The 100-month Swift Catalogue of
Supergiant Fast X-ray Transients

     We investigate the characteristics of bright flares for a sample of supergiant 
     fast X-ray transients and their relation to the orbital phase. We have retrieved 
     all Swift/BAT Transient Monitor light curves, and collected all detections in excess 
     of 5σ from both daily- and orbital-averaged light curves in the time range of
     2005-Feb-12 to 2013-May-31. We also considered all on-board detections as 
     recorded in the same time span and selected those within 4 arcmin of each source 
     in our sample and in excess of 5σ. 
     We present a catalogue of over a thousand BAT flares from 11 SFXTs, 
     down to 15-150keV fluxes of ~6x10-10 erg cm-2 s-1 (daily timescale) 
     and ~1.5x10-9 erg cm-2 s-1 (orbital timescale, averaging ~800 s) and spanning
     100 months. 
     The great majority of these flares are unpublished. This population is
     characterized by short (a few hundred seconds) and relatively bright (in excess
     of 100mCrab, 15-50keV) events. In the hard X-ray, these flares last in general 
     much less than a day. Clustering of hard X-ray flares can be used to indirectly 
     measure the length of an outburst, even when the low-level emission is not 
     detected. We construct the distributions of flares, of their significance (in 
     terms of σ) and their flux as a function of orbital phase, to infer the 
     properties of these binary systems. In particular, we observe a trend of clustering 
     of flares at some phases as the orbital period increases, as consistent with a 
     progression from tight, circular or mildly eccentric orbits at short periods, to
     wider and more eccentric orbits at longer orbital periods. Finally, we estimate 
     the expected number of flares for a given source for our limiting flux and 
     provide the recipe for calculating them for the limiting flux of future hard 
     X-ray observatories.