  We present Chandra X-ray observations of the nearby Seyfert 1.5 galaxy NGC
4151. The images show the extended soft X-ray emission on the several hundreds
of pc scale with better sensitivity than previously obtained. The spectrum of
the unresolved nuclear source may be described by a heavily absorbed (N_{H}
\simeq 3 \times 10^{22} cm^-2), hard power-law (\Gamma \simeq 0.3) plus soft
emission from either a power-law (\Gamma \simeq 2.6) or a thermal (kT \simeq
0.6 keV) component. The flux of the high energy component has decreased from
that observed by ASCA in 1993 and the spectrum is much harder.The large
difference between the soft and hard spectral shapes does not favor the partial
covering or scattering model of the ``soft excess''. Instead, it is likely that
the hard and soft nuclear components represent intrinsically different X-ray
sources. Spectra of the extended emission to almost 1 kpc NE and SW of the
nucleus have also been obtained. The spectra of these regions may be described
by either thermal bremsstrahlung (kT \simeq 0.4-0.7 keV) or power-law (\Gamma
\simeq 2.5-3.2) continua plus 3 emission lines. There is an excellent
correlation between the extended X-ray and [O III]\lambda 5007 line emissions.
We discuss the nature of the extended X-ray emission. Upper limit to the
electron scattering column was obtained. This upper limit is much too low for
the soft X-rays to be electron scattered nuclear radiation.
