  We study the relation between mesogranular flows, convectively driven sinks
and magnetic fields using high spatial resolution spectropolarimetric data
acquired with the Imaging Magnetograph eXperiment on board Sunrise. We obtain
the horizontal velocity flow fields of two quiet-Sun regions (31.2 $\times$
31.2 Mm$^{2}$) via local correlation tracking. Mesogranular lanes and the
central position of sinks are identified using Lagrange tracers. We find
$6.7\times10^{-2}$ sinks per Mm$^{2}$ in the two observed regions. The sinks
are located at the mesogranular vertices and turn out to be associated with (1)
horizontal velocity flows converging to a central point and (2) long-lived
downdrafts. The spatial distribution of magnetic fields in the quiet Sun is
also examined. The strongest magnetic fields are preferentially located at
sinks. We find that 40 \% of the pixels with longitudinal component of the
magnetic field stronger than 500 G are located in the close neighborhood of
sinks. In contrast, the small-scale magnetic loops detected by Mart\'{i}nez
Gonz\'{a}lez et al. in the same two observed areas do not show any preferential
distribution at mesogranular scales. The study of individual examples reveals
that sinks can play an important role in the evolution of quiet-Sun magnetic
features.
