| Abstract: | Line Intensity Mapping (LIM) with ongoing and upcoming radio and far infrared experiments, e.g. SKA, CONCERTO, COMAP, etc., is an emerging technique for probing the universe's large-scale structure using the integrated flux of a particular line emission from sources within a patch of the sky without resolving them. Mapping different line emissions from galaxies/IGM viz. [HI]21-cm, [CII]158 𝜇m, and CO rotational lines can reveal complementary information about the bias with which the line emitters trace the underlying matter distribution and how different astrophysical phenomena affect the clustering pattern of these signals. In this work, we carry out percolation analysis on simulated intensity maps of the 21-cm, CII, and CO(1-0) lines in the post-epoch of reionisation universe (epoch of galaxy assembly; z~3) to investigate the connectivity of structures. At this stage, large-scale matter distribution forms the so-called ‘cosmic web’ composed of voids, filaments, sheets, and volume-filling clusters (nodes). We probe the relative abundances of these structural elements using a quantity called local dimension (D) that takes values close to 1, 2, and 3 for filaments, sheets, and nodes, respectively. Our analysis shows that CII and CO maps exhibit poorer connectivity than the 21-cm maps, which is likely to be an influence of the gas metallicities and reduced star formation rates (SFR) due to quenching. The CII and CO emissions peak in sheet-like environments and have a lower contribution from nodes than the 21-cm emission. This indicates that star formation is quenched preferentially in high-density environments like nodes. |
