2011/09/30 by Olivera Rakic, Joop Schaye, Charles C. Steidel +1 · 2 citations
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Galaxies: Formation, Evolution, Phenomena #Galaxy #Halo #Optical depth #Physics #QSOS #Quasar #RADIUS #Redshift #Star formation #Stellar, planetary, and galactic studies #Virial theorem #astro-ph.CO
paper · pdf · doi:10.1088/0004-637x/751/2/94
Accepted for publication in the ApJ (replaced with revised version incorporating referee's comments)
arxiv created 2012/03/26 · openalex publication_date 2012/05/09 · arxiv updated 2012/06/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We study the interface between galaxies and the intergalactic medium by measuring the absorption by neutral hydrogen in the vicinity of star-forming galaxies at z ≈ 2.4. Our sample consists of 679 rest-frame UV-selected galaxies with spectroscopic redshifts that have impact parameters <2 (proper) Mpc to the line of sight of one of the 15 bright, background QSOs and that fall within the redshift range of its Lyα forest. We present the first two-dimensional maps of the absorption around galaxies, plotting the median Lyα pixel optical depth as a function of transverse and line-of-sight separation from galaxies. The Lyα optical depths are measured using an automatic algorithm that takes advantage of all available Lyman series lines. The median optical depth, and hence the median density of atomic hydrogen, drops by more than an order of magnitude around 100 kpc, which is similar to the virial radius of the halos thought to host the galaxies. The median remains enhanced, at the >3σ level, out to at least 2.8 Mpc (i.e., >9 comoving Mpc), but the scatter at a given distance is large compared with the median excess optical depth, suggesting that the gas is clumpy. Within 100 (200) kpc, and over ±165 km s −1 , the covering fraction of gas with Lyα optical depth greater than unity is 100 +0 − 32 % (66% ± 16%). Absorbers with τ Lyα > 0.1 are typically closer to galaxies than random. The mean galaxy overdensity around absorbers increases with the optical depth and also as the length scale over which the galaxy overdensity is evaluated is decreased. Absorbers with τ Lyα ∼ 1 reside in regions where the galaxy number density is close to the cosmic mean on scales ⩾0.25 Mpc. We clearly detect two types of redshift space anisotropies. On scales <200 km s −1 , or <1 Mpc, the absorption is stronger along the line of sight than in the transverse direction. This "finger of God" effect may be due to redshift errors, but is probably dominated by gas motions within or very close to the halos. On the other hand, on scales of 1.4–2.0 Mpc the absorption is compressed along the line of sight (with >3σ significance), an effect that we attribute to large-scale infall (i.e., the Kaiser effect).