Influence of CO versus CH_4 on organic haze formation in atmospheres of diverse terrestrial exoplanets

Terrestrial exoplanets are expected to host secondary, high-metallicity atmospheres derived from the outgassing of volatiles such as N_2, CO_2, H_2O, CH_4, and CO. Photochemical organic hazes are likely to form in such environments, significantly impacting both atmospheric observation and planetary habitability. This study aims to investigate haze formation across representative terrestrial exoplanet atmospheres and assess how CH_4 versus CO as the primary carbon source differentially affects haze production rates, particle properties, and chemical complexity. We conducted six laboratory simulations by exposing the initial gas mixture (a few millibars) to glow discharge at 300 K. Each simulated atmosphere comprises 75% of N_2, CO_2, or H_2O, 10% of each of the other two gases, and 5% of CH_4 or CO. We analyzed the gas-phase products using a residual gas analyzer. For solid products, we measured production rates and particle density, determined particle size distributions via atomic force microscopy, identified functional groups using Fourier-transform infrared spectroscopy, and characterized molecular composition with very high-resolution mass spectrometry. Experiments using CH_4 produce a wider diversity of gas-phase species and substantially higher haze yields compared to the corresponding CO-based experiments. CO-derived haze particles exhibit a restricted size range (10--80 nm), whereas CH_4-derived hazes form denser material with complex functional group signatures and thousands of unique molecular formulas. The pattern of the identified molecular formulas indicates molecular growth pathways linked to detected gaseous precursors such as HCN, CH_2O, and C_2H_4. The atmospheric redox state critically controls haze formation in simulated terrestrial exoplanet atmospheres. CH_4 is significantly more effective than CO in initiating organic growth, leading to higher haze production rates and greater chemical complexity. These results provide crucial constraints for exoplanet atmospheric modeling and spectral interpretation, and further support the possibility that reducing atmospheres may facilitate prebiotic organic chemistry relevant to the emergence of life.