In Table 1 all narrow-line OH sources found are listed. In total there are 202 sources, 90 of which have been identified with known OH-satellite-line masers. The references for previous OH detections are given in Table 2. We visually identified 166 double-peaked (D), 32 single-peaked (S) and 4 irregular (I) sources. A reliable IRAS identification is found for 151 sources.
For each source the table gives an entry number (Col. 1),
the OH
name (Col. 2), a type (D, S, I) identifier (Col. 3),
position in J2000 coordinates (Cols. 4, 5), a measure of
the error in the positions (Col. 6), the distance from the source
to the pointing centre (Col. 7), the peak, stellar and
outflow velocities (Cols. 8 to 11), the peak fluxes (Cols. 12, 13),
the noise in the field where the source was detected (Col. 14,
velocity resolution 
),
the number of the reference to previous observations if applicable
(Col. 15), the name of the nearest IRAS point source (Col. 16)
and the distance to this nearest IRAS point source expressed as a
fraction of the corresponding IRAS error ellipse (Col. 17).
Table 1 can be retrieved from the WWW (http://cdsweb.u-strasbg.fr/Abstract.html).
In Fig. 2 the longitude-latitude diagram and longitude-velocity diagramm are shown
for all 202 sources. The spectra for all sources are shown in
Fig. 6. They are displayed with 
on either side of the
stellar velocity, except for #71 that has an outflow velocity
higher than .
The peaks that were detected at the position of the object are marked
by dots on top. For source #46 that has a very irregular spectrum,
we marked the whole range of detected velocities for the broad peak.
The stellar velocities of the sources in this region of the Galaxy
have a much smaller spread than
those of the sources in the Bulge region (Fig. 3). Therefore,
the sidelobe problem (Paper I) is even more prominent. Spectrum #167 shows a
particularly clear example of this, where the real peak of the source
is almost masked out by a sidelobe from a neighbouring star that has
a higher flux density at this position than even the source
itself. Another example to be noted is spectrum #55 that has a strong negative sidelobe
from source #56.
For details on the extraction of the spectra see Paper I.