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 \geq 30 \degr , as it was obtained earlier from the optical photometry , in a good agreement with the H i data cube modelling .
However the re-processing of H i data cube we carried out showed that it is compatible with much lower value i \approx 13 \degr 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 Ã ) stellar age ( 4.2 , 2.6 and 2.3 Gyr ) for the bulge , disc and nuclear disc of this galaxy respectively .