We use observational properties of galaxies accumulated in the Updated Nearby Galaxy Catalog to derive a dark matter mass of luminous galaxies via motions of their companions .
The data on orbital-to-stellar mass ratio are presented for 15 luminous galaxies situated within 11 Mpc from us : the Milky Way , M31 , M81 , NGC5128 , IC342 , NGC253 , NGC4736 , NGC5236 , NGC6946 , M101 , NGC4258 , NGC4594 , NGC3115 , NGC3627 and NGC3368 , as well as for a composit suite around other nearby galaxies of moderate and low luminosity .
The typical ratio for them is M _ { orb } / M _ { * } = 31 , corresponding to the mean local density of matter \Omega _ { m } = 0.09 , i.e 1/3 of the global cosmic density .
This quantity seems to be rather an upper limit of dark matter density , since the peripheric population of the suites may suffer from the presence of fictitious unbound members .
We notice that the Milky Way and M31 haloes have lower dimensions and lower stellar masses than those of other 13 nearby luminous galaxies .
However , the dark-to-stellar mass ratio for both the Milky Way and M31 is the typical one for other neighboring luminous galaxies .
The distortion in the Hubble flow , observed around the Local Group and five other neighboring groups yields their total masses within the radius of zero velocity surface , R _ { 0 } , which are slightly lower than the orbital and virial values .
This difference may be due to the effect of dark energy , producing a kind of “ mass defect ” within R _ { 0 } .

Key words : cosmology : observations - dark matter - galaxies : groups : general