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 -25.200 sec. to 44.800 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.22042 ( -0.196324 0.202436 )
Norm@50keV : 3.79671E-03 ( -0.000438344 0.000434765 )
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#Fit statistic : Chi-Squared = 51.80 using 59 PHA bins.
# Reduced chi-squared = 0.9088 for 57 degrees of freedom
# Null hypothesis probability = 6.698382e-01
Photon flux (15-150 keV) in 70 sec: 0.446982 ( -0.055991 0.056556 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.68138e-06 ( -3.0422e-07 3.04473e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -25.200 sec. to 44.800 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.917786 ( -0.398436 0.909618 )
Epeak [keV] : 221.131 ( -221.135 -221.135 )
Norm@50keV : 5.05996E-03 ( -0.00194604 0.00627187 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 51.36 using 59 PHA bins.
# Reduced chi-squared = 0.9172 for 56 degrees of freedom
# Null hypothesis probability = 6.507826e-01
Photon flux (15-150 keV) in 70 sec: 0.438935 ( -0.059747 0.059566 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.66096e-06 ( -3.10958e-07 3.09599e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.200 sec. to 0.800 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.4283 ( -0.61119 0.58604 )
Norm@50keV : 1.06214E-02 ( -0.00373834 0.00373816 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 68.34 using 59 PHA bins.
# Reduced chi-squared = 1.199 for 57 degrees of freedom
# Null hypothesis probability = 1.443969e-01
Photon flux (15-150 keV) in 1 sec: 1.30204 ( -0.488792 0.50181 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.0207e-07 ( -3.70271e-08 3.72778e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.200 sec. to 0.800 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: 9.99987 ( -6.47343 -9.99996 )
Epeak [keV] : 68.6168 ( -8.37877 9.81709 )
Norm@50keV : 108.389 ( -108.188 307.708 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 60.91 using 59 PHA bins.
# Reduced chi-squared = 1.088 for 56 degrees of freedom
# Null hypothesis probability = 3.035969e-01
Photon flux (15-150 keV) in 1 sec: 0.830355 ( -0.229918 0.322865 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.81075e-08 ( 0 0 ) ergs/cm2
Time-resolved spectra
