English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Escaping Lyman continuum photons from galaxies likely reionized theintergalactic medium at redshifts $z\gtrsim6$. However, the Lyman continuum isnot directly observable at these redshifts and secondary indicators of Lymancontinuum escape must be used to estimate the budget of ionizing photons.Observationally, at redshifts $z\sim2-3$ where the Lyman continuum isobservationally accessible, surveys have established that many objects thatshow appreciable Lyman continuum escape fractions $f_{esc}$ also show enhanced[OIII]/[OII] (O$_{32}$) emission line ratios. Here, we use radiative transferanalyses of cosmological zoom-in simulations of galaxy formation to study thephysical connection between $f_{esc}$ and O$_{32}$. Like the observations, wefind that the largest $f_{esc}$ values occur at elevated O$_{32}\sim3-10$ andthat the combination of high $f_{esc}$ and low O$_{32}$ is extremely rare.While high $f_{esc}$ and O$_{32}$ often are observable concurrently, thetimescales of the physical origin for the processes are very different. LargeO$_{32}$ values fluctuate on short ($\sim$1 Myr) timescales during theWolf-Rayet-powered phase after the formation of star clusters, while channelsof low absorption are established over tens of megayears by collections ofsupernovae. We find that while there is no direct causal relation between$f_{esc}$ and O$_{32}$, high $f_{esc}$ most often occurs after continuous inputfrom star formation-related feedback events that have corresponding excursionsto large O$_{32}$ emission. These calculations are in agreement withinterpretations of observations that large $f_{esc}$ tends to occur whenO$_{32}$ is large, but large O$_{32}$ does not necessarily imply efficientLyman continuum escape.

the astrophysical journal. letters

The Lyman Continuum Escape Survey: Connecting Time-Dependent [OIII] and  [OII] Line Emission with Lyman Continuum Escape Fraction in Simulations of  Galaxy Formation