Kosmologietag Bielefeld, 3 May 2011 Thomas Schwetz-Mangold · 2012. 5. 7. · News from neutrinos...
Transcript of Kosmologietag Bielefeld, 3 May 2011 Thomas Schwetz-Mangold · 2012. 5. 7. · News from neutrinos...
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News from neutrinosKosmologietag Bielefeld, 3 May 2011
Thomas Schwetz-Mangold
Max-Planck-Institut für KernphysikHeidelberg
T. Schwetz 1
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Outline
Introduction
3-flavour oscillationsRecent developements on θ13Comments on lepton mixing patternOpen questions
Sterile neutrinosThe reactor anomalyGlobal sterile neutrino fit
Conclusions
T. Schwetz 2
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Introduction
Outline
Introduction
3-flavour oscillationsRecent developements on θ13Comments on lepton mixing patternOpen questions
Sterile neutrinosThe reactor anomalyGlobal sterile neutrino fit
Conclusions
T. Schwetz 3
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Introduction
Lepton mixing
if neutrinos have mass there can be a mis-match between neutrino andcharged-lepton mass basis
LCC = − g√2
W ρ∑
α=e,µ,τ
3∑i=1
νiLU∗αiγρ`αL + h.c.
LM = −12
3∑i=1
νTiL C−1νiLmν
i −∑
α=e,µ,τ
¯αR`αLm`
α + h.c.
⇒ Pontecorvo-Maki-Nakagawa-Sakata (PMNS) lepton mixing matrix: Uαi
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Introduction
Neutrino oscillations
W
lα
W
lβ
νβνα
detectorneutrino source
"long" distance
neutrino oscillations
|να〉 = U∗αi |νi 〉 e−i(Ei t−pi x) |νβ〉 = U∗βi |νi 〉
oscillation probability: Pνα→νβ=
∑jk
UαjU∗βjU∗αkUβk exp
[−i
∆m2kjL
2 Eν
]
∆m2kj ≡ m2
k −m2j : oscillations are sensitive only to mass-squared differences
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Introduction
Neutrino oscillations
W
lα
W
lβ
νβνα
detectorneutrino source
"long" distance
neutrino oscillations
|να〉 = U∗αi |νi 〉 e−i(Ei t−pi x) |νβ〉 = U∗βi |νi 〉
oscillation probability: Pνα→νβ=
∑jk
UαjU∗βjU∗αkUβk exp
[−i
∆m2kjL
2 Eν
]
∆m2kj ≡ m2
k −m2j : oscillations are sensitive only to mass-squared differences
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Introduction
2-neutrino oscillations
Two-flavour limit:
U =
(cos θ sin θ− sin θ cos θ
), P = sin2 2θ sin2 ∆m2L
4Eν
0.1 1 10 100L / Eν (arb. units)
0
0.2
0.4
0.6
0.8
1
Pαβ
4π / ∆m2
sin2 2θ
"short"distance
"long"distance
"very long"distance
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Introduction
Neutrinos oscillate!
KamLAND (νe → νe)
(km/MeV)eν/E0L
0 10 20 30 40 50 60 70
Surv
ival
Pro
babi
lity
0
0.2
0.4
0.6
0.8
1
1.2
1.4 eνData - BG - Geo CHOOZ dataExpectation based on osci. parameters
determined by KamLAND
> 5σ evidence for spectral distortion
MINOS (νµ → νµ)
Psurvival ≈ 1− sin2 2θ sin2(
∆m2
4LEν
)I neutrinos have to have mass (non-degenerate)I mixing: interaction state is a superposition of different mass states
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Introduction
Global data on neutrino oscillations
from various neutrino sources andvastly different energy and distance scales:
sun reactors atmosphere accelerators
Homestake,SAGE,GALLEX KamLAND, CHOOZ SuperKamiokande K2K, MINOS, T2KSuperK, SNO, Borexino
I global data fits nicely with the 3 neutrinos from the SM
I a few “anomalies” at 2-3 σ: LSND, MiniBooNE, reactor anomaly,no LMA MSW up-turn of solar neutrino spectrum
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3-flavour oscillations
Outline
Introduction
3-flavour oscillationsRecent developements on θ13Comments on lepton mixing patternOpen questions
Sterile neutrinosThe reactor anomalyGlobal sterile neutrino fit
Conclusions
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3-flavour oscillations
3-flavour oscillation parameters
νeνµ
ντ
=
Ue1 Ue2 Ue3Uµ1 Uµ2 Uµ3Uτ1 Uτ2 Uτ3
ν1ν2ν3
∆m231 ∆m2
31 ∆m221
U =
1 0 00 c23 s230 −s23 c23
c13 0 e−iδs130 1 0
−e iδs13 0 c13
c12 s12 0−s12 c12 0
0 0 1
atmos+LBL(dis) Chooz+LBL(app) solar+KamLAND
3-flavour effects are suppressed: ∆m221 ∆m2
31 and θ13 1 (Ue3 = s13e−iδ)
⇒ dominant oscillations are well described by effective two-flavour oscillations⇒ CP-violation is suppressed by θ13 and ∆m2
21/∆m231
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3-flavour oscillations
3-flavour oscillation parameters
νeνµ
ντ
=
Ue1 Ue2 Ue3Uµ1 Uµ2 Uµ3Uτ1 Uτ2 Uτ3
ν1ν2ν3
∆m2
31 ∆m231 ∆m2
21
U =
1 0 00 c23 s230 −s23 c23
c13 0 e−iδs130 1 0
−e iδs13 0 c13
c12 s12 0−s12 c12 0
0 0 1
atmos+LBL(dis) Chooz+LBL(app) solar+KamLAND
3-flavour effects are suppressed: ∆m221 ∆m2
31 and θ13 1 (Ue3 = s13e−iδ)
⇒ dominant oscillations are well described by effective two-flavour oscillations⇒ CP-violation is suppressed by θ13 and ∆m2
21/∆m231
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3-flavour oscillations
The dominanting oscillation modes
I solar neutrinos Homestake, SAGE+GNO, Super-K, SNO, Borexinoνe → νµ,τ LMA-MSW with ∆m2 ∼ 7× 10−5eV2 (matter effect)
I Kamland reactor neutrino experiment (180 km, vacuum osc)νe disappearance with Eν/L ∼ 7× 10−5eV2
I atmospheric neutrinos Super-Kamiokandelong-baseline accelerator experiments K2K (250 km), MINOS (735 km)νµ disappearance with Eν/L ∼ 2× 10−3eV2
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3-flavour oscillations
The dominanting oscillation modes
0.2 0.4 0.6 0.8
sin2θ12
0
5
10
15
∆m2 21
[ 10
-5eV
2 ]
solar neutrino exps.
KamLAND
combined
H
0 0.25 0.5 0.75 1
sin2θ23
1
2
3
4
∆m2 31
[ 10
-3 e
V2 ]
MINOS
atmospheric
global
sin2 θ12 ≈ 0.3 sin2 θ23 ≈ 0.5
∆m221
∆m231≈ 1
30
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3-flavour oscillations
Neutrino mass spectra and mixingINVERTEDNORMAL
[mas
s]2
3ν
ν2
ν1
ν2ν1
ν3
νe
µν
ντ
∆m231 > 0 ∆m2
31 < 0
I ν1 is dominantly νe (non-maximal but large θ12)close to equal mixing of νµ and ντ (θ23 ≈ 45)
I we know the sign of ∆m221 (matter effect in sun) but not of ∆m2
31I θ13: νe component of ν3
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3-flavour oscillations Recent developements on θ13
Effects of θ13
1. subleading effects in solar/KamLAND/atmospheric oscillations
2. transitions of νe involving ∆m231:
2.1 νe disappearance at reactors with L ' 1 km
“clean” measurment of θ13: P ≈ 1− sin2 2θ13 sin2(∆m231L/4E )
2.2 νµ → νe transitions at accelerator experiments
complicated function of all osc parameters (CP phase δ)
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3-flavour oscillations Recent developements on θ13
Effects of θ13
1. subleading effects in solar/KamLAND/atmospheric oscillations
2. transitions of νe involving ∆m231:
2.1 νe disappearance at reactors with L ' 1 km“clean” measurment of θ13: P ≈ 1− sin2 2θ13 sin2(∆m2
31L/4E )2.2 νµ → νe transitions at accelerator experiments
complicated function of all osc parameters (CP phase δ)
simulation: assume sin2 2θ13 = 0.1, δ = π/2
Huber, Lindner, TS, Winter, 09T. Schwetz 14
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3-flavour oscillations Recent developements on θ13
θ13 till June 2011
I sin2 θ13 . 0.04 (3σ) from global data (dominated by CHOOZ)
I weak indications for θ13 > 0 @ 1.8σ global fit(solar/KamL and MINOS/SK)TS, Tortola, Valle, 08, 1103; Fogli et al, 08; Gonzalez-Garcia, Maltoni, Salvado, 10
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3-flavour oscillations Recent developements on θ13
T2K data on νµ → νe appearance
search for νµ → νe oscillationswith L = 295 km andEν ' 0.7 GeV
K. Abe et al., 1106.2822
6 events obs1.5± 0.3 expected for θ13 = 02.5σ indication for θ13 > 0
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3-flavour oscillations Recent developements on θ13
T2K data on νµ → νe appearance
search for νµ → νe oscillationswith L = 295 km andEν ' 0.7 GeV
K. Abe et al., 1106.2822
6 events obs1.5± 0.3 expected for θ13 = 02.5σ indication for θ13 > 0
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3-flavour oscillations Recent developements on θ13
Recent data on νµ → νe appearance
I T2K: 6 events obs (1.5± 0.3 expected for θ13 = 0)2.5σ indication for θ13 > 0 T2K, 1106.2822
I MINOS: 62 events obs (49.6± 7.0± 2.7 expected for θ13 = 0)consistent with θ13 = 0 MINOS, 1108.0015
!
0 0.025 0.05 0.075 0.1sin2θ13
-1
-0.5
0
0.5
1
δ / π
!
0 0.025 0.05 0.075 0.1sin2θ13
68%, 90%, 1 dof
NH
68%, 90%, 1 dof
IH
T2KMINOS
MINOS
T2K
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3-flavour oscillations Recent developements on θ13
Global data on θ13 TS, Tortola, Valle, 1108.1376
sin2 θ13 = 0.013+0.007−0.005 sin2 θ13 = 0.016+0.008
−0.006
θ13 = 0 : ∆χ2 = 10.1 (3.2σ)
similar results by Fogli et al, 1106.6028; Maltoni @ EPS11T. Schwetz 18
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3-flavour oscillations Recent developements on θ13
New generation of θ13 reactor experiments
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3-flavour oscillations Recent developements on θ13
New generation of θ13 reactor experiments
DC: 1112.6353 101d 4121ev sin2 2θ13 = 0.086± 0.041± 0.030 (1.9σ)DB: 1203.1669 55d 10416ev sin2 2θ13 = 0.092± 0.016± 0.005 (5.2σ)RE: 1204.0626 229d 17102ev sin2 2θ13 = 0.113± 0.013± 0.019 (4.9σ)
naive comb.: sin2 2θ13 = 0.098± 0.013 (χ2 = 0.6/2 dof)
Gonzalez-Garcia, Maltoni, Salvado, TS, in prep.
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3-flavour oscillations Recent developements on θ13
Global fitwith SBL data:
sin2 θ13 = 0.022+0.0033−0.0030
sin2 2θ13 = 0.086± 0.012θ13 = (8.5+0.62
−0.61)
6.9σ significance
without SBL data using2011 flux pred.:
sin2 θ13 = 0.026+0.0034−0.0032
sin2 2θ13 = 0.101+0.013−0.012
θ13 = (9.3± 0.59)
8.0σ significance
Gonzalez-Garcia, Maltoni, Salvado,
TS, in prep.
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3-flavour oscillations Comments on lepton mixing pattern
CKM versus PMNSQuark mixing:
UCKM =
1 ε ε
ε 1 ε
ε ε 1
Lepton mixing:
UPMNS =1√3
O(1) O(1) εO(1) O(1) O(1)O(1) O(1) O(1)
10-3 10-2 10-1 100
sinθij
13
23
12
leptons (PMNS)
quarks (CKM)
3σ errors
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3-flavour oscillations Comments on lepton mixing pattern
Symmetry versus anarchy?
Are lepton mixing angles “special”?
Example: Tri-bimaximal mixing: Harrison, Perkins, Scott, hep-ph/0202074
UTBM =
√
2/3 1/√
3 0−1/
√6 1/
√3 1/
√2
1/√
6 −1/√
3 1/√
2
Lots of activity in the literature on predicting special flavour structure byimposing symmetries (discrete, non-abelian, An, Sn, Zn, Dn,...)
enforce relations such as:|Uµ3| = |Uτ3||Ue3| = 0|Ue2| = |Uµ2| = |Uτ2|
Is this approach still attractiveif θ13 is large?
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3-flavour oscillations Comments on lepton mixing pattern
Symmetry versus anarchy?
Are lepton mixing angles “special”?
Example: Tri-bimaximal mixing: Harrison, Perkins, Scott, hep-ph/0202074
UTBM =
√
2/3 1/√
3 0−1/
√6 1/
√3 1/
√2
1/√
6 −1/√
3 1/√
2
Lots of activity in the literature on predicting special flavour structure byimposing symmetries (discrete, non-abelian, An, Sn, Zn, Dn,...)
enforce relations such as:|Uµ3| = |Uτ3||Ue3| = 0|Ue2| = |Uµ2| = |Uτ2|
Is this approach still attractiveif θ13 is large?
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3-flavour oscillations Comments on lepton mixing pattern
Symmetry versus anarchy?
Maybe the mixing angles are just random numbers? Murayama et al.
probability of more special pattern is 44% deGouvea, Murayama, 1204.1249
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3-flavour oscillations Open questions
Open questions
I How close is θ23 to 45?
I Is the neutrino mass ordering normal or inverted?INVERTEDNORMAL
[mas
s]2
3ν
ν2
ν1
ν2ν1
ν3
νe
µν
ντ
look for matter effect in transitions involving ∆m231
I Is there CP violation in the lepton sector?search for difference in να → νβ and να → νβ oscillations
Current LBL experiments: T2K, NOvAActive investigations towards a facility beyond thoseSuperbeam (LBNE, LBNO, HyperK), Beta Beam, Neutrino Factoryrecent discovery of “large” θ13 is changing this discussion
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3-flavour oscillations Open questions
Open questions
I How close is θ23 to 45?
I Is the neutrino mass ordering normal or inverted?INVERTEDNORMAL
[mas
s]2
3ν
ν2
ν1
ν2ν1
ν3
νe
µν
ντ
look for matter effect in transitions involving ∆m231
I Is there CP violation in the lepton sector?search for difference in να → νβ and να → νβ oscillations
Current LBL experiments: T2K, NOvAActive investigations towards a facility beyond thoseSuperbeam (LBNE, LBNO, HyperK), Beta Beam, Neutrino Factoryrecent discovery of “large” θ13 is changing this discussion
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3-flavour oscillations Open questions
Majorana nature of neutrinos
Maybe lepton mixing is so different because neutrinos are Majorana?
Search for neutrinoless double beta decay: (A, Z ) → (A, Z + 2) + 2e−
⇒ violation of lepton number by 2 units
strong indication of Majorana nature of neutrinos Schechter, Valle, 1982; Takasugi, 1984
-5 -4 -3 -2 -1 0Log HmMIN @eVDL
-3
-2
-1
0
Log
HÈ<m>È@eVD
L sin2Θ13 = 0.03 ± 0.004
NH
IH QD
-5 -4 -3 -2 -1 0Log HmMIN @eVDL
-3
-2
-1
0
Log
HÈ<m>È@eVD
L
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3-flavour oscillations Open questions
Absolute mass of neutrinos
I Kinematical mass measurments(beta decay spectrum endpoint)
KATRIN sensitivity to∑
i |Uei |2mi ∼ 0.2 eV
I Cosmology (HDM)free streaming of neutrinos reduces matter power at small scales
current limits around∑
i mi . 0.1 eV
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3-flavour oscillations Open questions
Is the standard 3-neutrino scenario the end of the story?
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Sterile neutrinos
Outline
Introduction
3-flavour oscillationsRecent developements on θ13Comments on lepton mixing patternOpen questions
Sterile neutrinosThe reactor anomalyGlobal sterile neutrino fit
Conclusions
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Sterile neutrinos
Sterile neutrinos at the eV scale
Sterile neutrinos are genericin models for neutrino mass(though typically at muchhigher scales).
Why not assume that someof them have masses at theeV scale?
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Sterile neutrinos
Hints for eV neutrinos from νµ → νe searches
I LSND νµ → νe , 87.9± 22.4± 6.0 excess eventsP = (0.264± 0.067± 0.045)% ∼ 3.8σ away from zero
can be explained by oscillations with ∆m2 ∼ 1 eV2 and small mixing
not confirmed by any other experiment so-far
I KARMEN νµ → νe , tight constraint on LSND region(slightly smaller L/E than LSND)
I MiniBooNE νµ → νeE > 475 MeV: no excess, E < 475 MeV: ∼ 3σ excess
I MiniBooNE νµ → νe , inconclusiveconsistent with MBν as well as with LSND in 2ν framework
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Sterile neutrinos
Hints for eV neutrinos from νµ → νe searches
I LSND νµ → νe , 87.9± 22.4± 6.0 excess eventsP = (0.264± 0.067± 0.045)% ∼ 3.8σ away from zero
can be explained by oscillations with ∆m2 ∼ 1 eV2 and small mixing
not confirmed by any other experiment so-far
I KARMEN νµ → νe , tight constraint on LSND region(slightly smaller L/E than LSND)
I MiniBooNE νµ → νeE > 475 MeV: no excess, E < 475 MeV: ∼ 3σ excess
I MiniBooNE νµ → νe , inconclusiveconsistent with MBν as well as with LSND in 2ν framework
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Sterile neutrinos The reactor anomaly
New reactor flux calculations
I to predict the νe flux from nuclear reactors one has to convert themeasured e− spectra from 235U, 239Pu, 241Pu into neutrino spectraSchreckenbach et al., 82, 85, 89
I recent improved calculation Mueller et al., 1101.2663 yields∼ 3% higher fluxes
I confirmed by independent calculation P. Huber, 1106.0687
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Sterile neutrinos The reactor anomaly
New reactor flux calculations
data from short-baseline reactorexperiments:
µ = 0.927± 0.023
2.9σ away from 1
Mention et al, 1101.2755 (2012 upd)
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Sterile neutrinos The reactor anomaly
New reactor fluxes and reactor data
Mention et al., 1101.2755 (2012 upd)
I non-zero θ13 can reduce flux at L & 1 km but not shorter baselinesI sterile neutrino with ∆m2 ∼ 1 eV2 can account for rate reduction at
L & 10− 100 mI systematic error...?
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Sterile neutrinos The reactor anomaly
Reactor data and sterile neutrinos
3 4 5 6 7 8E
pos [MeV]
0.8
0.9
1
1.1
obse
rved
/ pr
edic
ted
rate
3 4 5 6 7 8E
pos [MeV]
0.9
1
Bugey3 15 m Bugey3 40 m
Bugey4
χ2
no osc = 59.0/69
χ2
3+1 = 50.1/67
χ2
3+2 = 46.5/65
10-2
10-1
100
sin22θ
react
10-1
100
101
∆m2 41
[eV
2 ]
90%, 99% CL (2 dof)
curves: old fluxescolors: new fluxes
∆m241 [eV2] |Ue4| ∆m2
51 [eV2] |Ue5| ∆χ2(no osc)3+1 1.78 0.151 8.5 (98% CL 2 dof)3+2 0.46 0.108 0.89 0.124 12.1 (98% CL 4 dof)
bounds on Ue4,5 become “preferred regions” with new reactor fluxesMention et al., 11; Kopp, Maltoni, TS, 11
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Sterile neutrinos The reactor anomaly
The Gallium anomaly
callibration data in galliumsolar neutrino experimentsνe +71 Ga →71 Ge + e−
ratio of measured topredicted rate:
RBahcall = 0.86± 0.05 (2.8σ)
RHaxton = 0.76± 0.09 (2.7σ)
Acero, Giunti, Laveder, 0711.4222; Giunti, Laveder, 1006.3244
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Sterile neutrinos Global sterile neutrino fit
Can we fit all this in a 3+1 (or 3+n) scheme3+1 νµ → νe appearance
Pµe = sin2 2θapp sin2 ∆m241L
4Esin2 2θapp = 4|Ue4|2|Uµ4|2
3+1 νe and νµ disappearance
Pαα = 1− sin2 2θdis sin2 ∆m241L
4Esin2 2θdis = 4|Uα4|2(1− |Uα4|2)
3+1: constraints from νe (νµ) disappearance experiments on Ue4 (Uµ4)imply that appearance mixing angle is quadratically suppressed
3+2: phase δ ≡ arg(
U∗e4Uµ4Ue5U∗
µ5
)→ CP violation
Karagiorgi et al. 06; Maltoni, TS 07
BUT: constrain |Uei | and |Uµi | (i = 4, 5) from disappearanceto be reconciled with appearance amplitudes |UeiUµi |
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Sterile neutrinos Global sterile neutrino fit
Can we fit all this in a 3+1 (or 3+n) scheme3+1 νµ → νe appearance
Pµe = sin2 2θapp sin2 ∆m241L
4Esin2 2θapp = 4|Ue4|2|Uµ4|2
3+1 νe and νµ disappearance
Pαα = 1− sin2 2θdis sin2 ∆m241L
4Esin2 2θdis = 4|Uα4|2(1− |Uα4|2)
3+1: constraints from νe (νµ) disappearance experiments on Ue4 (Uµ4)imply that appearance mixing angle is quadratically suppressed
3+2: phase δ ≡ arg(
U∗e4Uµ4Ue5U∗
µ5
)→ CP violation
Karagiorgi et al. 06; Maltoni, TS 07
BUT: constrain |Uei | and |Uµi | (i = 4, 5) from disappearanceto be reconciled with appearance amplitudes |UeiUµi |
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Sterile neutrinos Global sterile neutrino fit
Limits on Uµ4
H
10-3 10-2 10-1
|Uµ4|2
10-2
10-1
100
101
∆m2 41
[eV
2 ]
atmospheric
CDHS
Kopp, Maltoni, TS, in prepMiniBooNE, 1106.5685
sin2 2θ = 4|U2µ4|(1 − |U2
µ4|)
I νµ disappearance CDHSI atmospheric neutrinos Bilenky, Giunti, Grimus, TS 99; Maltoni, TS, Valle 01
I MINOS NC data 1001.0336, 1104.3922
I additional constraints from MiniB νµ(νµ) at ∆m2 & 1 eV2
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Sterile neutrinos Global sterile neutrino fit
3+1 global fit
10-4
10-3
10-2
10-1
sin22θ
SBL
10-1
100
101
∆m2 41
[eV
2 ]
99% CL (2 dof)
LSND + MBν−
MBνKARMENNOMAD
disappearance90, 99% CL
I no CP violation → LSND+MBν versus MBν
I despite relaxed constraints on Ue4 no improvement of global 3+1 fitI LSND+MBν versus rest: χ2
PG = 21.5(24.2) for new (old) flux→ compatibility of less than 10−5
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Sterile neutrinos Global sterile neutrino fit
3+2 global fit Kopp, Maltoni, TS, PRL 11
H
H
0.1 1 10∆m
241
0.1
1
10
∆m2 51
0.1 1 100.1
1
10
90%, 95%, 99%, 99.73% CL (2 dof)
3+2
1+3+1
some improvement in the fit:
I ∆χ2(old vs new fluxes)3+2 = 11.1
I ∆χ2 (3+1 vs 3+2) = 11.2(97.6% CL, 4 dof)6.3 for old flux
∆m241 |Ue4| |Uµ4| ∆m2
51 |Ue5| |Uµ5| δ/π χ2/1303+2 0.47 0.128 0.165 0.87 0.138 0.148 1.64 110.13+2’ 0.47 0.117 0.201 1.70 0.151 0.101 1.39 114.43+2’ 1.00 0.133 0.163 1.60 0.122 0.079 1.48 114.43+2’ 0.90 0.123 0.163 6.30 0.135 0.091 1.67 115.0
1+3+1 0.47 0.129 0.154 0.87 0.142 0.163 0.35 106.1
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Sterile neutrinos Global sterile neutrino fit
There is severe tension in the 3+2 fit
Giunti, Laveder, 1109.4033
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Sterile neutrinos Global sterile neutrino fit
There is severe tension in the 3+2 fit
LSND+MB(ν) vs rest appearance vs disapp.old new old new
χ2PG/dof 25.1/5 19.9/5 19.9/4 14.7/4PG 10−4 0.13% 5× 10−4 0.53%
adding MINOS NC Kopp, Maltoni, TS, work in prep.
χ2PG/dof 30.0/5 24.8/5 24.7/4 19.5/4PG 10−5 10−4 5× 10−5 6× 10−4
I explanation of appearance signal requires Uei and Uµi (i = 4, 5)I no hint for oscillations seen in νµ disappearance⇒ constraints on Uµi in tension with signals
I MINOS NC data makes compatibility worse by one order of magnitude
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Sterile neutrinos Global sterile neutrino fit
Summary sterile global fit
I If we assume that the 3+n oscillation scenario is correct at least oneof the experiments is “mis-interpreted”.
I If we neglect LSND, the hint for νe disappearance from the reactorand Gallium anomalies remains (relies on complicated theoreticalcalculations, uncertainties difficult to estimate)
I If we stick to LSND, probably we have to discard more than oneexperiment (several experiments constrain νµ disappearance)
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Sterile neutrinos Global sterile neutrino fit
Summary sterile global fit
I If we assume that the 3+n oscillation scenario is correct at least oneof the experiments is “mis-interpreted”.
I If we neglect LSND, the hint for νe disappearance from the reactorand Gallium anomalies remains (relies on complicated theoreticalcalculations, uncertainties difficult to estimate)
I If we stick to LSND, probably we have to discard more than oneexperiment (several experiments constrain νµ disappearance)
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Sterile neutrinos Global sterile neutrino fit
Summary sterile global fit
I If we assume that the 3+n oscillation scenario is correct at least oneof the experiments is “mis-interpreted”.
I If we neglect LSND, the hint for νe disappearance from the reactorand Gallium anomalies remains (relies on complicated theoreticalcalculations, uncertainties difficult to estimate)
I If we stick to LSND, probably we have to discard more than oneexperiment (several experiments constrain νµ disappearance)
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Sterile neutrinos
eV sterile neutrinos and cosmology
Hamann et al., 1006.5276
68, 95, 99% CL
I CMB, SDSS, HST: prefer some extra radiation, but limit on HDMexcludes two eV-scale neutrinos
I BBN: Ns < 1.2 (95% CL) Mangano, Serpico, 1103.1261
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Sterile neutrinos
eV sterile neutrinos and cosmology
How to accommodate eV sterile neutrinos with cosmology?
I invent a mechanism to avoid thermalization(large chemical potential?)
I assume very low re-heating temperature (dangerously close to BBN)
I Hamann, Hannestad, Raffelt, Wong, 1108.4136
I limit on neutrino mass (HDM) can be evaded by allowing extraradiation ∆Nml ' 1− 2 and/or DE equation of statew < −1 Elgaroy, Kristiansen, 1104.0704
I BBN constraints on extra radiation can be avoided by introducing achemical potential of νe .
I modifies other cosmological parameters, e.g. ΩCDM (+20%-75%)
⇒ requires substantial modification of standard cosmology
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Sterile neutrinos
eV sterile neutrinos and cosmology
How to accommodate eV sterile neutrinos with cosmology?
I invent a mechanism to avoid thermalization(large chemical potential?)
I assume very low re-heating temperature (dangerously close to BBN)
I Hamann, Hannestad, Raffelt, Wong, 1108.4136
I limit on neutrino mass (HDM) can be evaded by allowing extraradiation ∆Nml ' 1− 2 and/or DE equation of statew < −1 Elgaroy, Kristiansen, 1104.0704
I BBN constraints on extra radiation can be avoided by introducing achemical potential of νe .
I modifies other cosmological parameters, e.g. ΩCDM (+20%-75%)
⇒ requires substantial modification of standard cosmology
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Sterile neutrinos
eV sterile neutrinos and cosmology
How to accommodate eV sterile neutrinos with cosmology?
I invent a mechanism to avoid thermalization(large chemical potential?)
I assume very low re-heating temperature (dangerously close to BBN)
I Hamann, Hannestad, Raffelt, Wong, 1108.4136
I limit on neutrino mass (HDM) can be evaded by allowing extraradiation ∆Nml ' 1− 2 and/or DE equation of statew < −1 Elgaroy, Kristiansen, 1104.0704
I BBN constraints on extra radiation can be avoided by introducing achemical potential of νe .
I modifies other cosmological parameters, e.g. ΩCDM (+20%-75%)
⇒ requires substantial modification of standard cosmology
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Sterile neutrinos
More exotic ideas
I 3-neutrinos and CPT violation Murayama, Yanagida 01;
Barenboim, Borissov, Lykken 02; Gonzalez-Garcia, Maltoni, TS 03
I 4-neutrinos and CPT violation Barger, Marfatia, Whisnant 03
I Exotic muon-decay Babu, Pakvasa 02
I CPT viol. quantum decoherence Barenboim, Mavromatos 04
I Lorentz violation Kostelecky et al., 04, 06; Gouvea, Grossman 06
I mass varying ν Kaplan,Nelson,Weiner 04; Zurek 04; Barger,Marfatia,Whisnant 05
I shortcuts of sterile νs in extra dim Paes, Pakvasa, Weiler 05
I decaying sterile neutrino Palomares-Riuz, Pascoli, TS 05; Gninenko 10
I 2 decaying sterile neutrinos with CPVI energy dependent quantum decoherence Farzan, TS, Smirnov 07
I sterile neutrinos and new gauge boson Nelson, Walsh 07
I sterile ν with energy dep. mass or mixing TS 07
I sterile ν with nonstandard interactions Akhmedov, TS 10
most of these ideas
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Sterile neutrinos
More exotic ideas
I 3-neutrinos and CPT violation Murayama, Yanagida 01;
Barenboim, Borissov, Lykken 02; Gonzalez-Garcia, Maltoni, TS 03
I 4-neutrinos and CPT violation Barger, Marfatia, Whisnant 03
I Exotic muon-decay Babu, Pakvasa 02
I CPT viol. quantum decoherence Barenboim, Mavromatos 04
I Lorentz violation Kostelecky et al., 04, 06; Gouvea, Grossman 06
I mass varying ν Kaplan,Nelson,Weiner 04; Zurek 04; Barger,Marfatia,Whisnant 05
I shortcuts of sterile νs in extra dim Paes, Pakvasa, Weiler 05
I decaying sterile neutrino Palomares-Riuz, Pascoli, TS 05; Gninenko 10
I 2 decaying sterile neutrinos with CPVI energy dependent quantum decoherence Farzan, TS, Smirnov 07
I sterile neutrinos and new gauge boson Nelson, Walsh 07
I sterile ν with energy dep. mass or mixing TS 07
I sterile ν with nonstandard interactions Akhmedov, TS 10
most of these ideas involve sterile neutrinos
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Sterile neutrinos
More exotic ideasI 3-neutrinos and CPT violation Murayama, Yanagida 01;
Barenboim, Borissov, Lykken 02; Gonzalez-Garcia, Maltoni, TS 03
I 4-neutrinos and CPT violation Barger, Marfatia, Whisnant 03
I Exotic muon-decay Babu, Pakvasa 02
I CPT viol. quantum decoherence Barenboim, Mavromatos 04
I Lorentz violation Kostelecky et al., 04, 06; Gouvea, Grossman 06
I mass varying ν Kaplan,Nelson,Weiner 04; Zurek 04; Barger,Marfatia,Whisnant 05
I shortcuts of sterile νs in extra dim Paes, Pakvasa, Weiler 05
I decaying sterile neutrino Palomares-Riuz, Pascoli, TS 05; Gninenko 10
I 2 decaying sterile neutrinos with CPVI energy dependent quantum decoherence Farzan, TS, Smirnov 07
I sterile neutrinos and new gauge boson Nelson, Walsh 07
I sterile ν with energy dep. mass or mixing TS 07
I sterile ν with nonstandard interactions Akhmedov, TS 10
most of these ideas have problems with some data
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Sterile neutrinos
Many ideas to test eV sterile neutrinos experimentally
I radioactive source experiments (e.g., in Borexino, SNO+) Cribier et al,
1107.2335; Garvin et al, 1006.2103; Vergados, Novikov, 1006.3862; Grieb, Link, Raghavan, hep-ph/0611178,...
I several ideas at FNAL (MINOS+, MicroBooNE, MiniBooNEextensions, very-low-E NuFact) B. Louis @ NuFact11
I ICARUS at CERN PS C. Rubbia et al. 0909.0355
I experiments with ∼100 kW proton synchrotronsConrad, Shaevitz 09; Huber, Agarwalla 10; Agarwalla, Conrad, Shaevitz, 11
I signatures in IceCube (Deep Core)Nunokawa, Peres, Zukanovich, hep-ph/0302039; Coubey, 0709.1937; Razzaque, Smirnov, 1104.1390, 1203.5406
I 2011 sterile neutrino workshops: LNGS, Italy (May),FNAL, USA (May), Virginia Tech, Blacksburg, USA (2011)
I White paper on sterile neutrinos 1204.5379
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Sterile neutrinos
Many ideas to test eV sterile neutrinos experimentally
I radioactive source experiments (e.g., in Borexino, SNO+) Cribier et al,
1107.2335; Garvin et al, 1006.2103; Vergados, Novikov, 1006.3862; Grieb, Link, Raghavan, hep-ph/0611178,...
I several ideas at FNAL (MINOS+, MicroBooNE, MiniBooNEextensions, very-low-E NuFact) B. Louis @ NuFact11
I ICARUS at CERN PS C. Rubbia et al. 0909.0355
I experiments with ∼100 kW proton synchrotronsConrad, Shaevitz 09; Huber, Agarwalla 10; Agarwalla, Conrad, Shaevitz, 11
I signatures in IceCube (Deep Core)Nunokawa, Peres, Zukanovich, hep-ph/0302039; Coubey, 0709.1937; Razzaque, Smirnov, 1104.1390, 1203.5406
I 2011 sterile neutrino workshops: LNGS, Italy (May),FNAL, USA (May), Virginia Tech, Blacksburg, USA (2011)
I White paper on sterile neutrinos 1204.5379
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Conclusions
Outline
Introduction
3-flavour oscillationsRecent developements on θ13Comments on lepton mixing patternOpen questions
Sterile neutrinosThe reactor anomalyGlobal sterile neutrino fit
Conclusions
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Conclusions
Conclusions
I the bulk of data on neutrino oscillations is fitted perfectly within thethree-flavour framework, and we have evidence for oscillatorybehaviour of the survival probablility as function of neutrino energy
I recent results from reactor epxeriments (DoubleChooz, DayaBay,RENO) + T2K νe appearance establish non-zero value the lastunknown mixing angle θ13 ' 9 (not far from the previous upperbound)
I there are intriguing hints for sterile neutrinos at the eV scale:LSND, reactor anomaly, Gallium anomaly, cosmology?BUT: no consistent picture has emerged sofar
Thank you for your attention!
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Conclusions
Conclusions
I the bulk of data on neutrino oscillations is fitted perfectly within thethree-flavour framework, and we have evidence for oscillatorybehaviour of the survival probablility as function of neutrino energy
I recent results from reactor epxeriments (DoubleChooz, DayaBay,RENO) + T2K νe appearance establish non-zero value the lastunknown mixing angle θ13 ' 9 (not far from the previous upperbound)
I there are intriguing hints for sterile neutrinos at the eV scale:LSND, reactor anomaly, Gallium anomaly, cosmology?BUT: no consistent picture has emerged sofar
Thank you for your attention!
T. Schwetz 49
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Conclusions
Conclusions
I the bulk of data on neutrino oscillations is fitted perfectly within thethree-flavour framework, and we have evidence for oscillatorybehaviour of the survival probablility as function of neutrino energy
I recent results from reactor epxeriments (DoubleChooz, DayaBay,RENO) + T2K νe appearance establish non-zero value the lastunknown mixing angle θ13 ' 9 (not far from the previous upperbound)
I there are intriguing hints for sterile neutrinos at the eV scale:LSND, reactor anomaly, Gallium anomaly, cosmology?BUT: no consistent picture has emerged sofar
Thank you for your attention!
T. Schwetz 49
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Conclusions
Conclusions
I the bulk of data on neutrino oscillations is fitted perfectly within thethree-flavour framework, and we have evidence for oscillatorybehaviour of the survival probablility as function of neutrino energy
I recent results from reactor epxeriments (DoubleChooz, DayaBay,RENO) + T2K νe appearance establish non-zero value the lastunknown mixing angle θ13 ' 9 (not far from the previous upperbound)
I there are intriguing hints for sterile neutrinos at the eV scale:LSND, reactor anomaly, Gallium anomaly, cosmology?BUT: no consistent picture has emerged sofar
Thank you for your attention!
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