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Search for neutrinos from diffuse dark matter annihilation at Super-Kamiokande

Search for neutrinos from diffuse dark matter annihilation at Super-Kamiokande. Piotr Mijakowski Warsaw University / A.Soltan Institute For Nuclear Studies. DIFFUSE ANALYSIS. Search for diffuse DM annihilation signal:. EXAMPLE: illustration of 5.6 GeV WIMP annihilation signal in SK.

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Search for neutrinos from diffuse dark matter annihilation at Super-Kamiokande

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  1. Search for neutrinos from diffuse dark matter annihilation at Super-Kamiokande Piotr Mijakowski Warsaw University / A.Soltan Institute For Nuclear Studies

  2. DIFFUSE ANALYSIS

  3. Search for diffuse DM annihilationsignal: EXAMPLE: illustration of 5.6 GeV WIMP annihilation signal in SK assume 100% BR signal is before FIT signal shown only in 2 samples (out from 16) ‘golden channel’ • Distinctivesignatures: Monoenergetic En = Mc Isotropic • Search for such a signal in atmospheric neutrino data of Super-Kamiokande-I, -II & –III livetime:FC/PC 2806 days, UPMU 3109 days DATASK1,2,3 Mc= 5.6 GeV ATM MC with oscillationsSK 2 flavor best fit • Simulate signal & detector response DM signal shapeenhanced for illustration • FIT: for each tested WIMP mass, find the best configuration of ATM MC + DM signal that would match DATA the best Mc= 5.6 GeV • using all SK samples: e-like + mu-like FC+PC+UPMU (wide energy range) cosqreconstr. Moment.[GeV]

  4. FIT based on Evis & cosq distr., systematics included (120 sys. terms fitted) • No allowed excess of DM-induced n’s for Mc in range 3GeV – 3 TeV Limit on <sv> FIT results • Focus on signal arising from Milky Way halo (diffuse flux) • Conservative upper limit on WIMP total self-annihilation cross section<sV> (*) above is excluded MW Halo Average (*) JDW is integrated intensity over all sky DW=2p, depends on DM halo density profile Details on JDWcalculation and motivation for this analysis: (*) H.Yuksel et al., Phys. Rev. D76, 123506 (2007), arxiv: 0707.0196 [astro-ph]

  5. ILLUSTRATIONS

  6. Piotr Mijakowski Instytut Problemów Jądrowych, Warszawska Grupa Neutrinowa

  7. Piotr Mijakowski Instytut Problemów Jądrowych im. Andrzeja Sołtana, Warszawska Grupa Neutrinowa

  8. Super-Kamiokande Water Cerenkov detector in Kamioka, Japan • 50kton water, 22.5kton fiducial volume • 12k inner PMTs /2k outer PMTs • detect light; possible reconstruction of energy and direction of neutrinos • SK investigates atmopsheric/cosmic, solar & accelerator n • detect SN1987 n’s • neutrino oscilation discovery (1998) • in operation since 1996 40m 40m

  9. How neutrinos interact? n + N->m/t/e+p+… • Charged Current • Neutral Current • Elastic Scattering n + N->n+n+… n + e-->n+e- n

  10. SUPPLEMENTARY

  11. DM signal illustration FC Mc = 5.6 GeV PC DATASK1,2,3 plot for atm. n’s ATM MC with oscill.SK 2flavor best fit DM signal shapeenhanced for illustration UPMU Assuming f(ne)=f(nm)=f(nt)for WIMP signal cosq

  12. DM signalillustration Mc = 5.6 GeV DATASK1,2,3 DM signal shapeenhanced for illustration ATM MC with oscill.SK 2flavor best fit Momentum [GeV].

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