Transcript Dark Matter Detection with Liquid Xenon Masahiro Morii Harvard University

Dark Matter Detection
with Liquid Xenon
Masahiro Morii
Harvard University
Laboratory for Particle
Physics and Cosmology
21 August 2009
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Dark Matter
Existence of Dark Matter is well established
from its gravitational effects
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Coma cluster [Zwicky], Galaxy rotation curve [Rubin]
Weak gravitational lensing, Bullet cluster
Amount of Dark Matter is inferred from
cosmological data
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~22% of the energy of the Universe
Local density 0.3 GeV/cm3
Identity of Dark Matter is unknown
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Majority must be cold and non-baryonic
i.e. made of particles that are not a part of the SM
Dark Matter is a particle physics problem
as much as a cosmology problem
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WIMP Dark Matter
No shortage of candidates, but…
WIMPs are the front runners
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~100 GeV new particles with weak
(and gravitational) interactions
Such a particle would naturally have
the right thermal relic density
Predicted in many BSM theories
(e.g. the LSP)
Since the annihilation cross section
s (c c Æ ff ) is constrained by the
relic density, we can predict:
s (c f Æ c f )
Direct detection
s (ff Æ c c )
Production at colliders
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Direct WIMP Detection
Best limits on the WIMP-nucleon
cross section are ~5x10-44 cm2
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CDMS : Ge and Si crystals at 10
mK,
121 kg-day exposure
XENON10 : liquid Xe, 136 kg-day
For LSPs, the interesting region
is around 10-44 cm2
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Smaller cross sections possible, but
increasingly difficult to reconcile with
the flavor problem
Next generation of experiments
aim for <10-45 cm2
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Liquid Xenon
WIMP-nucleus cross section ∝ A2
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Xe (A = 131.3) gives high signal rate
100 kg-year exposure can probe
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(WIMP-p) < 10-45 cm2
Key liquid Xe properties
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High density: 3 g/cm3
High boiling point: 165K
Good scintillator: 42 photons/keV
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High ionization yield: W = 15.6 eV
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= 175 nm easy to detect with PMTs
High electron mobility, low diffusion
No long-lived radioactive isotopes besides double-beta decays
 85Kr
must be removed by charcoal chromatography
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Two-Phase Xe Detector
PMTs collect prompt (S1) and
proportional (S2) light signals
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S1-S2 delay  Drift length
S2 light pattern  Horizontal location
S2/S1 ratio differs markedly
between electron and nuclear recoil
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>98.5% rejection of EM backgrounds
Good scaling to larger masses
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1 m3 holds 3 tonnes
Instrumentation ∝ (mass)2/3
Backgrounds improve with size due to
self shielding
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LUX Experiment
LUX is a 350 kg (100 kg fiducial)
liquid Xe experiment
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Located in the Davis cavern, Sanford
Underground Lab in Homestake, SD
XENON10 technology has been
improved to achieve <1 bkgd. in
100 kg-year
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Xe purification system has 300 kg/day
throughput using a heat exchanger
Ultra-low activity Ti vacuum vessel replaces SS + Cu
PMTs have low activity (9/3 mBq of U/Th per tube) and high QE (27%)
183 m3 purified water tank shields the detector from neutrons
Recoil energy threshold <5 keV  
(WIMP-p) = 5x10-46 cm2
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LUX Collaboration
Brown, Case Western, LBNL, Harvard,
LLNL, Maryland, Texas A&M, Rochester,
South Dakota, Yale
Funded by DOE & NSF
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Harvard Group
Harvard joined LUX in June 2009
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Morii (50%) is the PI
Took up a critical-path item: post-amplifier
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preamp
PMT
120 channels of receiver-amplifier-shaper for the PMT signals
Full system is needed in November
postamp
Harvard took over production from UC Davis
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Recruiting a postdoc and 1–2 graduate students
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Will take part in detector integration, commissioning
Develop analysis software framework
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Analog Trigger
Digital Trigger
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FADC
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Oliver and Morii improved the LLNL design
New LPPC engineer, Meghna Kundoor, working on testing
Components in hand. PC boards in fabrication
On track for November delivery
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LUX Status and Schedule
Prototype LUX0.1 is operating at Case
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1 liter of liquid Xe viewed by 4 PMTs
Test cryogenics and Xe purification system
>1 m electron drift achieved in 3 days
Assembly of LUX in Sanford surface
building will start in November
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All major components are in hand
Building is being fitted out
Fully-assembled LUX lowered to
Davis cavern (4,850 ft) in Spring
2010
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Dark Matter search will start!
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LZ Proposal
LZ = LUX scaled up to 1500 kg (1200 kg fiducial)
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Joint collaboration of LUX and ZEPLIN-III
LUX infrastructure designed to accommodate LZ
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(WIMP-p) = 2x10-47 cm2 in 2 years
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2000-fold improvement over current limits
Cost of liquid Xe ~$1000/kg
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Maximize the fiducial/total mass ratio by rejecting
single-scatter -ray background with liquid scintillator
Harvard will assume larger responsibilities
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Development of low radioactivity, high-QE PMT
Complete analog electronics chain (pre + postamp)
MRI-R2 proposal submitted this month
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3-year construction  Data taking in 2013
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Summary and Prospect
Exciting time for Dark Matter detection
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Cosmology points us to compelling particle physics
Liquid Xe technology has the potential for first observation
Harvard is entering DM hunting with strong commitment
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Producing critical component for the LUX experiment
PMTs and analog electronics for the proposed LZ experiment
Discovery potential of LUX is excellent
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(WIMP-p) = 5x10-46 cm2 covers the SUSY-favored region
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Dark Matter search run will start in 2010
LZ will push the sensitivity to 2x10-47 cm2 by 2015
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