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 -5.604 sec. to 44.656 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.30371 ( -0.233708 0.235242 )
Norm@50keV : 1.20329E-03 ( -0.000151628 0.000151411 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 75.62 using 59 PHA bins.
# Reduced chi-squared = 1.327 for 57 degrees of freedom
# Null hypothesis probability = 5.004063e-02
Photon flux (15-150 keV) in 50.26 sec: 0.143656 ( -0.018527 0.018599 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.97149e-07 ( -8.46861e-08 8.5539e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -5.604 sec. to 44.656 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.30547 ( -0.230038 0.63704 )
Epeak [keV] : 9999.32 ( -9999.36 -9999.36 )
Norm@50keV : 1.20549E-03 ( -0.00120792 0.00106483 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 75.63 using 59 PHA bins.
# Reduced chi-squared = 1.351 for 56 degrees of freedom
# Null hypothesis probability = 4.134737e-02
Photon flux (15-150 keV) in 50.26 sec: 0.144593 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 6.00155e-07 ( -1.02724e-07 9.76959e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 24.792 sec. to 25.792 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.69041 ( -0.797865 0.703255 )
Norm@50keV : 2.68253E-03 ( -0.00122336 0.00111309 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 69.01 using 59 PHA bins.
# Reduced chi-squared = 1.211 for 57 degrees of freedom
# Null hypothesis probability = 1.323051e-01
Photon flux (15-150 keV) in 1 sec: 0.355099 ( -0.131712 0.131752 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.48599e-08 ( -1.09546e-08 1.16382e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 24.792 sec. to 25.792 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.6942 ( -1.10829 1.04221 )
Epeak [keV] : 9999.14 ( -9999.34 -9999.35 )
Norm@50keV : 2.66864E-03 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 69.01 using 59 PHA bins.
# Reduced chi-squared = 1.232 for 56 degrees of freedom
# Null hypothesis probability = 1.137162e-01
Photon flux (15-150 keV) in 1 sec: 0.355642 ( -0.132468 0.131373 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.50484e-08 ( -1.18306e-08 8.00529e-09 ) ergs/cm2
Time-resolved spectra
