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We have observed the central region of the nearby starburst galaxy NGC 253with the Kyoto Tridimensional Spectrograph II (Kyoto3DII) Fabry-Perot mode inorder to investigate the properties of its galactic wind. Since this galaxy hasa large inclination, it is easy to observe its galactic wind. We produced theHa, [N II]6583, and [S II]6716,6731 images, as well as those line ratio maps.The [N II]/Ha ratio in the galactic wind region is larger than those in H IIregions in the galactic disk. The [N II]/Ha ratio in the southeastern filament,a part of the galactic wind, is the largest and reaches about 1.5. These large[N II]/Ha ratios are explained by shock ionization/excitation. Using the [SII]/Ha ratio map, we spatially separate the galactic wind region from thestarburst region. The kinetic energy of the galactic wind can be sufficientlysupplied by supernovae in a starburst region in the galactic center. The shapeof the galactic wind and the line ratio maps are non-axisymmetric about thegalactic minor axis, which is also seen in M82. In the [N II]6583/[SII]6716,6731 map, the positions with large ratios coincide with the positionsof star clusters found in the Hubble Space Telescope (HST) observation. Thismeans that intense star formation causes strong nitrogen enrichment in theseregions. Our unique data of the line ratio maps including [S II] lines havedemonstrated their effectiveness for clearly distinguishing between shocked gasregions and starburst regions, determining the extent of galactic wind and itsmass and kinetic energy, and discovering regions with enhanced nitrogenabundance.

Galactic Wind in the Nearby Starburst Galaxy NGC 253 Observed with the Kyoto3DII Fabry-Perot Mode