down-to-earth searches for cosmological dark matter · 2016. 10. 21. · down-to-earth searches for...
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Down-to-earth searches for cosmological dark matterCarter Hall, University of Maryland
October 19, 2016
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Astrophysical evidence for dark matter
Ω Galaxy cluster collisions Rotation curves
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3 3
380,000 years after the big bang
Today
1970’s - 1980’s: Cold dark matter is needed to seed the formation of galaxy clusters
13.9 billion years
Credit: Andrey Kravtsov, KICP, U. Chicago
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Temperature and density fluctuations are 1 part in 105.
The cosmic microwave background anisotropy imaged Planck (2014).
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CMB multipole expansion - measured by Planck (2014)
Prominent 3rd peak indicates presence of matter which did not rebound.
~ 1°
~ 1/2°~ 1/3°
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Neutrinos? – not heavy enough
‘Weakly Interacting Massive Particle’
generalize
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Early universe plasma
Age of universe ~ 1 nanosecond;Temperature ~ 100 GeV
?
Dark matter
Dark matter
Normalmatter
Normal matter
Dark matter annihilation
Dark matter creation
The thermal hypothesis:Was the dark matter an interacting component in the very early universe?
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Correct dark
matter abundance
Large annihilation cross section
Small annihilation cross section
Typical weak nuclear force cross sections
J. Feng, Annu. Rev. Astron. Astrophys. 2010. 48:495–545
The thermal hypothesis:Was the dark matter an interacting component in the very early universe?
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The Milky Way’s dark matter halo
• Typical orbital vel. = 230 km/sec~ 0.1% speed of light
• Density: ~ 300 mproton / liter• WIMPs (~100 GeV): 3 per liter
• deBroglie wavelength:• WIMPs: larger than a nucleus.
Coherent scalar scattering on ordinary nuclear matter, σ ~ A2
• Production: • WIMPs: thermal
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?
Dark matter
Dark matter
Normalmatter
Normal matter
Dark matter annihilation
Dark matter creation
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HAWC projected five-year sensitivity (start 2015)
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?
Dark matter
Dark matter
Normalmatter
Normal matter
‘Direct detection’
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WIMP γ,β
‘Direct Detection’
nuclear recoil signal
electron recoil background
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The parameter space of direct detection
& XENONNT
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Nuclear recoil energy spectra
From: arXiv:1107.1295
A2 dependence
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Calibration of LUX: Beta spectrum of Carbon-14
Carbon-14 beta decay
Xenon-131 Gamma line
(164 keV)
Detector threshold = 1.3 keV
1- 8 keV: x-ray region
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Target
scintillating bolometers (CRESST)
Cryogenic semiconductors
(CDMS)
Light
Phonons/heat 100% energy slowest cryogenics
Ionization
WIMP
WIMP
• Nuclear recoils vs. electron recoils ◆ "Division of energy ◆ "Timing ◆ "Stopping power
Two-phase noble liquids (PandaX, XENON, LUX)
Detection modes for ionizing radiation
Single-Phase noble liquids (XMASS, DEAP/CLEAN)
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Typical Event in LUX
S1S2
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Strong background rejection from kinematics
~ MeV γ
must cross
full volume without
interacting again
~ keV deposition
forward scattering
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Simulation of self-shielding in liquid xenon
Volume cut rejects most gamma backgrounds.
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Particle ID: recoil discrimination in LUX
Light
Charge/Light
Charge/Light
Charge/Light
Electron recoils (background)
Nuclear recoils (signal)
Difference
Electron recoil rejection factor:
200 -500
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LUX assembly – 2010 - 2011
370 kg of liquid xenon
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Sanford Underground Research Facility
Davis Cavern 1480 m (4200 mwe)
LUX Water Tank South Dakota USA
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Davis Cavern @ SURF, March 2011
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Davis Campus dedication, May 30, 2012
Ana Davis, widow of Ray Davis
Davis Campus water tank, home of LUX
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On top of the water shield, Sept. 2012
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LUX installed underground, Sept. 2012
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LUX recoil bands and energy scales
more charge recombination
less charge recombination
electron recoil band
nuclear recoil band
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0 10 20 30 40 501
1.2
1.4
1.6
1.8
2
2.2
2.4
2.6
log 10
(S2 b/S
1) x
,y,z
cor
rect
ed
S1 x,y,z corrected (phe)
3 6 9 12 15 18 21 24 27 30 keVnr
1.3
1.8
3.5
4.65.9
7.1
keVee
LUX WIMP search data (2013) 160 events observed 85.3 days × 118.3 kg = 10,090 kg�days
2013 initial results (Run 3): Phys.Rev.Lett. 112 (2014) 091303. 2015 re-analysis of Run 3: Phys.Rev.Lett. 116 (2016) 161301.
Light
Charge Light
_______
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October 30, 2013
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Calibration: external gamma sources (137Cs)
Calibration source guide tubes
Self-shielding makesexternal gamma sources
mostly ineffectual
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Tritium: an ideal electron-recoil band calibration source
0 2 4 6 8 10 12 14 16 18 200
0.5
1
1.5
2
Electron Kinetic Energy [keV]
Coun
ts/k
eV/d
ay/1
0000
0 at
oms
Tritium Beta Spectrum (Q=18.6 keV, T1/2=12.3 years)
WIMP search range
C
H
H H
T
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Injection and removal of tritium from LUX, August 2013
−300 −200 −100 0 100 200 300 400 500
10−4
10−3
10−2
10−1
100
Time (hours)
Rat
e (H
z)
S1 <150 [Phe]. Fiducial Volume
Rateτ 1=6.0 ±0.5Hoursτ 2=6.4 ±0.1 Hours
August 8, 2013
Success
10/21/16
Fiducial count rate for S1 < 150 PE
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0 100 200 300 400 500 600
0
50
100
150
200
250
300
radius squared (cm2)
drift
tim
e (µ
s)
−20 −10 0 10 20−25
−20
−15
−10
−5
0
5
10
15
20
25
x (cm)
y (c
m)
Tritium event locations in LUX – August 2013
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Charge vs Light from tritium in LUX at 170 V/cm
178,000 fiducial tritium events 10/21/16 40
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Tritium “combined-energy” spectrum
178,000 fiducial tritium events 41
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Light yield of liquid xenon
LUX – tritium (100 & 180 V/cm)
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Nuclear-recoil calibration w/mono-energetic neutronsD + D → n + 3He En = 2.45 MeV
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Nuclear-recoil calibration of LUX Neutron scattering with a neutron generator
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LUX final WIMP search results – Run 3 & 4 combined, 2013 - 2016
LUX Run 3 & 4 (2016): arXiv:1608.07648
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LUX -> LZ (2020) Scale up LUX fiducial mass by x40
46
LUX
LZ:TotalXe-10TonAc5veXe–7TonFiducialXe–5.6Ton
LUX
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Xe TPC
Gd-doped liquid
scintillator outer
detector
50 kV high voltage
existing LUX water shield
The LZ Experiment – coming in 2020
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LZ Sensitivity (5.6 Tonnes, 1000 live days)
48
2.5×10-48cm2
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History of WIMP sensitivity @ 50 GeV
LUX & PandaX-II (2016) LZ
Ge, NaI no discrimination
Ge, w/discrim.
LXe, w/discrim. ZEPLIN
XENON 1T
XENON100
LUX (2013)
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Uranium-238 decay chain
Thorium-232 decay chain
end end
start
start
gamma sources
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Tl-208 (Th-232) Bi-214
(U-238) K-40
Ge-76
Xe-136 Te-130
ββ0ν Q values:
Ordinary radioactive decay here on earth
WIMP scattering
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Two problems from particle physics 1) Why is the weak scale so light? è New weak physics? è WIMPs
2) Why no CP violation in QCD ? è Peccei-Quinn symmetry?è Axions
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Electron-recoil and nuclear-recoil calibration data
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Is LUX a success?
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July 22, 2016