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
-3.844000 62.196000
120.096000 302.048000
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.03879 ( -0.0192978 0.0193978 )
Norm@50keV : 3.23134E-02 ( -0.000403656 0.000401333 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 39.72 using 59 PHA bins.
# Reduced chi-squared = 0.6969 for 57 degrees of freedom
# Null hypothesis probability = 9.602986e-01
Photon flux (15-150 keV) in 248 sec: 3.72906 ( -0.0496 0.04992 ) ph/cm2/s
Energy fluence (15-150 keV) : 8.55049e-05 ( -8.36479e-07 8.34984e-07 ) ergs/cm2
Cutoff power-law model
Multiple GTIs in the spectrum
tstart tstop
-3.844000 62.196000
120.096000 302.048000
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.03184 ( -0.0224617 0.0204746 )
Epeak [keV] : 9996.11 ( -9109.97 -9997.13 )
Norm@50keV : 3.24907E-02 ( -0.000349449 0.000455681 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 41.10 using 59 PHA bins.
# Reduced chi-squared = 0.7340 for 56 degrees of freedom
# Null hypothesis probability = 9.321325e-01
Photon flux (15-150 keV) in 248 sec: 1.38759 ( -0.08804 0.12735 ) ph/cm2/s
Energy fluence (15-150 keV) : 8.54992e-05 ( -8.30775e-07 8.26772e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 16.872 sec. to 17.872 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.98922 ( -0.0339992 0.0341892 )
Norm@50keV : 0.217868 ( -0.00392163 0.003911 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 37.51 using 59 PHA bins.
# Reduced chi-squared = 0.6580 for 57 degrees of freedom
# Null hypothesis probability = 9.785322e-01
Photon flux (15-150 keV) in 1 sec: 1.24323 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 2.36521e-06 ( -4.33822e-08 4.3475e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 16.872 sec. to 17.872 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.984461 ( -0.0328477 0.0661144 )
Epeak [keV] : 9999.36 ( -9999.36 -9999.36 )
Norm@50keV : 0.219212 ( -0.00391987 0.0078439 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 37.75 using 59 PHA bins.
# Reduced chi-squared = 0.6740 for 56 degrees of freedom
# Null hypothesis probability = 9.708759e-01
Photon flux (15-150 keV) in 1 sec: 25.0587 ( -0.4642 0.4648 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.17273e-07 ( -4.93389e-08 5.06345e-08 ) ergs/cm2
Time-resolved spectra
