katsushi arisaka - university of california, los angelesarisaka/talks/2012/arisaka_120224... ·...
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Katsushi Arisaka, UCLA 1
University of California, Los Angeles Department of Physics and Astronomy
arisaka@physics.ucla.edu
Katsushi Arisaka
2/24/2012
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MAX - Multi-ton Argon & Xenon
UMass Amherst, Arizona State University, Augustana College, Black Hills State University,
Coimbra University, Columbia University, Fermilab, University of Houston, INAF, LNG, MIT, University of Münster,
University of Notre Dame, Princeton University, Rice University, Temple University, UCLA, University of Virginia,
University of Zürich
Katsushi Arisaka, UCLA 2 2/24/2012
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4m
Katsushi Arisaka, UCLA 3
MAX G3 Detector (at DUSEL)
2 m Xe
20 ton (10 ton)
40Ar 70 ton
(50 ton)
Katsushi Arisaka, UCLA 3 2/24/2012
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Roadmap to MAX
Katsushi Arisaka, UCLA 4
2012 2013 2014 2015 2016 2017 2018 2019 2020
XENON100
G1
DarkSide50
Gran Sasso DUSEL
G3
Xe 10T
Ar 50T
MAX
(Paul Scovell)
XENON 1T
G2
DarkSide 5T
(Elena Aprile)
(Luca Grandi, Frank Calaprice)
Katsushi Arisaka, UCLA 4 2/24/2012
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2/24/2012 Katsushi Arisaka, UCLA 5
G1 CMSSM
F-SU(5)
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2/24/2012 Katsushi Arisaka, UCLA 6
G2
G1 CMSSM
F-SU(5)
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2/24/2012 Katsushi Arisaka, UCLA 7
G2
G3
G1
Xenon 10 ton-year
Argon 50 ton-year
CMSSM
F-SU(5)
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(SI) WIMP Energy Spectrum for LXe (Cross Section = 10-45cm2)
Katsushi Arisaka, UCLA 8
8 keVr 45 keVr Xenon
200 GeV
50 GeV
100 GeV
1000 GeV
500 GeV
20 GeV
Katsushi Arisaka, UCLA 8 2/24/2012
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(SI) WIMP Energy Spectrum for LAr (Cross Section = 10-45cm2)
Katsushi Arisaka, UCLA 9
20 GeV
200 GeV
50 GeV
100 GeV
1000 GeV
500 GeV
200 keVr 40 keVr Argon
(w/ pulse shaping)
Katsushi Arisaka, UCLA 9 2/24/2012
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1-σ Error of WIMP Mass vs SI Cross Section (10 ton*year Xe and 50 ton*year Ar)
Katsushi Arisaka, UCLA 10
50 GeV 100 GeV 200 GeV 500 GeV
10-45 cm2 Argon
Xenon
Katsushi Arisaka, UCLA 10 2/24/2012
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1-σ Error of WIMP Mass vs SI Cross Section (10 ton*year Xe and 50 ton*year Ar)
Katsushi Arisaka, UCLA 11
50 GeV 100 GeV 200 GeV 500 GeV
10-45
10-46
10-47
10
50
10 50
Argon
Xenon
10-46 cm2
Katsushi Arisaka, UCLA 11 2/24/2012
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1-σ Error of WIMP Mass vs SI Cross Section (10 ton*year Xe and 50 ton*year Ar)
Katsushi Arisaka, UCLA 12
Argon (42 events)
Xenon (56 events)
100 GeV
10-45
10-46
10-47
10
50
10 50
10-46 cm2
Katsushi Arisaka, UCLA 12 2/24/2012
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1-σ Error of WIMP Mass vs SI Cross Section (10 ton*year Xe and 50 ton*year Ar)
Katsushi Arisaka, UCLA 13
100 GeV
Argon (4.2 events)
Xenon (5.6 events)
10-46
10-47
10-48
10-47 cm2
10
50
10 50
Katsushi Arisaka, UCLA 13 2/24/2012
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(SI) WIMP Energy Spectrum for LXe (Cross Section = 10-45cm2)
Katsushi Arisaka, UCLA 14
Xenon 8 keVr 45 keVr
20 GeV
200 GeV
50 GeV
100 GeV
1000 GeV
500 GeV
Katsushi Arisaka, UCLA 14 2/24/2012
Summer Winter
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(SI) WIMP Energy Spectrum for LAr (Cross Section = 10-45cm2)
Katsushi Arisaka, UCLA 15
Argon
45 keVr 200 keVr
20 GeV
200 GeV
50 GeV
100 GeV
1000 GeV
500 GeV
Katsushi Arisaka, UCLA 15 2/24/2012
Summer Winter
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±1σ Error of Annual Modulation Amplitude vs WIMP Mass (10 ton*year Xe and 50 ton*year Ar, Cross Section = 10-45cm2)
Katsushi Arisaka, UCLA 16
Argon Xenon
10-45 cm2
±1σ
±1σ
Katsushi Arisaka, UCLA 16 2/24/2012
10
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±1σ Error of Annual Modulation Amplitude vs WIMP Mass (10 ton*year Xe and 50 ton*year Ar, Cross Section = 10-44cm2)
Katsushi Arisaka, UCLA 17
Argon Xenon
10-44 cm2
Katsushi Arisaka, UCLA 17 2/24/2012
10
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±1σ Error of Annual Modulation Amplitude for various WIMP velocities (50 ton*year Ar, Cross Section = 10-44cm2)
2/24/2012 Katsushi Arisaka, UCLA 18
10-44 cm2
Argon
170 km/s
220 km/s
270 km/s
V0 =
195 km/s
245 km/s
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Technological Challenges Ø External Backgrounds
§ Deep underground – DUSEL 4850 ft § > 5 m water shielding – Water Tank (15 m)
Ø Detector Materials § Photon Detectors – QUPID § Cryostat – Titanium § Others – Copper, PTFE…
Ø Purity of Liquid Xe/Ar § Radon (< 0.3 mBq / ton) § 39Ar (> 100 depletion) – Depleted Ar § 85K (< 0.2 ppt in Xe) – 1 event / 10 ton-year
Ø Physics Backgrounds in Xe § pp-chain solar neutrinos – 1 event / 10 ton-year § 2v Double beta decays from 136Xe – 1 event / 10 ton-year
Ø Neutron Active Veto § Boron doped Liquid Scintillator
Katsushi Arisaka, UCLA 19 Katsushi Arisaka, UCLA 19 2/24/2012
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Photo Cathode (-6 kV)
APD (0 V)
Quartz
Quartz
Al coating
APD (0 V)
Photo Cathode (-6 kV)
QUPID (QUartz Photon Intensifying Detector)
20 Katsushi Arisaka, UCLA
arXiv:1103.3689
Katsushi Arisaka, UCLA 20 2/24/2012
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Comparison of Low-radioactive Photon Detectors from Hamamatsu
QUPID 3 inch
R8520 1 inch
R8778 2 inch
XENON10 XENON100
LUX (XMASS)
DarkSide50 XENON1T MAX, XAX
< 0.3 mBq ~ 10 mBq ~ 1 mBq
2/24/2012 Katsushi Arisaka, UCLA 21
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QE of two types of QUPID
22 Katsushi Arisaka, UCLA
0
10
20
30
40
150 200 250 300 350 400 450 500 550 600
Qua
ntum
Effi
cien
cy [%
]
Wavelength [nm]
Xenon type
Argon type
Xenon (178 nm) Argon + TPB (420 nm)
Katsushi Arisaka, UCLA 22 2/24/2012
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1, 2 and 3 PE Distribution with 2 m cable
Katsushi Arisaka, UCLA 23
2 PE
3 PE
1 PE
G = 800 × 200 = 160,000
TTS = 160 ps (FWHM)
Katsushi Arisaka, UCLA 23 2/24/2012
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7 QUPID with Holder
Tested in both Xe and Ar at UCLA Ready for DarkSide 10 2/24/2012 Katsushi Arisaka, UCLA 24
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Katsushi Arisaka, UCLA 25
0.81 n / year
Before Cuts 1/8
Multi Hit Cut
0.10 n / year
1/4
0.03 n / year
Liquid Scinti. Veto
Xe 10 ton Neutron Background (100 Years)
Xenon 10 ton
arXiv:1107.1295
Katsushi Arisaka, UCLA 25 2/24/2012
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Katsushi Arisaka, UCLA 26
42 n / year 2.1 n / year 0.39 n / year
1/20 1/6 Multi Hit Cut Liquid Scinti. Veto Before Cuts
Argon 50 ton
Ar 50 ton Neutron Background (100 Years) arXiv:1107.1295
Katsushi Arisaka, UCLA 26 2/24/2012
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XAX (Xenon-Argon-Xenon)
Katsushi Arisaka, UCLA 27
4 m
129/131Xe 12 ton (6 ton)
40Ar 70 ton
(50 ton)
WIMP (Spin odd) pp Solar Neutrino
WIMP (Spin even) Double Beta Decay WIMP (Spin even)
2 m
136Xe 7 ton
(4 ton)
1.2 m
arXiv:0808.3968
2/24/2012
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(1022 yrs)
0ν DBD (1027 yrs)
0 cm
10 cm
30 cm
20 cm
B8 Solar Neutrino
40 cm 50 cm
2ν DBD (2 x 1021 yrs)
136Xe Double Beta Decay and Gamma Background (1 mBq / QUPID, 2m Xenon Detector)
Katsushi Arisaka, UCLA 28 2/24/2012
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Double Beta Decay Experiments (with 0.1 mBq QUPID)
Katsushi Arisaka, UCLA 29
EXO 1Ton
EXO200
NEMO3 (Mo)
NEMO3 (Se)
Mass (kg)
No.
of B
ackg
roun
ds (/
year
)
Cuoricino
GERDA I
GERDA II
GERDA III Super-NEMO (Se)
CUORE I
CUORE II
CUORE III
COBRA
CANDLES III
EXO 1Ton (Ba tag)
1025 yrs 1026 yrs 1027 yrs 1028 yrs
XAX (Enriched)
XAX (Natural)
XENON1T
2/24/2012
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2/24/2012 Katsushi Arisaka, UCLA 30
Water Tank
Liquid Scinti
Water Tank
Xe 20 ton (10 ton) 40Ar 70 ton (50 ton)
15 m 6 m
Liquid Scinti
Xe Ar
MAX G3 Detector (at DUSEL)
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MAX G3 Detector (at DUSEL)
Katsushi Arisaka, UCLA 31
Xe 20 ton
(10 ton)
40Ar 70 ton
(50 ton) 2/24/2012
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Schedule at DUSEL
Katsushi Arisaka, UCLA 32
Kevin Lesko
2/24/2012
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US Dark Matter Programs
Katsushi Arisaka, UCLA 33
G3 = Xe (10T) + Ar (50T)
2010
Xe
Xe
Ar
Ar
2/24/2012
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Conclusions
Ø MAX § 10 Ton Xe + 50 Ton Ar at DUSEL § Joint efforts by XENON and DarkSide
collaborations (currently at LNGS towards G2)
Ø Science cases § Sensitivity down to 10-48 cm2 § Precision measurements if > 10-46 cm2 § Possibility to combine with 0v Double Beta
Decays à XAX
Katsushi Arisaka, UCLA 34 2/24/2012
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