  The line intensity mapping technique involves measuring the cumulative
emission from specific spectral lines emitted by galaxies and intergalactic
gas. This method provides a way to study the matter distribution and the
evolution of large-scale structures throughout the history of the Universe.
However, modeling intensity mapping from ab-initio approaches can be
challenging due to significant astrophysical uncertainties and noticeable
degeneracies among astrophysical and cosmological parameters. To address these
challenges, we develop a semi-empirical, data-driven framework for galaxy
evolution, which features a minimal set of assumptions and parameters gauged on
observations. By integrating this with stellar evolution and radiative transfer
prescriptions for line emissions, we derive the cosmic [CII] intensity over an
extended redshift range $0 \lesssim z \lesssim 10$. Our approach is quite
general and can be easily applied to other key lines used in intensity mapping
studies, such as [OIII] and the CO ladder. We then evaluate the detectability
of the [CII] power spectra using current and forthcoming observational
facilities. Our findings offer critical insights into the feasibility and
potential contributions of intensity mapping for probing the large-scale
structure of the Universe and understanding galaxy evolution.
