Post on 19-Jan-2016
description
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...?