The number of globular clusters around the iconic UDG DF44 is as
  expected for dwarf galaxies
  There is a growing consensus that the vast majority of ultra-diffuse galaxies
(UDGs) are dwarf galaxies. However, there remain a few UDGs that seem to be
special in terms of their globular cluster (GC) systems. In particular,
according to some authors, certain UDGs exhibit large GC populations when
compared to expectations from their stellar (or total) mass. Among these
special UDGs, DF44 in the Coma cluster is one of the better-known examples.
DF44 has been claimed to have a relatively high number of GCs,
$N_{GC}=74^{+18}_{-18}$, for a stellar mass of only $3\times 10^8$ $M_{ \odot
}$ which would indicate a much larger dark halo mass than dwarfs of similar
stellar mass. In this paper we revisit this number and, contrary to previous
results, find $N_{GC}=21^{+7}_{-9}$ assuming that the distribution of the GCs
follows the same geometry as the galaxy. If we assume that the GCs around DF44
are distributed in a (projected) circularly symmetric way and, if we use a less
strict criterion for the selection of the GCs, we find $N_{GC}=18^{+23}_{-12}$.
Making use of the $M_{\rm GC} - M_{\rm halo}$ relation, this number of GCs
suggests a dark matter halo mass of $M_{halo}=1.1^{+0.4}_{-0.5} \times 10^{11}
M_{\odot}$, a value which is consistent with the expected total mass for DF44
based on its velocity dispersion, $\sigma=33^{+3}_{-3}$ km s$^{-1}$. We
conclude that the number of GCs around DF44 is as expected for regular dwarf
galaxies of similar stellar mass and DF44 is not extraordinary in this respect.
