A search for signatures of interactions of X-ray binary outflows with their environments with ALMA

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Table 1.

Observation log. LMXB and HMXB correspond to low-mass and high-mass X-ray binaries, respectively.

Source	Type	Compact	Orbital	Distance	Inclination	Observation date
		object	period (d)	(kpc)	(°)
Cir X-1	HMXB/LMXB?⁽¹⁾	NS⁽²⁾	16.6⁽³⁾	9.4⁽⁴⁾	≲70⁽⁵⁾	23 Oct. 2016 17:26–18:45
Sco X-1	LMXB⁽⁶⁾	NS⁽⁶⁾	0.79⁽⁷⁾	2.8⁽⁸⁾	≳40⁽⁹⁾	25 Oct. 2016 16:50–17:38
GRS 1915+105	LMXB⁽¹⁰⁾	BH⁽¹¹⁾	33.8⁽¹²⁾	8.6⁽¹³⁾	66 ± 2⁽¹¹⁾	25 Oct. 2016 17:41–18:23
GX 13+1	LMXB⁽¹⁴⁾	NS⁽¹⁴⁾	24.5⁽¹⁵⁾	7⁽¹⁶⁾	≲70⁽¹⁷⁾	05 Nov. 2016 22:46–23:27
Cyg X-1	HMXB⁽¹⁸⁾	BH⁽¹⁹⁾	5.6⁽²⁰⁾	2.22⁽²¹⁾	27.1 ± 0.8⁽¹⁹⁾	06 Nov. 2016 21:02–22:02
						29 Nov. 2016 20:39–21:40

Notes. NS and BH indicate the nature of the compact object in the X-ray binary, neutron star or black hole, respectively. We note that Cyg X-1 had to be observed on two different days to reach the requested sensitivity.

⁽¹⁾

References. Jonker et al. (2007), Johnston et al. (2016);

⁽²⁾

Tennant et al. (1986), Linares et al. (2010);

⁽³⁾

Kaluzienski et al. (1976);

⁽⁴⁾

Heinz et al. (2015);

⁽⁵⁾

From the presence of dips in its light curve (Clarkson et al. 2004);

⁽⁶⁾

Steeghs & Casares (2002);

⁽⁷⁾

Gottlieb et al. (1975);

⁽⁸⁾

Bradshaw et al. (1999);

⁽⁹⁾

Mata Sanchez et al. (2015);

⁽¹⁰⁾

Greiner et al. (2001a);

⁽¹¹⁾

Greiner et al. (2001b);

⁽¹²⁾

Steeghs et al. (2013);

⁽¹³⁾

Reid et al. (2014);

⁽¹⁴⁾

Fleischman (1985), Matsuba et al. (1995);

⁽¹⁵⁾

Bandyopadhyay et al. (2002);

⁽¹⁶⁾

Bandyopadhyay et al. (1999);

⁽¹⁷⁾

From the presence of dips in its light curve (Díaz Trigo et al. 2012; Iaria et al. 2014);

⁽¹⁸⁾

Webster & Murdin (1972);

⁽¹⁹⁾

Orosz et al. (2011);

⁽²⁰⁾

Holt et al. (1979);

⁽²¹⁾

Miller-Jones et al. (2021).

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