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 5.868 sec. to 206.680 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.86377 ( -0.0789212 0.0777441 )
Norm@50keV : 3.33414E-03 ( -0.000160588 0.000159786 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 88.84 using 59 PHA bins.
# Reduced chi-squared = 1.559 for 57 degrees of freedom
# Null hypothesis probability = 4.421823e-03
Photon flux (15-150 keV) in 200.8 sec: 0.471319 ( -0.021483 0.021519 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.15607e-06 ( -2.96389e-07 2.97857e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from 5.868 sec. to 206.680 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.329152 ( -0.451168 0.501856 )
Epeak [keV] : 49.5010 ( -3.45164 4.3706 )
Norm@50keV : 2.19279E-02 ( -0.0092747 0.0187229 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 46.11 using 59 PHA bins.
# Reduced chi-squared = 0.8234 for 56 degrees of freedom
# Null hypothesis probability = 8.243563e-01
Photon flux (15-150 keV) in 200.8 sec: 0.435178 ( -0.023269 0.023359 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.45272e-06 ( -3.30675e-07 3.38944e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 38.828 sec. to 39.828 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.66823 ( -0.316979 0.299432 )
Norm@50keV : 1.41677E-02 ( -0.00285587 0.00279874 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 65.63 using 59 PHA bins.
# Reduced chi-squared = 1.151 for 57 degrees of freedom
# Null hypothesis probability = 2.026216e-01
Photon flux (15-150 keV) in 1 sec: 1.86130 ( -0.35172 0.35208 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.31553e-07 ( -2.75035e-08 2.77926e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 38.828 sec. to 39.828 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.912667 ( -1.29019 1.57242 )
Epeak [keV] : 72.6505 ( -46.5543 -72.6503 )
Norm@50keV : 3.44005E-02 ( -0.0344017 0.165804 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 64.50 using 59 PHA bins.
# Reduced chi-squared = 1.152 for 56 degrees of freedom
# Null hypothesis probability = 2.036946e-01
Photon flux (15-150 keV) in 1 sec: 1.82764 ( -0.36021 0.35795 ) ph/cm2/s
Energy fluence (15-150 keV) : 9.43865e-08 ( -3.1676e-08 2.08075e-08 ) ergs/cm2
Time-resolved spectra
