in the Sun Holger Motz Physikalisches Institut, Universität Erlangen Nürnberg Erwin Rommel Straße 1, 91058 Erlangen KM3NeT collaboration meeting Pylos, April 16 th Page 1
Indirect Search for Dark Matter WIMP accumulation in the Sun Self annihilation produces neutrinos via decay of primary annihilation products Page 2
Calculation of Neutrino Flux Neutrino flux from Neutralino Annihilation in the Sun calculated with modified version of DarkSUSY Scan of msugra parameter space with random walk algorithm guided by Ωh². Boundary conditions: 0 < < 8000 GeV 0 < m ½ < 2000 GeV sign (µ) = +1 3 < A 0 < 3 0 < tan (β) < 60 => Flux for each set of parameters, differential in E ν Page 3
Expected Neutrino Flux from Sun _ Log 10 (flux of ν µ and ν µ ) per km² and yr Integrated flux above 10 GeV neutrino energy plotted versus m χ all models 0.094 < Ωh² < 0.129 Ωh² < 0.094 m top =172.5GeV Page 4
Parameter Space Regions (flux) Page 5
Calculation of Limits Effective area provided by Sebastian Kuch Detector with 225 strings in cubic grid (15x15) 36 spherical modules with 21 3 inch PMTs each Fully reconstructed events used to calculate A eff Signal: Multiplication of flux with effective area (up to 400 GeV) Background: Atmospheric Neutrinos (Volkova) from 3 cone (below 400 GeV) 3 year 90%CL upper limit calculated using Gaussian distribution and compared to expected signal Page 6
Detection Rate _ Log 10 (detected ν µ or ν µ ) in KM3NeT per 3yr Number of expected events in KM3Net per 3 years plotted versus m χ all models 0.094 < Ωh² < 0.129 Ωh² < 0.094 m top =172.5GeV Page 7
Exclusion Detection Rate _ Log 10 (detected ν µ or ν µ ) in KM3NeT per 3yr Number of expected events in KM3NeT per 3 years plotted versus m χ blue: excludable red: not excl. bright: 2 σ WMAP faint: not WMAP Page 8
Exclusion Flux _ Log 10 (flux of ν µ and ν µ ) per km² and yr Integrated flux above 10 GeV neutrino energy plotted versus m χ blue: excludable red: not excl. bright: 2 σ WMAP faint: not WMAP Page 9
Parameter Space Exclusion Page 10
Direct Detection (CDMS 2007) Log 10 (σ) [cm²] Spin independent WIMP Proton crosssection plotted versus m χ green: both blue: only KM3NeT black: only CDMS red: neither Page 11
Direct Detection Parameter Space Page 12
Direct Detection (CDMS 2007) _ Log 10 (detected ν µ or ν µ ) in KM3NeT per 3yr Number of expected events in KM3NeT per 3 years plotted versus m χ green: both blue: only KM3NeT black: only CDMS red: neither Page 13
Direct Detection (S CDMS 2009) Log 10 (σ) [cm²] Spin independent WIMP Proton crosssection plotted versus m χ green: both blue: only KM3NeT black: only S CDMS red: neither Page 14
Direct Detection (S CDMS 2009) _ Log 10 (detected ν µ or ν µ ) in KM3NeT per 3yr Number of expected events in KM3NeT per 3 years plotted versus m χ green: both blue: only KM3NeT black: only S CDMS red: neither Page 15
Summary KM3NeT has the potential to put limits on a significant portion of the msugra parameter space even with not low energy optimized detector configuration Sensitivity similar to those of future Direct Detection Projects, partly complementary Indirect detection approach could give additional information on nature of Dark Matter Publication of shown results in preparation Page 16