Absorption-Line Systems and Galaxies in Front of the Second Brightest Quasar, PHL 1811

Details Absorption-Line Systems and Galaxies in Front of the Second Brightest Quasar, PHL 1811 Absorption-Line Systems and Galaxies in Front of the Second Brightest Quasar, PHL 1811

2003-03-17

arxiv.org/abs/astro-ph/0303396v1

Astron.J.125:2824,2003

Astronomy and Astrophysics

Astrophysics

47 pages, 5 figures, to appear in the June 2003 issue of the Astronomical Journal

Scientific paper

10.1086/375321

The extraordinarily bright quasar PHL 1811 at a redshift z = 0.192 provides an attractive opportunity to use ultraviolet absorption-line spectroscopy to study the properties of gas systems in the local universe. An R = 20,000 far-UV spectrum recorded by FUSE revealed 7 extragalactic absorption systems, one of which is a Lyman limit system at z = 0.08093 accompanied by three systems having redshifts which differ from it by less than 0.008. The abundance of O with respect to Fe in the Lyman limit system is not much different from the solar abundance ratio. Supplementary low resolution spectra recorded by STIS (on HST) at longer wavelengths helped to substantiate our identifications of systems in the FUSE spectrum and suggested the presence of an additional 4 systems that could be detected only through their Ly-alpha features. Spectroscopy at visible wavelengths of 7 galaxies within approximately 2' of PHL 1811 indicated that 2 of them are near the redshift of the quasar and 4 have redshifts within 850 km/s of the extragalactic absorption systems. The Lyman limit system is likely associated with an L* galaxy lying 23" from the sightline. Finally, in addition to prominent features at very low velocities arising from the disk of our Galaxy, the strong resonance transitions of C II and Mg II show evidence for material at v = -200 km/s; the column densities of these two species suggest that 17.7 < log N(H I) < 18.1 if the material has a solar composition.

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