Suites of dwarfs around nearby giant galaxies
  We consider a sample of the Updated Nearby Galaxy Catalog that contains eight
hundred objects within 11 Mpc. Environment of each galaxy was characterized by
a tidal index $\Theta_1$ 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 $\Theta_1$. All suite
members with positive $\Theta_1$ are assumed to be physical companions of the
MD. The distribution of suites by the number of members, n, follows to a
relation $N(n) \sim n^{-2}$. The twenty most populated suites contain 468
galaxies, i.e. 59% of the UNGC sample. About 58% of our sample are members of
physical groups. 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 members of outskirts
have 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. The multiplicity of nearby groups
according to 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 members. (abridged)
