A HUBBLE-SPACE-TELESCOPE IMAGING SURVEY OF NEARBY ACTIVE GALACTIC NUCLEI

We have obtained WFPC2 images of 256 of the nearest (z less than or eq ual to 0.035) Seyfert 1, Seyfert 2, and starburst galaxies. Our 500 s broadband (F606W) exposures reveal much fine-scale structure in the ce nters of these galaxies, including dust lanes and patches, bars, rings , wisps, and filaments, and tidal features such as warps and tails. Mo st of this fine structure cannot be detected in ground-based images. W e have assigned qualitative classifications for these morphological fe atures and a Hubble type for the inner region of each galaxy, and we h ave also measured quantitative information such as 0.'' 18 and 0.'' 92 aperture magnitudes, position angles, and ellipticities, where possib le. There is little direct evidence for unusually high rates of intera ction in the Seyfert galaxies. Slightly less than 10% of all the galax ies show tidal features or multiple nuclei. The incidence of inner sta rburst rings is about 10% in both classes of Seyfert galaxies. In cont rast, galaxies with H II region emission-line spectra appear substanti ally more irregular and clumpy because of their much higher rates of c urrent star formation per unit of galactic mass. The presence of an un resolved central continuum source in our Hubble Space Telescope images is a virtually perfect indicator of a Seyfert 1 nucleus as seen by gr ound-based spectroscopy. Fifty-two percent of these Seyfert 1 point so urces are saturated in our images; we use their wings to estimate magn itudes ranging from 15.8 to 18.5. The converse is not universally true , however, as over one-third of Seyferts with direct spectroscopic evi dence for broad Balmer wings show no nuclear point source. These 34 re solved Seyfert 1's have fainter nonstellar nuclei, which appear to be more extinguished by dust absorption. Like the Seyfert 2's, they have central surface brightnesses consistent with those expected for the bu lges of normal galaxies. The rates for the occurrences of bars in Seyf ert 1's and 2's and non-Seyferts are the same. We found one significan t morphological difference between the host galaxies of Seyfert 1 and Seyfert 2 nuclei. The Seyfert 2 galaxies are significantly more likely to show nuclear dust absorption, especially in lanes and patches that are irregular or reach close to the nucleus. A few simple tests show that the difference cannot be explained by different average redshifts or selection techniques. It is confirmed by our galaxy morphology cla ssifications, which show that Seyfert 1 nuclei reside in earlier type galaxies than Seyfert 2 nuclei. If, as we believe, this is an intrinsi c difference in host galaxy properties, it undermines one of the postu lates of the strong unification hypothesis for Seyfert galaxies, that they merely appear different because of the orientation of their centr al engine. The excess galactic dust we see in Seyfert 2's may cause su bstantial absorption that obscures their hypothesized broad emission l ine regions and central nonstellar continua. This galactic dust could produce much of the absorption in Seyfert 2 nuclei that had instead be en attributed to a thick dusty accretion torus forming the outer part of the central engine.