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India-based Neutrino Observatory(INO)
Physics Prospects and Status Report
D. Indumathi
Institute of Mathematical Sciences, Chennai
For the INO Collaboration
(http://www.imsc.res.in/∼ino)
WHEPP 8, IIT Bombay, Jan 8 2004 – p.1/42
Outline of talk
Status report
The INO Collaboration
Motivation: Atmospheric neutrinos and oscillationphysics
Choice of detector/source
The ICAL detectorRPCs, the active detector elementsThe magnet designPhysics Simulation of ICAL
Choice of detector location: Site Survey
WHEPP 8, IIT Bombay, Jan 8 2004 – p.2/42
Outline of talk
Status report
The INO Collaboration
Motivation: Atmospheric neutrinos and oscillationphysics
Choice of detector/source
The ICAL detectorRPCs, the active detector elementsThe magnet designPhysics Simulation of ICAL
Choice of detector location: Site Survey
WHEPP 8, IIT Bombay, Jan 8 2004 – p.2/42
Outline of talk
Status report
The INO Collaboration
Motivation: Atmospheric neutrinos and oscillationphysics
Choice of detector/source
The ICAL detectorRPCs, the active detector elementsThe magnet designPhysics Simulation of ICAL
Choice of detector location: Site Survey
WHEPP 8, IIT Bombay, Jan 8 2004 – p.2/42
Outline of talk
Status report
The INO Collaboration
Motivation: Atmospheric neutrinos and oscillationphysics
Choice of detector/source
The ICAL detectorRPCs, the active detector elementsThe magnet designPhysics Simulation of ICAL
Choice of detector location: Site Survey
WHEPP 8, IIT Bombay, Jan 8 2004 – p.2/42
Outline of talk
Physics Prospects
Atmospheric neutrinos
Oscillation physics with atmospheric neutrinosDetailed analysis at ICAL without magnetic fieldDetailed analysis at ICAL with magnetic field
Neutrino-factory neutrinos
ICAL or upgraded-ICAL as far-end detector fornu-factory
Non-oscillation physics
Ultra high energy cosmic rays, “Kolar events”, . . . ✘
WHEPP 8, IIT Bombay, Jan 8 2004 – p.3/42
Outline of talk
Physics Prospects
Atmospheric neutrinos
Oscillation physics with atmospheric neutrinosDetailed analysis at ICAL without magnetic fieldDetailed analysis at ICAL with magnetic field
Neutrino-factory neutrinos
ICAL or upgraded-ICAL as far-end detector fornu-factory
Non-oscillation physics
Ultra high energy cosmic rays, “Kolar events”, . . . ✘
WHEPP 8, IIT Bombay, Jan 8 2004 – p.3/42
Outline of talk
Physics Prospects
Atmospheric neutrinos
Oscillation physics with atmospheric neutrinosDetailed analysis at ICAL without magnetic fieldDetailed analysis at ICAL with magnetic field
Neutrino-factory neutrinos
ICAL or upgraded-ICAL as far-end detector fornu-factory
Non-oscillation physics
Ultra high energy cosmic rays, “Kolar events”, . . . ✘
WHEPP 8, IIT Bombay, Jan 8 2004 – p.3/42
Status Report
WHEPP 8, IIT Bombay, Jan 8 2004 – p.4/42
The INO Collaboration
Phase I : Around 2 years (On-going)
Detector R & DPhysics StudiesSite SurveyHuman resources development
Phase II : Construction of the detector
Detector Possibilities
Magnetised iron with RPCs or glass spark chambers
Alternate design ✘
Should be an international facility
WHEPP 8, IIT Bombay, Jan 8 2004 – p.5/42
The INO Collaboration
Phase I : Around 2 years (On-going)
Detector R & DPhysics StudiesSite SurveyHuman resources development
Phase II : Construction of the detector
Detector Possibilities
Magnetised iron with RPCs or glass spark chambers
Alternate design ✘
Should be an international facility
WHEPP 8, IIT Bombay, Jan 8 2004 – p.5/42
The INO Collaboration
Phase I : Around 2 years (On-going)
Detector R & DPhysics StudiesSite SurveyHuman resources development
Phase II : Construction of the detector
Detector Possibilities
Magnetised iron with RPCs or glass spark chambers
Alternate design ✘
Should be an international facility
WHEPP 8, IIT Bombay, Jan 8 2004 – p.5/42
Physics goals of analysis
Stage I:Studyoscillation patternin atmosphericneutrino events.
θ
θ
down
up
L
(Pietropicchi)
WHEPP 8, IIT Bombay, Jan 8 2004 – p.6/42
The difficulty and the hope
WHEPP 8, IIT Bombay, Jan 8 2004 – p.7/42
Choice of Neutrino Source and detector
Neutrino Source
Need to cover a large L/E range
Use atmospheric neutrinos as source
Large L range; also large E range
Need good resolution in both E and L (that is, in zenithangle θz)
Detector choice
Should have large target mass: 30 kton, 50 kton,100 kton . . .
Good tracking and energy resolution
Good directionality (≤ 1 ns time resolution)
Good charge resolution (for Stage II)
Ease of construction
Use (magnetised) iron as target mass and RPC as activedetector element
Note: Is sensitive to muons only
WHEPP 8, IIT Bombay, Jan 8 2004 – p.8/42
Choice of Neutrino Source and detector
Detector choice
Should have large target mass: 30 kton, 50 kton,100 kton . . .
Good tracking and energy resolution
Good directionality (≤ 1 ns time resolution)
Good charge resolution (for Stage II)
Ease of construction
Use (magnetised) iron as target mass and RPC as activedetector element
Note: Is sensitive to muons only
WHEPP 8, IIT Bombay, Jan 8 2004 – p.8/42
The ICAL detector
WHEPP 8, IIT Bombay, Jan 8 2004 – p.9/42
The active detector elements: RPC
RPC Construction: Float glass, graphite, and spacers
at TIFR . . .
WHEPP 8, IIT Bombay, Jan 8 2004 – p.10/42
The active detector elements: RPC
RPC Principles of operation: Streamer vs Spark mode
at TIFR . . .
WHEPP 8, IIT Bombay, Jan 8 2004 – p.10/42
The active detector elements: RPC
at TIFR . . .
WHEPP 8, IIT Bombay, Jan 8 2004 – p.10/42
RPC Efficiency studies
Using different combinations of gas
WHEPP 8, IIT Bombay, Jan 8 2004 – p.11/42
RPC Time resolution
at TIFR
WHEPP 8, IIT Bombay, Jan 8 2004 – p.12/42
Other issues w.r.t RPC R & D
RPC timing
RPC charge distribution
Mean charge vs voltage (seen to be linear)
RPC noise
Gas composition (C2H2F4, C4H10, Ar, Isobutane (8%))
RPC Cross talk (as a function of gas mixture)
Gas mixing
WHEPP 8, IIT Bombay, Jan 8 2004 – p.13/42
Magnet studies
WHEPP 8, IIT Bombay, Jan 8 2004 – p.14/42
Detector and Physics Simulation
NUANCE Event generator: Generates atmosphericneutrino events inside ICAL
GEANT Monte Carlo package: Simulates the detectorresponse for the neutrino event
Event Reconstruction: Fits the “raw data” to extractneutrino energy and direction
Physics Performance: Analysis of reconstructed eventsto extract physics
WHEPP 8, IIT Bombay, Jan 8 2004 – p.15/42
Simulations: Status report
Neutrino Generator
– Nuance: ICAL configuration with 3-flavour oscillationcode (D. Casper)
– Local: (HRI)
– (Neugen : H. Gallagher) ✘ Not used so far
One-line status summary:
programs in place and being tested; “data” beinganalysed.
WHEPP 8, IIT Bombay, Jan 8 2004 – p.16/42
Simulations: Status report
Detector Simulation
– Geant (3.2.1 Fortran) program in place; now withmagnetic field map as well.
One-line status summary:
programs in place and being tested; “data” beinganalysed.
WHEPP 8, IIT Bombay, Jan 8 2004 – p.16/42
Simulations: Status report
Track Reconstruction using Fortran/ROOT in C++
– Without magnetic field: program fits muons to straightlines, with energy loss; still to be refined.
– With magnetic field: program fits muons to helicaltrajectory, with energy loss; still to be refined.
– Hadron hit reconstruction: to be refined.
One-line status summary:
programs in place and being tested; “data” beinganalysed.
WHEPP 8, IIT Bombay, Jan 8 2004 – p.16/42
Simulations: Status report
One-line status summary:
programs in place and being tested; “data” beinganalysed.
WHEPP 8, IIT Bombay, Jan 8 2004 – p.16/42
Site survey: PUSHEP
PUSHEP in Nilagiris, near Ooty (Masinagudi)
WHEPP 8, IIT Bombay, Jan 8 2004 – p.17/42
Site Survey: Rammam
Rammam in Darjeeling District
WHEPP 8, IIT Bombay, Jan 8 2004 – p.18/42
Physics Prospects
WHEPP 8, IIT Bombay, Jan 8 2004 – p.19/42
Physics with Atmospheric Neutrinos
Simplified ICAL detector geometry encoded in Nuancegenerator.
Events are generated using HONDA flux with someinput oscillation parameters δ23, θ23, and θ13 = 0 (ICALmay not be sensitive to 1-3 mixing).
Quasielastic, resonant, DIS events, roughly in1/3 : 1/3 : 1/3 ratio
Analysis ONLY of 5 year CC events with µ in the finalstate (electron CC events mostly lost); typicallyinteresting events have E > 1–2 GeV.
MAJOR ISSUE, YET TO BE STUDIED: Mis-identification of pionsas muons from NC as well as a subset of CC events.
Recall: ICAL geometry is similar to that of MONOLITH.WHEPP 8, IIT Bombay, Jan 8 2004 – p.20/42
Physics Analysis (2-flavour)
➢ Main goal: Study oscillation pattern in atmosphericneutrino events. θ
θ
down
up
L
(Pietropicchi)
up ratedown rate
= Pµµ = 1 −sin2 θ23
2
(
1 − R cos 2.54 δ23
L
E
)
,
Resolution function is given by the Lorentzian:
R(x = L/E) =1
π
(
σ
σ2 + (x − x0)2
)
;
σ is the resolution in L/E of the ICAL detector.
So, analysis needs a knowledge of this resolution function.
WHEPP 8, IIT Bombay, Jan 8 2004 – p.21/42
Physics Analysis (2-flavour)
up ratedown rate
= Pµµ = 1 −sin2 θ23
2
(
1 − R cos 2.54 δ23
L
E
)
,
Resolution function is given by the Lorentzian:
R(x = L/E) =1
π
(
σ
σ2 + (x − x0)2
)
;
σ is the resolution in L/E of the ICAL detector.
So, analysis needs a knowledge of this resolution function.
WHEPP 8, IIT Bombay, Jan 8 2004 – p.21/42
Energy Resolution
1
10
100
1000
10000
100000
1 10 100
Energy (GeV)
Energy distribution (neutrinos and muons)
0
10
20
30
40
50
60
70
80
90
-1 -0.8 -0.6 -0.4 -0.2 0 0.2 0.4 0.6 0.8 1
even
ts
(E(nu)-E(mu))/E(nu)
Energy resolution
• Energy resolution with muons alone and includinghadrons as well.
• Eµ ∼ 0.7Eν
WHEPP 8, IIT Bombay, Jan 8 2004 – p.22/42
Nuance output
400
500
600
700
800
900
1000
1100
1200
1300
1400
-1 -0.8 -0.6 -0.4 -0.2 0 0.2 0.4 0.6 0.8 1
cos(theta)
Zenith angle distribution (neutrinos)
200
300
400
500
600
700
800
900
1000
-1 -0.8 -0.6 -0.4 -0.2 0 0.2 0.4 0.6 0.8 1
cos(theta)
Zenith angle distribution (muons)
Neutrinos (left) Muons (right)with oscillations . . . . . . . . . . . . without oscillations
WHEPP 8, IIT Bombay, Jan 8 2004 – p.23/42
Analysis of GEANT-processed events
The Nuance events were generated with some startingoscillation parameters (δ23 and θ) for the neutrino fluxes.
The CC events containing muons are passed throughthe GEANT program to get a pattern of hits in thesimulated ICAL detector.
The hits are recontructed to get Eµ, θµ, Ehad.
The relevant resolutions including R are studied.
R is used to fit the oscillation pattern in thereconstructed ratio of up/down events.
The fit results in estimates of the oscillation parameters.
This determines the sensitivity of the detectorconfiguration to the oscillation parameters.
WHEPP 8, IIT Bombay, Jan 8 2004 – p.24/42
WITHOUT Magnetic Field
E & L distributions from reconstructing muon tracks in ICALdetector (hadron contribution not included here).
0
5
10
15
20
25
30
0 5 10 15 20 25 30
Efit
Emu
0
2000
4000
6000
8000
10000
12000
14000
0 2000 4000 6000 8000 10000 12000 14000
Lfit
Lmu
Left: Efit from hit reconstruction vs. Eµ from Nuance
Right: Lfit from hit reconstruction vs. Lµ from Nuance
WHEPP 8, IIT Bombay, Jan 8 2004 – p.25/42
L/E Resolution
0
100
200
300
400
500
600
-1 -0.8 -0.6 -0.4 -0.2 0 0.2 0.4 0.6 0.8 1
Eve
nts
(L/E (mu) - L/E(fit))/ L/E (mu)
Resolution obtained, in the absence of magnetic field:
∆L
E= 0.18
L
E
WHEPP 8, IIT Bombay, Jan 8 2004 – p.26/42
Physics analysis with Geant events
• Oscillation Parameters: δ23 = 3 × 10−3 eV2; sin2 2θ23 = 1.0
• Resolution function: σ = 0.18L/E
δ23 = (3.3+0.3−0.6) × 10−3 eV2 (3.0) NEW! since INSA meeting,
sin2 2θ23 = 0.98+0.02−0.07 (1.0) New Delhi, Nov 03
WHEPP 8, IIT Bombay, Jan 8 2004 – p.27/42
L/E Resolution with magnetic field
histoEntries 0Mean -0.1597RMS 0.3665
-2 -1.5 -1 -0.5 0 0.5 1 1.5 20
20
40
60
80
100
120
140
160
180
200
220
histoEntries 0Mean -0.1597RMS 0.3665
sigma=0.43
mean=-0.19
L/E Resolution for 5 yrs
h1Entries 1827Mean -0.09601RMS 0.4524
-2 -1.5 -1 -0.5 0 0.5 1 1.5 20
20
40
60
80
100
120
140
160
180h1
Entries 1827Mean -0.09601RMS 0.4524
sigma=0.30
mean=-0.13
L/E(mu) Resolution for 5 yrs
L/E resolution from reconstruction (left); muon only (right).Resolution obtained, with magnetic field:
∆L
E= 0.215
L
E.
Program has since been improved
WHEPP 8, IIT Bombay, Jan 8 2004 – p.28/42
Comments on resolutions
The worst data is at small L/E (small number ofevents.) Use of magnetic field improves the event ratehere.
Sensitivity to this small L/E region still to be studied.
One possibility is to look at vertical planes of iron.
Various refinements in progress.
WHEPP 8, IIT Bombay, Jan 8 2004 – p.29/42
Comments on resolutions
The worst data is at small L/E (small number ofevents.) Use of magnetic field improves the event ratehere.
Sensitivity to this small L/E region still to be studied.
One possibility is to look at vertical planes of iron.
Various refinements in progress.
WHEPP 8, IIT Bombay, Jan 8 2004 – p.29/42
Comments on resolutions
The worst data is at small L/E (small number ofevents.) Use of magnetic field improves the event ratehere.
Sensitivity to this small L/E region still to be studied.
One possibility is to look at vertical planes of iron.
Various refinements in progress.
WHEPP 8, IIT Bombay, Jan 8 2004 – p.29/42
Comments on resolutions
The worst data is at small L/E (small number ofevents.) Use of magnetic field improves the event ratehere.
Sensitivity to this small L/E region still to be studied.
One possibility is to look at vertical planes of iron.
Various refinements in progress.
WHEPP 8, IIT Bombay, Jan 8 2004 – p.29/42
Physics Results with Nuance
Nuance → Geant → Reconstruction → Analysis formsthe complete route from simulation to analysis.
Detailed studies only without magnetic field so far;others in progress. Expect results to improve withmagnetic field.
Have used the ICAL resolution function obtained aboveto analyse the Nuance output.
Here the route is Nuance → Analysis,that is, events are directly analysed without passingthrough detector and reconstructing hit pattern soreconstruction efficiency = 1 instead of 0.4.
Analysis done for different input values of oscillationparameters, δ23 and sin θ23.
WHEPP 8, IIT Bombay, Jan 8 2004 – p.30/42
Physics Results with Nuance
Nuance → Geant → Reconstruction → Analysis formsthe complete route from simulation to analysis.
Detailed studies only without magnetic field so far;others in progress. Expect results to improve withmagnetic field.
Have used the ICAL resolution function obtained aboveto analyse the Nuance output.
Here the route is Nuance → Analysis,that is, events are directly analysed without passingthrough detector and reconstructing hit pattern soreconstruction efficiency = 1 instead of 0.4.
Analysis done for different input values of oscillationparameters, δ23 and sin θ23.
WHEPP 8, IIT Bombay, Jan 8 2004 – p.30/42
Physics Results with Nuance
Nuance → Geant → Reconstruction → Analysis formsthe complete route from simulation to analysis.
Detailed studies only without magnetic field so far;others in progress. Expect results to improve withmagnetic field.
Have used the ICAL resolution function obtained aboveto analyse the Nuance output.
Here the route is Nuance → Analysis,that is, events are directly analysed without passingthrough detector and reconstructing hit pattern soreconstruction efficiency = 1 instead of 0.4.
Analysis done for different input values of oscillationparameters, δ23 and sin θ23.
WHEPP 8, IIT Bombay, Jan 8 2004 – p.30/42
Physics Results with Nuance
Nuance → Geant → Reconstruction → Analysis formsthe complete route from simulation to analysis.
Detailed studies only without magnetic field so far;others in progress. Expect results to improve withmagnetic field.
Have used the ICAL resolution function obtained aboveto analyse the Nuance output.
Here the route is Nuance → Analysis,that is, events are directly analysed without passingthrough detector and reconstructing hit pattern soreconstruction efficiency = 1 instead of 0.4.
Analysis done for different input values of oscillationparameters, δ23 and sin θ23.
WHEPP 8, IIT Bombay, Jan 8 2004 – p.30/42
Physics Results with Nuance
Nuance → Geant → Reconstruction → Analysis formsthe complete route from simulation to analysis.
Detailed studies only without magnetic field so far;others in progress. Expect results to improve withmagnetic field.
Have used the ICAL resolution function obtained aboveto analyse the Nuance output.
Here the route is Nuance → Analysis,that is, events are directly analysed without passingthrough detector and reconstructing hit pattern soreconstruction efficiency = 1 instead of 0.4.
Analysis done for different input values of oscillationparameters, δ23 and sin θ23.
WHEPP 8, IIT Bombay, Jan 8 2004 – p.30/42
δ = 2 × 10−3 eV2
1 2 3 40
100
200
1 2 3 40
0.5
1
1.5
0.8 0.9 1
WHEPP 8, IIT Bombay, Jan 8 2004 – p.31/42
δ = 3 × 10−3 eV2
1 2 3 40
100
200
1 2 3 40
0.5
1
1.5
0.8 0.9 1
WHEPP 8, IIT Bombay, Jan 8 2004 – p.32/42
δ = 5 × 10−3 eV2
1 2 3 40
100
200
1 2 3 40
0.5
1
1.5
0.8 0.9 1
WHEPP 8, IIT Bombay, Jan 8 2004 – p.33/42
δ = 8 × 10−3 eV2
1 2 3 40
100
200
1 2 3 40
0.5
1
1.5
0.8 0.9 1
WHEPP 8, IIT Bombay, Jan 8 2004 – p.34/42
Physics goals of analysis II
Stage II: Neutrino factories and INO (ICAL++)
Burning issue in neutrino physics: is the 1-3 mixingangle zero or not? If sin θ13 6= 0, can look for
A determination of sin θ13 itself
sign of the (23) mass-squared difference δ32 = m23 −m2
2
CP violation through a CP violating phase δ that occursin the mixing matrix when there are three activecoupled neutrino species.
WHEPP 8, IIT Bombay, Jan 8 2004 – p.35/42
Physics goals of analysis II
Stage II: Neutrino factories and INO (ICAL++)
Burning issue in neutrino physics: is the 1-3 mixingangle zero or not? If sin θ13 6= 0, can look for
A determination of sin θ13 itself
sign of the (23) mass-squared difference δ32 = m23 −m2
2
CP violation through a CP violating phase δ that occursin the mixing matrix when there are three activecoupled neutrino species.
WHEPP 8, IIT Bombay, Jan 8 2004 – p.35/42
Physics goals of analysis II
Stage II: Neutrino factories and INO (ICAL++)
Burning issue in neutrino physics: is the 1-3 mixingangle zero or not? If sin θ13 6= 0, can look for
A determination of sin θ13 itself
sign of the (23) mass-squared difference δ32 = m23 −m2
2
CP violation through a CP violating phase δ that occursin the mixing matrix when there are three activecoupled neutrino species.
WHEPP 8, IIT Bombay, Jan 8 2004 – p.35/42
Physics goals of analysis II
Stage II: Neutrino factories and INO (ICAL++)
Burning issue in neutrino physics: is the 1-3 mixingangle zero or not? If sin θ13 6= 0, can look for
A determination of sin θ13 itself
sign of the (23) mass-squared difference δ32 = m23 −m2
2
CP violation through a CP violating phase δ that occursin the mixing matrix when there are three activecoupled neutrino species.
WHEPP 8, IIT Bombay, Jan 8 2004 – p.35/42
INO as a far-end detector
INO (ICAL++) as a far-end detector for long baselineexperiments
Large L means large E (20 GeV or more), for seeinginteresting oscillation phenomena
Such a neutrino beam is far off into future, but lots ofwork going on (see neutrino oscillation industryweb-page)
WHEPP 8, IIT Bombay, Jan 8 2004 – p.36/42
INO as a far-end detector
INO (ICAL++) as a far-end detector for long baselineexperiments
Large L means large E (20 GeV or more), for seeinginteresting oscillation phenomena
Such a neutrino beam is far off into future, but lots ofwork going on (see neutrino oscillation industryweb-page)
WHEPP 8, IIT Bombay, Jan 8 2004 – p.36/42
INO as a far-end detector
INO (ICAL++) as a far-end detector for long baselineexperiments
Large L means large E (20 GeV or more), for seeinginteresting oscillation phenomena
Such a neutrino beam is far off into future, but lots ofwork going on (see neutrino oscillation industryweb-page)
WHEPP 8, IIT Bombay, Jan 8 2004 – p.36/42
Stage II: Inputs
Muon detection threshold = 2 GeV
Muon energy resolution = 5%.
All measurements involve wrong sign muon detection:low backgrounds
Beam has νe and νµ (or other way).
νµ → µ (detector)νe (beam) → νµ (oscillation)νµ (osc-beam) → µ (detector)
Result: wrong sign muon (10/kton = signal)
WHEPP 8, IIT Bombay, Jan 8 2004 – p.37/42
Stage II: Inputs
Muon detection threshold = 2 GeV
Muon energy resolution = 5%.
All measurements involve wrong sign muon detection:low backgrounds
Beam has νe and νµ (or other way).
νµ → µ (detector)νe (beam) → νµ (oscillation)νµ (osc-beam) → µ (detector)
Result: wrong sign muon (10/kton = signal)
WHEPP 8, IIT Bombay, Jan 8 2004 – p.37/42
Stage II: Inputs
Muon detection threshold = 2 GeV
Muon energy resolution = 5%.
All measurements involve wrong sign muon detection:low backgrounds
Beam has νe and νµ (or other way).
νµ → µ (detector)νe (beam) → νµ (oscillation)νµ (osc-beam) → µ (detector)
Result: wrong sign muon (10/kton = signal)
WHEPP 8, IIT Bombay, Jan 8 2004 – p.37/42
Stage II: Inputs
Muon detection threshold = 2 GeV
Muon energy resolution = 5%.
All measurements involve wrong sign muon detection:low backgrounds
Beam has νe and νµ (or other way).
νµ → µ (detector)νe (beam) → νµ (oscillation)νµ (osc-beam) → µ (detector)
Result: wrong sign muon (10/kton = signal)
WHEPP 8, IIT Bombay, Jan 8 2004 – p.37/42
Stage II: Inputs
Muon detection threshold = 2 GeV
Muon energy resolution = 5%.
All measurements involve wrong sign muon detection:low backgrounds
Beam has νe and νµ (or other way).
νµ → µ (detector)
νe (beam) → νµ (oscillation)νµ (osc-beam) → µ (detector)
Result: wrong sign muon (10/kton = signal)
WHEPP 8, IIT Bombay, Jan 8 2004 – p.37/42
Stage II: Inputs
Muon detection threshold = 2 GeV
Muon energy resolution = 5%.
All measurements involve wrong sign muon detection:low backgrounds
Beam has νe and νµ (or other way).
νµ → µ (detector)νe (beam) → νµ (oscillation)
νµ (osc-beam) → µ (detector)
Result: wrong sign muon (10/kton = signal)
WHEPP 8, IIT Bombay, Jan 8 2004 – p.37/42
Stage II: Inputs
Muon detection threshold = 2 GeV
Muon energy resolution = 5%.
All measurements involve wrong sign muon detection:low backgrounds
Beam has νe and νµ (or other way).
νµ → µ (detector)νe (beam) → νµ (oscillation)νµ (osc-beam) → µ (detector)
Result: wrong sign muon (10/kton = signal)
WHEPP 8, IIT Bombay, Jan 8 2004 – p.37/42
Stage II: Inputs
Muon detection threshold = 2 GeV
Muon energy resolution = 5%.
All measurements involve wrong sign muon detection:low backgrounds
Beam has νe and νµ (or other way).
νµ → µ (detector)νe (beam) → νµ (oscillation)νµ (osc-beam) → µ (detector)
Result: wrong sign muon (10/kton = signal)
WHEPP 8, IIT Bombay, Jan 8 2004 – p.37/42
Reach of sin θ13
JHF to Rammam Fermilab to PUSHEP
0.016
0.018
0.02
0.022
0.024
0.026
0.028
0.03
0.032
0.034
0.5 1 1.5 2 2.5 3
sinθ
13
Eµth (GeV)
Eµ+beam = 50 GeV
32 kT-yr
100 kT-yr
50 kT-yr
1019 µ decays/yr.
JHF - RAMMAM
0.0035
0.004
0.0045
0.005
0.0055
0.006
0.0065
0.007
0.0075
0.5 1 1.5 2 2.5 3
sinθ
13
Eµth (GeV)
Eµ+beam = 20 GeV
32 kT-yr
50 kT-yr
1021 µ decays/yr.
FERMILAB - PUSHEP
sin θ13 reach for different muon threshold energies.
WHEPP 8, IIT Bombay, Jan 8 2004 – p.38/42
Sign of δ23 vs wrong sign µ
JHF to Beijing, Rammam and PUSHEP
0
20
40
60
80
100
120
140
160
180
-0.004 -0.002 0 0.002 0.004
Num
ber o
f µ- /5
0 kT
-yr.
∆m213 eV2
Eµ+beam = 20 GeV
1019 µ decays/yr.
CHINA
PUSHEP
RAMM
AM
WHEPP 8, IIT Bombay, Jan 8 2004 – p.39/42
CP violation: δ vs L
JHF to Rammam and PUSHEP
0.01
0.1
1
10
100
5000 6000 7000 8000 9000 10000 11000
N(µ
+ )/N(µ
- )
L (Km.)
sinθ13 = 0.1 ∆m223 < 0
∆m223 > 0
Eµ+beam = 50 GeV
1021 µ decays/yr.
50 kt x (1 + 1) yrs.
FermiLab to Rammam and PUSHEP
WHEPP 8, IIT Bombay, Jan 8 2004 – p.40/42
Outlook
The ICAL detector
Proof-of-principle working of RPC shown
Accelerator neutrino programme:ICAL++, with suitable beam from future nu-factory, issensitive to sin2 2θ13, sign of δ23, and CP phase.JHF-PUSHEP baseline is near magic: may provideclean separation of matter and CP violation effects.
WHEPP 8, IIT Bombay, Jan 8 2004 – p.41/42
Outlook
The ICAL detector
Magnet studies under-way
Accelerator neutrino programme:ICAL++, with suitable beam from future nu-factory, issensitive to sin2 2θ13, sign of δ23, and CP phase.JHF-PUSHEP baseline is near magic: may provideclean separation of matter and CP violation effects.
WHEPP 8, IIT Bombay, Jan 8 2004 – p.41/42
Outlook
The ICAL detector
Hence detector prototype ready for construction
Accelerator neutrino programme:ICAL++, with suitable beam from future nu-factory, issensitive to sin2 2θ13, sign of δ23, and CP phase.JHF-PUSHEP baseline is near magic: may provideclean separation of matter and CP violation effects.
WHEPP 8, IIT Bombay, Jan 8 2004 – p.41/42
Outlook
The ICAL detector
Site survey: two possible sites, both seem good options
Accelerator neutrino programme:ICAL++, with suitable beam from future nu-factory, issensitive to sin2 2θ13, sign of δ23, and CP phase.JHF-PUSHEP baseline is near magic: may provideclean separation of matter and CP violation effects.
WHEPP 8, IIT Bombay, Jan 8 2004 – p.41/42
Outlook
The ICAL detector
Simulations: programs in place, need refining andtesting.
Atmospheric neutrino programme:ICAL sensitive to oscillation parameters to betteraccuracy than current Super-K.Also, may have the edge on MINOS if δ23 is smallerthan expected. Not sensitive to 1–3 mixing angle.
Accelerator neutrino programme:ICAL++, with suitable beam from future nu-factory, issensitive to sin2 2θ13, sign of δ23, and CP phase.JHF-PUSHEP baseline is near magic: may provideclean separation of matter and CP violation effects.
WHEPP 8, IIT Bombay, Jan 8 2004 – p.41/42
Outlook
The ICAL detector
Simulations: programs in place, need refining andtesting.
Atmospheric neutrino programme:ICAL sensitive to oscillation parameters to betteraccuracy than current Super-K.Also, may have the edge on MINOS if δ23 is smallerthan expected. Not sensitive to 1–3 mixing angle.
Accelerator neutrino programme:ICAL++, with suitable beam from future nu-factory, issensitive to sin2 2θ13, sign of δ23, and CP phase.JHF-PUSHEP baseline is near magic: may provideclean separation of matter and CP violation effects.
WHEPP 8, IIT Bombay, Jan 8 2004 – p.41/42
Outlook . . .
The INO Collaboration
MoU in place with several Institutes funded/aided by theDAE
Stage I studies with atmospheric neutrinos almostcomplete; Stage II with neutrinos from nu-factory to bestudied in more detail
Feasibility study in full swing; expect report by Janend/Feb 2004
The outlook looks good!
This is a massive project:
Looking for active collaboration both within India andabroad
WHEPP 8, IIT Bombay, Jan 8 2004 – p.42/42
Outlook . . .
The INO Collaboration
MoU in place with several Institutes funded/aided by theDAE
Stage I studies with atmospheric neutrinos almostcomplete; Stage II with neutrinos from nu-factory to bestudied in more detail
Feasibility study in full swing; expect report by Janend/Feb 2004
The outlook looks good!
This is a massive project:
Looking for active collaboration both within India andabroad
WHEPP 8, IIT Bombay, Jan 8 2004 – p.42/42
Outlook . . .
The INO Collaboration
MoU in place with several Institutes funded/aided by theDAE
Stage I studies with atmospheric neutrinos almostcomplete; Stage II with neutrinos from nu-factory to bestudied in more detail
Feasibility study in full swing; expect report by Janend/Feb 2004
The outlook looks good!
This is a massive project:
Looking for active collaboration both within India andabroad
WHEPP 8, IIT Bombay, Jan 8 2004 – p.42/42
Outlook . . .
The INO Collaboration
MoU in place with several Institutes funded/aided by theDAE
Stage I studies with atmospheric neutrinos almostcomplete; Stage II with neutrinos from nu-factory to bestudied in more detail
Feasibility study in full swing; expect report by Janend/Feb 2004
The outlook looks good!
This is a massive project:
Looking for active collaboration both within India andabroad
WHEPP 8, IIT Bombay, Jan 8 2004 – p.42/42
Outlook . . .
The INO Collaboration
MoU in place with several Institutes funded/aided by theDAE
Stage I studies with atmospheric neutrinos almostcomplete; Stage II with neutrinos from nu-factory to bestudied in more detail
Feasibility study in full swing; expect report by Janend/Feb 2004
The outlook looks good!
This is a massive project:
Looking for active collaboration both within India andabroad
WHEPP 8, IIT Bombay, Jan 8 2004 – p.42/42