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Line intensity mapping (LIM) proposes to efficiently observe distant faintgalaxies and map the matter density field at high redshift. Building upon theformalism in the companion paper, we first highlight the degeneracies betweencosmology and astrophysics in LIM. We discuss what can be constrained frommeasurements of the mean intensity and redshift-space power spectra. With asufficient spectral resolution, the large-scale redshift-space distortions ofthe 2-halo term can be measured, helping to break the degeneracy between biasand mean intensity. With a higher spectral resolution, measuring thesmall-scale redshift-space distortions disentangles the 1-halo and shot noiseterms. Cross-correlations with external galaxy catalogs or lensing surveysfurther break degeneracies. We derive requirements for experiments similar toSPHEREx, HETDEX, CDIM, COMAP and CONCERTO. We then revisit the question of theoptimality of the LIM observables, compared to galaxy detection, forastrophysics and cosmology. We use a matched filter to compute the luminositydetection threshold for individual sources. We show that LIM containsinformation about galaxies too faint to detect, in the high-noise orhigh-confusion regimes. We quantify the sparsity and clustering bias of thedetected sources and compare them to LIM, showing in which cases LIM is abetter tracer of the matter density. We extend previous work by answering thesequestions as a function of Fourier scale, including for the first time theeffect of cosmic variance, pixel-to-pixel correlations, luminosity-dependentclustering bias and redshift-space distortions.

Astrophysics & Cosmology from Line Intensity Mapping vs Galaxy Surveys