,*+.




1. #
2. #
3.

#
1.
 
2. "$% 3. '-),.(."$% 4.

/'-),.(.&!0• 1937 Zwikcy   


F.Zwicky, AstroPhys. J. 86 (1937) 217.
2019/12/12••   !

Y.Sofue and V.Rubin, Ann. Rev. Astron. Astrophys.
39 (2001) 137.

2019/12/12

AMS-02

• Alpha Magnetic Spectrometer•  ! • !c + c ® Z ®l +lc +c ®Z ® p+ p
2019/12/12

AMS-02

• 60 GV

• WIMPs
• 

• 30~70 GeV/c2• !" ≈ (1~6)×10+,- cm3/sec
AMS Collab. Phys. Rev. Lett. 117 (2016) 091103

2019/12/12

•  &• 
• " !-+• ,"&!"# = %"# &"#• '%(•'%&)'

'% %+)'#$"*&
2019/12/12

AXION, AXION-LIKE-PARTICLES (ALP)•  
 "CP#$

• Axion•  %(*&+$
• Axion %(*&+)+'• Heavy Axion (keV,!L. Di Lella and K. Zioutas, Astropart. Phys. 19, 145 (2003).

2019/12/12

STRONGLY INTERACTING MASSIVEPARTICLES (SIMPs)• 3  ./0*• !"# ~%&'' (&) +,~100 MeV%&'' ≈ 1 DM self-interaction

Y.Hochberg et al., Phys. Rev.Lett. 113 (2014) 171301.
Y.Hochberg et al., arXiv:1402.5143.

2019/12/12
S.M.Choi et al., arXiv:1707.01434.

WEAKLY INTERACTING MASSIVE PARTICLES(WIMPs)•8(80=<•52<-+#8; 5.7/734.<•

*&6"!
à WIMPs miracle:%9$

• ',(GeV/c2)•18/,>)G.Jungman, M.Kamionkowski, and K.Griest,Phys. Rep. 267 (1996) 195.

2019/12/12• WIMPs  • •• 

2019/12/12

WIMP  
2019/12/12

30

244km/sec

km/secAnnual modulation in WIMPs energy spectrum.
A.Drukier et al., Phys. Rev. D33 (1986) 3495.
K.Freese et al., Phys. Rev. D37 (1988) 3388.

2
æ vescöùdR(vE , vesc ) k0 é dR(vE , ¥) R0= ê
expçç - 2 ÷÷ú;dERk1 ë dERE0 r
è v0 øûæ vmin - vE öùdR(vE , ¥) R0 p 1/ 2 v0 é æ vmin + vE ö÷÷ - erf çç÷÷ú;=êerf ççdERE0 r 4 vE ë è v0øè v0øû
r=R0 =4 mc m N( mc + m N )p2

2 N A rc
1/ 2A mc,s N - c v0

J.D.Lewin and P.F.Smith, Astroparticle Physics 6 (1996) 87.

rc
öæv0540 æ s N - c öæö-1-1çç÷÷çç
÷=day×kg-2
3 ÷ç-1 ÷Amc è 1 pb øè 0.4 GeVc cm øè 230 km s ørcöæv0503 æ s N - c öæ
2019/12/12ö-1-1ç÷ç÷
=day×kg.
ç÷-23 ÷-1ç÷
ç
mc mN è 1 pb øè 0.4 GeVc cm øè 230 km s øvE = 244 + 15 sin( 2py ) km s The velocity of the Earth in the Galaxy.
-1-1vesc = 544 km s : The escape velocity of the Galaxy.
-1

v0 = 230 km s : The mean velocity of WIMPs.
ERvmin =: The minimum speed of WIMPs to give a recoil energy ER
rE0
k1= 1.01482
k0
2019/12/12

• 

mN (GeV / c ) = 931.478 A + DM - Zme
2me = 0.511 MeV / c23Na127I2
⊿M [MeV/c2]-9.528-88.984

mN[GeV/c2]
21.409118.18
2019/12/12

FORM FACTOR  QUENCHING FACTOR'( (#)* )(#/)0!(#) = 3
exp −,#)*
2
1'( (#)* ) =sin( #)* ) − #)* cos( #)* )0#)*#(MeV/<) =2=* >? : Momentum transfer.

)* = 1.18I(/J : Nuclear radius.
#N = 0.09 : The quenching factor of iodine ion in NaI(Tl).
#*V = 0.25 : The quenching factor of sodium ion in NaI(Tl).
2019/12/12


• Na, mx=50 GeV/c2• σp-x=1 pb

Cross over of event rate

NaI(Tl)

• I, mx=50 GeV/c2 Black; June• σp-x=1 pb
Red: December

Cross over of event rate • • 40K β• 210Pb β

K-X

3 keV) (46.5 keV) L-X(10~17 keV)

2019/12/12







2013 2019/12/12

ALP

Phys. Rev. Lett. 113 (2014) 12301

2019/12/12

CRESST

CdWO4 Cryogenic

H.Cluck et al.,arXiv: 1711.01285

2019/12/12

Technology

Implementation

StatusSensitivity
Sensitivity

Goal

22

SuperCDMS : TAUP2017
C20 RES
15 ST

2016DAMAM
CDiSSi te
Sl
M 15
CD 20

HVGeVSi H

IP
Ge i Z
IP
Si iZ

DAM
ICA
DAM

SuperCDMS LT 2014
5
CDMS II 201
Solar Neutrinos

Longt e r
goa ml13
LUX 20
1T 2017XENON
DEAPLZ

Atmospheric Neutrinos  

CUTE

XENON 1T• Xe• PI 
 

E.Aplire et al.,arXiv:1705.06655

2019/12/12

NaI(Tl)1736828'
• DAMA/LIBRA(/#.+&• Xe$• 28045$• Xe(-#)"!+&(9*!,%% .*
2019/12/12

2019/12/12

2019/12/12

2019/12/12

DAMAR.Maruyama talk in TAUP2017• PICOLON• DM-ICE• KIMS• SABRE• ANAIS
2019/12/12

 '$!(•   "!1'#'$  '###• )+(&./"# 2

"!1'#'$!,&0  0!-.,*+%2019/12/12

2019/12/12

ANAIS-112 (112 kg NaI(Tl) )• No significant modulation.
• Phys.Rev.Lett.123, 031301(2019)

2019/12/12

PICOLON• Pure Inorganic Crystal Observatory for LOw-energy Neutr(al)ino•     Univ. South Dacota• I.S.C.Lab.

2019/12/12

Status of NaI(Tl) purification(~April 2019)
RI

Ingot26
Ingot37(2015)(2016)Size
3”φX3”
4”φX3#40K (ppb)2630
120
232Th (ppt) 0.40.5
3.70.5
238U (ppt)
4.70.3
5.90.3210Pb
3072300(μBq/kg)
MethodResin for Pb I26+cation
resin

Ingot71(2018)
3”φX3”<20
1.70.2
9.70.8
1076

Ingot76(2019)
5”φX4”<20-4.40.2~560

double recrystallization

Pb resin +double recrystallization•

U-chain: 1ppt= 12.3μBq/kg•Th-chain: 1ppt= 4.0μBq/kg•210Pb:

1ppt=2.5kBq/kg

Goal5”φX5”<20 <4 <10 <50

EVENTS/keV/day/kg

BG STATUS OF INGOT #76
126I

125I210Pb

Still high BG of alpha rays.
~1000 μBq/kg (46.5 keV gamma from 210Pb.)~560 μBq/kg (Alpha ray from 210Po.)'&#$•• .1-*"$)

($)%• Mean event rate = 1/day/keV/kgmdet7 day• 371 events / 53 kg (9 modules)• 1734.6 events / 247.8 kg (42 modules)• *&$/+,0'* !.
2019/12/12

53 KG

250 KG

#  "   !
%'(    &$)
  

#  "   &$)
 !
%'(   

• Upper limits• 0.022/day/keV/kg







0.0035 /day/keV/kg

Observed PE yield (PE/keV)

MC deduced absorption
length (m)MC deduced scattering length(cm)+/0.5%

DETECTOR STABILITYXMASS
• We carried out weekly 57Co
calibration to monitor PE yield.
• We observed PE yield changes atpower outage. According to the MC
simulation, it is due to the change ofthe absorption parameter.
• In our analysis, the systematic errorof this data handling is taken intoaccount.

MC deduced scintillation lightyield

+/0.5%

2019/12/1239

MODEL INDEPENDENT ANALYSIS
Method 1 (pull term)
Method 2 (covariance matrix)  Method 1(pull term)

Method 2(covariantmatrix)

ndf

1709

1710

Minimum χ21845.01901.7

χ2 at nomodulation

1912.3

1961.8p-value

0.068 (1.8σ)

0.17 (1.4σ)• 1.1keVee (5keVr) analysis
threshold• The difference of twomethods are small.
• Small negative amplitude
is observed in 0.5-3keVeeregion. But both results are
consistent, but notstatistically significant.
2019/12/1240

" CALCULATING SENSITIVITY PLOT
• &+-'.),(*-  %

• &+-'. %#• 1~2 keVee : 2~3 keVee : 3~4 keVee : 4~5 keVee : 5~6 keVee• $$ "%!

2019/12/12

• Na recoil• 54 kg3 years• Thin line = Xenon1T• Thick lower line = Neutrino BG

2019/12/12

PICOLON

E 1 keVee, BG=1 /day/keVee/kg

9 modules (53 kg)
42 modules (247 kg)PUELACS

54 kg NaI(Tl)~2020
 (A)

250 kg NaI(Tl)
~2024


KamLAND-PICO
1000 kg NaI(Tl)~2025

NaI(Tl)(•  ' #"!*7• (16/23(Xe)$#*&(7•  ' • NaI(Tl)( *&+,!*7?

• )($(%-.+045 

2019/12/12

!,*"(• '•$)&- *,+7•  ' • .24/6$β/γ%

-$+7•  #'3560146 2019/12/12

• NaI(Tl)

Xe

2019/12/12

PERFORMANCE EVALUATION OF CaI2T.Iida, SCINTI2019• Emission wavelength (WL) and light yield (LY) werestudied using a small piece of CaI2.
• Emission WL : 410 nm, Excitation WL : 300 nm• From photo-electric peak of 662 keV gamma-ray, LY
was estimated as 107,000 ph./MeV (10  Liq. Scint.).
K. Kamada, T. Iida et al., Ceram. Int., Vol. 43, Suppl. 1, August 2017, Pages S423S427

CaI2(Peak at 410nm)

CaI2 = 2.7 NaI(Tl)T.Iida, SCINTI2019

PULSE SHAPE DISCRIMINATION STUDY• Half-inch crystal grown by Bridgman
method.
• 5mm square and 1mm thick piece wassliced off in a dry room whosehumidity was kept below 3%.
R7600-200U
Ultra-bialkali PMT

Waveform Digitizer
400MHz sampling rate

• Crystal was directly set on PMT andirradiated by alpha-ray source (241Am)
and gamma-ray source (137Cs).
• Waveform of 10 thousand events for
a/b were aquired by waveform
digitizer with 400MHz sampling rate.

T.Iida, SCINTI2019

AVERAGE WAVEFORM FOR A / BAlphaBeta• Average waveform for a/b were calculated from 10 thousand events and fitted by multi
exponential function.
• Slow component of ~800 ns and fast component of ~100 ns was obtained both for aand b.
• Very short component (18 ns) was appeared only in a.
T. Iida et al., Nucl. Inst. nd Meth. A, to be published DOI:
10.1016/j.nima.2019.162629

A/B SEPARATION BY “RATIO”

T.Iida, SCINTI2019

To evaluate PSD power, we defined “Ratio” and “Figureof Merit” as follows.
'$()# *++ ,) -./!"#$% =0%#"1 -./'%2 =34 − 36
74 + 76
Alpha
Beta

Energy[keV]• Obtained figure of merit wasFoM = 4.2 for CaI2 in 400 – 700 keV.
ref. FoM = 2.0 for CaF2(Eu)• Very good PSD capability was verified!!

Beta

Alpha

(:73• XMASS(2018 )14.6'232/0&8%

$5+• #4?G=;*+0@>BDFAG329'%•# NaI(Tl)1"→ -44)

• <DCEG=I;!1,HH
2019/12/12