Notes. Columns 1–4 give, respectively, the binaries’ primary (the more massive member) ZAMS mass, M_ZAMS, 1, secondary ZAMS mass, M_ZAMS, 2, initial semi-major-axis, a₀, and initial eccentricity, e₀. When the outcome of the binary evolution is two compact remnants, their masses are indicated across a “+” symbol in Cols. 5 and 6; the left and the right side mass are the derivative of the primary and secondary stellar member, respectively. If the two remnants remain bound, then the semi-major-axis (R_⊙) and eccentricity of the double-compact binary are also indicated at selected evolutionary times (indicated in parentheses). If the binary becomes detached in the course of evolution (due to e.g. SN natal kick), then only the remnant mass pair is indicated. If the binary evolution leads to only one remnant (due to star-star or star-remnant merger), then just this remnant’s mass is indicated. Owing to the adopted NS upper mass limit, a remnant of > 2.5 M_⊙ (≤2.5 M_⊙) is a BH (NS). These BSE and StarTrack evolutions are done for the F12-rapid+B16-PPSN/PSN remnant-mass model with the same choices of evolutionary parameters; the values of the most relevant parameters are Z = 0.0001, α_CE = 1.0, and f_mrg = 0.5.