Results with the Baksan Neutrino Telescope

1. Results with the Baksan Neutrino Telescope M.M.Boliev, A.V.Butkevich, S.P.Mikheyev,O.V. Suvorova Institute for Nuclear Research of Russian Academy of Sciences Moscow Uppsala, September 2006

2. Baksan Neutrino Observatory Site: North Caucasus Latitude 42.69 E Longitude 43.28 N BUST up/down  SAGE solar  Andyrchi shower CR Kover shower CR Neutron monitor

3. Baksan Underground ScintillatorTelescope Depth: 850 hg/cm2 17x17x11 m3 Tank size: 70x70x30 cm3 Number of tanks: 3150 In operation since 1978

4. Hardware triggers Nneutrino induced ------------------- ~ 10-7 Natmospheric • Trigger: > 10MeV in any plane • Rate: 17 Hz • Angular resolution: 1.5º • Time resolution: 5 ns • TRIGGER I. • 1.≥ 3 scintillator planes • 2.≥ 2 negative  t • 3. ≤ 3 external scintillator planes Efficiency 0.99 (tested with down-going muons) • TRIGGER II • 1.= 2 vertical scintillator planes • 2.= 0 horizontal scintillator plane • 3.  t≥ 30ns (pathlength≥ 10m) Trigger rate 0.02 Hz

5. Measured number of upward-going muons Nm =1102 events; L.T. = 21.15 yrs ~1 neutrino in week

6. Live time during observation

7. Upward-going muons distribution

8. Upward-going muons distribution

9. MC simulations of upward-going muons 1268.5 (22x21.15 y.) Ratio Data/MC = 0.87 ±0.03stat.±0.05syst. (Theoretical uncertainties = 15 ÷ 20%)

10. Zenith distribution of upward-going muons Data and MC results concern to measured 801 events in 15.7 y.

11. Summary status of zenith ratio Data/MC Upward through-going muons

12. Part I: Search for point-like sources Astrophysical analysis

13. Arrival directions of upward-going muons equatorial coordinates (, ) 90 ° 1102 Up-’s 360° 0° -90 ° With Baksan latitude,sky is observable for-90< <45°

14. Arrival directions of upward-going muons galactic coordinates (b, l) ° 90 ° 1102 Up-’s Sources with Baksan UpL (publ.1995y) catalogueSNR G.C. 360° 0° -90 ° With Baksan latitude, Galactic Center is observable 2/3 time

15. 10-12 Muon Flux (cm-2s-1) 90% CL Crab SS433 10-13 SMC X-1 SN1987a Vela X-1 LMC X-4 GC 10-14 10-15 -90 -60 -30 0 30 60 Declination Muon flux limits for point-like sources (known position)

16. Bootstrap method analysis Upward muons Expected noise 90 ° 90 ° 4°x4° 360° 8°x8° 360° -90 ° -90 °

17. SNR PKS 1209-51/52 60x90 arcmin b=+10°; l=296° Standard deviationsky map +90 ° -90 ° +90 ° -90 ° 360° 0° Upper limit on upward-going muon flux from Galactic Centre 6.3·10-15 cm-2 s-1

18. Part II: WIMPs annihilation in the Sun Astrophysical analysis

19. Limits on neutralino signal with NT Baksan upper limits on  fluxes and annihilation rates 130 days Earth Sun (publ.1996y) • Data 1978-1995: 558 upward in 11.9 yrs • Data 1978-2006: 1102 upward in 21.15 yrs 6 years 11.9 years 4.6 years 11.9 years 6. years Amanda-II 143,7 days 4.6 years Baikal 1038 days ~103 km-2·yr-1 could besensitive to current  models Not sensitive to current  models

20. Arrival directions of upward-going muons ecliptic coordinates (latd, long) 90 ° 1102 Up-’s 360° 0° -90 °

21. Upward-going muons in respect with Sun 90% c.l. Measured background is a correlation of ’ arrival directions and 5 fake ‘suns’ (same acceptance as true Sun)

22. Upper limits on  annihilation rate in Sun (equal fluxes of neutrino flavors from point generation) mSugra 14 benchmark points 53 GeV,M.Drees, hep-ph/0509105 DarkSusy mOmega wSUSY4 64 GeV; D.Kazakov, ICHEP’06 12 modeles of Battaglia et al, hep-ph/0306212.; (EGRET analysis)

23. Neutrino oscillations in absorption matter The propagaion of oscillating neutrinos can be descibed by their density matrix [Mikheyev and Smirnov 1985, Wolfenstein 1978,Stodolsky1987; etc] over processes: flavor-oscillations, coherent scattering (NC), absorption (CC) and neutrino regeneration in -decays Neutrino cross-sections N-> l X Summary effect in  flux for a case of DM: 1. Enhancement factor 4 ÷ 2 in τ+τ- channel and ~40% decreasing in other branches if m<100GeV; both in fluxes from the Sun and Earth For mx >200GeV decreasing in fluxes from the Sun (?) Changes in cone size to collect 90% signal ?? Neutrino spectra from  decays hep-ph/000000 A.Gouvea /0009183 M.Kowalski /0205116 P.Crotty /0506298 M.Cirelli et al. z=E/Eτ

24. Part III: Other searches for exotics Astrophysical analysis

25. Summary status of monopole search (M.Boliev et al., Nucl.Phys.B, 2006, v.151)

26. Search for correlations with solar flares Baksan Neutron Monitor Ground Level Enhancement of CR have been detected by the Shower Arrays (Kover ,Andyrchi) and BNM Observations of enhancements in sky-binning rate of HE downward-going muons with BUST during solar flares with GLE events BNM was running since Oct 2003 http://cr0.izmiran.rssi.ru/bksn/main.htm (S.Karpov et al., proc. ICRC05)

27. SUMMARY A/The Baksan Underground Scintillator Telescope is in continues operation since December 1978 up to now. B/There are 1102 neutrino events in total, detected with live time 21,15 years. C/No astrophysical local sources of neutrinos was found and upper limits were updated in comparison with the past analysis. D/New upper limits in search for DM signal from the Sun were set. The detector response on oscillation effects in matter is not accounted yet. E/Search for correlations of HE muon fluxes with solar flares is under investigations.

28. Baksan Baikal

29. THANK YOU!