impact of large q 13 on long-baseline measurements at pingu
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Impact of large q 13 on long-baseline measurements at PINGU. PINGU Workshop Erlangen university May 5, 2012 Walter Winter Universität Würzburg. TexPoint fonts used in EMF: A A A A A A A A. Contents. Introduction Oscillation physics using a core-crossing baseline - PowerPoint PPT PresentationTRANSCRIPT
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Impact of large 13 on long-baseline measurements at PINGU
PINGU WorkshopErlangen universityMay 5, 2012
Walter Winter
Universität Würzburg
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Contents
Introduction Oscillation physics using a core-crossing
baseline Neutrino beam to PINGU:
Beams and detector parameterization Detector requirements for large 13
Matter density measurement? Summary
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Three flavor mixing
Use same parameterization as for CKM matrix
Pontecorvo-Maki-Nakagawa-Sakata matrix
( ) ( ) ( )= xx
(sij = sin ij cij = cos ij)
Potential CP violation ~ 13
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13 discovery 2012
First evidence from T2K, Double Chooz Discovery (~ 5) independently (?)
by Daya Bay, RENO
(from arXiv:1204.1249)
1 error bars
Daya Bay 3
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Three flavors: 6 params(3 angles, one phase; 2 x m2)
Describes solar and atmospheric neutrino anomalies, as well as reactor antineutrino disapp.!
Three flavors: Summary
Coupling: 13
Atmosphericoscillations:Amplitude: 23
Frequency: m312
Solaroscillations:Amplitude: 12
Frequency: m212
Suppressed
effect: CP
(Super-K, 1998;Chooz, 1999; SNO 2001+2002; KamLAND 2002;Daya Bay, RENO 2012)
MH?
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Consequences
Parameter space for CP starts to become constrained; MH/CPV difficult (need to exclude CP=0 and )
Need new facility!
Huber, Lindner, Schwetz, Winter, 2009
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Mass hierarchy measurement?
Mass hierarchy [sgn(m2)] discovery possible with atmospheric neutrinos? (liquid argon, HyperK, MEMPHYS, INO, PINGU?, LENA?, …)
Barger et al, arXiv:1203.6012;Smirnov‘s talk!
However: also long-baseline proposals! (LBNO: superbeam ~ 2200 km – LAGUNA design study; CERN-SuperK ~ 8870 km – Agarwalla, Hernandez, arXiv:1204.4217)
Perhaps differentfacilities for MH and CPV
proposed/discussed?
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Oscillation physics using a core-crossing baseline
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Matter profile of the Earth… as seen by a neutrino
(PR
EM
: Prelim
inary R
eference E
arth M
odel)
Core
Innercore
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Beams to PINGU? Labs and potential detector locations (stars) in
“deep underground“ laboratories: (Agarw
alla, Hu
ber, Tang, W
inter, 2010)
FNAL-PINGU: 11620 kmCERN-PINGU: 11810 kmRAL-PINGU: 12020 kmJHF-PINGU: 11370 km
All these baselines cross the Earth‘s outer core!
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Matter effect (MSW) Ordinary matter:
electrons, but no , Coherent forward
scattering in matter: Net effect on electron flavor
Hamiltonian in matter (matrix form, flavor space):
Y: electron fraction ~ 0.5
(electrons per nucleon)
(Wolfenstein, 1978; Mikheyev, Smirnov, 1985)
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Parameter mapping (two flavors)
Oscillation probabilities invacuum:matter:
Matter resonance: In this case: - Effective mixing maximal- Effective osc. frequency minimal
For appearance, m312:
- ~ 4.7 g/cm3 (Earth’s mantle): Eres ~ 7 GeV- ~ 10.8 g/cm3 (Earth’s outer core): Eres ~ 3 GeV
Resonance energy:
MH
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Mantle-core-mantle profile
Probability for CERN-PINGU (numerical)
(Parametric enhancement: Akhmedov, 1998; Akhmedov, Lipari, Smirnov, 1998; Petcov, 1998)
Coreresonance
energy
Mantleresonance
energyInter-ference
Thresholdeffects
expected at:2 GeV 5 GeV 10 GeV
Beam energyand detector thresh. have
to pass these!
Is thatpart
useful?
Challenge: Relative size of
CP-termssmaller forlonger L
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Neutrino beam to PINGU?
Beams and detector parameterization
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There are three possibilities to artificially produce neutrinos
Beta decay:Example: Nuclear reactors, Beta beams
Pion decay:From accelerators:
Muon decay:Muons produced by pion decays! Neutrino Factory
Muons,neutrinos
Possible neutrino sources
Protons
Target Selection,focusing
Pions
Decaytunnel
Absorber
Neutrinos
Superbeam
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Considered setups
(for details: Tang, Winter, JHEP 1202 (2012) 028, arXiv:1110.5908; Sec. 3)
Single baseline reference setups:
Idea: similar beam, but detector replaced by PINGU/MICA [need to cover ~ 2 – 5 GeV]:
L [km]
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Want to study e- oscillations Beta beams:
In principle best choice for PINGU (need muon flavor ID only) Superbeams:
Need (clean) electron flavor sample. Difficult? Neutrino factory:
Need charge identification of + and - (normally)
Oscillation channels
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PINGU fiducial volume? In principle: Mton-size detector in relevant ranges:
Unclear how that evolves with cuts for flavor-ID etc. (background reduction); MICA even larger? Use effective detector parameterization to study requirements: Eth, Veff, Eres
(Tang, Winter, JHEP 1202 (2012) 028; Veff somewhat smaller than Jason‘s current results)
Eth
Veff
Eres (E) = E
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Detector paramet.: mis-ID
misIDtracks << misID <~ 1 ?
(Tang, Winter, JHEP 1202 (2012) 028)
misID: fraction of events of a
specific channel
mis-identified as signal
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Detector requirements for large 13
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Superbeam
Mass hierarchy measurement very robust(even with largemisID and totalrates only possible)
Even with much smaller-scale beam?
Existing equipment, such as CNGS? NuMI?
CPV not promising (requires flavor mis-ID at the level of 1%, Veff > 5 Mt, Eres = 0.2 E or better)
(Tang, Winter, JHEP 1202 (2012) 028)
(misIDtracks = 0.01)
Fra
ctio
n of
C
P
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NuMI-like beam to PINGU?
Difference to atmospherics: can even live without energy resolution and cascade ID (NC and added)(if some track ID and systematics controlled)
NuMI
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Beta beam
Similar results for mass hierarchy measurement (easy)
CPV not so promising:
long L, asymmetric beam energies (at least in CERN-SPS limited case
~656 for 8B and =390 for 8Li) although moderate detector requirements
(Tang, Winter, JHEP 1202 (2012) 028)
(misID ~ 0.001, Eth=2 GeV, Eres=50% E, Veff=5 Mt)
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Neutrino factory
No magnetic field, no charge identification Need to disentangle Pe and P by energy
resolution:
(from: Tang, Winter, JHEP 1202 (2012) 028; for non-magnetized detectors, see Huber, Schwetz, Phys. Lett. B669 (2008) 294)
)
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contamination
Challenge:
Reconstructed at lower energies!(Indumathi, Sinha, PRD 80 (2009) 113012; Donini, Gomez Cadenas, Meloni, JHEP 1102 (2011) 095)
Choose low enough E to avoid
Need event migration matrices (from detector simulation) for reliable predictions! (neutral currents etc)
(sin2213=0.1)
(Tang, Winter, JHEP 1202 (2012) 028)
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Precision measurements?
… only if good enough energy resolution ~ 10% E and misID (cascades versus tracks) <~ 1% can be achieved!
(Tang, Winter, JHEP 1202 (2012) 028)
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The BONUS program: Matter density measurement of the Earth‘s core?
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Example: Superbeam
Precision ~ 0.5% (1)
Highly competitive to seismic waves (seismic shear waves cannot propagate in the liquid core!)
(Tang, Winter, JHEP 1202 (2012) 028)
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Conclusions [my personal view]
Superbeams Electron sample (cascades) probably contaminated by other flavors;
therefore precision measurements unlikely Interesting option: Use more or less existing equipment for a
mass hierarchy measurement? (e.g. CNGS/MINOS with new beam line?)
Bonus: matter density measurement of Earth‘s core Unique experiment as low-budget alternative to LBNE?
Neutrino factory Energy resolution critical, since non-magnetized detector Detector simulation needed to produce event migration matrices
for reliable conclusions if Eres ~ 10% E achievable? Beta beams
Intrinsically best-suited for PINGU/MICA: flavor-clean beam, requires muon neutrino flavor-ID
However: need high intensity, high energy 8B-8Li setups for reasonable sensitivities; there are better ways to build a beta beam for large 13 to do both MH+CPV
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Statement of PINGU collaboration needed
now (or never)!?
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BACKUP
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Beams: Appearance channels
(Cervera et al. 2000; Freund, Huber, Lindner, 2000; Akhmedov et al, 2004)
Antineutrinos: Magic baseline:
L~ 7500 km: Clean measurement of 13 (and mass hierarchy) for any energy, value of oscillation parameters! (Huber, Winter, 2003; Smirnov 2006)
In combination with shorter baseline, a wide range of very long baseline will do! (Gandhi, Winter, 2006; Kopp, Ota, Winter, 2008)
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Quantification of performanceExample: CP violation discovery
Sensitive region as a
function of true 13 and CP
CP values now stacked for each 13
Read: If sin2213=10-3, we
expect a discovery for 80% of all values of CP
No CPV discovery ifCP too close to 0 or
No CPV discovery forall values of CP3
~ Precision inquark sector!
Best performanceclose to max.
CPV (CP = /2 or 3/2)
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Effective volume
Difference Eth = 2 GeV, Veff=5 Mt to actual (energy-dependent) fiducial volume:
(Tang, Winter, JHEP 1202 (2012) 028)
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Note:
Pure baseline effect!
A 1: Matter resonance
VL baselines (1)
(Factor 1)2
(Factor 2)2
(Factor 1)(Factor 2)Prop. To L2; compensated
by flux prop. to 1/L2
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Factor 1: Depends on energy; can be matter enhanced for long L; however: the longer L, the stronger change off the resonance
Factor 2:Always suppressed for longer L; zero at “magic baseline” (indep. of E, osc. Params)
VL baselines (2)
(m312 = 0.0025, =4.3 g/cm3, normal hierarchy)
Factor 2 always suppresses CP and solar terms for very long baselines; note that these terms include 1/L2-dep.!