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Neutrinos from AGN & GRB

Neutrinos from AGN & GRB. Expectations for a km 3 detector. Cosmic-ray factories?. Artist’s(*) conception of a massive, accreting, compact with accretion disk and relativistic jets * Artist = Todor Stanev. Active Galaxies: Jets. Radio Galaxy 3C296 (AUI, NRAO).

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Neutrinos from AGN & GRB

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  1. Neutrinos from AGN & GRB Expectations for a km3 detector PS638 Tom Gaisser

  2. Cosmic-ray factories? Artist’s(*) conception of a massive, accreting, compact with accretion disk and relativistic jets * Artist = Todor Stanev PS638 Tom Gaisser

  3. Active Galaxies: Jets Radio Galaxy 3C296 (AUI, NRAO). --Jets extend beyond host galaxy. Drawing of AGN core VLA image of Cygnus A PS638 Tom Gaisser M. Urry, astro-ph/0312545

  4. Spectral Energy Distribution for blazars Figure from Markus Bötcher, Astrophys. Space Sci 309 (2007) 95-104 PS638 Tom Gaisser

  5. Jet breakout in GRB following collapse of massive progenitor star 0 seconds fireball protons and photons interact Image: W. Zhang & S. Woosley See astro-ph/0308389v2 PeV EeV TeV - 10 seconds fireball protons interact with remnant of the star afterwards afterglow protons interact with inter-stellar medium PS638 Tom Gaisser

  6. PS638 Tom Gaisser Slide from Alexander Kappes

  7. PS638 Tom Gaisser

  8. Energy content of extra-galactic component depends on location of transition • Composition signature: • transition back to protons • Uncertainties: • Normalization point: • 1018 to 1019.5 used • Factor 10 / decade • Spectral slope • a=2.3 for rel. shock • =2.0 non-rel. • Emin ~ mp (gshock)2 PS638 Tom Gaisser

  9. Power needed for extragalactic cosmic rays assuming transition at 1019 eV • Energy density in UHECR, CR ~ 2 x 10-19 erg/cm3 • Such an estimate requires extrapolation of UHECR to low energy • CR = (4/c)  E(E) dE = (4/c){E2(E)}E=1019eV x ln{Emax/Emin} • This gives CR ~ 2 x 10-19 erg/cm3 for differential index  = 2, (E) ~ E-2 • Power required ~ CR/1010 yr ~ 1.3 x 1037 erg/Mpc3/s • Estimates depend on cosmology and extragalactic magnetic fields: • 3 x 10-3 galaxies/Mpc3 5 x 1039 erg/s/Galaxy • 3 x 10-6 clusters/Mpc3 4 x 1042 erg/s/Galaxy Cluster • 10-7 AGN/Mpc3 1044 erg/s/AGN • ~1000 GRB/yr 3 x 1052 erg/GRB • Assume E-2 spectrum. Then n signal ~ 10 to 100/km2yr • ~20% have E>50 TeV (greater than atmospheric background) PS638 Tom Gaisser

  10. GRB model Bahcall & Waxman, hep-ph/0206217 Waxman, astro-ph/0210638 • Assume E-2 spectrum at source, normalize @ 1019.5 • 1045 erg/Mpc3/yr • ~ 1053 erg/GRB • Evolution ~ star-formation rate • GZK losses included • Galactic extragalactic transition ~ 1019 eV PS638 Tom Gaisser

  11. Berezinsky et al. AGN • Assuming a cosmological distribution of sources with: • dN/dE ~ E-2, E < 1018 eV • dN/dE ~ E-g, 1018< E < 1021 • g = 2.7 (no evolution) • g = 2.5 (with evolution) • Need L0 ~ 3 ×1046 erg/Mpc3 yr • They interpret dip at 1019 as • p + g2.7 p + e+ + e- Berezinsky, Gazizov, Grigorieva astro-ph/0210095 PS638 Tom Gaisser

  12. 3 X 1018 eV 3 x 1017eV What is power needed for extra-galactic CR? Or start with a model of the extra-galactic component Subtract it from the observed spectrum to get the galactic component Allard, Olinto, Parizot, astro-ph/0703633 PS638 Tom Gaisser

  13. Model dependence of composition in galactic-extragalactic transition • Model extragalactic component • Subtract from observed • to get galactic component Allard, Olinto, Parizot, astro-ph/0703633 proton model mixed model PS638 Tom Gaisser

  14. 30 Heavies at end of galactic Extra-galactic protons Berezhko & Völk • Model galactic component • Subtract from observed • to get extragalactic Transition predicted: 1016.5 to 1017.5 eV arXiv:0704.1715v1 [astro-ph] PS638 Tom Gaisser

  15. Detecting neutrinos • Rate • Convolution of: • Neutrino flux • Absorption in Earth • Neutrino cross section • Range of muon • Size of detector Probability to detect nm-induced muon: PS638 Tom Gaisser

  16. Neutrino effective area • Rate: = ∫fn(En)Aeff(En)dEn • Earth absorption • 10-100 TeV • cos(q) > -0.8 • Main effect near vertical • Higher energy n’s absorbed at larger angles PS638 Tom Gaisser

  17. IceCube acceptance, resolution PS638 Tom Gaisser

  18. Diffuse (unresolved) sources--signature: • hard spectrum • charm background uncertain 1800 / yr 200 30 15 ~ 1 charm < 1 Expected signals in km3 • Possible point sources: • Galactic • SNR 0 - 10 events / yr • m-quasars 0.1 - 5 / burst ~ 100 / yr, steady source • Magnetars ~ 30 events / yr • Extra-galactic • AGN jets 0-100 / yr • GRB precursor (~100 s) • ~ 1000 bursts / yr • ~ 0.2 events / burst • GRB jet after breakout • smaller mean signal / burst • Nearby bursts give larger signal in both cases Thomas K. Gaisser

  19. Limits on excess of n above atmospheric background PS638 Tom Gaisser

  20. Point source search with 7 years of AMANDA 3.8 yrs livetime 26 candidate sources Jim Braun, UW Madison, presented at Cosmo-08 PS638 Tom Gaisser

  21. All flavor limits by AMANDA Cascade(Rolling) Cascade(Trig & Roll) Waxman-Bahcall PRL 78 (1997) 2292 Murase-Nagataki A PRD 73 (2006) 063002 Supranova, Razzaque et al. PRL 90 (2003) 241103 Choked bursts Meszaros-Waxman PRL 87 (2001) 171102 Limits on neutrinos from GRB from AMANDA: -from cascades (ne, nt), Ap.J. 664 (2007) 397 -from neutrino-induced muons, Ap.J (to be published) nm search Search for neutrinos from GRB GRB models PS638 Tom Gaisser

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