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 -12.036 sec. to 3.304 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.26912 ( -0.194615 0.197301 )
Norm@50keV : 3.23205E-03 ( -0.000377708 0.000377689 )
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#Fit statistic : Chi-Squared = 41.32 using 59 PHA bins.
# Reduced chi-squared = 0.7249 for 57 degrees of freedom
# Null hypothesis probability = 9.413339e-01
Photon flux (15-150 keV) in 15.34 sec: 0.383488 ( -0.046281 0.046409 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.93793e-07 ( -6.29041e-08 6.33738e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -12.036 sec. to 3.304 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.41315 ( -0.795498 0.980828 )
Epeak [keV] : 99.4525 ( -28.2812 422.257 )
Norm@50keV : 8.22327E-03 ( -0.00469827 0.0144547 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 37.90 using 59 PHA bins.
# Reduced chi-squared = 0.6768 for 56 degrees of freedom
# Null hypothesis probability = 9.695580e-01
Photon flux (15-150 keV) in 15.34 sec: 0.370049 ( -0.048202 0.048173 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.70235e-07 ( -6.70866e-08 6.75207e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 0.480 sec. to 1.480 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.02633 ( -0.33064 0.355027 )
Norm@50keV : 8.56837E-03 ( -0.00161202 0.00159077 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 74.81 using 59 PHA bins.
# Reduced chi-squared = 1.312 for 57 degrees of freedom
# Null hypothesis probability = 5.690410e-02
Photon flux (15-150 keV) in 1 sec: 0.987989 ( -0.189772 0.191191 ) ph/cm2/s
Energy fluence (15-150 keV) : 9.18142e-08 ( -1.78486e-08 1.79549e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.480 sec. to 1.480 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.02063 ( 0.958824 1.20566 )
Epeak [keV] : 1.00000E+04 ( -10000 -10000 )
Norm@50keV : 8.61811E-03 ( -0.00161727 -0.00861837 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 74.81 using 59 PHA bins.
# Reduced chi-squared = 1.336 for 56 degrees of freedom
# Null hypothesis probability = 4.728779e-02
Photon flux (15-150 keV) in 1 sec: 0.991427 ( -0.199362 0.194003 ) ph/cm2/s
Energy fluence (15-150 keV) : 9.20322e-08 ( -1.84166e-08 1.46716e-08 ) ergs/cm2
Time-resolved spectra
