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PROSPECTS IN LOW MASS DARK MATTER

30 November 2015 to 1 December 2015
Max-Planck-Institut für Physik, München
Europe/Berlin timezone

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Session

Session B

30 Nov 2015, 16:15
Auditorium (Max-Planck-Institut für Physik, München)

Auditorium

Max-Planck-Institut für Physik, München

Föhringer Ring 6 80805 München

Conveners

Session B

  • Klaus Eitel (KIT)

Presentation materials

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  1. 12. Search for Low-Mass Dark Matter with the CRESST Experiment
    Dr Raimund Strauß (MPI für Physik München)
    30/11/2015, 16:15
    The CRESST (Cryogenic Rare Event Search with Superconducting Thermometers) experiment aims at the direct detection of dark matter particles. The recent dark matter run was operated for 2 years with a total target mass of 5kg. With respect to previous measuring campaigns the intrinsic radiopurity of CaWO$_4$ crystals and the capability to reject recoil events from alpha surface contamination...
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  2. 10. Perspectives for low mass dark matter searches with the LUX and LZ experiments.
    Dr Paolo Beltrame (University of Edinburgh - School of Physics and Astronomy)
    30/11/2015, 16:45
    The Large Underground Xenon (LUX) experiment is a 350kg liquid xenon time projection chamber (TPC) designed to directly detect galactic dark matter, in particular as Weakly Interactive Massive Particle (WIMP). Currently deployed 1 mile underground in the Sanford Underground Research Facility in Lead, South Dakota, LUX completed its first physics run in 2013 collecting 85.3 live-days of science...
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  3. 19. Improving the sensitivity to low-mass WIMPs with XENON detectors
    Dr Moritz von Sivers (Albert Einstein Center for Fundamental Physics, University of Bern)
    30/11/2015, 17:15
    Dark matter experiments based on dual-phase Xe TPCs such as XENON100 and the upcoming XENON1T currently place the most stringent limits on the spin-independent WIMP-nucleon cross section for WIMP masses above 10GeV/c^2. In this talk, strategies to improve the sensitivity to lower WIMP masses such as using only the charge signal or increasing the light collection efficiency will be discussed.
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