Event

In the last few decades, statistical analysis of cosmic microwave background (CMB) temperature fluctuations has established the standard model of cosmology with high precision. The next frontier lies in measuring the spectral shape of the CMB and other molecular and atomic line emissions from galaxies. Line intensity mapping (LIM) has emerged as a powerful tool in astrophysics, leveraging statistical analysis of integrated spectral line emissions originating from distant star-forming galaxies. In this seminar, I will provide a basic overview of the origin of molecular and atomic lines and discuss how current and future LIM experiments are poised to measure the intensities of these lines. Additionally, I will illustrate several cross-correlation techniques between the LIM signal, galaxy surveys, and the 21 cm signal, which probe the physical properties of late-time structure formation and galaxy evolution. Finally, I will highlight our recent results on the detection of CO(3-2) molecular emission from galaxies at z~0.5, achieved by stacking galaxies from the Sloan Digital Sky Survey (SDSS) onto CO maps generated from Planck data.