  We present the K-band local luminosity function derived froma sample of 1056
bright (K<15) K-selected galaxies from the Hawaii-AAO K-band redshift survey.
The Hawaii-AAO K-band redshift survey covers 4 equatorial fields with a total
area of 8.22 $\deg^2$. We derive both the non-parametric and Schechter
luminosity function from our data, and determine
$M^*(K)=-23.70\pm0.08+5\log_{10}(h)$, $\alpha=-1.37\pm0.10$ and
$\phi^*=0.013\pm0.003 h^3 \Mpc^{-3}$ for a universe with $\Omega_m=0.3$ and
$\Omega_{\Lambda}=0.7$. We also measure the K-band luminosity function for the
early- and later-type galaxies from our morphologically classified subsample.
It appears that later-type galaxies have a fainter $M^*$ and a steep slope,
while early-type galaxies have a much brighter $M^*$ and a quite flat slope in
their K-band luminosity functions. This is consistent with what have been found
in optical type dependent luminosity function. The K-band luminosity density
derived using our luminosity function is now measured at a similar redshift
depth to optical luminosity densities in the SDSS redshift survey. It is 2
times higher than the previous measurement from the shallower 2MASS sample and
resolves the previously reported discrepancies between optical and near-IR
luminosity densities.
