We present a study of the intrinsic absorption lines in the ultraviolet spectra of Seyfert 1 galaxies. The study is based on spectra from the Hubble Space T elescope and includes the Seyfert 1 galaxies observed with the Faint Object Spectrograph and Goddard High-Resolution Spectrograph at spectral resolutions of j/*j B 1000È20,000 with good signal-to-noise ratios. We Ðnd that the fraction of Seyfert 1 galaxies that show intrinsic absorption associated with their active nuclei is more than one-half (10 of 17), which is much higher than previous estimates (3%È10%) based on IUE data. There is a one-to-one correspondence between Seyfert galaxies that show intrinsic UV absorption and X-ray "" warm absorbers, ÏÏ indicating that these two phenomena are related. Although our sample is not complete, we conclude that intrinsic absorption represents an important component that needs to be integrated into our overall physical picture of active galaxies. The intrinsic UV absorption is generally characterized by high ionization : C IV and N V are seen in all 10 Seyfert galaxies with detected absorption (in addition to Lya), whereas Si IV is present in only four of these Seyfert galaxies, and Mg II absorption is detected only in NGC 4151. The absorption lines are blueshifted (or in a few cases at rest) with respect to the narrow emission lines, indicating that the absorbing gas is undergoing net radial outÑow. At high resolution, the absorption often splits into distinct kinematic components that show a wide range in widths (20È400 km s~1 FWHM), indicating macroscopic motions (e.g., radial velocity subcomponents or turbulence) within a component. The strong absorption components have cores that are much deeper than the continuum Ñux levels, indicating that the regions responsible for these components lie completely outside of the broad emission-line regions. Additional information on the covering factors and column densities can be derived from the absorption proÐles in the high-resolution spectra. The covering factor of the absorbing gas in the line of sight, relative to the total underlying emission, is on average. The global C los º 0.86, covering factor, which is the fraction of emission intercepted by the absorber averaged over all lines of sight, is Thus, structures covering large solid angles as seen by the central continuum source C global º 0.5. (e.g., spherical shells, sheets, or cones with large opening angles) are required. The individual absorption components show a wide range in C IV column densities (0.1È14 ] 1014 cm~2), and the ratio of N V to C IV column density varies signiÐcantly from one absorption component to the next, even in the same Seyfert galaxy. Thus, the intrinsic absorption in a Seyfert 1 galaxy is typically comprised of distinct kinematic components that are characterized by a range in physical conditions (e.g., ionization parameter and hydrogen column density). Finally, we show evidence for extreme variability in the intrinsic absorption lines of NGC 3783. In addition to our earlier repo...

Coronagraphic imaging with the Space Telescope Imaging Spectrograph on board the Hubble Space T elescope reveals a D450 AU radius circumstellar disk around the Herbig Ae star HD 163296. A broadband (0.2È1.0 km) reÑected light image shows the disk oriented at a position angle of 140¡^5¡ and inclined to our line of sight by D60¡^5¡. The disk includes an annulus of reduced scattering at 325 AU and exhibits a Ñat trend of surface brightness in to 180È122 AU consistent with a cleared (1A .5È1A), central zone. For r º 370 AU the disk surface brightness drops as r to the approximately [3.5 power. The disk cannot be traced beyond 450 AU in our data. The disk is accompanied by a chain of nebulosities at compatible with detection of a Herbig-Haro Ñow. The HD 163296 disk most P.A.\42¡ .5^3¡ .5, closely resembles the disk of HD 141569. As in the HD 141569 system, the dynamical e †ects of a planet may be necessary to explain the structure in the outer disk.

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