Left panel: fraction of main sequence stars on radial orbits (e > 0.9) with apocenters in the range 10 < r_apo/kpc < 25 as a function of metallicity. Here, we only consider stars with eccentricity e > 0.5 in order to exclude disk stars. The navy blue and dark red dotted lines gives the fractions for toy models with isotropic and radial (β = 0.5) orbits, respectively. The “sausage stars” are discernible down to [Fe/H] ∼ −2, but they become more evident at higher metallicity. Right panel: metallicity distribution of high-eccentricity (e > 0.9) stars (dashed dark red line). For comparison, we show the distribution for stars with eccentricity 0.4 < e < 0.8 (solid navy blue line). The “sausage” progenitor has higher median metallicity than the average halo population ([Fe/H] = −1.5), and is likely at least as massive as the Sagittarius dSph (M_star ≳ 10⁸ M_⊙).