Scientists trace a cosmic neutrino by reconstructing where it came from, then testing whether that direction and arrival time match a plausible source better than expected from background events. A match can be strong evidence, especially when other observatories see the source active, but it is not a picture of the object emitting that individual neutrino.
From a rare interaction to a point on the sky
Neutrinos rarely interact with matter, so a detector cannot simply photograph one in flight. IceCube identifies candidate neutrinos from the light produced when they interact in or near the Antarctic ice instrumented with light sensors. Researchers reconstruct the event from that light, estimating its direction and other properties.
The direction is an estimate, not an exact address. Event topology and reconstruction method affect how precisely an arrival direction can be determined; track-like events can be especially useful for locating a source. That is why a single angular-precision figure should not be treated as applying to every event. The IceCube data release for the TXS 0506+056 analysis includes event times, reconstructed right ascension and declination, angular uncertainty, and an energy proxy. IceCube cautions that the proxies are approximate, not individual measurements of each neutrino’s energy. IceCube’s data release explains the fields and analysis.
How an arrival direction becomes a source hypothesis
Analysts compare reconstructed directions with known or cataloged objects. A useful correlation analysis can account for each event’s directional uncertainty, the likelihood that it is astrophysical rather than background, and the candidate source’s brightness. The aim is not merely to find an object near a plotted point: it is to ask whether the pattern of events is more consistent with the source hypothesis than with background.
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Timing can strengthen the case. If a candidate object is flaring when a neutrino arrives, that coincidence gives researchers another relationship to test. Follow-up observations in gamma rays, X-rays, optical light, or radio can show whether the source was active and help characterize what was happening there. Those observations add context; they do not reveal the neutrino’s path or directly show which object emitted it. IceCube’s explanation of searches involving active galaxies and blazars describes why event and source properties matter.
A directional alert is therefore a prompt to investigate a region, not a confirmed identification. The strength of any association depends on the event reconstruction, timing, background expectations, source activity, and the statistical test researchers defined.
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TXS 0506+056: two pieces of evidence, from different periods
The 2017 alert and multiwavelength follow-up
On September 22, 2017, IceCube detected a high-energy neutrino from a direction coincident with the blazar TXS 0506+056. NASA described the event’s energy as about 300 trillion electron volts. An automated notice enabled observatories to follow up, and Fermi observations found enhanced gamma-ray emission from the active galaxy around the time of the neutrino. The directional and temporal coincidence, together with observations across the electromagnetic spectrum, supported an association between the event and the blazar; it was not a direct image of the neutrino’s origin. NASA’s account of the 2017 event and follow-up describes that sequence.
The earlier 2014–2015 excess
IceCube also searched 9.5 years of data for events from the blazar’s direction and found an excess between September 2014 and March 2015. The collaboration reported this as 3.5 sigma evidence for neutrino emission. This was a separate archival result, independent of and earlier than the 2017 flare. IceCube’s announcement and its associated data release describe the analysis.
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“3.5 sigma” is the result of a statistical analysis under its assumptions; it is not a plain-language guarantee that the interpretation is certain. It should be read in the context of the search that produced it, not as a universal confidence label that can be compared casually with every other result.
Why different neutrino searches can give different answers
A time-dependent flare search asks whether events cluster during a particular active period. A steady-source search instead looks for emission that persists over a longer interval. Catalog searches test a defined group of possible sources. Because the questions differ, their results are not interchangeable. When comparing analyses, check:
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- Event class and reconstruction: which events were selected and how their directions were estimated.
- Time assumption: whether the search targets a flare or persistent emission.
- Data and processing: the sample dates, event selection, and analysis version.
- Background treatment: how the analysis evaluates the chance that events are unrelated background and the probability that they are astrophysical.
- Candidate definition: which catalog or source population was tested.
- Statistical result: the reported significance and the particular analysis it describes.
For example, NASA’s description of IceCube’s 10-year point-source sample covers events detected from April 2008 through July 2018. In a catalog of 110 potential sources, the combined analysis reported a 3.3 sigma cumulative excess, driven primarily by NGC 1068, TXS 0506+056, PKS 1424+240, and GB6 J1542+6129. That is a catalog-level result, not four individually confirmed detections. The dataset notes that later processing updates can change source significances. NASA’s dataset description gives the sample and catalog context.
Independent reader supportYour contribution helps us test, update, and keep practical guides available for everyone.What the evidence says about other sources—and what it does not
IceCube has reported evidence of high-energy neutrino emission from the active galaxy NGC 1068. The collaboration’s result is an important step in identifying sources, but it does not settle the origin of the entire cosmic neutrino flux. IceCube’s NGC 1068 announcement presents the finding as evidence of emission. The collaboration has also noted that steady point sources remain unresolved in broader searches; some source populations may be hard to reveal with available samples, and gamma rays can be absorbed near their production sites or during their journey to Earth. IceCube’s discussion of unresolved steady sources explains that limitation.
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There is no single, uniform source ranking established by these results. A reported significance belongs to a specific dataset, selection, catalog, and statistical method; a new processing version or a different search question can change the comparison. The careful conclusion is that multiple observations support progress in neutrino astronomy, while the source population and the contribution of individual objects remain open questions.
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