1 Introduction

The acquision of global parameters of galaxies from observations in the neutral hydrogen line [22, (Roberts 1969)] revealed a new approach in investigating the evolution of gaseous and stellar subsystems of galaxies. Over the past 30 years the number of galaxies with measured HI flux and line width has been increased by two orders, reaching $N\sim10^4$. Numerous publications were devoted to study relations between global HI and optical characteristics of galaxies. A vast comparison of HI data for about 6 000 galaxies was undertaken by [23, Roberts & Haynes (1994).] However, their sample, like is many others, limited by apparent magnitude or angular diameter of galaxies, but not by distance, which leads to a strong observational selection against intrinsically small objects.

For the analysis of global parameters of galaxies in a volume- limited sample, [11, Huchtmeier & Richter (1988)] (=HR) used the list of galaxies from [18, Kraan-Korteweg & Tammann (1979)] (=KKT) with corrected radial velocities, V₀ < 500 kms^-1. The sample studied by HR contained 146 galaxies mainly of low luminosity. For the past decade the initial KKT sample has been increased almost two times in number due to the mass surveys of redshifts of galaxies from the known catalogues, revealing new nearby galaxies in the Milky Way "Zone of Avoidance", as well as special searches for dwarf galaxies in nearby groups. The increasing numbers of galaxies in the LV is mainly due to many new dwarf galaxies. It should be emphisized that the numerical growth of the KKT sample was accompanied by improving its data quality. For many faint galaxies their apparent magnitudes, angular diameters and types were specified. However, even at present one may find cases of significant discrepancy in the published data.

It should be particularly emphasized that for galaxies with V₀ < 500 kms^-1 their corrected radial velocity is a rather unreliable distance indicator because of observed deviations from the perfect cosmic Hubble flow, $V = {\rm HD}$ [15, (Karachentsev & Makarov 1996).] That is why measurements of individual photometric distances for $\sim150$Local Volume galaxies made by different authors in the 90-ies allowed masses and other global parameters of nearby galaxies to be determined with a higher accuracy (see references in [12, Karachentsev 1994,] and [13, Karachentsev & Tikhonov 1994).] The mentioned circumstances give us grounds to consider once again the relations between the global parameters of nearby galaxies based on a more complete and homogeneous sample of observational data.