We calculate the angular correlation function of galaxies in the Two Micron All Sky Survey .
We minimize the possible contamination by stars , dust , seeing and sky brightness by studying their cross correlation with galaxy density , and limiting the galaxy sample accordingly .
We measure the correlation function at scales between 1 \arcmin < \theta < 18 \arcdeg using a half million galaxies .
We find a best fit power law to the correlation function has a slope of -0.79 \pm 0.02 and an amplitude at 1 \arcdeg of 0.10 \pm 0.01 in the range 1 \arcmin - 2.5 \arcdeg .
However , there are statistically significant oscillations around this power law .
The largest oscillation occurs at about 0.8 degrees , corresponding to 700 h ^ { -1 } kpc at the median redshift of our survey , as expected in halo occupation distribution descriptions of galaxy clustering .
In addition , there is a break in the power-law shape of the correlation function at \theta > 2.5 \arcdeg .
Our results are in good agreement with other measurements of the angular correlation function .

We invert the angular correlation function using Singular Value Decomposition to measure the three-dimensional power spectrum and find that it too is in good agreement with previous measurements .
A dip seen in the power spectrum at small wavenumber k is statistically consistent with CDM-type power spectra .
A fit of CDM-type power spectra in the linear regime ( k < 0.15 h Mpc ^ { -1 } ) give constraints of \Omega _ { m } h = 0.13 \pm 0.07 
and \sigma _ { 8 } = 1.0 \pm 0.09 for a spectral index of 1.0 .
This suggest a K _ { s } -band linear bias of 1.1 \pm 0.2 .
These measurements are in good agreement with other measurements of the power spectrum on linear scales .
On small scales the power-law shape of our power spectrum is shallower than that derived for the Sloan Digital Sky Survey .
This may imply a biasing for these different galaxies that could be either waveband or luminosity dependent .
The power spectrum derived here in combination with the results from other surveys can be used to constrain models of galaxy formation .