How big would a neutrino telescope have to be?

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Discussion Overview

The discussion centers around the size requirements for a neutrino telescope capable of observing the Cosmic Neutrino Background from the Big Bang, with comparisons to existing detectors like IceCube and considerations of detection sensitivity and resolution.

Discussion Character

  • Exploratory
  • Technical explanation
  • Debate/contested

Main Points Raised

  • One participant notes that the IceCube neutrino detector has detected about 28 neutrinos from outside the solar system, suggesting that its resolution is limited.
  • Another participant argues that the neutrino spectrum is challenging to translate into optical resolution, indicating that time may be a more critical factor than aperture size for neutrino detection.
  • A different participant questions the concept of "resolution," explaining that energy resolution depends on the spectral resolution of detectors, while spatial resolution relates to the ability to reconstruct neutrino paths based on Cherenkov light.
  • This participant also clarifies that increasing the size of the detector enhances detection probability rather than resolution, suggesting a potential misunderstanding between detection sensitivity and resolution.
  • One participant points out that neutrino cross-sections are highly energy-dependent, with IceCube focusing on high-energy neutrinos, while the cosmic neutrino background is expected to be at much lower energy levels.
  • Another participant proposes that for optimal look-back times, pulsar timing arrays may be a more effective method for detecting gravitational waves from the inflation period.

Areas of Agreement / Disagreement

Participants express differing views on the relationship between detector size, resolution, and detection sensitivity. There is no consensus on the optimal size for a neutrino telescope or the best method for observing the Cosmic Neutrino Background.

Contextual Notes

Participants highlight limitations related to energy dependence of neutrino cross-sections and the challenges in translating neutrino detection into optical terms. The discussion also reflects varying interpretations of resolution and detection sensitivity.

CosmicVoyager
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Greetings,

The IceCube neutrino detector array in the antartic is a cubic kilometer and has deceted about 28 neutrinos from outside the solar system. So the resolution is almost nothing.

I am wondering how large a detector array would have to be to serve as a telescope to observe what I am calling the Cosmic Neutrino Background from the big bang so we could see farther back than we can observing the Cosmic Microwave Background.

Thanks
 
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The neutrino spectrum is difficult to convert into an equivalent optical resolution. It's probably more a case of time than aperture. Neutrino's are more difficult to collect than photons.
 
CosmicVoyager said:
Greetings,

The IceCube neutrino detector array in the antartic is a cubic kilometer and has deceted about 28 neutrinos from outside the solar system. So the resolution is almost nothing.

I am wondering how large a detector array would have to be to serve as a telescope to observe what I am calling the Cosmic Neutrino Background from the big bang so we could see farther back than we can observing the Cosmic Microwave Background.

Thanks

I don't understand this. What "resolution" are you referring to?

The energy resolution depends on the spectral resolution of the detectors. The spatial resolution depends on how well one can reconstruct the path of the neutrino based on the Cherenkov light. The more and smaller the detectors you can surround the ice, the higher the spatial resolution you can detect. The size of the ice isn't the issue, the same way the size of the water tank used in many of these detection isn't an issue as far as resolution is concerned.

The size, however, will increase the detection probability. Maybe you are confusing detection sensitivity with resolution.

Zz.
 
Neutrino cross-sections are extremely energy dependent. IceCube succeeds because it looks for high-energy neutrinos, TeV or greater. The cosmic neutrino background is expected to be about 2 Kelvins, in the micro-eV range.
 
If you want unbeatable look-back times you got to go for pulsar timing arrays, they should be able to directly detect gravitational waves from around inflation.
 

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