Dependence of $X_{\mathrm{CO}}$ on metallicity, intensity, and spatial scale in a self-regulated interstellar medium

Abstract

We study the CO(1-0)-to-H${}_2$ conversion factor ($X_{\mathrm{CO}}$) and the line ratio of CO(2-1)-to-CO(1-0) ($R_{21}$) across a wide range of metallicity ($0.1\le Z/Z_{\odot }\le 3$) in high-resolution (~0.2 pc) hydrodynamical simulations of a self-regulated multiphase interstellar medium. We construct synthetic CO emission maps via radiative transfer and systematically vary the "observational" beam size to quantify the scale dependence. We find that the kpc-scale $X_{\mathrm{CO}}$ can be over-estimated at low $Z$ if assuming steady-state chemistry or assuming that the star-forming gas is H${}_2$-dominated. On parsec scales, $X_{\mathrm{CO}}$ varies by orders of magnitude from place to place, primarily driven by the transition from atomic carbon to CO. The pc-scale $X_{\mathrm{CO}}$ drops to the Milky Way value of $2\times 10^{20}\mathrm{c}{\mathrm{m}}^{-2}(\mathrm{K}\mathrm{km}{\mathrm{s}}^{-1}{)}^{-1}$ once dust shielding becomes effective, independent of $Z$. The CO lines become increasingly optically thin at lower $Z$, leading to a higher $R_{21}$. Most cloud area is filled by diffuse gas with high $X_{\mathrm{CO}}$ and low $R_{21}$, while most CO emission originates from dense gas with low $X_{\mathrm{CO}}$ and high $R_{21}$. Adopting a constant $X_{\mathrm{CO}}$ strongly over- (under-)estimates H${}_2$ in dense (diffuse) gas. The line intensity negatively (positively) correlates with $X_{\mathrm{CO}}$ ($R_{21}$) as it is a proxy of column density (volume density). On large scales, $X_{\mathrm{CO}}$ and $R_{21}$ are dictated by beam averaging, and they are naturally biased towards values in dense gas. Our predicted $X_{\mathrm{CO}}$ is a multivariate function of $Z$, line intensity, and beam size, which can be used to more accurately infer the H${}_2$ mass.

Published in ApJ (typos in the abstract fixed). Code for interpolating Lagrangian (particle) data onto an adaptive mesh (and auxiliary scripts for RADMC-3D) available at https://github.com/huchiayu/ParticleGridMapper.jl

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Cited by in corpus (1)

• Evidence for extended gaseous reservoirs around AGN at cosmic noon from ALMA CO(3-2) observations