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 -8.696 sec. to 95.944 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.132 ( -0.0746462 0.0751098 )
Norm@50keV : 3.33701E-03 ( -0.000133808 0.000133767 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 71.04 using 59 PHA bins.
# Reduced chi-squared = 1.246 for 57 degrees of freedom
# Null hypothesis probability = 9.993074e-02
Photon flux (15-150 keV) in 104.6 sec: 0.388362 ( -0.016179 0.016206 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.61337e-06 ( -1.59768e-07 1.6046e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -8.696 sec. to 95.944 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.777189 ( -0.295612 0.317992 )
Epeak [keV] : 194.566 ( -65.6532 572.498 )
Norm@50keV : 4.80441E-03 ( -0.00122957 0.00177958 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 66.79 using 59 PHA bins.
# Reduced chi-squared = 1.193 for 56 degrees of freedom
# Null hypothesis probability = 1.532620e-01
Photon flux (15-150 keV) in 104.6 sec: 0.380030 ( -0.017536 0.017542 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.52802e-06 ( -1.76426e-07 1.75814e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 9.212 sec. to 10.212 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.982843 ( -0.308872 0.326153 )
Norm@50keV : 9.00130E-03 ( -0.00153147 0.00151558 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 54.72 using 59 PHA bins.
# Reduced chi-squared = 0.9599 for 57 degrees of freedom
# Null hypothesis probability = 5.612463e-01
Photon flux (15-150 keV) in 1 sec: 1.03544 ( -0.178234 0.17938 ) ph/cm2/s
Energy fluence (15-150 keV) : 9.79445e-08 ( -1.76843e-08 1.78426e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 9.212 sec. to 10.212 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.988659 ( -0.303541 0.400576 )
Epeak [keV] : 9999.33 ( -9999.36 -9999.36 )
Norm@50keV : 9.05823E-03 ( -0.00150607 0.0162976 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 54.72 using 59 PHA bins.
# Reduced chi-squared = 0.9772 for 56 degrees of freedom
# Null hypothesis probability = 5.232697e-01
Photon flux (15-150 keV) in 1 sec: 1.03863 ( -0.189786 0.18045 ) ph/cm2/s
Energy fluence (15-150 keV) : 9.79084e-08 ( 0 0 ) ergs/cm2
Time-resolved spectra
