< Back to Navigation

Interactions.org - Particle Physics News and Resources

A communication resource from the world's particle physics laboratories

1175 Search Results

Sort By: Image # Lab Date  
  • Image# BN0051
  • BN
  • 04/10/2014

The STAR detector at Brookhaven's Relativistic Heavy Ion Collider (RHIC). As big as a house, STAR searches for signatures of the form of matter that RHIC aims to create: the quark-gluon plasma. Shown here is the central portion of the Heavy Flavor Tracker (HFT) being installed at the STAR detector. The HFT will track particles made of "charm" and "beauty" quarks, rare varieties (or "flavors") that are more massive than the lighter "up" and "down" quarks that make up ordinary matter. The Solenoidal Tracker at RHIC (STAR) is a detector which specializes in tracking the thousands of particles produced by each ion collision at RHIC. Weighing 1,200 tons and as large as a house, STAR is a massive detector. It is used to search for signatures of the form of matter that RHIC was designed to create: the quark-gluon plasma. It is also used to investigate the behavior of matter at high energy densities by making measurements over a large area. (Courtesy: BNL)

  • Image# BN0052
  • BN
  • 04/10/2014

The STAR detector at Brookhaven's Relativistic Heavy Ion Collider (RHIC). As big as a house, STAR searches for signatures of the form of matter that RHIC aims to create: the quark-gluon plasma. (Courtesy: BNL)

  • 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# SL0110
  • SL
  • 03/17/2014

The Dark Sector Lab (DSL), located 3/4 of a mile from the Geographic South Pole, houses the BICEP2 telescope (left) and the South Pole Telescope (right). (Courtesy: Steffen Richter, Harvard University)

  • Image# FN0427
  • FN
  • 02/11/2014

A view of the top of the nearly completed NOvA far detector in northern Minnesota. The detector is made up of 28 PVC blocks, each weighing 417,000 pounds, and spans 51 feet by 51 feet by 200 feet. When it is completed and filled with liquid scintillator, the far detector will weigh 14,000 tons. (Courtesy: NOvA collaboration)

  • 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# BN0047
  • BN
  • 02/03/2014

A welder works on the first superconducting radiofrequency cavity installed at RHIC. Superconductivity allows the cavity to operate at higher voltage than conventional cavities, thus producing a stronger focusing force for ion beams. After commissioning, the cavity should further increase RHIC's collision rates. (Courtesy: BNL)

  • Image# BN0048
  • BN
  • 02/03/2014

At the heart of the PHENIX detector (top), a silicon vertex tracker (green layers behind the "X" shaped black structure in bottom image) surrounds the point where collisions take place. Together with forward silicon vertex trackers at each end of the barrel (one being adjusted by technician Mike Lenz), these components identify and count the decay products of particles made of heavy quarks streaming out of RHIC collisions. (Courtesy: BNL)

  • 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# BN0050
  • BN
  • 02/03/2014

The central portion of the Heavy Flavor Tracker (HFT) being installed at RHIC's STAR detector (top), and the surrounding portion before installation (bottom). The HFT will track particles made of "charm" and "beauty" quarks, rare varieties (or "flavors") that are more massive than the lighter "up" and "down" quarks that make up ordinary matter. (Courtesy: BNL)

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

ASACUSA (Courtesy: Yasunori, Yamakazi)

  • Image# CE0341
  • CE
  • 01/21/2014

A schematic drawing of the Cusp Trap scheme. From left to right: the cusp trap to produce antihydrogen atoms, a microwave cavity (green) to induce hyperfine transitions, a sextupole magnet (red and grey), and an antihydrogen detector (gold). (Crourtesy: Stefan Meyer Institut.)

  • 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# DE0107
  • DE
  • 11/21/2013

The deployment of each of the 86 IceCube strings lasted about 11 hours. In each one, 60 sensors (called DOMs) had to be quickly installed before the ice completely froze around them. (Courtesy: IceCube/NSF)

  • Image# DE0108
  • DE
  • 11/21/2013

The IceCube Lab under the stars. 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: Felipe Pedreros, IceCube/NSF)

  • 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# OT0171
  • OT
  • 11/05/2013

InterAction Collaboration meeting at SLAC, Menlo Park, CA, USA November 2013.

  • 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)

Page 1 of 47

Images from the Interactions.org website may be downloaded, reproduced and published free of charge for use in newspapers, online news sites, educational materials and websites, and other not-for-profit educational outlets. For other uses, please request permission. All the images from the Interactions.org image bank are the property of the contributing organizations. The credit line accompanying each photo must appear, as listed, in the publication.