-distributions
The fragments of the BATSE daily records (DISCLA).
Two fragments of the BATSE daily records, each corresponding to one
orbital period of CGRO. Counts rates averaged over ten 1.024 bins are show
for 2 detectors in the 50 - 300 keV range.
Upper panel:
<51 800 s - noise from Cyg X-1; 51 800 s - descent of Cyg X-1;
52 400 s - CGRO reaches its most Southern latitude; 54 050 s - rise of Cyg X-1;
54 660 s - particle precipitation; 54 930 s - a solar flare;
55 200 s - CGRO reaches its most Northern latitude;
56 270 s - rise of the Crab nebula.
Lower panel:
78 500 s - particle precipitation; 79 550 s - descent of Cyg X-1; 80 250 s -
a non-triggered GRB;
81 700 s - rise of Cyg X-1; 83 030 s - a non-triggered GRB.
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The time profiles for the 11 weakest GRBs
detected in the scan (fitting count rate).
The time profiles have been shifted vertically for clarity.
The burst 10330a can hardly be recognized visually on this scale due to
its long duration (~150 s) and smoothness.
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The log N - log P distribution (3906 GRBs).
The distribution for long events is preferable for various
fits as it has a more uniform detection efficiency.
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The efficiency of a GRB detection in the scan
measured with test bursts.
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The peak flux
distribution of triggered and non-triggered GRBs.
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The hardness ratio versus peak flux.
Hardness ration for an incomplete sample of found triggered (green dots)
and non-triggered (red dots) GRBs.
Hardness ratio is defined as the ratio of integrals of net signals
in different energy channels: 2+3/1 and 3/2.
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The GRB duration distribution (T90).
Thin line histogram - triggered, thick line histogram - non-triggered
bursts.
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The sky map on Aitoff-Hammer projection in Galactic
coordinates (3906 bursts)
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only non-triggered GRBs -
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The GRB location errors distribution (for an incomplete sample) -
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The residual x2 maps of the GRB localizations on the sky.
The least reliable cases -- 09394b, 09575a, and 09590c.
The levels at 0.5$\sigma$, 1$\sigma$ (bold contour), 2$\sigma$,
3$\sigma$, 4$\sigma$ (bold contour), 6$\sigma$, and 8$\sigma$ are shown.
The dashed area represents the Earth.
The cross shows the location of Cyg X-1.
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The polar angle distributions (for an incomplete sample).
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The geocentric angle distributions (for an incomplete sample).
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The Cyg X-1 - GRB angle distributions (for an incomplete sample).
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The distribution of detected GRBs over the latitude of CGRO.
Upper panel: weak events (P < 0.2 photons/s/cm2);
lower panel: all events. Thick line histograms: real bursts;
thin line histograms: test bursts; dotted line histogram:
100 particle precipitation events.
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The hardness ratio: comparison GRBs with other phenomena.
The integral of the counts in channels #2 and #3, 50 - 300 keV
to that in channel 1, 20 - 50 keV versus the 50-300 keV peak flux
for GRBs (dots) and for non-GRB events: Cyg X-1(crosses),
ionospheric phenomena(squares), X-ray pulsars(stars),
solar flares(circles).
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The rate of GRB detection during the scan.
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The peak flux estimate: comparison
with the BATSE and Kommers et al. catalogs.
The 50 - 300 keV range, 1.024 s time resolution.
For non-triggered (crosses) and triggered bursts (dots).
For clarity, only first 30% of the sample is shown.
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The log N - log P distribution (for an incomplete sample):
comparison with Kommers et al. and 3BATSE catalog.
The distribution is done in absolute units
for first 2934 events found in the scan.
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The GRB duration distribution (T90): comparison
with BATSE catalog.
The distribution is done for the 1965 GRBs detected both by BATSE
and by Stern et al. up to TJD 11499.
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The GRB locations: comparison with BATSE catalog
(for an incomplete sample).
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The GRB locations: comparison with Kommers et al. catalog
(for an incomplete sample).
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The deviation in locations (BATSE, Kommers et al.,Stern et al.)
versus the location error.
Angular deviations between our and
the Kommers et al best fit locations (crosses)
and between our and the BATSE locations (dots) versus the 1sigma
localization errors according to our estimates.
For clarity, only first 30% of the sample is shown.
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Test bursts: the peak count rate distribution.
Test bursts are included here independently of
whether they were detected or missed. The BATSE threshold is around 0.15
counts/s/cm2.
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Test bursts: the measured vs expected peak count rates.
Several points having a measured count rate much lower than the expected one
are affected by data gaps causing the peak of the event to be lost.
Two points, where the measured count rate is much higher, are probably due to
confusion of the test burst with an overlapping brighter real event.
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Last Revised: April 25, 2001...................... Created by B.Stern&Ya.Tikhom
irova