DARK MATTER SEARCH Carter Hall, University of Maryland.

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Presentation transcript:

DARK MATTER SEARCH Carter Hall, University of Maryland

Direct detection of WIMP dark matter  00 proton masses per liter of space. If M WIMP ~ 100 GeV, then 3 WIMP/liter. Typical orbital velocity ~ 230 km/sec, or 0.1% speed of light. Coherent scaler interactions:  ~ A 2 Rate < 1 event / kg / 100 days, or much, much lower

It’s not difficult to shield at 10 keV typical WIMP recoil energies Gamma interaction cross section Only MeV  ’s can penetrate, but only keV  ’s can fake a WIMP

Self-shielding of liquid xenon is extremely powerful Fiducial volume cut rejects most backgrounds

Sensitivity improves quickly as target mass increases! Self-shielding effect

Particle ID: nuclear recoil discrimination Ionization-to-scintillation ratio allows discrimination between common radioactivity and WIMP events. Background rejection factor of ~180

The Hunters Hut Homestake (SD)

Davis Homestake, 9/21/09

Gaitskell - Brown University / LUX LUX Detector - Overview Titanium Vessels Dodecagonal field cage + PTFE reflector panels PMT holding copper plates Counterweight Feed-throughs for cables / pipesLN bath column Radiation shield 49 cm 59 cm Cathode grid Anode grid

LUX 350 kg detector under construction

Test fit of detector inside the titanium cryostat Assembly & commissioning in a new laboratory on the surface at Homestake

Xenon Purity measured in a 60 kg test run ~9 hr time constant for purification > 2 m electron drift length achieved (> 1000 us) with 60kg target Errors dominated by use of 5 cm test cell drift within large cryostat 0.2 tonnes circulation per day

Heat Exchanger Operates >96% Efficient Demonstrated - 18 W required to circulate 0.4 tonnes of Xe a day Evaporate Liquid > Gas / Purification -> Re-condense Liquid

LUX dark matter sensitivity Status: LUX is being now being assembled on the surface at Homestake. Expect to move underground in December 2010.

Collaboration Homestake mine, March 1, 2009