Backhaus, Bren E.Trump, Jonathan R.Pirzkal, NorBarro, GuillermoFinkelstein, Steven L.Arrabal Haro, PabloSimons, Raymond C.Wessner, JessicaCleri, Nikko J.Bagley, Micaela B.Hirschmann, MichaelaNicholls, David C.Dickinson, MarkKartaltepe, Jeyhan S.Papovich, CaseyKocevski, Dale D.Koekemoer, Anton M.Bisigello, LauraJaskot, Anne E.Lucas, Ray A.Jung, IntaeWilkins, Stephen M.Yung, L. Y. AaronFerguson, Henry C.Fontana, AdrianoGrazian, AndreaGrogin, Norman A.Kewley, Lisa J.Kirkpatrick, AllisonLotz, Jennifer M.Pentericci, LauraPerez-Gonzalez, Pablo G.Ravindranath, SwaraSomerville, Rachel S.Yang, GuangHolwerda, Benne W.Kurczynski, PeterHathi, Nimish P.Rose, CaitlinDavis, Kelcey2024-04-032024-04-032024-04-032024-02-0110.3847/1538-4357/ad1520https://infoscience.epfl.ch/handle/20.500.14299/206830WOS:001173963000001We use James Webb Space Telescope Near-Infrared Camera Wide Field Slitless Spectroscopy (NIRCam WFSS) and the Near-Infrared spectrograph (NIRSpec) in the Cosmic Evolution Early Release survey to measure rest-frame optical emission-line ratios of 155 galaxies at z > 2. The blind NIRCam grism observations include a sample of galaxies with bright emission lines that were not observed on the NIRSpec masks. We study the changes of the H alpha, [O III]/H beta, and [Ne III]/[O II] emission lines in terms of redshift by comparing to lower-redshift SDSS, CLEAR, and MOSDEF samples. We find a significant (>3 sigma) correlation between [O III]/H beta with redshift, while [Ne III]/[O II] has a marginal (2 sigma) correlation with redshift. We compare [O III]/H beta and [Ne III]/[O II] to stellar mass and H beta SFR. We find that both emission-line ratios have a correlation with H beta SFR and an anticorrelation with stellar mass across the redshifts 0 < z < 9. Comparison with MAPPINGS V models indicates that these trends are consistent with lower metallicity and higher ionization in low-mass and high-SFR galaxies. We additionally compare to IllustrisTNG predictions and find that they effectively describe the highest [O III]/H beta ratios observed in our sample, without the need to invoke MAPPINGS models with significant shock ionization components.Physical SciencesEmission Line GalaxiesGalaxy EvolutionGalaxiesActive Galaxiestext::journal::journal article::research article