The observations listed in Table 1 (click here) have been obtained with the
B&C+CCD spectrograph attached to the 1.82 m telescope operated on Mt. Ekar
(Asiago) by the Astronomical Observatory of Padua (Italy). All spectra of
programme stars and spectrophotometric standards have been obtained in
slitless mode for optimal flux calibration. The observations have been
secured during nights with photometric conditions. The covered wavelength
range is 
. The spectral resolution is dominated by the
dimension of the seeing PSF, on the average 20 Å. The Asiago spectra are
presented in Figs. 1 (click here) to 5 (click here).
Table 1: Journal of observations of programme stars observed at Asiago.
Type, Max and Min as listed by DS93. Code for spectral information
available in literature as given by DS93: N = no spectral information;
D = only a glass plate tracing or a description of the quiescence
spectrum. Status of the object when we have observed it: Q =
quiescence; Out = outburst
The objects listed in Table 2 (click here) have been observed with the BFOSC+CCD Imager & Spectrograph attached to the 1.5 m telescope operated in Loiano by the Astronomical Observatory of Bologna (Italy). The slit spectrograph was set to 2 arcsec, for a resolution of 12 Å and a covered wavelength range between 4000 and 7850 Å. In several cases the Loiano observations have been obtained in non-photometric conditions and thus the zero point of the flux scale is not accurate and no absolute fluxes and V magnitude are derived. The Loiano spectra are presented in Figs. 6 (click here) to 10 (click here).
Table 2: Journal of observations of programme stars observed at Loiano.
Type, Max and Min as listed by DS93. Code for spectral information
available in literature as given by DS93: N = no spectral information;
D = only a glass plate tracing or a description of the quiescence
spectrum
Table 3: Target objects without recorded spectra because at the time of our
observations they were too faint. Type, Max and Min as listed by DS93. The
scheme for spectral code (from DS93) is the same as in Table 2 (click here).
Last column: magnitude of the object as estimated on the TV screen of the
guiding system of the Asiago 1.82 m telescope
Table 4 (click here) gives the classification of the programme stars based on
our spectra, Table 5 (click here) the integrated flux of selected emission
lines, Table 6 (click here) the continuum fluxes (at the same reference
wavelengths as in Papers I, II and III) and Table 7 (click here) the 
magnitudes as derived on our spectra from convolution with the band
transmission profiles.
Table 4: Classification from spectra of the programme stars
Table 5: Integrated flux (in units of 
) of the most prominent emission lines
Table 6: Continuum fluxes for the programme stars. The fluxes have been
scaled to Flux (5200 Å) = 1.00. They were computed averaging over 50 Å\
wide bins centered at the given wavelength
Table 7: B-V, 
colour indices and V magnitude
of the programme stars as derived from our spectrophotometry
