3. Results

The flux calibrated spectra for the programme stars are presented in Figs. 4-13. As in previous papers in this series continuum fluxes at selected wavelengths, integrated emission line fluxes, UBVRI magnitudes as well as the spectrum classification are given in Tables 3 (click here) to 6 (click here) for each programme star.

The V magnitude and the U-B, B-V, and colors have been computed from the flux calibrated spectra of each object. They are primarily intended for statistical use and to improve or fill in the missing photometric entries in the DS93 catalogue. For the band transmission profiles we have used the same sources as adopted in previous papers in this series: Lamla (1982; Vilnius Observatory reconstruction) for U and B, and Bessell (1976) for V, and .

The error level of the magnitudes and colors has been estimated by a comparison of derived and tabulated values for each standard star calibrated against all the other ones observed during the same night. The error matches those listed above for the absolute flux calibration. A somewhat larger value is however to be expected for the programme stars because their recorded spectra have in general a lower S/N and their placement on the slit may be problematic for the faintest ones. Comparison with available literature and the results presented in previous papers in this series suggests that the bulk of the targets should have V magnitudes accurate to 0.10 mag, the U-B colors to 0.10 mag and B-V, , colors to 0.05 mag.

 

He I He I He I He I He II

(4471 Å) (5876 Å) (6678 Å) (7065 Å) (4686 Å)

1H 1025+220 21.5 13.9 8.9 5.6 2.1

V442 Cen 17.8 9.0 5.5

AP Cru 0.8

V485 Cen 5.8 3.8 3.4 2.3 2.6

PG 1510+234 4.4

EK TrA 138 104 77 62 16 34 14 9.9 6.7

BR Lup 12 11 9.2 6.9 2.1 2.8 2.0 0.6 1.1

HP Nor 45 34 32 28 7.9 3.4 34

IK Nor 25 17 13 12 2.7 4.9 2.1 1.5

PG 1633+115 3.3 2.9

HO Del 17 16 13 14 3.2 4.6 1.6 1.1

 

In Figs. 1 (click here) and 2 (click here) the colors of the programme stars are compared with the entries in the UBV photometric catalogue of CVs by Bruch & Engel (1994, hereafter BE94) and with the values of confirmed CVs from previous papers in this series. The agreement is excellent, arguing in favor of the accuracy of the flux calibration we have performed.

In Fig. 3 the H profiles of the emission line objects are plotted on an expanded scale. The profile of the night-sky line at 5577.4 Å in the spectrum of AP Cru is shown as a template of the instrumental resolution (AP Cru being the programme star with the narrowest H profile).

  
Figure 1: U-B, B-V diagram of programme stars. No reddening correction has been applied to the data given in Table 6 (click here). The reddening vector corresponding to E_B-V=0.5 is shown. The solid line is the ZAMS according to Caldwell et al. (1993). Legend: filled circles = confirmed CVs from the present paper; open circles = other programme stars; crosses = CVs in quiescence from the UBV photometric catalogue of Bruch & Engel (1994); plus signs = validated CVs in quiescence from previous papers in this series

  
Figure 2: , diagram of programme stars. The solid line is the ZAMS according to Caldwell et al. (1993). No reddening correction has been applied to the data given in Table 6 (click here). The reddening vector corresponding to E_B-V=0.5 is shown. The symbols are: filled circles = confirmed CVs from the present paper; open circles = other programme stars; plus signs = validated CVs in quiescence from previous papers in this series

 
Figure 3: H emission profiles for the validated CVs among the programme stars. Fluxes in units of 10^-15 erg cm^-2 s^-1 Å^-1. The night-sky line at 5577.4 Å from the NN Cen spectrum is shown on the same scale as a reference for the instrumental resolution and flux level of the background sky (computed on the same number of CCD columns as for the programme stars)