Constraining the halo-ISM connection through multi-transition carbon monoxide line-intensity mapping

Abstract

Line-intensity mapping (LIM) surveys will characterise the cosmological large-scale structure of emissivity in a range of atomic and molecular spectral lines, but existing literature rarely considers whether these surveys can recover excitation properties of the tracer gas species, such as the carbon monoxide (CO) molecule. Combining basic empirical and physical assumptions with the off-the-shelf Radex radiative transfer code or a Gaussian process emulator of Radex outputs, we devise a basic dark matter halo model for CO emission by tying bulk CO properties to halo properties, exposing physical variables governing CO excitation as free parameters. The CO Mapping Array Project (COMAP) is working towards a multi-band survey programme to observe both CO(1-0) and CO(2-1) at $z\sim 7$. We show that this programme, as well as a further 'Triple Deluxe' extension to higher frequencies covering CO(3-2), is fundamentally capable of successfully recovering the connection between halo mass and CO abundances, and constraining the molecular gas kinetic temperature and density within the star-forming interstellar medium in ways that single-transition CO LIM cannot. Given a fiducial thermal pressure of $\sim 10^4$ K cm${}^{-3}$ for molecular gas in halos of $\sim 10^{10}{M}_{\odot }$, simulated multi-band COMAP surveys successfully recover the thermal pressure within 68% interval half-widths of 0.5--0.6 dex. Construction of multi-frequency LIM instrumentation to access multiple CO transitions is crucial in harnessing this capability, as part of a cosmic statistical probe of gas metallicity, dust chemistry, and other physical parameters in star-forming regions of the first galaxies and proto-galaxies out of reionisation.

arXiv comment27 pages + appendices and bibliography (41 pages total including title page); 13 figures, 6 tables; accepted for publication in JCAP; v2 adds an appendix on model variations and halo-to-halo scatter

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