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We use time-resolved spectra from the Apache Point Observatory GalacticEvolution Experiment (APOGEE) to examine the distribution of radial velocity(RV) variations in 249 stars identified as members of the Sagittarius (Sgr)dwarf spheroidal (dSph) galaxy by Hayes et al (2020). We select Milky Way (MW)stars that have stellar parameters ($log(g)$, $T_{eff}$, and $[Fe/H]$) similarto those of the Sagittarius members by means of a k-d tree of dimension 3. Wefind that the shape of the distribution of RV shifts in Sgr dSph stars issimilar to that measured in their MW analogs, but the total fraction of RVvariable stars in the Sgr dSph is larger by a factor of $\sim 2$. After rulingout other explanations for this difference, we conclude that the fraction ofclose binaries in the Sgr dSph is intrinsically higher than in the MW. Wediscuss the implications of this result for the physical processes leading tothe formation of close binaries in dwarf spheroidal and spiral galaxies.

Multiplicity Statistics of Stars in the Sagittarius Dwarf Spheroidal Galaxy: Comparison to the Milky Way