Astronomy and Astrophysics – Astrophysics
Scientific paper
2000-05-11
Mon.Not.Roy.Astron.Soc. 322 (2001) 561-575
Astronomy and Astrophysics
Astrophysics
16 pages, 8 figures. Accepted for publication in MNRAS. Revised following referee's comments
Scientific paper
10.1046/j.1365-8711.2001.04108.x
Analytic derivations of the correlation function and the column density distribution for neutral hydrogen in the IGM are presented, assuming that the non-linear baryonic mass density distribution in the IGM is lognormal. This ansatz was used earlier by Bi & Davidsen (1997) to perform 1D simulations of lines-of-sight and analyse the properties of absorption systems. Our approach is completely analytic, which allows us to explore a wide region of the parameter space for our model. The analytic results have been compared with observations, whenever possible. Two kinds of correlation functions are defined: along the line-of-sight (LOS) and across the transverse direction. We find that the effects on the LOS correlation due to change in cosmology and the slope of the equation of state of the IGM, \gamma are of the same order, which means that we cannot constrain both the parameters simultaneously. However, it is possible to constrain \gamma and its evolution using the observed LOS correlation function at different epochs, provided one knows the background cosmology. We suggest that the constraints on the evolution of \gamma obtained using the LOS correlation can be used as an independent tool to probe the reionisation history of the universe. From the transverse correlation function, we find that the excess probability, over random, of finding two neutral hydrogen overdense regions separated by an angle \theta, is always less than 1 per cent for redshifts greater than 2. Our models also reproduce the observed column density distribution for neutral hydrogen and the shape of the distribution depends on \gamma. Our calculations suggest that one can rule out \gamma > 1.6 for z \simeq 2.31 using the column density distribution. However, one cannot rule higher values of \gamma at higher redshifts.
Choudhury Tirthankar Roy
Padmanabhan Thanu
Srianand Raghunathan
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