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The Lyman Continuum Escape Survey: Connecting Time-Dependent [OIII] and [OII] Line Emission with Lyman Continuum Escape Fraction in Simulations of Galaxy Formation
Astrophysics of Galaxies · Submitted 1 Oct 2020
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We find that while there is no direct causal relation between $f_{esc}$ and O$_{32}$, high $f_{esc}$ most often occurs after continuous input from star formation-related feedback events that have corresponding excursions to large O$_{32}$ emission.
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The abstract, sentence by sentence
Escaping Lyman continuum photons from galaxies likely reionized the intergalactic medium at redshifts $z\gtrsim6$. However, the Lyman continuum is not directly observable at these redshifts and secondary indicators of Lyman continuum escape must be used to estimate the budget of ionizing photons. Observationally, at redshifts $z\sim2-3$ where the Lyman continuum is observationally accessible, surveys have established that many objects that show appreciable Lyman continuum escape fractions $f_{esc}$ also show enhanced [OIII]/[OII] (O$_{32}$) emission line ratios. Here, we use radiative transfer analyses of cosmological zoom-in simulations of galaxy formation to study the physical connection between $f_{esc}$ and O$_{32}$. Like the observations, we find that the largest $f_{esc}$ values occur at elevated O$_{32}\sim3-10$ and that the combination of high $f_{esc}$ and low O$_{32}$ is extremely rare. While high $f_{esc}$ and O$_{32}$ often are observable concurrently, the timescales of the physical origin for the processes are very different. Large O$_{32}$ values fluctuate on short ($\sim$1 Myr) timescales during the Wolf-Rayet-powered phase after the formation of star clusters, while channels of low absorption are established over tens of megayears by collections of supernovae. We find that while there is no direct causal relation between $f_{esc}$ and O$_{32}$, high $f_{esc}$ most often occurs after continuous input from star formation-related feedback events that have corresponding excursions to large O$_{32}$ emission. These calculations are in agreement with interpretations of observations that large $f_{esc}$ tends to occur when O$_{32}$ is large, but large O$_{32}$ does not necessarily imply efficient Lyman continuum escape.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Escaping Lyman continuum photons from galaxies likely reionized the intergalactic medium at redshifts $z\gtrsim6$. | background 1.00 | 0.04 | 0.03 | hedged possibility 1.00 |
| s1 | However, the Lyman continuum is not directly observable at these redshifts and secondary indicators of Lyman continuum escape must be used to estimate the budget of ionizing photons. | background 0.83 | 0.04 | 0.02 | asserted 1.00 |
| s2 | Observationally, at redshifts $z\sim2-3$ where the Lyman continuum is observationally accessible, surveys have established that many objects that show appreciable Lyman continuum escape fractions $f_{esc}$ also show enhanced [OIII]/[OII] (O$_{32}$) emission line ratios. | background 1.00 | 0.04 | 0.04 | asserted 1.00 |
| s3 | Here, we use radiative transfer analyses of cosmological zoom-in simulations of galaxy formation to study the physical connection between $f_{esc}$ and O$_{32}$. | method 0.54 | 0.92 | 0.04 | asserted 0.84 |
| s4 | Like the observations, we find that the largest $f_{esc}$ values occur at elevated O$_{32}\sim3-10$ and that the combination of high $f_{esc}$ and low O$_{32}$ is extremely rare. | result 1.00 | 0.97 | 0.31 | asserted 1.00 |
| s5 | While high $f_{esc}$ and O$_{32}$ often are observable concurrently, the timescales of the physical origin for the processes are very different. | result 0.74 | 0.69 | 0.08 | asserted 1.00 |
| s6 | Large O$_{32}$ values fluctuate on short ($\sim$1 Myr) timescales during the Wolf-Rayet-powered phase after the formation of star clusters, while channels of low absorption are established over tens of megayears by collections of supernovae. | result 0.81 | 0.79 | 0.08 | asserted 1.00 |
| s7 | We find that while there is no direct causal relation between $f_{esc}$ and O$_{32}$, high $f_{esc}$ most often occurs after continuous input from star formation-related feedback events that have corresponding excursions to large O$_{32}$ emission. | result 0.60 | 0.95 | 0.67 | asserted 1.00 |
| s8 | These calculations are in agreement with interpretations of observations that large $f_{esc}$ tends to occur when O$_{32}$ is large, but large O$_{32}$ does not necessarily imply efficient Lyman continuum escape. | interpretation 0.97 | 0.36 | 0.44 | asserted 0.52 |
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The paper
Original abstract
Escaping Lyman continuum photons from galaxies likely reionized the intergalactic medium at redshifts $z\gtrsim6$. However, the Lyman continuum is not directly observable at these redshifts and secondary indicators of Lyman continuum escape must be used to estimate the budget of ionizing photons. Observationally, at redshifts $z\sim2-3$ where the Lyman continuum is observationally accessible, surveys have established that many objects that show appreciable Lyman continuum escape fractions $f_{esc}$ also show enhanced [OIII]/[OII] (O$_{32}$) emission line ratios. Here, we use radiative transfer analyses of cosmological zoom-in simulations of galaxy formation to study the physical connection between $f_{esc}$ and O$_{32}$. Like the observations, we find that the largest $f_{esc}$ values occur at elevated O$_{32}\sim3-10$ and that the combination of high $f_{esc}$ and low O$_{32}$ is extremely rare. While high $f_{esc}$ and O$_{32}$ often are observable concurrently, the timescales of the physical origin for the processes are very different. Large O$_{32}$ values fluctuate on short ($\sim$1 Myr) timescales during the Wolf-Rayet-powered phase after the formation of star clusters, while channels of low absorption are established over tens of megayears by collections of supernovae. We find that while there is no direct causal relation between $f_{esc}$ and O$_{32}$, high $f_{esc}$ most often occurs after continuous input from star formation-related feedback events that have corresponding excursions to large O$_{32}$ emission. These calculations are in agreement with interpretations of observations that large $f_{esc}$ tends to occur when O$_{32}$ is large, but large O$_{32}$ does not necessarily imply efficient Lyman continuum escape.
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References
How the literature uses it
2 arXiv papers cite this in 3 sentences
What it cites · 2 sentences without a confident label
Builds on 1 paper
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Previous studies are extended by additionally examining time-dependent and line emission, and their relation to the ionizing photon production of newly-formed stars [ref] .
New Methods for Identifying Lyman Continuum Leakers and Reionization-Epoch Analogues · Introduction · 0.88
Uses data or values from 1 paper
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The simulation is run with cosmological parameters $Ω_M = 0.3065$, $Ω_Λ = 0.6935$, $Ω_b = 0.0483$, $h = 0.679$, $σ_8 = 0.8344$, and $n = 0.9681$, which are taken from the most recent release of the [ref] .
Planck 2018 results. VI. Cosmological parameters · Cosmological Simulation · 0.94
Compares with 1 paper
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A complementary recent study explored the statistics of these quantities in static outputs of multi-galaxy simulations [ref] , and the results are broadly consistent despite this studies focus on examining a the time-evolution of only a pair galaxies.
New Methods for Identifying Lyman Continuum Leakers and Reionization-Epoch Analogues · Discussion and Conclusions · 0.99
Cites as background 1 paper
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These direct searches have been complemented by studies of the association of LyC production with ultraviolet or optical nebular lines [ref] , the correspondence between Lyman-$α$ and the ($λ$5007 + $λ$4959 )/$λ$3727 line ratio (O$_32$) [ref] , and the link between LyC escape, H$β$ emission, and the rest-frame UV spectral slope [ref] .
Testing an indirect method for identifying galaxies with high levels of Lyman continuum leakage · Introduction · 0.85
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