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The Muon g-2 storage ring, in its current location at Brookhaven National Laboratory in New York. The ring, which will capture muons in a magnetic field, must be transported in one piece, and moved flat to avoid undue pressure on the superconducting cable inside. (Courtesy: Brookhaven National Laboratory) |
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The COUPP-60 detector installed at the SNOLAB underground laboratory in Ontario, Canada. (Courtesy: SNOLAB) |
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Stephan Ettenauer, a post-doctorial fellow on the ATRAP experiment , with the Penning trap apparatus for trapping antiprotons. (Courtesy: CERN, Anna Pantelia) |
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Presentation of Large Hadron Collider (LHC) latest results at Moriond/QCD conference, Mar. 9-16, 2013 at La Thuile, Italy (Courtesy: CERN) |
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Presentation of Large Hadron Collider (LHC) latest results at Moriond/QCD conference, Mar. 9-16, 2013 at La Thuile, Italy (Courtesy: CERN) |
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Presentation of Large Hadron Collider (LHC) latest results at Moriond/QCD conference, Mar. 9-16, 2013 at La Thuile, Italy (Courtesy: CERN) |
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When stars explode, the supernovas send off shock waves like the one shown in this artist's rendition, which accelerate protons to cosmic-ray energies through a process known as Fermi acceleration. (Credit: Greg Stewart / SLAC National Accelerator Laboratory) |
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This image combines data from ESA's Herschel Space Observatory with Fermi's gamma-ray observations (magenta) of supernova remnant W44. This remnant is a prime example of the remains of a supernova interacting with dense interstellar material around it and was one of two supernova remnants that provided the data Fermi needed to prove that cosmic rays are accelerated in supernova shock waves. (Credit: NASA/DOE/Fermi LAT Collaboration and ESA/Herschel) |
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In order to understand the origin and acceleration of cosmic-ray protons, researchers used data from the Fermi Gamma-ray Space Telescope and targeted W44 and IC 443, two supernova remnants thousands of light years away. Both turned out to be strong sources of gamma rays, but not at energies below what neutral pion decay would produce - the observational proof scientists had been looking for. (Credit: NASA/DOE/Fermi LAT Collaboration) |
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IKAROS Spacecraft (Courtesy: JAXA) |
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The BigBOSS proposal adds a new widefield, prime-focus corrector to the Mayall 4-meter telescope. A focal array with 5,000 optical fibers, individually positioned by robotic actuators, delivers light to a set of 10 three-arm spectrometers. (Lawrence Berkeley National Laboratory. Background photo Mark Duggan) |
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LHCb Experiment - #LHCb say “THANKS!!” to #LHC operators for delivering them 2 fb-1 (hundred million million visible collisions) in 2012 (Courtesy: CERN) |
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Zoomed-in image from the Dark Energy Camera of the barred spiral galaxy NGC 1365, in the Fornax cluster of galaxies, which lies about 60 million light years from Earth. (Courtesy: Dark Energy Survey Collaboration) |
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The Dark Energy Camera features 62 charged-coupled devices (CCDs), which record a total of 570 megapixels per snapshot. (Courtesy: Fermilab) |
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Dark Energy Camera telescope simulator at Fermilab. (Courtesy: Fermilab) |
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The Blanco telescope in Chile as seen from the air. (Courtesy: NOAO/AURA/NSF) |
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Hyper Suprime-Cam. The instrument weighs 3 tons and is 3 m (9 ft.) high. (Courtesy: NAOJ) |
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The layout of the 116 CCDs with a total of 870 million pixels. (Courtesy: NAOJ) |
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The Wide Field Corrector (Courtesy: NAOJ) |
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Astronomers in the observation room of the Subaru Telescope carry out performance tests of HSC. (Courtesy: NAOJ) |
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BOSS is capturing accurate spectra for millions of astronomical objects by using 2,000 plug plates that are placed at the Sloan Foundation Telescope's focal plane. Each of the 1,000 holes drilled in a single plug plate captures the light from a specific galaxy, quasar, or other target, and conveys its light to a sensitive spectrograph through an optical fiber. The plates are marked to indicate which holes belong to which bundles of the thousand optical fibers that carry the object's light. (Courtesy: Berkeley Lab) |
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Photo montage showing the gamma-ray sky over Namibia, as measured by the four H.E.S.S. telescopes during the last years, superimposed onto an optical image, with one of the small H.E.S.S. telescopes in the foreground (Credit: H.E.S.S. Collaboration, Fabio Acero and Henning Gast) |
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View of the full H.E.S.S. array with the four 12 m telescopes and the new 28 m H.E.S.S. II telescope (Credit: H.E.S.S. Collaboration, Arnim Balzer) |
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The H.E.S.S. II steel structure before installation of the camera and mirror facets, on a (unusual) cloudy day (Credit: H.E.S.S. Collaboration, Christian Föhr) |
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The "camera" with photosensors and readout electronics is loaded into the nose of the telescope (Credit: H.E.S.S. Collaboration, Arnim Balzer) |
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