Table A.1
Ionizing stars toward the Ophiuchus complex (see Figure 1)
| Name | Spectral Type | V (mag) | log QH/1 s−1 | Distance (pc) | WISE neb | Hα neb |
|---|---|---|---|---|---|---|
| Antares | M0.5Iab+B3V | 0.91 | 46.37 | 170 ± 29 | Yes | Yes |
| δ Sco | B0.2IVe | 2.32 | 47.99 | 151 ± 20 | Yes | Yes |
| ζ Oph | O9.2IV | 2.56 | 48.36 | 112 ± 2 | Yes | Yes |
| β Sco | B1V | 2.62 | 47.28 | 124±12 | Yes | Yes |
| τ Sco | B0.2V | 2.81 | 47.70 | 145±12 | Yes | Yes |
| σ Sco | B1III+B1V | 2.89 | 47.99 | 214±27 | Yes | Yes |
| π Sco | B1V+B2 | 2.91 | 47.40 | 180±20 | Yes | Yes |
| ρ Sco | B2IV-V | 3.86 | 46.96 | 145±4 | Yes | No |
| 9 Sco | B1V | 3.97 | 47.28 | 145±6 | Yes | No? |
| ν Sco | B2V | 4.00 | 46.80 | 145±17 | Yes | Yes |
| χ Oph | B2Vne | 4.43 | 46.80 | 161±6 | Yes | Yes |
| 13 Sco | B2V | 4.57 | 46.80 | 147±4 | Yes | Yes |
| 2 Sco | B2.5Vn | 4.59 | 46.59 | 154±12 | Yes | No? |
| ρ Oph | B2V-B3V | 4.63 | 46.93 | 111±11 | Yes | Yes |
| b Sco | B1.5Vn | 4.64 | 47.05 | 152±6 | Yes | No? |
| i Sco | B3V | 4.79 | 46.37 | 127±4 | Yes | Yes? |
| λ Lib | B3V | 5.03 | 46.37 | 95 ± 8 | Yes | No |
| V1040 Sco | B2V | 5.40 | 46.80 | 131±6 | No | No |
| HR5934 | B3V | 5.85 | 46.37 | 141±6 | No | No |
| HD147889 | B2III/IV | 7.90 | 47.44 | 118±12 | Yes | Yes |
Notes. Distances are taken from van Leeuwen (2007). North et al. (2007) derived a closer distance of ![$\[174_{-18}^{+23}\]$](/articles/aa/full_html/2025/05/aa52881-24/aa52881-24-eq4.png)
pc to σ Sco from the orbital solution of the spectroscopic pair. Elias 2-9 (HD147889), in the vicinity of L1688, is extincted by about 5 mag of visual extinction (Lombardi et al. 2008a) and is then intrinsically brighter than the observed V = 7.9 mag.
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