Abstract High-velocity collisions between gas-rich ultradiffuse galaxies present a promising formation channel for dark-matter-deficient galaxies (DMDGs). Using hydrodynamical simulations, we show that the progenitors’ baryonic binding energy, ∣ E bind ∣, critically controls the outcome. Repeated potential fluctuations, e.g., from bursty feedback, inject energy and reduce ∣ E bind ∣ by ≈15%, yielding fewer but substantially more massive DMDGs. By contrast, elastic self-interacting dark matter (SIDM) produces comparable cores without lowering ∣ E bind ∣, perturbing DMDG masses without clear enhancement. This differs from what happens in host halos, where SIDM-induced cores enhance dark matter tidal stripping while keeping baryons compact and resilient to tidal effects. The contrasting roles of SIDM may provide a means to distinguish feedback-formed halo cores from those created by SIDM. Among 15 paired simulation runs, 13 show higher DMDG masses in the weakened-binding case, and about two-thirds exhibit >100% mass enhancements. The simulations also predict systematically lower gas fractions due to sustained postcollision star formation, yielding a clean observational signature. Upcoming wide-field imaging (CSST, LSST), HI surveys (FAST), and kinematic follow-up will be crucial to test this scenario.
Wang et al. (Wed,) studied this question.