INTENSITY MAPPING ACROSS COSMIC TIMES WITH THE Lyα LINE

We present a quantitative model of Ly alpha emission throughout cosmic history and determine the prospects for intensity mapping spatial fluctuations in the Lya signal. Since (1) our model assumes at z > 6 the minimum star formation required to sustain reionization and (2) is based atz < 6 on a luminosity function (LF) extrapolated from the few observed bright Lya emitters, this should be considered a lower limit. Mapping the line emission allows probes of reionization, star formation, and large-scale structure (LSS) as a function of redshift. While Lya emission during reionization has been studied, we also predict the postreionization signal to test predictions of the intensity and motivate future intensity mapping probes of reionization. We include emission from massive dark matter halos and the intergalactic medium (IGM) in our model. We find agreement with current, measured LFs of Lya emitters at z < 8. However, diffuse IGM emission, not associated with Lya emitters, dominates the intensity up to z similar to 10. While our model is applicable for deep-optical or near-infrared observers like the James Webb Space Telescope, only intensity mapping will detect the diffuse IGM emission. We also construct a three-dimensional power spectrum model of the Lya emission. Finally, we consider the prospects of an intensity mapper for measuring Lya fluctuations while identifying interloper contamination for removal. Our results suggest that while the reionization signal is challenging, Lya fluctuations can be an interesting new probe of LSS at late times when used in conjunction with other lines, e.g., Ha, to monitor low-redshift foreground confusion.