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: Fri Nov 7 18:57:26 EST 2014
Host Name: bat1
Current Working Dir: /local/data/bat1/alien/Swift_3rdBATcatalog/event/batevent_reproc/GRB140529A
======================================================================
Trigger: 00091901 Segment: 003
BAT Trigger Time: 423048493.169
UTC: 2014-05-29T09:28:01.098 [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: 228.805098433427 Dec: -41.0524965320466 [deg; J2000]
{ 15h 15m 13.2s , -41d -3' -9.0" }
+/- 1.37551948707 [arcmin] (estimated 90% radius based on SNR)
SNR: 19.2914805073
Angular difference between the analysis and refined position is Usage: arcmin
Partial Coding Fraction: Unavailable because the burst occurred during slew.
Duration
T90: 8.14400005340576 +/- 1.51087789797795
Measured from: 0.32
to: 8.464 [s; relative to TRIGTIME]
T50: 2.08000004291534 +/- 0.364856138331901
Measured from: 0.896
to: 2.976 [s; relative to TRIGTIME]
====== Table of the duration information =============================
Value tstart tstop
T100 13.088 0.000 13.088
T90 8.144 0.320 8.464
T50 2.080 0.896 2.976
Peak 1.000 0.516 1.516
====== 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 -1.861 -0.105 0.104 - - - 1.87e-02 -1.16e-03 1.15e-03 68.720 57
CPL -1.308 -0.422 0.468 60.044 -10.975 40.294 3.62e-02 -1.40e-02 2.65e-02 63.560 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 -1.538 -0.095 0.094 - - - 8.86e-02 -5.55e-03 5.55e-03 75.050 57
CPL -0.283 -0.454 0.502 71.789 -7.909 13.009 3.65e-01 -1.43e-01 2.63e-01 49.310 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 4.40e-07 6.50e-07 7.15e-07 1.48e-06 2.26e-06 3.29e-06 erg/cm2
90%_error_low -4.09e-08 -3.79e-08 -5.92e-08 -2.41e-07 -1.39e-07 -2.97e-07 erg/cm2
90%_error_hi 4.21e-08 3.78e-08 5.92e-08 2.70e-07 1.40e-07 3.18e-07 erg/cm2
Peak flux PL 3.78e+00 3.72e+00 2.56e+00 2.78e+00 1.12e+01 1.28e+01 ph/cm2/s
90%_error_low -3.81e-01 -2.50e-01 -1.89e-01 -3.78e-01 -7.19e-01 -7.97e-01 ph/cm2/s
90%_error_hi 3.92e-01 2.49e-01 1.88e-01 4.09e-01 7.20e-01 7.98e-01 ph/cm2/s
Fluence CPL 4.03e-07 6.85e-07 7.29e-07 6.87e-07 2.16e-06 2.50e-06 erg/cm2
90%_error_low -4.92e-08 -4.65e-08 -6.41e-08 -2.85e-07 -1.55e-07 -3.28e-07 erg/cm2
90%_error_hi 5.01e-08 4.74e-08 6.46e-08 5.28e-07 1.56e-07 5.40e-07 erg/cm2
Peak flux CPL 2.96e+00 4.17e+00 2.95e+00 1.05e+00 1.08e+01 1.11e+01 ph/cm2/s
90%_error_low -4.59e-01 -3.07e-01 -2.42e-01 -2.98e-01 -7.32e-01 -7.97e-01 ph/cm2/s
90%_error_hi 4.72e-01 3.12e-01 2.47e-01 4.01e-01 7.33e-01 8.17e-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 228.805 -41.052 0.003 29.447 -153.237 0.182 19.291 UNKNOWN Image time interval: 0.000 to 13.088 [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 13.088 sec. Spectral model in power-law: ------------------------------------------------------------ Parameters : value lower 90% higher 90% Photon index: -1.86134 ( -0.105392 0.103582 ) Norm@50keV : 1.87444E-02 ( -0.00115999 0.00115191 ) ------------------------------------------------------------ #Fit statistic : Chi-Squared = 68.72 using 59 PHA bins. # Reduced chi-squared = 1.206 for 57 degrees of freedom # Null hypothesis probability = 1.374628e-01 Photon flux (15-150 keV) in 13.09 sec: 2.64711 ( -0.15915 0.15959 ) ph/cm2/s Energy fluence (15-150 keV) : 2.25615e-06 ( -1.39403e-07 1.40194e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.000 sec. to 13.088 sec. Spectral model in the cutoff power-law: ------------------------------------------------------------ Parameters : value lower 90% higher 90% Photon index: -1.30829 ( -0.422013 0.46808 ) Epeak [keV] : 60.0437 ( -10.9749 40.2941 ) Norm@50keV : 3.62347E-02 ( -0.0140445 0.0264959 ) ------------------------------------------------------------ #Fit statistic : Chi-Squared = 63.56 using 59 PHA bins. # Reduced chi-squared = 1.135 for 56 degrees of freedom # Null hypothesis probability = 2.274951e-01 Photon flux (15-150 keV) in 13.09 sec: 2.56596 ( -0.16991 0.1704 ) ph/cm2/s Energy fluence (15-150 keV) : 2.16412e-06 ( -1.55488e-07 1.56105e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 0.516 sec. to 1.516 sec. Spectral model in power-law: ------------------------------------------------------------ Parameters : value lower 90% higher 90% Photon index: -1.53839 ( -0.0949503 0.0942237 ) Norm@50keV : 8.85856E-02 ( -0.00555237 0.00554569 ) ------------------------------------------------------------ #Fit statistic : Chi-Squared = 75.05 using 59 PHA bins. # Reduced chi-squared = 1.317 for 57 degrees of freedom # Null hypothesis probability = 5.476264e-02 Photon flux (15-150 keV) in 1 sec: 11.1775 ( -0.7192 0.7201 ) ph/cm2/s Energy fluence (15-150 keV) : 8.35468e-07 ( -5.51529e-08 5.53111e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.516 sec. to 1.516 sec. Spectral model in the cutoff power-law: ------------------------------------------------------------ Parameters : value lower 90% higher 90% Photon index: -0.283102 ( -0.454045 0.501881 ) Epeak [keV] : 71.7894 ( -7.90907 13.0089 ) Norm@50keV : 0.364900 ( -0.142839 0.263198 ) ------------------------------------------------------------ #Fit statistic : Chi-Squared = 49.31 using 59 PHA bins. # Reduced chi-squared = 0.8805 for 56 degrees of freedom # Null hypothesis probability = 7.244107e-01 Photon flux (15-150 keV) in 1 sec: 10.8305 ( -0.7316 0.7327 ) ph/cm2/s Energy fluence (15-150 keV) : 8.05972e-07 ( -5.67682e-08 5.69867e-08 ) ergs/cm2
Time-resolved spectra
Distribution
T90 vs. Hardness ratio plot
T90 = 8.144 sec. Hardness ratio (energy fluence ratio) = 1.10090533071
S(15-50 keV) vs. S(50-150 keV) plot
S(15-50 keV) = 1.0898417e-06 S(50-150 keV) = 1.166345e-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
