From the Outside Looking in: What can Milky Way Analogues Tell us About
  the Star Formation Rate of Our Own Galaxy?
  The Milky Way has been described as an anaemic spiral, but is its star
formation rate (SFR) unusually low when compared to its peers? To answer this
question, we define a sample of Milky Way Analogues (MWAs) based on stringent
cuts on the best literature estimates of non-transient structural features for
the Milky Way. This selection yields only 176 galaxies from the whole of the
SDSS DR7 spectroscopic sample which have morphological classifications in GZ2,
from which we infer SFRs from two separate indicators. The mean SFRs found are
$\log(\rm{SFR}_{SED}/\rm{M}_{\odot}~\rm{yr}^{-1})=0.53$ with a standard
deviation of 0.23 dex from SED fits, and
$\log(\rm{SFR}_{W4}/\rm{M}_{\odot}~\rm{yr}^{-1})=0.68$ with a standard
deviation of 0.41 dex from a mid-infrared calibration. The most recent estimate
for the Milky Way's star formation rate of
$\log(\rm{SFR}_{MW}/\rm{M}_{\odot}~\rm{yr}^{-1})=0.22$ fits well within
2$\sigma$ of these values, where $\sigma$ is the standard deviation of each of
the SFR indicator distributions. We infer that the Milky Way, while being a
galaxy with a somewhat low SFR, is not unusual when compared to similar
galaxies.
