GRB101114A

Analysis Summary

Notes:

1) No attempt has been made to eliminate the non-significant decimal places.
2) This batgrbproduct analysis is done using the HEASARC data.
3) This batgrbproduct analysis is using the flight position for the mask-weighting calculation.

==========================================================================
           BAT GROUND-DETECTED GRB DATA PROCESSING REPORT                 
    Process Script: hand-made scripts that follow steps in batgrbproduct
                    but without using TDRSS info
    Process Start Time: Mon Sep 29 23:58:53 EDT 2014
             Host Name: bat1
   Current Working Dir: /local/data/bat1/alien/Swift_3rdBATcatalog/event/ground_detect_bursts/scripts
==========================================================================
 
  BAT Trigger Time: 311387577.6
               UTC: 2010-11-14T00:32:51.233   [includes UTCF correction]
       Where From?: Ground analysis (best_duration.txt)
  NOTE: BAT trigger time for ground-detected burst is the T100 start time.
 
  Refined Position:   [ source = BAT pre-slew image ]
    RA: 303.189391847   Dec: 14.036478225  [deg; J2000]
        { 20h 12m 45.5s , +14d 02' 11.3" }
        +/- 1.7476366908 [arcmin] (estimated 90% radius based on SNR)
    SNR: 13.7030236201
 
 
  Angular difference between the analysis and refined position is Usage: arcmin
 
  Partial Coding Fraction: 3.046875e-01    [ including projection effects ]
 
  Duration
     T90: 8. +/- 1.6
        Measured from: 0
                   to: 8     [s; relative to TRIGTIME]
     T50: 4.80000001192093 +/- 1.6
        Measured from: 1.6
                   to: 6.4     [s; relative to TRIGTIME]
 
 
====== Table of the duration information =============================
 
        Value   tstart    tstop
T100    8.000    0.000    8.000
T90     8.000    0.000    8.000
T50     4.800    1.600    6.400
Peak    1.000    1.900    2.900
 
 
====== Spectral Analysis Summary =====================================
 
Model      : spectral model: simple power-law (PL) and cutoff power-law (CPL)
Ph_index   : photon index: E^{Ph_index}
Ph_90err   : 90% error of the photon index
Epeak      : Epeak in keV
Epeak_90err: 90% error of Epeak
Norm       : normalization at 50 keV in both the PL model and CPL model
Nomr_90err : 90% error of the normalization
chi2       : Chi-Squared
dof        : degree of freedo
 
=== Time-averaged spectral analysis ===
(Best model with acceptable fit: PL)
 
Model Ph_index Ph_90err_low Ph_90err_hi  Epeak  Epeak_90err_low  Epeak_90err_hi  Norm       Nomr_90err_low    Norm_90err_hi    chi2    dof
PL      -1.193    -0.192      0.196       -           -               -         1.23e-02     -1.32e-03          1.32e-03      54.430   57
CPL     -1.194    -0.188      0.203     9999.360    -9999.360      -9999.360      1.24e-02     -4.52e-03          7.88e-03      54.450   56
 
 
=== 1-s peak spectral analysis ===
(Best model with acceptable fit: PL)
 
Model Ph_index Ph_90err_low Ph_90err_hi  Epeak  Epeak_90err_low  Epeak_90err_hi  Norm       Nomr_90err_low    Norm_90err_hi    chi2    dof
PL      -1.099     -0.294     0.306       -           -               -         1.62e-02     -2.61e-03          2.60e-03      43.580   57
CPL     -1.102     -0.287     0.398     9999.350    -9999.350      -9999.350      1.62e-02     -2.55e-03          1.96e-02      43.590   56
 
 
=== Fluence/Peak Flux Summary ===
 
              Model    Band1     Band2     Band3     Band4     Band5     Total
                       15-25     25-50    50-100    100-350    15-150    15-350    keV
Fluence         PL   4.14e-08  9.18e-08  1.61e-07  6.56e-07  4.39e-07  9.49e-07   erg/cm2
      90%_error_low -8.47e-09 -1.15e-08 -2.06e-08 -1.72e-07 -5.18e-08 -1.87e-07   erg/cm2
      90%_error_hi   9.00e-09  1.13e-08  2.03e-08  2.12e-07  5.22e-08  2.21e-07   erg/cm2
Peak flux       PL   4.54e-01  5.81e-01  5.42e-01  8.91e-01  1.88e+00  2.47e+00   ph/cm2/s
      90%_error_low -1.46e-01 -1.20e-01 -9.78e-02 -3.11e-01 -3.12e-01 -4.17e-01   ph/cm2/s
      90%_error_hi   1.63e-01  1.16e-01  9.57e-02  4.07e-01  3.14e-01  4.33e-01   ph/cm2/s
 
Fluence        CPL   4.19e-08  9.12e-08  1.58e-07  7.00e-07  4.44e-07  9.59e-07   erg/cm2
      90%_error_low    N/A       N/A       N/A    -3.92e-07    N/A    -3.70e-07   erg/cm2
      90%_error_hi     N/A       N/A       N/A     5.01e-08    N/A     8.59e-08   erg/cm2
Peak flux      CPL   4.54e-01  5.82e-01  5.40e-01  9.71e-01  1.89e+00  2.47e+00   ph/cm2/s
      90%_error_low     N/A       N/A   -9.57e-02     N/A   -3.83e-01 -5.98e-01   ph/cm2/s
      90%_error_hi      N/A       N/A    1.04e-01     N/A    3.58e-01  3.83e-01   ph/cm2/s
 
======================================================================

Special notes of this burst

Image

15.0-350.0 keV image (Event data)

#RAcent DECcent POSerr Theta  Phi  Peak_Cts  SNR Name
303.189 14.036 0.014 31.440 77.365 0.665 13.703 TRIG_00438392
 
Image time interval: -0.600 to 3.501 [sec]

Light Curves

Note: The mask-weighted lightcurves have units of either count/det or counts/sec/det, where a det is 0.4 x 0.4 = 0.16 sq cm.

Best duration plot

Full-time range; 1 s binning

Bokeh Plot

Other quick-look light curves:

64 ms binning (zoomed)
16 ms binning (zoomed)
8 ms binning (zoomed)
2 ms binning (zoomed)
SN=5 or 10 s binning (full-time range)
Raw light curve

Spectra

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    0.000 sec. to    3.501 sec.
 
Spectral model in power-law:
------------------------------------------------------------
Parameters  : value       lower 90%   higher 90%
Photon index: -1.19321     ( -0.191866   0.195549 )
Norm@50keV  : 1.23366E-02    ( -0.00131663   0.0013163 )
------------------------------------------------------------
#Fit statistic : Chi-Squared =          54.43 using 59 PHA bins.
# Reduced chi-squared =         0.9549 for     57 degrees of freedom 
# Null hypothesis probability =   5.721633e-01
 
Photon flux (15-150 keV)    in 3.501 sec: 1.44670 ( -0.16  0.16047 ) ph/cm2/s
Energy fluence (15-150 keV)             : 4.39078e-07 ( -5.18362e-08  5.21828e-08 ) ergs/cm2

Cutoff power-law model

Time interval is from    0.000 sec. to    3.501 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters  : value       lower 90%   higher 90%
Photon index: -1.19442     ( -0.18811   0.202115 )
Epeak [keV] : 9999.36      ( -9999.36 -9999.36 )
Norm@50keV  : 1.23729E-02    ( -0.00454002   0.00785404 )
------------------------------------------------------------
#Fit statistic : Chi-Squared =          54.45 using 59 PHA bins.
# Reduced chi-squared =         0.9723 for     56 degrees of freedom 
# Null hypothesis probability =   5.338727e-01
 
Photon flux (15-150 keV)    in 3.501 sec: 1.45230 (    ) ph/cm2/s
Energy fluence (15-150 keV)             : 4.43591e-07 ( 0  0 ) ergs/cm2

1-s peak spectrum fit

Power-law model

Time interval is from    1.900 sec. to    2.900 sec.
 
Spectral model in power-law:
------------------------------------------------------------
Parameters  : value       lower 90%   higher 90%
Photon index: -1.09869     ( -0.293814   0.305605 )
Norm@50keV  : 1.61854E-02    ( -0.00260684   0.00259682 )
------------------------------------------------------------
#Fit statistic : Chi-Squared =          43.58 using 59 PHA bins.
# Reduced chi-squared =         0.7646 for     57 degrees of freedom 
# Null hypothesis probability =   9.045551e-01
 
Photon flux (15-150 keV)    in 1 sec: 1.87716 ( -0.31246  0.31356 ) ph/cm2/s
Energy fluence (15-150 keV)             : 1.69309e-07 ( -2.95467e-08  2.97583e-08 ) ergs/cm2

Cutoff power-law model

Time interval is from    1.900 sec. to    2.900 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters  : value       lower 90%   higher 90%
Photon index: -1.10245     ( -0.287704   0.397499 )
Epeak [keV] : 9999.35      ( -9999.36 -9999.36 )
Norm@50keV  : 1.62380E-02    ( -0.0025943   0.0195102 )
------------------------------------------------------------
#Fit statistic : Chi-Squared =          43.59 using 59 PHA bins.
# Reduced chi-squared =         0.7785 for     56 degrees of freedom 
# Null hypothesis probability =   8.864293e-01
 
Photon flux (15-150 keV)    in 1 sec: 1.89041 ( -0.38341  0.35779 ) ph/cm2/s
Energy fluence (15-150 keV)             : 3.95458e-08 ( 0  0 ) ergs/cm2

Time-resolved spectra

Distribution

T90 vs. Hardness ratio plot

T90                                   = N/A sec.
Hardness ratio (energy fluence ratio) = N/A

S(15-50 keV) vs. S(50-150 keV) plot

S(15-50 keV)  = N/A
S(50-150 keV) = N/A

The dash-dotted line and the dashed line traces the fluences calculated from the Band function with Epeak = 15 and 150 keV, respectively. Both lines assume a canonical values of alpha = -1 and beta = -2.5.

Mask shadow pattern

 IMX = 0.133731544302,

Spacecraft aspect plot

Bright

Event

 Time interval of the image: -0.600000 3.500590

# RAcent #  [deg] 245.0065 -15.5542 254.3226  35.3232 255.9467 -37.8593 256.2704 -36.3116 263.1587 -24.7028 264.8951 -44.3821 268.1737  -1.3751 270.4143 -25.1118 270.3020 -25.7722 274.0009 -14.1031 275.8793 -30.4152 284.9531 -24.9414 288.6382  10.9340 299.8142  35.1342 262.7849 -33.7412 303.1894  14.0365 320.0622 -31.0426 298.5601   3.7623 240.4492 -25.4406

 Webpage updated on: Sun Jun 14 11:04:24 EDT 2015

IMY = -0.596566400319 source in the event data image

data image of 15-350 keV band DECcent POSerr Theta Phi PeakCts SNR AngSep Name [deg] ['] [deg] [deg] ['] 2.7 33.8 -87.9 0.2009 4.3 5.4 Sco X-1 4.6 45.3 -3.2 0.1111 2.5 6.7 Her X-1 18.2 38.8 -128.7 0.0270 0.6 2.1 4U 1700-377 9.5 37.4 -127.6 -0.0503 -1.2 10.4 GX 349+2 8.9 24.6 -123.5 0.0369 1.3 8.6 GX 1+4 7.8 41.5 -142.7 0.0621 1.5 7.7 4U 1735-44 0.0 9.8 -48.7 0.0385 1.7 12.5 SW J1753.5-0127 4.3 21.8 -138.8 0.0710 2.7 7.3 GX 5-1 8.8 22.5 -139.1 0.0346 1.3 1.7 GRS 1758-258 4.8 10.3 -136.9 0.0597 2.4 4.0 GX 17+2 12.5 26.1 -153.1 0.0251 0.9 3.7 H1820-303 105.1 21.8 -174.8 -0.0026 -0.1 4.7 HT1900.1-2455 9.8 18.9 59.4 0.0340 1.2 9.5 GRS 1915+105 5.4 44.7 49.8 0.2508 2.1 11.7 Cyg X-1 6.9 32.4 -133.1 -0.0579 -1.7 11.6 GX 354-0 0.8 31.4 77.4 0.6654 13.7 ------ UNKNOWN 2.7 48.0 152.5 0.3738 4.2 ------ UNKNOWN 2.8 22.6 92.8 0.1342 4.1 ------ UNKNOWN 3.4 41.3 -100.8 0.3529 3.4 ------ UNKNOWN

Analysis Summary

Notes:

Image

15.0-350.0 keV image (Event data)

Light Curves

Best duration plot

Full-time range; 1 s binning

Other quick-look light curves:

64 ms binning (zoomed) 16 ms binning (zoomed) 8 ms binning (zoomed) 2 ms binning (zoomed) SN=5 or 10 s binning (full-time range) Raw light curve

Spectra

Notes:

Time averaged spectrum fit using the average DRM

Power-law model

Cutoff power-law model

1-s peak spectrum fit

Power-law model

Cutoff power-law model

Time-resolved spectra

Distribution

T90 vs. Hardness ratio plot

S(15-50 keV) vs. S(50-150 keV) plot

Mask shadow pattern

Spacecraft aspect plot

Bright

64 ms binning (zoomed)
16 ms binning (zoomed)
8 ms binning (zoomed)
2 ms binning (zoomed)
SN=5 or 10 s binning (full-time range)
Raw light curve