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Using cosmological hydrodynamical zoom-in simulations, we explore theproperties of subhalos in Milky Way analogs that contain a sub-component ofAtomic Dark Matter (ADM). ADM differs from Cold Dark Matter (CDM) due to thepresence of self interactions that lead to energy dissipation and bound-stateformation, analogous to Standard Model baryons. This model can arise in complexdark sectors that are natural and theoretically-motivated extensions to theStandard Model. The simulations used in this work were carried out using GIZMOand utilize the FIRE-2 galaxy formation physics in the Standard Model baryonicsector. For the parameter points we consider, the ADM gas cools efficiently,allowing it to collapse to the center of subhalos. This increases a subhalo'scentral density and affects its orbit, with more subhalos surviving smallpericentric passages. The subset of subhalos that host visible satellitegalaxies have cuspier density profiles and smaller stellar-half-mass radiirelative to CDM. The entire population of dwarf galaxies produced in the ADMsimulations is much more compact than those seen in CDM simulations, unable toreproduce the entire diversity of observed dwarf galaxy structures.Additionally, we also identify a population of highly compact subhalos thatconsist nearly entirely of ADM and form in the central region of the host,where they can leave distinctive imprints in the baryonic disk. This workpresents the first detailed exploration of subhalo properties in a stronglydissipative dark matter scenario, providing intuition for how other regions ofADM parameter space, as well as other dark sector models, would impactgalactic-scale observables.

Dissipative Dark Substructure: The Consequences of Atomic Dark Matter on Milky Way Analog Subhalos