Prompt Emission Properties of Swift GRBs
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1 Prompt Emission Properties of GRBs T. Sakamoto (Aoyama Gakuin University)
2 Outline Collaboration with KW team BAT 3 rd GRB catalog Duration and hardness Global properties of BAT GRBs Pre-/Post-GRB emission (survey data)
3 Collaboration with Konus-Wind Spectral cross-calibration work NASA/GSFC) Me (BAT) Masa (WAM) Kazu (WAM) Val (KW) Spectral Cross-Calibration of the Konus-Wind, the Suzaku/WAM, and the /BAT Data Using Gamma-Ray Bursts, T. Sakamoto, V. Pal shin, K. Yamaoka, M. Ohno et al., PASJ, 63, 215 (2011)
4 BAT 3 rd GRB Catalog Lien, Sakamoto et al. in prep.
5 BAT 3 rd GRB Catalog Lien et al. in prep. 833 GRBs (from GRB to GRB A), 778 GRBs are presented here (BAT2 cat: 476 GRBs) 331 known-z GRBs BAT survey data are also analyzed to search for pre/post GRB emission 778 GRBs 717 Long-duration GRBs (L-GRBs) 61 Short-duration GRBs (S-GRBs) (13 short GRBs with E.E.) (92%) (8%) Working definition of L-GRB vs. S-GRB: L-GRB: T 90 2 s S-GRB: T 90 < 2 s
6 Duration BAT T 90 distribution ( kev) L-GRB: ~80 s S-GRBs: > ~0.01 s
7 Number of GRBs Comparison of T 90 distribution T90 [s]
8 Short on S-GRBs in BAT BAT: 10% S-GRBs (90% L-GRBs) BATSE: 25% S-GRBs (75% L-GRBs) Preliminary (Sakamoto et al. Annapolis) Factor of 2.5 small # on S-GRBs in BAT BATSE - Rate trigger vs. BAT - Rate trigger - Imaging BATSE complete spectral catalog (Goldstein, Preece & Mallozzi) 306 BATSE short GRBs 36 BAT short GRBs BATSE short GRBs Band spectral parameters BAT energy response (30 d ) + background Simulate BAT fg/bg spectrum SNR Majority of the BATSE short GRBs is too faint in BAT
9 BAT partial coding fraction between L-GRBs and S-GRBs
10 Fluence ratio (Hardness) vs. T 90
11 BATSE Hardness of S-GRBs HR32= Fermi GBM (Paciesas et al. 2012) (Sakamoto et al. 2006) (*) E peak = (2+alpha)*E 0 HR > 4 requires low-energy photon index to be extremely flat or positive Clear anti-correlation between hardness and T 90
12 PL: Photon index distribution <BAT Photon index> ~ -1.6 Estimated E peak : ~85 kev (Sakamoto et al. 2009)
13 S( kev) [erg cm -2 ] S( kev) vs. S(15-50 kev) E peak = 100 kev E peak = 30 kev Long GRB Short GRB S(15-50 kev) [erg cm -2 ]
14 S( kev) [erg cm -2 ] S( kev) vs. S(15-50 kev) E peak = 100 kev E peak = 30 kev BAT S(15-50 kev) [erg cm -2 ]
15 S( kev) [erg cm -2 ] S( kev) vs. S(15-50 kev) E peak = 100 kev E peak = 30 kev BAT BATSE S(15-50 kev) [erg cm -2 ]
16 S( kev) [erg cm -2 ] S( kev) vs. S(15-50 kev) E peak = 100 kev E peak = 30 kev BAT BATSE Fermi-GBM S(15-50 kev) [erg cm -2 ]
17 S( kev) [erg cm -2 ] S( kev) vs. S(15-50 kev) E peak = 100 kev E peak = 30 kev BAT BATSE Fermi-GBM HETE-2 S(15-50 kev) [erg cm -2 ]
18 E peak Distribution 160 GRBs (750 GRBs in total)
19 BAT Survey data (DPH data) /BAT 70 months Hard X-ray Survey (Baumgartner et al. 2012) >1000 sources detected in this survey Detector Plane Histogram (DHP data; survey data): - 80 energy channel data (counts in each detector) - Every 5 min. - During the pointing observations
20 kev Rate [counts s -1 det -1 ] BAT Survey data on GRB analysis kev Rate [counts s -1 det -1 ] GRB A Event 1 s binning Survey T s Time since the BAT trigger [s] T s Time since the BAT trigger [s]
21 Search for emission in the survey data Processed data: - Latest BAT cleaned sky images from the BAT hard X-ray survey process - Standard 8 energy bands (14-20, 20-24, 24-35, 35-50,5 0-75, , , kev) - Exposure time of the image: a single pointing duration GRBs (GRB GRB B) Search interval: - Between T 0 (BAT) days (4.8 hours) and T 0 (BAT)+1 day - Excluding periods that overlap with the event data - Excluding the period between T 0 (BAT)-50 s and T 0 (BAT)+500 s Energy bands: - Standard 8 energy bands plus kev, kev and kev
22 Detection Search Motivation: - Search for a weak and extended emission before/after the GRB trigger time Detection threshold: as low as possible, but also minimize a false rate Approach to find the detection threshold: 1. Defined the background points around the GRB positions 2. Set the detection threshold (sigma) 3. Run the BAT detection software (batcelldetect) to the images and extract the significance of background points 4. Calculate the detection rate at the given threshold for the background points Detection threshold: 4.3 sigma ( kev image) false positive rate: x 10-5
23 Results - Detection at the pre-trigger time interval: GRB A GRB D : SN associated GRB, duration ~1300 s (Starling et al.) - Detection at the post trigger time for 15 GRBs GRB GRB : SN associated GRB, duration > 1000 s (Campana et al.) GRB B GRB GRB B : Naked-eye burst (Racusin et al.) GRB GRB GRB B : duration > 2300 s (Holland et al.) GRB : SN associated GRB GRB A GRB A : duration ~10,000 s (Levan et al.) GRB A : duration > 25,000 s (Gendre et al.) GRB A GRB A : duration ~6000 s (Levan et al.)
24 Rate [cts s -1 det -1 ] Rate [cts s -1 det -1 ] Rate [cts s -1 det -1 ] Flux [erg cm -2 s -1 ] Flux [erg cm -2 s -1 ] Flux [erg cm -2 s -1 ] Rate [cts s -1 det -1 ] Rate [cts s -1 det -1 ] Rate [cts s -1 det -1 ] Flux [erg cm -2 s -1 ] Flux [erg cm -2 s -1 ] Flux [erg cm -2 s -1 ] BAT detection at the epoch of bright XRT emission B XRT XRT XRT BAT Survey BAT Survey BAT Survey Time since trigger [s] Time since trigger [s] Time since trigger [s] B D XRT XRT XRT BAT Survey BAT Survey BAT Survey Time since trigger [s] Time since trigger [s] Time since trigger [s]
25 Rate [cts s -1 det -1 ] Rate [cts s -1 det -1 ] Flux [erg cm -2 s -1 ] Flux [erg cm -2 s -1 ] Rate [cts s -1 det -1 ] Rate [cts s -1 det -1 ] Rate [cts s -1 det -1 ] Flux [erg cm -2 s -1 ] Flux [erg cm -2 s -1 ] Flux [erg cm -2 s -1 ] BAT detection at the epoch of bright XRT emission A A A XRT XRT XRT BAT Survey BAT Survey BAT Survey Time since trigger [s] Time since trigger [s] Time since trigger [s] A A XRT XRT BAT Survey BAT Survey Time since trigger [s] Time since trigger [s]
26 Rate [cts s -1 det -1 ] Rate [cts s -1 det -1 ] Flux [erg cm -2 s -1 ] Flux [erg cm -2 s -1 ] Rate [cts s -1 det -1 ] Rate [cts s -1 det -1 ] Rate [cts s -1 det -1 ] Flux [erg cm -2 s -1 ] Flux [erg cm -2 s -1 ] Flux [erg cm -2 s -1 ]? B XRT XRT XRT BAT Survey BAT Survey BAT Survey Time since trigger [s] Time since trigger [s] Time since trigger [s] A XRT XRT BAT Survey BAT Survey Time since trigger [s] Time since trigger [s]
27 Prior GRB Emission - Only two GRBs (GRB A & GRB D) have the detection prior to the trigger time. Most of GRBs do not have a bright emission prior to the trigger time. Yamazaki 2009: By moving T 0 backward for 1-3 hrs, a temporal decay slope at a plateau phase in X- ray afterglow can go steeper (matches to a normal decay slope). Future: Look the survey data in finer time binning, and/or wait for higher sensitivity instrument.
28 Duration [s] B Post GRB Emission B B D A A A A A T 90 based on event data Duration including survey detection
29 Summary Great collaboration with KW team enable us to present our scientific results in high confidence. BAT 3 rd GRB catalog Short on short GRBs: Difficulty in localizing Spectral hardness in short GRBs: Mysterious hardness in BATSE and Fermi-GBM short GRBs. Global BAT GRB population: E peak of kev Pre-/Post-GRB emission search: only 1 pre-grb emission and 15 post-grb emissions (very few)
30 Backup slides
31 Fraction of BAT Deadtime
32 Number of Active Detectors
33 Crab Spectral Calibration: Photon Index
34 Crab Spectral Calibration: Flux
35 Background SNR in the survey images
36 BAT XRFs ~ 3% of /BAT GRBs are XRFs (definition of Sakamoto et al. 2008) GRB140103A GRB131120A GRB130608A GRB121212A GRB120816A GRB120724A GRB120403B GRB111229A GRB111129A GRB100425A GRB090417A GRB GRB GRB GRB080218B GRB070714A GRB GRB060923B GRB060428B GRB GRB GRB GRB050416A
37 121027A zoom
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