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Strategies for Dark Matter Search: WIMP Direct and Indirect Detection Approaches

This document discusses various strategies in the search for dark matter, specifically focusing on weakly interacting massive particles (WIMPs). Key methodologies include direct detection through nuclear recoil measurement and indirect detection involving neutrinos, antiprotons, positrons, and gamma rays. The document reviews current limits on WIMP searches, presents results from experiments like DAMA, and explores neutron capture and annihilation processes relevant to dark matter interactions. Insights into neutrino flux from the Earth and Sun, as well as implications of detection experiments like IceCube, are included.

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Strategies for Dark Matter Search: WIMP Direct and Indirect Detection Approaches

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  1. Search for Dark Matter physics 805 fall 2008

  2. WIMP search strategies • Direct detection • Indirect detection:– neutrinos from the Earth/Sun– antiprotons from the galactic halo– positrons from the galactic halo– gamma rays from the galactic halo– gamma rays from external galaxies/halos– synchrotron radiation from the galactic center / galaxy clusters– ...

  3. WIMP + nucleus WIMP + nucleus • Measure the nuclear recoil energy • Suppress backgrounds • Search for an annual modulation due to the Earth’s motion around the Sun direct detection - general principles c c c c c December June

  4. present limits

  5. DAMA result (> 8 sigma)

  6. c WIMP Capture and Annihilation n nm DETECTOR c + c W + W  n + n

  7. Inner Core Detector Inner Core (same region as AMANDA) 7 IceCube + 18 AMANDA strings 225 DOMs + 540 OMs

  8. rc velocity distribution c n interactions sscatt n int. m int. nm Gcapture Gannihilation m neutralino capture and annihilation sun Freese, ’86; Krauss, Srednicki &Wilczek, ’86 Gaisser, Steigman & Tilav, ’86 Silk, Olive and Srednicki, ’85Gaisser, Steigman & Tilav, ’86

  9. indirect detection for cyclists e.g.104 m2n-telescope searches for 500 GeV WIMP 300 km/s > LHC limit 1.  - flux 2. solar cross section

  10. Nsun = capture rate = annihilation rate _ c c WW 250 GeV 500 GeV mnm 3. Capture rate by the sun 4. Number of muon-neutrinos 0.1is the leptonic branching ratio

  11. 5.5 x 1023 cm-3 104 m2 ~ _ # events = 10 per year

  12. AMANDA 180d SK Antares 3 years 1km3 (IceCube) PRELIMINARY WIMP search Limits on muon flux from Earth Limits on muon flux from Sun Disfavored by direct search (CDMS II)

  13. IceCube 22 strings

  14. Status indirect search

  15. IceCube vs Direct Detection (Zeppelin4/Genius) Black: out Green: yes Blue: no

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