**Table 8:** The widest known binary systems in Sco OB2. For each of these binary systems we list the angular separation, the *Hipparcos* parallax, an estimate for the semi-major axis $a_{\rm est} \equiv D\tan \rho$ , the subgroup, and the spectral type of the primary. The last column lists the reference. Note that this list must be incomplete, as very wide binaries are difficult to detect. Furthermore, several of these binaries may be optical due to confusion with background stars, i.e., not physically bound. References: (1) Lindroos (1985); (2) Worley (1978); (3) Worley & Douglass (1997); (4) Oblak (1978); (5) Tokovinin (1997).
Member	$\rho$	$\pi$	$a_{\rm est}$	Group	SpT	Ref.
HIP	arcsec	mas	$10^6~{R}_\odot$
64004	25.1	7.92	0.68	LCC	B1.5V	1
71860	27.6	5.95	0.99	UCL	B1.5III	2
69113	28.6	4.57	1.34	UCL	B9V	1
75647	30.0	7.79	0.82	UCL	B5V	3
69749	30.2	4.07	1.59	UCL	B9IV	4
60320	32.4	9.71	0.71	LCC	Am	3
69618	33.9	6.71	1.08	UCL	B4Vne	3
77315	34.7	7.64	0.97	UCL	A0V	3
63003	34.8	8.64	0.86	LCC	B2IV-V	1
72192	35.3	7.72	0.98	UCL	A0V	1
78104	38.3	7.97	1.03	US	B2IV/V	3
72984	39.0	5.93	1.41	UCL	A0/A1V	3
79374	41.4	7.47	1.19	US	B2IV	5
83693	43.3	7.73	1.20	UCL	A2IV	3
80024	46.7	6.98	1.43	US	B9II/III	4
67472	48.0	6.19	1.66	UCL	B2IV/Ve	3
78265	49.2	7.10	1.48	US	B1V+B2V	3
64661	60.0	8.04	1.60	LCC	B8V	1
65271	60.0	9.20	1.40	LCC	B3V	5
78384	115.0	6.61	3.73	UCL	B2.5IV	5

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