MODERN COSMOLOGY

CDM direct detection 267 ρl= 0 .3 GeV cm−^3 ,whereρlis the local halo density (at the sun position); and ρχ=ξρl, withξ<1, wh ...

268 Dark matter search with innovative techniques (withMχ is the neutralino mass andMNthe target nucleus mass) andE 0 a characte ...

CDM direct detection 269 Sensitivity to arecoil-specific observable. This allows the ordinaryγand βbackground for which the ene ...

270 Dark matter search with innovative techniques theproper phaseis 152.5th day in the year (2 June); and theproper modulation ...

Phonon-mediated particle detection 271 Ta b l e 8. 1 .Nuclear quenching factors. Qn Detector Recoiling nucleus 0.25 Ge diode Ge ...

272 Dark matter search with innovative techniques Over the last few years, PMDs have provided better energy resolution, lower en ...

Innovative techniques based on phonon-mediated devices 273 the fluctuations of the excitation number, its value scales as the sq ...

274 Dark matter search with innovative techniques Sasso laboratory 4×250 g sapphire-TES detectors with a threshold of about 300 ...

Innovative techniques based on phonon-mediated devices 275 the charge and the phonon component of any single energy release. The ...

276 Dark matter search with innovative techniques Figure 8.1.Discrimination capability of the CDMS experiment. the parameterRin ...

Innovative techniques based on phonon-mediated devices 277 Figure 8.2.Discrimination capability of the CRESST test detector. In ...

278 Dark matter search with innovative techniques Figure 8.3.Gamma/beta background and nuclear recoils in CDMS results. neutron ...

Other innovative techniques 279 Figure 8.4.Exclusion plots (90% C.L.) and DAMA evidence. to resolve the dilemma could come from ...

280 Dark matter search with innovative techniques consists of detecting not the drift electrons, but the negative CS 2 ions, wit ...

References 281 [14] Freese Ket al 1988 Phys. Rev.D 373388 [15] Bernabei R 1995Riv. Nuovo Cimento 185 [16] Knoll G F 1989Radiatio ...

Chapter 9 Signature for signals from the dark universe The DAMA Collaboration R Bernabei^1 ,MAmato^2 , P Belli^1 , R Cerulli^1 , ...

Introduction 283 In particular, the WIMPs should be neutral particles in thermal equilibrium in the early stage of the universe, ...

284 Signature for signals from the dark universe Although exclusion plots are widely used in practice, many uncertainties arise ...

The highly radiopure∼ 100 kg NaI(Tl) set-up 285 (iii) many consistency checks and statistical tests [7–9, 12, 13, 15]. Therefore ...

286 Signature for signals from the dark universe Ta b l e 9. 1 .Released data-sets; the number 1 to 4 refer to different annual ...