Multitracer cosmological line intensity mapping mock lightcone simulation

TL;DR

This paper introduces a framework for creating realistic multitracer sub-millimeter line intensity maps from galaxy formation models, highlighting differences from empirical relations and their impact on future LIM survey predictions.

Contribution

The work presents a novel simulation framework for multitracer line intensity maps based on physically grounded galaxy models, improving predictions for future LIM observations.

Findings

Simulated line intensity maps for CII, CO, CI over a 2 deg$^2$ lightcone.

Significant differences in star formation and line emission relations at low halo masses.

Altered key statistics like the power spectrum and intensity PDF due to model differences.

Abstract

Sub-millimeter emission lines are important tracers of the cold gas and ionized environments of galaxies and are the targets for future line intensity mapping surveys. Physics-based simulations that predict multiple emission lines arising from different phases of the interstellar medium are crucial for constraining the global physical conditions of galaxies with upcoming LIM observations. In this work we present a general framework for creating multitracer mock sub-millimeter line intensity maps based on physically grounded galaxy formation and sub-mm line emission models. We simulate a mock lightcone of 2 deg$^2$ over a redshift range $0\leq z\leq10$, comprising discrete galaxies and galaxy CII, CO, CI emission. We present simulated line intensity maps for two fiducial surveys with resolution and observational frequency windows representative of COMAP and EXCLAIM. We show that the star formation rate and line emission scaling relations predicted by our simulation significantly differ at low halo masses from widely used empirical relations, which are often calibrated to observations of luminous galaxies at lower redshifts. We show that these differences lead to significant changes in key summary statistics used in intensity mapping, such as the one point intensity probability density function and the power spectrum. It will be critical to use more realistic and complex models to forecast the ability of future line intensity mapping surveys to measure observables such as the cosmic star formation rate density.