Table 1.
Parameters of the systems studied (see Sect. 2 for a discussion on their possible uncertainties).
| Parameter | Symbol | System |
||||
|---|---|---|---|---|---|---|
| BD+43°3654 | BD+60° 2522 | G1 | G3 | Vela X-1 | ||
| Peculiar velocity | V⋆ [km s−1] | 50(a, b) | 42(b) | 20(b) | 22(b) | 65(b) |
| Ambient density | nISM [cm−3] | 6 | 27 | 30 | 30 | 2 |
| Spectral type | O4If(c) | O6.5V(d) | O7V(e) | O5V(e) | B0.5Ia(f) | |
| Wind velocity | vw [km s−1] | 3000(g) | 2000(h) | 2100(e) | 2000(e) | 700(i) |
| Wind mass-loss rate | Ṁw [M⊙ yr−1] | 4 × 10−6 (h) | 1.3 × 10−6 (j) | 2.2 × 10−7 (e) | 4 × 10−7 (e) | 1 × 10−6 (i) |
| Distance | d [kpc] | 1.72(b) | 2.99(b) | 2.02(b) | 1.79(b) | 1.79(b) |
Notes. (a)Benaglia et al. (2021); (b)Gaia Collaboration (2021); stellar velocities are estimations based on tangential components; (c)Peri et al. (2012); (d)Sota et al. (2011); (e)Peri et al. (2015); (f)Houk (1978); (g)Muijres et al. (2012); (h)Moutzouri et al. (2022); (i)Grinberg et al. (2017); (j)Toalá et al. (2020). The ambient densities are calculated in terms of the projections R0, proj in the plane of the sky reported by Peri et al. (2012, 2015), Benaglia et al. (2021), Moutzouri et al. (2022) and Gvaramadze et al. (2018). We assume solar abundances.
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