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: Sat Mar 28 12:51:35 EDT 2015
Host Name: bat1
Current Working Dir: /local/data/bat1/alien/Swift_3rdBATcatalog/event/batevent_reproc/GRB141229A
======================================================================
Trigger: 00085478 Segment: 004
BAT Trigger Time: 441546552.0
UTC: 2014-12-29T11:48:59.019 [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: 72.452516342814 Dec: -19.2544033828349 [deg; J2000]
{ 04h 49m 48.6s , -19d -15' -15.9" }
+/- 4.674100778 [arcmin] (estimated 90% radius based on SNR)
SNR: 3.36096249581
Angular difference between the analysis and refined position is Usage: arcmin
Partial Coding Fraction: Unavailable because the burst occurred during slew.
Duration
T90: 6.40000003576279 +/- 1.6
Measured from: 0
to: 6.4 [s; relative to TRIGTIME]
T50: 3.19999998807907 +/- 1.6
Measured from: 1.6
to: 4.8 [s; relative to TRIGTIME]
====== Table of the duration information =============================
Value tstart tstop
T100 6.400 0.000 6.400
T90 6.400 0.000 6.400
T50 3.200 1.600 4.800
Peak 1.000 0.300 1.300
====== 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: 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
=== 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 N/A N/A N/A N/A N/A N/A erg/cm2
Image
Note1: The mosaic image is made with timebin = 0.05 s; energybin = 15-150 keV
Note2: The mosaic imsge uses Galactic coordinate.
#RAcent DECcent POSerr Theta Phi Peak_Cts SNR Name 72.453 -19.254 0.020 42.654 128.237 0.160 3.361 UNKNOWN Image time interval: 2.248 to 6.400 [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
Multiple GTIs in the spectrum tstart tstop XSPEC12>exit XSPEC: quit Photon index: ( ) ------------------------------------------------------------ Parameters : value lower 90% higher 90% Photon index: ( ) Norm@50keV : ( ) ------------------------------------------------------------ Photon flux (15-150 keV) in sec: ( ) ph/cm2/s Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
Cutoff power-law model
Multiple GTIs in the spectrum tstart tstop XSPEC: quit Photon index: ( ) ------------------------------------------------------------ Parameters : value lower 90% higher 90% Photon index: ( ) Epeak [keV] : ( ) Norm@50keV : ( ) ------------------------------------------------------------ Photon flux (15-150 keV) in sec: ( ) ph/cm2/s Energy fluence (15-150 keV) : 0 ( 0 0 ) 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 = N/A sec. Hardness ratio (energy fluence ratio) = N/A
S(15-50 keV) vs. S(50-150 keV) plot
S(15-50 keV) = N/A S(50-150 keV) = N/A
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
