  We have obtained long-slit observations in the optical and near infrared of
12 circumnuclear HII regions (CNSFR) in the early type spiral galaxies NGC
2903, NGC 3351 and NGC 3504 with the aim of deriving their chemical abundances.
Only for one of the regions, the [SIII] $\lambda$ 6312 \AA was detected
providing, together with the nebular [SIII] lines at $\lambda\lambda$ 9069,
9532 \AA, a value of the electron temperature of T$_e$([SIII])= 8400$^{+
4650}_{-1250}$K. A semi-empirical method for the derivation of abundances in
the high metallicity regime is presented.
  We obtain abundances which are comparable to those found in high metallicity
disc HII regions from direct measurements of electron temperatures and
consistent with solar values within the errors. The region with the highest
oxygen abundance is R3+R4 in NGC 3504, 12+log(O/H) = 8.85, about 1.5 solar if
the solar oxygen abundance is set at the value derived by Asplund et al.
(2005), 12+log(O/H)$_{\odot}$ = 8.66$\pm$0.05. Region R7 in NGC 3351 has the
lowest oxygen abundance of the sample, about 0.6 times solar. In all the
observed CNSFR the O/H abundance is dominated by the O$^+$/H$^+$ contribution,
as is also the case for high metallicity disc HII regions. For our observed
regions, however, also the S$^+$/S$^{2+}$ ratio is larger than one, contrary to
what is found in high metallicity disc HII regions for which, in general, the
sulphur abundances are dominated by S$^{2+}$/H$^+$...
