Post on 25-Jul-2020
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Prospects of INO
with Neutrino Beams
Sanjib Kumar Agarwallasanjib@mri.ernet.in
Harish-Chandra Research Institute, Allahabad, India
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.1/56
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Panjab University
!!! Thanks to all of you !!!
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.2/56
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PLAN
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.3/56
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PLAN
Present Status & Missing Links
Game Plan : ν Roadmap
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.3/56
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PLAN
Present Status & Missing Links
Game Plan : ν Roadmap
“Golden Channel”, Peµ
“Eight-fold” degeneracy
“Magic Baseline”
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.3/56
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PLAN
Present Status & Missing Links
Game Plan : ν Roadmap
“Golden Channel”, Peµ
“Eight-fold” degeneracy
“Magic Baseline”
India-Based Neutrino Observatory (INO)
β-beam and ν-factory
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.3/56
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PLAN
Present Status & Missing Links
Game Plan : ν Roadmap
“Golden Channel”, Peµ
“Eight-fold” degeneracy
“Magic Baseline”
India-Based Neutrino Observatory (INO)
β-beam and ν-factory
Results
Conclusions
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.3/56
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Then and Now
Then (1930): Pauli
I have hit upon a desperate remedy to save the
exchange theorem and the conservation of energy.
Namely, the possibility that there could exist
electrically neutral spin 12 particles of small mass . . . .
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.4/56
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Then and Now
Then (1930): Pauli
I have hit upon a desperate remedy to save the
exchange theorem and the conservation of energy.
Namely, the possibility that there could exist
electrically neutral spin 12 particles of small mass . . . .
Now (2004): APS Neutrino Study Group
Much of what we know about neutrinos we have
learned in the last six years. . . . . We have so many
new questions, . . . We are most certain of one thing :
neutrinos will continue to surprise us . . . .
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.4/56
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Past and Present
Neutrino physice, a bit player on the physics stage
in yesteryears, has now donned a central role
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.5/56
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Past and Present
Neutrino physice, a bit player on the physics stage
in yesteryears, has now donned a central role
↓Neutrino oscillations : Firmly established by
solar, atmospheric, reactor and accelerator expts
↓!!! We are now in precision regime !!!
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.5/56
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Past and Present
Neutrino physice, a bit player on the physics stage
in yesteryears, has now donned a central role
↓Neutrino oscillations : Firmly established by
solar, atmospheric, reactor and accelerator expts
↓!!! We are now in precision regime !!!
↓Next generation experiments : planned/proposed
world-wide to further pin down the values of the
oscillation parameters
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.5/56
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Present Status
Parameter Best fit 3σ (1 d.o.f)
∆m221 [10−5 eV 2] 7.6 7.1–8.3
|∆m231| [10−3 eV 2] 2.4 2.0–2.8
sin2 θ12 0.32 0.26–0.40
sin2 θ23 0.50 0.34–0.67
sin2 θ13 0.007 ≤ 0.050
M. Maltoni, T. Schwetz, M.A. Tortola, J.W.F. Valle, hep-ph/0405172v6
Best-fit values under 3 flavour scheme
Data from Solar + Atmospheric +
Reactor (KamLAND and CHOOZ) +
Accelerator (K2K and MINOS) expts
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.6/56
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Unsolved Issues
The sign of ∆m231 (m2
3 −m21) is not known.
Neutrino mass spectrum can be normal or
inverted hierarchical
∆m2
∆m2
∆m
2
12
3
3
12solar {
} solar
atm
osp
he
ric
ma
ss
νe νµ τν
NORMAL INVERTEDHIERARCHYHIERARCHY
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.7/56
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Unsolved Issues (Continued..)
Only an upper limit on
sin2 2θ13 (< 0.17 at 3σ) exists
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.8/56
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Unsolved Issues (Continued..)
The Dirac CP phase (δCP)
is unconstrained
We will focus on the first two issues. . .
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.9/56
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Game Plan : ν Roadmap
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.10/56
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Game Plan : ν Roadmap
1st Step : Transition Era ⇒ Ongoing : 2005-2010 (phase-0)
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.10/56
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Game Plan : ν Roadmap
1st Step : Transition Era ⇒ Ongoing : 2005-2010 (phase-0)
Aim
Improve the precision on the atmospheric
parameters looking at νµ disappearance
Study νµ → ντ to ascertain atm. osc
and first see νµ → νe
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.10/56
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Game Plan : ν Roadmap
1st Step : Transition Era ⇒ Ongoing : 2005-2010 (phase-0)
Aim
Improve the precision on the atmospheric
parameters looking at νµ disappearance
Study νµ → ντ to ascertain atm. osc
and first see νµ → νe
Candidates (Conventional Beam Expts)
K2K (terminated)
MINOS, OPERA (running)
ICARUS (starting soon)
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.10/56
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Game Plan : ν Roadmap
2nd Step : 1-3 mixing Era ⇒ Approved/Proposed : 2008-2015 (phase-1)
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.11/56
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Game Plan : ν Roadmap
2nd Step : 1-3 mixing Era ⇒ Approved/Proposed : 2008-2015 (phase-1)
Aim
Substantiate visibility of θ13 driven
transitions : νµ → νe, νe → νe
Penetrate sin2 2θ13 down to 0.01 (today < 0.17)
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.11/56
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Game Plan : ν Roadmap
2nd Step : 1-3 mixing Era ⇒ Approved/Proposed : 2008-2015 (phase-1)
Aim
Substantiate visibility of θ13 driven
transitions : νµ → νe, νe → νe
Penetrate sin2 2θ13 down to 0.01 (today < 0.17)
Candidates (Superbeam & Reactor Expts)
T2K [Superbeam] (Approved : Starting in 2009)
Noνa [Superbeam] (Proposed : Expected in 2012)
Double Chooz, Daya Bay, Reno, Angra, KASKA, ... [Reactor]
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.11/56
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Game Plan : ν Roadmap
3rd Step : Precision Era ⇒ To be prepared : 2015-2025 (phase-2)
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.12/56
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Game Plan : ν Roadmap
3rd Step : Precision Era ⇒ To be prepared : 2015-2025 (phase-2)
sin2 2θ13 > 0.01 ← Known by 2012 → sin2 2θ13 < 0.01
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.12/56
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Game Plan : ν Roadmap
3rd Step : Precision Era ⇒ To be prepared : 2015-2025 (phase-2)
sin2 2θ13 > 0.01 ← Known by 2012 → sin2 2θ13 < 0.01
sin2 2θ13 > 0.01
We can probe it by
existing facilities
...Keep in mind...
Very small sensitivity to
δCP and neutrino mass
ordering
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.12/56
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Game Plan : ν Roadmap
3rd Step : Precision Era ⇒ To be prepared : 2015-2025 (phase-2)
sin2 2θ13 > 0.01 ← Known by 2012 → sin2 2θ13 < 0.01
sin2 2θ13 > 0.01
We can probe it by
existing facilities
...Keep in mind...
Very small sensitivity to
δCP and neutrino mass
ordering
sin2 2θ13 < 0.01
Beyond the reach of on-
going expts at that time
Pure and more intense
beams with precisely
known spectrum
Larger detectors with
good energy resolution,
granularity, ...
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.12/56
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Game Plan : ν Roadmap
3rd Step : Precision Era ⇒ To be prepared : 2015-2025 (phase-2)
Beta Beam
OR
Neutrino Factory
Do not forget SPL, T2HK, WBB, ...
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.13/56
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Game Plan : ν Roadmap
3rd Step : Precision Era ⇒ To be prepared : 2015-2025 (phase-2)
Beta Beam
OR
Neutrino Factory
Do not forget SPL, T2HK, WBB, ...
They can penetrate sin2 2θ13 down to 0.0001
Excellent sensitivity to δCP and Sgn(∆m231)
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.13/56
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Game Plan : ν Roadmap
3rd Step : Precision Era ⇒ To be prepared : 2015-2025 (phase-2)
Beta Beam
OR
Neutrino Factory
Do not forget SPL, T2HK, WBB, ...
They can penetrate sin2 2θ13 down to 0.0001
Excellent sensitivity to δCP and Sgn(∆m231)
But journey from 0.01 to 0.0001
!!! Very Tough Ask !!!
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.13/56
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Golden Channel (Peµ)
The appearance probability (νe → νµ) in matter, upto second
order in the small parameters α ≡ ∆m2
21/∆m2
31and sin 2θ13,
Peµ ≃ sin2 2θ13 sin2 θ23
sin2[(1− A)∆]
(1− A)2
+ α sin 2θ13 ξ sin δCP sin(∆)sin(A∆)
A
sin[(1− A)∆]
(1− A)
+ α sin 2θ13 ξ cos δCP cos(∆)sin(A∆)
A
sin[(1− A)∆]
(1− A)
+ α2 cos2 θ23 sin2 2θ12
sin2(A∆)
A2;
where ∆ ≡ ∆m2
31L/(4E), ξ ≡ cos θ13 sin 2θ21 sin 2θ23,
and A ≡ ±(2√
2GF neE)/∆m2
31
Cervera et al., hep-ph/0002108
Freund, Huber, Lindner, hep-ph/0105071
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.14/56
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Eight-fold Degeneracy
(θ13, δCP ) intrinsic degeneracy
Burguet-Castell, Gavela, Gomez-Cadenas, Hernandez, Mena,
hep-ph/0103258
(sgn(∆m231), δCP ) degeneracy
Minakata, Nunokawa, hep-ph/0108085
(θ23, π/2− θ23) degeneracy
Fogli, Lisi, hep-ph/9604415
Severely deteriorates the sensitivity
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.15/56
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Problem & Solution
Degeneracies create “Clone” Solutions
Barger, Marfatia, Whisnant, hep-ph/0112119
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.16/56
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Problem & Solution
Degeneracies create “Clone” Solutions
Barger, Marfatia, Whisnant, hep-ph/0112119
Pµe ⇒ SuperBeam
Peµ ⇒ Beta Beam
Peµ ⇒ Neutrino Factory
Need smart ideas to play with these channels
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.16/56
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Solutions
Combine data from appearance expts at
different L and/or different E
Barger, Marfatia, Whisnant, hep-ph/0206038
Barger, Marfatia, Whisnant, hep-ph/0210428
Burguet-Castell et al, hep-ph/0103258
Huber, Lindner, Winter, hep-ph/0211300
Mena and Parke, hep-ph/0408070
and there are others also ...
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.17/56
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Solutions
Add data from different channels
The Silver Channel, Peτ
Autiero et al, hep-ph/0305185
Donini, Meloni, Migliozzi, hep-ph/0206034
The Disappearance Channel, Pµµ
Donini, Fernandez-Martinez, Meloni, Rigolin, hep-ph/0512038
Donini, Fernandez-Martinez, Rigolin, hep-ph/0411402
Adding reactor antineutrino data
Huber, Lindner, Schwetz, Winter, hep-ph/0303232
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.18/56
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Solutions
Adding atmospheric neutrino data
Huber, Maltoni, Schwetz, hep-ph/0501037
Campagne, Maltoni, Mezzetto, Schwetz, hep-ph/0603172
@@@@ One of the most elegant ideas @@@@
Kill the “Clones” at the “Magic” Baseline
Huber, Winter, hep-ph/0301257
Smirnov, hep-ph/0610198
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.19/56
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Magic Baseline
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.20/56
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Magic Baseline
If one chooses : sin(A∆) = 0
The δCP dependence disappears from Peµ
Golden channel enables a clean determination of
θ13 and sgn(∆m231)
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.20/56
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Magic Baseline
If one chooses : sin(A∆) = 0
The δCP dependence disappears from Peµ
Golden channel enables a clean determination of
θ13 and sgn(∆m231)
First non-trivial solution:√
2GF neL = 2π (indep of E)
Isoscalar medium of constant density ρ :
Lmagic[km] ≈ 32725/ρ[gm/cm3]
According to PREM, the “Magic Baseline”
Lmagic = 7600 km
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.20/56
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Resonance in matter effect
The very long CERN - INO baseline provides an
excellent avenue to pin-down matter induced
contributions
In particular, a resonance occurs at
Eres ≡ |∆m2
31| cos 2θ13
2√
2GF Ne
= 7.45 GeV
with |∆m231| = 2.5× 10−3 eV2, sin2 2θ13 = 0.1 and
ρav = 4.17 gm/cc (PREM) for the baseline of 7152 km
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.21/56
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Transition Probability Peµ
1 3 5 7 9 11Energy (GeV)
0
0.25
0.5
P eµ
NHIH
0.00
0.25
0.50
P eµ
L=1000 km L=4000 km
L=10000 kmL=7500 km
1 3 5 7 9 11Energy (GeV)
Agarwalla, Choubey, Raychaudhuri, hep-ph/0610333
Normal .vs. Inverted hierarchy sin2 2θ13 = 0.1
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.22/56
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Transition Probability Peµ
1 3 5 7 9 11Energy (GeV)
0
0.25
0.5
P eµ
sin22θ13=0.1
sin22θ13=0.05
0.00
0.25
0.50
P eµ
L=1000 km L=4000 km
L=10000 kmL=7500 km
1 3 5 7 9 11Energy (GeV)
Agarwalla, Choubey, Raychaudhuri, hep-ph/0610333
Two different values of sin2 2θ13 Normal hierarchy
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.23/56
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Neutrino Observatories
i
Location of main neutrino-related observatories
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.24/56
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INO
The India-based NeutrinoObservatory
The INO/ICAL will be the world’sfirst magnetized large mass iron
calorimeter with interleaved GlassRPC detectors
Funding considerations in final stage
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.25/56
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Location of INO
http://www.imsc.res.in/∼ino/
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.26/56
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ICAL Design
Spokesperson: Prof. N.K. Mondal, TIFR
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.27/56
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INO : 2nd Phase
3.4−4.0
2.6−2.9
12.71−13.1
9.9 − 12.15
4.4−5.6
(11300)FERMI LAB
(7145)CERN
PUSHEP Rammam
JHF(4828)
CERN(6871)
FERMI LAB(10480)
(6556)JHF
Artificial Source
Beta Beam ?
Neutrino Factory ?
Lmagic = 7600 km
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.28/56
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INO
A magnetized Iron calorimeter (ICAL) detector
with excellent efficiency of charge identification
(∼ 95%) and good energy determination
Preferred location is Singara (PUSHEP) in the
Nilgiris (near Bangalore), 7152 km from CERN
A (50+50) Kton Iron detector
Oscillation signal is the muon track
(νe → νµ channel)
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.29/56
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Detector assumptions
Total Mass 50 kton
Energy threshold 1 GeV
Detection Efficiency (ǫ) 80%
Charge Identification Efficiency (fID) 95%
Detector characteristics used in the simulations
All studies assume a Gaussian energy resolution
function with σ = 0.15E
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.30/56
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β-beam vs. ν-factory
Schematic Lay-out
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.31/56
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β-beam vs. ν-factory
Ultimate choice depends on future R&D
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.32/56
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β-beam vs. ν-factory
β-beam
Origin85B → 8
4Be + e+ + νe83Li → 8
4Be + e− + νe
CID (Mag Field)
Not Mandatory
Lumi (useful decays)
1.1× 1018/yr (ν)
2.9× 1018/yr (ν)
Parameters
Boost, γ (50 to 650)
Baseline, L
ν-factory
Origin
µ+ → e+νeνµ
µ− → e−νeνµ
CID (Mag Field)
Mandatory (ICAL)
Lumi (useful decays)
1.2× 1020/yr (1 MW)
4.8× 1020/yr (4 MW)
Parameters
Eµ (20 to 50 GeV)
Baseline, L
! They will draw the punch line in this business !
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.33/56
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What is Beta Beam?
A pure, intense, collimated beam of νe or νe,
essentially background free
P. Zucchelli, Phys. Lett. B 532 (2002) 166
Beta decay of completely ionized, radioactive ions
circulating in a storage ring. No contamination of
other types of neutrinos
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.34/56
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Beta Beam : Ion sources
Ion τ (s) E0 (MeV) f Decay fraction Beam
18
10Ne 2.41 3.92 820.37 92.1% νe
6
2He 1.17 4.02 934.53 100% νe
8
5B 1.11 14.43 600684.26 100% νe
8
3Li 1.20 13.47 425355.16 100% νe
Comparison of different source ions
Low-γ design, useful decays in case of anti-neutrinos
can be 2.9× 1018/year and for neutrinos
1.1× 1018/year
Larger total end-point energy, E0 is preferred
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.35/56
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β-beam flux at INO-ICAL
Flu
xy
r−
11
05
−2
mM
eV
−1
() ν
e 8B
250
350
500
650
CERN − INO
7152 Km
0
0.5
1
1.5
2
2.5
3
0 2 4 6 8 10 12 14 16 18 20
Energy (GeV)
Flu
xy
r−
11
05
−2
mM
eV
−1
() ν
e 8Li
250
350
CERN − INO
500
650
7152 Km
0
1
2
3
4
5
6
7
8
9
0 2 4 6 8 10 12 14 16 18
Energy (GeV)
Agarwalla, Choubey, Raychaudhuri, hep-ph/0610333
Boosted on-axis spectrum of νe and νe
at the INO-ICAL assuming no oscillation
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.36/56
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Event Rates in INO-ICAL
sin2θ132
500 & NH500 & IH350 & NH350 & IH250 & NH250 & IH
8B Neutrino Beam
CERN − INO
0
50
100
150
200
250
0.001 0.01 0.1 0.5
Ev
en
ts i
n 5
ye
ars
sin2θ132
500 & IH500 & NH350 & IH350 & NH250 & IH250 & NH
8Li Anti−neutrino beam
CERN − INO
0
50
100
150
200
250
300
350
0.001 0.01 0.1 0.5
Ev
en
ts i
n 5
ye
ars
Agarwalla, Choubey, Raychaudhuri, hep-ph/0610333
Event rates sharply depend on mass ordering and θ13
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.37/56
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See the “Magic”
Ev
en
ts i
n 5
yea
rs
CERN − INO
B8 & IH
Li8 & NH
B8 & NH
Li8 & IH
sin22θ13 = 0.01
δCP
= 0
0
10
20
30
40
50
60
70
80
250 300 350 400 450 500 550 600 650
γ
Magic Baselinesin 13
22θ = 0.01
sin 1322θ = 0.05
L (km)
Ev
en
ts i
n 5
ye
ars
Normal hierarchy
γ= 500
8B
��������������������������������������������������������������������������������������������������������������������������������������������������������������������������������
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������������������������������������������������
������������������������������������������������
50
100
150
200
250
300
350
400
2000 4000 6000 8000 10000 100 0
Agarwalla, Choubey, Raychaudhuri, 0711.1459
Event rates sharply depend on mass ordering and θ13
Effect of δCP is negligible at magic baseline
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.38/56
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Iso-event curves
100007152
732
4000
8B & NHγ 350=
sin2θ2
13
(deg
ree)
CP
δInputs
sin22
13
CPδ = 0
0.043=θ
10(−2
)
0
50
100
150
200
250
300
350
400
2.5 3.0 3.5 4.0 4.5 5.0 5.5 6.0 6.5 7.0
400010000
732
Inputs
sin22
13
CPδ = 0
0.043=θ8Li & IH
γ = 350
(deg
ree)
CP
δ
sin2θ2
13
7152
10( )−2
0
50
100
150
200
250
300
350
400
2.0 2.5 3.0 3.5 4.0 4.5 5.0 5.5 6.0 6.5
Agarwalla, Choubey, Raychaudhuri, hep-ph/0610333
At CERN-INO distance, the effect of δCP
on the measurement of θ13 is less
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.39/56
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Results
Measurement of sin2 2θ13
Full marginalization over
hierarchy
all oscillation parameters
the normalization factor of the Earth matter
density distribution
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.40/56
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IN
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IN
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IN
Measurement of sin2 2θ13
−4
+ Li8 (γ)B
8 (γ
+ )Li8 (γ)B
8 (γ
/1.67)
CERN − INO
3σ
−3
−2
−1sin
θ22
13
θ
13 sensitivity
250 300 350 400 450 500 550 600 650
γ
10
10
10
10
sin
θ2
13
2
−4
−3
−2
−1
(tru
e)
+ Li8 (γ)B
8 (γ
+ )Li8 (γ)B
8 (γ
/1.67)
CERN − INO
3σ
θ
13 discovery
Conservative
250 300 350 400 450 500 550 600 650
γ
10
10
10
10
Agarwalla, Choubey, Raychaudhuri, 0711.1459
Left panel shows the 3σ sensitivity limit for sin2 2θ13
Right panel shows the 3σ discovery reach for sin2 2θ13
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.41/56
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β-beam Optimization
2000 4000 6000 8000 10000L HkmL
500
1000
1500
2000
2500
3000
Boos
tfacto
rHΓL
1
3
5
7
9
11
Energ
yHGe
VL
18 Ne+6 He, No correlations
GLoBES 2008
10-3.4
10-3.8
10-4
.210-4
.6L�Γ=0
.8
2000 4000 6000 8000 10000L HkmL
500
1000
1500
2000
2500
3000
Boos
tfacto
rHΓL
1
3
5
7
9
11
Energ
yHGe
VL
18 Ne+6 He, Corrs+Degs
L�Γ=0
.8
10-3.4
10-4.2
10-3.8
GLoBES 2008
0 2000 4000 6000 8000 10000L HkmL
200
400
600
800
1000
Boos
tfacto
rHΓL
2
4
6
8
10
12
14
Energ
yHGe
VL
8 B+8 Li, No correlations
GLoBES 2008
L�Γ=2
.6
10-2.4
10-2.8
10-3
.2
10-3
.6
0 2000 4000 6000 8000 10000L HkmL
200
400
600
800
1000
Boos
tfacto
rHΓL
2
4
6
8
10
12
14
Energ
yHGe
VL
8 B+8 Li, Corrs+Degs
GLoBES 2008
10-2.4
10-2.8
Agarwalla, Choubey, Raychaudhuri, Winter, 0802.3621
sin22θ13 sensitivity at 3σ as a function of L and Boost factor γ
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.42/56
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ν-factory Optimization
2000 4000 6000 8000L @kmD
10
20
30
40
50
60
70
80
E Μ@G
eVD
Correlations
GLoBES 2006
2000 4000 6000 8000L @kmD
10
20
30
40
50
60
70
80
E Μ@G
eVD
Degeneracies
GLoBES 2006
2000 4000 6000 8000L @kmD
10
20
30
40
50
60
70
80
E Μ@G
eVD
Statistics
GLoBES 2006
0.5
1
2
5
10
2000 4000 6000 8000L @kmD
10
20
30
40
50
60
70
80
E Μ@G
eVD
Systematics
GLoBES 2006
Huber, Lindner, Rolinec, Winter, hep-ph/0606119
sin22θ13 sensitivity at 5σ, Eµ = 30 GeV , L = 7500 km (Optimal choice)
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.43/56
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Results
Sensitivity to Sgn(∆m231)
Full marginalization over
all oscillation parameters
the normalization factor of the Earth matter
density distribution
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.44/56
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IN
I
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IN
I
NO
IN
Measurement of Sgn(∆m231)
sin
θ2
13
2
−4
+ Li8 (γ)B
8 (γ
+ )Li8 (γ)B
8 (γ
/1.67)
−2
−3
−1(t
ru
e)
NH : TRUE
Mass ordering
CERN − INO
3σ
δCP
(true) = 0
250 300 350 400 450 500 550 600 650
γ
10
10
10
10
−4
−2
−3
−1
sin
θ2
13
2(t
ru
e)
IH : TRUE
+ Li8 (γ)B
8 (γ
+ )Li8 (γ)B
8 (γ
/1.67)
Mass ordering
CERN − INO
3σ
δCP
(true) = 0
250 300 350 400 450 500 550 600 650 10
10
10
10
γ
Agarwalla, Choubey, Raychaudhuri, 0711.1459
Minimum value of sin2 2θ13(true) for which the
the wrong hierarchy can be ruled out at the 3σ C.L.
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.45/56
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IN
β-beam Optimization
0 2000 4000 6000 8000 10000L HkmL
500
1000
1500
2000
2500
3000
Boos
tfacto
rHΓL
1
3
5
7
9
11
Energ
yHGe
VL
18 Ne+6 He, ∆CP HtrueL=Π�2
GLoBES 2008
10-4
10-3.610-3.2
0 2000 4000 6000 8000 10000L HkmL
500
1000
1500
2000
2500
3000
Boos
tfacto
rHΓL
1
3
5
7
9
11
Energ
yHGe
VL
18 Ne+6 He, ∆CP HtrueL=3Π�2
GLoBES 2008
10-4
10-3
.6
10-3
.2
0 2000 4000 6000 8000 10000L HkmL
200
400
600
800
1000
Boos
tfacto
rHΓL
2
4
6
8
10
12
14
Energ
yHGe
VL
8 B+8 Li, ∆CP HtrueL=Π�2
GLoBES 2008
10-2.4
10-2.8
10-3.2
0 2000 4000 6000 8000 10000L HkmL
200
400
600
800
1000
Boos
tfacto
rHΓL
2
4
6
8
10
12
14
Energ
yHGe
VL
8 B+8 Li, ∆CP HtrueL=3Π�2
GLoBES 2008
10-2
.4
10-2
.8
10-3
.2
Agarwalla, Choubey, Raychaudhuri, Winter, 0802.3621
Sensitivity to normal mass ordering at 3σ as a function of L and γ
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.46/56
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ν-factory Optimization
2000 4000 6000 8000
L @kmD
10
20
30
40
50
60
70
80
EΜ@G
eVD
∆CP=0
GL
oB
ES
20
06
sin
22Θ
13<
10-
3.5
sin
22Θ
13<
10-
3
sin
22Θ
13<
10-
2.5
sin
22Θ
13<
10-
2
2000 4000 6000 8000
L @kmD
10
20
30
40
50
60
70
80
EΜ@G
eVD
∆CP=Π�2
GL
oB
ES
20
06
sin
22Θ
13<
10-
4
sin
22Θ
13<
10-
3.5
sin
22Θ
13<
10-
3
sin
22Θ
13<
10-
2.5
2000 4000 6000 8000
L @kmD
10
20
30
40
50
60
70
80
EΜ@G
eVD
∆CP=3Π�2
GL
oB
ES
20
06
sin
22Θ
13<
10-
3.5
sin
22Θ
13<
10-
3
sin
22Θ
13<
10-
2.5
sin
22Θ
13<
10-
2
Huber, Lindner, Rolinec, Winter, hep-ph/0606119
Sensitivity to NH (true) at 3σ, Eµ = 20 to 40 GeV , L = 7500 km (Best)
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.47/56
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An ask : New PhysicsCan upcoming neutrino experiments probe
non-standard interactions (NSI) like 6Rsupersymmetry?
Can they become fatal in attempts to further
sharpen the neutrino properties?
A possible experiment
CERN based β-beam neutrino source
+
The proposed India-based Neutrino Observatory
(INO)
A baseline of ∼ 7152 Km
ν interacts with earth matter ⇒ a possible ground
for NSIS. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.48/56
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Extracting θ13 & sgn(∆m231)
Normal hierarchy
Standard Model
sin2θ2
13
0
20
40
60
80
100
120
140
160
180
0 0.02 0.04 0.06 0.08 0.1 0.12 0.14 0.16 0.18
ev
en
ts i
n 5
ye
ars
Inverted hierarchy
Standard Model
sin22
θ13
0
10
20
30
40
50
60
0 0.02 0.04 0.06 0.08 0.1 0.12 0.14 0.16 0.18
ev
en
ts i
n 5
ye
ars
Adhikari, Agarwalla, Raychaudhuri, hep-ph/0608034
Muon events .vs. sin2 2θ13 for NH and IH. The solid lines
correspond to the SM. The shaded area is covered if the
λ′ couplings are varied over their entire allowed range
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.49/56
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Constraining λ′
0.165
0.095
0.043
Solid & Thin Lines : λ/
λ/
Broken & Thick Lines : 331
λ/
|
0.011
|
Normal hierarchy
2m1
0
20
40
60
80
100
120
140
160
180
0 0.1 0.2 0.3 0.4 0.5 0.6
ev
en
ts i
n 5
yea
rs
0.011
λ/
||
0.165
0.095
Inverted hierarchy
0.043
331
0
10
20
30
40
50
60
0 0.1 0.2 0.3 0.4 0.5 0.6
ev
en
ts i
n 5
ye
ars
Adhikari, Agarwalla, Raychaudhuri, hep-ph/0608034
Event rates .vs. |λ′|, present singly, for NH and IH. The
thick (thin) lines are for |λ′
331| (|λ′
2m1|, m =2,3). The
chosen sin2 2θ13 are indicated next to the curvesS. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.50/56
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Long Range Forces at ICAL
Can upcoming long baseline neutrino ex-
periments probe flavor dependent long
range (LR) leptonic forces, mediated by the
Le − Lµ or Le − Lτ gauge bosons?
Can ICAL play an important role
along this direction?
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.51/56
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IN
Extracting θ13 & sgn(∆m231)
Le
− Lµ= 500γ
B8
NH
sin θ22 13
−2−3−4 −1 0
50
100
150
200
250
300
350SM
SM + 5.5e−54
SM + 5.5e−53
10 10 10 10
Ev
en
ts i
n 5
yea
rs
SM + 1.1e−53
SM + 1.1e−52
Le
− Lµ= 500γ
B8
IH
sin θ22 13
−2−3−4 −1 0
2
4
6
8
10
12
14SM
SM + 5.5e−54
SM + 5.5e−53
10 10 10 10
Ev
en
ts i
n 5
ye
ars
SM + 1.1e−52
SM + 1.1e−53
Coming soon → Agarwalla, Joshipura, Mohanty
Event rates for the normal and inverted mass
hierarchies in the presence of Le − Lµ symmetry with
γ = 500 and neutrino run
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.52/56
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IN
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IN
Constraining Long Range Forces
αeµ
Le
− Lµ= 500γ
B8
NH
0.165
0.095
0.043
0.011
0
50
100
150
200
250
300
1e−54 1e−53 1e−52 5.5e−52
Ev
en
ts i
n 5
yea
rs
αeµ
Le
− Lµ= 500γ
B8
IH
0.165
0.095
0.043
0.011
0
2
4
6
8
10
12
14
1e−54 1e−53 1e−52 5.5e−52
Ev
en
ts i
n 5
yea
rs
Coming soon → Agarwalla, Joshipura, Mohanty
Events vs. αeµ for the NH (left panel) and IH (right
panel) with Le − Lµ symmetry with γ = 500 and ν run.
Chosen sin2 2θ13 are indicated next to the curveS. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.53/56
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References
D. Choudhury, A. Datta,
JHEP 0507:058,2005, hep-ph/0410266
S. K. Agarwalla, A. Raychaudhuri, A. Samanta,
Phys.Lett.B629:33-40,2005, hep-ph/0505015
P. Huber, M. Lindner, M. Rolinec, W. Winter,
Phys.Rev.D74:073003,2006, hep-ph/0606119
R. Adhikari, S. K. Agarwalla, A. Raychaudhuri,
Phys.Lett.B642:111-118,2006, hep-ph/0608034
S. K. Agarwalla, S. Choubey, A. Raychaudhuri,
Nuclear Physics B 771 (2007) 1, hep-ph/0610333
R. Gandhi, W. Winter,
Phys.Rev.D75:053002,2007, hep-ph/0612158
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.54/56
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References (Continued...)
S. K. Agarwalla, S. Choubey, A. Raychaudhuri,
0711.1459
S. K. Agarwalla, S. Choubey, A. Raychaudhuri,
Walter Winter
0802.3621
S. K. Agarwalla, Anjan S. Joshipura, S.
Mohanty
In preparation
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.55/56
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ConclusionsLong baseline neutrino oscillation experiments
using neutrino factories and β-beams hold
promise of refining our knowledge of θ13, δ, and
the sign of ∆m231
! They will draw the punch line in this business !
ICAL at INO will be an admirable choice as a
far detector for a very long baseline experiment,
with a source either in CERN, or in JHF, or
even in Fermilab
A magnetized iron calorimeter detector like INO
is essential for Neutrino Factory and its
performance with Beta Beam is quite impressive
S. K. Agarwalla Panjab University, Chandigarh, India 29th February, 08– p.56/56