  We performed the long-slit observations of spiral galaxy UGC11919 with the
Russian 6-m telescope to study its kinematics and stellar population. The
previous studies gave basis to suspect that this galaxy possesses a peculiarly
low mass-to-light ratio $M/L_B$ of stellar population which could indicate the
presence of bottom-light stellar initial mass function (IMF). The ratio $M/L_B$
estimated for different evolutionary models of stellar population using both
the broad-band magnitudes and the detailed spectral data confirms this
peculiarity if the disc inclination angle $i>30^o$, as it was obtained earlier
from the optical photometry, in a good agreement with the HI data cube
modelling. However the re-processing of HI data cube we carried out showed that
it is compatible with much lower value $i=13^o$ corresponding to the "normal"
ratio $M/L_B$, which does not need any peculiar stellar IMF. Stellar velocity
dispersion measured at one disc radial scalelength from the center also better
agrees with the low disc inclination. However in this case we should admit that
the disc possesses a non-axisymmetric shape even after taking into account a
two-armed spiral structure.
  The derived stellar kinematic profiles reveal a signature of kinematically
decoupled nuclear disc in the galaxy. Using different evolution models of
stellar population we estimated the stellar metallicity [Z/H] (-0.4, -0.5 and
-0.3 dex) and the mean luminosity-weighted (for the luminosity in the spectral
range $4800-5570$ \AA) stellar age (4.2, 2.6 and 2.3 Gyr) for the bulge, disc
and nuclear disc of this galaxy respectively.
