The effects of an ionizing background on the HI column density distribution in the local Universe

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Abstract
Using data on the HI column density distribution in the local Universe, f(N_{HI}), we show how to determine g(N_{H}), the distribution of the total gas (HI+HII) column density. A simple power law fit to f(N_{HI}) fails due to bendings in the distributions when N_{HI}<10^{20} cm^{-2} and H is no longer fully neutral. If an ultraviolet background is responsible for the gas ionization, and g(N_{H}) is proportional N_{H}^{-alpha}, we find the values of alpha and of the intensity of the background radiation which are compatible with the present data. These best fitting values, however, depend upon the scaling law of the the gas volume densities with N_{H} and cannot be determined unambiguously. We examine in detail two models: one in which the average gas volume density decreases steadily with N_H, while in the other it stays constant at low column densities. The former model leads to a steep power law fit for g(N_{H}), with alpha of order 3.3 +- 0.4 and requires an ultraviolet flux larger than what the QSOs alone produce at z=0. For the latter alpha is 1.5 +- 0.1 and a lower ionizing flux is required. The ambiguities about the modelling and the resulting steep or shallow N_{H} distribution can be resolved only if new 21-cm observations and QSOs Lyman limit absorbers searches will provide more data in the HI-HII transition region at low redshifts. Using the best fit obtained for higher redshift data we outline two possible scenarios for the evolution of gaseous structures, compatible with the available data at z=0.

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