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 -0.116 sec. to 68.256 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.73124 ( -0.0611324 0.0606951 )
Norm@50keV : 4.09093E-03 ( -0.00013497 0.000134618 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 68.74 using 59 PHA bins.
# Reduced chi-squared = 1.206 for 57 degrees of freedom
# Null hypothesis probability = 1.370554e-01
Photon flux (15-150 keV) in 68.37 sec: 0.549412 ( -0.018451 0.018499 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.58419e-06 ( -8.85911e-08 8.89692e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.116 sec. to 68.256 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.21047 ( -0.25618 0.271762 )
Epeak [keV] : 74.9413 ( -10.8568 25.7813 )
Norm@50keV : 7.43716E-03 ( -0.00185624 0.00266603 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 56.01 using 59 PHA bins.
# Reduced chi-squared = 1.000 for 56 degrees of freedom
# Null hypothesis probability = 4.746309e-01
Photon flux (15-150 keV) in 68.37 sec: 0.528695 ( -0.020703 0.020778 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.46437e-06 ( -1.04947e-07 1.05231e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 0.960 sec. to 1.960 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.0979 ( -0.0867618 0.0872389 )
Norm@50keV : 3.04496E-02 ( -0.00142846 0.00142832 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 51.93 using 59 PHA bins.
# Reduced chi-squared = 0.9111 for 57 degrees of freedom
# Null hypothesis probability = 6.650848e-01
Photon flux (15-150 keV) in 1 sec: 3.53123 ( -0.16909 0.16926 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.18603e-07 ( -1.70803e-08 1.71733e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.960 sec. to 1.960 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.09382 ( -0.0865545 0.0915793 )
Epeak [keV] : 9999.21 ( -9999.28 -9999.28 )
Norm@50keV : 3.05571E-02 ( -0.00143533 0.00977455 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 51.95 using 59 PHA bins.
# Reduced chi-squared = 0.9277 for 56 degrees of freedom
# Null hypothesis probability = 6.288072e-01
Photon flux (15-150 keV) in 1 sec: 3.53857 ( -0.20352 0.18654 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.19463e-07 ( 0 0 ) ergs/cm2
Time-resolved spectra
