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 -14.352 sec. to 26.592 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.50825 ( -0.169434 0.169317 )
Norm@50keV : 3.49179E-03 ( -0.000343347 0.000341874 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 72.22 using 59 PHA bins.
# Reduced chi-squared = 1.267 for 57 degrees of freedom
# Null hypothesis probability = 8.429894e-02
Photon flux (15-150 keV) in 40.94 sec: 0.436898 ( -0.043329 0.043434 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.3545e-06 ( -1.4435e-07 1.45423e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -14.352 sec. to 26.592 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.50581 ( -0.844585 0.586407 )
Epeak [keV] : 9995.80 ( -9995.85 -9995.85 )
Norm@50keV : 3.50214E-03 ( -0.00120259 0.00397722 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 72.22 using 59 PHA bins.
# Reduced chi-squared = 1.290 for 56 degrees of freedom
# Null hypothesis probability = 7.113416e-02
Photon flux (15-150 keV) in 40.94 sec: 0.436867 ( -0.044255 0.043246 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.35428e-06 ( -1.59389e-07 1.44397e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 3.236 sec. to 4.236 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.34381 ( -0.273102 0.277147 )
Norm@50keV : 1.39827E-02 ( -0.00233849 0.00233307 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 40.76 using 59 PHA bins.
# Reduced chi-squared = 0.7151 for 57 degrees of freedom
# Null hypothesis probability = 9.486049e-01
Photon flux (15-150 keV) in 1 sec: 1.68240 ( -0.28833 0.28928 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.36773e-07 ( -2.47725e-08 2.50276e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 3.236 sec. to 4.236 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.644698 ( -0.88771 1.36312 )
Epeak [keV] : 98.3377 ( -38.4824 -98.3393 )
Norm@50keV : 3.14040E-02 ( -0.0190567 0.116158 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 39.48 using 59 PHA bins.
# Reduced chi-squared = 0.7051 for 56 degrees of freedom
# Null hypothesis probability = 9.537959e-01
Photon flux (15-150 keV) in 1 sec: 1.64386 ( -0.29476 0.29527 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.30551e-07 ( -2.71654e-08 2.69524e-08 ) ergs/cm2
Time-resolved spectra
