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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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Image of one of the first bubbles seen in the COUPP-60 detector, located half a mile underground at SNOLAB in Ontario, Canada. The bubble appears as a black semi-circle on the lower left-hand side of the image. The white ovals in the center are reflections of LED lights. (Courtesy: SNOLAB) |
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The COUPP-60 detector installed at the SNOLAB underground laboratory in Ontario, Canada. (Courtesy: SNOLAB) |
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Scientists install the COUPP-60 detector a mile and a half underground at SNOLAB in Ontario, Canada. (Courtesy: Fermilab) |
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When completed, the NOvA detector will comprise 28 detector blocks, each measuring about 50 feet tall, 50 feet wide and 6 feet deep. (Courtesy: Fermilab) |
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Electronics that make up part of the data acquisition system are installed on the top and side of the detector. The NOvA experiment is a collaboration of 169 scientists from 19 universities and laboratories in the U.S and another 15 institutions around the world. The scientists are funded by the U.S. Department of Energy, the National Science Foundation and funding agencies in the Czech Republic, Greece, India, Russia and the United Kingdom. (Courtesy: Fermilab) |
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Scientists and engineers at Fermi National Accelerator Laboratory developed the 750,000-pound pivoter machine that will put the blocks of the NOvA detector in place. (Courtesy: Fermilab) |
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Technicians glue modules for the NOvA detector using a machine developed at Argonne National Laboratory. (Courtesy: William Miller, NOvA installation manager) |
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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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IKAROS Spacecraft (Courtesy: JAXA) |
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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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XENON100 (Courtesy: XENON Collaboration) |
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Rolf Heuer at CERN Higgs Boson search update (Courtesy: Maximilien Brice, Laurent Egli) |
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