  We have mapped the J=1-0 line of SiO in a 1 degree x 12 arcmin. (lxb) region
around the Galactic center (GC) with an angular resolution of 2 arcmin.
(approx. 4 pc). In contrast to the spatial distribution of other high dipole
moment molecules like CS, whose emission is nearly uniform, the SiO emission is
very fragmented and it is only associated with some molecular clouds. In
particular, it is remarkable that the SiO emission closely follows the
non-thermal radio arc in the GC. The SiO clouds are more extended than the beam
with typical sizes between 4 and 20 pc. High angular resolution (26 arcsec.)
mapping in the J=1-0 line of SiO toward the molecular clouds in Sgr B2 and Sgr
A shows that the SiO emission is relatively smooth with structures of typically
2 pc. From the line intensities of the J=1-0, J=3-2 and J=5-4 transitions of
SiO we derive H2 densities for these clouds of a few 1e4 cm-3. The SiO
fractional abundances are approx. 1e-9 for the SiO clouds and 1e-10 for the
other molecular clouds in the GC. The characteristics (size and H2 densities)
of the SiO emission in the GC are completely different from those observed in
the Galactic disk, where the SiO emission arises from much smaller regions with
larger H2 densities. We briefly discuss the implications of the SiO emission in
the molecular clouds of the GC. We conclude that the particular chemistry in
these clouds is probably related to large scale fast shocks occurring in the
Galactic center region.
