India-based Neutrino Observatory (INO) · PDF fileD. Indumathi The Institute of Mathematical...
Transcript of India-based Neutrino Observatory (INO) · PDF fileD. Indumathi The Institute of Mathematical...
India-based Neutrino Observatory(INO)
Status Report
D. Indumathi
The Institute of Mathematical Sciences, Chennai
For the INO Collaboration
(http://www.imsc.res.in/∼ino)
NNN08, Sep 12, 2008 – p. 1
Outline of talk
The context
NNN08, Sep 12, 2008 – p. 2
Outline of talk
The context
The India-based Neutrino Observatory
The ICAL Detector: RPC’s and magnet design
Physics possibilities at ICAL: atmospheric andlong-baseline physics
Location
NNN08, Sep 12, 2008 – p. 2
Outline of talk
The context
The India-based Neutrino Observatory
The ICAL Detector: RPC’s and magnet design
Physics possibilities at ICAL: atmospheric andlong-baseline physics
Location
Current Status of INO
NNN08, Sep 12, 2008 – p. 2
From: www.bnl.gov/
The context
NNN08, Sep 12, 2008 – p. 3
A Schematic of Neutrino PropertiesNeutrino masses are not well-known. Oscillation studies only
determine the mass-squared differences: ∆m2
ij = m2
i − m2
j and the
mixing angles θij .
NNN08, Sep 12, 2008 – p. 4
A Schematic of Neutrino PropertiesNeutrino masses are not well-known. Oscillation studies only
determine the mass-squared differences: ∆m2
ij = m2
i − m2
j and the
mixing angles θij .
m2
0
solar~8×10−5eV2
atmospheric~2×10−3eV2
atmospheric~2×10−3eV2
m12
m22
m32
m2
0
m22
m12
m32
νe
νµντ
? ?
solar~8×10−5eV2
NNN08, Sep 12, 2008 – p. 4
A Schematic of Neutrino PropertiesNeutrino masses are not well-known. Oscillation studies only
determine the mass-squared differences: ∆m2
ij = m2
i − m2
j and the
mixing angles θij .
m2
0
solar~8×10−5eV2
atmospheric~2×10−3eV2
atmospheric~2×10−3eV2
m12
m22
m32
m2
0
m22
m12
m32
νe
νµντ
? ?
solar~8×10−5eV2
∆m221
∼ 0.8 × 10−4 eV2 ;
|∆m232| ∼ 2.0 × 10−3 eV2 ;
∑i mi < 0.7–2 eV.
NNN08, Sep 12, 2008 – p. 4
A Schematic of Neutrino PropertiesNeutrino masses are not well-known. Oscillation studies only
determine the mass-squared differences: ∆m2
ij = m2
i − m2
j and the
mixing angles θij .
m2
0
solar~8×10−5eV2
atmospheric~2×10−3eV2
atmospheric~2×10−3eV2
m12
m22
m32
m2
0
m22
m12
m32
νe
νµντ
? ?
solar~8×10−5eV2
∆m221
∼ 0.8 × 10−4 eV2 ;
|∆m232| ∼ 2.0 × 10−3 eV2 ;
∑i mi < 0.7–2 eV.
• m1 ∼ m2 ∼ m3 ∼ 0.2 eV
(Degenerate hierarchy)
• m1 < m2 ≪ m3
(Normal hierarchy)
• m3 ≪ m1 < m2
Inverted hierarchy
(APS multi-divisional neutrino study, physics/0411216)NNN08, Sep 12, 2008 – p. 4
India-based Neutrino
Observatory
.NNN08, Sep 12, 2008 – p. 5
The INO CollaborationAims to build an underground laboratory for science with
neutrino physics as a major activity
Spokesperson: N. K. Mondal, TIFR
Collaborating Institutions: AMU, BHU, BARC,CU, DU, HRI,
UoH, HPU, IITB, IITKh, IGCAR, IMSc, IOP, LU, NBU, PU, PRL,
SINP, SMIT, TIFR, VECC
NNN08, Sep 12, 2008 – p. 6
The INO CollaborationAims to build an underground laboratory for science with
neutrino physics as a major activity
Spokesperson: N. K. Mondal, TIFR
Collaborating Institutions: AMU, BHU, BARC,CU, DU, HRI,
UoH, HPU, IITB, IITKh, IGCAR, IMSc, IOP, LU, NBU, PU, PRL,
SINP, SMIT, TIFR, VECC
Stage I : Study of atmospheric neutrinos
Physics Studies (atmospheric neutrinos); Detector R & D;construction of a prototype (in progress); HRD
Site choice and clearances; lab and detector construction
NNN08, Sep 12, 2008 – p. 6
The INO CollaborationAims to build an underground laboratory for science with
neutrino physics as a major activity
Spokesperson: N. K. Mondal, TIFR
Collaborating Institutions: AMU, BHU, BARC,CU, DU, HRI,
UoH, HPU, IITB, IITKh, IGCAR, IMSc, IOP, LU, NBU, PU, PRL,
SINP, SMIT, TIFR, VECC
Stage I : Study of atmospheric neutrinos
Physics Studies (atmospheric neutrinos); Detector R & D;construction of a prototype (in progress); HRD
Site choice and clearances; lab and detector construction
Stage II : Study of long-baseline neutrinos, from a neutrino
factory/beta beam
Other detectors/physics like neutrinoless double beta decay?NNN08, Sep 12, 2008 – p. 6
The choice of detectorLarge target mass: began with 30 kton; current design 50kton
Good tracking and energy resolution
Nano-second time resolution for up/down discrimination;hence good directionality
Good charge resolution; magnetic field
Ease of construction (modular)
Use (magnetised) iron as target mass and RPC as activedetector element. Similar to MONOLITH.
Note: Is sensitive to muons only, not electrons
NNN08, Sep 12, 2008 – p. 7
The ICAL detector50 kton iron, magnetised to ∼ 1.2 T with 140 layers of 6cm plates in three modules
Each module = 16 × 16 × 12m3
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12m
16m
16m
16m16m
6cm
2.5cm
NNN08, Sep 12, 2008 – p. 8
The active detector elements: RPCRPC Construction: Float glass, graphite, and spacers
NNN08, Sep 12, 2008 – p. 9
Fabricating RPC’s
NNN08, Sep 12, 2008 – p. 10
Specifications of the ICAL detector
ICAL
No. of modules 3Module dimension 16 m × 16 m × 12 mDetector dimension 48 m × 16 m × 12 mNo. of layers 140Iron plate thickness ∼ 6 cmGap for RPC trays 2.5 cmMagnetic field 1.3 Tesla
RPC
RPC unit dimension 2 m × 2 mReadout strip width 3 cmNo. of RPC units/Road/Layer 8No. of Roads/Layer/Module 8No. of RPC units/Layer 192Total no. of RPC units ∼ 27000No. of electronic readout channels 3.6 × 106
NNN08, Sep 12, 2008 – p. 11
Physics Studies and SimulationsSource: Atmospheric Neutrinos, 6 years’ exposure,from Nuance neutrino generator.
ICAL simulation with GEANT-3, By = 1 T.
0.8 0.85 0.9 0.95 10.001
0.0015
0.002
0.0025
0.003
0.0035
0.004
Shown are 90 and99 CL contoursin comparisonwith Super-K andMINOS results.
Caution: MINOS ≡
3-flavour analysis,Schwetz et. al.hep-ph/0808.2016
NNN08, Sep 12, 2008 – p. 12
Physics Studies with ICAL
1 2 3 4
True value of ∆m2
31 [10
-3 eV
2]
-0.4
-0.2
0
0.2
0.4
Rel
ativ
e er
ror
at 2
σ
1 2 3 4-0.4
-0.2
0
0.2
0.4
SK+
K2K
MIN
OS
∆m2
31-precision
1 2 3 4
True value of ∆m2
31 [10
-3 eV
2]
1 2 3 4
CNGS
SK+
K2K
exluded at 3σ
MINOS
T2K
NOνACNGS
NOνA
T2K
SK+K2K current data
sin2θ
23-precision
ICAL
ICAL
old
old
NOVA
All experiments with 5 years’ running; NOVA 25kton, 6 years
(6 × 1021 pot).
Adapted from: P. Huber, M. Lindner, M. Rolinec, T. Schwetz and
W. Winter, hep-ph/0412133. NNN08, Sep 12, 2008 – p. 13
Matter effects with atmospheric neutrinos
5 10 15
0
0.2
0.4
0.6
0.8
1
vacuumδ32 > 0δ32 < 0
5 10 15
0
0.2
0.4
0.6
0.8
1
5 10 15
E (GeV)
0
0.2
0.4
0.6
0.8P(ν
µ→ν µ)
5 10 150
0.2
0.4
0.6
0.88000 km 10000 km
6000 km 7000 km
Matter effects involve the participation of all three (active) flavours;hence involves both sin θ13 and the CP phase δ.
Hence sensitive to the mass ordering of the 2–3 states, providedθ13 > 6◦; however, needs large exposures
NNN08, Sep 12, 2008 – p. 14
The difference asymmetry
D: Direct/normal; I: Inverted hierarchy
Sign of δ ≡ ∆m2
32for
θ13 = 5, 7, 9, 11◦
Hence sensitive to themass ordering (red vsblue) of the 2–3 states
With exposures of 500kton-years, can get a90%CL result ifsin
22θ13 > 0.09 (10% R)
sin22θ13 > 0.07 (5% R)
However, needs large ex-posures of about 800kton-years for smallersin
22θ13 > 0.07 (10% R)
sin22θ13 > 0.05 (5% R)
NNN08, Sep 12, 2008 – p. 15
Other physics possibilities
. . . with atmospheric neutrinos
Discrimination of octant of θ23 provided θ13 > 7◦
(sin2 2θ13 > 0.06); harder than mass ordering
Probing CPT violation from rates of neutrino- to rates ofanti-neutrino events in the detector: sensitive to δb,which adds to ∆m2
32/(2E) in oscillation probability
expression.
Constraining long-range leptonic forces by introducing amatter-dependent term in the oscillation probabilityeven in the absence of Ue3, so that neutrinos andanti-neutrinos oscillate differently.
Discrimination between oscillation of νµ to active ντ andsterile νs from up/down ratio in “muon-less” events?
NNN08, Sep 12, 2008 – p. 16
Stage II: Neutrino factories and INO
0.025
0.03
0.035
0.04
0.045
0.05
0.055
0.06
0.5 1 1.5 2 2.5 3
sinθ
13
Eµth (GeV)
32 kton-yr
50 kton-yr
100 kton-yr
Eµ+beam = 20 GeV
1019 µ decays/yr
JHF−PUSHEP
0
20
40
60
80
100
120
-0.004 -0.002 0 0.002 0.004
Num
ber
of
µ- /32 k
ton-y
r
δ32 eV2
Eµ+beam = 20 GeV
1019 µ decays/yr
CH
INA
PU
SH
EPRA
MM
AM
θ13 reach and sign of ∆m232
vs wrong sign µ
Can also study CP violation: note, JHF–PUSHEP (6556 km) and
CERN–PUSHEP (7145 km) are close to magic. NNN08, Sep 12, 2008 – p. 17
Location of INO
Singara in the Nilagiris, near Ooty (Masinagudi)NNN08, Sep 12, 2008 – p. 18
More on the site
• 2.1 km long access tun-nel into mountain; cavernbeneath the peak
• Experimental hall I:25m×130m×30m (height)built to accommodate 50kton + 50 kton modules(future expansion)
• Experimental Hall II:about half the size, toaccommodate other,smaller experiment(s).
NNN08, Sep 12, 2008 – p. 19
Current Status of
INO
NNN08, Sep 12, 2008 – p. 20
Prototype Studies at VECC/TIFR
Magnet Weight∼ 40 tons; 2.5 m × 2.3 m13 layers of 5 cm soft iron; 12 layers of 1 × 1m2 RPCsNImax = 10, 000 A.turnsBmax = 1.5 T (expected)800 channels of preamp, timing discriminators for avalanche RPCs
NNN08, Sep 12, 2008 – p. 21
RPC Efficiency StudiesRPCs now operated inavalanche mode R134a:95.5%;rest isobutane, at 9.3 KV
Round-the-clock monitoring of2 RPCs for two years now—temperature, relative humidity,pressure.
Efficiency stable; chamber cur-rents, noise rates, stable.
Testing bakelite RPCs at VECCand BARC
NNN08, Sep 12, 2008 – p. 22
Hardware issuesMechanical design and assembly project report being pepared byTata Consulting Engineers (TCE), Mumbai
In-house electronics development for prototype for both front andback-ends.
NNN08, Sep 12, 2008 – p. 23
Environment and Forest ClearancesMain issue: INO is located in Manipulation Zone of Nilgiri biospherereserve.
No clearance or occupation of forest. (Access and buildingscompletely within TNEB power house campus). However,
disruption in nearby elephant corridor;
disposal of stone excavated;
employment opportunities for locals.
Rapid-EIA by SACON; detailed EMP by Care-Earth:recommendations on each of these issues
Meetings with local bodies (panchayats), wildlife scientists, activists.One/two more interaction meetings planned.
NNN08, Sep 12, 2008 – p. 24
Other UpdatesSimulations for ICAL detector: comparison of GEANT3 and
GEANT4; differences in hadrons, yet to be fully understood
A DPR for a planned DBD experiment; bolometric 124Sn
prototype of 0.5 to 1 kg
INO Graduate School, began in August this year
Lectures at HRI/TIFR; Faculty from all over India
A new centre at Mysore will take charge of the INO related
activities
NNN08, Sep 12, 2008 – p. 25
Costs/SchedulesRs (crores)
11th plan 12th plan
Infrastructure (labs, services, ...) 100Soft iron 50 kton 100 200Detector (RPC, electronics, DAQ) 75 130Misc. inclusive. salaries 45 20Mysore Centre 50DST 100 100
TOTAL 470+ 450920 = 230 M$
•
t = 0 ≤ 6 months?
• 12–18 months: planning, permissions, engg design
• 22 months: excavation, detector fabrication
• 12–18 months assembly of 1–2 modules
NNN08, Sep 12, 2008 – p. 26
Approval Status
DAE has given an "in-principle" approval for the project.
The request for funding project is jointly submitted toDAE-DST.
The requested funding for the current plan periodending March 2012 has been allocated by the IndianPlanning Commission.
Detailed Project Report with year-wise funding requestis required for sanction of money, including forconstruction.
DPR is in the approval chain. Expected to take a fewmore months.
Thank You
NNN08, Sep 12, 2008 – p. 27
Additional Slides
NNN08, Sep 12, 2008 – p. 28
3σ Precision of parametersat ∆m2
32= 2.0 × 10−3 eV2 and sin
2 θ23 = 0.5
Experiment P(|∆m2
32) P(sin2 θ23) hierarchy
Current 88% 79% –
MINOS 17% 65% –
CNGS 37% – –
NOνA (6 × 1021 pot) ∼ 5% ∼ 9% in comb
T2K (Super-K, 0.75 MW) 12% 46%
ICAL (50 kton) 20% 60% sin22θ13 > 0.06
NNN08, Sep 12, 2008 – p. 29
NOVA 23 parameters
Caius Howcroft
"# Disappearance Measurement
20
• NO"A can still do "# disappearance measurement, measure the mixing angle !23 and %m2
23.
x10
Measure sin22!23 to 0.5-1%
NNN08, Sep 12, 2008 – p. 30
NOVA hierarchy parameters
Caius Howcroft
Hierarchy Sensitivity
18
)/!
Measurement unique to NO"A
Fraction
of !
covered
NNN08, Sep 12, 2008 – p. 31
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 (R-134a), Argon, Isobutane(≤ 8%))
RPC Cross talk (as a function of gas mixture)
Gas mixing
NNN08, Sep 12, 2008 – p. 32