The redshift evolution of rest-UV spectroscopic properties to z ∼ 5

April 2020 • 2020MNRAS.493.3194P

Authors • Pahl, Anthony J. • Shapley, Alice • Faisst, Andreas L. • Capak, Peter L. • Du, Xinnan • Reddy, Naveen A. • Laursen, Peter • Topping, Michael W.

Abstract • We perform a comprehensive analysis of the redshift evolution of the rest-UV spectra of star-forming galaxies out to z ∼ 5. We combine new z ∼ 5 measurements of H I Ly α and low- and high-ionization interstellar metal absorption features with comparable measurements at z ∼ 2-4. We measure the equivalent widths of interstellar absorption features using stacked spectra in bins of Ly α equivalent width, performing corrections to Ly α strengths based on a model for the transmission of the intergalactic medium. We find a strong correlation between decreasing low-ionization absorption strength and increasing Ly α emission strength over the redshift range z ∼ 2-5, suggesting that both of these quantities are fundamentally linked to neutral gas covering fraction. At the highest Ly α equivalent widths, we observe evolution at z ∼ 5 towards greater Ly α emission strength at fixed low-ionization absorption strength. If we interpret the non-evolving relationship of Ly α emission strength and low-ionization line strength at z ∼ 2-4 as primarily reflecting the radiative transfer of Ly α photons, this evolution at z ∼ 5 suggests a higher intrinsic production rate of Ly α photons than at lower redshift. Our conclusion is supported by the joint evolution of the relationships among Ly α emission strength, interstellar absorption strength, and dust reddening. We perform additional analysis in bins of stellar mass, star formation rate, UV luminosity, and age, examining how the relationships between galaxy properties and Ly α emission evolve towards higher redshift. We conclude that increasing intrinsic Ly α photon production and strong detection of nebular C IV emission (signalling lower metallicity) at z ∼ 5 indicate an elevated ionized photon production efficiency (ξion).


IPAC Authors


Andreas Faisst

Assistant Scientist