LAGUNA and Neutrino Physics

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LAGUNA and Neutrino Physics

• NOW 2008
• Lothar Oberauer
• TU München, Germany

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LAGUNA Physics

• Large Apparatus for Grand Unification and
  Neutrino Astrophysics
• Proton Decay
• Neutrinos as probes
• Supernova neutrinos
• Solar neutrinos
• Geoneutrinos
• Neutrino properties

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LAGUNA Physics

• Detecting proton decay implies de facto discovery
  of Grand Unification (GU)
• GU new symmetry between quarks and leptons
• GU guide of fermion masses and mixing
• GU one motivation for SUSY gt LSP is Dark Matter
  candidate
• GU motivation for See-Saw gt small n masses

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LAGUNA Physics

• Galactic Supernova neutrino burst
• understanding of gravitational collapse
• neutrino properties Q13 and mass hierarchy
• mass effects on flavor transitions within the
  supernova and when passing through the Earth
• early alert for astronomers
• Black Hole formation?
• Diffuse Supernova neutrinos
• link to supernova rates gt star formation rate
  probing models of gravitational collapse

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LAGUNA Physics

• Solar neutrinos
• Search for small flux variations in time
• Precise measurements of thermo nuclear fusion
  reactions
• measurement of inner solar metallicity (CNO
  neutrinos at high statistics)
• Neutrino beams
• Search for Q13
• Search for leptonic CP-violation (if Q13 is not
  to small)

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LAGUNA Physics

• Complementary to LHC and planned ILC goals
• LHC Higgs mechanism, SUSY, Rare decays
• LAGUNA Proton decay, neutrino astronomy, CP
  violation in leptons

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LAGUNA

• European ApPEC roadmap recommendation
• We recommend that a new large European
  infrastructure is put forward, as a
• future international multi-purpose facility
  on the 105-106 ton scale for improved
• studies of
• proton decay and of
• low-energy neutrinos from astrophysical
  origin

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LAGUNA structure and aims

• Proposed and accepted in the ApPEC meeting at
  Munich in November 2005
• Investigate common RD requirements
• Coherent work on common problems
• Take advantage of acquired technological know-how
  in Europe
• Kick-off meeting at ETH Zurich 3-4 July 07
• Mature design and proposals should emerge in 2010

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LAGUNA financial situation

• Design Study for future European observatory
• Volume of proposal 5 M
• Approved as a whole by the European Commission
  (EC)
• Funding 1.7 M
• Focus on the part of the programme which cannot
  be performed on a national (regional) basis
• Underground Sites infrastructure studies
• 2008 until 2010

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LAGUNA Collaboration
- Italy
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LAGUNA Collaboration

• Consortium composed of 21 beneficiaries
• 9 university entities (ETHZ, U-Bern, U-Jyväskylä,
  U-OULU, TUM, UAM, UDUR, USFD, UA)
• 8 research organizations (CEA, IN2P3, MPG, IPJ
  PAN, KGHM CUPRUM, GSMiE PAN, LSC, IFIN-HH)
• 4 SMEs (Rockplan, Technodyne, AGT, Lombardi)
• Additional university participants (IPJ Warsaw,
  U-Silesia, U-Wroclaw, U-Granada)

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LAGUNA Detector types

• Mt Water Cherencov
• MEMPHIS
• 100kt Liquid Argon
• GLACIER
• 50kt liquid Scintillator
• LENA

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MEMPHIS
1 shaft 215 kt water target Possible location
extension of Frejus laboratory Ongoing RD for
single photo detection Synergy with HK (Japan)
and UNO (USA)
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MEMPHIS

• PROS
• Simple Detector
• Large and useful experiences (SuperK)
• CHALLENGES
• Huge amount of photo-sensors (gt100,000)
• Very large underground cavities
• Costs?

Imaging with SuperK water Cherenkov detector
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GLACIER Liquid argon scintillation and electron
TPC
f70 m
h 20 m Max drift length
Passive perlite insulation
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GLACIER

• Liquid Argon TPC
• -gt 10 to 100 kt target mass
• Pioneering work in ICARUS RD program
• Two independent programs GLACIER in Europe and
  LARTPC in USA

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GLACIER

• PROS
• Brilliant energy and track resolution
• Particle ID and separation
• Basically background free for many applications
• CHALLENGES
• complicated detector technology
• Huge number of channels (depending on position
  resolution)
• Large span of the cavity

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LENA Liquid scintillator
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LENA

• Low Energy Neutrino Astronomy
• -gt 50 kt target mass
• RD on liquid scintillators
• BOREXINO successful in measuring solar neutrinos
  (7Be, 8B)
• DOUBLE-CHOOZ in France
• Hanohano project (10 kt at Hawai) in USA

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LENA

• PROS
• Mature technology
• Good energy and position resolution
• Cavity, PMs electronics standard
• (size like SuperK, also number of PMs)
• CHALLENGES
• Keep purity like BOREXINO but for 50 kt
• (relevant for solar neutrino detection in the
  sub-MeV range)

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Sensitivities on Proton Decay

• p -gt p0 e
• Water Cherenkov MEMPHIS ca. 1035 y (5000 kt y
  exposure)
• Limit SK-I and II t gt 8.4 x 1033 y
• p -gt K n
• Liquid Argon GLACIER ca. 1035 y (1000 kt y
  exposure)
• Liquid Scintillator LENA ca. 5 x 1034 y (500 kt
  y exposure)
• Limit SK-I t gt 2.3 x 1032 y

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Sensitivity on Supernova n
MEMPHIS mainly sensitive on ne Approx. rate for 1
Mt 40 events _at_ 1 Mpc Prop. lt 10 per year 4
events _at_ 3.3 Mpc Prop. 15 per year 0.4
events _at_ 10 Mpc Prop. 80 per year
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Sensitivity on Supernova n
Sensitive on ne ! Important for neutronisation
phase Sensitive on oscillation parameter and mass
hierarchy
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Sensitivity on Supernova n
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DSNB Detection via inverse beta decay

• Free protons as target

Delayed signal (200 ms)

• Threshold 1.8 MeV
• En Ee - Q (n spectroscopy)
• suppress background via delayed coincidence
  method
• n p -gt D g (2.2 MeV)
• position reconstruction gt fiducial volume
  (suppress external background)

Prompt signal
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LENA at Pyhäsalmi (Finland)
Outline DSNB
Background Event Rates
Spectroscopy
DSN event rate in 10yrsinside the energy window
from 9.7 to 25 MeV
25 of events are due to vsoriginating from SN
_at_ zgt1!
background events 13
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Solar Neutrinos

• 8B neutrinos MEMPHIS, GLACIER, LENA
• CNO and pep LENA ( 300 / d)
• 7Be LENA ( 6000/ d)
• Precise measurement of LMA prediction
• Accurate measurement of inner solar metallicity
• Search for small flux variations

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GEO Neutrinos

• LENA
• rate between 3 x 102 and 3 x 103 per year (at
  Pyhäsalmi, Finland)
• Background 240 per year in 1.8 MeV 3.2
  MeV from reactor neutrinos
• lt 30 per year due to 210Po alpha-n reaction on
  13C (Borexino purity assumed)
• 1 per year due to cosmogenic background
• (9Li - beta-neutron cascade)

Can be statistically subtracted
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Long baseline oscillations
Q13 dCP sign(DM2) nm -gt ne ne -gt nm
New neutrino source. Betabeams, nu-factory Time
scale 2020 (?)
High Intensity conventional neutrino
source. Superbeams Time scale gt 2014 (?)
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Long baseline oscillations
Study J-Parc -gt Okinoshima Distance 653 km Power
1.66 MW Measurement 5 years (arXiv0804.2111) Sim
ilar results for 300 kt Water Cherenkov
(fiducial mass)
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LENA and Reactor neutrinos

• At Frejus 17,000 events per year
• High precision on solar oscillation parameter
• Dm212 1
• Q12 10

S.T. Petcov, T. Schwetz, Phys. Lett. B 642,
(2006), 487 J. Kopp et al., JHEP 01 (2007), 053
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LENA and indirect Dark Matter search

• Light Wimp mass between 10 and 100 MeV
• Annihilation under neutrino emission in the Sun
• Monoenergetic electron-antineutrino detection in
  LENA
• S. Palomares-Ruiz, S. Pascoli, Phys. Rev. D 77,
  025025 (2008)

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Conclusions

• LAGUNA started July 2008
• Physics program aims on GUT (p-decay), LE n
  astrophysics, n oscillations
• High discovery potential
• Site studies for 7 candidates until 2010
• LAGUNA is European but open for world wide
  cooperation