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Table A.1

Astrometric properties.

(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11)
Year Name RA Dec Error† ℓ b d z Outb. Ref.
(h m s) (°′′′) ′′/(s, ′′) (°) (°) (kpc) (kpc)
IGR J17454-29191 17 45 27.69 −29 19 53.83 x 0.6 359.6444 −00.1765 Chenevez et al. (2014a); Paizis et al. (2015)
2014 IGR J17451-30222 17 45 06.72 −30 22 43.30 x 0.6 358.7115 −00.6580 Chenevez et al. (2014c); Chakrabarty et al. (2014)
MAXI J1828-249 18 28 58.07 −25 01 45.88 o 0.03 008.1145 −06.5458 Nakahira et al. (2013); Kennea et al. (2013)
2013 SWIFT J1753.7-2544 17 53 39.85 −25 45 14.20 i 0.3 003.6476 +00.1036 Krimm et al. (2013); Rau et al. (2013a)
SWIFT J174510.8-262411 17 45 10.85 −26 24 12.60 r (0.001,0.01) 002.1107 +01.4034 < 7 ∗ < 0.17 Cummings et al. (2012); Miller-Jones & Sivakoff (2012)
Muñoz-Darias et al. (2013)
SWIFT J1910.2-0546 19 10 22.80 −05 47 55.92 o 0.3 029.9026 −06.8440 Krimm et al. (2012); Usui et al. (2012); Rau et al. (2012)
(MAXI J1910-057)
2012 MAXI J1305-704 13 06 55.30 −70 27 05.11 r (0.003,0.07) 304.2375 −07.6177 Sato et al. (2012); Coriat et al. (2012)
MAXI J1836-1943 18 35 43.44 −19 19 10.48 e (0.000003 ,0.0002) 013.9456 −05.3542 7 ± 3 −0.70 ± 0.30 Negoro et al. (2011b); Russell et al. (2014, 2015)
MAXI J1543-5644 15 43 17.18 −56 24 49.61 r (0.049,0.775) 325.0855 −01.1214 Negoro et al. (2011a); Miller-Jones et al. (2011b)
2011 SWIFT J1357.2-0933 5 13 57 16.82 –09 32 38.55 oi 0.3 328.7019 +50.0042 > 2.29 > 1.75 Krimm et al. (2011b ); Rau et al. (2011b ); Mata Sánchez et al. (2015 )
2010 MAXI J1659-152 16 59 01.68 −15 15 28.73 e 0.0001 005.5003 +16.5167 8.60 ± 3.70 2.44 ± 1.05 Negoro et al. (2010); Paragi et al. (2010); Kuulkers et al. (2013)
XTE J1752-223 17 52 15.09 −22 20 32.36 e 0.0014 006.4231 +02.1143 6 ± 2 0.22 ± 0.07 Markwardt et al. (2009b); Miller-Jones et al. (2011a); Ratti et al. (2012)
2009 XTE J1652-4536 16 52 20.33 −45 20 39.99 r 0.32 340.5297 −00.7867 Markwardt et al. (2009c); Calvelo et al. (2009a)
SWIFT J1539.2-6227 15 39 11.96 −62 28 02.30 ox 0.5 321.0186 −05.6427 Krimm et al. (2008a, 2011c)
2008 SWIFT J1842.5-1124 18 42 17.45 −11 25 03.90 xo 0.6 021.7105 −03.1076 Krimm et al. (2008b); Markwardt et al. (2008)
SWIFT J174540.2-2900057 17 45 40.10 −29 00 06.40 x 3.6 359.9495 −00.0431 Kennea et al. (2006b,a)
IGR J17497-28218 17 49 38.04 −28 21 17.50 i 0.1 000.9531 −00.4527 Soldi et al. (2006); Torres et al. (2006a)
2006 XTE J1817-330 18 17 43.53 −33 01 07.57 r 0.2 359.8172 −07.9954 5.5 ± 4.5 ∗ −0.80 ± 0.60 Remillard et al. (2006); Rupen et al. (2006); Sala et al. (2007)
XTE J1726-476 17 26 49.28 −47 38 24.90 o 0.3 342.2032 −06.9231 Levine et al. (2005a); Turler et al. (2005); Maitra et al. (2005)
(IGR J17269-4737)
XTE J1818-245 18 18 24.43 −24 32 17.96 r (0.2,0.4) 007.4427 −04.1914 3.55 ± 0.75 −0.26 ± 0.05 Levine et al. (2005b); Rupen et al. (2005a); Cadolle Bel et al. (2009)
SWIFT J1753.5-01279 17 53 28.29 −01 27 06.22 r 0.05 024.8951 012.1842 ~ 6 ± 2 ~ 1.30 ± 0.40 Palmer et al. (2005); Fender et al. (2005); Cadolle Bel et al. (2007)
2005 IGR J17098-3628 17 09 45.93 −36 27 57.30 r (0.011,0.55) 349.5539 002.0745 ~ 10.5 ~ 0.38 Grebenev et al. (2005, 2007); Rupen et al. (2005b)
IGR J17091-362410 17 09 07.61 −36 24 25.7 r 0.1 349.5249 +02.2128 2 Kuulkers et al. (2003); Rodriguez et al. (2011)
(SAX J1709.1-3624)
2003 XTE J1720-318 17 19 58.99 −31 45 01.11 r 0.25 354.6237 +03.1013 6.5 ± 3.5 0.4 ± 0.2 Remillard et al. (2003); O’Brien et al. (2003); Chaty & Bessolaz (2006)
2002 XTE J1908+094 19 08 53.08 +09 23 04.84 r (0.001,0.01) 043.2615 +00.4377 6.5 ± 3.5 0.05 ± 0.03 1 Woods et al. (2002); Miller-Jones et al. (2013); Chaty et al. (2006)
SAX J1711.6-3808 17 11 37.10 −38 07 05.70 x 3.2 348.4200 +00.7880 in ’t Zand et al. (2001, 2002a)
2001 XTE J1650-500 16 50 00.98 − 49 57 43.60 x 0.6 336.7182 –03.4270 2.6 ± 0.7 −0.16 ± 0.04 Remillard (2001 ); Tomsick et al. (2004 ); Homan et al. (2006 )
XTE J1118+480 11 11 18 10.79 +48 02 12.42 r (0.004,0.02) 157.6607 +62.3206 1.7 ± 0.1 1.52 ± 0.09 1 Remillard et al. (2000 ); Fender et al. (2001 )
2000 (KV UMa) Gelino et al. (2006 )
XTE J1859+226 18 58 41.58 +22 39 29.40 o 0.5 054.0461 +08.6076 12.5 ± 1.5 1.90 ± 0.20 Wood et al. (1999 ); Garnavich et al. (1999 )
(V406 Vul) Corral-Santana et al. (2011 )
1999 SAX J1819.3-2525 18 19 21.58 –25 24 25.10 o 0.7 006.7740 –04.7891 6.2 ± 0.7 −0.52 ± 0.06 3 in ’t Zand et al. (1999 ); Samus et al. (1999 )
(V4641 Sgr) MacDonald et al. (2014 )
XTE J2012+38112 20 12 37.71 +38 11 01.10 o 0.35 075.3883 +02.2471 Remillard et al. (1998); Hynes et al. (1999)
XTE J1748-28813 17 48 05.06 −28 28 25.80 r 0.6 000.6756 −00.2220 ≳ 8 ≳ −0.03 Smith et al. (1998); Hjellming et al. (1998b,a)
Strohmayer & Marshall (1998)
XTE J1550-564 14 15 50 58.70 –56 28 35.20 r 0.3 325.8825 –01.8269 4.5 ± 0.5 −0.14 ± 0.02 5 Smith (1998 ); Corbel et al. (2001 ); Orosz et al. (2011b )
1998 (V381 Nor)
XTE J1755-32415 17 55 28.60 −32 28 39.00 x 60 358.0393 −03.6314 Remillard et al. (1997a)
1997 GRS 1737-3116 17 40 09.00 −31 02 24.00 x 30 357.5880 −00.0990 Sunyaev et al. (1997); Ueda et al. (1997)
GRS 1739-27817 17 42 40.03 −27 44 52.70 r (0.02,0.3) 000.6721 +01.1758 7.25 ± 1.25 ∗ 0.15 ± 0.03 1 Paul et al. (1996); Hjellming et al. (1996); Greiner et al. (1996)
1996 XTE J1856+05318 18 56 42.92 +05 18 34.30 i < 1 038.2690 +01.2720 2 Marshall et al. (1996); Torres et al. (2007b)
GRS 1730-31219 17 33 32.00 −31 12 16.00 x 180 356.6877 +01.0065 Borozdin et al. (1994); Vargas et al. (1996)
(KS 1730-312)
1994 GRO J1655-40 20 16 54 00.14 –39 50 44.90 o (0.015,0.2) 344.9819 +02.4560 3.2 ± 0.2 0.14 ± 0.01 2–4 Zhang et al. (1994 ); Bailyn et al. (1995 )
(N. Sco 1994) Hjellming & Rupen (1995 )
GRS 1716-249 17 19 36.93 −25 01 03.43 r 0.5 000.1423 +06.9909 2.4 ± 0.4 0.29 ± 0.05 Ballet et al. (1993); Harmon et al. (1993b)
(N. Oph 1993) Mirabel et al. (1993); della Valle et al. (1994)
(V2293 Oph)
GRS 1009-45 10 13 35.60 –45 04 35.28 o 275.8773 +09.3439 3.8 ± 0.3 0.62 ± 0.05 2 Lapshov et al. (1993 ); Harmon et al. (1993a )
(N. Vel 1993) della Valle & Benetti (1993 ); Gelino (2002 )
1993 (MM Vel)
GRS 1915+105 21 19 15 11.55 +10 56 44.80 e 0.001 045.3656 − 00.2194 9 ± 2 −0.03 ± 0.01 Castro-Tirado et al. (1992a ); Dhawan et al. (2000 )
(V1487 Aql) Reid et al. (2014 ); Zdziarski (2014 )
1992 GRO J0422+32 04 21 42.79 +32 54 27.10 r 0.2 165.8790 –11.9108 2.49 ± 0.30 −0.51 ± 0.06 Paciesas et al. (1992 ); Shrader et al. (1994 )
(V518 Per) Gelino & Harrison (2003 )
GRS 1124-684 11 26 26.65 − 68 40 32.83 o (0.015,0.17) 295.3005 –07.0726 5.9 ± 0.3 −0.73 ± 0.04 Lund et al. (1991 ); Makino et al. (1991 )
(N. Mus 1991) della Valle et al. (1991 ); Hynes (2005 )
1991 (GU Mus)
GS 2023+338 22 20 24 03.82 +33 52 01.90 e (0.000002,0.00005) 073.1188 –02.0914 2.39 ± 0.14 −0.09 ± 0.01 2 Makino (1989 ); Miller-Jones et al. (2009 )
1989 (V404 Cyg)
GS 1734-275 17 36 02.00 −27 25 41.00 x 7 000.1608 +02.5906 Makino (1988); Voges et al. (1999)
(GRO 1735-27)
(KS 1732-273)
1988 GS 2000+251 20 02 49.48 +25 14 11.36 r (0.07,1) 063.3666 –02.9989 2.7 ± 0.7 −0.14 ± 0.04 Makino & GINGA (1988 ); Okamura & Noguchi (1988 )
(QZ Vul) Hjellming et al. (1988 ); Jonker & Nelemans (2004 )
GS 1354-64 23 13 58 09.70 –64 44 05.80 r 0.2 309.9774 − 02.7797 ~ 25 ~-1.21 2 Makino (1987 ); Brocksopp et al. (2001 )
1987 (BW Cir) Casares et al. (2009 )
EXO 1846-03124 18 49 16.92 −03 03 54.74 x 11 029.9585 −00.9177 ~ 7 ~ −0.11 Parmar & White (1985); Parmar et al. (1993)
1985 SLX 1746-33125 17 49 48.94 −33 12 11.60 i 0.10 356.8092 −02.9736 2 Skinner et al. (1990); Torres et al. (2007a)
H 1705-250 17 08 15.52 –25 05 30.15 o 0.2 358.5874 +09.0569 8.6 ± 2.1 1.40 ± 0.30 Kaluzienski & Holt (1977 ); Yang et al. (2012 )
(N. Oph 1977) Griffiths et al. (1978 ); Jonker & Nelemans (2004 )
(V2107 Oph)
H 1743-32226 17 46 15.596 −32 14 00.860 r (0.0006,0.002) 357.2552 −01.8330 ~ 10 ~ −0.32 10 White & Marshall (1983); Miller-Jones et al. (2012)
(XTE J1746-322) Shaposhnikov & Titarchuk (2009); McClintock et al. (2009)
1977 (IGR J17464-3213)
3A 0620-003 27 06 22 44.50 − 00 20 44.72 r (0.012,0.1) 209.3382 –06.2225 1.06 ± 0.10 −0.11 ± 0.01 1 Elvis et al. (1975 ); Gallo et al. (2006 ); Cantrell et al. (2010 )
(N. Mon 1975)
1975 (V616 Mon)
1974 3A 1524-61728 15 28 16.97 −61 52 57.8 o 0.3 320.3191 −04.4272 1 Pounds et al. (1974); Holt et al. (1974); Zurita et al. (2015)
(KY TrA)
1H 1659-487 29 17 02 49.40 –48 47 23.40 r 0.3 338.9445 –04.3229 > 6 >-0.45 ~ 19 Markert et al. (1973 ); Gallo et al. (2004 )
1972 (GX 339-4) Hynes et al. (2004 )
4U 1755-33830 17 58 40.04 −33 48 26.80 o 1 357.2155 −04.8724 6.5 ± 2.5 −0.60 ± 0.20 Giacconi et al. (1972); Bradt & McClintock (1983)
(V4134 Sgr) Angelini & White (2003)
1971 4U 1543-475 31 15 47 08.32 –47 40 10.80 o 0.25 330.9266 +05.3626 7.5 ± 0.5 0.70 ± 0.05 3 Giacconi et al. (1972 ); Matilsky et al. (1972 )
(IL Lup) Park et al. (2004 ); Jonker & Nelemans (2004 )
1969 4U 1630-47232 16 34 01.61 −47 23 34.80 r (0.02,0.3) 336.9112 +00.2503 ~ 20 Giacconi et al. (1972); Priedhorsky (1986); Buxton et al. (1998)
(Nor X-1)
1966 Cen X-233 14 00 28.2 −64 47 35.6 x 7200 310.2000 −02.9000 Harries et al. (1967); Francey (1971)

Notes. Columns: (1) Year of detection; (2) Name (and counterpart name); (3–5) RA–Dec coordinates (J2000), error in astrometry and source of the coordinates; (6–7) Galactic longitude and latitude, respectively; (8–9) distance from Sun and above the Galactic plane; (10) number of outbursts reported after the discovery outburst and (11) references for detection, coordinates and distance. In this catalogue we have included all the BH candidates detected so far. Dynamical BHs are highlighted in grey boxes. .

(†)

In column 5, the letter preceding the error value indicate the source of the coordinates: radio (r), interferometry in radio (e), optical (o), infrared (i), X-rays (x) or a combination of them. In case of different errors in RA and DEC (respectively), both are shown in parenthesis.

(∗)

These values are uncertain estimates.

(1)

IGR J17454-2919: the nature of this transient source is still unclear. Paizis et al. (2015) has proposed that 2MASS J17452768-2919534 is the IR counterpart although it is 2.4′′away from the X-ray position.

(2)

IGR J17451-3022 has shown periodicity in its light curve of ~6.3 h (Jaisawal et al. 2015) which would imply a >70° inclination. However the nature of the compact object is still unclear and it might be a magnetar (Heinke et al. 2014).

(3)

MAXI J1836-194: there is a field star 0.37′′ away from the position of the BH candidate (Russell et al. 2014).

(4)

MAXI J1543-564 has no clear counterpart in optical/IR. Rau et al. (2011a) reported 3 possible objects close or within the radio (Miller-Jones et al. 2011b) and X-ray (Kennea et al. 2011b) error circles.

(5)

Swift J1357.2-0933 in rigour is not a dynamical BHT because it lacks a detection of the secondary star but it has robust mass function determination (Corral-Santana et al. 2013; Mata Sánchez et al. 2015). The distance is still uncertain (see Rau et al. 2011b; Shahbaz et al. 2013; Mata Sánchez et al. 2015)

(6)

XTE J1652-453 has no clear counterpart in IR and there are doubts between close objects.

(7)

Swift J174540.2-290005 is 1 pc from Sgr A* assuming an 8.5 kpc distance (Kennea et al. 2006b). If this transient is an X-ray binary it would be a LMXB (Wang et al. 2006).

(8)

IGR J17497-2821 seems to be blended with a bright star SE of the target (Torres et al. 2006a). Probably located in the Galactic bulge.

(9)

Swift J1753.5-0127 remains in a low/hard X-ray state since its outburst in 2005.

(10)

IGR J17091-3624 showed outbursts in 2007 (Capitanio et al. 2009) and 2011 (Krimm et al. 2011a). Re-examination of archival data showed that is was also active in 1994, 1996 and 2001 (Revnivtsev et al. 2003; in’t Zand et al. 2003; Capitanio et al. 2006).

(11)

XTE J1118+480 showed an outburst in 2005 (Zurita et al. 2005).

(12)

XTE J2012+381 is blended with a star at 1.1′′ (Hynes et al. 1999).

(13)

XTE J1748-288 showed hard spectrum. No counterpart has been found. An unresolved radio source was detected (Hjellming et al. 1998a) but it was located 1’ away from the center of the 1’ uncertainty RXTE position (Strohmayer & Marshall 1998).

(14)

XTE J1550-564 showed a second complete outburst in 2000 (Smith et al. 2000) and other three faint mini-outbursts in 2001, 2002 and 2003 (Tomsick et al. 2001; Belloni et al. 2002; Dubath et al. 2003).

(15)

XTEJ1755-324 has an error radius of 1’ in the coordinates (Remillardet al. 1997a).

(16)

GRS 1737-31 is supposed to be close to the Galactic center (Ueda et al. 1997).

(17)

GRS 1739-278 showed another outburst in 2014 (Miller et al. 2015b).

(18)

XTE J1856+053 has shown two consecutive outbursts with ~70 days interval between them (Sala et al. 2008). This behaviour was seen in the 1996 and 2007 outbursts (Levine & Remillard 2007; Krimm et al. 2007; Sala et al. 2008). This also appeared in the the recent 2015 outburst (Suzuki et al. 2015; Negoro et al. 2015).

(19)

KS 1730-312 has an error radius in the astrometry of 3’ (Vargas et al. 1996).

(20)

GRO J1655-40 (N. Sco 1994) has shown several outburst.

(21)

GRS J1915+105 has remained in outburst since its discovery in 1992 (Castro-Tirado et al. 1992a). It is included here because it was detected as a transient source.

(22)

GS 2023+338 (V404 Cyg) showed two outbursts detected in plate scales (1938 and 1956) prior to its detection in X-rays in 1989 (Wachmann 1948; Richter 1989). It has shown another outburst in 2015 (Barthelmy et al. 2015).

(23)

GS 1354-64 (BW Cir) is associated with MX 1353-64 which showed an outburst in 1971−1972. It showed another outburst in 1997 (Remillard et al. 1997b) and 2015 (Miller et al. 2015a).

(24)

EXO 1846-031 does not have a known counterpart. The error radius in the coordinates is 11′′ (Parmar et al. 1993).

(25)

SLX 1746-331 is a galactic centre source and therefore suffer of large extinction. It showed outbursts in 2003 (Markwardt 2003) and 2007 (Markwardt & Swank 2007). It also showed some activity in 2011 (Ozawa et al. 2011).

(26)

H 1743-322 has shown several outbursts.

(27)

3A 0620-003 showed an outburst in 1917 detected in plate scales prior to its detection in X-rays in 1975 (Eachus et al. 1976).

(28)

KY TrA showed another outburst in 1990 (Barret et al. 1992).

(29)

1H J1659-487 (GX 339-4) is a quasi persistent source.

(30)

4U 1755-338 is a quasi persistent system. This system stayed in outburst for 25 yr until 1996 (Roberts et al. 1996; Angelini & White 2003).

(31)

4U 1543-475 have shown outbursts in 1984, 1992 and 2002 (Kitamoto et al. 1984; Harmon et al. 1992; Miller & Remillard 2002).

(32)

4U 1630-472: It has shown quasi-periodic outbursts with recurrence times of ~600−700 d and durations of 100−200 d (Kuulkers et al. 1997).

(33)

Cen X-2 is the first transient XRB ever discovered. It has an uncertain position. Kitamoto et al. (1990) proposed that it might be GS 1354-64 (BW Cir), rediscovered in 1987. However, if this were true, it would imply an extreme X-ray flux at its distance of 25 kpc (Casares et al. 2009).

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