SNO+ ArtFest, May 2014, Kingston Dr. Christine Kraus...
Transcript of SNO+ ArtFest, May 2014, Kingston Dr. Christine Kraus...
SNO+ IS LOCATED AT SNOLAB
300 km
2 km or
6000 m.w.e.
CanadaOntarioSudburyCreighton mine
use existing SNO cavity
2Artfest 2014, Christine Kraus, Laurentian University
SNO DETECTOR (INHERITED)
1000 tonnes D2O
12 m acrylic vessel
1700 t H2O (inner)
18 m PSUP
5300 t H2O (outer)~9500 PMTs54% coverage
DCR = Deck Clean Room
Acrylic vessel AV,filled with 1000 tonnes of heavy water: 1999-2006 data takingin 3 phases (different n detection methods)
sunset in Sudbury
3Artfest May 2014, Christine Kraus, Laurentian University
780 tonnes liquid
org. scintillator
Hold-down
ropenet
LIQUID SCINTILLATOR
Detector to be filled with 780 tonnes of organic liquid scintillator (LS)
More light yield than Čerenkov , around 400 p.e./MeV, enabling lower energy threshold
Linear alkylbenzene (LAB)
High light yield
Long attenuation length
Safe: high flash point and low toxicity
More affordable than other scintillators
Add wavelength shifter
Initial plan: 2g/L PPO fluor4
SNO+ liquid scintillator ! Detector to be filled with 780 tonnes of organic liquid
scintillator
! ~100 times more light yield than Čerenkov ~ lower energy threshold
! Linear alkylebenzene (LAB) - High light yield
- Long attenuation length
- Safe: high flash point and low toxicity
- Cheaper than other scintillators
! 2g/L PPO fluor shifts the wavelength of the emitted light into detectable region
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Artfest May 2014, Christine Kraus, Laurentian University
SNO+ PHYSICS GOALS
Neutrinoless double beta decay
– scintillator loaded with 130Te
(0.3% loading – 800 kg of 130Te)
Geo- and Reactor neutrinos
Supernova neutrinos
Solar neutrinos (pep, CNO, low 8B)
Nucleon decay, sterile neutrinos
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Multi-purposedetector
Artfest May 2014, Christine Kraus, Laurentian University
NEUTRINOLESS DOUBLE BETA DECAY
Loading the scintillator with isotope
Can compare with and without source in the same detector
Can in principle investigate several isotopes with the same detector
What is the best isotope?
Originally decided on 150Nd due to it’s high Q-value and phase
space (away from many backgrounds), were hoping for
possibility to enrich
In principle SNO+ can measure different isotopes (source in/out)
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Artfest May 2014, Christine Kraus, Laurentian University
DOUBLE BETA ISOTOPES
35 known isotopesDecay
candidate
Q-
value
(MeV)
% natural
abundance
48Ca48Ti 4.271 0.187
76Ge76Se 2.040 7.8
82Ca82Kr 2.995 9.2
96Zr96Mo 3.350 2.8
100Mo100Ru 3.034 9.6
110Pd110Cd 2.013 11.8
116Cd116Sn 2.802 7.5
124Sn124Te 2.228 5.64
130Te130Xe 2.533 34.1
136Xe136Ba 2.479 8.9
150Nd150Sm 3.367 5.67
Artfest May 2014, Christine Kraus, Laurentian University
SNO+ WITH TELLURIUM
Fall 2011: Biller and Chen initiate new investigation by subgroup of collaboration
Early 2012: new loading techniques for Te in liquid scintillator was developed by Yeh at al.
Detailed studies of purification, optics properties, backgrounds by the collaboration followed
Also independent review and verification studies were completed
March 2013 – collaboration decides to focus on 130Te as the double beta isotope to pursue
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Artfest May 2014, Christine Kraus, Laurentian University
ADVANTAGES OF TELLURIUM
34% natural abundance
2νββ rate is low
no inherent optical absorption lines
High values of loading feasible (default 0.3%)
Internal U/Th background can be actively
suppressed by identifying 214Bi-214Po alphas
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Artfest May 2014, Christine Kraus, Laurentian University
LOADING SCINTILLATOR (BNL)
Conventional
Loading
Method
Carboxylate
Organometallic
Complex
New loading technique (BNL):
Dissolve telluric acid in water and add a few
percent of this mixture to LAB using a
surfactant. Clear and stable has been
demonstrated for more than 1 year.
ICP-MS determined U/Th content of telluric
acid to be 2-3 times 1011 g/g
U/Th purification factors of >400 in a single
pass have been achieved. 10
Artfest May 2014, Christine Kraus, Laurentian University
SNO+ EXPECTED SPECTRUM
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Expected
sensitivity
is below
100 meV
for 0.3%
loading
(800 kg)
★ 2 years lifetime and fiducial volume cut at 3.5 m (20%)
★ > 99.99% efficient 214 Bi tag, 97% efficient internal 208Tl tag
★ Factor 50 reduction 212BiPo and negligible cosmogenic isotopes
★ m0ν2β= 200 meV assumed for this plot
Artfest May 2014, Christine Kraus, Laurentian University
SOLAR NEUTRINOS: PEP
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★ pep solar neutrino component is favorable:
- single energy (1.442 MeV) and well predicted flux (1.1%)
★ Probes the vacuum-matter transition region
★ Can be measured during pure liquid scintillator phase
Probability vs. Energy Simulated spectrum
8Bpep
CNO
Artfest May 2014, Christine Kraus, Laurentian University
CONSTRUCTION STATUS
Hold-down system completed, Hold-up ropes exchanged
Water fill of cavity started
Cleaning the inner surface of AV completed
Scintillator purification plant coming together
STF completed, testing upcoming
PMT repairs ongoing
Calibration hardware starting to be installed
Detector electronics commissioning – air filled running
New covergas system installed and commissioned
Fiber system and camera system partially installed
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Artfest May 2014, Christine Kraus, Laurentian University
HOLD-DOWN SYSTEM
Feb. 2011: Install tarp –
Cleanliness protection May 2011:
drill 80 + 15 holes
Jan 2012
Install rope net
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Pre-tensioning – Jan 2013
May 2013: Set positions for
AV and hold-down sys.Jan 2012:
Replace hold-up
ropes
Sep 2013
Shorten hold-up
ropes
Completed !
Artfest May 2014, Christine Kraus, Laurentian University
AV CLEANING COMPLETE !
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Suspended
platform Carousel and access
Inside AV, looking
down Outside AV
Cleaning ladder
Cleaning entire
Inner surface:
Jan-Mar 2013
Artfest May 2014, Christine Kraus, Laurentian University
SCINTILLATOR PLANT
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All vessels, kettles,
etc. underground
and installation
ongoing
He-leak checking
of components
mostly completed
Large column
Slung, arriving UG
2h fire walls
Piping to do
Fire protection and
suppression to be
completed
Artfest May 2014, Christine Kraus, Laurentian University
DETECTOR
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Upgrade electronics, bring everything online
DAQ tests, LED system tests, air-filled running
Repair PMTs ~300 so far
Install
UI and acrylic pipes
May 2013
Getting ready for running with water - 2013
Artfest May 2014, Christine Kraus, Laurentian University
SNO+ DARK RUNNING – DECEMBER 2013
AND FEBRUARY 2014
With about 200 PMTs under water, turned on complete detector
with HV and ran for 8 days
Training detector experts and commissioning system components
Weekend and night shifts operated from surface
Took full set of PMT calibration data: electronics and timing
Data to test PMT calibration code
Testing new monitoring tools
Artfest May 2014, Christine Kraus, Laurentian University
WATER LINE – DECEMBER 2013
4 (out of 19) crates with HV, rates for PMTs
Under water higher (as expected)
Artfest May 2014, Christine Kraus, Laurentian University
USING INSTALLED FIBERS – FEBRUARY 2014
Water level 12 ft from cavity floor
Timing calibration data
Testing system
Stress test for DAQ
Optical calibration without need to Insert source into the detector, Minimize contamination risk.
Artfest May 2014, Christine Kraus, Laurentian University
FIBER DATA
11.2 million events total for timing calibrationArtfest May 2014, Christine Kraus, Laurentian University
NEW COVER GAS SYSTEM WAS
INSTALLED AND TESTED
Artfest May 2014, Christine Kraus, Laurentian University
SUMMARY AND OUTLOOK
Water fill has begun, plan to be filled by the end of the year
Remaining PSUP installations (fibers, cameras, etc.)
Water phase data taking (2014)
Fill with scintillator – start background studies
Introduction of isotope in stages: 2015
Exciting times ahead
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Artfest May 2014, Christine Kraus, Laurentian University
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Oxford UniversitySussex University
Liverpool UniversityQueen Mary UniversityLancaster University
University of PennsylvaniaUniversity of Chicago
University of Washington Armstrong Atlantic UniversityUniversity of North Carolina
UC Berkeley and LBNLUC Davis
Queen’s UniversityLaurentian UniversityUniversity of Alberta
TRIUMF
SNOLAB
LIP Lisboa and
CoimbraTechnical University
of Dresden
YESTERDAY’S COLLABORATION PHOTO
August 2013 Collaboration meeting
OPTICAL PROPERTIES
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Absorption vs. wavelength
Te does not have absorption lines
Optically clear
Wavelength shifter options under
investigation to further improve
Triggers vs. Total Charge
Average light level 200-300 hits/MeV
Artfest May 2014, Christine Kraus, Laurentian University
BACKGROUNDS
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214Po – 164.3μs
Q-value: 3.27 MeV
212Po – 3x10-7s
Q-value: 2.25 MeV
target level ~2.5x10-15gU/gcocktail
~3x10-16gTh/gcocktail
★ Several α and βemissions
★ Direct backgrounds
★ 212Bi-212Po w coinc. 98% rejection
★ 214Bi-214Po w coinc. 99.8% rejection
★ 214Bi-214Po iw coinc. 98% rejection
★ 212Bi-208Tl coinc. 97% rejection
★ Continue to investigate, improve
External backgrounds from
AV, rope net, PMTs, water shield Attenuated by fiducial
volume, 50%time likelihood cut
Artfest May 2014, Christine Kraus, Laurentian University
SOLAR NEUTRINOS Background studies in pure scintillator will be available years
before to determine strategy to achieve background goals
Radon daughters have accumulated on the surface of the AV
over the last few years in a significant way. If these leach into the
scintillator, the purification system has the capability to remove
them.
However, depending on the actual leach rate, that removal
might be inefficient and the 210Bi levels in the scintillator too high
for a pep/CNO solar neutrino measurement without further mitigation.
Mitigation should include enhancing online scintillator purification,
draining the detector and sanding the AV surface to remove
radon daughters, or deploying a bag
Double beta decay and low energy 8B solar neutrino
measurements are not effected by these backgrounds. 37
Artfest May 2014, Christine Kraus, Laurentian University
NUCLEON DECAY AND SN NEUTRINOS Water phase will allow to look for “invisible” nucleon decay
modes by observation of characteristic gammas.
SN neutrinos for a SN within our galaxy.
See presentation by Belina Von Krosigk on Sunday
Interesting physics by combining with results from HALO (a
dedicated SN detector at SNOLAB) CC and NC
combinations
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Artfest May 2014, Christine Kraus, Laurentian University
COSMOGENICS
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Short and long living isotopes can be produced by cosmogenicactivation of Tellurium – detailed studies by V. Lozza
Isotopes with value larger than 2 MeV and with half-life longer than 20 days have been considered as potential backgrounds. Productions rates were estimated using the program ACTIVIA and the neutron and proton flux parameterization a sea level from Armstrong and Gehrels.
Low energy rand (E<200 MeV) used TENDL database for cross sections where available
Purification factors needed have been determined based on exposure of one year at sea level.
Purification at surface will be able to reduce induced cosmogenicsby a factor larger than 104. Further purification underground and cooling times on the order of month for isotopes produced during transport will also be needed.
With these measures, cosmogenic isotopes are a negligible background contribution
Artfest May 2014, Christine Kraus, Laurentian University