The Estimated Limits For A 5g LE-Ge Detector

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Presentation transcript:

The Estimated Limits For A 5g LE-Ge Detector Q. Yue Tsinghua Univ. 2003.9.22

matter  0.3  baryon  0.01-0.03  lum  0.003  Components of the Universe: matter  0.3  baryon  0.01-0.03  lum  0.003  It shows: DM is the dominant component of the universe. Main part of it is Non-baryonic DM.

...... Massive neutrinos WIMP (Weekly Interactive Massive Particles ) Neutralino (Lightest super-symmetric particle) Axion ......

Direct Detection of WIMPs

The basic conditions of WIMP detector : High detection efficiency High pure target material Good shielding Good PSD capability Low threshold

Principles of direct detection: ER : the recoil energy E0 : the most probable incident energy of a dark matter particle of mass MD r : a kinematical factor R : the event rate ( 1/KeV · Day · Kg ) R0 : the total event rate ( 1/Day · Kg )

The possible mass range of WIMPs: 1 — 1000 GeV c-2 Typical recoil energies are in the range 0-100 keV. So good shielding is necessary to eliminate nuclear recoils from neutrons produced by cosmic ray muons. Methods of discriminating between nuclear recoils and electrons

The right-hand side is considerably complicated owing to the following corrections. a Detector on the Earth, in orbit around sun, and solar system moving through the Galaxy. b The Quenching Factor. c The target may consist of more than one elements. d Instrumental resolution and threshold effects. e SD & SI f Form factor

Take account all of these factors: vmax = vescape = 650km/s

DAMA results:

Our estimated results: Target mass: 5g QF: 0.25 Counts rate: 0.1 /keV·kg·day Threshold: 100KeV