Adam Para, Fermilab, December 10, 2009 Non-Standard Neutrino Interactions Workshop Madrid 1.
Adam Para 1. Or rather Stories about neutrino detection.
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Transcript of Adam Para 1. Or rather Stories about neutrino detection.
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NEUTRINO DETECTORSAdam 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 thoughtfulMany of them are quite completeMany of them are unbiasedMany 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 GeologyAstronomyDirac/Majorana
Oscillation/sterile neutrinos
Magnetic moments Cosmology
Reactor EarthSolarAtmos-pheric
AcceleratorRadioactive sources
Astro-objects
Relic-neutrino
Liquid scintillator
Semiconductorcrystals gaseousscintillator
EmulsionNuclear 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!= 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. Ray31
•CC: e, μ + 12Cgs (e-, μ-) + 12Ngs
•CC: e, μ + 12Cgs (e-, μ-) + 12N*
•CC: anti-e + p e+ + n
neutron thermalizationmean time = 200 s
two 0.511 MeV photons
one 2.2 MeV photon
happens so quickly you only see 1 light flash!
- e + 12C e- + 12Ngs
- 12Ngs 12C + e+ + e
- 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 showerMuon identificationConfusion 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
1 mm
interface films (CS)
ECC brick
electronictrackers
• 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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