Physics Capabilities of Future - Istituto Nazionale di ... · Physics Capabilities of Future...
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Physics Capabilities of Future
Atmospheric ν-Detectors
Srubabati Goswami
Physical Research Laboratory, Ahmedabad, India
Neutrino Oscillation WorkshopConca Specchiulla, Otranto, Italy
September 9-16, 2012
– p. 1/31
Atmospheric Neutrinos as Source
Cosmic Ray + Aair → π+ + . . .
π+ → µ+ + νµ
µ+ → e+ + νµ + νe
Provides a broad range of energy ascompared to any other natural and artificialsources Provides a wide range of path-length Hence a broad L/E band (1 to 105 km/GeV). The longer baseline allow matter effects todevelop Source of both neutrinos and antineutrinos Source of both νe and νµ
All these for free !!
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Future Detectors for Atm ν
Magnetized Iron Detector (INO) 50 - 100 kT Muon energy measurement, direction reconstruction and chargediscrimination capability Can determine the neutrino energy and direction through Hadronshower reconstruction
Megaton Water Cerenkov Detector (HK, MEMPHYS) Large volume No charge ID Both electron and muon energy and direction measurement
Liquid Argon TPC Excellent electron and muon energy and direction measurement Charge ID ?
Neutrino Telescope (IceCube, PINGU) Huge Volume (Multi-Mton)
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Physics Possibilities with Atmospheric νs
Measurement of |∆m231| and sin2 θ23
Determine if sin2 θ23 is maximal and if not then determination of its octant
Determination of Mass Hierarchy or sgn(∆m231)
CPT violation
Sterile Neutrinos,Non Standard Interactions, Long Range Forces...,
Plan of Talk
Determination of Mass Hierarchy and Octant in magnetized IronCalorimeter and Liquid Argon Detectors
– p. 4/31
Physics Possibilities with Atmospheric νs
An incomplete list of references...
Petcov (1998), Chizov, Maris, Petcov (1998), Akhmedov (1999),Akhmedov,Dighe,Lipari,Smirnov (1999),Kim (1998),Peres,Smirnov(1999),Bernabeu, Palomares-Ruiz, Perez, Petcov, (2002), Gonzalez-Garcia, Maltoni (2003), Bernabeu, Palomares-Ruiz, Petcov (2003), Peres, Smirnov (2004), Indumathi, Murthy (2004), Gandhi, Ghoshal, Goswami, Mehta, Sankar (2004), Gonzalez-Garcia, Maltoni, Smirnov (2004), Palomares-Ruiz, Petcov (2005), Choubey, Roy (2005), Fogli, Lisi, Marrone, Palazzo (2005); Huber, Maltoni, Schwetz (2005), T. Kajita (2005); E. K. Akhmedov, M. Maltoni and A. Y. Smirnov (2005), Petcov, Schwetz (2006), S. Choubey (2006); Indumathi, Murthy, Rajasekaran, Sinha (2006), E. K. Akhmedov, M. Maltoni and A. Y. Smirnov (2007), R. Gandhi, P. Ghoshal, S. Goswami, P. Mehta, S. U. Sankar and S. Shalgar (2007), E. K. Akhmedov, M. Maltoni and A. Y. Smirnov (2008), Gandhi, Ghoshal, Goswami, Sankar (2008), Mena, Mocioiu, Razzaque (2008), Peres, Smirnov (2009), Gandhi, Ghoshal, Goswami, Sankar (2009), Samanta (2006 - 10), Samanta, Smirnov (2010), Conrad, de Gouvea, Shalgar (2010), Gonzalez-Garcia, Maltoni, Salvado (2011), Barger, Gandhi, Ghoshal, Goswami, Marfatia, Prakash, Raut, Sankar (2012), Blennow, Schwetz (2012), Akhmedov, Razzaque, Smirnov (2012), ..........
S. Choubey, Nu2012
– p. 5/31
India Based Neutrino Observatory Proposal
Goal : To build an underground laboratory for science with neutrinophysics as major activity
The Detector: Magnetized Iron CALorimeter detector – (ICAL) fordetection of atmospheric neutrinos in its first phase.
Detector choice based on
Technological capabilities available in the country
Complementarity to Existing/Planned neutrino detectors in the world
Modularity and the possibility of phasing
Compactness and ease of construction
Other Possibilities
Neutrinoless double beta decay, Dark Matter Experiment (DINO)..
Second phase end detector for a beam experiment
International participation is welcome
– p. 6/31
INO: Approval Status
Approvals from Indian Funding Agencies for
Construction of an underground Laboratory and surface facilities atPottipuram village in South India
Construction of 50 kton magnetized Iron Calorimeter detector to studyneutrino properties
Construction of INO center (The National Center for High EnergyPhysics) at Madurai in South India
Human Resource Development
Detector R & D
Completion of project in 6 years
N. Mondal, LP2011
http://www.ino.tifr.res.in
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INO: Location
Bodi West Hills, Pottipuram,
Theni district, Tamil Nadu
9°58’ N and 77°16’ E
110 km from Madurai city •
South India,
of Madurai (has airport)
Flat terrain with good access to major roads
Low rainfall, low humidity
Portal outside the RF boundary, surface facilities not on Forest Land,no clearing of forests required
Environmental and Forest Clearances obtained
26 Hectre Land provided free of cost by state Govt.
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INO: Site at a GlanceT Location of INO & Unique Features
Cavern set in Charkonite Rock under the 1589 m peak;
Vertical cover 1289 m;
Accessible through a 2 km tunnel
Cavern 1 will host 50 kt ICAL ( space for 100 kt);
Other caverns for multiple experiments (0νββ, DM)
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The detector: ICAL@INO
Active Detector Element : Resistive Plate Chambers made of glass
Iron plates Separatd by RPCs
S. Agarwalla, NNN2011
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Salient Feautures of the Detector
Sensitive to muons
Good Energy determination from• Track length• Track curvature in a magnetic field
Directionality from tracking and ns timing resolution
Charge identification from track curvature in magnetic field
Hadron Shower reconstruction enables to determine the neutrino energy
– p. 11/31
Detector R&D Status
Development of RPC Full size RPC’s (2m X 2m ) being fabricated in INO Labs Large scale production developed with the help of Industry
Electronics Designing and Prototyping of electronics, trigger and data acquisitionsystems in progress
Magnet Prototype magnet running at VECC Calcutta
8m × 8m × 20 layers 800 ton engineering module is being planned
– p. 12/31
INO: Simulation Framework at a Glance
!" #$
%$" &
Neutrino Event Generation a+ X -> A + B + ...
Generates particles that result from a random interaction of a neutrino with matter using
theoretical models .
Output:i) Reaction Channelii) Vertex Information
Iii) Energy & Momentum of all Particles
Event SimulationA + B + ... through RPCs + Mag.Field
Simulate propagation of particles through the detector (RPCs + Magnetic Field)
Output:i) x,y,z,t of the particles at their
interaction point in detectorii) Energy deposited
iii) Momentum information
Event Digitisation(x,y,z,t) of A + B + ... + noise + detector efficiency
Add detector efficiency and noise to the hits
Output:i) Digitised output of the previous
stage (simulation)
Event Reconstruction(E,p) of + X = (E,p) of A + B + ...
Fit the tracks of A + B + ... to get their energy andmomentum.
Output:i) Energy & Momentum of the
initial neutrino
N. Mondal, LP2011
– p. 13/31
INO: Simulation Status
Neutrino 2012 Sandhya Choubey June 5, 2012
(GeV)µP0 5 10 15 20 25
µ/P
µP
σ
0.1
0.12
0.14
0.16
0.18
0.2
0.22
0.24=0.35θCos
=0.55θCos
=0.85θCos
Momentum Resolution
(GeV)µP0 5 10 15 20 25
θσ
0.005
0.01
0.015
0.02
0.025
0.03
0.035
0.04
0.045=0.35θCos
=0.55θCos
=0.85θCos
) Resolutionθcos(
(GeV)µP0 5 10 15 20 25
RE
C E
ff
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
=0.35θCos
=0.55θCos
=0.85θCos
Reconstruction Efficiency
(GeV)µP0 5 10 15 20 25
CID
E
ff
0.95
0.96
0.97
0.98
0.99
1
=0.35θCos
=0.55θCos
=0.85θCos
CID Efficiency
INO Collab, 2012
Inhomogeneous magnetic fieldimplemented
Muon energy and directionresolution from tracks achieved –improvements possible
Hadron energy resolution available
Neutrino energy and directionresolution using muon and hadroninformation possible
Optimization of iron plate thicknessin progress
– p. 14/31
Mass Hierarchy Sensitivity
Crux of the matter : Matter Effect
tan 2θ13m =
∆m2
31sin 2θ13
∆m2
31cos 2θ13±2
√2GF neE
For ∆m2atm > 0 matter resonance in neutrinos
For ∆m2atm < 0 matter resonance in anti neutrinos
Experiments sensitive to matter effects can probe the mass hierarchy
Matter effects for ∆m2atm channel depend crucially on θ13
Thus both parameters get related
Large measured θ13 =⇒ good news
Detectors with charge id that can discriminate between neutrinos andantineutrinos can be crucial
– p. 15/31
Matter effect at large baselines0 5 10 15
0
0.2
0.4
0.6
0.8
1
Pµe
NHIH
0
0.2
0.4
0.6
0.8
1
Pµµ
0 5 10 15E (GeV)
0.2
0.4
0.6
0.8
1
Pee
7000 km
0 5 10 15
0
0.2
0.4
0.6
0.8
1
Pµe
NHIH
0
0.2
0.4
0.6
0.8
1
Pµµ
0 5 10 15E (GeV)
0
0.2
0.4
0.6
0.8
1
Pee
10000 km
Large matter effects at long baselines in both µ and e events =⇒Hierarchy Sensitvity
νµ survival probability can rise or fall in matter
Energy and angular smearing important
– p. 16/31
Atmospheric Neutrinos at INO
Sensitive only to Muons
Differential Number of Muons
d2Nµ
dΩmdEm
=1
2π
∫ 100
1
dEt
∫
dΩtR(Et, Em)R(Ωt, Ωm)[ΦdµPµµ + Φd
ePeµ]σǫ
Energy and Angular Smearing Functions
R(Ωt, Ωm) = N exp
[
− (θt − θm)2 + sin2 θt(φt − φm)2
2(∆θ)2
]
.
R(Em, Et) =1√2πσ
exp
[
− (Em − Et)2
2σ2
]
.
Simplest ApproachUse fixed widths for energy and angular smearing
– p. 17/31
Effect of Smearing on muon χ2
5 10 15 20angular resolution (degree)
0
10
20
30
40
50
χ2 µ + χ
2 µ
5 10 15 20energy resolution (%)
0
10
20
30
40
50
15% energy resolution 10o angular resolution
INO, 1 Mt yr INO, 1 Mt yr
With increased energy or angular smearing the χ2 for muon like eventsdecrease.
Effect of energy smearing is more
R. Gandhi, P. Ghoshal, S.G., P. Mehta, S. Shalgar, S. Umashankar, PRD, 2007
Also, T. Schwetz and S.T. Petcov, Nucl. Phys. B, 2006
– p. 18/31
Hierarchy Sensitivity at INO
Events generated from NUANCE (50 kT, 10 yr exposure)
Two sets of energy/angular resolutions:’high’ (10%, 10o) and ’low’(15%, 15o)
Energy threshold 2 GeV, charge ID 100%, constant reconstructionefficiency 85%
True normal hierarchy, (θ23)tr = 45o, δCP = 0, (sin2 2θ13)tr = 0.1,∆m2
31 = 2.4 × 10−3 eV2, ∆m221 = 7.8 × 10−5 eV2, sin2 θ12 = 0.31
Res set χ2marg,no−pri χ2
marg,pri χ2fp
Low 1.5 3.1 4.5
High 5.4 8.2 9.7
Using Projected priors: ∆m231 = 2%, sin2 θ23 = 0.006 and fixed θ13
> 2σ to ∼ 3σ sensitivity to mass Hierarchy in 10 years
See also Blenow and Schwetz, 2010
– p. 19/31
Hierarchy Sensitivity from INO simulation
Using 50 Kton detector and events generated from NUANCE
Using ICAL resolutions in Muon energy and Zenith Angle
Using efficiency and Charge-ID from ICAL simulations
~2σ sensitivity for sin2θ =0.5, sin22θ =0.1 by 2022 (5 yrs)
θ
6 8 10 12 14 16 18 20
Years
0
2
4
6
8
10
12
14
16
18
20
22
24
!2
sin22"
13=0.1
sin22"
13=0.08
sin22"
13=0.12
3#
2#
Inverted Hierarchy
Marginalized over Δm2atm & θ23
with priors with projected errors
INO Preliminary INO Preliminary
6 8 10 12 14 16 18 20
Years
0
2
4
6
8
10
12
14
16
18
20
22
24
!2
sin22"
13=0.1
sin22"
!"#$%!&
sin22"
13=0.08
3#
2#
INO Preliminary
Normal HierarchyMarginalized over Δm2
atm & θ23
with priors with projected errors
INO Collab, 2012
True Values:∆m2
31 = 2.4 × 10−3 eV2
sin2 θ23 = 0.5
∆m221 = 7.8 × 10−5 eV2
sin2 θ12 = 0.31
δCP = 0
For sin2 2θ13 = 0.1 χ2proj−pri = 6.97 ∼ 2.7 σ sensitivity in 10 years
(Using Projected priors: ∆m231 = 2%, sin2 θ23 = 0.006 and fixed θ13)
– p. 20/31
Effect of δCP on hierarchy sensitivity
δ
δ
0 0.5 1 1.5 2
cp!
5
10
"#
2
all parameters are fixed
sin22$
13=.1
INO PreliminaryINO Preliminary
INO Collab, 2012
0 0.5 1 1.5 2δ [π]
0
5
10
15
∆χ
2 of
wro
ng m
ass
orde
ring
0
5
10
15
INO low resolution
INO high resolution
NOvA
Data simulated for NH and δCP = 0 and fitted for IH with varying δCP
MH sensitivity with atmospheric neutrinos almost independent of δCP
Complementarity with LBL experiments
– p. 21/31
Octant sensitivity in Pµµ
1 2 3 4 5 6 7 8 9 10 1 2 3 4 5 6 7 8 9 10
0
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1
1 2 3 4 5 6 7 8 9 10
P!!
E (GeV)
394551
0
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1
1 2 3 4 5 6 7 8 9 10
E (GeV)
394551 D ≡ 1/2 − sin2 θ23
|D| gives the deviation ofsin2 θ23
sgn(D) gives the octant ofsin2 θ23
NH, ν-resonance IH, anti-ν-resonance
Pmµµ ∼ sin4 θ23sin
2 2θm13 sin2 (1.27∆m
31L/E)
Octant sensitvity from the sin4 θ23 termS.Choubey. and P. Roy hep-ph/0509197
Indumathi,Murthy, Rajasekaran,Sinha hep-ph/0603264
– p. 22/31
Octant Sensitivity at INO
Events generated from NUANCE (50 kT, 10 yr exposure)
Results for ’high’ (10%, 10o) resolutions
Energy threshold 2 GeV, charge ID 100%, reconstruction efficiency 85%
39 40 41 42 43 44 45true θ
23
0
1
2
3
4
5
6
χ2 tot
Without priorWith prior
45 46 47 48 49 50 510
1
2
3
4
5
6
2 σ
True ParametersNormal Hierarchy(θ23)tr = 45o,δCP = 0,(sin2 2θ13)tr = 0.1,∆m2
21 = 7.8 × 10−5 eV2
sin2 θ12 = 0.31
< 2σ sensitvity for |θ23 − π/4| > 5
Analysis using INO simulation code in progress
– p. 23/31
Magentized Liquid-Ar TPC
50-100 Kton Magnetized LiqAr detector –
Energy threshold 1 GeV
Sensitive to both muons and electrons
100% CID for muons and 20% for electrons in the energy range 1-5 GeV
σEe= σEµ
= 0.01; σEhad=
√
(0.15)2/Ehad + (0.03)2
σEν=
√
(σEl)2 + (0.15)2/(yEν) + (0.03)2;
y → average rapidity = 0.45
σθe= 1.72; σθµ
= σθhad= 2.29; σθνe
= 2.8; σθνµ= 3.2
Barger,Gandhi,Ghosal,Goswami,Marfatia,Prakash,Raut,Umashankar, Phys. Rev.Lett., 2012
– p. 24/31
Hierarchy and Octant with electron events
excess of electron-like events:
Ne
N0e
− 1 ≃ (r s2
23− 1)P2ν(∆m2
31, θ13) θ13-effects
+ (r c2
23− 1)P2ν(∆m2
21, θ12) ∆m
2
21-effects
− 2s13s23c23 r Re(A∗
eeAµe) interference: δCP
r =F 0
µ
F 0e→ the flux ratio
0 0.02 0.04 0.06 0.08 0.1
sin22θ
13
1
1.1
1.2
1.3
1.4
Ne /
Ne0 f
or m
ulti-
GeV
eve
nts normal
sin2θ
23 = 0.64
sin2θ
23 = 0.36
normal
inverted
inverted
0.84 < cosθν
nadir < 1
Bernabeu, Palomares-Ruiz, Petcov, hep-ph/0305152
Resonant matter effect in P2ν(∆m231, θ13) for
multi-GeV neutrinos .
NH – neutrinos IH - antineutrinos
All three terms important for sub-GeVneutrinos
Sensitivity to both Hierarchy and Octant
– p. 25/31
Hierarchy Sensitivity using LiqAr TPC
0
10
20
30
40
0.04 0.06 0.08 0.1 0.12
χ2to
tpri
or
true sin2 2θ13
Liquid argon (250 kT yr), marginalized hierarchy sensitivity
|∆m2
31|tr = 0.0024 eV2, true NH, test IH
3σ sensitivity
DB RENO
sin2 θ23=0.5, no charge-id
sin2 θ23=0.4
sin2 θ23=0.5
sin2 θ23=0.6
0
10
20
30
40
0.04 0.06 0.08 0.1 0.12
χ2to
tpri
or
true sin2 2θ13
Liquid argon (250 kT yr), marginalized hierarchy sensitivity
|∆m2
31|tr = 0.0024 eV2, true IH, test NH
3σ sensitivity
DB RENO
sin2 θ23=0.5, no charge-id
sin2 θ23=0.4
sin2 θ23=0.5
sin2 θ23=0.6
χ2 = χ2µ + χ2
µ + (χ2e + χ2
e)1−5GeV + (χ2e+e)5−10GeV + χ2
prior
True values of undisplayed Parameters: (|∆m231|) = 2.4 × 10−3 eV2,
(δCP ) = 0, ∆m221 = 8 × 10−5 eV2, θ12 = 34
Marginalized over all parameters
> 5σ sensitivity for sin2 2θ13 = 0.1 and sin2 θ23 = 0.5
Drastic drop in sensitivity if no CID is assumed.
– p. 26/31
Octant Sensitivity using LiqAr TPC
0
5
10
15
20
40 42 44 46 48 50
χ2to
tpri
or
true θ23
Liquid argon (500 kT yr), marginalized octant sensitivity with priors
|∆m2
31|tr = 0.0024 eV2, NH
3σ sensitivity
2σ sensitivity
sin2 2θ13 (true) = 0.07
sin2 2θ13 (true) = 0.1
0
5
10
15
20
40 42 44 46 48 50
χ2to
tpri
or
true θ23
Liquid argon (500 kT yr), marginalized octant sensitivity with priors
|∆m2
31|tr = 0.0024 eV2, IH
3σ sensitivity
2σ sensitivity
sin2 2θ13 (true) = 0.07
sin2 2θ13 (true) = 0.1
500 Ktyr exposure
NH : 2σ discrimination for |θ23 − π/4| > 3.5 (sin2 2θ23 < 0.985).3σ Discrimination for |θ23 − π/4| > 5
IH : 2σ Discrimination for |θ23 − π/4| > 4 (sin2 2θ23 < 0.985).NH
θ23 χ2cid χ2
no−cid
39 15 12.5
42 3.3 2.8
Not having CIDdoes not affectthe results sodrastically.
IH
θ23 χ2cid χ2
no−cid
39 7.1 5.1
43 2.8 1.2
– p. 27/31
Conclusion
In view of large θ13 determination of of mass hierarchy and octant usingmatter effect in atmospheric neutrinos look very promising
INO a strong contender because of the possibility of magnetization andcharge identification
∼ 3σ sensitvity to mass hierarchy in 10 years for 50 kton detector
Hierarchy sensitivity from atmospheric neutrinos independent of δCP
Complimentary information to Long Baseline Experiments..
INO R&D going on full swing
Liquid Argon detectors with charge-id provides excellent hierarchysensitivity > 5σ for 250 ktyrs
Non-Magnetized LArTPC would necessarily need larger volume/exposure
Other possibilities ..CPT violation, Sterile Neutrinos,NSI, .....
– p. 28/31
AcknowledgementsINO collaboration
INO CollaborationAhmadabad: Physical Research Lab.
Aligarh: Aligarh Muslim University
Allahabad: HRI
Calicut : University of Calicut
Chandigarh: Panjab University
Chennai : IIT, Madras IMSc
Delhi : University of Delhi
Guwahati : IIT, Guwahati
Hawaii (USA) : University of Hawaii
Indore : IIT, Indore
Jammu : University of Jammu
Kalpakkam : IGCAR
Kolkata : Ramakrishna Mission Vivekananda University, SINP, VECC , University of Calcutta
Lucknow : Lucknow University
Madurai : American College
Mumbai : BARC
Mumbai : IIT, Bombay TIFR
Mysore : University of Mysore
Sambalpur : Sambalpur University;
Sr inagar : University of Kashmir
Varanasi : Banaras Hindu University
Special Thanks : Animesh Chatterjee, Sandhya Choubey,AnushreeGhosh, Pomita Ghoshal, Sushant Raut, Nita Sinha, Tarak Thakore
– p. 29/31
INO: Timeline
Neutrino 2012 Sandhya Choubey June 5, 2012N. Mondal, LP2011
– p. 30/31
Background
A preliminary study using a GEANT based simulation of cosmic ray muonbackground in INO shows that these are unlikely to mimic the signal
Indumathi and Murthy, hep-ph/0407336
NC background: the 6 cm thickness of the iron plates is sufficient toabsorb any pions and kaons in the 1−10 GeV range before they candecay.
Oscillated ντ induced muons softer in energy and can be eliminated bysuitable energy cuts
Agarwalla, Raychaudhuri, Samanta, hep-ph/0505015
– p. 31/31