Tracing the Local Volume galaxy halo-to-stellar mass ratio with
  satellite kinematics
  Rapid advance has been made recently in accurate distance measurements for
nearby ($D < 11$ Mpc) galaxies based on the magnitude of the tip of red giant
branch stars resolved with the Hubble Space Telescope. We use observational
properties of galaxies presented in the last version of Updated Nearby Galaxy
Catalog to derive a halo mass of luminous galaxies via orbital motion of their
companions. Our sample contains 298 assumed satellites with known radial
velocities around 25 Milky Way-like massive galaxies and 65 assumed satellites
around 47 fainter dominant galaxies. The average total mass-to-$K$-band
luminosity ratio is $31\pm6 M_\odot/L_\odot$ for the luminous galaxies,
increasing up to $\sim200 M_\odot/L_\odot$ toward dwarfs. The bulge-dominated
luminous galaxies are characterized with $\langle{}M_T/L_K\rangle = 73\pm15
M_\odot/L_\odot$, while the disc-dominated spirals have
$\langle{}M_T/L_K\rangle = 17.4\pm2.8 M_\odot/L_\odot$. We draw attention to a
particular subsample of luminous spiral galaxies with signs of declining
rotation curve, which have a radial velocity dispersion of satellites less than
55 km/s and a poor dark matter halo with $\langle{}M_T/L_K\rangle = 5.5\pm1.1
M_\odot/L_\odot$. We note that a fraction of quenched (dSph, dE) companions
around Milky Way-like galaxies decreases with their linear projected separation
as $0.75 \exp(-R_p/350\,\mathrm{kpc})$.
