Top-left panel: The Gaia DR3 distance distribution of the candidate members of Vel OB1 (cf. Tab. A.1); candidate members proposed by, respectively, Humphreys (1978) (orange) and Reed (2000) (blue) are indicated. A black vertical line represents the distance to a runaway with an observed bow shock (Runaways BS), and the green vertical lines to those without an observed bow shock (Runaways nBS). Lower panel: The Gaia DR3 proper motion of the candidate members of Vel OB1 (coloured circles) and runaways (triangles). Runaway stars with and without an associated bow shock are labelled black and green, respectively. Open circles are non-members (see Tab. A.1). Open triangles refer to candidate runaways (see Tab. A.2). The red cross indicates the proper motion of Vel OB1 as reported by Mel’nik & Dambis (2017). The red dashed ellipse indicates a tangential peculiar velocity of 15 km s⁻¹ with respect to the mean proper motion of the young massive clusters in Vel OB1. Top-right panel: The proper motion distribution of the members of young clusters in Vel OB1. The [KPS2012] MWSC 1594 open cluster and IRAS 08337-4028 are indicated as Cl 1594 and IRAS 08337, respectively.