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In this paper we investigate the statistical properties of the BaryonicTully-Fisher relation (BTFr) for a sample of 32 galaxies with accuratedistances based on Cepheids and/or TRGB stars. We make use of homogeneouslyanalysed photometry in 18 bands ranging from the FUV to 160 $\mu$m, allowing usto investigate the effect of the inferred stellar mass-to-light ratio$\Upsilon_{*}$ on the statistical properties of the BTFr. Stellar masses of oursample galaxies are derived with four different methods based on fullSED-fitting, studies of stellar dynamics, near-infrared colours, and theassumption of the same $\Upsilon_{*}^{[3.6]}$ for all galaxies. In addition, weuse high-quality, resolved HI kinematics to study the BTFr based on threekinematic measures: $W_{50}^{i}$ from the global HI profile, and $V_{max}$ and$V_{flat}$ from the rotation curve. We find the intrinsic perpendicularscatter, 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-basedTFr. 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 toplace important observational constraints on theoretical models of galaxyformation and evolution by making comparisons with theoretical predictionsbased on either the $\Lambda$CDM framework or modified Newtonian dynamics.

From light to baryonic mass: the effect of the stellar mass-to-light ratio on the Baryonic Tully-Fisher relation