Abundance matching with the mean star formation rate: there is no missing satellites problem in the Milky Way above $mathbf{M_{200} sim 10^9,{rm bf M}_odot}$. (arXiv:1807.07093v2 [astro-ph.GA] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Read_J/0/1/0/all/0/1">J. I. Read</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Erkal_D/0/1/0/all/0/1">D. Erkal</a>

We introduce a novel abundance matching technique that produces a more
accurate estimate of the pre-infall halo mass, $M_{200}$, for satellite
galaxies. To achieve this, we abundance match with the mean star formation
rate, averaged over the time when a galaxy was forming stars, $langle {rm
SFR}rangle$, instead of the stellar mass, $M_*$. Using data from the Sloan
Digital Sky Survey, the GAMA survey and the Bolshoi simulation, we obtain a
statistical $langle {rm SFR}rangle-{rm M}_{200}$ relation in $Lambda{rm
CDM}$. We then compare the pre-infall halo mass, $M^{rm abund}_{200}$, derived
from this relation with the pre-infall dynamical mass, $M^{rm dyn}_{200}$, for
21 nearby dSph and dIrr galaxies, finding a good agreement between the two. As
a first application, we use our new $langle {rm SFR}rangle-{rm M}_{200}$
relation to empirically measure the cumulative mass function of a
volume-complete sample of bright Milky Way satellites within 280 kpc of the
Galactic centre. Comparing this with a suite of cosmological ‘zoom’ simulations
of Milky Way-mass halos that account for subhalo depletion by the Milky Way
disc, we find no missing satellites problem above $M_{200} sim 10^9,{rm
M}_odot$ in the Milky Way. We discuss how this empirical method can be applied
to a larger sample of nearby spiral galaxies.

We introduce a novel abundance matching technique that produces a more
accurate estimate of the pre-infall halo mass, $M_{200}$, for satellite
galaxies. To achieve this, we abundance match with the mean star formation
rate, averaged over the time when a galaxy was forming stars, $langle {rm
SFR}rangle$, instead of the stellar mass, $M_*$. Using data from the Sloan
Digital Sky Survey, the GAMA survey and the Bolshoi simulation, we obtain a
statistical $langle {rm SFR}rangle-{rm M}_{200}$ relation in $Lambda{rm
CDM}$. We then compare the pre-infall halo mass, $M^{rm abund}_{200}$, derived
from this relation with the pre-infall dynamical mass, $M^{rm dyn}_{200}$, for
21 nearby dSph and dIrr galaxies, finding a good agreement between the two. As
a first application, we use our new $langle {rm SFR}rangle-{rm M}_{200}$
relation to empirically measure the cumulative mass function of a
volume-complete sample of bright Milky Way satellites within 280 kpc of the
Galactic centre. Comparing this with a suite of cosmological ‘zoom’ simulations
of Milky Way-mass halos that account for subhalo depletion by the Milky Way
disc, we find no missing satellites problem above $M_{200} sim 10^9,{rm
M}_odot$ in the Milky Way. We discuss how this empirical method can be applied
to a larger sample of nearby spiral galaxies.

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