  We investigate the dynamics of GN-z11, a luminous galaxy at $z=10.60$,
carefully analyzing the public deep integral field spectroscopy (IFS) data
taken with JWST NIRSpec IFU. While the observations of the IFS data originally
targeted a He II clump near GN-z11, we find that C
III]$\lambda\lambda1907,1909$ emission from ionized gas at GN-z11 is bright and
spatially extended significantly beyond the point-spread function (PSF) in
contrast with the GN-z11's compact UV-continuum morphology. The spatially
extended C III] emission of GN-z11 shows a velocity gradient, red- and
blue-shifted components in the NE and SW directions, respectively, which cannot
be explained by the variation of [C III]$\lambda$1907/C III]$\lambda$1909 line
ratios. We perform forward modeling with GalPak$^\mathrm{3D}$, including the
effects of PSF smearing and line blending, and find that the best-fit model is
a nearly edge-on disk with a rotation velocity of
$v_\mathrm{rot}$=$376_{-151}^{+110}$ km s$^{-1}$, a velocity dispersion of
$\sigma_v=113_{-48}^{+24}$ km s$^{-1}$, and a ratio of
$v_\mathrm{rot}/\sigma_v=3.3_{-1.5}^{+1.7}$, indicative of a rotation-dominated
disk at $z=10.6$. Interestingly, the disk rotation velocity is faster than the
circular velocity at the virial radius, $v_\mathrm{c}(r_{200})=205_{-34}^{+28}$
km s$^{-1}$, estimated from the stellar mass, suggesting a compact disk
produced under weak feedback such predicted in numerical simulations. In fact,
the half-light radius of the C III] emitting gas disk is only $294\pm45$ pc,
while the one of the stellar UV component is even smaller, $196\pm12$ pc. While
higher S/N data are necessary for a conclusion, these observational results
would suggest that GN-z11 has a fast-rotating gaseous disk whose center
possesses luminous stellar components or AGN providing weak feedback.
