Transcript LAGUNA and Neutrino Physics

LAGUNA and Neutrino Physics
NOW 2008
Lothar Oberauer
TU München, Germany
LAGUNA Physics
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Large Apparatus for Grand Unification and
Neutrino Astrophysics
Proton Decay
Neutrinos as probes
Supernova neutrinos
Solar neutrinos
Geoneutrinos
Neutrino properties
LAGUNA Physics
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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 n
masses
LAGUNA Physics
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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 => star formation
rate; probing models of gravitational collapse
LAGUNA Physics
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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)
LAGUNA Physics
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Complementary to LHC and planned
ILC goals
LHC: Higgs mechanism, SUSY, Rare
decays
LAGUNA: Proton decay, neutrino
astronomy, CP violation in leptons
LAGUNA
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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
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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
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LAGUNA Collaboration
- Italy
LAGUNA Collaboration
Consortium composed of 21 beneficiaries
9 university entities (ETHZ, U-Bern, U-Jyväskylä, UOULU, 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
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Mt Water Cherencov
MEMPHIS
100kt Liquid Argon
GLACIER
50kt liquid Scintillator
LENA
MEMPHIS
1 shaft = 215 kt
MEMPHYS
water target
TRE
Possible
location:
extension of
Frejus laboratory
Ongoing R&D for
single photo
detection
Synergy with HK
(Japan) and UNO
(USA)
MEMPHIS
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PROS
“Simple” Detector
Large and useful
experiences (SuperK)
CHALLENGES
Huge amount of photosensors (>100,000)
Very large underground
cavities
Costs?
Imaging with SuperK water Cherenkov
detector
GLACIER:
Liquid argon scintillation
and electron TPC
 ≈70 m
h =20 m
Max drift length
GLACIER
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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
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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
LENA:
Liquid
scintillator
LENA
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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
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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)
Sensitivities on Proton Decay
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p -> p0 e+
Water Cherenkov MEMPHIS ca. 1035 y (5000
kt y exposure)
Limit SK-I and II: t > 8.4 x 1033 y
p -> 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 > 2.3 x 1032 y
Sensitivity on Supernova n
MEMPHIS mainly sensitive
on ne
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 n
Sensitive on ne !
Important for
neutronisation
phase
Sensitive on
oscillation
parameter and
mass hierarchy
Sensitivity on Supernova n
DSNB Detection via inverse
beta decay
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Free protons as target
ne  p  e  n
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• Threshold 1.8 MeV
Delayed signal
(~200 ms)
Prompt signal
• En ~ Ee - Q (n spectroscopy)
• suppress background via delayed coincidence method
n + p -> D + g (2.2 MeV)
• position reconstruction => fiducial volume (suppress
external background)
Outline
DSNB
Background
LENA at Pyhäsalmi (Finland)
Event Rates
Spectroscopy
DSN event rate in 10yrs
inside the energy window
from 9.7 to 25 MeV
dependent on SN model
(assumed fSN=2.5)
LL:
KRJ:
TBP:
113
100
60
dependent on SNR
fSN=0.7 17
fSN=2.5 100
fSN=4.2 220
~25% of events are due to v’s
originating from SN @ z>1!
TU München
background events: 13
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
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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
Q13 dCP
nm -> ne
High Intensity
conventional neutrino
source.
“Superbeams”
Time scale > 2014 (?)
sign(DM2)
ne -> nm
New neutrino source.
“Betabeams, nu-factory”
Time scale ~ 2020 (?)
IUS
L=2300
Institute of Underground
Science in Boulby mine, UK
SUNLAB
Polkowice-Sieroszowice,
Poland
Laboratoire Souterrain
de Modane, France
LSC
Laboratorio Subterraneo
de Canfranc, Spain
L=1050
km
L=630
km
L=950
L=732
km
L=130
km
LNGS
Laboratori Nazionali del
Gran Sasso, Italy
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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
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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
LENA and indirect Dark Matter
search
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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)
Conclusions
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LAGUNA started July 2008
Physics program aims on GUT (pdecay), LE n astrophysics, n oscillations
High discovery potential
Site studies for 7 candidates until 2010
LAGUNA is European but open for world
wide cooperation