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 59.584 sec. to 165.124 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.39244 ( -0.106045 0.10632 )
Norm@50keV : 2.11957E-03 ( -0.000121878 0.00012183 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 49.58 using 59 PHA bins.
# Reduced chi-squared = 0.8699 for 57 degrees of freedom
# Null hypothesis probability = 7.466557e-01
Photon flux (15-150 keV) in 105.5 sec: 0.257688 ( -0.015669 0.015726 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.16432e-06 ( -1.35413e-07 1.36073e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from 59.584 sec. to 165.124 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.38911 ( -0.140548 0.359753 )
Epeak [keV] : 9999.25 ( -9999.25 -9999.25 )
Norm@50keV : 2.12730E-03 ( -0.000122238 0.00106612 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 49.59 using 59 PHA bins.
# Reduced chi-squared = 0.8855 for 56 degrees of freedom
# Null hypothesis probability = 7.147080e-01
Photon flux (15-150 keV) in 105.5 sec: 0.257952 ( -0.017048 0.015743 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.16637e-06 ( -1.47991e-07 7.36027e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 147.108 sec. to 148.108 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.23417 ( -0.208983 0.211519 )
Norm@50keV : 8.11185E-03 ( -0.000947142 0.000945399 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 46.18 using 59 PHA bins.
# Reduced chi-squared = 0.8102 for 57 degrees of freedom
# Null hypothesis probability = 8.466251e-01
Photon flux (15-150 keV) in 1 sec: 0.957005 ( -0.112382 0.112515 ) ph/cm2/s
Energy fluence (15-150 keV) : 8.15361e-08 ( -1.09417e-08 1.10616e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 147.108 sec. to 148.108 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.43249 ( -0.20678 0.312032 )
Epeak [keV] : 141.405 ( -9999.36 -9999.36 )
Norm@50keV : 1.63119E-03 ( -0.000731327 0.00164514 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 45.95 using 59 PHA bins.
# Reduced chi-squared = 0.8206 for 56 degrees of freedom
# Null hypothesis probability = 8.287201e-01
Photon flux (15-150 keV) in 1 sec: 0.956887 ( -0.112454 0.112443 ) ph/cm2/s
Energy fluence (15-150 keV) : 8.27942e-08 ( 0 0 ) ergs/cm2
Time-resolved spectra
