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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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A model of the truck that will be used to transport the Muon g-2 ring, placed on a streetscape for scale. The truck will be escorted by police and other vehicles when it moves from Brookhaven National Laboratory in New York to a barge, and then from the barge to Fermi National Accelerator Laboratory in Illinois. (Courtesy: Fermilab) |
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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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The light curve of PS1-10afx compared to a normal SNIa. The blue dots show the observations of PS1-10afx through a red (i-band) filter, which corresponds to ultra-violet (UV) light in the rest frame of the supernova. The red squares show UV observations of the nearby SNIa, 2011fe compressed slightly along the time axis to match the width of PS1-10afx in its rest frame. The dashed lines show a fit to the SN 2011fe data and this same curve shifted by a constant factor of 30. The good agreement with the PS1-10afx data shows that PS1-10afx has the lightcurve shape of a normal SNIa, but it is 30 times brighter than expected. (Courtesy: Kavli IPMU) |
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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 3D image shows a cosmic-ray muon producing a large shower of energy as it passes through the NOvA far detector in Minnesota. (Courtesy: NOvA collaboration) |
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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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InterAction Collaboration meeting in Rome, November 2012. |
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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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