The Rogers et al. white paper (arXiv:2605.26142, May 2026) correctly identifies that UV spectroscopy of polluted white dwarfs supplies the only direct bulk-composition measurements of rocky exoplanetary material, including the volatile budget (C, N, O, P, S) critical for habitability assessments. Yet the document understates the statistical fragility of the current sample: fewer than 30 systems have the full suite of rock-forming and volatile abundances required to map interior structure, a limitation that stems from HST's finite lifetime rather than intrinsic rarity. Extending COS and STIS operations to 2035 would more than double this sample before HWO launches, providing the empirical priors needed to interpret the far smaller number of directly imaged rocky worlds HWO is expected to characterize. Complementary work by Blouin et al. (2024, MNRAS) demonstrates that JWST MIRI photometry alone cannot distinguish between water-rich and dry mineralogies without the UV-derived Fe/Si and Mg/Si ratios; the synergy therefore is not additive but multiplicative. NASA’s 2023 HWO Science Case further reveals that the mission’s coronagraphic spectroscopy will be optimized for atmospheric retrievals, leaving bulk refractory abundances to be supplied externally—exactly the niche polluted white dwarfs fill. The white paper’s emphasis on “statistically significant samples” therefore translates into a concrete requirement: at least 80–100 systems with complete UV inventories before HWO’s 2035–2040 window, a threshold current HST scheduling cannot meet without protected UV time. Failure to secure this bridge risks leaving HWO’s biosignature detections interpretationally incomplete, repeating the post-Kepler situation in which occurrence rates outpaced compositional context.