The current state of disk wind observations in BHLMXBs through X-ray absorption lines in the iron band

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Volume 681 (January 2024)

A&A, 681 (2024) A49

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Table 1.

Sources included in our final sample.

Name	Mass (M_⊙)	Distance (kpc)	Inclination (°)	Absorption lines	Exposures in the sample
				reported in the iron band	EPIC pn	HETG
1E 1740.7-2942	8	8	> 50^R⁽¹⁾	X	6	1
4U 1543-475^D⁽²⁾	8.4 ± 1 ⁽³⁾	7.5 ± 0.5 ⁽⁴⁾	dips⁽⁵⁾, 20.7 ± 1.5^D⁽³⁾	X	0	1
4U 1630-47	8	8.1 ± 3.4 ⁽⁶⁾	dips⁽⁷⁾, [60 − 75]^D⁽⁷⁾	✓	8	12
4U 1957+115	8	8	∼13^D⁽⁸⁾/77.6(+1.5 − 2.2)^R⁽⁹⁾	X	2	4
AT 2019wey	8	8	< 30^R⁽¹⁰⁾	X	0	1
EXO 1846-031	8	∼7 ⁽¹¹⁾	/∼73^R⁽¹²⁾/∼40^R⁽¹³⁾	✓	2	6
GRO J1655-40^D⁽¹⁴⁾	5.4 ± 0.3 ⁽¹⁵⁾	3.2 ± 0.2 ⁽¹⁶⁾	dips⁽¹⁷⁾ 69 ± 2^D⁽¹⁵⁾	✓	6	2
GRS 1716-249	8	2.4 ± 0.4 ⁽¹⁸⁾	∼40 − 60^R⁽¹⁹⁾	X	0	1
GRS 1739-278	8	7.3 ± 1.3 ⁽²⁰⁾	∼33^R⁽²¹⁾	X	0	1
GRS 1758-258	8	8	/	✓	3	1
GRS 1915+105^D⁽²²⁾	⁽²²⁾	⁽²²⁾	dips⁽²³⁾ 60 ± 5^J⁽²²⁾	✓	17	22
GS 1354-64^D⁽²⁴⁾	8	∼25 ⁽²⁴⁾	< 79^D⁽²⁴⁾/∼70^R⁽²⁵⁾	X	2	0
GX 339-4^D⁽²⁶⁾	5.9 ± 3.6 ⁽²⁶⁾	8	[37 − 78]^D⁽²⁶⁾	X	21	4
H 1743-322	8	8.5 ± 0.8 ⁽²⁷⁾	dips⁽²⁸⁾, 75 ± 3^J⁽²⁷⁾	✓	8	9
IGR J17091-3624	8	8	dips⁽²³⁾ ∼70^H⁽²⁹⁾⁽³⁰⁾/∼30 − 40^R^(31, 32)	✓	6	9
IGR J17098-3628	8	∼10.5 ⁽³³⁾	/	X	2	0
IGR J17285-2922	8	8	/	X	1	0
IGR J17451-3022	8	8	dips⁽³⁴⁾ > 70^D⁽³⁴⁾	✓	1	0
IGR J17497-2821	8	8	/	X	1	1
MAXI J0637-430	8	8	64 ± 6^R⁽³⁵⁾	X	1	0
MAXI J1305-704^D⁽³⁶⁾	⁽³⁶⁾	⁽³⁶⁾	dips⁽³⁷⁾,⁽³⁶⁾	✓	0	1
MAXI J1348-630	8	⁽³⁸⁾	28 ± 3^J⁽³⁹⁾/65 ± 7 ⁽⁴⁰⁾/[30 − 45]^R⁽⁴¹⁾	✓	2	3
MAXI J1535-571	8	⁽⁴²⁾	≤45^J⁽⁴³⁾/70 − 74^R⁽⁴⁴⁾	X	6	5
MAXI J1659-152	8	8.6 ± 3.7 ⁽⁴⁵⁾	dips⁽⁴⁵⁾, 70 ± 10^D⁽⁴⁵⁾	X	2	0
MAXI J1803-298	8	8	dips⁽⁴⁶⁾, > 70^D⁽⁴⁶⁾	✓	0	4
MAXI J1820+070 ^D⁽⁴⁷⁾	6.9 ± 1.2 ⁽⁴⁸⁾	2.96 ± 0.33 ⁽⁴⁹⁾	dips⁽⁵⁰⁾, [67 − 81]^D⁽⁴⁸⁾	X	14	0
SAX J1711.6-3808	8	8	/	X	1	0
Swift J1357.2-0933	8	8	dips⁽⁵¹⁾, ≥80^D⁽⁵²⁾	X	1	0
Swift J1658.2-4242	8	8	dips⁽⁵³⁾, 64(+2 − 3)^R⁽⁵⁴⁾	✓	8	1
Swift J174510.8-262411	8	8	/	X	1	0
Swift J1753.5-0127	8	6 ± 2 ⁽⁵⁵⁾	55(+2 − 7)^R⁽⁵⁶⁾	X	6	1
Swift J1910.2-0546	8	8	/	X	1	1
V404 Cyg^D⁽⁵⁷⁾	⁽⁵⁷⁾	2.4 ± 0.2 ⁽⁵⁸⁾	67(+3 − 1)^D⁽⁵⁷⁾	✓	0	2
V4641 Sgr^D⁽⁵⁹⁾	6.4 ± 0.6 ⁽⁶⁰⁾	6.2 ± 0.7 ⁽⁶⁰⁾	72 ± 4^D⁽⁶⁰⁾	X	0	2
XTE J1550-564^D⁽⁶¹⁾	11.7 ± 3.9 ⁽⁶¹⁾	⁽⁶¹⁾	75 ± 4^D⁽⁶¹⁾/∼40^R⁽⁶²⁾	X	0	2
XTE J1650-500^D⁽⁶³⁾	8	2.6 ± 0.7 ⁽⁶⁴⁾	≥47^D⁽⁶³⁾	X	1	2
XTE J1652-453	8	8	≤32^R⁽⁶⁵⁾	✓	1	0
XTE J1720-318	8	6.5 ± 3.5 ⁽⁶⁶⁾	/	X	1	0
XTE J1752-223	8	6 ± 2 ⁽⁶⁷⁾	< 49^J⁽⁶⁸⁾/35 ± 4^R⁽⁶⁹⁾	X	2	2
XTE J1817-330	8	5.5 ± 4.5 ⁽⁷⁰⁾	dips⁽⁷¹⁾	X	1	4
XTE J1856+053	8	8	/	X	1	0
XTE J1901+014	8	8	/	X	1	0

Notes. The columns report relevant physical parameters and the number of spectra with sufficient quality for our analysis. The letter D in the object name column identifies dynamically confirmed BHs. A fiducial mass of 8 M_⊙ and a distance of 8 kpc were used when these values were not reliably known, including when dynamical constraints are only lower limits, according to the properties of the bulk of the Galactic BHLMXB population (see e.g., Corral-Santana et al. 2016). For inclination measurements, we highlight dippers in bold, and letters D, J, H, R respectively refer to dynamical inclination measurements (dips/eclipses/modulations), jets, heartbeats, and reflection fits. Details and references for line detection reports are provided in Table 2.

References. (1) Stecchini et al. (2020). (2) Orosz et al. (1998). (3) Orosz (2003). (4) Jonker & Nelemans (2004). (5) Park et al. (2004). (6) Kalemci et al. (2018). (7) Tomsick et al. (1998). (8) Gomez et al. (2015). (9) Maitra et al. (2013). (10) Yao et al. (2021). (11) Parmar et al. (1993). (12) Draghis et al. (2020). (13) Wang et al. (2020). (14) Van Der Hooft et al. (1998). (15) Beer & Podsiadlowski (2002). (16) Hjellming & Rupen (1995). (17) Kuulkers et al. (1998). (18) della Valle et al. (1994). (19) Bharali et al. (2019). (20) Greiner et al. (1996). (21) Miller et al. (2015b). (22) Reid et al. (2014). (23) Pahari et al. (2013). (24) Casares et al. (2009). (25) Pahari et al. (2017). (26) Heida et al. (2017). (27) Steiner et al. (2012). (28) Miller et al. (2006b). (29) Capitanio et al. (2012). (30) Rao & Vadawale (2012). (31) Xu et al. (2017). (32) Wang et al. (2018). (33) Grebenev et al. (2006). (34) Jaisawal et al. (2015). (35) Lazar et al. (2021). (36) Sánchez et al. (2021). (37) Shidatsu et al. (2013). (38) Lamer et al. (2021). (39) Carotenuto et al. (2022). (40) Titarchuk & Seifina (2023). (41) Chakraborty et al. (2021). (42) Chauhan et al. (2019). (43) Russell et al. (2019). (44) Dong et al. (2022). (45) Kuulkers et al. (2013). (46) Homan et al. (2021). (47) Torres et al. (2019). (48) Torres et al. (2020). (49) Atri et al. (2020). (50) Homan et al. (2018). (51) Corral-Santana et al. (2013). (52) Sánchez et al. (2015). (53) Xu et al. (2018b). (54) Xu et al. (2018a). (55) Cadolle Bel et al. (2007). (56) Reis et al. (2009). (57) Khargharia et al. (2010). (58) Miller-Jones et al. (2009). (59) Orosz et al. (2001). (60) Macdonald et al. (2014). (61) Orosz et al. (2011). (62) Connors et al. (2019). (63) Orosz et al. (2004). (64) Homan et al. (2006). (65) Chiang et al. (2012). (66) Chaty & Bessolaz (2006). (67) Ratti et al. (2012). (68) Miller-Jones et al. (2011). (69) García et al. (2018). (70) Sala et al. (2007). (71) Sriram et al. (2012).

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