Characteristic strain $h_c={\mathcal{A}}_{\mathrm{gw}}\sqrt{f_{\mathrm{gw}}{T}_{\mathrm{obs}}}$ of resolved double white dwarf binaries in our mock simulation for a mission duration of T_obs = 4 yr. Triples are shown with green points, and the isolated binary channel is shown with purple points. This is compared to the LISA instrumental noise (black solid line). Triples with highly eccentric orbits (e > 0.9) and other low signal-to-noise sources are marked in black and dark gray markers, respectively. The confusion background from the Galactic double white dwarf population is represented by green, purple, and orange lines for triples, binaries, and their combined contribution, respectively. All the eccentric systems (black markers) tend to have a narrow periapsis time (10⁴ s), and hence they occupy a narrow frequency range. The astrophysical noise from these backgrounds remains significantly lower than the instrumental noise.