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Clear out junk files and repair common Windows errorsFree Scan →Scan for outdated or missing drivers - takes under a minuteDriver Scan →IceCube detects neutrinos indirectly: it records Cherenkov light from charged particles created when a neutrino interacts in or near the detector. The timing and pattern of that light let scientists reconstruct what happened, including an event’s likely direction and energy. The neutrino itself is not photographed or seen directly.
How the detection process works
- A neutrino passes through the ice. Neutrinos rarely interact with matter, so most travel through Earth without leaving a signal. Occasionally, one interacts in or near IceCube’s instrumented volume and produces charged secondary particles. IceCube’s detector overview and its educational explanation describe this indirect detection method.
- Those particles emit Cherenkov light. A charged particle moving through ice can travel faster than light travels through that same ice. It then emits a faint cone of light called Cherenkov radiation. This does not mean the particle exceeds the speed of light in a vacuum.
- Buried sensors capture the light. IceCube’s digital optical modules (DOMs) detect the photons that reach them. Their electronics digitize and time-stamp the signals, which are sent to computing systems at the surface.
- Scientists reconstruct the event. The locations and arrival times of the recorded light form a pattern. Researchers compare that pattern with models of light production and propagation to estimate the event’s properties, such as its direction and energy.
How IceCube is laid out in the ice
The in-ice detector instruments roughly one cubic kilometer of Antarctic ice. Its 5,160 DOMs are deployed on 86 vertical strings, at depths of approximately 1,450 to 2,450 meters. On standard strings, DOMs are spaced about 17 meters apart; the strings are arranged on an approximately 125-meter grid. The ice serves both as the material in which neutrino interactions can occur and as the medium through which the resulting light travels. These are specifications in IceCube’s current detector overview.
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IceCube also includes IceTop, a surface array above the in-ice detector. It is used for cosmic-ray air-shower measurements and as a veto and calibration detector; it is not the source of the primary in-ice neutrino signal.
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Not every neutrino interaction makes the same shape of light. Two useful broad categories are tracks and cascades. They are event signatures, not images of neutrinos: each is inferred from the light detected by the DOMs.
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| Event signature | What the light looks like | What scientists can infer |
|---|---|---|
| Track | A long, elongated pattern, often associated with a muon traveling through the detector after a neutrino interaction. | The sequence and timing of light along the path help estimate the particle’s direction and energy. |
| Cascade | A more localized shower of secondary particles, producing a roughly spherical or blob-like pattern. | The light pattern and timing support estimates of the event’s direction and energy, though direction reconstruction is challenging. |
Cascades are harder to reconstruct precisely because their light is diffuse, the detector is sparsely instrumented relative to the event volume, and light propagation depends on the optical properties of the South Pole ice. IceCube’s March 6, 2024 account of improved particle-shower models explains why modeling those showers matters for event reconstruction.
How DeepCore reaches lower energies
DeepCore is a denser cluster of eight strings in the lower central part of the array. Its tighter sensor spacing makes it more sensitive to lower-energy events than the widely spaced main array. IceCube gives DeepCore a neutrino threshold of about 10 GeV and identifies it as an instrument for neutrino-oscillation studies. That threshold is a stated detector capability, not a guarantee that every event at that energy will be detected.
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What changed with the IceCube Upgrade
In February 2026, IceCube reported successful deployment of the IceCube Upgrade, which includes two new sensor designs: the multi-PMT digital optical module (mDOM) and D-Egg. The Upgrade is a development of the observatory, distinct from the original array’s 5,160-DOM description. It does not change the basic detection principle: IceCube still looks for light produced by charged particles after neutrino interactions. See the February 2026 deployment announcement.
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