High Energy Neutrino Astronomy

1. High Energy Neutrino Astronomy Christian Spiering DESY Zeuthen TAUP 2001

2. Predictions and Bounds

3. Classes of Models log(E2 Flux) pp core AGN p blazar jet Top-Bottom model Various recent models for transient sources GRB (W&B) 3 6 9 log(E/GeV) TeV PeV EeV

4. Bounds to diffuse fluxes: WB Waxman & Bahcall, 1999 atmospheric flux  sources optically thin to primary cosmic rays  fix the spectral index to 2  normalize to cosmic rays at 1019 -1020 eV bound with evolution * bound without evolution * moderately dependent on cosmology

5. optically thick for neutrons MPR optically thin atmospheric flux W & B Bounds to diffuse fluxes: MPR Mannheim, Protheroe, Rachen, 2000  do not assume a specific CR spectrum, use available upper limit on extragalactic proton contribution  allow also for optically thick sources (no neutrons escape)

6. 3 107 109 Emax=106 3 1010 1012 3 1013 MPR limit for optically thin sources cosmic ray spectrum after propagation through Universe source spectra of neutrons Qn(En)  En-1 exp(-En / Emax) neutrino spectrum after propagation through Universe red: limit without GZK shift blue: renormaliztion after GZK shift

7. More bounds .... generic blazar optically thick E-1 exp (-E/Emax ) optically thin with evolution E-2, one source type without evolution Bound construction parallels that for optically thin sources. Energy dependent opacities. Averaging over luminosity functions and z-distributions of EGRET blazars and BL Lac objects. EGRET blazar BL Lac

8. 1 pp core AGN (Nellen) 2 p core AGN Stecker & Salomon) 3 p „maximum model“ (Mannheim et al.) 4 p blazar jets (Mannh) 5 p AGN (Rachen & Biermann) 6 pp AGN (Mannheim) 7 GRB (Waxman & Bahcall) 8 TD (Sigl) Mannheim & Learned, 2000 Diffuse Fluxes: Predictions and Limits Macro Baikal Amanda IceCube

9. Hidden Sources Young SN shells, binary submerged in red giant, coooned MBH, ... Pre-AGN (prior to formation of massive black hole) Berezinsky & Dokuchaev, 2000 Collision & destruction o normal stars in a contracting central cluster Massive gas envelope NS & BH survive, further contraction and collisions Repeating fireballs, particle acceleration in rarified cavity

10. Hidden sources (2) Interactions in envelope HE neutrinos Muon events per source with E > 1 TeV, in 1 km2 detector: N ~ 70 (assuming Lp = 1048 erg s-1 and distance = 103 Mpc) Duration of pre-AGN hidden source phase ~ 10 years Average number of galaxies just in hidden source phase: ~ 10-100

11.  -faint, high  flux Low  flux, high energy 100 300 1000  GRB “Reference” model: Waxman & Bahcall, 1997   emission from protons accelerated at internal & external shocks in fireball,  ~ 300  normalization to CR  E2  dN/dE ~ 310-9 cm-2 s-1 sr-1 GeV between 100 TeV and 10 PeV Alvarez-Muniz, Halzen, Hooper, 2000 z = 1  z distribution expect up to  = 300  thousands of  events/yrkm2 Also multiple events from -faint-bursts !

12. GRB Meszaros & Waxman, 2001 Core collapse of massive stars  relativistic fireball jet may either penetrate stellar envelope or may be choked N ~ 0.2 (E /1053 erg) km-2for z =1 (E 5 TeV)  103 events correlated with -bursts + more from -dark bursts Paolis et al., 2001 Shock-accelerated protons from GRB interact with external protons in dense cloud  neutrinos with few GeV to ~ 1 PeV  single GRB at z=1 yields 0.1-1 event per km2 (E > 1 TeV)

13. GRB  (quasi-thermal)  from 0 decay neutrinos ‘s extremely forward collimated - the stronger the higher their energy SN shell Cannon Balls Cannon Ball Model of GRB(Dar, De Rujula, Plaga)

14. Neutrinos from Microquasars Waxman, Loeb, 2001  Accreting stellar-mass BH or neutron star ejecting jets  Radio outbursts with L ~ 1043 erg   of order 1-10  Shock acceleration in electron proton plasma  Neutrino burst of several hours, preceding radio outburst 1-100 TeV neutrinos from proton–X-ray interactions N (1km2) ~ 10-2  -1 3 (for distance 10 kpc)  8 for source along line of sight  several neutrino events per outburst

15. Experiments under ground

16. MACRO Since 1989: 1356 upward going   Limit on flux from point sources  Limit on diffuse flux  Limit on neutrino emission from GRB

17. MACRO point source search MACRO sky-map in equatorial coordinates 90% c.l. upper limits for 42 selected sources (red dots)

18. MACRO: limit on diffuse E-2 flux • Selection of HE neutrinos: • timing cut (upward) • energy deposition in scintillators E2 < 4.5 10-6 cm -2 s -1 sr –1 GeV

19. MACRO: Neutrinos from GRB Search for space-time correlation With 2527 BATSE GRB between 1991 and 1999 Flux < 0.8 x 10-9 cm-2 per average burst about 10 times above optimistic predictions (Paolis et al., Halzen & Hooper), about 100 times above Waxman & Bahcall)

20. Superkamiokande 1761 upward going muons (through-going and stopping) from 1264 live days (April 96-May 00) 1200 m2 acceptance area

21. Super-K: point source search

22. Upward muons underground Super-Kamiokande 2.0 k events MACRO 1.4 k events Baksan 1.0 k events IMB + K-II + KGF + Soudan + ... ~ 1.5 k events (?)  ~ 6000 events sets scale for underwater/ice experiments

23. Experiments under water

24. 3600 m 1366 m Lake Baikal, NT-200: The Site

25. NT-200: the detector pair of 37 cm Quasar PMTs

26. Lake Baikal: atmospheric neutrinos „Gold plated“ neutrino event, 4-string stage (1996) NT-200: zenith angle distribution 234 days in 1998/99 19 hits

27. Upper limit on diffuse flux of HE e  Request upward moving light front (like from e.m. shower below detector) Vertex distribution forE-2 e  Then cut on # hits Blue dots: time cut Red squares: # hit > 45 •  E2 < 1.9 10-6 cm-2 s-1 sr-1 GeV

28. NT-214 0.11101001000PeV Reach upper limit in   E2  3.5 10-7 cm-2 s-1 sr-1 GeV !

29. Antares Nestor Nemo test site The Mediterranean Projects

30. NESTOR First Mediterranean project (founded 1991) Site: Pylos (Greece), 3800m depth towers of 12 titanium floors each supporting 12 PMTs

31. Nestor Tower

32. Deployment plans Schedule: 2001: re-lay cable to site and deploy 2 floors 2003: full tower

33. 40 km Submarine cable -2400m ANTARES

34. Site, History, Schedule Marseille Toulon La Seyne sur Mer New Cable (2001) La Seyne-ANTARES Demonstrator Site 42°59 N, 5°17 E Depth 1200 m Existing cable Marseille-Corsica ANTARES Site 42°50 N, 6°10 E Depth 2400 m Demonstrator Line: 8 OMs Nov 1999 - June 2000 0.05 km2 Detector: 900 OMs , Deploy 2002- 2004

35. Shore station Optical module 10 strings 12 m between storeys hydrophone Compass, tilt meter 2500m float ~60m Electro-optic submarine cable ~40km 300m active Electronics containers Readout cables ~100m Junction box anchor Acoustic beacon The Detector

36. ANTARES Performance Very good angular accuracy below 3 TeV angular error is dominated by kinematics, above 3 TeV by recon- struction error (~ 0.4°) Effective area: ~ 10 000 m2 at 1 TeV ~ 50 000 m2 at 100 TeV E/E ~ 3 (1-10 TeV) 2 (> 10 TeV)

37. 0.0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1.0 ANTARES Northern Hemisphere Galactic Centre seen 80% of time AMANDA Southern Hemisphere Galactic Centre not visible View of Sky: Complementary to AMANDA Fraction of time sky visible

38. NEMO

39. Nemo-2

40. Nemo3

41. Experiments under ice

42. AMANDA Location: Geographic South Pole Amanda –II: 677 PMTs at 19 strings

43. AMANDA: Atmospheric neutrinos ~ 300 neutrinos from 130 days in 1997 (Amanda-B10) Systematic still error ~ 50% (prediction atm.  ~ 30%, experiment ~ 40% (ice properties, OM sensitivity)

44. AMANDA: limit on diffuse flux Search for excess of high energy neutrinos Optimize analysis for HE neutrinos Use number of hit PMT as energy estimator. Place cut according to Feldman- Cousins (using only MC) Full: Experiment Dots: Atmos. „AGN“ with 10-5 E-2 GeV-1 cm-2 s-1 sr-1 E2 F < 0.9 10-6 GeV-1 cm-2 s-1 sr-1

45. Search for point sources Optimize analysis on HE neutrinos and good angular resolution Accept large background contribution Systematic uncertainties

46. Other limits from AMANDA and BAIKAL AMANDA, 78 BATSE bursts in 1997 Relativistic Magnetic Monopoles Baikal WIMPs from center of Earth

47. AMANDA-II dramatically increased acceptance towards horizon Trigger Level A-II B-10 After BG rejection Nearly horizontal event (experiment) up horizon

48. Physics Reach of AMANDA-II Search for  from TeV  sources Milagrito all-sky search sets limit at > 1 TeV: 7-30  10-7 m-2 s-1, ( E-2.5) Amanda probes similar flux if/ > 1 Mk-501 Sensitivity to diffuse flux E2 F ~ 5 10-8 GeV cm-2 s-1 sr-1

49. AMANDA-II and EeV search Transmission of Earth for Neutrinos as a function of zenith angle and energy Earth opaque above a few PeV Downward- background at high energies is small. PeV acceptance around horizon EeV acceptance above horizon

50. AMANDA-II and EeV search • Look for bright tracks passing inside and outside array • Background rejection “straightforward” • Total energy and “energy flow” variables • SPASE vetoes large DW at relevant ECR • Calibration possible using in-situ N2 laser • Equivalent to 200 TeV cascade in energy Improve sensitivity above 10-100 PeV to E2 F ~ 2 10-8 GeV cm-2 s-1 sr-1 Sensitive to some trans-GZK models !