1. April 23, 2009PS638 Tom Gaisser 1 Neutrinos from AGN & GRB Expectations for a km 3 detector

2. April 23, 2009PS638 Tom Gaisser 2 Cosmic-ray factories? Artist’s(*) conception of a massive, accreting, compact with accretion disk and relativistic jets * Artist = Todor Stanev

3. April 23, 2009PS638 Tom Gaisser 3 Active Galaxies: Jets VLA image of Cygnus A Radio Galaxy 3C296 (AUI, NRAO). --Jets extend beyond host galaxy. Drawing of AGN core M. Urry, astro-ph/0312545

4. April 23, 2009PS638 Tom Gaisser 4 Spectral Energy Distribution for blazars Figure from Markus Bötcher, Astrophys. Space Sci 309 (2007) 95-104

5. April 23, 2009PS638 Tom Gaisser 5 - 10 seconds fireball protons interact with remnant of the star 0 seconds fireball protons and photons interact afterwards afterglow protons interact with inter- stellar medium TeV PeV EeV Image: W. Zhang & S. Woosley See astro-ph/0308389v2 Jet breakout in GRB following collapse of massive progenitor star

6. April 23, 2009PS638 Tom Gaisser 6 Slide from Alexander Kappes

7. April 23, 2009PS638 Tom Gaisser 7

8. April 23, 2009PS638 Tom Gaisser 8 Energy content of extra-galactic component depends on location of transition Composition signature: transition back to protons Uncertainties: Normalization point: 10 18 to 10 19.5 used Factor 10 / decade Spectral slope  =2.3 for rel. shock =2.0 non-rel. E min ~ m p (  shock ) 2

9. April 23, 2009PS638 Tom Gaisser 9 Power needed for extragalactic cosmic rays assuming transition at 10 19 eV Energy density in UHECR,  CR ~ 2 x 10  erg/cm 3 –Such an estimate requires extrapolation of UHECR to low energy –  CR = (4  /c)  E  (E) dE = (4  /c){E 2  (E)}  E=10 19 eV x ln{E max /E min } –This gives  CR ~ 2 x 10  erg/cm 3 for differential index  = 2,  (E) ~ E -2 Power required ~  CR /10 10 yr ~ 1.3 x 10 37 erg/Mpc 3 /s –Estimates depend on cosmology and extragalactic magnetic fields: –3 x 10 -3 galaxies/Mpc 3 5 x 10 39 erg/s/Galaxy –3 x 10 -6 clusters/Mpc 3 4 x 10 42 erg/s/Galaxy Cluster –10 -7 AGN/Mpc 3 10 44 erg/s/AGN –~1000 GRB/yr 3 x 10 52 erg/GRB Assume E -2 spectrum. Then signal ~ 10 to 100/km 2 yr –~20% have E  >50 TeV (greater than atmospheric background)

10. April 23, 2009PS638 Tom Gaisser 10 GRB model Assume E -2 spectrum at source, normalize @ 10 19.5 10 45 erg/Mpc 3 /yr ~ 10 53 erg/GRB Evolution ~ star-formation rate GZK losses included Galactic  extragalactic transition ~ 10 19 eV Bahcall & Waxman, hep-ph/0206217 Waxman, astro-ph/0210638

11. April 23, 2009PS638 Tom Gaisser 11 Berezinsky et al. AGN Assuming a cosmological distribution of sources with: –dN/dE ~ E -2, E < 10 18 eV –dN/dE ~ E , 10 18 < E < 10 21 –  = 2.7 (no evolution) –  = 2.5 (with evolution) Need L 0 ~ 3 ×10 46 erg/Mpc 3 yr They interpret dip at 10 19 as –p +  2.7   p + e + + e - Berezinsky, Gazizov, Grigorieva astro-ph/0210095

12. April 23, 2009PS638 Tom Gaisser 12 Allard, Olinto, Parizot, astro-ph/0703633 Or start with a model of the extra- galactic component Subtract it from the observed spectrum to get the galactic component What is power needed for extra-galactic CR? 3 x 10 17 eV 3 X 10 18 eV

13. April 23, 2009PS638 Tom Gaisser 13 Model dependence of composition in galactic-extragalactic transition Allard, Olinto, Parizot, astro-ph/0703633 proton model mixed model Model extragalactic component Subtract from observed to get galactic component

14. April 23, 2009PS638 Tom Gaisser 14 Heavies at end of galactic Extra-galactic protons Berezhko & Völk arXiv:0704.1715v1 [astro-ph] Model galactic component Subtract from observed to get extragalactic Transition predicted: 10 16.5 to 10 17.5 eV 30

15. April 23, 2009PS638 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   -induced muon:

16. April 23, 2009PS638 Tom Gaisser 16 Neutrino effective area Rate: = ∫  ( E )A eff ( E ) dE Earth absorption –10-100 TeV cos(  ) > -0.8 Main effect near vertical –Higher energy ’s absorbed at larger angles

17. April 23, 2009PS638 Tom Gaisser 17 IceCube acceptance, resolution

18. Review of Particle Astrophysics Iowa State University, March 3, 2003 Thomas K. Gaisser 18 Expected signals in km 3 Possible point sources: –Galactic SNR 0 - 10 events / yr  -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 1800 / yr 200 30 15 < 1 ~ 1 charm Diffuse (unresolved) sources--signature: hard spectrum charm background uncertain

19. April 23, 2009PS638 Tom Gaisser 19 Limits on excess of  above atmospheric background

20. April 23, 2009PS638 Tom Gaisser 20 Jim Braun, UW Madison, presented at Cosmo-08 Point source search with 7 years of AMANDA 3.8 yrs livetime 26 candidate sources

21. April 23, 2009PS638 Tom Gaisser 21 Search for neutrinos from GRB Cascade (Trig & Roll) Cascade (Rolling)  search All flavor limits by AMANDA GRB models 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 ( e,  ), Ap.J. 664 (2007) 397 -from neutrino-induced muons, Ap.J (to be published)