The Void Galaxy Survey: Star Formation Properties
  We study the star formation properties of 59 void galaxies as part of the
Void Galaxy Survey (VGS). Current star formation rates are derived from
$\rm{H\alpha}$ and recent star formation rates from near-UV imaging. In
addition, infrared 3.4 $\rm{\mu m}$, 4.6 $\rm{\mu m}$, 12 $\rm{\mu m}$ and 22
$\rm{\mu m}$ WISE emission is used as star formation and mass indicator.
Infrared and optical colours show that the VGS sample displays a wide range of
dust and metallicity properties. We combine these measurements with stellar and
HI masses to measure the specific SFRs ($\rm{SFR/M_{*}}$) and star formation
efficiencies ($\rm{SFR/M_{HI}}$). We compare the star formation properties of
our sample with galaxies in the more moderate density regions of the cosmic
web, 'the field'. We find that specific SFRs of the VGS galaxies as a function
of stellar and HI mass are similar to those of the galaxies in these field
regions. Their $\rm{SFR\alpha}$ is slightly elevated than the galaxies in the
field for a given total HI mass. In the global star formation picture presented
by Kennicutt-Schmidt, VGS galaxies fall into the regime of low average star
formation and correspondingly low HI surface density. Their mean
$\rm{SFR\alpha/M_{HI}}$ and $\rm{SFR\alpha/M_{*}}$ are of the order of
$\rm{10^{-9.9}}$ $\rm{yr^{-1}}$. We conclude that while the large scale
underdense environment must play some role in galaxy formation and growth
through accretion, we find that even with respect to other galaxies in the more
mildly underdense regions, the increase in star formation rate is only
marginal.
