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.
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UNVERDICTED 3representative citing papers
Time-dependent chemistry in 3D MHD simulations leads to H3+ abundances that, when analyzed under steady-state assumptions, imply CRIR values 2-5 times higher than the true input rate, with a median factor of ~3.
First velocity-resolved [O I] 63/145 um maps of the Orion BN/KL outflow show broad components from dense warm postshock gas, with line ratios matching 30-40 km/s dissociative J-shocks illuminated by external UV, yielding [O I] luminosity 86.5 L_sun and mass-loss rate ~9e-3 M_sun/yr.
citing papers explorer
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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.
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The cosmic ray ionization rate from H3+ observations can be overestimated due to neglect of time-dependent chemistry
Time-dependent chemistry in 3D MHD simulations leads to H3+ abundances that, when analyzed under steady-state assumptions, imply CRIR values 2-5 times higher than the true input rate, with a median factor of ~3.
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Velocity-resolved [O I] 63,145 um, [C II] 158 um, and OH mapping along the Orion BN/KL explosive outflow and irradiated shocks
First velocity-resolved [O I] 63/145 um maps of the Orion BN/KL outflow show broad components from dense warm postshock gas, with line ratios matching 30-40 km/s dissociative J-shocks illuminated by external UV, yielding [O I] luminosity 86.5 L_sun and mass-loss rate ~9e-3 M_sun/yr.