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LAGUNA and Neutrino Physics
NOW 2008Lothar Oberauer
TU München, Germany
LAGUNA Physics Large Apparatus for Grand Unification
and Neutrino Astrophysics Proton Decay Neutrinos as probes
Supernova neutrinos Solar neutrinosGeoneutrinos
Neutrino properties
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 => LSP is
Dark Matter candidate GU: motivation for See-Saw => small
masses
LAGUNA Physics Galactic Supernova neutrino burst
understanding of gravitational collapseneutrino properties: and mass hierarchymass effects on flavor transitions within the supernova and when passing through the Earthearly alert for astronomersBlack Hole formation?
Diffuse Supernova neutrinoslink to supernova rates => star formation rate; probing models of gravitational collapse
LAGUNA Physics Solar neutrinos
Search for small flux variations in timePrecise measurements of thermo nuclear fusion reactionsmeasurement of inner solar metallicity (CNO neutrinos at high statistics)
Neutrino beamsSearch for
Search for leptonic CP-violation (if is not to small)
LAGUNA Physics
Complementary to LHC and planned ILC goals
LHC: Higgs mechanism, SUSY, Rare decays
LAGUNA: Proton decay, neutrino astronomy, CP violation in leptons
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
LAGUNA structure and aims Proposed and accepted in the ApPEC
meeting at Munich in November 2005 Investigate common R&D 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
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
LAGUNA Collaboration
- Italy
LAGUNA CollaborationConsortium 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)
LAGUNA Detector types
Mt Water CherencovMEMPHIS
100kt Liquid ArgonGLACIER
50kt liquid ScintillatorLENA
MEMPHIS
TRE
MEMPHYS
1 shaft = 215 kt
water target
Possible location: extension of Frejus laboratory
Ongoing R&D for single photo detection
Synergy with HK (Japan) and UNO (USA)
MEMPHIS PROS
“Simple” DetectorLarge and useful experiences (SuperK)
CHALLENGESHuge amount of photo-sensors (>100,000)Very large underground cavitiesCosts?
Imaging with SuperK water Cherenkov detector
GLACIER: Liquid argon scintillation and electron TPC
φ≈70 m
h =20 mMax drift length
Passive perlite insulation
GLACIER
Liquid Argon TPC -> 10 to 100 kt target mass Pioneering work in ICARUS R&D
program Two independent programs:
GLACIER in Europe and LARTPC in USA
GLACIER PROS
Brilliant energy and track resolutionParticle ID and separationBasically background free for many applications
CHALLENGES“complicated” detector technologyHuge number of channels (depending on position resolution)Large span of the cavity
LENA: Liquid scintillator
LENA Low Energy Neutrino Astronomy -> 50 kt target mass R&D on liquid scintillators BOREXINO successful in measuring
solar neutrinos (7Be, 8B) DOUBLE-CHOOZ in France Hanohano project (10 kt at Hawai)
in USA
LENA
PROSMature technologyGood energy and position resolutionCavity, PMs electronics standard(size like SuperK, also number of PMs)
CHALLENGESKeep purity like BOREXINO but for 50 kt(relevant for solar neutrino detection in the sub-MeV range)
Sensitivities on Proton Decay p -> e+
Water Cherenkov MEMPHIS ca. 1035 y (5000 kt y exposure)Limit SK-I and II: xy
p -> K+ 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: xy
Sensitivity on Supernova MEMPHIS mainly sensitive on e
Approx. rate for 1 Mt:
~ 40 events @ 1 Mpc
Prop. < 10% per year
~ 4 events @ 3.3 Mpc
Prop. ~ 15% per year
~ 0.4 events @ 10 Mpc
Prop. ~ 80% per year
Sensitivity on Supernova
Sensitive on e !
Important for neutronisation phase
Sensitive on oscillation parameter and mass hierarchy
Sensitivity on Supernova
DSNB Detection via inverse beta decay Free protons as target
nepe • Threshold 1.8 MeV
• E~ Ee - Q ( spectroscopy)
• suppress background via delayed coincidence method
n + p D + (2.2 MeV)
• position reconstruction => fiducial volume (suppress external background)
Delayed signal (~200 s)
Prompt signal
LENA at Pyhäsalmi (Finland)
dependent on SN model(assumed fSN=2.5)
LL:LL: 113113KRJ:KRJ: 100100TBP:TBP: 6060
dependent on SNR
ffSNSN=0.7=0.7 17 17ffSNSN=2.5=2.5 100 100ffSNSN=4.2=4.2 220 220
DSN event rate in 10yrsinside the energy window
from 9.7 to 25 MeV
background events: 13~25% of events are due to v’soriginating from SN @ z>1!
TU München
Outline DSNB Background Event Rates Spectroscopy
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
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< 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
Long baseline oscillations
CPsign(M2)
e e
High Intensity conventional neutrino source.
“Superbeams”
Time scale > 2014 (?)
New neutrino source. “Betabeams, nu-factory”
Time scale ~ 2020 (?)
31
Laboratorio Subterraneo de Canfranc, Spain
LSCLSC
Laboratori Nazionali delGran Sasso, Italy
LNGS
SUNLABPolkowice-Sieroszowice,
Poland
Institute of UndergroundScience in Boulby mine, UK
IUS
Laboratoire Souterrainde Modane, France
L=630 L=630 kmkm
L=130 L=130 kmkm
L=2300
L=950
L=732 L=732 kmkm
L=1050 L=1050 kmkm
Long baseline oscillations
Study J-Parc -> Okinoshima
Distance 653 km
Power 1.66 MW
Measurement 5 years
(arXiv:0804.2111)
Similar results for ~ 300 kt Water Cherenkov (fiducial mass)
LENA and Reactor neutrinos
At Frejus ~ 17,000 events per year High precision on solar oscillation
parameter: m2
12
S.T. Petcov, T. Schwetz, Phys. Lett. B 642, (2006), 487
J. Kopp et al., JHEP 01 (2007), 053
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 LENAS. Palomares-Ruiz, S. Pascoli, Phys. Rev. D 77, 025025 (2008)
Conclusions
LAGUNA started July 2008 Physics program aims on GUT (p-
decay), LE astrophysics, oscillations High discovery potential Site studies for 7 candidates until 2010 LAGUNA is European but open for
world wide cooperation