The Search for Muon Neutrinos from Gamma-Ray Bursts with AMANDA B-10 and AMANDA-II Kyler Kuehn, UC-Irvine for the AMANDA Collaboration TAUP 2003 University.

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Presentation transcript:

The Search for Muon Neutrinos from Gamma-Ray Bursts with AMANDA B-10 and AMANDA-II Kyler Kuehn, UC-Irvine for the AMANDA Collaboration TAUP 2003 University of Washington

Science Motivation Cannot see the inner engine of GRBs If protons are accelerated in the GRB environment, neutrinos will be produced: p +    ±   ± +   e ± + e +  Probe inner engine and physics of the explosion Predicted neutrino flux varies depending upon specific model parameters

Fireball Model of GRB Emission Image courtesy of T. Piran (Science v.295, p.986)

2704 Gamma-Ray Bursts (1999ApJ, 512: 362F) Burst location and timing determined by: BATSE 4B Catalog Stern, Kommers GUSBAD IPN3 IPN Circulars Archival search (K. Hurley et al.) Observation Procedure

Observation Procedure (continued) Blinded (10) minute window - (5) minutes + (5) minutes ~110 (120-10) minute background used to set cuts and check for data quality & stability - (~60) minutes + (~60) minutes Background region is approximately ±60 minutes surrounding each GRB Omit ±5 minutes surrounding GRB trigger time

Observation Procedure (continued) N events /10 s Occurrences in 2 hr. window Detector stability evaluated for all bursts 564 GRBs in 4 years ( ) (BATSE#6610) Off-Time

AMANDA-II Effective Area log (E µ /GeV) Quality Cuts – Location/Duration (T 90 ) – Track reconstruction likelihood, smoothness – Number of direct hits – Number of hit channels A eff (100TeV) > 70,000 m 2 A eff (km 2 ) Includes ν Attenuation

GRBs in the Dataset 312 BATSE Triggered Bursts 206 BATSE Non-Triggered Bursts 44 IPN Bursts in 2000 (Excluding BATSE) –19 Bursts from IPN Circulars –14 Additional Well-Localized Bursts –11 Additional Bursts with Annular Localization 2 GUSBAD Bursts in 2000

Summary of Observations YearDetectorN Bursts N BG, Pred N Obs Event U.L. 1997B-1078 (BT) B-1094 (BT) B-1096 (BT) A-II (2 analyses) 44 (BT)0.83/0.400/01.72/ A-II24 (BNT) A-II46 (New) B-10/A-II312 (BT) Flux (at Earth): E 2 Φ ν < 4x10 -8 GeV cm -2 s -1 sr -1 for 312 bursts with Waxman-Bahcall-type spectrum BT = BATSE Triggered BNT = BATSE Non-Triggered New = IPN & GUSBAD

Green’s Function Fluence Limit following SuperKamiokande method (2002ApJ, 578:317F) log 10 (  /cm -2 ) Preliminary! Super-K (BATSE Trig Only) w/ Attenuation A-II, 2000 (BATSE Trig Only) A-II, 2000 (All Bursts) log 10 (E /GeV)

What’s Next? Expanding analysis into 2001 and 2002 – Approximately 40 bursts in IPN Circulars – Total with archival search: ~ Determining burst distance/luminosity  ν flux predictions for each burst Set limits for specific theoretical models Swift will dramatically increase burst detection rate, starting in 2004

S. Desai and D. Turcan for helpful clarifications of the Super-Kamiokande limit-setting method K. Hurley and the IPN3 collaboration for burst localizations which allowed AMANDA-II follow- up observations Acknowledgements