Influence of the spectral energy distribution of reionization-era sources on the Lyman-α forest

ABSTRACT Interpreting Lyman-$\alpha$ forest properties during the epoch of reionization requires assumptions about the spectral energy distribution (SED) of ionizing sources. These are often simplified to blackbody or power-law spectra, potentially overlooking contributions from high-energy processes. In this work, we investigate how different SED models of reionization-era sources shape the thermal and ionization state of the intergalactic medium (IGM) and imprint on the Ly $\alpha$ forest during the late stages of reionization. We perform 3D radiative transfer simulations with crash, post-processed on Sherwood-type hydrodynamical outputs, exploring both physically motivated SEDs i.e. SED including X-ray binaries, Bremsstrahlung from shock-heated interstellar medium, and binary stars, and idealized blackbody and power-law spectra. While the large-scale morphology of ionized regions is broadly similar across all models, harder spectral components extend partially ionized zones, produce larger He iii regions, and heat the surrounding IGM. By adopting simplified spectra there is the risk of underestimating the contribution of high-energy sources, which for most models we consider are found to alter the effective optical depth, the flux power, and the local transmissivity within the current ${\sim} 1 \sigma$ measurement uncertainties. The differences across models are most pronounced in the behaviour of the proximity zone and in the power at intermediate scales, offering the most promising diagnostics to disentangle source populations. With upcoming high-precision measurements from ELT and DESI, realistic SED modelling will be essential for robustly connecting Ly $\alpha$ forest observations to the sources driving the end of reionization.