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Sample Properties

In this subsection we utilize the data given in Tables 4 and 6 to calculate basic parameters such as X-ray and radio luminosities. The distributions of these parameters will be analyzed in upcoming sections. In Figure 3, we plot the redshift distribution of DXRBS FSRQs opposite that of the 1 Jy and S4 samples. In Figure 4, we plot the redshift distribution of DXRBS BL Lacs opposite the Slew and 1 Jy samples. In Figure 5, we have plotted the X-ray and radio luminosities of all the FSRQs in our sample, as well as those of the 1 Jy and S4 samples. A similar plot is given in Figure 6 for the BL Lacs, with the comparison samples being the 1 Jy, Slew and EMSS samples. The apparent deficit of objects at the very highest luminosities is a result of the smaller area of sky covered by DXRBS compared to, e.g., the Slew and 1 Jy samples. The 1 keV X-ray luminosities plotted in Figs. 5 and 6 have been K-corrected and de-absorbed using the X-ray spectral indices derived from the WGACAT hardness ratios as detailed in Padovani & Giommi (1996). Where an object was observed more than once by ROSAT, the X-ray luminosity plotted represents the average luminosity.

When complete, the DXRBS blazar sample will include more than 300 blazars, considerably larger than any previous complete sample of blazars. Combining the objects for which we have announced identifications in this paper with previously identified objects, the sample is now over 50% identified. All further analysis in this paper will be done using all identified objects with redshifts (including both newly and previously identified objects).