Astrometric signature vs. orbital period for the simulated binary sources (orange), the 384 DR3 NSS ORBT solutions (magenta), the 1332 DR3 NSS ASB1 solutions (blue) and the currently confirmed exoplanets (Schneider et al. 2011) (gray). The red dashed vertical line represents the DR3 time baseline of 34 months in comparison to the shorter periods of the Gaia DR3 unresolved binary orbital solutions. For the DR3 NSS solutions we used the expression α=a₀/d to compute the astrometric signature. a₀ was computed using the Thiele-Innes elements (A, B, F, G) of the corresponding Gaia DR3 NSS solution and the recipe available in Halbwachs et al. (2023, Appendix A), and d was computed as the inverse of the source parallax. For the simulated sources we used α=M₂/M₁ × a₁/d from Perryman et al. (2014), where M₁ and M₂ are the primary and secondary masses, respectively, and a₁ is the semimajor axis of the orbit of the secondary.