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Table 5.

HIPPARCOS astrometry from van Leeuwen (2007) of bright stellar members in Sco-Cen.

HIP Name SigMA(a) SpT HIPPARCOS
 Gaia DR3
l b ϖ μδ ϖ μδ
(deg) (mas) (mas yr−1) (mas) (mas yr−1)
80473 * rho Oph 1 B2V 353.69 17.69 9.03 ± 0.90 −5.53 ± 0.89 −21.74 ± 0.93 7.26 ± 0.13 −4.38 ± 0.19 −23.30 ± 0.16
79374 * nu Sco (Jabbah) 2 B2IV 354.61 22.70 6.88 ± 0.76 −7.65 ± 0.71 −23.71 ± 0.47 7.06 ± 0.22 −7.44 ± 0.25 −28.20 ± 0.16
78401 * del Sco (Dschubba) 3 B0.2IV 350.10 22.49 6.64 ± 0.89 −10.21 ± 1.01 −35.41 ± 0.71
78820 * bet Sco (Acrab) 4 B0.5V 353.19 23.60 8.07 ± 0.78 −5.20 ± 0.92 −24.04 ± 0.64
80112 * sig Sco (Alniyat) 5 B1III 351.31 17.00 4.68 ± 0.60 −10.60 ± 0.78 −16.28 ± 0.43
79404 * c02 Sco 5 B2V 348.12 16.84 6.81 ± 0.16 −10.38 ± 0.18 −23.94 ± 0.14 6.78 ± 0.14 −12.26 ± 0.18 −24.25 ± 0.14
81266 * tau Sco 6 B0V 351.53 12.81 6.88 ± 0.53 −9.89 ± 0.61 −22.83 ± 0.55
80763 * alf Sco (Antares) 6 M1Ib + B2.5V 351.95 15.06 5.89 ± 1.00 −12.11 ± 1.22 −23.30 ± 0.76
78104 * rho Sco (Iklil) 7 B2IV/V 344.63 18.27 6.91 ± 0.19 −15.68 ± 0.21 −24.88 ± 0.19 7.32 ± 0.29 −17.03 ± 0.33 −23.66 ± 0.27
78265 * pi Sco 9 B1V + B2V 347.21 20.23 5.57 ± 0.64 −11.42 ± 0.78 −26.83 ± 0.74 9.67 ± 0.70 −12.40 ± 0.52 −26.21 ± 0.57
81477 V* V1062 Sco 10 Ap Si 343.57 5.18 7.54 ± 0.61 −10.25 ± 0.69 −21.59 ± 0.45 5.72 ± 0.03 −12.45 ± 0.04 −21.17 ± 0.04
82545 * mu02 Sco (Pipirima) 10 B2IV 346.20 3.86 6.88 ± 0.12 −11.09 ± 0.13 −23.32 ± 0.11 5.66 ± 0.28 −12.11 ± 0.30 −22.57 ± 0.27
82514 * mu01 Sco (Xamidimura) 11 B1.5IV + B 346.12 3.91 6.51 ± 0.91 −10.58 ± 0.87 −22.06 ± 0.74
78533 V* LL Lup 13 Ap Si 339.64 11.41 8.61 ± 0.69 −12.65 ± 0.75 −24.14 ± 0.68 6.18 ± 0.03 −12.18 ± 0.03 −24.02 ± 0.02
78384 * eta Lup 14 B2.5IV 338.77 11.01 7.38 ± 0.18 −16.96 ± 0.19 −27.83 ± 0.19 7.59 ± 0.43 −17.59 ± 0.49 −27.26 ± 0.37
71865 * b Cen 15 B2.5V 325.90 20.10 9.62 ± 0.18 −29.92 ± 0.14 −30.68 ± 0.13 10.03 ± 0.31 −29.83 ± 0.37 −31.91 ± 0.52
76945 * psi02 Lup 15 B5V 338.48 16.08 8.97 ± 0.27 −21.37 ± 0.30 −29.98 ± 0.25
75304 * phi02 Lup 15 B4V 333.84 16.75 6.28 ± 0.20 −18.24 ± 0.22 −20.72 ± 0.16 6.49 ± 0.22 −18.47 ± 0.30 −20.41 ± 0.29
71860 * alf Lup 17 B1.5III 321.61 11.44 7.02 ± 0.17 −20.94 ± 0.14 −23.67 ± 0.14
74449 * e Lup 17 B3IV 327.83 11.43 6.47 ± 0.21 −22.01 ± 0.18 −21.75 ± 0.19 7.24 ± 0.20 −21.67 ± 0.20 −21.90 ± 0.18
76371 * d Lup 17 B3IVp 331.02 8.76 7.62 ± 0.43 −20.53 ± 0.33 −21.23 ± 0.31 6.85 ± 0.13 −20.79 ± 0.15 −20.79 ± 0.11
71536 * rho Lup 19 B5V 320.13 9.86 10.32 ± 0.16 −28.26 ± 0.12 −28.82 ± 0.13 9.35 ± 0.20 −28.92 ± 0.22 −29.21 ± 0.32
72800 V* V1019 Cen 20 B7II/III 327.93 19.11 6.63 ± 0.22 −20.48 ± 0.23 −19.20 ± 0.22 6.96 ± 0.17 −20.60 ± 0.16 −20.35 ± 0.20
67464 * nu Cen 20 B2IV 314.41 19.89 7.47 ± 0.17 −26.77 ± 0.12 −20.18 ± 0.08 8.05 ± 0.35 −26.14 ± 0.42 −21.23 ± 0.94
63945 * f Cen 21 B5V 305.47 14.34 8.36 ± 0.25 −29.85 ± 0.18 −15.17 ± 0.15 8.16 ± 0.16 −29.56 ± 0.12 −15.69 ± 0.10
60823 * sig Cen 21 B3V 299.10 12.47 7.92 ± 0.18 −32.36 ± 0.15 −12.51 ± 0.13 7.92 ± 0.23 −32.17 ± 0.18 −13.17 ± 0.16
60009 * zet Cru 22 B2.5V 299.32 −1.36 9.12 ± 0.45 −33.80 ± 0.48 −10.15 ± 0.43
60718 * alf Cru (Acrux) 22 B0.5IV 300.13 −0.36 10.13 ± 0.50 −35.83 ± 0.47 −14.86 ± 0.43
58484 * eps Cha 24 B9Vn 300.21 −15.62 9.02 ± 0.36 −40.34 ± 0.38 −8.30 ± 0.40
42637 * eta Cha 24 B9IV 292.40 −21.65 10.53 ± 0.16 −28.89 ± 0.16 27.21 ± 0.16 10.17 ± 0.07 −29.43 ± 0.18 26.83 ± 0.12
84970 * tet Oph 28 B2IV 0.46 6.55 7.48 ± 0.17 −7.37 ± 0.18 −23.94 ± 0.10
86670 * kap Sco 31 B1.5III 351.04 −4.72 6.75 ± 0.17 −6.05 ± 0.21 −25.54 ± 0.13

Notes. The Gaia DR3 astrometry is given if available. Shown are mostly B-type stars that are either part of the SigMA-selected clusters or which are the name-givers of some clusters. This is not a complete list of B-stars in Sco-Cen. The HIPPARCOS astrometry can be compared to average parameters of the SigMA clusters as derived from Gaia astrometry in Tables 3–4, to evaluate possible correlations. The HIPPARCOS parallaxes should be treated with caution, since significant deviations to Gaia parallaxes are possible (on the order of about 60 pc when converted to distances), while proper motions show deviations on the order of about ±2 mas yr−1, when comparing sources that are both in HIPPARCOS and Gaia DR3 within about 500 pc from the Sun.

(a)

Column 3 gives the index of the SigMA cluster that is hosting the given star.

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