Notes. The left side of the table provides information associated with the runaway stars, while the right side provides information associated with the corresponding bow shock and bubble candidates. Spectral types (STs) were taken from the GOSC (Maíz Apellániz et al. 2013) and the BeSS (Neiner et al. 2011) catalogs. Ṁ, mass-loss rates, were linearly interpolated from Vink & Sander (2021). Wind terminal velocities were obtained by applying a linear regression to Vink & Sander (2021) data. Radial velocity references: (1) de Bruijne & Eilers (2012); (2) Kobulnicky & Chick (2022); (3) Kharchenko et al. (2007). $V_{\text{PEC}}^{2\text{D}}$ are those from Carretero-Castrillo et al. (2023) and $V_{\text{PEC}}^{3\text{D}}$ are obtained with the same methodology using the quoted υ_r values (see text for details). The right side of the table provides the classification id of the IR structure around the runaway star: BS for bow shocks; BU for bubbles; and BU/BS and BS/BU for intermediate structures between BS and BU. R is the projected standoff distance from the star to the midpoint of the bow shock, l is the length, and w is the width of the bow shock structure. These distances are projected in the plane of the sky. For bubbles, only the width was measured. Column e provides the eccentricity of the ellipse used to measure the bow shocks. $n_{\text{ISM}}^{2\text{D}}$ and $n_{\text{ISM}}^{3\text{D}}$ are the ISM densities of the medium around the bow shock position considering either $V_{\text{PEC}}^{2\text{D}}$ or $V_{\text{PEC}}^{3\text{D}}$ as V_PEC in Eq. (1). The horizontal line separates O-type stars (upper part) from Be-type stars (bottom part). This table is available at the CDS.