NEUTRINO DETECTORS 1 ART AND SCIENCE OF NEUTRINO DETECTORS Or - - PowerPoint PPT Presentation

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NEUTRINO DETECTORS 1 ART AND SCIENCE OF NEUTRINO DETECTORS Or - - PowerPoint PPT Presentation

Jan 20, 2023 169 likes •902 views

Adam Para NEUTRINO DETECTORS 1 ART AND SCIENCE OF NEUTRINO DETECTORS Or rather Stories about neutrino detection Lecturing in XXI Century Many of these talks/lectures are very thoughtful Many of them are quite complete Many of them are

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NEUTRINO DETECTORS

Adam Para

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ART AND SCIENCE OF NEUTRINO DETECTORS

Or rather Stories about neutrino detection

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Lecturing in XXI Century

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Many of these talks/lectures are very thoughtful Many of them are quite complete Many of them are unbiased Many of them are very interesting and inspiring I have borrowed most of my materials from some of them

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An intricate Web of Neutrino Physics and Experiments

Mass Geology Astronomy Dirac/ Majorana Oscillation /sterile neutrinos Magnetic moments Cosmology

Reactor Earth Solar Atmos- pheric

Accelerator

Radioactive

sources

Astro-

  • bjects

Relic- neutrino Liquid scintillator Semiconductor crystals gaseous scintillator Emulsion Nuclear chemistry Water Cerenkov Sampling detector Liquid Argon

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Neutrino industry

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Neutrino Experiments: A Confluence of Multiple Disciplines

  • High Energy Physics
  • Nuclear Physics
  • Radiochemistry
  • Chemistry
  • Computing
  • Electrical Engineering
  • Structural Engineering
  • Civil Engineering
  • Optics
  • Photonics
  • Geophysics
  • Mining
  • Nuclear Power Engineering
  • Safety
  • Cryogenics
  • Material Science
  • Quality Control
  • Helioseismology

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Theory of Neutrino Experiment According to Boris Kayser

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Theory of Neutrino Experiment According to Boris Kayser – An Example

John Bahcall Ray Davies

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How the Sun Burns ?

  • The Sun emits light because nuclear fusion produces a lot of

energy

John Bahcall

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25 years of ‘Solar Neutrino Anomaly ‘ – an Amazing Story of Professional Persistence

  • Calculated the expected

rate of events related to a minute (~10-4) fraction of the solar neutrino flux

  • 600 tons of a washing

powder solution

  • 15 unstable atoms produced

per month (t=34 days)

  • Atoms extracted and

counted with known efficiency

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  • Experimental results and theoretical calculations

agree within a factor of three: given the complexity of a problem a huge success for mere mortals

  • Unbelievable confidence in the correctness of the

prediction and the understanding of the experiment: trademark of highest level of science

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Evolving Physics of/with Neutrinos

  • Do neutrinos exist?
  • How many different kinds?
  • Theory of weak interactions? V-A? Neutral currents?
  • Neutrinos as a probe of a nucleon structure and the theory of

strong interactions

  • Precision tests of the Standard Model
  • How many families? Does the nt really exist?
  • Neutrino properties? Masses? Mixing? Magnetic moment?
  • Nature of neutrinos? Dirac vs Majorana?
  • Neutrinos as a probe of astrophysical objects: supernovae
  • Neutrinos as a probe of the Earth interior
  • Neutrinos as a probe of physics beyond the standard model

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Neutrino Experiments

  • Neutrino source (man-made or natural)
  • Neutrino flux (measure, monitor, calculate)
  • Neutrino detector

All these elements are quite specific to the physics problem in question. Examples of dual/triple purpose experiments are exceptions rather than a rule.

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Neutrino Experiments: What do we Want to Measure?

  • Counting neutrino interactions (== cross section)
  • Identify the flavor (CC reactions)
  • Identify the interaction (NC, CC)
  • Measure the parent neutrino energy/spectrum
  • Details of the final state (inclusive, exclusive)

Depending on the physics requirements AND the neutrino source AND the neutrino energy range the detectors are completely different. Not to mention dedicated experiments for neutrino mass measurement and double beta decay experiments.

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PRODUCING NEUTRINOS

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Comments on Neutrino Beams/Sources

For a precision experiment one needs to know:

  • Neutrino beam composition (neutrino/antineutrino

contamination)

  • Flavor composition (electron neutrino background,

tau neutrino component of the beam)

  • Total flux of neutrinos (measured or calculated,

see the reactor neutrino ‘anomaly’)

  • Energy distribution

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Conventional Neutrino Beam

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Near and Far Detector: Experimental Determination of the Beam Properties

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For a number of reasons the far and near detectors ‘see’ a different energy spectrum of the ‘same’ beam. Both beam spectra are correlated: they come from the same parent hadron beam. Far detector spectrum can be constructed from the event spectrum observed in the near detector.

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Off-axis Neutrino Beams

  • An un-avoidable

consequence of the beam production procedure.

  • With some luck

could provide a highly optimized (intensity and energy spectrum) beam

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Spallation Neutron Source

Target Area - absorbed by target + DAR Mono-Energetic! n= 29.8 MeV E range up to 52.8 MeV

Accelerator based Decay at Rest

  • H. Ray
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DETECTING NEUTRINOS

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Experimenting with Neutrinos (especially lately)

  • Interacting neutrino flavor of primary

importance, charged current reactions a principal detection channel

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Energy Regimes Available for Studies

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Detection and Measurement of Neutrino Interactions

  • E < 100 MeV

 Electron neutrinos and antineutrinos CC only  Neutral currents  Rate  Energy spectra  Electron direction

  • 100 MeV < E < 1 GeV (enter muon neutrinos CC)

 Mostly quasi-elastic interactions, low multiplicity  Neutrino energy from kinematics

  • E>1 GeV (enter, slowly, tau neutrinos CC)

 Increasingly complex final states  Calorimetric measurement of neutrino energy

  • E > 1 TeV: surpisingly clean separation of neutrino flavors

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CC Low Energy Physics

  • H. Ray

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  • CC: ne, μ + 12Cgs  (e-, μ-) + 12Ngs
  • CC: ne, μ + 12Cgs  (e-, μ-) + 12N*
  • CC: anti-ne + p  e+ + n

neutron thermalization mean time = 200 s two 0.511 MeV photons

  • ne 2.2 MeV

photon happens so quickly you only see 1 light flash!

  • ne + 12C  e- + 12Ngs
  • 12Ngs  12C + e+ + ne
  • 11 ms half life
  • n + p  d + 2.2 MeV photon
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Principal Challenges

  • Light yield ( energy resolution)
  • Radiopurity ( low detection thresholds)
  • Gd loading
  • Transparency (light attenuation)
  • Photodetector coverage ( affordable

photodetectors)

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A Buble Chamber: Ultimate Tracking Detector

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A Perfect Experiment: GGM at PS

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A single event a tantalizing hint. Three events a major discovery Precision view of the final state of critical importance.

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Difficult Experiment: Search for NC with GGM at PS

  • Exquisite view of the final

state.

  • Clear interaction of a neutral

particle with no muon or electron in the final state

  • Neutrino or neutron?
  • It is not detector alone which

decides about the quality of the expriement. Beam and environment is an important factor too.

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High Energy Neutrinos Era: Decline of the Bubble Chambers

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Leakage of hadronic shower Muon identification Confusion caused by electromagnetic showers form pi-zeros

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(typical) Detector Requirements

  • Large volume (inexpensive, please)
  • Identify the flavor of the neutrino (i.e. identify

the charged lepton)

  • Measure the total energy of the event (~

estimator of the neutrino energy)

  • Provide some kinematical information about the

event (direction of a hadronic jet)

  • Determine the direction of the incoming neutrino

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Challenges of High Energies

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CDHS(W): magnetized iron- scintillator calorimeter CHARM: marble – drift tubes

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Interactions Classification with Iron-Scintillator Tracking Calorimeter (MINOS)

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The Ultimate Tracking Calorimeter

  • Fully active
  • Good energy resolution
  • Excellent electron identification
  • Good electron-pizero rejection

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Searching for tau neutrinos

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With Nuclear Emulsions

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Exquisite spatial resolution and granularity

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The New Principle

Pb emulsion layers nt t 1 mm interface films (CS) ECC brick electronic trackers

  • Intense, high-energy long baseline muon-neutrino beam
  • Massive active target with micrometric space resolution
  • Detect tau-lepton production and decay
  • Underground location
  • Use electronic detectors to provide “time resolution” to the emulsions and

preselect the interaction region

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…and as seen in emulsion

(Animation)

Proof of the Pudding

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An Alternative Approach: Kinematical Reconstruction

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Very High Granularity Tracking Detector

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ULTRA HIGH ENERGY NEUTRINOS

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Ultimate Heavy Liquid Bubble Chamber: Liquid Argon Detectors

  • ICARUS T600@LNGS
  • ArgoNEUT@FNAL
  • MicroBOONE@FNAL
  • 250L@JPARC
  • LBNE (USA)
  • GLACIER (dual phase) (Europe)
  • Exquisite granularity/tracking resulotion
  • Good hadron energy resolution DE/E ~ 10%

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ICARUS, LNGS beam

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Instead of Summary

  • After all these years of experimentation and R&D we have

developed experimental techniques which allow us most of the conceivable questions regarding neutrinos.

  • However not all the solutions may be affordable.
  • Even affordable solutions may not be available all/many at the

same time. Global collaboration/coordination may be called for.

  • For man-made neutrino beams: physics potential = beam intensity

x detector mass. Careful optimization is necessary.

  • Optimization is considerably more difficult if multi-purpose

facilities are considered.

  • For subtle effects a careful inclusion of systematics: background

and efficiencies, calibrations, etc.. is critical..

  • We live in a golden age of neutrino physics. Let’s convince others

(i.e. funding agencies) about it.

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