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
(This burst occurred during telescope slew)
Process Script Ver: batgrbproduct v2.46
Process Start Time: Tue Nov 11 10:27:46 EST 2014
Host Name: bat1
Current Working Dir: /local/data/bat1/alien/Swift_3rdBATcatalog/event/batevent_reproc/GRB081203B
======================================================================
Trigger: 00336489 Segment: 000
BAT Trigger Time: 250005073.6
UTC: 2008-12-03T13:51:10.295 [includes UTCF correction]
Where From?: Ground analysis (best_duration.txt)
NOTE: BAT trigger time for ground-detected burst during slew is the T100 start time.
Refined Position: [ source = BAT mosaic image ]
RA: 228.777643512081 Dec: 44.4213141022708 [deg; J2000]
{ 15h 15m 06.6s , +44d 25' 16.7" }
+/- 2.19924039821 [arcmin] (estimated 90% radius based on SNR)
SNR: 9.86766032176
Angular difference between the analysis and refined position is Usage: arcmin
Partial Coding Fraction: Unavailable because the burst occurred during slew.
Duration
T90: 161.600000023842 +/- 1.6
Measured from: 8
to: 169.6 [s; relative to TRIGTIME]
T50: 88.0000000298023 +/- 1.6
Measured from: 41.6
to: 129.6 [s; relative to TRIGTIME]
====== Table of the duration information =============================
Value tstart tstop
T100 177.600 0.000 177.600
T90 161.600 8.000 169.600
T50 88.000 41.600 129.600
Peak 1.000 32.300 33.300
====== 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: PL)
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 -1.690 -0.139 0.136 - - - 2.65e-03 -1.91e-04 1.89e-04 51.690 57
CPL -1.687 -0.142 0.135 9999.360 -9999.350 -9999.360 2.66e-03 -2.30e-03 -1.24e-03 51.730 56
=== 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 4.58e-07 7.50e-07 9.30e-07 2.28e-06 2.78e-06 4.42e-06 erg/cm2
90%_error_low -5.72e-08 -5.45e-08 -9.18e-08 -4.63e-07 -2.10e-07 -5.33e-07 erg/cm2
90%_error_hi 5.96e-08 5.42e-08 9.07e-08 5.37e-07 2.11e-07 5.89e-07 erg/cm2
Peak flux PL N/A N/A N/A N/A N/A N/A ph/cm2/s
Image
Note1: The mosaic image is made with timebin = 0.50 s; energybin = 15-350 keV
Note2: The mosaic image uses Galactic coordinate.
#RAcent DECcent POSerr Theta Phi Peak_Cts SNR Name 228.778 44.421 0.007 29.955 16.462 0.011 9.868 UNKNOWN Image time interval: 0.000 to 177.600 [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
Time interval is from 64.400 sec. to 177.600 sec. Spectral model in power-law: ------------------------------------------------------------ Parameters : value lower 90% higher 90% Photon index: -1.69001 ( -0.138514 0.136295 ) Norm@50keV : 2.65222E-03 ( -0.000190555 0.000188928 ) ------------------------------------------------------------ #Fit statistic : Chi-Squared = 51.69 using 59 PHA bins. # Reduced chi-squared = 0.9068 for 57 degrees of freedom # Null hypothesis probability = 6.739070e-01 Photon flux (15-150 keV) in 113.2 sec: 0.351039 ( -0.025563 0.025705 ) ph/cm2/s Energy fluence (15-150 keV) : 2.78244e-06 ( -2.0988e-07 2.10966e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from 64.400 sec. to 177.600 sec. Spectral model in the cutoff power-law: ------------------------------------------------------------ Parameters : value lower 90% higher 90% Photon index: -2.70974 ( -0.141444 0.1349 ) Epeak [keV] : 234.869 ( -9999.35 -9999.36 ) Norm@50keV : 8.41988E-04 ( -0.000484526 0.000582559 ) ------------------------------------------------------------ #Fit statistic : Chi-Squared = 43.75 using 59 PHA bins. # Reduced chi-squared = 0.7813 for 56 degrees of freedom # Null hypothesis probability = 8.829536e-01 Photon flux (15-150 keV) in 113.2 sec: 0.351058 ( -0.025628 0.025655 ) ph/cm2/s Energy fluence (15-150 keV) : 1.84386e-06 ( -3.19959e-07 2.84998e-07 ) ergs/cm2
1-s peak spectrum fit
1-s peak spectrum unavailable, likely because there are no event data in the 1-s peak range.
Time-resolved spectra
Distribution
T90 vs. Hardness ratio plot
T90 = 161.6 sec. Hardness ratio (energy fluence ratio) = 1.2397098395
S(15-50 keV) vs. S(50-150 keV) plot
S(15-50 keV) = 1.2084127e-06 S(50-150 keV) = 1.5740198e-06
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
Mask shadow pattern unavailable because this burst occurs during telescope slews.Spacecraft aspect plot
