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 12.788 sec. to 51.820 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.33005 ( -0.250274 0.252181 )
Norm@50keV : 1.21333E-03 ( -0.000177329 0.000176939 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 73.48 using 59 PHA bins.
# Reduced chi-squared = 1.289 for 57 degrees of freedom
# Null hypothesis probability = 6.986298e-02
Photon flux (15-150 keV) in 39.03 sec: 0.145587 ( -0.021543 0.021589 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.64683e-07 ( -7.53529e-08 7.63556e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 12.788 sec. to 51.820 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.890499 ( -0.643679 1.08997 )
Epeak [keV] : 129.147 ( -129.146 -129.146 )
Norm@50keV : 2.00696E-03 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 72.78 using 59 PHA bins.
# Reduced chi-squared = 1.300 for 56 degrees of freedom
# Null hypothesis probability = 6.524765e-02
Photon flux (15-150 keV) in 39.03 sec: 0.142938 ( -0.022235 0.022237 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.49633e-07 ( -8.27834e-08 8.22405e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 31.892 sec. to 32.892 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.42603 ( -0.611933 0.630705 )
Norm@50keV : 3.27851E-03 ( -0.00112355 0.00109226 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 69.49 using 59 PHA bins.
# Reduced chi-squared = 1.219 for 57 degrees of freedom
# Null hypothesis probability = 1.240238e-01
Photon flux (15-150 keV) in 1 sec: 0.401692 ( -0.132539 0.132878 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.15195e-08 ( -1.16531e-08 1.21321e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 31.892 sec. to 32.892 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.43525 ( -0.604289 0.644794 )
Epeak [keV] : 9999.35 ( -9999.36 -9999.36 )
Norm@50keV : 3.26866E-03 ( -0.00328429 0.18245 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 69.49 using 59 PHA bins.
# Reduced chi-squared = 1.241 for 56 degrees of freedom
# Null hypothesis probability = 1.062544e-01
Photon flux (15-150 keV) in 1 sec: 0.402668 ( -0.133723 0.13219 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.18105e-08 ( -1.45501e-08 8.30941e-09 ) ergs/cm2
Time-resolved spectra
