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We present an analysis of high‐resolution hydrodynamical  N ‐body simulations of coupled dark energy cosmologies which focuses on the statistical properties of the transmitted Lyman α flux in the high‐redshift intergalactic medium (IGM). In these models the growth of the diffuse cosmic web differs from the standard ΛCDM case: the density distribution is skewed towards underdense regions and the matter power spectra are typically larger (in a scale‐dependent way). These differences are also appreciable in the Lyman α flux and are larger than 5 per cent (10 per cent) at   z = 2–4  in the flux probability distribution function (pdf) for high‐transmissivity regions and for values of the coupling parameter  β= 0.08 (β= 0.2 ). The flux power spectrum is also affected at the ∼2 per cent (∼5–10 per cent) level for  β= 0.08 (β= 0.2 ) in a redshift‐dependent way. We infer the behaviour of flux pdf and flux power for a reasonable range of couplings and present constraints using present high‐ and low‐resolution data sets. We find an upper limit  β≲ 0.15  (at 2σ confidence level), which is obtained using only IGM data and is competitive with those inferred from other large‐scale structure probes.

The impact of coupled dark energy cosmologies on the high‐redshift intergalactic medium