We observed small scale magnetic flux emergence in a sunspot moat region by the Solar Optical Telescope ( SOT ) aboard the Hinode satellite .
We analyzed filtergram images observed in the wavelengths of Fe 6302 Å , G-band and Ca \emissiontype II H. In Stokes I images of Fe 6302 Å , emerging magnetic flux were recognized as dark lanes .
In G-band , they showed their shapes almost the same as in Stokes I images .
These magnetic flux appeared as dark filaments in Ca \emissiontype II H images .
Stokes V images of Fe 6302 Å showed pairs of opposite polarities at footpoints of each filament .
These magnetic concentrations are identified to correspond to bright points in G-band/Ca \emissiontype II H images .
From the analysis of time-sliced diagrams , we derived following properties of emerging flux , which are consistent with the previous works .
( 1 ) Two footpoints separate each other at a speed of 4.2 km s ^ { -1 } during the initial phase of evolution and decreases to about 1 km s ^ { -1 } in 10 minutes later .
( 2 ) Ca \emissiontype II H filaments appear almost simultaneously with the formation of dark lanes in Stokes I in the observational cadence of 2 minutes .
( 3 ) The lifetime of the dark lanes in Stokes I and G-band is 8 minutes , while that of Ca filament is 12 minutes .

An interesting phenomena was observed that an emerging flux tube expands laterally in the photosphere with a speed of 3.8 km s ^ { -1 } .
Discussion on the horizontal expansion of flux tube will be given with refernce to previous simulation studies .