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We introduce a novel abundance matching technique that produces a moreaccurate estimate of the pre-infall halo mass, $M_{200}$, for satellitegalaxies. To achieve this, we abundance match with the mean star formationrate, averaged over the time when a galaxy was forming stars, $\langle {\rmSFR}\rangle$, instead of the stellar mass, $M_*$. Using data from the SloanDigital Sky Survey, the GAMA survey and the Bolshoi simulation, we obtain astatistical $\langle {\rm SFR}\rangle-{\rm M}_{200}$ relation in $\Lambda{\rmCDM}$. We then compare the pre-infall halo mass, $M^{\rm abund}_{200}$, derivedfrom this relation with the pre-infall dynamical mass, $M^{\rm dyn}_{200}$, for21 nearby dSph and dIrr galaxies, finding a good agreement between the two. Asa first application, we use our new $\langle {\rm SFR}\rangle-{\rm M}_{200}$relation to empirically measure the cumulative mass function of avolume-complete sample of bright Milky Way satellites within 280 kpc of theGalactic centre. Comparing this with a suite of cosmological 'zoom' simulationsof Milky Way-mass halos that account for subhalo depletion by the Milky Waydisc, we find no missing satellites problem above $M_{200} \sim 10^9\,{\rmM}_\odot$ in the Milky Way. We discuss how this empirical method can be appliedto a larger sample of nearby spiral galaxies.

monthly notices of the royal astronomical society

Abundance matching with the mean star formation rate: there is no  missing satellites problem in the Milky Way above $\mathbf{M_{200} \sim  10^9\,{\rm \bf M}_\odot}$