Multi-Messenger Astronomy with GLAST and IceCube Kyler Kuehn, UC-Irvine UCLA GLAST Workshop May 22, 2007

A New Astronomical Messenger Neutrinos open a new window onto astrophysical processes in ways which no other particle can DM GRBsAGNsTDs

South Pole AMANDA-II: 19 Strings, 677 Optical Modules Signal: ν µ + N  μ + X (also, EM cascades) Trigger rate: ~70 Hz (mostly downgoing muons) Angular resolution: δθ ~ 3° (likelihood reconstruction) No. Hem. “pointing” (constant full sky FoV) South Pole

A Distant GRB CGRO IceCube AMANDA γ, ν ν IPN Satellites (Swift, GLAST, etc.) GRB timing/localization information from correlations among satellites: >10 6 BG Rejection for AMANDA

GRB Model Neutrino Spectra Waxman, E., Nuc. Phys. B 118 (2003) Razzaque et al., PRD (2003) Razzaque et al., PRL (2003) (100% efficiency) Murase & Nagataki PRD (2006)

Observations Combined Event Upper Limit: 1.10 (Also Observed 0 Events from 153 Additional Non-Triggered BATSE Bursts) YearN Bursts N BG N Obs Total

Flux Upper Limits & MRFs MRF(Waxman & Bahcall) = 1.3 Assuming N obs = 0, this canonical flux prediction could be eliminated with a few more years of data. MRF(Murase & Nagataki) = 0.79 Observations eliminate predictions of Parameter Set A at 90% CL. Parameter Set B still unconstrained. MRF(Razzaque et al.) = 0.46 Observations eliminate most optimistic assumptions: 100% SN/GRB correlation “Fine tuned” T(SN) relative to T(GRB)  observations already constrain these parameters. Preliminary! MRF ≡ Event Upper Limit/Expected Signal (Excluded if MRF<1.0)

Status of the GRB Search AMANDA has been searching for high-energy ν’s in spatial and temporal correlation with GRBs since 1997 After application of data selection criteria, AMANDA had the largest collecting area of any neutrino detector Null result from 7 years of observations places stringent limits on (average) ν emission from GRBs & precursors See also arXiv:astro-ph/ (Achterberg et al., ApJ, submitted) Ongoing observations with IceCube…

IceCube Today 9 strings for 2006 (IC-9) –137.4 live days 13 more for 2007 (IC-22) –Physics analyses underway –numerous contributions to 2007 International Cosmic Ray Conference (ICRC) AMANDA/IC common trigger in 2007

Cumulative km 3 ·yr of IceCube exposure volume shown, not including AMANDA (still operational) 1 km 3 ·yr reached 2 years before detector is completed Close to 4 km 3 ·yr at the beginning of 2 nd year of full array operation. IceCube Tomorrow

Outlook: IceCube and GLAST Assuming GLAST observes 200 GRBs/yr: –GBM localizations sufficient (even without Swift) –Improved localizations compared to IPN: significant fraction of IPN bursts were only localized to annuli –Current flux upper limits matched in < 3 years with AMANDA-sized detector –Current flux upper limits matched in one year with a full- sized (~80 string) IceCube –W-B sensitivity (4.5 x GeV cm -2 s -1 sr -1 ) reached with current AMANDA + partial IceCube observations –Multiwavelength observations allow burst-specific N predictions (10 2 variation for, e.g., GRB compared to an “average” burst)

Outlook: IceCube and GLAST Possible Outcomes –Confirm fireball scenario, detection becomes ongoing observation of GRB neutrinos –Constrain available parameter space with null result… –Refute fireball scenario, test alternate hypotheses, e.g. “external” shock model (Dermer) or Poynting flux-driven mechanism (Lyutikov & Blandford) Other (transient) sources –Orphan afterglows? –AGN –jet-driven SNe, SGR Giant flares –?