neutrino masses in cosmology, neutrinoless double-beta...
TRANSCRIPT
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Neutrino Masses in Cosmology, Neutrinoless
Double-Beta Decay and Direct Neutrino Masses
Carlo Giunti
INFN, Sezione di Torino, and Dipartimento di Fisica Teorica, Università di Torino
mailto://[email protected]
Neutrino Unbound: http://www.nu.to.infn.it
LIONeutrino2012
Neutrinos at the forefront of elementary particle physics
and astrophysics
22-24 October 2012, Lyon, France
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 1/33
mailto://[email protected]://www.nu.to.infn.it
-
Three-Neutrino Mixing Paradigm
νe νµ ντ
∆m2A
∆m2S
ν2
ν1
ν3
m2
Normal Spectrum
m2
∆m2S
ν2
ν1
∆m2A
ν3
Inverted Spectrum
∆m2S ≃ 7.5× 10−5 eV2 ∆m2A ≃ 2.5× 10
−3 eV2
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 2/33
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Open Problems
◮ CP violation ?◮ Nova, LAGUNA, CERN-GS, HyperK, . . .
◮ Mass Hierarchy ?◮ Nova, Atmospheric Neutrinos, Day Bay II, Supernova Neutrinos, . . .
◮ Absolute Mass Scale ?◮ β Decay, Neutrinoless Double-β Decay, Cosmology, . . .
◮ Dirac or Majorana ?◮ Neutrinoless Double-β Decay, . . .
Cosmology: see Verde and Saviano talks
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 3/33
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Absolute Scale of Neutrino Masses
Lightest mass: m1 [eV]
m1,
m2,
m3
[e
V]
10−4 10−3 10−2 10−1 110−4
10−3
10−2
10−1
1
m1
m2
m3 Cosm
ological Limit
Normal Hierarchy
Quasi−DegenerateNormal Spectrum1σ2σ3σ
m22 = m21 +∆m
221 = m
21 +∆m
2S
m23 = m21 +∆m
231 = m
21 +∆m
2A
Lightest mass: m3 [eV]m
3, m
1, m
2
[eV
]
10−4 10−3 10−2 10−1 110−4
10−3
10−2
10−1
1
m3
m1
m2
Cosm
ological Limit
Inverted Hierarchy
Quasi−DegenerateInverted Spectrum1σ2σ3σ
m21 = m23 −∆m
231 = m
23 +∆m
2A
m22 = m21 +∆m
221 ≃ m
23 +∆m
2A
Quasi-Degenerate for m1 ≃ m2 ≃ m3 ≃ mν &√
∆m2A ≃ 5× 10−2 eV
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 4/33
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Tritium Beta-Decay
3H → 3He + e− + ν̄edΓ
dT=
(cosϑCGF)2
2π3|M|2 F (E) pE (Q − T )
√
(Q − T )2 −m2νe
Q = M3H −M3He −me = 18.58 keV
Kurie plot
K(T ) =
√
√
√
√
√
dΓ/dT
(cosϑCGF)2
2π3|M|2 F (E) pE
=
[
(Q − T )√
(Q − T )2 −m2νe
]1/2
mνe > 0
Q−mνe Q
mνe = 0
T
K(T
)
mνe < 2.2 eV (95% C.L.)
Mainz & Troitsk[Weinheimer, hep-ex/0210050]
future: KATRIN[www.katrin.kit.edu]
start data taking in 2015
sensitivity: mνe ≃ 0.2 eV
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 5/33
www.katrin.kit.edu
-
Neutrino Mixing =⇒ K (T ) =
[
(Q − T )∑
k
|Uek |2√
(Q − T )2 −m2k
]1/2
Q−m2 T Q−m1
K(T
)
Q
analysis of data isdifferent from theno-mixing case:2N − 1 parameters(
∑
k
|Uek |2 = 1
)
if experiment is not sensitive to masses (mk ≪ Q − T )
effective mass: m2β =∑
k
|Uek |2m2k
K2 = (Q − T )2
∑
k
|Uek |2
√
1−m2
k
(Q − T )2≃ (Q − T )2
∑
k
|Uek |2
[
1−1
2
m2k
(Q − T )2
]
= (Q − T )2[
1−1
2
m2β
(Q − T )2
]
≃ (Q − T )√
(Q − T )2 −m2β
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 6/33
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Predictions of 3ν-Mixing Paradigm
m2β = |Ue1|2 m21 + |Ue2|
2 m22 + |Ue3|2m23
mmin [eV]
mβ
[e
V]
NS
IS
Current Bound
KATRIN Sensitivity
Cosm
ological Limit
10−3 10−2 10−1 1 1010−3
10−2
10−1
1
10
1σ2σ3σ
◮ Quasi-Degenerate:
m2β ≃ m2ν
∑
k|Uek |
2 = m2ν
◮ Inverted Hierarchy:
m2β ≃ (1− s213)∆m
2A ≃ ∆m
2A
◮ Normal Hierarchy:
m2β ≃ s212c
213∆m
2S + s
213∆m
2A
≃ 2× 10−5 + 6× 10−5 eV2
◮ mβ . 4× 10−2 eV
⇓Normal Spectrum
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 7/33
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Neutrinoless Double-Beta Decay
7632Ge
7633As
7634Se
0+
2+
0+
β−
β−β−
β+
Effective Majorana Neutrino Mass: mββ =∑
k
U2ek mk
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 8/33
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Two-Neutrino Double-β Decay: ∆L = 0
N (A,Z ) → N (A,Z + 2) + e− + e− + ν̄e + ν̄e
(T 2ν1/2)−1 = G2ν |M2ν |
2
second order weak interaction processin the Standard Model
d u
W
W
d u
��
e
��
e
e
�
e
�
Neutrinoless Double-β Decay: ∆L = 2
N (A,Z ) → N (A,Z + 2) + e− + e−
(T 0ν1/2)−1 = G0ν |M0ν |
2 |mββ |2
effectiveMajoranamass
|mββ| =
∣
∣
∣
∣
∣
∑
k
U2ek mk
∣
∣
∣
∣
∣
d u
W
�
k
m
k
U
ek
U
ek
W
d u
e
�
e
�
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 9/33
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Effective Majorana Neutrino Mass
mββ =∑
k
U2ek mk complex Uek ⇒ possible cancellations
mββ = |Ue1|2 m1 + |Ue2|
2 e iα2 m2 + |Ue3|2 e iα3 m3
α2 = 2λ2 α3 = 2 (λ3 − δ13)
α3
α2
Im[mββ]
|Ue2|2e
iα2m2
|Ue1|2m1
mββ
Re[mββ]
|Ue3|2e
iα3m3
α2
α3
Im[mββ]
|Ue2|2e
iα2m2
|Ue1|2m1 Re[mββ]
mββ
|Ue3|2e
iα3m3
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 10/33
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Experimental Bounds
EXO (136Xe) [PRL 109 (2012) 032505]
T 0ν1/2 > 1.6× 1025 y (90% C.L.) =⇒ |mββ | . 0.14 − 0.38 eV
CUORICINO (130Te) [AP 34 (2011) 822]
T 0ν1/2 > 2.8× 1024 y (90% C.L.) =⇒ |mββ | . 0.3− 0.7 eV
Heidelberg-Moscow (76Ge) [EPJA 12 (2001) 147]
T 0ν1/2 > 1.9× 1025 y (90% C.L.) =⇒ |mββ| . 0.32 − 1.0 eV
IGEX (76Ge) [PRD 65 (2002) 092007]
T 0ν1/2 > 1.57 × 1025 y (90% C.L.) =⇒ |mββ| . 0.33 − 1.35 eV
NEMO 3 (100Mo) [PRL 95 (2005) 182302]
T 0ν1/2 > 4.6× 1023 y (90% C.L.) =⇒ |mββ | . 0.7− 2.8 eV
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 11/33
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Experimental Positive Indication[Klapdor et al., MPLA 16 (2001) 2409]
T 0ν1/2 = (2.23+0.44−0.31)× 10
25 y 6.5σ evidence [MPLA 21 (2006) 1547]
0 500 1000 1500 2000 2500 30000
10
20
30
40
50
60
70
Energy ,keV
Cou
nts
/ keV
SSE2n2b Rosen − Primakov Approximation
Q=2039 keV
[PLB 586 (2004) 198]
2000 2010 2020 2030 2040 2050 2060
0
1
2
3
4
5
6
7
8
[MPLA 21 (2006) 1547]
|mββ | = 0.32 ± 0.03 eV [MPLA 21 (2006) 1547]
very exciting: Majorana ν and large mass scale
partially excluded by EXO and CUORICINO
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 12/33
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Predictions of 3ν-Mixing Paradigm
mββ = |Ue1|2 m1 + |Ue2|
2 e iα2 m2 + |Ue3|2 e iα3 m3
mmin [eV]
|mββ
| [
eV]
NS
IS
Cosm
ological Limit
Current Bound or Positive Indication
10−4 10−3 10−2 10−1 110−4
10−3
10−2
10−1
1
1σ2σ3σ
◮ Positive indication:tension with cosmology
◮ Quasi-Degenerate:
|mββ | ≃ mν√
1− s22ϑ12s2α2
◮ Inverted Hierarchy:
|mββ | ≃√
∆m2A(1− s22ϑ12
s2α2)
◮ Normal Hierarchy:
|mββ| ≃ |s212
√
∆m2S + eiαs213
√
∆m2A|
≃ |2.7 + 1.2e iα| × 10−3 eV
m1 & 10−3 eV⇒cancellation?
|mββ | . 10−2 eV =⇒ Normal Spectrum
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 13/33
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ββ0ν Decay ⇔ Majorana Neutrino Mass
|mββ | can vanish because of unfortunate cancellations among m1, m2, m3contributions or because neutrinos are Dirac
ββ0ν decay can be generated by another mechanism beyond SM
d
d u
u
e−
e−
ββ0ν =⇒
d
d u
u
e−
W+
W+
e−ββ0ν
ν̄e ≡ νe(h = +1)
νe ≡ νe(h = −1)
[Schechter, Valle, PRD 25 (1982) 2951] [Takasugi, PLB 149 (1984) 372]
Majorana Mass Term: LMeL
= −12 mee(
νceLνeL + νeL ν
c
eL
)
four-loop diagram calculation: mee ∼ 10−24 eV [Duerr, Lindner, Merle, JHEP 06 (2011) 091]
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 14/33
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◮ In any case finding ββ0ν decay is important information to solve theDirac-Majorana question in favor of Majorana
◮ On the other hand, it is not possible to prove experimentally thatneutrinos are Dirac.A Dirac neutrino is equivalent to 2 Majorana neutrinos with the samemass.Impossible to prove experimentally that mass splitting is exactly zero.
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 15/33
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Beyond Three-Neutrino Mixing
ν1
m21 logm2m22
ν2 ν3
m23
νe
νµ
ντνs1 · · ·
ν4 ν5 · · ·
m24 m25
νs2
3ν-mixing
∆m2ATM ∆m2SBL∆m
2SOL
[see Schwetz and Cribier talks]
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 16/33
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Sterile Neutrinos
◮ Sterile means no standard model interactions (e.g. νcR= νsL)
◮ Oscillation observables:
◮ Disappearance of active neutrinos (neutral current deficit)
◮ Indirect evidence through combined fit of data (current indication)
◮ Short-baseline anomalies + 3ν-mixing:
∆m221 ≪ |∆m231| ≪ |∆m
241| ≤ . . .
ν1 ν2 ν3 ν4 . . .
νe νµ ντ νs1 . . .
◮ Neutrino number and mass observable:
◮ Number of thermalized relativistic particles in early Universe (BBN, CMB,BAO)
◮ m4 effects in cosmology (CMB, LLS), direct β-decay neutrino massmeasurements and neutrinoless double-β decay (if Majorana)
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 17/33
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Reactor Electron Antineutrino Anomaly
[Mention et al, PRD 83 (2011) 073006]
[update in White Paper, arXiv:1204.5379
new reactor ν̄e fluxes[Mueller et al, PRC 83 (2011) 054615]
[Huber, PRC 84 (2011) 024617]
2.8σ anomaly
0 20 40 60 80 100
0.7
0.8
0.9
1.0
1.1
1.2
L [m]
R
R = 0.93 ± 0.024
Reactor Rates
Bugey3−15Bugey3−40Bugey3−95Bugey4ROVNOGosgen−38
Gosgen−45Gosgen−65ILLKrasno−33Krasno−92Krasno−57
Average Rate
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 18/33
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Gallium Anomaly
Gallium Radioactive Source Experiments: GALLEX and SAGE
Detection Process: νe +71Ga → 71Ge + e−
νe Sources: e− + 51Cr → 51V + νe e
− + 37Ar → 37Cl + νe
Anomaly supported by new 71Ga(3He, 3H)71Ge cross section measurement[Frekers et al., PLB 706 (2011) 134]
0.7
0.8
0.9
1.0
1.1
R
Cr1GALLEX
CrSAGE
Cr2GALLEX
ArSAGE
R = 0.84 ± 0.05
E ∼ 0.7MeV
〈L〉GALLEX = 1.9m
〈L〉SAGE = 0.6m
2.9σ anomaly
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 19/33
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3+1 SBL νe and ν̄e Survival Probability
P(−)νe→
(−)νe
= 1− sin2 2ϑee sin2
(
∆m241L
4E
)
sin2 2ϑee = 4|Ue4|2(
1− |Ue4|2)
standard parameterization
Ue1 = c12c13c14 Ue2 = s12c13c14 Ue3 = s13c14e−iδ13 Ue4 = s14e
−iδ14
sin2 2ϑee = sin2 2ϑ14
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 20/33
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Global νe and ν̄e Disappearance[Giunti, Laveder, Y.F. Li, Q.Y. Liu, H.W. Long, arXiv:1210.5715]
sin22ϑee
∆m412
[e
V2 ]
+
10−2 10−1 110−2
10−1
1
10
102
++
+
95% CL
GalliumReactorsνeCSunCombined
95% CL
GalliumReactorsνeCSunCombined
νe +12C → 12Ng.s. + e−
KARMEN + LSND[Conrad, Shaevitz, PRD 85 (2012) 013017]
[Giunti, Laveder, PLB 706 (2011) 200]
sin22ϑee
∆m412
[e
V2 ]
10−2 10−1 110−1
1
10
+
GAL+REA+νeC+SUN68.27% CL (1σ)90.00% CL95.45% CL (2σ)99.00% CL99.73% CL (3σ)
GAL+REA+νeC+SUN68.27% CL (1σ)90.00% CL95.45% CL (2σ)99.00% CL99.73% CL (3σ)
solar νe + KamLAND ν̄e + ϑ13[Giunti, Li, PRD 80 (2009) 113007]
[Palazzo, PRD 83 (2011) 113013]
[Palazzo, PRD 85 (2012) 077301]
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 21/33
-
The existence of ν4 with m4 & 1 eV can have dramatic effects not only onneutrino oscillations but also on all phenomena sensitive to the absolutevalue of neutrino masses:
◮ direct β-decay neutrino mass measurements
◮ neutrinoless double-β decay (if Majorana)
◮ cosmology
Information on νe and ν̄e disappearance is crucial for β decay andneutrinoless double-β decay
◮ νe and ν̄e disappearance depends on sin2 2ϑee = 4|Ue4|
2(1− |Ue4|2)
◮ In β decay and neutrinoless double-β decay ν4 contribution depends on|Ue4|
2
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 22/33
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Direct β-Decay Neutrino Mass Measurements
−5 −4 −3 −2 −1 0
T − Q [eV]
1−
K(T
)/(Q
−T
)
10−4
10−3
10−2
(sin22ϑee,∆m412 [eV2])
( 0.12 , 7.6 )( 0.1 , 2 )( 0.07 , 0.9 )( 0.052 , 0.46 )
sin22ϑee∆m
412
[eV
2 ]10−2 10−1 1
10−1
1
10
+
++
+ GAL+REA+νeC+SUN68.27% CL (1σ)90.00% CL95.45% CL (2σ)99.00% CL99.73% CL (3σ)
GAL+REA+νeC+SUN68.27% CL (1σ)90.00% CL95.45% CL (2σ)99.00% CL99.73% CL (3σ)
(
K (T )
Q − T
)2
= 1− |Ue4|2 + |Ue4|
2
√
1−m24
(Q − T )2θ(Q − T −m4)
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 23/33
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Mainz Neutrino Mass Experiment[Kraus, Singer, Valerius, Weinheimer, arXiv:1210.4194]
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 24/33
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∆m241 Upper Bound
sin22ϑee
∆m412
[e
V2 ]
10−2 10−1 110−2
10−1
1
10
102
103
104
+
Osc. vs Mainz
68.27% CL (1σ)90.00% CL95.45% CL (2σ)99.00% CL99.73% CL (3σ)
Osc. vs Mainz
68.27% CL (1σ)90.00% CL95.45% CL (2σ)99.00% CL99.73% CL (3σ)
sin22ϑee
∆m412
[e
V2 ]
10−2 10−1 110−2
10−1
1
10
102
103
104
+
Osc. + Mainz
68.27% CL (1σ)90.00% CL95.45% CL (2σ)99.00% CL99.73% CL (3σ)
Osc. + Mainz
68.27% CL (1σ)90.00% CL95.45% CL (2σ)99.00% CL99.73% CL (3σ)
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 25/33
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KATRIN Sensitivity
[Formaggio, Barrett, PLB 706 (2011) 68]
10-2 10-1 110-2
10-1
1
10
20
Sin22ΘsD
m41
2He
V2 L
Bugey4+Rovno , 99% C.L.Bugey3 , 99% C.L.
global fit , 90% C.L.m1 = 2 eV , 90% C.L.m1 = 1 eV , 90% C.L.
m1 = 0 , 90% C.L.
[Esmaili, Peres, PRD 85 (2012) 117301]
[see also Sejersen Riis, Hannestad, JCAP (2011) 1475; Sejersen Riis, Hannestad, Weinheimer, PRC 84 (2011) 045503]
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 26/33
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Neutrinoless Double-β Decay0
24
68
10
mββ(4)
[eV]
∆χ2
EXO90% CL
KK10−3 10−2 10−1 1
68.27%
90%
95.45%
99%
99.73%
GAL+REA+νeC+SUN
|mββ| =∣
∣
∣
∑4k=1 U
2ek
mk
∣
∣
∣
m(4)ββ = |Ue4|
2√
∆m241
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 27/33
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Cancellation with m(light)ββ ?
[Barry, Rodejohann, Zhang, JHEP 07 (2011) 091]; Li, Liu, PLB 706 (2012) 406; Rodejohann, arXiv:1206.2560]
m(light)ββ =
∣
∣
∣
∣
∣
3∑
k=1
U2ek mk
∣
∣
∣
∣
∣
m(4)ββ = |Ue4|
2√
∆m241
mββ = m(light)ββ + e
iα4m(4)ββ m
(4)ββ & 10
−2 eV
◮ Normal Hierarchy: m(light)ββ . 4.5× 10
−3 eV (95%CL)no cancellation is possible
◮ Inverted Hierarchy: 1.4× 10−2 . m(light)ββ . 5.0× 10
−2 eV (95%CL)cancellation is possible
◮ Quasi-Degenerate: m(light)ββ & 5.0 × 10
−2 eV cancellation is possible
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 28/33
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Lightest mass: m1 [eV]
mββ
[e
V]
EXO90% CL
10−4 10−3 10−2 10−1 110−4
10−3
10−2
10−1
Normal Spectrum
1σ2σ3σ
Lightest mass: m3 [eV]
mββ
[e
V]
EXO90% CL
10−4 10−3 10−2 10−1 110−4
10−3
10−2
10−1
Inverted Spectrum
1σ2σ3σ
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 29/33
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Assumption: no cancellation
mββ ≥ m(4)ββ
= |Ue4|2√
∆m241
∆m241 =
m(4)ββ
|Ue4|2
2
≤
(
mββ
|Ue4|2
)2
sin22ϑee
∆m412
[e
V2 ]
EXO90% CL
KK
10−2 10−1 110−2
10−1
1
10
102
103
104
+
GAL+REA+νeC+SUN
68.27% CL (1σ)90.00% CL95.45% CL (2σ)99.00% CL99.73% CL (3σ)
GAL+REA+νeC+SUN
68.27% CL (1σ)90.00% CL95.45% CL (2σ)99.00% CL99.73% CL (3σ)
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 30/33
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Cosmology
◮ Ns = number of thermalized sterile neutrinos (not necessarily integer)[see Saviano talk]
◮ CMB and LSS in ΛCDM: Ns = 1.3 ± 0.9 ms < 0.66 eV (95% C.L.)[Hamann, Hannestad, Raffelt, Tamborra, Wong, PRL 105 (2010) 181301]
Ns = 1.61± 0.92 ms < 0.70 eV (95% C.L.)[Giusarma, Corsi, Archidiacono, de Putter, Melchiorri, Mena, Pandolfi, PRD 83 (2011) 115023]
◮ BBN:
{
Ns ≤ 1 at 95% C.L. [Mangano, Serpico, PLB 701 (2011) 296]Ns = 0.0 ± 0.5 [Pettini, Cooke, arXiv:1205.3785]
◮ CMB+LSS+BBN: Ns = 0.85+0.39−0.56 (95% C.L.)
[Hamann, Hannestad, Raffelt, Wong, JCAP 1109 (2011) 034]
◮ Standard ΛCDM: 3+1 allowed, 3+2 disfavored
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 31/33
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2 3 4 5 6 7Neff
0.0
0.5
1.0
1.5
2.0
∑ mν [
eV
]
CMBWMAP+CMBSPT+H(z)+SNLS+BAO+WiggleZ
CMBWMAP+H0CMBWMAP+H0+CMBSPTCMBWMAP+H0+H(z)
CMBWMAP+BAO
CMBWMAP+H0+WiggleZ
68% and 95% CL[Riemer-Sørensen, Parkinson, Davis, Blake, arXiv:1210.2131]
Σ mν
Ne
ff
0 0.5 1 1.5 2
2
4
6
8
CMB (blue), CMB+WL (red)CMB+BAO+OHD (magenta)CMB+BAO+SNIa (green)
CMB+WL+BAO+OHD+SNIa (cyan)
[Wang et al., arXiv:1210.2136]
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 32/33
-
Conclusions
◮ Cosmology◮ Very powerful probe of neutrino number and masses
◮ Model dependent. Thermalization loophole
◮ Bright future (Plank, . . . )
◮ Direct β-Decay Neutrino Mass Measurements◮ Model independent and robust
◮ Sensitive to large neutrino masses beyond three-neutrino mixing
◮ KATRIN will start in 2015
◮ Unclear future (bolometers, project 8: radio-frequency)
◮ Neutrinoless Double-β Decay◮ Crucial for Majorana discovery
◮ Sensitive to large neutrino masses beyond three-neutrino mixing
◮ Many running and future experiments
C. Giunti − Neutrino Masses − LIONeutrino2012 − 24 Oct 2012 − 33/33