The spectroscopic observations were made between Apr. 15, 1994 and
Feb. 15, 1996. We obtained a total of 123 galaxy spectra.
All of the observations were made with 2.16 m telescope at
the Xinglong Station of
Beijing Astronomical Observatory using Zeiss universal
spectrograph with a grating of 
dispersion.
Before Nov. 5, 1994, a Tek 
CCD which covered a
range from 
to 7100
at a resolution of 
(2 pixels) was used. After that,
a Tek 
CCD
which covered a 
range from
to 
at a resolution of 
(2 pixels) was employed.
In most cases, slit width of about 3'' was chosen to match
the typical seeing disc
at Xinglong Station, but occasionally, the seeing disc was
smaller than 2'' or larger than 5'' .
Thus may affect the spectral classification. Slit position angles of
were generally used.
For objects with two close nuclei (separation 
), the slit was rotated
such that two spectra could be obtained simultaneously.
The seeing was about 3'' to 4'' on most of the observation nights. In order to perform a relative flux calibration, KPNO standard stars were also observed on each night.
Table 2 lists the observations by target objects. The standard IRAS name, together with one upper case letters representing the individual components (See Fig. 9 for identifications) are listed in Col. 1. Column 2 to Col. 10 give for each source: coordinates, observation date (Beijing Time), exposure time, airmass, slit width and position angle respectively. The sources flagged with ticks in Col. 11 were observed during good weather condition.