1 For SWIFT J174510.8-262411, we have used a power-law {Gamma}=1.53 
 1  (Tomsick et al., 2012ATel.4393....1T).
 2 For SWIFT J1539.2-6227, we have used a power-law {Gamma}=2.15 
 2  (Krimm et al., 2009ATel.1893....1K).
 3 For XTE J1818-245, we have used a power-law {Gamma}=2.44 (Markwardt et al.,
 3  2005ATel..579....1M). The quiescent magnitude was taken ~72-days after the 
 3  peak of the outburst, probably not in real quiescence 
 3  (Cadolle Bel et al., 2009A&A...501....1C).
 4 For SWIFT J1753.5-0127, we have used a power-law {Gamma}=2.11 (Morris et al.,
 4  2005ATel..552....1M).
 5 For IGR J17091-3624, we have used a power-law {Gamma}=1.60 
 5  (Kennea & Capitanio, 2007ATel.1140....1K).
 6 For XTE J1720-318, we have used a power-law {Gamma}=2.70 
 6  (Chaty & Bessolaz, 2006A&A...455..639C).
 7 For XTE J1908+094, we have used a power-law {Gamma}=1.55 
 8  (Woods et al., 2002IAUC.7856....1W).
 8 SAX J1711.6-3808: The infrared magnitudes are from a star within the X-ray 
 8  error circle in a crowded field, but it is not confirmed as the true 
 8  counterpart (Wang & Wang (2014ApJ...788..184W).
 9 For XTE J1650-500, we have used a power-law {Gamma}=1.66 
 9  (Tomsick et al. (2004ApJ...601..439T)).
10 For XTE J1118+480, we have used a power-law {Gamma}=1.73 (Brocksopp et al., 
10  2010MNRAS.404..908B). The peak X-ray flux is taken from the 2005 outburst 
10  (Brocksopp et al., 2010MNRAS.404..908B). 
11 For XTE J1859+226, we have used a power-law {Gamma}=1.70 
11  (Wood et al., 1999IAUC.7274Q...1W).
12 GRS 1739-278: The peak X-ray flux is taken from the MAXI SSC light curve of 
12  the 2014 outburst.
13 For GRS 1730-312, we have used a power-law {Gamma}=3.88 
13  (Kaniovsky et al., 1993IAUC.5878....1K).
14 GRO J1655-40 (Nova Sco. 1994): The peak X-ray flux is taken from the 2005 
14  outburst, the brightest one so far (Brocksopp et al., 2006MNRAS.365.1203B).
15 For GRS 1009-45 (N. Vel 1993), we have used a power-law {Gamma}=1.57 
15  (Kaniovsky et al., 1993IAUC.5878....1K).
16 GRS J1915+105: The peak X-ray flux was obtained from the maximum value in 
16  the XTE/ASM light curves (MJD=50317.68034).
17 For GRS 1124-684 (N. Mus 1991), we have used a power-law {Gamma}=2.50 
17  (Sunyaev et al., 1992ApJ...389L..75S).
18 For EXO 1846-031, we have used a power-law {Gamma}=1.43 
18  (Parmar et al., 1993A&A...279..179P).
19 For SLX 1746-331, we have used a power-law {Gamma}=1.70 (Homan & Wijnands, 
19  2003ATel..169....1H). The peak X-ray flux is taken from the 2003 outburst.
20 For H 1743-322, we have used a power-law {Gamma}=1.49 (Markwardt, 
20  2003ATel..143....1M). The X-ray data is taken from the 2003 outburst 
20  (Markwardt, 2003ATel..143....1M). 
21 3A 1524-617 (KY TrA): The orbital period estimate is very uncertain.
22 1H J1659-487 (GX 339-4): The peak X-ray flux is taken from the 2002 outburst 
22  (Homan et al., 2005ApJ...624..295H). The peak outburst magnitude was 
22  obtained from (Buxton et al., 2012AJ....143..130B) (MJD=54132).
23 4U 1543-475 (IL Lup): The peak X-ray flux is taken from the 2002 outburst 
23  (Park et al., 2004ApJ...610..378P).
24 4U 1630-472 (Nor X-1): The peak X-ray flux is taken from the 2003 outburst 
24  (Tomsick et al., 2005ApJ...630..413T), the brightest one detected so far.