Analysis Summary
Notes:
- 1) No attempt has been made to eliminate the non-significant decimal places.
- 2) This batgrbproduct analysis is done using the HEASARC data.
- 3) This batgrbproduct analysis is using the flight position for the mask-weighting calculation.
==========================================================================
BAT GROUND-DETECTED GRB DATA PROCESSING REPORT
Process Script Ver: batgrbproduct v2.46
Process Start Time: Thu Dec 17 18:08:19 EST 2015
Host Name: bat1
Current Working Dir: /local/data/bat1/alien/Swift_3rdBATcatalog/event/batevent_reproc/trigger361029
======================================================================
Trigger: 00361029 Segment: 000
BAT Trigger Time: 273092788.8
UTC: 2009-08-27T19:06:23.766 [includes UTCF correction]
Where From?: Ground analysis (best_duration.txt)
NOTE: BAT trigger time for ground-detected burst is the T100 start time.
Analysis Position: [ source = GCN ]
RA: 18.442 Dec: -50.902 [deg; J2000]
Refined Position: [ source = BAT pre-slew image ]
RA: 18.4420916897 Dec: -50.9023673069 [deg; J2000]
{ 01h 13m 46.1s , -50d -54' -8.5" }
+/- 2.36842828844 [arcmin] (estimated 90% radius based on SNR)
SNR: 8.87630053438
Angular difference between the analysis and refined position is 0.022310 arcmin
Partial Coding Fraction: 0.03173828 [ including projection effects ]
Duration
T90: 8. +/- 1.6
Measured from: 0
to: 8 [s; relative to TRIGTIME]
T50: 4.80000007152557 +/- 1.6
Measured from: 1.6
to: 6.4 [s; relative to TRIGTIME]
====== Table of the duration information =============================
Value tstart tstop
T100 8.000 0.000 8.000
T90 8.000 0.000 8.000
T50 4.800 1.600 6.400
Peak 1.000 1.900 2.900
====== Spectral Analysis Summary =====================================
Model : spectral model: simple power-law (PL) and cutoff power-law (CPL)
Ph_index : photon index: E^{Ph_index}
Ph_90err : 90% error of the photon index
Epeak : Epeak in keV
Epeak_90err: 90% error of Epeak
Norm : normalization at 50 keV in both the PL model and CPL model
Nomr_90err : 90% error of the normalization
chi2 : Chi-Squared
dof : degree of freedo
=== Time-averaged spectral analysis ===
(Best model with acceptable fit: N/A)
Model Ph_index Ph_90err_low Ph_90err_hi Epeak Epeak_90err_low Epeak_90err_hi Norm Nomr_90err_low Norm_90err_hi chi2 dof
PL N/A N/A N/A - - - N/A N/A N/A N/A N/A
CPL N/A N/A N/A N/A N/A N/A N/A N/A N/A N/A N/A
=== 1-s peak spectral analysis ===
(Best model with acceptable fit: N/A)
Model Ph_index Ph_90err_low Ph_90err_hi Epeak Epeak_90err_low Epeak_90err_hi Norm Nomr_90err_low Norm_90err_hi chi2 dof
PL N/A N/A N/A - - - N/A N/A N/A N/A N/A
CPL N/A N/A N/A N/A N/A N/A N/A N/A N/A N/A N/A
=== Fluence/Peak Flux Summary ===
Model Band1 Band2 Band3 Band4 Band5 Total
15-25 25-50 50-100 100-350 15-150 15-350 keV
Fluence PL N/A N/A N/A N/A N/A N/A erg/cm2
Image
15.0-350.0 keV image (Event data with DETECTION mask)
#RAcent DECcent POSerr Theta Phi Peak_Cts SNR Name 18.442 -50.902 0.022 52.693 31.781 1.758 8.876 TRIG_00361029 Image time interval: 0.576 to 8.250 [sec]
Light Curves
Note: The mask-weighted lightcurves have units of either count/det or counts/sec/det, where a det is 0.4 x 0.4 = 0.16 sq cm.
Best duration plot
Full-time range; 1 s binning
Other quick-look light curves:
- 64 ms binning (zoomed)
- 16 ms binning (zoomed)
- 8 ms binning (zoomed)
- 2 ms binning (zoomed)
- SN=5 or 10 s binning (full-time range)
- Raw light curve
Spectra
- 64 ms binning (zoomed)
- 16 ms binning (zoomed)
- 8 ms binning (zoomed)
- 2 ms binning (zoomed)
- SN=5 or 10 s binning (full-time range)
- Raw light curve
Spectra
Notes:
- 1) The fitting includes the systematic errors.
- 2) When the burst includes telescope slew time periods, the fitting uses an average response file made from multiple 5-s response files through out the slew time plus single time preiod for the non-slew times, and weighted by the total counts in the corresponding time period using addrmf. An average response file is needed becuase a spectral fit using the pre-slew DRM will introduce some errors in both a spectral shape and a normalization if the PHA file contains a lot of the slew/post-slew time interval.
- 3) For fits to more complicated models (e.g. a power-law over a cutoff power-law), the BAT team has decided to require a chi-square improvement of more than 6 for each extra dof.
Time averaged spectrum fit using the average DRM
Power-law model
Multiple GTIs in the spectrum tstart tstop Photon index: ( )
Cutoff power-law model
Multiple GTIs in the spectrum tstart tstop Photon index: ( )
1-s peak spectrum fit
Power-law model
Time interval is from 0.576 sec. to 8.250 sec. Photon index: ( )
Cutoff power-law model
Time interval is from 0.576 sec. to 8.250 sec. Photon index: ( )
Time-resolved spectra
Distribution
T90 vs. Hardness ratio plot
T90 = N/A sec. Hardness ratio (energy fluence ratio) = N/A
S(15-50 keV) vs. S(50-150 keV) plot
S(15-50 keV) = N/A S(50-150 keV) = N/A
The dash-dotted line and the dashed line traces the fluences calculated from the Band function with Epeak = 15 and 150 keV, respectively. Both lines assume a canonical values of alpha = -1 and beta = -2.5.
Mask shadow pattern (with DETECTION mask)
IMX = 1.11560440957, IMY = -0.691194000048
Spacecraft aspect plot
Bright source in the event data image
Event data image of 15-350 keV band
Time interval of the image: 0.576000 8.250000 # RAcent DECcent POSerr Theta Phi PeakCts SNR AngSep Name # [deg] [deg] ['] [deg] [deg] ['] 18.4420 -50.9023 1.3 52.7 31.8 1.7593 8.9 ------ UNKNOWN 21.0232 -10.7637 2.3 20.7 77.3 0.1559 5.0 ------ UNKNOWN 51.4820 -36.4455 1.9 36.8 -0.9 0.2311 6.0 ------ UNKNOWN 72.4495 -5.4314 2.3 33.1 -66.9 0.2097 5.1 ------ UNKNOWN
Webpage updated on: Thu Dec 17 18:11:40 EST 2015