We present an all-sky catalog of 869 nearby galaxies, having individual distance estimates within 11 Mpc or corrected radial velocities V LG < 600 km s −1 .The catalog is a renewed and expanded version of the "Catalog of Neighboring Galaxies" by Karachentsev et al. (2004). It collects data on the following observables for the galaxies: angular diameters, apparent magnitudes in F UV -, B-, and K s -bands, Hα and HI fluxes, morphological types, HI-line widths, radial velocities and distance estimates. In this Local Volume (LV) sample 108 dwarf galaxies remain to be still without measured radial velocities.The catalog yields also calculated global galaxy parameters: linear Holmberg diameter, absolute B-magnitude, surface brightness, HI-mass, stellar mass estimated via K-band luminosity, HI rotational velocity corrected for galaxy inclination, indicative mass within the Holmberg radius, and three kinds of "tidal index", which quantify the local density environment. The catalog is supplemented with the data based on the local galaxies (http://www.sao.ru/lv/lvgdb), which presents their optical and available Hα images, as well as other service.We briefly discuss the Hubble flow within the LV, and different scaling relations that characterize galaxy structure and global star formation in them. We also trace the behavior of the mean stellar mass density, HI-mass density and star formation rate density within the considered volume.

A distance-limited sample of 869 objects from the Updated Nearby Galaxy Catalog is used to characterize the star formation status of the Local Volume population. We present a compiled list of 1217 star formation rate (SFR) estimates for 802 galaxies within 11 Mpc from us, derived from the H-alpha imaging surveys and GALEX far-ultraviolet survey. We briefly discuss some basic scaling relations between SFR and luminosity, morphology, HI-mass, surface brightness, as well as environment of the galaxies. About 3/4 of our sample consist of dwarf galaxies, for which we offer a more refined classification. We note that the specific star formation rate of nearly all luminous and dwarf galaxies does not exceed the maximum value: log(SF R/L K ) = −9.4 [yr −1 ]. The bulk of spiral and blue dwarf galaxies have enough time to generate their stellar mass during the cosmological time, T 0 , with the observed SFRs. They dispose of a sufficient amount of gas to support their present SFRs over the next T 0 term. We note that only a minor part of BCD, Im, and Ir galaxies ( about 1/20) proceeds in a mode of vigorous star-burst activity. In general, the star formation history of spiral and blue dwarf galaxies is mainly driven by their internal processes. The present SFRs of E, S0 and dSph galaxies are typically (1/30 -1/300) of their former activity.

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 ⊙ 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 σ * tends to follow nearly the same bTF relation, having slightly lower masses than that of late-type dwarfs.

We use the measured B band axial ratios of galaxies from an updated catalog of Local Volume galaxies to determine the intrinsic shape of dwarf irregular galaxies (de Vacouleurs' morphological types 8, 9 and 10). We find that the shapes change systematically with luminosity, with fainter galaxies being thicker. In particular, we divide our sample into sub-samples and find that the most luminous dwarfs (−19.6 < M B < −14.8) have thin discs (thickness ∼ 0.2), with the disc being slightly elliptical (axial ratio ∼ 0.8). At intermediate luminosity, viz. −14.8 < M B < −12.6, the galaxies are still characterized by elliptical discs (axial ratio ∼ 0.7), but the discs are somewhat thicker (thickness ∼ 0.4). The faintest dwarfs, viz. those with −12.6 < M B < −6.7 are well described as being oblate spheroids with an axial ratio ∼ 0.5. The increasing thickness of the stellar discs of dwarf irregulars with decreasing luminosity is compatible with the increasing ratio of velocity dispersion to rotational velocity with decreasing galaxy size.

Updated Nearby Galaxy Catalog (=UNGC) contains the most comprehensive summary of distances, radial velocities and luminosities for eight hundred galaxies located within 11 Mpc from us. The highest density of observables in UNGC makes this sample indispensable for checking results of N-body simulations of cosmic structures on a ∼ 1 Mpc scale.Environment of each galaxy in UNGC was characterized by a tidal index Θ 1 depending on the separation and mass of the galaxy's Main Disturber (=MD). We ascribed the UNGC galaxies with a common MD to its suite, and ranked suite members according to their Θ 1 . All suite members with positive Θ 1 are assumed to be physical companions of the MD. About 58% of the sample are members of physical groups.The distribution of suites by the number of members, n, follows to a relation N (n) ∼ n −2 . The twenty most populated suites contain 468 galaxies, i.e. 59% of the UNGC sample. The fraction of MDs among the brightest galaxies is almost 100% and drops to 50% at M B = −18 m .We discuss various properties of MDs, as well as galaxies belonging to their suites. The suite abundance practically does not depend on morphological type, linear diameter or hydrogen mass of MD, revealing the tightest correlation with the MD dynamical mass. Dwarf galaxies around MDs exhibit well-known segregation effects: the population of outskirts has later morphological types, richer HI-contents and higher rates of star formation activity. Nevertheless, there are some intriguing cases when dwarf spheroidal galaxies occur at the far periphery of the suites, as well as some late-type dwarfs residing close to MDs.Comparing simulation results with galaxy groups, most studies assume the Local Group is fairly typical. However, we recognize that the nearby groups significantly differ from each other and there is a considerable variation in their properties. The suites of companions around the Milky Way and M 31, consisting the Local Group, do not look as a quite typical nearby group.The multiplicity of nearby groups on number of their physical members can be described by the Hirsh-like index h g = 9, indicating that the Local Volume contains 9 groups with populations exceeding 9 companions to their MDs.