LAGUNA

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LAGUNA

• Large Apparatus for Grand Unification and
  Neutrino Astronomy
• Future Observatory for n-Astronomy at low
  energies
• Search for proton decay (GUT)
• Detector for long-baseline experiments

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LAGUNADETECTOR LOCATIONS
Rrumania
Institute of Physics and Nuclear Engineering,
Bucharest IFIN-HH Romania
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Beneficiary for the design study 1.
(Coordinator) Swiss Federal Institute of
Technology Zurich ETH Zurich Switzerland 2.
University of Bern U-Bern Switzerland 3.
University of Jyväskylä U-Jyväskylä Finland 4.
University of Oulu U-Oulu Finland 5.
Kalliosuunnittelu Oy Rockplan Ltd Rockplan
Finland 6.Commissariat àlEnergie Atomique
/Direction des Sciencesde la Matière CEA
France 7.Institut National de Physique Nucléaire
et de Physique des Particules (CNRS/IN2P3) IN2P3
France 8.Max-Planck-Gesellschaft 9. Technische
Universität München TUM Germany 10.
H.Niewodniczanski Institute of Nuclear Physics of
the Polish IFJ PAN Poland 11. Academy of
Sciences, Krakow KGHM CUPRUM Ltd Research
and Development Centre KGHM CUPRUM Poland 12.
Mineral and Energy Economy Research Institute of
the Polish Academy of SciencesIGSMiEPAN
Poland 13. Laboratorio Subterraneo de Canfranc
LSC Spain 14. Universidad Autonoma, Madrid UAM
Spain 15. University of Granada UGR Spain 16.
University of Durham UDUR United Kingdom 17. The
University of Sheffield U-Sheffield United
Kingdom 18. Technodyne International Ltd
Technodyne United Kingdom 19. University of
Aarhus U-Aarhus Denmark 20. AGT Ingegneria Srl,
Perugia AGT Italy 21.Institute of Physics and
Nuclear Engineering, Bucharest IFIN-HH Romania
22. Lombardi Engineering Limited Lombardi
Switzerland
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FP 7 design study recommendations
LAGUNA Design of a pan-European Infrastructure
for Large Apparatus studying Grand Unification
and Neutrino Astrophysics Key questions in
particle and astroparticle physics can be
answered only by construction of new giant
underground observatories to search for rare
events and to study sources of terrestrial and
extra-terrestrial neutrinos. In this context,
the European Astroparticle Roadmap of 03/07, via
ApPEC and ASPERA, states ...recommend a new
large European infrastructure, an international
multi-purpose facility of 100-1000 kton scale for
improved studies of proton decay and low-energy
neutrinos. Water-Cherenkov, Liq. Scintillator
Liq. Argon should be evaluated as a common design
study together with the underground
infrastructure and eventual detection of
accelerator neutrino beams. This study should
take into account worldwide efforts and converge
by 2010... Furthermore, the latest particle
physics roadmap from CERN of 11/06
states ...very important non-accelerator
experiments takes place at the overlap of
particle and astroparticle physics exploring
otherwise inaccessible phenomena Council will
seek with ApPEC a coordinated strategy in these
areas of mutual interest.
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LAGUNALarge Apparatus for Grand Unificationand
Neutrino Astrophysics
100m
30m
coordinated FE Design StudyEuropean
Collaboration,FP7 Proposal APPEC Roadmap
LENAliquid scintillator13,500 PMs for 50 kt
targetWater Cerenkov muon veto
MEMPHYSWater Cerenkov 500 kt target in 3
tanks,3x 81,000 PMs
GLACIERliquid-Argon100 kt target, 20m
driftlength,28,000 PMs foor Cerenkov- und
szintillation
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• Location of Phyasalmi in Finnland

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• possible orientation of LENA tank

Blue zones are regions with high mechanical
stress due to horizontal rock pressure
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Cost estimate from rockplan predesign
study Excavation site investigation 55
M LAB construction tank 60 M Detector
Scintillator electronics 190 M Engeneering 30
M Costs not including Tax and 20 uncertainty
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Astrophysics

• Details of a gravitational collapse (Supernova
  Neutrinos)
• Studies of star formation in former epochs of the
  universe (Diffuse Supernovae Neutrinos
  Background DSNB)
• High precision studies of thermo-nuclear fusion
  processes (Solar Neutrinos)
• Test of geophysical models (Geo-neutrinos)

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Galactic Supernova in Lena
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OBSERVING SN NEUTRINOS sensitive to SN dynamics
-gt matter induced oscillation
Core Collapse
Event rate spectra

• f from simulations of SN explosions
• P from n oscillations simulations (density
  profile)
• s (well) known
• e under control

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Supernova neutrino luminosity (rough sketch)
T. Janka, MPA
Relative size of the different luminosities is
not well known it depends on uncertainties of
the explosion mechanism and the equation of
state of hot neutron star matter. Info on all
neutrino flavors and energies desired!
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All n flavours mono-energetic 15.1 MeV gamma line
ne interaction delayed coincidence with 11.0
msec
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Event rates in LENA
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Separation of SN models ?

• Yes, independent from oscillation model
  ! neutral current reactions in LENA
• e.g. TBP KRJ LL
• 12C 700 950
  2100
• n p 1500 2150 5750

Lawrence, Livermore
Berkeley,Arizona
Garching, Munich
for 8 solar mass progenitor and 10 kpc distance
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Neutrinos from remnanant Supernovae
Early star formation rate
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LENA Diffuse SN Background

• ne p -gt e n
• Delayed coincidence
• Spectral information
• Event rate depends on
• Supernova type II rates
• Supernova model
• Range 20 to 220 / 10 y
• Background 1 per year

M. Wurm et al., Phys. Rev D 75 (2007) 023007
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SN Neutrino predicted rates vary with -
distance and progenitor mass (here 10 kpc, 8
solar masses)- the used SN neutrino model
(mean energies, pinching)- neutrino physics
(value of q13, mass hierarchy) variation 10-19
x103 ev _at_ 10kpcAims- physics of the
core-collapse (neutronisation burst, n cooling
)- determine neutrino parameters- look for
matter oscillation effects (envelope, shock
wave, Earth)
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• Matter effects in the Earth
• mass hierarchy
• theta_13
• Matter effects in the SN
• mass hierarchy and theta_13
• time development of the shock wave?

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Solare Neutrinos
Since May 07 BOREXINO
Direct observation SuperK, SNO
Gallium integral
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BOREXINO 1st result (astro-ph 0708.2251v2)

• Scattering rate of 7Be solar n on electrons
• 7Be n Rate 47 7STAT 12SYS c/d/100 t

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Brexino new results
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Estimated sol Be7 spectrum for 2 days data in
LENA
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Expected from Borexino using new data Be7
neutrino flux with high precission (lt 10) B 8
neutrino spectrum to low energy - shape
information for oscillations New limit on
neutrino magnetic moment CNO flux measurement
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Geo-Neutrinos a new probe of Earths interior
gianni fiorentini, ferrara univ. _at_ n2004
Antineutrino detection with inverse ß-decay
reaction

• Determine the radiogenic contribution to
  terrestrial heat flow, only half of the energy
  emission from the earth is understood
• Test a fundamental geochemical paradigm about
  Earhs origin the Bulk Sylicate Earth
• Test un-orthodox / heretical models of Earths
  interior (K in the core, Herndon giant reactor)
• A new era of applied neutrino physics ?

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Where are U, Th and K?
crust
U. M.

• The crust (and the upper mantle only) are
  directly accessible to geochemical analysis.
• U, K and Th are lithofile, so they accumulate
  in the (continental) crust.
• U In the crust is
• Mc(U) (0.3-0.4)1017Kg.
• The 30 Km crust should contains roughly as much
  as the 3000 km deep mantle.
• Concerning other elements
• Th/U 4 and 40K/U 1

L. M.
Core

• For the lower mantle essentially no direct
  information one relies on data from meteorites
  through geo-(cosmo)-chemical (BSE) model
• According to geochemistry, no U, Th and K should
  be present in the core.

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What to use

• Bulk Silicate Earth Model
• Preliminary Reference Earth Model
• Laboratory Experiments suggesting potassium-iron
  alloys in the core

http//www.edu.pe.ca/southernkings/compositionch.h
tm
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• Proton Decay and LENA
• p K n
• This decay mode is favoured in SUSY theories
• The primary decay particle K is invisible in
  Water Cherenkov detectors
• It and the K-decay particles are visible in
  scintillation detectors
• Better energy solution further reduces
  background

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P -gt K n event structure
T (K) 105 MeV
t (K) 12.8 nsec K -gt m n
(63.5 ) K -gt p p0 (21.2 ) T
(m) 152 MeV T (p) 108 MeV
electromagnetic shower
E 135 MeV m -gt e
n n (t 2.2 ms) p -gt m n (T 4
MeV) m -gt e n n (t 2.2 ms)
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• 3 - fold coincidence !
• the first 2 events are monoenergetic !
• use time- and position correlation !
• How good can one separate the
• first two events ?
• ....results of a first Monte-Carlo calculation

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P decay into K and n
m
m
K
K
time (nsec)
Signal in LENA
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• Background
• Rejection
• monoenergetic K- and m-signal!
• position correlation
• pulse-shape analysis
• (after correction on
• reconstructed position)

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• In LENA, we expect a background of 5 / y
  without PSD discrimination
• and after PSD-analysis this could be suppressed
  in LENA to
• 0.25 / y ! (efficiency 70 )
• A 30 kt detector ( 1034 protons as target)
  would have a sensitivity of t lt a few 1034
  years for the K-decay after 10 years measuring
  time
• The minimal SUSY SU(5) model predicts the K-decay
  mode to be dominant with a partial lifetime
  varying from 1029y to 1035 y !
• actual best limit from SK t gt 6.7 x 1032 y
  (90 cl)

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Results on fundamental physics from borexino
counting test facility 1/100 of Brexino Target
mass

• electron decay
• Back et al.,Phys Lett.B 525 (2002) 29-40
• nucleon decay into invisible. channels.
• Back et al.,Phys Lett.B 563 (2003) 23-34
• ? magnetic moment
• Back et al.,Phys Lett.B 563 (2003) 35-47
• Heavy ? mixing
• Back et al.,JETP Lett. Vol.78 N.5 (2003) 261-266
• Pauli exclusion principle
• Eur.Phys.Journ. C (2004)

Lena 10000 CTF
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Conclusions

• Low Energy Neutrino Astrophysics is very
  successful (Borexino direct observation of
  sub-MeV neutrinos)
• Strong impact on questions in particle- and
  astrophysics
• New technologies (photo-sensors, extremely low
  level background)
• Strong European groups