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

A Distant GRB

CGRO

IceCube

AMANDA

γ, ν

ν

IPN Satellites(HETE, Swift, etc.)

GRB timing/localization informationfrom correlations among satellites

Observation ProcedureBlinded 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 (determined by BATSE/IPN)

• Omit ±5 minutes surrounding GRB trigger time

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

log 10

(Eν2 Φ

ν/ G

eV c

m-2 s

-1 s

r-1)

log10(Eν/GeV)

Supranova

Precursor

Waxman-Bahcall

Closest GRB observed: z ~ 0.17Bright: 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

GRB 030329

[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.

Cut SelectionCuts 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

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

Previous Observations

BT = BATSE Triggered BNT = BATSE Non-Triggered IPN = InterPlanetary Network

Year NBursts NBG, Exp NObs Event U.L.

2000 44 (BT) 0.41 0 2.05

2000 26 (BNT) 0.24 0 2.19

2000 44 (IPN) 0.60 0 2.01

2000 88 (BT+IPN) 1.02 0 1.61

2000 114 (All) 1.25 0 1.47

Preliminary Resultsof Current Analysis

*Relative to W-B model, modified for ν oscillation

Year Nbursts

(BT+IPN)

NBG, Exp NObs Event U.L. MRF* MRF* (Sensitivity)

2001

Precursor

15

15

0.06

0.05

0

0

2.38

2.39

64 66

2002

Precursor

17

17

0.08

0.06

0

0

2.36

2.38

54 54

2003

Precursor

19

18

0.10

0.06

0

0

2.34

2.38

52 54

01-03

Precursor

51

50

0.24

0.16

0

0

2.19

2.28

16 20

00-03 139 1.25 0 1.47 5 10

Green’s Function Fluence Limitfollowing Super-Kamiokande method (2002ApJ, 578:317F)

SuperKamiokande (1454)

BT only (44)

BT+IPN (88)

All (114)

Super-Kamiokande

(1996-2000: 1454 bursts)

AMANDA-II

(2000-2003: Sensitivity)

(2000-2003: 139 bursts)

Sensitivity of Current AnalysisCoincident Sensitivity at Earth:

N = 3x10-8 GeV cm-2 s-1 sr-1

N = 3x10-8 GeV cm-2 s-1 sr-1

9x10-9 GeV cm-2 s-1 sr-1

For 139 bursts w/ Broken Power-Law Spectrum (Ebreak = 100 TeV/300 TeV)

Precursor Sensitivity at Earth:

N = 5x10-8 GeV cm-2 s-1 sr-1

1x10-9 GeV cm-2 s-1 sr-1

For 50 bursts w/ Broken E-2 Spectrum (Ebreak = 25 TeV)

W-B, Supranova, Precursor with ν osc.

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?

So...where’s the GRB Paper?

Draft v.0 is right here.

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

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!

Extending the Transient Point-Source Search II: SGR 1806-20

• From Halzen, et al., astro-ph/0503348:• Non-thermal emission from magnetar (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!

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...?