Galaxies in the Epoch of Reionization Are All Bark and No Bite -- Plenty of Ionizing Photons, Low Escape Fractions

Casey Papovich, Justin W. Cole, Weida Hu, Steven L. Finkelstein, Lu Shen, Pablo Arrabal Haro, Ricardo O. Amorín, Bren Backhaus, Micaela B. Bagley, Rachana Bhatawdekar, Antonello Calabró, Adam C. Carnall, Nikko Cleri, Emanuele Daddi, Mark Dickinson, Norman Grogin, Benne W. Holwerda, Anne E. Jaskot, Anton M. Koekemoer, Mario Llerena, Ray A. Lucas, Sara Mascia, Fabio Pacucci, Laura Pentericci, Pablo G. Pérez-González, Nor Pirzkal, Srinivasan Raghunathan, Lisa-Marie Seillé, Rachel Somerville, L. Y. Aaron Yung

First listed 2025-05-13 | Last updated 2026-01-17

Abstract

Early results from JWST suggest that epoch-of-reionization (EoR) galaxies produce copious ionizing photons, which, if they escape efficiently, could cause reionization to occur too early. We study this problem using \jwst\ imaging and prism spectroscopy for 412 galaxies at 4.5 < z < 9.0. We fit these data simultaneously with stellar-population and nebular-emission models that include a parameter for the fraction of ionizing photons that escape the galaxy, $f_\mathrm{esc}$. We find that the ionization production efficiency, $ξ_\mathrm{ion}$ = Q(H) / L(UV), increases with redshift and decreasing UV luminosity, but shows significant scatter, $σ( \log ξ_\mathrm{ion})$ = 0.3 dex. The inferred escape fractions averaged over the population are low, ranging from $\langle f_\mathrm{esc} \rangle$ = $2.6\pm 1.4$\% at 6 < z < 9 to $6.5\pm 2.2$\% at 4.5 < z < 6 with weak or no indication of evolution with redshift. This implies that in our models most of the ionizing photons need to be absorbed to account for the nebular emission. We compute the impact of our results on reionization, including the distributions for $ξ_\mathrm{ion}$ and $f_\mathrm{esc}$, and the evolution and uncertainty of the UV luminosity function. Considering galaxies brighter than M(UV) < -16 mag, we would produce an IGM hydrogen-ionized fraction of $x_e = 0.5$ at 5.3 < z < 5.8, possibly too late compared to constraints from from QSO sightlines. Including fainter galaxies, M(UV) < -14 mag, we obtain $x_e = 0.5$ at 6.0 < z < 8.1, fully consistent with QSO and CMB data. This implies that EoR galaxies produce plenty of ionizing photons, but these do not efficiently escape. This may be a result of high gas column densities combined with burstier star-formation histories, which limit the time massive stars are able to clear channels through the gas for ionizing photons to escape.

Short digest

Using JWST imaging plus NIRSpec/prism spectra for hundreds of galaxies at 4.5<z<9 from JADES and CEERS, the authors fit joint stellar+nebular SEDs with f_esc as a free parameter to infer both ξ_ion and the ionizing escape fraction. They find ξ_ion rises toward higher redshift and fainter UV luminosity with ~0.3 dex scatter, while the population-averaged escape fractions remain low: ⟨f_esc⟩ ≈ 2.6±1.4% at 6<z<9 and 6.5±2.2% at 4.5<z<6, with little evolution. Propagating these distributions through reionization models yields x_e≈0.5 at z≈5.3–5.8 for M_UV<−16 (possibly late vs. QSO constraints), but consistent timing (x_e≈0.5 at z≈6.0–8.1) once galaxies down to M_UV<−14 are included. Bottom line: EoR galaxies make plenty of ionizing photons, yet low f_esc—likely tied to dense gas and bursty SFHs—keeps most of them trapped.

Key figures to inspect

• Figure 1: Inspect the JADES vs CEERS redshift–magnitude distributions to see how sample weighting differs across 4.5<z<9 and which survey supplies most high‑z, faint systems that drive the ξ_ion trends.
• Figure 2: CEERS SED+prism fits—use the stellar (yellow) and nebular (blue) decompositions to see where Balmer lines and strong nebular continua anchor Q(H) and thus ξ_ion for individual high‑z galaxies.
• Figure 3: JADES counterparts—compare nebular EWs and continuum slopes with CEERS examples to gauge how ξ_ion varies with luminosity and redshift within the joint modeling framework.
• Figure 4: Hβ–vs–Hα derived ξ_ion—check the scatter about unity to verify Hβ is a reliable surrogate when Hα falls outside the spectral range, noting the assumed equal dust attenuation for stars and nebulae.