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Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
Neutrino LBL Experiments and Guidancefrom Theory
Nu Horizons VII, 21-23 Feb 2018, Harish-ChandraResearch Institute, Allahbad, India
Mary BishaiBrookhaven National Lab
February 20, 2018
1 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
Outline
1 Constraining 3-Flavor νSMCPV and δcp
Unitarity tests
2 Physics Beyond ν SMLBL and SterileNSIOther νBSM
3 Future LBL and νBSM
4 What to do with ND’s
5 Conclusion
2 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
Overview of Accelerator Long-Baseline Experiments
For 50 kton.years∗ of exposure. No detector effectsExperiment Baseline νµ → νµ νµ → ντ νµ → νe
δCP rangeCurrent Experiments
T2K 295km (off-axis)30 GeV, 750 kW
9× 1020 POT/year 900 < 1 40 - 70MINOS LE 735km120 GeV, 700 kW
6× 1020 POT/year 11,000 115 230-340NOνA 810km (off-axis)120 GeV, 700 kW
6× 1020 POT/year 1500 10 120 - 200
Future Experiments
LBNF/DUNE LE† 1,300km80 GeV, 1.1MW
1.5× 1021 POT/year 4300 160 350 - 600
LBNF/DUNE ME† 1,300km120 GeV, 1.2MW
1.1× 1021 POT/year 12,000 690 290 - 430T2HK (see T2K numbers)30 GeV, 1.3 MW∗ Facility duty factor taken into consideration† 2012 LBNE CDR Reference Design with NuMI style focusing
Even with maximal CP, event rate is ≤ 10 νµ → νe per kT.MW.yr3 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
Latest from NOνA and T2K
T2K
2.2× 1021 P.O.TNOνA
4 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
Latest Results on δcp (Global Fits)
P. F. de Salas et. al. arXiv 1708.01186 (Aug 2017):— 99% CL — 90% CL
The current results favor maximal CP at NH5 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
T2K+NOνA CPV Prospects
T2K (7.8× 1021 POT ) and NOνA (1.8× 1021 POT) combined,exclusion of δcp = 0 at 90% C.L. (K. Abe et. al.PTEP 2015 (2015) no.4, 043C01;
arXiv:1409.7469):Normal Hierarchy
6 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
T2K+NOνA CPV Prospects
T2K (7.8× 1021 POT ) and NOνA (1.8× 1021 POT) combined,exclusion of δcp = 0 at 90% C.L. (K. Abe et. al.PTEP 2015 (2015) no.4, 043C01;
arXiv:1409.7469):Inverted Hierarchy
7 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
T2K II
Y, Fujii, NBI2017Maxmimal CPV > 3σ within our sights!
How does this change the physics goals from next gen. LBL ?
8 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
Tokai to HyperKamiokande (T2HK)
Hyper-Kamiokande water Cherenkovdetector: 60m tall X 74m diameter186 kton fiducial (10x SuperK)40,000 HQE 20” PMTs295 km baseline
1.3 MW from JPARC starting 2024
Budget request submitted to startconstructionin FY2018. Data takingstarts 2026 same timeline as DUNE
Optional 2nd detector in Kamioka ORKorea at ∼ 1000 km baseline.
Signal candidate events: 186 kton, 1.3MW x 10 years, ν : ν̄ = 1 : 3
If CPV maximal will reach well over 5σ sensitivity9 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
Long Baseline ν Facility (LBNF) and DeepUnderground ν Experiment (DUNE)
GOAL: Precision measurements of the parameters that governνµ → νx and νµ → νx to determine δCP, sign of ∆m2
31, octant of θ23.
Long baseline experiment with atunable wide-band beam and a1300km baseline from Fermilab tothe Sanford Underground ResearchFacility in Lead, SD.
Baseline (km)500 1000 1500 2000 2500 3000
Req
uir
ed E
xpo
sure
(kt
-MW
-yr)
0
500
1000
1500
2000
2500
3000
CoverageCPδ CPV with 75% σExposure to reach 3
NH (IH considered)
M. Bass et. al. Phys.Rev. D91 (2015) 052015
Highly capable multi-purpose Near Detector at Fermilab
40 kton fiducial Liquid Argon TPC Far Detector (80 kton total).Both single and dual-phase LArTPC options under consideration.
10 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
DUNE Event Spectra Exposure: 150 kT.MW.yr (equal ν/ν̄) 1MW.yr = 1× 1021
p.o.t at 120 GeV. (sin2 2θ13 = 0.085, sin2 θ23 = 0.45, δm231 = 2.46× 10−3 eV2)
930 νe, 5 ν̄e, 204 νbeame , 17 NC, 19 ντ , 3 νµ 154 ν̄e,32 νe, 98 νbeam
e , 7 NC, 8 ντ , 1 νµ
8329 νµ, 192 ν̄µ, 72 NC, 29 ντ 2420 ν̄µ, 791 νµ, 33 NC, 13 ντ
Simultaneous fit to all four samples. Richness of spectral informationin both νµ and ν̄µ ⇒ explicit demonstraction of CPV
11 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
DUNE Event Spectra Exposure: 150 kT.MW.yr (equal ν/ν̄) 1MW.yr = 1× 1021
p.o.t at 120 GeV. (sin2 2θ13 = 0.085, sin2 θ23 = 0.45, δm231 = 2.46× 10−3 eV2)
1171 νe,3 ν̄e, 204 νbeame , 17 NC, 19 ντ , 3 νµ 94 ν̄e,39 νe, 98 νBeam
e , 7 NC, 8 ντ , 1 νµ
8329 νµ, 192 ν̄µ, 72 NC, 29 ντ 2420 ν̄µ, 791 νµ, 33 NC, 13 ντ
Simultaneous fit to all four samples. Richness of spectral informationin both νµ and ν̄µ ⇒ explicit demonstraction of CPV
12 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
DUNE CP Sensitivity
With 550 kT.MW.yr ≥ 5σ sensitivity for 50% δcp
With 850 kT.MW.yr ≥ 3σ sensitivity for 75% δcp
π/CP
δ1 0.8 0.6 0.4 0.2 0 0.2 0.4 0.6 0.8 1
2χ
∆ =
σ
0
2
4
6
8
10
12
CP Violation Sensitivity
π/CP
δ1 0.8 0.6 0.4 0.2 0 0.2 0.4 0.6 0.8 1
2χ
∆ =
σ
0
2
4
6
8
10
12DUNE CPV Sensitivity
Normal Hierarchy
= 0.08513
θ22
sin
= 0.4523θ2
sin
σ3
σ5
No Energy Scale Unc.
1% Energy Scale Unc.
2% Energy Scale Unc.
5% Energy Scale Unc.
CP Violation Sensitivity
Exposure (ktMWyears)0 200 400 600 800 1000 1200 1400
2χ
∆ =
σ
0
1
2
3
4
5
6
7
8
9
50% CP Violation Sensitivity
DUNE Sensitivity
Normal Hierarchy
= 0.08513
θ22
sin
= 0.4523θ2
sin
CDR Reference Design
Optimized Design
1%⊕5%
2%⊕5%
3%⊕5%
50% CP Violation Sensitivity
13 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
DUNE Physics νSM Milestones (NH)
Even if CP is maximally violated → several years to 5σ discovery
14 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
How well do we need to know δcp?
T2HK
For maximal CPV - how well should we know σ(δcp)? ν/ν̄ separately ?
15 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
How well do we need to know θ23?
Exposure (ktMWyears)0 200 400 600 800 1000 1200 1400
Reso
luti
on
23
θ2sin
0
0.005
0.01
0.015
0.02
0.025
0.03
0.035
0.04
Resolution23θ2sin
DUNE Sensitivity
Normal Hierarchy
= 0.08513θ22sin
= 0.4523
θ2sin
Resolution23θ2sin
HyperK Octant (Atmospheric) DUNE θ23 resolution (beam)
We need to resolve the θ23 octant - but what about the resolution?
16 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
Unitarity tests (?): θ13 Measurements
Exposure (ktMWyears)0 200 400 600 800 1000 1200 1400
Res
olut
ion
13θ22
sin
0
0.002
0.004
0.006
0.008
0.01
0.012
0.014
0.016
0.018
0.02
Resolution13θ22sin
DUNE Sensitivity
Normal Hierarchy
= 0.08513θ22sin
= 0.4523
θ2sin
Resolution13θ22sin
DUNE can eventually reach same σ(θ13) as reactors
Is this useful? How far should we push on this?
17 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
Unitarity tests (?) : νµ → ντ
Recent results from SuperKamiokande (arXiv:1711.09436):
ντ appearance experimentally v. challenging
HyperK atmospheric data will add a lot more statistics
18 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
The LBNF Beamline for DUNE
Initial conceptual design was of a tunable wide-band NuMI-stylefocusing:
(GeV)νE 0 2 4 6 8 10 12 14 16 18 20
CC
ev
en
ts/G
eV
/10
kt/
MW
.yr
µ ν
0
100
200
300
400
500
600
700
800
Low Energy Tune
Medium Energy Tune
High Energy Tune
LBNF Beam Tunes
LBNF has switched to CPV optimized focusing design with 3 horns !
19 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
ντ Appearance in DUNE
Use LBNF CD1R reference design, NuMI-like focusing with 2 horns,230kA and change tune by varying target and horn distances, horncurrents and sizes. No detector effects included!
2015 two horn optimized design Ep = 66 GeV:
GeVνE 0 2 4 6 8 10 12 140
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1 (Events/GeV/kt/1e20 pot.)σ × P × Φ
p.o.t)10
/2x102/GeV/m ν) (µν(ΦUnoscillated
) x 10e ν → µ νP(
/GeV) 2 cm -38
/E (10 σ CC e ν
)2 cm -38
(10 σ × P
Appearance at 1300 kme ν → µ ν
GeVνE 0 5 10 15 20 25 300
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1 (CC Events/GeV/kt/1e20 pot.)σ × P × Φ
(QE Events/GeV/kt/1e20 pot.)σ × P × Φ
p.o.t)10
/2x102/GeV/m ν) (µν(ΦUnoscillated
) τ ν → µ νP(
/GeV) 2 cm -38
/E (10 σ CC τ ν
)2 cm -38
(10 σ ×P
Appearance at 1300 kmτ ν → µ ν
νµ → νe 292 events νµ → ντ 60 eventsin 40 ktons, 1 year at 1.2 MW
Increase ντ appearance 10x!!!
Increase high energy νe appearance - good for BSM searches20 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
ντ Appearance in DUNE
Use LBNF CD1R reference design, NuMI-like focusing with 2 horns,230kA and change tune by varying target and horn distances, horncurrents and sizes. No detector effects included!
LBNF target -2m from horn 1, NuMI focusing 230 kA, horns 17m apart
GeVνE 0 2 4 6 8 10 12 140
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1 (Events/GeV/kt/1e20 pot.)σ × P × Φ
p.o.t)10
/2x102/GeV/m ν) (µν(ΦUnoscillated
) x 10e ν → µ νP(
/GeV) 2 cm -38
/E (10 σ CC e ν
)2 cm -38
(10 σ × P
Appearance at 1300 kme ν → µ ν
GeVνE 0 5 10 15 20 25 300
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1 (CC Events/GeV/kt/1e20 pot.)σ × P × Φ
(QE Events/GeV/kt/1e20 pot.)σ × P × Φ
p.o.t)10
/2x102/GeV/m ν) (µν(ΦUnoscillated
) τ ν → µ νP(
/GeV) 2 cm -38
/E (10 σ CC τ ν
)2 cm -38
(10 σ ×P
Appearance at 1300 kmτ ν → µ ν
νµ → νe 330 events νµ → ντ 700 eventsin 40 ktons, 1 year at 1.2 MW
Increase ντ appearance 10x!!!
Increase high energy νe appearance - good for BSM searches21 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
Challenges for ντ Appearance
Experimental constraints:
We dont have a 100kton OPERA detector!.
HyperK will significantly increase the statistical significance ofthe atmospheric appearance but almost no L/E resolution.
DUNE has better E resolution for beam ντ appearance. Howgood? How to handle huge νµ,e CC and NC backgrounds?
DUNE tunable beam is NO LONGER reference design. Needstrong theory and experimental input to convince beam projectto enable deployment of a HE option ASAP!!!!.
Theory challenges
What is the expected ντ cross-section? New data on νµcross-sections is/is not included in “latest” predictions of ντ?
Xsec predictions on different targets (H2O and Ar)
We need better understanding of the nuclear models andintranuclear effects both for νµ and ντ
Theoretical uncertainties on ντ xsecs ?
22 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
Physics Beyond ν SM in Long-Baseline Oscillations
Due to the very small masses and large mixing of neutrinos, theiroscillations over a long distance act as an exquisitely precise interfer-ometer with high sensitivity to very small perturbations (W. Marciano,BNL) caused by new physics phenomena, such as:
sterile neutrino states that mix with the three known activeneutrino states
nonstandard interactions in matter that manifest inlong-baseline oscillations as deviations from the three-flavormixing model
new long-distance potentials arising from discrete symmetriesthat manifest as small perturbations on neutrino andantineutrino oscillations over a long baseline
large compactified extra dimensions from String Theorymodels that manifest through mixing between theKaluza-Klein states and the three active neutrino states
We need more guidance from theory
23 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
Impact of Sterile Neutrinos on Long-Baseline νOscillations
L/E (km/GeV)-210 -110 1 10 210 310 410
Pro
babi
lity
0
0.2
0.4
0.6
0.8
1
1.2
2 = 0.05 eV412m∆
)µν→µνStd. Osc. P( 5)×)(eν→µνP(
)µν→µνP()τν→µνP(
)sν→µν1-P(
ND FD
Neutrino Energy (GeV)-110110210
Neutrino Energy (GeV)-110110210
A. Sousa, U. Cinncinati
24 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
Impact of Sterile Neutrinos on Long-Baseline νOscillations
L/E (km/GeV)-210 -110 1 10 210 310 410
Pro
babi
lity
0
0.2
0.4
0.6
0.8
1
1.2
2 = 0.50 eV412m∆
)µν→µνStd. Osc. P( 5)×)(eν→µνP(
)µν→µνP()τν→µνP(
)sν→µν1-P(
ND FD
Neutrino Energy (GeV)-110110210
Neutrino Energy (GeV)-110110210
A. Sousa, U. Cinncinati
25 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
Impact of Sterile Neutrinos on Long-Baseline νOscillations
L/E (km/GeV)-210 -110 1 10 210 310 410
Pro
babi
lity
0
0.2
0.4
0.6
0.8
1
1.2
2 = 5.0000 eV412m∆
)µν→µνStd. Osc. P( 5)×)(eν→µνStd. Osc. P(
)µν→µνP()τν→µνP(
)sν→µν1-P(
ND FD
Neutrino Energy (GeV)-110110210
Neutrino Energy (GeV)-110110210
A. Sousa, U. Cinncinati
26 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
CP Asymmetry 3-flavor and with a Sterile Neutrino∆m2
41 ∼ 1 eV2
The integrated CP asymmetry at the DUNE/LBNF baseline of1300km :
(D. Dutta et. al. JHEP 1511 (2015) 039; arXiv:1508.06275)
Observation of a CP asymmetry is not sufficient to determine its origin.27 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
Latest Results on Sterile Searches
Daya Bay fuel evolution result:
There is NO Reactor Anomaly. Theory must move on.
28 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
Latest Results on Sterile Searches
Latest from MINOS/MINOS+:
νµ disappearance is experimentally “clean”
Exclusion of νe appearance hints is a strong constraint.
29 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
Non-Standard Interactions
30 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
Non-Standard Interactions
NSI could also impact CPV interpretation in long-baseline:
(M. Masud, A. Chatterjee, P. Mehta arXiv:1510.08261)
31 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
Beyond νSM: Large Extra Dimensions
Phys.Rev. D84 (2011) 013003:
Requires wide-band, detailed spectral information at higher energies
32 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
Beyond νSM: Long Range Interactions
Phys.Rev. D84 (2011) 013009Modifies P(νµ → νµ)Example at 1300km baseline with α′ = 1.0, 0.5, 0.1× 10−52
corresponding to thick solid, dashed, and dotted curves, respectively:
Requires long baselines and detailed spectral information
33 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
Recent Results on ν BSM Searches in LBL Expts
“New Constraints on Sterile Neutrinos with MINOS/MINOS+ andDaya Bay” e-Print: arXiv:1705.05064
“Search for active-sterile neutrino mixing using neutral-currentinteractions in NOvA” NOvA Collaboration (P. Adamson (Fermilab)et al.) Phys.Rev. D96 (2017)
“Search for flavor-changing nonstandard neutrino interactions using νe
appearance in MINOS” MINOS Collaboration (P. Adamson(Fermilab) et al.). Phys.Rev. D95 (2017)
“Constraints on Large Extra Dimensions from the MINOSExperiment“ MINOS Collaboration (P. Adamson (Fermilab) et al.).Phys.Rev. D94 (2016)
No sign of the “usual” stuff Need “unusual” ideas from theorists
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Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
LBNF/DUNE High Energy Beams and NSI P. Mehta, M.
Masud, M. Bishai
Study NSI sensitivity with GLoBeS using νµ → νµ,e and 3 sampleLBNF-like beam tunes : LE, ME and HE∗.NSI parameters used:|εeµ| = 0.04, |εeτ | = 0.04, εee = 0.4, φeµ=0, φeτ
NSI effects in νµ → νe are larger at higher energy∗
2 NuMI horns, 230kA, 6.6m apart and horns were not moved for higher energy beam tunes
(non-optimal beams). Decay pipe was assumed to be 250m.
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Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
SI/NSI Separation with Different Beams
M. Masud, P. Mehta, M. Bishai arXiv:1704.08650
SI/NSI separation metric:
36 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
SI/NSI Separation with Different Beams
M. Masud, P. Mehta, M. Bishai arXiv:1704.08650
Fraction of SI δcp for which SI/NSI can be separated at the 3/5σlevel:
Can achieve 3σ separation for > 80% of true δcp
No beam optimization attempted yet!
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Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
Sensitivity to BνSM Physics: Sterile
νµ Disappearance νe Appearance
(J. Berryman et. al. Phys.Rev. D92 (2015) no.7, 073012 )
Sensitive to lower mass ranges than SBN/MINOS+
Only tried CPV optimized beam. No HE tunes considered.
38 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
Sensitivity to BνSM Physics: Sterile
νµ Disappearance νe Appearance
(J. Berryman et. al. Phys.Rev. D92 (2015) no.7, 073012 )
Sensitive to lower mass ranges than SBN/MINOS+
Only tried CPV optimized beam. No HE tunes considered.
39 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
Example of DUNE/T2HK combinations andphysics tests
From Agarwalla et. al. (arXiv: 1711.02017), tests of differentneutrino mixing schemes with DUNE/T2HK:
What can DUNE/T2HK combinations tell us about the new physics40 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
The DUNE Near Detector CD1 Reference Design
CD1 Reference design was a Fine Grained Tracker. Several alterna-tive/additional designs currently under consideration by DUNE.
Magnet Coils
Forward ECAL
End RPCs
Backward ECAL Barrel ECAL
STT Module
Barrel RPCs
End RPCs
41 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
T2HK ND Concepts
B. Richards, EPS 2017
NuPRISM primarily for cross-section measurements
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Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
What do we do with ND’s
Next generation LBL experiments are ALSO next generationSBN experiments - but can they add anything new?
ND ν scattering physics vs e scattering physics at JLAB : NEEDHONEST ASSESSMENT of pros and cons
Searches for heavy neutrinos and dark matter from beam dumpin NDs - is there really a compelling case? Is phase spaceaccessible mostly ruled out by previous experiments?
43 / 45
Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
Summary and Conclusions
The current generation of experiments after a decade of runningcould rule out δCP = 0 at 90% C.L. over a large fraction ofδCP − θ23 space. Combined results from running NOνA andT2K(II) at maximum power could produce evidence for CPV at3σ if it is maximal by mid 2020’s.
Future long-baseline experiments need to be able to separateany observed CP asymmetries from asymmetries induced by theexpected MSW effect as well as new physics effects such assterile neutrinos and NSI (if they exist).
DUNE and T2HK can establish νSM CPV at ≥ 5σ over a widerange of δcp
The LBNF/DUNE wide-band tunable beam can also access νµ →ντ and possibly disentangle BνSM effects from νs, or NSI.Combination of T2HK and DUNE could enable further disentanglingof ν BSM that is baseline dependant effects.Theoretical input is needed to expand physics program of LBL expts.BEYOND CPV searches.What do we do with NDs other than constrain flux?
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Neutrino LBLExperimentsand Guidancefrom Theory
Mary BishaiBrookhavenNational Lab
Constraining3-Flavor νSM
CPV and δcpUnitarity tests
PhysicsBeyond ν SM
LBL and Sterile
NSI
Other νBSM
Future LBLand νBSM
What to dowith ND’s
Conclusion
THANK YOU
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