MW-mass SIDM halos bypass core formation and enter immediate core collapse due to baryonic preconditioning, allowing the compact stellar disk and bulge to survive close pericenter passages while the diffuse halo is more easily disrupted.
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Baryonic feedback mildly delays but does not stall gravothermal collapse in high-concentration SIDM halos and allows resumption in median-concentration cases, yielding feedback-history-dependent central densities.