The new detections and their spectra are compiled in Table 1 and shown in Fig. 1.
For most sources in Table 1, at least two observations at different times were taken. We report here only the spectrum with higher signal/noise ratio. Owing to the complexity of the H2O spectral features and also the rather low signal/noise ratio of the weak sources detected, only the most significant parameters have been included in the table. The items of the table are:
Column 1: name of the source,
Columns 2, 3: right ascension and declination (1950.0),
Column 4: class of the source,
Column 5: flux density (Jy) of the strongest component in the spectrum,
Column 6: peak velocity (km s-1) with respect to the LSR,
Column 7: noise level of the spectrum 
(Jy),
Column 8: integrated flux (Jy km s-1) computed over the velocity interval related to the strongest component of the spectrum,
Column 9: date (yymmdd) of observation.
The source is considered to be detected if the strongest component in the spectrum is greater than 4 times the noise level of the spectrum and has been confirmed by additional observations. It is also checked that there is no strong nearby maser source, to rule out the possibility of strong sources seen in the antenna sidelobes. We have also followed the general rule to consider positions with a separation less than half of HPBW as a single source.
The atlas of spectra of Fig. 1 (flux density in Jy versus velocity in 
) contains only those sources where at least one spectral feature was
detected.
The sources that have been detected on the 13.7 m telescope independently but already reported by Brand et al. (1994) and Xiang et al. (1995) are not included in Table 1.