1 / 12

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.

elroy
Download Presentation

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

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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].

More Related