COLIBRE simulations find the galaxy gas-phase MZR already in place at z≈10 with little evolution until z≈5, then shallowens at low z, with high-mass turnover set by AGN feedback and low-mass end by core-collapse supernovae.
CN and HCN in Dense Interstellar Clouds
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abstract
We present a theoretical investigation of CN and HCN molecule formation in dense interstellar clouds. We study the gas-phase CN and HCN production efficiencies from the outer photon-dominated regions (PDRs) into the opaque cosmic-ray dominated cores. We calculate the equilibrium densities of CN and HCN, and of the associated species C+, C, and CO, as functions of the far-ultraviolet (FUV) optical depth. We consider isothermal gas at 50 K, with hydrogen particle densities from 10^2 to 10^6 cm^-3. We study clouds that are exposed to FUV fields with intensities 20 to 2*10^5 times the mean interstellar FUV intensity. We assume cosmic-ray H2 ionization rates ranging from 5*10^-17 s^-1, to an enhanced value of 5*10^-16 s^-1. We also examine the sensitivity of the density profiles to the gas-phase sulfur abundance.
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The evolution of the galaxy gas-phase mass-metallicity relation from $z=15$ to $z=0$ in the COLIBRE cosmological simulations
COLIBRE simulations find the galaxy gas-phase MZR already in place at z≈10 with little evolution until z≈5, then shallowens at low z, with high-mass turnover set by AGN feedback and low-mass end by core-collapse supernovae.