Speaker
Description
The opacity of the intergalactic medium does not allow a direct measurement of Lyman continuum (LyC) emission at redshifts exceeding 4.5. Consequently, we are increasingly relying on indirect indicators of LyC emission that are well tested at low and intermediate redshift. In this study, we use several such indirect indicators, based on parameters like UV-beta slope, E(B-V), UV magnitude, and EW([O III]+Hβ) to refine estimation of LyC emission for galaxies in the epoch of reionization. Leveraging on a very large statistical sample comprising over 750 confirmed sources in the epoch of reionization from several spectroscopic JWST surveys, we analyze the statistical contribution of galaxies to cosmic reionization. In addition, combining NIRCAM imaging and spectroscopy we investigate the relationship between predicted fesc fractions and the morphological properties of the sources (such as clumpiness and asymmetry). Our aim is to unveil the mechanisms that favor the escape of Lyman continuum photons, and understand the complex interplay between galaxy structure and Lyman continuum radiation. In particular we investigate if mergers and interactions can play a significant role in the formation of channels through which the LyC radiation can escape, for example by offsetting the neutral gas from the center of the galaxies where the LyC emission production is located as recently found in the local leaker Haro11.
