Left: the fraction of systems that would be detectable after 1 Gyr as a function of the total mass in surviving terrestrial planets for six different wavelengths between 5 and 500   μm. Each curve represents a horizontal slice through Fig. 15 at a different vertical height. The chosen “detection limits” in F/F_star were: 10^-8 at 5   μm, 10^-3 at 15   μm, 0.054 at 25   μm, 0.55 at 70   μm, 10 at 160   μm, and 100 at 500   μm. The error bars are 1-σ and were calculated using binomial statistics (Burgasser et al. 2003). Note that the different curves are offset by up to  ± 0.1   M_⊕ for clarity. The bins themselves are at: zero, 0−1   M_⊕, 1−2   M_⊕, 2−3   M_⊕, and  > 3   M_⊕. Right: the fraction of systems with 0.5   M_⊕ or more in terrestrial planets as a function of F/F_star(70   μm) (1 Gyr). Systems with F/F_star < 10^-2 are included in the bin at F/F_star ≈ 10^-2. The Spitzer detection limit is shown as the dashed line. This represents a vertical slice through Fig. 14.