We study different incarnations of the Tully-Fisher ( TF ) relation for the Local Volume ( LV ) galaxies taken from Updated Nearby Galaxy Catalog .
The UNGC sample contains 656 galaxies with W _ { 50 } HI-line-width estimates , mostly belonging to low mass dwarfs .
Of them , 296 objects have distances measured with accuracy better than 10 % .
For the sample of 331 LV galaxies having baryonic masses \log M _ { bar } > 5.8 \log M _ { \sun } we obtain a relation \log M _ { bar } = 2.49 \log W _ { 50 } +3.97 with observed scatter of 0.38 dex .
The largest factors affecting the scatter are observational errors in K -band magnitudes and W _ { 50 } line widths for the tiny dwarfs , as well as uncertainty of their inclinations .
We find that accounting for the surface brightness of the LV galaxies , or their gas fraction , or specific star formation rate , or the isolation index do not reduce essentially the observed scatter on the baryonic TF-diagram .
We also notice that a sample of 71 dSph satellites of the Milky Way and M31 with known stellar velocity dispersion \sigma ^ { * } tends to follow nearly the same bTF relation , having slightly lower masses than that of late-type dwarfs .