Speaker
Description
Standard galaxy surveys often fail to detect distant galaxies. Distant sources emit low flux levels due to their extreme distance. Line Intensity Mapping (LIM) addresses this limitation. LIM experiments map spatial fluctuations from all sources, including low-flux galaxies. They further detect redshifted line emission along the line of sight, producing 3D tomographic map of the early Universe. Therefore LIM experiments provide access to previously elusive data at high redshifts. Key targets include the Epoch of Reionization and Cosmic Noon.
However, LIM experiments are currently in the pathfinder stage. They have not yet yielded confirmed detections. This limitation underscores the importance of mock maps. These simulated carbon monoxide (CO) maps are fundamental to statistical cosmology.
Simulated dark matter halos must be populated with line emissions to make mock maps. Therefore, generating accurate mock maps requires precise characterization of the line emission as a function of underlying matter field. Here we present our CO response function model to populate these halos with line luminosities for a given halo properties. These models are in the form of single-variable and multi-variable power-law relations. This presentation discusses the linking between synthetic CO emissions with fundamental galactic properties.
We obtain CO emissions by post-processing FIRE simulations. This step utilizes SKIRT and CLOUDY radiative transfer codes to predict the CO emission from the multi-phase molecular gas. The calculated synthetic line emission is modeled as a function of halo properties to predict CO luminosity. They account for a wide range of halo masses, stellar masses, star formation rates, and metallicities. These models allow us to assign CO(1–0) and CO(2–1) emission to simulated dark matter halos at z=0, 1, 2, and 3. They then allow rapid production of mock maps for COMAP, CCAT, CONCERTO, mmIME, and EXCLAIM in various cosmological settings.
