Broadening of QSO Ly α forest absorbers

We investigate the dependence of QSO Ly α absorption features on the temperature of the absorbing gas and on the amplitude of the underlying dark‐matter fluctuations. We use high‐resolution hydrodynamic simulations in cold dark matter dominated cosmological models. In models with a hotter intergalactic medium (IGM), the increased temperature enhances the pressure gradients between low‐ and high‐density regions and this changes the spatial distribution and the velocity field of the gas. Combined with more thermal broadening, this leads to significantly wider absorption features in hotter models. Cosmological models with little small‐scale power also have broader absorption features, because fluctuations on the scale of the Jeans length are still in the linear regime. Consequently, both the amplitude of dark‐matter fluctuations on small scales and thermal smoothing affect the flux decrement distribution in a similar way. However, the b ‐parameter distribution of Voigt profile fits, obtained by deblending the absorption features into a sum of thermally broadened lines, is largely independent of the amount of small‐scale power, but does depend strongly on the IGM temperature. The same is true for the two‐point function of the flux and for the flux power spectrum on small scales. These three flux statistics are thus sensitive probes of the temperature of the IGM. We compare the values computed for our models and obtained from a HIRES spectrum of the quasar Q1422+231 and conclude that the IGM temperature at z ∼3.25 is fairly high, T 0 ≳15 000 K. The flux decrement distribution of the observed spectrum is fitted well by that of a ΛCDM model with that temperature.