From light to baryonic mass: the effect of the stellar mass-to-light
  ratio on the Baryonic Tully-Fisher relation
  In this paper we investigate the statistical properties of the Baryonic
Tully-Fisher relation (BTFr) for a sample of 32 galaxies with accurate
distances based on Cepheids and/or TRGB stars. We make use of homogeneously
analysed photometry in 18 bands ranging from the FUV to 160 $\mu$m, allowing us
to investigate the effect of the inferred stellar mass-to-light ratio
$\Upsilon_{*}$ on the statistical properties of the BTFr. Stellar masses of our
sample galaxies are derived with four different methods based on full
SED-fitting, studies of stellar dynamics, near-infrared colours, and the
assumption of the same $\Upsilon_{*}^{[3.6]}$ for all galaxies. In addition, we
use high-quality, resolved HI kinematics to study the BTFr based on three
kinematic measures: $W_{50}^{i}$ from the global HI profile, and $V_{max}$ and
$V_{flat}$ from the rotation curve. We find the intrinsic perpendicular
scatter, or tightness, of our BTFr to be $\sigma_{\perp} = 0.026 \pm 0.013$
dex, consistent with the intrinsic tightness of the 3.6 $\mu$m luminosity-based
TFr. However, we find the slope of the BTFr to be $2.99 \pm 0.2$ instead of
$3.7 \pm 0.1$ for the luminosity-based TFr at 3.6 $\mu$m. We use our BTFr to
place important observational constraints on theoretical models of galaxy
formation and evolution by making comparisons with theoretical predictions
based on either the $\Lambda$CDM framework or modified Newtonian dynamics.
