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A neutrino interaction with the electrons or nuclei of water can produce an electron or positron that moves faster than the speed of light in water not to be confused with exceeding the speed of light in a vacuum.

This creates a cone of Cherenkov radiation light, which is the optical equivalent to a sonic boom. The Cherenkov light is recorded by the photomultiplier tube.

Using the information recorded by each tube, the direction and "flavor" type of the incoming neutrino is determined. It consists of a cylindrical stainless steel tank that is The tank volume is divided by a stainless steel superstructure into an inner detector ID region, which is There is a Tyvek and blacksheet barrier attached to the superstructure that optically separates the ID and OD.

A neutrino interaction with the electrons or nuclei of water can produce a charged particle that moves faster than the speed of light in water not to be confused with exceeding the speed of light in a vacuum.

This creates a cone of light known as Cherenkov radiation , which is the optical equivalent to a sonic boom.

The Cherenkov light is projected as a ring on the wall of the detector and recorded by the PMTs. Using the timing and charge information recorded by each PMT, the interaction vertex, ring direction and flavor of the incoming neutrino is determined.

From the sharpness of the edge of the ring the type of particle can be inferred. The multiple scattering of electrons is large, so electromagnetic showers produce fuzzy rings.

Highly relativistic muons , in contrast, travel almost straight through the detector and produce rings with sharp edges.

Construction of the predecessor of the present Kamioka Observatory , the Institute for Cosmic Ray Research , University of Tokyo began in and was completed in April, The purpose of the observatory was to detect whether proton decay exists, one of the most fundamental questions of elementary particle physics.

The detector was upgraded, starting in , to allow it to observe solar neutrinos. The ability of the Kamiokande experiment to observe the direction of electrons produced in solar neutrino interactions allowed experimenters to directly demonstrate for the first time that the sun was a source of neutrinos.

Despite successes in neutrino astronomy and neutrino astrophysics, Kamiokande did not achieve its primary goal, the detection of proton decay.

Higher sensitivity was also necessary to obtain high statistical confidence in its results. This led to the construction of Super-Kamiokande, with fifteen times the water and ten times as many PMTs as Kamiokande.

Super-Kamiokande started operation in The Super-Kamiokande Collaboration announced the first evidence of neutrino oscillation in The detector was partially restored by redistributing the photomultiplier tubes which did not implode, and by adding protective acrylic shells that are hoped will prevent another chain reaction from recurring Super-Kamiokande-II.

In July , preparations began to restore the detector to its original form by reinstalling about 6, PMTs. This phase of the experiment collected data from October till August At that time, significant upgrades were made to the electronics.

After the upgrade, the new phase of the experiment has been referred to as Super-Kamiokande-IV. The Super-Kamiokande SK is a Cherenkov detector used to study neutrinos from different sources including the Sun, supernovae, the atmosphere, and accelerators.

It is also used to search for proton decay. The experiment began in April and was shut down for maintenance in July , a period known as "SK-I".

Since an accident occurred during maintenance, the experiment resumed in October with only half of its original number of ID-PMTs.

In order to prevent further accidents, all of the ID-PMTs were covered by fiber-reinforced plastic with acrylic front windows. In July , the experiment resumed with the full number of PMTs and stopped in September for electronics upgrades.

The period after is known as "SK-IV". The phases and their main characteristics are summarised in table 1.

Charge-to-analog converters QAC and time-to-analog converters TAC are contained in these modules that had dynamic range from 0 to picocoulombs pC with 0.

For each range, analog to digital conversion is conducted separately, but the only range used is that with the highest resolution that is not being saturated.

The overall charge dynamic range of the QTC is 0. The charge and timing resolution of the QBEE at the single photoelectron level is 0.

PMTs used in SK. The QBEE achieves good charge linearity over a wide dynamic range. This threshold was chosen to replicate the behavior of the detector during its previous ATM-based phases.

The outer shell of the water tank is a cylindrical stainless-steel tank 39 m in diameter and 42 m in height. The tank is self-supporting, with concrete backfilled against the rough-hewn stone walls to counteract water pressure when the tank is filled.

The capacity of the tank exceeds 50 ktons of water. Supermodule frames are 2. These frames are connected to each other in both the vertical and horizontal directions.

Then the whole support structure is connected to the bottom of the tank and to the top structure. In addition to serving as rigid structural elements, supermodules simplified the initial assembly of the ID.

Each supermodule was assembled on the tank floor and then hoisted into its final position. Thus the ID is in effect tiled with supermodules.

The support structure for the bottom PMTs is attached to the bottom of the stainless-steel tank by one vertical beam per supermodule frame.

The support structure for the top of the tank is also used as the support structure for the top PMTs. Cables from each group of 3 PMTs are bundled together.

All cables run up the outer surface of the PMT support structure, i. The thickness of the OD varies slightly, but is on average about 2.

OD PMTs were distributed with on the top layer, on the bottom, and on the barrel wall. To protect against low energy background from radon decay products in the air, the roof of the cavity and the access tunnels were sealed with a coating called Mineguard.

Mineguard is a spray-applied polyurethane membrane developed for use as a rock support system and radon gas barrier in the mining industry.

This presents a problem for the large and very sensitive PMTs which prefer a much lower ambient field. The strength and uniform direction of the geomagnetic field could systematically bias photoelectron trajectories and timing in the PMTs.

To counteract this 26 sets of horizontal and vertical Helmholtz coils are arranged around the inner surfaces of the tank.

With these in operation the average field in the detector is reduced to about 50 mG. The magnetic field at various PMT locations were measured before the tank was filled with water.

A standard fiducial volume of approximately It provides shift operators with a flexible tool for selecting event display features, makes online and recent-history histograms to monitor detector performance, and performs a variety of additional tasks needed to efficiently monitor status and diagnose detector and DAQ problems.

Events in the data stream can be skimmed off and elementary analysis tools can be applied to check data quality during calibrations or after changes in hardware or online software.

To detect and identify such bursts as efficiently and promptly as possible Super-Kamiokande is equipped with an online supernova monitor system.

About 10, total events are expected in Super-Kamiokande for a supernova explosion at the center of our Galaxy. Super-Kamiokande can measure a burst with no dead-time, up to 30, events within the first second of a burst.

Theoretical calculations of supernova explosions suggest that neutrinos are emitted over a total time-scale of tens of seconds with about a half of them emitted during the first one or two seconds.

The Super-K will search for event clusters in specified time windows of 0. These thresholds were determined by extrapolation from SNA data.

If the burst candidate passes these checks, the data will be reanalyzed using an offline process and a final decision will be made within a few hours.

During the Super-Kamiokande I running, this never occurred. One of the important capabilities for [Super-Kamiokande] is to reconstruct the direction to supernova.

When any deviation from norms is detected, it will alert physicists to prompt to investigate, take appropriate action, or notify experts.

To monitor and control the offline processes that analyze and transfer data, a set of software was sophisticatedly developed.

This monitor allows non-expert shift physicists to identify and repair common problems to minimize down time, and the software package was a significant contribution to the smooth operation of the experiment and its overall high lifetime efficiency for data taking.

The energy of Sun comes from the nuclear fusion in its core where a helium atom and an electron neutrino are generated by 4 protons.

These neutrinos emitted from this reaction are called solar neutrinos. Photons, created by the nuclear fusion in the center of the Sun, take millions of years to reach the surface; on the other hand, solar neutrinos arrive at the earth in eight minutes due to their lack of interactions with matter.

Hence, solar neutrinos make it possible for us to observe the inner Sun in "real-time" that takes millions of years for visible light. In , the Super-Kamiokande detected strong evidence of neutrino oscillation that successfully explained the solar neutrino problem.

The Super-Kamiokande detector is a 50, ton tank of water, located approximately 1 km underground.

The water in the tank acts as both the target for neutrinos, and the detecting medium for the by-products of neutrino interactions.

The inside surface of the tank is lined with 11, cm diameter light collectors called "photo-multiplier tubes". In addition to the inner detector, which is used for physics studies, an additional layer of water called the outer detector is also instrumented light sensors to detect any charged particles entering the central volume, and to shield it by absorbing any neutrons produced in the nearby rock.

In addition to the light collectors and water, a forest of electronics, computers, calibration devices, and water purification equipment is installed in or near the detector cavity.

A view from inside the Super-Kamiokande tank during filling Below: Illustration of the conical geometry of Cherenkov radiation.

To detect the high-energy particles which result from neutrino interactions, Super-Kamiokande exploits a phenomenon known as Cherenkov radiation. Bluish Cherenkov light is transmitted through the highly-pure water of the tank, and eventually falls on the inner wall of the detector, which is covered with photo-multiplier tubes PMT's.

These PMT's are each sensitive to illumination by a single photon of light - a light level approximately the same as the light visible on Earth from a candle at the distance of the moon!

Each PMT measures the total amount of light reaching it, as well as the time of arrival. These measurements are used to reconstruct energy and starting position, respectively, of any particles passing through the water.

Equally important, the array of over 11, PMTs samples the projection of the distinctive ring pattern, which can be used to determine the direction of a particle.

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Construction of the predecessor of the present Kamioka Observatory , the Institute for Cosmic Ray Research , University of Tokyo began in and was completed in April, The purpose of the observatory was to detect whether proton decay exists, one of the most fundamental questions of elementary particle physics.

The detector was upgraded, starting in , to allow it to observe solar neutrinos. The ability of the Kamiokande experiment to observe the direction of electrons produced in solar neutrino interactions allowed experimenters to directly demonstrate for the first time that the sun was a source of neutrinos.

Despite successes in neutrino astronomy and neutrino astrophysics, Kamiokande did not achieve its primary goal, the detection of proton decay.

Higher sensitivity was also necessary to obtain high statistical confidence in its results. This led to the construction of Super-Kamiokande, with fifteen times the water and ten times as many PMTs as Kamiokande.

Super-Kamiokande started operation in The Super-Kamiokande Collaboration announced the first evidence of neutrino oscillation in The detector was partially restored by redistributing the photomultiplier tubes which did not implode, and by adding protective acrylic shells that are hoped will prevent another chain reaction from recurring Super-Kamiokande-II.

In July , preparations began to restore the detector to its original form by reinstalling about 6, PMTs. This phase of the experiment collected data from October till August At that time, significant upgrades were made to the electronics.

After the upgrade, the new phase of the experiment has been referred to as Super-Kamiokande-IV.

The Super-Kamiokande SK is a Cherenkov detector used to study neutrinos from different sources including the Sun, supernovae, the atmosphere, and accelerators.

It is also used to search for proton decay. The experiment began in April and was shut down for maintenance in July , a period known as "SK-I".

Since an accident occurred during maintenance, the experiment resumed in October with only half of its original number of ID-PMTs. In order to prevent further accidents, all of the ID-PMTs were covered by fiber-reinforced plastic with acrylic front windows.

In July , the experiment resumed with the full number of PMTs and stopped in September for electronics upgrades.

The period after is known as "SK-IV". The phases and their main characteristics are summarised in table 1. Charge-to-analog converters QAC and time-to-analog converters TAC are contained in these modules that had dynamic range from 0 to picocoulombs pC with 0.

For each range, analog to digital conversion is conducted separately, but the only range used is that with the highest resolution that is not being saturated.

The overall charge dynamic range of the QTC is 0. The charge and timing resolution of the QBEE at the single photoelectron level is 0. PMTs used in SK.

The QBEE achieves good charge linearity over a wide dynamic range. This threshold was chosen to replicate the behavior of the detector during its previous ATM-based phases.

The outer shell of the water tank is a cylindrical stainless-steel tank 39 m in diameter and 42 m in height.

The tank is self-supporting, with concrete backfilled against the rough-hewn stone walls to counteract water pressure when the tank is filled.

The capacity of the tank exceeds 50 ktons of water. Supermodule frames are 2. These frames are connected to each other in both the vertical and horizontal directions.

Then the whole support structure is connected to the bottom of the tank and to the top structure. In addition to serving as rigid structural elements, supermodules simplified the initial assembly of the ID.

Each supermodule was assembled on the tank floor and then hoisted into its final position. Thus the ID is in effect tiled with supermodules.

The support structure for the bottom PMTs is attached to the bottom of the stainless-steel tank by one vertical beam per supermodule frame.

The support structure for the top of the tank is also used as the support structure for the top PMTs. Cables from each group of 3 PMTs are bundled together.

All cables run up the outer surface of the PMT support structure, i. The thickness of the OD varies slightly, but is on average about 2.

OD PMTs were distributed with on the top layer, on the bottom, and on the barrel wall. To protect against low energy background from radon decay products in the air, the roof of the cavity and the access tunnels were sealed with a coating called Mineguard.

Mineguard is a spray-applied polyurethane membrane developed for use as a rock support system and radon gas barrier in the mining industry.

This presents a problem for the large and very sensitive PMTs which prefer a much lower ambient field.

The strength and uniform direction of the geomagnetic field could systematically bias photoelectron trajectories and timing in the PMTs. To counteract this 26 sets of horizontal and vertical Helmholtz coils are arranged around the inner surfaces of the tank.

With these in operation the average field in the detector is reduced to about 50 mG. The magnetic field at various PMT locations were measured before the tank was filled with water.

A standard fiducial volume of approximately It provides shift operators with a flexible tool for selecting event display features, makes online and recent-history histograms to monitor detector performance, and performs a variety of additional tasks needed to efficiently monitor status and diagnose detector and DAQ problems.

Events in the data stream can be skimmed off and elementary analysis tools can be applied to check data quality during calibrations or after changes in hardware or online software.

To detect and identify such bursts as efficiently and promptly as possible Super-Kamiokande is equipped with an online supernova monitor system.

About 10, total events are expected in Super-Kamiokande for a supernova explosion at the center of our Galaxy. Super-Kamiokande can measure a burst with no dead-time, up to 30, events within the first second of a burst.

Theoretical calculations of supernova explosions suggest that neutrinos are emitted over a total time-scale of tens of seconds with about a half of them emitted during the first one or two seconds.

The Super-K will search for event clusters in specified time windows of 0. These thresholds were determined by extrapolation from SNA data.

If the burst candidate passes these checks, the data will be reanalyzed using an offline process and a final decision will be made within a few hours.

During the Super-Kamiokande I running, this never occurred. One of the important capabilities for [Super-Kamiokande] is to reconstruct the direction to supernova.

When any deviation from norms is detected, it will alert physicists to prompt to investigate, take appropriate action, or notify experts.

To monitor and control the offline processes that analyze and transfer data, a set of software was sophisticatedly developed. This monitor allows non-expert shift physicists to identify and repair common problems to minimize down time, and the software package was a significant contribution to the smooth operation of the experiment and its overall high lifetime efficiency for data taking.

The energy of Sun comes from the nuclear fusion in its core where a helium atom and an electron neutrino are generated by 4 protons. These neutrinos emitted from this reaction are called solar neutrinos.

Photons, created by the nuclear fusion in the center of the Sun, take millions of years to reach the surface; on the other hand, solar neutrinos arrive at the earth in eight minutes due to their lack of interactions with matter.

Hence, solar neutrinos make it possible for us to observe the inner Sun in "real-time" that takes millions of years for visible light.

In , the Super-Kamiokande detected strong evidence of neutrino oscillation that successfully explained the solar neutrino problem.

Consequently, stars are a source of neutrinos, including our Sun. These neutrinos primarily come through the pp-chain in lower masses, and for cooler stars, primarily through CNO-chains of heavier masses.

In the early s, particularly with the uncertainties that accompanied the initial results from Kamioka II and the Ga experiments, no individual experiment required a non-astrophysical solution of the solar neutrino problem.

But in aggregate, the Cl, Kamioka II, and Ga experiments indicated a pattern of neutrino fluxes that was not compatible with any adjustment of the SSM.

This in turn helped motivate a new generation of spectacularly capable active detectors. Super-Kamiokande was able to detect elastic scattering ES events.

Atmospheric neutrinos are secondary cosmic rays produced by the decay of particles resulting from interactions of primary cosmic rays mostly protons with Earth atmosphere.

The observed atmospheric neutrino events fall into four categories. Fully contained FC events have all their tracks in the inner detector, while partially contained PC events have escaping tracks from the inner detector.

Upward through-going muons UTM are produced in the rock beneath the detector and go through the inner detector.

Upward stopping muons USM are also produced in the rock beneath the detector, but stop in the inner detector. The number of observed number of neutrinos is predicted uniformly regardless of the zenith angle.

However, Super-Kamiokande found that the number of upward going muon neutrinos generated on the other side of the Earth is half of the number of downward going muon neutrinos in This can be explained by the neutrinos changing or oscillating into some other neutrinos that are not detected.

In addition to the light collectors and water, a forest of electronics, computers, calibration devices, and water purification equipment is installed in or near the detector cavity.

A view from inside the Super-Kamiokande tank during filling Below: Illustration of the conical geometry of Cherenkov radiation. To detect the high-energy particles which result from neutrino interactions, Super-Kamiokande exploits a phenomenon known as Cherenkov radiation.

Bluish Cherenkov light is transmitted through the highly-pure water of the tank, and eventually falls on the inner wall of the detector, which is covered with photo-multiplier tubes PMT's.

These PMT's are each sensitive to illumination by a single photon of light - a light level approximately the same as the light visible on Earth from a candle at the distance of the moon!

Each PMT measures the total amount of light reaching it, as well as the time of arrival. These measurements are used to reconstruct energy and starting position, respectively, of any particles passing through the water.

Equally important, the array of over 11, PMTs samples the projection of the distinctive ring pattern, which can be used to determine the direction of a particle.

Finally, the details of the ring pattern - most notably whether it has the sharp edges characteristic of a muon, or the fuzzy, blurred edges characteristic of an electron, can be used to reliably distinguish muon-neutrino and electron-neutrino interactions.

Neutrino Interactions Since neutrinos themselves cannot be directly detected, Super-Kamiokande detects the by-products of their interactions inside the water volume of the detector and the nearby rock outside.

Two sources of neutrinos are available for our studies. Neutrinos are produced in the atmosphere above Super-Kamiokande, and everyplace else on Earth.

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