of the brightest 33 short bursts (peak flux in 64ms$ > $4.37$ ph/(sec\cdot cm^{2}) $) with a good TTE data coverage. In order to get a reasonable signal to noise ratio we have binned this data into 2ms time bins. In this resolution the S/N of the brightest peak in the faintest burst (from our sample) is 4.7. As described in the appendix we consider a peak as statically significant only if it is more then 4$ \sigma  $ above the background. Hence this is the largest sample we could consider. The minimal recognized pulse width with this resolution is 4ms.

The *’long’* data samples\[noisy\]
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We need a sample of long bursts that could be compared to the *’short’* sample. \[longs\]The first sample we considered is a sample of 34 long bursts (called *’long’* sample) with the same 64ms peak fluxes (one to one) as the bursts in the *’short’* sample. This sample contain fairly bright long bursts, but not the brightest long bursts. This way we prevent differences that arise from different brightness.

However, the *’long’* sample cannot be compared directly with the *’short’* sample. The *’long’* sample is binned in 64ms bins while the *’short’* sample is 