# Presentation: 639980

## 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

- <date/time>

**CGRO**

**IceCube**

**AMANDA**

**γ, ν**

**ν**

- IPN Satellites
- (HETE, Swift, etc.)

- GRB timing/localization information
- from correlations among satellites

## Observation Procedure

_**Observation Procedure**_

** **Background region is approximately ±60 minutes 	surrounding each GRB (determined by BATSE/IPN)
-  Omit ±5 minutes surrounding GRB trigger time

**Notes:**
I use the hour of data before a BATSE-detected GRB and the hour after to characterize the background in the region of the sky.  This is a very similar technique to traditional photon astronomy.  I then look for an excess on-time, on-source, I.e., where and when the GRB occurred.

## 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****(E****ν****2****Φ****ν****/ GeV cm****-2**** s****-1**** sr****-1****)**

**log****10****(E****ν****/GeV)**

**Supranova**

**Precursor**

**Waxman-Bahcall**

## 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

- 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/km****2**
- 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 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

## Previous Observations

- 1997-2000 flux limit at Earth for 312 BATSE triggered bursts:
**E****ν****2****Φ****ν**** < 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 Resultsof 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 Limitfollowing 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 Analysis

_**Sensitivity of Current Analysis**_

- Coincident 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.](file:///../Desktop/GRBpaper.pdf)_

## 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...?