The ionizing photon production efficiency of star-forming galaxies at $z\sim 4-10$

Abstract

Investigating the ionizing emission of star-forming galaxies is critical to understanding their contribution to reionization and their impact on the surrounding environment. The number of ionizing photons available to reionize the intergalactic medium (IGM) depends not only on the abundance of galaxies but also on their efficiency in producing ionizing photons (${\xi }_{ion}$). We aim to estimate the ${\xi }_{ion}$ using Balmer lines in a sample of 761 galaxies at $4\le z\le 10$ selected from different JWST surveys. We used the available HST and JWST photometry to perform a SED fitting in the sample to determine their physical properties. We used the BAGPIPES code and assumed a delayed exponential model for the star formation history. We used the NIRSpec spectra from prism or grating configurations to estimate Balmer luminosities and then constrained ${\xi }_{ion}$ values after dust correction. We find a mean value of 10${}^{25.22}$Hz erg${}^{-1}$ for ${\xi }_{ion}$ in the sample with an observed scatter of 0.42dex. We find an increase in the median values of ${\xi }_{ion}$ which confirms the redshift evolution of ${\xi }_{ion}$ found in other works. Regarding the relation with physical properties, we find a decrease of ${\xi }_{ion}$ with increasing stellar mass, indicating that low-mass galaxies are efficient producers of ionizing photons. We also find an increase of ${\xi }_{ion}$ with increasing specific star formation rate (sSFR) and increasing UV absolute magnitude, which indicates that faint galaxies and with high sSFR are also efficient producers. We also investigated the relation of ${\xi }_{ion}$ with the EW([OIII]$\lambda$5007) and find that galaxies with the higher EW([OIII]) are the more efficient producers of ionizing photons. Similarly, we find that galaxies with higher O32 ratios and lower gas-phase metallicities (based on the R23 calibration) show higher ${\xi }_{ion}$ values.

Accepted for publication in A&A

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