On the dark matter content of ultra-diffuse galaxies

I compare the dark matter content within stellar half-mass radius expected in a $\Lambda$CDM-based galaxy formation model with existing observational estimates for the observed dwarf satellites of the Milky Way and ultra-diffuse galaxies (UDGs).

The model reproduces the main properties and scaling relations of dwarf galaxies, in particular their stellar mass-size relation.

I show that the model also reproduces the relation between the dark matter mass within the half-mass radius, $M_{\rm dm}(

The scatter in the $M_{\rm dm}(

I also show the $M_{\rm dm}(

The upper limits on $M_{\rm dm}(

The most dark matter-deficient galaxies of a given size correspond to halos with the smallest concentrations and the largest ratios of $M_\star/M_{\rm 200c}$.

Conversely, the most dark matter-dominated galaxies are hosted by the highest concentration halos with the smallest $M_\star/M_{\rm 200c}$ ratios.

The model indicates that the scatter between $M_{\rm dm}(

Results presented in this paper indicate that dark matter-deficient UDGs may represent a tail of the expected dark matter profiles, especially if the effect of feedback on these profiles is taken into account.

;Comment: 9 pages, 6 figures