'Wimp' diaporamas de présentation

Stefano Scopel

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Megaton Water Cherenkov Detectors and Astrophysical Neutrinos

Megaton Water Cherenkov Detectors and Astrophysical Neutrinos. Maury Goodman, Argonne National Lab. Megaton Water Detectors. 1 Megaton = 1000 milli-Megaton UNO (650 milli-Megaton) US Collaboration, focusing on Henderson Mine Frejus/CERN initiative Hyper-Kamiokande (1000 milli-Megaton).

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LUX : A Liquid Xenon Dark Matter Detector

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Low-threshold Results from the Cryogenic Dark Matter Search Experiment

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LHC PROSPECTS FOR COSMOLOGY

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Predicted Special Signatures for Direct Dark Matter Detection

Predicted Special Signatures for Direct Dark Matter Detection. J.D. Vergados Technical University of Cyprus, Lemesos, Cyprus. EVIDENCE FOR THE EXISTENCE OF DARK MATTER. Gravitational effects around galaxies

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COUPP: First Results Dark Matter Limits From a Bubble Chamber

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COUPP: First Results and Current Status Dark Matter Limits From a Bubble Chamber

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Satoru Yamada for the Super-Kamiokande collaboration

Search for WIMP annihilation in the Sun with Super-Kamiokande. Satoru Yamada for the Super-Kamiokande collaboration Institute of cosmic ray research, University of Tokyo. 1, Indirect WIMP search for the Sun. Spin Independent (SI) scattering and Spin Dependent (SD) scattering.

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WIMPS AND THEIR RELATIONS

WIMPS AND THEIR RELATIONS. Jonathan Feng University of California, Irvine. 27 October 2008 MIT Nuclear and Particle Physics Colloquium. DARK MATTER. Unambiguous evidence for new physics Intimately connected to central problems electroweak symmetry breaking structure formation

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WIMP AND RELATED MIRACLES

WIMP AND RELATED MIRACLES. Jonathan Feng, UC Irvine Manoj Kaplinghat, Jason Kumar, Huitzu Tu, Haibo Yu Inaugural Workshop, Center for Particle Cosmology University of Pennsylvania 11 December 2009. INTRODUCTION. The WIMP miracle is the fact that weak scale particles make good dark matter

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Summary on Cosmological Connections Session

Summary on Cosmological Connections Session. Nobuchika Okada (KEK & Grad. Univ. Advanced Studies). LCWS05, March 22th, 2005. From CMB + SN1a + structure formation. 1. Introduction. Observations of the present Universe after WMAP. Dark energy: 73% Dark matter: 23%

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LHC PROSPECTS FOR COSMOLOGY

LHC PROSPECTS FOR COSMOLOGY. Jonathan Feng University of California, Irvine. COSMO 09, CERN 7 September 2009. LARGE HADRON COLLIDER. 7 Sep 09. Feng 2. LHC PHYSICS. Higgs Boson Particle Physics Beyond the Standard Model Supersymmetry Extra Dimensions

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The Tokyo Dark Matter Experiment

The Tokyo Dark Matter Experiment. NDM03 13 Jun. 2003 , Nara Hiroyuki Sekiya University of Tokyo. Tokyo Group. Dark Matter Search Projects. LiF / NaF bolometer for SPIN DEPENDENT interacting neutralino search. Recoil direction sensitive organic crystal scintillator

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Experimental dark matter searches

Experimental dark matter searches. Weakly Interacting Massive Particles. A WIMP c is like a massive neutrino: produced when T >> m c via annihilation through Z (+ other channels); annihilation/pair creation maintain thermal equilibrium

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Status of Cold Dark Matter Searches Dan Bauer, Fermilab

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Monday colloquium

Monday colloquium. Probing Kaluza-Klein dark matter with neutrino telescopes Phys.Rev D67,055003 (2003) D.Hooper et.al. 2009 5/18 ?????. Dark Matter ??????.

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Gravitino Dark matter

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S uper WIMP Dark matter

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Testing the Standard Model and Beyond

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