  The X-ray spectrum in a $1^{\circ}\times1^{\circ}$ region of the Galactic
center observed with the ASCA satellite is examined in detail, following the
first report by Koyama et al. (1996, AAA 65.155.208). The observed spectrum
contains prominent emission lines from helium-like and hydrogen-like ions of
various elements, and is essentially the same all over the region. If the
observed spectrum is thermal emission from hot plasmas, it requires
multi-temperature plasma components, each at a different degree of ionization
and with a different amount of absorption. The absence of adiabatic cooling and
of systematic changes in the degree of ionization over the region is against
the Galactic center origin of hot plasmas. A significant broadening of the
helium-like and hydrogen-like iron K-lines is confirmed. The line width
corresponds to a rms velocity of $\sim3300$ km~s$^{-1}$, which far exceeds the
sound velocity in a plasma of $kT\sim14$ keV measured with the Ginga satellite.
These facts cast doubt on a thermal origin of the observed X-ray emission.
