Search for Neutrinos from GRBs with AMANDA and IceCube Alexander Kappes University Wisconsin-Madison For the IceCube Collaboration 6 th International Workshop on New Worlds in Astroparticle Physics 6. 8. September 2007, Faro Portugal Alexander Kappes, UW-MadisonAstro 2007, Faro Portugal, Sept Outline of Talk The AMANDA and IceCube detectors (see talk of D. Bertrand) Gamma-Ray Bursts and models of neutrino production Search for GRBs with neutrino telescopes Latest results from AMANDA IceCube and GRBs Alexander Kappes, UW-MadisonAstro 2007, Faro Portugal, Sept Gamma-Ray Bursts Very intense, short (0.11000 s) g-ray flashes Known since late 1960s (discovered by US Vela nuclear test detection satellite) Major progress in 1990s with BATSE and Beppo Sax (two categories, isotropic distribution, distance measurement) 2 Vela satellites BATSE on CGRO short long Alexander Kappes, UW-MadisonAstro 2007, Faro Portugal, Sept Gamma-Ray Bursts Additional observations: Long GRBs (LGRBs, T > 2 s): Occur mainly in star forming regions Often optical supernova (SN) observed Interpreted as core collapse SNe Short GRBs (SGRBs, T < 2 s): Occur mainly in outer regions of older galaxies By factor ~10 lower luminosity than LGRBs Interpreted as accreting Black Holes in merging binary systems But also GRBs with mixed features observed (e.g., GRB060624) Alexander Kappes, UW-MadisonAstro 2007, Faro Portugal, Sept Development of Long GRBs Progenator star with > 10 M Sun and Fe core ~2 M Sun Formation of black hole after collapse Accretion of envelope material on black hole creates relativistic jet along rotation axis Jet propagates through envelop (O 100 s) Jet emerges from progenitor envelop and produces gamma-ray signal Artist's view of a GRB Collapses to highly magnetized pulsars may also produce jets Emerging jet (Zhang & Woosley) Alexander Kappes, UW-MadisonAstro 2007, Faro Portugal, Sept Models of Neutrino Production in (Long) GRBs Fireball model p + p/g p + X p n m + m m n m + n e + e n oscillations: (n e,n m,n t ) = (1 : 1 : 1) Precursor ~-100 sT0T0 Precursor (Dt~100 s): Jet collides with star envelop TeV neutrinos (Not visible in g-rays) [Meszaros & Waxman, 2001] ~100 s> 1000 s Main burst (Dt~100 s): Internal shocks in jet 100 TeV PeV neutrinos [Waxman & Bahcall, 1997] [Razzaque et al. 2003] [Murase & Nagataki 2006] Afterglow (Dt > 1000 s): Flares PeV neutrinos [Dermer 2001] Collision with interstellar medium EeV neutrinos [Waxman & Bahcall 2000] Alexander Kappes, UW-MadisonAstro 2007, Faro Portugal, Sept Neutrino Flux Predictions main burst afterglow precursor Neutrinos from GRBs (all flavors) failed GRBs Waxman & Bahcall Murase & Nagataki Meszaros & Waxman Razzaque et al Waxman multiplied with E 2 ! flavor ratio at Earth (1 : 1 : 1) successfull GRBs Only average fluxes large burst-to-burst fluctuations ! Purely electromagnetic models (Poynting-flux) no neutrinos (Lyutikov and Blandford 2003) Alexander Kappes, UW-MadisonAstro 2007, Faro Portugal, Sept GRB Detection in Neutrino Telescopes Two basic channels: Muons: track of hits good angular resolution (IceCube ~1 for E n > 1 TeV) Cascades (all flavors): concentric hits no direction information but low atm. background Neutrino effective area rises strongly with energy cross section increases light output increases n m :muon range grows; 14 PeV ! Interesting E range TeV PeV (afterglow flux probably very low) IceCube 80 trigger level (preliminary) muon neutrinos electron neutrinos Alexander Kappes, UW-MadisonAstro 2007, Faro Portugal, Sept Event Rates in Neutrino Telescopes GRB neutrinos in short time window ( ~ 50 s) assuming 670 bursts per year GRB neutrinos during burst ~10 -3 Hz from specific position in sky (1 x 1 search window) atm. muons ~10 -2 Hz, atm. neutrinos ~10 -7 Hz southern hemisphere northern hemisphere Triggered in IceCube with 22 strings: atmospheric muons (500 Hz) atmospheric neutrinos (10 -2 Hz) GRB muon neutrinos (WB, integrated) (10 -6 Hz) very clean signal for northern hemisphere reduced sensitivity for southern hemisphere Alexander Kappes, UW-MadisonAstro 2007, Faro Portugal, Sept Search Strategies GCN triggered searches (cascades, muon): profit from known time (and direction) Untriggered sliding window searches (cascades): large fraction of GRBs not observed by satellites possible large population of choked GRBs not visible in g-rays (jet doesn't emerge from progenitor envelop only precursor neutrinos) sliding window: 1h on-time (T90) precursor noff-time always blind T GRB 10 min time events 3 evts 2 evts 1 evt Alexander Kappes, UW-MadisonAstro 2007, Faro Portugal, Sept Latest Results from AMANDA II Muon channel: Model Years# Bursts Satellite(s)bkg (exp)obs. main burst1997 BATSE+IPN precursor2001 IPN Note: 0.8 events for Waxman-Bahcall GRB (main burst) flux expected A. Achterberg etal, ApJ in press (astro-ph/ ) Cascade channel: Method Years# Bursts Satellite(s)bkg (exp)obs. triggered BATSE rolling20012003 two window sizes: 1 and 100 s number of triplets and doublets compatible with background A. Achterberg etal, ApJ 664:397, 2007 (astro-ph/ ) Alexander Kappes, UW-MadisonAstro 2007, Faro Portugal, Sept All Flavor GRB Limits from AMANDA II Limits from triggered searches assume ~700 bursts per year AMANDA starts to exclude flux models! Cascade search in IceCube much more competitive (factor 70 in instrumented vol.) Eff. volume (cascades) grows faster than eff. area (muon)! Cascade searches (trig + roll) only rolling Muon searches (only trig) Alexander Kappes, UW-MadisonAstro 2007, Faro Portugal, Sept GRB Detection in the IceCube Era GCN: Network of satellite and ground based observatories Satellites send GRB alerts to ground stations for follow up observations Swift currently workhorse (~100 GRBs per year) Burst Alert Monitor: FoV=1.4 sr; E range 15150 keV GLAST (satellite): Launch planned Jan. 2008; science from March '08!? GBM (Burst Alert Monitor): FoV = 9.5 sr; E range: 8 keV25 MeV LAT (Large Area Telescope): FoV = 2.4 sr; E range: 20 MeV300 GeV ! Expected to observe ~200 GRBs per year GCN network GLAST Alexander Kappes, UW-MadisonAstro 2007, Faro Portugal, Sept ANTARES Design Study KM3NeT? Accumulated 100 TeV AMANDA onlyIceCube muon eff. area (km 2 yr) IceCube: Status and Further Construction 2007:22 strings; already 6 times larger than AMANDA 2008:36+ (40) strings; 2011:80 strings (full detector) AMANDA IceCube-22 Alexander Kappes, UW-MadisonAstro 2007, Faro Portugal, Sept IceCube: The GRB Filter Only limited satellite bandwidth for data transfer (~30 GB per day) triggered data has to be filtered (all data written to tape) reduce atm. muons by zenith cut (typical > 70) no sensitivity to GRBs in southern sky Dedicated GRB filter writes out all data 1 h around GCN trigger Trigger Buffer (2 d) GRB Buffer (90 d) GCN GRB South Pole Computer(Iridium, 24/7) 2 h per GRB Online proces- ing planned TDRSS satellite Data Warehouse (North) In operation since June 2007 Alexander Kappes, UW-MadisonAstro 2007, Faro Portugal, Sept Sensitivity of IceCube to GRBs IceCube-80 more than a magnitude more sensitive than AMANDA larger effective area + better angular resolution signal efficiency for AMANDA 2575% 3s sensitivity for Waxman-Bahcall GRB flux with ~100 (~300) detected bursts in muon (cascade) channel (GLAST ~200 bursts per year, 4 p) IceCube is looking both in the northern and the southern sky AMANDA IceCube-22 IceCube-40 IceCube-80 Alexander Kappes, UW-MadisonAstro 2007, Faro Portugal, Sept Optical Follow-up Observations Potentially many choked GRBs (all SNe?) (not visible in X-rays) Increase chance to detect GRB by optical observation of afterglow/SN Look for neutrino doublets within spatial (~3) and time (~100 s) window pointing resolution ~0.5 ~30 evts/yr from background Optical follow-up observations: 80% of IceCube PSF covert by telescope with 2 x 2 FoV many fully automatic telescopes exist worldwide ROTSE III: 4 x 0.45 m FoV: 2 O x 2 O rapid follow-up Others: RoboNet, Stella Preliminary Feasibility currently under study Alexander Kappes, UW-MadisonAstro 2007, Faro Portugal, Sept Summary AMANDA started to exclude GRB neutrino flux models with integrated exposure of 0.1 km 2yr (420 bursts) IceCube's integrated exposure will reach 1(3) km 2yr in 2009 (2011) Full IceCube detector reaches 3 s sensitivity for Waxman-Bahcall GRB flux with ~100 triggered bursts (from 2008 on GLAST + Swift will detect ~200 GRBs per year) IceCube will be able to observe current GRB model neutrino fluxes within a few years There are exciting times ahead! Alexander Kappes, UW-MadisonAstro 2007, Faro Portugal, Sept Cascade searches (trig + roll) only rolling Muon searches (only trig)