We considered 292 GRBs observed by BATSE [(Brainerd 1998)]
during occurred in the field of view of EASTOP
with a zenith angle
.
For each event the measured number of counts C
during the
time interval
in which BATSE detected 90% of the flux
is compared with the average number of counts B expected from the background
(evaluated in 600 s around the burst).
No significant excess has been observed and the distribution of the excesses C-B is fully explained by poissonian fluctuations (see Fig. 1). Looking for possible delayed or anticipated excesses with respect to the BATSE event, the same analysis procedure has been performed in a 2 hours interval centered on the BATSE time, changing the width of the time window from 1 to 200 s. Also in this case no excess was found.
Figure 2 shows the obtained upper limits on the energy fluence in the
range for the 292 bursts analyzed,
in the time window
,as a function of the zenith angle.
The fluence upper limits have been calculated at 5 standard deviations level,
assuming a GRB spectrum
dN/dE
with
, extending up to
1 TeV.
The gamma-ray absorption in the intergalactic space
through pair production
affects the high energy part of the spectra of GRBs located
at cosmological distances.
According to [(Salomon&Stecker)]
the gamma-ray flux from a source at redshift z=1
is reduced by a factor
at E=50 GeV and by a factor
at E=100 GeV.
Assuming the GRB sources at z=0.5(1.0), the obtained
fluence upper limits have to be increased by a factor
.
b) All sky survey
GRBs can be searched as short duration
increases ( s) in the flux of secondary
charged particles.
In each
second, the counting rate C is compared with the expected
background B calculated averaging the counting rate in 15 minutes around.
Figure 3
shows the distribution of the differences
in unit of standard
deviations, obtained assuming poissonian fluctuations,
for a total time of measurement of 3.6 104 hours.
The data are well fitted by a Gauss distribution with
,showing the stability and good performance of the detector
over a long time exposure.
A single statistical
significant excess (10.6 standard deviation) has been observed
on 1992 July 15 at 13:22:26 UT [(Aglietta 1993)].
Assuming this excess due to a gamma-ray burst with a zenith angle
, the correspondent
energy fluence
is
.
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Figure 3:
Distribution of the excesses of duration ![]() |
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