All Tables

Table 1: List of observed sources. Columns 2 and 3 give the coordinates used in the observations and for correlation, Col. 4 gives the source distances in Mpc. Column 5 gives the classification according to Véron-Cetty & Véron (2001).
Table 2: Results from the observations. "Tapered'' 6 cm flux densities were measured using images tapered and restored with the 18 cm beam size. The MERLIN 18 cm and 6 cm positions differ by 35 mas because the coordinates used at the correlator were changed in an unknown way and the resulting offset could not be removed accurately. We have precessed the MERLIN B1950 coordinates to J2000 using NRAO's scheduling software SCHED. Positions are absolute for observations that were phase-referenced and the phase-referencing worked; such positions are given in h, m, s (for RA) and $^{\circ }$ , $^{\prime }$ , $^{\prime \prime }$ (for Dec). Otherwise the positions are given in mas relative to the strongest component. The flux density error estimates represent $1~\sigma$ .
Table 3: All Seyferts observed with VLBI. Column 1 lists the names we used, Col. 2 the names used by Véron-Cetty & Véron (2001), Col. 3 the Seyfert types as described by Véron-Cetty & Véron (2001), Col. 4 the linear resolution in pc, Col. 5 the instrument and frequency used, and Col. 6 the reference to the publication.
Table 4: Seyferts from Table 3 that have dual-frequency (18 cm and 6 cm) VLBI observations with matching beam sizes, from which the spectral index is derived. Asterisks denote objects with at least one component with a flat or inverted spectrum.
Table 5: Fraction of flat- and inverted-spectrum components in various Seyfert samples. The column " $N_{\alpha >-0.3}$ '' gives the number of components with spectral indices $\alpha >-0.3$ (i.e., components with flat or inverted spectra). The column " $N_{\rm total}$ '' gives the total number of components in each sample. The column % gives $(N_{\alpha >-0.3}/N_{\rm total})\times 100$ . The column P gives the level of significance from a comparison of the fraction of flat- and inverted-spectrum components in the VLBI sample of this paper (limits treated as detections), to that of each comparison sample at arcsec resolution, using the difference-of-two-proportions test with Yates correction for continuity (e.g., Glanz 1992).
Table 6: Comparison of the spectral index distribution of the VLBI Seyfert sample to various other Seyfert samples. The level of significance gives the probability that the spectral index distribution of the comparison sample and the VLBI seyfert sample in this paper were drawn from the same parent population.
Table 7: Subset of sources from Table 3 for which both pc and kpc-scale structures have been observed. The misalignment angle, $\Delta \Theta$ , is calculated as $\Theta ({\rm pc}){-}\Theta ({\rm kpc})$ , and has then been reflected onto the range of $0^{\circ }$ to $90^{\circ }$ . For the seven objects at the end of the table, either the PA information of the kpc scale structure was not completely reliable or was unavailable. The position angles of the galaxy minor axes in the last column were drawn from de Vaucouleurs et al. (1991), except for those marked a taken from Schmitt & Kinney (2000) and those marked b measured by us from Hubble Space Telescope archival images (see Sect. 4.3).