low energy neutrino astronomy · low energy neutrino astronomy ... liquid scintillator technology...
TRANSCRIPT
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LENA
Low Energy Neutrino Astronomy
Seminar Universität Tübingen
11.7.08
Lothar Oberauer, TUM
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Physics GoalsDiffuse Supernova Neutrino BackgroundProton DecayGalactic Supernova BurstSolar NeutrinosGeo neutrinosReactor neutrinosBeta-beam neutrinosAtmospheric neutrinosDark Matter indirect search
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Liquid Scintillator Technology
High light outputLow energy thresholdGood energy, timing, and position resolutionVariety of neutrino detection channelsInverse beta decay detection basically background free
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~ 50 kt Liquid Scintillator
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Large Liquid Scintillator Detectors
Counting Test FacilityCTF at Gran Sasso(Italy)
~ 5 tBOREXINO at Gran Sasso; 300 t; incl. buffer 1,4 kt
KamLAND (Japan) with 1kt scintillator
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BOREXINO Detector layout
Water Tank:γ and n shieldµ water Č detector208 PMTs in water2100 m3
Carbon steel plates
Scintillator:270 t PC+PPO in a 150 µm thick nylon vessel
Stainless Steel Sphere:2212 PMTs +
concentrators1350 m3
Nylon vessels:Inner: 4.25 mOuter: 5.50 m
Excellent shielding of external background
Increasing purity from outside to the central region
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BOREXINO
Neutrino electron scattering ν e −> ν e
Liquid scintillator technology (~300t):
Low energy threshold (~60 keV)
Good energy resolution (~4.5% @ 1 MeV)
Sensitivity on sub-MeV neutrinos
Online since May 16th, 2007
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First Detection of Solar 7-Be Neutrinos by BOREXINO
astro-ph:08053842
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Borexino results
N(Be) = 49 + 3 + 4 /(day x 100 t)N(SM-no-osc) = 74 + 4 /(day x 100 t)
⇒ ν-oscillation confirmed (large mixing angle solution)
⇒ ΦBe = (5.18 + 0.51) 109 /cm2 sec⇒ fBe = ΦBe/ΦSM = 1.02 + 0.10⇒ fpp = 1.005 + 0.008
⇒ fCNO < 3.8 (90% CL)- 0.020
_
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Search for theDiffuse Supernova Neutrino Background
in LENA
M. Wurm, F. v. Feilitzsch, M. Göger-Neff,T. Marrodán Undagoitia, L. Oberauer, W. Potzel, J. Winter
Technische Universität Mü[email protected]
http://www.e15.physik.tu-muenchen.de/research/lena.html
Phys.Rev.D 75 (2007) 023007
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DSNB Detection via inverse beta decay
Free protons as target
nepe +→+ +ν• Threshold 1.8 MeV
• Eν ~ Ee - Q (ν spectroscopy)
• suppress background via delayed coincidence method
n + p −> D + γ (2.2 MeV)
• position reconstruction => fiducial volume (suppress external background)
Delayed signal (~200 µs)
Prompt signal
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LENA at Pyhäsalmi (Finland)
dependent on SN model(assumed fSN=2.5)
LL:LL: 113113KRJ:KRJ: 100100TBP:TBP: 6060
dependent on SNRffSNSN=0.7=0.7 1717ffSNSN=2.5=2.5 100100ffSNSN=4.2=4.2 220220
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
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⌦ Due to the excellent background discrimination, a liquid-scintillator detector enables a detection of the Diffuse Supernova Neutrinos in an almost background-free energy window 10 to 30 MeV.
⌦ The discovery potential for the DSN in LENA is very high. According to current models, ~2 to 20events per year are expected.
⌦ After 10 years, statistics will be large enough to give constraints on both Supernova Rate and SN explosion models.
Diffuse Supernova Neutrino Background Detection
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GalacticSupernova
neutrino burst in LENA
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SN Neutrino predicted ratesvary with …- the used SN neutrino model(mean energies, pinching)
- neutrino physics(value of θ13, mass hierarchy)
variation: 10-19 x103 ev @ 10kpc
Aims- physics of the core-collapse- constraints on neutrino parameters- look for matter oscillation effects
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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?
• coherent neutrino oscillations ?
(neutrino self-interaction)
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Separation of SN models ?Possible independent from oscillation modeldue to neutral current reactions in LENA
TBP KRJ LL
12-C: 700 950 2100
Nu-p: 1500 2150 5700
for 8 solar mass progenitor and 10 kpc distance
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Supernova neutrinos with LENA
Antielectron ν spectrum with high precisionElectron ν flux with 8% - 11% precisionTotal flux via neutral current reactionsSeparation of SN modelsSpectroscopy of all ν flavorsTime evolution of neutrino burstDetails of SN gravitational collapseChance to separate low/high Θ13 and mass hierarchy (normal/inverted)
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Solar Neutrino Detection in LENA
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Solar Neutrinos and LENA
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Solar Neutrinos and LENA
High statistics in 7-BeSearch for time fluctuationsCNO and pep νTest of MSW effectSearch for non-standard ν interactionsCC and NC measurements of 8-BSpectrum deformation
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LENA and proton decay
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LENA and proton decay
High efficiency and very good background rejection for p -> K+ ν
Good time resolution:
K and µ, π from K decay (12 nsec)
K µ, π
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P -> K+ ν
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LENA and proton decay
High sensitivity to p -> K ν(eff. ~ 65% instead 6% in SKτ ~ 4 x 1034 y)
Sensitive to a variety of decay channels“invisible” modes, e.g. n -> ν ν νFor e.g. p -> e+ π0 we expect ~ 1033 y(work in progress)
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LENA and neutrinos from the
Earth
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Sensitivity on U, Th
Energy threshold
1st detection of Geo-neutrinos in KamLAND in 2005 (1kt liquid scintillator detector)
arbi
trary
uni
ts
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Expected event ratesBOREXINO around ~ 10 per year
LENAbetween ~ 3 x 102 and ~ 3 x 103 per year(in Pyhäsalmi, Finland, continental crust)this is extrapolated from KamLAND result
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Backgrounds in LENA
~ 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)
K. Hochmuth et al., Astropart.Phys. 27 (2007) 21-29
Can be statistically subtracted
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LENA and Geo-neutrinos
In LENA we expect between 300 to 3000 events per year (“best bet” ~ 1500 / year)Good signal / background ratiomost significant contribution can be subtracted statisticallySeparation of geological models
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LENA and other topics
-Beta beams
-Reactor neutrinos
-Atmospheric neutrinos
-Dark Matter search
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LENA and Reactor neutrinos
At Frejus ~ 17,000 events per yearHigh precision on solar oscillation parameter:∆m2
12 ∼ 1%Θ12 ∼ 10%
S.T. Petcov, T. Schwetz, Phys. Lett. B 642, (2006), 487
J. Kopp et al., JHEP 01 (2007), 053
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Atmospheric and beta beams
Separation between e- and µ-like eventsPulse shape discrimination (risetime, width)Muon decay µ −> e ν νWork in progress
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Dark Matter search
Light Wimp mass between 10 and 100 MeVAnnihilation under neutrino emission in the SunMonoenergetic electron-antineutrino detection in LENAS. Palomares-Ruiz, S. Pascoli, Phys. Rev. D 77, 025025 (2008)
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Technology studies for
LENA
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⇒Absorption length > 20 m
Scattering length ~ 20 m (@ 430 nm)
>
Preliminary result
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Results optical properties
PXE, LAB as candidates for the solventC14, Dodecane as additivesPPO, PMP, bis-MSB as wavelengthshiftersL ~ 180 pe/MeVλabs > 20 m, λsca ~ 20 m τsci ~ 3 nsec (PXE)Suitable for LENA => Towards a full optical model for LENATeresa Marrodan, Michael Wurm, Patrick Pfahler, Jürgen Winter, Andreas Ulrich
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PM encapsulation
Designed at TUM
Under successful operation in Borexino
Similar design for GERDA, DOUBLE-CHOOZ (Vetos)
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Light Cones
Designed and realized at TUM for
BOREXINO
Light enhancement ~ 2.5
Costs ~ 125 Euro / channel
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Underground Lab at TUMHigh sensitivity gammaspectroscopy
Neutron activationanalysis at FRM II (closeby)
•Low Background Technology for
BOREXINO,
CRESST,
DOUBLE-CHOOZ, LENA
Martin Hofmann, Niels Haag
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Pre-feasibility study for LENA at Pyhäsalmi
Contract with Rockplan, FinlandDepth at 1400 m – 1500 m possibleVertical positionLogistics (Vent, Electricity, etc.)Construction time of cavern ~ 4 yearsConstruction time of tank plus instrumentation ~ 4 years
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Cost Overview
Excavation, reinforcements 47 M€Infrastructure 28 M€Detector construction 37 M€Liquids, PMTs 185 M€Design, consulting 30 M€Reservations, uncertainty 82 M€Sum 409 M€
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One Option:
+ Tank Construction: 8 years
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Conclusions
LENA has a high discovery potentialScintillator optical properties within specificationSuitable candidates: LAB, PXEVarious wavelength-shifters Pre-feasibility study for LENA at Pyhäsalmi completed (Rockplan)
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LENA related papersM. Wurm et al., Phys.Rev.D 75 (2007) 023007
K. Hochmuth et al., Astropart.Phys. 27 (2007) 21-29
T. Marrodan et al., Phys. Rev. D 72 (2005) 075014
S.T. Petcov, T. Schwetz, Phys. Lett. B 642, (2006), 487J. Kopp et al., JHEP 01 (2007), 053 S. Palomares-Ruiz, S. Pascoli, Phys. Rev. D 77, 025025
(2008)