Sun Kee Kim Seoul National University
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Transcript of Sun Kee Kim Seoul National University
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Sun Kee KimSeoul National University
Highlight of the KIMS Highlight of the KIMS research program and plan research program and plan
2nd China-Korea Workshop on Dark Matter SearchNov. 23-25, Seoul
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Brief History
2000.12.16 Mini-workshop on WIMP search with crystals, Seoul (Henry Wong, Jin Li)
2001.3.21 Beijing Mini-workshop, Beijing 2001.9.13 Cold Dark Matter Mini-workshop, Taipei 2003.9.23 TEXONO-KIMS joint meeting, Beijing 2004.1.29 TEXONO-KIMS Joint workshop, Yongpyung 2006.2.6 Workshop on the underground experiments at
Yangyang 2006.10.11 1st China-Korea joint seminar 2007.11.22 2nd China-Korea joint seminar
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Questions on Universe
What is the Universe made of?How large is the Universe?How did the Universe begin?What is the destiny of the Universe?What is the meaning of life in the Universe?…
“The most incomprehensible thing about the world is that it is comprehensible”- A. Einstein -
Some of these questions can be answered by understanding the nature of Dark matter and Neutrinos
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Mostly Dark matter, Dark energy
Composition of Universe
02.002.1 matter
Known ~ 4%
property of neutrinosnot known very well
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Galactic Dark Matter
Density of dark matter around the sun ~ 0.3 GeV /cm3
~ 5 x 10-28 kg/cm3
rotation velocity curve
WIMP
Cs
IRecoiled nucleus
Direct detection of galactic dark matter
Recoil energy ~ 10’s keVEvent rate < 1/kg/day
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WIMPWIMP(Weakly Interacting Massive Particles)(Weakly Interacting Massive Particles)
Excellent CDM candidate
Relic abundancev
hA
13272 scm103
Annihilation cross section of a particle with a weak scale interaction
132522 scm10~)GeV100(~ vA
velocityrealtive : section, crossn annhilatio: ,7.0~//100
AMpcskm
Hh
LSP in SUSY
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First idea of WIMP in 1977by B.W.Lee and S. Weinberg
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Spin Dependent Interaction qqdL qaxial55
2 2 232( 1)spin FG J J
1
( )p p n na S a SJ
Spin Independent Interaction
qqaL qscalar 224
( )scalar p nZf A Z f
2A
Isotope J Abun <Sp> <Sn>133Cs 7/2 100% -0.370 0.003
127I 5/2 100% 0.309 0.07573Ge 9/2 7.8% 0.03 0.38129Xe 1/2 26% 0.028 0.359131Xe 3/2 21% -0.009 -0.227
Elastic scattering of SUSY WIMP with ordinary nucleusElastic scattering of SUSY WIMP with ordinary nucleus
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Gaitskell’s summary talk IDM2004
current best limit(CDMS)
only positive result(DAMA)
Status of Direct Dark Matter Search
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Neutrino oscillation
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Neutrino mass and mixing
needs to be measured DayaBay, DCHOOZ, RENO
needs to be measured
measurable by neutrino oscillation
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Neutrinoless Double Beta Decay
S13
2022/1 ~0
MmT
100 meV
25 meV
2meV
from Ejiri’s talk (IDM2006)
need 1 ton detector
energy resolution is very importantsum electron energy / Q
R = 5%
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Status of DBD searches
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Issues
Dark Matter What is it ? WIMP?, Axion,… What is its nature? Mass, SUSY,…
Neutrinos What is absolute mass? Majorana or Dirac? Magentic moment? Mixing angle?
Underground experiments on-Direct dark matter search-Neutrinoless double beta decay search-Neutrino magnetic moment with strong source
may shed light on these issues
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Research Program of KIMS
Dark Matter Search - CsI(Tl) crystal detector
Running result was published talks today- Ultra-low energy HPGe detector R&D setup is running talks today
Neutrinoless Double Beta Decay Search- Metal loaded liquid scintillator Pilot experiment is running – a preliminary result
- CaMoO4 crystal
R&D effort is on going talks tomorrow
Rare event experimentBackground reduction is a critical research programUnderground laboratory is essential
Development of Cryogenic Detector R&D effort is on going talk tomorrow
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Yangyang Underground Laboratory
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Korea Middleland Power Co.Yangyang Pumped Storage Power Plant
Yangyang Underground Laboratory
Minimum depth : 700 m / Access to the lab by car (~2km)
(Upper Dam)
(Lower Dam)
(Power Plant)
Construction of Lab. buildings done in 2003
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Easy to get large mass with an affordable cost Good for AM study High light yield ~60,000/MeV Pulse shape discrimination Moderate background rejection Easy fabrication and handling Cs-133, I-127 (SI cross section ~ A2) Both Cs-133, I-127 are sensitive to SD interaction
WIMP search with CsI(Tl) Crystals
nuclear recoil
electron recoil
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Name Weight (kg)
Data(kg days)
S0406 6.7 237
S0501A 8.7 1147
S0501B 8.7 1030
B0510A 8.7 616
B0510B 8.7 616
B0511 8.7
B0601 8.7
B0605A 8.7
B0605B 8.7
B0606A 8.7
B0606B 8.7
B0607 8.7
B0608 8.7
published PLB(2006)
made of new powderexpecting ~ 2cpd
Total crystals 8.7 kg x 12 = 104.4 kg
started data taking
Pilot run
Engineering run
published PRL(2007)
Crystals and data taking
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Spin independent limitSpin independent limit
Nuclear recoil of 127Iof DAMA signal region
is ruled out unambiguiously
Nuclear recoil of 127Iof DAMA signal region
is ruled out unambiguiously
ρD=0.3 GeV/c2/cm3
v0=220km/s
vesc=650km/s
PRL 99, 091301 (2007)
Systematic uncertaintyFitting, Quenching factor
energy resolution...combined in quadrature
~ 15% higher than w/o syst.
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Spin dependent limitsSpin dependent limits
Pure proton casePure proton case Pure neutron Pure neutron casecase
PRL 99, 091301 (2007)
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SCIENCE, July 2007SCIENCE, July 2007
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ULE HPGe Detector for low mass WIMP
5g detector in operation at Y2L
20 g detector in preparation by TEXONO
Talks by See Yue Qian Shin Kai LinHau-Bin Li
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Loading Snbase scintillator: PC+PPO(4g/l)+POPOP(30mg/l)
Liquid Scintilator for 0
very stable over a year
NIMA 570, 454(2007)
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1.1 liter 30% Tin-loaded Liquid scintilator124Sn 124Te + 2-decay
Liquid Scintilator for 0
T1/2 > 4x1019 yr at 90% C.L
9 Months data
2287keV
previous limit :T1/2 < 2.4x1017 yr at 90% C.L
TMSN loading
paper in preparation
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DBD search with HPGe
124Sn (5.79%) 124Te* 124Te+γ
(1) > 2.31018 y (2) > 6.71018 y
(3) > 7.91018 y
Nucl. Phys. A 793, 171 (2007)
(TB-Sn)
0 Search with HPGe
140 hours
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> 1.31020 yearsZn plate : 8cm x 8cm x 1cm
F.A.Danevich et al., Nucl. Instrum. Meth. A 544, 553 (2005)
I.Bikit, et al., Appl. Radiat. Isot. 46, 455 (1995)
Nucl. Phys. A 793, 171 (2007)
HPGe + CsI(Tl) 0
332 hours
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CaMoO4 for ββ
CaMoO4 (PbMoO4 , SrMoO4...) DBD for Mo-100 (3034 keV), Ca-48(4272 keV) Similar to CdWO4 but no hazard with Cd. and
low Z Light output; 10-20% of CsI(Tl) at 20o, increase
with lower temp. Decay time ; 16 μ sec Wavelength; 450-650ns-> RbCs PMT or APD Pulse shape discrimination
resolutionCompton edge
CaMoO4 + LAAPD at -159oCPSD for alpha/gamma
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Sensitivity of CaMoO4
Mo-100 2nuMo-100 2nu
Ca-48 2nuCa-48 2nu
Tl-208Tl-208
Bi-214Bi-214 Signal (m=0.3eV)Signal (m=0.3eV)
10kg (100Mo) 0.01 /kg/keV/year 6% FWHM resolution 5year 8x1024 y(~200 meV)
Ca,Mo purification : 0.01 evt/keV/kg/y at 3MeVCa,Mo purification : 0.01 evt/keV/kg/y at 3MeVActive veto(5cm PbWo4(PbMoO4)) + 15cm low bg Active veto(5cm PbWo4(PbMoO4)) + 15cm low bg Pb + 30cm LSCPb + 30cm LSCTime correlation , Pulse shape discriminationTime correlation , Pulse shape discrimination
Current best limit on 100Mo : 4.6x1023 y by NEMO3 with 6.9kg 100Mo
Proc. New View in Particle Physics (VIETNAM ’2004) Aug. 2004, p.449
IEEE Nucl. Sci. 52, 1131 (2005)
NIMA, in print (2007)
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Crystal Growth (ISTC program)
New crystal 25 mm x 25 mm x 123 mm
installed @ Y2L, taking data now J.I.Lee’s talk tomorrow
Newer crystals
Newest crystal
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Underground Lab. Space
Current Lab. ~ 100m2
New Lab. space40 m x 20 m = 800 m2
909090909090
실험실 공간
320 sq m8m
40m
실험실공간
800 sq m
20m
40m
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Planned underground Lab.
지하공간
800 sq m
실험실 1
100 sq m
실험실 1
100 sq m
실험실 1
100 sq m
실험실 1
50 sq m
실험실 1
50 sq m
지원시설
50 sq m
40.00
20.0
0
사무실
49 sq m실험실 1
100 sq m
Current Lab. space
Underground Lab.
•Lab. 10x10=100m2 x 3•Lab. 10x5 = 50m2 x 2•Mini Machine shop•Liquid N2/He facility•Parking space•Service/utility space
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Summary
DM/DBD : Hottest research topicsKIMS started to produce good physics
resultsA lot of efforts for new detector
developmentCompetitive DBD search can be realized
rather soonPossibility of larger underground
laboratory space at Y2L is being exploredCooperative and harmonious
international collaboration will be essential