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We present a suite of 16 high-resolution hydrodynamic simulations of anisolated dwarf galaxy (gaseous and stellar disk plus a stellar bulge) within aninitially cuspy dark matter (DM) halo, including self-interactions between theDM particles (SIDM); as well as stochastic star formation and subsequentsupernova feedback (SNF), implemented using the stellar feedback model SMUGGLE.The simulations start from identical initial conditions and we regulate thestrength of SIDM and SNF by systematically varying the SIDM momentum transfercross section and the gas density threshold for star formation. The DM haloforms a constant density core of similar size and shape for severalcombinations of those two parameters. Haloes with cores that are formed due toSIDM (adiabatic cusp-core transformation) have velocity dispersion profileswhich are closer to isothermal than those of haloes with cores that are formeddue to SNF in simulations with bursty star formation (impulsive cusp-coretransformation). Impulsive SNF can generate positive stellar age gradients andincrease random motion in the gas at the centre of the galaxy. Simulatedgalaxies in haloes with cores that were formed adiabatically are spatially moreextended, with stellar metallicity gradients that are shallower (at late times)than those of galaxies in other simulations. Such observable properties of thegas and the stars, which indicate either an adiabatic or an impulsive evolutionof the gravitational potential, may be used to determine whether observed coresin DM haloes are formed through self-interactions between the DM particles orin response to impulsive SNF.

Degeneracies Between Self-interacting Dark Matter and Supernova Feedback as cusp-core transformation mechanisms