'Nuclear recoil' diaporamas de présentation

Searching For Dark Matter in the Universe:

675 views • 57 slides

Collaboration

686 views • 56 slides

Searches for Dark Matter (the Quest)

Searches for Dark Matter (the Quest). Harry Nelson UCSB 2003 SLAC Summer Insitute Aug. 5-6 2003. Recap - Direct Detection. How to dredge the small (0.01 DRU= ev/(kg d keV)) up out of a bigger background (1 DRU typical) of recoil electrons from comptons?.

524 views • 45 slides

Expected rates for various targets

Expected rates for various targets. For a heavy target nucleus such as Xe, a very low recoil energy threshold is crucial. The expected rate, integrated above threshold of ~16 keV is 1 events/ kg/day. WIMP Direct Searches with Recoil Discrimination.

553 views • 42 slides

Results from the Final Runs of the CDMSII Experiment

Results from the Final Runs of the CDMSII Experiment. Mark Kos Syracuse University. Detect energy deposited from WIMP-nucleus scattering Discriminate between nuclear and electron recoils. CDMS: Z -sensitive I onization and P honon detectors. Terrestrial dark matter detection.

430 views • 32 slides

Background issues for the Cryogenic Dark Matter Search

Background issues for the Cryogenic Dark Matter Search. Laura Baudis Stanford University. The Cryogenic Dark Matter Search. phonon and ionization detectors to measure WMP-nucleus elastic scattering current location: SUF ~ 16 mwe future location: Soudan ~ 2000 mwe

413 views • 32 slides

Direct Detection of Dark Matter

Direct Detection of Dark Matter. Ankur Deep Bordoloi , Cristian Gaidau. Outline. Cold Dark Matter (WIMP hypothesis) Why? What? Direct detection techniques What to detect Detector types Cryogenic Dark Matter Detection Experimental method Results. Indirect means:.

403 views • 28 slides

Dark Matter Detection

Dark Matter Detection. Andrew Sonnenschein Fermilab Users Meeting June 4, 2009. Cartoon of a Galaxy. Dark Matter Halo Unknown Composition ~85% of mass. Neutralinos?. Stars and gas. ~ 200 kpc. ? V. Generic 1st Generation WIMP Detection Experiment ca 1987. ?. Voltage bias. 200 km/s.

260 views • 25 slides

Dark Matter Search with Stilbene Scintillator

Dark Matter Search with Stilbene Scintillator. 9th ICEPP Symposium in Hakuba 20 Feb 2003 Hiroyuki Sekiya University of Tokyo. Dark Matter in the Universe. Flat Universe ? ??? ? ? ??? ? ? ???. Results of WMAP. 2/12 Asahi.com. COBE & WMAP. Accurate measurements of CBR anisotropies

236 views • 23 slides

Future, satellite experiments CMB: Planck (ESA) 2007 better angular resolution

Future, satellite experiments CMB: Planck (ESA) 2007 better angular resolution (high multipoles) SN: SNAP (NASA) wide field (2000 SN per year)). CMB+LSGS+HzSN:. at the periphery. M31-Andromeda at 2.2x10 6 light years (690 kpc). M 31.

266 views • 17 slides

Status of DRIFT II

Why DRIFT II ?. Directional sensitivity. Head tail discrimination. Readout electronics. Future. Ed Daw. Status of DRIFT II. Overview. representing the DRIFT collaboration : Univ. of Sheffield, Univ. of Edinburgh, Occidental College, Univ. of New Mexico. Why DRIFT II ?.

273 views • 12 slides

Status of DRIFT II

Why DRIFT II ?. Directional sensitivity. Head tail discrimination. Readout electronics. Future. Ed Daw. Status of DRIFT II. Overview. representing the DRIFT collaboration : Univ. of Sheffield, Univ. of Edinburgh, Occidental College, Univ. of New Mexico. Why DRIFT II ?.

252 views • 11 slides

collimator

Delay Plot. Large Exposure, Background: DAMA (58K kg-days, NaI) ZEPLIN-I (230 kg-days, Xe) IGEX (276 kg-days, Ge Ioniz). D. A. 25% Al area coverage, 25% quasiparticle collection efficiency. Surface-electron recoils (selected via nearest-neighbor multiple scatters from 60 Co source).

99 views • 1 slides