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  • Image# ST0031
  • ST
  • 12/18/2014

An overview of how the LHC at CERN can look for dark matter. (Credit: STFC/Ben Gilliland)

  • Image# OT0172
  • OT
  • 03/19/2014

This graphic shows the four individual top quark mass measurements published by the ATLAS, CDF, CMS and DZero collaborations, together with the joint and most precise measurement obtained in a joint analysis. The ATLAS and CMS experiment recorded top quark events using the Large Hadron Collider at CERN, and the CDF and DZero experiments recorded top quark events using the Tevatron collider at Fermilab. Image courtesy ATLAS, CDF, CMS and DZero collaborations. (Credit: CERN/Fermilab)

  • Image# SL0111
  • SL
  • 03/17/2014

The bottom part of this illustration shows the scale of the universe versus time. Specific events are shown such as the formation of neutral Hydrogen at 380 000 years after the big bang. Prior to this time, the constant interaction between matter (electrons) and light (photons) made the universe opaque. After this time, the photons we now call the CMB started streaming freely. The fluctuations (differences from place to place) in the matter distribution left their imprint on the CMB photons. The density waves appear as temperature and "E-mode" polarization. The gravitational waves leave a characteristic signature in the CMB polarization: the "B-modes". Both density and gravitational waves come from quantum fluctuations which have been magnified by inflation to be present at the time when the CMB photons were emitted. (Courtesy: SLAC)

  • Image# FN0428
  • FN
  • 02/11/2014

A graphic representation of one of the first neutrino interactions captured at the NOvA far detector in northern Minnesota. The dotted red line represents the neutrino beam, generated at Fermilab in Illinois and sent through 500 miles of earth to the far detector. The image on the left is a simplified 3-D view of the detector, the top right view shows the interaction from the top of the detector, and the bottom right view shows the interaction from the side of the detector. (Courtesy: Fermilab)

  • Image# FN0429
  • FN
  • 02/11/2014

Workers at the NOvA hall in northern Minnesota assemble the final block of the far detector in early February 2014, with the nearly completed detector in the background. Each block of the detector measures about 50 feet by 50 feet by 6 feet and is made up of 384 plastic PVC modules, assembled flat on a massive pivoting machine. (Courtesy: NOvA collaboration)

  • Image# BN0049
  • BN
  • 02/03/2014

Technician Mike Myers checks components of stochastic cooling "kickers," which generate electric fields to nudge ions in RHIC's gold beams back into tightly packed bunches. This system of squeezing and cooling beams has produced dramatic increases in collision rates—and the data coming out of RHIC. (Courtesy: BNL)

  • Image# CE0340
  • CE
  • 01/21/2014

ASACUSA (Courtesy: Yasunori, Yamakazi)

  • Image# CE0342
  • CE
  • 01/21/2014

Electrostatic protocol treatment lens. The purpose of this device is to transport Antiprotons from the new ELENA storage beam to all AD experiments. The electrostatic device was successfully tested in ASACUSA two weeks ago. (Courtesy: Maximilien Brice)

  • Image# CE0343
  • CE
  • 01/21/2014

Electrostatic protocol treatment lens device transport Antiprotons new ELENA storage beam AD experiments successfully tested ASACUSA

  • Image# LB0058
  • LB
  • 01/08/2014

An artist's conception of the measurement scale of the universe. Baryon acoustic oscillations are the tendency of galaxies and other matter to cluster in spheres, which originated as density waves traveling through the plasma of the early universe. The clustering is greatly exaggerated in this illustration. The radius of the spheres (white line) is the scale of a “standard ruler” allowing astronomers to determine, within one percent accuracy, the large-scale structure of the universe and how it has evolved. (Courtesy: Zosia Rostomian, Lawrence Berkeley National Laboratory)

  • Image# DE0109
  • DE
  • 11/21/2013

This is the highest energy neutrino ever observed, with an estimated energy of 1.14 PeV. It was detected by the IceCube Neutrino Observatory at the South Pole on January 3, 2012. IceCube physicists named it Ernie. (Courtesy: IceCube Collaboration)

  • Image# DE0110
  • DE
  • 11/21/2013

An aurora australis illuminates the IceCube Lab. The IceCube Laboratory at the Amundsen-Scott South Pole Station, in Antarctica, hosts the computers collecting raw data. Due to satellite bandwidth allocations, the first level of reconstruction and event filtering happens in near real time in this lab. Only events selected as interesting for physics studies are sent to UW–Madison, where they are prepared for used by any member of the IceCube Collaboration. (Courtesy: Keith Vanderlinde, IceCube/NSF)

  • Image# OT0166
  • OT
  • 10/30/2013

Photomultiplier tubes capable of detecting as little as a single photon of light line the top and bottom of the LUX dark matter detector. They will record the position and intensity of collisions between dark matter particles and xenon nuclei. (Courtesy: Matt Kapust, Sanford Underground Research Facility)

  • Image# OT0167
  • OT
  • 10/30/2013

LUX researchers, seen here in a clean room on the surface at the Sanford Lab, work on the interior of the detector, before it is inserted into its titanium cryostat. (Courtesy: Matt Kapust, Sanford Underground Research Facility)

  • Image# OT0168
  • OT
  • 10/30/2013

White Teflon lines the interior of the LUX detector, to better gather faint signals of light that will be recorded by the photomultiplier tubes (center). (Courtesy: Matt Kapust, Sanford Underground Research Facility)

  • Image# OT0169
  • OT
  • 10/30/2013

The LUX dark matter detector suspended in its protective water tank. The detector is a titanium cryostat—that is, a vacuum thermos—that will keep xenon cool enough to remain a liquid, at about minus 150 degrees F. (Courtesy: Matt Kapust, Sanford Underground Research Facility)

  • Image# LB0056
  • LB
  • 08/21/2013

The Daya Bay Neutrino Experiment is designed to provide new understanding of neutrino oscillations that can help answer some of the most mysterious questions about the universe. Shown here are the photomultiplier tubes in the Daya Bay detectors. (Courtesy: Roy Kaltschmidt)

  • Image# LB0057
  • LB
  • 08/21/2013

Daya Bay's detectors are immersed in the large water pools of the muon veto system. (Courtesy: Roy Kaltschmidt)

  • Image# FN0420
  • FN
  • 07/11/2013

At Fermilab's Vertical Magnet Test Facility, the new HQ02a quadrupole achieved all its challenging objectives. (Courtesy: Guram Chlachidze, Fermilab)

  • Image# FN0418
  • FN
  • 06/12/2013

Crews work to attach the red stabilizing apparatus to the Muon g-2 rings at Brookhaven National Laboratory in New York in preparation for moving them over land and sea to Fermi National Accelerator Laboratory in Illinois. (Courtesy: Brookhaven National Laboratory)

  • Image# FN0413
  • FN
  • 05/02/2013

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)

  • Image# OT0159
  • OT
  • 04/23/2013

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)

  • Image# OT0160
  • OT
  • 04/23/2013

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)

  • Image# FN0412
  • FN
  • 03/28/2013

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)

  • Image# CE0336
  • CE
  • 03/26/2013

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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