The abundances of other elements are increased as well, in particular that of nitrogen which can be enhanced by a factor 4-5 (Van Rensbergen priv. comm.).

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From a list of O and B stars with $v_{\rm rad} > 30$ km s^-1 provided by the late Jan van Paradijs.

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... runaways)

The sample criteria exclude the known runaways, e.g., $\alpha$ Cam, 68 Cyg (Blaauw 1993), HIP 35707 (Comerón et al. 1998), and HIP 60350 (Maitzen et al. 1998) which all have distances larger than 1 kpc.

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... PSR J1932+1059

Recently, Walter (2000) suggested that RX J185635-3754 as another candidate neutron star that could have encountered $\zeta$ Oph in the past. We show in Appendix B that this is unlikely.

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...)

Upoints in the direction of the Galactic centre, V points in the direction of Galactic rotation, and W points towards the North Galactic pole.

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... distance

The Hipparcos parallax of $\mu$ Col ( $2.52\pm0.55$ mas) deviates more than 1.5 $\sigma$ from the photometric parallax ( $\sim$ 1.3 mas). The random realisations of $\pi_{\mu~{\rm Col}}$ which are consistent with $\pi_{\rm phot}$ thus need to fall outside the -1.5 $\sigma$ confidence level which occurs in fewer than 10% of the cases.

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... 53 Ari

The Hipparcos Input Catalogue (Turon et al. 1992) lists the radial velocity from the Catalogue de Vitesses Radiales Moyennes Stellaires (Barbier-Brossat 1989) which is incorrect (-8.5 km s^-1). The radial velocity in the Troisième Catalogue Bibliographique de Vitesses Radiales Stellaires (Barbier-Brossat et al. 1994) is also incorrect. They list a radial velocity corrected for Solar motion of 15.3 km s^-1 adopted from Sterken (1988). The uncorrected radial velocity is 24.2 km s^-1.

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...)

We assume that Vel R2 has a motion similar to all other groups in the direction of the constellation Vela, i.e., $\sim$ 20 km s^-1, almost independent of distance.

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... HIP 29678

HIP 29678 is a visual double star. Gies & Bolton (1986) did not detect any radial velocity variations.

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...)

Dolan & Mathieu (1999) report that long term monitoring of $\lambda$ Ori's radial velocity indicates that this star is a binary with a systematic velocity ( $v_{\rm rad} \sim 18$ km s^-1) which differs by 6-8 km s^-1 from that of the clusters in the $\lambda$ Ori region. However, the simulations show that $\lambda$ Ori cannot be related to the event that created the runaways HIP 22061 and HIP 29678.

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