The Hubble Space Telescope Quasar Absorption Line Key Project XIII. A Census of Absorption Line Systems at Low Redshift

Details The Hubble Space Telescope Quasar Absorption Line Key Project XIII. A Census of Absorption Line Systems at Low Redshift The Hubble Space Telescope Quasar Absorption Line Key Project XIII. A Census of Absorption Line Systems at Low Redshift

1998-05-13

arxiv.org/abs/astro-ph/9805148v2

Astrophys.J.Suppl. 118 (1998) 1

Astronomy and Astrophysics

Astrophysics

27 pages, LaTeX file (no figs. and tables). Full version of article (including figures and tables) plus separate files for fig

Scientific paper

10.1086/313130

We present a catalogue of absorption lines obtained from the analysis of the ultra-violet spectra of 66 quasars. The data were acquired with the Faint Object Spectrograph of the HST as part of the Quasar Absorption Line Survey, a Key Project for the first four cycles of HST observations. This is the third of a series of catalogues of absorption lines produced from the survey and increases the number of quasars whose higher resolution (R=1300) spectra we have published from 17 to 83. The general properties and execution of the survey are reviewed, including descriptions of the final sample of observed objects and the algorithmic processes used to construct the catalogue. The detection of a single damped Ly-a system in a path length of Delta_z=49 yields an observed number of damped systems per unit redshift of (dN/dz)_{damp}(z=0.58)=0.020 with 95% confidence boundaries of 0.001 to 0.096 systems per unit redshift. We include notes on our analysis of each of the observed quasars and the absorption systems detected in each spectrum. Some especially interesting systems include low redshift Ly-a absorbers suitable for extensive follow-up observations (in the spectra of TON28 and PG1216+069), possibly physically associated pairs of extensive metal line absorption systems (e.g., in the spectrum of PG0117+213), and systems known to be associated with galaxies (e.g., in the spectrum of 3C232).

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