High-redshift JWST predictions from IllustrisTNG: II. Galaxy line and continuum spectral indices and dust attenuation curves

Abstract

We present predictions for high redshift (z = 2-10) galaxy populations based on the BlustrisTNG simulation suite and a full Monte Carlo dust radiative transfer post-processing. Specifically, we discuss the H alpha and H beta [O III] luminosity functions up to z = 8. The predicted H beta + [O III] luminosity functions are consistent with present observations at z less than or similar to 3 with less than or similar to 0.1 dex differences in luminosities. However, the predicted H alpha luminosity function is similar to 0.3 dex dimmer than the observed one at z similar or equal to 2. Furthermore, we explore continuum spectral indices, the Balmer break at 4000 angstrom; (D4000) and the UV continuum slope beta. The median D4000 versus specific star formation rate relation predicted at z = 2 is in agreement with the local calibration despite a different distribution pattern of galaxies in this plane. In addition, we reproduce the observed A(UV) versus beta relation and explore its dependence on galaxy stellar mass, providing an explanation for the observed complexity of this relation. We also find a deficiency in heavily attenuated, UV red galaxies in the simulations. Finally, we provide predictions for the dust attenuation curves of galaxies at z = 2-6 and investigate their dependence on galaxy colours and stellar masses. The attenuation curves arc steeper in galaxies at higher redshifts, with bluer colours, or with lower stellar masses. We attribute these predicted trends to dust geometry. Overall, our results are consistent with present observations of high-redshift galaxies. Future James Webb Space Telecope observations will further test these predictions.