学术文献库

We compute synthetic, rest-frame optical and ultraviolet (UV) emission-line properties of galaxy populations at redshifts from z$\approx$0 to z=8 in a full cosmological framework. We achieve this by coupling, in post-processing, the cosmological IllustrisTNG simulations with new-generation nebular-emission models, accounting for line emission from young stars, post-asymptotic-giant-branch (PAGB) stars, accreting black holes (BHs) and, for the first time, fast radiative shocks. The optical emission-line properties of simulated galaxies dominated by different ionizing sources are largely consistent with those expected from classical diagnostic diagrams and reflect the observed increase in [OIII]/H$β$ at fixed [NII]/H$α$ and the evolution of the H$α$, [OIII]$\lambda5007$ and [OII]$\lambda3727$ luminosity functions from z$\approx$0 to z$\sim$2. At higher redshift, we find that the emission-line galaxy population is dominated by star-forming and active galaxies, with negligible fractions of shock- and PAGB-dominated galaxies. We highlight 10 UV-diagnostic diagrams able to robustly identify the dominant ionizing sources in high-redshift galaxies. We also compute the evolution of several optical- and UV-line luminosity functions from z=4 to z=7, and the number of galaxies expected to be detectable per field of view in deep, medium-resolution spectroscopic observations with the NIRSpec instrument on board the James Webb Space Telescope. We find that 2-hour-long exposures are sufficient to achieve unbiased censuses of H$α$ and [OIII]$\lambda5007$ emitters, while at least 5 hours are required for H$β$, and even 10 hours will detect only progressively smaller fractions of [OII]$\lambda3727$, OIII]$\lambda1663$, CIII]$\lambda1908$, CIV$\lambda1550$, [NII]$\lambda6584$, SiIII]$\lambda1888$ and HeII$\lambda1640$ emitters, especially in the presence of dust.