  We present a method to derive positions of molecular clouds along the lines
of sight from a quantitative comparison between 2.6 mm CO emission lines and 18
cm OH absorption lines, and apply it to the central kiloparsecs of the Milky
Way. With some simple but justifiable assumptions, we derive a face-on
distribution of the CO brightness and corresponding radial velocity in the
Galactic centre without any help of kinematical models. The derived face-on
distribution of the gas is elongated and inclined so that the Galactic-eastern
(positive longitude) side is closer to us. The gas distribution is dominated by
a barlike central condensation, whose apparent size is 500x200 pc. A ridge
feature is seen to stretch from one end of the central condensation, though its
elongated morphology might be artificial. The velocity field shows clear signs
of noncircular motion in the central condensation. The `expanding molecular
ring' feature corresponds to the peripheral region surrounding the central
condensation with the Galactic-eastern end being closer to us. These
characteristics agree with a picture in which the kinematics of the gas in the
central kiloparsec of the Galaxy is under a strong influence of a barred
potential. The face-on distribution of the in situ pressure of the molecular
gas is derived from the CO multiline analysis. The derived pressure is found to
be highest in the central 100 pc. In this region, the gas is accumulating and
is forming stars.
