**Table 1:** List of X-ray bursts from 2S 0918-549. Bursts 2, 3 and 7have been published before. Values between parentheses represent uncertainties in the last digit.
No.	Date	Instr.	Peak	Persistent	$\tau$
			flux	flux
			(Crab units $^\star$ )		(s)
1	1996 Oct. 1	WFC	3.7(3)	0.0048(5)	117(2)
2 $^\dag$	1999 Jun. 10	WFC	3.3(3)	0.0037(5)	29(4)
3 $^\ddag$	2000 May 12	PCA	>3.2	<0.0146	8.95(5)
4	2001 May 18	WFC	2.5(3)	0.0094(5)	5.8(4)
5	2001 Sep. 29	ASM	2.9(1)	0.0061(7) $^\P$	25(3)
6	2003 Aug. 5	ASM	2.1(1)	0.0080(8) $^\P$	22(10) $^\times$
7 $^\ast$	2004 Jun. 18	PCA	0.26(1)	0.0126(3)	12.5(5)

$^\star$ For a burst peak spectrum as determined in this paper for the first burst, one Crab unit translates to a bolometric flux of $2.7\times10^{-8}$ erg cm^-2 s^-1. For the persistent flux, one may adhere to a 2-10 keV flux of $2.0\times10^{-8}$ erg cm^-2 s^-1 (the bolometric correction is less certain in that case).
$^\dag$ Cornelisse et al. (2002). This burst was erroneously dated four days earlier in that paper.
$^\ddag$ Jonker et al. (2001).
$^\ast$ Galloway et al. (2005) this paper mentioned 2 more faint bursts from 2S 0918-549, but the data do not allow confirmation as type-I X-ray bursts.
$^\P$ These are 14-d averages.
$^\times$ This burst was only partly observed. The observation stopped 18 s after burst onset.

Source LaTeX | All tables | In the text

	1 Introduction
	2 Synopsis of X-ray bursts from 2S 0918-549
	3 Analysis of the long burst
	4 Flux history of persistent emission
	5 Discussion
	6 Conclusion
	References