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Neutrino Astronomy: 

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

Why Neutrinos: 

Why Neutrinos

Why not protons?: 

Why not protons? Protons are bent in the magnetic fields of our galaxy and local cluster Energy of >1019eV needed to point back to even galactic sources Above a few 1019eV GZK cutoff limits their range too

Effect of IR Absorption on Distant Sources: 

Effect of IR Absorption on Distant Sources e+ e- ~eV g ~TeV g 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)

Photon Attenuation on IR: 

Photon Attenuation on IR

Questions in ultra high energy astrophysics: 

Questions in ultra high energy astrophysics Source of UHE cosmic rays GRBs AGN Dark Matter Other Physics Questions

Origin of Cosmic Rays: 

Origin of Cosmic Rays Extragalactic flux sets scale for many acceleration models Atmospheric neutrinos See Monday PM & Thursday AM

Alternative Models: 

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 n’s (Z-bursts) Mostly pions (ns,gs,not protons) Disfavored! Highest energy cosmic rays are not gamma rays Overproduce TeV-neutrinos

SNRs: 

SNRs

HESS: RXJ1713: 

HESS: RXJ1713 First resolved TeV g-ray image of a Shell type SNR (Resolution ~10 arcmin) Acceleration source of Cosmic Rays, but is it evidence of Protons?

HESS: RXJ1713 – Molecular Clouds : 

HESS: RXJ1713 – Molecular Clouds

RXJ1713 Spectrum: 

RXJ1713 Spectrum In favor of p0: no cut-off in the HE tail of HESS spectrum signal from the direction of molecular clouds See HESS Talk Tuesday Afternoon

Have g-rays from p0 decay been discovered?: 

Have g-rays from p0 decay been discovered? En Nn (En) =  Eg Ng (Eg) 1 <  < 8 transparent source p0 = p+ = p- accelerator beam dump (hidden source) n flux predicted observed g-ray flux ~40 per km2 RX J1713-3946 per year (galactic center)

Milagro (TeV) Diffuse Source: 

Milagro (TeV) Diffuse Source See Milagro Talk Tues Afternoon

Active Galactic Nuclei: 

Produces cosmic ray beam Radiation field: Active Galactic Nuclei

Active Galactic Nuclei (AGN): 

Active Galactic Nuclei (AGN)

VLA image of Cygnus A: 

VLA image of Cygnus A See Monday Morning AGN Session

GZK: 

GZK g p n p n n n E = 6 x10 19 eV E ~4 x 10 19 eV p + gCMB → p+ + n = (ncmb s p + g )-1 l= 10 Mpc Cutoff above 50 EeV

GZK: 

GZK Cosmogenic neutrinos are guaranteed if primaries are nucleons. May be much larger fluxes, for some models, such as topological defects

GZK: 

GZK See Monday PM + Thurs AM Sess.

GRBs: 

GRBs

GRBs: 

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

Slide25: 

e- p+ R < 108 cm R  1014 cm, T  3 x 103 seconds R  1018 cm, T  3 x 1016 seconds E  1051 – 1054 ergs Shock variability is reflected in the complexity of the GRB time profile. 6 Hours 3 Days Radio Optical -ray X-ray (2-10 keV) Fireball Phenomenology & The Gamma-Ray Burst (GRB) Neutrino Connection Progenitor (Massive star) Meszaros, P

Generic GRB Explosion Models: 

Generic GRB Explosion Models

Slide27: 

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. Dt ~ x(E/EQG)a L/c E2-c2p2~E2x(E/EQG)a - 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. E2 = m2c4 +p2c2 - 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

Galactic Microquasars: 

Galactic Microquasars See Talk Monday Morning

What About Dark Matter?: 

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

Wimp Capture: 

Wimp Capture

Wimp Detection: 

Wimp Detection

Neutrino Astronomy Explores Extra Dimensions: 

Neutrino Astronomy Explores Extra Dimensions 100 x SM GZK range TeV-scale gravity increases PeV n-cross section See Wednesday Afternoon Session

Cosmic Neutrino Factory: 

radiation enveloping black hole black hole p + g -> n + p+ ~ cosmic ray + neutrino -> p + p0 ~ cosmic ray + gamma Cosmic Neutrino Factory

W-B Bound: 

W-B Bound

Evading the Bound: 

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

Mannheim, Protheore and Rachen Model: 

Mannheim, Protheore and Rachen Model

Neutrinos from Cosmic Rays: 

Neutrinos from Cosmic Rays ~50 events/km2/yr

Size Perspective for KM3: 

Size Perspective for KM3 50 m 1500 m 2500 m 300 m AMANDAII

Detection Technique: 

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

Detection of e , , : 

Detection of e , ,  O(km) long muon tracks direction determination by cherenkov light timing  17 m

Muon Events : 

Eµ= 10 TeV Eµ= 6 PeV Measure energy by counting the number of fired PMT. (This is a very simple but robust method) Muon Events

Determining Energy: 

Determining Energy 10 TeV m 6 PeV m 375 TeV Cascade

Double Bang: 

 Double Bang 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 nµ (Beacom et al.., astro/ph 0111482) Learned, Pakvasa, 1995

Tau Cascades: 

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)

Neutrino ID (solid)Energy and angle (shaded): 

Neutrino ID (solid) Energy and angle (shaded) Neutrino flavor

Tau Transparency/Regeneration: 

Tau Transparency/Regeneration ne and nµ are absorbed in the Earth via charged current interactions (muons range out) Above ~100 TeV the Earth is opaque to ne & νµ. But, the Earth never becomes completely opaque to nt Due to the short t lifetime, t’s produced in nt charged-current interactions decay back into nt Also, secondary ne & νµ. fluxes are produced in the tau decays.

Flavor Ratios: 

Flavor Ratios The ratio of flavors at the source is expected to be 0:2:1= nt : nm : ne Since the distance to the source is >> than the oscillation length – any admixture at the source should wind up: 1:1:1= nt : nm : ne when arriving at earth What if that isn’t true?

Exotic neutrino properties if not 1:1:1: 

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 δm2 (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)

Supernova Monitor: 

Amanda-II Amanda-B10 IceCube Supernova Monitor B10: 60% of Galaxy A-II: 95% of Galaxy IceCube: up to LMC

Large Scale Neutrino Detectors: 

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

Radio Cherenkov Detectors: 

Radio Cherenkov Detectors Rice Anita Salsa

Acoustic Detectors: 

Acoustic Detectors SAUND (Study of Acoustic Underwater Neutrino Detection)

Conclusions: 

Conclusions Now Soon Future Amanda Cherenkov arrays ??? SK Radio Detectors Neutrino Astronomy is just beginning to open a new window on the Universe!