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 09:09:37 EST 2014
Host Name: bat1
Current Working Dir: /local/data/bat1/alien/Swift_3rdBATcatalog/event/batevent_reproc/GRB090306B
======================================================================
Trigger: 00031369 Segment: 001
BAT Trigger Time: 258073644.0
UTC: 2009-03-06T23:07:19.447 [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: 231.205735469434 Dec: -6.96613028439822 [deg; J2000]
{ 15h 24m 49.4s , -6d -57' -58.1" }
+/- 0.557460176597 [arcmin] (estimated 90% radius based on SNR)
SNR: 70.1014245266
Angular difference between the analysis and refined position is Usage: arcmin
Partial Coding Fraction: Unavailable because the burst occurred during slew.
Duration
T90: 21. +/- 1.
Measured from: 1
to: 22 [s; relative to TRIGTIME]
T50: 8. +/- 1.
Measured from: 4
to: 12 [s; relative to TRIGTIME]
====== Table of the duration information =============================
Value tstart tstop
T100 26.000 0.000 26.000
T90 21.000 1.000 22.000
T50 8.000 4.000 12.000
Peak 1.000 7.000 8.000
====== 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: 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 -1.400 -0.049 0.049 - - - 1.29e-02 -3.22e-04 3.22e-04 59.670 57
CPL -1.177 -0.192 0.201 203.417 -70.326 730.762 1.63e-02 -2.88e-03 3.68e-03 55.710 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 -1.200 -0.097 0.098 - - - 2.61e-02 -1.46e-03 1.46e-03 45.130 57
CPL -0.584 -0.404 0.446 124.151 -31.154 125.078 5.08e-02 -1.76e-02 3.02e-02 38.020 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 3.90e-07 7.62e-07 1.15e-06 3.80e-06 3.24e-06 6.11e-06 erg/cm2
90%_error_low -2.02e-08 -2.27e-08 -3.53e-08 -2.67e-07 -8.65e-08 -2.84e-07 erg/cm2
90%_error_hi 2.06e-08 2.26e-08 3.52e-08 2.81e-07 8.66e-08 2.96e-07 erg/cm2
Peak flux PL 8.06e-01 9.69e-01 8.44e-01 1.26e+00 3.06e+00 3.88e+00 ph/cm2/s
90%_error_low -8.42e-02 -6.29e-02 -5.58e-02 -1.68e-01 -1.75e-01 -2.32e-01 ph/cm2/s
90%_error_hi 8.73e-02 6.25e-02 5.55e-02 1.83e-01 1.75e-01 2.35e-01 ph/cm2/s
Fluence CPL 3.69e-07 7.71e-07 1.17e-06 2.81e-06 3.19e-06 5.12e-06 erg/cm2
90%_error_low -2.64e-08 -2.42e-08 -3.93e-08 -6.17e-07 -9.82e-08 -6.21e-07 erg/cm2
90%_error_hi 2.69e-08 2.43e-08 3.96e-08 8.28e-07 9.78e-08 8.27e-07 erg/cm2
Peak flux CPL 7.00e-01 1.01e+00 8.96e-01 6.85e-01 2.98e+00 3.29e+00 ph/cm2/s
90%_error_low -1.05e-01 -7.05e-02 -6.63e-02 -2.11e-01 -1.83e-01 -2.87e-01 ph/cm2/s
90%_error_hi 1.08e-01 7.15e-02 6.74e-02 3.24e-01 1.83e-01 3.65e-01 ph/cm2/s
======================================================================
Image
Note1: The mosaic image is made with timebin = 0.10 s; energybin = 15-350 keV
Note2: The mosaic image uses Galactic coordinate.
#RAcent DECcent POSerr Theta Phi Peak_Cts SNR Name 231.206 -6.966 0.001 34.231 -94.818 0.183 70.101 UNKNOWN Image time interval: 0.000 to 26.000 [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 26.000 sec. Spectral model in power-law: ------------------------------------------------------------ Parameters : value lower 90% higher 90% Photon index: -1.40044 ( -0.0486554 0.0486998 ) Norm@50keV : 1.28966E-02 ( -0.000322053 0.000322052 ) ------------------------------------------------------------ #Fit statistic : Chi-Squared = 59.67 using 59 PHA bins. # Reduced chi-squared = 1.047 for 57 degrees of freedom # Null hypothesis probability = 3.787723e-01 Photon flux (15-150 keV) in 26 sec: 1.57075 ( -0.0431 0.04324 ) ph/cm2/s Energy fluence (15-150 keV) : 3.24015e-06 ( -8.64971e-08 8.66284e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.000 sec. to 26.000 sec. Spectral model in the cutoff power-law: ------------------------------------------------------------ Parameters : value lower 90% higher 90% Photon index: -1.17721 ( -0.191873 0.200683 ) Epeak [keV] : 203.417 ( -70.3265 730.762 ) Norm@50keV : 1.62799E-02 ( -0.00288462 0.00367888 ) ------------------------------------------------------------ #Fit statistic : Chi-Squared = 55.71 using 59 PHA bins. # Reduced chi-squared = 0.9949 for 56 degrees of freedom # Null hypothesis probability = 4.857287e-01 Photon flux (15-150 keV) in 26 sec: 1.54392 ( -0.04837 0.04854 ) ph/cm2/s Energy fluence (15-150 keV) : 3.18651e-06 ( -9.82517e-08 9.77959e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 7.000 sec. to 8.000 sec. Spectral model in power-law: ------------------------------------------------------------ Parameters : value lower 90% higher 90% Photon index: -1.20023 ( -0.097275 0.0975217 ) Norm@50keV : 2.60747E-02 ( -0.00145999 0.00145987 ) ------------------------------------------------------------ #Fit statistic : Chi-Squared = 45.13 using 59 PHA bins. # Reduced chi-squared = 0.7918 for 57 degrees of freedom # Null hypothesis probability = 8.720575e-01 Photon flux (15-150 keV) in 1 sec: 3.06075 ( -0.17482 0.17499 ) ph/cm2/s Energy fluence (15-150 keV) : 2.64551e-07 ( -1.66776e-08 1.67751e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 7.000 sec. to 8.000 sec. Spectral model in the cutoff power-law: ------------------------------------------------------------ Parameters : value lower 90% higher 90% Photon index: -0.583931 ( -0.403799 0.445751 ) Epeak [keV] : 124.151 ( -31.1537 125.078 ) Norm@50keV : 5.08128E-02 ( -0.0176178 0.0301888 ) ------------------------------------------------------------ #Fit statistic : Chi-Squared = 38.02 using 59 PHA bins. # Reduced chi-squared = 0.6789 for 56 degrees of freedom # Null hypothesis probability = 9.685808e-01 Photon flux (15-150 keV) in 1 sec: 2.97532 ( -0.18345 0.18334 ) ph/cm2/s Energy fluence (15-150 keV) : 2.54273e-07 ( -1.8285e-08 1.82417e-08 ) ergs/cm2
Time-resolved spectra
Distribution
T90 vs. Hardness ratio plot
T90 = 21.0 sec. Hardness ratio (energy fluence ratio) = 1.51527042248
S(15-50 keV) vs. S(50-150 keV) plot
S(15-50 keV) = 1.1517688e-06 S(50-150 keV) = 2.0883329e-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
