1m plots in the study region, which were then analyzed for distribution of vegetation types in the plots. Statistical relationships were developed between spectral and topographic characteristics and vegetation type distributions at the vegetation plots. These derived relationships were employed to statistically upscale the vegetation distributions for the landscape based on spectral characteristics. Vegetation distributions developed are being used to provide Plant Functional Type (PFT) maps for use in the Community Land Model (CLM).

  17. GLAST Observatory Renamed for Fermi, Reveals Entire Gamma-Ray Sky

    Broader source: Energy.gov [DOE]

    WASHINGTON, D.C. - The U.S. Department of Energy (DOE) and NASA announced today that the Gamma-Ray Large Area Space Telescope (GLAST) has revealed its first all-sky map in gamma rays.  The onboard...

  18. Digital Elevation Model, 0.25 m, Barrow Environmental Observatory, Alaska, 2013

    DOE Data Explorer [Office of Scientific and Technical Information (OSTI)]

    Cathy Wilson; Garrett Altmann

    2015-11-20

    This 0.25m horizontal resolution digital elevation model, DEM, was developed from Airborne Laser Altimetry flown by Aerometric Inc, now known as Quantum Spatial, Inc. on 12 July, 2013. One Mission was flown and the data jointly processed with LANL personnel to produce a 0.25m DEM covering a region approximately 2.8km wide and 12.4km long extending from the coast above North Salt Lagoon to south of Gas Well Road. This DEM encompasses a diverse range of hydrologic, geomorphic, geophysical and biological features typical of the Barrow Peninsula. Vertical accuracy at the 95% confidence interval was computed as 0.143m. The coordinate system, datum, and geoid for this DEM are UTM Zone 4N, NAD83 (2011), NAVD88 (GEOID09).

  19. The Princeton Tritium Observatory for Light, Early Universe, Massive Neutrino Yield (PTOLEMY) Prototype

    Office of Environmental Management (EM)

    and Potential of Geothermal Energy The Power and Potential of Geothermal Energy October 3, 2011 - 7:03pm Addthis Dan Leistikow Dan Leistikow Former Director, Office of Public Affairs As Secretary Chu noted this weekend, America finds itself in a fierce global competition for the clean energy jobs and industries of the future - with countries like China, Germany and others investing tens of billions of dollars to expand their domestic renewable energy industry and capture the lead in a rapidly

  20. Remote sensing-based characterization of plant functional type distributions at the Barrow Environmental Observatory

    DOE Data Explorer [Office of Scientific and Technical Information (OSTI)]

    Kumar, Jitendra; Hoffman, Forrest M.

    2014-03-18

    Arctic ecosystems have been observed to be warming faster than the global average and are predicted to experience accelerated changes in climate due to global warming. Arctic vegetation is particularly sensitive to warming conditions and likely to exhibit shifts in species composition, phenology and productivity under changing climate. Mapping and monitoring of changes in vegetation is essential to understand the effect of climate change on the ecosystem functions. Vegetation exhibits unique spectral characteristics which can be harnessed to discriminate plant types and develop quantitative vegetation indices. We have combined high resolution multi-spectral remote sensing from the WorldView 2 satellite with LIDAR-derived digital elevation models to characterize the tundra landscape on the North Slope of Alaska. Classification of landscape using spectral and topographic characteristics yields spatial regions with expectedly similar vegetation characteristics. A field campaign was conducted during peak growing season to collect vegetation harvests from a number of 1m x 1m plots in the study region, which were then analyzed for distribution of vegetation types in the plots. Statistical relationships were developed between spectral and topographic characteristics and vegetation type distributions at the vegetation plots. These derived relationships were employed to statistically upscale the vegetation distributions for the landscape based on spectral characteristics. Vegetation distributions developed are being used to provide Plant Functional Type (PFT) maps for use in the Community Land Model (CLM).

  1. A Nobel for Neutrinos: Sudbury Neutrino Observatory | U.S. DOE...

    Office of Science (SC) Website

    produced by neutrino interactions in the heavy water with which the vessel will be filled. ... He proposed a detector based on heavy water that could detect all flavors equally. The ...

  2. Cosmic-ray physics with the milagro gamma-ray observatory (Journal...

    Office of Scientific and Technical Information (OSTI)

    Milagro has made the first measurement of the Galactic diffuse emission in the TeV energy ... also discovered a time dependence to this anisotropy, perhaps due to solar modulation. ...

  3. Comparative risk analysis for the Rocky Flats Plant integrated project planning

    SciTech Connect (OSTI)

    Jones, M.E.; Shain, D.I.

    1994-05-01

    The Rocky Flats Plant is developing, with active stakeholder a comprehensive planning strategy that will support transition of the Rocky Flats Plant from a nuclear weapons production facility to site cleanup and final disposition. Final disposition of the Rocky Flats Plant materials and contaminants requires consideration of the interrelated nature of sitewide problems, such as material movement and disposition, facility and land use endstates, costs relative risks to workers and the public, and waste disposition. Comparative Risk Analysis employs both incremental risk and cumulative risk evaluations to compare risks from postulated options or endstates. These postulated options or endstates can be various remedial alternatives, or future endstate uses of federal agency land. Currently, there does not exist any approved methodology that aggregates various incremental risk estimates. Comparative Risk Analysis has been developed to aggregate various incremental risk estimates to develop a site cumulative risk estimate. This paper discusses development of the Comparative Risk Analysis methodology, stakeholder participation and lessons learned from these challenges.

  4. END POINTS MANAGEMENT End Points Management The Need for End...

    Office of Environmental Management (EM)

    End Points End-state has been used to refer to the overall status and disposition of a ... They are equally applicable and usable for planning of stabilization and decommissioning ...

  5. Beamline 1.4.3

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

    cm-1 Interferometer resolution Up to 0.125 cm-1 Endstations Nicolet Magna 760 FTIR, Nic-Plan IR Microscope (N2 purged) Characteristics Motorized sample stage, 0.1-micron...

  6. Beamline 12.2.2

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

    2.2.2 Print High-Pressure Endstations: High-pressure single-crystal diffraction(in development, February 2015) High pressure laser heating GENERAL BEAMLINE INFORMATION Operational...

  7. Beamline 11.0.1

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

    eV Endstations 11.0.1.1: Photoemission electron microscope (PEEM3) 11.0.1.2: Soft x-ray scattering Special notes Polarization is user selectable; linear polarization continuously...

  8. Beamline 11.0.1

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

    materials, surface science, polymers Endstations: 11.0.1.1: Photoemission Electron Microscope (PEEM3) 11.0.1.2: Soft X-Ray Scattering GENERAL BEAMLINE INFORMATION Operational Yes...

  9. Beamline 5.4.1

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

    10,000 cm-1 Interferometer resolution Up to 0.125 cm-1 Endstations FTIR bench and IR microscope (N2 purged) Characteristics Computerized sample stage, 0.1-micron resolution;...

  10. Beamline 5.4.1

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

    range 650 - 10,000 cm-1 Interferometer resolution Up to 0.125 cm-1 Endstations FTIR bench and IR microscope (N2 purged) Characteristics Computerized sample stage,...