Dark-Matter-Deficient Galaxies from Collisions: A New Probe of Bursty Feedback and Dark Matter Physics

High-velocity collisions between gas-rich ultra-diffuse galaxies present a promising formation channel for dark-matter-deficient galaxies (DMDGs). Using hydrodynamical simulations, we show that the progenitors’ baryonic binding energy, $\mathrm{\mid }{E}_{\mathrm{b}\mathrm{i}\mathrm{n}\mathrm{d}}\mathrm{\mid }$, critically controls the outcome. Repeated potential fluctuations, e.g., from bursty feedback, inject energy and reduce $\mathrm{\mid }{E}_{\mathrm{b}\mathrm{i}\mathrm{n}\mathrm{d}}\mathrm{\mid }$ by $\approx 15\mathrm{\%}$, yielding fewer but substantially more massive DMDGs. By contrast, elastic self-interacting dark matter (SIDM) produces comparable cores without lowering $\mathrm{\mid }{E}_{\mathrm{b}\mathrm{i}\mathrm{n}\mathrm{d}}\mathrm{\mid }$, 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 $>100\mathrm{\%}$ mass enhancements. The simulations also predict systematically lower gas fractions due to sustained post-collision 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.