1. MEMPHYS non-oscillation physics
NOW Conca Specchiulla 9-16/09/06
MEMPHYS non-oscillation physics
Alessandra Tonazzo
APC et Université Paris 7

2. Laboratoire Souterrain de Modane Contacts: J.E.Campagne and M.Mezzetto
The MEMPHYS detector
[see talk by S.Katsanevas]
Modane, France
Laboratoire Souterrain de Modane
Megaton Mass
Water Cherenkov (“cheap and stable”)
Total fiducial mass: 440 kt
Baseline:
3 Cylindrical modules 65X65 m
Size limited by light attenuation length (λ~80m) and pressure on PMTs
Readout: 12” PMTs, 30% geom. cover (#PEs =40%cov. with 20” PMTs)
PMT R&D + detailed study on excavation existing & ongoing
Frejus Tunnel
4800 m.w.e.
Bardonecchia, Italy
65m
60m
arXiv: hep-ex/
Contacts: J.E.Campagne and M.Mezzetto
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A.Tonazzo - MEMPHYS: non-oscillation physics

3. Physics goals (=outline of my talk)
SuperNovae core-collapse
Early SN trigger
Diffuse SuperNovae Neutrinos
Astrophysical sources of neutrinos
Proton decay
Oscillation measurements with  beams
[see talk by T.Schwetz]
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A.Tonazzo - MEMPHYS: non-oscillation physics

4. SN neutrinos @ detector
n emission
Flavor conversion
Shock wave
EARTH
[slide “stolen” from A.Mirizzi]
Core Collapse
Event rate spectra
f : from simulations of SN explosions
P : from n oscillations + simulations (density profile)
s : (well) known
e : under control
[see talk by Cardall]
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A.Tonazzo - MEMPHYS: non-oscillation physics

5. SN neutrinos Neutronization burst Accretion + K-H cooling
[see talk by Cardall]
Neutronization burst
E~1051 erg t~25 ms
Accretion + K-H cooling
E~1053 erg t~10 s
99% of total explosion energy
Propagation to Earth:
Matter effects Pee(12)
Level-crossing probability PH(E, V(x,t), m2,13)
Survival prob. p= Pee*PH
“Sensitivity to θ13 one order of magnitude better than planned terrrestrial experiments” [see for ex. Lunardini-Smirnov hep-ph/ ]
Hierarchy of interaction strength 
Fogli et al., hep-ph/
Raffelt et al., astro-ph/
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A.Tonazzo - MEMPHYS: non-oscillation physics

6. Detection of SN neutrinos
Inverse-beta (89%)
Large statistics in detectors with lots of free p
Good determination of  time and energy
Option: add Gd to tag neutron from delayed-γ
Elastic scattering (~3%)
Pointing
NC on Oxygen (8%) n
g
[see talk by Vagins] e-
ne,x
Fogli et al.,
hep-ph/
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A.Tonazzo - MEMPHYS: non-oscillation physics

7. A.Tonazzo - MEMPHYS: non-oscillation physics
MEMPHYS
Evidence up to ~1Mpc
Galactic SN: Huge statistics 
we can do spectral analyses
in time
in energy
in flavour composition
 Access to
SN explosion mechanism:
shock waves, neutronization burst
Neutrino production parameters:
rate, spectra
Neutrino properties
(a partial overview in the following)
Fogli et al.,
hep-ph/
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A.Tonazzo - MEMPHYS: non-oscillation physics

8. SN spectral analyses (1)
Extracting the astrophysical parameters
Learning about black-hole formation
Abrupt cut-off of neutrino
flux visible if a black-hole
forms in the middle of a
SN explosion
Just an example (“old” paper) to get a feeling of the sensitivity w.r.t. smaller detectors
Minakata et al.,
hep-ph/
from UNO whitepaper
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A.Tonazzo - MEMPHYS: non-oscillation physics

9. SN spectral analyses (2)
Learning about the shock wave
Crossing of resonances can induce time-dependent matter effects in neutrino oscillations
Shock-wave effects on survival probabilities (PH) depend on 13.
m2atm,13
m2sol,sol
 self-interactions ?
Duan et al.,
Raffelt et al.,
Schirato and Fuller, astro-ph/
Fogli et al., hep-ph/
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A.Tonazzo - MEMPHYS: non-oscillation physics

10. SN spectral analyses (2)
Learning about the shock wave
“Double-dip” in <Ee>
“Double-peak” in <E2e>/<Ee>2
vs time
Time-dips are Energy-dependent:
Compare bins of “low” and “high” E
Fogli et al., hep-ph/
Forward shock Forward+Reverse shock
IH shock
IH static NH
For NH, some information can be gathered from time-spectrum of e+O events
Tomas et al., astro-ph/
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A.Tonazzo - MEMPHYS: non-oscillation physics

11. SN spectral analyses (2’)
Stochastic density fluctuations behind the shock front
can have significant damping effects on the transition pattern and modify the observed spectrum
Fogli et al., hep-ph/
 =
fractional (random) variations of average  potential
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A.Tonazzo - MEMPHYS: non-oscillation physics

12. SN spectral analyses (3)
Earth matter effects
Dighe et al., hep-ph/
Modulations of energy spectrum
of and/or
Observable with a single detector in Fourier-transform of y~1/E
In water-Cherenkov, due to poor energy resolution, need >60k events:
For
Earth effect not seen  Inverted Hierarchy + large θ13
Earth effect seen  Degeneracy: NH or IH+small θ13
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A.Tonazzo - MEMPHYS: non-oscillation physics

13. SN spectral analyses (4)
Neutronization burst
Kachelrieβ et al., astro-ph/
Signal:
Bkg:
mainly
rejected by angle and E cuts + Gd n-tag
ES of other  flavours
Observation of time peak depends on oscillation scenario
Burst / no-burst  break degeneracy A/C if θ13 unknown
Measurement of SN distance within 5%
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A.Tonazzo - MEMPHYS: non-oscillation physics

14. A.Tonazzo - MEMPHYS: non-oscillation physics
SN trigger
Detection of SN from galaxies up to ~10Mpc
Coincidence of two neutrinos in the same detector within ~10sec
Bkg <0.7 ev/yr
Rate > 0.15/yr
 Identify SN without optical confirmation (= anticipate by few hrs)
 Detect SN heavily obscured by dust or optically dark
Neutrino-Optical coincidence
 improve knowledge of start time of core collapse from ~1day (optical) to ~10s
@Mton
RSN
@SK
Ando et al.,
astro-ph/
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A.Tonazzo - MEMPHYS: non-oscillation physics

15. Diffuse SN neutrinos We don’t need to wait and hope to be lucky…
[see talk by C.Lunardini]
(thanks for these slides!)
Lunardini, astro-ph/
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A.Tonazzo - MEMPHYS: non-oscillation physics

16. Diffuse SN ’s @H2O detectors
Small signal over very large bkg:
Decay e from “invisible ”
generated by CC interaction of -atm and with E<Cherenkov threshold
atmospheric e
Reactor (E<~10 MeV)
Can be reduced with Gd
(reject non- anti-e )
Malek et al. [SK Coll.],
hep-ex/
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A.Tonazzo - MEMPHYS: non-oscillation physics

17. Diffuse SN ’s @ MEMPHYS
We WILL see them
in few years
Direct measurement of  emission parameters
5y SK+Gd
=1y MEMPHYS+Gd
Fogli et al.,
hep-ph/
7-60 events in 4 yrs:
“most conservative” estimate
by C.Lunardini
What can we learn ?
astro-ph/
Yuksel et al.,
astro-ph/
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A.Tonazzo - MEMPHYS: non-oscillation physics

18. Diffuse SN ’s @ MEMPHYS
Decays of DSN
modifications of spectrum
Constraints on Dark Energy parameters
+estimate of SN rate from future SN surveys
10 y
with Gd
Mirizzi et al.,
hep-ph/
Hall et al.,
hep-ph/
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A.Tonazzo - MEMPHYS: non-oscillation physics

19. Neutrino astrophysics
Low-E ’s from GRB
accompanying UHE-’s and
optical emission seen in other
experiments
“GRB  background” detectable
in few years
’s from Black-Hole formation
death of stars with M>40Msun
’s from interaction of ’s “from below”
Point-sources, such as AGNs
WIMPs annihilating in Earth, Sun or Galaxy
[cfr SK analysis: hep-ex/ ]
High-E ’s from GRBs
Nagataki et al., astro-ph/
Sumiyoshi et al., astro-ph/
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A.Tonazzo - MEMPHYS: non-oscillation physics

20. A.Tonazzo - MEMPHYS: non-oscillation physics
Proton decay
Complete review:
Nath and Perez,
hep-ph/
Forbidden in SM
Non-SUSY GUTs (dim-6 operators)
Favours p  e+ 0
Predictions: p~ yrs
Predictions depend only on fermion mixing
SUSY GUTs (dim-4 and dim-5 operators)
Favours p  K+ nu-bar
Predictions: p~3x1033-3x1034 yrs
Predictions depend on SUSY particle spectrum, Higgs sector and fermion masses (note interplay with direct
Current limits by SuperKamiokande:
p  K+ nu-bar p>2.3x1033y
p  e+ 0 p>1.6x1033y
Complementarity of the two main decay channels
No dedicated study done for MEMPHYS: rely on UNO simulation results (see UNO whitepaper)
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A.Tonazzo - MEMPHYS: non-oscillation physics

21. A.Tonazzo - MEMPHYS: non-oscillation physics
Proton decay
Search for p  e+ π0
Main bkg:
Ask: 2 or 3 “e-like” rings, Ptot<PFermi, Minv~Mp
=> Eff. ~44%
MEMPHYS coverage 30% with 12”PMTs is equivalent to SK coverage 40% with 20”PMTs in terms of #PE
H2O is best for this channel
MEMPHYS
XXX
XXX
MEMPHYS
From UNO whitepaper
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A.Tonazzo - MEMPHYS: non-oscillation physics

22. Proton decay Search for p  K+ + anti- K below Ch. Threshold :
infer from decays 90% of K decay at rest
K decay channels:
K   monoenergetic 
+ 6.3 MeV prompt- from capture
K  +0 with 
H2O is not as good as
LAr, LScint for this channel
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A.Tonazzo - MEMPHYS: non-oscillation physics

23. A.Tonazzo - MEMPHYS: non-oscillation physics
Summary and outlook
MEMPHYS - Megaton Mass Fréjus
Supernova Explosion
Evidence up to 1 Mpc
Spectral analyses  information on explosion mechanism,  emission and propagation
Diffuse Supernova Neutrinos
Evidence within few years
Information on  emission parameters and more
Early SN trigger
Neutrino astrophysics
Proton decay:
Optimal detector for p  e+ π0
Important synergies with LAr, LiqScint  LAGUNA
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A.Tonazzo - MEMPHYS: non-oscillation physics

24. BACKUP

25. SN spectral analyses (2)
Learning about the shock wave: Normal Hierarchy
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A.Tonazzo - MEMPHYS: non-oscillation physics

26. A.Tonazzo - MEMPHYS: non-oscillation physics
SN187A by Lunardini
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A.Tonazzo - MEMPHYS: non-oscillation physics

27. A.Tonazzo - MEMPHYS: non-oscillation physics
SN1987A
Yukserl et al., astro-ph
Other analyses:
Jegerlehner et al., PRD 54 (1996) 1194
Lunardini, astro-ph/ (5-par fit)
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A.Tonazzo - MEMPHYS: non-oscillation physics

28. SN spectral analyses (2)
Learning about the shock wave
Time-dips are Energy-dependent:
Compare bins of “low” and “high” E
“Double-dip” in <Ee>
“Double-peak” in <E2e>/<Ee>2
vs time
Fogli et al., hep-ph/
Tomas et al., astro-ph/
NOW06 15/09/06
A.Tonazzo - MEMPHYS: non-oscillation physics