Flavor ratios in neutrino telescopes for decay and oscillation measurements
Neutrino mixing at high energy neutrino telescopes
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Transcript of Neutrino mixing at high energy neutrino telescopes
Neutrino mixing at Neutrino mixing at high energy neutrino high energy neutrino
telescopes telescopes
Pasquale D. SerpicoPasquale D. Serpico
MPl –MunichMPl –Munich
CARE ’05 - ECFA/BENECARE ’05 - ECFA/BENE
• “Galactic -beams” and muon-damped sources
• Conclusions
• Neutrino telescopes: an overview
Overview of the TalkOverview of the Talk
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week – CERNCERN
• Neutrino mixing at neutrino telescopes
High-Energy High-Energy astronomy: a new skyastronomy: a new sky
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week – CERNCERN
NeutrinosNeutrinos a a powerful tool for powerful tool for high energy high energy astrophysicsastrophysics
+)Directional signal (differently from CR)
+)No absorption(differently from )
+) HE guaranteed(HECR & HEobserved
Main problem-)Small
50 m
1500 m
2500 m
300
m
IceCube Collaboration
Solutions (I)Solutions (I)
huge volumes
sparse instrumentation
natural media
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week – CERNCERN
1 km1 km3: : Gigaton Gigaton scale!scale!
80’s: DUMAND R&D
90’s: BAIKAL, AMANDA, NESTOR
2k’s: ANTARES, NEMO R&D
<2010: ICECUBE (km3 at the
SouthPole)
……? Mediterranean km3 (Km3Net)
AMANDAICECUBE
Mediterraneankm3
BAIKAL
DUMAND
Pylos
La Seyne
Capo Passero
Baikal
South Pole
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week – CERNCERN
Status of Optical Cherenkov TelescopesStatus of Optical Cherenkov Telescopes
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week –
CERNCERN
Flavour discrimination (I)Flavour discrimination (I)
+ N + N →→ + X (DIS) + X (DIS)11stst detection channel: detection channel: O(km) O(km) tracks tracksdirectional error: ~ 1°σ[log10(E/TeV)] : ~ 0.3coverage: 2energy range: ~ 50 GeV to 100 PeV
Cherenkov light cone(blue light)
optical sensors(PMT)
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week –
CERNCERN
Flavour discrimination (II)Flavour discrimination (II)22ndnd detection channel: detection channel: cascades from cascades from e e & &
CC CC + all flavors + all flavors NCNCdirectional error: ~ 10-40°σ[log10(E/TeV)] : ~ 0.1coverage: 4energy range: ~ 1 TeV to 100 PeV
ee + N + N →→ e + X (DIS) e + X (DIS)
“Glashow Resonance”
ee- →W- → anything-
e -
+ N + N →→ + X (DIS) + X (DIS)
E > few PeV
Unique to e enhanced at E ≈ 6.3
PeV
-
Gandhi et al. ‘95
Flavour discrimination (III)Flavour discrimination (III)
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week – CERNCERN
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week –
CERNCERN
3000 3000 kmkm2
Solutions (II)Solutions (II)
Upgoing shower (seen by Los Leones telescope)P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week –
CERNCERN
600 km radius,1.1 million km2
ANtarctic Impulsive Transient Antenna
Solutions (III)Solutions (III)
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week – CERNCERN
Astrophysical fluxes come from pp→Xp→X
flavour ratios at source → e:≈⅓:⅔:0at Earth after oscillations → e:≈⅓:⅓:⅓
quite insensitive to mixing parametersdsource>> Losc → no sensitivity to msol
2 , matm2
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week – CERNCERN
-telescopes and -telescopes and -mixing-mixing
Standard Paradigm: Neutrino mixing Standard Paradigm: Neutrino mixing studies studies
hopeless at high energy neutrino hopeless at high energy neutrino telescopestelescopes
I shall try to argue that this is misleading!
1. Standard oscillation phenomenology “rescues” signals, allowing some interesting measurements
2. Matter effects might imply observations sensitive to m2’s, e.g. to hierarchy
Only standard oscillation
Only standard oscillation
scenarios considered!
scenarios considered!
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week – CERNCERN
-telescopes and -telescopes and -mixing-mixing
3. Input from -mixing very important for diagnostics of astrophysical sources
4. “Peculiar” (but not “exotic”!) neutrino sources may exist sensitive to mixing parameters (including and CP)
Event rate of O(1 yr-1 sr-1) fortwo separable and contained showers with E ≈ PeV in a km3 -telescope
H. Athar et al. APP 18 (2003) 581
Atmospheric background issofter (relevant energy losses of mesons)-suppressed (prompt ) Losc(E≈TeV-PeV) is too large
Independent confirmation of the (large) mixing in the sector via appearence
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week – CERNCERN
A “rescued” signal: The Galactic diffuse A “rescued” signal: The Galactic diffuse
-flux from CR hitting Galactic matter develops a large -component via oscillations.
Earth matter effectEarth matter effect with a SN at IceCubewith a SN at IceCube
Dighe et al. 06 (2003) JCAP 005
Flux vs. time at IceCube + SK (or HK)can detect Earth matter effects(normal hierarchy and sin2 13 >10-3)Exploits high statisticsfor a galactic SN
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week – CERNCERN
Livermore
Garching
The measurable ratio
RGR ≡ eGR
CC≈ 15[Sin2 212 +(1-0.5 Sin2 212)] (=0oand =45o)
is sensitive both to mixing angles (mainly ) AND to the production mechanism (% of pp “contamination”
≡ )(Bhattacharjee & Gupta, astro-ph/0501191)
- -
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week – CERNCERN
-telescopes, the Glashow resonance and -telescopes, the Glashow resonance and 1212
“Standard” astrophysical sources produce both and via
pp→X p→X
Both give flavour ratios at production e:≈⅓:⅔:0
but pmainly gives e (via +), while pp almost equally e and e
-
-
=40o
=45o
=0o
=45o
=32.5o
=15o
=0o
=45o
=9o
=0o
=45o
=32.5o
=15o
=0o
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week – CERNCERN
-telescopes, the Glashow resonance and -telescopes, the Glashow resonance and 1212
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week –
CERNCERN
““Peculiar” high energy neutrino (re)sourcesPeculiar” high energy neutrino (re)sources
In both cases, the observable ratio of tracks to e+ showers
ee
is sensitive to crucial information of the neutrino mixing matrix !!!
R=R=
1. neutrons beams from nuclear dissociations → pure e
beam
-
2. pion beams from muon damped sources → pure
beam
-
P.S. & M. Kachelrieß PRL 94, 211102 (2005) [hep-ph/0502088],P.S., work in progress
Mixing Matrix UMixing Matrix U slk ≡ Sin lk , clk≡ Cos lk
•Matter effects negligible•dsource>> Losc :Terms sensitive to m2, sign(CP) average out•Also imply equal expressions for neutrinos and antineutrinos
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week – CERNCERN
Neutrino Mixing - ProbabilitiesNeutrino Mixing - Probabilities
Flavor ratios at detector
Flavor ratios at source
Sensitivity to Sensitivity to 13 13 (and (and 2323))
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week – CERNCERN
=/6 =/4
Variation of order 25-50% in 0o<< 10o, depending on
(=32.5o, best case CP=)
For =45o, R is reduced even to ½ of the canonical R=0.5
Note the octant
dependence!
R Pe
Pee+Pe
e
For experimental best fit =32.5o and =45o, the flux ratio has a maximal variation of about 30%
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week – CERNCERN
Sensitivity to Sensitivity to CPCP
NOTE: onlysensitive to
Cos (CP)[CP-even term]
not “direct”observation
of CP-violation
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week –
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Determination of the octant of Determination of the octant of 2323
R=Pe
Pee+Pe
Model-independent statement
R<0.21 → 23 > /4
Backgrounds can only increase R!
In cosmic rays, at E ≈ O(1 EeV) a transition between High-Z nuclei
of the Galactic spectrum (acceleration and confinementrequirements are alleviated) and p-dominated Extragalactic contribution is expected. Recent CR data support this
scenario
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week – CERNCERN
n from nuclei dissociations in matter and fields in (a few) galactic accelerators might become visible at EeV. Favored regions: Nuclear Bulge, dense clouds (high B-field) …
Neutrinos from nuclei in the GalaxyNeutrinos from nuclei in the Galaxy
L. Anchordoqui et al. Ann. Phys. 314 (2004) 145
AGASA reported a 4% excess in UHECR around 1018 eV (1 EeV) from a couple of hot-spots in the galactic disk
Similar, indepentent hints also from SUGAR and Fly’s Eye(but negative results from preliminary analysis of Auger
data)P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week – CERNCERN
Hint: A Galactic Plane excess in EeV Cosmic Hint: A Galactic Plane excess in EeV Cosmic RaysRays
Neutrons are natural candidates to explain the signal
no GMF bending (huge for p too!)
Energy-range of the Signal ≈ boosted n-lifetime
cn ≈ 10 kpc (En / EeV)
Harari et al. JHEP 9908
The birth of Galactic neutron Astronomy? The birth of Galactic neutron Astronomy?
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week – CERNCERN
This energy range nicely fits the energy-window accessible to -telescopes under construction.
If neutrons come from nuclear photodissociations on Optical/UV photons, the flux is likely to extend
down to (at least) TeV region
Notice that n are undetectable as CR anisotropies below E~ 1017 eV: similar sources of lower Energy might show-up only in the e channel !!!-
The existence of galactic neutron beams would imply e fluxes up to the PeV from n-decay.
(E / En ~ Q / mn ~ 10-3→ E ~ PeV, for En ~ EeV)
-
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week – CERNCERN
From Neutrons to Neutrinos From Neutrons to Neutrinos
L. Anchordoqui, H. Goldberg, F. Halzen & T.J. Weiler
PLB 593 (2004) 42
Normalizing to the CR anisotropy, ~ 20 events per year from Cygnus region in IceCube (under construction at the South pole)
In a few years, IceCube should attain discovery sensitivity for n → e → !!!
Standard oscillation phenomenology implies
≈ 4 /yr tracks in 0.7o circle (Atm. background is~2.3 /yr)≈ 16 e showers/yr in 25o,
cone, due to poor resolution.(Atm. background fluctuation is~12 e/yr)
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week – CERNCERN
Detectability in IceCubeDetectability in IceCube
Viable models of A → n → scenarios exist, e.g.:Cygnus region: L. Anchordoqui et al. PLB 593 (2004) 42SGR A East SN remnant: Grasso and Maccione
[astro-ph/0504323]
Within the expected statistical accuracy of IceCube & at the same subleading level of other effects neglected in our estimate
From astrophysical data e.g. on the Cygnus region (e.g. UV density) and hadronic physics data (e.g. secondary populationyields in hadronic interactions)
Vnuclear dissociation ≈ 27 x Vpp hadronic interactions
In this case, likely contaminations to flux are at the O(10%) level → R ≈ + 0.02 only!
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week – CERNCERN
How large is the expected “pion How large is the expected “pion contamination”? contamination”?
Normalizing the anisotropy to the “n-chain” model,
n → fluxes should easily observable in IceCube,
with a detailed measurement in a decade.
High flux and R=0.5 would disprove
the dominance of A → n →
Also -rays constraints!
If the chain dominates, the flux should be much
higher, though with a flavour ratio of about 1:1:1
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week – CERNCERN
Is this scenario falsifiable?Is this scenario falsifiable?
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week –
CERNCERN
Sensitivity to the octant of Sensitivity to the octant of 2323
Model-independent statement
R>0.78 → 23 > /4
Backgrounds can only decrease R!
R P
1-P
e
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week –
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Why pion beams?Why pion beams?
Effective “pion beams” produced in sources where muons (but not pions) are damped sources → pure beam-
For AGN, beams @ O(106) TeV → unobservable at OCTFor GRB, beams possibily @ O(10) TeV→ optimal for
OCT!!!Flavour ratios can be used for astrophysical diagnostics
Kahsti & Waxman, PRL 95 (2005) 181101
Boosted Lifetime E
E.m. cooling time E-1 (Inv. Compton), E0 adiabatic expansion),…Their ratio increases with E, at a certain 0 the particle is stopped before decaying. The lifetime implies 00
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week –
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Overview - IOverview - I
Neutrinotelescopes are optimized for astrophysical purposes, but they may have a potential for -mixing physics, too.
appearence expected to be seen within 3-4 years (IceCube completed + 1 year of running)
“Calorimentric” detection of a galactic core-collapse SN possible. Earth matter effect (and thus hierarchy/13) possibly identified at IceCube+”HK”, or +Mediterranean km3
I showed that it is conceivable or even likely that Nature might provide “-beams” (or pion beams) for free, that could be studied at -telescopes already in construction.
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week – CERNCERN
Overview - IIOverview - II
Going beyond the paradigm of a “canonical” flavor equipartition would repropose at neutrino telescopes the fruitful synergy between neutrino physics and astrophysical diagnostics
Measurable flavor ratios are sensitive to 13CP , and
to the octant of 23 The latter is particularly suitable
for a model-independent determination (if 23 /4)
Atmospheric/K2KAtmospheric/K2KBest FitSin2atm=0.5, matm
2=2.2 x 10-3 eV2
3 range 0.34 < Sin2 atm < 0.66; 1.4 x 10-3matm2/eV2 < 3.3 x
10-3
Best Fit:atm= 45°
3 range: 35.7 °< sol <54.3°
Solar/KamlandSolar/KamlandBest Fit:Sin2sol=0.29, msol
2=8.1 x 10-5 eV2
3 range: 0.23 < Sin2 12 < 0.37, 7.3x 10-5 msol2/eV2 <
9.1 x 10-5
Best Fit:sol= 32.6°
3 range: 28.7 °< sol <37.5°
Global (CHOOZ+others)Global (CHOOZ+others)Best Fit: Sin213 =03 range:Sin213<0.047, 13 <12.5°
Maltoni et al., Maltoni et al., NJP 6 (2004) 122NJP 6 (2004) 122
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week – CERNCERN
NNeutrino mixing parameterseutrino mixing parameters
R. Gandhi, C. Quigg, M. H. Reno and I. Sarcevic, Neutrino interactions at ultrahigh energies,
Phys. Rev. D 58, 093009 (1998) [hep-ph/9807264].
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week – CERNCERN
((N) vs. EN) vs. E
R. Gandhi, C. Quigg, M. H. Reno and I. Sarcevic, Neutrino interactions at ultrahigh energies,
Phys. Rev. D 58, 093009 (1998) [hep-ph/9807264].
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week – CERNCERN
((N) vs. EN) vs. E--
P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE P. D. Serpico, MPIfP (WHI)- Munich “Neutrino mixing @ HE telescopes” 23-25/11 /05 ECFA/BENE Week – telescopes” 23-25/11 /05 ECFA/BENE Week –
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Clarification on Clarification on CPCP
CP-even
CP-odd
Jarlskog determinant
Apollonio et al. hep-ph/0210192