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Shedding Light on Dark Matter from Deep Underground with XENON
Kaixuan Ni (Columbia)
University of Maryland, 11-25-2008
A well-known mystery for astronomers
2
Fritz Zwicky, The Astrophysical Journal, 85 (1937) 217
... All curves show a fairly rapid velocity rise to V ~ 125 km s-1 at R ~ 5 kpc, and a slower rise thereafter. Most rotation curves are rising slowly even at the farthest measured point. Neither high nor low luminosity Sc galaxies have falling rotation curves. Sc galaxies of all luminosities must have significant mass located beyond the optical image. ...
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Modern Precision Cosmology
Dark Matter is a stable, neutral, and heavy particle that interacts very weakly, or only through gravity.
Leading DM candidates, such as neutralinos and axions, are from theories beyond the Standard Model!
Three ways to probe the nature of dark matter
5
Indirectly search for DM annihilation products (gamma rays, neutrinos, electrons, positrons, etc.)
Produce dark matter in the Collider
Directly detect DM interacting with a terrestrial target
A fruitful year for indirect DM searches
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Observation of an anomalous positron abundance in the cosmic radiation [arXiv:0810.4995]
PAMELA
A fruitful year for indirect DM searches
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J Chang et al. Nature 456, 362-365 (2008) doi:10.1038/nature07477
ATIC
DM local density 0.43 GeV/cm3
Kaluza-Klein mass 620 GeVAnnihilation rate 10-23 cm3/s
An excess of cosmic electrons.
Dark Matter Equation of State
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Ωχh2 =mχnχ
ρc=
3 × 10−27 cm3/s〈σAv〉freezout
〈σAv〉freezout = 3 × 10−26 cm3/s
dnχ
dt+ 3Hnχ = −〈σAv〉
[(nχ)2 −
(neq
χ
)2]
A fruitful year for indirect DM searches
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J Chang et al. Nature 456, 362-365 (2008) doi:10.1038/nature07477
ATIC
Kaluza-Klein mass 620 GeVAnnihilation rate 10-23 cm3/s
A boost factor of ~200 is required
Also a busy year for direct DM searches
in the summer, moving against wind
in the winter, moving away from wind
expect an annual modulation in signal!WIMP “wind”
Also a busy year for direct DM searches
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in the summer, moving against wind
in the winter, moving away from wind
expect an annual modulation in signal!WIMP “wind”
Also a busy year for direct DM searches
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DAMA/LIBRA reconfirmed their early observation of annual modulation signal [arXiv:0804.2741]
in the summer, moving against wind
in the winter, moving away from wind
expect an annual modulation in signal!WIMP “wind”
Also a busy year for direct DM searches
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CDMS further improves Spin-Independent after XENON10 [arXiv:0802.3530]
DAMA allowed
Also a busy year for direct DM searches
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XENON10 Spin-Dependent pure-neutron coupling [PRL 101, 091301 (2008)]
COUPP further improves Spin-dependent proton coupling
[Science 319:933-936,2008]
arXiv:0810.0713
arXiv:0810.0713
arXiv:0810.0713
Are we at the edge of uncovering the nature of DM?
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Galactic WIMP Halo
(ρ = 0.3 GeV/cm3)
ElasticScattering
TargetNucleus
<V> = 220 km/s
Recoil Nucleus~10-100 keV or less
χχ
σχ-p can be as low as 10-46 cm2
Direct Dark Matter Detection
Goodman and Witten,coherent scattering for WIMPsPhys Rev D 31, 3059 (1985)
Recoil Energy [keVr]
0 10 20 30 40 50 60 70 80
Rate
[evts
/keV
r/kg
/day]
-710
-610
-510
Xe (A=131)
Ge (A=73)
Ar (A=40)
18 evts/100-kg/year (Eth=5 keVr)
8 evts/100-kg/year (Eth=15 keVr)
WIMP Scattering Rates
The Challenges for Direct DM Detection
large mass (ton scale)
low energy threshold (a few keV)
background suppression
deep underground
passive shield
low intrinsic radioactivity
gamma background discrimination
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Mχ = 100 GeV,σχ−p = 10−45cm2
R ∼ Mdet
Mχρσ〈v〉
Why do we need go to deep underground?
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Why do we need go to deep underground?
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Homestake
muon induced neutron flux
Mei and Hime, PRD (2006)
Why do we need go to deep underground?
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100 GeV WIMPs, 10-46 cm2
signal/background event rates
Homestake
muon induced neutron flux
Mei and Hime, PRD (2006)
World Wide Dark Matter Searches
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Gran SassoCRESST
DAMA/LIBRAWARP
XENON
SNOLABDEAP/CLEAN
PICASSO
KamiokaXMASS
YangyangKIMS
SoudanCDMS
HomestakeLUX
BoulbyZEPLINDRIFT
Frejus/Modane
EDELWEISS
Dark Matter physicists
Dark Matter physicists
Cryogenic (CDMS etc.)
Dark Matter physicists
Cryogenic (CDMS etc.)
Noble Liquids (XENON etc.)
The Merits of Noble Liquids for Dark Matter Detection
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Xe*
+Xe
Xe2*
Triplet27ns
Singlet3ns
2Xe2Xe
175nm175nm
Xe** + Xe
Xe2+
+e-
(recombination)
Xe+
+XeIonisation
Excitation
Electron/nuclear recoil
time constants depend on gase.g. Xe 3/27nsAr 10/1500ns
wavelengthdepends on gase.g. Xe 175nmAr 128nm
Nigel Smith, RAL
Recombination depends on type of recoils (stronger for nuclear recoils)
scalability : relatively cheap and “easy” cryogenics at 170 K (LXe), 87 K (LAr)
bkg reduction: via self-shielding
low threshold : high scintillation yield
gamma rejection: electron and nuclear recoil discrimination
The Noble Liquid Revolution
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• Noble liquids (LAr, LXe) are relatively inexpensive, easy to scale up
• Self-shielding reduce external background
• Excellent gamma background rejection (pulse-shape, or ionization/scintillation)
Single Phase(XMASS, CLEAN/DEAP)
Two Phase(XENON,LUX,ZEPLIN II/III,WARP,ArDM.)
XMASS 800-kg WARP
Two-phase Xenon Detectors for Dark Matter Detection
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WIMPs/Neutrons
nuclear recoil
electron recoil
Gammas
Top PMT Array
Signals from XENON10
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S1 S2
S1
S2
The Phased XENON Program
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XENON10(2006-2007) XENON100
(2007-2012)
XENON R&D (2001-2005)
XENON1T(2012)
136 kg-days Exposure= 58.6 live days x 5.4 kg x 0.86 (ε) x 0.50 (50% NR)
(data collected between Oct.2006 and Feb.2007)
4.5 –27 keVr
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XENON10 WIMP Search Data
~1800 events
WIMP Search Windownoise event
Statistical leakage from
electron recoil band
Anomalous events due to non-active Xe
XENON10 WIMP-Nucleon Cross-Section Upper Limits
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XENON10
CDMS II
(NO BKG SUBTRACTION)
8.8 x 10-44 cm2 at 100 GeV
4.5 x 10-44 cm2 at 30 GeV
Constrained Minimal
Supersymmetric Model
Spin-independent
Phys. Rev. Lett. 100, 021303 (2008)
Spin-dependent
Phys. Rev. Lett. 101, 091301 (2008)
XENON10
CDMS ZEPLIN-II
(NO BKG SUBTRACTION)
6 x 10-39 cm2 at 30 GeV
Can XENON10 anomalous events be explained by “iDM”?
27
δ ≤ 12µβ2c2 ≈ 100 keV
µ =MχMN
Mχ + MN
No longer elastic scattering.If dark matter can only scatter off of a nucleus
by transitioning to an excited state, the kinematics are changed dramatically
inelastic Dark Matter (iDM)
N. Weiner
Spencer Chang, Graham D. Kribs, David Tucker-Smith, Neal Weiner [arXiv:0807.2250]
visible to DAMA and XENON
visible to CDMS and
WARPf(v)
must have enough kinetic energy to scatter
modulation is also significantly enhanced
N. Weiner
Spectrum is dramatically modifiedStandard WIMPs have a spectrum that
peaks at low energies
Mχ=100 GeV, δ = 120 keV,normalized to DAMA 2-6 keV
XENON10 “background” data adjusted for efficiencies (taking unpublished acceptance x efficiency = 0.3, error bars estimated)
Mχ=100 GeV, δ=0 keV,normalized to inelastic XENON10 signal
Status of XENON100: the TPC Assembly
3112
the
170 kg LXe(70 kg target)
XENON100: The TPC Assembly
XENON100 Collaboration
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An international collaboration of 46 physicists from 9 institutions
Laboratori Nazionali del Gran Sasso, Italy
XENON100
LVDICARUS
OPERA
LNGS 1400 m Rock (3100 w.m.e)
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LNGS: 1.4km rock (3100 mwe)
XENON100
inside shield
XENON10
XENON100
outside shield
XENON100
XENON10
XENON100 Underground at the Laboratori Nazionali del Gran Sasso
3516
• 242 PMTs (Hamamatsu R8520-06-Al )
• 1 “ square metal channel developed for XENON
• Low radioactivity (<1 mBq U/Th per PMT)
• 80 PMTs for bottom array (33% QE)
• 98 PMTs for top array (23% QE)
• 64 PMTs for top/bottom/side Veto (23% QE)
XENON100: The PMTs Bottom Array
Top Array PMTs for Side & Bottom Shield
PMT Base
Ultra-low radioactive material selection
36
All materials used in XENON100 detector were selected based on low radioactivity
Background simulation
37
• 0.15 mBq/PMT x 242 PMTs gives 3000 238U decays/day• Each 238U decay produces 15 gammas and 9 alphas• 16M gamma/year• (alpha,n) reaction results 7 neutron/year
A realistic model based on Geant4 was constructed to propagate all the gammas/neutrons to simulate the
background rate.
Expected Background and Sensitivity Reach
38
R (cm)0 2 4 6 8 10 12 14
Z (c
m)
-30
-25
-20
-15
-10
-5
0 )ee
(dru
-510
-410
-310
-210
-110
50 kg30 kg
Current XENON100: gamma bkgdruee = evts/keVee/kg/day
e assume cross section 10-44 cm2
XENON100: Data Acqusition System
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Requirements:
digitize full waveform (320!s) of 242 PMTs
with no deadtime and with high rate capability for calibration
CAEN V1724 Flash ADC: 14bit, 100MHz
circular buffer: no deadtime
on board FPGA: Zero Length Encoding only relevant signal portion transferred from ADCto DAQ computer to allow faster event transfer rates >60 Hz in calibration mode
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First signals from XENON100
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0 5000 10000 15000 20000 25000 300000
1
2
3
4
5
6
7
8
13900 14000 14100 14200 143000
0.1
0.2
0.3
0.4
0.5
0.6
0.7
14400 14600 14800 15000 152000
1
2
3
4
5
6
7
8
Gamma Event Digitized
S1 S2
Gamma Event Localized
1
2
3
4
5 6
7 8 9 10 11
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22 23 24 25 26
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68 69 70 71
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84 85 86
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94 95
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97 98179
180
181
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183
184185
186 187 188189
190
191
192
193
194
195
196
197
198
199
200201
202203204205
206
207
208
209
210
Top Array
1
2
3
4
5 6
7 8 9 10 11
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20 21
22 23 24 25 26
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48 49 50 51
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97 98179
180
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184185
186 187 188189
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200201
202203204205
206
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210
E [keV]
0 500 1000 1500 2000 2500 3000
Ra
te [
ev
ts/k
g/d
ay
/ke
V]
-310
-210
-110
1
XENON100 MC Background
XENON100 background run
41
S1 [keVee]
0 500 1000 1500 2000 2500 3000
Evts/keVee/kg/day
-310
-210
-110
1
xe100_080620_2018xe100_080620_2018
data Simulation
Detector has been fully filled with liquid xenon.First Measured background Spectrum in good agreement with MC prediction!
WIMP search run is planned to start in April 2009.
all single/multiple scattering events
all single/multiple scattering events
single scatter only with ~46 kg fiducial mass cut
edge events with poor light collection, will be removed by radial position cut
A proposal to upgrade XENON100 (2009-2012)
42
Sensitivity Reach of the XENON100 Program
43
Exposure Time with Zero Bkg [month]
0 5 10 15 20 25 30 35 40
]2
(90%
C.L
. u
pp
er
lim
it)
[cm
-p!"
-4610
-4510
-4410
-4310
)2
cm
-44
= 1
0-p!"
Exp
ecte
d #
of
WIM
P E
ven
ts (
-110
1
10
210
XENON Sensitivity Projection - 100 GeV WIMPs
2009 2011-2012
Current Best Sensitivity
Multi-ton scale XENON Detector for DUSEL (beyond 2012)
• Explore the full region/accumulate WIMP statistics
• New design with full coverage of ultra-low background photodetectors and cryostat
• Larger International Collaboration
• Total project cost: $50M-$100M
• neutrinoless double beta decay
• pp solar neutrinos
44