Circumsecondary in situ formation: Initial planet location relative to the disk truncation radius ($a_{\mathrm{p},0}/R_{\text{trunc}}^{\mathrm{\prime }}$, top), the primary star’s Hill radius (a_p,0/R_Hill,2, bottom). Top panel: Color bar shows the final planet mass and the gray dashed line marks $0.4\cdot R_{\text{trunc}}^{\mathrm{\prime }}$. Bottom panel: Color bar shows the binary mass ratio and the gray and black dashed lines mark 1/3 and 1/2 · R_Hill,2. Circles denote surviving planets, while crosses indicate planets lost by ejection or instability from close encounters with the central star.