Many subsequent radiochemical and water Cerenkov detectors confirmed the deficit, including the Sudbury Neutrino Observatory.

Unambiguous detection of solar neutrinos was provided by the Kamiokande-II experiment, a water Cerenkov detector with a low enough energy threshold to detect neutrinos through neutrino-electron elastic scattering.

Muons will be distinguished from other particles in the beam using a combination of the spectrometers and the so-called Particle Identification (PID) detectors, three time of flight scintillators, a Cerenkov detector and an electron-muon calorimeter.

The water Cerenkov detectors only detect neutrinos above about 5MeV, while the radiochemical experiments were sensitive to lower energy (0.8MeV for chlorine, 0.2MeV for gallium), and this turned out to be the source of the difference in the observed neutrino rates at the two types of experiments.

No clear consensus was reached on the choice of technology for particle identification, therefore two octants were equipped with dE/dx ionization chambers, two octants were equipped with high pressure gas Cerenkov detectors, and four octants were equipped with low pressure gas Cerenkov detectors.

A number of Cherenkov detector geometries have been used.

Using the light direction are differential Cherenkov detectors.

"I'd say we look at the ring-imaging Cherenkov detector," Alicia said to them all.

Instruments like the Cherenkov detector were first used on Skyhook balloons.

In a Cherenkov detector, a large volume of clear material such as water or ice is surrounded by light-sensitive photomultiplier tubes.

"Ring-imaging" Cherenkov detectors take advantage of a phenomenon called Cherenkov light.

Most Cherenkov detectors aim at recording the Cherenkov light produced by a primary charged particle.

Surface detectors typically use Cherenkov detectors or Scintillation counters to detect the charged secondary particles at ground level.

The water Cherenkov detector array is one of two cosmic ray detection systems used by the currently operating Pierre Auger Observatory.

The most advanced type of a detector is the RICH, or ring imaging Cherenkov detector, developed in the 1980s.

The instrumentation was also similar, including scintillation counters, geiger counters, a magnetometer, Cherenkov detectors, and micrometeorite detectors.

The RICH-1 detector (Ring imaging Cherenkov detector) is located directly after the vertex detector.

RICH (Ring Imaging Cherenkov Detector)

The Cherenkov detectors use three large photomultiplier tubes to detect the Cherenkov radiation produced by high-energy particles passing through water in the tank.

Traditional Cherenkov detectors usually cost hundreds of thousands of dollars (USD), while Wilson invented a working detector that cost a few hundred dollars.

The IceTop array is a series of Cherenkov detectors on the surface of the glacier, two detectors approximately above each IceCube string.

Surrounding the stainless steel vessel is a 3.2 kiloton cylindrical water Cherenkov detector, which acts as a muon veto counter and provides shielding from cosmic rays and radioactivity in the rock.

Eponymously, it was dubbed the Cherenkov effect, as was the Cherenkov detector, which has become a standard piece of equipment in atomic research for observing the existence and velocity of high-speed particles.

The success of Kamiokande, through Totsuka's leadership, led to the funding of a substantially larger water Cherenkov detector in 1991, the storied Super-Kamiokande (Super-K) detector, which is still an active international collaboration.

It is a design of a ring imaging Cherenkov detector where Cherenkov light that is contained by total internal reflection inside the solid radiator has its angular information preserved until it reaches the light sensors at the detector perimeter.

Specifically, in 1954, John Linsley used a cloud chamber triggered by a cherenkov detector to study the charge distribution of heavy nuclei, and in 1955, Frank McDonald used one triggered by a scintillation counter for a similar purpose.

Many subsequent radiochemical and water Cherenkov detectors confirmed the deficit, but neutrino oscillation was not conclusively identified as the source of the deficit until the Sudbury Neutrino Observatory provided clear evidence of neutrino flavor change in 2001.

The Haverah Park experiment was a cosmic ray air shower detection array consisting of water Cherenkov detectors distributed over an area of 12 kmon Haverah Park on the Pennine moorland near Harrogate, North Yorkshire.

The same year, McDonald combined the scintillation counter of his thesis with a cherenkov detector into a balloon instrument that not only provided a novel measurement of the energy spectrum of primary cosmic ray helium nuclei, but also served as a prototype for devices carried on many spacecraft.