Naba K Mondal Tata Institute, Mumbai · Neutrino 2006, Santa Fe, USA Location of the Underground Laboratory • Studies were performed on two potential sites. – Pykara Ultimate

Neutrino 2006, Santa Fe, USA

FFuuture Atmospheric Neutrino Experimentsture Atmospheric Neutrino Experiments

NabaNaba K K MondalMondalTataTata Institute, MumbaiInstitute, Mumbai


Need for new Atmospheric Neutrino Need for new Atmospheric Neutrino DetectorsDetectors

• Experimental field of Neutrino Physics has moved to the phase of decisive and precision measurement of oscillation parameters.

• New and planned long base line experiments will provide bulk of the data necessary to achieve this.

• Is there still need for new atmospheric neutrino experiments?


Physics with Atmospheric NeutrinosPhysics with Atmospheric Neutrinos

• It span a large range of L/E .• Oscillation can be seen as a function of L/E.• Possibility of observing matter effect .• Sensitivity to the sign of Δm2

23.

• Measuring θ13.

• CP Phase measurement.


Magnetised Iron Tracking Calorimeter


IndiaIndia--based Neutrino Observatory (INO) initiativebased Neutrino Observatory (INO) initiative

• Two phase approach:

R & D and ConstructionPhase I

Physics studies,Detector R & D,Site survey,Human resource development

Phase IIConstruction of the detector

Operation of the Detector

Phase IPhysics with Atmospheric Neutrinos

Phase IIPhysics with Neutrino beam from

a factory

Goal: A large mass detector with charge identification capability


Choice of Neutrino Source and DetectorChoice of Neutrino Source and Detector• Neutrino Source

– Need to cover a large L/E range.• Large L range• Large Eν range

– Use Atmospheric neutrinos as source.• 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• Modularity• Complimentarity with other existing and proposed detectors

– Use magnetised iron as target mass and RPC as active detector medium.


INO Detector ConceptINO Detector Concept


Construction of RPCConstruction of RPC

Pickup strips

Two 2 mm thick float GlassSeparated by 2 mm spacer2 mm thick spacer

Glass plates

Resistive coating on the outer surfaces of glass


ICAL Detector SpecificationsICAL Detector Specifications

3.6 X 106 No of Electronic channels27000Total no of RPC units192No. of RPC units/Layer8No. of Roads/Layer/Module8No. of RPCs/Road/Layer3 cmReadout strip width2 m X 2 mRPC unit dimension1.3 TeslaMagnetic field2.5 cmGap for RPC trays6 cmIron plate thickness140No of layers48 m X 16 m X 12 mDetector dimension16 m X 16 m X 12 mModule dimension3No of modules


RPC R & DRPC R & D

• Built RPCs of different sizes– 30 cm X 30 cm – 120 cm X 90 cm


RPC Efficiencies and TimingRPC Efficiencies and Timing

RPC working in Streamer mode


Cosmic Cosmic MuonMuon TestTest

Stack of 10 RPCs

Gas unit

Telescope

DAQ

• Streamer mode (R134a=62%,Argon=30% and the rest Iso-Butane)

• Recording hits, timing, noise rates etc


Location of the Underground LaboratoryLocation of the Underground Laboratory• Studies were performed on two potential sites.

– Pykara Ultimate Stage Hydro Electric Project (PUSHEP) at Masinagudi, Tamilnadu

– Rammam Hydro Electric Project Site at Darjeeling District in West Bengal

• INO Site Selection Committee after thorough evaluation have now recommended PUSHEP at Tamilnadu as the preferred site for the underground lab.


Underground CavernUnderground Cavern

Layout of the Underground Cavern

Size of the experimental hall150 m X 22 m X 30 m

Access tunnel

Experimental Hall

Parking & Storage

Electronics

Experimental Hall


Physics using atmospheric neutrinos during Phase IPhysics using atmospheric neutrinos during Phase I

• Improved measurement of oscillation parameters.• Search for potential matter effect in neutrino oscillation.• Determining the sign of Δm2

23 using matter effect.• Is θ23 maximal ? If not θ23 < π/4 or > π/4 ?• Probing CPT violation in neutrino sector.• Ultra high energy muons in cosmic rays.


Physics with Neutrino beam from NUFACT Physics with Neutrino beam from NUFACT –– Phase IIPhase II

• Determination of θ13.

• Determining the sign of Δm223.

• Matter effect in νμ ντ oscillation.• Probing CP violation in leptonic sector.


Disappearance of Disappearance of ννμμ vs. L/Evs. L/EThe disappearance probability can be measured with a single detector and two equal sources:

= P(νμ → νμ; L/E) N up(L/E)

N down(L’/E)= 1 - sin2 (2Θ) sin2 (1.27 Δm2 L/E)


Precision Measurement of Oscillation ParametersPrecision Measurement of Oscillation Parameters


Matter EffectMatter Effect

)(),(cos

),(cos

cos22

ELEPdEd

dLEPdEd

dddEMNN e

z

e

zzYn μμμμ

μμ σ

θφ

θφ

θ⎥⎥⎦

⎤

⎢⎢⎣

⎡+×= ∫ ∫

)/27.1(sin2sinsin)( 312

132

232 ELP mm

emat Δ=→ θθνν μ

)/27.1(sin2sinsin)( 312

132

232 ELP e

vac Δ=→ θθνν μ

Total no. of νμ charge current events:

Neglecting Δ21

R. Gandhi et al PRL 94, 051801, 2005


Mass Hierarchy from matter induced Mass Hierarchy from matter induced asymmetryasymmetry


Deviation from Deviation from maximalitymaximality ofof θθ2323


CPT ViolationCPT Violation

⎥⎦

⎤⎢⎣

⎡⎟⎠⎞

⎜⎝⎛ +−= Lb

ELP

24sin2sin1)( 3222 δδθμμ

( )bLELPPPCPT δδθμμμμμμ sin

2sin2sin 322 ⎟

⎠⎞

⎜⎝⎛−=−=Δ

The expression for survival probability for the case of CPTV 2-flavour oscillations

and


Future water Cherenkov detectors


HyperHyper--KamiokandeKamiokande

～1 Mton water Cherenkov detector at Kamioka


Why this design has been chosen ?Why this design has been chosen ?

• Water depth < 50 m(If the present 20-inch PMT or similar one will be used.)

• Linear dimensions for light path < 100 m• Optimization of MFID/MTOTAL• Rock stability

– Avoid sharp edges. Spherical shape is the best. • solution: Tunnel-shaped cavity• Single Cavity or Twin Cavities?

– Single Cavity• MFID/MTOTAL is better• Cost is lower• Larger area of stable rock mass needed.

– Twin Cavities• Two detectors are independent. One detector is alive when the other is

calibrated or maintained.• Both cavities should be excavated at the same time. But staging scenario is

possible for the later phase of the detector construction.• solution: Twin cavities


UNOUNO


-> a very large Laboratory to allow the installation of a Megaton-scale Cerenkov Detector ( ≈ 106 m3)

Present Tunnel

Future Safety Tunnel

Present Laboratory

Future Laboratory with Water Cerenkov Detectors

.

MEMPHYSMEMPHYS


Physics reach of

Megaton scale Water Cherenkov Detectors

Octant of θ23

Nonzero θ13

δCP


oscillation effects in oscillation effects in ννee

resonance 13ϑ

ceinterferenLMA

)1(~2

)sin(cos2sin~~

)1(1)()(

range)GeV-Sub(at ph/0309312-hep Smirnov and Pares

223

213

22232

1313

2232

0

−⋅+

⋅−⋅⋅⋅⋅−

−⋅≅−ΨΨ

srs

IRcsr

crPee

CPCP δδϑ

νν

r : μ/e flux ratio (~2 at low energy)

P2 = |Aeμ|2 : 2ν transition probability νe νμτ in matterR2 = Re(A*eeAeμ)I2 = Im(A*eeAeμ)Aee : survival amplitude of the 2ν systemAeμ : transition amplitude of the 2ν system


0.9

0.95

1

1.05

1.1

1.15

1.2

-1 -0.8 -0.6 -0.4 -0.2 0 0.2 0.4 0.6 0.8 1

cosΘ

Ne/

Ne0

Effect of Effect of θθ23 23 after after νν interactionsinteractions

0.9

0.95

1

1.05

1.1

1.15

1.2

-1 -0.8 -0.6 -0.4 -0.2 0 0.2 0.4 0.6 0.8 1

cosΘ

Ne/

Ne0

0.9

0.95

1

1.05

1.1

1.15

1.2

-1 -0.8 -0.6 -0.4 -0.2 0 0.2 0.4 0.6 0.8 1

cosΘ

Ne/

Ne0

no osc. with 20yrs stat.errors223=0.40

0.450.500.550.60

s22θ12=0.825s2θ23=0.4 ~ 0.6s2θ13=0.04δcp=45o

Δm212=8.3e-5Δm223=2.5e-3


0

0.02

0.04

0.06

0.08

0.1

0.12

0.14

0.16

0.18

0.3 0.35 0.4 0.45 0.5 0.55 0.6 0.65 0.7

SK 20yrs, 90% C.L.

sin2θ23

sin

2 θ 13

0

0.02

0.04

0.06

0.08

0.1

0.12

0.14

0.16

0.18

0.3 0.35 0.4 0.45 0.5 0.55 0.6 0.65 0.7

SK 20yrs, 90% C.L.

sin2θ23

sin

2 θ 13

Discrimination of Discrimination of θθ2323 octantoctant

0

0.02

0.04

0.06

0.08

0.1

0.12

0.14

0.16

0.18

0.3 0.35 0.4 0.45 0.5 0.55 0.6 0.65 0.7

SK 20yrs, 90% C.L.

sin2θ23

sin

2 θ 13

0

0.02

0.04

0.06

0.08

0.1

0.12

0.14

0.16

0.18

0.3 0.35 0.4 0.45 0.5 0.55 0.6 0.65 0.7

SK 20yrs, 90% C.L.

sin2θ23

sin

2 θ 13

s22θ12=0.825s2θ23=0.4 or 0.6s2θ13=0.00~0.04δcp=45o

Δm212=8.3e-5Δm223=2.5e-3

With 20yrs SK, discriminationis possible for large θ13.

s2θ23 = 0.40 or 0.60s22θ23=0.96


Discrimination of Discrimination of θθ2323 octantoctant

0

0.02

0.04

0.06

0.08

0.1

0.12

0.14

0.16

0.18

0.3 0.35 0.4 0.45 0.5 0.55 0.6 0.65 0.7

SK 20yrs, 90% C.L.

sin2θ23

sin

2 θ 13

0

0.02

0.04

0.06

0.08

0.1

0.12

0.14

0.16

0.18

0.3 0.35 0.4 0.45 0.5 0.55 0.6 0.65 0.7

SK 20yrs, 90% C.L.

sin2θ23

sin

2 θ 130

0.02

0.04

0.06

0.08

0.1

0.12

0.14

0.16

0.18

0.3 0.35 0.4 0.45 0.5 0.55 0.6 0.65 0.7

SK 20yrs, 90% C.L.

sin2θ23

sin

2 θ 13

s22θ12=0.825s2θ23=0.45 or 0.55s2θ13=0.00~0.04δcp=45o

Δm212=8.3e-5Δm223=2.5e-3

With 20yrs SK, discriminationis very hard.

0

0.02

0.04

0.06

0.08

0.1

0.12

0.14

0.16

0.18

0.3 0.35 0.4 0.45 0.5 0.55 0.6 0.65 0.7

SK 20yrs, 90% C.L.

sin2θ23

sin

2 θ 13

s2θ23 = 0.45 or 0.55s22θ23=0.99


0

0.02

0.04

0.06

0.08

0.1

0.12

0.14

0.16

0.18

0.3 0.35 0.4 0.45 0.5 0.55 0.6 0.65 0.7

SK 80yrs, 90% C.L.

sin2θ23

sin

2 θ 13

0

0.02

0.04

0.06

0.08

0.1

0.12

0.14

0.16

0.18

0.3 0.35 0.4 0.45 0.5 0.55 0.6 0.65 0.7

SK 80yrs, 90% C.L.

sin2θ23

sin

2 θ 13

Discrimination of Discrimination of θθ2323 octant, SKx80yrsoctant, SKx80yrs

s22θ12=0.825s2θ23=0.40 ~ 0.60s2θ13=0.00~0.04δcp=45o

Δm212=8.3e-5Δm223=2.5e-3

With 80yrs SK, discriminationis better and possible for many test points.

80yrs SK ~ 4yrs HK


0

2

4

6

8

10

12

14

16

18

20

0 0.01 0.02 0.03 0.04 0.05

sin2θ13

Δχ2 ((

tru

e θ 13

) -

(zer

o θ

13))

Significance for nonzero Significance for nonzero θθ1313

s22θ12=0.825s2θ23=0.40 ~ 0.60s2θ13=0.00~0.04δcp=45o

Δm212=8.3e-5Δm223=2.5e-3

Positive signal for nonzero θ13 can be seen if θ13

is near the CHOOZ limit and s2θ23 > 0.5

20yrs SK

3σ

3σ for 80yrs SK~4yrs HK

s223=0.400.450.500.550.60


0

0.02

0.04

0.06

0.08

0.1

0.12

0.14

0.16

0.18

0 50 100 150 200 250 300 350

CP phase

sin

2 θ 13

δδCPCP sensitivitysensitivity

0

0.02

0.04

0.06

0.08

0.1

0.12

0.14

0.16

0.18

0 50 100 150 200 250 300 350

CP phase

sin

2 θ 13

0

0.02

0.04

0.06

0.08

0.1

0.12

0.14

0.16

0.18

0 50 100 150 200 250 300 350

CP phase

sin

2 θ 13

0

0.02

0.04

0.06

0.08

0.1

0.12

0.14

0.16

0.18

0 50 100 150 200 250 300 350

CP phase

sin

2 θ 13

s22θ12=0.825s2θ23=0.5s2θ13=0.00~0.04δcp=0o~360o

Δm212=8.3e-5Δm223=2.5e-3

0

0.02

0.04

0.06

0.08

0.1

0.12

0.14

0.16

0.18

0 50 100 150 200 250 300 350

CP phase

sin

2 θ 13

0

0.02

0.04

0.06

0.08

0.1

0.12

0.14

0.16

0.18

0 50 100 150 200 250 300 350

CP phase

sin

2 θ 13

0

0.02

0.04

0.06

0.08

0.1

0.12

0.14

0.16

0.18

0 50 100 150 200 250 300 350

CP phase

sin

2 θ 13

0

0.02

0.04

0.06

0.08

0.1

0.12

0.14

0.16

0.18

0 50 100 150 200 250 300 350

CP phase

sin

2 θ 13

0

0.02

0.04

0.06

0.08

0.1

0.12

0.14

0.16

0.18

0 50 100 150 200 250 300 350

CP phase

sin

2 θ 13

0

0.02

0.04

0.06

0.08

0.1

0.12

0.14

0.16

0.18

0 50 100 150 200 250 300 350

CP phase

sin

2 θ 13

0

0.02

0.04

0.06

0.08

0.1

0.12

0.14

0.16

0.18

0 50 100 150 200 250 300 350

CP phase

sin

2 θ 13

0

0.02

0.04

0.06

0.08

0.1

0.12

0.14

0.16

0.18

0 50 100 150 200 250 300 350

CP phase

sin

2 θ 13

80yrs SK ~ 4yrs HK

CP phase could be seen if θ13 is close to the CHOOZ limit.


Summary• A large magnetised detector of 50-100 Kton like INO is needed to

achieve some of the very exciting physics goals using atmospheric neutrinos.

• It will complement the existing and planned water cherenkovdetectors.

• Can be used as a far detector during neutrino factory era.• R & D for setting up such a detector in India is in progress.

• If θ13 is close to the CHOOZ limit, then next generation water Cherenkov detectors could give us precious information on;

– octant of θ23

– nonzero θ13

– δCP

Documents

Naba K Mondal Tata Institute, Mumbai · Neutrino 2006, Santa Fe, USA Location of the Underground Laboratory • Studies were performed on two potential sites. – Pykara Ultimate