the Milky Way include $\sim1\times10^{12}$ [$M_{\odot}$]{}(Watkins, Evans & An 2010) and $\sim2.5\times10^{12}$ [$M_{\odot}$]{}(Sakamoto et al 2003). However, given that the mass of the Milky Way is thought to be dominated by dark matter, the stellar mass is expected to be 1/20 of the dynamical mass (eg Moore et al 1999), giving a stellar mass in the range $\sim5-12\times10^{11}$ [$M_{\odot}$]{}. Our simulations therefore imply one SX Phe star per 7.6$-18\times10^{5}$ stars and that SX Phe stars are significantly less abundant per unit mass in our Galaxy compared to than that found in globular clusters (eg one per $\sim4\times10^{4}$ [$M_{\odot}$]{}for $\omega$ Cen, Olech et al 2005) and dwarf spheroidal galaxies (eg one per $2.1\times10^{4}$ [$M_{\odot}$]{}for the Fornax dSph, Poretti et al 2008). (We have assumed no dark matter is present in globular clusters and used the results of $\L$okas 2009 in determining the stellar mass of the Fornax dSph). Given we have assumed that all eleven stars at low Galactic latitude are SX Phe stars (and the spectra of seven are consistent with this) our estimate of the number of SX Phe stars in our Galaxy may be an overestimate, indicating an even greater discrepancy between the relative number of SX Phe 