  We have modelled 38 barred galaxies by using near-IR and optical data from
the Ohio State University Bright Spiral Galaxy Survey. We constructed the
gravitational potentials of the galaxies from $H$-band photometry, assuming
constant mass-to-light ratio. The halo component we chose corresponds to the so
called universal rotation curve. In each case, we used the response of gaseous
and stellar particle disc to rigidly rotating potential to determine the
pattern speed.
  We find that the pattern speed of the bar depends roughly on the
morphological type. The average value of corotation resonance radius to bar
radius, $\mathcal{R}$, increases from $1.15 \pm 0.25$ in types SB0/a -- SBab to
$1.44 \pm 0.29$ in SBb and $1.82\pm 0.63$ in SBbc -- SBc. Within the error
estimates for the pattern speed and bar radius, all galaxies of type SBab or
earlier have a fast bar ($\mathcal{R} \le 1.4$), whereas the bars in later type
galaxies include both fast and slow rotators. Of 16 later type galaxies with a
nominal value of $\mathcal{R} > 1.4$, there are five cases, where the fast
rotating bar is ruled out by the adopted error estimates.
  We also study the correlation between the parameter $\mathcal{R}$ and other
galactic properties. The clearest correlation is with the bar size: the slowest
bars are also the shortest bars when compared to the galaxy size. A weaker
correlation is seen with bar strength in a sense that slow bars tend to be
weaker. These correlations leave room for a possibility that the determined
pattern speed in many galaxies corresponds actually that of the spiral, which
rotates more slowly than the bar. No clear correlation is seen with either the
galaxy luminosity or colour.
