Observationnal constraints on the nature of the low redshift Lyman-alpha absorbers

Details Observationnal constraints on the nature of the low redshift Lyman-alpha absorbers Observationnal constraints on the nature of the low redshift Lyman-alpha absorbers

1995-09-28

arxiv.org/abs/astro-ph/9509146v1

Astronomy and Astrophysics

Astrophysics

20 pages of LATEX source without figures, using l-aa.sty. The Postscript version including figures is available at the followi

Scientific paper

We present results from a spectroscopic and imaging survey of galaxies in the fields of quasars from the HST Quasar Absorption Line Key Project. The aim of this survey is to identify galaxies within 3.5' from the quasar sightline, to a limiting r-band magnitude mr = 22.5. The data are then compared to the HST homogeneous sample of Lyman-alpha-only absorbers in order to put constraints on the nature of these absorbers, and in particular on their relation to galaxies. The analysis of our sample combined with those of previous studies shows that: 1) the redshift agreements of the Ly-alpha absorber-galaxy associations cannot be due to chance coincidence; 2) there is no clear anti-correlation between the Ly-alpha rest-frame equivalent width and the impact parameter for the whole sample. Our results suggest that most Ly-alpha absorbers are not gaseous clouds that belong in a strict sense to galaxies, as is the case for MgII absorbers. The fraction of associations to the total number of galaxies at impact parameter < D as a function of D drops from 1 to 0.65 at D = 200 H50 kpc and flattens at larger values of D (> 300 H50 kpc), which leads to Ly-alpha galactic halos sizes about three times larger than the inner MgII halo region; 3) there is no correlation between the galaxy luminosity and the impact parameter. This again suggests that a significant Ly-alpha clouds do not belong to individual galaxies, but instead are distributed in the local large-scale structure. 4) the HWHM=120 km/s of the relative velocity distribution of the Ly-alpha absorber-galaxy associations is consistent with either galaxy rotation velocities or the local velocity dispersion in large-scale structures.

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