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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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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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Schematic illustration of the magnification of PS1-10afx. A massive object between us and the supernova bends light rays much as a glass lens can focus light. As more light rays are directed toward the observer than would be without the lens, the supernova appears magnified. (Courtesy: Kavli IPMU) |
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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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LHC consolidations 2013-14 (Courtesy: CERN) |
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Finding evidence for the acceleration of protons has long been a key issue in the efforts to explain the origin of cosmic rays. This pair of spectra from two supernova remnants, shown here with data from various satellites and wavelengths, are the "smoking gun" that researchers have been looking for. The Fermi Large Area Telescope's observations fit neatly with predictions of neutral pion decay. (Credit: NASA/DOE/Fermi LAT Collaboration, Chandra X-ray Observatory, ESA Herschel/XMM-Newton) |
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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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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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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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RHIC's two large experiments, STAR and PHENIX, have multiple detector components and complex electronics for tracking and identifying the particles that fly out after ions collide at nearly the speed of light. (Courtesy: BNL) |
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The nuclear phase diagram: RHIC sits in the energy "sweet spot" for exploring the transition between ordinary matter made of hadrons and the early universe matter known as quark-gluon plasma. Courtesy: BNL) |
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An artist's rendering of the proposed Large Synoptic Survey Telescope. The 8.4-meter LSST will use a special three-mirror design, creating an exceptionally wide field of view and will have the ability to survey the entire sky in only three nights. (Courtesy: LSST Corporation) |
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A proton-proton collision event in the CMS experiment producing two high-energy photons (red towers). This is what we would expect to see from the decay of a Higgs boson but it is also consistent with background Standard Model physics processes. (Courtesy: CERN) |
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Event recorded with the CMS detector in 2012 at a proton-proton centre of mass energy of 8 TeV. The event shows characteristics expected from the decay of the SM Higgs boson to a pair of Z bosons, one of which subsequently decays to a pair of electrons (green lines and green towers) and the other Z decays to a pair of muons (red lines). The event could also be due to known standard model background processes. (CourtesyL Taylor, L.) |
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The latest results from the BaBar experiment may suggest a surplus over Standard Model predictions of a type of particle decay called “B to D-star-tau-nu.” In this conceptual art, an electron and positron collide, resulting in a B meson (not shown) and an antimatter B-bar meson, which then decays into a D meson and a tau lepton as well as a smaller antineutrino. (Courtesy: Greg Stewart, SLAC National Accelerator Laboratory) |
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This graph shows the parameters for muon neutrino mixing. The red curve shows the latest MINOS result for the boundary of the region of allowed values for the mixing parameters. The MINOS result is compared with its own earlier results (blue) and measurements from other experiments (black, green).The red star is the set of parameters preferred by the MINOS data, specifically a delta m squared of 2.39x10-3 ev2 and a value for sin2(2theta) of 0.96. The new MINOS result uses all neutrino beam and antineutrino beam data from the NuMI beamline and also includes data from atmospheric neutrinos collected at the MINOS detector. (Courtesy: Fermilab) |
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The blue and red regions in both plots show the areas allowed by MINOS for the parameters of electron-neutrino appearance. The top plot shows the MINOS measurement for one ordering of neutrino masses; the bottom plot shows the same measurement assuming the other mass ordering. The vertical axis shows allowed values of an unknown parameter that controls how much neutrinos and antineutrinos show different behavior in this process. (Courtesy: Fermilab) |
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The Enriched Xenon Observatory is a neutrino experiment housed 2150 feet below ground in a salt basin at the Waste Isolation Pilot Plant (WIPP). The subterranean location isolates it from cosmic rays and other sources of natural radioactivity. (Credit: EXO/WIPP/SLAC) |
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Illustration of the IceCube sensors (photomultipliers), of which more than 5000 are deployed up to 2.5km deep in the Antarctic ice. (Courtesy: NSF/J. Yang) |
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Little is known about the ultra high-energy cosmic rays that regularly penetrate the atmosphere. Recent IceCube research rules out the leading theory that they come from Gamma Ray Bursts. (Courtesy: NSF/J. Yang) |
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Protons, neutrons melt to produce 'quark-gluon plasma' at RHIC |
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Observed and expected exclusion limits for a Standard Model Higgs boson at the 95-percent confidence level for the combined CDF and DZero analyses. The limits are expressed as multiples of the SM prediction for test masses chosen every 5 GeV/c2 in the range of 100 to 200 GeV/c2. The points are joined by straight lines for better readability. The yellow and green bands indicate the 68- and 95-percent probability regions, in the absence of a signal.The difference between the observed and expected limits around 124 GeV could be explained by the presense of a Higgs boson whose mass would lie between 115 to 135 GeV. The CDF and DZero data exclude a Higgs boson between 147 and 179 GeV/c2 at the 95-percent confidence level. (Courtesy: Fermilab) |
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The new CDF and Dzero combined result for the W boson mass (vertical section of green oval), combined with the world's best value for the top quark mass (horizontal section of green oval), restricts the Higgs mass requiring it to be less than 152 GeV/c^2 with 95 percent probability. Direct searches have narrowed the allowed Higgs mass range to 115-127 GeV/c^2. The grey bar shows the remaining area the Higgs could reside in. (Courtesy: Fermilab) |
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