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 11:02:08 EST 2014
Host Name: bat1
Current Working Dir: /local/data/bat1/alien/Swift_3rdBATcatalog/event/batevent_reproc/GRB080702B
======================================================================
Trigger: 00315630 Segment: 003
BAT Trigger Time: 236653843.832
UTC: 2008-07-02T01:10:40.923 [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: 355.576325943458 Dec: -5.49188820465085 [deg; J2000]
{ 23h 42m 18.3s , -5d -29' -30.8" }
+/- 1.8234060085 [arcmin] (estimated 90% radius based on SNR)
SNR: 12.8968798117
Angular difference between the analysis and refined position is Usage: arcmin
Partial Coding Fraction: Unavailable because the burst occurred during slew.
Duration
T90: 15.4120000004768 +/- 3.93351190549334
Measured from: 0.644
to: 16.056 [s; relative to TRIGTIME]
T50: 6.31999999284744 +/- 1.6121340057803
Measured from: 3.036
to: 9.356 [s; relative to TRIGTIME]
====== Table of the duration information =============================
Value tstart tstop
T100 18.292 0.000 18.292
T90 15.412 0.644 16.056
T50 6.320 3.036 9.356
Peak 1.000 1.780 2.780
====== 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 -1.329 -0.190 0.190 - - - 2.89e-03 -3.08e-04 3.07e-04 51.110 57
CPL -1.235 -0.270 0.807 410.609 -410.609 -410.609 3.21e-03 -1.29e-03 4.44e-03 51.080 56
=== 1-s peak 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 -1.066 -0.419 0.447 - - - 5.53e-03 -1.36e-03 1.35e-03 47.600 57
CPL -0.638 0.638 2.298 181.888 -181.888 -181.888 8.60e-03 N/A N/A 47.400 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 5.75e-08 1.17e-07 1.87e-07 6.62e-07 5.19e-07 1.02e-06 erg/cm2
90%_error_low -1.09e-08 -1.37e-08 -2.53e-08 -1.78e-07 -6.19e-08 -1.98e-07 erg/cm2
90%_error_hi 1.15e-08 1.35e-08 2.50e-08 2.19e-07 6.25e-08 2.33e-07 erg/cm2
Peak flux PL 1.50e-01 1.96e-01 1.87e-01 3.18e-01 6.39e-01 8.52e-01 ph/cm2/s
90%_error_low -6.78e-02 -6.04e-02 -5.05e-02 -1.51e-01 -1.60e-01 -2.17e-01 ph/cm2/s
90%_error_hi 8.00e-02 5.83e-02 4.94e-02 2.21e-01 1.62e-01 2.30e-01 ph/cm2/s
Fluence CPL 5.65e-08 1.18e-07 1.88e-07 5.76e-07 5.15e-07 9.39e-07 erg/cm2
90%_error_low -1.35e-08 -1.45e-08 -2.53e-08 -3.69e-07 -6.75e-08 -3.73e-07 erg/cm2
90%_error_hi 1.05e-08 1.61e-08 1.41e-08 2.25e-07 6.48e-08 2.09e-07 erg/cm2
Peak flux CPL 1.35e-01 2.01e-01 1.97e-01 2.10e-01 6.28e-01 7.43e-01 ph/cm2/s
90%_error_low -8.55e-02 -6.45e-02 -5.80e-02 -2.10e-01 -1.67e-01 -2.54e-01 ph/cm2/s
90%_error_hi 9.19e-02 6.62e-02 6.44e-02 1.68e-01 1.66e-01 3.15e-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 355.576 -5.492 0.005 25.174 -7.408 0.042 12.897 UNKNOWN Image time interval: 0.000 to 18.292 [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 18.292 sec. Spectral model in power-law: ------------------------------------------------------------ Parameters : value lower 90% higher 90% Photon index: -1.329 ( -0.190156 0.190456 ) Norm@50keV : 2.88922E-03 ( -0.000307796 0.000307237 ) ------------------------------------------------------------ #Fit statistic : Chi-Squared = 51.11 using 59 PHA bins. # Reduced chi-squared = 0.8967 for 57 degrees of freedom # Null hypothesis probability = 6.944328e-01 Photon flux (15-150 keV) in 18.29 sec: 0.346605 ( -0.037517 0.037601 ) ph/cm2/s Energy fluence (15-150 keV) : 5.18661e-07 ( -6.19471e-08 6.25236e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.000 sec. to 18.292 sec. Spectral model in the cutoff power-law: ------------------------------------------------------------ Parameters : value lower 90% higher 90% Photon index: -1.23487 ( -0.26697 0.810024 ) Epeak [keV] : 410.609 ( -445.518 -445.518 ) Norm@50keV : 3.20760E-03 ( -0.00127681 0.00444919 ) ------------------------------------------------------------ #Fit statistic : Chi-Squared = 51.08 using 59 PHA bins. # Reduced chi-squared = 0.9121 for 56 degrees of freedom # Null hypothesis probability = 6.613478e-01 Photon flux (15-150 keV) in 18.29 sec: 0.345183 ( -0.039274 0.037529 ) ph/cm2/s Energy fluence (15-150 keV) : 5.15482e-07 ( -6.74552e-08 6.48064e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 1.780 sec. to 2.780 sec. Spectral model in power-law: ------------------------------------------------------------ Parameters : value lower 90% higher 90% Photon index: -1.06562 ( -0.41931 0.447311 ) Norm@50keV : 5.53000E-03 ( -0.00135728 0.00135027 ) ------------------------------------------------------------ #Fit statistic : Chi-Squared = 47.60 using 59 PHA bins. # Reduced chi-squared = 0.8351 for 57 degrees of freedom # Null hypothesis probability = 8.079676e-01 Photon flux (15-150 keV) in 1 sec: 0.639476 ( -0.160392 0.1616 ) ph/cm2/s Energy fluence (15-150 keV) : 5.84736e-08 ( -1.53167e-08 1.55159e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 1.780 sec. to 2.780 sec. Spectral model in the cutoff power-law: ------------------------------------------------------------ Parameters : value lower 90% higher 90% Photon index: -0.637974 ( 0.637804 2.29738 ) Epeak [keV] : 181.888 ( -181.845 -181.845 ) Norm@50keV : 8.60267E-03 ( ) ------------------------------------------------------------ #Fit statistic : Chi-Squared = 47.40 using 59 PHA bins. # Reduced chi-squared = 0.8464 for 56 degrees of freedom # Null hypothesis probability = 7.865795e-01 Photon flux (15-150 keV) in 1 sec: 0.628499 ( -0.167147 0.1661 ) ph/cm2/s Energy fluence (15-150 keV) : 5.73258e-08 ( -1.62855e-08 1.60833e-08 ) ergs/cm2
Time-resolved spectra
Distribution
T90 vs. Hardness ratio plot
T90 = 15.412 sec. Hardness ratio (energy fluence ratio) = 1.59220903641
S(15-50 keV) vs. S(50-150 keV) plot
S(15-50 keV) = 1.7481991e-07 S(50-150 keV) = 3.438405e-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
