Extremely High Energy Neutrinos
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1 Extremely High Energy Neutrinos A. Ringwald ringwald DESY 6 th National Astroparticle Physics Symposium February 3, 2006, Vrije Universiteit, Amsterdam, Netherlands
2 Extremely high energy neutrinos 1 1. Introduction Existing observatories for (Extremely) High Energy Cosmic ν s provide sensible upper bounds on flux Upcoming decade: progressively larger detectors for EHECν s E ev: Astrophysics of cosmic rays E ev: Particle physics beyond LHC E ev: Cosmology: relics of phase transitions; absorption on big bang relic neutrinos BAIKAL Neutrino Telescope: [baikalweb.jinr.ru/]
3 Extremely high energy neutrinos 2 1. Introduction Existing observatories for (Extremely) High Energy Cosmic ν s provide sensible upper bounds on flux Upcoming decade: progressively larger detectors for EHECν s E ev: Astrophysics of cosmic rays E ev: Particle physics beyond LHC E ev: Cosmology: relics of phase transitions; absorption on big bang relic neutrinos AMANDA: Antarctic Muon And Neutrino Detector Array [amanda.wisc.edu]
4 Extremely high energy neutrinos 3 1. Introduction Existing observatories for (Extremely) High Energy Cosmic ν s provide sensible upper bounds on flux Upcoming decade: progressively larger detectors for EHECν s E ev: Astrophysics of cosmic rays E ev: Particle physics beyond LHC E ev: Cosmology: relics of phase transitions; absorption on big bang relic neutrinos ANTARES: Astronomy with a Neutrino Telescope and Abyss environmental RESearch A. Ringwald (DESY) Astroparticle Physics Symposium, [antares.in2p3.fr/index.html] Amsterdam, Netherlands
5 Extremely high energy neutrinos 4 1. Introduction Existing observatories for (Extremely) High Energy Cosmic ν s provide sensible upper bounds on flux Upcoming decade: progressively larger detectors for EHECν s E ev: Astrophysics of cosmic rays E ev: Particle physics beyond LHC E ev: Cosmology: relics of phase transitions; absorption on big bang relic neutrinos RICE: Radio Ice Cerenkov Experiment [www2.phys.canterbury.ac.nz/rice]
6 Extremely high energy neutrinos 5 1. Introduction Existing observatories for (Extremely) High Energy Cosmic ν s provide sensible upper bounds on flux Upcoming decade: progressively larger detectors for EHECν s E ev: Astrophysics of cosmic rays E ev: Particle physics beyond LHC E ev: Cosmology: relics of phase transitions; absorption on big bang relic neutrinos GLUE: Goldstone Lunar Ultra-high energy neutrino Experiment [ moonemp/public/]
7 Extremely high energy neutrinos 6 1. Introduction Existing observatories for (Extremely) High Energy Cosmic ν s provide sensible upper bounds on flux Upcoming decade: progressively larger detectors for EHECν s E ev: Astrophysics of cosmic rays E ev: Particle physics beyond LHC E ev: Cosmology: relics of phase transitions; absorption on big bang relic neutrinos GLUE: Goldstone Lunar Ultra-high energy to earth front side partial Cherenkov cone neutrino Experiment cascade back side [Gorham et al. 04] neutrino enters moon
8 Extremely high energy neutrinos 7 1. Introduction Existing observatories for (Extremely) High Energy Cosmic ν s provide sensible upper bounds on flux FORTE: Fast On-orbit Recording of Transient Events Upcoming decade: progressively larger detectors for EHECν s E ev: Astrophysics of cosmic rays E ev: Particle physics beyond LHC E ev: Cosmology: relics of phase transitions; absorption on big bang relic neutrinos [nis-
9 Extremely high energy neutrinos 8 1. Introduction Existing observatories for (Extremely) High Energy Cosmic ν s provide sensible upper bounds on flux FORTE: Fast On-orbit Recording of Transient Events Upcoming decade: progressively larger detectors for EHECν s E ev: Astrophysics of cosmic rays E ev: Particle physics beyond LHC E ev: Cosmology: relics of phase transitions; absorption on big bang relic neutrinos [Lehtinen et al. 04]
10 Extremely high energy neutrinos 9 1. Introduction Existing observatories for (Extremely) High Energy Cosmic ν s provide sensible upper bounds on flux Upcoming decade: progressively larger detectors for EHECν s E ev: Astrophysics of cosmic rays E ev: Particle physics beyond LHC E ev: Cosmology: relics of phase transitions; absorption on big bang relic neutrinos ANITA-LITE: Prototype of ANtarctic Impulsive Transient Antenna [ anita/web/index.htm]
11 Extremely high energy neutrinos Introduction Existing observatories for (Extremely) High Energy Cosmic ν s provide sensible upper bounds on flux Upcoming decade: progressively larger detectors for EHECν s E ev: Astrophysics of cosmic rays E ev: Particle physics beyond LHC E ev: Cosmology: relics of phase transitions; absorption on big bang relic neutrinos ANITA-LITE: Prototype of ANtarctic Impulsive Transient Antenna [cosray2.wustl.edu/tiger/index.html]
12 Extremely high energy neutrinos Introduction Existing observatories for (Extremely) High Energy Cosmic ν s provide sensible upper bounds on flux Upcoming decade: progressively larger detectors for EHECν s E ev: Astrophysics of cosmic rays E ev: Particle physics beyond LHC E ev: Cosmology: relics of phase transitions; absorption on big bang relic neutrinos
13 Extremely high energy neutrinos Introduction Existing observatories for (Extremely) High Energy Cosmic ν s provide sensible upper bounds on flux Upcoming decade: progressively larger detectors for EHECν s E ev: Astrophysics of cosmic rays E ev: Particle physics beyond LHC E ev: Cosmology: relics of phase transitions; absorption on big bang relic neutrinos PAO: Pierre Auger Observatory [
14 Extremely high energy neutrinos Introduction Existing observatories for (Extremely) High Energy Cosmic ν s provide sensible upper bounds on flux Upcoming decade: progressively larger detectors for EHECν s E ev: Astrophysics of cosmic rays E ev: Particle physics beyond LHC E ev: Cosmology: relics of phase transitions; absorption on big bang relic neutrinos IceCube: [icecube.wisc.edu]
15 Extremely high energy neutrinos Introduction Existing observatories for (Extremely) High Energy Cosmic ν s provide sensible upper bounds on flux Upcoming decade: progressively larger detectors for EHECν s E ev: Astrophysics of cosmic rays E ev: Particle physics beyond LHC E ev: Cosmology: relics of phase transitions; absorption on big bang relic neutrinos ANITA: [ anita/]
16 Extremely high energy neutrinos Introduction Existing observatories for (Extremely) High Energy Cosmic ν s provide sensible upper bounds on flux WSRT: WeSterbork Radio Telescope Upcoming decade: progressively larger detectors for EHECν s E ev: Astrophysics of cosmic rays E ev: Particle physics beyond LHC E ev: Cosmology: relics of phase transitions; absorption on big bang relic neutrinos [Bacelar, ARENA Workshop 05]
17 Extremely high energy neutrinos Introduction Existing observatories for (Extremely) High Energy Cosmic ν s provide sensible upper bounds on flux WSRT: WeSterbork Radio Telescope Upcoming decade: progressively larger detectors for EHECν s E ev: Astrophysics of cosmic rays E ev: Particle physics beyond LHC E ev: Cosmology: relics of phase transitions; absorption on big bang relic neutrinos [Bacelar, ARENA Workshop 05]
18 Extremely high energy neutrinos Introduction Existing observatories for (Extremely) High Energy Cosmic ν s provide sensible upper bounds on flux Upcoming decade: progressively larger detectors for EHECν s E ev: Astrophysics of cosmic rays E ev: Particle physics beyond LHC E ev: Cosmology: relics of phase transitions; absorption on big bang relic neutrinos LOFAR: [
19 Extremely high energy neutrinos Introduction Existing observatories for (Extremely) High Energy Cosmic ν s provide sensible upper bounds on flux Upcoming decade: progressively larger detectors for EHECν s E ev: Astrophysics of cosmic rays E ev: Particle physics beyond LHC E ev: Cosmology: relics of phase transitions; absorption on big bang relic neutrinos
20 Extremely high energy neutrinos Introduction Existing observatories for (Extremely) High Energy Cosmic ν s provide sensible upper bounds on flux Upcoming decade: progressively larger detectors for EHECν s E ev: Astrophysics of cosmic rays E ev: Particle physics beyond LHC E ev: Cosmology: relics of phase transitions; absorption on big bang relic neutrinos
21 Extremely high energy neutrinos Introduction Existing observatories for (Extremely) High Energy Cosmic ν s provide sensible upper bounds on flux Upcoming decade: progressively larger detectors for EHECν s E ev: Astrophysics of cosmic rays E ev: Particle physics beyond LHC E ev: Cosmology: relics of phase transitions; absorption on big bang relic neutrinos
22 Extremely high energy neutrinos 21 Further content: 2. Sources and fluxes of EHEC neutrinos 3. Fun with EHEC neutrinos 4. Conclusions
23 Extremely 2. Sources high energy neutrinos and fluxes of EHEC neutrinos 22 Paradigm for astrophysical extragalactic source of protons and neutrinos: shock acceleration p s, confined by magnetic fields, accelerate through repeated scattering by plasma shock fronts production of π s and n s through collisions of the trapped p s with ambient plasma produces γ s, ν s and CR s (n diffusion from source) Hillas: E p < ev E ν < ev EHEC (E ν > ev) neutrinos yet unknown acceleration sites other acceleration mechanism decay of superheavy particles
24 Extremely 2. Sources high energy neutrinos and fluxes of EHEC neutrinos 23 Paradigm for astrophysical extragalactic source of protons and neutrinos: shock acceleration p s, confined by magnetic fields, accelerate through repeated scattering by plasma shock fronts production of π s and n s through collisions of the trapped p s with ambient plasma produces γ s, ν s and CR s (n diffusion from source) ν e ν µ ν µ e µ π p n e + p µ + π + ν e ν µ SHOCK ν µ Hillas: E p < ev E ν < ev EHEC (E ν > ev) neutrinos yet unknown acceleration sites other acceleration mechanism decay of superheavy particles [Ahlers PhD in prep.]
25 Extremely 2. Sources high energy neutrinos and fluxes of EHEC neutrinos 24 Paradigm for astrophysical extragalactic source of protons and neutrinos: shock acceleration p s, confined by magnetic fields, accelerate through repeated scattering by plasma shock fronts production of π s and n s through collisions of the trapped p s with ambient plasma produces γ s, ν s and CR s (n diffusion from source) Hillas: E p < ev E ν < ev n p π + ν e ν µ e + µ + ν µ SHOCK EHEC (E ν > ev) neutrinos yet unknown acceleration sites other acceleration mechanism decay of superheavy particles [Ahlers PhD in prep.]
26 Extremely 2. Sources high energy neutrinos and fluxes of EHEC neutrinos 25 Paradigm for astrophysical extragalactic source of protons and neutrinos: shock acceleration p s, confined by magnetic fields, accelerate through repeated scattering by plasma shock fronts production of π s and n s through collisions of the trapped p s with ambient plasma produces γ s, ν s and CR s (n diffusion from source) Hillas: E p < ev E ν < ev log(magnetic field, gauss) Hillas-plot (candidate sites for E=100 EeV and E=1 ZeV) Neutron star GRB White dwarf Fe (100 EeV) Protons (100 EeV) Protons (1 ZeV) Colliding galaxies nuclei SNR jets Galactic disk halo Active galaxies hot-spots lobes Clusters EHEC (E ν > ev) neutrinos yet unknown acceleration sites other acceleration mechanism decay of superheavy particles E max~ ZBL E ~ ZBL Γ max 1 au 1 pc 1 kpc 1 Mpc log(size, km) (Fermi) (Ultra-relativistic shocks-grb) [Pierre Auger Observatory]
27 Extremely 2. Sources high energy neutrinos and fluxes of EHEC neutrinos 26 Paradigm for astrophysical extragalactic source of protons and neutrinos: shock acceleration p s, confined by magnetic fields, accelerate through repeated scattering by plasma shock fronts production of π s and n s through collisions of the trapped p s with ambient plasma produces γ s, ν s and CR s (n diffusion from source) Hillas: E p < ev E ν < ev EHEC (E ν > ev) neutrinos yet unknown acceleration sites other acceleration mechanism decay of superheavy particles
28 Extremely 2. Sources high energy neutrinos and fluxes of EHEC neutrinos 27 Paradigm for astrophysical extragalactic source of protons and neutrinos: shock acceleration p s, confined by magnetic fields, accelerate through repeated scattering by plasma shock fronts production of π s and n s through collisions of the trapped p s with ambient plasma produces γ s, ν s and CR s (n diffusion from source) Hillas: E p < ev E ν < ev EHEC (E ν > ev) neutrinos yet unknown acceleration sites other acceleration mechanism decay of superheavy particles [Barbot,Drees 02]
29 Extremely 2. Sources high energy neutrinos and fluxes of EHEC neutrinos 28 Paradigm for astrophysical extragalactic source of protons and neutrinos: shock acceleration p s, confined by magnetic fields, accelerate through repeated scattering by plasma shock fronts production of π s and n s through collisions of the trapped p s with ambient plasma produces γ s, ν s and CR s (n diffusion from source) Hillas: E p < ev E ν < ev EHEC (E ν > ev) neutrinos yet unknown acceleration sites other acceleration mechanism decay of superheavy particles
30 Extremely high energy neutrinos 29 Top-down scenarios for EHEC neutrinos Existence of superheavy particles with GeV < m X < GeV, produced during and after inflation through e.g. particle creation in time-varying gravitational field EHEC ν s from decay or annihilation of superheavy dark matter (for τ X > τ U ) decomposition of topological defects, formed during preheating, into their constituents EHEC ν s from topological defects [Kolb,Chung,Riotto 98]
31 Extremely high energy neutrinos 30 Top-down scenarios for EHEC neutrinos Existence of superheavy particles with GeV < m X < GeV, produced during and after inflation through e.g. t= t= particle creation in time-varying gravitational field EHEC ν s from decay or annihilation of superheavy dark matter (for τ X > τ U ) decomposition of topological defects, formed during preheating, into their constituents EHEC ν s from topological defects 0 t= t=330 [Tkachev,Khlebnikov,Kofman,Linde 98]
32 tot I halo I halo N I extr p I Extremely high energy neutrinos 31 Top-down scenarios for EHEC neutrinos Existence of superheavy particles with GeV < m X < GeV, produced during and after inflation through e.g. particle creation in time-varying gravitational field EHEC ν s from decay or annihilation of superheavy dark matter (for τ X > τ U ) decomposition of topological defects, formed during preheating, into their constituents EHEC ν s from topological defects log 10 (E 3 I); m?2 s?1 sr?1 ev log (E=eV) [Berezinsky,Kachelriess,Vilenkin 97]
33 Extremely high energy neutrinos 32 Top-down scenarios for EHEC neutrinos Existence of superheavy particles with GeV < m X < GeV, produced during and after inflation through e.g. particle creation in time-varying gravitational field EHEC ν s from decay or annihilation of superheavy dark matter (for τ X > τ U ) decomposition of topological defects, formed during preheating, into their constituents EHEC ν s from topological defects [Bhattacharjee,Hill,Schramm 92]
34 Extremely high energy neutrinos 33 Top-down scenarios for EHEC neutrinos Injection spectra: fragmentation functions D i (x,µ), i = p, e,γ,ν, determined via Monte Carlo generators DGLAP evolution from experimental initial distributions at e.g. µ = m Z to µ = m X dn/dx Photons Neutrinos Electrons Protons m X = GeV Reliably predicted! 0.1 Spectra at Earth: 0.01 for superheavy dark matter, injection nearby: j ν j γ j p for topological defects, injection far away: j ν j γ j p x [Birkel,Sarkar 98]
35 Extremely high energy neutrinos 34 Top-down scenarios for EHEC neutrinos Injection spectra: fragmentation functions D i (x,µ), i = p, e,γ,ν, determined via Monte Carlo generators DGLAP evolution from experimental initial distributions at e.g. µ = m Z to µ = m X Reliably predicted! Spectra at Earth: for superheavy dark matter, injection nearby: j ν j γ j p for topological defects, injection far away: j ν j γ j p 1/σ had dσ/dx 1/σ had dσ/dx 1/σ had dσ/dx π ± ( s = 91 GeV) π ± ( s = 29 GeV) π ± ( s = 10 GeV) K ± ( s = 91 GeV) K ± ( s = 29 GeV) K ± ( s = 10 GeV) p, _ p ( s = 91 GeV) p, _ p ( s = 29 GeV) p, _ p ( s = 10 GeV) (a) (b) (c) x p = p/p beam [Particle Data Group 04]
36 Extremely high energy neutrinos 35 Top-down scenarios for EHEC neutrinos Injection spectra: fragmentation functions D i (x,µ), i = p, e,γ,ν, determined via Monte Carlo generators DGLAP evolution from experimental initial distributions at e.g. µ = m Z to µ = m X Reliably predicted! Spectra at Earth: for superheavy dark matter, injection nearby: j ν j γ j p for topological defects, injection far away: j ν j γ j p [Fodor,Katz 01]
37 Ü Ô Õ Ü Å µ Extremely high energy neutrinos 36 Top-down scenarios for EHEC neutrinos Injection spectra: fragmentation functions D i (x,µ), i = p, e,γ,ν, determined via Monte Carlo generators DGLAP evolution from experimental initial distributions at e.g. µ = m Z to µ = m X Reliably predicted! Spectra at Earth: for superheavy dark matter, injection nearby: j ν j γ j p for topological defects, injection far away: j ν j γ j p this work Barbot-Drees Sarkar-Toldra 1e-05 1e Ü Å ½ ½¼ ½ [Aloisio,Berezinsky,Kachelriess 04] Î
38 Extremely high energy neutrinos 37 Top-down scenarios for EHEC neutrinos Injection spectra: fragmentation functions D i (x,µ), i = p, e,γ,ν, determined via Monte Carlo generators DGLAP evolution from experimental initial distributions at e.g. µ = m Z to µ = m X Reliably predicted! Spectra at Earth: for superheavy dark matter, injection nearby: j ν j γ j p for topological defects, injection far away: j ν j γ j p [Aloisio,Berezinsky,Kachelriess 04]
39  µ Î ¾ Ñ ¾ ½ Ö ½ µ Extremely high energy neutrinos 38 Top-down scenarios for EHEC neutrinos Injection spectra: fragmentation functions D i (x,µ), i = p, e,γ,ν, determined via Monte Carlo generators DGLAP evolution from experimental initial distributions at e.g. µ = m Z to µ = m X Reliably predicted! Spectra at Earth: for superheavy dark matter, injection nearby: j ν j γ j p for topological defects, injection far away: j ν j γ j p 1e+27 1e+26 1e+25 1e+24 1e+23 Å ½ ½¼ ½ Ô Î 1e+22 1e+18 1e+19 1e+20 1e+21 1e+22 ε [Aloisio,Berezinsky,Kachelriess 04] Ô
40 Extremely high energy neutrinos 39 Top-down scenarios for EHEC neutrinos How natural? Superheavy dark matter: need symmetry to prevent fast X decay gauge X stable discrete stable or quasi-stable Topological defects: generic prediction of symmetry breaking (SB) in GUT s, including fundamental string theory, e.g. G H U(1) SB: monopoles U(1) SB: ordinary or superconducting strings G H U(1) H Z N SB: monopoles connected by strings
41 Extremely high energy neutrinos 40 Top-down scenarios for EHEC neutrinos How natural? Superheavy dark matter: need symmetry to prevent fast X decay gauge X stable discrete stable or quasi-stable Topological defects: generic prediction of symmetry breaking (SB) in GUT s, including fundamental string theory, e.g. G H U(1) SB: monopoles U(1) SB: ordinary or superconducting strings G H U(1) H Z N SB: monopoles connected by strings x z Imφ Reφ y [Rajantie 03]
42 Extremely high energy neutrinos 41 Top-down scenarios for EHEC neutrinos How natural? Superheavy dark matter: need symmetry to prevent fast X decay gauge X stable discrete stable or quasi-stable Topological defects: generic prediction of symmetry breaking (SB) in GUT s, including fundamental string theory, e.g. G H U(1) SB: monopoles U(1) SB: ordinary or superconducting strings G H U(1) H Z N SB: monopoles connected by strings M M M NECKLACE M M MS NETWORK M [Berezinsky 05]
43 Extremely high energy neutrinos Fun with EHEC neutrinos EHEC ν s in reach! Strong impact of measurement for particle physics GUT parameters, e.g. m X particle content of the desert, e.g. SM vs. MSSM νn scattering at s LHC cosmology window on early phase transition Hubble expansion rate H(z) existence of the big bang relic neutrino background
44 Extremely high energy neutrinos Fun with EHEC neutrinos EHEC ν s in reach! Strong impact of measurement for particle physics GUT parameters, e.g. m X particle content of the desert, e.g. SM vs. MSSM νn scattering at s LHC cosmology window on early phase transition Hubble expansion rate H(z) existence of the big bang relic neutrino background
45 Extremely high energy neutrinos Fun with EHEC neutrinos EHEC ν s in reach! Strong impact of measurement for particle physics GUT parameters, e.g. m X particle content of the desert, e.g. SM vs. MSSM νn scattering at s LHC cosmology window on early phase transition Hubble expansion rate H(z) existence of the big bang relic neutrino background [Barbot,Drees 02]
46 Extremely high energy neutrinos Fun with EHEC neutrinos EHEC ν s in reach! Strong impact of measurement for particle physics GUT parameters, e.g. m X particle content of the desert, e.g. SM vs. MSSM νn scattering at s LHC cosmology window on early phase transition Hubble expansion rate H(z) existence of the big bang relic neutrino background [Tu 04]
47 Extremely high energy neutrinos Fun with EHEC neutrinos EHEC ν s in reach! Strong impact of measurement for particle physics GUT parameters, e.g. m X particle content of the desert, e.g. SM vs. MSSM νn scattering at s LHC cosmology window on early phase transition Hubble expansion rate H(z) existence of the big bang relic neutrino background (CνB)
48 Absorption of EHEC neutrinos by the CνB Extremely high energy neutrinos 47 At the resonance energies E res ν = m2 Z 2m ν ev ( ) ev m ν EHEC neutrinos annihilate with relic neutrinos into Z bosons Absorption dips in EHEC neutrino spectra Detectable within next decade if EHEC neutrino flux close to current observational bounds neutrino mass sufficiently large, m νi > 0.1 ev
49 Absorption of EHEC neutrinos by the CνB Extremely high energy neutrinos 48 At the resonance energies E res ν = m2 Z 2m ν ev ( ) ev m ν EHEC neutrinos annihilate with relic neutrinos into Z bosons Absorption dips in EHEC neutrino spectra Detectable within next decade if EHEC neutrino flux close to current observational bounds neutrino mass sufficiently large, m νi > 0.1 ev [Weiler 82]
50 Absorption of EHEC neutrinos by the CνB Extremely high energy neutrinos 49 At the resonance energies E res ν = m2 Z 2m ν ev ( ) ev m ν EHEC neutrinos annihilate with relic neutrinos into Z bosons Absorption dips in EHEC neutrino spectra Detectable within next decade if EHEC neutrino flux close to current observational bounds neutrino mass sufficiently large, m νi > 0.1 ev [Eberle,AR,Song,Weiler 04]
51 Absorption of EHEC neutrinos by the CνB Extremely high energy neutrinos 50 At the resonance energies E res ν = m2 Z 2m ν ev ( ) ev m ν EHEC neutrinos annihilate with relic neutrinos into Z bosons Absorption dips in EHEC neutrino spectra Detectable within next decade EHEC neutrino flux close to current observational bounds neutrino mass sufficiently large, m νi > 0.1 ev [Barenboim,Mena,Quigg 05]
52 Absorption of EHEC neutrinos by the CνB Extremely high energy neutrinos 51 At the resonance energies E res ν = m2 Z 2m ν ev ( ) ev m ν Y EHEC neutrinos annihilate with relic neutrinos into Z bosons Absorption dips in EHEC neutrino spectra Detectable within next decade if EHEC neutrino flux close to current observational bounds neutrino mass sufficiently large, m νi > 0.1 ev Y X X [D Olivo,Nellen,Sahu,Van Elewyck 05]
53 Absorption of EHEC neutrinos by the CνB Extremely high energy neutrinos 52 At the resonance energies E res ν = m2 Z 2m ν ev ( ) ev m ν EHEC neutrinos annihilate with relic neutrinos into Z bosons Absorption dips in EHEC neutrino spectra Detectable within next decade if m X > GeV EHEC neutrino flux close to current observational bounds [Fodor,Katz,AR,Weiler,Wong,in prep.]
54 Absorption of EHEC neutrinos by the CνB Extremely high energy neutrinos 53 At the resonance energies E res ν = m2 Z 2m ν ev ( ) ev m ν EHEC neutrinos annihilate with relic neutrinos into Z bosons Absorption dips in EHEC neutrino spectra Detectable within next decade if m X > GeV EHEC neutrino flux close to current observational bounds [Fodor,Katz,AR,Weiler,Wong,in prep.]
55 Absorption of EHEC neutrinos by the CνB Extremely high energy neutrinos 54 At the resonance energies E res ν = m2 Z 2m ν ev ( ) ev m ν EHEC neutrinos annihilate with relic neutrinos into Z bosons Absorption dips in EHEC neutrino spectra Detectable within next decade if m X > GeV EHEC neutrino flux close to current observational bounds Z-bursts as EHEC recovery [Fodor,Katz,AR,Weiler,Wong,in prep.]
56 Extremely high energy neutrinos Conclusions Exciting times for EHEC neutrinos: many observatories under construction appreciable event samples Expect strong impact on astrophysics particle physics cosmology
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