Year: 1994
Type: article
Abstract: If gravitational clustering is a hierarchical process, the present large-scale structure of the galaxy distribution implies that structures on smaller scales must have formed at high redshift. We simulate the formation of small-scale structure (average cell mass: δm^bar^_b_ = 10^4.2^ M_sun_) and the evolution of photoionized gas, in the specific case of the CDM + {LAMBDA} model. The photoionized gas has a natural minimal scale of collapse, the Jeans scale (m_b,J_ ~ 10^9^ M_sun_). We find that low column density (N_HI_ <= 10^14^ cm^-2^) lines originate in regions resembling Zel'dovich pancakes, where gas with overdensities in the range 3-30 is enclosed by two shocks but is typically reexpanding at approximately the Hubble velocity. However, higher column density lines stem from more overdense regions where the shocked gas is cooling. We show that this model can probably account for the observed number of lines, their distribution in column density and b-parameters, as well as the cloud physical sizes as observed in gravitationally lensed quasars. We find a redshift evolution that is too steep; however, this may be due to insufficient dynamical range in the simulation or because the specific model is incorrect. The model predicts that high signal-to-noise observations should find systematic deviations from Voigt profiles, mainly in the form of broad wings in the line profiles, and that a fluctuating Gunn-Peterson effect will be detected, which can be modeled as a superposition of weak lines with a wide range of b-parameters.
Source: The Astrophysical Journal
DOI: 10.1086/187670
Authors: Renyue Cen, Jordi Miralda-Escude, Jeremiah P. Ostriker, Michael Rauch
Language: English
Subfield: Astronomy and Astrophysics
Field: Physics and Astronomy
Domain: Physical Sciences
Open Access status: green
OpenAlex ID: W1994777058