Spectral Analysis of the Lyα Forest in a Cold Dark Matter Cosmology

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Abstract

We simulate the Lya forest in a standard cold dark matter universe using a two-level hierarchical grid code to evolve the dark and baryonic matter components self-consistently. We solve the time-dependent ionization equations for hydrogen and helium, adopting Haardt & Madaus recent estimate for the metagalactic UV radiation background. We compare our simulation results with the measured properties of the Lya forest by constructing synthetic spectra and analyzing them using an automated procedure to identify, deblend, and t Voigt line proles to the absorption features. The H I column density and Doppler parameter distributions that we obtain agree closely with those measured by the Keck Obser-vatorys High Resolution Eschelle Spectrograph (HIRES) and earlier high spectral resolution observations over the column density range 1012 cm~2. In particular, we nd that a cm~2 \ N H I \ 1016 power-law column density distribution persists to the lowest values (D1012 cm~2) reported from the HIRES measurements, in agreement with the incompleteness-corrected observations. We are able to match the normalization of the column density distribution at the low end using the Haardt & Madau spectrum and a baryon density consistent with nucleosynthesis limits. We nd, however, a signicant decit of systems at higher column densities, greater than a few times 1016 cm~2. The decit arises N H I from a curvature in the column density distribution that may not be removed by an overall renormalization. We nd evolution in the cloud number density and opacity comparable to the observed evolution, though growing somewhat too quickly at the highest redshifts. The evolution, however, is sensitive to the assumed UV radiation eld, which becomes increasingly uncertain at higher redshifts (z [ 3.5). We also compare with measured values of the intergalactic He II opacity. Our results require an He II ionizing background lower than the Haardt & Madau estimate by a factor of 4, corresponding to a soft intrinsic QSO spectrum, with a Q B 1.82.

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