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 Cepheïds and/or TRGB stars. We make use of homogeneously analysed photometry in 18 bands ranging from the FUV to 160 µm, allowing us to investigate the effect of the inferred stellar mass-to-light ratio (Υ ) on the statistical properties of the BTFr. Stellar masses of our sample galaxies are derived with four different methods based on full SEDfitting, studies of stellar dynamics , near-infrared colours, and the assumption of the same Υ [3.6] for all galaxies. In addition, we use high-quality, resolved Hi kinematics to study the BTFr based on three kinematic measures: W i 50 from the global HI profile, and V max and V f lat from the rotation curve. We find the intrinsic perpendicular scatter, or tightness, of our BTFr to be σ ⊥ = 0.026 ± 0.013 dex, consistent with the intrinsic tightness of the 3.6 µm luminosity-based TFr. However, we find the slope of the BTFr to be 2.99±0.2 instead of 3.7±0.1 for the luminosity-based TFr at 3.6µm. 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 ΛCDM framework or modified Newtonian dynamics.

In this paper we investigate the statistical properties of the Tully-Fisher relation for a sample of 32 galaxies with measured distances from the Cepheid period-luminosity relation and/or TRGB stars. We take advantage of panchromatic photometry in 12 bands (from FUV to 4.5 µm) and of spatially resolved Hi kinematics. We use these data together with three kinematic measures (W i 50 , V max and V f lat ) extracted from the global Hi profiles or Hi rotation curves, so as to construct 36 correlations allowing us to select the one with the least scatter. We introduce a tightness parameter σ ⊥ of the TFr, in order to obtain a slope-independent measure of the goodness of fit. We find that the tightest correlation occurs when we select the 3.6 µm photometric band together with the V f lat parameter extracted from the Hi rotation curve.

We present spatially-resolved Hi kinematics of 32 spiral galaxies which have Cepheid or/and Tip of the Red Giant Branch distances, and define a calibrator sample for the Tully-Fisher relation. The interferometric Hi data for this sample were collected from available archives and supplemented with new GMRT observations. This paper describes an uniform analysis of the Hi kinematics of this inhomogeneous data set. Our main result is an atlas for our calibrator sample that presents global Hi profiles, integrated Hi column-density maps, Hi surface density profiles and, most importantly, detailed kinematic information in the form of high-quality rotation curves derived from highly-resolved, two-dimensional velocity fields and position-velocity diagrams.With the developments of new methods and instruments, the observed scatter in the Tully-Fisher relation has decreased significantly, mainly due to more accurate pho-