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Current GRB Search Results & Future Prospects: Extending the Transient Point-Source Search

Current GRB Search Results & Future Prospects: Extending the Transient Point-Source Search. Kyler Kuehn, UC-Irvine http://www.ps.uci.edu/~kuehn IceCube Collaboration Meeting Berkeley, CA March 19-23, 2005. AMANDA. ν. IceCube. CGRO. IPN Satellites (HETE, Swift, etc.). γ, ν.

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Current GRB Search Results & Future Prospects: Extending the Transient Point-Source Search

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  1. Current GRB Search Results & Future Prospects: Extending the Transient Point-Source Search Kyler Kuehn, UC-Irvine http://www.ps.uci.edu/~kuehn IceCube Collaboration Meeting Berkeley, CA March 19-23, 2005

  2. AMANDA ν IceCube CGRO IPN Satellites (HETE, Swift, etc.) γ, ν GRB timing/localization information from correlations among satellites A Distant GRB

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

  4. Model Neutrino Spectra Waxman, E., Nuc. Phys. B 118 (2003) Razzaque et al., PRD 68 083001 (2003) Razzaque et al., PRL 90 241103 (2003) (100% efficiency) no ν oscillation Waxman-Bahcall Supranova log10(Eν2Φν/ GeV cm-2 s-1 sr-1) Precursor log10(Eν/GeV)

  5. GRB 030329 Closest GRB observed: z ~ 0.17 Bright: 10-4 erg/cm2 (30-400 keV) Peak flux: 7 x 10-6 erg cm-2 s-1 TeV-PeV νμ’s expected from • burst: 1.8 events/km2 • afterglow: 0.03 events/km2 • supranova: 12.4 events/km2 • precursor: 4.1 events/km2 [Razzaque et al., PRD 69 023001 (2004)] This research has made use of data obtained from the HETE science team via the website http://space.mit.edu/HETE/Bursts/Data. HETE is an international mission of the NASA Explorer program, run by the Massachusetts Institute of Technology.

  6. Cut Selection Cuts to separate signal from background based on: • event time: (t0 - 110 s) to (t0 – 10 s) for precursor search (t0 - 10 s) to (t0 + duration + 1 s) for coincident search • reconstructed track direction relative to burst position • uniformity of hits along reconstructed track • event-wise angular resolution of reconstructed track Minimize Model Rejection Factor* (W-B, precursor): MRF = Event Upper Limit (= FC†[90%]) . Expected Signal (from MC simulations) • Hill, G., and K. Rawlins, Astropart. Phys.19 (2003) 393-402 † Feldman, G., and R. Cousins, PRD 57 (7) 3873

  7. Previous Observations 1997-2000 flux limit at Earth for 312 BATSE triggered bursts: Eν2Φν < 4x10-8 GeV cm-2 s-1 sr-1 for Waxman-Bahcall-type spectrum with Ebreak=100 TeV, Γ = 300 BT = BATSE Triggered BNT = BATSE Non-Triggered IPN = InterPlanetary Network

  8. Preliminary Resultsof Current Analysis *Relative to W-B model, modified for ν oscillation

  9. Green’s Function Fluence Limitfollowing Super-Kamiokande method (2002ApJ, 578:317F) Super-Kamiokande (1996-2000: 1454 bursts) AMANDA-II (2000-2003: Sensitivity) (2000-2003: 139 bursts) SuperKamiokande (1454) BT only (44) BT+IPN (88) All (114)

  10. Sensitivity of Current Analysis Coincident Sensitivity at Earth: N = 3x10-8GeVcm-2 s-1 sr-1 N = 3x10-8GeVcm-2 s-1 sr-1 9x10-9GeVcm-2 s-1 sr-1 For 139 bursts w/ Broken Power-Law Spectrum (Ebreak = 100 TeV/300 TeV) Precursor Sensitivity at Earth: N = 5x10-8GeVcm-2 s-1 sr-1 1x10-9GeV cm-2 s-1 sr-1 For 50 bursts w/ Broken E-2 Spectrum (Ebreak = 25 TeV) W-B, Supranova, Precursor with ν osc.

  11. Wrapping Up... • Preliminary Analysis of BATSE+IPN Bursts Complete • 0 events observed • Waxman-Bahcall broken power-law flux limit • Razzaque et al. precursor, supranova flux limit • Green’s Function fluence limit: pick your favorite spectrum! • To Do... • Additional bursts with large localization errors • Based on annular-localized burst analysis • Stability, cut selection underway • IPN bursts—localizations from K. Hurley delayed • Final determination of systematic errors, limits • 1997-2003 combined limit?

  12. So...where’s the GRB Paper? Draft v.0 is right here.

  13. Extending the Transient Point-Source Search I: “Failed” GRBs • GRB/SN: 980425/1998bw, 030329/2003dh, 020903 (also, XRF020903—see astro-ph/0502553) • “Failed” GRB: no γ signal (perhaps afterglow) • Up to 100x observed GRB rate • Uncorrelated searches: rolling time-window, diffuse • PRD 68 (8) 2003, PRL 87 (17) 2001, astro-ph/0206392 • Correlated search: (some fraction of) SNe Ib/c are correlated with GRBs, so use SNe spatial/temporal information to isolate potential GRB ν signals

  14. Extending the Transient Point-Source Search I: Jet-Driven SuperNovae • Mildly relativistic jet (Γ~2-6) can produce TeV ν’s: • SNa at 3 Mpc (0.1/yr) may produce ~300 events in IceCube • SNa at 20 Mpc (several/yr) may produce “several” ν • 3%-25% of SNe may be jet-driven • astro-ph/0502521, 0407064, 0403421, 0402163, 0307228, 0303621 • CBAT catalogue (1997-2004): ~1400 SN, 119 SNIb/c • GRB-like supernovae are promising candidates!

  15. Extending the Transient Point-Source Search II: SGR 1806-20 • From Halzen, et al., astro-ph/0503348: • Non-thermal emission frommagnetar (B>1014 G) “starquake” • Sufficient baryon load for ν production (γ~ν, coincident) • With angle cut, BG: ~10-3, Signal: 0.1 – a few (s-1) • However, predictions of O(100 s.) delay in ν signal: • Zhang et al., astro-ph/0210382 • Heyl & Hernquist, astro-ph/0312608 • Thompson & Duncan, ApJ 473:322, MNRAS 275:255 • Post-Flare and Coincident search both needed!

  16. Extending the Transient Point-Source Search II: SGR 1806-20 • Relevant data (±1 hr) downloaded from Madison: • ab_2004_361_9047_014... (21:30 UTC, 27 December 2004) • Δt and detector stability tests... • 2 Hz BG rate * 380 s. (KONUS-Wind) folded into: • Ψ = 12° cut  1.3 BG • Ψ = 6° cut  0.34 BG • Additional BG rejection needed: other GRB cuts...?

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