peter b. denton · 2021. 1. 15. · peter b. denton(bnl het group) bnl friday lunch discussion:...
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LMA-Dark: Large New Physics Effects in Neutrino Oscillations
Peter B. Denton
BNL Friday Lunch Discussion
February 28, 2020
LMA-Dark: Large New Physics Effects in Neutrino Oscillations
Peter B. Denton
BNL Friday Lunch Discussion
February 28, 2020
Oscillating Oscillation Degeneracies
There is a degeneracy that can be repeatedly broken and restored:
1. Can’t determine mass orderings
2. Matter effect breaks this
3. NSIs restore the degeneracy
4. Quark contribution breaks this
5. Specific NSIs restores the degeneracy
6. Scattering experiments breaks this
7. The degeneracy is restored for light mediators
8. BBN and CMB cover light mediators
9. LMA-Dark, light mediator, diagonal degeneracy restore the degeneracy
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 2/39
1. Oscillation DegeneraciesSince neutrinos oscillate there are 7+ new parameters in the SMOscillations are sensitive to 6 of them
H =1
2EU
0∆m2
21
∆m231
U †
1. Diagonal degeneracy ⇒ no sensitivity to m1.
2. By CPT can send H → −H∗
∆m221 → −∆m2
21 , ∆m231 → −∆m2
31 , δ → −δThat is, it is impossible to determine either mass ordering
A. de Gouvea, A. Friedland, H. Murayama hep-ph/0002064
P. Bakhti and Y. Farzan, 1403.0744
P. Coloma, T. Schwetz 1604.05772
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 3/39
Neutrino Mass Eigenstate Definition: AsideThe mass eigenstates can be numbered in a number of different ways
1. |Ue1| > |Ue2| > |Ue3|2. m1 < m2 < m3
3. m1 < m2 and |Ue3| < |Ue1| and |Ue3| < |Ue2|
4....
I #3 was commonly used in solar neutrinos
I We know that in the solar sector all three are equivalent
I We take #1 as our definition
Under definition #3 the LMA-Dark degeneracy is
sin θ12 ↔ cos θ12 , ∆m231 → −∆m2
32 , δ → π − δ
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 4/39
Neutrino Mass Eigenstate Definition: AsideThe mass eigenstates can be numbered in a number of different ways
1. |Ue1| > |Ue2| > |Ue3|2. m1 < m2 < m3
3. m1 < m2 and |Ue3| < |Ue1| and |Ue3| < |Ue2|
4....
I #3 was commonly used in solar neutrinos
I We know that in the solar sector all three are equivalent
I We take #1 as our definition
Under definition #3 the LMA-Dark degeneracy is
sin θ12 ↔ cos θ12 , ∆m231 → −∆m2
32 , δ → π − δ
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 4/39
2. Solar Neutrinos
In matter
H =1
2E
U
0∆m2
21
∆m231
U † + a
10
0
a ≡ 2√
2GFNeESubtracted NC matter effect: diagonal degeneracy
10−1 100 101
E [MeV]
0.0
0.2
0.4
0.6
0.8
1.0
PD ee
∆m221 > 0
∆m221 < 0
We know ∆m221 > 0 so degeneracy is broken by matter effects.
Measuring the atmospheric mass ordering in DUNE would also break this degeneracy.
Unless . . .
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 5/39
3. New Physics
In matter
H =1
2E
U
0∆m2
21
∆m231
U † + a
1− 20
0
This factor of −2 restores the degeneracy in matter as well.
New physics like this is called neutrino non-standard interactions: NSIs, the ε’s.L. Wolfenstein, PRD 17 (1978)
Recent overview: PBD, et al. 1907.00991
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 6/39
NSI at the Lagrangian Level
EFT Lagrangian:
LNSI = −2√
2GF∑
f,P,α,β
εf,Pα,β (ναγµPLνβ)(fγµPf)
with Λ = 1√2√
2εGF.
Simplified model Lagrangian:
LNSI = gνZ′µνγ
µν + gfZ′µfγ
µf
which gives a potential
VNSI ∝gνgf
q2 +m2Z′
Models with large NSIs consistent with CLFV:Y. Farzan, I. Shoemaker 1512.09147 Y. Farzan, J. Heeck 1607.07616 D. Forero and W. Huang 1608.04719
K. Babu, A. Friedland, P. Machado, I. Mocioiu 1705.01822 PBD, Y. Farzan, I. Shoemaker 1804.03660U. Dey, N. Nath, S. Sadhukhan 1804.05808 Y. Farzan 1912.09408
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 7/39
Matter Effects in Feynman Diagrams
Z
f
να
f
να
W
e−
νe
νe
e−
VNC = ∓1
2
√2GFnn VCC = ±
√2GFne
f
να
f
νβ
VNSI = ±εf,Xαβ√
2GFnf
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 8/39
Matter Effects in Feynman Diagrams
Z
f
να
f
να
W
e−
νe
νe
e−
VNC = ∓1
2
√2GFnn VCC = ±
√2GFne
Z ′
f
να
f
νβ
VNSI =nf2
gνgfq2 +m2
Z′
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 8/39
NSI at the Hamiltonian Level
Hvac =1
2EU
0∆m2
21
∆m231
U †
Hmat,SM =a
2E
10
0
Hmat,NSI =a
2E
εee εeµ εeτε∗eµ εµµ εµτε∗eτ ε∗µτ εττ
H = Hvac +Hmat,SM +Hmat,NSI
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 9/39
LMA-Dark in Matter
Even in matter the LMA-Dark degeneracy is still exact
∆m221 → −∆m2
21 , ∆m231 → −∆m2
31 , δ → −δ
εee → εee − 2 , εαβ → −ε∗αβ (αβ 6= ee)
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 10/39
NSI: The EpsilonsThe εαβ have 9 dof’s, it’s actually must worse
εαβ =∑
f=e,u,d
Yf εf,Vαβ
withYf =
nfne
dof’s = 9× 3× 2 = 54If SPVAT then 135
In SNe/early universe νν NSSI as well
1 -0.2 0 0.2
εA
0
10
20
∆χ2
I Axial is not constrained by oscillations, only scatteringAxial constraints from SNO-NC by O. Miranda, M. Tortola, J. Valle, hep-ph/0406280
I Limit to just vector, up, down, real: dof=12
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 11/39
NSI: The EpsilonsThe εαβ have 9 dof’s, it’s actually must worse
εαβ =∑
f=e,u,d
Yf εf,Vαβ
withYf =
nfne
dof’s = 9× 3× 2 = 54If SPVAT then 135
In SNe/early universe νν NSSI as well
1 -0.2 0 0.2
εA
0
10
20
∆χ2
I Axial is not constrained by oscillations, only scatteringAxial constraints from SNO-NC by O. Miranda, M. Tortola, J. Valle, hep-ph/0406280
I Limit to just vector, up, down, real: dof=12
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 11/39
NSI: The EpsilonsThe εαβ have 9 dof’s, it’s actually must worse
εαβ =∑
f=e,u,d
Yf εf,Vαβ
withYf =
nfne
dof’s = 9× 3× 2 = 54If SPVAT then 135
In SNe/early universe νν NSSI as well
1 -0.2 0 0.2
εA
0
10
20
∆χ2
I Axial is not constrained by oscillations, only scatteringAxial constraints from SNO-NC by O. Miranda, M. Tortola, J. Valle, hep-ph/0406280
I Limit to just vector, up, down, real: dof=12
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 11/39
Numerical Exploration
“Dark Side” from: A. de Gouvea, A. Friedland, H. Murayama, hep-ph/0002064
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 12/39
Best Fit Assuming Standard Neutrino Physics
★ ★
0 0.2 0.4 0.6 0.8 1
sin2θ
SOL
10-5
10-4
∆m
2 SO
L [
eV
2]
★
0 0.2 0.4 0.6 0.8 1
sin2θ
SOL90%, 95%, 99% and 99.73% CL O. Miranda, M. Tortola, J. Valle, hep-ph/0406280
KamLAND (color), solar (black)Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 13/39
Best Fit Assuming Standard Neutrino Physics
★
0 0.2 0.4 0.6 0.8 1
sin2θ
SOL
10-6
10-5
10-4
10-3
∆m
2 SO
L [
eV
2]
★
0 0.2 0.4 0.6 0.8 1
sin2θ
SOL
LMA-I
LMA-0
LMA-D
90%, 95%, 99% and 99.73% CL O. Miranda, M. Tortola, J. Valle, hep-ph/0406280Solar (left), solar + KamLAND (right), ∆χ2 = 80.2− 79.7.
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 14/39
NSI Global Fit Oscillation Data
0
5
10
15
20∆
χ2
f=u
-2 -1 0 1
εf,V
ee− ε
f,V
µµ
0
5
10
15
20
∆χ
2
-0.25 0 0.25
εf,V
ττ− ε
f,V
µµ
-0.2 0 0.2
εf,V
eµ
-0.5 0 0.5
εf,V
eτ
-0.05 0 0.05
εf,V
µτ
f=d
Blue: ∆m221 > 0, Red: ∆m2
21 < 0 P. Coloma, PBD, M. Gonzalez-Garcia, M. Maltoni, T. Schwetz 1701.04828
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 15/39
A Global Fit Reveals
A global fit reveals:
I LMA-Dark solution is very much accommodated by oscillation data
I εee = 0 slightly disfavoredI Solar upturn
I Slight information from quark composition
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 16/39
4. Quark Contribution in NSI
Need εee = −2,εee = (2 + Yn)εu,Vee + (1 + 2Yn)εd,Vee = −2
Yn = Nn/Ne and is ∼ 1/3 in the sun and 1.05 in the Earth’s crust
If εu = εd, in the sun εu,Vee = −1/2.For the same parameters in the Earth, εee = −3.1 which is detectable!
Matter effect has only been measured in the sun,DUNE will make a ∼ 30% measurement.
K. Kelly, S. Parke 1802.06784
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 17/39
4. Quark Contribution in NSI
Need εee = −2,εee = (2 + Yn)εu,Vee + (1 + 2Yn)εd,Vee = −2
Yn = Nn/Ne and is ∼ 1/3 in the sun and 1.05 in the Earth’s crust
If εu = εd, in the sun εu,Vee = −1/2.For the same parameters in the Earth, εee = −3.1 which is detectable!
Matter effect has only been measured in the sun,DUNE will make a ∼ 30% measurement.
K. Kelly, S. Parke 1802.06784
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 17/39
4. Quark Contribution in NSI
Need εee = −2,εee = (2 + Yn)εu,Vee + (1 + 2Yn)εd,Vee = −2
Yn = Nn/Ne and is ∼ 1/3 in the sun and 1.05 in the Earth’s crust
If εu = εd, in the sun εu,Vee = −1/2.For the same parameters in the Earth, εee = −3.1 which is detectable!
Matter effect has only been measured in the sun,DUNE will make a ∼ 30% measurement.
K. Kelly, S. Parke 1802.06784
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 17/39
5. Quark Combinations
−2.0 −1.5 −1.0 −0.5 0.0 0.5 1.0 1.5 2.0εu,Vee
−2.0
−1.5
−1.0
−0.5
0.0
0.5
1.0
1.5
2.0
εd,Vee
COHERENT
95%
εd,Vee
=εu,V
ee
LMA–D
,Earth
LM
A–D,
Sun
Oscillations 90%
PBD, Y. Farzan, I. Shoemaker 1804.03660
I Clear that matter effect measurementcomes from solar
I Precision measurements can break this ifI εu = 0I εu = εd
I εd = 0
I No oscillation measurements in anymaterials and for any level of precision canbreak this if:
εu,Vee = −4/3 , εd,Vee = 2/3
Oscillations can go no further
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 18/39
NSI in Scattering Experiments Probe Different Scales
NSI affects:
I Oscillation: q2 = 0, the effect is valid for any m∗Z′∗See e.g. M. Wise, Y. Zhang 1803.00591
I Scattering: the NSI potential is suppressed if q2 > m2Z′
Regime mZ′
Tevatron/LHC & 10− 100 GeVCHARM/NuTeV (DIS) & 1 GeVCOHERENT (CEvNS) & 10 MeV
Early universe . 5 MeVReactor CEvNS & 1 MeV
Oscillation Any
For mZ′ & 1 TeV, ε ∼ O(1) is no longer perturbative.
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 19/39
High Energy Collider Constraints
lowP
TC
DF
GS
NP
highPT
veryHighP
T
Broadresonance
CDF ADD
100 101 102 103 10410-3
10-2
10-1
100
101
MZ ' @GeVD
¶
●
●
●
NuTeV (εμμ ) :
νN scattering
CHARM (εee) :
νe N scattering
j+MET
jj+ℓ+MET
τ+e+META
B
C
10 50 100 5001000 5000104
0.001
0.010
0.100
1
�� [���]ε
A. Friedland, et al., 1111.5331 D. Franzosi, M. Frandsen, and I. Shoemaker, 1507.07574
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 20/39
−2 −1 0 1 2εu,Vee
−2
−1
0
1
2
εd,Vee
CHARM
CHARM measured NC and CC (ν )
e cross sections with nuclei,
RNC/CC = (gLe )2 + (gRe )2 = 0.406± 0.140
at 〈Eν〉 = 54 GeV on Fe.
CHARM Collaboration, PLB180 (1986)
(gPe )2 =∑
q=u,d
(gPq + εq,Pee )2 +
∑
α 6=e|εq,Peα |2
2-loop radiative corrections for SM couplingsJ. Erler, S. Su, 1303.5522
Re,SM = 0.333 for q2 ∼ 20 GeV2.
PBD, et al., 1701.04828 1, 2, 3 σ contours for 2 d.o.f.
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 21/39
NuTeV
NuTeV measured NC and CC νµ and νµ cross sections with nuclei.
Rνµ =σ(νµX → νµX)
σ(νµX → µX)= (gLµ )2 + r(gRµ )2 = 0.3919± 0.0013
Rνµ =σ(νµX → νµX)
σ(νµX → µX)= (gLµ )2 +
1
r(gRµ )2 = 0.4050± 0.0027
at 〈Eν〉 = 60 GeV on Fe.
r =σ(νµX→µX)
σ(νµX→µX)
NuTeV Collaboration, hep-ex/0110059
G. P. Zeller PhD thesis
This leads to χ2NuTeV,SM ∼ 9 which is the NuTeV anomaly.
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 22/39
NuTeV Corrected
Measurements need to be corrected,
I Improved nuclear models
I Iron is not isoscalar
I Updated PDFs including the strange quark
NNPDF Collaboration, 0906.1958
W. Bentz, et al., 0908.3198
δRνµ,exp = 0.0017 , δRνµ,exp = −0.0016 ,
Rexp,true = Rexp,orig + δR
▲
▲
▲ Best-fit (corrected) SM
0.00 0.05 0.10 0.15
0.00
0.05
0.10
0.15
ϵμμ���
ϵ μμ���
1, 2, 3 σ2 d.o.f.
Corrected χ2NuTeV,SM ∼ 2.3.
PBD, et al., 1701.04828
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 23/39
Heavy NSI Constraints
0
5
10
15
20∆
χ2 O
SC
+S
CA
T
f=u
-1 0 1
εf,V
ee
0
5
10
15
20
∆χ
2 OS
C+S
CA
T
-0.015 0 0.015
εf,V
µµ
-0.2 0 0.2
εf,V
ττ
-0.1 0 0.1
εf,V
eµ
-0.5 0 0.5
εf,V
eτ
-0.03 0 0.03
εf,V
µτ
f=d
Heavy ⇒ mZ′ & 1 GeV. All oscillation experiments, CHARM, and NuTeV.
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 24/39
Coherent Elastic ν Nucleus Scattering: CEvNS (“Sevens”)
CEvNS := ν scattering off the weak charge of entire nucleus
The CEvNS cross section is very high, but recoil energies are very low:
Our suggestion may be an act of hubris, because the inevitable constraints ofinteraction rate, resolution, and background pose grave experimental difficultiesfor elastic neutrino-nucleus scattering.
D. Freedman, PRD 9 (1974)
Thanks to DM direct detection efforts, this is now possible.
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 25/39
Coherent Elastic ν Nucleus Scattering: CEvNS (“Sevens”)
CEvNS := ν scattering off the weak charge of entire nucleus
The CEvNS cross section is very high, but recoil energies are very low:
Our suggestion may be an act of hubris, because the inevitable constraints ofinteraction rate, resolution, and background pose grave experimental difficultiesfor elastic neutrino-nucleus scattering.
D. Freedman, PRD 9 (1974)
Thanks to DM direct detection efforts, this is now possible.
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 25/39
0 10 20 30 40 50 60Eν (MeV)
0.00
0.01
0.02
0.03
0.04
0.05
f α(M
eV−1
)
νµ
νµ
νe
COHERENT
Spallation Neutron Source at Oak Ridge in a π-DAR configuration.K. Scholberg, hep-ex/0511042
π+ → µ+ + νµ
µ+ → e+ + νµ + νe
fνµ= δ
(Eν −
m2π −m2
µ
2mπ
),
fνµ=64
mµ
[(Eνmµ
)2(3
4− Eνmµ
)],
fνe=192
mµ
[(Eνmµ
)2(1
2− Eνmµ
)].
Detector 22 m from source with Etr = 5 keV.
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 26/39
COHERENTObserved spectrum:
dNα
dEr= Nt∆t
∫dEνφα(Eν)
dσαdEr
(Eν) ,
Neutrino nucleon cross section:
dσαdEr
=G2F
2π
Q2wα
4F 2(2MEr)M
(2− MEr
E2ν
),
Form factors from: C. Horowitz, K. Coakley, D. McKinsey, astro-ph/0302071
Electroweak charge:
1
4Q2wα =
[Z(gVp + 2εu,Vαα + εd,Vαα ) +N(gVn + εu,Vαα + 2εd,Vαα )
]2
+∑
β 6=α
[Z(2εu,Vαβ + εd,Vαβ ) +N(εu,Vαβ + 2εd,Vαβ )
]2.
Z = 32, N = 44.
gVp = 12− 2 sin2 θW , gVn = − 1
2.
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 27/39
SNS Beam Details
Pulsed beam: flavor discrimination
I The νµ from the π+ decay forms the prompt signal.
I The νe and νµ form the delayed signal.
I Probability that the muon decays within the pulse width,
Pc =1
tw
∫ tw
0dt[1− e−(tw−t)/Γτ
]= 0.138
I We expect ∼ 100 prompt and ∼ 200 delayed.
Systematics: beam normalization at 10% and 20% background.
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 28/39
COHERENT Sensitivity to Exclude LMA-Dark
−1.0 −0.8 −0.6 −0.4 −0.2 0.0 0.2 0.4 0.6εu,Vee
−0.2
−0.1
0.0
0.1
0.2
0.3
0.4
0.5
0.6
εu,Vµµ
LMA
LMA−D
Predicted sensitivity measuring SM with 10 kg·yrs of 76Ge.PBD, et al., 1701.04828
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 29/39
6. COHERENT Excludes LMA-Dark
•
-� -��� -��� -��� -��� � ��� ��� ��� ���-���
-���
�
���
���
���
���
���
ϵ�����
ϵ μμ���
���-�
���
Counts only, no timing P. Coloma, et al., 1708.02899
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 30/39
Recap: Oscillations and the Diagonal Terms
SolarChlorine, Gallex/GNO, SAGE,Super-K, Borexino, and SNO.
AtmosphericSuper-K, MINOS, and T2K.
ReactorCHOOZ, Palo Verde, Double CHOOZ,Daya Bay, and RENO.
Short baselineBugey, ROVNO, Krasnoyarsk, ILL,Gosgen, and SRP.
Global fit to oscillation data
ǫuee
ǫuµµ
ǫuττ
ǫdee
ǫdµµ
ǫdττ
Oscillation
CHARM
NuTeV
COHERENT
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 31/39
7. General LMA-Dark Constraints from COHERENT
100 101 102 103
MZ ′ (MeV)
0
5
10
15
20
25
χ2
LMA–D at COHERENT
95% CL limit = 48 MeV
x
Marginalized
0
1
3/2
2
BBN + CMB
PBD, Y. Farzan, I. Shoemaker, 1804.03660
1. Assume εu = εd
2. LMA-Dark ruled out for MZ′ > 17 MeV
3. Oscillations sensitive to diagonaldegeneracy:General Oscillation Degeneracy:
(εee, εµµ, εττ ) = (x− 2, x, x)
4. LMA-Dark and diagonal degeneracy ruledout for MZ′ > 48 MeV
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 32/39
0 2 4 6 8 10Years
0
10
20
30
40
50
60
MZ′(M
eV) LMA–D at COHERENT
95% Sensitivity
Current (data)
Projected : CsI (SM)
BBN + CMB
Future LMA-Dark Sensitivity at COHERENT
← Gap?
PBD, Y. Farzan, I. Shoemaker, 1804.03660
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 33/39
Light Mediator Coverage
1. Early universe: mZ′ . 0.1− 1 MeV⇒ Z ′ is relativistic at BBN, ∆Neff = 3× 4/7 = 1.7
Neff -BBN measurements require mZ′ > 5.3 MeV and gν < 10−9 mZ′MeV
A. Kamada, H. Yu, 1504.00711
2. Reactor CEvNS: Sensitive to MZ′ & 1 MeV
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 34/39
2 3 4 5 6 7 8 9Eνe [MeV]
10−7
10−6
10−5
10−4
10−3
10−2
10−1
100
101
φ[M
eV−1
fiss
ion
−1]
Reactor CEvNS ExperimentsUpcoming program of measuring CEvNS with reactors:
I High statistics
I Low q2 ⇒ “more coherent”I Less form factor uncertainty
I Flux uncertaintyI Reactor anti-neutrino anomalyI 5 MeV bump
Experimental program includes:
I NOSTOS hep-ex/0503031
I TEXONO hep-ex/0511001
I GEMMA 1411.2279
I νGeN JINST 10 (2015)
I CONNIE 1604.01343
I MINER 1609.02066
I CONUS 1612.04150
I Ricochet 1612.09035
I ν-cleus 1704.04320
...
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 35/39
8. Reactor Sensitivity for CONUS
0.0 0.5 1.0 1.5 2.0MZ ′ [MeV]
0.0
0.1
0.2
0.3
0.4
0.5
NN
SI/N
SM−
1
Si
Ge
95%
νe only ⇒ LMA-Dark at x = 0 only
PBD, Y. Farzan, I. Shoemaker, 1804.03660
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 36/39
8. Reactor Sensitivity for CONUS
0.0 0.5 1.0 1.5 2.0MZ ′ [MeV]
0.0
0.1
0.2
0.3
0.4
0.5
NN
SI/N
SM−
1
Si
Ge
95%
νe only ⇒ LMA-Dark at x = 0 only
PBD, Y. Farzan, I. Shoemaker, 1804.03660
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 36/39
10−1 100 101 102 103
MZ ′ [MeV]
10−6
10−5
10−4
10−3
√|g νg q|
(gν)eegq < 0
95% (2 d.o.f.)
COHERENT
BBN + CMB
COHERENT+10 yrs (SM)
CONUS Ge (SM)
LMA–Dark
10−1 100 101 102 103
MZ ′ [MeV]
10−6
10−5
10−4
10−3
√|g νg q|
(gν)µµgq = (gν)ττgq > 0
95% (2 d.o.f.)
COHERENT
BBN + CMB
COHERENT+10 yrs (SM)
LMA–Dark
9. Present and Future LMA-Dark Bounds
εee onlyx = 0
εµµ, εττ onlyx = 2
PBD, Y. Farzan, I. Shoemaker, 1804.03660
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 37/39
Experimental Connections
1. All oscillation experimentsI Solar neutrinos in particular
2. CHARM and NuTeV
3. COHERENT
4. Early universe
5. CONUS and other reactor CEvNS
6. DUNE (matter effect) orCOHERENT with different materials −2.0 −1.5 −1.0 −0.5 0.0 0.5 1.0 1.5 2.0
εu,Vee
−2.0
−1.5
−1.0
−0.5
0.0
0.5
1.0
1.5
2.0
εd,Vee
COHERENT
95%
εd,Vee
=εu,V
ee
LMA–D
,Earth
LM
A–D,
Sun
Oscillations 90%
COHERENT constraints for large mZ′ .PBD, Y. Farzan, I. Shoemaker 1804.03660
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 38/39
Summary
I Exact degeneracies will be present in every oscillation experiment
I Measuring the sign of ∆m2ij requires the matter effect
I New physics (NSIs) makes probing the mass ordering impossible
I Oscillation experiments in different materials (Earth, Sun) helps, somewhat
I Scattering experiments help a lot, but only for heavy enough mediators
I Early universe constrains light mediators
I Gap will be covered by reactor CEvNS experiments
I LMA-Dark + diagonal: (εee, εµµ, εττ ) ' (0, 2, 2) with εu ' 4/3 and εd ' −2/3and mZ′ ∈ [5, 50] MeV may never be probable
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 39/39
Backups
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 40/39
−1.0 −0.5 0.0 0.5
εq,Vαβ
Oscillations90% CL
ud
θ12 45◦><
ee− µµ ee− µµ
ττ − µµ
eµ
eτ
µτ
NSI Global Fit: Oscillations
Oscillations are independent of mZ′ . PBD, et al., 1701.04828
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 41/39
−1.0 −0.5 0.0 0.5
εq,Vαβ
Osc + CHARM + NuTeV90% CL
ud
θ12 45◦><
ee ee
µµ
ττ
eµ
eτ
µτ
Heavy NSI Global Fit: CHARM & NuTeV
Heavy ⇒ mZ′ & 1 GeV. PBD, et al., 1701.04828
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 42/39
−0.2 −0.1 0.0 0.1 0.2 0.3 0.4εq,Vee
−0.10
−0.05
0.00
0.05
0.10
0.15
0.20
0.25
εq,V µµ
1, 2, 3 σ
2 d.o.f.
−0.4
0.0
0.4
εq,V eτ
−0.4 0.0 0.4
εq,Veµ
−0.4
0.0
0.4
εq,V µτ
−0.4 0.0 0.4εq,Veτ
∆χ2
1, 2, 3 σ2 d.o.f.
(χ2min = 2.9)
NSI Projections: COHERENT
Limit ourselves to εu = εd
Diagonal Off-Diagonal
PBD, Y. Farzan, I. Shoemaker, 1804.03660
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 43/39
−1.0 −0.5 0.0 0.5
εq,Vαβ
COHERENT90% CL
εu = εd θ12 45◦><
ee ee
µµ µµ
ττ ττ (w/osc)
eµ
eτ
µτ
NSI Constraints: COHERENT
Valid down to mZ′ & 10 MeV PBD, Y. Farzan, I. Shoemaker, 1804.03660
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 44/39
−0.05 0.00 0.05 0.10 0.15 0.20εq,Vee
−0.15
−0.10
−0.05
0.00
0.05
0.10
0.15
εq,V eτ
Looking to the COHERENT FutureInterference of different materials is powerful.
100 kg·yrs Xe with Etr = 10 keV100 kg·yrs Ne with Etr = 10 keV
10% systematic
εq,Vee,deg =1
3
Yn − (1− 4 sin2 θW )
Yn + 1
Yn ∈ [1, 1.43]
εq,Vee,deg ∈ [0.15, 0.18]
Solar upturn?
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 45/39
COHERENT Results Last YearCOHERENT measured CEvNS at 6.7σ.14.6 kg CsI (Na doped) for 15 months.
COHERENT Collaboration, 1708.01294 SciencePeter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 46/39
Further LMA-Dark DegeneracyThere is a further exact degeneracy with scattering.
Q2wα ∝ (Xq − εq,Vαα )2 ,
with
Xu = −ZgVp +NgVn
2Z +N,Xd = −
ZgVp +NgVnZ + 2N
.
This leads to an exact degeneracy at
εu,Vee =
{−0.15
0.842, εd,Vee =
{−0.224
0.886.
I In this case a scattering experiment cannot break the degeneracy.
I Multiple materials can break this degeneracy in theory, in practice this is hard.
I Best fit points seem to be far from these points, so there is no problem.
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 47/39
0.0 0.2 0.4 0.6 0.8 1.0Er [keV]
0
50000
100000
150000
200000
250000
300000
350000
dN
dE
r[e
vent
syr
−1ke
V−1
]
SM
MZ ′ = 0.1 MeV
MZ ′ = 1 MeV
0.0 0.2 0.4 0.6 0.8 1.0Er [keV]
0
1
2
3
4
5
6
7
8
dN
dE
r[a
rbit
rary
]
SM
MZ ′ = 0.1 MeV
MZ ′ = 1 MeV
Reactor Spectrum Shape Analysis
LMA-Dark x = 0 shape sensitivity down to ∼ 1 MeV.
Peter B. Denton (BNL HET Group) BNL Friday Lunch Discussion: February 28, 2020 48/39