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
Multiple GTIs in the spectrum
tstart tstop
-0.740000 38.175800
39.512000 164.704000
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.54232 ( -0.0559775 0.055888 )
Norm@50keV : 4.71213E-03 ( -0.000136436 0.000136414 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 45.94 using 59 PHA bins.
# Reduced chi-squared = 0.8060 for 57 degrees of freedom
# Null hypothesis probability = 8.526935e-01
Photon flux (15-150 keV) in 164.1 sec: 0.595227 ( -0.019189 0.019285 ) ph/cm2/s
Energy fluence (15-150 keV) : 7.28868e-06 ( -2.22113e-07 2.22333e-07 ) ergs/cm2
Cutoff power-law model
Multiple GTIs in the spectrum
tstart tstop
-0.740000 38.175800
39.512000 164.704000
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.54973 ( -0.0579607 0.0627077 )
Epeak [keV] : 9999.36 ( -9999.36 -9999.36 )
Norm@50keV : 4.67574E-03 ( -0.000134581 0.000785757 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 46.38 using 59 PHA bins.
# Reduced chi-squared = 0.8281 for 56 degrees of freedom
# Null hypothesis probability = 8.168565e-01
Photon flux (15-150 keV) in 164.1 sec: 0.598145 ( -0.013017 0.016252 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.22599e-06 ( -3.4655e-07 3.35524e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 0.204 sec. to 1.204 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.23969 ( -0.134268 0.135699 )
Norm@50keV : 5.79965E-02 ( -0.0045266 0.00451536 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 49.73 using 59 PHA bins.
# Reduced chi-squared = 0.8725 for 57 degrees of freedom
# Null hypothesis probability = 7.418092e-01
Photon flux (15-150 keV) in 1 sec: 6.84818 ( -0.56932 0.57173 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.82076e-07 ( -4.74132e-08 4.75462e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.204 sec. to 1.204 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.2353 ( -0.135116 0.520168 )
Epeak [keV] : 9984.67 ( -9986.85 -9986.85 )
Norm@50keV : 5.82622E-02 ( -0.00449964 0.0389517 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 49.73 using 59 PHA bins.
# Reduced chi-squared = 0.8880 for 56 degrees of freedom
# Null hypothesis probability = 7.096673e-01
Photon flux (15-150 keV) in 1 sec: 6.84698 ( -0.56925 0.57069 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.82023e-07 ( -4.8e-08 4.64983e-08 ) ergs/cm2
Time-resolved spectra
