UV slopes of Starforming Galaxies in Strong Lensing fields at the Epoch of Reionization with JWST

Giordano Felicioni; Maruša Bradač; Yoshihisa Asada; Nicholas S. Martis; Ghassan T. E. Sarrouh; Guillaume Desprez; Gregor Rihtaršič; Naadiyah Jagga; Anishya Harshan; Jon Judež; Chris J. Willott; Roberto Abraham; Gabriel Brammer; Vince Estrada-Carpenter; Jasleen Matharu; Adam Muzzin; Gaël Noirot; Marcin Sawicki; Sunna Withers; Vladan Markov; Rosa M. Mérida; Vesna Pirc Jevšenak; Roberta Tripodi

paper

UV slopes of Starforming Galaxies in Strong Lensing fields at the Epoch of Reionization with JWST

arXiv:2602.17499

Abstract

UV slopes ( $β$ ) are a powerful diagnostics for galaxies at the Epoch of Reionization, tracing star formation, ISM ionization, and the escape fraction $f_{esc}$ of ionizing photons. Studies at low and intermediate z find a gradual $β$ reddening with time and steeper slopes for fainter galaxies, however recent JWST studies reveal a flattening of this trend at $z > 7$ . We want measure $β$ for galaxies at $z > 7.5$ using the strong lensing around massive galaxy clusters to observe high-redshift and faint galaxies. The low-brightness regime is of particular interest for reionization, as most of the recent models of this process posit that numerous faint galaxies are the prime drivers of reionization. We use NIRCam and NIRSpec data from CANUCS, Technicolor, JUMPS, Silver Bullet, UNCOVER and MEGASCIENCE across 7 strong lensing fields. We find galaxies down to $M_{U V} \sim - 16$ and 7.5<z<12.5. We measure \b{eta} with a forward-modelling procedure and estimate $f_{esc}$ for a subsample with emission line data using a relation, calibrated from a low-z sample, with UV slope, galaxy size and H $β$ equivalent width. We find 378 galaxies (45 with spectrum), yielding average values $β = - 2.3 \pm 0.4$ , $z = 8.5 \pm 1.0$ , and $M_{U V} = - 18 \pm 1$ . We find no significant $β$ evolution across our redshift range, suggesting a flattening of the $β - z$ trend above $z \sim 7.5$ . We find a weak negative trend between $β$ and $M_{U V}$ . For 14 galaxies we estimate an average $f_{esc} = 0.26 \pm 0.22$ . The flat trend of $β$ at $z > 7.5$ suggests similar properties between $300$ and $600 M y r$ after the Big Bang. The weak trend between $β$ and $M_{U V}$ suggests an analogous composition for low- and high-mass galaxies' ISM, likely due to a lack of time for dust buildup. While average $f_{esc}$ is higher than necessary to ionize the IGM by z~6, the model extrapolated at low-z may overestimate its value.

9 pages, 6 figures, 2 tables, submitted to A&A