Title: Caught in the Act of Quenching? Local Volume Dwarf Satellites with On-Going Star 
Formation

Abstract:
The majority of dwarf satellites in the Local Group are gas-devoid dwarf spheroidal galaxies; 
however, dwarf systems at larger separations from the Milky Way or M31 tend to have gas 
reserved and show recent or ongoing star formation (dwarf Irregulars). Historically termed the 
density-morphology relationship (Grebel 1999), this dichotomy is demonstrated across the 
SDSS volume (Geha et al 2012) and, with comparisons to numerical simulations, implies the e-
folding quenching timescale for dwarf systems is ~1 Gyr (Wetzel et al. 2013). Given the long 
dynamical timescales associated with interactions of this mass ratio, this occurs quickly and 
the relative dearth of intermediate morphological systems in the Local Group is a natural 
consequence. 
In a survey for tidal stream debris in the Local Volume (Martinez-Delgado et al. 2010), we have 
discovered dwarf satellites with tidal debris, whose morphologies are not seen in the Local 
Group census. The bright satellite of NGC5387 is currently in undergoing a starburst (Beaton et 
al. 2014) and the stellar tidal debris of IC2209 (interacting with NGC2460) contains several HII 
regions (Beaton et al. in prep). The dynamical morphologies of the stellar tidal debris estimate 
that these interactions are relatively young, with the debris forming in less than 1 Gyr -- 
suggesting that these mergers could probe the quenching process and offer a unique window 
into this evolutionary phase of dwarf satellites. Using N-body simulations, we study the later 
stages of the merger to connect these unique cases to canonical satellites and debris in the 
Local Group to draw inferences on their earlier evolution. Lastly, we discuss how studies of 
intermediate aged stellar populations in the Milky Way and M31 haloes can elucidate the 
fraction of dwarf systems whose star formation continues through the early stages of their 
accretion.