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We use surface brightness fluctuation (SBF) measurements to constrain thedistance to low surface brightness (LSB) dwarfs in the vicinity of M101. Recentwork has discovered many LSB candidate satellite companions of M101. However,without accurate distances, it is problematic to identify these dwarfs asphysical satellites of M101. We use CFHT Legacy Survey (CFHTLS) data to measurethe SBF signal for 43 candidate dwarfs. The data is deep enough that weconstrain 29 of these to be unassociated background galaxies by their lack ofSBF. We measure high S/N SBF signals for two of the candidate dwarfs, which areconsistent with being at the distance of M101. The remaining candidates are tooLSB and/or small for their distances to be constrained. Still, by comparisonwith Local Group dwarfs, we argue that the M101 satellite system is likely nowcomplete down to stellar masses of $\sim5\times10^5$ M$_\odot$. We also providea new SBF distance for the nearby dwarf UGC 8882, which suggests that it issignificantly outside of the virial radius of M101 and is thus not a physicalsatellite. By constraining the distances to a majority of the candidates usingonly archival data, our work demonstrates the usefulness of SBF for nearby LSBgalaxies and for studying the satellite systems of nearby massive galaxies.

Using Surface Brightness Fluctuations to Study Nearby Satellite Galaxy Systems: the Complete Satellite System of M101