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

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

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/

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

April 23, 2009PS638 Tom Gaisser 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/ v2 Jet breakout in GRB following collapse of massive progenitor star

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

April 23, 2009PS638 Tom Gaisser 7

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: to used Factor 10 / decade Spectral slope  =2.3 for rel. shock =2.0 non-rel. E min ~ m p (  shock ) 2

April 23, 2009PS638 Tom Gaisser 9 Power needed for extragalactic cosmic rays assuming transition at 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 erg/Mpc 3 /s –Estimates depend on cosmology and extragalactic magnetic fields: –3 x galaxies/Mpc 3 5 x erg/s/Galaxy –3 x clusters/Mpc 3 4 x erg/s/Galaxy Cluster –10 -7 AGN/Mpc erg/s/AGN –~1000 GRB/yr 3 x erg/GRB Assume E -2 spectrum. Then signal ~ 10 to 100/km 2 yr –~20% have E  >50 TeV (greater than atmospheric background)

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

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

April 23, 2009PS638 Tom Gaisser 12 Allard, Olinto, Parizot, astro-ph/ 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 eV 3 X eV

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

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

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:

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

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

Review of Particle Astrophysics Iowa State University, March 3, 2003 Thomas K. Gaisser 18 Expected signals in km 3 Possible point sources: –Galactic SNR events / yr  -quasars / burst ~ 100 / yr, steady source Magnetars ~ 30 events / yr –Extra-galactic AGN jets / 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 < 1 ~ 1 charm Diffuse (unresolved) sources--signature: hard spectrum charm background uncertain

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

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

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) Supranova, Razzaque et al. PRL 90 (2003) Choked bursts Meszaros-Waxman PRL 87 (2001) Limits on neutrinos from GRB from AMANDA: -from cascades ( e,  ), Ap.J. 664 (2007) 397 -from neutrino-induced muons, Ap.J (to be published)