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The Ultraviolet Emission Properties of Five Low-Redshift Active Galactic Nuclei at High Signal to Noise and Spectral Resolution

We analyze the ultraviolet (UV) emission line and continuum properties of five low-redshift active galactic nuclei (four luminous quasars: PKS~0405$-$123, H1821+643, PG~0953+414, and 3C273, and one bright Seyfert 1 galaxy: Mrk~205). The HST spectra have higher signal-to-noise ratios (typically $\sim 60$ per resolution element) and spectral resolution ($R = 1300$) than all previously- published UV spectra used to study the emission characteristics of active galactic nuclei. We include in the analysis ground-based optical spectra covering \hb\ and the narrow [O III] $λλ$4959,5007 doublet. The following new results are obtained: \lyb/\lya=0.03$-$0.12 for the four quasars, which is the first accurate measurement of the long-predicted \lyb\ intensity in QSOs. The cores of \lya\ and C~IV are symmetric to an accuracy of better than 2.5% within about 2000 km s$^{-1}$ of the line peak. This high degree of symmetry of \lya\ argues against models in which the broad line cloud velocity field has a significant radial component. The observed smoothness of the \lya\ and C~IV line profiles requires at least $\sim 10^4$ individual clouds if bulk velocity is the only line-broadening mechanism. The overall similarity of the \lya\ and C IV $λ$1549 profiles rules out models for the broad line region (BLR) with a radial distribution of virialized....