Limits on non-canonical heating and turbulence in the intergalactic medium from the low redshift Lyman-alpha forest

Abstract

We examine the column density distribution function (CDDF) and Doppler parameter distribution from hydrodynamical simulations and Cosmic Origins Spectrograph (COS) observations of the Lyman-alpha forest at redshift $0\le z\le 0.2$. Allowing for a factor of two uncertainty in the metagalactic HI photoionisation rate, our hydrodynamical simulations are in good agreement ($1$-$1.5\sigma$) with the shape and amplitude of the observed CDDF at HI column densities $10^{13.3}\mathrm{c}{\mathrm{m}}^{-2}\le {\mathrm{N}}_{\mathrm{HI}}\le 10^{14.5}\mathrm{c}{\mathrm{m}}^{-2}$. However, the Doppler widths of the simulated lines remain too narrow with respect to the COS data. We argue that invoking AGN feedback does not resolve this discrepancy. We also disfavour enhanced photoheating rates as a potential solution, as this requires an unphysically hard UV background spectrum. If instead appealing to a non-canonical source of heating, an additional specific heat injection of $u\lesssim 6.9\mathrm{eV}{\mathrm{m}}_{\mathrm{p}}^{-1}$ is required at $z\lesssim 2.5$ for gas that has $N_{\mathrm{HI}}\simeq 10^{13.5}\mathrm{c}{\mathrm{m}}^{-2}$ by $z=0.1$. Alternatively, there may be an unresolved line of sight turbulent velocity component of $v_{\mathrm{turb}}\lesssim 8.5\mathrm{km}{\mathrm{s}}^{-1}({\mathrm{N}}_{\mathrm{HI}}/10^{13.5}\mathrm{c}{\mathrm{m}}^{-2}{)}^{0.21}$ for the coldest gas in the diffuse IGM.

arXiv comment21 pages, 13 figures, MNRAS accepted following revision. The accepted version includes an extra panel in figure 2 and some additional clarifications on the line broadening within the models. Conclusions unchanged

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