2002/08/30 by David V. Bowen, Max Pettini, J. Chris Blades +1 · 2 citations
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Cosmic Phenomena #Astrophysics and Star Formation Studies #Emission spectrum #Equivalent width #Galaxies: Formation, Evolution, Phenomena #Galaxy #Geometry #Hubble space telescope #Line (geometry) #Line-of-sight #Physics #Quasar #Redshift #Space Telescope Imaging Spectrograph #Spectral line #Spectrograph #astro-ph
paper · pdf · doi:10.1086/343106
published as Astrophys.J.580:169-193,2002 · Accepted for publication in Nov 20, 2002 issue of ApJ. Paper with all figures can be found at http://www.astro.princeton.edu/~dvb/lyapaper.ps (preferable). Minor typos fixed
arxiv created 2002/08/30 · openalex publication_date 2002/11/20 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We have used the Space Telescope Imaging Spectrograph (STIS) aboard the Hubble Space Telescope to search for Lyα absorption lines in the outer regions of eight nearby galaxies using background quasars and AGNs as probes. Lyα lines are detected within a few hundred kilometers per second of the systemic velocity of the galaxy in all cases. We conclude that a background line of sight that passes within 26-200 h -1 kpc of a foreground galaxy is likely to intercept low column density neutral hydrogen with log N ≳ 13.0. The ubiquity of detections implies a covering factor of ≃100% for low N (H I) gas around galaxies within 200 h -1 kpc. We find, however, that the Lyα lines are usually composed of individual components spread out in velocity over ranges of 300-900 km s -1 . Two sight lines show components that are unusually broad for low-redshift Lyα systems, with Doppler parameters ~150 km s -1 . These may arise in intragroup gas at temperatures of (1-2) × 10 6 K. We discuss the difficulty in trying to associate individual absorption components with the selected galaxies and their neighbors but show that by degrading our STIS data to lower resolutions, we are able to reproduce the anticorrelation of Lyα equivalent width and impact parameter found at higher redshift. The anticorrelation does not improve by correcting for the absolute magnitude of a galaxy in the same way as found at higher z . We also show that the equivalent width and column density of Lyα complexes (when individual components are summed over ~1000 km s -1 ) correlate well with a simple estimate of the volume density of galaxies brighter than M B = -17.5 at the same redshift as a Lyα complex. We do not reject the hypothesis that the selected galaxies are directly responsible for the observed Lyα lines, but our analysis indicates that absorption by clumpy intragroup gas is an equally likely explanation.