Atmospheric Neutrinos
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Transcript of Atmospheric Neutrinos
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Atmospheric Neutrinos
Atmospheric neutrino detector at Kolar Gold Field –1965
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Need For A Large Mass Magnetised Detector
• Atmospheric Neutrino Physics now entering a new era.
– From observation of oscillation to precision measurement of parameters.
• A large mass detector with a magnetic field is essential to achieve many of the physics goals.
– Reconfirmation of atmospheric neutrino oscillation through explicit observation of first oscillation swing as a fn. of L/E
– Improved measurement of the oscillation parameters
– Search for potential matter effect and sign of m23
– Discrimination between vs s
– CP violation in neutrino sector
– Probing CPT violation
– Constraining long range leptonic forces
• Need a detector of size 50 to 100 Kton having charge measurement capability
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Disappearance of Vs. L/E
The disappearance probability can be measured with a single detector and two equal sources:
= P( ; L/E) N up(L/E)
N down(L’/E)
= 1 - sin2 (2) sin2 (1.27 m2 L/E)
Expect to measure m2 with 10% precision
Down
Up
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Matter Effect
)(),(cos
),(cos
cos22
ELEPdEd
dLEP
dEd
dddEMNN e
z
e
zzYn
Total no. of charge current events:
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Matter Effect
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Sign of m232
The neutrino and anti-neutrino
up/down event ratios are different from each other as well as different with direct and inverted mass hierarchies.
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vs s
events will give rise to excess of muon less events. There will be excess of upgoing muonless events.
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CPT Violation
L
b
ELP
24sin2sin1)( 3222
bLE
LPPPCPT sin
2sin2sin 322
The expression for survival probability for the case of CPTV 2-flavour oscillations
and
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Choice of Neutrino Source and Detector
• Neutrino Source– Need to cover a large L/E range
• Large L range• Large E range
– Use Atmospheric neutrinos as source : Phase I– Beam from Neutrino factory : Phase II
• Detector Choice• Should have large target mass ( 50-100 KT)• Good tracking and Energy resolution ( Tracking calorimeter)• Good directionality ( <= 1 nsec time resolution )• Ease of construction• Modular with a possibility of phasing
– Use magnetised iron as target mass and RPC as active detector medium
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Current INO related activities
• Detector Development.
• Detector Simulation.
• Physics Studies.
• Data Acquisition System.
• Site Survey.
• International Collaboration.
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INO Detector Concept
INO IRON CALORIMETER
RPC Trays
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Construction of RPC
Two 2 mm thick float GlassSeparated by 2 mm spacer
2 mm thick spacer
Glass plates
Complete RPC Graphite coating on the outer surfaces of glass
Pickup strips
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Test of RPCs
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RPC Efficiency & timing Studies
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Detector and Physics Simulation
• NUANCE Event Generator:– Generate atmospheric neutrino events inside INO detector
• GEANT Monte Carlo Package:– Simulate the detector response for the neutrino event
• Event Reconstruction:– Fits the raw data to extract neutrino energy and direction
• Physics Performance of the baseline INO detector.– Analysis of reconstructed events to extract physics.
These studies are going on at all the collaborating institutes
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Possible INO sites
• PUSHEP (Pykara Ultimate Stage Hydro Electric Project) in South India
or
• RAMMAM Hydro Electric Project Site
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PUSHEP
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Location of Rammam
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Underground Cavern
Width : 22 mHeight : 25 mLength : > 120 m
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Interim Report
Will submit the INO Interim Project ReportTo Indian funding agencies on 1 May, 2005
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Summary
• A large magnetised detector of 50-100 Kton is needed to achieve some of the very exciting physics goals using neutrinos.
• A case for such a detector was highlighted earlier by the Monolith Collaboration.
• Physics case for such a detector is strong as evident from recent publications.
• It will complement the existing and planned water cherenkov detectors.
• Can be used as a far detector during neutrino factory era.
• We have started a very active R & D work towards building such a detector.
• Looking for participation from international neutrino community.
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Ultimate Long Base Line Neutrino Experiment
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Physics withNeutrinos from Beam
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Measure of
232m
13sin
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Sign of 232m