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 -51.152 sec. to 660.040 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.17561 ( -0.0184726 0.0185717 )
Norm@50keV : 5.13108E-02 ( -0.000628703 0.000625252 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 19.53 using 59 PHA bins.
# Reduced chi-squared = 0.3426 for 57 degrees of freedom
# Null hypothesis probability = 9.999992e-01
Photon flux (15-150 keV) in 711.2 sec: 6.00300 ( -0.08277 0.08334 ) ph/cm2/s
Energy fluence (15-150 keV) : 0.000372865 ( -3.67355e-06 3.67545e-06 ) ergs/cm2
Cutoff power-law model
Time interval is from -51.152 sec. to 660.040 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.16939 ( -0.0188031 0.0384872 )
Epeak [keV] : 9995.16 ( -9996.47 -9996.47 )
Norm@50keV : 5.15600E-02 ( -0.00057434 0.000942426 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 19.98 using 59 PHA bins.
# Reduced chi-squared = 0.3568 for 56 degrees of freedom
# Null hypothesis probability = 9.999978e-01
Photon flux (15-150 keV) in 711.2 sec: 2.22969 ( -0.1455 0.21412 ) ph/cm2/s
Energy fluence (15-150 keV) : 0.000372951 ( -3.7511e-06 3.57206e-06 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -43.424 sec. to -42.424 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.722392 ( -0.0228961 0.0230173 )
Norm@50keV : 3.13131 ( -0.045534 0.0454065 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 46.32 using 59 PHA bins.
# Reduced chi-squared = 0.8126 for 57 degrees of freedom
# Null hypothesis probability = 8.431694e-01
Photon flux (15-150 keV) in 1 sec: 10.9140 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 3.78443e-05 ( -4.8145e-07 4.81392e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -43.424 sec. to -42.424 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.501537 ( -0.0982835 0.100265 )
Epeak [keV] : 467.392 ( -122.351 303.925 )
Norm@50keV : 3.77096 ( -0.294584 0.324213 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 31.44 using 59 PHA bins.
# Reduced chi-squared = 0.5614 for 56 degrees of freedom
# Null hypothesis probability = 9.967497e-01
Photon flux (15-150 keV) in 1 sec: 358.634 ( -5.072 5.082 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.78896e-05 ( -4.83709e-07 4.83775e-07 ) ergs/cm2
Time-resolved spectra
