1. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Neutrino Astronomy Why Neutrinos Questions in ultra high energy astrophysics –Source of UHE cosmic rays –GRBs –AGN –Other Physics Questions – DM, Top Down models, etc Understanding the W-B bound –Why the kilometer scale or bigger Overview of experimental approach –Cherenkov Detectors- IceCube – Nestor, Antares, Baikal –Radio - Rice, Anita, Salsa

2. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Why Neutrinos

3. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Why not protons? Protons are bent in the magnetic fields of our galaxy and local cluster Energy of >10 19 eV needed to point back to even galactic sources Above a few 10 19 eV GZK cutoff limits their range too

4. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Effect of IR Absorption on Distant Sources z = 0.03 z = 0.1 z = 0.2 z = 0.3 z = 0.0 e+e+ e-e- ~eV  ~TeV  No direct measurement of IR extragalactic background light exists due to zodiacal foreground. TeV absorption constrains IR which depends on cosmology of galaxy and star formation models. IR Model of Stecker & deJager (1998)

5. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Photon Attenuation on IR

6. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Questions in ultra high energy astrophysics Source of UHE cosmic rays GRBs AGN Dark Matter Other Physics Questions

7. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Origin of Cosmic Rays Extragalactic flux sets scale for many acceleration models Atmospheric neutrinos See Monday PM & Thursday AM

8. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Knee Ankle New component with hard spectrum?

9. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Alternative Models Bottom up –GRB fireballs –Jets in active galaxies –Accretion shocks in galaxy clusters –Galaxy mergers –Young supernova remnants –Pulsars, Magnetars –Mini-quasars –… Observed showers either protons (or nuclei) Top-down –Radiation from topological defects –Decays of massive relic particles in Galactic halo –Resonant neutrino interactions on relic ’s (Z-bursts) Mostly pions ( s,  s,not protons) Disfavored!Disfavored! Highest energy cosmic rays Highest energy cosmic rays are not gamma rays are not gamma rays Overproduce TeV-neutrinos Overproduce TeV-neutrinos

10. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland

11. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland SNRs

12. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland HESS: RXJ1713 First resolved TeV  -ray image of a Shell type SNR (Resolution ~10 arcmin) Acceleration source of Cosmic Rays, but is it evidence of Protons?

13. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland HESS: RXJ1713 – Molecular Clouds

14. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland RXJ1713 Spectrum H.E.S.S.: full remnant CANGAROO: hotspot Index 2.2±0.07±0.1 preliminary Index 2.84±0.15±0.20 In favor of  0 : no cut-off in the HE tail of HESS spectrum signal from the direction of molecular clouds See HESS Talk Tuesday Afternoon

15. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Have  -rays from  0 decay been discovered? E N (E ) =  E  N  (E  ) 1 <  < 8 transparentsource  0 =  + =   0 =  + =  - accelerator beam dump (hidden source) flux predicted observed  -ray flux ~40 per km2 RX J1713-3946 per year (galactic center) per year (galactic center)

16. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Milagro (TeV) Diffuse Source See Milagro Talk Tues Afternoon

17. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Produces cosmic ray beam Radiation field: Radiation field: Active Galactic Nuclei

18. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Active Galactic Nuclei (AGN) Fermi acceleration Jets Black Hole Accretion Disk Shock fronts

19. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland VLA image of Cygnus A See Monday Morning AGN Session

20. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland GZK 0.6 x 10 -27 cm 2  p n p π ＋ μ ＋ e ＋ E = 6 x10 19 eV E ~4 x 10 19 eV p +  CMB →  + + n = (n cmb  p +  ) -1 = (n cmb  p +  ) -1 = 10 Mpc = 10 Mpc Cutoff above 50 EeV

21. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland GZK Cosmogenic neutrinos are guaranteed if primaries are nucleons. May be much larger fluxes, for some models, such as topological defects

22. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland GZK See Monday PM + Thurs AM Sess.

23. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland GRBs

24. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland GRBs Shocks: external collisions with interstellar material or internal collisions when slower material is overtaken by faster in the fireball. See Wed AM+ Thu PM GRB sessions

25. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland e-p+e-p+ R < 10 8 cm R  10 14 cm, T  3 x 10 3 seconds R  10 18 cm, T  3 x 10 16 seconds E  10 51 – 10 54 ergs Shock variability is reflected in the complexity of the GRB time profile. 6 Hours3 Days Radio Optical  -ray X-ray (2-10 keV) Fireball Phenomenology & The Gamma-Ray Burst (GRB) Neutrino Connection Progenitor (Massive star) Magnetic Field --- Electron  - ray Meszaros, P

26. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Generic GRB Explosion Models

27. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Lorentz Invariance Violation Bounds on energy dependence of the speed of light can be used to place constraints on the effective energy scale for quantum gravitational effects.  t ~  ( E/E QG )  L/c E 2 -c 2 p 2 ~E 2  (E/E QG )  - This may be modified in some quantum gravity models. This has the important observational consequence that this will give rise to energy dependent delays between arrival times of photons. E 2 = m 2 c 4 +p 2 c 2 - in the Lorentz invariant case, The expected time delay is : This may be measurable for very high energy photons/neutrinos coming from large distances. See Wed. Afternoon

28. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Galactic Microquasars See Talk Monday Morning

29. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland What About Dark Matter? ~85% of the matter in the Universe is Dark Matter –At most a few % of the matter is baryons –Most people believe that the lightest SUSY particle is a stable neutralino and is probably the dark matter –These are weakly interacting and heavy –Evidence of clustering See Friday Afternoon Session on Dark Matter

30. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Wimp Capture  Earth Detector 

31. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Wimp Detection

32. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Neutrino Astronomy Explores Extra Dimensions 100 x SM GZK range TeV-scale gravity increases PeV -cross section See Wednesday Afternoon Session

33. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland radiation enveloping black hole p +  -> n +  + ~ cosmic ray + neutrino -> p +  0 -> p +  0 ~ cosmic ray + gamma Cosmic Neutrino Factory

34. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland W-B Bound

35. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Evading the Bound “Neutrino only” sources that are optically thick to proton photo-meson interactions and from which protons cannot escape. –No observational evidence (from baryons or high energy photons) Cores of AGNs (rather than in the jets) by photo-meson interactions or via p−p collisions in a collapsing galactic nucleus or in a cacooned black hole. –The most optimistic predictions of the AGN core model have already been ruled out by AMANDA

36. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Mannheim, Protheore and Rachen Model

37. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Neutrinos from Cosmic Rays ~50 events/km 2 /yr

38. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Size Perspective for KM 3 50 m 1500 m 2500 m 300 m AMANDAII

39. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Detection Technique neutrino muon or tau Cerenkov light cone detector interaction The muon radiates blue light in its wake Optical sensors capture (and map) the light See Talks in this Session

40. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Detection of  e       ~ 5 m Electromagnetic and hadronic cascades O(km) long muon tracks direction determination by cherenkov light timing  17 m

41. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland E µ = 10 TeVE µ = 6 PeV Measure energy by counting the number of fired PMT. (This is a very simple but robust method) Muon Events

42. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Determining Energy 10 TeV  6 PeV  375 TeV Cascade

43. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland   Double Bang  + N -->  - + X  + X (82%) E << 1PeV: Single cascade (2 cascades coincide) E ≈ 1PeV: Double bang E >> 1 PeV: partially contained (reconstruct incoming tau track and cascade from decay) Regeneration makes Earth quasi transparent for high energie  ; (Halzen, Salzberg 1998, …) Also enhanced muon flux due to Secondary µ, and µ (Beacom et al.., astro/ph 0111482) Learned, Pakvasa, 1995

44. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Tau Cascades E << 1PeV: Single cascade (2 cascades coincide) E ≈ 1PeV: Double bang E >> 1 PeV: partially contained (reconstruct incoming tau track and cascade from decay)

45. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland

46. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Neutrino ID (solid) Energy and angle (shaded) Neutrino flavor

47. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Tau Transparency/Regeneration e and µ are absorbed in the Earth via charged current interactions (muons range out) Above ~100 TeV the Earth is opaque to e & ν µ. But, the Earth never becomes completely opaque to  Due to the short  lifetime,  ’s produced in  charged-current interactions decay back into  Also, secondary e & ν µ. fluxes are produced in the tau decays.

48. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Flavor Ratios The ratio of flavors at the source is expected to be 0:2:1=  :  : e Since the distance to the source is >> than the oscillation length – any admixture at the source should wind up: 1:1:1=  :  : e when arriving at earth What if that isn’t true?

49. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Exotic neutrino properties if not 1:1:1 Neutrino decay (Beacom, Bell, Hooper, Pakvasa& Weiler) CPT violation (Barenboim& Quigg) Oscillation to steriles with very tiny delta δm 2 (Crocker et al; Berezinskyet al.) Pseudo-Dirac mixing (Beacom, Bell, Hooper, Learned, Pakvasa& Weiler) 3+1 or 2+2 models with sterile neutrinos (Dutta, Reno and Sarcevic) Magnetic moment transitions (Enqvist, Keränen, Maalampi) Varying mass neutrinos (Fardon, Nelson & Weiner; Hung & Pas)

50. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Amanda-II Amanda-B10 IceCube 0 5 10 sec Count rates Supernova Monitor B10: 60% of Galaxy A-II: 95% of Galaxy IceCube: up to LMC

51. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Large Scale Neutrino Detectors NESTOR Pylos, Greece ANTARES La-Seyne-sur-Mer, France BAIKAL Russia IceCube, South Pole, Antarctica NEMO Catania, Italy See Talks in this Session

52. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Radio Cherenkov Detectors Rice AnitaSalsa

53. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Acoustic Detectors SAUND (Study of Acoustic Underwater Neutrino Detection)

54. Neutrino Astronomy March 2005J. Goodman – Univ. of Maryland Conclusions Now SoonFuture Amanda Cherenkov arrays??? SK Radio Detectors Neutrino Astronomy is just beginning to open a new window on the Universe!