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: Sun Mar 22 22:31:47 EDT 2015
Host Name: bat1
Current Working Dir: /local/data/bat1/alien/Swift_3rdBATcatalog/event/batevent_reproc/GRB131001A
======================================================================
Trigger: 00082217 Segment: 006
BAT Trigger Time: 402298654.0
UTC: 2013-10-01T05:37:22.903 [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: 8.29800465311854 Dec: 25.5556455978071 [deg; J2000]
{ 00h 33m 11.5s , +25d 33' 20.3" }
+/- 1.38048375868 [arcmin] (estimated 90% radius based on SNR)
SNR: 19.1924527976
Angular difference between the analysis and refined position is Usage: arcmin
Partial Coding Fraction: Unavailable because the burst occurred during slew.
Duration
T90: 5. +/- 1.
Measured from: 0
to: 5 [s; relative to TRIGTIME]
T50: 2. +/- 1.
Measured from: 1
to: 3 [s; relative to TRIGTIME]
====== Table of the duration information =============================
Value tstart tstop
T100 6.000 0.000 6.000
T90 5.000 0.000 5.000
T50 2.000 1.000 3.000
Peak 1.000 1.000 2.000
====== 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: CPL)
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 -1.850 -0.123 0.120 - - - 1.01e-02 -7.86e-04 7.77e-04 70.220 57
CPL -0.906 -0.558 0.638 52.456 -7.592 15.263 3.28e-02 -1.62e-02 3.94e-02 61.220 56
=== 1-s peak spectral analysis ===
(Best model with acceptable fit: CPL)
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 -1.546 -0.160 0.157 - - - 2.06e-02 -2.16e-03 2.14e-03 78.380 57
CPL 0.147 -0.858 1.058 61.981 -8.500 16.914 1.52e-01 -9.55e-02 3.58e-01 65.020 56
=== 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 1.07e-07 1.60e-07 1.77e-07 3.71e-07 5.57e-07 8.15e-07 erg/cm2
90%_error_low -1.10e-08 -1.09e-08 -1.85e-08 -7.29e-08 -4.33e-08 -9.26e-08 erg/cm2
90%_error_hi 1.13e-08 1.09e-08 1.86e-08 8.37e-08 4.37e-08 1.01e-07 erg/cm2
Peak flux PL 8.86e-01 8.68e-01 5.95e-01 6.41e-01 2.61e+00 2.99e+00 ph/cm2/s
90%_error_low -1.36e-01 -9.03e-02 -7.67e-02 -1.48e-01 -2.63e-01 -3.04e-01 ph/cm2/s
90%_error_hi 1.42e-01 9.00e-02 7.63e-02 1.70e-01 2.64e-01 3.05e-01 ph/cm2/s
Fluence CPL 9.54e-08 1.77e-07 1.78e-07 1.03e-07 5.16e-07 5.53e-07 erg/cm2
90%_error_low -1.32e-08 -1.47e-08 -2.14e-08 -5.03e-08 -4.72e-08 -6.92e-08 erg/cm2
90%_error_hi 1.33e-08 1.51e-08 2.10e-08 1.03e-07 4.86e-08 1.10e-07 erg/cm2
Peak flux CPL 6.65e-01 1.01e+00 6.67e-01 1.57e-01 2.48e+00 2.50e+00 ph/cm2/s
90%_error_low -1.70e-01 -1.18e-01 -9.54e-02 -8.09e-02 -2.73e-01 -2.87e-01 ph/cm2/s
90%_error_hi 1.76e-01 1.22e-01 9.65e-02 1.43e-01 2.73e-01 2.97e-01 ph/cm2/s
======================================================================
Image
Note1: The mosaic image is made with timebin = 0.05 s; energybin = 15-350 keV
Note2: The mosaic image uses Galactic coordinate.
#RAcent DECcent POSerr Theta Phi Peak_Cts SNR Name 8.298 25.556 0.003 41.679 27.769 0.128 19.192 UNKNOWN Image time interval: 0.000 to 6.000 [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 0.000 sec. to 6.000 sec. Spectral model in power-law: ------------------------------------------------------------ Parameters : value lower 90% higher 90% Photon index: -1.84986 ( -0.123439 0.120215 ) Norm@50keV : 1.00890E-02 ( -0.000785817 0.000777339 ) ------------------------------------------------------------ #Fit statistic : Chi-Squared = 70.22 using 59 PHA bins. # Reduced chi-squared = 1.232 for 57 degrees of freedom # Null hypothesis probability = 1.121428e-01 Photon flux (15-150 keV) in 6 sec: 1.41811 ( -0.09845 0.09854 ) ph/cm2/s Energy fluence (15-150 keV) : 5.56687e-07 ( -4.32926e-08 4.37274e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.000 sec. to 6.000 sec. Spectral model in the cutoff power-law: ------------------------------------------------------------ Parameters : value lower 90% higher 90% Photon index: -0.906274 ( -0.558105 0.637727 ) Epeak [keV] : 52.4560 ( -7.59228 15.2635 ) Norm@50keV : 3.28081E-02 ( -0.0162399 0.0393633 ) ------------------------------------------------------------ #Fit statistic : Chi-Squared = 61.22 using 59 PHA bins. # Reduced chi-squared = 1.093 for 56 degrees of freedom # Null hypothesis probability = 2.940555e-01 Photon flux (15-150 keV) in 6 sec: 1.36237 ( -0.10351 0.10354 ) ph/cm2/s Energy fluence (15-150 keV) : 5.16263e-07 ( -4.72327e-08 4.86492e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 1.000 sec. to 2.000 sec. Spectral model in power-law: ------------------------------------------------------------ Parameters : value lower 90% higher 90% Photon index: -1.5455 ( -0.160389 0.156945 ) Norm@50keV : 2.06085E-02 ( -0.00215557 0.00214293 ) ------------------------------------------------------------ #Fit statistic : Chi-Squared = 78.38 using 59 PHA bins. # Reduced chi-squared = 1.375 for 57 degrees of freedom # Null hypothesis probability = 3.170541e-02 Photon flux (15-150 keV) in 1 sec: 2.60562 ( -0.26338 0.26358 ) ph/cm2/s Energy fluence (15-150 keV) : 1.94156e-07 ( -2.18144e-08 2.20013e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 1.000 sec. to 2.000 sec. Spectral model in the cutoff power-law: ------------------------------------------------------------ Parameters : value lower 90% higher 90% Photon index: 0.147475 ( -0.857899 1.05794 ) Epeak [keV] : 61.9806 ( -8.49951 16.915 ) Norm@50keV : 0.152028 ( -0.0955367 0.357968 ) ------------------------------------------------------------ #Fit statistic : Chi-Squared = 65.02 using 59 PHA bins. # Reduced chi-squared = 1.161 for 56 degrees of freedom # Null hypothesis probability = 1.915238e-01 Photon flux (15-150 keV) in 1 sec: 2.47524 ( -0.273 0.27252 ) ph/cm2/s Energy fluence (15-150 keV) : 1.76986e-07 ( -2.2311e-08 2.32167e-08 ) ergs/cm2
Time-resolved spectra
Distribution
T90 vs. Hardness ratio plot
T90 = 5.0 sec. Hardness ratio (energy fluence ratio) = 1.00713997623
S(15-50 keV) vs. S(50-150 keV) plot
S(15-50 keV) = 2.7215794e-07 S(50-150 keV) = 2.4410954e-07
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
