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While dwarf galaxies observed in the field are overwhelmingly star-forming,dwarf galaxies in environments as dense or denser than the Milky Way areoverwhelmingly quenched. In this paper, we explore quenching in the lowerdensity environment of the Small-Magellanic-Cloud-mass galaxy NGC 3109($\text{M}_* \sim 10^8 \, \text{M}_\odot$), which hosts two known dwarfsatellite galaxies (Antlia and Antlia B), both of which are HI deficientcompared to similar galaxies in the field and have recently stopped formingstars. Using a new semi-analytic model in concert with the measured starformation histories and gas masses of the two dwarf satellite galaxies, we showthat they could not have been quenched solely by direct ram pressure strippingof their interstellar media, as is common in denser environments. Instead, wefind that separation of the satellites from pristine gas inflows, coupled withstellar-feedback-driven outflows from the satellites (jointly referred to asthe starvation quenching model), can quench the satellites on timescalesconsistent with their likely infall times into NGC 3109's halo. It is currentlybelieved that starvation is caused by "weak" ram pressure that preventslow-density, weakly-bound gas from being accreted onto the dwarf satellite, butcannot directly remove the denser interstellar medium. This suggests thatstar-formation-driven outflows serve two purposes in quenching satellites inlow-mass environments: outflows from the host form a low-density circumgalacticmedium that cannot directly strip the interstellar media from its satellites,but is sufficient to remove loosely-bound gaseous outflows from the dwarfsatellites driven by their own star formation.

The Dual Role of Outflows in Quenching Satellites of Low-Mass Hosts: NGC 3109