CECILIA: Ultra-Deep Rest-Optical Spectra of Faint Galaxies at Cosmic Noon

TL;DR

This study presents ultra-deep JWST spectroscopy of faint galaxies at cosmic noon, revealing their low metallicity, low SFR, and ionization properties, providing insights into early galaxy formation and reionization-era analogs.

Contribution

First ultra-deep rest-optical spectra of faint $z\sim2.5$ galaxies, offering new diagnostics of metallicity and ionization in low-mass, low-luminosity systems.

Findings

Low SFRs and dust reddening in faint galaxies.

Low metallicities indicated by emission-line diagnostics.

First constraints on O1-BPT diagram at high redshift.

Abstract

Intrinsically faint galaxies at $z\sim2-3$ offer critical insights into early galaxy formation, tracing low-metallicity, low-mass systems during Cosmic Noon and serving as analogs to reionization-era galaxies. We present ultra-deep JWST/NIRSpec spectroscopy of nine low-luminosity galaxies ($-17 \lesssim M_{\rm UV} \lesssim -20$, $M_\star \lesssim 10^9\,M_\odot$) at $z\sim2.5$ from the CECILIA program, with $\sim$29.5 hr in G235M/F170LP and 1 hr in G395M/F290LP. Our sample includes four LAEs, three rest-UV color-selected galaxies, and two serendipitous detections -- providing the most sensitive rest-optical spectra of individual faint galaxies at this epoch to date. Balmer-line measurements reveal low SFRs ($0.63 < \mathrm{SFR}/(M_\odot\,\mathrm{yr}^{-1}) < 5.43$) and a broad range of dust reddening ($0 < E(B-V) < 1$), with SFRs systematically below those of continuum-selected galaxies. Electron densities are low ($n_e \lesssim 200$cm$^{-3}$), and emission-line diagnostics indicate low [NII]/H$\alpha$, high [OIII]/H$\beta$, suggesting metallicities $12+\log({\rm O/H})\lesssim8.0$. We also present the first O1-BPT constraints in such faint high-redshift galaxies. Notably, two galaxies show low [OIII]/H$\beta$ despite high Ly$\alpha$ EWs and very low [NII]/H$\alpha$, consistent with the predicted turnover in this ratio at very low metallicities -- highlighting the need for complementary diagnostics (e.g., N2, O32) to identify metal-poor systems. Direct $T_e$-based abundances and expanded samples are needed to further trace metallicity and ionization trends in low-mass galaxies.