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Status of the BOREXINO experiment. Hardy Simgen Max-Planck-Institut für Kernphysik / Heidelberg for the BOREXINO collaboration. Outline. BOREXINO physics program The BOREXINO detector Scintillator purification techniques Removal of gaseous impurities 11 C background reduction - PowerPoint PPT Presentation
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Status of the BOREXINO experiment
Hardy SimgenMax-Planck-Institut für Kernphysik / Heidelberg
for the BOREXINO collaboration
Outline
BOREXINO physics program The BOREXINO detector Scintillator purification techniques
Removal of gaseous impurities 11C background reduction Water and scintillator filling First neutrino events: The CNGS beam Conclusions
The Borexino Collaboration Italy (INFN & University of Milano and
Genova, Perugia Univ., LNGS) USA (Princeton Univ., Virginia Tech) Russia (RRC KI, JINR, INP MSU, INP
St. Petersburg) Germany (MPIK Heidelberg,
TU München) France (APC Paris) Hungary (Research Institute for
Particle & Nuclear Physics) Poland (Institute of Physics,
Jagiellonian University, Cracow)
BOREXINO physics program
Solar neutrinos
Supernova neutrinos
Reactor anti-neutrinos
Geological anti-neutrinos
Rare decay search
Solar neutrino physics
Two types of solar neutrino experiments Radiochemical experiments (low energy
threshold, integrated flux) Water experiments (real-time information, higher
energy threshold: Only ~10-4 of total flux)
BOREXINO (and KamLAND solar phase): 1st real-time experiment at low energies
Solar neutrino spectrum
BOREXINO
m2 ≈ 8·10-5 eV2
27< < 38°Vacuum
oscillations
Matter effects
Transition region
Solar neutrino physics
Measurement of 7Be--flux (~35 per day) 10% measurement yields pp--flux with <1%
uncertainty (Gallium experiments!) Measurement of pep--flux (~1 per day)
directly linked with pp--flux Measurement of CNO--fluxes (~1 per day)
Energy production in heavy stars SS
M +
fla
vour
con
vers
ion
Supernova neutrinos
Main reaction channels
NEvents
Inverse beta decay (anti-e)
~80
12C(,’)12C*(E= 15.1 MeV)
~20
-proton elastic scattering
~55
Galactic supernova: 10 kpc 31053 ergs
threshold: 250 keV
Anti-neutrino physics: European reactors
Gran Sasso laboratory
≥ 800 km baseline
Averaged oscillation signal expected.
Anti-neutrino physics:Geo-neutrinos from U/Th
KamLAND resultsNature 436 (2005) 499-503.
Expected spectrum:
Large fraction of earth’s total heat (40 TW) from radioactivity (U/Th).
e-
Radiopurity requirements in the BOREXINO scintillator
Expected 7Be-ν-rate: ~35 events per day Each background contribution ≤1 event per day
14C/12C ~10-18
natK (40K) ~10-14 g/g (10-18 g/g)232Th ~10-16 g/g
238U (226Ra) ~10-16 g/g (3·10-23 g/g)
Ar (39Ar) ~70 Vol.-ppb (STP)
Kr (85Kr) ~0.1 Vol.-ppt (STP)
Suppression of radioactive background
15 years of R&D: Development of new purification and detection techniques
Careful material selection (-spectrometry, mass spectrometry, 222Rn emanation studies) e.g. Inner Vessel: U/Th: ~10-12 g/g
222Rn emanation: <1 Bq/m2
Scintillator purification: Distillation, H2O extraction, Silicagel column,
nitrogen sparging
BOREXINO purification columns
Counting Test Facility (CTF)
Experimentally proven:Purity requirements can be fulfilled!
Example: Nitrogen sparging of scintillator
Countercurrent N2/PC flow
Gaseous impurities transferred to N2
Achievable purity determined by N2 purity
Ultrapure N2 required!
N2 purity requirements
PC Nitrogen
Argon (39Ar) <70 vol-ppb <0.4 vol-ppm
Krypton (85Kr) <0.1 vol-ppt <0.1 vol-ppt222Rn (210Pb) <70 Bq/m3 (STP) <7 Bq/m3 (STP)
BOREXINO N2 purification plant
Production rate: 100 m3/h222Rn ≤0.5 Bq/m3 (STP)
≤1 222Rn-atom in 4 m3!
Nitrogen tests
Nitrogen from different European suppliers investigated.
Several plants can produce low Ar/Kr N2
However, strong deviations after delivery (contamination during storage, transport and refilling)
N2 delivery chain has to be tested under realistic conditions
SOL LN2-tank @ MPIK
Delivery chain succesfully tested:
Ar: ~0.01 ppb (Goal: 0.4 ppm)Kr: ~0.02 ppt (Goal: 0.1 ppt)
11C background reduction
Cylindrical cut around muon-track
Spherical cut aroundneutron capture to reject 11C event
11C production with neutron (95% prob)
PR C 71, 055805 (2005)
Vetoing the intersection of the 2 volumes for 5-10 11C-lifetimes.11C production measured in CTF: PR C 74, 045805 (2006)
Main background for pep / CNO neutrinos: Cosmogenically produced 11C muon track
BOREXINO filling
Long stop after spill accident in 2002 Improvement of Gran Sasso safety and
environmental standards Operations with liquid resumed in 2006 BOREXINO filling strategy:
1: Filling inner detector with pure water
2: Replacing water by scintillator
3: Using same (+new) water to fill outer detector
PC procurement
Since January: Fresh-PC trucking from Sarroch to LNGS
Background data taking started
The CNGSneutrino beam
-beam from CERN
Laura Perasso
First neutrino events
First CNGS run in August 200630 h of data taking
55 t of water (hmax ~1.8 m) No reconstruction, only
time difference used Expectation:
5 -events (neutrino interactions in the rock)
seen 5 events
Second CNGS run in October
Detector filled with 1120 t of water (80% full), hmax ~ 10 m
10 h of running timeExpected:
10 CNGS events
seen: 12 events
A CNGS event
from CERN
Conclusions
After a long forced stop: BOREXINO water filling started in August 2006 Scintillator filling since end 2006 Detector is alive: Background data taking has
started (not yet fully shielded) First -events from CNGS beam detected BOREXINO detector expected to be in its final
configuration around May
Physics data taking in 2007!