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Table 1:

Overview of the properties1 of the observed flashes discussed in this paper.

Source
$F_{\rm bb,peak}$ (10-8  $F_{\rm pers}$  $F_{\rm pers,bol}/F_{\rm bb,peak}$ $L_{\rm x,bol}$ (1036 $\Delta t_{\rm last}$  $\Delta t_{\rm next}$ 
  erg cm-2 s-1)  (10-10 erg cm-2 s-1) $\equiv$ $L_{\rm x,bol}/L_{\rm Edd}$erg s-1)(days) (days) 
Cen X-4 $\sim$120[1] <20a (2-10 keV)[1]$\lesssim$0.0033$\lesssim$0.7>40[1,2]$\simeq$2[1,3]
2S 1711-339 $3.0 \pm 1.0^b$[4] <0.7 (2-28 keV)[4]$\lesssim$0.0047$\lesssim$1$\sim$340[4]$\simeq$1440[5]
GRS 1747-312 $\simeq$2.5c[6] <0.6 (0.1-200 keV)[6]$\lesssim$0.0024$\lesssim$0.5$\simeq$26[6]$\simeq$28[6]
IGR J17473-2721 $\simeq$11d[7] <1.7 (2-10 keV)[8]$\lesssim$0.0031$\lesssim$0.4$\sim$960[9,10]$\simeq$2[8,11]
2S 1803-245 $3.1 \pm 0.7$[12] <2e (2-28 keV)[4]$\lesssim$0.013$\lesssim$3$\sim$7990[13]$\simeq$7[12]
SAX J1808.4-3658 $25 \pm 2^c$[14] <3 (2-28 keV)[14]$\lesssim$0.0024$\lesssim$0.5$\simeq$17[14]$\simeq$543[15]
a Vela 5B 56 h upper limit; b highest peak flux among the flash sample in [4]; c photospheric radius-expansion flash; d peak flux observed during another flash reported by [7]; e no limits are quoted in [12]; we, therefore, assume the highest BeppoSAX/WFC flux upper limit from [4].
Note 1. In the first two columns we give the observed flash bolometric peak fluxes ( $F_{\rm bb,peak}$) and the 3$\sigma$ upper limits on the flux around the flashes ( $F_{\rm pers}$). From these we infer the flash peak luminosities in terms of the Eddington luminosity ( $L_{\rm Edd}$), assuming $L_{\rm x,bol}/L_{\rm Edd} \equiv F_{\rm pers,bol}/F_{\rm bb,peak}$ (see Sect. 3), where $F_{\rm pers,bol}$ and $L_{\rm x,bol}$ are the bolometric pre-flash source flux and luminosity, respectively. Assuming $L_{\rm Edd} = 2 \times 10^{38}$ erg s (see Sect. 2) we derive an upper limit on $L_{\rm x,bol}$. In the last two columns we provide the time since the last and to the next detected X-ray outburst with respect to the time of the flash, $\Delta t_{\rm last}$ and $\Delta t_{\rm next}$, respectively. References are given in brackets: [1] this paper; [2] Conner et al. (1969); [3] Belian et al. (1972); [4] Cornelisse et al. (2002a); [5] Markwardt & Swank (2004); [6] in 't Zand et al. (2003b); [7] Altamirano et al. (2008); [8] Markwardt et al. (2008); [9] Grebenev et al. (2005); [10] Markwardt & Swank (2005); [11] Del Monte et al. (2008); [12] Cornelisse et al. (2007); [13] Jernigan (1976); [14] in 't Zand et al. (2001); [15] Marshall (1998).

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