  We report results from lithium abundance determinations using high resolution
spectral analysis of the 107 metal-rich stars from the Calan-Hertfordshire
Extrasolar Planet Search programme.
  We set out to understand the lithium distribution of the population of stars
taken from this survey.
  The lithium abundance with account NLTE effects was determined from the fits
to the Li I 6708 \AA~resonance doublet profiles in the observed spectra.
  We find that a) fast rotators tend to have higher lithium abundances, b)
$\log$ N(Li) is higher in more massive/hot stars, c) $\log$ N(Li) is higher in
less evolved stars, i.e. stars of lower \logg, d) stars with the metallicities
$>$0.25~dex do not show the presence of lithium lines in their spectra, e) most
of our planet hosts rotate slower, f) our estimate of a lower limit of lithium
isotopic ratio is \Li $>$10 in the atmospheres of two SWP and two non-SWP
stars.
  Measurable lithium abundances were found in the atmospheres of 45 stars
located at distances of 20-170 pc from the Sun, for the other 62 stars the
upper limits of log N(Li) were computed. We found well defined dependences of
lithium abundances on \Teff, \vsini, and less pronounced for the \logg. In case
of \vsini we see two sequences of stars: with measurable lithium and with the
upper limit of log N(Li). About 10\% of our targets are known to host planets.
Only two SWP have notable lithium abundances, so we found a lower proportion of
stars with detectable Li among known planet hosts than among stars without
planets. However, given the small sample size of our planet-host sample, our
analysis does not show any statistically significant differences in the lithium
abundance between SWP and stars without known planets.
