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

([email protected])

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



ij = m2

i − m2

j and the


m2

0

solar~8×10−5eV2

atmospheric~2×10−3eV2


m12

m22

m32

m2

0

m22

m12

m32

νe

νµντ

? ?

solar~8×10−5eV2

NNN08, Sep 12, 2008 – p. 4



ij = m2

i − m2

j and the


m2

0

solar~8×10−5eV2



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



ij = m2

i − m2

j and the


m2

0

solar~8×10−5eV2



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







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







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

��

��

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

India-based Neutrino Observatory (INO) · PDF fileD. Indumathi The Institute of Mathematical...

Documents

Transcript of India-based Neutrino Observatory (INO) · PDF fileD. Indumathi The Institute of Mathematical...